Initial commit

1004 files changed, 140148 insertions, 0 deletions

diff --git a/noao/imred/Revisions b/noao/imred/Revisions
new file mode 100644
index 00000000..2d7bdc46
--- /dev/null
+++ b/noao/imred/Revisions
@@ -0,0 +1,237 @@
+.help revisions Jun88 noao.imred
+.nf
+
+imred$src/doecslit/apslitproc.par
+imred$src/dofoe/apscript.par
+imred$src/doslit/apslitproc.par
+imred$src/fibers/apscript.par
+imred$src/fibers/params.par
+    Changed the default maxsep from 1000 to 100000.  Unless users reset
+    the default their expectation is that marking apertures will not
+    skip an aperture number no matter how far apart the aperturers are.
+    (2/17/09, Valdes)
+
+imred$src/fibers/skysub.cl
+imred$src/fibers/skysub.par
+    Added sum as an enumerated "combine" choice.  (8/11/08, Valdes)
+
+=======
+V2.14.1
+=======
+
+imred$irs/dispcor.par
+imred$iids/dispcor.par
+    Changed "Conserve flux" to "Conserve total flux" per user request.
+    (6/13/08)
+
+=====
+V2.12
+=====
+
+imred$quadred/	+
+imred$imred.cl
+imred$imred.par
+imred$imred.hd
+imred$imred.men
+imred$mkpkg
+    Added new package QUADRED.  (8/24/01, Valdes)
+
+imred$crutil/	+
+imred$imred.cl
+imred$imred.par
+imred$imred.hd
+imred$imred.men
+imred$mkpkg
+    Added new package CRUTIL.  (8/22/01, Valdes)
+
+imred$argus/argus.cl
+imred$argus/hydra.cl
+imred$argus/echelle.cl
+imred$argus/kpnocoude.cl
+imred$argus/specred.cl
+    Increased the minimum min_lenuserarea from 40000 to 100000.
+    (7/31/96, Valdes)
+
+imred$hydra/demos/xgdonessie.dat
+    Fixed playback.  (7/26/94, Valdes)
+
+imred$argus/argus.cl
+imred$argus/argus.men
+imred$ctioslit/ctioslit.cl
+imred$ctioslit/ctioslit.men
+imred$echelle/echelle.cl
+imred$echelle/echelle.men
+imred$hydra/hydra.cl
+imred$hydra/hydra.men
+imred$iids/iids.cl
+imred$iids/iids.men
+imred$irs/irs.cl
+imred$irs/irs.men
+imred$kpnocoude/kpnocoude.cl
+imred$kpnocoude/kpnocoude.men
+imred$kpnoslit/kpnoslit.cl
+imred$kpnoslit/kpnoslit.men
+imred$specred/specred.cl
+imred$specred/specred.men
+    Added new SFLIP task to packages.  (7/18/94, Valdes)
+
+imred$doc/demos.hlp
+    Added noao.twodspec.longslit to the packages with demos.  (7/24/92, Valdes)
+
+=======
+V2.10.0
+=======
+
+imred$imred.cl
+imred$imred.men
+imred$<spectroscopy packages>
+    Removed the SETAIRMASS task definition from IMRED and added it to
+    all the spectroscopy packages.  Also added the new SETJD task to
+    the spectroscopy packages.  (1/29/92, Valdes)
+
+imred$imred.cl
+imred$imred.men
+imred$imred.hd
+imred$ctioslit/* +
+imred$kpnocoude/* +
+imred$kpnoslit/* +
+imred$msred --> imred$specred
+imred$kpcoude/* -
+imred$foe/* -
+imred$echelle/*
+imred$src/slits/*
+    Reorganized the slit reductions packages and merged the fiber and
+    slit processing tasks into the kpnocoude package and the
+    echelle slit and FOE tasks in the echelle package.  (1/15/92, Valdes)
+
+imred$imred.cl
+imred$imred.men
+imred$imred.hd
+imred$nessie/* -
+imred$hydra/* +
+    Changed package from NESSIE to HYDRA.  (7/26/91, Valdes)
+
+imred$imred.cl
+imred$imred.men
+imred$imred.hd
+imred$foe/*
+    Added new package for Fiber Optic Echelle reductions.
+    (3/22/91, Valdes)
+
+imred$echelle
+imred$src/ecslits/*
+    Added new echelle slit reduction scripts and documentation.
+    (3/22/91, Valdes)
+
+imred$argus
+imred$echelle
+imred$goldcam
+imred$msred
+imred$nessie
+imred$specred
+imred$src
+    Miscellaneous minor updates.  (3/22/91, Valdes)
+
+imred$imred.cl
+imred$imred.men
+imred$imred.hd
+imred$observatory.par -
+imred$observatory.cl -
+    Removed observatory from here and replaced it with a new version in
+    noao.  (11/6/90, Valdes)
+
+imred$imred.cl
+    1.  Changed logical directory bias to biasdir to avoid incorrect
+	interpretation of the command:
+		cl> imrename foo bias
+	to be a move to the logical directory.  Bias is a likely name to
+	be used in CCDRED which will always have bias defined.
+	(10/2/90, Valdes)
+      
+imred$doc +
+imred$imred.hd
+imred$observatory.hlp -> noao$imred/doc
+imred$tutorial.hlp -> noao$imred/doc
+imred$demos.hlp +
+    1. Created doc directory and moved above help to it.
+    2. The help for the demos task which appear in a number of packages was
+	added to the IMRED help for lack of a more obvious place to put it.
+	(9/20/90, Valdes)
+
+imred$argus +
+imred$goldcam +
+imred$kpcoude +
+imred$nessie +
+imred$specred +
+imred$specphot -
+imred$coude -
+imred$echelle
+imred$msred
+imred$iids
+imred$irs
+imred$mkpkg
+imred$imred.cl
+imred$imred.men
+imred$imred.hd
+imred$imred.par
+    A major update of the IMRED spectroscopy packages was made.  New packages
+    were added, one was removed, COUDE was renamed to KPCOUDE, new versions
+    of ECHELLE and MSRED based on major changes to APEXTRACT and ONEDSPEC
+    were installed, and minor changes made.
+    (8-9/90, Valdes)
+
+imred$irred
+    Valdes, June 2, 1989
+    Added the SETAIRMASS task.
+
+imred$irred
+    Davis, April 1, 1989
+    1. Installed the IRRED package. At present this is simply a collection
+    of tasks useful for IR observers.
+
+imred$cryomap -
+noao$mkpkg
+noao$imred.cl
+noao$imred.men
+noao$imred.hd
+    Valdes, February 27, 1987
+    1.  The CRYOMAP (Cryogenic Camera Multi-Aperture Plate) package was
+	archived (Tape 2977 - J. Barnes) and removed.  It was never used
+	and data has not been taken with this system in many years.  The
+	APEXTRACT pacakge is better anyway.  The MULTISPEC package remains.
+    2.  The IMRED package was modified to delete the CRYOMAP package.
+
+imred$dtoi
+    Hammond, February 13. 1987
+    1. Installed the DTOI package
+
+imred$observatory.cl
+    Valdes, October 6, 1986
+    1.  The OBSERVATORY task now calls EPARAM to edit the parameters.
+    2.  The help page was modified.
+
+imred$specphot/* +
+    Valdes/Barnes, October 6, 1986
+    1.  New IMRED package called SPECPHOT added.  The focus of the package
+	is extraction of 1D spectra from 2D detectors and spectrophotometric
+	reduction of the spectra.
+      
+imred$tutor.cl +
+imred$tutor.hlp +
+imred$imred.cl
+imred$imred.men
+imred$imred.hd
+    Valdes, August 18, 1986:
+    1. Added experimental online TUTOR task.
+
+====================================
+Version 2.3 Release, August 18, 1986
+====================================
+
+imred$imred.cl:  Valdes, April 30, 1986
+    1.  Removed the commands to load plot and images since this is now
+	done when the NOAO package is loaded.
+
+imred$observatory.cl:  Valdes, April 7, 1986
+    1.  Task OBSERVATORY added to contain observatory parameters.
+.endhelp
diff --git a/noao/imred/argus/Revisions b/noao/imred/argus/Revisions
new file mode 100644
index 00000000..55828da5
--- /dev/null
+++ b/noao/imred/argus/Revisions
@@ -0,0 +1,60 @@
+.help revisions Jul91 noao.imred.argus
+.nf
+imred$argus/doc/doargus.hlp
+    Fixed minor formating problem.  (4/22/99, Valdes)
+
+imred$argus/doc/dohdydra.hlp
+imred$argus/doc/dohdydra.ms
+    Updated for change where if both crval and cdelt are INDEF then the
+    automatic identification is not done.  (5/2/96, Valdes)
+
+imred$argus/demos/mkdoargus.cl
+    Made the ARTDATA package parameters explicit (4/15/97, Valdes)
+
+imred$argus/argus.cl
+    Increased the minimum min_lenuserarea from 40000 to 100000.
+    (7/31/96, Valdes)
+
+imred$argus/doargus.cl
+imred$argus/doargus.par
+imred$argus/params.par
+imred$argus/doc/doargus.hlp
+imred$argus/doc/doargus.ms
+    Added crval/cdelt parameters used in new version with automatic arc
+    line identification.  (4/5/96, Valdes)
+
+imred$argus/doc/doargus.hlp
+imred$argus/doc/doargus.ms
+    Describes the new header option for the aperture identification table.
+    (7/25/95, Valdes)
+
+imred$argus/argus.cl
+imred$argus/doargus.cl
+imred$argus/doargus.par
+imred$argus/doc/doargus.hlp
+imred$argus/doc/doargus.ms
+imred$argus/demos/xgdoargus.dat
+    Added sky alignment option.  (7/19/95, Valdes)
+
+imred$argus/argus.cl
+imred$argus/argus.men
+    Added APSCATTER to the package.  (6/30/95, Valdes)
+
+=======
+V2.10.4
+=======
+
+imred$argus/argus.cl
+    Renamed the fiber response task to fibresponse. (12/31/94, Valdes)
+
+imred$argus/argus.cl
+    The task was incorrectly defined as being in the logical directory
+    msred instead of specred.  (8/24/92, Valdes)
+
+=======
+V2.10.1
+=======
+
+imred/argus/*
+    Installed (7/24/91, Valdes)
+.endhelp
diff --git a/noao/imred/argus/argus.cl b/noao/imred/argus/argus.cl
new file mode 100644
index 00000000..66e8949e
--- /dev/null
+++ b/noao/imred/argus/argus.cl
@@ -0,0 +1,82 @@
+#{ ARGUS package definition
+
+proto		# bscale
+
+s1 = envget ("min_lenuserarea")
+if (s1 == "")
+    reset min_lenuserarea = 100000
+else if (int (s1) < 100000)
+    reset min_lenuserarea = 100000
+
+# Define ARGUS package
+package argus
+
+# Package script tasks
+task	doargus		= "argus$doargus.cl"
+task	params		= "argus$params.par"
+
+# Fiber reduction script tasks
+task	proc		= "srcfibers$proc.cl"
+task	fibresponse	= "srcfibers$fibresponse.cl"
+task	arcrefs		= "srcfibers$arcrefs.cl"
+task	doarcs		= "srcfibers$doarcs.cl"
+task	doalign		= "srcfibers$doalign.cl"
+task	skysub		= "srcfibers$skysub.cl"
+task	batch		= "srcfibers$batch.cl"
+task	listonly	= "srcfibers$listonly.cl"
+task	getspec		= "srcfibers$getspec.cl"
+
+task	msresp1d	= "specred$msresp1d.cl"
+
+# Demos
+set	demos		= "argus$demos/"
+task	demos		= "demos$demos.cl"
+task	mkfibers	= "srcfibers$mkfibers.cl"
+
+# Onedspec tasks
+task	autoidentify,
+	continuum,
+	dispcor,
+	dopcor,
+	identify,
+	refspectra,
+	reidentify,
+	sapertures,
+	sarith,
+	sflip,
+	slist,
+	specplot,
+	specshift,
+	splot		= "onedspec$x_onedspec.e"
+task	scombine	= "onedspec$scombine/x_scombine.e"
+task	aidpars		= "onedspec$aidpars.par"
+task	bplot		= "onedspec$bplot.cl"
+task	scopy		= "onedspec$scopy.cl"
+task	dispcor1	= "onedspec$dispcor1.par"
+
+# Apextract tasks
+task	apall,
+	apedit,
+	apfind,
+	aprecenter,
+	apresize,
+	apscatter,
+	apsum,
+	aptrace		= "apextract$x_apextract.e"
+task	apdefault	= "apextract$apdefault.par"
+task	apparams	= "apextract$apparams.par"
+task	apall1		= "apextract$apall1.par"
+task	apscript	= "srcfibers$x_apextract.e"
+task	apscat1		= "apextract$apscat1.par"
+task	apscat2		= "apextract$apscat2.par"
+
+# Astutil tasks
+task	setairmass,
+	setjd		= "astutil$x_astutil.e"
+
+# Hide tasks from the user
+hidetask apparams, apall1, apscript, apscat1, apscat2, dispcor1, mkfibers
+hidetask params, proc, batch, arcrefs, doarcs, listonly, fibresponse, getspec
+hidetask doalign
+
+clbye()
diff --git a/noao/imred/argus/argus.dat b/noao/imred/argus/argus.dat
new file mode 100644
index 00000000..6caa8ccd
--- /dev/null
+++ b/noao/imred/argus/argus.dat
@@ -0,0 +1,48 @@
+1 1
+2 0
+3 1
+4 0
+5 1
+6 0
+7 1
+8 0
+9 1
+10 0
+11 1
+12 0
+13 1
+14 0
+15 1
+16 0
+17 1
+18 0
+19 1
+20 0
+21 1
+22 0
+23 1
+24 0
+25 1
+26 0
+27 1
+28 0
+29 1
+30 0
+31 1
+32 0
+33 1
+34 0
+35 1
+36 0
+37 1
+38 0
+39 1
+40 0
+41 1
+42 0
+43 1
+44 0
+45 1
+46 0
+47 1
+48 0
diff --git a/noao/imred/argus/argus.hd b/noao/imred/argus/argus.hd
new file mode 100644
index 00000000..a3fb1064
--- /dev/null
+++ b/noao/imred/argus/argus.hd
@@ -0,0 +1,7 @@
+# Help directory for the ARGUS package.
+
+$doc		 = "./doc/"
+
+doargus		hlp=doc$doargus.hlp
+
+revisions	sys=Revisions
diff --git a/noao/imred/argus/argus.men b/noao/imred/argus/argus.men
new file mode 100644
index 00000000..d5769d30
--- /dev/null
+++ b/noao/imred/argus/argus.men
@@ -0,0 +1,32 @@
+          apall - Extract 1D spectra (all parameters in one task)
+      apdefault - Set the default aperture parameters
+         apedit - Edit apertures interactively
+	 apfind - Automatically find spectra and define apertures
+     aprecenter - Recenter apertures
+       apresize - Resize apertures
+      apscatter - Fit and remove scattered light
+          apsum - Extract 1D spectra
+	aptrace - Trace positions of spectra
+
+          bplot - Batch plots of spectra
+      continuum - Fit the continuum in spectra
+        dispcor - Dispersion correct spectra
+	 dopcor - Doppler correct spectra
+       identify - Identify features in spectrum for dispersion solution
+       msresp1d - Create 1D response spectra from flat field and sky spectra
+     refspectra - Assign wavelength reference spectra to other spectra
+     reidentify - Automatically identify features in spectra
+     sapertures - Set or change aperture header information
+	 sarith - Spectrum arithmetic
+       scombine - Combine spectra having different wavelength ranges
+          scopy - Select and copy apertures in different spectral formats
+     setairmass - Compute effective airmass and middle UT for an exposure
+          setjd - Compute and set Julian dates in images
+	  sflip - Flip data and/or dispersion coordinates in spectra
+          slist - List spectrum header parameters
+       specplot - Stack and plot multiple spectra
+      specshift - Shift spectral dispersion coordinate systems
+          splot - Preliminary spectral plot/analysis
+
+        doargus - Process ARGUS spectra
+	  demos - Demonstrations and tests
diff --git a/noao/imred/argus/argus.par b/noao/imred/argus/argus.par
new file mode 100644
index 00000000..c2c381a5
--- /dev/null
+++ b/noao/imred/argus/argus.par
@@ -0,0 +1,13 @@
+# ARGUS parameter file
+observatory,s,h,"observatory",,,Observatory of data
+interp,s,h,"poly5","nearest|linear|poly3|poly5|spline3|sinc",,Interpolation type
+dispaxis,i,h,2,1,3,Image axis for 2D/3D images
+nsum,s,h,"1",,,"Number of lines/columns/bands to sum for 2D/3D images
+"
+database,f,h,"database",,,Database
+verbose,b,h,no,,,Verbose output?
+logfile,s,h,"logfile",,,Log file
+plotfile,s,h,"",,,"Plot file
+"
+records,s,h,""
+version,s,h,"ARGUS V1: January 1992"
diff --git a/noao/imred/argus/demos/demos.cl b/noao/imred/argus/demos/demos.cl
new file mode 100644
index 00000000..5b065c51
--- /dev/null
+++ b/noao/imred/argus/demos/demos.cl
@@ -0,0 +1,18 @@
+# DEMOS -- Run specified demo provided a demo file exists.
+
+procedure demos (demoname)
+
+file	demoname	{prompt="Demo name"}
+
+begin
+	file	demo, demofile
+
+	if ($nargs == 0 && mode != "h")
+	    type ("demos$demos.men")
+	demo = demoname
+	demofile = "demos$" // demo // ".cl"
+	if (access (demofile))
+	    cl (< demofile)
+	else
+	    error (1, "Unknown demo " // demo)
+end
diff --git a/noao/imred/argus/demos/demos.men b/noao/imred/argus/demos/demos.men
new file mode 100644
index 00000000..ee467bdf
--- /dev/null
+++ b/noao/imred/argus/demos/demos.men
@@ -0,0 +1,4 @@
+	MENU of ARGUS Demonstrations
+
+      doargus - Quick test of DOARGUS (small images, no comments, no delays)
+    mkdoargus - Make DOARGUS test data (12 fibers, 100x256)
diff --git a/noao/imred/argus/demos/demos.par b/noao/imred/argus/demos/demos.par
new file mode 100644
index 00000000..4181ed59
--- /dev/null
+++ b/noao/imred/argus/demos/demos.par
@@ -0,0 +1,2 @@
+demoname,f,a,"",,,"Demo name"
+mode,s,h,"ql",,,
diff --git a/noao/imred/argus/demos/doargus.cl b/noao/imred/argus/demos/doargus.cl
new file mode 100644
index 00000000..51e7f0d9
--- /dev/null
+++ b/noao/imred/argus/demos/doargus.cl
@@ -0,0 +1,13 @@
+# Create demo data if needed.
+
+cl (< "demos$mkdoargus.cl")
+
+delete ("demologfile,demoplotfile", verify=no, >& "dev$null")
+
+unlearn doargus params
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgdoargus.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/argus/demos/header.dat b/noao/imred/argus/demos/header.dat
new file mode 100644
index 00000000..2e104ae7
--- /dev/null
+++ b/noao/imred/argus/demos/header.dat
@@ -0,0 +1,36 @@
+OBJECT  = 'V640Mon 4500      '  /  object name
+OBSERVAT= 'CTIO              '  /  observatory
+OBSERVER= 'Massey            '  /  observers
+COMMENTS= 'Final New Ice     '  /  comments
+EXPTIME =                1200.  /  actual integration time
+DARKTIME=                1200.  /  total elapsed time
+IMAGETYP= 'object            '  /  object, dark, bias, etc.
+DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+UT      = '12:19:55.00       '  /  universal time
+ST      = '09:13:15.00       '  /  sidereal time
+RA      = '06:37:02.00       '  /  right ascension
+DEC     = '06:08:52.00       '  /  declination
+EPOCH   =               1991.9  /  epoch of ra and dec
+ZD      = '44.580            '  /  zenith distance
+TELESCOP= 'kpcdf             '  /  telescope name
+DETECTOR= 'te1k              '  /  detector
+PREFLASH=                    0  /  preflash time, seconds
+GAIN    =                  5.4  /  gain, electrons per adu
+DWELL   =                    5  /  sample integration time
+RDNOISE =                  3.5  /  read noise, electrons per adu
+DELAY0  =                    0  /  time delay after each pixel
+DELAY1  =                    0  /  time delay after each row
+CAMTEMP =                 -111  /  camera temperature
+DEWTEMP =                 -183  /  dewar temperature
+CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+CCDSUM  = '1 1               '  /  on chip summation
+INSTRUME= 'IRAF/ARTDATA      '  /  instrument
+APERTURE= '250micron slit    '  /  aperture
+TVFILT  = '4-96              '  /  tv filter
+DISPAXIS= '2                 '  /  dispersion axis
+GRATPOS =               4624.3  /  grating position
+TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/argus/demos/mkdoargus.cl b/noao/imred/argus/demos/mkdoargus.cl
new file mode 100644
index 00000000..39c94db0
--- /dev/null
+++ b/noao/imred/argus/demos/mkdoargus.cl
@@ -0,0 +1,22 @@
+# Create demo data if needed.
+
+artdata
+artdata.nxc = 5
+artdata.nyc = 5
+artdata.nxsub = 10
+artdata.nysub = 10
+artdata.nxgsub = 5
+artdata.nygsub = 5
+artdata.dynrange = 100000.
+artdata.psfrange = 10.
+artdata.ranbuf = 0
+
+mkfibers ("demoobj", type="object", fibers="demos$mkdoargus.dat",
+    title="Argus artificial image", header="demos$header.dat",
+    ncols=100, nlines=256, wstart=5786., wend=7362., seed=1)
+mkfibers ("demoflat", type="flat", fibers="demos$mkdoargus.dat",
+    title="Argus artificial image", header="demos$header.dat",
+    ncols=100, nlines=256, wstart=5786., wend=7362., seed=2)
+mkfibers ("demoarc", type="henear", fibers="demos$mkdoargus.dat",
+    title="Argus artificial image", header="demos$header.dat",
+    ncols=100, nlines=256, wstart=5786., wend=7362., seed=3)
diff --git a/noao/imred/argus/demos/mkdoargus.dat b/noao/imred/argus/demos/mkdoargus.dat
new file mode 100644
index 00000000..8f9311c0
--- /dev/null
+++ b/noao/imred/argus/demos/mkdoargus.dat
@@ -0,0 +1,13 @@
+ 1 1 1.096679 gauss 2.7 0 86.801 0.002
+ 2 0 1.164292 gauss 2.7 0 81.093 0.002
+ 3 1 0.457727 gauss 2.7 0 74.824 0.002
+ 4 0 1.269284 gauss 2.7 0 68.719 0.002
+ 5 1 1.309297 gauss 2.7 0 62.536 0.002
+ 7 1 1.283618 gauss 2.7 0 50.218 0.002
+ 8 0 0.687173 gauss 2.7 0 43.963 0.002
+ 9 1 1.175850 gauss 2.7 0 38.0091 0.002
+10 0 0.757532 gauss 2.7 0 31.9606 0.002
+11 1 0.939866 gauss 2.7 0 25.1000 0.002
+12 0 1.015546 gauss 2.7 0 19.5097 0.002
+13 1 0.372036 gauss 2.7 0 13.5889 0.002
+14 0 1.065080 gauss 2.7 0 07.4535 0.002
diff --git a/noao/imred/argus/demos/xgdoargus.dat b/noao/imred/argus/demos/xgdoargus.dat
new file mode 100644
index 00000000..e3fb9dfd
--- /dev/null
+++ b/noao/imred/argus/demos/xgdoargus.dat
@@ -0,0 +1,76 @@
+\O=NOAO/IRAF IRAFX valdes@puppis Mon 14:58:37 15-Nov-93
+\T=xgterm
+\G=xgterm
+epar\sargus\n
+\r
+\r
+\r
+\r
+\r
+y\r
+demologfile\r
+demoplotfile\r
+^Z
+epar\sdoargus\n
+demoobj\r
+demoflat\r
+demoflat\r
+\r
+demoarc\r
+\r
+\r
+rdnoise\r
+gain\r
+\r
+13\r
+4\r
+5\r
+7\r
+\r
+6600\r
+6.1\r
+\r
+\r
+\r
+\r
+\r
+\r
+n\r
+\r
+\r
+\r
+\r
+\r
+y\r
+^Z
+doargus\sredo+\n
+\n
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\r
+j/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+n\n
+y\n
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\n
+n\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\n
+\n
+\n
+#/<-5\s\s\s\s/=(.\s=\r 3\r
+#/<-5\s\s\s\s/=(.\s=\r 14\r
+q/<-5\s\s\s\s/=(.\s=\r
diff --git a/noao/imred/argus/doargus.cl b/noao/imred/argus/doargus.cl
new file mode 100644
index 00000000..a34e61c8
--- /dev/null
+++ b/noao/imred/argus/doargus.cl
@@ -0,0 +1,71 @@
+# DOARGUS -- Process ARGUS spectra from 2D to wavelength calibrated 1D.
+#
+# The task PROC does all of the interactive work and BATCH does the
+# background work.  This procedure is organized this way to minimize the
+# dictionary space when the background task is submitted.
+
+procedure doargus (objects)
+
+string	objects = ""		{prompt="List of object spectra"}
+
+file	apref = ""		{prompt="Aperture reference spectrum"}
+file	flat = ""		{prompt="Flat field spectrum"}
+file	throughput = ""		{prompt="Throughput file or image (optional)"}
+string	arcs1 = ""		{prompt="List of arc spectra"}
+string	arcs2 = ""		{prompt="List of shift arc spectra"}
+file	arctable = ""		{prompt="Arc assignment table (optional)\n"}
+
+string	readnoise = "0."	{prompt="Read out noise sigma (photons)"}
+string	gain = "1."		{prompt="Photon gain (photons/data number)"}
+real	datamax = INDEF		{prompt="Max data value / cosmic ray threshold"}
+int	fibers = 48		{prompt="Number of fibers"}
+real	width = 6.		{prompt="Width of profiles (pixels)"}
+real	minsep = 8.	{prompt="Minimum separation between fibers (pixels)"}
+real	maxsep = 10.	{prompt="Maximum separation between fibers (pixels)"}
+file	apidtable = ""		{prompt="Aperture identifications"}
+string	crval = "INDEF"		{prompt="Approximate central wavelength"}
+string	cdelt = "INDEF"		{prompt="Approximate dispersion"}
+string	objaps = ""		{prompt="Object apertures"}
+string	skyaps = "2x2"		{prompt="Sky apertures"}
+string	objbeams = ""		{prompt="Object beam numbers"}
+string	skybeams = ""		{prompt="Sky beam numbers\n"}
+
+bool	scattered = no		{prompt="Subtract scattered light?"}
+bool	fitflat = yes		{prompt="Fit and ratio flat field spectrum?"}
+bool	clean = yes		{prompt="Detect and replace bad pixels?"}
+bool	dispcor = yes		{prompt="Dispersion correct spectra?"}
+bool	skyalign = no		{prompt="Align sky lines?"}
+bool	skysubtract = yes	{prompt="Subtract sky?"}
+bool	skyedit = yes		{prompt="Edit the sky spectra?"}
+bool	saveskys = yes		{prompt="Save sky spectra?"}
+bool	splot = no		{prompt="Plot the final spectrum?"}
+bool	redo = no		{prompt="Redo operations if previously done?"}
+bool	update = yes		{prompt="Update spectra if cal data changes?"}
+bool	batch = no		{prompt="Extract objects in batch?"}
+bool	listonly = no		{prompt="List steps but don't process?\n"}
+
+pset	params = ""		{prompt="Algorithm parameters"}
+
+begin
+	apscript.readnoise = readnoise
+	apscript.gain = gain
+	apscript.nfind = fibers
+	apscript.width = width
+	apscript.t_width = width
+	apscript.minsep = minsep
+	apscript.maxsep = maxsep
+	apscript.radius = minsep
+	apscript.clean = clean
+	proc.datamax = datamax
+
+	proc (objects, apref, flat, throughput, arcs1, arcs2, "",
+	    arctable, fibers, apidtable, crval, cdelt, objaps, skyaps, "",
+	    objbeams, skybeams, "", scattered, fitflat, no, no, no, no,
+	    clean, dispcor, no, skyalign, skysubtract, skyedit, saveskys,
+	    splot, redo, update, batch, listonly)
+
+	if (proc.dobatch) {
+	    print ("-- Do remaining spectra as a batch job --")
+	    print ("batch&batch") | cl
+	}
+end
diff --git a/noao/imred/argus/doargus.par b/noao/imred/argus/doargus.par
new file mode 100644
index 00000000..fb55934c
--- /dev/null
+++ b/noao/imred/argus/doargus.par
@@ -0,0 +1,39 @@
+objects,s,a,"",,,"List of object spectra"
+apref,f,h,"",,,"Aperture reference spectrum"
+flat,f,h,"",,,"Flat field spectrum"
+throughput,f,h,"",,,"Throughput file or image (optional)"
+arcs1,s,h,"",,,"List of arc spectra"
+arcs2,s,h,"",,,"List of shift arc spectra"
+arctable,f,h,"",,,"Arc assignment table (optional)
+"
+readnoise,s,h,"0.",,,"Read out noise sigma (photons)"
+gain,s,h,"1.",,,"Photon gain (photons/data number)"
+datamax,r,h,INDEF,,,"Max data value / cosmic ray threshold"
+fibers,i,h,48,,,"Number of fibers"
+width,r,h,6.,,,"Width of profiles (pixels)"
+minsep,r,h,8.,,,"Minimum separation between fibers (pixels)"
+maxsep,r,h,10.,,,"Maximum separation between fibers (pixels)"
+apidtable,f,h,"",,,"Aperture identifications"
+crval,s,h,INDEF,,,"Approximate central wavelength"
+cdelt,s,h,INDEF,,,"Approximate dispersion"
+objaps,s,h,"",,,"Object apertures"
+skyaps,s,h,"2x2",,,"Sky apertures"
+objbeams,s,h,"",,,"Object beam numbers"
+skybeams,s,h,"",,,"Sky beam numbers
+"
+scattered,b,h,no,,,"Subtract scattered light?"
+fitflat,b,h,yes,,,"Fit and ratio flat field spectrum?"
+clean,b,h,yes,,,"Detect and replace bad pixels?"
+dispcor,b,h,yes,,,"Dispersion correct spectra?"
+skyalign,b,h,no,,,"Align sky lines?"
+skysubtract,b,h,yes,,,"Subtract sky?"
+skyedit,b,h,yes,,,"Edit the sky spectra?"
+saveskys,b,h,yes,,,"Save sky spectra?"
+splot,b,h,no,,,"Plot the final spectrum?"
+redo,b,h,no,,,"Redo operations if previously done?"
+update,b,h,yes,,,"Update spectra if cal data changes?"
+batch,b,h,no,,,"Extract objects in batch?"
+listonly,b,h,no,,,"List steps but don\'t process?
+"
+params,pset,h,"",,,"Algorithm parameters"
+mode,s,h,"ql",,,
diff --git a/noao/imred/argus/doc/doargus.hlp b/noao/imred/argus/doc/doargus.hlp
new file mode 100644
index 00000000..0ffc4bb6
--- /dev/null
+++ b/noao/imred/argus/doc/doargus.hlp
@@ -0,0 +1,1464 @@
+.help doargus Jul95 noao.imred.argus
+.ih
+NAME
+doargus -- Argus data reduction task
+.ih
+USAGE
+doargus objects
+.ih
+SUMMARY
+The \fBdoargus\fR reduction task is specialized for scattered light
+subtraction, extraction, flat fielding, fiber throughput correction,
+wavelength calibration, and sky subtraction of \fIArgus\fR fiber spectra.
+It is a command language script which collects and combines the functions
+and parameters of many general purpose tasks to provide a single complete
+data reduction path.  The task provides a degree of guidance, automation,
+and record keeping necessary when dealing with the large amount of data
+generated by this multifiber instrument.
+.ih
+PARAMETERS
+.ls objects
+List of object spectra to be processed.  Previously processed spectra are
+ignored unless the \fIredo\fR flag is set or the \fIupdate\fR flag is set and
+dependent calibration data has changed.  Extracted spectra are ignored.
+.le
+.ls apref = ""
+Aperture reference spectrum.  This spectrum is used to define the basic
+extraction apertures and is typically a flat field spectrum.
+.le
+.ls flat = "" (optional)
+Flat field spectrum.  If specified the one dimensional flat field spectra
+are extracted and used to make flat field calibrations.  If a separate
+throughput file or image is not specified the flat field is also used
+for computing a fiber throughput correction.
+.le
+.ls throughput = "" (optional)
+Throughput file or image.  If an image is specified, typically a blank sky
+observation, the total flux through each fiber is used to correct for fiber
+throughput.  If a file consisting of lines with the aperture number and
+relative throughput is specified then the fiber throughput will be
+corrected by those values.  If neither is specified but a flat field image
+is given it is used to compute the throughput.
+.le
+.ls arcs1 = "" (at least one if dispersion correcting)
+List of primary arc spectra.  These spectra are used to define the dispersion
+functions for each fiber apart from a possible zero point correction made
+with secondary shift spectra or arc calibration fibers in the object spectra.
+One fiber from the first spectrum is used to mark lines and set the dispersion
+function interactively and dispersion functions for all other fibers and
+arc spectra are derived from it.
+.le
+.ls arcs2 = "" (optional)
+List of optional shift arc spectra.  Features in these secondary observations
+are used to supply a wavelength zero point shift through the observing
+sequence.  One type of observation is dome lamps containing characteristic
+emission lines.
+.le
+.ls arctable = "" (optional) (refspectra)
+Table defining arc spectra to be assigned to object
+spectra (see \fBrefspectra\fR).  If not specified an assignment based
+on a header parameter, \fIparams.sort\fR, such as the observation time is made.
+.le
+
+.ls readnoise = "0." (apsum)
+Read out noise in photons.  This parameter defines the minimum noise
+sigma.  It is defined in terms of photons (or electrons) and scales
+to the data values through the gain parameter.  A image header keyword
+(case insensitive) may be specified to get the value from the image.
+.le
+.ls gain = "1." (apsum)
+Detector gain or conversion factor between photons/electrons and
+data values.  It is specified as the number of photons per data value.
+A image header keyword (case insensitive) may be specified to get the value
+from the image.
+.le
+.ls datamax = INDEF (apsum.saturation)
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the flat field or arc
+spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.le
+.ls fibers = 48 (apfind)
+Number of fibers.  This number is used during the automatic definition of
+the apertures from the aperture reference spectrum.  It is best if this
+reflects the actual number of fibers which may be found in the aperture
+reference image.  Note that Argus fibers which are unassigned will still
+contain enough light for identification and the aperture identification
+table will be used to eliminate the unassigned fibers.  The interactive
+review of the aperture assignments allows verification and adjustments
+to the automatic aperture definitions.
+.le
+.ls width = 6. (apedit)
+Approximate base full width of the fiber profiles.  This parameter is used
+for the profile centering algorithm.
+.le
+.ls minsep = 8. (apfind)
+Minimum separation between fibers.  Weaker spectra or noise within this
+distance of a stronger spectrum are rejected.
+.le
+.ls maxsep = 10. (apfind)
+Maximum separation between adjacent fibers.  This parameter
+is used to identify missing fibers.  If two adjacent spectra exceed this
+separation then it is assumed that a fiber is missing and the aperture
+identification assignments will be adjusted accordingly.
+.le
+.ls apidtable = "" (apfind)
+Aperture identification table.  This may be either a text file or an
+image.  A text file contains the fiber number, beam number defining object
+(1), sky (0), and arc (2) fibers, and a object title.  An image contains
+the keywords SLFIBnnn with string value consisting of the fiber number,
+beam number, optional right ascension and declination, and an object
+title.  Unassigned and broken fibers (beam of -1)
+should be included in this list since they will automatically be excluded.
+.le
+.ls crval = INDEF, cdelt = INDEF (autoidentify)
+These parameters specify an approximate central wavelength and dispersion.
+They may be specified as numerical values, INDEF, or image header keyword
+names whose values are to be used.
+If both these parameters are INDEF then the automatic identification will
+not be done.
+.le
+.ls objaps = "", skyaps = "2x2"
+List of object and sky aperture numbers.  These are used to identify
+object and sky
+apertures for sky subtraction.  Note sky apertures may be identified as
+both object and sky if one wants to subtract the mean sky from the
+individual sky spectra.  Because the fibers typically alternate
+sky and object the default is to define the sky apertures by their
+aperture numbers and select both object and sky fibers for sky subtraction.
+.le
+.ls objbeams = "", skybeams = ""
+List of object and sky beam numbers.
+The beam numbers are typically the same as the aperture numbers unless
+set in the \fIapidtable\fR.
+.le
+
+.ls scattered = no (apscatter)
+Smooth and subtracted scattered light from the object and flat field
+images.  This operation consists of fitting independent smooth functions
+across the dispersion using data outside the fiber apertures and then
+smoothing the individual fits along the dispersion.  The initial
+flat field, or if none is given the aperture reference image, are
+done interactively to allow setting the fitting parameters.  All
+subsequent subtractions use the same fitting parameters.
+.le
+.ls fitflat = yes (flat1d)
+Fit the composite flat field spectrum by a smooth function and divide each
+flat field spectrum by this function?  This operation removes the average
+spectral signature of the flat field lamp from the sensitivity correction to
+avoid modifying the object fluxes.
+.le
+.ls clean = yes (apsum)
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction and requires reasonably good values
+for the readout noise and gain.  In addition the datamax parameters
+can be useful.
+.le
+.ls dispcor = yes
+Dispersion correct spectra?  Depending on the \fIparams.linearize\fR
+parameter this may either resample the spectra or insert a dispersion
+function in the image header.
+.le
+.ls skyalign = no
+Align sky lines?  If yes then for the first object spectrum you are asked
+to mark one or more sky lines to use for alignment.  Then these lines will
+be found in all spectra and an average zeropoint shift computed and applied
+to the dispersion solution to align these lines.  Note that this assumes
+the sky lines are seen in all fibers.
+.le
+.ls skysubtract = yes
+Subtract sky from the object spectra?  If yes the sky spectra are combined
+and subtracted from the object spectra as defined by the object and sky
+aperture/beam parameters.
+.le
+.ls skyedit = yes
+Overplot all the sky spectra and allow contaminated sky spectra to be
+deleted?
+.le
+.ls saveskys = yes
+Save the combined sky spectrum?  If no then the sky spectrum will be
+deleted after sky subtraction is completed.
+.le
+.ls splot = no
+Plot the final spectra with the task \fBsplot\fR?
+.le
+.ls redo = no
+Redo operations previously done?  If no then previously processed spectra
+in the objects list will not be processed (unless they need to be updated).
+.le
+.ls update = yes
+Update processing of previously processed spectra if aperture, flat
+field, or dispersion reference definitions are changed?
+.le
+.ls batch = no
+Process spectra as a background or batch job provided there are no interactive
+options (\fIskyedit\fR and \fIsplot\fR) selected.
+.le
+.ls listonly = no
+List processing steps but don't process?
+.le
+
+.ls params = "" (pset)
+Name of parameter set containing additional processing parameters.  The
+default is parameter set \fBparams\fR.  The parameter set may be examined
+and modified in the usual ways (typically with "epar params" or ":e params"
+from the parameter editor).  Note that using a different parameter file
+is not allowed.  The parameters are described below.
+.le
+
+.ce
+-- PACKAGE PARAMETERS
+
+Package parameters are those which generally apply to all task in the
+package.  This is also true of \fBdoargus\fR.
+.ls dispaxis = 2
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.  The default value defers to the
+package parameter of the same name.
+.le
+.ls observatory = "observatory"
+Observatory at which the spectra were obtained if not specified in the
+image header by the keyword OBSERVAT.  For Argus data the image headers
+identify the observatory as "kpno" so this parameter is not used.
+For data from other observatories this parameter may be used
+as describe in \fBobservatory\fR.
+.le
+.ls interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc)
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.nf
+	nearest - nearest neighbor
+	 linear - linear
+	  poly3 - 3rd order polynomial
+	  poly5 - 5th order polynomial
+	spline3 - cubic spline
+	   sinc - sinc function
+.fi
+.le
+.ls database = "database"
+Database (directory) used for storing aperture and dispersion information.
+.le
+.ls verbose = no
+Print verbose information available with various tasks.
+.le
+.ls logfile = "logfile", plotfile = ""
+Text and plot log files.  If a filename is not specified then no log is
+kept.  The plot file contains IRAF graphics metacode which may be examined
+in various ways such as with \fBgkimosaic\fR.
+.le
+.ls records = ""
+Dummy parameter to be ignored.
+.le
+.ls version = "ARGUS: ..."
+Version of the package.
+.le
+
+.ce
+PARAMS PARAMETERS
+
+The following parameters are part of the \fBparams\fR parameter set and
+define various algorithm parameters for \fBdoargus\fR.
+
+.ce
+--  GENERAL PARAMETERS --
+.ls line = INDEF, nsum = 10
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, recentering, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.le
+.ls order = "decreasing" (apfind)
+When assigning aperture identifications order the spectra "increasing"
+or "decreasing" with increasing pixel position (left-to-right or
+right-to-left in a cross-section plot of the image).
+.le
+.ls extras = no (apsum)
+Include extra information in the output spectra?  When cleaning or using
+variance weighting the cleaned and weighted spectra are recorded in the
+first 2D plane of a 3D image, the raw, simple sum spectra are recorded in
+the second plane, and the estimated sigmas are recorded in the third plane.
+.le
+
+.ce
+-- DEFAULT APERTURE LIMITS --
+.ls lower = -3., upper = 3. (apdefault)
+Default lower and upper aperture limits relative to the aperture center.
+These limits are used when the apertures are first found and may be
+resized automatically or interactively.
+.le
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+.ls ylevel = 0.05 (apresize)
+Data level at which to set aperture limits during automatic resizing.
+It is a fraction of the peak relative to a local background.
+.le
+
+.ce
+-- TRACE PARAMETERS --
+.ls t_step = 10 (aptrace)
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \fInsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.le
+.ls t_function = "spline3", t_order = 3 (aptrace)
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.le
+.ls t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+Default number of rejection iterations and rejection sigma thresholds.
+.le
+
+.ce
+-- SCATTERED LIGHT PARAMETERS --
+.ls buffer = 1. (apscatter)
+Buffer distance from the aperture edges to be excluded in selecting the
+scattered light pixels to be used.
+.le
+.ls apscat1 = "" (apscatter)
+Fitting parameters across the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat1"
+parameter set.
+.le
+.ls apscat2 = "" (apscatter)
+Fitting parameters along the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat2"
+parameter set.
+.le
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+.ls weights = "none" (apsum)
+Type of extraction weighting.  Note that if the \fIclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+.ls "none"
+The pixels are summed without weights except for partial pixels at the
+ends.
+.le
+.ls "variance"
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \fIgain\fR and \fIreadnoise\fR
+parameters.
+.le
+.le
+.ls pfit = "fit1d" (apsum) (fit1d|fit2d)
+Profile fitting algorithm for cleaning and variance weighted extractions.
+The default is generally appropriate for Argus data but users
+may try the other algorithm.  See \fBapprofiles\fR for further information.
+.le
+.ls lsigma = 3., usigma = 3. (apsum)
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.le
+.ls nsubaps = 1 (apsum)
+During extraction it is possible to equally divide the apertures into
+this number of subapertures.
+.le
+
+.ce
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --
+.ls f_interactive = yes (fit1d)
+Fit the composite one dimensional flat field spectrum interactively?
+This is used if \fIfitflat\fR is set and a two dimensional flat field
+spectrum is specified.
+.le
+.ls f_function = "spline3", f_order = 10 (fit1d)
+Function and order used to fit the composite one dimensional flat field
+spectrum.  The functions are "legendre", "chebyshev", "spline1", and
+"spline3".  The spline functions are linear and cubic splines with the
+order specifying the number of pieces.
+.le
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+.ls threshold = 10. (autoidentify/identify/reidentify)
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.le
+.ls coordlist = "linelists$ctiohenear.dat" (autoidentify/identify)
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelists$".
+.le
+.ls match = -3. (autoidentify/identify)
+The maximum difference for a match between the dispersion function prediction
+value and a wavelength in the coordinate list.
+.le
+.ls fwidth = 4. (autoidentify/identify)
+Approximate full base width (in pixels) of arc lines.
+.le
+.ls cradius = 10. (reidentify)
+Radius from previous position to reidentify arc line.
+.le
+.ls i_function = "chebyshev", i_order = 3 (autoidentify/identify)
+The default function and order to be fit to the arc wavelengths as a
+function of the pixel coordinate.  The functions choices are "chebyshev",
+"legendre", "spline1", or "spline3".
+.le
+.ls i_niterate = 2, i_low = 3.0, i_high = 3.0 (autoidentify/identify)
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.le
+.ls refit = yes (reidentify)
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.le
+.ls addfeatures = no (reidentify)
+Add new features from a line list during each reidentification?
+This option can be used to compensate for lost features from the
+reference solution.  Care should be exercised that misidentified features
+are not introduced.
+.le
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+.ls select = "interp" (refspectra)
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+.ls average
+Average two reference spectra without regard to any sort parameter.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.
+This option is used to assign two reference spectra, with equal weights,
+independent of any sorting parameter.
+.le
+.ls following
+Select the nearest following spectrum in the reference list based on the
+sorting parameter.  If there is no following spectrum use the nearest preceding
+spectrum.
+.le
+.ls interp
+Interpolate between the preceding and following spectra in the reference
+list based on the sorting parameter.  If there is no preceding and following
+spectrum use the nearest spectrum.  The interpolation is weighted by the
+relative distances of the sorting parameter.
+.le
+.ls match
+Match each input spectrum with the reference spectrum list in order.
+This overrides the reference aperture check.
+.le
+.ls nearest
+Select the nearest spectrum in the reference list based on the sorting
+parameter.
+.le
+.ls preceding
+Select the nearest preceding spectrum in the reference list based on the
+sorting parameter.  If there is no preceding spectrum use the nearest following
+spectrum.
+.le
+.le
+.ls sort = "jd", group = "ljd" (refspectra)
+Image header keywords to be used as the sorting parameter for selection
+based on order and to group spectra.
+A null string, "", or the word "none" may be use to disable the sorting
+or grouping parameters.
+The sorting parameter
+must be numeric but otherwise may be anything.  The grouping parameter
+may be a string or number and must simply be the same for all spectra within
+the same group (say a single night).
+Common sorting parameters are times or positions.
+In \fBdoargus\fR the Julian date (JD) and the local Julian day number (LJD)
+at the middle of the exposure are automatically computed from the universal
+time at the beginning of the exposure and the exposure time.  Also the
+parameter UTMIDDLE is computed.
+.le
+.ls time = no, timewrap = 17. (refspectra)
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.le
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+.ls linearize = yes (dispcor)
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling
+If no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data are not interpolated.
+.le
+.ls log = no (dispcor)
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.le
+.ls flux = yes (dispcor)
+Conserve the total flux during interpolation?  If \fIno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \fIyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.le
+
+.ce
+-- SKY SUBTRACTION PARAMETERS --
+.ls combine = "average" (scombine) (average|median)
+Option for combining sky pixels at the same dispersion coordinate after any
+rejection operation.  The options are to compute the  "average" or "median"
+of the pixels.  The median uses the average of the two central
+values when the number of pixels is even.
+.le
+.ls reject = "none" (scombine) (none|minmax|avsigclip)
+Type of rejection operation performed on the pixels which overlap at each
+dispersion coordinate.  The algorithms are discussed in the
+help for \fBscombine\fR.  The rejection choices are:
+
+.nf
+      none - No rejection
+    minmax - Reject the low and high pixels
+ avsigclip - Reject pixels using an averaged sigma clipping algorithm
+.fi
+
+.le
+.ls scale = "none" (none|mode|median|mean)
+Multiplicative scaling to be applied to each spectrum.  The choices are none
+or scale by the mode, median, or mean.  This should not be necessary if the
+flat field and throughput corrections have been properly made. 
+.le
+.ih
+ENVIRONMENT PARAMETERS
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
+.ih
+DESCRIPTION
+The \fBdoargus\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, fiber throughput correction, wavelength calibration, and sky
+subtraction of \fIArgus\fR fiber spectra.  It is a
+command language script which collects and combines the functions and
+parameters of many general purpose tasks to provide a single, complete data
+reduction path.  The task provides a degree of guidance, automation, and
+record keeping necessary when dealing with the large amount of data
+generated by these multifiber instruments.
+
+The general organization of the task is to do the interactive setup steps
+first using representative calibration data and then perform the majority
+of the reductions automatically, and possibly as a background process, with
+reference to the setup data.  In addition, the task determines which setup
+and processing operations have been completed in previous executions of the
+task and, contingent on the \fIredo\fR and \fIupdate\fR options, skip or
+repeat some or all the steps.
+
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage for
+Argus since there are many variations possible.  Because \fBdoargus\fR
+combines many separate, general purpose tasks the description given here
+refers to these tasks and leaves some of the details to their help
+documentation.
+
+\fBUsage Outline\fR
+
+.ls 6 [1]
+The images are first processed with \fBccdproc\fR for overscan,
+bias, and dark corrections.
+The \fBdoargus\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+.le
+.ls [2]
+Set the \fBdoargus\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed, the flat field image as the aperture reference and
+the flat field, and one or more arc images.  A throughput file or image,
+such as a blank sky observation, may also be specified.  If there are many
+object or arc spectra per setup you might want to prepare "@ files".
+Prepare and specify the aperture identification table if desired.  If
+the image headers contain the fiber identification information with
+SLFIB keywords then specify an image for the aperture identification table.
+You might wish to verify the geometry parameters,
+separations, dispersion direction, etc., which may change with different
+detector setups.  The processing parameters are set for complete reductions
+but for quicklook you might not use the clean option or dispersion
+calibration and sky subtraction.
+
+The parameters are set for a particular Argus configuration and different
+configurations may use different flat fields, arcs, and aperture
+identification tables.
+.le
+.ls [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the execution and no further queries of that
+type will be made.
+.le
+.ls [4]
+The apertures are defined using the specified aperture reference image.
+The spectra are found automatically and apertures assigned based on
+task parameters and the aperture identification table.  Unassigned
+fibers may have a negative beam number and will be ignored in subsequent
+processing.  The resize option sets the aperture size to the widths of
+the profiles at a fixed fraction of the peak height.  The interactive
+review of the apertures is recommended.  If the identifications are off
+by a shift the 'o' key is used.  To exit the aperture review type 'q'.
+.le
+.ls [5]
+The fiber positions at a series of points along the dispersion are measured
+and a function is fit to these positions.  This may be done interactively to
+adjust the fitting parameters.  Not all fibers need be examined and the "NO"
+response will quit the interactive fitting.  To exit the interactive
+fitting type 'q'.
+.le
+.ls [6]
+If scattered light subtraction is to be done the flat field image is
+used to define the scattered light fitting parameters interactively.
+If one is not specified then the aperture reference image is used for
+this purpose.
+
+There are two queries for the interactive fitting.  A graph of the
+data between the defined reference apertures separated by a specified
+buffer distance is first shown.  The function order and type may be
+adjusted.  After quiting with 'q' the user has the option of changing
+the buffer value and returning to the fitting, changing the image line
+or column to check if the fit parameters are satisfactory at other points,
+or to quit and accept the fit parameters.  After fitting all points
+across the dispersion another graph showing the scattered light from
+the individual fits is shown and the smoothing parameters along the
+dispersion may be adjusted.  Upon quiting with 'q' you have the option
+of checking other cuts parallel to the dispersion or quiting and finishing
+the scattered light function smoothing and subtraction.
+
+If there is a throughput image then this is corrected for scattered light
+noninteractively using the previous fitting parameters.
+.le
+.ls [7]
+If flat fielding is to be done the flat field spectra are extracted.  The
+average spectrum over all fibers is determined and a function is fit
+interactively (exit with 'q').  This function is generally of sufficiently
+high order that the overall shape is well fit.  This function is then used
+to normalize the individual flat field spectra.  If a throughput image, a
+sky flat, is specified then the total sky counts through each fiber are
+used to correct the total flat field counts.  Alternatively, a separately
+derived throughput file can be used for specifying throughput corrections.
+If neither type of throughput is used the flat field also provides the
+throughput correction.  The final response spectra are normalized to a unit
+mean over all fibers.  The relative average throughput for each fiber is
+recorded in the log and possibly printed to the terminal.
+.le
+.ls [8]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  The middle fiber is used to identify the arc lines and define
+the dispersion function using the task \fBautoidentify\fR.  The
+\fIcrval\fR and \fIcdelt\fR parameters are used in the automatic
+identification.  Whether or not the automatic identification is
+successful you will be shown the result of the arc line identification.
+If the automatic identification is not successful identify a few arc
+lines with 'm' and use the 'l' line list identification command to
+automatically add additional lines and fit the dispersion function.  Check
+the quality of the dispersion function fit with 'f'.  When satisfied exit
+with 'q'.
+.le
+.ls [9]
+The remaining fibers are automatically reidentified.  You have the option
+to review the line identifications and dispersion function for each fiber
+and interactively add or delete arc lines and change fitting parameters.
+This can be done selectively, such as when the reported RMS increases
+significantly.
+.le
+.ls [10]
+If the spectra are to be resampled to a linear dispersion system
+(which will be the same for all spectra) default dispersion parameters
+are printed and you are allowed to adjust these as desired.
+.le
+.ls [11]
+If the sky line alignment option is selected and the sky lines have not
+been identified for a particular aperture identification table then you are
+asked to mark one or more sky lines.  You may simply accept the wavelengths
+of these lines as defined by the dispersion solution for this spectrum and
+fiber or you may specify knowns wavelengths for the lines. These lines will
+be reidentified in all object spectra extracted and a mean zeropoint shift
+will be added to the dispersion solution.  This has the effect of aligning
+these lines to optimize sky subtraction.
+.le
+.ls [12]
+The object spectra are now automatically scattered light subtracted,
+ extracted, flat fielded, and dispersion corrected.
+.le
+.ls [13]
+When sky subtracting, the individual sky spectra may be reviewed and some
+spectra eliminated using the 'd' key.  The last deleted spectrum may be
+recovered with the 'e' key.  After exiting the review with 'q' you are
+asked for the combining option.  The type of combining is dictated by the
+number of sky fibers.
+.le
+.ls [14]
+The option to examine the final spectra with \fBsplot\fR may be given.
+To exit type 'q'.
+.le
+.ls [15]
+If scattered light is subtracted from the input data a copy of the
+original image is made by appending "noscat" to the image name.
+If the data are reprocessed with the \fIredo\fR flag the original
+image will be used again to allow modification of the scattered
+light parameters.
+
+The final spectra will have the same name as the original 2D images
+with a ".ms" extension added.  The flat field and arc spectra may
+also have part of the aperture identification table name added, if
+used, to
+allow different configurations to use the same 2D flat field and arcs
+but with different aperture definitions.  If using the sky alignment
+option an image "align" with the aperture identification table name
+applied will also be created.
+.le
+
+\fBSpectra and Data Files\fR
+
+The basic input consists of Argus object and
+calibration spectra stored as IRAF images.
+The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+The raw CCD images must
+be processed to remove overscan, bias, and dark count effects.
+This is generally done using the \fBccdred\fR package.
+The \fBdoargus\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+Flat fielding is
+generally not done at this stage but as part of \fBdoargus\fR.
+If flat fielding is done as part of the basic CCD processing then
+a flattened flat field, blank sky observation, or throughput file
+should still be created for applying fiber throughput corrections.
+
+The task \fBdoargus\fR uses several types of calibration spectra.  These
+are flat fields, blank sky flat fields, comparison lamp spectra, and auxiliary
+mercury line (from the dome lights) or sky line spectra.  The flat field,
+throughput image or file, and auxiliary emission line spectra are optional.
+If a flat field is used then the sky flat
+or throughput file is optional assuming the flat field has the same fiber
+iillumination.  It is legal to specify only a throughput image or file and
+leave the flat field blank in order to simply apply a throughput
+correction.  Because only the total counts through each fiber are used from
+a throughput image, sky flat exposures need not be of high signal per
+pixel.
+
+There are two types of dispersion calibration methods.  One is to take arc
+calibration exposures through all fibers periodically and apply the
+dispersion function derived from one or interpolated between pairs to the
+object fibers.  This is the usual method with Argus.
+A second (uncommon) method is to use \fIauxiliary
+line spectra\fR such as lines in the dome lights or sky lines to monitor
+shifts relative to a few actual arc exposures.  The main reason to do this
+is if taking arc exposures through all fibers is inconvenient.
+
+The assignment of arc or auxiliary line calibration exposures to object
+exposures is generally done by selecting the nearest in time and
+interpolating.  There are other options possible which are described under
+the task \fBrefspectra\fR.  The most general option is to define a table
+giving the object image name and the one or two arc spectra to be assigned
+to that object.  That file is called an \fIarc assignment table\fR and it
+is one of the optional setup files which can used with \fBdoargus\fR.
+
+The first step in the processing is identifying the spectra in the images.
+The default method is to use the fact that object and sky fibers alternate
+and assign sequential numbers to the fibers so that the sky fibers are the
+even aperture numbers and the object fibers are the odd aperture numbers.
+In this case the beam numbers are not used (and are the same as the
+aperture numbers) and there are no object identifications associated with the
+spectra.
+
+A very useful, optional, setup parameter is an \fIaperture identification
+table\fR.  The table contains information about the fiber assignments
+including object titles.  The table is either a text file or an image
+containing the keywords SLFIB.  An aperture identification file contains
+lines consisting of an aperture number, a beam number, and an object
+identification.  In an image the SLFIB keywords contain the aperture
+number, the beam numbers, optional right ascension and declination, and a
+title.  The aperture identification information must be in the same order
+as the fibers in the image.  The aperture number may be any unique number
+but it is recommended that the normal sequential fiber numbers be used.
+The beam number may be used to flag object or sky spectra or simply be the
+same as the aperture number.  The object identifications are optional but
+it is good practice to include them so that the data will contain the
+object information independent of other records.  Figure 1 shows an example
+of a file for a configuration called LMC123.
+
+.nf
+
+    Figure 1: Example Aperture Identification File
+
+    cl> type LMC124
+    1 1 143
+    2 0 sky
+    3 1 121
+       .
+       .
+       .
+    47 1 s92
+    48 0 sky
+
+.fi
+Note the identification of the sky fibers with beam number 0 and the
+object fibers with 1.  Any broken fibers should be included and
+identified by a different beam number, say beam number -1, to give the
+automatic spectrum finding operation the best chance to make the
+correct identifications.  Naturally the identification table will vary
+for each configuration.
+Additional information about the aperture identification
+table may be found in the description of the task \fBapfind\fR.
+
+In more recent Argus data the fiber information is included in the
+image header under the keywords SLFIB.  In this case you don't need
+to prepare a file and simply specify the name of an image, typically
+the same as the aperture reference image, for the aperture identification
+table.
+
+The final reduced spectra are recorded in two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ms" extension.  Each line in the reduced image is a one dimensional
+spectrum with associated aperture, wavelength, and identification
+information.  When the \fIextras\fR parameter is set the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tools such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.  The special task \fBscopy\fR may be used to extract
+specific apertures or to change format to individual one dimensional
+images.
+
+\fBPackage Parameters\fR
+
+The \fBargus\fR package parameters set parameters affecting all the
+tasks in the package.
+The dispersion axis parameter defines the image axis along which the
+dispersion runs.  This is used if the image header doesn't define the
+dispersion axis with the DISPAXIS keyword.
+The observatory parameter is only required
+for data taken with fiber instruments other than Argus.
+The spectrum interpolation type might be changed to "sinc" but
+with the cautions given in \fBonedspec.package\fR.
+The other parameters define the standard I/O functions.
+The verbose parameter selects whether to print everything which goes
+into the log file on the terminal.  It is useful for monitoring
+what the \fBdoargus\fR task does.  The log and plot files are useful for
+keeping a record of the processing.  A log file is highly recommended.
+A plot file provides a record of apertures, traces, and extracted spectra
+but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+
+\fBProcessing Parameters\fR
+
+The list of objects and arcs can be @ files if desired.  The aperture
+reference spectrum is usually the same as the flat field spectrum though it
+could be any exposure with enough signal to accurately define the positions
+and trace the spectra.  The first list of arcs are the standard Th-Ar or
+HeNeAr comparison arc spectra (they must all be of the same type).  The
+second list of arcs are the auxiliary emission line exposures mentioned
+previously.
+
+The detector read out noise and gain are used for cleaning and variance
+(optimal) extraction.
+The dispersion axis defines the wavelength direction of spectra in
+the image if not defined in the image header by the keyword DISPAXIS.  The
+width and separation parameters define the dimensions (in pixels) of the
+spectra (fiber profile) across the dispersion.  The width parameter
+primarily affects the centering.  The maximum separation parameter is
+important if missing spectra are to
+be correctly skipped.  The number of fibers can be left at the default
+and the task will try to account for unassigned or missing fibers.
+However, this may lead to occasional incorrect
+identifications so it is recommended that only the true number of
+fibers be specified.  The aperture identification table was described
+earlier.
+
+The approximate central wavelength and dispersion are used for the
+automatic identification of the arc reference.  They may be specified
+as image header keywords or values.  The INDEF values search the
+entire range of the coordinate reference file but the automatic
+line identification algorithm works much better and faster if
+approximate values are given.
+
+The task needs to know which fibers are object and which are sky
+if sky subtraction is to be done.  One could explicitly
+give the aperture numbers but the recommended way is to use the default
+of selecting every second fiber as sky.  If no list of aperture or beam
+numbers is given
+then all apertures or beam numbers are selected.  Sky subtracted sky
+spectra are useful for evaluating the sky subtraction.  Since only
+the spectra identified as objects are sky subtracted one can exclude
+fibers from the sky subtraction.  For example, to eliminate the sky
+spectra from the final results the \fIobjaps\fR parameter could be
+set to "1x2".  All other fibers will remain in the extracted spectra
+but will not be sky subtracted.
+
+The next set of parameters select the processing steps and options.  The
+scattered light option allows fitting and subtracting a scattered light
+surface from the input object and flat field.  If there is significant
+scattered light which is not subtracted the fiber throughput correction
+will not be accurate.  The
+flat fitting option allows fitting and removing the overall shape of the
+flat field spectra while preserving the pixel-to-pixel response
+corrections.  This is useful for maintaining the approximate object count
+levels and not introducing the reciprocal of the flat field spectrum into
+the object spectra.  The \fIclean\fR option invokes a profile fitting and
+deviant point rejection algorithm as well as a variance weighting of points
+in the aperture.  These options require knowing the effective (i.e.
+accounting for any image combining) read out noise and gain.  For a
+discussion of cleaning and variance weighted extraction see
+\fBapvariance\fR and \fBapprofiles\fR.
+
+The dispersion correction option selects whether to extract arc spectra,
+determine a dispersion function, assign them to the object spectra, and,
+possibly, resample the spectra to a linear (or log-linear) wavelength
+scale.  If simultaneous arc fibers are defined there is an option to delete
+them from the final spectra when they are no longer needed.
+
+The sky alignment option allows applying a zeropoint dispersion shift
+to all fibers based on one or more sky lines.  This requires all fibers
+to have the sky lines visible.  When there are sky lines this will
+improve the sky subtraction if there is a systematic error in the
+fiber iillumination between the sky and the arc calibration.
+
+The sky subtraction option selects whether to combine the sky fiber spectra
+and subtract this sky from the object fiber spectra.  It is also possible
+to subtract the sky and object fibers by pairs.  \fIDispersion
+correction and sky subtraction are independent operations.\fR  This means
+that if dispersion correction is not done then the sky subtraction will be
+done with respect to pixel coordinates.  This might be desirable in some
+quick look cases though it is incorrect for final reductions.
+
+The sky subtraction option has two additional options.  The individual sky
+spectra may be examined and contaminated spectra deleted interactively
+before combining.  This can be a useful feature in crowded regions.  The
+final combined sky spectrum (or individual skys if subtracting by
+pairs) may be saved for later inspection in an image
+with the spectrum name prefixed by \fBsky\fR.
+
+After a spectrum has been processed it is possible to examine the results
+interactively using the \fBsplot\fR tasks.  This option has a query which
+may be turned off with "YES" or "NO" if there are multiple spectra to be
+processed.
+
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\fIupdate\fR flag is set.  The changes which will cause an update are a new
+aperture identification table, a new reference image, new flat fields, and a
+new arc reference.  If all input spectra are to be processed regardless of
+previous processing the \fIredo\fR flag may be used.  Note that
+reprocessing clobbers the previously processed output spectra.
+
+The \fIbatch\fR processing option allows object spectra to be processed as
+a background or batch job.  This will only occur if sky spectra editing and
+\fBsplot\fR review (interactive operations) are turned off, either when the
+task is run or by responding with "NO" to the queries during processing.
+
+The \fIlistonly\fR option prints a summary of the processing steps which
+will be performed on the input spectra without actually doing anything.
+This is useful for verifying which spectra will be affected if the input
+list contains previously processed spectra.  The listing does not include
+any arc spectra which may be extracted to dispersion calibrate an object
+spectrum.
+
+The last parameter (excluding the task mode parameter) points to another
+parameter set for the algorithm parameters.  The way \fBdoargus\fR works
+this may not have any value and the parameter set \fBparams\fR is always
+used.  The algorithm parameters are discussed further in the next section.
+
+\fBAlgorithms and Algorithm Parameters\fR
+
+This section summarizes the various algorithms used by the \fBdoargus\fR
+task and the parameters which control and modify the algorithms.  The
+algorithm parameters available to the user are collected in the parameter
+set \fBparams\fR.  These parameters are taken from the various general
+purpose tasks used by the \fBdoargus\fR processing task.  Additional
+information about these parameters and algorithms may be found in the help
+for the actual task executed.  These tasks are identified in the parameter
+section listing in parenthesis.  The aim of this parameter set organization
+is to collect all the algorithm parameters in one place separate from the
+processing parameters and include only those which are relevant for
+Argus.  The parameter values can be changed from the
+defaults by using the parameter editor,
+.nf
+
+	cl> epar params
+
+.fi
+or simple typing \fIparams\fR.  The parameter editor can also be
+entered when editing the \fBdoargus\fR parameters by typing \fI:e
+params\fR or simply \fI:e\fR if positioned at the \fIparams\fR
+parameter.
+
+\fBExtraction\fR
+
+The identification of the spectra in the two dimensional images and their
+scattered light subtraction and extraction to one dimensional spectra
+in multispec format is accomplished
+using the tasks from the \fBapextract\fR package.  The first parameters
+through \fInsubaps\fR control the extractions.
+
+The dispersion line is that used for finding the spectra, for plotting in
+the aperture editor, and as the starting point for tracing.  The default
+value of \fBINDEF\fR selects the middle of the image.  The aperture
+finding, adjusting, editing, and tracing operations also allow summing a
+number of dispersion lines to improve the signal.  The number of lines is
+set by the \fInsum\fR parameter.
+
+The order parameter defines whether the order of the aperture
+identifications in the aperture identification table (or the default
+sequential numbers if no table is used) is in the same sense as the image
+coordinates (increasing) or the opposite sense (decreasing).  If the
+aperture identifications turn out to be opposite to what is desired when
+viewed in the aperture editing graph then simply change this parameter.
+
+The basic data output by the spectral extraction routines are the one
+dimensional spectra.  Additional information may be output when the
+\fIextras\fR option is selected and the cleaning or variance weighting
+options are also selected.  In this case a three dimensional image is
+produced with the first element of the third dimension being the cleaned
+and/or weighted spectra, the second element being the uncleaned and
+unweighted spectra, and the third element being an estimate of the sigma
+of each pixel in the extracted spectrum.  Currently the sigma data is not
+used by any other tasks and is only for reference.
+
+The initial step of finding the fiber spectra in the aperture reference
+image consists of identifying the peaks in a cut across the dispersion,
+eliminating those which are closer to each other than the \fIminsep\fR
+distance, and then keeping the specified \fInfibers\fR highest peaks.  The
+centers of the profiles are determined using the \fBcenter1d\fR algorithm
+which uses the \fIwidth\fR parameter.
+
+Apertures are then assigned to each spectrum.  The initial edges of the
+aperture relative to the center are defined by the \fIlower\fR and
+\fIupper\fR parameters.
+The initial apertures are the same for all spectra but they can each be
+automatically resized.  The automatic resizing sets the aperture limits
+at a fraction of the peak relative to the interfiber minimum.
+The default \fIylevel\fR is to resize the apertures to 5% of the peak.
+See the description for the task \fBapresize\fR for further details.
+
+The user is given the opportunity to graphically review and adjust the
+aperture definitions.  This is recommended
+and it is fundamentally important that the correct aperture/beam numbers
+be associated with the proper fibers;
+otherwise the spectrum
+identifications will not be for the objects they say.  An important command in
+this regard is the 'o' key which allows reordering the identifications.
+This is required if the first
+fiber is actually missing since the initial assignment begins with the
+first spectrum found.  The
+aperture editor is a very powerful tool and is described in detail as
+\fBapedit\fR.
+
+The next set of parameters control the tracing and function fitting of the
+aperture reference positions along the dispersion direction.  The position
+of a spectrum across the dispersion is determined by the centering
+algorithm (see \fBcenter1d\fR) at a series of evenly spaced steps, given by
+the parameter \fIt_step\fR, along the dispersion.  The step size should be
+fine enough to follow position changes but it is not necessary to measure
+every point.  The fitted points may jump around a little bit due to noise
+and cosmic rays even when summing a number of lines.  Thus, a smooth
+function is fit.  The function type, order, and iterative rejection of
+deviant points is controlled by the other trace parameters.  For more
+discussion consult the help pages for \fBaptrace\fR and \fBicfit\fR.  The
+default is to fit a cubic spline of three pieces with a single iteration of
+3 sigma rejection.
+
+The actual extraction of the spectra by summing across the aperture at each
+point along the dispersion is controlled by the next set of parameters.
+The default extraction simply sums the pixels using partial pixels at the
+ends.  The options allow selection of a weighted sum based on a Poisson
+variance model using the \fIreadnoise\fR and \fIgain\fR detector
+parameters.  Note that if the \fIclean\fR option is selected the variance
+weighted extraction is used regardless of the \fIweights\fR parameter.  The
+sigma thresholds for cleaning are also set in the \fBparams\fR parameters.
+For more on the variance weighted extraction and cleaning see
+\fBapvariance\fR and \fBapprofiles\fR as well as \fBapsum\fR.
+
+The last parameter, \fInsubaps\fR, is used only in special cases when it is
+desired to subdivide the fiber profiles into subapertures prior to
+dispersion correction.  After dispersion correction the subapertures are
+then added together.  The purpose of this is to correct for wavelength
+shifts across a fiber.
+
+\fBScattered Light Subtraction\fR
+
+Scattered light may be subtracted from the input two dimensional image as
+the first step.  This is done using the algorithm described in
+\fBapscatter\fR.  This can be important if there is significant scattered
+light since the flat field/throughput correction will otherwise be
+incorrect.  The algorithm consists of fitting a function to the data
+outside the defined apertures by a specified \fIbuffer\fR at each line or
+column across the dispersion.  The function fitting parameters are the same
+at each line.  Because the fitted functions are independent at each line or
+column a second set of one dimensional functions are fit parallel to the
+dispersion using the evaluated fit values from the cross-dispersion step.
+This produces a smooth scattered light surface which is finally subtracted
+from the input image.  Again the function fitting parameters are the
+same at each line or column though they may be different than the parameters
+used to fit across the dispersion.
+
+The first time the task is run with a particular flat field (or aperture
+reference image if no flat field is used) the scattered light fitting
+parameters are set interactively using that image.  The interactive step
+selects a particular line or column upon which the fitting is done
+interactively with the \fBicfit\fR commands.  A query is first issued
+which allows skipping this interactive stage.  Note that the interactive
+fitting is only for defining the fitting functions and orders.  When
+the graphical \fBicfit\fR fitting is exited (with 'q') there is a second prompt
+allowing you to change the buffer distance (in the first cross-dispersion
+stage) from the apertures, change the line/column, or finally quit.
+
+The initial fitting parameters and the final set parameters are recorded
+in the \fBapscat1\fR and \fBapscat2\fR hidden parameter sets.  These
+parameters are then used automatically for every subsequent image
+which is scattered light corrected.
+
+The scattered light subtraction modifies the input 2D images.  To preserve
+the original data a copy of the original image is made with the same
+root name and the word "noscat" appended.  The scattered light subtracted
+images will have the header keyword "APSCATTE" which is how the task
+avoids repeating the scattered light subtraction during any reprocessing.
+However if the \fIredo\fR option is selected the scattered light subtraction
+will also be redone by first restoring the "noscat" images to the original
+input names.
+
+\fBFlat Field and Fiber Throughput Corrections\fR
+
+Flat field corrections may be made during the basic CCD processing; i.e.
+direct division by the two dimensional flat field observation.  In that
+case do not specify a flat field spectrum; use the null string "".  The
+\fBdoargus\fR task provides an alternative flat field response correction
+based on division of the extracted object spectra by the extracted flat field
+spectra.  A discussion of the theory and merits of flat fielding directly
+verses using the extracted spectra will not be made here.  The
+\fBdoargus\fR flat fielding algorithm is the \fIrecommended\fR method for
+flat fielding since it works well and is not subject to the many problems
+involved in two dimensional flat fielding.
+
+In addition to correcting for pixel-to-pixel response the flat field step
+also corrects for differences in the fiber throughput.  Thus, even if the
+pixel-to-pixel flat field corrections have been made in some other way it
+is desirable to use a sky or dome flat observation for determining a fiber
+throughput correction.  Alternatively, a separately derived throughput
+file may be specified.  This file consists of the aperture numbers
+(the same as used for the aperture reference) and relative throughput
+numbers.
+
+The first step is extraction of the flat field spectrum, if specified,
+using the reference apertures.  Only one flat field is allowed so if
+multiple flat fields are required the data must be reduced in groups.
+After extraction one or more corrections are applied.  If the \fIfitflat\fR
+option is selected (the default) the extracted flat field spectra are
+averaged together and a smooth function is fit.  The default fitting
+function and order are given by the parameters \fIf_function\fR and
+\fIf_order\fR.  If the parameter \fIf_interactive\fR is "yes" then the
+fitting is done interactively using the \fBfit1d\fR task which uses the
+\fBicfit\fR interactive fitting commands.
+
+The fitted function is divided into the individual flat field spectra to
+remove the basic shape of the spectrum while maintaining the relative
+individual pixel responses and any fiber to fiber differences.  This step
+avoids introducing the flat field spectrum shape into the object spectra
+and closely preserves the object counts.
+
+If a throughput image is available (an observation of blank sky
+usually at twilight) it is extracted.  If no flat field is used the average
+signal through each fiber is computed and this becomes the response
+normalization function.  Note that a dome flat may be used in place of a
+sky in the sky flat field parameter for producing throughput only
+corrections.  If a flat field is specified then each sky spectrum is
+divided by the appropriate flat field spectrum.  The total counts through
+each fiber are multiplied into the flat field spectrum thus making the sky
+throughput of each fiber the same.  This correction is important if the
+iillumination of the fibers differs between the flat field source and the
+sky.  Since only the total counts are required the sky or dome flat field
+spectra need not be particularly strong though care must be taken to avoid
+objects.
+
+Instead of a sky flat or other throughput image a separately derived
+throughput file may be used.  It may be used with or without a
+flat field.
+
+The final step is to normalize the flat field spectra by the mean counts of
+all the fibers.  This normalization step is simply to preserve the average
+counts of the extracted object and arc spectra after division by the
+response spectra.  The final relative throughput values are recorded in the
+log and possibly printed on the terminal.
+
+These flat field response steps and algorithm are available as a separate
+task called \fBmsresp1d\fR.
+
+\fBDispersion Correction\fR
+
+Dispersion corrections are applied to the extracted spectra if the
+\fBdispcor\fR parameter is set.  This can be a complicated process which
+the \fBdoargus\fR task tries to simplify for you.  There are three basic
+steps involved; determining the dispersion functions relating pixel
+position to wavelength, assigning the appropriate dispersion function to a
+particular observation, and resampling the spectra to evenly spaced pixels
+in wavelength.
+
+The comparison arc spectra are used to define dispersion functions for the
+fibers using the tasks \fBautoidentify\fR and \fBreidentify\fR.  The
+interactive \fBautoidentify\fR task is only used on the central fiber of the
+first arc spectrum to define the basic reference dispersion solution from
+which all other fibers and arc spectra are automatically derived using
+\fBreidentify\fR. \fBAutoidentify\fR attempts to automatically identify
+the arc lines using the \fIcrval\fR and \fIcdelt\fR parameters.  Whether
+or not it is successful the user is presented with the interactive
+identification graph.  The automatic identifications can be reviewed and a
+new solution or corrections to the automatic solution may be performed.
+
+The set of arc dispersion function parameters are from \fBautoidentify\fR and
+\fBreidentify\fR.  The parameters define a line list for use in
+automatically assigning wavelengths to arc lines, a parameter controlling
+the width of the centering window (which should match the base line
+widths), the dispersion function type and order, parameters to exclude bad
+lines from function fits, and parameters defining whether to refit the
+dispersion function, as opposed to simply determining a zero point shift,
+and the addition of new lines from the line list when reidentifying
+additional arc spectra.  The defaults should generally be adequate and the
+dispersion function fitting parameters may be altered interactively.  One
+should consult the help for the two tasks for additional details of these
+parameters and the operation of \fBautoidentify\fR.
+
+Generally, taking a number of comparison arc lamp exposures interspersed
+with the program spectra is sufficient to accurately dispersion calibrate
+Argus spectra.  Dispersion functions are
+determined independently for each fiber of each arc image and then assigned
+to the matching fibers in the program object observations.  The assignment
+consists of selecting one or two arc images to calibrate each object
+image.
+
+However, there is another calibration option which may be of interest.
+This option uses auxiliary line spectra, such as from dome lights or night
+sky lines, to monitor wavelength zero point shifts which are added to the
+basic dispersion function derived from a single reference arc.  Initially
+one of the auxiliary fiber spectra is plotted interactively by
+\fBidentify\fR with the reference dispersion function for the appropriate
+fiber.  The user marks one or more lines which will be used to compute zero
+point wavelength shifts in the dispersion functions automatically.  In this
+case it is auxiliary arc images which are assigned to particular objects.
+
+The arc or auxiliary line image assignments may be done either explicitly with an arc assignment
+table (parameter \fIarctable\fR) or based on a header parameter.  The task
+used is \fBrefspectra\fR and the user should consult this task if the
+default behavior is not what is desired.  The default is to interpolate
+linearly between the nearest arcs based on the Julian date (corrected to
+the middle of the exposure).  The Julian date and a local Julian day number
+(the day number at local noon) are computed automatically by the task
+\fBsetjd\fR and recorded in the image headers under the keywords JD and
+LJD.  In addition the universal time at the middle of the exposure, keyword
+UTMIDDLE, is computed by the task \fBsetairmass\fR and this may also be used
+for ordering the arc and object observations.
+
+An optional step is to use sky lines in the spectra to compute a zeropoint
+dispersion shift that will align the sky lines.  This may improve sky
+subtraction if the iillumination is not the same between the arc calibration
+and the sky.  When selected the object spectrum is dispersion corrected
+using a non-linear dispersion function to avoid resampling the spectrum.
+The sky lines are then reidentified in wavelength space from a template
+list of sky lines.  The mean shift in the lines for each fiber relative to
+the template in that fiber is computed to give the zeropoint shift.  The
+database file is created when the first object is extracted.  You are asked
+to mark the sky lines in one fiber and then the lines are automatically
+reidentified in all other fibers.  Note that this technique requires the
+sky lines be found in all fibers.
+
+The last step of dispersion correction (resampling the spectrum to evenly
+spaced pixels in wavelength) is optional and relatively straightforward.
+If the \fIlinearize\fR parameter is no then the spectra are not resampled
+and the nonlinear dispersion information is recorded in the image header.
+Other IRAF tasks (the coordinate description is specific to IRAF) will use
+this information whenever wavelengths are needed.  If linearizing is
+selected a linear dispersion relation, either linear in the wavelength or
+the log of the wavelength, is defined once and applied to every extracted
+spectrum.  The resampling algorithm  parameters allow selecting the
+interpolation function type, whether to conserve flux per pixel by
+integrating across the extent of the final pixel, and whether to linearize
+to equal linear or logarithmic intervals.  The latter may be appropriate
+for radial velocity studies.  The default is to use a fifth order
+polynomial for interpolation, to conserve flux, and to not use logarithmic
+wavelength bins.  These parameters are described fully in the help for the
+task \fBdispcor\fR which performs the correction.  The interpolation
+function options and the nonlinear dispersion coordinate system is
+described in the help topic \fBonedspec.package\fR.
+
+\fBSky Subtraction\fR
+
+Sky subtraction is selected with the \fIskysubtract\fR processing option.
+The sky spectra are selected by their aperture and beam numbers.
+If the \fIskyedit\fR
+option is selected the sky spectra are plotted using the task
+\fBspecplot\fR.  By default they are superposed to allow identifying
+spectra with unusually high signal due to object contamination.  To
+eliminate a sky spectrum from consideration point at it with the cursor and
+type 'd'.  The last deleted spectrum may be undeleted with 'e'.  This
+allows recovery of incorrect or accidental deletions.
+
+If the combining option is "none" then the sky and object fibers are
+paired and one sky is subtracted from one object and the saved sky will
+be the individual sky fiber spectra.
+
+However, the usual
+case is to combine the individual skys into a single master sky spectrum
+which is then subtracted from each object spectrum.
+The sky combining algorithm parameters define how the individual sky fiber
+spectra, after interactive editing, are combined before subtraction from
+the object fibers.  The goals of combining are to reduce noise, eliminate
+cosmic-rays, and eliminate fibers with inadvertent objects.  The common
+methods for doing this to use a median and/or a special sigma clipping
+algorithm (see \fBscombine\fR for details).  The scale
+parameter determines whether the individual skys are first scaled to a
+common mode.  The scaling should be used if the throughput is uncertain,
+but in that case you probably did the wrong thing in the throughput
+correction.  If the sky subtraction is done interactively, i.e. with the
+\fIskyedit\fR option selected, then after selecting the spectra to be
+combined a query is made for the combining algorithm.  This allows
+modifying the default algorithm based on the number of sky spectra
+selected since the "avsigclip" rejection algorithm requires at least
+three spectra.
+
+The combined sky spectrum is subtracted from only those spectra specified
+by the object aperture and beam numbers.  Other spectra
+are retained unchanged.  One may include the sky spectra as
+object spectra to produce residual sky spectra for analysis.  The combined
+master sky spectra may be saved if the \fIsaveskys\fR parameter is set.
+The saved sky is given the name of the object spectrum with the prefix
+"sky".
+.ih
+EXAMPLES
+1.  The following example uses artificial data and may be executed
+at the terminal (with IRAF V2.10).  This is also the sequence performed
+by the test procedure "demos qtest".
+
+.nf
+ar> demos mkqdata
+Creating image demoobj ...
+Creating image demoflat ...
+Creating image demoarc ...
+hy> argus.verbose = yes
+hy> doargus demoobj apref=demoflat flat=demoflat arcs1=demoarc \
+>>> fib=13 width=4. minsep=5. maxsep=7. clean- splot+
+Set reference apertures for demoflat
+Resize apertures for demoflat?  (yes):
+Edit apertures for demoflat?  (yes):
+<Exit with 'q'>
+Fit curve to aperture 1 of demoflat interactively  (yes):
+<Exit with 'q'>
+Fit curve to aperture 2 of demoflat interactively  (yes): N
+Create response function demoflatnorm.ms
+Extract flat field demoflat
+Fit and ratio flat field demoflat
+<Exit with 'q'>
+Extract flat field demoflat
+Fit and ratio flat field demoflat
+Create the normalized response demoflatnorm.ms
+demoflatnorm.ms -> demoflatnorm.ms  using bzero: 0.
+    and bscale: 1.000001
+    mean: 1.000001  median: 1.110622  mode: 1.331709
+    upper: INDEF  lower: INDEF
+Average aperture response:
+1.  1.136281
+2.  1.208727
+3.  0.4720535
+4.  1.308195
+5.  1.344551
+6.  1.330406
+7.  0.7136359
+8.  1.218975
+9.  0.7845755
+10.  0.9705642
+11.  1.02654
+12.  0.3745525
+13.  1.110934
+Extract arc reference image demoarc
+Determine dispersion solution for demoarc
+<A dispersion solution is found automatically.>
+<Type 'f' to look at fit.  Type 'q' to exit fit.>
+<Exit with 'q'>
+
+REIDENTIFY: NOAO/IRAF V2.10BETA valdes@puppis Tue 16:01:07 11-Feb-92
+  Reference image = d....ms.imh, New image = d....ms, Refit = yes
+     Image Data Found    Fit Pix Shift User Shift  Z Shift     RMS
+d....ms - Ap 7  29/29  29/29   9.53E-4    0.00409  2.07E-7   0.273
+Fit dispersion function interactively? (no|yes|NO|YES) (yes): n
+d....ms - Ap 5  29/29  29/29   -0.0125    -0.0784  -1.2E-5   0.315
+Fit dispersion function interactively? (no|yes|NO|YES) (no): y
+d....ms - Ap 5  29/29  29/29   -0.0125    -0.0784  -1.2E-5   0.315
+d....ms - Ap 4  29/29  29/29   -0.0016    -0.0118  -2.7E-6   0.284
+Fit dispersion function interactively? (no|yes|NO|YES) (yes): N
+d....ms - Ap 4  29/29  29/29   -0.0016    -0.0118  -2.7E-6   0.284
+d....ms - Ap 3  29/29  29/29  -0.00112   -0.00865  -1.8E-6   0.282
+d....ms - Ap 2  29/29  29/29  -0.00429    -0.0282  -4.9E-6   0.288
+d....ms - Ap 1  29/29  28/29   0.00174    0.00883  6.63E-7   0.228
+d....ms - Ap 9  29/29  29/29  -0.00601    -0.0387  -6.5E-6   0.268
+d....ms - Ap 10 29/29  29/29  -9.26E-4   -0.00751  -1.7E-6   0.297
+d....ms - Ap 11 29/29  29/29   0.00215     0.0114  1.05E-6   0.263
+d....ms - Ap 12 29/29  29/29  -0.00222    -0.0154  -2.8E-6   0.293
+d....ms - Ap 13 29/29  29/29   -0.0138    -0.0865  -1.4E-5    0.29
+d....ms - Ap 14 29/29  29/29  -0.00584    -0.0378  -6.8E-6   0.281
+
+Dispersion correct demoarc
+demoarc.ms: w1 = 5785.8..., w2 = 7351.6..., dw = 6.14..., nw = 256
+  Change wavelength coordinate assignments? (yes|no|NO): n
+Extract object spectrum demoobj
+Assign arc spectra for demoobj
+[demoobj] refspec1='demoarc'
+Dispersion correct demoobj
+demoobj.ms.imh: w1 = 5785.833, w2 =  7351.63, dw = 6.140378, nw = 256
+Sky subtract demoobj:  skybeams=0
+Edit the sky spectra? (yes):
+<Exit with 'q'>
+Sky rejection option (none|minmax|avsigclip) (avsigclip):
+demoobj.ms.imh:
+Splot spectrum? (no|yes|NO|YES) (yes):
+Image line/aperture to plot (1:) (1):
+<Look at spectra and change apertures with # key>
+<Exit with 'q'>
+.fi
+.ih
+REVISIONS
+.ls DOARGUS V2.11
+A sky alignment option was added.
+
+The aperture identification can now be taken from image header keywords.
+
+The initial arc line identifications is done with the automatic line
+identification algorithm.
+.le
+.ls DOARGUS V2.10.3
+The usual output WCS format is "equispec".  The image format type to be
+processed is selected with the \fIimtype\fR environment parameter.  The
+dispersion axis parameter is now a package parameter.  Images will only
+be processed if the have the CCDPROC keyword.  A \fIdatamax\fR parameter
+has been added to help improve cosmic ray rejection.  A scattered
+light subtraction processing option has been added.
+.le
+.ih
+SEE ALSO
+apedit, apfind, approfiles, aprecenter, apresize, apsum, aptrace, apvariance,
+ccdred, center1d, dispcor, fit1d, icfit, identify, msresp1d, observatory,
+onedspec.package, refspectra, reidentify, scombine, setairmass, setjd,
+specplot, splot
+.endhelp
diff --git a/noao/imred/argus/doc/doargus.ms b/noao/imred/argus/doc/doargus.ms
new file mode 100644
index 00000000..f68883c1
--- /dev/null
+++ b/noao/imred/argus/doc/doargus.ms
@@ -0,0 +1,1725 @@
+.nr PS 9
+.nr VS 11
+.de V1
+.ft CW
+.nf
+..
+.de V2
+.fi
+.ft R
+..
+.de LS
+.br
+.in +2
+..
+.de LE
+.br
+.sp .5v
+.in -2
+..
+.ND July 1995
+.TL
+Guide to the ARGUS Reduction Task DOARGUS
+.AU
+Francisco Valdes
+.AI
+IRAF Group - Central Computer Services
+.K2
+.DY
+
+.AB
+The \fBdoargus\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, fiber throughput correction, wavelength calibration, and sky
+subtraction of \fIArgus\fR fiber spectra.  It is a
+command language script which collects and combines the functions and
+parameters of many general purpose tasks to provide a single complete data
+reduction path.  The task provides a degree of guidance, automation, and
+record keeping necessary when dealing with the large amount of data
+generated by this multifiber instrument.  This guide describes what
+this task does, it's usage, and parameters.
+.AE
+.NH
+Introduction
+.LP
+The \fBdoargus\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, fiber throughput correction, wavelength calibration, and sky
+subtraction of \fIArgus\fR fiber spectra.  It is a
+command language script which collects and combines the functions and
+parameters of many general purpose tasks to provide a single, complete data
+reduction path.  The task provides a degree of guidance, automation, and
+record keeping necessary when dealing with the large amount of data
+generated by these multifiber instruments.
+.LP
+The general organization of the task is to do the interactive setup steps
+first using representative calibration data and then perform the majority
+of the reductions automatically, and possibly as a background process, with
+reference to the setup data.  In addition, the task determines which setup
+and processing operations have been completed in previous executions of the
+task and, contingent on the \f(CWredo\fR and \f(CWupdate\fR options, skip or
+repeat some or all the steps.
+.LP
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage for
+Argus since there are many variations possible.  Because \fBdoargus\fR
+combines many separate, general purpose tasks, the description given here
+refers to these tasks and leaves some of the details to their help
+documentation.
+.NH
+Usage Outline
+.LP
+.IP [1] 6
+The images are first processed with \fBccdproc\fR for overscan,
+bias, and dark corrections.
+The \fBdoargus\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+.IP [2]
+Set the \fBdoargus\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed, the flat field image as the aperture reference and
+the flat field, and one or more arc images.  A throughput file or image,
+such as a blank sky observation, may also be specified.  If there are many
+object or arc spectra per setup you might want to prepare "@ files".
+Prepare and specify an aperture identification table if desired.
+You might wish to verify the geometry parameters,
+separations, dispersion direction, etc., which may change with different
+detector setups.  The processing parameters are set for complete reductions
+but for quicklook you might not use the clean option or dispersion
+calibration and sky subtraction.
+.IP
+The parameters are set for a particular Argus configuration and different
+configurations may use different flat fields, arcs, and aperture
+identification tables.
+.IP [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the execution and no further queries of that
+type will be made.
+.IP [4]
+The apertures are defined using the specified aperture reference image.
+The spectra are found automatically and apertures assigned based on
+task parameters and the aperture identification table.  Unassigned
+fibers may have a negative beam number and will be ignored in subsequent
+processing.  The resize option sets the aperture size to the widths of
+the profiles at a fixed fraction of the peak height.  The interactive
+review of the apertures is recommended.  If the identifications are off
+by a shift the 'o' key is used.  To exit the aperture review type 'q'.
+.IP [5]
+The fiber positions at a series of points along the dispersion are measured
+and a function is fit to these positions.  This may be done interactively to
+adjust the fitting parameters.  Not all fibers need be examined and the "NO"
+response will quit the interactive fitting.  To exit the interactive
+fitting type 'q'.
+.IP [6]
+If scattered light subtraction is to be done the flat field image is
+used to define the scattered light fitting parameters interactively.
+If one is not specified then the aperture reference image is used for
+this purpose.
+
+There are two queries for the interactive fitting.  A graph of the
+data between the defined reference apertures separated by a specified
+buffer distance is first shown.  The function order and type may be
+adjusted.  After quiting with 'q' the user has the option of changing
+the buffer value and returning to the fitting, changing the image line
+or column to check if the fit parameters are satisfactory at other points,
+or to quit and accept the fit parameters.  After fitting all points
+across the dispersion another graph showing the scattered light from
+the individual fits is shown and the smoothing parameters along the
+dispersion may be adjusted.  Upon quiting with 'q' you have the option
+of checking other cuts parallel to the dispersion or quiting and finishing
+the scattered light function smoothing and subtraction.
+
+If there is a throughput image then this is corrected for scattered light
+noninteractively using the previous fitting parameters.
+.IP [7]
+If flat fielding is to be done the flat field spectra are extracted.  The
+average spectrum over all fibers is determined and a function is fit
+interactively (exit with 'q').  This function is generally of sufficiently
+high order that the overall shape is well fit.  This function is then used
+to normalize the individual flat field spectra.  If a throughput image, a
+sky flat, is specified then the total sky counts through each fiber are
+used to correct the total flat field counts.  Alternatively, a separately
+derived throughput file can be used for specifying throughput corrections.
+If neither type of throughput is used the flat field also provides the
+throughput correction.  The final response spectra are normalized to a unit
+mean over all fibers.  The relative average throughput for each fiber is
+recorded in the log and possibly printed to the terminal.
+.IP [8]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  The middle fiber is used to identify the arc lines and define
+the dispersion function using the task \fBautoidentify\fR.  The
+\fIcrval\fR and \fIcdelt\fR parameters are used in the automatic
+identification.  Whether or not the automatic identification is
+successful you will be shown the result of the arc line identification.
+If the automatic identification is not successful identify a few arc
+lines with 'm' and use the 'l' line list identification command to
+automatically add additional lines and fit the dispersion function.  Check
+the quality of the dispersion function fit with 'f'.  When satisfied exit
+with 'q'.
+.IP [9]
+The remaining fibers are automatically reidentified.  You have the option
+to review the line identifications and dispersion function for each fiber
+and interactively add or delete arc lines and change fitting parameters.
+This can be done selectively, such as when the reported RMS increases
+significantly.
+.IP [10]
+If the spectra are to be resampled to a linear dispersion system
+(which will be the same for all spectra) default dispersion parameters
+are printed and you are allowed to adjust these as desired.
+.IP [11]
+If the sky line alignment option is selected and the sky lines have not
+been identified for a particular aperture identification table then you are
+asked to mark one or more sky lines.  You may simply accept the wavelengths
+of these lines as defined by the dispersion solution for this spectrum and
+fiber or you may specify knowns wavelengths for the lines. These lines will
+be reidentified in all object spectra extracted and a mean zeropoint shift
+will be added to the dispersion solution.  This has the effect of aligning
+these lines to optimize sky subtraction.
+.IP [12]
+The object spectra are now automatically scattered light subtracted,
+ extracted, flat fielded, and dispersion corrected.
+.IP [13]
+When sky subtracting, the individual sky spectra may be reviewed and some
+spectra eliminated using the 'd' key.  The last deleted spectrum may be
+recovered with the 'e' key.  After exiting the review with 'q' you are
+asked for the combining option.  The type of combining is dictated by the
+number of sky fibers.
+.IP [14]
+The option to examine the final spectra with \fBsplot\fR may be given.
+To exit type 'q'.
+.IP [15]
+If scattered light is subtracted from the input data a copy of the
+original image is made by appending "noscat" to the image name.
+If the data are reprocessed with the \fIredo\fR flag the original
+image will be used again to allow modification of the scattered
+light parameters.
+
+The final spectra will have the same name as the original 2D images
+with a ".ms" extension added.  The flat field and arc spectra may
+also have part of the aperture identification table name, if used, added to
+allow different configurations to use the same 2D flat field and arcs
+but with different aperture definitions.  If using the sky alignment
+option an image "align" with the aperture identification table name
+applied will also be created.
+.NH
+Spectra and Data Files
+.LP
+The basic input consists of Argus object and
+calibration spectra stored as IRAF images.
+The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+The raw CCD images must
+be processed to remove overscan, bias, and dark count effects.  This
+is generally done using the \fBccdred\fR package.
+The \fBdoargus\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+ Flat fielding is
+generally not done at this stage but as part of \fBdoargus\fR.
+If flat fielding is done as part of the basic CCD processing then
+a flattened flat field, blank sky observation, or throughput file
+should still be created for applying fiber throughput corrections.
+.LP
+The task \fBdoargus\fR uses several types of calibration spectra.  These
+are flat fields, blank sky flat fields, comparison lamp spectra, and auxiliary
+mercury line (from the dome lights) or sky line spectra.  The flat field,
+throughput image or file, and auxiliary emission line spectra are optional.
+If a flat field is used then the sky flat
+or throughput file is optional assuming the flat field has the same fiber
+illumination.  It is legal to specify only a throughput image or file and
+leave the flat field blank in order to simply apply a throughput
+correction.  Because only the total counts through each fiber are used from
+a throughput image, sky flat exposures need not be of high signal per
+pixel.
+.LP
+There are two types of dispersion calibration methods.  One is to take arc
+calibration exposures through all fibers periodically and apply the
+dispersion function derived from one or interpolated between pairs to the
+object fibers.  This is the usual method with Argus.
+A second (uncommon) method is to \fIauxiliary
+line spectra\fR such as lines in the dome lights or sky lines to monitor
+shifts relative to a few actual arc exposures.  The main reason to do this
+is if taking arc exposures through all fibers is inconvenient.
+.LP
+The assignment of arc or auxiliary line calibration exposures to object
+exposures is generally done by selecting the nearest in time and
+interpolating.  There are other options possible which are described under
+the task \fBrefspectra\fR.  The most general option is to define a table
+giving the object image name and the one or two arc spectra to be assigned
+to that object.  That file is called an \fIarc assignment table\fR and it
+is one of the optional setup files which can used with \fBdoargus\fR.
+.LP
+The first step in the processing is identifying the spectra in the images.
+The default method is to use the fact that object and sky fibers alternate
+and assign sequential numbers to the fibers so the sky fibers are the
+even aperture numbers and the object fibers are the odd aperture numbers.
+In this case the beam numbers are not used and are the same as the
+aperture numbers and there are no object identifications associated with the
+spectra.
+.LP
+A very useful, optional, setup parameter is an \fIaperture identification
+table\fR.  The table contains information about the fiber assignments
+including object titles.  The table is either a text file or an image
+containing the keywords SLFIB.  An aperture identification file contains
+lines consisting of an aperture number, a beam number, and an object
+identification.  In an image the SLFIB keywords contain the aperture
+number, the beam numbers, optional right ascension and declination, and a
+title.  The aperture identification information must be in the same order
+as the fibers in the image.  The aperture number may be any unique number
+but it is recommended that the normal sequential fiber numbers be used.
+The beam number may be used to flag object or sky spectra or simply be the
+same as the aperture number.  The object identifications are optional but
+it is good practice to include them so that the data will contain the
+object information independent of other records.  Figure 1 shows an example
+of a file for a configuration called LMC123.
+
+.ce
+Figure 1: Example Aperture Identification File
+
+.V1
+    cl> type LMC124
+    1 1 143
+    2 0 sky
+    3 1 121
+       .
+       .
+       .
+    47 1 s92
+    48 0 sky
+.V2
+
+Note the identification of the sky fibers with beam number 0 and the
+object fibers with 1.  Any broken fibers should be included and
+identified by a different beam number, say beam number -1, to give the
+automatic spectrum finding operation the best chance to make the
+correct identifications.  Naturally the identification table will vary
+for each configuration.
+Additional information about the aperture identification
+file may be found in the description of the task \fBapfind\fR.
+.LP
+The final reduced spectra are recorded in two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ms" extension.  Each line in the reduced image is a one dimensional
+spectrum with associated aperture, wavelength, and identification
+information.  When the \f(CWextras\fR parameter is set the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tools such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.  The special task \fBscopy\fR may be used to extract
+specific apertures or to change format to individual one dimensional
+images.
+.NH
+Package Parameters
+.LP
+The \fBargus\fR package parameters, shown in Figure 1, set parameters
+affecting all the tasks in the package.
+.KS
+.V1
+
+.ce
+Figure 1: Package Parameter Set for ARGUS
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = imred
+   TASK = argus
+
+(dispaxi=            2) Image axis for 2D images
+(observa=  observatory) Observatory of data
+(interp =        poly5) Interpolation type
+
+(databas=     database) Database
+(verbose=           no) Verbose output?
+(logfile=      logfile) Log file
+(plotfil=             ) Plot file
+
+(records=             )
+(version= ARGUS V1: January 1992)
+
+.KE
+.V2
+The dispersion axis parameter defines the image axis along which the
+dispersion runs.  This is used if the image header doesn't define the
+dispersion axis with the DISPAXIS keyword.
+The observatory parameter is only required
+for data taken with fiber instruments other than Argus.
+The spectrum interpolation type might be changed to "sinc" but
+with the cautions given in \fBonedspec.package\fR.
+The other parameters define the standard I/O functions.
+The verbose parameter selects whether to print everything which goes
+into the log file on the terminal.  It is useful for monitoring
+what the \fBdoargus\fR task does.  The log and plot files are useful for
+keeping a record of the processing.  A log file is highly recommended.
+A plot file provides a record of apertures, traces, and extracted spectra
+but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+.NH
+Processing Parameters
+.LP
+The \fBdoargus\fR parameters are shown in Figure 2.
+.KS
+.V1
+
+.ce
+Figure 2: Parameter Set for DOARGUS
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = argus
+   TASK = doargus
+
+objects =               List of object spectra
+(apref  =             ) Aperture reference spectrum
+(flat   =             ) Flat field spectrum
+(through=             ) Throughput file or image (optional)
+(arcs1  =             ) List of arc spectra
+(arcs2  =             ) List of shift arc spectra
+(arcrepl=             ) Special aperture replacements
+(arctabl=             ) Arc assignment table (optional)
+
+.KE
+.V1
+(readnoi=      RDNOISE) Read out noise sigma (photons)
+(gain   =         GAIN) Photon gain (photons/data number)
+(datamax=        INDEF) Max data value / cosmic ray threshold
+(fibers =           97) Number of fibers
+(width  =          12.) Width of profiles (pixels)
+(minsep =           8.) Minimum separation between fibers (pixels)
+(maxsep =          15.) Maximum separation between fibers (pixels)
+(apidtab=             ) Aperture identifications
+(crval  =        INDEF) Approximate wavelength
+(cdelt  =        INDEF) Approximate dispersion
+(objaps =             ) Object apertures
+(skyaps =             ) Sky apertures
+(arcaps =             ) Arc apertures
+(objbeam=          0,1) Object beam numbers
+(skybeam=            0) Sky beam numbers
+(arcbeam=             ) Arc beam numbers
+
+(scatter=           no) Subtract scattered light?
+(fitflat=          yes) Fit and ratio flat field spectrum?
+(clean  =          yes) Detect and replace bad pixels?
+(dispcor=          yes) Dispersion correct spectra?
+(savearc=          yes) Save simultaneous arc apertures?
+(skysubt=          yes) Subtract sky?
+(skyedit=          yes) Edit the sky spectra?
+(savesky=          yes) Save sky spectra?
+(splot  =           no) Plot the final spectrum?
+(redo   =           no) Redo operations if previously done?
+(update =          yes) Update spectra if cal data changes?
+(batch  =           no) Extract objects in batch?
+(listonl=           no) List steps but don't process?
+
+(params =             ) Algorithm parameters
+
+.V2
+The list of objects and arcs can be @ files if desired.  The aperture
+reference spectrum is usually the same as the flat field spectrum though it
+could be any exposure with enough signal to accurately define the positions
+and trace the spectra.  The first list of arcs are the standard Th-Ar or
+HeNeAr comparison arc spectra (they must all be of the same type).  The
+second list of arcs are the auxiliary emission line exposures mentioned
+previously.
+.LP
+The detector read out noise and gain are used for cleaning and variance
+(optimal) extraction.
+The variance
+weighting and cosmic-ray cleanning are sensitive to extremely strong
+cosmic-rays; ones which are hundreds of times brighter than the
+spectrum.  The \fIdatamax\fR is used to set an upper limit for any
+real data.  Any pixels above this value will be flagged as cosmic-rays
+and will not affect the extractions.
+The dispersion axis defines the wavelength direction of spectra in
+the image if not defined in the image header by the keyword DISPAXIS.  The
+width and separation parameters define the dimensions (in pixels) of the
+spectra (fiber profile) across the dispersion.  The width parameter
+primarily affects the centering.  The maximum separation parameter is
+important if missing spectra are to
+be correctly skipped.  The number of fibers can be left at the default
+and the task will try to account for unassigned or missing fibers.
+However, this may lead to occasional incorrect
+identifications so it is recommended that only the true number of
+fibers be specified.  The aperture identification table was described
+earlier.
+.LP
+The approximate central wavelength and dispersion are used for the
+automatic identification of the arc reference.  They may be specified
+as image header keywords or values.  The INDEF values search the
+entire range of the coordinate reference file but the automatic
+line identification algorithm works much better and faster if
+approximate values are given.
+.LP
+The task needs to know which fibers are object and which are sky
+if sky subtraction is to be done.  One could explicitly
+give the aperture numbers but the recommended way is to use the default
+of selecting every second fiber as sky.  If no list of aperture or beam
+numbers is given
+then all apertures or beam numbers are selected.  Sky subtracted sky
+spectra are useful for evaluating the sky subtraction.  Since only
+the spectra identified as objects are sky subtracted one can exclude
+fibers from the sky subtraction.  For example, to eliminate the sky
+spectra from the final results the \fIobjaps\fR parameter could be
+set to "1x2".  All other fibers will remain in the extracted spectra
+but will not be sky subtracted.
+.LP
+The next set of parameters select the processing steps and options.  The
+scattered light option allows fitting and subtracting a scattered light
+surface from the input object and flat field.  If there is significant
+scattered light which is not subtracted the fiber throughput correction
+will not be accurate.  The
+flat fitting option allows fitting and removing the overall shape of the
+flat field spectra while preserving the pixel-to-pixel response
+corrections.  This is useful for maintaining the approximate object count
+levels and not introducing the reciprocal of the flat field spectrum into
+the object spectra.  The \f(CWclean\fR option invokes a profile fitting and
+deviant point rejection algorithm as well as a variance weighting of points
+in the aperture.  These options require knowing the effective (i.e.
+accounting for any image combining) read out noise and gain.  For a
+discussion of cleaning and variance weighted extraction see
+\fBapvariance\fR and \fBapprofiles\fR.
+.LP
+The dispersion correction option selects whether to extract arc spectra,
+determine a dispersion function, assign them to the object spectra, and,
+possibly, resample the spectra to a linear (or log-linear) wavelength
+scale.  If simultaneous arc fibers are defined there is an option to delete
+them from the final spectra when they are no longer needed.
+.LP
+The sky alignment option allows applying a zeropoint dispersion shift
+to all fibers based on one or more sky lines.  This requires all fibers
+to have the sky lines visible.  When there are sky lines this will
+improve the sky subtraction if there is a systematic error in the
+fiber illumination between the sky and the arc calibration.
+.LP
+The sky subtraction option selects whether to combine the sky fiber spectra
+and subtract this sky from the object fiber spectra.  It is also possible
+to subtract the sky and object fibers by pairs.  \fIDispersion
+correction and sky subtraction are independent operations.\fR  This means
+that if dispersion correction is not done then the sky subtraction will be
+done with respect to pixel coordinates.  This might be desirable in some
+quick look cases though it is incorrect for final reductions.
+.LP
+The sky subtraction option has two additional options.  The individual sky
+spectra may be examined and contaminated spectra deleted interactively
+before combining.  This can be a useful feature in crowded regions.  The
+final combined sky spectrum (or individual skys if subtracting by
+pairs) may be saved for later inspection in an image
+with the spectrum name prefixed by \fBsky\fR.
+.LP
+After a spectrum has been processed it is possible to examine the results
+interactively using the \fBsplot\fR tasks.  This option has a query which
+may be turned off with "YES" or "NO" if there are multiple spectra to be
+processed.
+.LP
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\f(CWupdate\fR flag is set.  The changes which will cause an update are a new
+aperture identification table, a new reference image, new flat fields, and a
+new arc reference.  If all input spectra are to be processed regardless of
+previous processing the \f(CWredo\fR flag may be used.  Note that
+reprocessing clobbers the previously processed output spectra.
+.LP
+The \f(CWbatch\fR processing option allows object spectra to be processed as
+a background or batch job.  This will only occur if sky spectra editing and
+\fBsplot\fR review (interactive operations) are turned off, either when the
+task is run or by responding with "NO" to the queries during processing.
+.LP
+The \f(CWlistonly\fR option prints a summary of the processing steps which
+will be performed on the input spectra without actually doing anything.
+This is useful for verifying which spectra will be affected if the input
+list contains previously processed spectra.  The listing does not include
+any arc spectra which may be extracted to dispersion calibrate an object
+spectrum.
+.LP
+The last parameter (excluding the task mode parameter) points to another
+parameter set for the algorithm parameters.  The way \fBdoargus\fR works
+this may not have any value and the parameter set \fBparams\fR is always
+used.  The algorithm parameters are discussed further in the next section.
+.NH
+Algorithms and Algorithm Parameters
+.LP
+This section summarizes the various algorithms used by the \fBdoargus\fR
+task and the parameters which control and modify the algorithms.  The
+algorithm parameters available to the user are collected in the parameter
+set \fBparams\fR.  These parameters are taken from the various general
+purpose tasks used by the \fBdoargus\fR processing task.  Additional
+information about these parameters and algorithms may be found in the help
+for the actual task executed.  These tasks are identified in the parameter
+section listing in parenthesis.  The aim of this parameter set organization
+is to collect all the algorithm parameters in one place separate from the
+processing parameters and include only those which are relevant for
+Argus.  The parameter values can be changed from the
+defaults by using the parameter editor,
+.V1
+
+	cl> epar params
+
+.V2
+or simple typing \f(CWparams\fR.  The parameter editor can also be
+entered when editing the \fBdoargus\fR parameters by typing \f(CW:e
+params\fR or simply \f(CW:e\fR if positioned at the \f(CWparams\fR
+parameter.  Figure 3 shows the parameters set.
+.KS
+.V1
+
+.ce
+Figure 3: Algorithm Parameter Set
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = argus
+   TASK = params
+
+(line   =        INDEF) Default dispersion line
+(nsum   =           10) Number of dispersion lines to sum
+(order  =   decreasing) Order of apertures
+(extras =           no) Extract sky, sigma, etc.?
+
+                        -- DEFAULT APERTURE LIMITS --
+(lower  =          -5.) Lower aperture limit relative to center
+(upper  =           5.) Upper aperture limit relative to center
+
+                        -- AUTOMATIC APERTURE RESIZING PARAMETERS --
+(ylevel =         0.05) Fraction of peak or intensity for resizing
+
+.KE
+.KS
+.V1
+                        -- TRACE PARAMETERS --
+(t_step =           10) Tracing step
+(t_funct=      spline3) Trace fitting function
+(t_order=            3) Trace fitting function order
+(t_niter=            1) Trace rejection iterations
+(t_low  =           3.) Trace lower rejection sigma
+(t_high =           3.) Trace upper rejection sigma
+
+.KE
+.KS
+.V1
+                        -- SCATTERED LIGHT PARAMETERS --
+(buffer =           1.) Buffer distance from apertures
+(apscat1=             ) Fitting parameters across the dispersion
+(apscat2=             ) Fitting parameters along the dispersion
+
+.KE
+.KS
+.V1
+                        -- APERTURE EXTRACTION PARAMETERS --
+(weights=         none) Extraction weights (none|variance)
+(pfit   =        fit1d) Profile fitting algorithm (fit1d|fit2d)
+(lsigma =           3.) Lower rejection threshold
+(usigma =           3.) Upper rejection threshold
+(nsubaps=            1) Number of subapertures
+
+.KE
+.KS
+.V1
+                        -- FLAT FIELD FUNCTION FITTING PARAMETERS --
+(f_inter=          yes) Fit flat field interactively?
+(f_funct=      spline3) Fitting function
+(f_order=           10) Fitting function order
+
+.KE
+.KS
+.V1
+                        -- ARC DISPERSION FUNCTION PARAMETERS --
+(coordli=linelists$idhenear.dat) Line list
+(match  =          10.) Line list matching limit in Angstroms
+(fwidth =           4.) Arc line widths in pixels
+(cradius=          10.) Centering radius in pixels
+(i_funct=      spline3) Coordinate function
+(i_order=            3) Order of dispersion function
+(i_niter=            2) Rejection iterations
+(i_low  =           3.) Lower rejection sigma
+(i_high =           3.) Upper rejection sigma
+(refit  =          yes) Refit coordinate function when reidentifying?
+(addfeat=           no) Add features when reidentifying?
+
+.KE
+.KS
+.V1
+                        -- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+(select =       interp) Selection method for reference spectra
+(sort   =           jd) Sort key
+(group  =          ljd) Group key
+(time   =           no) Is sort key a time?
+(timewra=          17.) Time wrap point for time sorting
+
+.KE
+.KS
+.V1
+                        -- DISPERSION CORRECTION PARAMETERS --
+(lineari=          yes) Linearize (interpolate) spectra?
+(log    =           no) Logarithmic wavelength scale?
+(flux   =          yes) Conserve flux?
+
+.KE
+.KS
+.V1
+                        -- SKY SUBTRACTION PARAMETERS --
+(combine=      average) Type of combine operation
+(reject =    avsigclip) Sky rejection option
+(scale  =         none) Sky scaling option
+
+.KE
+.V2
+.NH 2
+Extraction
+.LP
+The identification of the spectra in the two dimensional images and their
+scattered light subtraction and extraction to one dimensional spectra
+in multispec format is accomplished
+using the tasks from the \fBapextract\fR package.  The first parameters
+through \f(CWnsubaps\fR control the extractions.
+.LP
+The dispersion line is that used for finding the spectra, for plotting in
+the aperture editor, and as the starting point for tracing.  The default
+value of \fBINDEF\fR selects the middle of the image.  The aperture
+finding, adjusting, editing, and tracing operations also allow summing a
+number of dispersion lines to improve the signal.  The number of lines is
+set by the \f(CWnsum\fR parameter.
+.LP
+The order parameter defines whether the order of the aperture
+identifications in the aperture identification table (or the default
+sequential numbers if no file is used) is in the same sense as the image
+coordinates (increasing) or the opposite sense (decreasing).  If the
+aperture identifications turn out to be opposite to what is desired when
+viewed in the aperture editing graph then simply change this parameter.
+.LP
+The basic data output by the spectral extraction routines are the one
+dimensional spectra.  Additional information may be output when the
+\f(CWextras\fR option is selected and the cleaning or variance weighting
+options are also selected.  In this case a three dimensional image is
+produced with the first element of the third dimension being the cleaned
+and/or weighted spectra, the second element being the uncleaned and
+unweighted spectra, and the third element being an estimate of the sigma
+of each pixel in the extracted spectrum.  Currently the sigma data is not
+used by any other tasks and is only for reference.
+.LP
+The initial step of finding the fiber spectra in the aperture reference
+image consists of identifying the peaks in a cut across the dispersion,
+eliminating those which are closer to each other than the \f(CWminsep\fR
+distance, and then keeping the specified \f(CWnfibers\fR highest peaks.  The
+centers of the profiles are determined using the \fBcenter1d\fR algorithm
+which uses the \f(CWwidth\fR parameter.
+.LP
+Apertures are then assigned to each spectrum.  The initial edges of the
+aperture relative to the center are defined by the \f(CWlower\fR and
+\f(CWupper\fR parameters.
+.LP
+The initial apertures are the same for all spectra but they can each be
+automatically resized.  The automatic resizing sets the aperture limits
+at a fraction of the peak relative to the interfiber minimum.
+The default \f(CWylevel\fR is to resize the apertures to 5% of the peak.
+See the description for the task \fBapresize\fR for further details.
+.LP
+The user is given the opportunity to graphically review and adjust the
+aperture definitions.  This is recommended
+and it is fundamentally important that the correct aperture/beam numbers
+be associated with the proper fibers;
+otherwise the spectrum
+identifications will not be for the objects they say.  An important command in
+this regard is the 'o' key which allows reordering the identifications.
+This is required if the first
+fiber is actually missing since the initial assignment begins with the
+first spectrum found.  The
+aperture editor is a very powerful tool and is described in detail as
+\fBapedit\fR.
+.LP
+The next set of parameters control the tracing and function fitting of the
+aperture reference positions along the dispersion direction.  The position
+of a spectrum across the dispersion is determined by the centering
+algorithm (see \fBcenter1d\fR) at a series of evenly spaced steps, given by
+the parameter \f(CWt_step\fR, along the dispersion.  The step size should be
+fine enough to follow position changes but it is not necessary to measure
+every point.  The fitted points may jump around a little bit due to noise
+and cosmic rays even when summing a number of lines.  Thus, a smooth
+function is fit.  The function type, order, and iterative rejection of
+deviant points is controlled by the other trace parameters.  For more
+discussion consult the help pages for \fBaptrace\fR and \fBicfit\fR.  The
+default is to fit a cubic spline of three pieces with a single iteration of
+3 sigma rejection.
+.LP
+The actual extraction of the spectra by summing across the aperture at each
+point along the dispersion is controlled by the next set of parameters.
+The default extraction simply sums the pixels using partial pixels at the
+ends.  The options allow selection of a weighted sum based on a Poisson
+variance model using the \f(CWreadnoise\fR and \f(CWgain\fR detector
+parameters.  Note that if the \f(CWclean\fR option is selected the variance
+weighted extraction is used regardless of the \f(CWweights\fR parameter.  The
+sigma thresholds for cleaning are also set in the \fBparams\fR parameters.
+For more on the variance weighted extraction and cleaning see
+\fBapvariance\fR and \fBapprofiles\fR as well as \fBapsum\fR.
+.LP
+The last parameter, \f(CWnsubaps\fR, is used only in special cases when it is
+desired to subdivide the fiber profiles into subapertures prior to
+dispersion correction.  After dispersion correction the subapertures are
+then added together.  The purpose of this is to correct for wavelength
+shifts across a fiber.
+.NH 2
+Scattered Light Subtraction
+.LP
+Scattered light may be subtracted from the input two dimensional image as
+the first step.  This is done using the algorithm described in
+\fBapscatter\fR.  This can be important if there is significant scattered
+light since the flat field/throughput correction will otherwise be
+incorrect.  The algorithm consists of fitting a function to the data
+outside the defined apertures by a specified \fIbuffer\fR at each line or
+column across the dispersion.  The function fitting parameters are the same
+at each line.  Because the fitted functions are independent at each line or
+column a second set of one dimensional functions are fit parallel to the
+dispersion using the evaluated fit values from the cross-dispersion step.
+This produces a smooth scattered light surface which is finally subtracted
+from the input image.  Again the function fitting parameters are the
+same at each line or column though they may be different than the parameters
+used to fit across the dispersion.
+.LP
+The first time the task is run with a particular flat field (or aperture
+reference image if no flat field is used) the scattered light fitting
+parameters are set interactively using that image.  The interactive step
+selects a particular line or column upon which the fitting is done
+interactively with the \fBicfit\fR commands.  A query is first issued
+which allows skipping this interactive stage.  Note that the interactive
+fitting is only for defining the fitting functions and orders.  When
+the graphical \fBicfit\fR fitting is exited (with 'q') there is a second prompt
+allowing you to change the buffer distance (in the first cross-dispersion
+stage) from the apertures, change the line/column, or finally quit.
+.LP
+The initial fitting parameters and the final set parameters are recorded
+in the \fBapscat1\fR and \fBapscat2\fR hidden parameter sets.  These
+parameters are then used automatically for every subsequent image
+which is scattered light corrected.
+.LP
+The scattered light subtraction modifies the input 2D images.  To preserve
+the original data a copy of the original image is made with the same
+root name and the word "noscat" appended.  The scattered light subtracted
+images will have the header keyword "APSCATTE" which is how the task
+avoids repeating the scattered light subtraction during any reprocessing.
+However if the \fIredo\fR option is selected the scattered light subtraction
+will also be redone by first restoring the "noscat" images to the original
+input names.
+.NH 2
+Flat Field and Fiber Throughput Corrections
+.LP
+Flat field corrections may be made during the basic CCD processing; i.e.
+direct division by the two dimensional flat field observation.  In that
+case do not specify a flat field spectrum; use the null string "".  The
+\fBdoargus\fR task provides an alternative flat field response correction
+based on division of the extracted object spectra by the extracted flat field
+spectra.  A discussion of the theory and merits of flat fielding directly
+verses using the extracted spectra will not be made here.  The
+\fBdoargus\fR flat fielding algorithm is the \fIrecommended\fR method for
+flat fielding since it works well and is not subject to the many problems
+involved in two dimensional flat fielding.
+.LP
+In addition to correcting for pixel-to-pixel response the flat field step
+also corrects for differences in the fiber throughput.  Thus, even if the
+pixel-to-pixel flat field corrections have been made in some other way it
+is desirable to use a sky or dome flat observation for determining a fiber
+throughput correction.  Alternatively, a separately derived throughput
+file may be specified.  This file consists of the aperture numbers
+(the same as used for the aperture reference) and relative throughput
+numbers.
+.LP
+The first step is extraction of the flat field spectrum, if specified,
+using the reference apertures.  Only one flat field is allowed so if
+multiple flat fields are required the data must be reduced in groups.
+After extraction one or more corrections are applied.  If the \f(CWfitflat\fR
+option is selected (the default) the extracted flat field spectra are
+averaged together and a smooth function is fit.  The default fitting
+function and order are given by the parameters \f(CWf_function\fR and
+\f(CWf_order\fR.  If the parameter \f(CWf_interactive\fR is "yes" then the
+fitting is done interactively using the \fBfit1d\fR task which uses the
+\fBicfit\fR interactive fitting commands.
+.LP
+The fitted function is divided into the individual flat field spectra to
+remove the basic shape of the spectrum while maintaining the relative
+individual pixel responses and any fiber to fiber differences.  This step
+avoids introducing the flat field spectrum shape into the object spectra
+and closely preserves the object counts.
+.LP
+If a throughput image is available (an observation of blank sky
+usually at twilight) it is extracted.  If no flat field is used the average
+signal through each fiber is computed and this becomes the response
+normalization function.  Note that a dome flat may be used in place of a
+sky in the sky flat field parameter for producing throughput only
+corrections.  If a flat field is specified then each sky spectrum is
+divided by the appropriate flat field spectrum.  The total counts through
+each fiber are multiplied into the flat field spectrum thus making the sky
+throughput of each fiber the same.  This correction is important if the
+illumination of the fibers differs between the flat field source and the
+sky.  Since only the total counts are required the sky or dome flat field
+spectra need not be particularly strong though care must be taken to avoid
+objects.
+.LP
+Instead of a sky flat or other throughput image a separately derived
+throughput file may be used.  It may be used with or without a
+flat field.
+.LP
+The final step is to normalize the flat field spectra by the mean counts of
+all the fibers.  This normalization step is simply to preserve the average
+counts of the extracted object and arc spectra after division by the
+response spectra.  The final relative throughput values are recorded in the
+log and possibly printed on the terminal.
+.LP
+These flat field response steps and algorithm are available as a separate
+task called \fBmsresp1d\fR.
+.NH 2
+Dispersion Correction
+.LP
+Dispersion corrections are applied to the extracted spectra if the
+\fBdispcor\fR parameter is set.  This can be a complicated process which
+the \fBdoargus\fR task tries to simplify for you.  There are three basic
+steps involved; determining the dispersion functions relating pixel
+position to wavelength, assigning the appropriate dispersion function to a
+particular observation, and resampling the spectra to evenly spaced pixels
+in wavelength.
+.LP
+The comparison arc spectra are used to define dispersion functions for the
+fibers using the tasks \fBautoidentify\fR and \fBreidentify\fR.  The
+interactive \fBautoidentify\fR task is only used on the central fiber of the
+first arc spectrum to define the basic reference dispersion solution from
+which all other fibers and arc spectra are automatically derived using
+\fBreidentify\fR. \fBAutoidentify\fR attempts to automatically identify
+the arc lines using the \fIcrval\fR and \fIcdelt\fR parameters.  Whether or
+not it is successful the user is presented with the interactive
+identification graph.  The automatic identifications can be reviewed and a
+new solution or corrections to the automatic solution may be performed.
+.LP
+The set of arc dispersion function parameters are from \fBautoidentify\fR and
+\fBreidentify\fR.  The parameters define a line list for use in
+automatically assigning wavelengths to arc lines, a parameter controlling
+the width of the centering window (which should match the base line
+widths), the dispersion function type and order, parameters to exclude bad
+lines from function fits, and parameters defining whether to refit the
+dispersion function, as opposed to simply determining a zero point shift,
+and the addition of new lines from the line list when reidentifying
+additional arc spectra.  The defaults should generally be adequate and the
+dispersion function fitting parameters may be altered interactively.  One
+should consult the help for the two tasks for additional details of these
+parameters and the operation of \fBautoidentify\fR.
+.LP
+Generally, taking a number of comparison arc lamp exposures interspersed
+with the program spectra is sufficient to accurately dispersion calibrate
+Argus spectra. Dispersion functions are
+determined independently for each fiber of each arc image and then assigned
+to the matching fibers in the program object observations.  The assignment
+consists of selecting one or two arc images to calibrate each object
+image.
+.LP
+However, there is another calibration option which may be of interest.
+This option uses auxiliary line spectra, such as from dome lights or night
+sky lines, to monitor wavelength zero point shifts which are added to the
+basic dispersion function derived from a single reference arc.  Initially
+one of the auxiliary fiber spectra is plotted interactively by
+\fBidentify\fR with the reference dispersion function for the appropriate
+fiber.  The user marks one or more lines which will be used to compute zero
+point wavelength shifts in the dispersion functions automatically.  In this
+case it is auxiliary arc images which are assigned to particular objects.
+.LP
+The arc or auxiliary line image assignments may be done either explicitly with
+an arc assignment
+table (parameter \f(CWarctable\fR) or based on a header parameter.  The task
+used is \fBrefspectra\fR and the user should consult this task if the
+default behavior is not what is desired.  The default is to interpolate
+linearly between the nearest arcs based on the Julian date (corrected to
+the middle of the exposure).  The Julian date and a local Julian day number
+(the day number at local noon) are computed automatically by the task
+\fBsetjd\fR and recorded in the image headers under the keywords JD and
+LJD.  In addition the universal time at the middle of the exposure, keyword
+UTMIDDLE, is computed by the task \fBsetairmass\fR and this may also be used
+for ordering the arc and object observations.
+.LP
+An optional step is to use sky lines in the spectra to compute a zeropoint
+dispersion shift that will align the sky lines.  This may improve sky
+subtraction if the illumination is not the same between the arc calibration
+and the sky.  When selected the object spectrum is dispersion corrected
+using a non-linear dispersion function to avoid resampling the spectrum.
+The sky lines are then reidentified in wavelength space from a template
+list of sky lines.  The mean shift in the lines for each fiber relative to
+the template in that fiber is computed to give the zeropoint shift.  The
+database file is created when the first object is extracted.  You are asked
+to mark the sky lines in one fiber and then the lines are automatically
+reidentified in all other fibers.  Note that this technique requires the
+sky lines be found in all fibers.
+.LP
+The last step of dispersion correction (resampling the spectrum to evenly
+spaced pixels in wavelength) is optional and relatively straightforward.
+If the \f(CWlinearize\fR parameter is no then the spectra are not resampled
+and the nonlinear dispersion information is recorded in the image header.
+Other IRAF tasks (the coordinate description is specific to IRAF) will use
+this information whenever wavelengths are needed.  If linearizing is
+selected a linear dispersion relation, either linear in the wavelength or
+the log of the wavelength, is defined once and applied to every extracted
+spectrum.  The resampling algorithm  parameters allow selecting the
+interpolation function type, whether to conserve flux per pixel by
+integrating across the extent of the final pixel, and whether to linearize
+to equal linear or logarithmic intervals.  The latter may be appropriate
+for radial velocity studies.  The default is to use a fifth order
+polynomial for interpolation, to conserve flux, and to not use logarithmic
+wavelength bins.  These parameters are described fully in the help for the
+task \fBdispcor\fR which performs the correction.  The interpolation
+function options and the nonlinear dispersion coordinate system is
+described in the help topic \fBonedspec.package\fR.
+.NH 2
+Sky Subtraction
+.LP
+Sky subtraction is selected with the \f(CWskysubtract\fR processing option.
+The sky spectra are selected by their aperture and beam numbers.
+If the \f(CWskyedit\fR
+option is selected the sky spectra are plotted using the task
+\fBspecplot\fR.  By default they are superposed to allow identifying
+spectra with unusually high signal due to object contamination.  To
+eliminate a sky spectrum from consideration point at it with the cursor and
+type 'd'.  The last deleted spectrum may be undeleted with 'e'.  This
+allows recovery of incorrect or accidental deletions.
+.LP
+If the combining option is "none" then the sky and object fibers are
+paired and one sky is subtracted from one object and the saved sky will
+be the individual sky fiber spectra.
+.LP
+However, the usual
+case is to combine the individual skys into a single master sky spectrum
+which is then subtracted from each object spectrum.
+The sky combining algorithm parameters define how the individual sky fiber
+spectra, after interactive editing, are combined before subtraction from
+the object fibers.  The goals of combining are to reduce noise, eliminate
+cosmic-rays, and eliminate fibers with inadvertent objects.  The common
+methods for doing this to use a median and/or a special sigma clipping
+algorithm (see \fBscombine\fR for details).  The scale
+parameter determines whether the individual skys are first scaled to a
+common mode.  The scaling should be used if the throughput is uncertain,
+but in that case you probably did the wrong thing in the throughput
+correction.  If the sky subtraction is done interactively, i.e. with the
+\f(CWskyedit\fR option selected, then after selecting the spectra to be
+combined a query is made for the combining algorithm.  This allows
+modifying the default algorithm based on the number of sky spectra
+selected since the "avsigclip" rejection algorithm requires at least
+three spectra.
+.LP
+The combined sky spectrum is subtracted from only those spectra specified
+by the object aperture and beam numbers.  Other spectra
+are retained unchanged.  One may include the sky spectra as
+object spectra to produce residual sky spectra for analysis.  The combined
+master sky spectra may be saved if the \f(CWsaveskys\fR parameter is set.
+The saved sky is given the name of the object spectrum with the prefix
+"sky".
+.NH
+References
+.NH 2
+IRAF Introductory References
+.LP
+Work is underway on a new introductory guide to IRAF.  Currently, the
+work below is the primary introduction.
+.IP
+P. Shames and D. Tody, \fIA User's Introduction to the IRAF Command
+Language\fR, Central Computer Services, NOAO, 1986.
+.NH 2
+CCD Reductions
+.IP
+F. Valdes, \fIThe IRAF CCD Reduction Package -- CCDRED\fR, Central
+Computer Services, NOAO, 1987.
+.IP
+F. Valdes, \fIUser's Guide to the CCDRED Package\fR, Central
+Computer Services, NOAO, 1988.  Also on-line as \f(CWhelp ccdred.guide\fR.
+.IP
+P. Massey, \fIA User's Guide to CCD Reductions with IRAF\fR, Central
+Computer Services, NOAO, 1989.
+.NH 2
+Aperture Extraction Package
+.IP
+F. Valdes, \fIThe IRAF APEXTRACT Package\fR, Central Computer Services,
+NOAO, 1987 (out-of-date).
+.NH 2
+Task Help References
+.LP
+Each task in the \fBargus\fR package and tasks used by \fBdoargus\fR have
+help pages describing the parameters and task in some detail.  To get
+on-line help type
+.V1
+
+cl> help \fItaskname\fR
+
+.V2
+The output of this command can be piped to \fBlprint\fR to make a printed
+copy.
+
+.V1
+      apall - Extract 1D spectra (all parameters in one task)
+  apdefault - Set the default aperture parameters
+     apedit - Edit apertures interactively
+     apfind - Automatically find spectra and define apertures
+ aprecenter - Recenter apertures
+   apresize - Resize apertures
+      apsum - Extract 1D spectra
+    aptrace - Trace positions of spectra
+
+      bplot - Batch plots of spectra
+  continuum - Fit the continuum in spectra
+    dispcor - Dispersion correct spectra
+     dopcor - Doppler correct spectra
+   identify - Identify features in spectrum for dispersion solution
+   msresp1d - Create 1D response spectra from flat field and sky spectra
+ refspectra - Assign wavelength reference spectra to other spectra
+ reidentify - Automatically identify features in spectra
+ sapertures - Set or change aperture header information
+     sarith - Spectrum arithmetic
+   scombine - Combine spectra having different wavelength ranges
+      scopy - Select and copy apertures in different spectral formats
+ setairmass - Compute effective airmass and middle UT for an exposure
+      setjd - Compute and set Julian dates in images
+      slist - List spectrum header parameters
+   specplot - Stack and plot multiple spectra
+      splot - Preliminary spectral plot/analysis
+
+    doargus - Process ARGUS spectra
+      demos - Demonstrations and tests
+
+	    Additional help topics
+
+   onedspec.package - Package parameters and general description of package
+  apextract.package - Package parameters and general description of package
+ approfiles - Profile determination algorithms
+ apvariance - Extractions, variance weighting, cleaning, and noise model
+   center1d - One dimensional centering algorithm
+      icfit - Interactive one dimensional curve fitting
+.V2
+.SH
+Appendix A:  DOARGUS Parameters
+.LP
+.nr PS 8
+.nr VS 10
+objects
+.LS
+List of object spectra to be processed.  Previously processed spectra are
+ignored unless the \f(CWredo\fR flag is set or the \f(CWupdate\fR flag is set and
+dependent calibration data has changed.  Extracted spectra are ignored.
+.LE
+apref = ""
+.LS
+Aperture reference spectrum.  This spectrum is used to define the basic
+extraction apertures and is typically a flat field spectrum.
+.LE
+flat = "" (optional)
+.LS
+Flat field spectrum.  If specified the one dimensional flat field spectra
+are extracted and used to make flat field calibrations.  If a separate
+throughput file or image is not specified the flat field is also used
+for computing a fiber throughput correction.
+.LE
+throughput = "" (optional)
+.LS
+Throughput file or image.  If an image is specified, typically a blank sky
+observation, the total flux through each fiber is used to correct for fiber
+throughput.  If a file consisting of lines with the aperture number and
+relative throughput is specified then the fiber throughput will be
+corrected by those values.  If neither is specified but a flat field image
+is given it is used to compute the throughput.
+.LE
+arcs1 = "" (at least one if dispersion correcting)
+.LS
+List of primary arc spectra.  These spectra are used to define the dispersion
+functions for each fiber apart from a possible zero point correction made
+with secondary shift spectra or arc calibration fibers in the object spectra.
+One fiber from the first spectrum is used to mark lines and set the dispersion
+function interactively and dispersion functions for all other fibers and
+arc spectra are derived from it.
+.LE
+arcs2 = "" (optional)
+.LS
+List of optional shift arc spectra.  Features in these secondary observations
+are used to supply a wavelength zero point shift through the observing
+sequence.  One type of observation is dome lamps containing characteristic
+emission lines.
+.LE
+arctable = "" (optional) (refspectra)
+.LS
+Table defining arc spectra to be assigned to object
+spectra (see \fBrefspectra\fR).  If not specified an assignment based
+on a header parameter, \f(CWparams.sort\fR, such as the observation time is made.
+.LE
+
+readnoise = "0." (apsum)
+.LS
+Read out noise in photons.  This parameter defines the minimum noise
+sigma.  It is defined in terms of photons (or electrons) and scales
+to the data values through the gain parameter.  A image header keyword
+(case insensitive) may be specified to get the value from the image.
+.LE
+gain = "1." (apsum)
+.LS
+Detector gain or conversion factor between photons/electrons and
+data values.  It is specified as the number of photons per data value.
+A image header keyword (case insensitive) may be specified to get the value
+from the image.
+.LE
+datamax = INDEF (apsum.saturation)
+.LS
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the flat field or
+arc spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.LE
+fibers = 48 (apfind)
+.LS
+Number of fibers.  This number is used during the automatic definition of
+the apertures from the aperture reference spectrum.  It is best if this
+reflects the actual number of fibers which may be found in the aperture
+reference image.  Note that Argus fibers which are unassigned will still
+contain enough light for identification and the aperture identification
+table will be used to eliminate the unassigned fibers.  The interactive
+review of the aperture assignments allows verification and adjustments
+to the automatic aperture definitions.
+.LE
+width = 6. (apedit)
+.LS
+Approximate base full width of the fiber profiles.  This parameter is used
+for the profile centering algorithm.
+.LE
+minsep = 8. (apfind)
+.LS
+Minimum separation between fibers.  Weaker spectra or noise within this
+distance of a stronger spectrum are rejected.
+.LE
+maxsep = 10. (apfind)
+.LS
+Maximum separation between adjacent fibers.  This parameter
+is used to identify missing fibers.  If two adjacent spectra exceed this
+separation then it is assumed that a fiber is missing and the aperture
+identification assignments will be adjusted accordingly.
+.LE
+apidtable = "" (apfind)
+.LS
+Aperture identification table.  This may be either a text file or an
+image.  A text file contains the fiber number, beam number defining object
+(1), sky (0), and arc (2) fibers, and a object title.  An image contains
+the keywords SLFIBnnn with string value consisting of the fiber number,
+beam number, optional right ascension and declination, and an object
+title.  Unassigned and broken fibers (beam of -1)
+should be included in this list since they will automatically be excluded.
+.LE
+crval = INDEF, cdelt = INDEF (autoidentify)
+.LS
+These parameters specify an approximate central wavelength and dispersion.
+They may be specified as numerical values, INDEF, or image header keyword
+names whose values are to be used.
+If both these parameters are INDEF then the automatic identification will
+not be done.
+.LE
+objaps = "", skyaps = "2x2"
+.LS
+List of object and sky aperture numbers.  These are used to
+identify object and sky
+apertures for sky subtraction.  Note sky apertures may be identified as
+both object and sky if one wants to subtract the mean sky from the
+individual sky spectra.  Because the fibers typically alternate
+sky and object the default is to define the sky apertures by their
+aperture numbers and select both object and sky fibers for sky subtraction.
+.LE
+objbeams = "", skybeams = ""
+.LS
+List of object and sky beam numbers.
+The beam numbers are typically the same as the aperture numbers unless
+set in the \fIapidtable\fR.
+.LE
+
+scattered = no (apscatter)
+.LS
+Smooth and subtracted scattered light from the object and flat field
+images.  This operation consists of fitting independent smooth functions
+across the dispersion using data outside the fiber apertures and then
+smoothing the individual fits along the dispersion.  The initial
+flat field, or if none is given the aperture reference image, are
+done interactively to allow setting the fitting parameters.  All
+subsequent subtractions use the same fitting parameters.
+.LE
+fitflat = yes (flat1d)
+.LS
+Fit the composite flat field spectrum by a smooth function and divide each
+flat field spectrum by this function?  This operation removes the average
+spectral signature of the flat field lamp from the sensitivity correction to
+avoid modifying the object fluxes.
+.LE
+clean = yes (apsum)
+.LS
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction and requires reasonably good values
+for the readout noise and gain.  In addition the datamax parameters
+can be useful.
+.LE
+dispcor = yes
+.LS
+Dispersion correct spectra?  Depending on the \f(CWparams.linearize\fR
+parameter this may either resample the spectra or insert a dispersion
+function in the image header.
+.LE
+skyalign = no
+.LS
+Align sky lines?  If yes then for the first object spectrum you are asked
+to mark one or more sky lines to use for alignment.  Then these lines will
+be found in all spectra and an average zeropoint shift computed and applied
+to the dispersion solution to align these lines.  Note that this assumes
+the sky lines are seen in all fibers.
+.LE
+skysubtract = yes
+.LS
+Subtract sky from the object spectra?  If yes the sky spectra are combined
+and subtracted from the object spectra as defined by the object and sky
+aperture/beam parameters.
+.LE
+skyedit = yes
+.LS
+Overplot all the sky spectra and allow contaminated sky spectra to be
+deleted?
+.LE
+saveskys = yes
+.LS
+Save the combined sky spectrum?  If no then the sky spectrum will be
+deleted after sky subtraction is completed.
+.LE
+splot = no
+.LS
+Plot the final spectra with the task \fBsplot\fR?
+.LE
+redo = no
+.LS
+Redo operations previously done?  If no then previously processed spectra
+in the objects list will not be processed (unless they need to be updated).
+.LE
+update = yes
+.LS
+Update processing of previously processed spectra if aperture, flat
+field, or dispersion reference definitions are changed?
+.LE
+batch = no
+.LS
+Process spectra as a background or batch job provided there are no interactive
+options (\f(CWskyedit\fR and \f(CWsplot\fR) selected.
+.LE
+listonly = no
+.LS
+List processing steps but don't process?
+.LE
+
+params = "" (pset)
+.LS
+Name of parameter set containing additional processing parameters.  The
+default is parameter set \fBparams\fR.  The parameter set may be examined
+and modified in the usual ways (typically with "epar params" or ":e params"
+from the parameter editor).  Note that using a different parameter file
+is not allowed.  The parameters are described below.
+.LE
+
+.ce
+-- PACKAGE PARAMETERS
+
+Package parameters are those which generally apply to all task in the
+package.  This is also true of \fBdoargus\fR.
+
+dispaxis = 2
+.LS
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.  The default value defers to the
+package parameter of the same name.
+.LE
+observatory = "observatory"
+.LS
+Observatory at which the spectra were obtained if not specified in the
+image header by the keyword OBSERVAT.  For Argus data the image headers
+identify the observatory as "kpno" so this parameter is not used.
+For data from other observatories this parameter may be used
+as describe in \fBobservatory\fR.
+.LE
+interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc)
+.LS
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.V1
+	nearest - nearest neighbor
+	 linear - linear
+	  poly3 - 3rd order polynomial
+	  poly5 - 5th order polynomial
+	spline3 - cubic spline
+	   sinc - sinc function
+.V2
+.LE
+database = "database"
+.LS
+Database (directory) used for storing aperture and dispersion information.
+.LE
+verbose = no
+.LS
+Print verbose information available with various tasks.
+.LE
+logfile = "logfile", plotfile = ""
+.LS
+Text and plot log files.  If a filename is not specified then no log is
+kept.  The plot file contains IRAF graphics metacode which may be examined
+in various ways such as with \fBgkimosaic\fR.
+.LE
+records = ""
+.LS
+Dummy parameter to be ignored.
+.LE
+version = "ARGUS: ..."
+.LS
+Version of the package.
+.LE
+
+.ce
+PARAMS PARAMETERS
+
+The following parameters are part of the \fBparams\fR parameter set and
+define various algorithm parameters for \fBdoargus\fR.
+
+.ce
+--  GENERAL PARAMETERS --
+
+line = INDEF, nsum = 10
+.LS
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, recentering, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.LE
+order = "decreasing" (apfind)
+.LS
+When assigning aperture identifications order the spectra "increasing"
+or "decreasing" with increasing pixel position (left-to-right or
+right-to-left in a cross-section plot of the image).
+.LE
+extras = no (apsum)
+.LS
+Include extra information in the output spectra?  When cleaning or using
+variance weighting the cleaned and weighted spectra are recorded in the
+first 2D plane of a 3D image, the raw, simple sum spectra are recorded in
+the second plane, and the estimated sigmas are recorded in the third plane.
+.LE
+
+.ce
+-- DEFAULT APERTURE LIMITS --
+
+lower = -3., upper = 3. (apdefault)
+.LS
+Default lower and upper aperture limits relative to the aperture center.
+These limits are used when the apertures are first found and may be
+resized automatically or interactively.
+.LE
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+
+ylevel = 0.05 (apresize)
+.LS
+Data level at which to set aperture limits during automatic resizing.
+It is a fraction of the peak relative to a local background.
+.LE
+
+.ce
+-- TRACE PARAMETERS --
+
+t_step = 10 (aptrace)
+.LS
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \f(CWnsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.LE
+t_function = "spline3", t_order = 3 (aptrace)
+.LS
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.LE
+t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+.LS
+Default number of rejection iterations and rejection sigma thresholds.
+.LE
+
+.ce
+-- SCATTERED LIGHT PARAMETERS --
+
+buffer = 1. (apscatter)
+.LS
+Buffer distance from the aperture edges to be excluded in selecting the
+scattered light pixels to be used.
+.LE
+apscat1 = "" (apscatter)
+.LS
+Fitting parameters across the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat1"
+parameter set.
+.LE
+apscat2 = "" (apscatter)
+.LS
+Fitting parameters along the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat2"
+parameter set.
+.LE
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+
+weights = "none" (apsum)
+.LS
+Type of extraction weighting.  Note that if the \f(CWclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+
+"none"
+.LS
+The pixels are summed without weights except for partial pixels at the
+ends.
+.LE
+"variance"
+.LS
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \f(CWgain\fR and \f(CWreadnoise\fR
+parameters.
+.LE
+.LE
+pfit = "fit1d" (apsum) (fit1d|fit2d)
+.LS
+Profile fitting algorithm for cleaning and variance weighted extractions.
+The default is generally appropriate for Argus data but users
+may try the other algorithm.  See \fBapprofiles\fR for further information.
+.LE
+lsigma = 3., usigma = 3. (apsum)
+.LS
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.LE
+nsubaps = 1 (apsum)
+.LS
+During extraction it is possible to equally divide the apertures into
+this number of subapertures.
+.LE
+
+.ce
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --
+
+f_interactive = yes (fit1d)
+.LS
+Fit the composite one dimensional flat field spectrum interactively?
+This is used if \f(CWfitflat\fR is set and a two dimensional flat field
+spectrum is specified.
+.LE
+f_function = "spline3", f_order = 10 (fit1d)
+.LS
+Function and order used to fit the composite one dimensional flat field
+spectrum.  The functions are "legendre", "chebyshev", "spline1", and
+"spline3".  The spline functions are linear and cubic splines with the
+order specifying the number of pieces.
+.LE
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+
+threshold = 10. (autoidentify/identify/reidentify)
+.LS
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.LE
+coordlist = "linelists$ctiohenear.dat" (autoidentify/identify)
+.LS
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelists$".
+.LE
+match = -3. (autoidentify/identify)
+.LS
+The maximum difference for a match between the dispersion function prediction
+value and a wavelength in the coordinate list.
+.LE
+fwidth = 4. (autoidentify/identify)
+.LS
+Approximate full base width (in pixels) of arc lines.
+.LE
+cradius = 10. (reidentify)
+.LS
+Radius from previous position to reidentify arc line.
+.LE
+i_function = "chebyshev", i_order = 3 (autoidentify/identify)
+.LS
+The default function and order to be fit to the arc wavelengths as a
+function of the pixel coordinate.  The functions choices are "chebyshev",
+"legendre", "spline1", or "spline3".
+.LE
+i_niterate = 2, i_low = 3.0, i_high = 3.0 (autoidentify/identify)
+.LS
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.LE
+refit = yes (reidentify)
+.LS
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.LE
+addfeatures = no (reidentify)
+.LS
+Add new features from a line list during each reidentification?
+This option can be used to compensate for lost features from the
+reference solution.  Care should be exercised that misidentified features
+are not introduced.
+.LE
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+
+select = "interp" (refspectra)
+.LS
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+
+average
+.LS
+Average two reference spectra without regard to any sort parameter.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.
+This option is used to assign two reference spectra, with equal weights,
+independent of any sorting parameter.
+.LE
+following
+.LS
+Select the nearest following spectrum in the reference list based on the
+sorting parameter.  If there is no following spectrum use the nearest preceding
+spectrum.
+.LE
+interp
+.LS
+Interpolate between the preceding and following spectra in the reference
+list based on the sorting parameter.  If there is no preceding and following
+spectrum use the nearest spectrum.  The interpolation is weighted by the
+relative distances of the sorting parameter.
+.LE
+match
+.LS
+Match each input spectrum with the reference spectrum list in order.
+This overrides the reference aperture check.
+.LE
+nearest
+.LS
+Select the nearest spectrum in the reference list based on the sorting
+parameter.
+.LE
+preceding
+.LS
+Select the nearest preceding spectrum in the reference list based on the
+sorting parameter.  If there is no preceding spectrum use the nearest following
+spectrum.
+.LE
+.LE
+sort = "jd", group = "ljd" (refspectra)
+.LS
+Image header keywords to be used as the sorting parameter for selection
+based on order and to group spectra.
+A null string, "", or the word "none" may be use to disable the sorting
+or grouping parameters.
+The sorting parameter
+must be numeric but otherwise may be anything.  The grouping parameter
+may be a string or number and must simply be the same for all spectra within
+the same group (say a single night).
+Common sorting parameters are times or positions.
+In \fBdoargus\fR the Julian date (JD) and the local Julian day number (LJD)
+at the middle of the exposure are automatically computed from the universal
+time at the beginning of the exposure and the exposure time.  Also the
+parameter UTMIDDLE is computed.
+.LE
+time = no, timewrap = 17. (refspectra)
+.LS
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.LE
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+
+linearize = yes (dispcor)
+.LS
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling
+If no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data are not interpolated.
+.LE
+log = no (dispcor)
+.LS
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.LE
+flux = yes (dispcor)
+.LS
+Conserve the total flux during interpolation?  If \f(CWno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \f(CWyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.LE
+
+.ce
+-- SKY SUBTRACTION PARAMETERS --
+
+combine = "average" (scombine) (average|median)
+.LS
+Option for combining sky pixels at the same dispersion coordinate after any
+rejection operation.  The options are to compute the  "average" or "median"
+of the pixels.  The median uses the average of the two central
+values when the number of pixels is even.
+.LE
+reject = "none" (scombine) (none|minmax|avsigclip)
+.LS
+Type of rejection operation performed on the pixels which overlap at each
+dispersion coordinate.  The algorithms are discussed in the
+help for \fBscombine\fR.  The rejection choices are:
+
+.V1
+      none - No rejection
+    minmax - Reject the low and high pixels
+ avsigclip - Reject pixels using an averaged sigma clipping algorithm
+.V2
+
+.LE
+scale = "none" (none|mode|median|mean)
+.LS
+Multiplicative scaling to be applied to each spectrum.  The choices are none
+or scale by the mode, median, or mean.  This should not be necessary if the
+flat field and throughput corrections have been properly made. 
+.LE
+
+.ce
+ENVIRONMENT PARAMETERS
+.LP
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
diff --git a/noao/imred/argus/params.par b/noao/imred/argus/params.par
new file mode 100644
index 00000000..72e01ace
--- /dev/null
+++ b/noao/imred/argus/params.par
@@ -0,0 +1,67 @@
+line,i,h,INDEF,,,"Default dispersion line"
+nsum,i,h,10,,,"Number of dispersion lines to sum or median"
+order,s,h,"decreasing","increasing|decreasing",,"Order of apertures"
+extras,b,h,no,,,"Extract sky, sigma, etc.?
+
+-- DEFAULT APERTURE LIMITS --"
+lower,r,h,-3.,,,"Lower aperture limit relative to center"
+upper,r,h,3.,,,"Upper aperture limit relative to center
+
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --"
+ylevel,r,h,0.05,,,"Fraction of peak or intensity for resizing
+
+-- TRACE PARAMETERS --"
+t_step,i,h,10,,,"Tracing step"
+t_function,s,h,"spline3","chebyshev|legendre|spline1|spline3",,"Trace fitting function"
+t_order,i,h,2,,,"Trace fitting function order"
+t_niterate,i,h,1,0,,"Trace rejection iterations"
+t_low,r,h,3.,0.,,"Trace lower rejection sigma"
+t_high,r,h,3.,0.,,"Trace upper rejection sigma
+
+-- SCATTERED LIGHT PARAMETERS --"
+buffer,r,h,1.,0.,,Buffer distance from apertures
+apscat1,pset,h,"",,,Fitting parameters across the dispersion
+apscat2,pset,h,"",,,"Fitting parameters along the dispersion
+
+-- APERTURE EXTRACTION PARAMETERS --"
+weights,s,h,"none","none|variance",,Extraction weights (none|variance)
+pfit,s,h,"fit1d","fit1d|fit2d",,Profile fitting algorithm (fit1d|fit2d)
+lsigma,r,h,3.,,,Lower rejection threshold
+usigma,r,h,3.,,,Upper rejection threshold
+nsubaps,i,h,1,1,,"Number of subapertures
+
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --"
+f_interactive,b,h,yes,,,"Fit flat field interactively?"
+f_function,s,h,"spline3",spline3|legendre|chebyshev|spline1,,"Fitting function"
+f_order,i,h,20,1,,"Fitting function order
+
+-- ARC DISPERSION FUNCTION PARAMETERS --"
+threshold,r,h,10.,0.,,"Minimum line contrast threshold"
+coordlist,f,h,linelists$idhenear.dat,,,"Line list"
+match,r,h,-3.,,,"Line list matching limit in Angstroms"
+fwidth,r,h,4.,,,"Arc line widths in pixels"
+cradius,r,h,10.,,,Centering radius in pixels
+i_function,s,h,"chebyshev","legendre|chebyshev|spline1|spline3",,"Coordinate function"
+i_order,i,h,3,1,,"Order of dispersion function"
+i_niterate,i,h,2,0,,"Rejection iterations"
+i_low,r,h,3.,0.,,"Lower rejection sigma"
+i_high,r,h,3.,0.,,"Upper rejection sigma"
+refit,b,h,yes,,,"Refit coordinate function when reidentifying?"
+addfeatures,b,h,no,,,"Add features when reidentifying?
+
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --"
+select,s,h,"interp",,,"Selection method for reference spectra"
+sort,s,h,"jd",,,"Sort key"
+group,s,h,"ljd",,,"Group key"
+time,b,h,no,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting
+
+-- DISPERSION CORRECTION PARAMETERS --"
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+log,b,h,no,,,"Logarithmic wavelength scale?"
+flux,b,h,yes,,,"Conserve flux?
+
+-- SKY SUBTRACTION PARAMETERS --"
+combine,s,h,"average","average|median",,Type of combine operation
+reject,s,h,"avsigclip","none|minmax|avsigclip",,"Sky rejection option"
+scale,s,h,"none","none|mode|median|mean",,"Sky scaling option"
diff --git a/noao/imred/bias/Revisions b/noao/imred/bias/Revisions
new file mode 100644
index 00000000..6c67e622
--- /dev/null
+++ b/noao/imred/bias/Revisions
@@ -0,0 +1,97 @@
+.help revisions Jun88 noao.imred.bias
+.nf
+noao$imred/bias/colbias.x
+noao$imred/bias/linebias.x
+noao$imred/bias/doc/colbias.hlp
+noao$imred/bias/doc/linebias.hlp
+    The output pixel type is now changed to real rather than preserving
+    the input pixel type.  (3/2/93, Valdes)
+
+=======
+V2.10.2
+=======
+
+noao$imred/bias/colbias.x
+    Valdes, January 6, 1990
+    The graphics device parameter was being ignored and "stdgraph" always
+    opened.
+
+===
+V2.8
+====
+
+noao$imred/bias/colbias.x,linebias.x,colbias.par,linebias.par
+    Davis, October 4, 1988
+    1. The parameters low_reject, high_reject and niterate have been added
+    to the linebias and colbias tasks which then pass them to the icfit
+    package.
+
+noao$imred/bias/linebias.x
+    Valdes, May, 1, 1987
+    1.  The fix of December 3 was slightly wrong.
+	296: ...Memr[buf2+(k-1)*n+i-1] ==> ...Memr[buf2+k*n+i-j]
+    2.  Increased the maximum buffer MAXPIX from 10000 to 100000.
+
+noao$imred/bias/colbias.x
+noao$imred/bias/linebias.x
+    Valdes, January 15, 1986
+    1.  When the bias section consists of just one column or line the
+	dimensionality of the mapped bias decreases.  The code had to be
+	modified to recognize and work properly in this case.
+
+noao$imred/bias/linebias.x
+    Valdes, December, 3, 1986
+    1.  There was a bug in using the median option which gave incorrect
+	results for the bias vector.
+	291: n = min (nx - j - 1, maxn)	==> n = min (nx - j + 1, maxn)
+	296: ...Memr[buf2+(k-1)*n+i-1]	==> ...Memr[buf2+(k-1)*n+i-j]
+
+noao$imred/bias/linebias.x
+    Valdes, October 29, 1986
+    1.  The log information for LINEBIAS identified itself as COLBIAS.
+
+====================================
+Version 2.3 Release, August 18, 1986
+====================================
+
+noao$imred/bias/colbias.x
+noao$imred/bias/linebias.x
+    Valdes, July 3, 1986
+    1.  COLBIAS and LINEBIAS modified to use new ICFIT package.
+
+=========================================
+STScI Pre-release and 1st SUN 2.3 Release
+=========================================
+
+===========
+Release 2.2
+===========
+
+From Valdes Dec 12, 1985:
+
+1.  COLBIAS and LINEBIAS changes to allow taking a median instead of an
+average when generating the 1D bias data.
+------
+From Valdes Dec 11, 1985:
+
+1.  COLBIAS and LINEBIAS changed to use image templates instead of filename
+templates.  This allows use of the concatenation function even though the
+images should not have images sections.
+
+2.  REVS task removed.
+------
+From Valdes Oct 4, 1985:
+
+1.  Colbais and linebias recompiled because of the change in the icfit package
+for low and high rejection and rejection iteration.
+------
+From Valdes Aug 7, 1985:
+
+1.  The task revisions has been added to page package revisions.
+To get the system revisions type system.revisions.
+
+2.  The parameters to linebias and colbias now include control over
+the graphics output device, the graphics input cursor, and multiple logfiles.
+
+3.  Changes have been made to use the "improved" icfit and gtools packages.
+.endhelp
diff --git a/noao/imred/bias/bias.cl b/noao/imred/bias/bias.cl
new file mode 100644
index 00000000..18624a2c
--- /dev/null
+++ b/noao/imred/bias/bias.cl
@@ -0,0 +1,8 @@
+#{ BIAS -- Bias Package
+
+package bias
+
+task	colbias,
+	linebias	= biasdir$x_bias.e
+
+clbye
diff --git a/noao/imred/bias/bias.hd b/noao/imred/bias/bias.hd
new file mode 100644
index 00000000..b55e1b6c
--- /dev/null
+++ b/noao/imred/bias/bias.hd
@@ -0,0 +1,7 @@
+# Help directory for the BIAS package.
+
+$doc = "./doc/"
+
+colbias		hlp=doc$colbias.hlp,	src=colbias.x
+linebias	hlp=doc$linebias.hlp,	src=linebias.x
+revisions	sys=Revisions
diff --git a/noao/imred/bias/bias.men b/noao/imred/bias/bias.men
new file mode 100644
index 00000000..7bf225d4
--- /dev/null
+++ b/noao/imred/bias/bias.men
@@ -0,0 +1,2 @@
+        colbias - Fit and subtract an average column bias
+       linebias - Fit and subtract an average line bias
diff --git a/noao/imred/bias/bias.par b/noao/imred/bias/bias.par
new file mode 100644
index 00000000..4bdb4e20
--- /dev/null
+++ b/noao/imred/bias/bias.par
@@ -0,0 +1,3 @@
+# BIAS package parameter file.
+
+version,s,h,"May 1985"
diff --git a/noao/imred/bias/colbias.par b/noao/imred/bias/colbias.par
new file mode 100644
index 00000000..8c3ba4b3
--- /dev/null
+++ b/noao/imred/bias/colbias.par
@@ -0,0 +1,16 @@
+# COLBIAS -- Subtract a column bias
+
+input,s,a,,,,Input images
+output,s,a,,,,Output images
+bias,s,h,"[]",,,Bias section
+trim,s,h,"[]",,,Trim section
+median,b,h,no,,,Use median instead of average in column bias?
+interactive,b,h,yes,,,Interactive?
+function,s,h,"spline3","spline3|legendre|chebyshev|spline1",,Fitting function
+order,i,h,1,1,,Order of fitting function
+low_reject,r,h,3.0,,,Low sigma rejection factor
+high_reject,r,h,3.0,,,High sigma rejection factor
+niterate,i,h,1,,,Number of rejection iterations
+logfiles,s,h,"",,,Log files
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
diff --git a/noao/imred/bias/colbias.x b/noao/imred/bias/colbias.x
new file mode 100644
index 00000000..f7aac840
--- /dev/null
+++ b/noao/imred/bias/colbias.x
@@ -0,0 +1,308 @@
+include	<imhdr.h>
+include	<imio.h>
+include <pkg/gtools.h>
+include	<pkg/xtanswer.h>
+
+# COLBIAS -- Remove line by line bias from images.
+#
+# A one dimensional bias vector is extracted from the bias columns.
+# A function is fit to the bias vector and the function is subtracted
+# from the image lines.  A trim section may be specified to output
+# only a part of the bias subtracted image.
+
+# Control procedure for mapping the images.
+#
+# The input and output images are given by image templates.  The
+# number of output images must match the number of input images.  Image
+# sections are not allowed.  The output image may be the same as the input
+# image.
+
+procedure colbias ()
+
+int	listin				# List of input images
+int	listout				# List of output images
+int	logfiles			# List of log files
+char	biassec[SZ_FNAME]		# Bias section
+char	trimsec[SZ_FNAME]		# Trim section
+int	median				# Use median of bias section?
+int	interactive			# Interactive?
+
+char	function[SZ_LINE]		# Curve fitting function
+int	order				# Order of curve fitting function
+
+char	image[SZ_FNAME]
+char	input[SZ_FNAME]
+char	biasimage[SZ_FNAME]
+char	output[SZ_FNAME]
+char	logfile[SZ_FNAME]
+char	original[SZ_FNAME]
+char	title[SZ_LINE]
+
+int	logfd
+pointer	in, bias, out, ic, gt
+
+int	clgeti(), clpopnu(), clgfil(), open(), gt_init(), nowhite()
+int	imtopen(), imtlen(), imtgetim(), btoi()
+bool	clgetb()
+long	clktime()
+pointer	immap()
+real	clgetr()
+
+begin
+	# Get input and output lists and check that the number of images
+	# are the same.
+
+	call clgstr ("input", title, SZ_LINE)
+	listin = imtopen (title)
+	call clgstr ("output", title, SZ_LINE)
+	listout = imtopen (title)
+	if (imtlen (listin) != imtlen (listout)) {
+	    call imtclose (listin)
+	    call imtclose (listout)
+	    call error (0, "Input and output image lists do not match")
+	}
+
+	# Get the bias and trim sections.
+
+	call clgstr ("bias", biassec, SZ_FNAME)
+	call clgstr ("trim", trimsec, SZ_FNAME)
+	if (nowhite (biassec, biassec, SZ_FNAME) == 0)
+	    ;
+	if (nowhite (trimsec, trimsec, SZ_FNAME) == 0)
+	    ;
+	median = btoi (clgetb ("median"))
+
+	# Determine if the task is interactive.  If not set the interactive
+	# flag to always no.
+
+	if (clgetb ("interactive"))
+	    interactive = YES
+	else
+	    interactive = ALWAYSNO
+
+	# Initialize the curve fitting package.
+
+	call ic_open (ic)
+	call clgstr ("function", function, SZ_LINE)
+	call ic_pstr (ic, "function", function)
+	order = clgeti ("order")
+	call ic_puti (ic, "order", order)
+	call ic_putr (ic, "low", clgetr ("low_reject"))
+	call ic_putr (ic, "high", clgetr ("high_reject"))
+	call ic_puti (ic, "niterate", clgeti ("niterate"))
+	call ic_pstr (ic, "xlabel", "Line")
+	call ic_pstr (ic, "ylabel", "Bias")
+
+	gt = gt_init ()
+	call gt_sets (gt, GTTYPE, "line")
+
+	# Get the log files.
+
+	logfiles = clpopnu ("logfiles")
+
+	# For each input and output image map the bias image, the
+	# trimmed input image, and the output image.  Use a temporary
+	# image header for overwritting the input image.
+
+	while ((imtgetim (listin, image, SZ_FNAME) != EOF) &&
+	    (imtgetim (listout, output, SZ_FNAME) != EOF)) {
+
+	    call sprintf (biasimage, SZ_FNAME, "%s%s")
+		call pargstr (image)
+		call pargstr (biassec)
+	    call sprintf (input, SZ_FNAME, "%s%s")
+		call pargstr (image)
+		call pargstr (trimsec)
+
+	    in = immap (input, READ_ONLY, 0)
+	    bias = immap (biasimage, READ_ONLY, 0)
+	    call xt_mkimtemp (image, output, original, SZ_FNAME)
+	    out = immap (output, NEW_COPY, in)
+	    IM_PIXTYPE(out) = TY_REAL
+
+	    call sprintf (title, SZ_LINE, "colbias %s")
+		call pargstr (image)
+	    call xt_answer (title, interactive)
+	    call gt_sets (gt, GTTITLE, title)
+
+	    # Enter log header.
+
+	    while (clgfil (logfiles, logfile, SZ_FNAME) != EOF) {
+		logfd = open (logfile, APPEND, TEXT_FILE)
+	        call cnvtime (clktime (0), title, SZ_LINE)
+	        call fprintf (logfd, "\nCOLBIAS:  %s\n")
+		    call pargstr (title)
+		call fprintf (logfd, "input = %s\noutput = %s\nbias = %s\n")
+		    call pargstr (input)
+		    call pargstr (output)
+		    call pargstr (biasimage)
+		if (median == YES)
+		    call fprintf (logfd, "Median of bias section used.\n")
+		call close (logfd)
+	    }
+	    call clprew (logfiles)
+
+	    call cb_colbias (in, bias, out, ic, gt, median, logfiles,
+		interactive)
+
+	    call imunmap (in)
+	    call imunmap (bias)
+	    call imunmap (out)
+	    call xt_delimtemp (output, original)
+	}
+
+	call ic_closer (ic)
+	call gt_free (gt)
+	call clpcls (logfiles)
+	call imtclose (listin)
+	call imtclose (listout)
+end
+
+
+# CB_COLBIAS -- Get an average column bias vector from the bias image.
+# Fit a function to the bias vector and subtract it from the input image
+# to form the output image.  Line coordinates are in terms of the full
+# input image.
+
+procedure cb_colbias (in, bias, out, ic, gt, median, logfiles, interactive)
+
+pointer	in			# Input image pointer
+pointer	bias			# Bias image pointer
+pointer	out			# Output image pointer
+pointer	ic			# ICFIT pointer
+pointer	gt			# GTOOLS pointer
+int	median			# Median of bias section?
+int	logfiles		# List of log files
+int	interactive		# Interactive curve fitting?
+
+char	graphics[SZ_FNAME]	# Graphics output device
+char	logfile[SZ_FNAME]
+int	i, nbias, nx, ny, ydim, yoff, ystep, ylen
+real	y, z
+pointer	cv, gp, sp, ybias, zbias, wts
+
+int	clgfil()
+real	cveval()
+pointer	gopen(), imgl2r(), impl2r()
+
+begin
+	# The bias coordinates are in terms of the full input image because
+	# the input and bias images may have different sections.
+
+	nx = IM_LEN(in, 1)
+	ny = IM_LEN(in, 2)
+
+	ydim = IM_VMAP(in, 2)
+	yoff = IM_VOFF(in, ydim)
+	ystep = IM_VSTEP(in, ydim)
+	ylen = IM_SVLEN(in, ydim)
+
+	# Get the bias vector and set the weights.
+
+	call cb_getcolbias (bias, ybias, zbias, nbias, median)
+	call smark (sp)
+	call salloc (wts, nbias, TY_REAL)
+	call amovkr (1., Memr[wts], nbias)
+
+	# Do the curve fitting using the interactive curve fitting package.
+	# Free memory when the fit is complete.
+
+	call ic_putr (ic, "xmin", 1.)
+	call ic_putr (ic, "xmax", real (ylen))
+	if ((interactive == YES) || (interactive == ALWAYSYES)) {
+	    call clgstr ("graphics", graphics, SZ_FNAME)
+	    gp = gopen (graphics, NEW_FILE, STDGRAPH)
+	    call gt_setr (gt, GTXMIN, 1.)
+	    call gt_setr (gt, GTXMAX, real (ylen))
+	    call icg_fit (ic, gp, "cursor", gt, cv, Memr[ybias], Memr[zbias],
+		Memr[wts], nbias)
+	    call gclose (gp)
+	} else {
+	    call ic_fit (ic, cv, Memr[ybias], Memr[zbias], Memr[wts], nbias,
+		YES, YES, YES, YES)
+	}
+
+	# Log the fitting information.
+
+	while (clgfil (logfiles, logfile, SZ_FNAME) != EOF) {
+	    call ic_show (ic, logfile, gt)
+	    call ic_errors (ic, logfile, cv, Memr[ybias], Memr[zbias],
+		Memr[wts], nbias)
+	}
+	call clprew (logfiles)
+
+	call mfree (ybias, TY_REAL)
+	call mfree (zbias, TY_REAL)
+	call sfree (sp)
+
+	# Subtract the bias function from the input image.
+
+	do i = 1, ny {
+	    y = yoff + i * ystep
+	    z = cveval (cv, y)
+	    call asubkr (Memr[imgl2r(in,i)], z, Memr[impl2r(out,i)], nx)
+	}
+
+	# Free curve fitting memory.
+
+	call cvfree (cv)
+end
+
+
+# CB_GETCOLBIAS -- Get the column bias vector.
+# The ybias line values are in terms of the full image.
+
+procedure cb_getcolbias (bias, ybias, zbias, nbias, median)
+
+pointer	bias			# Bias image pointer
+pointer	ybias, zbias		# Bias vector
+int	nbias			# Number of bias points
+int	median			# Median of bias section?
+
+int	i, nx, ny, ydim, yoff, ystep
+
+real	amedr(), asumr()
+pointer	imgl1r(), imgl2r()
+
+begin
+	# Check for a bias consisting of a single column which is turned
+	# into a 1D image by IMIO.
+	if (IM_NDIM(bias) == 1) {
+	    ny = IM_LEN(bias, 1)
+	    ydim = IM_VMAP(bias, 1)
+	    yoff = IM_VOFF(bias, ydim)
+	    ystep = IM_VSTEP(bias, ydim)
+
+	    nbias = ny
+	    call malloc (ybias, nbias, TY_REAL)
+	    call malloc (zbias, nbias, TY_REAL)
+
+	    do i = 1, nbias
+		Memr[ybias+i-1] = yoff + i * ystep
+	    call amovr (Memr[imgl1r(bias)], Memr[zbias], nbias)
+
+	    return
+	}
+		
+	nx = IM_LEN(bias, 1)
+	ny = IM_LEN(bias, 2)
+	ydim = IM_VMAP(bias, 2)
+	yoff = IM_VOFF(bias, ydim)
+	ystep = IM_VSTEP(bias, ydim)
+	
+	nbias = ny
+	call malloc (ybias, nbias, TY_REAL)
+	call malloc (zbias, nbias, TY_REAL)
+
+	if (median == YES) {
+	    do i = 1, ny {
+	        Memr[ybias+i-1] = yoff + i * ystep
+	        Memr[zbias+i-1] = amedr (Memr[imgl2r(bias,i)], nx)
+	    }
+	} else {
+	    do i = 1, ny {
+	        Memr[ybias+i-1] = yoff + i * ystep
+	        Memr[zbias+i-1] = asumr (Memr[imgl2r(bias,i)], nx) / nx
+	    }
+	}
+end
diff --git a/noao/imred/bias/doc/colbias.hlp b/noao/imred/bias/doc/colbias.hlp
new file mode 100644
index 00000000..a95e4694
--- /dev/null
+++ b/noao/imred/bias/doc/colbias.hlp
@@ -0,0 +1,113 @@
+.help colbias Mar93 noao.imred.bias
+.ih
+NAME
+colbias -- Fit and subtract an average column bias
+.ih
+USAGE	
+.nf
+colbias input output
+.fi
+.ih
+PARAMETERS
+.ls input
+Images to be bias subtracted.  The images may not contain image sections.
+.le
+.ls output
+Output bias subtracted images.  An output images may be the same as its
+matching input image.  The output pixel type will be real regardless
+of the input pixel type.
+.le
+.ls bias = "[]"
+Bias section appended to the input image to define the bias region.
+The default section or an empty string will use the full image.
+.le
+.ls trim = "[]"
+Trim section appended to the input image to define the region to be
+bias subtracted and output.  The default section or an empty string
+will use the full image.
+.le
+.ls median = no
+Take the median of the bias columns?  If no then the bias
+columns are averaged.
+.le
+.ls function = "spline3"
+The function fit to the average bias line.  The functions are "legendre",
+"chebyshev", "spline1", or "spline3".  Abbreviations are allowed.
+.le
+.ls order
+The order (number of terms or number of spline pieces) in the function.
+.le
+.ls low_reject = 3.0
+The low sigma rejection factor.
+.le
+.ls high_reject = 3.0
+The high sigma rejection factor.
+.le
+.ls niterate = 1
+The maximum number of rejection iterations.
+.le
+.ls interactive = yes
+Fit the average bias line interactively?
+.le
+.ls logfiles = ""
+List of log files.  If no file name is given then no log file is kept.
+.le
+.ls graphics = "stdgraph"
+Graphics output device for interactive graphics.
+.le
+.ls cursor = ""
+Graphics cursor input
+.le
+.ih
+DESCRIPTION
+For each input image in the input image list an average or median bias
+column is determined from the bias region.  The bias region is defined by
+the bias section applied to the input image.  A function of the image lines
+is fit to the average bias column.  This function is subtracted from each
+image column in the trim region.  The trim region is defined by the trim
+section applied to the input image.  The bias subtracted and trimmed image
+is output to the output image.  The input and output images may not contain
+sections and the number of images in each list must be the same.
+
+If the interactive flag is set then the user may interactively examine
+and fit the average bias column.  The interactive fitting is done using the
+interactive curve fitting routine (see icfit).  Before each image is
+processed a prompt of the form "colbias image (yes)? " is given.
+A response of yes allows interactive fitting for the specified image
+while a response of no uses the last defined fitting parameters.
+The default value is accepted with a carriage return.  The possible
+responses are "yes", "no", "YES", or "NO".  The capitalized responses
+permanently set the response to yes or no and the prompt is not
+issued again for the remaining images.  Thus, a response of NO processes
+the remaining images non-interactively while a response of YES processes
+the remaining image interactively without prompting.
+.ih
+EXAMPLES
+The bias region for a set of images occupies columns 801 to 832 and lines
+1 to 800.  To subtract the bias and remove the bias region:
+
+.nf
+	cl> colbias.bias = "[801:832,*]"
+	cl> colbias.trim = "[1:800,*]"
+	cl> colbias ccd* ccd*
+	colbias ccd001 (yes)? yes
+	colbias ccd002 (yes)?
+	colbias ccd003 (no)? NO
+.fi
+
+The first two lines set the bias and trim parameters.  These parameters
+could be temporarily set on the command line but generally these parameters
+are only changed when new instruments are used.  The first image
+is interactively fit and the fitting order is change to 2.  The
+second image is examined and the fit found to be acceptable.  All remaining
+image are then fit non-interactively using the same fitting parameters.
+.ih
+REVISIONS
+.ls COLBIAS V2.10.3
+The output pixel type is now real instead of preserving the pixel type
+of the input image.
+.le
+.ih
+SEE ALSO
+icfit
+.endhelp
diff --git a/noao/imred/bias/doc/linebias.hlp b/noao/imred/bias/doc/linebias.hlp
new file mode 100644
index 00000000..6c5d73a5
--- /dev/null
+++ b/noao/imred/bias/doc/linebias.hlp
@@ -0,0 +1,115 @@
+.help linebias Mar93 noao.imred.bias
+.ih
+NAME
+linebias -- Fit and subtract an average line bias
+.ih
+USAGE	
+.nf
+linebias input output
+.fi
+.ih
+PARAMETERS
+.ls input
+Images to be bias subtracted.  The images may not contain image sections.
+.le
+.ls output
+Output bias subtracted images.  An output images may be the same as its
+matching input image.  The output image pixel type will real regardless
+of the input image pixel type.
+.le
+.ls bias = "[]"
+Bias section appended to the input image to define the bias region.
+The default section or an empty string will use the full image.
+.le
+.ls trim = "[]"
+Trim section appended to the input image to define the region to be
+bias subtracted and output.  The default section or an empty string
+will use the full image.
+.le
+.ls median = no
+Take the median of the bias lines?  If no then the bias lines are averaged.
+.le
+.ls function = "spline3"
+The function fit to the average bias line.  The functions are "legendre",
+"chebyshev", "spline1", or "spline3".  Abbreviations are allowed.
+.le
+.ls order
+The order (number of terms or number of spline pieces) in the function.
+.le
+.ls low_reject = 3.0
+The low sigma rejection factor.
+.le
+.ls high_reject = 3.0
+The high sigma rejection factor.
+.le
+.ls niterate = 1
+The maximum number of rejection iterations.
+.le
+.ls interactive = yes
+Fit the average bias line interactively?
+.le
+.ls logfile = ""
+Name of a log file.  If no file name is given then no log file is kept.
+.le
+.ls logfiles = ""
+List of log files.  If no file name is given then no log file is kept.
+.le
+.ls graphics = "stdgraph"
+Graphics output device for interactive graphics.
+.le
+.ls cursor = ""
+Graphics cursor input
+.le
+.ih
+DESCRIPTION
+For each input image in the input image list an average or median bias line
+is determined from the bias region.  The bias region
+is defined by the bias section applied to the input image.  A function of
+the image columns is fit to the average bias line.  This function is subtracted
+from each image line in the trim region.  The trim region is defined by the
+trim section applied to the input image.  The bias subtracted and trimmed
+image is output to the output image.  The input and output images may not
+contain sections and the number of images in each list must be the same.
+
+If the interactive flag is set then the user may interactively examine
+and fit the average bias line.  The interactive fitting is done using the
+interactive curve fitting routine (see icfit).  Before each image is
+processed a prompt of the form "linebias image (yes)? " is given.
+A response of yes allows interactive fitting for the specified image
+while a response of no uses the last defined fitting parameters.
+The default value is accepted with a carriage return.  The possible
+responses are "yes", "no", "YES", or "NO".  The capitalized responses
+permanently set the response to yes or no and the prompt is not
+issued again for the remaining images.  Thus, a response of NO processes
+the remaining images non-interactively while a response of YES processes
+the remaining image interactively without prompting.
+.ih
+EXAMPLES
+The bias region for a set of images occupies columns 1 to 800 and lines
+801 to 832.  To subtract the bias and remove the bias region:
+
+.nf
+	cl> linebias.bias = "[*, 801:832]"
+	cl> linebias.trim = "[*, 1:800]"
+	cl> linebias ccd* ccd*
+	linebias ccd001 (yes)? yes
+	linebias ccd002 (yes)?
+	linebias ccd003 (no)? NO
+.fi
+
+The first two lines set the bias and trim parameters.  These parameters
+could be temporarily set on the command line but generally these parameters
+are only changed when new instruments are used.  The first image
+is interactively fit and the fitting order is change to 2.  The
+second image is examined and the fit found to be acceptable.  All remaining
+image are then fit non-interactively using the same fitting parameters.
+.ih
+REVISIONS
+.ls LINEBIAS V2.10.3
+The output pixel type is now real instead of preserving the pixel type
+of the input image.
+.le
+.ih
+SEE ALSO
+icfit
+.endhelp
diff --git a/noao/imred/bias/linebias.par b/noao/imred/bias/linebias.par
new file mode 100644
index 00000000..a056f02d
--- /dev/null
+++ b/noao/imred/bias/linebias.par
@@ -0,0 +1,16 @@
+# LINEBIAS -- Subtract a line bias
+
+input,s,a,,,,Input images
+output,s,a,,,,Output images
+bias,s,h,"[]",,,Bias section
+trim,s,h,"[]",,,Trim section
+median,b,h,no,,,Use median instead of average in line bias?
+interactive,b,h,yes,,,Interactive?
+function,s,h,"spline3","spline3|legendre|chebyshev|spline1",,Fitting function
+order,i,h,1,1,,Order of fitting function
+low_reject,r,h,3.0,,,Low sigma rejection factor
+high_reject,r,h,3.0,,,High sigma rejection factor
+niterate,i,h,1,,,Number of rejection iterations
+logfiles,s,h,"",,,Log files
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
diff --git a/noao/imred/bias/linebias.x b/noao/imred/bias/linebias.x
new file mode 100644
index 00000000..91d789af
--- /dev/null
+++ b/noao/imred/bias/linebias.x
@@ -0,0 +1,330 @@
+include	<imhdr.h>
+include	<imio.h>
+include <pkg/gtools.h>
+include	<pkg/xtanswer.h>
+
+# LINEBIAS -- Remove column by column bias from images.
+#
+# A one dimensional bias vector is extracted from the bias lines.
+# A function is fit to the bias vector and the function is subtracted
+# from the image columns.  A trim section may be specified to output
+# only a part of the bias subtracted image.
+
+# Control procedure for mapping the images.
+#
+# The input and output images are given by image templates.  The
+# number of output images must match the number of input images.  Image
+# sections are not allowed.  The output image may be the same as the input
+# image.
+
+procedure linebias ()
+
+int	listin				# List of input images
+int	listout				# List of output images
+int	logfiles			# List of log files
+char	biassec[SZ_FNAME]		# Bias section
+char	trimsec[SZ_FNAME]		# Trim section
+int	median				# Median of bias section?
+int	interactive			# Interactive?
+
+char	function[SZ_LINE]		# Curve fitting function
+int	order				# Order of curve fitting function
+
+char	image[SZ_FNAME]
+char	input[SZ_FNAME]
+char	biasimage[SZ_FNAME]
+char	output[SZ_FNAME]
+char	logfile[SZ_FNAME]
+char	original[SZ_FNAME]
+char	title[SZ_LINE]
+
+int	logfd
+pointer	in, bias, out, ic, gt
+
+int	clgeti(), clpopnu(), clgfil(), open(), gt_init(), nowhite()
+int	imtopen(), imtlen(), imtgetim(), btoi()
+bool	clgetb()
+long	clktime()
+pointer	immap()
+real	clgetr()
+
+begin
+	# Get input and output lists and check that the number of images
+	# are the same.
+
+	call clgstr ("input", title, SZ_LINE)
+	listin = imtopen (title)
+	call clgstr ("output", title, SZ_LINE)
+	listout = imtopen (title)
+	if (imtlen (listin) != imtlen (listout)) {
+	    call imtclose (listin)
+	    call imtclose (listout)
+	    call error (0, "Input and output image lists do not match")
+	}
+
+	# Get the bias and trim sections.
+
+	call clgstr ("bias", biassec, SZ_FNAME)
+	call clgstr ("trim", trimsec, SZ_FNAME)
+	if (nowhite (biassec, biassec, SZ_FNAME) == 0)
+	    ;
+	if (nowhite (trimsec, trimsec, SZ_FNAME) == 0)
+	    ;
+	median = btoi (clgetb ("median"))
+
+	# Determine if the task is interactive.  If not set the interactive
+	# flag to always no.
+
+	if (clgetb ("interactive"))
+	    interactive = YES
+	else
+	    interactive = ALWAYSNO
+
+	# Initialize the curve fitting package.
+
+	call ic_open (ic)
+	call clgstr ("function", function, SZ_LINE)
+	call ic_pstr (ic, "function", function)
+	order = clgeti ("order")
+	call ic_puti (ic, "order", order)
+	call ic_putr (ic, "low", clgetr ("low_reject"))
+	call ic_putr (ic, "high", clgetr ("high_reject"))
+	call ic_puti (ic, "niterate", clgeti ("niterate"))
+	call ic_pstr (ic, "xlabel", "Column")
+	call ic_pstr (ic, "ylabel", "Bias")
+
+	gt = gt_init()
+	call gt_sets (gt, GTTYPE, "line")
+
+	# Get the list of log files.
+
+	logfiles = clpopnu ("logfiles")
+
+	# For each input and output image map the bias image, the
+	# trimmed input image, and the output image.  Use a temporary
+	# image header for overwritting the input image.
+
+	while ((imtgetim (listin, image, SZ_FNAME) != EOF) &&
+	    (imtgetim (listout, output, SZ_FNAME) != EOF)) {
+
+	    call sprintf (biasimage, SZ_FNAME, "%s%s")
+		call pargstr (image)
+		call pargstr (biassec)
+	    call sprintf (input, SZ_FNAME, "%s%s")
+		call pargstr (image)
+		call pargstr (trimsec)
+
+	    in = immap (input, READ_ONLY, 0)
+	    bias = immap (biasimage, READ_ONLY, 0)
+	    call xt_mkimtemp (image, output, original, SZ_FNAME)
+	    out = immap (output, NEW_COPY, in)
+	    IM_PIXTYPE(out) = TY_REAL
+
+	    call sprintf (title, SZ_LINE, "linebias %s")
+		call pargstr (image)
+	    call xt_answer (title, interactive)
+	    call gt_sets (gt, GTTITLE, title)
+
+	    # Enter a header in the log file.
+
+	    while (clgfil (logfiles, logfile, SZ_FNAME) != EOF) {
+		logfd = open (logfile, APPEND, TEXT_FILE)
+	        call cnvtime (clktime (0), title, SZ_LINE)
+	        call fprintf (logfd, "\nLINEBIAS:  %s\n")
+		    call pargstr (title)
+		call fprintf (logfd, "input = %s\noutput = %s\nbias = %s\n")
+		    call pargstr (input)
+		    call pargstr (output)
+		    call pargstr (biasimage)
+		if (median == YES)
+		    call fprintf (logfd, "Median of bias section used.\n")
+		call close (logfd)
+	    }
+	    call clprew (logfiles)
+
+	    call lb_linebias (in, bias, out, ic, gt, median, logfiles,
+		interactive)
+
+	    call imunmap (in)
+	    call imunmap (bias)
+	    call imunmap (out)
+	    call xt_delimtemp (output, original)
+	}
+
+	call ic_closer (ic)
+	call gt_free (gt)
+	call clpcls (logfiles)
+	call imtclose (listin)
+	call imtclose (listout)
+end
+
+
+# LB_LINEBIAS -- Get an average line bias vector from the bias image.
+# Fit a function to the bias vector and subtract it from the input image
+# to form the output image.  Column coordinates are in terms of the full
+# input image.
+
+procedure lb_linebias (in, bias, out, ic, gt, median, logfiles, interactive)
+
+pointer	in			# Input image pointer
+pointer	bias			# Bias image pointer
+pointer	out			# Output image pointer
+pointer	ic			# ICFIT pointer
+pointer	gt			# GTOOLS pointer
+int	median			# Median of bias section?
+int	logfiles		# List of log files
+int	interactive		# Interactive curve fitting?
+
+char	graphics[SZ_FNAME]	# Graphics output device
+char	logfile[SZ_FNAME]
+int	i, nbias, nx, ny, xdim, xoff, xstep, xlen
+real	x
+pointer	cv, gp, sp, xbias, zbias, wts, z
+
+int	clgfil()
+real	cveval()
+pointer	gopen(), imgl2r(), impl2r()
+
+begin
+	# The bias coordinates are in terms of the full input image because
+	# the input and bias images may have different sections.
+
+	nx = IM_LEN(in, 1)
+	ny = IM_LEN(in, 2)
+
+	xdim = IM_VMAP(in, 1)
+	xoff = IM_VOFF(in, xdim)
+	xstep = IM_VSTEP(in, xdim)
+	xlen = IM_SVLEN(in, xdim)
+
+	# Get the bias vector and set the weights.
+
+	call lb_getlinebias (bias, xbias, zbias, nbias, median)
+	call smark (sp)
+	call salloc (wts, nbias, TY_REAL)
+	call amovkr (1., Memr[wts], nbias)
+
+	# Do the curve fitting using the interactive curve fitting package.
+	# Free memory when the fit is complete.
+
+	call ic_putr (ic, "xmin", 1.)
+	call ic_putr (ic, "xmax", real (xlen))
+	if ((interactive == YES) || (interactive == ALWAYSYES)) {
+	    call clgstr ("graphics", graphics, SZ_FNAME)
+	    gp = gopen (graphics, NEW_FILE, STDGRAPH)
+	    call gt_setr (gt, GTXMIN, 1.)
+	    call gt_setr (gt, GTXMAX, real (xlen))
+	    call icg_fit (ic, gp, "cursor", gt, cv, Memr[xbias], Memr[zbias],
+		Memr[wts], nbias)
+	    call gclose (gp)
+	} else {
+	    call ic_fit (ic, cv, Memr[xbias], Memr[zbias], Memr[wts], nbias,
+		YES, YES, YES, YES)
+	}
+
+	# Log the fitting information.
+
+	while (clgfil (logfiles, logfile, SZ_FNAME) != EOF) {
+	    call ic_show (ic, logfile, gt)
+	    call ic_errors (ic, logfile, cv, Memr[xbias], Memr[zbias],
+		Memr[wts], nbias)
+	}
+	call clprew (logfiles)
+
+	call mfree (xbias, TY_REAL)
+	call mfree (zbias, TY_REAL)
+	call sfree (sp)
+
+	# Subtract the bias function from the input image..
+
+	call smark (sp)
+	call salloc (z, nx, TY_REAL)
+	do i = 1, nx {
+	    x = xoff + i * xstep
+	    Memr[z+i-1] = cveval (cv, x)
+	}
+
+	do i = 1, ny
+	    call asubr (Memr[imgl2r(in,i)], Memr[z], Memr[impl2r(out,i)], nx)
+
+	# Free allocated memory.
+
+	call cvfree (cv)
+	call sfree (sp)
+end
+
+
+# LB_GETLINEBIAS -- Get the line bias vector.
+# The xbias column values are in terms of the full image.
+
+define	MAXPIX	100000		# Maximum number of pixels to buffer
+
+procedure lb_getlinebias (bias, xbias, zbias, nbias, median)
+
+pointer	bias			# Bias image pointer
+pointer	xbias, zbias		# Bias vector
+int	nbias			# Number of bias points
+int	median			# Median of bias section?
+
+int	i, j, k, n, nx, ny, xdim, xoff, xstep, maxn
+pointer	buf1, buf2
+
+real	amedr()
+pointer	imgl1r(), imgl2r(), imgs2r()
+
+begin
+	# Check for a bias consisting of a single line which is turned
+	# into a 1D image by IMIO.
+	if (IM_NDIM(bias) == 1) {
+	    nx = IM_LEN(bias, 1)
+	    xdim = IM_VMAP(bias, 1)
+	    xoff = IM_VOFF(bias, xdim)
+	    xstep = IM_VSTEP(bias, xdim)
+
+	    nbias = nx
+	    call malloc (xbias, nbias, TY_REAL)
+	    call malloc (zbias, nbias, TY_REAL)
+
+	    do i = 1, nbias
+		Memr[xbias+i-1] = xoff + i * xstep
+	    call amovr (Memr[imgl1r(bias)], Memr[zbias], nbias)
+
+	    return
+	}
+
+	nx = IM_LEN(bias, 1)
+	ny = IM_LEN(bias, 2)
+	xdim = IM_VMAP(bias, 1)
+	xoff = IM_VOFF(bias, xdim)
+	xstep = IM_VSTEP(bias, xdim)
+	
+	nbias = nx
+	call malloc (xbias, nbias, TY_REAL)
+	call calloc (zbias, nbias, TY_REAL)
+
+	if (median == NO) {
+	    do i = 1, ny
+	        call aaddr (Memr[imgl2r(bias,i)], Memr[zbias], Memr[zbias], nx)
+	    call adivkr (Memr[zbias], real (ny), Memr[zbias], nx)
+	} else {
+	    call malloc (buf1, ny, TY_REAL)
+
+	    maxn = MAXPIX / ny
+	    j = 1
+	    do i = 1, nx {
+		if (i == j) {
+	            n = min (nx - j + 1, maxn)
+		    buf2 = imgs2r (bias, j, j + n - 1, 1, ny)
+		    j = j + n
+		}
+		do k = 1, ny
+		    Memr[buf1+k-1] = Memr[buf2+k*n+i-j]
+		Memr[zbias+i-1] = amedr (Memr[buf1], ny)
+	    }
+
+	    call mfree (buf1, TY_REAL)
+	}
+
+	do i = 1, nx
+	    Memr[xbias+i-1] = xoff + i * xstep
+end
diff --git a/noao/imred/bias/mkpkg b/noao/imred/bias/mkpkg
new file mode 100644
index 00000000..fefd744a
--- /dev/null
+++ b/noao/imred/bias/mkpkg
@@ -0,0 +1,30 @@
+# Make the BIAS package.
+
+$call	relink
+$exit
+
+update:
+	$call	relink
+	$call	install
+	;
+
+relink:
+	$update	libpkg.a
+	$call	bias
+	;
+
+install:
+	$move	x_bias1.e noaobin$x_bias.e
+	;
+
+bias:
+	$omake	x_bias.x
+	$link	x_bias.o libpkg.a -lxtools -lcurfit -o x_bias1.e
+	;
+
+libpkg.a:
+	colbias.x	<imhdr.h> <imio.h> <pkg/xtanswer.h>\
+			<pkg/gtools.h>
+	linebias.x	<imhdr.h> <imio.h> <pkg/xtanswer.h>\
+			<pkg/gtools.h>
+	;
diff --git a/noao/imred/bias/x_bias.x b/noao/imred/bias/x_bias.x
new file mode 100644
index 00000000..e0ade131
--- /dev/null
+++ b/noao/imred/bias/x_bias.x
@@ -0,0 +1,2 @@
+task	colbias,
+	linebias
diff --git a/noao/imred/ccdred/Revisions b/noao/imred/ccdred/Revisions
new file mode 100644
index 00000000..982ed391
--- /dev/null
+++ b/noao/imred/ccdred/Revisions
@@ -0,0 +1,1236 @@
+.help revisions Jun88 noao.imred.ccdred
+.nf
+t_ccdgroups.x
+t_ccdhedit.x
+t_ccdinst.x
+t_ccdlist.x
+t_ccdproc.x
+t_combine.x
+t_mkfringe.x
+t_mkillumcor.x
+t_mkillumft.x
+t_mkskycor.x
+t_mkskyflat.x
+    Added a check that the filename given to the hdmopen() procedure wasn't 
+    empty.  This provides a more informative error message than the "floating
+    invalid operation' one gets now when e.g. no 'instrument' file is 
+    specified (10/12/13, MJF)
+
+src/ccdcache.x
+    The 'bufs' pointer was declared as TY_REAL instead of TY_SHORT (5/4/13)
+
+t_cosmicrays.x
+    A pointer to a an array of pointers was used in one place as a real.  This
+    is an error when integer and real arrays are not of the same size; i.e.
+    on 64-bit architectures.  (8/2/12, Valdes)
+
+=======
+V2.16.1
+=======
+
+various
+    Separated the generic combine code to a subdirectory as is done
+    for imcombine, mscred, etc.  This is only a partial step towards
+    sharing the standard imcombine code.  Because this is really old,
+    working code that has diverged significantly it will take some time
+    to update/merge the new imcombine code.  (1/6/11, Valdes)
+
+=====
+V2.15
+=====
+
+src/icstat.gx
+    Fixed type declarations for the asum() procedures (8/25/09, MJF)
+
+doc/ccdproc.hlp
+    Removed the statements that calibration images are not reprocessed
+    if they have CCDPROC even if they lack the keywords for specific
+    operations.  I looked at the code and did not see much dependence
+    on CCDPROC though there could be something I'm missing.  For now,
+    since a user reported this, I will assume the behavior reported by
+    the user is correct and the documentation is wrong for some historical
+    reason.  (5/27/08, Valdes)
+
+x_ccdred.x
+    Added the alias qccdproc for use in the quadred.quadproc task.
+    (3/12/08, Valdes)
+
+=====
+V2.14
+=====
+
+=======
+V2.12.2
+=======
+
+ccdred/ccdred.hd
+    Hooked up help pages for ccdtest package.  (2/14/04, Valdes)
+
+ccdred/ccdtest/t_mkimage.x
+    Removed unused variable.  (8/8/02, Valdes)
+
+ccdred/src/icscale.x
+    Error dereferencing a string pointer.  (8/8/02, Valdes)
+
+ccdred/src/t_mkfringe.x
+ccdred/src/t_mkillumcor.x
+ccdred/src/t_mkillumft.x
+ccdred/src/t_mkskycor.x
+ccdred/src/t_mkskyflat.x
+    There was a confusion with the "output" parameter which is also in
+    the ccdproc pset.  Each task now explicitly calls its own output
+    parameter.  (7/31/02, Valdes)
+
+=======
+V2.12.1
+=======
+
+=====
+V2.12
+=====
+
+ccdred/src/icsetout.x
+    When computing offsets the registration point was the reference pixel
+    returned by mw_gwterm for the first image.  The code then went on to
+    assume this was a logical pixel when comparing with the other images,
+    which is not true when there is a physical coordinate system.  The
+    algorithm was fixed by converting the reference point to logical
+    coordinates.  (4/18/02, Valdes)
+
+ccdred/src/t_ccdmask.x
+    Fixed bug where the if the last line or last column had a bad pixel
+    without a neighboring interior pixel then the mask value would be
+    some number corresponding to the number of pixels in that last line
+    or column.  (2/28/02, Valdes)
+
+ccdred/ccdred.cl
+ccdred/ccdred.men
+ccdred/ccdred.hd
+ccdred/src/mkpkg
+ccdred/x_ccdred.x
+    Removed COSMICRAYS from package tasks.  The source is still not
+    removed.  (8/22/01, Valdes)
+
+ccdred/src/setdark.x
+    Added a check for a zero divide in calculating the dark time scaling
+    which results in an appropriate error message.  (7/5/01, Valdes)
+
+========
+V2.11.3b
+========
+
+t_combine.x
+    Modified the conversion of pclip from a fraction to a number of images
+    because for even number of images the number above/below the median
+    is one too small.  (9/26/00, Valdes)
+
+ccdred/src/icmedian.gx
+    Replaced with faster Wirth algorithm.  (5/16/00, Valdes)
+
+ccdred/src/icgdata.gx
+ccdred/src/iclog.x
+ccdred/src/icmask.x
+ccdred/src/icombine.gx
+ccdred/src/icscale.x
+ccdred/src/icsetout.x
+    Changed declarations for the array "out" to be ARB rather than 3 in
+    some places (because it was not changed when another element was added)
+    or 4.  This will insure that any future output elements added will
+    no require changing these arguments for the sake of cosmetic correctness.
+    (1/13/99, Valdes)
+
+ccdred/src/t_combine.x
+    Added workaround for error recovery problem that loses the error
+    message.  (10/21/99, Valdes)
+
+ccdred$doc/ccdproc.hlp
+    The overscan type name was incorrectly given as "average" instead of
+    "mean".  This was corrected in the documentation.  (10/15/99, Valdes)
+
+ccdred$src/generic/mkpkg
+ccdred$src/cosmic/mkpkg
+ccdred$src/mkpkg
+    Added missing dependencies.  (10/11/99, Valdes)
+
+=======
+V2.11.2
+=======
+
+ccdred$src/t_ccdlist.x
+    Date accidentally changed.  File not modified.  (5/13/99, Valdes)
+
+ccdred$doc/ccdproc.hlp
+ccdred$doc/mkskyflat.hlp
+    Fixed minor formating problems. (4/22/99, Valdes)
+
+ccdred$src/imcombine/icsetout.x
+    The updating of the WCS for offset images was not being done correctly.
+    (10/6/98, Valdes)
+
+ccdred$src/t_ccdmask.x
+    The overlapping of groups of columns was not quite working because
+    you can't overlap imp... calls.  (9/10/98, Valdes)
+
+ccdred$src/t_ccdproc.x
+ccdred$ccdproc.par
+ccdred$doc/ccdproc.hlp
+ccdred$darkcombine.cl
+ccdred$flatcombine.cl
+ccdred$zerocombine.cl
+    1.  Added output image option to CCDPROC.
+    2.  The combine scripts all still do in place processing.
+    (6/19/98, Valdes)
+
+ccdred$doc/ccdproc.hlp
+    Fixed font change typo in Revisions section.  (6/16/98, Valdes)
+
+ccdred$src/t_ccdmask.x
+    The test for a bad pixel used && instead of ||.  (4/24/98, Valdes)
+
+=======
+V2.11.1
+=======
+
+ccdred$src/icscale.x
+ccdred$doc/combine.hlp
+    When zero offsets or weights are specified in a file the weights
+    are not modified for zero offsets.  (10/3/97, Valdes)
+
+ccdred$src/setoutput.x
+    It is now allowed to go from ushort input to short output.
+    (9/29/97, Valdes)
+
+ccdred$src/t_combine.x
+    Fixed a segmentation violation caused by attempting to close the
+    mask data structures during error recovery when the error occurs
+    before the data structures are defined.  (8/14/97, Valdes)
+
+ccdred$src/cosmic/crfind.x
+ccdred$src/cosmic/crlist.x
+    Changed arguments with adjustable arrays to use ARB.  (8/6/97, Valdes)
+
+ccdred$src/setsections.
+    Generalized the LTERM update to work with arbitrary WCSDIM.
+    (7/24/97, Valdes)
+
+ccdred$src/ccdcheck.x
+    No change except date modified.
+    (7/17/97, Valdes)
+
+=====
+V2.11
+=====
+
+ccdred$src/setoverscan.x
+ccdred$src/proc.gx
+ccdred$src/ccdred.h
+ccdred$doc/ccdproc.hlp
+    The overscan fitting function now allows "average", "median", and "minmax"
+    for line-by-line overscan determination.
+    (2/21/97, Valdes)
+
+ccdred$src/setfixpix.x
+ccdred$src/setproc.x
+ccdred$src/proc.gx
+ccdred$src/setsections.x
+ccdred$src/setheader.x
+ccdred$src/ccdred.h
+ccdred$src/corinput.gx		-
+ccdred$src/generic/corinput.x	-
+ccdred$src/mkpkg
+ccdred$src/generic/mkpkg
+ccdred$doc/ccdproc.hlp
+    The bad pixel fixing is now done with the new fixpix routines from xtools.
+    As part of this the physical coordinate system is set to be that of
+    the CCD.
+    (2/21/97, Valdes)
+
+ccdred$src/t_ccdmask.x  +
+ccdred$ccdmask.par      +
+ccdred$doc/ccdmask.hlp  +
+ccdred$src/mkpkg
+ccdred$ccdred.cl
+ccdred$ccdred.hd
+ccdred$ccdred.men
+ccdred$x_ccdred.x
+    A new task, CCDMASK, has been added.  This task finds deviant pixels
+    in CCD data and creates a pixel mask.  (2/21/97, Valdes)
+
+ccdred$src/icscale.x
+    The ccdmean keyword is now updated rather than deleted.  However
+    the ccdmeant keyword is delete to force a later computation if needed.
+    (1/7/97, Valdes)
+
+ccdred$src/icsetout.x
+ccdred$doc/combine.hlp
+    A new option for computing offsets from the image WCS has been added.
+    (1/7/97, Valdes)
+
+ccdred$src/icmask.x
+ccdred$src/iclog.x
+ccdred$src/icombine.com
+ccdred$src/icmask.h	+
+ccdred$src/icmask.com	-
+    Changed to use a mask structure.  (1/7/97, Valdes)
+
+ccdred$src/t_combine.x
+ccdred$src/icombine.gx
+ccdred$src/icimstack.x +
+ccdred$src/iclog.x
+ccdred$src/mkpkg
+ccdred$doc/combine.hlp
+    The limit on the maximum number of images that can be combined, set by
+    the maximum number of logical file descriptors, has been removed.  If
+    the condition of too many files is detected the task now automatically
+    stacks all the images in a temporary image and then combines them with
+    the project option.
+
+    The project option probably did not work previously.  May not still
+    work.
+    (1/7/97, Valdes)
+
+ccdred$src/icsort.gx
+    There was an error in the ic_2sort routine when there are exactly
+    three images that one of the explicit cases did not properly keep
+    the image identifications.  See buglog 344.  (1/17/97, Valdes)
+
+ccdred$src/calimage.x
+    The use of SZ_SUBSET-1 can cause problems because the names are
+    unique to SZ_SUBSET but if unique part is the SZ_SUBSET character
+    this causes problems.  (1/17/97, Valdes)
+
+==========
+V2.10.4-p2
+==========
+
+ccdred$src/icpclip.gx
+    Fixed a bug where a variable was improperly used for two different
+    purposes causing the algorithm to fail (bug 316).  (10/19/95, Valdes)
+
+ccdred$src/cosmic/crlist.x
+    The output bad pixel data accidentally included some extra fields
+    making it incorrect to use the file directly with BADPIXIMAGE.
+    The extra diagnostic fields were removed.  (9/25/95, Valdes)
+
+ccdred$src/cosmic/t_cosmicrays.x
+    Added a test for interactive mode before opening the graphics
+    stream and whether to call the training routine.  This change
+    was needed to allow the task to run non-interactively on
+    dumb, non-graphics terminals.  (7/24/95, Valdes)
+
+=======
+V2.10.4
+=======
+
+ccdred$src/t_combine.x
+    If an error occurs while opening an input image header the error
+    recovery will close all open images and then propagate the error.
+    For the case of running out of file descriptors with STF format
+    images this will allow the error message to be printed rather
+    than the error code.  (4/3/95, Valdes)
+
+ccdred$src/icscale.x
+ccdred$doc/combine.hlp
+    The behavior of the weights when using both multiplicative and zero
+    point scaling was incorrect; the zero levels have to account for
+    the scaling.  (3/27/95, Valdes)
+
+ccdred$src/cosmic/t_cosmicrays.x
+    There was an error in setting the x,y coordinates of the window
+    such that it left some of the coordinates undefined.  This causes
+    an FPE on the Alpha.  (2/17/94, Valdes)
+
+ctype.h
+ccdred$src/ccdsubsets.x
+    Change the test for non-filename characters to map all characters
+    but alphabetic, numbers, and period to '_'.  (2/17/95, Valdes)
+
+ccdred$src/proc.gx
+    The asum$t function was not properly declared.  (9/13/94, Valdes)
+
+ccdred$src/t_mkfringe.x
+ccdred$src/t_mkillumcor.x
+ccdred$src/t_mkillumft.x
+ccdred$src/t_mkskycor.x
+ccdred$src/t_mkskyflat.x
+    Added calls to ccd_open/ccd_close in order to initialize the image
+    caching even if images are not actually cached.  (9/13/94, Valdes)
+
+ccdred$src/cosmic/t_cosmicrays.x
+ccdred$src/cosmic/crexamine.x
+ccdred$doc/cosmicrays.hlp
+    1.  A new parameter was added to the crexamine subroutine in the
+	previous modification for "training" the program.  In the
+	subroutine the parameter was used as a modifyable parameter but it
+	was being called with a fixed constant.  The effect was the costant
+	value was no longer correct after the first execution and the
+	program would act as if a 'q' was typed after the first interactive
+	execution.  This was fixed to treat the input argument as input
+	only.
+    2.  The help page now emphasizes that the "answer" parameter is not
+	to be used on the command line and if it is then the task will
+	ignored the value and act as if the user always responds with
+	"yes".
+    (8/17/94, Valdes)
+
+ccdred/src/cosmic/t_cosmicrays.x
+ccdred/src/cosmic/crfind.x
+ccdred/src/cosmic/crexamine.x
+ccdred/src/cosmic/crlist.x
+ccdred/src/cosmic/crlist.h
+ccdred/cosmicrays.par
+ccdred/doc/cosmicrays.hlp
+noao$lib/scr/cosmicrays.key
+    Added some new parameters and a new functionality to allow setting
+    the flux ratio threshold by training with respect to a user supplied
+    list of classifications.  Normally the list would be the image
+    display cursor.  (6/29/94, Valdes)
+
+ccdred/src/cosmic/t_cosmicrays.x
+    Added an imflush() and imseti() after the initial copy of the input
+    image to the output is done and before the random access to replace
+    the detected cosmic rays.  The imseti sets the image I/O advice to
+    RANDOM.  (6/24/94, Valdes)
+
+ccdred/src/ccdcheck.x
+ccdred/src/ccdmean.x
+ccdred/src/setheader.x
+ccdred/src/scancor.x
+ccdred/src/setillum.x
+ccdred/src/t_mkillumcor.x
+ccdred/src/t_mkfringe.x
+ccdred/src/t_mkskycor.x
+ccdred/src/t_mkillumft.x
+ccdred/src/t_mkskyflat.x
+ccdred/doc/ccdproc.hlp
+ccdred/doc/ccdinst.hlp
+    Added a CCDMEANT keyword giving the time when the CCDMEAN value was
+    calculated.  Routines that later access this keyword check this time
+    against the image modify time to determine whether to invalidate
+    the value and recompute it.  This solves the problem of people
+    modifying the image outside the CCDRED package and possibly using
+    an incorrect scaling value.  For backwards compatiblity if the
+    new keyword is missing it is assumed to be same as the modify time;
+    i.e. the CCDMEAN keyword is valid.  (6/22/94, Valdes)
+
+ccdred/src/t_mkillumcor.x
+ccdred/src/t_mkillumft.x
+ccdred/src/t_mkskycor.x
+ccdred/src/t_mkskyflat.x
+    Added an extra argument to the millumination subroutine to specify
+    whether to print log information.  This is because this procedure
+    is used as an intermediate step in things like the fringe correction
+    the message is confusing to users.  (6/21/94, Valdes)
+
+
+ccdred/src/icaclip.gx
+ccdred/src/iccclip.gx
+ccdred/src/icpclip.gx
+ccdred/src/icsclip.gx
+    1.	The restoration of deleted pixels to satisfy the nkeep parameter
+	was being done inside the iteration loop causing the possiblity
+	of a non-terminating loop; i.e. pixels are rejected, they are
+	restored, and the number left then does not statisfy the termination
+	condition.  The restoration step was moved following the iterative
+	rejection.
+    2.	The restoration was also incorrectly when mclip=no and could
+	lead to a segmentation violation.
+    (6/13/94, Valdes)
+
+ccdred/src/iccclip.gx
+ccdred/src/icsclip.gx
+    Found and fixed another typo bug.  (6/7/94, Valdes/Zhang)
+
+ccdred/src/t_combine.x
+    For some reason the clget for the nkeep parameter was deleted
+    (it was in V2.10.2 but was gone in the version as of this date).
+    It was added again.  (6/6/94, Valdes)
+
+ccdred/src/icscale.x
+    The sigma scaling flag, doscale1, would not be set in the case of
+    a mean offset of zero though the scale factors could be different.
+    (5/25/94, Valdes/Zhang)
+
+ccdred/src/icsclip.gx
+    There was a missing line: l = Memi[mp1].  (5/25/94, Valdes/Zhang)
+
+pkg/images/imarith/icaclip.gx
+ccdred/src/icaclip.gx
+ccdred/src/iccclip.gx
+ccdred/src/icpclip.gx
+ccdred/src/icsclip.gx
+    The reordering step when a central median is used during rejection
+    but the final combining is average was incorrect if the number
+    of rejected low pixels was greater than the number of pixel
+    number of pixels not rejected.  (5/25/94, Valdes)
+
+ccdred/src/t_combine.x
+    Added a workaround for image header copy problem which leaves part
+    of the TEMPNAME keyword in the output image headers.  For an output
+    pixel list file this could cause the file to be screwed up.
+    (5/6/94, Valdes)
+
+ccdred/src/icscale.x
+ccdred/src/t_combine.x
+    1.  There is now a warning error if the scale, zero, or weight type
+	is unknown.
+    2.  An sfree was being called before the allocated memory was finished
+	being used.
+    (5/2/94, Valdes)
+
+ccdred/src/iclog.x
+    Changed the mean, median, mode, and zero formats from 6g to 7.5g to
+    insure 5 significant digits regardless of signs and decimal points.
+    (4/13/94, Valdes)
+
+ccdred/src/icaclip.gx
+ccdred/src/iccclip.gx
+ccdred/src/icsclip.gx
+    The image sigma was incorrectly computed when an offset scaling is used.
+    (3/8/94, Valdes)
+
+ccdred/src/setoverscan.x
+ccdred/doc/ccdproc.hlp
+    It is an error if no bias section is given or if the whole image is
+    given.  (1/3/94, Valdes)
+
+ccdred/src/t_ccdinst.x
+    There was an error causing reentrant formats which was fixed.
+    (12/16/93, Valdes)
+
+ccdred/src/ccdnscan.x	+
+ccdred/src/scancor.x
+ccdred/src/setzero.x
+ccdred/src/setdark.x
+ccdred/src/setflat.x
+ccdred/src/calimage.x
+ccdred/src/proc.gx
+
+ccdred/src/t_ccdinst.x
+ccdred/src/t_mkskyflat.x
+ccdred/src/t_ccdproc.x
+ccdred/src/ccdproc.x
+ccdred/src/setfringe.x
+ccdred/src/setillum.x
+ccdred/src/mkpkg
+
+ccdred/doc/ccdproc.hlp
+ccdred/doc/ccdinst.hlp
+ccdred/doc/instruments.hlp
+    For short scan data the task now looks for the number of scan lines
+    in the image header.  Also when a calibration image is software
+    scanned a new image is created.  This allows processing objects with
+    different numbers of scan lines and preserving the unscanned
+    calibration image.  (12/15/93, Valdes)
+
+ccdred/src/setoutput.x
+ccdred/doc/ccdproc.hlp
+ccdred/doc/ccdred.hlp
+    1.  The output datatypes were extended from just short and real to
+	include ushort, integer, long, and double.  The calculation types
+	are still only short or real.
+    2.  The output datatype is no longer allowed to be of lower precision
+	than the input datatype.
+    (12/4/93, Valdes)
+
+ccdred/src/t_combine.x
+ccdred/combine.par
+ccdred/doc/combine.hlp
+ccdred/doc/darkcombine.hlp
+ccdred/doc/flatcombine.hlp
+ccdred/doc/zerocombine.hlp
+    1.  The "outtype" parameter was being ignored and the package "pixeltype"
+	parameter was used instead.  This was fixed to use the "outtype"
+	parameter.
+    2.  The output pixel datatypes now include unsigned short.
+    3.  The DARKCOMBINE, FLATCOMBINE, and ZEROCOMBINE scripts specified
+	that the output datatype be "real" because of the bug noted
+	above the output type was being determined by the package
+	"pixeltype" parameter.  The change above fixes this so that
+	the combined output will always be real.  The help pages did
+	not state that what the output datatype would be so a sentence
+	was added specifying the output datatype is real.
+    (12/4/93, Valdes)
+
+ccdred/icgrow.gx
+ccdred/icpclip.gx
+ccdred/icsclip.gx
+ccdred/icaclip.gx
+ccdred/iccclip.gx
+ccdred/t_combine.x
+ccdred/doc/combine.hlp
+    If there were fewer initial pixels than specified by nkeep then the
+    task would attempt to add garbage data to achieve nkeep pixels.  This
+    could occur when using offsets, bad pixel masks, or thresholds.  The
+    code was changed to check against the initial number of pixels rather
+    than the number of images.  Also a negative nkeep is no longer
+    converted to a positive value based on the number of images.  Instead
+    it specifies the maximum number of pixels to reject from the initial
+    set of pixels.  (11/8/93, Valdes)
+
+ccdred/doc/ccdproc.hlp
+    Added a sentence explicitly saying the fixpix option provides
+    the same algorithm as FIXPIX.  (11/1/93, Valdes)
+
+ccdred/src/icscale.x
+ccdred/doc/combine.hlp
+    The help indicated that user input scale or zero level factors
+    by an @file or keyword are multiplicative and additive while the
+    task was using then as divisive and subtractive.  This was
+    corrected to agree with the intend of the documentation.
+    Also the factors are no longer normalized.  (9/24/93, Valdes)
+
+ccdred/src/icsetout.x
+    The case in which absolute offsets are specified but the offsets are
+    all the same did not work correctly.  (9/24/93, Valdes)
+
+ccdred/doc/geometry.hlp
+ccdred/doc/ccdproc.hlp
+ccdred/doc/guide.hlp
+    The help was modified to say that the overscan region length is
+    determine from trimsec and is ignored in biassec.  (9/23/93, Valdes)
+
+ccdred/doc/instruments.hlp
+ccdred/doc/subsets.hlp
+    Added notes that comments are allowed.  Also if there is more than
+    one translation for the same CCDRED parameter the last one takes
+    effect.  (9/20/93, Valdes)
+
+ccdred/doc/combine.hlp
+    Clarified how bad pixel masks work with the "project" option.
+    (9/13/93, Valdes)
+
+ccdred/src/t_combine.x
+    The algorithm for making sure there are enough file descriptors failed
+    to account for the need to reopen the output image header for an
+    update.  Thus when the number of input images + output images + logfile
+    was exactly 60 the task would fail.  The update occurs when the output
+    image is unmapped so the solution was to close the input images first
+    except for the first image whose pointer is used in the new copy of the
+    output image.  (8/4/93, Valdes)
+
+============
+V2.10.3 beta
+============
+
+ccdred/src/icgdata.gx
+    There was an indexing error in setting up the ID array when using
+    the grow option.  This caused the CRREJECT/CCDCLIP algorithm to
+    fail with a floating divide by zero error when there were non-zero
+    shifts.  (5/26/93, Valdes)
+
+ccdred/src/icmedian.gx
+    The median calculation is now done so that the original input data
+    is not lost.  This slightly greater inefficiency is required so
+    that an output sigma image may be computed if desired.  (5/10/93, Valdes)
+
+ccdred/darkcombine.cl
+ccdred/doc/darkcombine.hlp
+ccdred/doc/flatcombine.hlp
+ccddb/kpno/direct.cl
+ccddb/kpno/coude.cl
+ccddb/kpno/cryocam.cl
+ccddb/kpno/echelle.cl
+ccddb/kpno/foe.cl
+ccddb/kpno/specphot.cl
+ccddb/kpno/sunlink.cl
+    1.	Updated FLATCOMBINE defaults for KPNO data.
+    2.	Changed package defaults for DARKCOMBINE to use "minmax" rejection.
+    (4/19/93, Valdes)
+
+ccdred/src/icombine.gx
+    There was no error checking when writing to the output image.  If
+    an error occurred (the example being when an imaccessible imdir was
+    set) obscure messages would result.  Errchks were added.
+    (4/16/93, Valdes)
+
+ccdred/src/setfpix.x
+ccdred/src/ccdproc.x
+ccdred/src/t_ccdproc.x
+ccdred/doc/ccdproc.hlp
+ccdred/doc/instrument.hlp
+    If a specified bad pixel file is not found an abort now occurs.  Also
+    the FIXPIX processing header flag is set even if there are no
+    bad pixels.  The documentation was revised to stress that an "untrimmed"
+    bad pixel file refers to the original CCD coordinates which is
+    especially important with subraster readouts.  (2/23/93, Valdes)
+
+ccdred/src/icaclip.gx
+ccdred/src/iccclip.gx
+ccdred/src/icpclip.gx
+ccdred/src/icsclip.gx
+    When using mclip=yes and when more pixels are rejected than allowed by
+    the nkeep parameter there was a subtle bug in how the pixels are added
+    back which can result in a segmentation violation.
+	if (nh == n2)  ==>  if (nh == n[i])
+    (1/20/93, Valdes)
+
+ccdred/zerocombine.cl
+ccdred/darkcombine.cl
+ccdred/flatcombine.cl
+    Explicitly set ccdproc.noproc to no.  (11/23/92, Valdes)
+
+=======
+V2.10.2
+=======
+
+ccdred/src/calimage.x
+    Added test on the requested ccdtype when setting up the calibration images
+    to avoid mapping a calibration type image which is not going to be
+    used.  (11/17/92, Valdes)
+
+ccdred/darkcombine.cl
+    Fixed typo in output parameter prompt string refering to a flat field.
+    (11/10/92, Valdes)
+
+ccdred/src/ccdred.h
+ccdred/src/t_ccdproc.x
+ccdred/src/proc.gx
+    Separated the minreplace operation from the findmean operation.  It
+    is now a separate operation only applied to flat images.
+    (10/26/92, Valdes)
+
+ccdred/ccdtest/demo.dat
+    Removed display commands.  Because DISPLAY is always loaded in V2.10
+    there was no way to escape the displaying.
+    (9/30/92, Valdes)
+
+ccdred$darkcombine.cl
+ccdred$flatcombine.cl
+ccdred$zerocombine.cl
+ccdred$doc/darkcombine.hlp
+ccdred$doc/flatcombine.hlp
+ccdred$doc/zerocombine.hlp
+    Added "blank", "nkeep", and "snoise" parameters.
+    (9/30/92, Valdes)
+
+ccdred$src/t_combine.x
+ccdred$src/icaclip.gx
+ccdred$src/iccclip.gx
+ccdred$src/icgrow.gx
+ccdred$src/iclog.x
+ccdred$src/icombine.com
+ccdred$src/icombine.gx
+ccdred$src/icombine.h
+ccdred$src/icpclip.gx
+ccdred$src/icscale.x
+ccdred$src/icsclip.gx
+ccdred$src/icsetout.x
+ccdred$combine.par
+ccdred$doc/combine.hlp
+    The weighting was changed from using the square root of the exposure time
+    or image statistics to using the values directly.  This corresponds
+    to variance weighting.  Other options for specifying the scaling and
+    weighting factors were added; namely from a file or from a different
+    image header keyword.  The \fInkeep\fR parameter was added to allow
+    controlling the maximum number of pixels to be rejected by the clipping
+    algorithms.  The \fIsnoise\fR parameter was added to include a sensitivity
+    or scale noise component to the noise model.  Errors will now delete
+    the output image.
+    (9/30/92, Valdes)
+
+ccdred$src/t_combine.x
+ccdred$src/iclog.x
+    The log now prints the final image name rather than the temp name when
+    using the clobber option.  (8/25/92, Valdes)
+
+ccdred$src/icaclip.gx
+ccdred$src/iccclip.gx
+ccdred$src/icpclip.gx
+ccdred$src/icsclip.gx
+    There was a very unlikely possibility that if all the input pixels had
+    exactly the same number of rejected pixels the weighted average would
+    be done incorrectly because the dflag would not be set.  (8/11/92, Valdes)
+
+ccdred$src/icmm.gx
+    This procedure failed to set the dflag resulting in the weighted average
+    being computed in correctly.  (8/11/92, Valdes)
+
+ccdred$src/icscale.x
+    When scaling and zero offseting the zero level factors were incorrectly
+    computed.  (8/10/92, Valdes)
+
+ccdred$src/ic[acs]clip.gx
+ccdred$src/icstat.gx
+    Corrected type mismatches in intrinsic functions.  (8/10/92, Valdes)
+
+=======
+V2.10.1
+=======
+
+=======
+V2.10.0
+=======
+
+=====
+V2.10
+=====
+
+ccdred$src/icombine.gx
+    Needed to clear buffers returned by impl1 during the memory check
+    to avoid possible invalid values.  (4/27/92, Valdes)
+
+ccdred$src/t_ccdproc.x
+ccdred$src/calimage.x
+    Made it an error if an explicit calibration image is specified but cannot
+    be opened.  Previously it would then look in the input list for the
+    appropriate type.  (4/24/92, Valdes)
+
+ccdred$ccdproc.x
+ccdred$t_ccdproc.x
+    Made the COMP type be processed like and OBJECT rather that the
+    default case.  The only effect of this is to not have CCDMEAN
+    calculated.  (4/8/92, Valdes)
+
+ccdred$src/icalip.gx
+ccdred$src/icclip.gx
+ccdred$src/ipslip.gx
+ccdred$src/icslip.gx
+ccdred$src/icmedian.gx
+    The median calculation with an even number of points for short data
+    could overflow (addition of two short values) and be incorrect.
+    (3/16/92, Valdes)
+
+ccdred$src/iclog.x
+    Added listing of read noise and gain.  (2/10/92, Valdes)
+
+ccdred$src/icpclip.gx
+    Reduced the minimum number of images allowed for PCLIP to 3.
+    (1/7/92, Valdes)
+
+ccdred$darkcombine.cl
+ccdred$flatcombine.cl
+    Set default parameters as requested by the support people.
+    (12/12/91, Valdes)
+
+ccdred$src/icgrow.gx
+    The first pixel to be checked was incorrectly set to 0 instead of 1
+    resulting in a segvio when using the grow option.  (12/6/91, Valdes)
+
+ccdred$src/proc.gx
+ccdred$src/icgdata.gx
+ccdred$src/icscale.x
+ccdred$src/setfixpix.x
+ccdred$src/t_combine.x
+    Fixed argument mismatch errors found by SPPLINT.  (11/22/91, Valdes)
+
+ccdred$src
+    Replaced COMBINE with new version.  (9/1/91, Valdes)
+
+ccdred$ccdtest/observe.cl -> artobs.cl
+ccdred$ccdtest/observe.hlp -> artobs.hlp
+ccdred$ccdtest/subsection.cl
+ccdred$ccdtest/subsection.hlp
+ccdred$ccdtest/mkimage.hlp
+ccdred$ccdtest/demo.dat
+ccdred$ccdtest/ccdtest.men
+ccdred$ccdtest/ccdtest.hd
+ccdred$ccdtest/ccdtest.cl
+ccdred$ccddb/kpno/demo.dat
+    Renamed OBSERVE to ARTOBS to avoid conflict with the CCDACQ task of
+    the same name.  (8/29/91, Valdes)
+
+ccdred$src/setoutput.x
+ccdred$src/setproc.x
+ccdred$src/setdark.x
+ccdred$src/setzero.x
+ccdred$src/setflat.x
+ccdred$src/setfringe.x
+ccdred$doc/ccdred.hlp
+    The default output pixel type and computation type are now real.  
+    The computation type may be separately specified.  (5/29/91, Valdes)
+
+ccdred$src/t_mkskycor.x
+    The computation of CCDMEAN failed to accumlate the last few lines causing
+    the mean to be underestimated.  (4/16/91, Valdes)
+
+ccdred$src/t_ccdinst.x +
+ccdred$src/ccdinst1.key +
+ccdred$src/ccdinst2.key +
+ccdred$src/ccdinst3.key +
+ccdred$src/hdrmap.x
+ccdred$src/mkpkg
+ccdred$ccdinstrument.par +
+ccdred$ccdred.cl
+ccdred$ccdred.hd
+ccdred$ccdred.men
+ccdred$x_ccdred.x
+    Added the new task CCDINSTRUMENT.  This also involved some changes to
+    the header translation package hdrmap.x.  (10/23/90, Valdes)
+
+ccdred$src/imcscales.x
+ccdred$src/imcmode.gx
+ccdred$src/mkpkg
+    Added error check for incorrect mode section specification.
+    (10/3/90, Valdes)
+
+ccdred$src/ccdred.h
+ccdred$src/proc.gx
+ccdred$src/setproc.x
+ccdred$ccdproc.par
+    Added a minreplace parameter to replace flat field values less than this
+    value by the value.  This provides zero division prevention without
+    requiring specific flat field checking.
+    (10/3/90, Valdes)
+
+ccdred$src/t_ccdproc.x
+ccdred$src/ccdproc.x
+ccdred$src/scancor.x
+    1.  The scan correction now computes the CCDMEAN to account for the
+	ramp down.
+    2.  Did a simple move of the ccdmean call from before scancor to
+	after scancor.  Since CCDMEAN is now computed in SCANCOR this
+	has no real affect and is just cosmetic.  If CCDMEAN were not
+	computed in SCANCOR then the new placement would have computed
+	the right value at the expense of another pass through the image.
+    (9/21/90, Valdes)
+
+ccdred$src/t_badpixim.x
+    The template image cannot be closed immediately after opening the NEW_COPY
+    mask image because the STF kernel doesn't make the header copy until
+    pixel I/O occurs.  This only affects STF images.  (6/19/90, Valdes)
+
+====
+V2.9
+====
+
+ccdred$src/t_combine.x
+    Changed:
+	char images[SZ_FNAME-1,nimages] --> char images[SZ_FNAME,nimages-1]
+    The incorrect declaration results in each successive image name have
+    additional leading characters.  Apparently, since this has not be
+    found previously, the leading characters have generally been blanks.
+    (3/30/90, Valdes)
+
+ccdred$doc/combine.hlp
+    Clarified and documented definitions of the scale, offset, and weights.
+    (11/30/89, Valdes)
+
+ccdred$ccdproc.par
+    1.  All parameters now have default values.  (10/31/89, Valdes)
+
+ccdred$src/cosmic/mkpkg
+ccdred$src/gtascale.x -
+ccdred$t_cosmicrays.x
+    1.  Removed duplicate of gtools procedure.
+    2.  Fixed transfer out of IFERR block message when input image was wrong.
+    3.  The badpixel file was not initialized to null if the user did not
+	want a badpixel file output.  (9/21/89, Valdes)
+
+====
+V2.8
+===
+
+ccdred$src/imcmode.gx
+    Fixed bug causing infinite loop when computing mode of constant value
+    section.  (8/14/89, Valdes)
+
+ccdred$src/ccdproc.x
+ccdred$src/ccddelete.x
+ccdred$src/t_ccdproc.x
+ccdred$src/t_mkfringe.x
+ccdred$src/t_mkskyflat.x
+ccdred$src/t_mkskycor.x
+ccdred$src/t_mkillumft.x
+ccdred$src/t_mkillumcor.x
+ccdred$src/t_combine.x
+ccdred$src/scancor.x
+ccdred$src/readcor.x
+    1. Added error checking for procedure ccddelete.
+    2. Made workaround for error handling problem with procedure imrename
+       so that specifying a bad backup prefix would result in an abort
+       with an error message.  (6/16/89, Valdes)
+
+ccdred$src/imcombine.gx
+   Made same changes made to image.imcombine to recover from too many VOS
+   file description error.  (6/14/89, Valdes)
+
+ccdred$setinstrument.cl
+ccdred$setinstrument.hlp
+   Incorrect instrument names are now reported to the user, a menu is
+   printed if there is one, and a second opportunity is given.
+   (6/14/89, Valdes)
+
+ccdred$ccdred.par
+   Added an ennumerated subset for the output datatype.  (5/12/89, Valdes)
+
+ccdred$src/imcombine.gx
+   Because a file descriptor was not reserved for string buffer operations
+   and a call to stropen in cnvdate was not error checked the task would
+   hang when more than 115 images were combined.  Better error checking
+   was added and now an error message is printed when the maximum number
+   of images that can be combined is exceeded.  (5/9/89, Valdes)
+
+ccdred$src/sigma.gx
+ccdred$src/imcaverage.gx
+    1.  Weighted sigma was being computed incorrectely.
+    2.  Added errchk to imcaverage.gx.
+    (5/6/89, Valdes)
+
+ccdred$src/setdark.x
+ccdred$src/setflat.x
+ccdred$src/setfringe.x
+ccdred$src/setillum.x
+ccdred$src/setoverscan.x
+ccdred$src/settrim.x
+ccdred$src/setzero.x
+    Made the trimsec, biassec, datasec, and ccdsec error messages more
+    informative.  (3/13/89, Valdes)
+ 
+ccdred$src/imcmode.gx
+    For short data a short variable was wraping around when there were
+    a significant number of saturated pixels leading to an infinite loop.
+    The variables were made real regardless of the image datatype.
+    (3/1/89, Valdes)
+ 
+ccdred$src/t_mkskyflat.x
+ccdred$src/t_mkskycor.x
+    1.  Added warning if images have not been flat fielded.
+    2.  Allowed flat field image to be found even if flatcor=no.
+    (2/24/89, Valdes)
+ 
+ccdred$src/imcthresh.gx
+ccdred$combine.par
+ccdred$doc/combine.hlp
+ccdred$src/imcscales.x
+    1.  Added provision for blank value when all pixels are rejected by the
+        threshold.
+    2.  Fixed a bug that improperly scaled images in the threshold option.
+    3.  The offset printed in the log now has the opposite sign so that it
+	is the value "added" to bring images to a common level.
+    (2/16/89, Valdes)
+
+ccdred$src/proc.gx
+    When the data section had fewer lines than the output image (which occurs
+    when not trimming and the overscan being along lines) pixel out of
+    bounds errors occured.  This bug was due to a sign error when reading
+    the non-trimmed overscan lines.  (2/13/89, Valdes)
+
+ccdred$src/setoverscan.gx
+    The overscan buffer for readaxis=column was not initialized yielding
+    unpredictable and incorrect overscan data.
+    (3/13/89, Valdes)
+
+ccdred$src/imcmode.gx
+    Added test for nx=1.  (2/8/89, Valdes)
+ 
+ccdred$darkcombine.cl
+ccdred$flatcombine.cl
+    Changed the default parameters to use "avsigclip" combining and
+    no scaling or weighting.  (1/27/89, Valdes)
+ 
+ccdred$src/ccdcheck.x
+ccdred$src/setillum.x
+ccdred$src/t_ccdproc.x
+    1.  If the illumination image does not have CCDMEAN in its header
+	it is calculated.
+    2.  If an error occurs in setting up for illumination or fringe
+	correction during processing a warning is issued and these
+	processing steps are skipped.  They can be done later if
+	desired.  Previously this caused an abort.
+    (1/27/89, Valdes)
+ 
+ccdred$ccdgroups.par
+ccdred$src/t_ccdgroups.x
+ccdred$doc/ccdgroups.hlp
+    Added two new group types; ccdtype and subset.  (1/26/89, Valdes)
+ 
+ccdred$src/t_ccdlist.x
+ccdred$doc/ccdlist.hlp
+    The exposure time and dark time are now printed in long format.  This
+    is useful to allow verifying the header translation is working
+    correctly.  (1/26/89, Valdes)
+ 
+ccdred$src/setfixpix.x
+ccdred$src/t_badpixim.x
+    The magic word "untrimmed" no longer needs whitespace preceding it.
+    (1/24/89, Valdes)
+ 
+imred$ccdred/src/imcscales.x
+    Valdes, Dec 8, 1988
+    1.  COMBINE now prints the scale as a multiplicative quantity.
+    2.  The combined exposure time was not being scaled by the scaling
+	factors resulting in a final exposure time inconsistent with the
+	data.
+
+imred$ccdred/src/t_mkskyflat.x
+imred$ccdred/src/t_mkillumft.x
+imred$ccdred/src/t_mkskycor.x
+imred$ccdred/src/t_mkskyflat.x
+imred$ccdred/src/t_mkfringe.x
+imred$ccdred/doc/mkillumcor.hlp
+imred$ccdred/doc/mkillumflat.hlp
+imred$ccdred/mkillumflat.par
+imred$ccdred/mkillumflat.par
+    1.  Minor typo in declaration (calimage.x) which had no effect.
+    2.  Missing include file (t_mkskyflat.x) caused "Cannot open image"
+	when using MKSKYFLAT.
+    3.  Added checks for division by zero which are reported at the end as
+	the number of divisions by zero and the replacement value.
+	The replacement value was added as a parameter value in MKILLUMCOR
+	and MKILLUMFLAT.
+    4.	Updated the help pages to reflect the new division by zero parameter.
+    5.	Modified the log strings to be more informative about what
+	was done and which images were used.
+	(10/20/88 Valdes)
+
+imred$ccdred/src/imcombine.gx
+    A vops clear routine was not called generically causing a crash with
+    double images.  (10/19/88 Valdes)
+
+imred$ccdred/src/t_mkskycor.x
+    Replaced calls to recipricol vops procedure to one with zero checking.
+    (10/13/88 Valdes)
+
+imred$ccdred/src/imcscales.x
+    It is now an error if the mode is not positive for mode scaling or
+    weighting.  (9/28/88 Valdes)
+
+imred$ccdred/ccdred.par
+imred$ccdred/doc/ccdred.hlp
+    The plotfile parameter was changed to reflect the "" character
+    as the new default.  (9/23/88 jvb)
+
+imred$ccdred/src/imcmedian.gx
+    The median option was selecting the n/2 value instead of (n+1)/2.  Thus,
+    for an odd number of images the wrong value was being determined for the
+    median. (8/16/88 Valdes)
+
+imred$ccdred/src/scancor.x
+imred$ccdred/src/calimage.x
+imred$ccdred/src/ccdcmp.x +
+imred$ccdred/src/mkpkg
+    1.  The shortscan correction was incorrectly writing to the input image
+	rather than the output image causing a cannot write to file error.
+    2.  It is now a trapped error if the input image is the same as a
+	calibration image.  (4/18/88 Valdes)
+
+imred$ccdred/src/imcmode.gx
+    The use of a mode sections was handled incorrectly.  (4/11/88 Valdes)
+
+noao$imred/ccdred/src/setoverscan.x
+    Minor bug fix:
+	gt_setr (gt, GTXMIN, 1.) -> gt_setr (gt, GTXMIN, x[1])
+	gt_setr (gt, GTXMAX, real(npts)) -> gt_setr (gt, GTXMAX, x[npts])
+    (2/11/88 Valdes)
+
+noao$imred/ccdred/src/t_mkillumflat.x -> t_mkillumft.x
+noao$imred/ccdred/src/t_mkfringecor.x -> t_mkfringe.x
+noao$imred/ccdred/src/t_badpiximage.x -> t_badpixim.x
+noao$imred/ccdred/src/imcthreshold.gx -> imcthresh.gx
+noao$imred/ccdred/src/generic/imcthresh.x -> imcthresh.x
+noao$imred/ccdred/src/mkpkg
+noao$imred/ccdred/src/generic/mkpkg
+    Shortened long names. (2/10/88 Valdes)
+
+noao$imred/ccdred/src/t_mkskycor.x
+noao$imred/ccdred/doc/mkskycor.hlp
+noao$imred/ccdred/doc/mkillumcor.hlp
+noao$imred/ccdred/doc/mkskyflat.hlp
+noao$imred/ccdred/doc/mkillumflat.hlp
+noao$imred/ccdred/doc/mkfringecor.hlp
+    1. 	When not clipping the first 3 lines of the illumination were always
+	zero.
+    2.  The clipping algorithm had several errors.
+    3.  It was unclear what a box size of 1. meant and whether one could
+	specify the entire image as the size of the box.
+    4.  The smoothing box has been generalize to let the user chose the minimum
+	and maximum box size.  This lets the user do straight box smoothing
+	and the growing box smoothing. (2/2/88 Valdes)
+
+noao$imred/ccdred/src/ccdtypes.h
+    Added the comparison CCD image type. (1/21/88 Valdes)
+
+noao$imred/ccdred/src/t_mkskycor.x
+noao$imred/ccdred/src/t_mkillumcor.x
+noao$imred/ccdred/src/t_mkskyflat.x
+noao$imred/ccdred/src/t_mkillumflat.x
+noao$imred/ccdred/src/t_mkfringecor.x
+    Calling sequences to the set_ procedures were wrong. (1/20/88 Valdes)
+
+noao$imred/ccdred/src/imcscales.x
+    The exposure time is now read as real. (1/15/88 Valdes)
+
+noao$imred/ccdred/src/corinput.gx
+    Discovered an initialization bug which caused the fixing of bad lines
+    to fail after the first image.  (11/12/87 Valdes)
+
+noao$imred/ccdred/ccdtest/observe.cl
+noao$imred/ccdred/ccdtest/subsection.cl
+noao$imred/ccdred/ccdtest/demo.dat
+    Made modification to allow the demo to work with STF format images.
+    The change was in being more explicit with image extensions; i.e.
+    obs* --> obs*.??h.  (11/12/87 Valdes)
+
+noao$imred/ccdred/src/mkpkg
+noao$imred/ccdred/src/ccdmean.x		 +
+noao$imred/ccdred/src/ccdcache.h	 +
+noao$imred/ccdred/src/ccdcache.com
+noao$imred/ccdred/src/ccdcache.x
+noao$imred/ccdred/src/t_ccdproc.x
+noao$imred/ccdred/src/ccdproc.x
+noao$imred/ccdred/src/ccdcheck.x
+noao$imred/ccdred/src/setflat.x
+noao$imred/ccdred/src/setdark.x
+noao$imred/ccdred/src/setzero.x
+noao$imred/ccdred/src/setfixpix.x
+noao$imred/ccdred/src/setillum.x
+noao$imred/ccdred/src/setfringe.x
+noao$imred/ccdred/src/t_ccdlist.x
+    1.  There was a recursion problem caused by the absence of the CCDPROC
+	flag in a zero level image which did not need any processing
+	because there was no trimming, overscan subtraction, or bad
+	pixel correction.  The procedure CCDPROC left the image
+	unmodified (no CCDPROC flag) which meant that later another unprocessed
+	calibration image would again try to process it leading to
+	recursion.  Since I was uncomfortable with relying on the
+	CCDPROC flag I added the routine CCDCHECK to actually check
+	each processing flag against the defined operations.  This will
+	also allow additional automatic processing of calibration
+	images if the users sets new flags after an initial pass
+	through the data.  The CCDPROC flag is still set in the data
+	but it is not used.
+    2.  It is possible in data which has no object types for the flat
+	field image never to have its mean computed for later scaling.
+	There were two modifications to address this problem.  If an
+	image is processed without a ccdtype then the mean will be
+	computed at a very small cost in time.  If the image is later
+	used as a flat field this information will then be present.
+	Second, if a flat field calibration image does not have the
+	mean value, even if it has been processed, the mean value
+	will still be calculated.
+    3.  In looking at the recursion problem I realized that some of
+	the calibration images could be opened more than once, though
+	READ_ONLY, once for the image being processed and later if the
+	task has to backtrack to process a another calibration frame.  I
+	was surprise that this was not found on VMS until I realized
+	that for OIF format images the image header is read and the
+	file is then closed.  No file is actually left open until pixel
+	I/O is done.  However, this should cause STF images to fail on
+	VMS because VMS does not allow a file to be open more than once
+	and the STF image header is kept open.  I rewrote the image
+	caching interface to cache the IMIO pointer even if the pixel
+	data was not cached.  This will insure any calibration image
+	is only opened once even if it is accessed independently from
+	different parts of the program.
+    4.  The error message when using fringe and illumination correction
+	images which have not been processed by MKFRINGECOR and
+	MKILLUMCOR was misleading when refering to the absence of the
+	MKFRINGE and MKILLUM flag.  A user thought that the missing
+	flag was FRINGCOR which refers to an image being fringe corrected.
+	The message was made a little more clear.
+    5.  The CCDLIST listing for fringe correction in long format was wrong.
+    (11/12/87 Valdes)
+
+noao$imred/ccdred/src/t_combine.x
+noao$imred/ccdred/src/t_ccdhedit.x
+noao$imred/ccdred/src/setoverscan.x
+noao$imred/ccdred/src/setinput.x
+noao$imred/ccdred/src/imcscales.x
+noao$imred/ccdred/src/imclogsum.x
+noao$imred/ccdred/src/ccdlog.x
+noao$imred/ccdred/src/ccddelete.x
+    Added calls to XT_STRIPWHITE to allow null strings to be recognized
+    with whitespace.  It should probably use NOWHITE but this would make
+    it incompatible with V2.5.  (11/6/87 Valdes)
+.endhelp
diff --git a/noao/imred/ccdred/badpiximage.par b/noao/imred/ccdred/badpiximage.par
new file mode 100644
index 00000000..9a964701
--- /dev/null
+++ b/noao/imred/ccdred/badpiximage.par
@@ -0,0 +1,5 @@
+fixfile,f,a,,,,Bad pixel file
+template,f,a,,,,Template image
+image,f,a,,,,Bad pixel image to be created
+goodvalue,i,h,1,,,Value assigned to the good pixels
+badvalue,i,h,0,,,Value assigned to the bad pixels
diff --git a/noao/imred/ccdred/ccddb/ctio/OLD/ccd.dat b/noao/imred/ccdred/ccddb/ctio/OLD/ccd.dat
new file mode 100644
index 00000000..45e38898
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/OLD/ccd.dat
@@ -0,0 +1,23 @@
+exptime itime
+darktime itime
+imagetyp data-typ
+subset none 
+biassec biassec [405:425,7:572]
+datasec datasec [35:340,4:570]
+fixfile fixfile home$badpix
+ 
+fixpix		bp-flag 0
+overscan 	bt-flag 0
+zerocor		bi-flag 0
+darkcor		dk-flag 0
+flatcor		ff-flag 0
+fringcor	fr-flag 0
+ 
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		other
+COMPARISON		other
+BIAS			zero
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/ctio/OLD/cfccd.dat b/noao/imred/ccdred/ccddb/ctio/OLD/cfccd.dat
new file mode 100644
index 00000000..35af13e9
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/OLD/cfccd.dat
@@ -0,0 +1,23 @@
+exptime exptime
+darktime darktime
+imagetyp imagetyp
+subset filters
+biassec biassec
+datasec datasec
+fixfile fixfile
+ 
+fixpix		bp-flag 0
+overscan 	bt-flag 0
+zerocor		bi-flag 0
+darkcor		dk-flag 0
+flatcor		ff-flag 0
+fringcor	fr-flag 0
+ 
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		other
+COMPARISON		other
+BIAS			zero
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/ctio/OLD/csccd.dat b/noao/imred/ccdred/ccddb/ctio/OLD/csccd.dat
new file mode 100644
index 00000000..d46f11c0
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/OLD/csccd.dat
@@ -0,0 +1,23 @@
+exptime exptime
+darktime darktime
+imagetyp data-typ
+subset none 
+biassec biassec
+datasec datasec
+fixfile fixfile
+ 
+fixpix		bp-flag 0
+overscan 	bt-flag 0
+zerocor		bi-flag 0
+darkcor		dk-flag 0
+flatcor		ff-flag 0
+fringcor	fr-flag 0
+ 
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		other
+COMPARISON		other
+BIAS			zero
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/ctio/OLD/ech.dat b/noao/imred/ccdred/ccddb/ctio/OLD/ech.dat
new file mode 100644
index 00000000..32cf5ee1
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/OLD/ech.dat
@@ -0,0 +1,19 @@
+exptime exptime
+darktime darktime
+subset none 
+biassec biassec
+trimsec datasec
+imagetyp imagetyp
+
+'OBJECT'	        object
+'COMPARISON'        	other
+'BIAS'	                zero
+'DOME FLAT'	        flat
+'PROJECTOR FLAT'	flat
+
+fixpix bp-flag 0
+overscan bt-flag 0
+zerocor bi-flag 0
+darkcor dk-flag 0
+flatcor ff-flag 0
+fringcor fr-flag 0
diff --git a/noao/imred/ccdred/ccddb/ctio/OLD/epi5.dat b/noao/imred/ccdred/ccddb/ctio/OLD/epi5.dat
new file mode 100644
index 00000000..7b7613de
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/OLD/epi5.dat
@@ -0,0 +1,23 @@
+exptime		exptime
+darktime	darktime
+imagetyp	imagetyp
+subset		none
+biassec		biassec		[420:431,10:576]
+trimsec		trimsec		[15:393,10:576]
+fixfile		fixfile	home$ccds/epi5_badpix.dat
+ 
+fixpix		bp-flag 0
+overscan 	bt-flag 0
+zerocor		bi-flag 0
+darkcor		dk-flag 0
+flatcor		ff-flag 0
+fringcor	fr-flag 0
+ 
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		other
+COMPARISON		other
+BIAS			zero
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/ctio/OLD/epi5_badpix.dat b/noao/imred/ccdred/ccddb/ctio/OLD/epi5_badpix.dat
new file mode 100644
index 00000000..d4ccc345
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/OLD/epi5_badpix.dat
@@ -0,0 +1,22 @@
+# EPI5_BADPIX.DAT - GEC EPI5 Blue Air Schmidt untrimmed coordinates
+#
+# Map includes columns which bleed due to very poor charge transfer at low
+# light levels.
+#
+# SRH 8 December 87
+#
+ 37  37 396 313
+ 37  37 510 528
+ 46  46 482 307
+ 77  77 148 490
+129 129  21  48
+154 154 346 446
+262 262 199 450
+284 284 493 549
+307 308 196 210
+307 309 395 576
+312 312 480 496
+347 348  88 111
+347 347 112 468
+352 352 127 438
+378 378 515 529
diff --git a/noao/imred/ccdred/ccddb/ctio/OLD/fpccd.dat b/noao/imred/ccdred/ccddb/ctio/OLD/fpccd.dat
new file mode 100644
index 00000000..a56c56c0
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/OLD/fpccd.dat
@@ -0,0 +1,23 @@
+EXPTIME exptime
+DARKTIME darktime
+IMAGETYP imagetyp
+subset FPZ
+biassec biassec
+datasec datasec
+fixfile fixfile
+ 
+fixpix		bp-flag 0
+overscan 	bt-flag 0
+zerocor		bi-flag 0
+darkcor		dk-flag 0
+flatcor		ff-flag 0
+fringcor	fr-flag 0
+ 
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		other
+COMPARISON		other
+BIAS			zero
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/ctio/OLD/instruments.men b/noao/imred/ccdred/ccddb/ctio/OLD/instruments.men
new file mode 100644
index 00000000..8fe97635
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/OLD/instruments.men
@@ -0,0 +1,5 @@
+ccd         CTIO genetic CCD
+ech         CTIO generic Echelle/CCD
+cfccd       CTIO generic CF/CCD
+csccd       CTIO generic CS/CCD
+fpccd       CTIO generic FP/CCD
diff --git a/noao/imred/ccdred/ccddb/ctio/cfccd_both.dat b/noao/imred/ccdred/ccddb/ctio/cfccd_both.dat
new file mode 100644
index 00000000..37991738
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/cfccd_both.dat
@@ -0,0 +1,27 @@
+# CFCCD.DAT -- Instrument file to be used with quad when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+subset			filters
+#subset			filter1
+#subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/ctio/cfccd_f1.dat b/noao/imred/ccdred/ccddb/ctio/cfccd_f1.dat
new file mode 100644
index 00000000..68cd2063
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/cfccd_f1.dat
@@ -0,0 +1,27 @@
+# CFCCD.DAT -- Instrument file to be used with quad when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+#subset			filters
+subset			filter1
+#subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/ctio/cfccd_f2.dat b/noao/imred/ccdred/ccddb/ctio/cfccd_f2.dat
new file mode 100644
index 00000000..c4d03cb8
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/cfccd_f2.dat
@@ -0,0 +1,27 @@
+# CFCCD.DAT -- Instrument file to be used with quad when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+#subset			filters
+#subset			filter1
+subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/ctio/csccd.dat b/noao/imred/ccdred/ccddb/ctio/csccd.dat
new file mode 100644
index 00000000..000f8c07
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/csccd.dat
@@ -0,0 +1,23 @@
+# CCD.DAT -- Instrument file to be used with ccdred when reducing spectroscopic
+# data obtained with ArCon.
+
+subset			none
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		object
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/ctio/echccd.dat b/noao/imred/ccdred/ccddb/ctio/echccd.dat
new file mode 100644
index 00000000..90d08173
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/echccd.dat
@@ -0,0 +1,23 @@
+# ECHCCD.DAT -- Instrument file to be used with ccdred when reducing echelle
+# spectroscopic data obtained with ArCon.
+
+subset			none
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
+FOCUS			object
diff --git a/noao/imred/ccdred/ccddb/ctio/instruments.men b/noao/imred/ccdred/ccddb/ctio/instruments.men
new file mode 100644
index 00000000..144c41d5
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/instruments.men
@@ -0,0 +1,9 @@
+cfccd_f1	- Cassegrain focus CCD direct subset=filter1
+cfccd_f2	- Cassegrain focus CCD direct subset=filter2
+cfccd_both	- Cassegrain focus CCD direct subset=filters
+csccd		- Cassegrain focus spectroscopy
+echccd		- Echelle spectroscopy
+nfccd		- Newtonian focus CCD direct (Schmidt)
+pfccd_f1	- Prime focus CCD direct subset=filter1
+pfccd_f2	- Prime focus CCD direct subset=filter2
+pfccd_both	- Prime focus CCD direct subset=filters
diff --git a/noao/imred/ccdred/ccddb/ctio/nfccd.dat b/noao/imred/ccdred/ccddb/ctio/nfccd.dat
new file mode 100644
index 00000000..06a173cf
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/nfccd.dat
@@ -0,0 +1,23 @@
+# NFCCD.DAT -- Instrument file to be used with ccdred when reducing direct
+# imageing data obtained with ArCon.
+
+subset			filter1
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/ctio/pfccd_both.dat b/noao/imred/ccdred/ccddb/ctio/pfccd_both.dat
new file mode 100644
index 00000000..ac8e03a6
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/pfccd_both.dat
@@ -0,0 +1,27 @@
+# PFCCD.DAT -- Instrument file to be used with quad when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+subset			filters
+#subset			filter1
+#subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/ctio/pfccd_f1.dat b/noao/imred/ccdred/ccddb/ctio/pfccd_f1.dat
new file mode 100644
index 00000000..9893d7f1
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/pfccd_f1.dat
@@ -0,0 +1,27 @@
+# PFCCD.DAT -- Instrument file to be used with quad when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+#subset			filters
+subset			filter1
+#subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/ctio/pfccd_f2.dat b/noao/imred/ccdred/ccddb/ctio/pfccd_f2.dat
new file mode 100644
index 00000000..89028468
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/ctio/pfccd_f2.dat
@@ -0,0 +1,27 @@
+# PFCCD.DAT -- Instrument file to be used with quad when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+#subset			filters
+#subset			filter1
+subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/ccdred/ccddb/kpno/Revisions b/noao/imred/ccdred/ccddb/kpno/Revisions
new file mode 100644
index 00000000..47195a53
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/Revisions
@@ -0,0 +1,35 @@
+.help revisions Dec91 ccddb$kpno
+.nf
+hydra.dat	+
+hydra.cl	+
+direct.cl	+
+coude.cl
+cryocam.cl
+default.cl
+echelle.cl
+fibers.cl
+foe.cl
+specphot.cl
+sunlink.cl
+instruments.men
+    1.  Added hydra entry.
+    2.  Linked all the entries to the new "default.cl" so that each
+	setup script only contains the differences from the default.
+    (9/8/97, Valdes)
+
+*.cl
+    1.	(all) ccdred.plotfile = "".
+    2.	(all) ccdred.pixeltype = "real real".
+    3.  (direct,fibers) ccdproc.interactive = yes
+    4.  (coude, specphot) ccdproc.ccdtype = ""
+			  ccdproc.flatcor = no
+			  ccdproc.trimsec = ""
+    (12/12/91, Valdes)
+
+instruments.men
+    Removed sunlink from the instrument menu.  (12/12/91, Valdes)
+
+coude.dat
+    Changed the subset parameter from FILTER to GRATPOS.  (12/11/91, Valdes)
+
+.endhelp
diff --git a/noao/imred/ccdred/ccddb/kpno/camera.dat b/noao/imred/ccdred/ccddb/kpno/camera.dat
new file mode 100644
index 00000000..841a37b9
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/camera.dat
@@ -0,0 +1,21 @@
+exptime		otime
+darktime	ttime
+imagetyp	data-typ
+subset		f1pos
+biassec		biassec []
+datasec		datasec []
+
+fixpix		bp-flag 0
+overscan	bt-flag 0
+zerocor		bi-flag 0
+darkcor		dk-flag 0
+flatcor		ff-flag 0
+fringcor	fr-flag 0
+
+'OBJECT (0)'		object
+'DARK (1)'		dark
+'PROJECTOR FLAT (2)'	flat
+'SKY FLAT (3)'		other
+'COMPARISON LAMP (4)'	other
+'BIAS (5)'		zero
+'DOME FLAT (6)'		flat
diff --git a/noao/imred/ccdred/ccddb/kpno/coude.cl b/noao/imred/ccdred/ccddb/kpno/coude.cl
new file mode 100644
index 00000000..1eb1a73e
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/coude.cl
@@ -0,0 +1,4 @@
+cl < "ccddb$kpno/default.cl"
+
+ccdred.instrument = "ccddb$kpno/coude.dat"
+ccdproc.trimsec = ""
diff --git a/noao/imred/ccdred/ccddb/kpno/coude.dat b/noao/imred/ccdred/ccddb/kpno/coude.dat
new file mode 100644
index 00000000..f32350aa
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/coude.dat
@@ -0,0 +1,9 @@
+subset		gratpos
+
+DARK		dark
+BIAS		zero
+OBJECT		object
+'DOME FLAT'	flat
+'PROJECTOR FLAT' flat
+'COMPARISON'	comp
+'SKY FLAT'      object
diff --git a/noao/imred/ccdred/ccddb/kpno/cryocam.cl b/noao/imred/ccdred/ccddb/kpno/cryocam.cl
new file mode 100644
index 00000000..1e917ff2
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/cryocam.cl
@@ -0,0 +1,3 @@
+cl < "ccddb$kpno/default.cl"
+
+ccdred.instrument = "ccddb$kpno/cryocam.dat"
diff --git a/noao/imred/ccdred/ccddb/kpno/cryocam.dat b/noao/imred/ccdred/ccddb/kpno/cryocam.dat
new file mode 100644
index 00000000..f0a6134b
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/cryocam.dat
@@ -0,0 +1,9 @@
+subset		filters
+
+DARK		dark
+BIAS		zero
+OBJECT		object
+'DOME FLAT'	flat
+'PROJECTOR FLAT' flat
+'COMPARISON'	comp
+'SKY FLAT'      object
diff --git a/noao/imred/ccdred/ccddb/kpno/default.cl b/noao/imred/ccdred/ccddb/kpno/default.cl
new file mode 100644
index 00000000..df16c7b6
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/default.cl
@@ -0,0 +1,41 @@
+# Default KPNO parameters.
+
+ccdred.pixeltype = "real real"
+ccdred.verbose = yes
+ccdred.logfile = "logfile"
+ccdred.plotfile = ""
+ccdred.backup = ""
+ccdred.instrument = "ccddb$kpno/default.dat"
+ccdred.ssfile = "subsets"
+ccdred.graphics = "stdgraph"
+ccdred.cursor = ""
+
+ccdproc.ccdtype = ""
+ccdproc.fixpix = no
+ccdproc.overscan = yes
+ccdproc.trim = yes
+ccdproc.zerocor = yes
+ccdproc.darkcor = no
+ccdproc.flatcor = no
+ccdproc.readcor = no
+ccdproc.scancor = no
+ccdproc.readaxis = "line"
+ccdproc.biassec = "image"
+ccdproc.trimsec = "image"
+ccdproc.interactive = yes
+ccdproc.function = "chebyshev"
+ccdproc.order = 1
+ccdproc.sample = "*"
+ccdproc.naverage = 1
+ccdproc.niterate = 1
+ccdproc.low_reject = 3
+ccdproc.high_reject = 3
+ccdproc.grow = 0
+
+combine.rdnoise= "rdnoise"
+combine.gain="gain"
+zerocombine.rdnoise= "rdnoise"
+zerocombine.gain="gain"
+flatcombine.rdnoise= "rdnoise"
+flatcombine.gain="gain"
+flatcombine.reject = "crreject"
diff --git a/noao/imred/ccdred/ccddb/kpno/demo.cl b/noao/imred/ccdred/ccddb/kpno/demo.cl
new file mode 100644
index 00000000..51c54909
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/demo.cl
@@ -0,0 +1,72 @@
+# Demonstration parameter setting script.
+
+# Set package parameters:
+ccdred.pixeltype = "real real"
+ccdred.verbose = yes
+ccdred.logfile = "Demo.log"
+ccdred.plotfile = "Demo.plots"
+ccdred.backup = "B"
+ccdred.ssfile = "Demo.subsets"
+
+# Set processing parameters:
+ccdproc.fixpix = yes
+ccdproc.overscan = yes
+ccdproc.trim = yes
+ccdproc.zerocor = yes
+ccdproc.darkcor = yes
+ccdproc.flatcor = yes
+ccdproc.illumcor = no
+ccdproc.fringecor = no
+ccdproc.readcor = no
+ccdproc.scancor = no
+ccdproc.readaxis = "line"
+ccdproc.fixfile = "ccdtest$badpix.dat"
+ccdproc.biassec = "image"
+ccdproc.trimsec = "image"
+ccdproc.zero = ""
+ccdproc.dark = ""
+ccdproc.flat = ""
+ccdproc.illum = ""
+ccdproc.fringe = ""
+ccdproc.scantype = "shortscan"
+ccdproc.nscan = 1
+ccdproc.interactive = yes
+ccdproc.function = "legendre"
+ccdproc.order = 1
+ccdproc.sample = "*"
+ccdproc.naverage = 1
+ccdproc.niterate = 1
+ccdproc.low_reject = 3.
+ccdproc.high_reject = 3.
+ccdproc.grow = 0.
+flatcombine.process = no
+
+# Set demonstration observation parameters:
+artobs.ncols = 132
+artobs.nlines = 100
+artobs.filter = ""
+artobs.datasec = "[1:100,1:100]"
+artobs.trimsec = "[3:98,3:98]"
+artobs.biassec = "[103:130,*]"
+artobs.imdata = ""
+artobs.skyrate = 0.
+artobs.badpix = "ccdtest$badpix.dat"
+artobs.biasval = 500.
+artobs.badval = 500.
+artobs.zeroval = 100.
+artobs.darkrate = 1.
+artobs.zeroslope = 0.01
+artobs.darkslope = 0.002
+artobs.flatslope = 3.0000000000000E-4
+artobs.sigma = 5.
+artobs.seed = 0
+artobs.overwrite = no
+
+# Set demonstration subsection readout parameters:
+subsection.ncols = 82
+subsection.nlines = 50
+subsection.ccdsec = "[26:75,26:75]"
+subsection.datasec = "[1:50,1:50]"
+subsection.trimsec = ""
+subsection.biassec = "[51:82,1:50]"
+subsection.overwrite = no
diff --git a/noao/imred/ccdred/ccddb/kpno/demo.dat b/noao/imred/ccdred/ccddb/kpno/demo.dat
new file mode 100644
index 00000000..72697f58
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/demo.dat
@@ -0,0 +1,3 @@
+imagetyp	ccdtype
+exptime		integ
+subset		filter
diff --git a/noao/imred/ccdred/ccddb/kpno/direct.cl b/noao/imred/ccdred/ccddb/kpno/direct.cl
new file mode 100644
index 00000000..dfa9bc51
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/direct.cl
@@ -0,0 +1,4 @@
+cl < "ccddb$kpno/default.cl"
+
+ccdred.instrument = "ccddb$kpno/direct.dat"
+ccdproc.flatcor = yes
diff --git a/noao/imred/ccdred/ccddb/kpno/direct.dat b/noao/imred/ccdred/ccddb/kpno/direct.dat
new file mode 100644
index 00000000..f0a6134b
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/direct.dat
@@ -0,0 +1,9 @@
+subset		filters
+
+DARK		dark
+BIAS		zero
+OBJECT		object
+'DOME FLAT'	flat
+'PROJECTOR FLAT' flat
+'COMPARISON'	comp
+'SKY FLAT'      object
diff --git a/noao/imred/ccdred/ccddb/kpno/echelle.cl b/noao/imred/ccdred/ccddb/kpno/echelle.cl
new file mode 100644
index 00000000..a011cc8f
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/echelle.cl
@@ -0,0 +1,3 @@
+cl < "ccddb$kpno/default.cl"
+
+ccdred.instrument = "ccddb$kpno/echelle.dat"
diff --git a/noao/imred/ccdred/ccddb/kpno/echelle.dat b/noao/imred/ccdred/ccddb/kpno/echelle.dat
new file mode 100644
index 00000000..f0a6134b
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/echelle.dat
@@ -0,0 +1,9 @@
+subset		filters
+
+DARK		dark
+BIAS		zero
+OBJECT		object
+'DOME FLAT'	flat
+'PROJECTOR FLAT' flat
+'COMPARISON'	comp
+'SKY FLAT'      object
diff --git a/noao/imred/ccdred/ccddb/kpno/fibers.cl b/noao/imred/ccdred/ccddb/kpno/fibers.cl
new file mode 100644
index 00000000..bb1e0398
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/fibers.cl
@@ -0,0 +1,3 @@
+cl < "ccddb$kpno/default.cl"
+
+ccdred.instrument = "ccddb$kpno/fibers.dat"
diff --git a/noao/imred/ccdred/ccddb/kpno/fibers.dat b/noao/imred/ccdred/ccddb/kpno/fibers.dat
new file mode 100644
index 00000000..f0a6134b
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/fibers.dat
@@ -0,0 +1,9 @@
+subset		filters
+
+DARK		dark
+BIAS		zero
+OBJECT		object
+'DOME FLAT'	flat
+'PROJECTOR FLAT' flat
+'COMPARISON'	comp
+'SKY FLAT'      object
diff --git a/noao/imred/ccdred/ccddb/kpno/fits.dat b/noao/imred/ccdred/ccddb/kpno/fits.dat
new file mode 100644
index 00000000..f47abf8d
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/fits.dat
@@ -0,0 +1,21 @@
+exptime		itime
+darktime	itime
+imagetyp	data-typ
+subset		f1pos
+biassec		biassec []
+datasec		datasec []
+
+fixpix		bp-flag 0
+overscan	bt-flag 0
+zerocor		bi-flag 0
+darkcor		dk-flag 0
+flatcor		ff-flag 0
+fringcor	fr-flag 0
+
+'object (  0 )'		object
+'dark (  1 )'		dark
+'proj flat (  2 )'	flat
+'sky flat (  3 )'	other
+'comp (  4 )'		other
+'bias (  5 )'		zero
+'dome flat (  6 )'	flat
diff --git a/noao/imred/ccdred/ccddb/kpno/foe.cl b/noao/imred/ccdred/ccddb/kpno/foe.cl
new file mode 100644
index 00000000..da4081cb
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/foe.cl
@@ -0,0 +1,3 @@
+cl < "ccddb$kpno/default.cl"
+
+ccdred.instrument = "ccddb$kpno/foe.dat"
diff --git a/noao/imred/ccdred/ccddb/kpno/foe.dat b/noao/imred/ccdred/ccddb/kpno/foe.dat
new file mode 100644
index 00000000..f0a6134b
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/foe.dat
@@ -0,0 +1,9 @@
+subset		filters
+
+DARK		dark
+BIAS		zero
+OBJECT		object
+'DOME FLAT'	flat
+'PROJECTOR FLAT' flat
+'COMPARISON'	comp
+'SKY FLAT'      object
diff --git a/noao/imred/ccdred/ccddb/kpno/hydra.cl b/noao/imred/ccdred/ccddb/kpno/hydra.cl
new file mode 100644
index 00000000..b24dc05e
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/hydra.cl
@@ -0,0 +1,12 @@
+cl < "ccddb$kpno/default.cl"
+
+ccdred.instrument = "ccddb$kpno/hydra.dat"
+
+combine.gain = "gain_12"
+combine.rdnoise = "noise_12"
+zerocombine.gain = "gain_12"
+zerocombine.rdnoise = "noise_12"
+darkcombine.gain = "gain_12"
+darkcombine.rdnoise = "noise_12"
+flatcombine.gain = "gain_12"
+flatcombine.rdnoise = "noise_12"
diff --git a/noao/imred/ccdred/ccddb/kpno/hydra.dat b/noao/imred/ccdred/ccddb/kpno/hydra.dat
new file mode 100644
index 00000000..f0a6134b
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/hydra.dat
@@ -0,0 +1,9 @@
+subset		filters
+
+DARK		dark
+BIAS		zero
+OBJECT		object
+'DOME FLAT'	flat
+'PROJECTOR FLAT' flat
+'COMPARISON'	comp
+'SKY FLAT'      object
diff --git a/noao/imred/ccdred/ccddb/kpno/instruments.men b/noao/imred/ccdred/ccddb/kpno/instruments.men
new file mode 100644
index 00000000..5dea4af6
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/instruments.men
@@ -0,0 +1,12 @@
+direct          Current headers for Sun plus CCDPROC setup for direct CCD
+specphot        Current headers for Sun plus CCDPROC setup for spectropho-
+                  tometry, ie GoldCam, barefoot CCD
+hydra           WIYN Hydra with Arcon
+foe             Current headers for Sun plus CCDPROC setup for FOE
+fibers          Current headers for Sun plus CCDPROC setup for fiber array
+coude           Current headers for Sun plus CCDPROC setup for Coude
+cyrocam         Current headers for Sun plus CCDPROC setup for Cryo Cam
+echelle         Current headers for Sun plus CCDPROC setup for Echelle
+kpnoheaders     Current headers with no changes to CCDPROC parameters
+fits	        Mountain FITS header prior to Aug. 87 (?)
+camera		Mountain CAMERA header for IRAF Version 2.6 and earlier
diff --git a/noao/imred/ccdred/ccddb/kpno/kpnoheaders.dat b/noao/imred/ccdred/ccddb/kpno/kpnoheaders.dat
new file mode 100644
index 00000000..f0a6134b
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/kpnoheaders.dat
@@ -0,0 +1,9 @@
+subset		filters
+
+DARK		dark
+BIAS		zero
+OBJECT		object
+'DOME FLAT'	flat
+'PROJECTOR FLAT' flat
+'COMPARISON'	comp
+'SKY FLAT'      object
diff --git a/noao/imred/ccdred/ccddb/kpno/specphot.cl b/noao/imred/ccdred/ccddb/kpno/specphot.cl
new file mode 100644
index 00000000..4359279d
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/specphot.cl
@@ -0,0 +1,5 @@
+cl < "ccddb$kpno/default.cl"
+
+ccdred.instrument = "ccddb$kpno/specphot.dat"
+ccdproc.trimsec = ""
+ccdproc.grow = 1
diff --git a/noao/imred/ccdred/ccddb/kpno/specphot.dat b/noao/imred/ccdred/ccddb/kpno/specphot.dat
new file mode 100644
index 00000000..f0a6134b
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/specphot.dat
@@ -0,0 +1,9 @@
+subset		filters
+
+DARK		dark
+BIAS		zero
+OBJECT		object
+'DOME FLAT'	flat
+'PROJECTOR FLAT' flat
+'COMPARISON'	comp
+'SKY FLAT'      object
diff --git a/noao/imred/ccdred/ccddb/kpno/sunlink.cl b/noao/imred/ccdred/ccddb/kpno/sunlink.cl
new file mode 100644
index 00000000..1f5fe7fe
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/sunlink.cl
@@ -0,0 +1,4 @@
+cl < "ccddb$kpno/default.cl"
+
+ccdred.instrument = "ccddb$kpno/sunlink.dat"
+ccdproc.flatcor = yes
diff --git a/noao/imred/ccdred/ccddb/kpno/sunlink.dat b/noao/imred/ccdred/ccddb/kpno/sunlink.dat
new file mode 100644
index 00000000..44d237d6
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/sunlink.dat
@@ -0,0 +1,8 @@
+subset		filters
+
+DARK		dark
+BIAS		zero
+OBJECT		object
+'DOME FLAT'	flat
+'PROJECTOR FLAT' flat
+'COMPARISON'	comp
diff --git a/noao/imred/ccdred/ccddb/kpno/template.cl b/noao/imred/ccdred/ccddb/kpno/template.cl
new file mode 100644
index 00000000..b5284029
--- /dev/null
+++ b/noao/imred/ccdred/ccddb/kpno/template.cl
@@ -0,0 +1,25 @@
+# Template parameter setting script.  These parameters should be
+# set for a particular instrument.
+
+ccdproc.fixpix =
+ccdproc.overscan =
+ccdproc.trim =
+ccdproc.zerocor =
+ccdproc.darkcor =
+ccdproc.flatcor =
+ccdproc.readcor =
+ccdproc.scancor =
+ccdproc.readaxis =
+ccdproc.fixfile = 
+ccdproc.biassec = 
+ccdproc.datasec = 
+ccdproc.scantype =
+ccdproc.interactive =
+ccdproc.function =
+ccdproc.order =
+ccdproc.sample =
+ccdproc.naverage =
+ccdproc.niterate =
+ccdproc.low_reject =
+ccdproc.high_reject =
+ccdproc.grow =
diff --git a/noao/imred/ccdred/ccdgroups.par b/noao/imred/ccdred/ccdgroups.par
new file mode 100644
index 00000000..4b8d5007
--- /dev/null
+++ b/noao/imred/ccdred/ccdgroups.par
@@ -0,0 +1,5 @@
+images,s,a,,,,CCD images to group
+output,s,a,,,,Output root group filename
+group,s,h,"ccdtype","position|title|date|ccdtype|subset",,Group type
+radius,r,h,"60",,,Group position radius (arc sec)
+ccdtype,s,h,"",,,CCD image types to select
diff --git a/noao/imred/ccdred/ccdhedit.par b/noao/imred/ccdred/ccdhedit.par
new file mode 100644
index 00000000..5695dffa
--- /dev/null
+++ b/noao/imred/ccdred/ccdhedit.par
@@ -0,0 +1,4 @@
+images,s,a,,,,CCD images
+parameter,s,a,,,,Image header parameter
+value,s,a,,,,Parameter value
+type,s,h,"string","string|real|integer",,Parameter type (string|real|integer)
diff --git a/noao/imred/ccdred/ccdinstrument.par b/noao/imred/ccdred/ccdinstrument.par
new file mode 100644
index 00000000..99bec801
--- /dev/null
+++ b/noao/imred/ccdred/ccdinstrument.par
@@ -0,0 +1,5 @@
+images,s,a,,,,List of images
+instrument,s,h,)_.instrument,,,CCD instrument file
+ssfile,s,h,)_.ssfile,,,Subset translation file
+edit,b,h,yes,,,Edit instrument translation file?
+parameters,s,h,"basic","basic|common|all",,Parameters to be displayed
diff --git a/noao/imred/ccdred/ccdlist.par b/noao/imred/ccdred/ccdlist.par
new file mode 100644
index 00000000..3eb82917
--- /dev/null
+++ b/noao/imred/ccdred/ccdlist.par
@@ -0,0 +1,5 @@
+images,s,a,,,,CCD images to listed
+ccdtype,s,h,"",,,CCD image type to be listed
+names,b,h,no,,,List image names only?
+long,b,h,no,,,Long format listing?
+ccdproc,pset,h,,,,CCD processing parameters
diff --git a/noao/imred/ccdred/ccdmask.par b/noao/imred/ccdred/ccdmask.par
new file mode 100644
index 00000000..8127f4dc
--- /dev/null
+++ b/noao/imred/ccdred/ccdmask.par
@@ -0,0 +1,12 @@
+image,f,a,,,,Input image
+mask,f,a,,,,Output pixel mask
+ncmed,i,h,7,1,,Column box size for median level calculation
+nlmed,i,h,7,1,,Line box size for median level calculation
+ncsig,i,h,15,10,,Column box size for sigma calculation
+nlsig,i,h,15,10,,Line box size for sigma calculation
+lsigma,r,h,6.,,,Low clipping sigma
+hsigma,r,h,6.,,,High clipping sigma
+ngood,i,h,5,1,,Minimum column length of good pixel seqments
+linterp,i,h,2,1,,Mask value for line interpolation 
+cinterp,i,h,3,1,,Mask value for column interpolation 
+eqinterp,i,h,2,1,,Mask value for equal interpolation
diff --git a/noao/imred/ccdred/ccdproc.par b/noao/imred/ccdred/ccdproc.par
new file mode 100644
index 00000000..f86ad07d
--- /dev/null
+++ b/noao/imred/ccdred/ccdproc.par
@@ -0,0 +1,39 @@
+images,s,a,"",,,List of CCD images to correct
+output,s,h,"",,,List of output CCD images
+ccdtype,s,h,"object",,,CCD image type to correct
+max_cache,i,h,0,0,,Maximum image caching memory (in Mbytes)
+noproc,b,h,no,,,"List processing steps only?
+"
+fixpix,b,h,yes,,,Fix bad CCD lines and columns?
+overscan,b,h,yes,,,Apply overscan strip correction?
+trim,b,h,yes,,,Trim the image?
+zerocor,b,h,yes,,,Apply zero level correction?
+darkcor,b,h,yes,,,Apply dark count correction?
+flatcor,b,h,yes,,,Apply flat field correction?
+illumcor,b,h,no,,,Apply illumination correction?
+fringecor,b,h,no,,,Apply fringe correction?
+readcor,b,h,no,,,Convert zero level image to readout correction?
+scancor,b,h,no,,,"Convert flat field image to scan correction?
+"
+readaxis,s,h,"line","column|line",, Read out axis (column|line)
+fixfile,s,h,"",,,File describing the bad lines and columns
+biassec,s,h,"",,,Overscan strip image section
+trimsec,s,h,"",,,Trim data section
+zero,s,h,"",,,Zero level calibration image
+dark,s,h,"",,,Dark count calibration image
+flat,s,h,"",,,Flat field images
+illum,s,h,"",,,Illumination correction images
+fringe,s,h,"",,,Fringe correction images
+minreplace,r,h,1.,,,Minimum flat field value
+scantype,s,h,"shortscan","shortscan|longscan",,Scan type (shortscan|longscan)
+nscan,i,h,1,1,,"Number of short scan lines
+"
+interactive,b,h,no,,,Fit overscan interactively?
+function,s,h,"legendre",,,Fitting function
+order,i,h,1,1,,Number of polynomial terms or spline pieces
+sample,s,h,"*",,,Sample points to fit
+naverage,i,h,1,,,Number of sample points to combine
+niterate,i,h,1,0,,Number of rejection iterations
+low_reject,r,h,3.,0.,,Low sigma rejection factor
+high_reject,r,h,3.,0.,,High sigma rejection factor
+grow,r,h,0.,0.,,Rejection growing radius
diff --git a/noao/imred/ccdred/ccdred.cl b/noao/imred/ccdred/ccdred.cl
new file mode 100644
index 00000000..d289b1ed
--- /dev/null
+++ b/noao/imred/ccdred/ccdred.cl
@@ -0,0 +1,29 @@
+#{ CCDRED -- CCD Reduction Package
+
+set	ccddb	= "ccdred$ccddb/"
+set	ccdtest	= "ccdred$ccdtest/"
+
+package ccdred
+
+task	$ccdtest	= ccdtest$ccdtest.cl
+
+task	badpiximage,
+	ccdgroups,
+	ccdhedit,
+	ccdinstrument,
+	ccdlist,
+	ccdmask,
+	ccdproc,
+	combine,
+	mkfringecor,
+	mkillumcor,
+	mkillumflat,
+	mkskycor,
+	mkskyflat	= ccdred$x_ccdred.e
+
+task	darkcombine	= ccdred$darkcombine.cl
+task	flatcombine	= ccdred$flatcombine.cl
+task	setinstrument	= ccdred$setinstrument.cl
+task	zerocombine	= ccdred$zerocombine.cl
+
+clbye()
diff --git a/noao/imred/ccdred/ccdred.hd b/noao/imred/ccdred/ccdred.hd
new file mode 100644
index 00000000..c98f5a87
--- /dev/null
+++ b/noao/imred/ccdred/ccdred.hd
@@ -0,0 +1,38 @@
+# Help directory for the CCDRED package.
+
+$doc = "./doc/"
+
+badpiximage	hlp=doc$badpiximage.hlp
+ccdgroups	hlp=doc$ccdgroups.hlp
+ccdhedit	hlp=doc$ccdhedit.hlp
+ccdlist		hlp=doc$ccdlist.hlp
+ccdmask		hlp=doc$ccdmask.hlp
+ccdproc		hlp=doc$ccdproc.hlp
+combine		hlp=doc$combine.hlp
+darkcombine	hlp=doc$darkcombine.hlp
+flatcombine	hlp=doc$flatcombine.hlp
+mkfringecor	hlp=doc$mkfringecor.hlp
+mkillumcor	hlp=doc$mkillumcor.hlp
+mkillumflat	hlp=doc$mkillumflat.hlp
+mkskycor	hlp=doc$mkskycor.hlp
+mkskyflat	hlp=doc$mkskyflat.hlp
+setinstrument	hlp=doc$setinstrument.hlp
+zerocombine	hlp=doc$zerocombine.hlp
+
+ccdgeometry	hlp=doc$ccdgeometry.hlp
+ccdinstrument	hlp=doc$ccdinst.hlp
+ccdtypes	hlp=doc$ccdtypes.hlp
+flatfields	hlp=doc$flatfields.hlp
+guide		hlp=doc$guide.hlp
+instruments	hlp=doc$instruments.hlp
+package		hlp=doc$ccdred.hlp
+subsets		hlp=doc$subsets.hlp
+
+revisions	sys=Revisions
+
+$ccdtest	= "noao$imred/ccdred/ccdtest/"
+
+ccdtest		men=ccdtest$ccdtest.men,
+		hlp=..,
+		pkg=ccdtest$ccdtest.hd,
+		src=ccdtest$ccdtest.cl
diff --git a/noao/imred/ccdred/ccdred.men b/noao/imred/ccdred/ccdred.men
new file mode 100644
index 00000000..cbd02af8
--- /dev/null
+++ b/noao/imred/ccdred/ccdred.men
@@ -0,0 +1,28 @@
+    badpiximage - Create a bad pixel mask image from a bad pixel file
+      ccdgroups - Group CCD images into image lists
+       ccdhedit - CCD image header editor
+  ccdinstrument - Review and edit instrument translation files
+        ccdlist - List CCD processing information
+	ccdmask - Create bad pixel mask from CCD flat field images
+        ccdproc - Process CCD images
+        ccdtest - CCD test and demonstration package
+        combine - Combine CCD images
+    darkcombine - Combine and process dark count images
+    flatcombine - Combine and process flat field images
+    mkfringecor - Make fringe correction images from sky images
+     mkillumcor - Make flat field illumination correction images
+    mkillumflat - Make illumination corrected flat fields
+       mkskycor - Make sky illumination correction images
+      mkskyflat - Make sky corrected flat field images
+  setinstrument - Set instrument parameters
+    zerocombine - Combine and process zero level images
+
+    	      ADDITIONAL HELP TOPICS
+
+    ccdgeometry - Discussion of CCD coordinate/geometry keywords
+       ccdtypes - Description of the CCD image types
+     flatfields - Discussion of CCD flat field calibrations
+          guide - Introductory guide to using the CCDRED package
+    instruments - Instrument specific data files
+        package - CCD image reduction package
+        subsets - Description of CCD subsets
diff --git a/noao/imred/ccdred/ccdred.par b/noao/imred/ccdred/ccdred.par
new file mode 100644
index 00000000..218e7421
--- /dev/null
+++ b/noao/imred/ccdred/ccdred.par
@@ -0,0 +1,12 @@
+# CCDRED package parameter file
+
+pixeltype,s,h,"real real",,,Output and calculation pixel datatypes
+verbose,b,h,no,,,Print log information to the standard output?
+logfile,f,h,"logfile",,,Text log file
+plotfile,f,h,"",,,Log metacode plot file
+backup,s,h,"",,,Backup directory or prefix
+instrument,s,h,"",,,CCD instrument file
+ssfile,s,h,"subsets",,,Subset translation file
+graphics,s,h,"stdgraph",,,Interactive graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+version,s,h,"2: October 1987"
diff --git a/noao/imred/ccdred/ccdtest/artobs.cl b/noao/imred/ccdred/ccdtest/artobs.cl
new file mode 100644
index 00000000..b64294a6
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/artobs.cl
@@ -0,0 +1,109 @@
+# ARTOBS -- Make a CCD observation
+
+procedure artobs (image, exptime, ccdtype)
+
+string	image			{prompt="Image name"}
+real	exptime			{prompt="Exposure time"}
+string	ccdtype			{prompt="CCD type"}
+
+int	ncols=132		{prompt="Number of columns"}
+int	nlines=100		{prompt="Number of lines"}
+string	filter=""		{prompt="Filter"}
+string	datasec="[1:100,1:100]"	{prompt="Data section"}
+string	trimsec="[3:98,3:98]"	{prompt="Trim section"}
+string	biassec="[103:130,*]"	{prompt="Bias section"}
+
+file	imdata=""		{prompt="Image data"}
+real	skyrate=0.		{prompt="Sky count rate"}
+file	badpix=""		{prompt="Bad pixel regions"}
+real	biasval=500.		{prompt="Bias value"}
+real	badval=500.		{prompt="Bad pixel value"}
+real	zeroval=100.		{prompt="Zero level value"}
+real	darkrate=1.		{prompt="Dark count rate"}
+real	zeroslope=0.01		{prompt="Slope of zero level"}
+real	darkslope=0.002		{prompt="Slope of dark count rate"}
+real	flatslope=0.0003	{prompt="Flat field slope"}
+real	sigma=5.		{prompt="Gaussian sigma"}
+int	seed=0			{prompt="Random number seed"}
+bool	overwrite=no		{prompt="Overwrite existing image?"}
+
+begin
+	int	c1, c2, l1, l2
+	real	exp, value, valslope
+	string	im, type, s
+
+	im = image
+	exp = exptime
+	type = ccdtype
+
+	if (access (im//".imh") == yes)
+	    im = im // ".imh"
+	if (access (im//".hhh") == yes)
+	    im = im // ".hhh"
+	if (access (im) == yes) {
+	    if (overwrite == yes)
+		imdelete (im, verify=no)
+	    else
+	        return
+	}
+
+	# Create the image.
+	s = str (ncols) // " " // str (nlines)
+	mkimage (im, "make", 0., 2, s, pixtype="short", slope=0., sigma=sigma,
+	    seed=seed)
+
+	# Add a data image.
+	if (access (imdata//".imh") == yes)
+	    imdata = imdata // ".imh"
+	if (access (imdata//".hhh") == yes)
+	    imdata = imdata // ".hhh"
+	if (access (imdata) == yes)
+	    imcopy (imdata//datasec, im//datasec, verbose=no)
+
+	# Add sky.
+	value = exp * skyrate
+	if (value != 0.)
+	    mkimage (im//datasec, "add", value, slope=0., sigma=0.)
+
+	# Add flat field response.
+	if (flatslope != 0.)
+	    mkimage (im//datasec, "mul", 1., slope=flatslope, sigma=0.)
+	    
+	# Add zero level and dark count.
+	value = zeroval + exp * darkrate
+	valslope = zeroslope + exp * darkslope
+	if ((value != 0.) && (valslope != 0.))
+	    mkimage (im//datasec, "add", value, slope=valslope, sigma=0.)
+
+	# Add bias.
+	if (biasval != 0.)
+	    mkimage (im, "add", biasval, slope=0., sigma=sigma, seed=0)
+
+	# Set bad pixels.
+	if (access (badpix)) {
+	    list = badpix
+	    while (fscan (list, c1, c2, l1, l2) != EOF) {
+	        if (nscan() != 4)
+		    next
+	        c1 = max (1, c1)
+	        c2 = min (ncols, c2)
+	        l1 = max (1, l1)
+	        l2 = min (nlines, l2)
+	        s = "["//c1//":"//c2//","//l1//":"//l2//"]"
+	        mkimage (im//s, "replace", badval, slope=0., sigma=0.)
+	    }
+	}
+
+	# Set image header
+	ccdhedit (im, "exptime", exp, type="real")
+	if (type != "")
+	    ccdhedit (im, "imagetyp", type, type="string")
+	if (datasec != "")
+	    ccdhedit (im, "datasec", datasec, type="string")
+	if (trimsec != "")
+	    ccdhedit (im, "trimsec", trimsec, type="string")
+	if (biassec != "")
+	    ccdhedit (im, "biassec", biassec, type="string")
+	if (filter != "")
+	    ccdhedit (im, "subset", filter, type="string")
+end
diff --git a/noao/imred/ccdred/ccdtest/artobs.hlp b/noao/imred/ccdred/ccdtest/artobs.hlp
new file mode 100644
index 00000000..02f2cf0f
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/artobs.hlp
@@ -0,0 +1,127 @@
+.help artobs Oct87 noao.imred.ccdred.ccdtest
+.ih
+NAME
+artobs -- Make a demonstration CCD observation
+.ih
+USAGE
+artobs image exptime ccdtype
+.ih
+PARAMETERS
+.ls image
+Observation to be created.
+.le
+.ls exptime
+Exposure time of observation.
+.le
+.ls ccdtype
+CCD image type of observation.  This type is one of the standard types
+for the CCDRED package.
+.le
+.ls ncols = 132, nlines = 100
+The number of columns and lines in the full image created including
+bias section.
+.le
+.ls filter = ""
+Filter string for the observation.
+.le
+.ls datasec = "[1:100,1:100]"
+Data section of the observation.
+.le
+.ls trimsec = "[3:98,3:98]"
+Trim section for later processing.
+.le
+.ls biassec = "[103:130,*]"
+Prescan or overscan bias section.
+.le
+.ls imdata = ""
+Image to be used as source of observation if specified.  The image must
+be at least as large as the data section.
+.le
+.ls skyrate = 0.
+Sky counting rate.  The total sky value will be scaled by the exposure time.
+.le
+.ls badpix = ""
+Bad pixel region file in the standard CCDRED bad pixel file format.
+.le
+.ls biasval = 500.
+Mean bias value of the entire image.
+.le
+.ls badval = 500.
+Bad pixel value placed at the specified bad pixel regions.
+.le
+.ls zeroval = 100.
+Zero level of the data section.
+.le
+.ls darkrate = 1.
+Dark count rate.  The total dark count will be scaled by the exposure time
+.le
+.ls zeroslope = 0.01
+Slope of the zero level per pixel.
+.le
+.ls darkslope = 0.002
+Slope of the dark count rate per pixel.  This is also scaled by the exposure
+time.
+.le
+.ls flatslope = 3.0000000000000E-4
+The mean flat field response is 1 with a slope given by this value.
+.le
+.ls sigma = 5.
+Gaussian noise sigma per pixel.
+.le
+.ls seed = 0
+Random number seed.  If zero new values are used for every observation.
+.le
+.ls overwrite = no
+Overwrite an existing image?  If no a new observation is not created.
+There is no warning message.
+.le
+.ih
+DESCRIPTION
+This script task generates artificial CCD observations which include
+bad pixels, bias and zero levels, dark counts, flat field response
+variations and sky brightness levels.  Optionally, image data from
+a reference image may be included.  This task is designed to be used
+with the \fBccdred\fR package and includes appropriate image header
+information.
+
+First the task checks whether the requested image exists.  If it does
+exist and the overwrite flag is no then a new observations is not created.
+If the overwrite flag is set then the old image is deleted and a new
+observation is created.
+
+An empty image of the specified size and of pixel data type short is
+first created.  If a noise sigma is specified it is added to the entire
+image.  If a reference image is specified then image section given by
+the \fIdatasec\fR parameter is copied into the data section of the
+observation.  Next a sky level, specified by the \fIskyrate\fR
+parameter times the exposure time, is added to the data section.
+The flat field response with a mean of one and a slope given by the
+\fIflatslope\fR parameter is multiplied into the data section.  If
+a dark count rate and/or a zero level is specified then these effects
+are added to the data section.  Then the specified bias level
+is added to the entire image; i.e. including the bias section.
+Finally, the pixels specified in the bad pixel region file, if one
+is specified, are set to the bad pixel value.
+
+The CCD reduction parameters for the data section, the trim section,
+the bias section, exposure time, the CCD image type, and the filter
+are added to the image header (if they are specified) using \fBccdhedit\fR
+to apply any keyword translation.
+.ih
+EXAMPLES
+1. To create some test CCD images first set the task parameters such as
+number of columns and lines, data, bias, and trim sections, and data
+values.  The images are then created as follows:
+
+	cl> artobs.filter = "V"		# Set the filter
+	cl> artobs zero 0. zero		# Zero level image
+	cl> artobs dark 1000. dark skyrate=0.	# Dark count image
+	cl> artobs flat 1. flat skyrate=1000.	# Flat field image
+	cl> artobs obj 10. object		# Object image
+
+Note that the CCD image type is not used explicitly so that for a
+dark count image you must set the sky count rate to zero.
+.ih
+SEE ALSO
+mkimage, subsection, demo
+.endhelp
diff --git a/noao/imred/ccdred/ccdtest/badpix.dat b/noao/imred/ccdred/ccdtest/badpix.dat
new file mode 100644
index 00000000..92b13aa9
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/badpix.dat
@@ -0,0 +1,4 @@
+10 10 1 1000
+20 20 1 20
+30 30 50 100
+1 1000 50 50
diff --git a/noao/imred/ccdred/ccdtest/ccdtest.cl b/noao/imred/ccdred/ccdtest/ccdtest.cl
new file mode 100644
index 00000000..eb3f8b68
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/ccdtest.cl
@@ -0,0 +1,10 @@
+#{ CCDTEST -- CCDRED Test package
+
+package ccdtest
+
+task	mkimage		= ccdtest$x_ccdred.e
+task	artobs		= ccdtest$artobs.cl
+task	subsection	= ccdtest$subsection.cl
+task	demo		= ccdtest$demo.cl
+
+clbye()
diff --git a/noao/imred/ccdred/ccdtest/ccdtest.hd b/noao/imred/ccdred/ccdtest/ccdtest.hd
new file mode 100644
index 00000000..4218f9b0
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/ccdtest.hd
@@ -0,0 +1,6 @@
+# Help directory for the CCDTEST package.
+
+demo		hlp=demo.hlp,		src=demo.cl
+mkimage		hlp=mkimage.hlp,	src=t_mkimage.x
+artobs		hlp=artobs.hlp,		src=artobs.cl
+subsection	hlp=subsection.hlp,	src=subsection.cl
diff --git a/noao/imred/ccdred/ccdtest/ccdtest.men b/noao/imred/ccdred/ccdtest/ccdtest.men
new file mode 100644
index 00000000..f2b3909d
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/ccdtest.men
@@ -0,0 +1,4 @@
+	 artobs - Create an artificial CCD observation
+	   demo - Run a demonstration of the CCD reduction package
+	mkimage - Make or modify an image with simple values
+     subsection - Create an artificial subsection CCD observation
diff --git a/noao/imred/ccdred/ccdtest/demo.cl b/noao/imred/ccdred/ccdtest/demo.cl
new file mode 100644
index 00000000..213500c4
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/demo.cl
@@ -0,0 +1 @@
+stty (playback=demofile, verify=yes)
diff --git a/noao/imred/ccdred/ccdtest/demo.dat b/noao/imred/ccdred/ccdtest/demo.dat
new file mode 100644
index 00000000..733a319b
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/demo.dat
@@ -0,0 +1,182 @@
+\O=NOAO/IRAF V2.5 valdes@lyra Mon 15:42:35 12-Oct-87
+\T=vt640
+\G=vt640
+clear\n\{%V-%!200\}
+\n\{%10000
+			CCD REDUCTION DEMONSTRATION
+
+    In this demonstration we are going to make some (artificial) CCD
+    observations which we will reduce using the CCDRED package.  The
+    dome is opening and we are ready to begin observing...\}
+\n\{%V-\}
+unlearn\sccdred;unlearn\sccdtest\n\{	# Initialize parameters and data...\}
+imdelete\s%B%%*.*\sv-\n\{%V-\}
+imrename\sB*.*\s%B%%*.*\sv-\n\{%V-\}
+imdelete\sZero*.*,Flat*.*\n\{%V-\}
+delete\sDemo*\sv-\n\{%V-\}
+\n\{%V-\}
+setinstrument\sdemo\sreview-\n\{		# Set instrument parameters...\}
+lpar\sartobs\n\{				# List observing parameters...\}
+artobs\sobs001\s0.\szero\n\{%15000		# Observe zero level images...\}
+artobs\sobs002\s0.\szero\n\{%V-\}
+artobs\sobs003\s0.\szero\n\{%V-\}
+artobs\sobs004\s0.\szero\n\{%V-\}
+artobs\sobs005\s0.\szero\n\{%V-\}
+\n\{%V-\}
+artobs.skyrate=0\n\{			# Observe a long dark count...\}
+artobs\sobs006\s1000.\sdark\n\{%V-\}
+\n\{%V-\}
+artobs.filter="V"\n\{			# Observe V flat fields...\}
+artobs.skyrate=2000\n\{%V-\}
+artobs\sobs007\s1.\sflat\n\{%V-\}
+artobs\sobs008\s1.\sflat\n\{%V-\}
+artobs\sobs009\s1.\sflat\n\{%V-\}
+artobs\sobs010\s1.\sflat\n\{%V-\}
+artobs\sobs011\s2.\sflat\n\{%V-\}
+artobs\sobs012\s2.\sflat\n\{%V-\}
+\n\{%V-\}
+artobs.filter="B"\n\{			# Observe B flat fields...\}
+artobs.skyrate=1000\n\{%V-\}
+artobs\sobs013\s1.\sflat\n\{%V-\}
+artobs\sobs014\s2.\sflat\n\{%V-\}
+artobs\sobs015\s3.\sflat\n\{%V-\}
+artobs\sobs016\s3.\sflat\n\{%V-\}
+artobs\sobs017\s3.\sflat\n\{%V-\}
+artobs\sobs018\s3.\sflat\n\{%V-\}
+\n\{%V-\}
+artobs.filter="V"\n\{			# Observe objects...\}
+artobs.skyrate=100\n\{%V-\}
+artobs\sobs019\s10.\sobject\simdata=dev$pix\n\{%V-\}
+artobs\sobs020\s20.\sobject\simdata=dev$pix\n\{%V-\}
+artobs.filter="B"\n\{%V-\}
+artobs\sobs021\s30.\sobject\simdata=dev$pix\n\{%V-\}
+artobs\sobs022\s40.\sobject\simdata=dev$pix\n\{%V-\}
+\n\{%V-\}
+lpar\ssubsection\n\{			# Subsection readout parameters...\}
+subsection\sobs023\sobs019\n\{%5000		# Readout a subsection of the CCD...\}
+dir\n\{					# Check directory of observations...\}
+clear\n\{%10000				# Continue...\}
+\n\{%15000
+			INSTRUMENT SETUP
+
+    Because there are a variety of instruments, observatories, and data
+    formats there are many parameters.  To set all of these conveniently
+    there is a task which reads setup files prepared by the observing
+    staff.  The setup task:
+	1.  Defines an instrument header translation file which
+	    translates the image header parameters to something
+	    the CCDRED package understands.  This is an important
+	    feature of the package.
+	2.  It runs a setup script which sets parameters and performs
+	    other functions desired by the observing staff.
+	3.  The user is then given the opportunity to modify the
+	    package and processing parameters...\}
+\n\{%V-\}
+setinstrument\smode=m\n\{		# Set demo instrument parameters...\}
+demo\r
+\{%5000\}^Z
+\{%5000\}^Z
+\{%5000\}\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+Zero\r
+\r
+Flat*.*\r
+^Z
+clear\n\{%5000				# Continue...\}
+\n\{%20000
+				IMAGE HEADERS
+
+    The CCDRED package uses image header information if present.  This
+    includes the type of data (object, flat field, etc.), exposure
+    time, region of image containing the data, processing status, and
+    more.  To make this more general there is a instrument header
+    translation file to translate image header keywords to the standard
+    names used by the package.  In this example the image header
+    keywords are identical to the package except that the image type is
+    CCDTYPE, the exposure time is INTEG and the subset parameter is
+    FILTER.  Let's look at the image header using the the standard
+    image header lister and the special one in the CCDRED package.
+    This special lister provides additional information about image
+    types and processing status...\}
+
+\n\{%V-\}
+imheader\sobs023\sl+\n\{			# List object image header...\}
+ccdlist\sobs*.*\n\{%5000			# List short CCD status...\}
+ccdlist\sobs023\sl+\n\{%5000			# List long CCD status...\}
+clear\n\{%5000					# Continue...\}
+\n\{%20000
+			COMBINE CALIBRATION IMAGES
+
+    In order to reduce calibration noise and eliminate cosmic ray events
+    we combine many zero level and flat field calibration images.  The
+    combining task provides many options.  We will combine the images by
+    scaling each image to the same exposure time, rejecting the highest
+    pixel at each image point, and taking a weighted average of the
+    remainder.  Flat field images must be combined separately for each
+    filter.  We will simply specify all the images and the task automatically
+    selects the appropriate images to combine! ...\}
+\n\{%V-\}
+zerocombine\smode=m\n\{			# Combine zero level images...\}
+obs*.*\r
+\{%5000\}^Z
+flatcombine\smode=m\n\{			# Combine flat field images...\}
+obs*.*\r
+\{%5000\}^Z
+clear\n\{%5000			# Continue...\}
+\n\{%15000
+			PROCESS OBSERVATIONS
+
+    We are now ready to process our observations.  The processing steps we
+    have selected are to replace bad pixels by interpolation, fit and
+    subtract a readout bias given by an overscan strip, subtract the zero
+    level calibration image, scale and subtract a dark count calibration,
+    divide by a flat field, trim the image of the overscan strip and border
+    columns and lines.  The task which does this is "ccdproc".  The task is
+    expert at reducing CCD observations easily and efficiently.  It checks
+    the image types, applies the proper filter flat field, applies the
+    proper part of the calibration images to subsection readouts, does only
+    the processing steps selected if not done previously, and automatically
+    processes the calibration images as needed.  As before we simply specify
+    all the images and the task selects the appropriate images to process
+    including finding the one dark count image "obs006".  Watch the log
+    messages to see what the task is doing...\}
+\n\{%V-\}
+ccdproc\sobs*.*\n\{			# Process object images...\}
+\n\{%V-\}
+\{%V-\}q0,+,\r
+NO\n\{%V-\}
+\n\{%10000
+    That's it!  We're done.  Now lets check the results.  The "ccdlist"
+    listing will show the processing status and the images are now smaller
+    and of pixel datatype real.  The CCDSEC parameter identifies the relation
+    of the image to the actual CCD pixels of the detector...\}
+\n\{%V-\}
+ccdlist\sobs*.*\sccdtype=object\n\{		# List short CCD status...\}
+ccdlist\sobs023\sl+\n\{%5000			# List long CCD status...\}
+imhead\sobs023\sl+\n\{%5000			# List object image header...\}
+dir\n\{%5000				# Check the data directory...\}
+\n\{%V-
+    We specified that the original images be saved by using the prefix B.
+    We are also left with a text log file, a metacode file containing the
+    fits to the overscan regions, and a file which maps the filter subset
+    strings to short identifiers used in CCDLIST and when creating the
+    combined images "FlatV" and "FlatB".  You may look through these files,
+    or use GKIMOSAIC to examine the metacode file, now if you want.
+\}
diff --git a/noao/imred/ccdred/ccdtest/demo.hlp b/noao/imred/ccdred/ccdtest/demo.hlp
new file mode 100644
index 00000000..c03d5efb
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/demo.hlp
@@ -0,0 +1,27 @@
+.help demo Oct87 noao.imred.ccdred.ccdtest
+.ih
+NAME
+demo -- Run a demonstration of the CCD reduction package
+.ih
+USAGE
+demo
+.ih
+PARAMETERS
+.ls demofile = "ccdtest$demo.dat"
+Demonstration playback file.
+.le
+.ih
+DESCRIPTION
+This script task runs a demonstration playback.  The playback file
+is specified by a hidden parameter.  Normally this default playback file
+is used.  The default demonstration will use the task \fBtv.display\fR if it
+is loaded to show you the CCD frames being processed.
+.ih
+EXAMPLES
+1. To run a demonstration of the \fBccdred\fR package:
+
+	cl> demo
+.ih
+SEE ALSO
+stty
+.endhelp
diff --git a/noao/imred/ccdred/ccdtest/demo.par b/noao/imred/ccdred/ccdtest/demo.par
new file mode 100644
index 00000000..70bee0f3
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/demo.par
@@ -0,0 +1 @@
+demofile,s,h,"ccdtest$demo.dat",,,Demonstration playback file
diff --git a/noao/imred/ccdred/ccdtest/mkimage.hlp b/noao/imred/ccdred/ccdtest/mkimage.hlp
new file mode 100644
index 00000000..2be4ab5b
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/mkimage.hlp
@@ -0,0 +1,87 @@
+.help mkimage Oct87 noao.imred.ccdred.ccdtest
+.ih
+NAME
+mkimage -- Make or modify and image with simple values
+.ih
+USAGE
+mkimage image option value [ndim dims]
+.ih
+PARAMETERS
+.ls image
+Image to create or modify.
+.le
+.ls option
+Editing option which is one of the following:
+.ls make
+Make a new image of the specified size, dimensionality, pixel type, and values.
+.le
+.ls replace
+Replace pixel values in the image.
+.le
+.ls add
+Add to the pixel values in the image.
+.le
+.ls multiply
+Multiply the pixel values in the image.
+.le
+.le
+.ls value
+Mean pixel value to be used.
+.le
+.ls ndim
+Number of dimensions when creating a new image.
+.le
+.ls dims
+Image dimensions given as a white space separated string (see the examples).
+.le
+.ls pixtype = "real"
+Pixel datatype when creating an image.  The types are "real", "short",
+"integer", "long", and "double".
+.le
+.ls slope = 0.
+Slope of pixel values per pixel.
+.le
+.ls sigma = 0.
+Gaussian noise of pixel values if not zero.
+.le
+.ls seed = 0
+Seed for random numbers.  If zero then the first time the task is
+called a seed of 1 is used and all subsequent calls while the task is in
+the process cache continue with new random numbers.
+.le
+.ih
+DESCRIPTION
+An image is created or modified using simple values.  This task is intended
+for test and demonstration purposes.  A image may be created of a specified
+size, dimensionality, and pixel datatype.  The pixel values used in creating
+or editing an image consist of a sloped plane (which repeats for dimensions
+greater than 2) with pseudo-Gaussian noise. The sloped plane is defined such
+that:
+
+   pix[i,j] = value + slope * ((ncols + nlines) / 2 - 1) + slope * (i + j)
+
+where i and j are the pixel indices (starting with 1) and ncols and nlines
+are the number of columns and lines.  The interpretation of "value" is that
+it is the mean of the plane.  The Gaussian noise is only approximately random
+for purposes of speed!
+.ih
+EXAMPLES
+1. To create an 2 dimensional real image of size 100 x 200 with all zero
+values:
+
+	cl> mkimage name make 0 2 "100 200"
+
+Note that the dimension string is quoted because of the blank separated
+values.
+
+2. To add noise with a sigma of 5:
+
+	cl> mkimage name add 0 sigma=5
+
+2. To replace a region of the image with the value 10:
+
+	cl> mkimage name[10:20,30:40] replace 10
+.ih
+SEE ALSO
+artobs, subsection
+.endhelp
diff --git a/noao/imred/ccdred/ccdtest/mkimage.par b/noao/imred/ccdred/ccdtest/mkimage.par
new file mode 100644
index 00000000..148bf7ea
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/mkimage.par
@@ -0,0 +1,10 @@
+image,s,a,,,,Image to make or modify
+option,s,a,,"make|replace|add|multiply",,Editing option
+value,r,a,,,,Mean pixel value
+slope,r,h,0.,,,Slope of pixel values
+sigma,r,h,0.,0.,,Noise sigma
+seed,i,h,0,0,,Seed for noise generator
+
+ndim,i,a,,1,7,Number of dimensions
+dims,s,a,,,,Image dimensions
+pixtype,s,h,"real","short|real",,Pixel datatype
diff --git a/noao/imred/ccdred/ccdtest/mkpkg b/noao/imred/ccdred/ccdtest/mkpkg
new file mode 100644
index 00000000..79fcb59c
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/mkpkg
@@ -0,0 +1,10 @@
+# Make CCDTEST Package.
+
+$checkout libpkg.a ..
+$update   libpkg.a
+$checkin  libpkg.a ..
+$exit
+
+libpkg.a:
+	t_mkimage.x	<imhdr.h>
+	;
diff --git a/noao/imred/ccdred/ccdtest/subsection.cl b/noao/imred/ccdred/ccdtest/subsection.cl
new file mode 100644
index 00000000..60522c8b
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/subsection.cl
@@ -0,0 +1,53 @@
+# SUBSECTION -- Make a subsection CCD observation
+
+procedure subsection (subimage, image)
+
+string	subimage		{prompt="Subsection image name"}
+string	image			{prompt="Full image name"}
+
+int	ncols=82		{prompt="Number of columns"}
+int	nlines=50		{prompt="Number of lines"}
+string	ccdsec="[26:75,26:75]"	{prompt="CCD section"}
+string	datasec="[1:50,1:50]"	{prompt="Data section"}
+string	trimsec=""		{prompt="Trim section"}
+string	biassec="[51:82,1:50]"	{prompt="Bias section"}
+bool	overwrite=no		{prompt="Overwrite existing image?"}
+
+begin
+	string	im, imdata, s
+	real	biasval, sigma
+
+	im = subimage
+	imdata = image
+	biasval = artobs.biasval
+	sigma = artobs.sigma
+
+	if (access (im//".imh") == yes)
+	    im = im // ".imh"
+	if (access (im//".hhh") == yes)
+	    im = im // ".hhh"
+	if (access (im) == yes) {
+	    if (overwrite == yes)
+		imdelete (im, verify=no)
+	    else
+	        return
+	}
+
+	# Create the image.
+	s = "[1:" // str (ncols) // ",1:" // str(nlines) // "]"
+	imcopy (imdata//s, im, verbose=no)
+
+	# Copy subsection image.
+	imcopy (imdata//ccdsec, im//datasec, verbose=no)
+
+	# Add bias.
+	if (biasval != 0.)
+	    mkimage (im//biassec, "replace", biasval, slope=0., sigma=sigma,
+		seed=0)
+
+	# Set image header
+	ccdhedit (im, "ccdsec", ccdsec, type="string")
+	ccdhedit (im, "datasec", datasec, type="string")
+	ccdhedit (im, "trimsec", trimsec, type="string")
+	ccdhedit (im, "biassec", biassec, type="string")
+end
diff --git a/noao/imred/ccdred/ccdtest/subsection.hlp b/noao/imred/ccdred/ccdtest/subsection.hlp
new file mode 100644
index 00000000..a2779500
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/subsection.hlp
@@ -0,0 +1,73 @@
+.help subsection Oct87 noao.imred.ccdred.ccdtest
+.ih
+NAME
+subsection -- Make a subsection readout CCD image
+.ih
+USAGE
+subsection subimage image
+.ih
+PARAMETERS
+.ls subimage
+Subsection image to be created.
+.le
+.ls image
+Full image from which to take the subsection readout.
+.le
+.ls ncols = 82, nlines = 50
+Number of image columns and lines in the full subsection image including
+bias regions.
+.le
+.ls ccdsec="[26:75,26:75]"
+CCD section of the subsection.  This is the image section of the full
+image to be used.
+.le
+.ls datasec = "[1:50,1:50]"
+Data section of the image.
+.le
+.ls trimsec = ""
+Trim section for later processing.
+.le
+.ls biassec="[51:82,1:50]"
+Prescan or overscan bias section.
+.le
+.ls overwrite = no
+Overwrite an existing image?  If no a new observation is not created.
+There is no warning message.
+.le
+.ih
+DESCRIPTION
+This script task generates artificial CCD subsection observations
+which include bad pixels, bias and zero levels, dark counts, flat
+field response variations and sky brightness levels.  It creates an
+subsection image which includes a bias section from a previously
+created image (created by the task \fBartobs\fR).  This task is
+designed to be used with the \fBccdred\fR package and includes
+appropriate image header information.
+
+First the task checks whether the requested image exists.  If it does
+exist and the overwrite flag is no then a new observations is not created.
+If the overwrite flag is set then the old image is deleted and a new
+observation is created.
+
+The image section give by the parameter \fIccdsec\fR of the reference
+image is copied to the new image.  It is assumed the reference image
+contains any desired zero level, bias, flat field, and dark count
+effects.  The bias section is then added with a bias value given by
+\fBartobs.biasval\fR with noise given by \fBartobs.sigma\fR.
+
+Also the image header parameters from the reference image are
+copied and the data, bias, trim, and ccd section parameters are
+updated.
+.ih
+EXAMPLES
+1. To create some test CCD images first create full frame observations with
+the task \fBartobs\fR.  Then set the subsection parameters
+for the size of the subsection observation, the data section, trim section,
+bias section, and the CCD section of the subsection observation.
+
+	cl> artobs obj 5 object filter=V
+	cl> subsection obj1 object
+.ih
+SEE ALSO
+mkimage, artobs, demo
+.endhelp
diff --git a/noao/imred/ccdred/ccdtest/t_mkimage.x b/noao/imred/ccdred/ccdtest/t_mkimage.x
new file mode 100644
index 00000000..ff0d5f26
--- /dev/null
+++ b/noao/imred/ccdred/ccdtest/t_mkimage.x
@@ -0,0 +1,204 @@
+include	<imhdr.h>
+
+define	OPTIONS		"|make|replace|add|multiply|"
+define	MAKE		1	# Create a new image
+define	REPLACE		2	# Replace pixels
+define	ADD		3	# Add to pixels
+define	MULTIPLY	4	# Multiply pixels
+
+# T_MKIMAGE -- Make or edit an image with simple values.
+# An image may be created of a specified size, dimensionality, and pixel
+# datatype.  The image may also be edited to replace, add, or multiply
+# by specified values.  The values may be a combination of a sloped plane
+# (repeated for dimensions greater than 2) and Gaussian noise.
+# The editing may be confined to sections of the image by use of image
+# sections in the input image.  This task is a simple tool for
+# specialized uses in test applications.
+#
+# The sloped plane is defined such that:
+#
+#    pix[i,j] = value + slope * ((ncols + nlines) / 2 - 1) + slope * (i + j)
+#
+# The interpretation of value is that it is the mean of the plane.
+#
+# The Gaussian noise is only approximately random for purposes of speed!
+
+procedure t_mkimage ()
+
+char	image[SZ_FNAME]			# Image to edit
+char	option[7]			# Edit option
+real	value				# Edit value
+real	slope				# Slope
+real	sigma				# Gaussian noise sigma
+long	seed				# Random number seed
+
+int	i, op, ncols, nlines
+long	vin[IM_MAXDIM], vout[IM_MAXDIM]
+pointer	sp, rannums, im, buf, bufin, bufout
+
+int	clgwrd(), clgeti(), clscan(), nscan() imgnlr(), impnlr()
+char	clgetc()
+real	clgetr()
+long	clgetl()
+pointer	immap()
+
+data	seed/1/
+
+begin
+	call smark (sp)
+	call clgstr ("image", image, SZ_FNAME)
+	op = clgwrd ("option", option, 7, OPTIONS)
+	value = clgetr ("value")
+	slope = clgetr ("slope")
+	sigma = clgetr ("sigma")
+	if (clgetl ("seed") > 0)
+	    seed = clgetl ("seed")
+
+	call amovkl (long (1), vin, IM_MAXDIM)
+	call amovkl (long (1), vout, IM_MAXDIM)
+	switch (op) {
+	case MAKE:
+	    im = immap (image, NEW_IMAGE, 0)
+	    IM_NDIM(im) = clgeti ("ndim")
+	    i = clscan ("dims")
+	    do i = 1, IM_NDIM(im)
+		call gargi (IM_LEN(im, i))
+	    if (nscan() != IM_NDIM(im))
+		call error (0, "Bad dimension string")
+	    switch (clgetc ("pixtype")) {
+	    case 's':
+	        IM_PIXTYPE(im) = TY_SHORT
+	    case 'i':
+	        IM_PIXTYPE(im) = TY_INT
+	    case 'l':
+	        IM_PIXTYPE(im) = TY_LONG
+	    case 'r':
+	        IM_PIXTYPE(im) = TY_REAL
+	    case 'd':
+	        IM_PIXTYPE(im) = TY_DOUBLE
+	    default:
+		call error (0, "Bad pixel type")
+	    }
+
+	    ncols = IM_LEN(im,1)
+	    nlines = IM_LEN(im,2)
+	    call salloc (rannums, 2 * ncols, TY_REAL)
+	    call mksigma (sigma, seed, Memr[rannums], 2*ncols)
+
+	    while (impnlr (im, bufout, vout) != EOF)
+		call mkline (value, slope, sigma, seed, Memr[rannums],
+		    Memr[bufout], vout[2] - 1, ncols, nlines)
+	case REPLACE:
+	    im = immap (image, READ_WRITE, 0)
+
+	    ncols = IM_LEN(im,1)
+	    nlines = IM_LEN(im,2)
+	    call salloc (rannums, 2 * ncols, TY_REAL)
+	    call mksigma (sigma, seed, Memr[rannums], 2*ncols)
+
+	    while (impnlr (im, bufout, vout) != EOF)
+		call mkline (value, slope, sigma, seed, Memr[rannums],
+		    Memr[bufout], vout[2] - 1, ncols, nlines)
+	case ADD:
+	    im = immap (image, READ_WRITE, 0)
+
+	    ncols = IM_LEN(im,1)
+	    nlines = IM_LEN(im,2)
+	    call salloc (buf, ncols, TY_REAL)
+	    call salloc (rannums, 2 * ncols, TY_REAL)
+	    call mksigma (sigma, seed, Memr[rannums], 2*ncols)
+
+	    while (imgnlr (im, bufin, vin) != EOF) {
+		i = impnlr (im, bufout, vout)
+		call mkline (value, slope, sigma, seed, Memr[rannums],
+		    Memr[buf], vout[2] - 1, ncols, nlines)
+		call aaddr (Memr[bufin], Memr[buf], Memr[bufout], ncols)
+	    }
+	case MULTIPLY:
+	    im = immap (image, READ_WRITE, 0)
+
+	    ncols = IM_LEN(im,1)
+	    nlines = IM_LEN(im,2)
+	    call salloc (buf, ncols, TY_REAL)
+	    call salloc (rannums, 2 * ncols, TY_REAL)
+	    call mksigma (sigma, seed, Memr[rannums], 2*ncols)
+
+	    while (imgnlr (im, bufin, vin) != EOF) {
+		i = impnlr (im, bufout, vout)
+		call mkline (value, slope, sigma, seed, Memr[rannums],
+		    Memr[buf], vout[2] - 1, ncols, nlines)
+		call amulr (Memr[bufin], Memr[buf], Memr[bufout], ncols)
+	    }
+	}
+
+	call imunmap (im)
+	call sfree (sp)
+end
+
+
+# MKLINE -- Make a line of data.  A slope of zero is a special case.
+# The Gaussian random numbers are taken from the sequence of stored
+# values with starting point chosen randomly in the interval 1 to ncols.
+# This is not very random but is much more efficient.
+
+procedure mkline (value, slope, sigma, seed, rannums, data, line, ncols, nlines)
+
+real	value		# Mean value
+real	slope		# Slope in mean
+real	sigma		# Sigma about mean
+long	seed		# Random number seed
+real	rannums[ARB]	# Random numbers
+real	data[ncols]	# Data for line
+int	line		# Line number
+int	ncols		# Number of columns
+int	nlines		# Number of lines
+
+int	i
+real	a, urand()
+
+begin
+	if (slope == 0.)
+	    call amovkr (value, data, ncols)
+	else {
+	    a = value + slope * (line - (ncols + nlines) / 2. - 1)
+	    do i = 1, ncols
+	        data[i] = a + slope * i
+	}
+	if (sigma > 0.) {
+	    i = (ncols - 1) * urand (seed) + 1
+	    call aaddr (rannums[i], data, data, ncols)
+	}
+end
+
+
+# MKSIGMA -- A sequence of random numbers of the specified sigma and
+# starting seed is generated.  The random number generator is modeled after
+# that in Numerical Recipes by Press, Flannery, Teukolsky, and Vetterling.
+
+procedure mksigma (sigma, seed, rannums, nnums)
+
+real	sigma		# Sigma for random numbers
+long	seed		# Seed for random numbers
+real	rannums[nnums]	# Random numbers
+int	nnums		# Number of random numbers
+
+int	i
+real	v1, v2, r, fac, urand()
+
+begin
+	if (sigma > 0.) {
+	    for (i=1; i<=nnums; i=i+1) {
+		repeat {
+		    v1 = 2 * urand (seed) - 1.
+		    v2 = 2 * urand (seed) - 1.
+		    r = v1 ** 2 + v2 ** 2
+		} until ((r > 0) && (r < 1))
+		fac = sqrt (-2. * log (r) / r) * sigma
+		rannums[i] = v1 * fac
+		if (i == nnums)
+		    break
+		i = i + 1
+		rannums[i] = v2 * fac
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/combine.par b/noao/imred/ccdred/combine.par
new file mode 100644
index 00000000..0a1ae2f8
--- /dev/null
+++ b/noao/imred/ccdred/combine.par
@@ -0,0 +1,40 @@
+# COMBINE -- Image combine parameters
+
+input,s,a,,,,List of images to combine
+output,s,a,,,,List of output images
+plfile,s,h,"",,,List of output pixel list files (optional)
+sigma,s,h,"",,,"List of sigma images (optional)
+"
+ccdtype,s,h,"",,,CCD image type to combine (optional)
+subsets,b,h,no,,,Combine images by subset parameter?
+delete,b,h,no,,,Delete input images after combining?
+clobber,b,h,no,,,"Clobber existing output image?
+"
+combine,s,h,"average","average|median",,Type of combine operation
+reject,s,h,"none","none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip",,Type of rejection
+project,b,h,no,,,Project highest dimension of input images?
+outtype,s,h,"real","short|ushort|integer|long|real|double",,Output image pixel datatype
+offsets,f,h,"none",,,Input image offsets
+masktype,s,h,"none","none|goodvalue|badvalue|goodbits|badbits",,Mask type
+maskvalue,r,h,0,,,Mask value
+blank,r,h,0.,,,"Value if there are no pixels
+"
+scale,s,h,"none",,,Image scaling
+zero,s,h,"none",,,Image zero point offset
+weight,s,h,"none",,,Image weights
+statsec,s,h,"",,,"Image section for computing statistics
+"
+lthreshold,r,h,INDEF,,,Lower threshold
+hthreshold,r,h,INDEF,,,Upper threshold
+nlow,i,h,1,0,,minmax: Number of low pixels to reject
+nhigh,i,h,1,0,,minmax: Number of high pixels to reject
+nkeep,i,h,1,,,Minimum to keep (pos) or maximum to reject (neg)
+mclip,b,h,yes,,,Use median in sigma clipping algorithms?
+lsigma,r,h,3.,0.,,Lower sigma clipping factor
+hsigma,r,h,3.,0.,,Upper sigma clipping factor
+rdnoise,s,h,"0.",,,ccdclip: CCD readout noise (electrons)
+gain,s,h,"1.",,,ccdclip: CCD gain (electrons/DN)
+snoise,s,h,"0.",,,ccdclip: Sensitivity noise (fraction)
+sigscale,r,h,0.1,0.,,Tolerance for sigma clipping scaling corrections
+pclip,r,h,-0.5,,,pclip: Percentile clipping parameter
+grow,i,h,0,,,Radius (pixels) for 1D neighbor rejection
diff --git a/noao/imred/ccdred/cosmicrays.par b/noao/imred/ccdred/cosmicrays.par
new file mode 100644
index 00000000..3d14b146
--- /dev/null
+++ b/noao/imred/ccdred/cosmicrays.par
@@ -0,0 +1,15 @@
+input,s,a,,,,List of images in which to detect cosmic rays
+output,s,a,,,,List of cosmic ray replaced output images (optional)
+badpix,s,h,"",,,"List of bad pixel files (optional)
+"
+ccdtype,s,h,"",,,CCD image type to select (optional)
+threshold,r,h,25.,,,Detection threshold above mean
+fluxratio,r,h,2.,,,Flux ratio threshold (in percent)
+npasses,i,h,5,1,,Number of detection passes
+window,s,h,"5","5|7",,"Size of detection window
+"
+interactive,b,h,yes,,,Examine parameters interactively?
+train,b,h,no,,,Use training objects?
+objects,*imcur,h,"",,,Cursor list of training objects
+savefile,f,h,"",,,File to save train objects
+answer,s,q,,"no|yes|NO|YES",,Review parameters for a particular image?
diff --git a/noao/imred/ccdred/darkcombine.cl b/noao/imred/ccdred/darkcombine.cl
new file mode 100644
index 00000000..715456eb
--- /dev/null
+++ b/noao/imred/ccdred/darkcombine.cl
@@ -0,0 +1,48 @@
+# DARKCOMBINE -- Process and combine dark count CCD images.
+
+procedure darkcombine (input)
+
+string	input			{prompt="List of dark images to combine"}
+file	output="Dark"		{prompt="Output dark image root name"}
+string	combine="average"	{prompt="Type of combine operation",
+				 enum="average|median"}
+string	reject="minmax"	{prompt="Type of rejection",
+		enum="none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip"}
+string	ccdtype="dark"	{prompt="CCD image type to combine"}
+bool	process=yes	{prompt="Process images before combining?"}
+bool	delete=no	{prompt="Delete input images after combining?"}
+bool	clobber=no	{prompt="Clobber existing output image?"}
+string	scale="exposure"	{prompt="Image scaling",
+			 enum="none|mode|median|mean|exposure"}
+string	statsec=""	{prompt="Image section for computing statistics"}
+int	nlow=0		{prompt="minmax: Number of low pixels to reject"}
+int	nhigh=1		{prompt="minmax: Number of high pixels to reject"}
+int	nkeep=1		{prompt="Minimum to keep (pos) or maximum to reject (neg)"}
+bool	mclip=yes	{prompt="Use median in sigma clipping algorithms?"}
+real	lsigma=3.	{prompt="Lower sigma clipping factor"}
+real	hsigma=3.	{prompt="Upper sigma clipping factor"}
+string	rdnoise="0."	{prompt="ccdclip: CCD readout noise (electrons)"}
+string	gain="1."	{prompt="ccdclip: CCD gain (electrons/DN)"}
+string	snoise="0."	{prompt="ccdclip: Sensitivity noise (fraction)"}
+real	pclip=-0.5	{prompt="pclip: Percentile clipping parameter"}
+real	blank=0.	{prompt="Value if there are no pixels"}
+
+begin
+	string	ims
+
+	ims = input
+
+	# Process images first if desired.
+	if (process == YES)
+	    ccdproc (ims, output="", ccdtype=ccdtype, noproc=no)
+
+	# Combine the flat field images.
+	combine (ims, output=output, plfile="", sigma="", combine=combine,
+	    reject=reject, ccdtype=ccdtype, subsets=no, delete=delete,
+	    clobber=clobber, project=no, outtype="real", offsets="none",
+	    masktype="none", blank=blank, scale=scale, zero="none", weight=no,
+	    statsec=statsec, lthreshold=INDEF, hthreshold=INDEF, nlow=nlow,
+	    nhigh=nhigh, nkeep=nkeep, mclip=mclip, lsigma=lsigma, hsigma=hsigma,
+	    rdnoise=rdnoise, gain=gain, snoise=snoise, sigscale=0.1,
+	    pclip=pclip, grow=0)
+end
diff --git a/noao/imred/ccdred/doc/Notes b/noao/imred/ccdred/doc/Notes
new file mode 100644
index 00000000..209faf30
--- /dev/null
+++ b/noao/imred/ccdred/doc/Notes
@@ -0,0 +1,96 @@
+12/15/93:
+I have modified CCDPROC to more fully support scan table observations.  In
+combination with the ability to have the number of scan rows encoded in the
+image header automatically, this allows such data to be processed in a
+fairly foolproof and documented way.
+
+First if ccdproc.scancor=no then the NSCANROW keyword and nscan parameter
+are ignored.  For actual scanned data this may be useful to override
+things.  Otherwise the following steps are taken.  The logic is slightly
+complex so that everything is done in the right order and only as needed.
+
+The task wants to apply dark count and flat field calibration images which
+have been scanned by the same number of rows.  [Zero calibration images are
+assumed not to be scanned.  This made sense to me but if desired the zero
+images can also be treated like the darks and flats.]  This is similar to
+the way flat fields are checked for subset (filter/grating).  If the
+appropriate dark or flat has not been scanned then it is scanned in
+software; i.e. a moving average is taken over the unscanned image.
+
+The number of scan rows is determined for each object being processed from
+the NSCANROW keyword or appropriate translation in the header translation
+file.  If this keyword is not found the nscan parameter value is used;
+i.e.  it is assumed the object image has been scanned by the specified
+amount.  This allows using the software in cases where the number of scan
+rows is not encoded in the header.  In the case of dark and flat images if
+NSCANROW is not found a value of 1 (unscanned) is assumed.
+
+The set of possible calibration images (from the zero and flat parameters
+or the list of input images) is searched for one which has been scanned
+with the same number of lines as the object being processed.  If one is
+found it is processed as needed before applying to the object.  If one is
+not found then an unscanned one is sought.  It is an error if neither can
+be found.  An unscanned image is first processed as necessary (overscan,
+trim, etc.) and then scanned in software to create a new image.  The new
+image has the name of the unscanned image with the number of scan lines
+appended, for example Flat1.32.  It also has the NSCANROW keyword added as
+well as a comment indicating the image from which it was created.  This
+approach allows the calibration image to be created only once for each
+different scan format and the number of scan lines may be changed for
+different observations and the appropriate calibration made from the
+unscanned image.
+
+The following example shows how this all works.  There are four object
+images using two filters and two scan row values and unscanned
+zero, dark, and flats.
+
+cc> dir
+Dark.imh     FlatV.imh    obs019.imh   obs021.imh   pixels
+FlatB.imh    Zero.imh     obs020.imh   obs022.imh
+cc> hselect obs* $I,filter,nscanrow yes
+obs019.imh      V       24
+obs020.imh      V       32
+obs021.imh      B       24
+obs022.imh      B       32
+cc> ccdproc obs* overscan+ trim+ zerocor+ darkcor+ flatcor+ scancor+
+obs019.imh: Dec 15 17:53 Zero level correction image is Zero
+Dark.imh: Dec 15 17:53 Zero level correction image is Zero
+Dark.24.imh: Dec 15 17:53 Converted to shortscan from Dark.imh with nscan=24
+obs019.imh: Dec 15 17:53 Dark count correction image is Dark.24.imh
+FlatV.imh: Dec 15 17:53 Zero level correction image is Zero
+FlatV.imh: Dec 15 17:53 Dark count correction image is Dark.imh
+FlatV.24.imh: Dec 15 17:53 Converted to shortscan from FlatV.imh with nscan=24
+obs019.imh: Dec 15 17:53 Flat field image is FlatV.24.imh
+obs020.imh: Dec 15 17:53 Zero level correction image is Zero
+Dark.32.imh: Dec 15 17:53 Converted to shortscan from Dark.imh with nscan=32
+obs020.imh: Dec 15 17:53 Dark count correction image is Dark.32.imh
+FlatV.32.imh: Dec 15 17:53 Converted to shortscan from FlatV.imh with nscan=32
+obs020.imh: Dec 15 17:53 Flat field image is FlatV.32.imh
+obs021.imh: Dec 15 17:53 Zero level correction image is Zero
+obs021.imh: Dec 15 17:53 Dark count correction image is Dark.24.imh
+FlatB.imh: Dec 15 17:53 Zero level correction image is Zero
+FlatB.imh: Dec 15 17:53 Dark count correction image is Dark.imh
+FlatB.24.imh: Dec 15 17:53 Converted to shortscan from FlatB.imh with nscan=24
+obs021.imh: Dec 15 17:53 Flat field image is FlatB.24.imh
+obs022.imh: Dec 15 17:53 Zero level correction image is Zero
+obs022.imh: Dec 15 17:53 Dark count correction image is Dark.32.imh
+FlatB.32.imh: Dec 15 17:53 Converted to shortscan from FlatB.imh with nscan=32
+obs022.imh: Dec 15 17:53 Flat field image is FlatB.32.imh
+cc> ccdlist *.imh
+cc> ccdlist *.imh
+Dark.24.imh[96,96][real][dark][][OTZ]:
+Dark.32.imh[96,96][real][dark][][OTZ]:
+Dark.imh[96,96][real][dark][][OTZ]:
+FlatB.24.imh[96,96][real][flat][B][OTZD]:
+FlatB.32.imh[96,96][real][flat][B][OTZD]:
+FlatB.imh[96,96][real][flat][B][OTZD]:
+FlatV.24.imh[96,96][real][flat][V][OTZD]:
+FlatV.32.imh[96,96][real][flat][V][OTZD]:
+FlatV.imh[96,96][real][flat][V][OTZD]:
+Zero.imh[96,96][real][zero][][OT]:
+obs019.imh[96,96][real][object][V][OTZDF]:
+obs020.imh[96,96][real][object][V][OTZDF]:
+obs021.imh[96,96][real][object][B][OTZDF]:
+obs022.imh[96,96][real][object][B][OTZDF]:
+
+Frank
diff --git a/noao/imred/ccdred/doc/badpiximage.hlp b/noao/imred/ccdred/doc/badpiximage.hlp
new file mode 100644
index 00000000..46e13160
--- /dev/null
+++ b/noao/imred/ccdred/doc/badpiximage.hlp
@@ -0,0 +1,51 @@
+.help badpiximage Jun87 noao.imred.ccdred
+.ih
+NAME
+badpiximage -- Create a bad pixel mask image from a bad pixel file
+.ih
+USAGE
+badpiximage fixfile template image
+.ih
+PARAMETERS
+.ls fixfile
+Bad pixel file.
+.le
+.ls template
+Template image used to define the size of the bad pixel mask image.
+.le
+.ls image
+Bad pixel mask image to be created.
+.le
+.ls goodvalue = 1
+Integer value assigned to the good pixels.
+.le
+.ls badvalue = 0
+Integer value assigned to the bad pixels.
+.le
+.ih
+DESCRIPTION
+A bad pixel mask image is created from the specified bad pixel file.
+The format of the bad pixel file is that used by \fBccdproc\fR to
+correct CCD defects (see instruments).  The bad pixel image is of pixel type short and
+has the value given by the parameter \fBgoodvalue\fR for the good
+pixels and the value given by the parameter \fBbadvalue\fR for the bad pixels.
+The image size and header parameters are taken from the specified
+template image.  The bad pixel mask image may be used to view the
+location of the bad pixels and blink against an data image using an
+image display, to mask or flag bad pixels later by image arithmetic,
+and to propagate the positions of the bad pixels through the
+reductions.
+.ih
+EXAMPLES
+1. To make a bad pixel mask image from the bad pixel file "cryocambp.dat"
+using the image "ccd005" as the template:
+
+	cl> badpiximage cryocambp.dat ccd005 cryocambp
+
+2. To make the bad pixel mask image with good values of 0 and bad values of 1:
+
+	cl> badpixim cryomapbp.dat ccd005 cryocambp good=0 bad=1
+.ih
+SEE ALSO
+ccdproc, instruments
+.endhelp
diff --git a/noao/imred/ccdred/doc/ccdgeometry.hlp b/noao/imred/ccdred/doc/ccdgeometry.hlp
new file mode 100644
index 00000000..a051ae5e
--- /dev/null
+++ b/noao/imred/ccdred/doc/ccdgeometry.hlp
@@ -0,0 +1,73 @@
+.help ccdgeometry Sep87 noao.imred.ccdred
+.ih
+NAME
+ccdgeometry - Discussion of CCD geometry and header parameters
+.ih
+DESCRIPTION
+The \fBccdred\fR package maintains and updates certain geometry
+information about the images.  This geometry is described by four image
+header parameters which may be present.  These are defined below by the
+parameter names used in the package.  Note that these names may be
+different in the image header using the image header translation
+feature of the package.
+
+.ls DATASEC
+The section of the image containing the CCD data.  If absent the
+entire image is assumed to be data.  Only the pixels within the
+data section are modified during processing.  Therefore, there may be
+additional calibration or observation information in the image.
+If after processing, the data section is the entire image it is
+not recorded in the image header.
+.le
+.ls CCDSEC
+The section of the CCD to corresponding to the data section.  This
+refers to the physical format, columns and lines, of the detector.  This is
+the coordinate system used during processing to relate calibration
+data to the image data; i.e. image data pixels are calibrated by
+calibration pixels at the same CCD coordinates regardless of image pixel
+coordinates.  This allows recording only parts of the CCD during data
+taking and calibrating with calibration frames covering some or all of
+the CCD.  The CCD section is maintained during trimming operations.
+Note that changing the format of the images by image operators outside
+of the \fBccdred\fR package will invalidate this coordinate system.
+The size of the CCD section must agree with that of the data section.
+If a CCD section is absent then it defaults to the data section such
+that the first pixel of the data section has CCD coordinate (1,1).
+.le
+.ls BIASSEC
+The section of the image containing prescan or overscan bias information.
+It consists of a strip perpendicular to the readout axis.  There may be
+both a prescan and overscan but the package currently only uses one.
+This parameter may be overridden during processing by the parameter
+\fIccdproc.biassec\fR.  Only the part of the bias section along the
+readout is used and the length of the bias region is determined by
+the trim section.  If one wants to limit the region of the bias
+strip used in the fit then the \fIsample\fR parameter should be used.
+.le
+.ls TRIMSEC
+The section of the image extracted during processing when the trim
+operation is selected (\fIccdproc.trim\fR).  If absent when the trim
+operation is selected it defaults to the data section; i.e. the processed
+image consists only of the data section.  This parameter may be overridden
+during processing by the parameter \fIccdproc.trimsec\fR.  After trimming
+this parameter, if present, is removed from the image header.  The
+CCD section, data section, and bias section parameters are also modified
+by trimming.
+.le
+
+The geometry is as follows.  When a CCD image is recorded it consists
+of a data section corresponding to part or all of the CCD detector.
+Regions outside of the data section may contain additional information
+which are not affected except by trimming.  Most commonly this consists
+of prescan and overscan bias data.  When recording only part of the
+full CCD detector the package maintains information about that part and
+correctly applies calibrations for that part of the detector.  Also any
+trimming operation updates the CCD coordinate information.  If the
+images include the data section, bias section, trim section, and ccd
+section the processing may be performed entirely automatically.
+
+The sections are specified using the notation [c1:c2,l1:l2] where c1
+and c2 are the first and last columns and l1 and l2 are the first and
+last lines.  Currently c1 and l1 must be less than c2 and l2
+respectively and no subsampling is allowed.  This may be added later.
+.endhelp
diff --git a/noao/imred/ccdred/doc/ccdgroups.hlp b/noao/imred/ccdred/doc/ccdgroups.hlp
new file mode 100644
index 00000000..48c29b99
--- /dev/null
+++ b/noao/imred/ccdred/doc/ccdgroups.hlp
@@ -0,0 +1,163 @@
+.help ccdgroups Jun87 noao.imred.ccdred
+.ih
+NAME
+ccdgroups -- Group CCD images into image lists
+.ih
+USAGE
+ccdgroups images output
+.ih
+PARAMETERS
+.ls images
+List of CCD images to be grouped.
+.le
+.ls output
+Output root group filename.  The image group lists will be put in files
+with this root name followed by a number.
+.le
+.ls group = "ccdtype"
+Group type.  There are currently four grouping types:
+.ls ccdtype
+Group by CCD image type.
+.le
+.ls subset
+Group by subset parameter.
+.le
+.ls position
+Group by position in right ascension (in hours) and declination (in degrees).
+The groups are defined by a radius parameter (in arc seconds).
+.le
+.ls title
+Group by identical titles.
+.le
+.ls date
+Group by identical dates.
+.le
+.le
+.ls radius = 60.
+Grouping radius when grouping by positions.  This is given in arc seconds.
+.le
+.ls ccdtype = ""
+CCD image types to select from the input image list.  If null ("") then
+all image types are used.
+.le
+.ih
+DESCRIPTION
+The input images, possible restricted to a particular CCD image type,
+are grouped into image lists.  The "ccdtype" or "subset" groups
+produce output image lists with the given root name and the CCD type
+or subset as an extension (without a period).  For the other group
+types the
+image lists have file names given by
+the root output name and a numeric extension (without a period).
+If the package parameter \fIccdred.verbose\fR is yes then the
+image name and output group list is printed for each image.  The image lists can
+be used with the @ list feature for processing separate groups of observations.
+Note that grouping by CCD image type and subset is often not necessary since
+the \fBccdred\fR tasks automatically use this information (see
+\fBccdtypes\fR and \fBsubsets\fR).
+
+Besides CCD image type and subsets there are currently three ways to
+group images.  These are by position in the sky, by title, and by
+date.  Further groups may be added as suggested.  The title grouping is
+useful if consistent titles are used when taking data.  The date
+grouping is useful if multiple nights of observations are not organized
+by directories (it is recommended that data from separate nights be
+kept in separate directories).  The position grouping finds
+observations within a given radius on the sky of the first member of
+the group (this is not a clustering algorithm).  The right ascension
+and declination coordinates must be in standard units, hours and
+degrees respectively.  The grouping radius is in arc seconds.  This
+grouping type is useful for making sets of data in which separate
+calibration images are taken at each position.
+
+The date, title, and coordinates are accessed through the instrument
+translation file.  The standard names used are "date-obs", "title", "ra",
+and "dec".
+.ih
+EXAMPLES
+1. For each object 5 exposures were taken to be combined in order to remove
+cosmic rays.  If the titles are the same then (with ccdred.verbose=yes):
+
+.nf
+    cl> ccdgroups *.imh group group=title ccdtype=object
+    ccd005.imh  --> group1
+    ccd006.imh  --> group1
+    ccd007.imh  --> group1
+    ccd008.imh  --> group1
+    ccd009.imh  --> group1
+    ccd012.imh  --> group2
+    ccd013.imh  --> group2
+    ccd014.imh  --> group2
+    ccd015.imh  --> group2
+    ccd016.imh  --> group2
+    [... etc ...]
+    cl> combine @group1 obj1 proc+
+    cl> combine @group2 obj2 proc+
+    [... etc ...]
+.fi
+
+Note the numeric suffixes to the output root name "group".
+ 
+2. CCD observations were made in groups with a flat field, the object, and
+a comparison spectrum at each position.  To group and process this data:
+
+.nf
+    cl> ccdgroups *.imh obs group=position >> logfile
+    cl> ccdproc @obs1
+    cl> ccdproc @obs2
+    cl> ccdproc @obs3
+.fi
+
+Since no flat field is specified for the parameter \fIccdproc.flat\fR
+the flat field is taken from the input image list.
+
+3. If for some reason you want to group by date and position it is possible
+to use two steps.
+
+.nf
+    cl> ccdgroups *.imh date group=date
+    cl> ccdgroups @data1 pos1
+    cl> ccdgroups @data2 pos2
+.fi
+ 
+4. To get groups by CCD image type:
+ 
+.nf
+    cl> ccdgroups *.imh "" group=ccdtype
+    ccd005.imh  --> zero
+    ccd006.imh  --> zero
+    ccd007.imh  --> zero
+    ccd008.imh  --> dark
+    ccd009.imh  --> flat
+    ccd012.imh  --> flat
+    ccd013.imh  --> object
+    ccd014.imh  --> object
+    ccd015.imh  --> object
+    ccd016.imh  --> object
+    [... etc ...]
+.fi
+ 
+Note the use of a null root name and the extension is the standard
+CCDRED types (not necessarily those used in the image header).
+ 
+5. To get groups by subset:
+ 
+.nf
+    cl> ccdgroups *.imh filt group=subset
+    ccd005.imh  --> filt
+    ccd006.imh  --> filtB
+    ccd007.imh  --> filtB
+    ccd008.imh  --> filtB
+    ccd009.imh  --> filtV
+    ccd012.imh  --> filtV
+    ccd013.imh  --> filtV
+    ccd014.imh  --> filtB
+    ccd015.imh  --> filtB
+    ccd016.imh  --> filtB
+    [... etc ...]
+.fi
+ 
+.ih
+SEE ALSO
+ccdlist, ccdtypes, instruments, subsets
+.endhelp
diff --git a/noao/imred/ccdred/doc/ccdhedit.hlp b/noao/imred/ccdred/doc/ccdhedit.hlp
new file mode 100644
index 00000000..1bc27d29
--- /dev/null
+++ b/noao/imred/ccdred/doc/ccdhedit.hlp
@@ -0,0 +1,108 @@
+.help ccdhedit Jun87 noao.imred.ccdred
+.ih
+NAME
+ccdhedit -- CCD image header editor
+.ih
+USAGE
+ccdhedit images parameter value
+.ih
+PARAMETERS
+.ls images
+List of CCD images to be edited.
+.le
+.ls parameter
+Image header parameter.  The image header parameter will be translated by
+the header translation file for the images.
+.le
+.ls value
+The parameter value.  If the null string ("") is specified then the
+parameter is deleted from the image header, otherwise it is added or
+modified.  If the parameter is "imagetyp" then the value string giving
+the CCD image type is translated from the package CCD type to the
+instrument specific string.
+.le
+.ls type = "string"
+The parameter type.  The parameter types are "string", "real", or "integer".
+.le
+.ih
+DESCRIPTION
+The image headers of the specified CCD images are edited to add, modify,
+or delete a parameter.  The parameters may be those used by the \fBccdred\fR
+package.  The parameter name is translated to an image header parameter by the
+instrument translation file (see \fBinstruments\fR) if a translation is
+given.  Otherwise the parameter is that in the image header.  If the parameter
+is "imagetyp" the parameter value for the CCD image type may be that
+used by the package; i.e. dark, object, flat, etc.  The value string will be
+translated to the instrument image string in this case.  The translation
+facility allows use of this task in an instrument independent way.
+
+The value string is used to determine whether to delete or modify the
+image parameter.  If the null string, "", is given the specified parameter
+is deleted.  If parameters are added the header type must be specified
+as a string, real, or integer parameter.  The numeric types convert the
+value string to a number.
+.ih
+EXAMPLES
+The \fBccdred\fR package is usable even with little image header information.
+However, if desired the header information can be added to images which
+lack it.  In all the examples the parameters used are those of the package
+and apply equally well to any image header format provided there is an
+instrument translation file.
+
+.nf
+1.   cl> ccdhedit obj* imagetyp object
+2.   cl> ccdhedit flat* imagetyp flat
+3.   cl> ccdhedit zero* imagetyp zero
+4.   cl> ccdhedit obj0![1-3]* subset "V filter"
+5.   cl> ccdhedit obj0![45]* subset "R filter"
+6.   cl> ccdhedit flat001 subset "R filter"
+7.   cl> ccdhedit obj* exptime 500 type=integer
+.fi
+
+8. The following is an example of a CL script which sets the CCD image type,
+the subset, and the exposure time simultaneously.  The user may expand
+on this example to include other parameters or other initialization
+operations.
+
+.nf
+    cl> edit ccdheader.cl
+
+    ----------------------------------------------------------------
+    # Program to set CCD header parameters.
+
+    procedure ccdheader (images)
+
+    string	images			{prompt="CCD images"}
+    string	imagetyp		{prompt="CCD image type"}
+    string	subset			{prompt="CCD subset"}
+    string	exptime			{prompt="CCD exposure time"}
+
+    begin
+	    string	ims
+
+	    ims = images
+	    ccdhedit (ims, "imagetyp", imagetyp, type="string")
+	    ccdhedit (ims, "subset", subset, type="string")
+	    ccdhedit (ims, "exptime", exptime, type="real")
+    end
+    ----------------------------------------------------------------
+
+    cl> task ccdheader=ccdheader.cl
+    cl> ccdheader obj* imagetyp=object subset="V" exptime=500
+.fi
+
+9. The image header may be changed to force processing a calibration image
+as an object.  For example to flatten a flat field:
+
+.nf
+    cl> ccdhedit testflat imagetyp other
+    cl> ccdproc testflat
+.fi
+
+10. To delete processing flags:
+
+    cl> ccdhedit obj042 flatcor ""
+.ih
+SEE ALSO
+hedit, instruments, ccdtypes, subsets
+.endhelp
diff --git a/noao/imred/ccdred/doc/ccdinst.hlp b/noao/imred/ccdred/doc/ccdinst.hlp
new file mode 100644
index 00000000..ea90f4a7
--- /dev/null
+++ b/noao/imred/ccdred/doc/ccdinst.hlp
@@ -0,0 +1,391 @@
+.help ccdinstrument Dec93 noao.imred.ccdred
+.ih
+NAME
+ccdinstrument -- Setup and verify CCD instrument translation files
+.ih
+USAGE	
+ccdinstrument images
+.ih
+PARAMETERS
+.ls images
+List of images to be verified or used to setup a CCD instrument translation
+file.
+.le
+.ls instrument = ")_.instrument"
+CCD instrument translation file.  The default is to use the translation
+file defined in the \fBccdred\fR package parameters.  Note that one would
+need write permission to update this file though the task has a write
+command to save any changes to a different file.
+.le
+.ls ssfile = ")_.ssfile"
+Subset translation file.  The default is to use the file defined in
+the \fBccdred\fR package parameters.
+.le
+.ls edit = yes
+Edit the instrument translation file?  If "yes" an interactive
+mode is entered allowing translation parameters to be modified while if
+"no" the task is simply used to verify the translations noninteractively.
+.le
+.ls parameters = "basic"
+Parameters to be displayed.  The choices are "basic" to display only the
+most basic parameters (those needed for the simplest automation of
+\fBccdred\fR tasks),  "common" to display the common parameters used
+by the package (most of these are keywords to be written to the image
+rather than translated), and "all" to display all the parameters
+referenced by the package including the most obscure.  For most uses
+the "basic" set is all that is important and the other options are
+included for completeness.
+.le
+.ih
+DESCRIPTION
+The purpose of this task is to provide an interface to simplify setting
+up CCD instrument translation files and to verify the translations
+for a set of images.  Before this task was written users who needed to
+set up translation files for new instruments and observatories had
+to directly create the files with an editor.  Many people encountered
+difficulties and were prone to errors.  Also there was no task that
+directly verified the translations though \fBccdlist\fR provided some
+clues.
+
+The \fBccdred\fR package was designed to make intelligent use of
+information in image headers for determining things such as image
+calibration or object type and exposure times.  While the package may
+be used without this capability it is much more convenient to be
+able to use information from the image.  The package was also intended
+to be used with many different instruments, detectors, and observatories.
+The key to providing image header access across different observatories
+is the ability to translate the needs of the package to the appropriate
+keywords in the image header.  This is done through a file called
+an "instrument translation file".  For a complete description of
+this file and other instrument setup features of the package see
+\fBccdred.instruments\fR.
+
+The instrument translation file translates the parameter names used by
+the \fBccdred\fR package into image specific parameters and also
+supplies default values for parameters.  The translation proceeds as
+follows.  When a package task needs a parameter for an image, for
+example "imagetyp", it looks in the instrument translation file.  If
+the file is not found or none is specified then the image header
+keyword that is requested is assumed to have the same name.  If an
+instrument translation file is defined then the requested parameter is
+translated to an image header keyword, provided a translation entry is
+given.  If no translation is given the package name is used.  For
+example the package parameter "imagetyp" might be translated to
+"data-typ" (the old NOAO CCD keyword).  If the parameter is not found
+then the default value specified in the translation file, if present,
+is returned.
+
+For recording parameter information in the header, such
+as processing flags, translation is also used.  For example, if the
+flag specifying that the image has been corrected by a flat field is to
+be set then the package parameter name "flatcor" might be translated to
+"ff-flag".  If no translation is given then the new image header
+parameter is entered as "flatcor".
+
+The CCD image type requires a second level of translation also defined
+in the translation file.  Once the image keyword which identifies the
+type of CCD image, for example a flat field or object, is translated
+to an imahe keyword the specific
+string value must be translated to one of the CCD image types used
+by the package.  The translation works in the same way, the specific
+string found is translated to the \fBccdred\fR type and returned to
+the task.  This translation is tricky in that the exact string
+including all spaces and capitalizations must be correctly defined
+in the translation file.  The \fBccdinstrument\fR allows doing
+this automatically thus minimizing typing errors.
+
+The basic display format of the task is a table of five columns
+giving the parameter name used by the package, the image keyword
+to which it is translated, the default value (if any), the value
+the task will receive for the current image after translation,
+and the actual keyword value in the image.  A "?" is printed if
+a value cannot be determined.  The idea of the task is to make sure
+that the value a \fBccdred\fR task sees is the correct one and if not
+to modify the translation appropriately.  In verify mode when the
+\fBedit\fR parameter is not set the translation table is simply
+printed for each input image.
+
+In edit mode the user interactively gives commands at the ccdinstrument
+prompt to display or modify keywords.  The modifications can then be
+written to the instrument file or saved in a private copy.  The
+list of commands is shown below and may be printed using ? or help.
+
+.in 4
+.nf
+			CCDINSTRUMENT COMMANDS
+
+?	    Print command summary
+help	    Print command summary
+imheader    Page image header
+instrument  Print current instrument translation file
+next	    Next image
+newimage    Select a new image
+quit	    Quit
+read	    Read instrument translation file
+show	    Show current translations
+write	    Write instrument translation file
+
+translate   Translate image string selected by the imagetyp
+	    parameter to one of the CCDRED types given as an
+	    argument or queried:
+	    object, zero, dark, flat, comp, illum, fringe, other
+
+.fi
+The following are CCDRED parameters which may be translated.  You are
+queried for the image keyword to use or it may be typed after the command.
+An optional default value (returned if the image does not contain the
+keyword) may be typed as the second argument of the command.
+.nf
+
+	BASIC PARAMETERS
+imagetyp	Image type parameter (see also translate)
+subset		Subset or filter parameter
+exptime		Exposure time
+darktime	Dark time (may be same as the exposure time)
+.fi
+.in -4
+
+The commands may be followed by values such as file names for some of
+the general commands or the keyword and default value for the parameters
+to be translated.  Note this is the only way to specify a default value.
+If no arguments are given the user is prompted with the current value
+which may then be changed.
+
+The set of parameters shown above are only those considered "basic".
+In order to avoid confusion the task can limit the set of parameters
+displayed.  Without going into great detail, it is only the basic
+parameters which are generally required to have valid translations to
+allow the package to work well.  However, for completeness, and if someone
+wants to go wild with translations, further parameters may be displayed
+and changed.  The parameters displayed is controlled by the \fIparameters\fR
+keyword.  The additional parameters not shown above are:
+
+.in 4
+.nf
+	USEFUL DEFAULT GEOMETRY PARAMETERS
+biassec		Bias section (often has a default value)
+trimsec		Trim section (often has a default value)
+
+	COMMON PROCESSING FLAGS
+fixpix		Bad pixel replacement flag
+overscan	Overscan correction flag
+trim		Trim flag
+zerocor		Zero level correction flag
+darkcor		Dark count correction flag
+flatcor		Flat field correction flag
+
+	RARELY TRANSLATED PARAMETERS
+ccdsec		CCD section
+datasec		Data section
+fixfile		Bad pixel file
+
+fringcor	Fringe correction flag
+illumcor	Ilumination correction flag
+readcor		One dimensional zero level read out correction
+scancor		Scan mode correction flag
+nscanrow	Number of scan rows
+
+illumflt	Ilumination flat image
+mkfringe	Fringe image
+mkillum		Iillumination image
+skyflat		Sky flat image
+
+ccdmean		Mean value
+ccdmeant	Mean value compute time
+fringscl	Fringe scale factor
+ncombine	Number of images combined
+date-obs	Date of observations
+dec		Declination
+ra		Right Ascension
+title		Image title
+.fi
+.in -4
+.ih
+EXAMPLES
+1. To verify the translations for a set of images using the default
+translation file:
+
+.nf
+	cl> setinst "" review-
+	cl> ccdinst dev$pix edit-
+	Image: dev$pix
+	Instrument file: 
+	Subset file: subsets
+
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	--------------------------------
+	imagetyp  imagetyp            none      ?
+	subset    subset                        ?
+	exptime   exptime             ?         ?
+	darktime  darktime            ?         ?
+
+	cl> setinst "" site=kpno dir=ccddb$ review-
+	cl> ccdinst dev$pix edit-
+	Image: dev$pix
+
+	Instrument file: ccddb$kpno/camera.dat
+	Subset file: subsets
+
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	--------------------------------
+	imagetyp  data-typ            object    OBJECT (0)
+	subset    f1pos               2         2
+	exptime   otime               600       600
+	darktime  ttime               600       600
+.fi
+
+2.  Set up an  instrument translation file from scratch.
+
+.nf
+	ccdinst ech???.imh instr=myccd edit+
+	Warning: OPEN: File does not exist (myccd)
+	Image: ech001.imh
+	Instrument file: myccd
+	Subset file: subsets
+	
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	------------------------------------------------------
+	imagetyp  imagetyp            none      ?
+	subset    subset                        ?
+	exptime   exptime             ?         ?
+	darktime  darktime            ?         ?
+	
+	ccdinstrument> imagetyp
+	Image keyword for image type (imagetyp): ccdtype
+	imagetyp  ccdtype             unknown   BIAS
+	ccdinstrument> translate
+	CCDRED image type for 'BIAS' (unknown): zero
+	imagetyp  ccdtype             zero      BIAS
+	ccdinstrument> subset
+	Image keyword for subset parameter (subset): filters
+	subset    filters             1         1 0
+	ccdinstrument> exptime integ
+	exptime   integ               0.        0.
+	ccdinstrument> darktime integ
+	darktime  integ               0.        0.
+	ccdinstrument> show
+	Image: ech001.imh
+	Instrument file: myccd
+	Subset file: subsets
+	
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	------------------------------------------------------
+	imagetyp  ccdtype             zero      BIAS
+	subset    filters             1         1 0
+	exptime   integ               0.        0.
+	darktime  integ               0.        0.
+	
+	ccdinstrument> next
+	Image: ech002.imh
+	Instrument file: myccd
+	Subset file: subsets
+	
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	------------------------------------------------------
+	imagetyp  ccdtype             unknown   PROJECTOR FLAT
+	subset    filters             1         1 0
+	exptime   integ               20.       20.
+	darktime  integ               20.       20.
+	
+	ccdinstrument> trans
+	CCDRED image type for 'PROJECTOR FLAT' (unknown): flat
+	imagetyp  ccdtype             flat      PROJECTOR FLAT
+	ccdinstrument> next
+	Image: ech003.imh
+	Instrument file: myccd
+	Subset file: subsets
+	
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	------------------------------------------------------
+	imagetyp  ccdtype             unknown   COMPARISON
+	subset    filters             1         1 0
+	exptime   integ               300       300
+	darktime  integ               300       300
+	
+	ccdinstrument> translate comp
+	imagetyp  ccdtype             comp      COMPARISON
+	ccdinstrument> next
+	Image: ech004.imh
+	Instrument file: myccd
+	Subset file: subsets
+	
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	------------------------------------------------------
+	imagetyp  ccdtype             unknown   OBJECT
+	subset    filters             1         1 0
+	exptime   integ               3600      3600
+	darktime  integ               3600      3600
+	
+	ccdinstrument> translate object
+	imagetyp  ccdtype             object    OBJECT
+	ccdinstrument> inst
+	imagetyp                      ccdtype 
+	BIAS                          zero    
+	subset                        filters 
+	exptime                       integ   
+	darktime                      integ   
+	'PROJECTOR FLAT'              flat    
+	COMPARISON                    comp    
+	OBJECT                        object  
+
+	ccdinstrument> next
+	Update instrument file myccd (yes)? 
+.fi
+
+3.  Set default geometry parameters.  Note that to set a default the
+arguments must be on the command line.
+
+.nf
+	cc> ccdinst ech001 instr=myccd param=common edit+
+	Image: ech001
+	Instrument file: myccd
+	Subset file: subsets
+	
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	------------------------------------------------------
+	imagetyp  ccdtype             zero      BIAS
+	subset    filters             1         1 0
+	exptime   integ               0.        0.
+	darktime  integ               0.        0.
+	
+	biassec   biassec             ?         ?
+	trimsec   trimsec             ?         ?
+	
+	fixpix    fixpix              no        ?
+	overscan  overscan            no        ?
+	trim      trim                no        ?
+	zerocor   zerocor             no        ?
+	darkcor   darkcor             no        ?
+	flatcor   flatcor             no        ?
+	
+	ccdinstrument> biassec biassec [803:830,*]
+	biassec   biassec   [803:830,*]  [803:830,*]  ?
+	ccdinstrument> trimsec trimsec [2:798,2:798]
+	trimsec   trimsec   [2:798,2:798]  [2:798,2:798]  ?
+	ccdinstrument> instr
+	trimsec                       trimsec  [2:798,2:798]
+	biassec                       biassec  [803:830,*]
+	imagetyp                      ccdtype 
+	BIAS                          zero    
+	subset                        filters 
+	exptime                       integ   
+	darktime                      integ   
+	'PROJECTOR FLAT'              flat    
+	COMPARISON                    comp    
+	OBJECT                        object  
+	
+	ccdinstrument> q
+	Update instrument file myccd (yes)? 
+.fi
+.ih
+SEE ALSO
+instruments, setinstrument
+.endhelp
diff --git a/noao/imred/ccdred/doc/ccdlist.hlp b/noao/imred/ccdred/doc/ccdlist.hlp
new file mode 100644
index 00000000..9ce7dfdd
--- /dev/null
+++ b/noao/imred/ccdred/doc/ccdlist.hlp
@@ -0,0 +1,133 @@
+.help ccdlist Jun87 noao.imred.ccdred
+.ih
+NAME
+ccdlist -- List CCD processing information
+.ih
+USAGE
+ccdlist images
+.ih
+PARAMETERS
+.ls images
+CCD images to be listed.  A subset of the these may be selected using the
+CCD image type parameter.
+.le
+.ls ccdtype = ""
+CCD image type to be listed.  If no type is specified then all the images
+are listed.  If an image type is specified then only images
+of that type are listed.  See \fBccdtypes\fR for a list of the package
+image types.
+.le
+.ls names = no
+List the image names only?  Used with the CCD image type parameter to make
+a list of the images of the specified type.
+.le
+.ls long = no
+Long format listing?  The images are listed in a long format containing some
+image parameters and the processing history.
+.le
+.ls ccdproc (pset)
+CCD processing parameter set.
+.le
+.ih
+DESCRIPTION
+Information from the specified input images is listed on the standard
+output.  A specific CCD image type may be selected from the input
+images by the parameter \fIccdtype\fR.  There are three list formats;
+the default one line per image format, an image name only format, and a
+multi-line long format.  The default one line format consists of the
+image name, image size, image pixel type, CCD image type, subset ID (if
+defined), processing flags, and title.  This format contains the same
+information as that produced by \fBimheader\fR as well as CCD specific
+information.  The processing flags identifying the processing operations
+performed on the image are given by the following single letter codes.
+
+.nf
+	B - Bad pixel replacement
+	O - Overscan bias subtraction
+	T - Trimming
+	Z - Zero level subtraction
+	D - Dark count subtraction
+	F - Flat field calibration
+	I - Iillumination correction
+	Q - Fringe correction
+.fi
+
+The long format has the same first line as the default format plus additional
+instrument information such as the exposure time and the full processing
+history.  In addition to listing the completed processing, the operations
+not yet done (as specified by the \fBccdproc\fR parameters) are also
+listed.
+
+The image name only format is intended to be used to generate lists of
+images of the same CCD image type.  These lists may be used as "@" file
+lists in IRAF tasks.
+.ih
+EXAMPLES
+1. To list the default format for all images:
+
+.nf
+    cl> ccdlist *.imh
+    ccd001.imh[544,512][short][unknown][V]:FOCUS L98-193
+    ccd007.imh[544,512][short][object][V]:N2968 V 600s
+    ccd015.imh[544,512][short][object][B]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R]:N4036 R 600s
+    ccd045.imh[544,512][short][flat][V]:dflat 6v+blue 5s
+    ccd066.imh[544,512][short][flat][B]:dflat 6v+blue 5s
+    ccd103.imh[544,512][short][flat][R]:dflat 6v+blue 5s
+    ccd104.imh[544,512][short][zero][]:bias
+    ccd105.imh[544,512][short][dark][]:dark 3600s
+.fi
+
+These images have not been processed.
+
+2. To restrict the listing to just the object images:
+
+.nf
+    cl> ccdlist *.imh ccdtype=object
+    ccd007.imh[544,512][short][object][V]:N2968 V 600s
+    ccd015.imh[544,512][short][object][B]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R]:N4036 R 600s
+.fi
+
+3. The long list for image "ccd007" is obtained by:
+
+.nf
+    cl> ccdlist ccd007 l+
+    ccd007[544,512][short][object][V]:N2968 R 600s
+	exptime = 200. darktime = 200.
+        [TO BE DONE] Overscan strip is [520:540,*]
+        [TO BE DONE] Trim image section is [3:510,3:510]
+        [TO BE DONE] Flat field correction
+.fi
+
+4. After processing the images have the short listing:
+
+.nf
+    cl> ccdlist *.imh ccdtype=object
+    ccd007.imh[508,508][real][object][V][OTF]:N2968 V 600s
+    ccd015.imh[508,508][real][object][B][OTF]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R][OTF]:N4036 R 600s
+.fi
+
+The processing indicated is overscan subtraction, trimming, and flat fielding.
+
+5. The long listing for "ccd007" after processing is:
+
+.nf
+    cl> ccdlist ccd007 l+
+    ccd007[508,508][real][object][V][OTF]:N2968 R 600s
+	exptime = 200. darktime = 200.
+        Jun  2 18:18 Overscan section is [520:540,*] with mean=481.8784
+        Jun  2 18:18 Trim data section is [3:510,3:510]
+        Jun  2 18:19 Flat field image is FlatV.imh with scale=138.2713
+.fi
+
+6. To make a list file containing all the flat field images:
+
+    cl> ccdlist *.imh ccdtype=flat name+ > flats
+
+This file can be used as an @ file for processing.
+.ih
+SEE ALSO
+ccdtypes ccdgroups
+.endhelp
diff --git a/noao/imred/ccdred/doc/ccdmask.hlp b/noao/imred/ccdred/doc/ccdmask.hlp
new file mode 100644
index 00000000..190ef016
--- /dev/null
+++ b/noao/imred/ccdred/doc/ccdmask.hlp
@@ -0,0 +1,138 @@
+.help ccdmask Jun96 noao.imred.ccdred
+.ih
+NAME
+ccdmask -- create a pixel mask from a CCD image
+.ih
+USAGE	
+.nf
+ccdmask image mask
+.fi
+.ih
+PARAMETERS
+.ls image
+CCD image to use in defining bad pixels.  Typically this is
+a flat field image or, even better, the ratio of two flat field
+images of different exposure levels.
+.le
+.ls mask
+Pixel mask name to be created.  A pixel list image, .pl extension,
+is created so no extension is necessary.
+.le
+.ls ncmed = 7, nlmed = 7
+The column and line size of a moving median rectangle used to estimate the
+uncontaminated local signal.  The column median size should be at least 3
+pixels to span single bad columns.
+.le
+.ls ncsig = 15, nlsig = 15
+The column and line size of regions used to estimate the uncontaminated
+local sigma using a percentile.  The size of the box should contain
+of order 100 pixels or more.
+.le
+.ls lsigma = 6, hsigma = 6
+Positive sigma factors to use for selecting pixels below and above
+the median level based on the local percentile sigma.
+.le
+.ls ngood = 5
+Gaps of undetected pixels along the column direction of length less
+than this amount are also flagged as bad pixels.
+.le
+.ls linterp = 2
+Mask code for pixels having a bounding good pixel separation which is
+smaller along lines; i.e.  to use line interpolation along the narrower
+dimension.
+.le
+.ls cinterp = 3
+Mask code for pixels having a bounding good pixel separation which is
+smaller along columns; i.e.  to use columns interpolation along the narrower
+dimension.
+.le
+.ls eqinterp = 2
+Mask code for pixels having a bounding good pixel separation which is
+equal along lines and columns.
+.le
+.ih
+DESCRIPTION
+\fBCcdmask\fR makes a pixel mask from pixels deviating by a specified
+statistical amount from the local median level.  The input images may be of
+any type but this task was designed primarily for detecting column oriented
+CCD defects such as charge traps that cause bad columns and non-linear
+sensitivities.  The ideal input is a ratio of two flat fields having
+different exposure levels so that all features which would normally flat
+field properly are removed and only pixels which are not corrected by flat
+fielding are found to make the pixel mask.  A single flat field may also be
+used but pixels of low or high sensitivity may be included as well as true
+bad pixels.
+
+The input image is first subtracted by a moving box median.  The median is
+unaffected by bad pixels provided the median size is larger that twice
+the size of a bad region.  Thus, if 3 pixel wide bad columns are present
+then the column median box size should be at least 7 pixels.  The median
+box can be a single pixel wide along one dimension if needed.  This may be
+appropriate for spectroscopic long slit data.
+
+The median subtracted image is then divided into blocks of size
+\fInclsig\fR by \fInlsig\fR.  In each block the pixel values are sorted and
+the pixels nearest the 30.9 and 69.1 percentile points are found; this
+would be the one sigma points in a Gaussian noise distribution.  The
+difference between the two count levels divided by two is then the local
+sigma estimate.  This algorithm is used to avoid contamination by the bad
+pixel values.  The block size must be at least 10 pixels in each dimension
+to provide sufficient pixels for a good estimate of the percentile sigma.  The
+sigma uncertainty estimate of each pixel in the image is then the sigma
+from the nearest block.
+
+The deviant pixels are found by comparing the median subtracted residual to
+a specified sigma threshold factor times the local sigma above and below
+zero (the \fIlsigma\fR and \fIhsigma\fR parameters).  This is done for
+individual pixels and then for column sums of pixels (excluding previously
+flagged bad pixels) from two to the number of lines in the image.  The sigma
+of the sums is scaled by the square root of the number of pixels summed so
+that statistically low or high column regions may be detected even though
+individual pixels may not be statistically deviant.  For the purpose of
+this task one would normally select large sigma threshold factors such as
+six or greater to detect only true bad pixels and not the extremes of the
+noise distribution.
+
+As a final step each column is examined to see if there are small
+segments of unflagged pixels between bad pixels.  If the length
+of a segment is less than that given by the \fIngood\fR parameter
+all the pixels in the segment are also marked as bad.
+
+The bad pixel mask is created with good pixels identified by zero values
+and the bad pixels by non-zero values.
+The nearest good pixels along the columns and lines for
+each bad pixel are located and the separation along the columns and lines
+between those pixels is computed.  The smaller separation is used to select
+the mask value.  If the smaller separation is along lines the \fIlinterp\fR
+value is set, if the smaller separation is along columns the \fIcinterp\fR
+value is set, and if the two are equal the \fIeqinterp\fR value is set.
+The purpose of this is to allow interpolating across bad pixels using the
+narrowest dimension.  The task \fBfixpix\fR can select the type of pixel
+replacement to use for each mask value.  So one can chose, for example,
+line interpolation for the linterp values and the eqinterp values, and
+column interpolation for the cinterp values.
+
+In addition to this task, pixel mask images may be made in a variety of
+ways.  Any task which produces and modifies image values may be used.  Some
+useful tasks are \fBimexpr, imreplace, imcopy, text2mask\fR and
+\fBmkpattern\fR.  If a new image is specified with an explicit ".pl"
+extension then the pixel mask format is produced.
+.ih
+EXAMPLES
+1.  Two flat fields of exposures 1 second and 3 seconds are taken,
+overscan and zero corrected, and trimmed.  These are then used
+to generate a CCD mask.
+
+.nf
+    cl> imarith flat1 / flat2 ratio
+    cl> ccdmask ratio mask
+.fi
+.ih
+REVISIONS
+.ls CCDMASK V2.11
+This task is new.
+.le
+.ih
+SEE ALSO
+imreplace, imexpr, imcopy, imedit, fixpix, text2mask
+.endhelp
diff --git a/noao/imred/ccdred/doc/ccdproc.hlp b/noao/imred/ccdred/doc/ccdproc.hlp
new file mode 100644
index 00000000..26ec6d1d
--- /dev/null
+++ b/noao/imred/ccdred/doc/ccdproc.hlp
@@ -0,0 +1,825 @@
+.help ccdproc Dec93 noao.imred.ccdred
+.ih
+NAME
+ccdproc -- Process CCD images
+.ih
+USAGE	
+ccdproc images
+.ih
+PARAMETERS
+.ls images
+List of input CCD images to process.  The list may include processed
+images and calibration images.
+.le
+.ls output = ""
+List of output images.  If no list is given then the processing will replace
+the input images with the processed images.  If a list is given it must
+match the input image list.  \fINote that any dependent calibration images
+still be processed in-place with optional backup.\fR
+.le
+.ls ccdtype = ""
+CCD image type to select from the input image list.  If no type is given
+then all input images will be selected.  The recognized types are described
+in \fBccdtypes\fR.
+.le
+.ls max_cache = 0
+Maximum image caching memory (in Mbytes).  If there is sufficient memory
+the calibration images, such as zero level, dark count, and flat fields,
+will be cached in memory when processing many input images.  This
+reduces the disk I/O and makes the task run a little faster.  If the
+value is zero image caching is not used.
+.le
+.ls noproc = no
+List processing steps only?
+.le
+
+.ce
+PROCESSING SWITCHES
+.ls fixpix = yes
+Fix bad CCD lines and columns by linear interpolation from neighboring
+lines and columns?  If yes then a bad pixel mask, image, or file must be
+specified.
+.le
+.ls overscan = yes
+Apply overscan or prescan bias correction?  If yes then the overscan
+image section and the readout axis must be specified.
+.le
+.ls trim = yes
+Trim the image of the overscan region and bad edge lines and columns?
+If yes then the data section must be specified.
+.le
+.ls zerocor = yes
+Apply zero level correction?  If yes a zero level image must be specified.
+.le
+.ls darkcor = yes
+Apply dark count correction?  If yes a dark count image must be specified.
+.le
+.ls flatcor = yes
+Apply flat field correction?  If yes flat field images must be specified.
+.le
+.ls illumcor = no
+Apply iillumination correction?  If yes iillumination images must be specified.
+.le
+.ls fringecor = no
+Apply fringe correction?  If yes fringe images must be specified.
+.le
+.ls readcor = no
+Convert zero level images to readout correction images?  If yes then
+zero level images are averaged across the readout axis to form one
+dimensional zero level readout correction images.
+.le
+.ls scancor = no
+Convert zero level, dark count and flat field images to scan mode flat
+field images?  If yes then the form of scan mode correction is specified by
+the parameter \fIscantype\fR.
+.le
+
+.ce
+PROCESSING PARAMETERS
+.ls readaxis = "line"
+Read out axis specified as "line" or "column".
+.le
+.ls fixfile
+Bad pixel mask, image, or file.  If "image" is specified then the name is
+specified in the image header or instrument translation file.  If "BPM" is
+specified then the standard BPM image header keyword defines a bad pixel
+mask.  A bad pixel mask is a compact format (".pl" extension) with zero
+values indicating good pixels and non-zero values indicating bad pixels.  A
+bad pixel image is a regular image in which zero values are good pixels and
+non-zero values are bad pixels.  A bad pixel file specifies bad pixels or
+rectangular bad pixel regions as described later.  The direction of
+interpolation is determined by the mask value with a value of two
+interpolating across columns, a value of three interpolating across lines,
+and any other non-zero value interpolating along the narrowest dimension.
+.le
+.ls biassec
+Overscan bias strip image section.  If "image" is specified then the overscan
+bias section is specified in the image header or instrument translation file.
+Only the part of the bias section along the readout axis is used.  The
+length of the bias region fit is defined by the trim section.  If one
+wants to limit the region of the overscan used in the fit to be less
+than that of the trim section then the sample region parameter,
+\fIsample\fR, should be used.  It is an error if no section or the
+whole image is specified.
+.le
+.ls trimsec
+image section for trimming.  If "image" is specified then the trim
+image section is specified in the image header or instrument translation file.
+.le
+.ls zero = ""
+Zero level calibration image.  The zero level image may be one or two
+dimensional.  The CCD image type and subset are not checked for these
+images and they take precedence over any zero level calibration images
+given in the input list.
+.le
+.ls dark = ""
+Dark count calibration image.  The CCD image type and subset are not checked
+for these images and they take precedence over any dark count calibration
+images given in the input list.
+.le
+.ls flat = ""
+Flat field calibration images.  The flat field images may be one or
+two dimensional.  The CCD image type is not checked for these
+images and they take precedence over any flat field calibration images given
+in the input list.  The flat field image with the same subset as the
+input image being processed is selected.
+.le
+.ls illum = ""
+Iillumination correction images.  The CCD image type is not checked for these
+images and they take precedence over any iillumination correction images given
+in the input list.  The iillumination image with the same subset as the
+input image being processed is selected.
+.le
+.ls fringe = ""
+Fringe correction images.  The CCD image type is not checked for these
+images and they take precedence over any fringe correction images given
+in the input list.  The fringe image with the same subset as the
+input image being processed is selected.
+.le
+.ls minreplace = 1.
+When processing flat fields, pixel values below this value (after
+all other processing such as overscan, zero, and dark corrections) are
+replaced by this value.  This allows flat fields processed by \fBccdproc\fR
+to be certain to avoid divide by zero problems when applied to object
+images.
+.le
+.ls scantype = "shortscan"
+Type of scan format used in creating the CCD images.  The modes are:
+.ls "shortscan"
+The CCD is scanned over a number of lines and then read out as a regular
+two dimensional image.  In this mode unscanned zero level, dark count and
+flat fields are numerically scanned to form scanned flat fields comparable
+to the observations.
+.le
+.ls "longscan"
+In this mode the CCD is clocked and read out continuously to form a long
+strip.  Flat fields are averaged across the readout axis to
+form a one dimensional flat field readout correction image.  This assumes
+that all recorded image lines are clocked over the entire active area of the
+CCD.
+.le
+.le
+.ls nscan
+Number of object scan readout lines used in short scan mode.  This parameter
+is used when the scan type is "shortscan" and the number of scan lines
+cannot be determined from the object image header (using the keyword
+nscanrows or it's translation).
+.le
+
+
+.ce
+OVERSCAN FITTING PARAMETERS
+
+There are two types of overscan (or prescan) determinations.  One determines
+a independent overscan value for each line  and is only available for a
+\fIreadaxis\fR of 1.  The other averages the overscan along the readout
+direction to make an overscan vector, fits a smoothing function to the vector,
+and then evaluate and then evaluates the smooth function at each readout
+line or column.  The line-by-line determination only uses the
+\fIfunction\fR parameter and the smoothing determinations uses all
+the following parameters.
+
+.ls function = "legendre"
+Line-by-line determination of the overscan is specified by:
+
+.nf
+         mean - the mean of the biassec columns at each line
+       median - the median of the biassec columns at each line
+       minmax - the mean at each line with the min and max excluded
+.fi
+
+The smoothed overscan vector may be fit by one of the functions:
+
+.nf
+     legendre - legendre polynomial
+    chebyshev - chebyshev polynomial
+      spline1 - linear spline
+      spline3 - cubic spline
+.fi
+.le
+.ls order = 1
+Number of polynomial terms or spline pieces in the overscan fit.
+.le
+.ls sample = "*"
+Sample points to use in the overscan fit.  The string "*" specified all
+points otherwise an \fBicfit\fR range string is used.
+.le
+.ls naverage = 1
+Number of points to average or median to form fitting points.  Positive
+numbers specify averages and negative numbers specify medians.
+.le
+.ls niterate = 1
+Number of rejection iterations to remove deviant points from the overscan fit.
+If 0 then no points are rejected.
+.le
+.ls low_reject = 3., high_reject = 3.
+Low and high sigma rejection factors for rejecting deviant points from the
+overscan fit.
+.le
+.ls grow = 0.
+One dimensional growing radius for rejection of neighbors to deviant points.
+.le
+.ls interactive = no
+Fit the overscan vector interactively?  If yes and the overscan function type
+is one of the \fBicfit\fR types then the average overscan vector is fit
+interactively using the \fBicfit\fR package.  If no then the fitting parameters
+given below are used.
+.le
+.ih
+DESCRIPTION
+\fBCcdproc\fR processes CCD images to correct and calibrate for
+detector defects, readout bias, zero level bias, dark counts,
+response, iillumination, and fringing.  It also trims unwanted
+lines and columns and changes the pixel datatype.  It is efficient
+and easy to use; all one has to do is set the parameters and then
+begin processing the images.  The task takes care of most of the
+record keeping and automatically does the prerequisite processing
+of calibration images.  Beneath this simplicity there is much that
+is going on.  In this section a simple description of the usage is
+given.  The following sections present more detailed discussions
+on the different operations performed and the order and logic
+of the processing steps.  For a user's guide to the \fBccdred\fR
+package see \fBguide\fR.  Much of the ease of use derives from using
+information in the image header.  If this information is missing
+see section 13.
+
+One begins by setting the task parameters.  There are many parameters
+but they may be easily reviewed and modified using the task \fBeparam\fR.
+The input CCD images to be processed are given as an image list.
+Previously processed images are ignored and calibration images are
+recognized, provided the CCD image types are in the image header (see
+\fBinstruments\fR and \fBccdtypes\fR).  Therefore it is permissible to
+use simple image templates such as "*.imh".  The \fIccdtype\fR parameter
+may be used to select only certain types of CCD images to process
+(see \fBccdtypes\fR).
+
+The processing operations are selected by boolean (yes/no) parameters.
+Because calibration images are recognized and processed appropriately,
+the processing operations for object images should be set.
+Any combination of operations may be specified and the operations are
+performed simultaneously.  While it is possible to do operations in
+separate steps this is much less efficient.  Two of the operation
+parameters apply only to zero level and flat field images.  These
+are used for certain types of CCDs and modes of operation.
+
+The processing steps selected have related parameters which must be
+set.  These are things like image sections defining the overscan and
+trim regions and calibration images.  There are a number of parameters
+used for fitting the overscan or prescan bias section.  These are
+parameters used by the standard IRAF curve fitting package \fBicfit\fR.
+The parameters are described in more detail in the following sections.
+
+In addition to the task parameters there are package parameters
+which affect \fBccdproc\fR.  These include the instrument and subset
+files, the text and plot log files, the output pixel datatype,
+the amount of memory available for calibration image caching,
+the verbose parameter for logging to the terminal, and the backup
+prefix.  These are described in \fBccdred\fR.
+
+Calibration images are specified by task parameters and/or in the
+input image list.  If more than one calibration image is specified
+then the first one encountered is used and a warning is issued for the
+extra images.  Calibration images specified by
+task parameters take precedence over calibration images in the input list.
+These images also need not have a CCD image type parameter since the task
+parameter identifies the type of calibration image.  This method is
+best if there is only one calibration image for all images
+to be processed.  This is almost always true for zero level and dark
+count images.  If no calibration image is specified by task parameter
+then calibration images in the input image list are identified and
+used.  This requires that the images have CCD image types recognized
+by the package.  This method is useful if one may simply say "*.imh"
+as the image list to process all images or if the images are broken
+up into groups, in "@" files for example, each with their own calibration
+frames.
+
+When an input image is processed the task first determines the processing
+parameters and calibration images.  If a requested operation has been
+done it is skipped and if all requested operations have been completed then
+no processing takes place.  When it determines that a calibration image
+is required it checks for the image from the task parameter and then
+for a calibration image of the proper type in the input list.
+
+Having
+selected a calibration image it checks if it has been processed for
+all the operations selected by the CCDPROC parameters.
+After the calibration images have been identified, and processed if
+necessary, the images may be cached in memory.  This is done when there
+are more than two input images (it is actually less efficient to
+cache the calibration images for one or two input images) and the parameter
+\fImax_cache\fR is greater than zero.  When caching, as many calibration
+images as allowed by the specified memory are read into memory and
+kept there for all the input images.  Cached images are, therefore,
+only read once from disk which reduces the amount of disk I/O.  This
+makes a modest decrease in the execution time.  It is not dramatic
+because the actual processing is fairly CPU intensive.
+
+Once the processing parameters and calibration images have been determined
+the input image is processed for all the desired operations in one step;
+i.e. there are no intermediate results or images.  This makes the task
+efficient.  If a matching list of output images is given then the processed
+image is written to the specified output image name.  If no output image
+list is given then the corrected image is output as a temporary image until
+the entire image has been processed.  When the image has been completely
+processed then the original image is deleted (or renamed using the
+specified backup prefix) and the corrected image replaces the original
+image.  Using a temporary image protects the data in the event of an abort
+or computer failure.  Keeping the original image name eliminates much of
+the record keeping and the need to generate new image names.
+.sh
+1. Fixpix
+Regions of bad lines and columns may be replaced by linear
+interpolation from neighboring lines and columns when the parameter
+\fIfixpix\fR is set.  This algorithm is the same as used in the
+task \fBfixpix\fR.  The bad pixels may be specified by a pixel mask,
+an image, or a text file.  For the mask or image, values of zero indicate
+good pixels and other values indicate bad pixels to be replaced.
+
+The text file consists of lines with four fields, the starting and
+ending columns and the starting and ending lines.  Any number of
+regions may be specified.  Comment lines beginning with the character
+'#' may be included.  The description applies directly to the input
+image (before trimming) so different files are needed for previously
+trimmed or subsection readouts.  The data in this file is internally
+turned into the same description as a bad pixel mask with values of
+two for regions which are narrower or equal across the columns and
+a value of three for regions narrower across lines.
+
+The direction of interpolation is determined from the values in the
+mask, image, or the converted text file.  A value of two interpolates
+across columns, a value of three interpolates across lines, and any
+other value interpolates across the narrowest dimension of bad pixels
+and using column interpolation if the two dimensions are equal.
+
+The bad pixel description may be specified explicitly with the parameter
+\fIfixfile\fR or indirectly if the parameter has the value "image".  In the
+latter case the instrument file must contain the name of the file.
+.sh
+2. Overscan
+If an overscan or prescan correction is specified (\fIoverscan\fR
+parameter) then the image section (\fIbiassec\fR parameter) defines
+the overscan region.
+
+There are two types of overscan (or prescan) determinations.  One determines
+a independent overscan value for each line  and is only available for a
+\fIreadaxis\fR of 1.  The other averages the overscan along the readout
+direction to make an overscan vector, fits a smoothing function to the vector,
+and then evaluate and then evaluates the smooth function at each readout
+line or column.
+
+The line-by-line determination provides an mean, median, or
+mean with the minimum and maximum values excluded.  The median
+is lowest value of the middle two when the number of overscan columns
+is even rather than the mean.
+
+The smoothed overscan vector determination uses the \fBicfit\fR options
+including interactive fitting.  The fitting function is generally either a
+constant (polynomial of 1 term) or a high order function which fits the
+large scale shape of the overscan vector.  Bad pixel rejection is also
+available to eliminate cosmic ray events.  The function fitting may be done
+interactively using the standard \fBicfit\fR iteractive graphical curve
+fitting tool.  Regardless of whether the fit is done interactively, the
+overscan vector and the fit may be recorded for later review in a metacode
+plot file named by the parameter \fIccdred.plotfile\fR.  The mean value of
+the bias function is also recorded in the image header and log file.
+.sh
+3. Trim
+When the parameter \fItrim\fR is set the input image will be trimmed to
+the image section given by the parameter \fItrimsec\fR.  This trim
+should, of course, be the same as that used for the calibration images.
+.sh
+4. Zerocor
+After the readout bias is subtracted, as defined by the overscan or prescan
+region, there may still be a zero level bias.  This level may be two
+dimensional or one dimensional (the same for every readout line).  A
+zero level calibration is obtained by taking zero length exposures;
+generally many are taken and combined.  To apply this zero
+level calibration the parameter \fIzerocor\fR is set.  In addition if
+the zero level bias is only readout dependent then the parameter \fIreadcor\fR
+is set to reduce two dimensional zero level images to one dimensional
+images.  The zero level images may be specified by the parameter \fIzero\fR
+or given in the input image list (provided the CCD image type is defined).
+
+When the zero level image is needed to correct an input image it is checked
+to see if it has been processed and, if not, it is processed automatically.
+Processing of zero level images consists of bad pixel replacement,
+overscan correction, trimming, and averaging to one dimension if the
+readout correction is specified.
+.sh
+5. Darkcor
+Dark counts are subtracted by scaling a dark count calibration image to
+the same exposure time as the input image and subtracting.  The
+exposure time used is the dark time which may be different than the
+actual integration or exposure time.  A dark count calibration image is
+obtained by taking a very long exposure with the shutter closed; i.e.
+an exposure with no light reaching the detector.  The dark count
+correction is selected with the parameter \fIdarkcor\fR and the dark
+count calibration image is specified either with the parameter
+\fIdark\fR or as one of the input images.  The dark count image is
+automatically processed as needed.  Processing of dark count images
+consists of bad pixel replacement, overscan and zero level correction,
+and trimming.
+.sh
+6. Flatcor
+The relative detector pixel response is calibrated by dividing by a
+scaled flat field calibration image.  A flat field image is obtained by
+exposure to a spatially uniform source of light such as an lamp or
+twilight sky.  Flat field images may be corrected for the spectral
+signature in spectroscopic images (see \fBresponse\fR and
+\fBapnormalize\fR), or for iillumination effects (see \fBmkillumflat\fR
+or \fBmkskyflat\fR).  For more on flat fields and iillumination corrections
+see \fBflatfields\fR.  The flat field response is dependent on the
+wavelength of light so if different filters or spectroscopic wavelength
+coverage are used a flat field calibration for each one is required.
+The different flat fields are  automatically selected by a subset
+parameter (see \fBsubsets\fR).
+
+Flat field calibration is selected with the parameter \fBflatcor\fR
+and the flat field images are specified with the parameter \fBflat\fR
+or as part of the input image list.  The appropriate subset is automatically
+selected for each input image processed.  The flat field image is
+automatically processed as needed.  Processing consists of bad pixel
+replacement, overscan subtraction, zero level subtraction, dark count
+subtraction, and trimming.  Also if a scan mode is used and the
+parameter \fIscancor\fR is specified then a scan mode correction is
+applied (see below).  The processing also computes the mean of the
+flat field image which is used later to scale the flat field before
+division into the input image.  For scan mode flat fields the ramp
+part is included in computing the mean which will affect the level
+of images processed with this flat field.  Note that there is no check for
+division by zero in the interest of efficiency.  If division by zero
+does occur a fatal error will occur.  The flat field can be fixed by
+replacing small values using a task such as \fBimreplace\fR or
+during processing using the \fIminreplace\fR parameter.  Note that the
+\fIminreplace\fR parameter only applies to flat fields processed by
+\fBccdproc\fR.
+.sh
+7. Illumcor
+CCD images processed through the flat field calibration may not be
+completely flat (in the absence of objects).  In particular, a blank
+sky image may still show gradients.  This residual nonflatness is called
+the iillumination pattern.  It may be introduced even if the detector is
+uniformly illuminated by the sky because the flat field lamp
+iillumination may be nonuniform.  The iillumination pattern is found from a
+blank sky, or even object image, by heavily smoothing and rejecting
+objects using sigma clipping.  The iillumination calibration image is
+divided into the data being processed to remove the iillumination
+pattern.  The iillumination pattern is a function of the subset so there
+must be an iillumination correction image for each subset to be
+processed.  The tasks \fBmkillumcor\fR and \fBmkskycor\fR are used to
+create the iillumination correction images.  For more on iillumination
+corrections see \fBflatfields\fR.
+
+An alternative to treating the iillumination correction as a separate
+operation is to combine the flat field and iillumination correction
+into a corrected flat field image before processing the object
+images.  This will save some processing time but does require creating
+the flat field first rather than correcting the images at the same
+time or later.  There are two methods, removing the large scale
+shape of the flat field and combining a blank sky image iillumination
+with the flat field.  These methods are discussed further in the
+tasks which create them; \fBmkillumcor\fR and \fBmkskycor\fR.
+.sh
+8. Fringecor
+There may be a fringe pattern in the images due to the night sky lines.
+To remove this fringe pattern a blank sky image is heavily smoothed
+to produce an iillumination image which is then subtracted from the
+original sky image.  The residual fringe pattern is scaled to the
+exposure time of the image to be fringe corrected and then subtracted.
+Because the intensity of the night sky lines varies with time an
+additional scaling factor may be given in the image header.
+The fringe pattern is a function of the subset so there must be
+a fringe correction image for each subset to be processed.
+The task \fBmkfringecor\fR is used to create the fringe correction images.
+.sh
+9. Readcor
+If a zero level correction is desired (\fIzerocor\fR parameter)
+and the parameter \fIreadcor\fR is yes then a single zero level
+correction vector is applied to each readout line or column.  Use of a
+readout correction rather than a two dimensional zero level image
+depends on the nature of the detector or if the CCD is operated in
+longscan mode (see below).  The readout correction is specified by a
+one dimensional image (\fIzero\fR parameter) and the readout axis
+(\fIreadaxis\fR parameter).  If the zero level image is two dimensional
+then it is automatically processed to a one dimensional image by
+averaging across the readout axis.  Note that this modifies the zero
+level calibration image.
+.sh
+10. Scancor
+CCD detectors may be operated in several modes in astronomical
+applications.  The most common is as a direct imager where each pixel
+integrates one point in the sky or spectrum.  However, the design of most CCD's
+allows the sky to be scanned across the CCD while shifting the
+accumulating signal at the same rate.  \fBCcdproc\fR provides for two
+scanning modes called "shortscan" and "longscan".  The type of scan
+mode is set with the parameter \fIscanmode\fR.
+
+In "shortscan" mode the detector is scanned over a specified number of
+lines (not necessarily at sideral rates).  The lines that scroll off the
+detector during the integration are thrown away.  At the end of the
+integration the detector is read out in the same way as an unscanned
+observation.  The advantage of this mode is that the small scale, zero
+level, dark count and flat field responses are averaged in one dimension
+over the number of lines scanned.  A zero level, dark count or flat field may be
+observed in the same way in which case there is no difference in the
+processing from unscanned imaging and the parameter \fIscancor\fR may be
+no.  If it is yes, though, checking is done to insure that the calibration
+image used has the same number of scan lines as the object being
+processed.  However, one obtains an increase in the statistical accuracy of
+if they are not scanned during the observation but
+digitally scanned during the processing.  In shortscan mode with
+\fIscancor\fR set to yes, zero level, dark count and flat field images are
+digitally scanned, if needed, by the same number of scan lines as the
+object.  The number of scan lines is determined from the object image
+header using the keyword nscanrow (or it's translation).  If not found the
+object is assumed to have been scanned with the value given by the
+\fInscan\fR parameter.  Zero, dark and flat calibration images are assumed
+to be unscanned if the header keyword is not found.
+
+If a scanned zero level, dark count or flat field image is not found
+matching the object then one may be created from the unscanned calibration
+image.  The image will have the root name of the unscanned image with an
+extension of the number of scan rows; i.e. Flat1.32 is created from Flat1
+with a digital scanning of 32 lines.
+
+In "longscan" mode the detector is continuously read out to produce an
+arbitrarily long strip.  Provided data which has not passed over the entire
+detector is thrown away, the zero level, dark count, and flat field
+corrections will be one dimensional.  If \fIscancor\fR is specified and the
+scan mode is "longscan" then a one dimensional zero level, dark count, and
+flat field correction will be applied.
+.sh
+11. Processing Steps
+The following describes the steps taken by the task.  This detailed
+outline provides the most detailed specification of the task.
+
+.ls 5 (1)
+An image to be processed is first checked that it is of the specified
+CCD image type.  If it is not the desired type then go on to the next image.
+.le
+.ls (2)
+A temporary output image is created of the specified pixel data type
+(\fBccdred.pixeltype\fR).  The header parameters are copied from the
+input image.
+.le
+.ls (3)
+If trimming is specified and the image has not been trimmed previously,
+the trim section is determined.
+.le
+.ls (4)
+If bad pixel replacement is specified and this has not been done
+previously, the bad pixel file is determined either from the task
+parameter or the instrument translation file.  The bad pixel regions
+are read.  If the image has been trimmed previously and the bad pixel
+file contains the word "untrimmed" then the bad pixel coordinates are
+translated to those of the trimmed image.
+.le
+.ls (5)
+If an overscan correction is specified and this correction has not been
+applied, the overscan section is averaged along the readout axis.  If
+trimming is to be done the overscan section is trimmed to the same
+limits.  A function is fit either interactively or noninteractively to
+the overscan vector.  The function is used to produce the overscan
+vector to be subtracted from the image.  This is done in real
+arithmetic.
+.le
+.ls (6)
+If the image is a zero level image go to processing step 12.
+If a zero level correction is desired and this correction has not been
+performed, find the zero level calibration image.  If the zero level
+calibration image has not been processed it is processed at this point.
+This is done by going to processing step 1 for this image.  After the
+calibration image has been processed, processing of the input image
+continues from this point.
+The processed calibration image may be
+cached in memory if it has not been previously and if there is enough memory.
+.le
+.ls (7)
+If the image is a dark count image go to processing step 12.
+If a dark count correction is desired and this correction has not been
+performed, find the dark count calibration image.  If the dark count
+calibration image has not been processed it is processed at this point.
+This is done by going to processing step 1 for this image.  After the
+calibration image has been processed, processing of the input image
+continues from this point.  The ratio of the input image dark time
+to the dark count image dark time is determined to be multiplied with
+each pixel of the dark count image before subtracting from the input
+image.
+The processed calibration image may be
+cached in memory if it has not been previously and if there is enough memory.
+.le
+.ls (8)
+If the image is a flat field image go to processing step 12.  If a flat
+field correction is desired and this correction has not been performed,
+find the flat field calibration image of the appropriate subset.  If
+the flat field calibration image has not been processed it is processed
+at this point.  This is done by going to processing step 1 for this
+image.  After the calibration image has been processed, processing of
+the input image continues from this point.  The mean of the image
+is determined from the image header to be used for scaling.  If no
+mean is found then a unit scaling is used.
+The processed calibration image may be
+cached in memory if it has not been previously and if there is enough memory.
+.le
+.ls (9)
+If the image is an iillumination image go to processing step 12.  If an
+iillumination correction is desired and this correction has not been performed,
+find the iillumination calibration image of the appropriate subset.
+The iillumination image must have the "mkillum" processing flag or the
+\fBccdproc\fR will abort with an error.  The mean of the image
+is determined from the image header to be used for scaling.  If no
+mean is found then a unit scaling is used.  The processed calibration
+image may be
+cached in memory if it has not been previously and there is enough memory.
+.le
+.ls (10)
+If the image is a fringe image go to processing step 12.  If a fringe
+correction is desired and this correction has not been performed,
+find the fringe calibration image of the appropriate subset.
+The iillumination image must have the "mkfringe" processing flag or the
+\fBccdproc\fR will abort with an error.  The ratio of the input
+image exposure time to the fringe image exposure time is determined.
+If there is a fringe scaling in the image header then this factor
+is multiplied by the exposure time ratio.  This factor is used
+for scaling.  The processed calibration image may be
+cached in memory if it has not been previously and there is enough memory.
+.le
+.ls (11)
+If there are no processing operations flagged, delete the temporary output
+image, which has been opened but not used, and go to 14.
+.le
+.ls (12)
+The input image is processed line by line with trimmed lines ignored.
+A line of the input image is read.  Bad pixel replacement and trimming
+is applied to the image.  Image lines from the calibration images
+are read from disk or the image cache.  If the calibration is one
+dimensional (such as a readout zero
+level correction or a longscan flat field correction) then the image
+vector is read only once.  Note that IRAF image I/O is buffered for
+efficiency and accessing a line at a time does not mean that image
+lines are read from disk a line at a time.  Given the input line, the
+calibration images, the overscan vector, and the various scale factors
+a special data path for each combination of corrections is used to
+perform all the processing in the most efficient manner.  If the
+image is a flat field any pixels less than the \fIminreplace\fR
+parameter are replaced by that minimum value.  Also a mean is
+computed for the flat field and stored as the CCDMEAN keyword and
+the time, in a internal format, when this value was calculated is stored
+in the CCDMEANT keyword.  The time is checked against the image modify
+time to determine if the value is valid or needs to be recomputed.
+.le
+.ls (13)
+The input image is deleted or renamed to a backup image.  The temporary
+output image is renamed to the input image name.
+.le
+.ls (14)
+If the image is a zero level image and the readout correction is specified
+then it is averaged to a one dimensional readout correction.
+.le
+.ls (15)
+If the image is a zero level, dark count, or flat field image and the scan
+mode correction is specified then the correction is applied.  For shortscan
+mode a modified two dimensional image is produced while for longscan mode a
+one dimensional average image is produced.
+.le
+.ls (16)
+The processing is completed and either the next input image is processed
+beginning at step 1 or, if it is a calibration image which is being
+processed for an input image, control returns to the step which initiated
+the calibration image processing.
+.le
+.sh
+12. Processing Arithmetic
+The \fBccdproc\fR task has two data paths, one for real image pixel datatypes
+and one for short integer pixel datatype.  In addition internal arithmetic
+is based on the rules of FORTRAN.  For efficiency there is
+no checking for division by zero in the flat field calibration.
+The following rules describe the processing arithmetic and data paths.
+
+.ls (1)
+If the input, output, or any calibration image is of type real the
+real data path is used.  This means all image data is converted to
+real on input.  If all the images are of type short all input data
+is kept as short integers.  Thus, if all the images are of the same type
+there is no datatype conversion on input resulting in greater
+image I/O efficiency.
+.le
+.ls (2)
+In the real data path the processing arithmetic is always real and,
+if the output image is of short pixel datatype, the result
+is truncated.
+.le
+.ls (3)
+The overscan vector and the scale factors for dark count, flat field,
+iillumination, and fringe calibrations are always of type real.  Therefore,
+in the short data path any processing which includes these operations
+will be coerced to real arithmetic and the result truncated at the end
+of the computation.
+.le
+.sh
+13. In the Absence of Image Header Information
+The tasks in the \fBccdred\fR package are most convenient to use when
+the CCD image type, subset, and exposure time are contained in the
+image header.  The ability to redefine which header parameters contain
+this information makes it possible to use the package at many different
+observatories (see \fBinstruments\fR).  However, in the absence of any
+image header information the tasks may still be used effectively.
+There are two ways to proceed.  One way is to use \fBccdhedit\fR
+to place the information in the image header.
+
+The second way is to specify the processing operations more explicitly
+than is needed when the header information is present.  The parameter
+\fIccdtype\fR is set to "" or to "none".  The calibration images are
+specified explicitly by task parameter since they cannot be recognized
+in the input list.  Only one subset at a time may be processed.
+
+If dark count and fringe corrections are to be applied the exposure
+times must be added to all the images.  Alternatively, the dark count
+and fringe images may be scaled explicitly for each input image.  This
+works because the exposure times default to 1 if they are not given in
+the image header.
+.ih
+EXAMPLES
+The user's \fBguide\fR presents a tutorial in the use of this task.
+
+1. In general all that needs to be done is to set the task parameters
+and enter
+
+	cl> ccdproc *.imh &
+
+This will run in the background and process all images which have not
+been processed previously.
+.ih
+TIME REQUIREMENTS
+.nf
+o SUN-3, 15 MHz 68020 with 68881 floating point hardware (no FPA)
+o 8 Mb RAM, 2 Fuji Eagle disks.
+o Input images = 544 x 512 short
+o Output image = 500 x 500 real
+o Operations are overscan subtraction (O), trimming to 500x500 (T),
+  zero level subtraction (Z), dark count scaling and subtraction (D),
+  and flat field scaling and subtraction (F).
+o UNIX statistics
+  (user, system, and clock time, and misc. memory and i/o statistics):
+
+[OTF] One calibration image and 9 object images:
+No caching:  110.6u 25.5s 3:18 68% 28+ 40K 3093+1645io   9pf+0w
+Caching:     111.2u 23.0s 2:59 74% 28+105K 2043+1618io   9pf+0w
+
+[OTZF] Two calibration images and 9 object images:
+No caching:  119.2u 29.0s 3:45 65% 28+ 50K 4310+1660io   9pf+0w
+Caching:     119.3u 23.0s 3:07 75% 28+124K 2179+1601io   9pf+0w
+
+[OTZDF] Three calibration images and 9 object images:
+No caching:  149.4u 31.6s 4:41 64% 28+ 59K 5501+1680io  19pf+0w
+Caching:     151.5u 29.0s 4:14 70% 27+227K 2346+1637io 148pf+0w
+
+[OTZF] 2 calibration images and 20 images processed:
+No caching:  272.7u 63.8u 8:47 63% 28+ 50K 9598+3713io  12pf+0w
+Caching:     271.2u 50.9s 7:00 76% 28+173K 4487+3613io  51pf+0w
+.fi
+.ih
+REVISIONS
+.ls CCDPROC V2.11.2
+A new "output" parameter is available to specify an output image leaving
+the input image unchanged.  If this parameter is not specified then
+the previous behavior of "in-place" operation with an optional backup
+occurs.
+.le
+.ls CCDPROC V2.11
+The bad pixel fixing was modified to allow use of pixel masks,
+images, or the text file description.  Bad pixel masks are the
+desired description and use of text files is only supported for
+backward compatibility.  Note that support for the trimmed
+or untrimmed conversion from text files has been eliminated.
+
+Line-by-line overscan/prescan subtraction is now provided with
+three simple algorithms.
+.le
+.ls CCDPROC: V2.10.3
+The output pixel datatypes (specified by the package parameter
+\fIpixeltype\fR have been extended to include unsigned short
+integers.  Also it was previously possible to have the output
+pixel datatype be of lower precision than the input.  Now the
+output pixel datatype is not allowed to lose precision; i.e.
+a real input image may not be processed to a short datatype.
+
+For short scan data the task now looks for the number of scan lines in the
+image header.  Also when a calibration image is software scanned a new
+image is created.  This allows processing objects with different numbers of
+scan lines and preserving the unscanned calibration image.
+
+It is an error if no biassec is specified rather than defaulting to
+the whole image.
+
+The time, in a internal format, when the CCDMEAN value is calculated is
+stored in the CCDMEANT keyword.  The time is checked against the image
+modify time to determine if the value is valid or needs to be recomputed.
+.le
+.ih
+SEE ALSO
+.nf
+instruments, ccdtypes, flatfields, icfit, ccdred, guide, mkillumcor,
+mkskycor, mkfringecor
+.fi
+.endhelp
diff --git a/noao/imred/ccdred/doc/ccdred.hlp b/noao/imred/ccdred/doc/ccdred.hlp
new file mode 100644
index 00000000..f2cca5bd
--- /dev/null
+++ b/noao/imred/ccdred/doc/ccdred.hlp
@@ -0,0 +1,104 @@
+.help package Dec93 noao.imred
+.ih
+NAME
+ccdred -- CCD image reduction package
+.ih
+USAGE
+ccdred
+.ih
+PARAMETERS
+.ls pixeltype = "real real"
+Output pixel datatype and calculation datatype.  When images are processed
+or created the output pixel datatype is determined by this parameter if the
+specified datatype is of equal or higher precision otherwise the input
+image datatype is preserved.  For example if the output datatype is
+specified as "input" then input images which are "short" or "ushort" will
+be output as integer but any real datatype input images will remain real.
+The allowed types and order of precision are "short", "ushort", "int",
+"long", "real", or "double", for short signed integer, short unsigned
+integer, integer, long integers, and real or double floating point.  Note
+that if short input images are processed into real images the disk space
+required will generally increase.  The calculation datatypes may only be
+short and real with a default of real if none is specified.
+.le
+.ls verbose = no
+Print log information to the standard output?
+.le
+.ls logfile = "logfile"
+Text log file.  If no filename is specified then no log file is kept.
+.le
+.ls plotfile = ""
+Log metacode plot file for the overscan bias vector fits.  If no filename
+is specified then no metacode plot file is kept.
+.le
+.ls backup = ""
+Backup prefix for backup images.  If no prefix is specified then no backup
+images are kept when processing.  If specified then the backup image
+has the specified prefix.
+.le
+.ls instrument = ""
+CCD instrument translation file.  This is usually set with
+\fBsetinstrument\fR.
+.le
+.ls ssfile = "subsets"
+Subset translation file used to define the subset identifier.  See
+\fBsubsets\fR for more.
+.le
+.ls graphics = "stdgraph"
+Interactive graphics output device when fitting the overscan bias vector.
+.le
+.ls cursor = ""
+Graphics cursor input.  The default is the standard graphics cursor.
+.le
+.ls version = "June 1987"
+Package version.
+.le
+.ih
+DESCRIPTION
+The CCD reduction package is loaded when this command is entered.  The
+package contains parameters which affect the operation of the tasks it
+defines.  When images are processed or new image are created the output
+pixel datatype is that specified by the parameter \fBpixeltype\fR.  Note
+that CCD processing replaces the original image by the processed image so
+the pixel type of the CCD images may change during processing.  The output
+pixel type is not allowed to change to a lower precision but it is common
+for input short images to be processed to real images.  Processing images
+from short to real pixel datatypes will generally increase the amount of
+disk space required (a factor of 2 on most computers).
+
+The tasks produce log output which may be printed on the standard
+output (the terminal unless redirected) and appended to a file.  The
+parameter \fIverbose\fR determines whether processing information
+is printed.  This may be desirable initially, but when using background
+jobs the verbose output should be turned off.  The user may look at
+the end of the log file (for example with \fBtail\fR) to determine
+the status of the processing.
+
+The package was designed to work with data from many different observatories
+and instruments.  In order to accomplish this an instrument translation
+file is used to define a mapping between the package parameters and
+the particular image header format.  The instrument translation file
+is specified to the package by the parameter \fIinstrument\fR.  This
+parameter is generally set by the task \fBsetinstrument\fR.  The other
+file used is a subset file.  This is generally created and maintained
+by the package and the user need not do anything.  For more sophisticated
+users see \fBinstruments\fR and \fBsubsets\fR.
+
+The package has very little graphics
+output.  The exception is the overscan bias subtraction.  The bias
+vector is logged in the metacode plot file if given.  The plot file
+may be examined with the tasks in the \fBplot\fR package such as
+\fBgkimosaic\fR.  When interactively fitting the overscan vector
+the graphics input and output devices must be specified.  The defaults
+should apply in most cases.
+
+Because processing replaces the input image by the processed image it
+may be desired to save the original image.  This may be done by
+specifying a backup prefix with the parameter \fIbackup\fR.  For
+example, if the prefix is "orig" and the image is "ccd001", the backup
+image will be "origccd001".  The prefix may be a directory but it must
+end with '/' or '$' (for logical directories).
+.ih
+SEE ALSO
+ccdproc, instruments, setinstrument, subsets
+.endhelp
diff --git a/noao/imred/ccdred/doc/ccdred.ms b/noao/imred/ccdred/doc/ccdred.ms
new file mode 100644
index 00000000..645514ec
--- /dev/null
+++ b/noao/imred/ccdred/doc/ccdred.ms
@@ -0,0 +1,787 @@
+.RP
+.TL
+The IRAF CCD Reduction Package -- CCDRED
+.AU
+Francisco Valdes
+.AI
+IRAF Group - Central Computer Services
+.K2
+P.O. Box 26732, Tucson, Arizona 85726
+September 1987
+.AB
+The IRAF\(dg CCD reduction package, \fBccdred\fR, provides tools
+for the easy and efficient reduction of CCD images.  The standard
+reduction operations are replacement of bad pixels, subtraction of an
+overscan or prescan bias, subtraction of a zero level image,
+subtraction of a dark count image, division by a flat field calibration
+image, division by an illumination correction, subtraction of a fringe
+image, and trimming unwanted lines or columns.  Another common
+operation provided by the package is scaling and combining images with
+a number of algorithms for rejecting cosmic rays.  Data in the image
+header is used to make the reductions largely automated and
+self-documenting though the package may still be used in the absence of
+this data.  Also a translation mechanism is used to relate image header
+parameters to those used by the package to allow data from a variety of
+observatories and instruments to be processed.  This paper describes
+the design goals for the package and the main tasks and algorithms
+which satisfy these goals.
+.PP
+This paper is to be published as part of the proceedings of the
+Santa Cruz Summer Workshop in Astronomy and Astrophysics,
+\fIInstrumentation for Ground-Based Optical Astronomy:  Present and
+Future\fR, edited by Lloyd B. Robinson and published by
+Springer-Verlag.
+.LP
+\(dgImage Reduction and Analysis Facility (IRAF), a software system
+distributed by the National Optical Astronomy Observatories (NOAO).
+.AE
+.NH
+Introduction
+.PP
+The IRAF CCD reduction package, \fBccdred\fR, provides tools
+for performing the standard instrumental corrections and calibrations
+to CCD images.  The major design goals were:
+.IP
+.nf
+\(bu To be easy to use
+\(bu To be largely automated
+\(bu To be image header driven if the data allows
+\(bu To be usable for a variety of instruments and observatories
+\(bu To be efficient and capable of processing large volumes of data
+.fi
+.LP
+This paper describes the important tasks and algorithms and shows how
+these design goals were met.  It is not intended to describe every
+task, parameter, and usage in detail; the package has full
+documentation on each task plus a user's guide.
+.PP
+The standard CCD correction and calibration operations performed are
+replacement of bad columns and lines by interpolation from neighboring
+columns and lines, subtraction of a bias level determined from overscan
+or prescan columns or lines, subtraction of a zero level using a zero
+length exposure calibration image, subtraction of a dark count
+calibration image appropriately scaled to the dark time exposure of the
+image, division by a scaled flat field calibration image, division by
+an illumination image (derived from a blank sky image), subtraction of
+a scaled fringe image (also derived from a blank sky image), and
+trimming the image of unwanted lines or columns such as the overscan
+strip.  The processing may change the pixel datatype on disk (IRAF allows
+seven image datatypes); usually from 16 bit integer to real format.
+Two special operations are also supported for scan mode and one
+dimensional zero level and flat field calibrations; i.e. the same
+calibration is applied to each CCD readout line.  Any set of operations
+may be done simultaneously over a list of images in a highly efficient
+manner.  The reduction operations are recorded in the image header and
+may also be logged on the terminal and in a log file.
+.PP
+The package also provides tools for combining multiple exposures
+of object and calibration images to improve the statistical accuracy of
+the observations and to remove transient bad pixels.  The combining
+operation scales images of different exposure times, adjusts for
+variable sky background, statistically weights the images by their
+signal-to-noise, and provides a number of useful algorithms for
+detecting and rejecting transient bad pixels.
+.PP
+Other tasks are provided for listing reduction information about
+the images, deriving secondary calibration images (such as sky
+corrected flat fields or illumination correction images), and easily
+setting the package parameters for different instruments.
+.PP
+This paper is organized as follows.  There is a section giving an
+overview of how the package is used to reduce CCD data.  This gives the
+user's perspective and illustrates the general ease of use.  The next
+section describes many of the features of the package contributing to
+its ease of use, automation, and generality.  The next two sections
+describe the major tools and algorithms in some detail.  This includes
+discussions about achieving high efficiency.  Finally the status of the
+package and its use at NOAO is given.  References to additional
+documentation about IRAF and the CCD reduction package and an appendix
+listing the individual tasks in the package are found at the end of
+this paper.
+.NH
+A User's Overview
+.PP
+This section provides an overview of reducing data with the IRAF CCD
+reduction package.  There are many variations in usage depending on the
+type of data, whether the image headers contain information about the
+data which may be used by the tasks, and the scientific goal.  Only a
+brief example is given.  A more complete discussion of usage and
+examples is given in \fIA User's Guide to the IRAF CCDRED Package\fR.
+The package was developed within the IRAF system and so makes use of
+all the sophisticated features provided.  These features are also
+summarized here for those not familiar with IRAF since they are an
+important part of using the package.
+.PP
+Since the IRAF system is widely distributed and runs on a wide variety
+of computers, the site of the CCD reductions might be at the telescope,
+a system at the observatory provided for this purpose, or at the
+user's home computer.  The CCD images to be processed are either
+available immediately as the data is taken, transferred from the data taking
+computer via a network link (the method adopted at NOAO), or transferred
+to the reduction computer via a medium such as magnetic tape in FITS
+format.  The flexibility in reduction sites and hardware is one of the
+virtues of the IRAF-based CCD reduction package.
+.PP
+IRAF tasks typically have a number of parameters which give the user
+control over most aspects of the program.  This is possible since the
+parameters are kept in parameter files so that the user need not enter
+a large number of parameters every time the task is run.  The user may
+change any of these parameters as desired in several ways, such as by
+explicit assignment and using an easy to learn and use,
+fill-in-the-value type of screen editor.  The parameter values are
+\fIlearned\fR so that once a user sets the values they are maintained
+until the user changes them again; even between login sessions.
+.PP
+The first step in using the CCD reduction package is to set the default
+processing parameters for the data to be reduced.  These parameters include
+a database file describing the image header keyword translations and
+default values, the processing operations desired (operations
+required vary with instrument and observer), the calibration image names,
+and certain special parameters for special types of observations such
+as scan mode.  A special script task (a command procedure) is available
+to automatically set the default values, given the instrument name, to standard
+values defined by the support staff.  Identifying the instrument in this
+way may be all the novice user need do though most people quickly learn
+to adjust parameters at will.
+.PP
+As an example suppose there is an instrument identified as \fLrca4m\fR
+for an RCA CCD at the NOAO 4 meter telescope.  The user gives the command
+
+.ft L
+    cl> setinstrument rca4m
+.ft R
+
+which sets the default parameters to values suggested by the support staff
+for this instrument.  The user may then change these suggested values if
+desired.  In this example the processing switches are set to perform
+overscan bias subtraction, zero level image subtraction, flat fielding,
+and trimming.
+.PP
+The NOAO image headers contain information identifying the type of
+image, such as object, zero level, and flat field, the filter used to
+match flat fields with object images, the location of the overscan bias
+data, the trim size for the data, and whether the image has been
+processed.  With this information the user need not worry about
+selecting images, pairing object images with calibration images, or
+inadvertently reprocessing an image.
+.PP
+The first step is to combine multiple zero level and flat field observations
+to reduce the effects of statistical noise.  This is done by the
+commands
+
+.nf
+.ft L
+	cl> zerocombine *.imh
+	cl> flatcombine *.imh
+.ft R
+.fi
+
+The "cl> " is the IRAF command language prompt.  The first command says
+look through all the images and combine the zero level images.  The
+second command says look through all the images and combine the flat
+field images by filter.  What could be simpler?  Some \fIhidden\fR (default)
+parameters the user may modify are the combined image name, whether to
+process the images first, and the type of combining algorithm to use.
+.PP
+The next step is to process the images using the combined calibration
+images.  The command is
+
+.ft L
+	cl> ccdproc *.imh
+.ft R
+
+This command says look through all the images, find the object images,
+find the overscan data based on the image header and subtract the
+bias, subtract the zero level calibration image, divide by the flat field
+calibration image, and trim the bias data and edge lines and columns.
+During this operation the task recognizes that the
+zero level and flat field calibration images have not been processed
+and automatically processes them when they are needed.  The log output
+of this task, which may be to the terminal, to a file, or both, shows
+how this works.
+
+.nf
+.ft L
+  ccd003: Jun  1 15:12 Trim data section is [3:510,3:510]
+  ccd003: Jun  1 15:12 Overscan section is [520:540,*], mean=485.0
+  Dark:   Jun  1 15:12 Trim data section is [3:510,3:510]
+  Dark:   Jun  1 15:13 Overscan section is [520:540,*], mean=484.6
+  ccd003: Jun  1 15:13 Dark count image is Dark.imh
+  FlatV:  Jun  1 15:13 Trim data section is [3:510,3:510]
+  FlatV:  Jun  1 15:14 Overscan section is [520:540,*], mean=486.4
+  ccd003: Jun  1 15:15 Flat field image is FlatV.imh, scale=138.2
+  ccd004: Jun  1 15:16 Trim data section is [3:510,3:510]
+  ccd004: Jun  1 15:16 Overscan section is [520:540,*], mean=485.2
+  ccd004: Jun  1 15:16 Dark count image is Dark.imh
+  ccd004: Jun  1 15:16 Flat field image is FlatV.imh, scale=138.2
+                \fI<... more ...>\fL
+  ccd013: Jun  1 15:22 Trim data section is [3:510,3:510]
+  ccd013: Jun  1 15:23 Overscan section is [520:540,*], mean=482.4
+  ccd013: Jun  1 15:23 Dark count image is Dark.imh
+  FlatB:  Jun  1 15:23 Trim data section is [3:510,3:510]
+  FlatB:  Jun  1 15:23 Overscan section is [520:540,*], mean=486.4
+  ccd013: Jun  1 15:24 Flat field image is FlatB.imh, scale=132.3
+                \fI<... more ...>\fL
+.ft R
+.fi
+
+.PP
+The log gives the name of the image and a time stamp for each entry.
+The first image is ccd003.  It is to be trimmed to the specified
+size given as an \fIimage section\fR, an array notation used commonly
+in IRAF to specify subsections of images.  The location of the
+overscan data is also given by an image section which, in this case,
+was found in the image header.  The mean bias level of the overscan
+is also logged though the overscan is actually a function of the
+readout line with the order of the function selected by the user.
+.PP
+When the task comes to subtracting the zero level image it first
+notes that the calibration image has not been processed and switches
+to processing the zero level image.  Since it knows it is a zero level
+image the task does not attempt to zero level or flat field correct
+this image.  After the zero level image has been processed the task
+returns to the object image only to find that the flat field image
+also has not been processed.  It determines that the object image was
+obtained with a V filter and selects the flat field image having the same
+filter.  The flat field image is processed through the zero level correction
+and then the task again returns to the object image, ccd003, which it
+finishes processing.
+.PP
+The next image, ccd004, is also a V filter
+observation.  Since the zero level and V filter flat field have been
+processed the object image is processed directly.  This continues
+for all the object images except for a detour to process the B filter flat
+field when the task first encounters a B filter object image.
+.PP
+In summary, the basic usage of the CCD reduction package is quite simple.
+First, the instrument is identified and some parameters for the data
+are set.  Calibration images are then combined if needed.  Finally,
+the processing is done with the simple command
+
+.ft L
+    cl> ccdproc *.imh&
+.ft R
+
+where the processing is performed as a \fIbackground job\fR in this example.
+This simplicity was a major goal of the package.
+.NH
+Features of the Package
+.PP
+This section describes some of the special features of the package
+which contribute to its ease of use, generality, and efficiency.
+The major criteria for ease of use are to minimize the user's record keeping
+involving input and output image names, the types of images, subset
+parameters such as filters which must be kept separate, and the state
+of processing of each image.  The goal is to allow input images to
+be specified using simple wildcards, such as "*.imh" to specify all
+images, with the knowledge that the task will only operate on images
+for which it makes sense.  To accomplish this the tasks must be able to
+determine the type of image, subset, and the state of processing from
+the image itself.  This is done by making use of image header parameters.
+.PP
+For generality the package does not require any image header information
+except the exposure time.  It is really not very much more difficult to
+reduce such data.  Mainly, the user must be more explicit about specifying
+images and setting task parameters or add the information to the image
+headers.  Some default header information may also be set in the image
+header translation file (discussed below).
+.PP
+One important image header parameter is the image type.  This
+discriminates between object images and various types of calibration
+images such as flat field, zero level, dark count, comparison arcs,
+illumination, and fringe images.  This information is used in two
+ways.  For most of the tasks the user may select that only one type of
+image be considered.  Thus, all the flat field images may be selected
+for combining or only the processing status of the object images be
+listed.  The second usage is to allow the processing tasks to identify
+the standard calibration images and apply only those operations which
+make sense.  For example, flat field images are not divided by a
+flat field.  This allows the user to set the processing operations
+desired for the object images without fear of misprocessing the
+calibration images.  The image type is also used to automatically
+select calibration images from a list of images to be processed instead
+of explicitly identifying them.
+.PP
+A related parameter specifies the subset.  For certain operations the
+images must have a common value for this parameter.  This parameter is
+often the filter but it may also apply to a grating or aperture, for example.
+The subset parameter is used to identify the appropriate flat field
+image to apply to an image or to select common flat fields to be combined
+into a higher quality flat field.  This is automatic and the user need not
+keep track of which image was taken with which filter or grating.
+.PP
+The other important image header parameters are the processing flags.
+These identify when an image has been processed and also act as a history
+of the operation including calibration images used and other parameter
+information.  The usage of these parameters is obvious; it allows the
+user to include processed images in a wildcard list knowing that the
+processing will not be repeated and to quickly determine the processing
+status of the image.
+.PP
+Use of image header parameters often ties the software to the a
+particular observatory.  To maintain generality and usefulness for data
+other than that at NOAO, the CCD reduction package was designed to
+provide a translation between parameters requested by the package and
+those actually found in the image header.  This translation is defined
+in a simple text file which maps one keyword to another and also gives
+a default value to be used if the image header does not include a
+value.  In addition the translation file maps the arbitrary strings
+which may identify image types to the standard types which the package
+recognizes.  This is a relatively simple scheme and does not allow for
+forming combinations or for interpreting values which are not simple
+such as embedding an exposure time as part of a string.  A more complex
+translation scheme may prove desirable as experience is gained with
+other types of image header formats, but by then a general header translation
+ability and/or new image database structure may be a standard IRAF
+feature.
+.PP
+This feature has proven useful at NOAO.  During the course of
+developing the package the data taking system was modernized by
+updating keywords and adding new information in the image headers,
+generally following the lines laid out by the \fBccdred\fR package.
+However, there is a period of transition and it is also desirable to
+reduce preexisting data.  There are several different formats for this
+data.  The header translation files make coping with these different
+formats relatively easy.
+.PP
+A fundamental aspect of the package is that the processing
+modifies the images.  In other words, the reduction operations are
+performed directly on the image.  This "feature" further simplifies
+record keeping, frees the user from having to form unique output image
+names, and minimizes the amount of disk space required.  There
+are two safety features in this process.  First, the modifications do
+not take effect until the operation is completed on the image.  This
+allows the user to abort the task without leaving the image data in a
+partially processed state and protects data if the computer
+crashes.  The second feature is that there is a parameter which may be
+set to make a backup of the input data with a particular prefix; for
+example "b", "orig", or "imdir$" (a logical directory prefix).  This
+backup feature may be used when there is sufficient disk space, when
+learning to use the package, or just to be cautious.
+.PP
+In a similar effort to efficiently manage disk space, when combining
+images into a master object or calibration image, there is an option to
+delete the input images upon completion of the combining operation.
+Generally this is desirable when there are many calibration exposures,
+such as zero level or flat field images, which are not used after they
+are combined into a final calibration image.
+.PP
+The goal of generality for many instruments at
+different observatories inherently conflicts with the goal of ease of
+use.  Generality requires many parameters and options.  This is
+feasible in the CCD reduction package, as well as the other IRAF packages,
+because of the IRAF parameter handling mechanism.  In \fBccdred\fR
+there still remains the problem of setting the parameters appropriately
+for a particular instrument, image header format, and observatory.
+.PP
+To make this convenient there is a task, \fBsetinstrument\fR, that,
+based on an instrument name, runs a setup script for the instrument.
+An example of this task was given in the previous section.
+The script may do any type of operation but mainly it sets default
+parameters.  The setup scripts are generally created by the support staff
+for the instrument.  The combination of the setup script and the
+instrument translation file make the package, in a sense, programmable
+and achieves the desired instrument/observatory generality with ease of use.
+.NH
+CCD Processing
+.PP
+This section describes in some detail how the CCD processing is performed.
+The task which does the basic CCD processing is call \fBccdproc\fR.
+From the point of view of usage the task is very simple but a great deal
+is required to achieve this simplicity.  The approach we take in describing
+the task is to follow the flow of control as the task runs with digressions
+as appropriate.
+.PP
+The highest level of control is a loop over the input images; all the
+operations are performed successively on each image.  It is common for
+IRAF tasks which operate on individual images to allow the operation to
+be repeated automatically over a list of input images.  This is important
+in the \fBccdred\fR package because data sets are often large and the
+processing is generally the same for each image.  It would be tedious
+to have to give the processing command for each image to be processed.
+If an error occurs while processing an image the error is
+printed as a warning and processing continues with the next image.
+This provides protection primarily against mistyped or nonexistent images.
+.PP
+Before the first image is processed the calibration images are
+identified.  There are two ways to specify calibration images;
+explicitly via task parameters or implicitly as part of the list of
+images to be processed.  Explicitly identifying calibration images
+takes precedence over calibration images in the input list.  Specifying
+calibration images as part of the input image list requires that the
+image types can be determined from the image header.  Using the input
+list provides a mechanism for breaking processing up into sets of
+images (possibly using files containing the image names for each set)
+each having their own calibration images.  One can, of course,
+selectively specify input and calibration images, but whenever possible
+one would like to avoid having to specify explicit images to process
+since this requires record keeping by the user.
+.PP
+The first step in processing an image is to check that it is of the
+appropriate image type.  The user may select to process images of only
+one type.  Generally this is object images since calibration images are
+automatically processed as needed.  Images which are not of the desired
+type are skipped and the next image is considered.
+.PP
+A temporary output image is created next.  The output pixel datatype on
+disk may be changed at this point as selected by the user.
+For example it is common for the raw CCD images to be digitized as 16
+bit integers but after calibration it is sometimes desirable to have
+real format pixels.  If no output pixel datatype is specified the
+output image takes the same pixel datatype as the input image.  The
+processing is done by operating on the input image and writing the
+results to a temporary output image.  When the processing is complete
+the output image replaces the input image.  This gives the effect of
+processing the images in place but with certain safeguards.  If the
+computer crashes or the processing is interrupted the integrity of the
+input image is maintained.  The reasons for chosing to process the
+images in this way are to avoid having to generate new image names (a
+tiresome record keeping process for the user), to minimize disk
+usage, and generally the unprocessed images are not used once they have
+been processed.  When dealing with large volumes of data these reasons
+become fairly important.  However, the user may specify a backup prefix
+for the images in which case, once the processing is completed, the
+original input image is renamed by appending it to the prefix (or with
+an added digit if a previous backup image of the same name exits)
+before the processed output image takes the original input name.
+.PP
+The next step is to determine the image geometry.  Only a subsection of
+the raw image may contain the CCD data.  If this region is specified by
+a header parameter then the processing will affect only this region.
+This allows calibration and other data to be part of the image.
+Normally, the only other data in a image is overscan or prescan data.
+The location of this bias data is determined from the image header or
+from a task parameter (which overrides the image header value).  To
+relate calibration images of different sizes and to allow for readout
+of only a portion of the CCD detector, a header parameter may relate
+the image data coordinates to the full CCD coordinates.  Application of
+calibration image data and identifying bad pixel regions via a bad
+pixel file is done in this CCD coordinate system.  The final
+geometrical information is the region of the input image to be output
+after processing; an operation called trimming.  This is defined by an
+image header parameter or a task parameter.  Trimming of the image is
+selected by the user.  Any or all of this geometry information may be
+absent from the image and appropriate defaults are used.
+.PP
+Each selected operation which is appropriate for the image type is then
+considered.  If the operation has been performed previously it will not
+be repeated.  If all selected operations have been performed then the
+temporary output image is deleted and the input image is left
+unchanged.  The next image is then processed.
+.PP
+For each selected operation to be performed the pertinent data is
+determined.  This consists of such things as the name of the
+calibration image, scaling factors, the overscan bias function, etc.
+Note that at this point only the parameters are determined, the
+operation is not yet performed.  This is because operations are not
+performed sequentially but simultaneously as described below.  Consider
+flat fielding as an example.  First the input image is checked to see
+if it has been flat fielded.  Then the flat field calibration image is
+determined.  The flat field image is checked to see if it has been
+processed.  If it has not been processed then it is processed by
+calling a procedure which is essentially a copy of the main processing
+program.  After the flat field image has been processed, parameters
+affecting the processing, such as the flat field scale factor
+(essentially the mean of the flat field image), are determined.  A log
+of the operation is then printed if desired.
+.PP
+Once all the processing operations and parameters have been defined the
+actual processing begins.  One of the key design goals was that the
+processing be efficient.  There are two primary methods used to achieve
+this goal; separate processing paths for 16 bit integer data and
+floating point data and simultaneous operations.  If the image, the
+calibration images, and the output image (as selected by the user) are
+16 bit integer pixel datatypes then the image data is read and written
+as integer data.  This eliminates internal datatype conversions both
+during I/O and during computations.  However, many operations include
+use of real factors such as the overscan bias, dark count exposure
+scaling, and flat field scaling which causes the computation to be done
+in real arithmetic before the result is stored again as an integer
+value.  In any case there is never any loss of precision except when
+converting the output pixel to short integer.  If any of the images are
+not integer then a real internal data path is used in which input and
+output image data are converted to real as necessary.
+.PP
+For each data path the processing proceeds line-by-line.  For each line
+in the output image data region (ignoring pixels outside the data area
+and pixels which are trimmed) the appropriate input data and
+calibration data are obtained.  The calibration data is determined from
+the CCD coordinates of the output image and are not necessarily from
+the same image line or columns.  The input data is copied to the output
+array while applying bad pixel corrections and trimming.  The line is
+then processed using a specially optimized procedure.  This procedure
+applies all operations simultaneously for all combinations of
+operations.  As an example, consider subtracting an overscan bias,
+subtracting a zero level, and dividing by a flat field.  The basic
+kernel of the task, where the bulk of the CPU time is used, is
+
+.nf
+.ft L
+  do i = 1, n
+      out[i] = (out[i] - overscan - zero[i]) * flatscale / flat[i]
+.ft R
+.fi
+
+Here, \fIn\fR is the number of pixels in the line, \fIoverscan\fR is
+the overscan bias value for the line, \fIzero\fR is the zero level data
+from the zero level image, \fIflatscale\fR is the mean of the flat
+field image, and \fIflat\fR is the flat field data from the flat
+field image.  Note the operations are not applied sequentially but
+in a single statement.  This is the most efficient method and there is
+no need for intermediate images.
+.PP
+Though the processing is logically performed line-by-line in the program,
+the image I/O from the disk is not done this way.  The IRAF virtual
+operating system image interface automatically provides multi-line
+buffering for maximal I/O efficiency.
+.PP
+In many image processing systems it has been standard to apply operations
+sequentially over an image.  This requires producing intermediate images.
+Since this is clearly inefficient in terms of I/O it has been the practice
+to copy the images into main memory and operate upon them there until
+the final image is ready to be saved.  This has led to the perception
+that in order to be efficient an image processing system \fImust\fR
+store images in memory.  This is not true and the IRAF CCD reduction
+package illustrates this.  The CCD processing does not use intermediate
+images and does not need to keep the entire image in main memory.
+Furthermore, though of lesser importance than I/O, the single statement method
+illustrated above is more efficient than multiple passes through the
+images even when the images are kept in main memory.  Finally, as CCD
+detectors increase in size and small, fast, and cheap processors become
+common it is a distinct advantage to not require the large amounts of
+memory needed to keep entire images in memory.
+.PP
+There is one area in which use of main memory can improve performance
+and \fBccdproc\fR does take advantage of it if desired.  The calibration
+images usually are the same for many input images.  By specifying the
+maximum amount of memory available for storing images in memory
+the calibration images may be stored in memory up to that amount.
+By parameterizing the memory requirement there is no builtin dependence
+on large memory!
+.PP
+After processing the input image the last steps are to log the operations
+in the image header using processing keywords and replace the input
+image by the output image as described earlier.  The CCD coordinates
+of the data are recorded in the header, even if not there previously, to
+allow further processing on the image after the image has been trimmed.
+.NH
+Combining Images
+.PP
+The second important tool in the CCD reduction package is a task to combine
+many images into a single, higher quality image.  While this may also be
+done with more general image processing tools (the IRAF task \fBimsum\fR
+for example) the \fBccdred\fR tasks include special CCD dependent features such
+as recognizing the image types and using the image header translation
+file.  Combining images is often done
+with calibration images, which are easy to obtain in number, where it
+is important to minimize the statistical noise so as to not affect the
+object images.  Sometimes object images also are combined.
+The task is called \fBcombine\fR and there are special versions of
+this task called \fBzerocombine, darkcombine\fR, and \fBflatcombine\fR
+for the standard calibration images.
+.PP
+The task takes a list of input images to be combined.  As output there
+is the combined image, an optional sigma image, and optional log output either
+to the terminal, to a log file, or both.  A subset or subsets
+of the input images may be selected based on the image type and a
+subset parameter such as the filter.  As with the processing task,
+this allows selecting images without having to explicitly list each
+image from a large data set.  When combining based on a subset parameter
+there is an output image, and possibly a sigma image, for each separate subset.
+The output image pixel datatype may also be changed during combining;
+usually from 16 bit integer input to real output.
+The sigma image is the standard deviation of the input images about the
+output image.
+.PP
+Except for summing the images together,
+combining images may require correcting for variations between the images
+due to differing exposure times, sky background, extinctions, and
+positions.  Currently, extinction corrections and registration are
+not included but scaling and shifting corrections are included.
+The scaling corrections may be done by exposure times or by computing
+the mode in each image.  Additive shifting is also done by computing
+the mode in the images.  The region of the image in which the mode
+is computed can be specified but by default the whole image is used.
+A scaling correction is used when the flux level or sensitivity is varying.
+The offset correction is used when the sky brightness is varying independently
+of the object brightness.  If the images are not scaled then special
+data paths combine the images more efficiently.
+.PP
+Except for medianing and summing, the images are combined by averaging.
+The average may be weighted by
+
+.nf
+.ft L
+	weight = (N * scale / mode) ** 2
+.ft R
+.fi
+
+where \fIN\fR is the number of images previously combined (the task
+records the number of images combined in the image header), \fIscale\fR
+is the relative scale (applied by dividing) from the exposure time or
+mode, and \fImode\fR is the background mode estimate used when adding a
+variable offset.
+.PP
+The combining operation is the heart of the task.  There are a number
+algorithms which may be used as well as applying statistical weights.
+The algorithms are used to detect and reject deviant pixels, such as
+cosmic rays.
+The choice of algorithm depends on the data, the number of images,
+and the importance of rejecting cosmic rays.  The more complex the
+algorithm the more time consuming the operation.
+The list below summarizes the algorithms.
+Further algorithms may be added in time.
+
+.IP "Sum - sum the input images"
+.br
+The input images are combined by summing.  Care must be taken
+not to exceed the range of the 16 bit integer datatype when summing if the
+output datatype is of this type.  Summing is the only algorithm in which
+scaling and weighting are not used.  Also no sigma image is produced.
+.IP "Average - average the input images"
+.br
+The input images are combined by averaging.  The images may be scaled
+and weighted.  There is no pixel rejection.  A sigma image is produced
+if more than one image is combined.
+.IP "Median - median the input images"
+.br
+The input images are combined by medianing each pixel.  Unless the images
+are at the same exposure level they should be scaled.  The sigma image
+is based on all the input images and is only an approximation to the
+uncertainty in the median estimates.
+.IP "Minreject, maxreject, minmaxreject - reject extreme pixels"
+.br
+At each pixel the minimum, maximum, or both are excluded from the
+average.  The images should be scaled and the average may be
+weighted.  The sigma image requires at least two pixels after rejection
+of the extreme values.  These are relatively fast algorithms and are
+a good choice if there are many images (>15).
+.IP "Threshold - reject pixels above and below specified thresholds"
+.br
+The input images are combined with pixels above and below specified
+threshold values (before scaling) excluded.  The images may be scaled
+and the average weighted.  The sigma image also has the rejected
+pixels excluded.
+.IP "Sigclip - apply a sigma clipping algorithm to each pixel"
+.br
+The input images are combined by applying a sigma clipping algorithm
+at each pixel.  The images should be scaled.  This only rejects highly
+deviant points and so
+includes more of the data than the median or minimum and maximum 
+algorithms.  It requires many images (>10-15) to work effectively.
+Otherwise the bad pixels bias the sigma significantly.  The mean
+used to determine the sigmas is based on the "minmaxrej" algorithm
+to eliminate the effects of bad pixels on the mean.  Only one
+iteration is performed and at most one pixel is rejected at each
+point in the output image.  After the deviant pixels are rejected the final
+mean is computed from all the data.  The sigma image excludes the
+rejected pixels.
+.IP "Avsigclip - apply a sigma clipping algorithm to each pixel"
+.br
+The input images are combined with a variant of the sigma clipping
+algorithm which works well with only a few images.  The images should
+be scaled.  For each line the mean is first estimated using the
+"minmaxrej" algorithm.  The sigmas at each point in the line are scaled
+by the square root of the mean, that is a Poisson scaling of the noise
+is assumed.  These sigmas are averaged to get a line estimate of the
+sigma.  Then the sigma at each point in the line is estimated by
+multiplying the line sigma by the square root of the mean at that point.  As
+with the sigma clipping algorithm only one iteration is performed and
+at most one pixel is rejected at each point.  After the deviant pixels
+are rejected the file mean is computed from all the data.  The sigma
+image excludes the rejected pixels.
+.RE
+.PP
+The "avsigclip" algorithm is the best algorithm for rejecting cosmic
+rays, especially with a small number of images, but it is also the most
+time consuming.  With many images (>10-15) it might be advisable to use
+one of the other algorithms ("maxreject", "median", "minmaxrej") because
+of their greater speed.
+.PP
+This task also has several design features to make it efficient and
+versatile.  There are separate data paths for integer data and real
+data; as with processing, if all input images and the output image are
+of the same datatype then the I/O is done with no internal conversions.
+With mixed datatypes the operations are done as real.  Even in the
+integer path the operations requiring real arithmetic to preserve the
+accuracy of the calculation are performed in that mode.  There is
+effectively no limit to the number of images which may be combined.
+Also, the task determines the amount of memory available and buffers
+the I/O as much as possible.  This is a case where operating on images
+from disk rather than in memory is essential.
+.NH
+Status and Conclusion
+.PP
+The initial implementation of the IRAF \fBccdred\fR package was
+completed in June 1987.  It has been in use at the National Optical
+Astronomy Observatories since April 1987.  The package was not
+distributed with Version 2.5 of IRAF (released in August 1987) but is
+available as a separate installation upon request.  It will be part of
+future releases of IRAF.
+.PP
+At NOAO the CCD reduction package is available at the telescopes as the
+data is obtained.  This is accomplished by transferring the images from
+the data taking computer to a Sun workstation (Sun Microsystems, Inc.)
+initially via tape and later by a direct link.  There are several
+reasons for adopting this architecture.  First, the data acquisition
+system is well established and is dedicated to its real-time function.
+The second computer was phased in without disrupting the essential
+operation of the telescopes and if it fails data taking may continue
+with data being stored on tape.  The role of the second computer is to
+provide faster and more powerful reduction and analysis capability not
+required in a data acquisition system.  In the future it can be more
+easily updated to  follow the state of the art in small computers.  As
+CCD detectors get larger the higher processing speeds will be essential
+to keep up with the data flow.
+.PP
+By writing the reduction software in the high level, portable, IRAF
+system the users have the capability to process their data from the
+basic CCD reductions to a full analysis at the telescope.  Furthermore,
+the same software is widely available on a variety of computers if
+later processing or reprocessing is desired; staff and visitors at NOAO
+may also reduce their data at the headquarters facilities.  The use of
+a high level system was also essential in achieving the design goals;
+it would be difficult to duplicate this complex package without
+the rich programming environment provided by the IRAF system.
+.NH
+References
+.PP
+The following documentation is distributed by the National Optical
+Astronomy Observatories, Central Computer Services, P.O. Box 26732,
+Tucson, Arizona, 85726.  A comprehensive description of the IRAF system
+is given in \fIThe IRAF Data Reduction and Analysis System\fR by Doug
+Tody (also appearing in \fIProceedings of the SPIE - Instrumentation in
+Astronomy VI\fR, Vol. 627, 1986).  A general guide to using IRAF is \fIA
+User's Introduction to the IRAF Command Language\fR by Peter Shames
+and Doug Tody.  Both these documents are also part of the IRAF
+documentation distributed with the system.
+.PP
+A somewhat more tutorial description of the \fBccdred\fR package is
+\fIA User's Guide to the IRAF CCDRED Package\fR by the author.
+Detailed task descriptions and supplementary documentation are
+given in the on-line help library and are part of the user's guide.
+.NH
+Appendix
+.PP
+The current set of tasks making up the IRAF CCD Reduction Package,
+\fBccdred\fR, are summarized below.
+
+.nf
+.ft L
+  badpiximage - Create a bad pixel mask image from a bad pixel file
+    ccdgroups - Group CCD images into image lists
+     ccdhedit - CCD image header editor
+      ccdlist - List CCD processing information
+      ccdproc - Process CCD images
+      combine - Combine CCD images
+  darkcombine - Combine and process dark count images
+  flatcombine - Combine and process flat field images
+  mkfringecor - Make fringe correction images from sky images
+   mkillumcor - Make flat field illumination correction images
+  mkillumflat - Make illumination corrected flat fields
+     mkskycor - Make sky illumination correction images
+    mkskyflat - Make sky corrected flat field images
+setinstrument - Set instrument parameters
+  zerocombine - Combine and process zero level images
+.fi
+.ft R
diff --git a/noao/imred/ccdred/doc/ccdtypes.hlp b/noao/imred/ccdred/doc/ccdtypes.hlp
new file mode 100644
index 00000000..2cec33ea
--- /dev/null
+++ b/noao/imred/ccdred/doc/ccdtypes.hlp
@@ -0,0 +1,124 @@
+.help ccdtypes Jun87 noao.imred.ccdred
+.ih
+NAME
+ccdtypes -- Description of the CCD image types
+.ih
+CCDTYPES
+The following CCD image types may be specified as the value of the parameter
+\fIccdtype\fR:
+
+.nf
+	""	- (the null string) all image types
+	object	- object images
+	zero	- zero level images such as a bias or preflash
+	dark	- dark count images
+	flat	- flat field images
+	illum	- iillumination images
+	fringe	- fringe correction images
+	other   - other image types defined in the translation file
+	none	- images without an image type parameter
+	unknown - image types not defined in the translation file
+.fi
+.ih
+DESCRIPTION
+The \fBccdred\fR package recognizes certain standard CCD image types
+identified in the image header.  The tasks may select images of a
+particular CCD image type from image lists with the parameter
+\fIccdtype\fR and also recognize and take special actions for
+calibration images.
+
+In order to make use of CCD image type information the header keyword
+identifying the image type must be specified in the instrument
+translation file.  This entry has the form
+
+	imagetyp keyword
+
+where keyword is the image header keyword.  This allows the package to
+access the image type string.  There must also be a translation between
+the image type strings and the CCD types as recognized by the package.
+This information consists of lines in the instrument translation file
+of the form
+
+	header	package
+
+where header is the exact string given in the image header and package
+is one of the types recognized by the package.  The image header string
+can be virtually anything and if it contains blanks it must be
+quoted.  The package image types are those given above except for
+the null string, "none", and "unknown".  That is, these types may
+be specified as a CCD image type in selecting images but not as a translations
+of image type strings.
+
+There may be more than one image type that maps to the same package
+type.  In particular other standard CCD image types, such as comparison
+spectra, multiple exposure, standard star, etc., should be mapped to
+object or other.  There may also be more than one type of flat field, i.e. dome
+flat, sky flat, and lamp flat.  For more on the instrument translation
+file see the help for \fBinstruments\fR.
+.ih
+EXAMPLES
+1. The example entries in the instrument translation file are from the 1986
+NOAO CCD image header format produced by the CAMERA format tape writer.
+
+.nf
+    imagetyp			data-typ
+
+    'OBJECT (0)'		object
+    'DARK (1)'			dark
+    'PROJECTOR FLAT (2)'	flat
+    'SKY FLAT (3)'		other
+    'COMPARISON LAMP (4)'	other
+    'BIAS (5)'			zero
+    'DOME FLAT (6)'		flat
+.fi
+
+The image header keyword describing the image type is "data-typ".
+The values of the image type strings in the header contain blanks so they
+are quoted.  Also the case of the strings is important.  Note that there
+are two types of flat field images and two types of other images.
+
+2. One way to check the image types is with the task \fBccdlist\fR.
+
+.nf
+    cl> ccdlist *.imh
+    Zero.imh[504,1][real][zero][1][OT]:FOCUS L98-193
+    Flat1.imh[504,1][real][flat][1][OTZ]:dflat 6v+blue 5s
+    ccd002.imh[504,504][real][unknown][1][OTZF]:FOCUS L98-193
+    ccd003.imh[544,512][short][object][1]:L98-193
+    ccd004.imh[544,512][short][object][1]:L98-193
+    ccd005.imh[544,512][short][object][1]:L98-193
+    oldformat.imh[544,512][short][none][1]:M31 V
+.fi
+
+The unknown type has a header image type of "MUL (8)".  The old format
+image does not have any header type.
+
+3. To select only images of a particular type:
+
+.nf
+    cl> ccdlist *.imh ccdtype=object
+    ccd003.imh[544,512][short][object][1]:L98-193
+    ccd004.imh[544,512][short][object][1]:L98-193
+    ccd005.imh[544,512][short][object][1]:L98-193
+    cl> ccdlist *.imh ccdtype=unknown
+    ccd002.imh[504,504][real][unknown][1][OTZF]:FOCUS L98-193
+    cl> ccdlist *.imh ccdtype=none
+    oldformat.imh[544,512][short][none][1]:M31 V
+.fi
+
+4. To process images with \fBccdproc\fR:
+
+.nf
+    cl> ccdproc *.imh
+    cl> ccdproc *.imh ccdtype=object
+.fi
+
+In the first case all the images will be processed (the default value of
+\fIccdtype\fR is "").  However, the task recognizes the calibration
+images, such as zero level and flat fields, and processes them appropriately.
+In the second case only object images are processed and all other images
+are ignored (except if needed as a calibration image).
+.ih
+SEE ALSO
+instruments
+.endhelp
diff --git a/noao/imred/ccdred/doc/combine.hlp b/noao/imred/ccdred/doc/combine.hlp
new file mode 100644
index 00000000..474937bf
--- /dev/null
+++ b/noao/imred/ccdred/doc/combine.hlp
@@ -0,0 +1,1146 @@
+.help combine Aug96 noao.imred.ccdred
+.ih
+NAME
+combine -- Combine CCD images using various algorithms
+.ih
+USAGE	
+combine input output
+.ih
+PARAMETERS
+.ls input
+List of CCD images to combine.  Images of a particular CCD image type may be
+selected with the parameter \fIccdtype\fR with the remaining images ignored.
+.le
+.ls output
+Output combined image or list of images.  If the \fIproject\fR parameter is
+no (the typical case for CCD acquisition) then there will be one output
+image or, if the \fIsubsets\fR parameter is selected, one
+output image per subset.  If the images consist of stacks then
+the \fIproject\fR option allows combining each input stack into separate
+output images as given by the image list.
+.le
+.ls plfile = "" (optional)
+Output pixel list file or list of files.  If no name is given or the
+list ends prematurely then no file is produced.  The pixel list file
+is a map of the number of pixels rejected or, equivalently,
+the total number of input images minus the number of pixels actually used.
+The file name is also added to the output image header under the
+keyword BPM.
+.le
+.ls sigma = "" (optional)
+Output sigma image or list of images.  If no name is given or the list ends
+prematurely then no image is produced.  The sigma is standard deviation,
+corrected for a finite population, of the input pixel values (excluding
+rejected pixels) about the output combined pixel values.
+.le
+
+.ls ccdtype = ""
+CCD image type to combine.  If specified only input images of the specified
+type are combined.  See \fBccdtypes\fR for the possible image types.
+.le
+.ls amps = yes
+Combine images by amplifier?  If yes then the input images are grouped by
+the amplifier parameter and each group combined into a separate output
+image.  The amplifier identifier is appended to the output image name(s).
+See \fBsubsets\fR for more on the amplifier parameter.
+.le
+.ls subsets = no
+Combine images by subset parameter?  If yes then the input images are
+grouped by subset parameter and each group combined into a separate output
+image.  The subset identifier is appended to the output image
+name(s).  See \fBsubsets\fR for more on the subset parameter.
+.le
+.ls delete = no
+Delete input images after combining?  Only those images combined are deleted.
+.le
+.ls clobber = no
+Clobber existing output images?  THIS OPTION IS NO LONGER SUPPORTED BUT
+THE PARAMETER REMAINS FOR NOW FOR BACKWARD COMPATIBILITY.  IF SET TO
+yes AN ERROR ABORT WILL OCCUR.
+.le
+
+.ls combine = "average" (average|median)
+Type of combining operation performed on the final set of pixels (after
+offsetting, masking, thresholding, and rejection).  The choices are
+"average" or "median".  The median uses the average of the two central
+values when the number of pixels is even.
+.le
+.ls reject = "none" (none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip)
+Type of rejection operation performed on the pixels remaining after offsetting,
+masking and thresholding.  The algorithms are discussed in the
+DESCRIPTION section.  The rejection choices are:
+
+.nf
+      none - No rejection
+    minmax - Reject the nlow and nhigh pixels
+   ccdclip - Reject pixels using CCD noise parameters
+  crreject - Reject only positive pixels using CCD noise parameters
+   sigclip - Reject pixels using a sigma clipping algorithm
+ avsigclip - Reject pixels using an averaged sigma clipping algorithm
+     pclip - Reject pixels using sigma based on percentiles
+.fi
+
+.le
+.ls project = no
+Project (combine) across the highest dimension of the input images?  If
+no then all  the input images are combined to a single output image.  If
+yes then the highest dimension elements of each input image are combined to
+an output image and optional pixel list and sigma images.  Each element of
+the highest dimension may have a separate offset but there can only be one
+mask image.
+.le
+.ls outtype = "real" (short|ushort|integer|long|real|double)
+Output image pixel datatype.  The pixel datatypes are "double", "real",
+"long", "integer", unsigned short ("ushort") and "short" with highest
+precedence first.  If none is specified then the highest precedence
+datatype of the input images is used.   A mixture of short and unsigned
+short images has a highest precedence of integer.
+The datatypes may be abbreviated to
+a single character.
+.le
+.ls offsets = "none" (none|wcs|grid|<filename>)
+Integer offsets to add to each image axes.  The options are:
+.ls "none"
+No offsets are applied.
+.le
+.ls "wcs"
+The world coordinate system (wcs) in the image is used to derive the
+offsets.  The nearest integer offset that matches the world coordinate
+at the center of the first input image is used.
+.le
+.ls "grid"
+A uniform grid of offsets is specified by a string of the form
+
+.nf
+	grid [n1] [s1] [n2] [s2] ...
+.fi
+
+where ni is the number of images in dimension i and si is the step
+in dimension i.  For example "grid 5 100 5 100" specifies a 5x5
+grid with origins offset by 100 pixels.
+.le
+.ls <filename>
+The offsets are given in the specified file.  The file consists
+of one line per image with the offsets in each dimension forming the
+columns.
+.le
+.le
+.ls masktype = "none" (none|goodvalue|badvalue|goodbits|badbits)
+Type of pixel masking to use.  If "none" then no pixel masking is done
+even if an image has an associated  pixel mask.  The other choices
+are to select the value in the pixel mask to be treated as good
+(goodvalue) or bad (badvalue) or the bits (specified as a value)
+to be treated as good (goodbits) or bad (badbits).  The pixel mask
+file name comes from the image header keyword BPM.
+Note that when
+combining images by projection of the highest dimension only one
+pixel mask is applied to all the images.  \fBAlso if the number of
+input images becomes too large (currently about 115 .imh or 57 .hhh
+images) then the images are temporarily stacked and combined by projection
+which also means the bad pixel mask from the first image will be used
+for all images.\fR
+.le
+.ls maskvalue = 0
+Mask value used with the \fImasktype\fR parameter.  If the mask type
+selects good or bad bits the value may be specified using IRAF notation
+for decimal, octal, or hexadecimal; i.e 12, 14b, 0cx to select bits 3
+and 4.
+.le
+.ls blank = 0.
+Output value to be used when there are no pixels.
+.le
+
+.ls scale = "none" (none|mode|median|mean|exposure|@<file>|!<keyword>)
+Multiplicative image scaling to be applied.  The choices are none, scale
+by the mode, median, or mean of the specified statistics section, scale
+by the exposure time in the image header, scale by the values in a specified
+file, or scale by a specified image header keyword.  When specified in
+a file the scales must be one per line in the order of the input
+images.
+.le
+.ls zero = "none" (none|mode|median|mean|@<file>|!<keyword>)
+Additive zero level image shifts to be applied.  The choices are none or
+shift by the mode, median, or mean of the specified statistics section,
+shift by values given in a file, or shift by values given by an image
+header keyword.  When specified in a file the zero values must be one
+per line in the order of the input images.  File or keyword zero offset
+values do not allow a correction to the weights.
+.le
+.ls weight = "none" (none|mode|median|mean|exposure|@<file>|!<keyword>)
+Weights to be applied during the final averaging.  The choices are none,
+the mode, median, or mean of the specified statistics section, the exposure
+time, values given in a file, or values given by an image header keyword.
+When specified in a file the weights must be one per line in the order of
+the input images and the only adjustment made by the task is for the number of
+images previously combined.   In this case the weights should be those
+appropriate for the scaled images which would normally be the inverse
+of the variance in the scaled image.
+.le
+.ls statsec = ""
+Section of images to use in computing image statistics for scaling and
+weighting.  If no section is given then the entire region of the input is
+sampled (for efficiency the images are sampled if they are big enough).
+When the images are offset relative to each other one can precede the image
+section with one of the modifiers "input", "output", "overlap".  The first
+interprets the section relative to the input image (which is equivalent to
+not specifying a modifier), the second interprets the section relative to
+the output image, and the last selects the common overlap and any following
+section is ignored.
+.le
+
+.ce
+Algorithm Parameters
+.ls lthreshold = INDEF, hthreshold = INDEF
+Low and high thresholds to be applied to the input pixels.  This is done
+before any scaling, rejection, and combining.  If INDEF the thresholds
+are not used.
+.le
+.ls nlow = 1,  nhigh = 1 (minmax)
+The number of low and high pixels to be rejected by the "minmax" algorithm.
+These numbers are converted to fractions of the total number of input images
+so that if no rejections have taken place the specified number of pixels
+are rejected while if pixels have been rejected by masking, thresholding,
+or nonoverlap, then the fraction of the remaining pixels, truncated
+to an integer, is used.
+.le
+.ls nkeep = 1
+The minimum number of pixels to retain or the maximum number to reject when
+using the clipping algorithms (ccdclip, crreject, sigclip, avsigclip, or
+pclip).  When given as a positive value this is the minimum number to
+keep.  When given as a negative value the absolute value is the maximum
+number to reject.  If there are fewer pixels at some point due to
+offsetting, thresholding, or masking then if the number to keep (positive
+nkeep) is greater than the number of pixels no pixels will be rejected and
+if the number to reject is given (negative nkeep) then up to that number
+may be rejected.
+.le
+.ls mclip = yes (ccdclip, crreject, sigclip, avsigcliip)
+Use the median as the estimate for the true intensity rather than the
+average with high and low values excluded in the "ccdclip", "crreject",
+"sigclip", and "avsigclip" algorithms?  The median is a better estimator
+in the presence of data which one wants to reject than the average.
+However, computing the median is slower than the average.
+.le
+.ls lsigma = 3., hsigma = 3. (ccdclip, crreject, sigclip, avsigclip, pclip)
+Low and high sigma clipping factors for the "ccdclip", "crreject", "sigclip",
+"avsigclip", and "pclip" algorithms.  They multiply a "sigma" factor
+produced by the algorithm to select a point below and above the average or
+median value for rejecting pixels.  The lower sigma is ignored for the
+"crreject" algorithm.
+.le
+.ls rdnoise = "0.", gain = "1.", snoise = "0." (ccdclip, crreject)
+CCD readout noise in electrons, gain in electrons/DN, and sensitivity noise
+as a fraction.  These parameters are used with the "ccdclip" and "crreject"
+algorithms.  The values may be either numeric or an image header keyword
+which contains the value.  The noise model for a pixel is:
+
+.nf
+    variance in DN = (rdnoise/gain)^2 + DN/gain + (snoise*DN)^2
+    variance in e- = (rdnoise)^2 + (gain*DN) + (snoise*(gain*DN))^2
+		   = rdnoise^2 + Ne + (snoise * Ne)^2
+.fi
+
+where DN is the data number and Ne is the number of electrons.  Sensitivity
+noise typically comes from noise introduced during flat fielding.
+.le
+.ls sigscale = 0.1 (ccdclip, crreject, sigclip, avsigclip)
+This parameter determines when poisson corrections are made to the
+computation of a sigma for images with different scale factors.  If all
+relative scales are within this value of unity and all relative zero level
+offsets are within this fraction of the mean then no correction is made.
+The idea is that if the images are all similarly though not identically
+scaled, the extra computations involved in making poisson corrections for
+variations in the sigmas can be skipped.  A value of zero will apply the
+corrections except in the case of equal images and a large value can be
+used if the sigmas of pixels in the images are independent of scale and
+zero level.
+.le
+.ls pclip = -0.5 (pclip)
+Percentile clipping algorithm parameter.  If greater than
+one in absolute value then it specifies a number of pixels above or
+below the median to use for computing the clipping sigma.  If less
+than one in absolute value then it specifies the fraction of the pixels
+above or below the median to use.  A positive value selects a point
+above the median and a negative value selects a point below the median.
+The default of -0.5 selects approximately the quartile point.
+See the DESCRIPTION section for further details.
+.le
+.ls grow = 0
+Number of pixels to either side of a rejected pixel along image lines
+to also be rejected.  This applies only to pixels rejected by one of
+the rejection algorithms and not the masked or threshold rejected pixels.
+.le
+
+PACKAGE PARAMETERS
+
+The package parameters are used to specify verbose and log output and the
+instrument and header definitions.
+.ih
+DESCRIPTION
+A set of CCD images are combined by weighted averaging or medianing.  Pixels
+may be rejected from the combining by using pixel masks, threshold levels,
+and rejection algorithms.  The images may be scaled multiplicatively or
+additively based on image statistics, image header keywords, or text files
+before rejection.  The images may be combined with integer pixel coordinate
+offsets to produce an image bigger than any of the input images.
+This task is a variant of the \fBimages.imcombine\fR task specialized
+for CCD images.
+
+The input images to be combined are specified by a list.  A subset or
+subsets of the input list may be selected using the parameters
+\fIccdtype\fR and \fIsubsets\fR.  The \fIccdtype\fR parameter
+selects only images of a specified standard CCD image type.
+The \fIsubsets\fR parameter breaks up the input
+list into sublists of common subset parameter (filter, grating, etc.).  For
+more information see \fBccdtypes\fR and \fBsubsets\fR.  This selection
+process is useful with wildcard templates to combine, for example, the flat
+field images for each filter in one step (see \fBflatcombine\fR).  When
+subsets of the input list are used the output image and optional pixel file
+and sigma image are given by root names with an amplifier and subset
+identifier appended by the task.
+
+If the \fBproject\fR parameter is yes then the highest dimension elements
+of each input image are combined to make an output image of one lower
+dimension.  There is no limit to the number of elements combined in this
+case.  This case is If the \fBproject\fR is no then the entire input list
+is combined to form a single output image per subset.   In this case the
+images must all have the same dimensionality but they may have different
+sizes.  There is a software limit of approximately 100 images in this
+case.
+
+The output image header is a copy of the first image in the combined set.
+In addition, the number of  images combined is recorded under the keyword
+NCOMBINE, the exposure time is updated as the weighted average of the input
+exposure times, and any pixel list file created is recorded under the
+keyword BPM.  The output pixel type is set by the parameter \fIouttype\fR.
+If left blank then the input datatype of highest precision is used.
+A mixture of short and unsigned short images has a highest precision of
+integer.
+
+In addition to one or more output combined images there may also be a pixel
+list image containing the number of pixels rejected at each point in the
+output image, an image containing the sigmas of the pixels combined about
+the final output combined pixels, and a log file.  The pixel list image is
+in the compact pixel list format which can be used as an image in other
+programs.  The sigma computation is the standard deviation corrected for a
+finite population (the n/(n-1) factor) including weights if a weighted
+average is used.
+
+Other input/output parameters are \fIdelete\fR and \fIclobber\fR.  The
+\fIdelete\fR parameter may be set to "yes" to delete the input images
+used in producing an output image after it has been created.  This is
+useful for minimizing disk space, particularly with large
+sets of calibration images needed to achieve high statistical accuracy
+in the final calibration image.  The \fBclobber\fR parameter allows
+the output image names to be existing images which are overwritten (at
+the end of the operation).
+
+An outline of the steps taken by the program is given below and the
+following sections elaborate on the steps.
+
+.nf
+o   Set the input image offsets and the final output image size.
+o   Set the input image scales and weights
+o   Write the log file output
+.fi
+
+For each output image line:
+
+.nf
+o   Get input image lines that overlap the output image line
+o   Reject masked pixels
+o   Reject pixels outside the threshold limits
+o   Reject pixels using the specified algorithm
+o   Reject neighboring pixels along each line
+o   Combine remaining pixels using the weighted average or median
+o   Compute sigmas of remaining pixels about the combined values
+o   Write the output image line, rejected pixel list, and sigmas
+.fi
+
+
+OFFSETS
+
+The images to be combined need not be of the same size or overlap.  They
+do have to have the same dimensionality which will also be the dimensionality
+of the output image.  Any dimensional images supported by IRAF may be
+used.  Note that if the \fIproject\fR flag is yes then the input images
+are the elements of the highest dimension; for example the planes of a
+three dimensional image.
+
+The overlap of the images is determined by a set of integer pixel offsets
+with an offset for each dimension of each input image.  For example
+offsets of 0, 10, and 20 in the first dimension of three images will
+result in combining the three images with only the first image in the
+first 10 colums, the first two images in the next 10 columns and
+all three images starting in the 31st column.  At the 31st output column
+the 31st column of the first image will be combined with the 21st column
+of the second image and the 1st column of the third image.
+
+The output image size is set by the maximum extent in each dimension
+of any input image after applying the offsets.  In the above example if
+all the images have 100 columns then the output image will have 130
+columns corresponding to the 30 column offset in the third image.
+
+The input image offsets are set using the \fIoffset\fR parameter.  There
+are four ways to specify the offsets.  If the word "none" or the empty
+string "" are used then all offsets will be zero and all pixels with the
+same coordinates will be combined.  The output image size will be equal to
+the biggest dimensions of the input images.
+
+If "wcs" offsets are specified then the world coordinate systems (wcs)
+in the image headers are used to derived the offsets.  The world coordinate
+at the center of the first input image is evaluated.  Then integer pixel
+offsets are determined for each image to bring the same world coordinate
+to the same point.  Note the following caveats.  The world coordinate
+systems must be of the same type, orientation, and scale and only the
+nearest integer shift is used.
+
+If the input images have offsets in a regular grid or one wants to make
+an output image in which the input images are "mosaiced" together in
+a grid then the special offset string  beginning with the word "grid"
+is used.  The format is
+
+.nf
+	grid [n1] [s1] [n2] [s2] ...
+.fi
+
+where ni is the number of images in dimension i and si is the step in
+dimension i.  For example "grid 5 100 5 100" specifies a 5x5 grid with
+origins offset by 100 pixels.  Note that one must insure that the input
+images are specified in the correct order.  This may best be accomplished
+using a "@" list.  One useful application of the grid is to make a
+nonoverlapping mosaic of a number of images for display purposes.  Suppose
+there are 16 images which are 100x100.  The offset string "grid 4 101 4
+101" will produce a mosaic with a one pixel border having the value set
+by \fIblank\fR parameter between the images.
+
+The offsets may be defined in a file by specifying the file name
+in the \fIoffset\fR parameter.  (Note that the special file name STDIN
+may be used to type in the values terminated by the end-of-file
+character).  The file consists of a line for each input image.  The lines
+must be in the same order as the input images and so an "@" list may
+be useful.  The lines consist of whitespace separated offsets one for
+each dimension of the images.  In the first example cited above the
+offset file might contain:
+
+.nf
+	0 0
+	10 0
+	20 0
+.fi
+
+where we assume the second dimension has zero offsets.
+
+The offsets need not have zero for one of the images.  The offsets may
+include negative values or refer to some arbitrary common point.
+When the offsets are read by the program it will find the minimum
+value in each dimension and subtract it from all the other offsets
+in that dimension.  The above example could also be specified as:
+
+.nf
+	225 15
+	235 15
+	245 15
+.fi
+
+There may be cases where one doesn't want the minimum offsets reset
+to zero.  If all the offsets are positive and the comment "# Absolute"
+appears in the offset file then the images will be combined with
+blank values between the first output pixel and the first overlapping
+input pixel.  Continuing with the above example, the file
+
+.nf
+	# Absolute
+	10 10
+	20 10
+	30 10
+.fi
+
+will have the first pixel of the first image in the 11th pixel of the
+output image.  Note that there is no way to "pad" the other side of
+the output image.
+
+
+SCALES AND WEIGHTS
+
+In order to combine images with rejection of pixels based on deviations
+from some average or median they must be scaled to a common level.  There
+are two types of scaling available, a multiplicative intensity scale and an
+additive zero point shift.  The intensity scaling is defined by the
+\fIscale\fR parameter and the zero point shift by the \fIzero\fR
+parameter.  These parameters may take the values "none" for no scaling,
+"mode", "median", or "mean" to scale by statistics of the image pixels,
+"exposure" (for intensity scaling only) to scale by the exposure time
+keyword in the image header, any other image header keyword specified by
+the keyword name prefixed by the character '!', and the name of a file
+containing the scale factors for the input image prefixed by the
+character '@'.
+
+Examples of the possible parameter values are shown below where
+"myval" is the name of an image header keyword and "scales.dat" is
+a text file containing a list of scale factors.
+
+.nf
+	scale = none		No scaling
+	zero = mean		Intensity offset by the mean
+	scale = exposure	Scale by the exposure time
+	zero = !myval		Intensity offset by an image keyword
+	scale = @scales.dat	Scales specified in a file
+.fi
+
+The image statistics factors are computed by sampling a uniform grid
+of points with the smallest grid step that yields less than 10000
+pixels; sampling is used to reduce the time need to compute the statistics.
+If one wants to restrict the sampling to a region of the image the
+\fIstatsec\fR parameter is used.  This parameter has the following
+syntax:
+
+.nf
+	[input|output|overlap] [image section]
+.fi
+
+The initial modifier defaults to "input" if absent.  The modifiers are useful
+if the input images have offsets.  In that case "input" specifies
+that the image section refers to each input image, "output" specifies
+that the image section refers to the output image coordinates, and
+"overlap" specifies the mutually overlapping region of the input images.
+In the latter case an image section is ignored.
+
+The statistics are as indicated by their names.  In particular, the
+mode is a true mode using a bin size which is a fraction of the
+range of the pixels and is not based on a relationship between the
+mode, median, and mean.  Also masked pixels are excluded from the
+computations as well as during the rejection and combining operations.
+
+The "exposure" option in the intensity scaling uses the exposure time
+from the image header.  If one wants to use a nonexposure time image
+header keyword the !<keyword> syntax is available.
+
+If both an intensity scaling and zero point shift are selected the
+multiplicative scaling is done first.  Use of both makes sense
+if the intensity scaling is the exposure time to correct for
+different exposure times and then the zero point shift allows for
+sky brightness changes.
+
+The image statistics and scale factors are recorded in the log file
+unless they are all equal, which is equivalent to no scaling.  The
+intensity scale factors are normalized to a unit mean and the zero
+point shifts are adjust to a zero mean.  When the factors are specified
+in an @file or by a keyword they are not normalized.
+
+Scaling affects not only the mean values between images but also the
+relative pixel uncertainties.  For example scaling an image by a
+factor of 0.5 will reduce the effective noise sigma of the image
+at each pixel by the square root of 0.5.  Changes in the zero
+point also changes the noise sigma if the image noise characteristics
+are Poissonian.  In the various rejection algorithms based on
+identifying a noise sigma and clipping large deviations relative to
+the scaled median or mean, one may need to account for the scaling induced
+changes in the image noise characteristics.
+
+In those algorithms it is possible to eliminate the "sigma correction"
+while still using scaling.  The reasons this might be desirable are 1) if
+the scalings are similar the corrections in computing the mean or median
+are important but the sigma corrections may not be important and 2) the
+image statistics may not be Poissonian, either inherently or because the
+images have been processed in some way that changes the statistics.  In the
+first case because computing square roots and making corrections to every
+pixel during the iterative rejection operation may be a significant
+computational speed limit the parameter \fIsigscale\fR selects how
+dissimilar the scalings must be to require the sigma corrections.  This
+parameter is a fractional deviation which, since the scale factors are
+normalized to unity, is the actual minimum deviation in the scale factors.
+For the zero point shifts the shifts are normalized by the mean shift
+before adjusting the shifts to a zero mean.  To always use sigma scaling
+corrections the parameter is set to zero and to eliminate the correction in
+all cases it is set to a very large number.
+
+If the final combining operation is "average" then the images may be
+weighted during the averaging.  The weights are specified in the
+same way as the scale factors.  In addition
+the NCOMBINE keyword, if present, will be used in the weights.
+The weights, scaled to a unit sum, are printed in the log output.
+
+The weights are only used for the final weighted average and sigma image
+output.  They are not used to form averages in the various rejection
+algorithms.  For weights in the case of no scaling or only multiplicative
+scaling the weights are used as given or determined so that images with
+lower signal levels will have lower weights.  However, for cases in which
+zero level scaling is used and the zero levels are determined from image
+statistics (not from an input file or keyword) the weights are computed
+from the initial weights (the exposure time, image statistics, or input
+values) using the formula:
+
+.nf
+	weight_final = weight_initial / (scale * sky)
+.fi
+
+where the sky values are those from the image statistics before conversion
+to zero level shifts and adjustment to zero mean over all images.  The
+reasoning is that if the zero level is high the sky brightness is high and
+so the S/N is lower and the weight should be lower.  If any sky value
+determined from the image  statistics comes out to be negative a warning is
+given and the none of the weight are adjusted for sky levels.
+
+The weights are not adjusted when the zero offsets are input from a file
+or keyword since these values do not imply the actual image sky value.
+In this case if one wants to account for different sky statistics
+in the weights the user must specify the weights in a file taking
+explicit account of changes in the weights due to different sky
+statistics.
+
+
+PIXEL MASKS
+
+A pixel mask is a type of IRAF file having the extension ".pl" which
+identifies an integer value with each pixel of the images to which it is
+applied.  The integer values may denote regions, a weight, a good or bad
+flag, or some other type of integer or integer bit flag.  In the common
+case where many values are the same this file is compacted to be small and
+efficient to use.  It is also most compact and efficient if the majority of
+the pixels have a zero mask value so frequently zero is the value for good
+pixels.  Note that these files, while not stored as a strict pixel array,
+may be treated as images in programs.  This means they may be created by
+programs such as \fBmkpattern\fR, edited by \fBimedit\fR, examined by
+\fBimexamine\fR, operated upon by \fBimarith\fR, graphed by \fBimplot\fR,
+and displayed by \fBdisplay\fR.
+
+At the time of introducing this task, generic tools for creating
+pixel masks have yet to be written.  There are two ways to create a
+mask in V2.10.  First if a regular integer image can be created
+then it can be converted to pixel list format with \fBimcopy\fR:
+
+.nf
+	cl> imcopy template plfile.pl
+.fi
+
+by specifically using the .pl extension on output.  Other programs that
+can create integer images (such \fBmkpattern\fR or \fBccdred.badpiximage\fR)
+can create the pixel list file directly by simply using the ".pl"
+extension in the output image name.
+
+To use pixel masks with \fBcombine\fR one must associate a pixel
+mask file with an image by entering the pixel list file name in the
+image header under the keyword BPM (bad pixel mask).  This can be
+done with \fBhedit\fR.  Note that the same pixel mask may be associated
+with more than one image as might be the case if the mask represents
+defects in the detector used to obtain the images.
+
+If a pixel mask is associated with an image the mask is used when the
+\fImasktype\fR parameter is set to a value other than "none".  Note that
+when it is set to "none" mask information is not used even if it exists for
+the image.  The values of \fImasktype\fR which apply masks are "goodvalue",
+"badvalue", "goodbits", and "badbits".  They are used in conjunction with
+the \fImaskvalue\fR parameter.  When the mask type is "goodvalue" the
+pixels with mask values matching the specified value are included in
+combining and all others are rejected.  Similarly, for a mask type of
+"badvalue" the pixels with mask values matching the specified value are
+rejected and all others are accepted.  The bit types are useful for
+selecting a combination of attributes in a mask consisting of bit flags.
+The mask value is still an integer but is interpreted by bitwise comparison
+with the values in the mask file.
+
+If a mask operation is specified and an image has no mask image associated
+with it then the mask values are taken as all zeros.  In those cases be
+careful that zero is an accepted value otherwise the entire image will be
+rejected.
+
+In the case of combining the higher dimensions of an image into a
+lower dimensional image, the "project" option, the same pixel mask
+is applied to all of the data being combined; i.e. the same 2D
+pixel mask is applied to every plane of a 3D image.  This is because
+a higher dimensional image is treated as a collection of lower
+dimensional images having the same header and hence the same
+bad pixel mask.  It would be tempting to use a bad pixel mask with
+the same dimension as the image being projected but this is not
+currently how the task works.
+
+When the number of input images exceeds the maximum number of open files
+allowed by IRAF (currently about 115 .imh or 57 .hhh images) the input
+images are stacked and combined with the project option.  \fBThis means
+that the bad pixel mask from the first input image will be applied to all
+the images.\fR
+
+
+THRESHOLD REJECTION
+
+In addition to rejecting masked pixels, pixels in the unscaled input
+images which are below or above the thresholds given by the parameters
+\fIlthreshold\fR and \fIhthreshold\fR are rejected.  Values of INDEF
+mean that no threshold value is applied.  Threshold rejection may be used
+to exclude very bad pixel values or as an alternative way of masking
+images.  In the latter case one can use a task like \fBimedit\fR
+or \fBimreplace\fR to set parts of the images to be excluded to some
+very low or high magic value.
+
+
+REJECTION ALGORITHMS
+
+The \fIreject\fR parameter selects a type of rejection operation to
+be applied to pixels not masked or thresholded.  If no rejection
+operation is desired the value "none" is specified.
+
+MINMAX
+.in 4
+A specified fraction of the highest and lowest pixels are rejected.
+The fraction is specified as the number of high and low pixels, the
+\fInhigh\fR and \fInlow\fR parameters, when data from all the input images
+are used.  If pixels have been rejected by offseting, masking, or
+thresholding then a matching fraction of the remaining pixels, truncated
+to an integer, are used.  Thus,
+
+.nf
+	nl = n * nlow/nimages + 0.001 
+	nh = n * nhigh/nimages + 0.001 
+.fi
+
+where n is the number of pixels surviving offseting, masking, and
+thresholding, nimages is the number of input images, nlow and nhigh
+are task parameters and nl and nh are the final number of low and
+high pixels rejected by the algorithm.  The factor of 0.001 is to
+adjust for rounding of the ratio.
+
+As an example with 10 input images and specifying one low and two high
+pixels to be rejected the fractions to be rejected are nlow=0.1 and nhigh=0.2
+and the number rejected as a function of n is:
+
+.nf
+	 n   0  1  2  3  4  5  6  7  8  9 10
+	 nl  0  0  0  0  0  0  0  0  0  0  1
+	 nh  0  0  0  0  0  1  1  1  1  1  2
+.fi
+
+.in -4
+CCDCLIP
+.in 4
+If the images are obtained using a CCD with known read out noise, gain, and
+sensitivity noise parameters and they have been processed to preserve the
+relation between data values and photons or electrons then the noise
+characteristics of the images are well defined.  In this model the sigma in
+data values at a pixel with true value <I>, as approximated by the median
+or average with the lowest and highest value excluded, is given by:
+
+.nf
+	sigma = ((rn / g) ** 2 + <I> / g + (s * <I>) ** 2) ** 1/2
+.fi
+
+where rn is the read out noise in electrons, g is the gain in
+electrons per data value, s is a sensitivity noise given as a fraction,
+and ** is the exponentiation operator.  Often the sensitivity noise,
+due to uncertainties in the pixel sensitivities (for example from the
+flat field), is not known in which case a value of zero can be used.
+See the task \fBstsdas.wfpc.noisemodel\fR for a way to determine
+these vaues (though that task expresses the read out noise in data
+numbers and the sensitivity noise parameter as a percentage).
+
+The read out noise is specified by the \fIrdnoise\fR parameter.  The value
+may be a numeric value to be applied to all the input images or a image
+header keyword containing the value for each image.  Similarly, the
+parameter \fIgain\fR specifies the gain as either a value or image header
+keyword and the parameter \fIsnoise\fR specifies the sensitivity
+noise parameter as either a value or image header keyword.
+
+The algorithm operates on each output pixel independently.  It starts by
+taking the median or unweighted average (excluding the minimum and maximum)
+of the unrejected pixels provided there are at least two input pixels.  The
+expected sigma is computed from the CCD noise parameters and pixels more
+that \fIlsigma\fR times this sigma below or \fIhsigma\fR times this sigma
+above the median or average are rejected.  The process is then iterated
+until no further pixels are rejected.  If the average is used as the
+estimator of the true value then after the first round of rejections the
+highest and lowest values are no longer excluded.  Note that it is possible
+to reject all pixels if the average is used and is sufficiently skewed by
+bad pixels such as cosmic rays.
+
+If there are different CCD noise parameters for the input images
+(as might occur using the image header keyword specification) then
+the sigmas are computed for each pixel from each image using the
+same estimated true value.
+
+If the images are scaled and shifted and the \fIsigscale\fR threshold
+is exceedd then a sigma is computed for each pixel based on the
+image scale parameters; i.e. the median or average is scaled to that of the
+original image before computing the sigma and residuals.
+
+After rejection the number of retained pixels is checked against the
+\fInkeep\fR parameter.  If there are fewer pixels retained than specified
+by this parameter the pixels with the smallest residuals in absolute
+value are added back.  If there is more than one pixel with the same
+absolute residual (for example the two pixels about an average
+or median of two will have the same residuals) they are all added
+back even if this means more than \fInkeep\fR pixels are retained.
+Note that the \fInkeep\fR parameter only applies to the pixels used
+by the clipping rejection algorithm and does not apply to threshold
+or bad pixel mask rejection.
+
+This is the best clipping algorithm to use if the CCD noise parameters are
+adequately known.  The parameters affecting this algorithm are \fIreject\fR
+to select this algorithm, \fImclip\fR to select the median or average for
+the center of the clipping, \fInkeep\fR to limit the number of pixels
+rejected, the CCD noise parameters \fIrdnoise, gain\fR and \fIsnoise\fR,
+\fIlsigma\fR and \fIhsigma\fR to select the clipping thresholds,
+and \fIsigscale\fR to set the threshold for making corrections to the sigma
+calculation for different image scale factors.
+
+.in -4
+CRREJECT
+.in 4
+This algorithm is identical to "ccdclip" except that only pixels above
+the average are rejected based on the \fIhsigma\fR parameter.  This
+is appropriate for rejecting cosmic ray events and works even with
+two images.
+
+.in -4
+SIGCLIP
+.in 4
+The sigma clipping algorithm computes at each output pixel the median or
+average excluding the high and low values and the sigma about this
+estimate.  There must be at least three input pixels, though for this method
+to work well there should be at least 10 pixels.  Values deviating by more
+than the specified sigma threshold factors are rejected.  These steps are
+repeated, except that after the first time the average includes all values,
+until no further pixels are rejected or there are fewer than three pixels.
+
+After rejection the number of retained pixels is checked against the
+\fInkeep\fR parameter.  If there are fewer pixels retained than specified
+by this parameter the pixels with the smallest residuals in absolute
+value are added back.  If there is more than one pixel with the same
+absolute residual (for example the two pixels about an average
+or median of two will have the same residuals) they are all added
+back even if this means more than \fInkeep\fR pixels are retained.
+Note that the \fInkeep\fR parameter only applies to the pixels used
+by the clipping rejection algorithm and does not apply to threshold
+or bad pixel mask rejection.
+
+The  parameters affecting this algorithm are \fIreject\fR to select
+this algorithm, \fImclip\fR to select the median or average for the
+center of the clipping, \fInkeep\fR to limit the number of pixels
+rejected, \fIlsigma\fR and \fIhsigma\fR to select the
+clipping thresholds, and \fIsigscale\fR to set the threshold for
+making corrections to the sigma calculation for different image scale
+factors.
+
+.in -4
+AVSIGCLIP
+.in 4
+The averaged sigma clipping algorithm assumes that the sigma about the
+median or mean (average excluding the low and high values) is proportional
+to the square root of the median or mean at each point.  This is
+described by the equation:
+
+.nf
+	sigma(column,line) = sqrt (gain(line) * signal(column,line))
+.fi
+
+where the \fIestimated\fR signal is the mean or median (hopefully excluding
+any bad pixels) and the gain is the \fIestimated\fR proportionality
+constant having units of photons/data number.
+
+This noise model is valid for images whose values are proportional to the
+number of photons recorded.  In effect this algorithm estimates a
+detector gain for each line with no read out noise component when
+information about the detector noise parameters are not known or
+available.  The gain proportionality factor is computed
+independently for each output line by averaging the square of the residuals
+(at points having three or more input values) scaled by the median or
+mean.  In theory the proportionality should be the same for all rows but
+because of the estimating process will vary somewhat.
+
+Once the proportionality factor is determined, deviant pixels exceeding the
+specified thresholds are rejected at each point by estimating the sigma
+from the median or mean.  If any values are rejected the median or mean
+(this time not excluding the extreme values) is recomputed and further
+values rejected.  This is repeated until there are no further pixels
+rejected or the number of remaining input values falls below three.  Note
+that the proportionality factor is not recomputed after rejections.
+
+If the images are scaled differently and the sigma scaling correction
+threshold is exceedd then a correction is made in the sigma
+calculations for these differences, again under the assumption that
+the noise in an image scales as the square root of the mean intensity.
+
+After rejection the number of retained pixels is checked against the
+\fInkeep\fR parameter.  If there are fewer pixels retained than specified
+by this parameter the pixels with the smallest residuals in absolute
+value are added back.  If there is more than one pixel with the same
+absolute residual (for example the two pixels about an average
+or median of two will have the same residuals) they are all added
+back even if this means more than \fInkeep\fR pixels are retained.
+Note that the \fInkeep\fR parameter only applies to the pixels used
+by the clipping rejection algorithm and does not apply to threshold
+or bad pixel mask rejection.
+
+This algorithm works well for even a few input images.  It works better if
+the median is used though this is slower than using the average.  Note that
+if the images have a known read out noise and gain (the proportionality
+factor above) then the "ccdclip" algorithm is superior.  The two algorithms
+are related in that the average sigma proportionality factor is an estimate
+of the gain.
+
+The  parameters affecting this algorithm are \fIreject\fR to select
+this algorithm, \fImclip\fR to select the median or average for the
+center of the clipping, \fInkeep\fR to limit the number of pixels
+rejected, \fIlsigma\fR and \fIhsigma\fR to select the
+clipping thresholds, and \fIsigscale\fR to set the threshold for
+making corrections to the sigma calculation for different image scale
+factors.
+
+.in -4
+PCLIP
+.in 4
+The percentile clipping algorithm is similar to sigma clipping using the
+median as the center of the distribution except that, instead of computing
+the sigma of the pixels from the CCD noise parameters or from the data
+values, the width of the distribution is characterized by the difference
+between the median value and a specified "percentile" pixel value.  This
+width is then multipled by the scale factors \fIlsigma\fR and \fIhsigma\fR
+to define the clipping thresholds above and below the median.  The clipping
+is not iterated.
+
+The pixel values at each output point are ordered in magnitude and the
+median is determined.  In the case of an even number of pixels the average
+of the two middle values is used as the median value and the lower or upper
+of the two is the median pixel when counting from the median pixel to
+selecting the percentile pixel.  The parameter \fIpclip\fR selects the
+percentile pixel as the number (if the absolute value is greater
+than unity) or fraction of the pixels from the median in the ordered set.
+The direction of the percentile pixel from the median is set by the sign of
+the \fIpclip\fR parameter with a negative value signifying pixels with
+values less than the median.  Fractional values are internally converted to
+the appropriate number of pixels for the number of input images.  A minimum
+of one pixel and a maximum corresponding to the extreme pixels from the
+median are enforced.  The value used is reported in the log output.  Note
+that the same percentile pixel is used even if pixels have been rejected by
+offseting, masking, or thresholding; for example, if the 3nd pixel below
+the median is specified then the 3rd pixel will be used whether there are
+10 pixels or 5 pixels remaining after the preliminary steps.
+
+Some examples help clarify the definition of the percentile pixel.  In the
+examples assume 10 pixels.  The median is then the average of the
+5th and 6th pixels.  A \fIpclip\fR value of 2 selects the 2nd pixel
+above the median (6th) pixel which is the 8th pixel.  A \fIpclip\fR
+value of -0.5 selects the point halfway between the median and the
+lowest pixel.  In this case there are 4 pixels below the median,
+half of that is 2 pixels which makes the percentile pixel the 3rd pixel.
+
+The percentile clipping algorithm is most useful for clipping small
+excursions, such as the wings of bright objects when combining
+disregistered observations for a sky flat field, that are missed when using
+the pixel values to compute a sigma.  It is not as powerful, however, as
+using the CCD noise parameters (provided they are accurately known) to clip
+about the median.
+
+The  parameters affecting this algorithm are \fIreject\fR to select this
+algorithm, \fIpclip\fR to select the percentile pixel, \fInkeep\fR to limit
+the number of pixels rejected, and \fIlsigma\fR and \fIhsigma\fR to select
+the clipping thresholds.
+
+.in -4
+GROW REJECTION
+
+Neighbors of pixels rejected by the rejection algorithms along image lines
+may also be rejected.  The number of neighbors to be rejected on either
+side is specified by the \fIgrow\fR parameter.  The rejection only
+applies to neighbors along each image line.  This is because the
+task operates independently on each image line and does not have the
+ability to go back to previous lines or maintain a list of rejected
+pixels to later lines.
+
+This rejection step is also checked against the \fInkeep\fR parameter
+and only as many pixels as would not violate this parameter are
+rejected.  Unlike it's application in the rejection algorithms at
+this stage there is no checking on the magnitude of the residuals
+and the pixels retained which would otherwise be rejected are randomly
+selected.
+
+
+COMBINING
+
+After all the steps of offsetting the input images, masking pixels,
+threshold rejection, scaling, and applying a rejection algorithms the
+remaining pixels are combined and output.  The pixels may be combined
+by computing the median or by computing a weighted average.
+
+
+SIGMA OUTPUT
+
+In addition to the combined image and optional sigma image may be
+produced.  The sigma computed is the standard deviation, corrected for a
+finite population by a factor of n/(n-1), of the unrejected input pixel
+values about the output combined pixel values.
+.ih
+EXAMPLES
+1.  To average and median images without any other features:
+
+.nf
+	cl> combine obj* avg combine=average reject=none
+	cl> combine obj* med combine=median reject=none
+.fi
+
+2.  To reject cosmic rays:
+
+.nf
+	cl> combine obs1,obs2 Obs reject=crreject rdnoise=5.1, gain=4.3
+.fi
+
+3.  To make a grid for display purposes with 21 64x64 images:
+
+.nf
+	cl> combine @list grid offset="grid 5 65 5 65"
+.fi
+
+4.  To apply a mask image with good pixels marked with a zero value and
+    bad pixels marked with a value of one:
+
+.nf
+	cl> hedit ims* bpm badpix.pl add+ ver-
+	cl> combine ims* final combine=median masktype=goodval
+.fi
+
+5.  To scale image by the exposure time and then adjust for varying
+    sky brightness and make a weighted average:
+
+.nf
+	cl> combine obj* avsig combine=average reject=avsig \
+	>>> scale=exp zero=mode weight=exp  expname=exptime
+.fi
+.ih
+TIME REQUIREMENTS
+The following times were obtain with a Sun 4/470.  The tests combine
+1000x200 images consisting of Poisson noise and cosmic rays generated
+with the \fBartdata\fR package.  The times, especially the total time,
+are approximate and depend on user loads.
+
+.nf
+IMAGES:   Number of images (1000x200) and datatype (R=real, S=short)
+COMBINE:  Combine option
+REJECT:   Rejection option with grow = 0
+	      minmax:    nlow = 1, nhigh = 1
+	      ccdclip:   lsigma = 3., hsigma = 3, sigscale = 0.
+	      sigclip:   lsigma = 3., hsigma = 3, sigscale = 0.
+	      avsigclip: lsigma = 3., hsigma = 3, sigscale = 0.
+	      pclip:     lsigma = 3., hsigma = 3, pclip = -0.5
+	      /a:        mclip = no  (clip about the average)
+	      /m:        mclip = yes (clip about the median)
+O M T S:  Features used (Y=yes, N=no)
+O:        offset = "grid 5 10 2 10"
+M:        masktype = goodval, maskval = 0
+	      Pixel mask has 2 bad lines and 20 bad columns 
+T:        lthreshold = INDEF, hthreshold = 1100.
+S:        scale = mode, zero = none, weight = mode
+TIME:     cpu time in seconds, total time in minutes and seconds
+
+
+IMAGES  COMBINE  REJECT        O M T S     TIME
+
+  10R   average  none          N N N N    1.3 0:08
+  10R   average  minmax        N N N N    4.3 0:10
+  10R   average  pclip         N N N N   17.9 0:32
+  10R   average  ccdclip/a     N N N N   11.6 0:21
+  10R   average  crreject/a    N N N N   11.4 0:21
+  10R   average  sigclip/a     N N N N   13.6 0:29
+  10R   average  avsigclip/a   N N N N   15.9 0:35
+  10R   average  ccdclip/m     N N N N   16.9 0:32
+  10R   average  crreject/m    N N N N   17.0 0:28
+  10R   average  sigclip/m     N N N N   19.6 0:42
+  10R   average  avsigclip/m   N N N N   20.6 0:43
+
+  10R   median   none          N N N N    6.8 0:17
+  10R   median   minmax        N N N N    7.8 0:15
+  10R   median   pclip         N N N N   16.9 1:00
+  10R   median   ccdclip/a     N N N N   18.0 0:34
+  10R   median   crreject/a    N N N N   17.7 0:30
+  10R   median   sigclip/a     N N N N   21.1 1:13
+  10R   median   avsigclip/a   N N N N   23.1 0:41
+  10R   median   ccdclip/m     N N N N   16.1 0:27
+  10R   median   crreject/m    N N N N   16.0 0:27
+  10R   median   sigclip/m     N N N N   18.1 0:29
+  10R   median   avsigclip/m   N N N N   19.6 0:32
+
+  10R   average  none          N N N Y    6.1 0:36
+  10R   median   none          N N N Y   10.4 0:49
+  10R   median   pclip         N N N Y   20.4 1:10
+  10R   median   ccdclip/m     N N N Y   19.5 0:36
+  10R   median   avsigclip/m   N N N Y   23.0 1:06
+
+  10R   average  none          N Y N N    3.5 0:12
+  10R   median   none          N Y N N    8.9 0:21
+  10R   median   pclip         N Y N N   19.9 0:45
+  10R   median   ccdclip/m     N Y N N   18.0 0:44
+  10R   median   avsigclip/m   N Y N N   20.9 0:28
+
+  10R   average  none          Y N N N    4.3 0:13
+  10R   median   none          Y N N N    9.6 0:21
+  10R   median   pclip         Y N N N   21.8 0:54
+  10R   median   ccdclip/m     Y N N N   19.3 0:44
+  10R   median   avsigclip/m   Y N N N   22.8 0:51
+
+  10R   average  none          Y Y Y Y   10.8 0:22
+  10R   median   none          Y Y Y Y   16.1 0:28
+  10R   median   pclip         Y Y Y Y   27.4 0:42
+  10R   median   ccdclip/m     Y Y Y Y   25.5 0:39
+  10R   median   avsigclip/m   Y Y Y Y   28.9 0:44
+
+  10S   average  none          N N N N    2.2 0:06
+  10S   average  minmax        N N N N    4.6 0:12
+  10S   average  pclip         N N N N   18.1 0:33
+.fi
+.ih
+REVISIONS
+.ls COMBINE V2.11
+The limit of the number of images that may be combined has been removed.
+If the number of images exceeds the maximum number of open images permitted
+then the images are stacked in a single temporary image and then combined
+with the project option.  Note that this will double the amount of
+diskspace temporarily.  There is also a limitation in this case that the
+bad pixel mask from the first image in the list will be applied to all the
+images.
+
+Integer offsets may be determined from the image world coordinate system.
+.le
+.ls COMBINE V2.10.3
+The output pixel datatype parameter, \fIouttype\fR was previously ignored
+and the package \fIpixeltype\fR was used.  The task output pixel type
+parameter is now used.
+
+The factors specified by an @file or keyword are not normalized.
+.le
+.ls COMBINE V2.10.2
+The weighting was changed from using the square root of the exposure time
+or image statistics to using the values directly.  This corresponds
+to variance weighting.  Other options for specifying the scaling and
+weighting factors were added; namely from a file or from a different
+image header keyword.  The \fInkeep\fR parameter was added to allow
+controlling the maximum number of pixels to be rejected by the clipping
+algorithms.  The \fIsnoise\fR parameter was added to include a sensitivity
+or scale noise component to the noise model.  Errors will now delete
+the output images.
+.le
+.ls COMBINE V2.10
+This task was greatly revised to provide many new features.  These features
+are:
+
+.nf
+    o Bad pixel masks
+    o Combining offset and different size images
+    o Blank value for missing data
+    o Combining across the highest dimension (the project option)
+    o Separating threshold rejection, the rejection algorithms,
+      and the final combining statistic
+    o New CCDCLIP, CRREJECT, and PCLIP algorithms
+    o Rejection now may reject more than one pixel per output pixel
+    o Choice of a central median or average for clipping
+    o Choice of final combining operation
+    o Simultaneous multiplicative and zero point scaling
+.fi
+.le
+.ih
+LIMITATIONS
+Though the previous limit on the number of images that can be combined
+was removed in V2.11 the method has the limitation that only a single
+bad pixel mask will be used for all images.
+.ih
+SEE ALSO
+image.imcombine, instruments, ccdtypes, icfit, ccdred, guide, darkcombine,
+flatcombine, zerocombine, onedspec.scombine wfpc.noisemodel
+.endhelp
diff --git a/noao/imred/ccdred/doc/contents.ms b/noao/imred/ccdred/doc/contents.ms
new file mode 100644
index 00000000..8ba2624a
--- /dev/null
+++ b/noao/imred/ccdred/doc/contents.ms
@@ -0,0 +1,34 @@
+.sp 1i
+.ps +2
+.ft B
+.ce
+Contents
+.sp 3
+.ps -2
+.ft R
+.sp
+1.\h'|0.4i'\fBIntroduction\fP\l'|5.6i.'\0\01
+.sp
+2.\h'|0.4i'\fBGetting Started\fP\l'|5.6i.'\0\02
+.sp
+3.\h'|0.4i'\fBProcessing Your Data\fP\l'|5.6i.'\0\05
+.br
+\h'|0.4i'3.1.\h'|0.9i'Combining Calibration Images\l'|5.6i.'\0\06
+.br
+\h'|0.4i'3.2.\h'|0.9i'Calibrations and Corrections\l'|5.6i.'\0\07
+.sp
+4.\h'|0.4i'\fBSpecial Processing Operations\fP\l'|5.6i.'\0\08
+.br
+\h'|0.4i'4.1.\h'|0.9i'Spectroscopic Flat Fields\l'|5.6i.'\0\08
+.br
+\h'|0.4i'4.2.\h'|0.9i'Illumination Corrections\l'|5.6i.'\0\09
+.br
+\h'|0.4i'4.3.\h'|0.9i'Sky Flat Fields\l'|5.6i.'\010
+.br
+\h'|0.4i'4.4.\h'|0.9i'Illumination Corrected Flat Fields\l'|5.6i.'\010
+.br
+\h'|0.4i'4.5.\h'|0.9i'Fringe Corrections\l'|5.6i.'\010
+.sp
+5.\h'|0.4i'\fBSummary\fP\l'|5.6i.'\011
+.sp
+\h'|0.4i'\fBReferences\fP\l'|5.6i.'\011
diff --git a/noao/imred/ccdred/doc/darkcombine.hlp b/noao/imred/ccdred/doc/darkcombine.hlp
new file mode 100644
index 00000000..c545a13e
--- /dev/null
+++ b/noao/imred/ccdred/doc/darkcombine.hlp
@@ -0,0 +1,120 @@
+.help darkcombine Aug91 noao.imred.ccdred
+.ih
+NAME
+darkcombine -- Combine and process dark count images
+.ih
+USAGE
+darkcombine input
+.ih
+PARAMETERS
+.ls input
+List of dark count images to combine.  The \fIccdtype\fR parameter
+may be used to select the zero level images from a list containing all
+types of data.
+.le
+.ls output = "Dark"
+Output dark count root image name.
+.le
+.ls combine = "average" (average|median)
+Type of combining operation performed on the final set of pixels (after
+rejection).  The choices are
+"average" or "median".  The median uses the average of the two central
+values when the number of pixels is even.
+.le
+.ls reject = "minmax" (none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip)
+Type of rejection operation.  See \fBcombine\fR for details.
+.le
+.ls ccdtype = "dark"
+CCD image type to combine.  If no image type is given then all input images
+are combined.
+.le
+.ls process = yes
+Process the input images before combining?
+.le
+.ls delete = no
+Delete input images after combining?  Only those images combined are deleted.
+.le
+.ls clobber = no
+Clobber existing output images?
+.le
+.ls scale = "exposure" (none|mode|median|mean|exposure)
+Multiplicative image scaling to be applied.  The choices are none, scale
+by the mode, median, or mean of the specified statistics section, or scale
+by the exposure time given in the image header.
+.le
+.ls statsec = ""
+Section of images to use in computing image statistics for scaling.
+If no section is given then the entire region of the image is
+sampled (for efficiency the images are sampled if they are big enough).
+.le
+
+.ce
+Algorithm Parameters
+.ls nlow = 0,  nhigh = 1 (minmax)
+The number of low and high pixels to be rejected by the "minmax" algorithm.
+.le
+.ls nkeep = 1
+The minimum number of pixels to retain or the maximum number to reject
+when using the clipping algorithms (ccdclip, crreject, sigclip,
+avsigclip, or pclip).  When given as a positive value this is the minimum
+number to keep.  When given as a negative value the absolute value is
+the maximum number to reject.  This is actually converted to a number
+to keep by adding it to the number of images.
+.le
+.ls mclip = yes (ccdclip, crreject, sigclip, avsigcliip)
+Use the median as the estimate for the true intensity rather than the
+average with high and low values excluded in the "ccdclip", "crreject",
+"sigclip", and "avsigclip" algorithms?  The median is a better estimator
+in the presence of data which one wants to reject than the average.
+However, computing the median is slower than the average.
+.le
+.ls lsigma = 3., hsigma = 3. (ccdclip, crreject, sigclip, avsigclip, pclip)
+Low and high sigma clipping factors for the "ccdclip", "crreject", "sigclip",
+"avsigclip", and "pclip" algorithms.  They multiply a "sigma" factor
+produced by the algorithm to select a point below and above the average or
+median value for rejecting pixels.  The lower sigma is ignored for the
+"crreject" algorithm.
+.le
+.ls rdnoise = "0.", gain = "1.", snoise = "0." (ccdclip, crreject)
+CCD readout noise in electrons, gain in electrons/DN, and sensitivity noise
+as a fraction.  These parameters are used with the "ccdclip" and "crreject"
+algorithms.  The values may be either numeric or an image header keyword
+which contains the value.
+.le
+.ls pclip = -0.5 (pclip)
+Percentile clipping algorithm parameter.  If greater than
+one in absolute value then it specifies a number of pixels above or
+below the median to use for computing the clipping sigma.  If less
+than one in absolute value then it specifies the fraction of the pixels
+above or below the median to use.  A positive value selects a point
+above the median and a negative value selects a point below the median.
+The default of -0.5 selects approximately the quartile point.
+See \fBcombine\fR for further details.
+.le
+.ls blank = 0.
+Output value to be used when there are no pixels.
+.le
+.ih
+DESCRIPTION
+The dark count images in the input image list are combined.
+The input images may be processed first if desired.
+The original images may be deleted automatically if desired.
+The output pixel datatype will be real.
+
+This task is a script which applies \fBccdproc\fR and \fBcombine\fR.  The
+parameters and combining algorithms are described in detail in the help for
+\fBcombine\fR.  This script has default parameters specifically set for
+dark count images and simplifies the combining parameters.  There are other
+combining options not included in this task.  For these additional
+features, such as thresholding, offseting, masking, and projecting, use
+\fBcombine\fR.
+.ih
+EXAMPLES
+1. The image data contains four dark count images.  To automatically select
+them and combine them as a background job using the default combining algorithm:
+
+    cl> darkcombine ccd*.imh&
+.ih
+SEE ALSO
+ccdproc, combine
+.endhelp
diff --git a/noao/imred/ccdred/doc/flatcombine.hlp b/noao/imred/ccdred/doc/flatcombine.hlp
new file mode 100644
index 00000000..549c912c
--- /dev/null
+++ b/noao/imred/ccdred/doc/flatcombine.hlp
@@ -0,0 +1,133 @@
+.help flatcombine Aug91 noao.imred.ccdred
+.ih
+NAME
+flatcombine -- Combine and process flat field images
+.ih
+USAGE
+flatcombine input
+.ih
+PARAMETERS
+.ls input
+List of flat field images to combine.  The \fIccdtype\fR parameter
+may be used to select the flat field images from a list containing all
+types of data.
+.le
+.ls output = "Flat"
+Output flat field root image name.  The subset ID is appended.
+.le
+.ls combine = "average" (average|median)
+Type of combining operation performed on the final set of pixels (after
+rejection).  The choices are
+"average" or "median".  The median uses the average of the two central
+values when the number of pixels is even.
+.le
+.ls reject = "avsigclip" (none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip)
+Type of rejection operation.  See \fBcombine\fR for details.
+.le
+.ls ccdtype = "flat"
+CCD image type to combine.  If no image type is given then all input images
+are combined.
+.le
+.ls process = yes
+Process the input images before combining?
+.le
+.ls subsets = yes
+Combine images by subset parameter?  If yes then the input images are
+grouped by subset parameter and each group combined into a separate output
+image.  The subset identifier is appended to the output and sigma image
+names.  See \fBsubsets\fR for more on the subset parameter.  This is generally
+used with flat field images.
+.le
+.ls delete = no
+Delete input images after combining?  Only those images combined are deleted.
+.le
+.ls clobber = no
+Clobber existing output images?
+.le
+.ls scale = "mode" (none|mode|median|mean|exposure)
+Multiplicative image scaling to be applied.  The choices are none, scale
+by the mode, median, or mean of the specified statistics section, or scale
+by the exposure time given in the image header.
+.le
+.ls statsec = ""
+Section of images to use in computing image statistics for scaling.
+If no section is given then the entire region of the image is
+sampled (for efficiency the images are sampled if they are big enough).
+.le
+
+.ce
+Algorithm Parameters
+.ls nlow = 1,  nhigh = 1 (minmax)
+The number of low and high pixels to be rejected by the "minmax" algorithm.
+.le
+.ls nkeep = 1
+The minimum number of pixels to retain or the maximum number to reject
+when using the clipping algorithms (ccdclip, crreject, sigclip,
+avsigclip, or pclip).  When given as a positive value this is the minimum
+number to keep.  When given as a negative value the absolute value is
+the maximum number to reject.  This is actually converted to a number
+to keep by adding it to the number of images.
+.le
+.ls mclip = yes (ccdclip, crreject, sigclip, avsigcliip)
+Use the median as the estimate for the true intensity rather than the
+average with high and low values excluded in the "ccdclip", "crreject",
+"sigclip", and "avsigclip" algorithms?  The median is a better estimator
+in the presence of data which one wants to reject than the average.
+However, computing the median is slower than the average.
+.le
+.ls lsigma = 3., hsigma = 3. (ccdclip, crreject, sigclip, avsigclip, pclip)
+Low and high sigma clipping factors for the "ccdclip", "crreject", "sigclip",
+"avsigclip", and "pclip" algorithms.  They multiply a "sigma" factor
+produced by the algorithm to select a point below and above the average or
+median value for rejecting pixels.  The lower sigma is ignored for the
+"crreject" algorithm.
+.le
+.ls rdnoise = "0.", gain = "1.", snoise = "0." (ccdclip, crreject)
+CCD readout noise in electrons, gain in electrons/DN, and sensitivity noise
+as a fraction.  These parameters are used with the "ccdclip" and "crreject"
+algorithms.  The values may be either numeric or an image header keyword
+which contains the value.
+.le
+.ls pclip = -0.5 (pclip)
+Percentile clipping algorithm parameter.  If greater than
+one in absolute value then it specifies a number of pixels above or
+below the median to use for computing the clipping sigma.  If less
+than one in absolute value then it specifies the fraction of the pixels
+above or below the median to use.  A positive value selects a point
+above the median and a negative value selects a point below the median.
+The default of -0.5 selects approximately the quartile point.
+See \fBcombine\fR for further details.
+.le
+.ls blank = 1.
+Output value to be used when there are no pixels.
+.le
+.ih
+DESCRIPTION
+The flat field images in the input image list are combined.  If there
+is more than one subset (such as a filter or grating) then the input
+flat field images are grouped by subset and an combined separately.
+The input images may be processed first if desired.  However if all
+zero level bias effects are linear then this is not necessary and some
+processing time may be saved.  The original images may be deleted
+automatically if desired.  The output pixel datatype will be real.
+
+This task is a script which applies \fBccdproc\fR and \fBcombine\fR.  The
+parameters and combining algorithms are described in detail in the help for
+\fBcombine\fR.  This script has default parameters specifically set for
+flat field images and simplifies the combining parameters.  There are other
+combining options not included in this task.  For these additional
+features, such as thresholding, offseting, masking, and projecting, use
+\fBcombine\fR.
+.ih
+EXAMPLES
+1. The image data contains four flat field images for three filters.
+To automatically select them and combine them as a background job
+using the default combining algorithm:
+
+    cl> flatcombine ccd*.imh&
+
+The final images are "FlatV", "FlatB", and "FlatR".
+.ih
+SEE ALSO
+ccdproc, combine, subsets
+.endhelp
diff --git a/noao/imred/ccdred/doc/flatfields.hlp b/noao/imred/ccdred/doc/flatfields.hlp
new file mode 100644
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+.help flatfields Jun87 noao.imred.ccdred
+
+.ih
+NAME
+flatfields -- Discussion of CCD flat field calibrations
+.ih
+DESCRIPTION
+This topic describes the different types of CCD flat fields and
+the tasks available in the \fBccdred\fR and spectroscopy packages for
+creating them.  Flat field calibration is the most important operation
+performed on CCD data.  This operation calibrates the relative response
+of the detector at each pixel.  In some cases this is as simple as
+taking a special type of observation called a flat field.  However, in
+many cases this calibration observation must be corrected for
+iillumination, scanning, wavelength, and aperture effects.
+
+The discussion is in three sections; direct imaging, scan mode,
+and spectroscopy.  Though there are many similarities between these
+modes of operation there are important differences in how corrections
+are applied to the basic flat field observations.  The application of
+the flat field calibrations to the observations using \fBccdproc\fR is
+the same in all cases, however.
+.sh
+1. Direct Imaging
+The starting point for determining the flat field calibration is an
+observation of something which should have uniform response at all
+points on the detector.  In addition the color of the light falling at
+each pixel should be the same as that in an observation so the same
+filter must be used when determining the flat field (the issue of the
+matching the color of the objects observed at the appropriate pixels is
+ignored here).  The best calibration observation is of a blank sky.  If
+an accurate blank sky observation can be obtained then this is all that
+is needed for a flat field calibration.  This type of flat field might
+be called a \fIsky flat\fR, though this term is more often used for a
+type of flat field described below.  There are two difficulties with
+this type of calibration; finding a really blank sky and getting a
+sufficiently accurate measurement without using all the observing
+time.
+
+It is usually not possible to get a blank sky observation accurate
+enough to calibrate the individual pixels without introducing
+undesirable noise.  What is generally done is to use a lamp to either
+uniformly illuminate a part of the dome or directly illuminate the
+field of view.  The first type of observation is called a \fIdome
+flat\fR and the second is called a \fIprojection flat\fR.  We shall call
+both of these types of observations \fBlamp flat fields\fR.  If the
+iillumination is truely uniform then these types of observations are
+sufficient for flat field calibration.  To get a very accurate flat
+field many observations are made and then combined (see
+\fBflatcombine\fR).
+
+Unfortunately, it is sometimes the case that the lamp flat fields
+do not illuminate the telescope/detector in the same way as the actual
+observations.  Calibrating with these flat fields will introduce a
+residual large scale iillumination pattern, though it will correctly
+calibrate the relative pixel responses locally.  There are two ways to
+correct for this effect.  The first is to correct the flat field
+observation.  The second is to apply the uncorrected flat field to the
+observations and then apply an \fIiillumination\fR correction as a
+separate operation.  The first is more efficient since it consists of a
+single correction applied to each observation but in some cases the
+approximate correction is desired immediately, the observation needed
+to make the correction has not been taken yet, or the residual
+iillumination error is not discovered until later.
+
+For the two methods there are two types of correction.  One is to
+use a blank sky observation to correct for the residual iillumination
+pattern.  This is different than using the sky observation directly as
+a flat field calibration in that only the large scale pattern is
+needed.  Determining the large scale iillumination does not require high
+signal-to-noise at each pixel and faint objects in the image can be
+either eliminated or ignored.  The second method is to remove the large
+scale shape from the lamp flat field.  This is not as good as using a
+blank sky observation but, if there is no such observation and the
+iillumination pattern is essentially only in the lamp flat field, this
+may be sufficient.
+
+From the above two paragraphs one sees there are four options.
+There is a task in the \fBccdred\fR package for each of these options.
+To correct a lamp flat field observation by a blank sky observation,
+called a \fIsky flat\fR, the task is \fBmkskyflat\fR.  To correct the
+flat field for its own large scale gradients, called an \fIiillumination
+flat\fR, the task is \fBmkillumflat\fR.  To create a secondary
+correction to be applied to data processed with the lamp flat field
+image the tasks are \fBmkskycor\fR and \fBmkillumcor\fR which are,
+respectively, based on a blank sky observation and the lamp flat field
+iillumination pattern.
+
+With this introduction turn to the individual documentation for these
+four tasks for further details.
+.sh
+2. Scan Mode
+There are two types of scan modes supported by the \fBccdred\fR
+package; \fIshortscan\fR and \fIlongscan\fR (see \fBccdproc\fR for
+further details).  They both affect the manner in which flat field
+calibrations are handled.  The shortscan mode produces images which are
+the same as direct images except that the light recorded at each pixel
+was collected by a number of different pixels.  This improves the flat
+field calibration.  If the flat field images, of the same types
+described in the direct imaging section, are observed in the same way
+as all other observations, i.e. in scan mode, then there is no
+difference from direct imaging (except in the quality of the flat
+fields).  There is a statistical advantage to observing the lamp or sky
+flat field without scanning and then numerically averaging to simulate
+the result of the scanning.  This improves the accuracy of
+the flat fields and might possibly allow direct blank sky observations
+to be used for flat fields.  The numerical scanning is done in
+\fBccdproc\fR by setting the appropriate scanning parameters.
+
+In longscan mode the CCD detector is read out in such a way that
+each output image pixel is the sum of the light falling on all pixels
+along the direction of the scan.  This reduces the flat field calibration
+to one dimension, one response value for each point across the scan.
+The one dimensional calibration is obtained from a longscan observation
+by averaging all the readout lines.
+This is done automatically in \fBccdproc\fR by setting the appropriate
+parameters.  In this case very good flat fields can be obtained from
+one or more blank sky observations or an unscanned lamp observation.  Other
+corrections are not generally used.
+.sh
+3. Spectroscopy
+Spectroscopic flat fields differ from direct imaging in that the
+spectrum of the sky or lamp and transmission variations with wavelength
+are part of the observation.  Application of such images will introduce
+the inverse of the spectrum and transmission into the observation.  It
+also distorts the observed counts making signal-to-noise estimates
+invalid.  This, and the low signal in the dispersed light, makes it
+difficult to use blank sky observations directly as flat fields.  As
+with direct imaging, sky observation may be used to correct for
+iillumination errors if necessary.  At sufficiently high dispersion the
+continuous lamp spectrum may be flat enough that the spectral signature
+of the lamp is not a problem.  Alternatively, flux calibrating the
+spectra will also remove the flat field spectral signature.  The
+spectroscopic flat fields also have to be corrected for regions outside
+of the slit or apertures to avoid bad response effects when applying
+the flat field calibration to the observations.
+
+The basic scheme for removing the spectral signature is to average
+all the lines or columns across the dispersion and within the aperture
+to form an estimate of the spectrum.  In addition to the averaging, a
+smooth curve is fit to the lamp spectrum to remove noise.  This smooth
+shape is then divided back into each line or column to eliminate the
+shape of the spectrum without changing the shape of the spectrum
+in the spatial direction or the small scale response variations.
+Regions outside of the apertures are replaced by unity.
+This method requires that the dispersion be aligned fairly close to
+either the CCD lines or columns.
+
+This scheme is used in both longslit and multiaperture spectra.
+The latter includes echelle, slitlets, aperture masks, and fiber feeds.
+For narrow apertures which do not have wider slits for the lamp
+exposures there may be problems with flexure and defining a good
+composite spectrum.  The algorithm for longslit spectra is simpler and
+is available in the task \fBresponse\fR in the \fBlongslit\fR package.
+For multiaperture data there are problems of defining where the spectra
+lie and avoiding regions off of the aperture where there is no signal.
+The task which does this is \fBapnormalize\fR in the \fBapextract\fR
+package.   Note that the lamp observations must first be processed
+explicitly for bias and dark count corrections.
+
+Longslit spectra may also suffer the same types of iillumination
+problems found in direct imaging.  However, in this case the iillumination
+pattern is determined from sky observations (or the flat field itself)
+by finding the large scale pattern across the dispersion and at a number
+of wavelengths while avoiding the effects of night sky spectrum.  The
+task which makes this type of correction in the \fBlongslit\fR package
+is \fBiillumination\fR.  This produces an iillumination correction.
+To make sky flats or the other types of corrections image arithmetic
+is used.  Note also that the sky observations must be explicitly
+processed through the flat field stage before computing the iillumination.
+.ih
+SEE ALSO
+.nf
+ccdproc, guide, mkillumcor, mkillumflat, mkskycor, mkskyflat
+apextract.apnormalize, longslit.response, longslit.iillumination
+.fi
+.endhelp
diff --git a/noao/imred/ccdred/doc/guide.hlp b/noao/imred/ccdred/doc/guide.hlp
new file mode 100644
index 00000000..5006a6ec
--- /dev/null
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@@ -0,0 +1,717 @@
+.help guide Feb88 noao.imred.ccdred
+.ce
+User's Guide to the CCDRED Package
+.sh
+1. Introduction
+
+     This guide provides a brief description of the IRAF CCD reduction
+package \fBccdred\fR and examples of reducing simple CCD data.  It is a
+generic guide in that it is not tied to any particular type of data.
+There may be more specific guides (or "cookbooks") for your data.
+Detailed descriptions of the tasks and features of the package are
+provided in the help documentation for the package.
+
+     The purpose of the CCDRED package is to provide tools for the easy
+and efficient reduction of CCD images.  The standard reduction
+operations are replacement of bad columns and lines by interpolation
+from neighboring columns and lines, subtraction of a bias level
+determined from overscan or prescan columns or lines, subtraction of a
+zero level using a zero length exposure calibration image, subtraction
+of a dark count calibration image appropriately scaled to the dark time
+exposure, division by a scaled flat field calibration image, division
+by an iillumination image (derived from a blank sky image), subtraction
+of a scaled fringe image (also derived from a blank sky image), and
+trimming the image of unwanted lines or columns such as the overscan
+strip.  Any set of operations may be done simultaneously over a list of
+images in a highly efficient manner.  The reduction operations are
+recorded in the image header and may also be logged on the terminal and
+in a log file.
+
+     The package also provides tools for combining multiple exposures
+of object and calibration images to improve the statistical accuracy of
+the observations and to remove transient bad pixels.  The combining
+operation scales images of different exposure times, adjusts for
+variable sky background, statistically weights the images by their
+signal-to-noise, and provides a number of useful algorithms for
+detecting and rejecting transient bad pixels.
+
+     Other tasks are provided for listing reduction information about
+the images, deriving secondary calibration images (such as sky
+corrected flat fields or iillumination correction images), and easily
+setting the package parameters for different instruments.
+
+     There are several important features provided by the package to
+make the reduction of CCD images convenient; particularly to minimize
+record keeping.  One of these is the ability to recognize the different
+types of CCD images.  This ability allows the user to select a certain
+class of images to be processed or listed and allows the processing
+tasks to identify calibration images and process them differently from
+object images.  The standard CCD image types are \fIobject\fR,
+\fIzero\fR level, \fIdark\fR count, and \fIflat\fR field.  For more on
+the image types see \fBccdtypes\fR.
+
+     The tasks can also identify the different filters (or other subset
+parameter) which require different flat field images.  This means you don't
+have to separate the images by filter and process each set separately.
+This feature is discussed further in \fBsubsets\fR.
+
+     The tasks keep track of the reduction steps completed on each
+image and ignore images which have been processed.  This feature,
+along with recognizing the image types and subsets, makes it possible to
+specify all the images to a task with a wildcard template, such as
+"*.imh", rather than indicating each image by name.  You will find this
+extremely important with large sets of observations.
+
+     A fundamental aspect of the package is that the processing
+modifies the images.  In other words, the reduction operations are
+performed directly on the image.  This "feature" further simplifies
+record keeping, frees the user from having to form unique output image
+names, and minimizes the amount of disk space required.  There
+are two safety features in this process.  First, the modifications do
+not take effect until the operation is completed on the image.  This
+allows you to abort the task without messing up the image data and
+protects data if the computer crashes.  The second feature is that
+there is a package parameter which may be set to make a backup of the
+input data with a particular prefix such as "orig" or "imdir$".  This
+backup feature may be used when there is sufficient disk space, when learning
+to use the package, or just to be cautious.
+
+     In a similar effort to efficiently manage disk space, when combining
+images into a master object or calibration image there is an option to
+delete the input images upon completion of the combining operation.
+Generally this is desirable when there are many calibration exposures,
+such as zero level or flat field images, which are not used after they
+are combined into a final calibration image.
+
+     The following sections guide you through the basic use of the
+\fBccdred\fR package.  Only the important parameters which you might
+want to change are described.  It is assumed that the support personnel
+have created the necessary instrument files (see \fBinstruments\fR)
+which will set the default parameters for the data you will be
+reducing.  If this is not the case you may need to delve more deeply
+into the details of the tasks.  Information about all the parameters
+and how the various tasks operate are given in the help documentation
+for the tasks and in additional special help topics.  Some useful help
+documentation is indicated in the discussion and also in the
+\fBReferences\fR section.
+.sh
+2. Getting Started
+
+     The first step is to load \fBccdred\fR.  This is done by loading
+the \fBnoao\fR package, followed by the image reduction package
+\fBimred\fR, and finally the \fBccdred\fR package.  Loading a
+package consists of typing its name.  Note that some of these packages may be
+loaded automatically when you logon to IRAF.
+
+     When you load the \fBccdred\fR package the menu of tasks or commands
+is listed.  This appears as follows:
+
+.nf
+    cl> ccdred
+      badpiximage       ccdtest           mkfringecor       setinstrument
+      ccdgroups         combine           mkillumcor        zerocombine
+      ccdhedit          cosmicrays        mkillumflat       
+      ccdlist           darkcombine       mkskycor          
+      ccdproc           flatcombine       mkskyflat         
+.fi
+
+A summary of the tasks and additional help topics is obtained by typing:
+
+    cl> help
+
+This list and how to get additional help on specific topics is described
+in the \fBReferences\fR section at the end of this guide.
+
+     The first command to use is \fBsetinstrument\fR, which sets the package
+appropriately for the CCD images to be reduced.  The support personnel
+should tell you the instrument identification, but if not a list
+of known instruments may be listed by using '?' for the instrument name.
+
+.nf
+    cl> setinstrument
+    Instrument ID (type ? for a list) \fI<enter instrument id or ?>\fR
+        <Set ccdred package parameters using eparam>
+        <Set ccdproc task parameters using eparam>
+.fi
+
+This task sets the default parameters and then allows you to modify the
+package parameters and the processing parameters using the parameter
+editor \fBeparam\fR.  If you are not familiar with \fBeparam\fR see the
+help or CL introduction documentation.  For most terminals you move up
+and down through the parameters with the terminal arrow keys, you
+change the parameters by simply typing the desired value, and you exit
+with control Z or control D.  Note that you can change parameters for
+any task at any time with \fBeparam\fR and you do not have to run
+\fBsetinstrument\fR again, even if you logout, until you need to reduce
+data from a different instrument.
+
+     The \fBccdred\fR package parameters control general I/O functions of
+the tasks in the package.  The parameters you might wish to change are
+the output pixel type and the verbose option.  Except when the input
+images are short integers, the noise is significantly greater than one
+digital unit, and disk space is critical, it is probably better to
+allow the processing to convert the images to real pixel datatype.  The
+verbose parameter simply prints the information written to the log file
+on the terminal.  This can be useful when little else is being done and
+you are just beginning.  However, when doing background processing and
+other IRAF reduction tasks it is enough to simply look at the end of
+the logfile with the task \fBtail\fR to see the current state of the
+processing.
+
+     The \fBccdproc\fR parameters control the CCD processing.  There are
+many parameters but they all may be conveniently set at this point.
+Many of the parameters have default values set appropriately for the
+instrument you specified.  The images to be processed can be specified
+later.  What needs to be set are the processing operations that you
+want done and the parameters required for each operation.  The
+processing operations are selected by entering yes or no for each one.
+The following items briefly describe each of the possible processing
+operations and the additional parameters required.
+
+.ls \fIfixpix\fR - Fix bad CCD lines and columns?
+The bad pixels (cosmetic defects) in the detector are given in a file
+specified by the parameter \fIfixfile\fR.  This information is used
+to replace the pixels by interpolating from the neighboring pixels.
+A standard file for your instrument may be set by \fBsetinstrument\fR
+or if the word "image" is given then the file is defined in the instrument
+data file.  For more on the bad pixel file see \fBinstruments\fR.
+.le
+.ls \fIoverscan\fR - Apply overscan strip correction?
+The overscan or prescan region is specified by the parameter
+\fIbiassec\fR.  This is given as an IRAF image section.  Only the
+part of the section corresponding to the readout axis is used and
+the other part is ignored.  The length of the overscan region is
+set by the \fItrimsec\fR parameter.  The overscan
+region is averaged along the readout axis, specified by the parameter
+\fIreadaxis\fR, to create a one dimensional bias vector.  This bias is
+fit by a function to remove cosmic rays and noise.  There are a number
+of parameters at the end of the parameter list which control the
+fitting.  The default overscan bias section and fitting parameters for
+your instrument should be set by \fBsetinstrument\fR.  If the word
+"image" is given the overscan bias section is defined in the image
+header or the instrument translation file.  If an overscan section is
+not set you can use \fBimplot\fR to determine the columns or rows for
+the bias region and define an overscan image section.  If you are
+unsure about image sections consult with someone or read the
+introductory IRAF documentation.
+.le
+.ls \fItrim\fR - Trim the image?
+The image is trimmed to the image section given by the parameter
+\fItrimsec\fR.  A default trim section for your instrument should be
+set by \fBsetinstrument\fR, however, you may override this default if
+desired.  If the word "image" is given the data
+image section is given in the image header or the instrument
+translation file.  As with the overscan image section it is
+straightforward to specify, but if you are unsure consult someone.
+.le
+.ls \fIzerocor\fR - Apply zero level correction?
+The zero level image to be subtracted is specified by the parameter
+\fIzero\fR.  If none is given then the calibration image will be sought
+in the list of images to be processed.
+.le
+.ls \fIdarkcor\fR - Apply dark count correction?
+The dark count image to be subtracted is specified by the parameter
+\fIdark\fR.  If none is given then the calibration image will be sought
+in the list of images to be processed.
+.le
+.ls \fIflatcor\fR - Apply flat field correction?
+The flat field images to be used are specified by the parameter
+\fIflat\fR.  There must be one flat field image for each filter
+or subset (see \fBsubsets\fR) to be processed.  If a flat field
+image is not given then the calibration image will be sought
+in the list of images to be processed.
+.le
+.ls \fIreadcor\fR - Convert zero level image to readout correction?
+If a one dimensional zero level readout correction vector is to be subtracted
+instead of a two dimensional zero level image then, when this parameter is set,
+the zero level images will be averaged to one dimension.  The readout axis
+must be specified by the parameter \fIreadaxis\fR.  The default for your
+instrument is set by \fBsetinstrument\fR.
+.le
+.ls \fIscancor\fR - Convert flat field image to scan correction?
+If the instrument is operated in a scan mode then a correction to the
+flat field may be required.  There are two types of scan modes, "shortscan"
+and "longscan".  In longscan mode flat field images will be averaged
+to one dimension and the readout axis must be specified.  Shortscan mode
+is a little more complicated.  The scan correction is used if the flat
+field images are not observed in scan mode.  The number of scan lines
+must be specified by the parameter \fInscan\fR.  If they are observed in
+scan mode, like the object observations, then the scan correction
+operations should \fInot\fR be specified.  For details of scan mode operations
+see \fBccdproc\fR.  The scan parameters
+should be set by \fBsetinstrument\fR.  If in doubt consult someone
+familiar with the instrument and mode of operation.
+.le
+
+     This description of the parameters is longer than the actual operation of
+setting the parameters.  The only parameters likely to change during processing
+are the calibration image parameters.
+
+     When processing many images using the same calibration files a modest
+performance improvement can be achieved by keeping (caching) the
+calibration images in memory to avoid disk accesses.  This option
+is available by specifying the amount of memory available for image
+caching with the parameter \fImax_cache\fR.  If the value is zero then
+the images are accessed from disk as needed while if there is
+sufficient memory the calibration images may be kept in memory during
+the task execution.
+.sh
+3. Processing Your Data
+
+     The processing path depends on the type of data, the type of
+instrument, types of calibration images, and the observing
+sequence.  In this section we describe two types of operations common
+in reducing most data; combining calibration images and performing the
+standard calibration and correction operations.  Some additional special
+operations are described in the following section.
+
+     However, the first thing you might want to try before any
+processing is to get a listing of the CCD images showing the CCD image
+types, subsets, and processing flags.  The task for this is
+\fBccdlist\fR.  It has three types of output; a short one line per
+image format, a longer format which shows the state of the processing,
+and a format which prints the image names only (used to create files
+containing lists of images of a particular CCD image type).  To get a
+quick listing type:
+
+.nf
+    cl> ccdlist *.imh
+    ccd001.imh[544,512][short][unknown][V]:FOCUS L98-193
+    ccd007.imh[544,512][short][object][V]:N2968 V 600s
+    ccd015.imh[544,512][short][object][B]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R]:N4036 R 600s
+    ccd045.imh[544,512][short][flat][V]:dflat 5s
+    ccd066.imh[544,512][short][flat][B]:dflat 5s
+    ccd103.imh[544,512][short][flat][R]:dflat 5s
+    ccd104.imh[544,512][short][zero][]:bias
+    ccd105.imh[544,512][short][dark][]:dark 3600s
+.fi
+
+     The example shows only a sample of the images.  The short format
+listing tells you the name of the image, its size and pixel type, the
+CCD image type as seen by the package, the subset identifier (in this
+case the filter), and the title.  If the data had been processed then
+there would also be processing flags.  If the CCD image types do not
+seem right then there may be a problem with the instrument
+specification.
+
+     Many of the tasks in the \fBccdred\fR package have the parameter
+\fIccdtype\fR which selects a particular type of image.  To list
+only the object images from the previous example:
+
+.nf
+    cl> ccdlist *.imh ccdtype=object
+    ccd007.imh[544,512][short][object][V]:N2968 V 600s
+    ccd015.imh[544,512][short][object][B]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R]:N4036 R 600s
+.fi
+
+If no CCD image type is specified (by using the null string "")
+then all image types are selected.  This may be
+necessary if your instrument data does not contain image type identifications.
+.sh
+3.1 Combining Calibration Images
+
+     If you do not need to combine calibration images because you only
+have one image of each type, you can skip this section.  Calibration
+images, particularly zero level and flat field images, are combined in
+order to minimize the effects of noise and reject bad pixels in the
+calibrations.  The basic tool for combining images is the task
+\fBcombine\fR.  There are simple variants of this task whose default
+parameters are set appropriately for each type of calibration image.
+These are the ones you will use for calibration images leaving
+\fBcombine\fR for combining object images.  Zero level images are
+combined with \fBzerocombine\fR, dark count images with
+\fBdarkcombine\fR, and flat field images with \fBflatcombine\fR.
+
+     For example, to combine flat field images the command is:
+
+.nf
+    cl> flatcombine *.imh
+    Jun  1 14:26 combine: maxreject
+            Images      N    Exp   Mode  Scale Offset Weight
+        ccd045.imh      1    5.0  INDEF  1.000     0.  0.048
+        ccd046.imh      1    5.0  INDEF  1.000     0.  0.048
+        	<... list of files ...>
+        ccd065.imh      1    5.0  INDEF  1.000     0.  0.048
+        ----------- ------ ------
+         FlatV.imh     21    5.0
+.fi
+
+This output is printed when verbose mode is set.  The same information
+is recorded in the log file.  In this case the flat fields are combined
+by rejecting the maximum value at each point in the image (the
+"maxreject" algorithm).  The images are scaled by the exposure times,
+which are all the same in this example.  The mode is not evaluated for
+exposure scaling and the relative weights are the same because the
+exposure times are the same.  The example only shows part of the
+output; \fBflatcombine\fR automatically groups the flat field images by
+filter to produce the calibration images "FlatV", "FlatB", and
+"FlatR".
+.sh
+3.2 Calibrations and Corrections
+
+     Processing the CCD data is easy and largely automated.
+First, set the task parameters with the following command:
+
+    cl> eparam ccdproc
+
+You may have already set the parameters when you ran
+\fBsetinstrument\fR, though the calibration image parameters
+\fIzero\fR, \fIdark\fR, and \fIflat\fR may still need to be set or
+changed.  Once this is done simply give the command
+
+.nf
+    cl> ccdproc *.imh
+    ccd003: Jun  1 15:13 Overscan section is [520:540,*] with mean=485.0
+    ccd003: Jun  1 15:14 Trim data section is [3:510,3:510]
+    ccd003: Jun  1 15:14 Overscan section is [520:540,*] with mean=485.0
+    FlatV:  Jun  1 15:14 Trim data section is [3:510,3:510]
+    FlatV:  Jun  1 15:15 Overscan section is [520:540,*] with mean=486.4
+    ccd003: Jun  1 15:15 Flat field image is FlatV.imh with scale=138.2
+    ccd004: Jun  1 15:16 Trim data section is [3:510,3:510]
+    ccd004: Jun  1 15:16 Overscan section is [520:540,*] with mean=485.2
+    ccd004: Jun  1 15:16 Flat field image is FlatV.imh with scale=138.2
+                <... more ...>
+    ccd013: Jun  1 15:22 Trim data section is [3:510,3:510]
+    ccd013: Jun  1 15:23 Overscan section is [520:540,*] with mean=482.4
+    FlatB:  Jun  1 15:23 Trim data section is [3:510,3:510]
+    FlatB:  Jun  1 15:23 Overscan section is [520:540,*] with mean=486.4
+    ccd013: Jun  1 15:24 Flat field image is FlatB.imh with scale=132.3
+                <... more ...>
+.fi
+
+     The output shown is with verbose mode set.  It is the same as
+recorded in the log file.  It illustrates the principle of automatic
+calibration image processing.  The first object image, "ccd003", was
+being processed when the flat field image was required.  Since the
+image was taken with the V filter the appropriate flat field was
+determined to be "FlatV".  Since it had not been processed, the
+processing of "ccd003" was interrupted to process "FlatV".  The
+processed calibration image may have been cached if there was enough
+memory.  Once "FlatV" was processed (note that the flat field was not
+flattened because the task knows this image is a flat field) the
+processing of "ccd003" was completed.  The next image, "ccd004", is
+also a V filter image so the already processed, and possibly cached,
+flat field "FlatV" is used again.  The first B band image is "ccd013"
+and, as before, the B filter flat field calibration image is processed
+automatically.  The same automatic calibration processing and image
+caching occurs when using zero level and dark count calibration
+images.
+
+     Commonly the processing is done with the verbose mode turned off
+and the task run as a background job.  This is done with the commands
+
+.nf
+    cl> ccdred.verbose=no
+    cl> ccdproc *.imh &
+.fi
+
+The already processed images in the input list are recognized as having been
+processed and are not affected.  To check the status of the processing we
+can look at the end of the log file with:
+
+    cl> tail logfile
+
+After processing we can repeat the \fBccdlist\fR command to find:
+
+.nf
+    cl> ccdlist *.imh ccdtype=object
+    ccd007.imh[508,508][real][object][V][OTF]:N2968 V 600s
+    ccd015.imh[508,508][real][object][B][OTF]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R][OTF]:N4036 R 600s
+.fi
+
+The processing flags indicate the images have been overscan corrected,
+trimmed, and flat fielded.
+
+     As you can see, processing images is very easy.  There is one source
+of minor confusion for beginning users and that is dealing with calibration
+images.  First, there is no reason that calibration images
+may not be processed explicitly with \fBccdproc\fR, just remember to set
+the \fIccdtype\fR to the calibration image type or to "".  When processing
+object images the calibration images to be used may be specified either
+with the task parameter for the particular calibration image or by
+including the calibration image in the list of input images.  Calibration
+images specified by parameter value take precedence and the task
+does not check its CCD image type.  Calibration images given in the
+input list must have a valid CCD image type.  In case too many
+calibration images are specified, say because the calibration images
+combined to make the master calibration images were not deleted and
+so are part of the image list "*.imh", only the first one will be used.
+Another point to know is that flat field, iillumination, and fringe images
+are subset (filter) dependent and so a calibration image for each filter
+must be specified.
+.sh
+4. Special Processing Operations
+
+     The special processing operations are mostly concerned with the
+flat field response correction.  There are also special processing
+operations available in \fBccdproc\fR for one dimensional readout
+corrections in the zero level and flat field calibrations.  These
+were described briefly above and in more detail in \fBccdproc\fR
+and are not discussed further in this guide.  The processing
+operations described in this section are for preparing flat fields
+for two dimensional spectroscopic data, for correcting flat fields
+for iilluminations effects, for making a separate iillumination correction,
+and for applying corrections for fringe effects.  For additional
+discussion about flat fields and iillumination corrections see the
+help topic \fBflatfields\fR.
+.sh
+4.1 Spectroscopic Flat Fields
+
+     For spectroscopic data the flat fields may have to be processed to
+remove the general shape of the lamp spectrum and to replace regions outside
+of the aperture where there is no flat field information with values that
+will not cause bad response effects when the flat field is applied to the
+data.  If the shape of the lamp spectrum is not important and if the
+longslit spectra have the regions outside of the slit either off the
+detector or trimmed then you may use the flat field without special
+processing.
+
+   First you must process the flat field images explicitly with
+
+    cl> ccdproc *.imh ccdtype=flat
+
+where "*.imh" may be replaced with any list containing the flat fields.
+If zero level and dark count corrections are required these calibration
+images must be available at this time.
+
+     Load the \fBtwodspec\fR package and then either the \fBlongslit\fR
+package, for longslit data, or the \fBapextract\fR package, for
+multiaperture data such as echelles, multifiber, or aperture mask
+spectra.  The task for removing the longslit quartz spectrum is
+\fBresponse\fR.  There is also a task for removing iillumination
+effects, including the slit profile, from longslit spectra called
+\fBiillumination\fR.  For more about processing longslit spectra see the
+help for these tasks and the paper \fIReduction of Longslit Spectra
+with IRAF\fR.  The cookbook \fIReduction of Longslit Spectroscopic
+Data Using IRAF (KPNO ICCD and Cryogenic Camera Data)\fR also provides
+a very good discussion even if your data is from a different instrument.
+
+     For multiaperture data the task for removing the relative shapes of
+the spectra is called \fBapnormalize\fR.  Again, consult the help documentation
+for this task for further details.  Since you will probably also be
+using the package for extracting the spectra you may be interested
+in the document \fIThe IRAF APEXTRACT Package\fR.
+.sh
+4.2 Iillumination Corrections
+
+     The flat field calibration images may not have the same iillumination
+pattern as the observations of the sky due to the way the lamp illuminates the
+optical system.  In this case when the flat field correction is applied
+to the data there will be gradients in the sky background.  To remove
+these gradients a blank sky calibration image is heavily smoothed
+to produce an iillumination image.  The iillumination image
+is then divided into the images during processing to correct for the
+iillumination difference between the flat field and the objects.
+Like the flat fields, the iillumination corrections images may be subset
+dependent so there should be an iillumination image for each subset.
+
+The task which makes iillumination correction images is \fBmkskycor\fR.
+Some examples are
+
+.nf
+    cl> mkskycor sky004 Illum004
+    cl> mkskycor sky*.imh ""
+.fi
+
+In the first example the sky image "sky004" is used to make the iillumination
+correction image "Illum004".  In the second example the sky images are
+converted to iillumination correction images by specifying no output image
+names.  Like \fBccdproc\fR if the input images have not been processed they
+are first processed automatically.
+
+To apply the iillumination correction
+
+.nf
+    cl> ccdproc *.imh ccdtype=object illumcor+ illum=Illum004
+    cl> ccdproc *.imh ccdtype=object illumcor+ illum=sky*.imh
+.fi
+
+The iillumination images could also be set using \fBeparam\fR or given
+on the command line.
+.sh
+4.3 Sky Flat Fields
+
+    You will notice that when you process images with an iillumination
+correction you are dividing each image by a flat field calibration and
+an iillumination correction.  If the iillumination corrections are not
+done as a later step but at the same time as the rest of the processing
+one will get the same calibration by multiplying the flat field by
+the iillumination correction and using this product alone as the
+flat field.  Such an image is called a \fIsky flat\fR since it is
+a flat field which has been corrected to yield a flat sky when applied
+to the observations.  This approach has the advantage of one less
+calibration image and two less computations (scaling and dividing the
+iillumination correction).  As an added short cut, rather than compute
+the iillumination image with \fBmkskycor\fR and then multiplying, the
+task \fBmkskyflat\fR does all this in one step.  Thus, \fBmkskyflat\fR
+takes an input blank sky image, processes it if needed, determines the
+appropriate flat field (sky flats are also subset dependent) from the
+\fBccdproc\fR parameters or the input image list, and produces an
+output sky flat.  Further if no output image is specified the task
+converts the input blank sky calibration image into a sky flat.
+
+     Two examples in which a new image is created and in which the
+input images are converted to sky flats are
+
+.nf
+    cl> mkskyflat sky004 Skyflat
+    cl> mkskyflat sky*.imh ""
+.fi
+.sh
+4.4 Iillumination Corrected Flat Fields
+
+     A third method to account for iillumination problems in the flat fields
+is to remove the large scale pattern from the flat field itself.  This is
+useful if there are no reasonable blank sky calibration images and the
+astronomical exposures are evenly illuminated but the flat fields are not.
+This is done by smoothing the flat field images instead of blank sky
+images.  As with using the sky images there are two methods, creating
+an iillumination correction to be applied as a separate step or fixing
+the original flat field.  The smoothing algorithm is
+the same as that used in the other tasks.  The tasks to make these types
+of corrections are \fBmkillumcor\fR and \fBmkillumflat\fR.  The usage
+is pretty much the same as the other iillumination correction tasks
+except that it is more reasonable to replace the original flat fields
+by the corrected flat fields when fixing the flat field.  Examples
+of an iillumination correction and removing the iillumination pattern
+from the flat field are
+
+.nf
+    cl> mkillumcor flat025 Illum025
+    cl> mkillumflat flat*.imh ""
+.fi
+
+As with the other tasks, the input images are processed if necessary.
+.sh
+4.5 Fringe Corrections
+
+    Some CCD detectors suffer from fringing effects due to the night
+sky emission lines which are not removed by the other calibration
+and correction operations.  To correct for the fringing you need a
+really blank sky image.  There is not yet a task to remove objects from
+sky images because this is often done with an interactive image display
+tool (which will soon be added).  The blank sky image is heavily smoothed
+to determine the mean sky background and then this is subtracted from the
+original image.  The image should then be essentially zero except for the
+fringe pattern.  This fringe correction image is scaled to the same
+exposure time as the image to be corrected and then subtracted to remove
+the fringing.  Note that since the night sky lines are variable there
+may need to be an additional scaling applied.  Determining this scaling
+requires either an interactive display tool or a very clever task.
+Such tasks will also be added in the future.
+
+     The task to make a fringe correction image is \fBmkfringecor\fR.
+the sky background is determined in exactly the same way as the iillumination
+pattern, in fact the same sky image may be used for both the sky
+iillumination and for the fringe correction.  The task works consistently
+with the "mk" tasks in that the input images are processed first if needed
+and then the output correction image is produced with the specified name
+or replaces the input image if no output image is specified.
+As examples,
+
+.nf
+    cl> mkfringecor sky004 Fringe
+    cl> mkfringecor sky*.imh ""
+.fi
+.sh
+5. Demonstration
+
+     A simple demonstration task is available.  To run this demonstration
+load the \fBccdtest\fR package; this is a subpackage of the main
+\fBccdred\fR package.  Then simply type
+
+	cl> demo
+
+The demonstration will then create some artificial CCD data and reduce
+them giving descriptive comments as it goes along.  This demonstration uses
+the "playback" facility of the command language and is actually substituting
+it's own commands for terminal input.  Initially you must type carriage return
+or space after each comment ending with "...".  If you wish to have the
+demonstration run completely automatically at it's own speed then type 'g'
+a the "..." prompt.  Thereafter, it will simple pause long enough to give
+you a chance to read the comments.  When the demo is finished you will
+need to remove the files created.  However, feel free to examine the reduced
+images, the log file, etc.  \fINote that the demonstration changes the
+setup parameters so be sure to run \fBsetinstrument\fI again and check
+the setup parameters.\fR
+.sh
+6. Summary
+
+     The \fBccdred\fR package is very easy to use.  First load the package;
+it is in the \fBimred\fR package which is in the \fBnoao\fR package.
+If this is your first time reducing data from a particular instrument
+or if you have changed instruments then run \fBsetinstrument\fR.
+Set the processing parameters for the operations you want performed.
+If you need to combine calibration images to form a master calibration
+image use one of the combine tasks.  Spectroscopic flat fields may
+need to be processed first in order to remove the lamp spectrum.
+Finally, just type
+
+    cl> ccdproc *.imh&
+.sh
+7. References
+
+     A general guide to using IRAF is \fIA User's Introduction to the IRAF
+Command Language\fR.  This document may be found in the IRAF documentation
+sets and is available from the National Optical Astronomy Observatories,
+Central Computer Services (NOAO-CCS).
+
+     A more detailed description of the \fBccdred\fR package including
+a discussion of the design and some of the algorithms see \fIThe IRAF
+CCD Reduction Package -- CCDRED\fR by F. Valdes.  This paper is available
+from NOAO-CCS and appears in the proceedings of the Santa Cruz Summer
+Workshop in Astronomy and Astrophysics, \fIInstrumentation for Ground-Based
+Optical Astronomy: Present and Future\fR, edited by Lloyd B. Robinson and
+published by Springer-Verlag.
+
+     The task descriptions and supplementary documentation are available
+in printed form in the IRAF documentation sets, a special set
+containing documentation for just the \fBccdred\fR package, and on-line
+through the help task by typing
+
+    cl> help \fItopic\fR
+
+where \fItopic\fR is one of the following.
+
+.nf
+  badpiximage - Create a bad pixel mask image from a bad pixel file
+    ccdgroups - Group CCD images into image lists
+     ccdhedit - CCD image header editor
+      ccdlist - List CCD processing information
+      ccdproc - Process CCD images
+      ccdtest - CCD test and demonstration package
+      combine - Combine CCD images
+   cosmicrays - Detect and replace cosmic rays
+  darkcombine - Combine and process dark count images
+  flatcombine - Combine and process flat field images
+  mkfringecor - Make fringe correction images from sky images
+   mkillumcor - Make flat field iillumination correction images
+  mkillumflat - Make iillumination corrected flat fields
+     mkskycor - Make sky iillumination correction images
+    mkskyflat - Make sky corrected flat field images
+setinstrument - Set instrument parameters
+  zerocombine - Combine and process zero level images
+
+          ADDITIONAL HELP TOPICS
+
+       ccdred - CCD image reduction package
+     ccdtypes - Description of the CCD image types
+   flatfields - Discussion of CCD flat field calibrations
+        guide - Introductory guide to using the CCDRED package
+  instruments - Instrument specific data files
+      subsets - Description of CCD subsets
+.fi
+
+Printed copies of the on-line help documentation may be made with the
+command
+
+    cl> help topic | lprint
+
+     In addition to the package documentation for \fBccdred\fR,
+\fBlongslit\fR, and \fBapextract\fR there may be specific guides for
+certain instruments.  These specific guides, called "cookbooks", give
+specific examples and parameter values for the CCD data.
+.endhelp
diff --git a/noao/imred/ccdred/doc/guide.ms b/noao/imred/ccdred/doc/guide.ms
new file mode 100644
index 00000000..62d87bb9
--- /dev/null
+++ b/noao/imred/ccdred/doc/guide.ms
@@ -0,0 +1,794 @@
+.RP
+.TL
+User's Guide to the CCDRED Package
+.AU
+Francisco Valdes
+.AI
+IRAF Group - Central Computer Services
+.K2
+P.O. Box 26732, Tucson, Arizona 85726
+June 1987
+Revised February 1988
+.AB
+The IRAF CCD reduction package, \fBccdred\fR, provides tools
+for the easy and efficient reduction of CCD images.  The standard
+reduction operations are replacement of bad pixels, subtraction of an
+overscan or prescan bias, subtraction of a zero level image,
+subtraction of a dark count image, division by a flat field calibration
+image, division by an illumination correction, subtraction of a fringe
+image, and trimming unwanted lines or columns.  Another common
+operation provided by the package is scaling and combining images with
+a number of algorithms for rejecting cosmic rays.  Data in the image
+header is used to make the reductions largely automated and
+self-documenting though the package may still be used in the absence of
+this data.  Also a translation mechanism is used to relate image header
+parameters to those used by the package to allow data from a variety of
+observatories and instruments to be processed.  This guide provides a brief
+description of the IRAF CCD reduction package and examples of reducing
+simple CCD data.
+.AE
+.NH
+Introduction
+.LP
+     This guide provides a brief description of the IRAF CCD reduction
+package \fBccdred\fR and examples of reducing simple CCD data.  It is a
+generic guide in that it is not tied to any particular type of data.
+There may be more specific guides (or "cookbooks") for your data.
+Detailed descriptions of the tasks and features of the package are
+provided in the help documentation for the package.
+
+     The purpose of the CCDRED package is to provide tools for the easy
+and efficient reduction of CCD images.  The standard reduction
+operations are replacement of bad columns and lines by interpolation
+from neighboring columns and lines, subtraction of a bias level
+determined from overscan or prescan columns or lines, subtraction of a
+zero level using a zero length exposure calibration image, subtraction
+of a dark count calibration image appropriately scaled to the dark time
+exposure, division by a scaled flat field calibration image, division
+by an illumination image (derived from a blank sky image), subtraction
+of a scaled fringe image (also derived from a blank sky image), and
+trimming the image of unwanted lines or columns such as the overscan
+strip.  Any set of operations may be done simultaneously over a list of
+images in a highly efficient manner.  The reduction operations are
+recorded in the image header and may also be logged on the terminal and
+in a log file.
+
+     The package also provides tools for combining multiple exposures
+of object and calibration images to improve the statistical accuracy of
+the observations and to remove transient bad pixels.  The combining
+operation scales images of different exposure times, adjusts for
+variable sky background, statistically weights the images by their
+signal-to-noise, and provides a number of useful algorithms for
+detecting and rejecting transient bad pixels.
+
+     Other tasks are provided for listing reduction information about
+the images, deriving secondary calibration images (such as sky
+corrected flat fields or illumination correction images), and easily
+setting the package parameters for different instruments.
+
+     There are several important features provided by the package to
+make the reduction of CCD images convenient; particularly to minimize
+record keeping.  One of these is the ability to recognize the different
+types of CCD images.  This ability allows the user to select a certain
+class of images to be processed or listed and allows the processing
+tasks to identify calibration images and process them differently from
+object images.  The standard CCD image types are \fIobject\fR,
+\fIzero\fR level, \fIdark\fR count, and \fIflat\fR field.  For more on
+the image types see \fBccdtypes\fR.
+
+     The tasks can also identify the different filters (or other subset
+parameter) which require different flat field images.  This means you don't
+have to separate the images by filter and process each set separately.
+This feature is discussed further in \fBsubsets\fR.
+
+     The tasks keep track of the reduction steps completed on each
+image and ignore images which have been processed.  This feature,
+along with recognizing the image types and subsets, makes it possible to
+specify all the images to a task with a wildcard template, such as
+"*.imh", rather than indicating each image by name.  You will find this
+extremely important with large sets of observations.
+
+     A fundamental aspect of the package is that the processing
+modifies the images.  In other words, the reduction operations are
+performed directly on the image.  This "feature" further simplifies
+record keeping, frees the user from having to form unique output image
+names, and minimizes the amount of disk space required.  There
+are two safety features in this process.  First, the modifications do
+not take effect until the operation is completed on the image.  This
+allows you to abort the task without messing up the image data and
+protects data if the computer crashes.  The second feature is that
+there is a package parameter which may be set to make a backup of the
+input data with a particular prefix such as "orig" or "imdir$".  This
+backup feature may be used when there is sufficient disk space, when learning
+to use the package, or just to be cautious.
+
+     In a similar effort to efficiently manage disk space, when combining
+images into a master object or calibration image there is an option to
+delete the input images upon completion of the combining operation.
+Generally this is desirable when there are many calibration exposures,
+such as zero level or flat field images, which are not used after they
+are combined into a final calibration image.
+
+     The following sections guide you through the basic use of the
+\fBccdred\fR package.  Only the important parameters which you might
+want to change are described.  It is assumed that the support personnel
+have created the necessary instrument files (see \fBinstruments\fR)
+which will set the default parameters for the data you will be
+reducing.  If this is not the case you may need to delve more deeply
+into the details of the tasks.  Information about all the parameters
+and how the various tasks operate are given in the help documentation
+for the tasks and in additional special help topics.  Some useful help
+documentation is indicated in the discussion and also in the
+\fBReferences\fR section.
+.NH
+Getting Started
+.LP
+     The first step is to load \fBccdred\fR.  This is done by loading
+the \fBnoao\fR package, followed by the image reduction package
+\fBimred\fR, and finally the \fBccdred\fR package.  Loading a
+package consists of typing its name.  Note that some of these packages may be
+loaded automatically when you logon to IRAF.
+
+     When you load the \fBccdred\fR package the menu of tasks or commands
+is listed.  This appears as follows:
+
+.nf
+.KS
+.ft L
+    cl> ccdred
+      badpiximage       ccdtest           mkfringecor       setinstrument
+      ccdgroups         combine           mkillumcor        zerocombine
+      ccdhedit          cosmicrays        mkillumflat       
+      ccdlist           darkcombine       mkskycor          
+      ccdproc           flatcombine       mkskyflat         
+.ft R
+.KE
+.fi
+
+A summary of the tasks and additional help topics is obtained by typing:
+
+.ft L
+    cl> help
+.ft R
+
+This list and how to get additional help on specific topics is described
+in the \fBReferences\fR section at the end of this guide.
+
+     The first command to use is \fBsetinstrument\fR, which sets the package
+appropriately for the CCD images to be reduced.  The support personnel
+should tell you the instrument identification, but if not a list
+of known instruments may be listed by using '?' for the instrument name.
+
+.nf
+.ft L
+    cl> setinstrument
+    Instrument ID (type ? for a list) \fI<enter instrument id or ?>
+        <Set ccdred package parameters using eparam>
+        <Set ccdproc task parameters using eparam>
+.ft R
+.fi
+
+This task sets the default parameters and then allows you to modify the
+package parameters and the processing parameters using the parameter
+editor \fBeparam\fR.  If you are not familiar with \fBeparam\fR see the
+help or CL introduction documentation.  For most terminals you move up
+and down through the parameters with the terminal arrow keys, you
+change the parameters by simply typing the desired value, and you exit
+with control Z or control D.  Note that you can change parameters for
+any task at any time with \fBeparam\fR and you do not have to run
+\fBsetinstrument\fR again, even if you logout, until you need to reduce
+data from a different instrument.
+
+     The \fBccdred\fR package parameters control general I/O functions of
+the tasks in the package.  The parameters you might wish to change are
+the output pixel type and the verbose option.  Except when the input
+images are short integers, the noise is significantly greater than one
+digital unit, and disk space is critical, it is probably better to
+allow the processing to convert the images to real pixel datatype.  The
+verbose parameter simply prints the information written to the log file
+on the terminal.  This can be useful when little else is being done and
+you are just beginning.  However, when doing background processing and
+other IRAF reduction tasks it is enough to simply look at the end of
+the logfile with the task \fBtail\fR to see the current state of the
+processing.
+
+     The \fBccdproc\fR parameters control the CCD processing.  There are
+many parameters but they all may be conveniently set at this point.
+Many of the parameters have default values set appropriately for the
+instrument you specified.  The images to be processed can be specified
+later.  What needs to be set are the processing operations that you
+want done and the parameters required for each operation.  The
+processing operations are selected by entering yes or no for each one.
+The following items briefly describe each of the possible processing
+operations and the additional parameters required.
+
+.LP
+\fIfixpix\fR - Fix bad CCD lines and columns?
+.IP
+The bad pixels (cosmetic defects) in the detector are given in a file
+specified by the parameter \fIfixfile\fR.  This information is used
+to replace the pixels by interpolating from the neighboring pixels.
+A standard file for your instrument may be set by \fBsetinstrument\fR
+or if the word "image" is given then the file is defined in the instrument
+data file.  For more on the bad pixel file see \fBinstruments\fR.
+.LP
+\fIoverscan\fR - Apply overscan strip correction?
+.IP
+The overscan or prescan region is specified by the parameter
+\fIbiassec\fR.  This is given as an IRAF image section.  The overscan
+region is averaged along the readout axis, specified by the parameter
+\fIreadaxis\fR, to create a one dimensional bias vector.  This bias is
+fit by a function to remove cosmic rays and noise.  There are a number
+of parameters at the end of the parameter list which control the
+fitting.  The default overscan bias section and fitting parameters for
+your instrument should be set by \fBsetinstrument\fR.  If the word
+"image" is given the overscan bias section is defined in the image
+header or the instrument translation file.  If an overscan section is
+not set you can use \fBimplot\fR to determine the columns or rows for
+the bias region and define an overscan image section.  If you are
+unsure about image sections consult with someone or read the
+introductory IRAF documentation.
+.LP
+\fItrim\fR - Trim the image?
+.IP
+The image is trimmed to the image section given by the parameter
+\fItrimsec\fR.  A default trim section for your instrument should be
+set by \fBsetinstrument\fR, however, you may override this default if
+desired.  If the word "image" is given the data
+image section is given in the image header or the instrument
+translation file.  As with the overscan image section it is
+straightforward to specify, but if you are unsure consult someone.
+.LP
+\fIzerocor\fR - Apply zero level correction?
+.IP
+The zero level image to be subtracted is specified by the parameter
+\fIzero\fR.  If none is given then the calibration image will be sought
+in the list of images to be processed.
+.LP
+\fIdarkcor\fR - Apply dark count correction?
+.IP
+The dark count image to be subtracted is specified by the parameter
+\fIdark\fR.  If none is given then the calibration image will be sought
+in the list of images to be processed.
+.LP
+\fIflatcor\fR - Apply flat field correction?
+.IP
+The flat field images to be used are specified by the parameter
+\fIflat\fR.  There must be one flat field image for each filter
+or subset (see \fBsubsets\fR) to be processed.  If a flat field
+image is not given then the calibration image will be sought
+in the list of images to be processed.
+.LP
+\fIreadcor\fR - Convert zero level image to readout correction?
+.IP
+If a one dimensional zero level readout correction vector is to be subtracted
+instead of a two dimensional zero level image then, when this parameter is set,
+the zero level images will be averaged to one dimension.  The readout axis
+must be specified by the parameter \fIreadaxis\fR.  The default for your
+instrument is set by \fBsetinstrument\fR.
+.LP
+\fIscancor\fR - Convert flat field image to scan correction?
+.IP
+If the instrument is operated in a scan mode then a correction to the
+flat field may be required.  There are two types of scan modes, "shortscan"
+and "longscan".  In longscan mode flat field images will be averaged
+to one dimension and the readout axis must be specified.  Shortscan mode
+is a little more complicated.  The scan correction is used if the flat
+field images are not observed in scan mode.  The number of scan lines
+must be specified by the parameter \fInscan\fR.  If they are observed in
+scan mode, like the object observations, then the scan correction
+operations should \fInot\fR be specified.  For details of scan mode operations
+see \fBccdproc\fR.  The scan parameters
+should be set by \fBsetinstrument\fR.  If in doubt consult someone
+familiar with the instrument and mode of operation.
+.LP
+
+     This description of the parameters is longer than the actual operation of
+setting the parameters.  The only parameters likely to change during processing
+are the calibration image parameters.
+
+     When processing many images using the same calibration files a modest
+performance improvement can be achieved by keeping (caching) the
+calibration images in memory to avoid disk accesses.  This option
+is available by specifying the amount of memory available for image
+caching with the parameter \fImax_cache\fR.  If the value is zero then
+the images are accessed from disk as needed while if there is
+sufficient memory the calibration images may be kept in memory during
+the task execution.
+.NH
+Processing Your Data
+.LP
+     The processing path depends on the type of data, the type of
+instrument, types of calibration images, and the observing
+sequence.  In this section we describe two types of operations common
+in reducing most data; combining calibration images and performing the
+standard calibration and correction operations.  Some additional special
+operations are described in the following section.
+
+     However, the first thing you might want to try before any
+processing is to get a listing of the CCD images showing the CCD image
+types, subsets, and processing flags.  The task for this is
+\fBccdlist\fR.  It has three types of of output; a short one line per
+image format, a longer format which shows the state of the processing,
+and a format which prints the image names only (used to create files
+containing lists of images of a particular CCD image type).  To get a
+quick listing type:
+
+.nf
+.ft L
+    cl> ccdlist *.imh
+    ccd001.imh[544,512][short][unknown][V]:FOCUS L98-193
+    ccd007.imh[544,512][short][object][V]:N2968 V 600s
+    ccd015.imh[544,512][short][object][B]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R]:N4036 R 600s
+    ccd045.imh[544,512][short][flat][V]:dflat 5s
+    ccd066.imh[544,512][short][flat][B]:dflat 5s
+    ccd103.imh[544,512][short][flat][R]:dflat 5s
+    ccd104.imh[544,512][short][zero][]:bias
+    ccd105.imh[544,512][short][dark][]:dark 3600s
+.ft R
+.fi
+
+     The example shows only a sample of the images.  The short format
+listing tells you the name of the image, its size and pixel type, the
+CCD image type as seen by the package, the subset identifier (in this
+case the filter), and the title.  If the data had been processed then
+there would also be processing flags.  If the CCD image types do not
+seem right then there may be a problem with the instrument
+specification.
+
+     Many of the tasks in the \fBccdred\fR package have the parameter
+\fIccdtype\fR which selects a particular type of image.  To list
+only the object images from the previous example:
+
+.nf
+.ft L
+    cl> ccdlist *.imh ccdtype=object
+    ccd007.imh[544,512][short][object][V]:N2968 V 600s
+    ccd015.imh[544,512][short][object][B]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R]:N4036 R 600s
+.ft R
+.fi
+
+If no CCD image type is specified (by using the null string "")
+then all image types are selected.  This may be
+necessary if your instrument data does not contain image type identifications.
+.NH 2
+Combining Calibration Images
+.LP
+     If you do not need to combine calibration images because you only
+have one image of each type, you can skip this section.  Calibration
+images, particularly zero level and flat field images, are combined in
+order to minimize the effects of noise and reject bad pixels in the
+calibrations.  The basic tool for combining images is the task
+\fBcombine\fR.  There are simple variants of this task whose default
+parameters are set appropriately for each type of calibration image.
+These are the ones you will use for calibration images leaving
+\fBcombine\fR for combining object images.  Zero level images are
+combined with \fBzerocombine\fR, dark count images with
+\fBdarkcombine\fR, and flat field images with \fBflatcombine\fR.
+
+     For example, to combine flat field images the command is:
+
+.nf
+.ft L
+    cl> flatcombine *.imh
+    Jun  1 14:26 combine: maxreject
+            Images      N    Exp   Mode  Scale Offset Weight
+        ccd045.imh      1    5.0  INDEF  1.000     0.  0.048
+        ccd046.imh      1    5.0  INDEF  1.000     0.  0.048
+        	\fI<... list of files ...>\fL
+        ccd065.imh      1    5.0  INDEF  1.000     0.  0.048
+        ----------- ------ ------
+         FlatV.imh     21    5.0
+.ft R
+.fi
+
+This output is printed when verbose mode is set.  The same information
+is recorded in the log file.  In this case the flat fields are combined
+by rejecting the maximum value at each point in the image (the
+"maxreject" algorithm).  The images are scaled by the exposure times,
+which are all the same in this example.  The mode is not evaluated for
+exposure scaling and the relative weights are the same because the
+exposure times are the same.  The example only shows part of the
+output; \fBflatcombine\fR automatically groups the flat field images by
+filter to produce the calibration images "FlatV", "FlatB", and
+"FlatR".
+.NH 2
+Calibrations and Corrections
+.LP
+     Processing the CCD data is easy and largely automated.
+First, set the task parameters with the following command:
+
+.ft L
+    cl> eparam ccdproc
+.ft R
+
+You may have already set the parameters when you ran
+\fBsetinstrument\fR, though the calibration image parameters
+\fIzero\fR, \fIdark\fR, and \fIflat\fR may still need to be set or
+changed.  Once this is done simply give the command
+
+.nf
+.ft L
+    cl> ccdproc *.imh
+    ccd003: Jun  1 15:13 Overscan section is [520:540,*] with mean=485.0
+    ccd003: Jun  1 15:14 Trim data section is [3:510,3:510]
+    ccd003: Jun  1 15:14 Overscan section is [520:540,*] with mean=485.0
+    FlatV:  Jun  1 15:14 Trim data section is [3:510,3:510]
+    FlatV:  Jun  1 15:15 Overscan section is [520:540,*] with mean=486.4
+    ccd003: Jun  1 15:15 Flat field image is FlatV.imh with scale=138.2
+    ccd004: Jun  1 15:16 Trim data section is [3:510,3:510]
+    ccd004: Jun  1 15:16 Overscan section is [520:540,*] with mean=485.2
+    ccd004: Jun  1 15:16 Flat field image is FlatV.imh with scale=138.2
+                \fI<... more ...>\fL
+    ccd013: Jun  1 15:22 Trim data section is [3:510,3:510]
+    ccd013: Jun  1 15:23 Overscan section is [520:540,*] with mean=482.4
+    FlatB:  Jun  1 15:23 Trim data section is [3:510,3:510]
+    FlatB:  Jun  1 15:23 Overscan section is [520:540,*] with mean=486.4
+    ccd013: Jun  1 15:24 Flat field image is FlatB.imh with scale=132.3
+                \fI<... more ...>\fL
+.ft R
+.fi
+
+     The output shown is with verbose mode set.  It is the same as
+recorded in the log file.  It illustrates the principle of automatic
+calibration image processing.  The first object image, "ccd003", was
+being processed when the flat field image was required.  Since the
+image was taken with the V filter the appropriate flat field was
+determined to be "FlatV".  Since it had not been processed, the
+processing of "ccd003" was interrupted to process "FlatV".  The
+processed calibration image may have been cached if there was enough
+memory.  Once "FlatV" was processed (note that the flat field was not
+flattened because the task knows this image is a flat field) the
+processing of "ccd003" was completed.  The next image, "ccd004", is
+also a V filter image so the already processed, and possibly cached,
+flat field "FlatV" is used again.  The first B band image is "ccd013"
+and, as before, the B filter flat field calibration image is processed
+automatically.  The same automatic calibration processing and image
+caching occurs when using zero level and dark count calibration
+images.
+
+     Commonly the processing is done with the verbose mode turned off
+and the task run as a background job.  This is done with the commands
+
+.nf
+.ft L
+    cl> ccdred.verbose=no
+    cl> ccdproc *.imh &
+.ft R
+.fi
+
+The already processed images in the input list are recognized as having been
+processed and are not affected.  To check the status of the processing we
+can look at the end of the log file with:
+
+.ft L
+    cl> tail logfile
+.ft R
+
+After processing we can repeat the \fBccdlist\fR command to find:
+
+.nf
+.ft L
+    cl> ccdlist *.imh ccdtype=object
+    ccd007.imh[508,508][real][object][V][OTF]:N2968 V 600s
+    ccd015.imh[508,508][real][object][B][OTF]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R][OTF]:N4036 R 600s
+.ft R
+.fi
+
+The processing flags indicate the images have been overscan corrected,
+trimmed, and flat fielded.
+
+     As you can see, processing images is very easy.  There is one source
+of minor confusion for beginning users and that is dealing with calibration
+images.  First, there is no reason that calibration images
+may not be processed explicitly with \fBccdproc\fR, just remember to set
+the \fIccdtype\fR to the calibration image type or to "".  When processing
+object images the calibration images to be used may be specified either
+with the task parameter for the particular calibration image or by
+including the calibration image in the list of input images.  Calibration
+images specified by parameter value take precedence and the task
+does not check its CCD image type.  Calibration images given in the
+input list must have a valid CCD image type.  In case too many
+calibration images are specified, say because the calibration images
+combined to make the master calibration images were not deleted and
+so are part of the image list "*.imh", only the first one will be used.
+Another point to know is that flat field, illumination, and fringe images
+are subset (filter) dependent and so a calibration image for each filter
+must be specified.
+.NH
+Special Processing Operations
+.LP
+     The special processing operations are mostly concerned with the
+flat field response correction.  There are also special processing
+operations available in \fBccdproc\fR for one dimensional readout
+corrections in the zero level and flat field calibrations.  These
+were described briefly above and in more detail in \fBccdproc\fR
+and are not discussed further in this guide.  The processing
+operations described in this section are for preparing flat fields
+for two dimensional spectroscopic data, for correcting flat fields
+for illuminations effects, for making a separate illumination correction,
+and for applying corrections for fringe effects.  For additional
+discussion about flat fields and illumination corrections see the
+help topic \fBflatfields\fR.
+.NH 2
+Spectroscopic Flat Fields
+.LP
+     For spectroscopic data the flat fields may have to be processed to
+remove the general shape of the lamp spectrum and to replace regions outside
+of the aperture where there is no flat field information with values that
+will not cause bad response effects when the flat field is applied to the
+data.  If the shape of the lamp spectrum is not important and if the
+longslit spectra have the regions outside of the slit either off the
+detector or trimmed then you may use the flat field without special
+processing.
+
+   First you must process the flat field images explicitly with
+
+.ft L
+    cl> ccdproc *.imh ccdtype=flat
+.ft R
+
+where "*.imh" may be replaced with any list containing the flat fields.
+If zero level and dark count corrections are required these calibration
+images must be available at this time.
+
+     Load the \fBtwodspec\fR package and then either the \fBlongslit\fR
+package, for longslit data, or the \fBapextract\fR package, for
+multiaperture data such as echelles, multifiber, or aperture mask
+spectra.  The task for removing the longslit quartz spectrum is
+\fBresponse\fR.  There is also a task for removing illumination
+effects, including the slit profile, from longslit spectra called
+\fBillumination\fR.  For more about processing longslit spectra see the
+help for these tasks and the paper \fIReduction of Longslit Spectra
+with IRAF\fR.  The cookbook \fIReduction of Longslit Spectroscopic
+Data Using IRAF (KPNO ICCD and Cryogenic Camera Data)\fR also provides
+a very good discussion even if your data is from a different instrument.
+
+     For multiaperture data the task for removing the relative shapes of
+the spectra is called \fBapnormalize\fR.  Again, consult the help documentation
+for this task for further details.  Since you will probably also be
+using the package for extracting the spectra you may be interested
+in the document \fIThe IRAF APEXTRACT Package\fR.
+.NH 2
+Illumination Corrections
+.LP
+     The flat field calibration images may not have the same illumination
+pattern as the observations of the sky due to the way the lamp illuminates the
+optical system.  In this case when the flat field correction is applied
+to the data there will be gradients in the sky background.  To remove
+these gradients a blank sky calibration image is heavily smoothed
+to produce an illumination image.  The illumination image
+is then divided into the images during processing to correct for the
+illumination difference between the flat field and the objects.
+Like the flat fields, the illumination corrections images may be subset
+dependent so there should be an illumination image for each subset.
+
+The task which makes illumination correction images is \fBmkskycor\fR.
+Some examples are
+
+.nf
+.ft L
+    cl> mkskycor sky004 Illum004
+    cl> mkskycor sky*.imh ""
+.ft R
+.fi
+
+In the first example the sky image "sky004" is used to make the illumination
+correction image "Illum004".  In the second example the sky images are
+converted to illumination correction images by specifying no output image
+names.  Like \fBccdproc\fR if the input images have not been processed they
+are first processed automatically.
+
+To apply the illumination correction
+
+.nf
+.ft L
+    cl> ccdproc *.imh ccdtype=object illumcor+ illum=Illum004
+    cl> ccdproc *.imh ccdtype=object illumcor+ illum=sky*.imh
+.ft R
+.fi
+
+The illumination images could also be set using \fBeparam\fR or given
+on the command line.
+.NH 2
+Sky Flat Fields
+.LP
+    You will notice that when you process images with an illumination
+correction you are dividing each image by a flat field calibration and
+an illumination correction.  If the illumination corrections are not
+done as a later step but at the same time as the rest of the processing
+one will get the same calibration by multiplying the flat field by
+the illumination correction and using this product alone as the
+flat field.  Such an image is called a \fIsky flat\fR since it is
+a flat field which has been corrected to yield a flat sky when applied
+to the observations.  This approach has the advantage of one less
+calibration image and two less computations (scaling and dividing the
+illumination correction).  As an added short cut, rather than compute
+the illumination image with \fBmkskycor\fR and then multiplying, the
+task \fBmkskyflat\fR does all this in one step.  Thus, \fBmkskyflat\fR
+takes an input blank sky image, processes it if needed, determines the
+appropriate flat field (sky flats are also subset dependent) from the
+\fBccdproc\fR parameters or the input image list, and produces an
+output sky flat.  Further if no output image is specified the task
+converts the input blank sky calibration image into a sky flat.
+
+     Two examples in which a new image is created and in which the
+input images are converted to sky flats are
+
+.nf
+.ft L
+    cl> mkskyflat sky004 Skyflat
+    cl> mkskyflat sky*.imh ""
+.ft R
+.fi
+.NH 2
+Illumination Corrected Flat Fields
+.LP
+     A third method to account for illumination problems in the flat fields
+is to remove the large scale pattern from the flat field itself.  This is
+useful if there are no reasonable blank sky calibration images and the
+astronomical exposures are evenly illuminated but the flat fields are not.
+This is done by smoothing the flat field images instead of blank sky
+images.  As with using the sky images there are two methods, creating
+an illumination correction to be applied as a separate step or fixing
+the original flat field.  The smoothing algorithm is
+the same as that used in the other tasks.  The tasks to make these types
+of corrections are \fBmkillumcor\fR and \fBmkillumflat\fR.  The usage
+is pretty much the same as the other illumination correction tasks
+except that it is more reasonable to replace the original flat fields
+by the corrected flat fields when fixing the flat field.  Examples
+of an illumination correction and removing the illumination pattern
+from the flat field are
+
+.nf
+.ft L
+    cl> mkillumcor flat025 Illum025
+    cl> mkillumflat flat*.imh ""
+.ft R
+.fi
+
+As with the other tasks, the input images are processed if necessary.
+.NH 2
+Fringe Corrections
+.LP
+    Some CCD detectors suffer from fringing effects due to the night
+sky emission lines which are not removed by the other calibration
+and correction operations.  To correct for the fringing you need a
+really blank sky image.  There is not yet a task to remove objects from
+sky images because this is often done with an interactive image display
+tool (which will soon be added).  The blank sky image is heavily smoothed
+to determine the mean sky background and then this is subtracted from the
+original image.  The image should then be essentially zero except for the
+fringe pattern.  This fringe correction image is scaled to the same
+exposure time as the image to be corrected and then subtracted to remove
+the fringing.  Note that since the night sky lines are variable there
+may need to be an additional scaling applied.  Determining this scaling
+requires either an interactive display tool or a very clever task.
+Such tasks will also be added in the future.
+
+     The task to make a fringe correction image is \fBmkfringecor\fR.
+the sky background is determined in exactly the same way as the illumination
+pattern, in fact the same sky image may be used for both the sky
+illumination and for the fringe correction.  The task works consistently
+with the "mk" tasks in that the input images are processed first if needed
+and then the output correction image is produced with the specified name
+or replaces the input image if no output image is specified.
+As examples,
+
+.nf
+.ft L
+    cl> mkfringecor sky004 Fringe
+    cl> mkfringecor sky*.imh ""
+.ft R
+.fi
+.NH
+Demonstration
+.LP
+     A simple demonstration task is available.  To run this demonstration
+load the \fBccdtest\fR package; this is a subpackage of the main
+\fBccdred\fR package.  Then simply type
+
+.ft L
+	cl> demo
+.ft R
+
+The demonstration will then create some artificial CCD data and reduce
+them giving descriptive comments as it goes along.  This demonstration uses
+the "playback" facility of the command language and is actually substituting
+it's own commands for terminal input.  Initially you must type carriage return
+or space after each comment ending with "...".  If you wish to have the
+demonstration run completely automatically at it's own speed then type 'g'
+a the "..." prompt.  Thereafter, it will simple pause long enough to give
+you a chance to read the comments.  When the demo is finished you will
+need to remove the files created.  However, feel free to examine the reduced
+images, the log file, etc.  \fINote that the demonstration changes the
+setup parameters so be sure to run \fBsetinstrument\fI again and check
+the setup parameters.\fR
+.NH
+Summary
+.LP
+     The \fBccdred\fR package is very easy to use.  First load the package;
+it is in the \fBimred\fR package which is in the \fBnoao\fR package.
+If this is your first time reducing data from a particular instrument
+or if you have changed instruments then run \fBsetinstrument\fR.
+Set the processing parameters for the operations you want performed.
+If you need to combine calibration images to form a master calibration
+image use one of the combine tasks.  Spectroscopic flat fields may
+need to be processed first in order to remove the lamp spectrum.
+Finally, just type
+
+.ft L
+    cl> ccdproc *.imh&
+.ft R
+.SH
+References
+.LP
+     A general guide to using IRAF is \fIA User's Introduction to the IRAF
+Command Language\fR.  This document may be found in the IRAF documentation
+sets and is available from the National Optical Astronomy Observatories,
+Central Computer Services (NOAO-CCS).
+
+     A more detailed description of the \fBccdred\fR package including
+a discussion of the design and some of the algorithms see \fIThe IRAF
+CCD Reduction Package -- CCDRED\fR" by F. Valdes.  This paper is available
+from NOAO-CCS and appears in the proceedings of the Santa Cruz Summer
+Workshop in Astronomy and Astrophysics, \fIInstrumentation for Ground-Based
+Optical Astronomy: Present and Future\fR, edited by Lloyd B. Robinson and
+published by Springer-Verlag.
+
+     The task descriptions and supplementary documentation are available
+in printed form in the IRAF documentation sets, a special set
+containing documentation for just the \fBccdred\fR package, and on-line
+through the help task by typing
+
+.ft L
+    cl> help \fItopic\fR
+.ft R
+
+where \fItopic\fR is one of the following.
+
+.nf
+.ft L
+  badpiximage - Create a bad pixel mask image from a bad pixel file
+    ccdgroups - Group CCD images into image lists
+     ccdhedit - CCD image header editor
+      ccdlist - List CCD processing information
+      ccdproc - Process CCD images
+      ccdtest - CCD test and demonstration package
+      combine - Combine CCD images
+   cosmicrays - Detect and replace cosmic rays
+  darkcombine - Combine and process dark count images
+  flatcombine - Combine and process flat field images
+  mkfringecor - Make fringe correction images from sky images
+   mkillumcor - Make flat field illumination correction images
+  mkillumflat - Make illumination corrected flat fields
+     mkskycor - Make sky illumination correction images
+    mkskyflat - Make sky corrected flat field images
+setinstrument - Set instrument parameters
+  zerocombine - Combine and process zero level images
+
+          ADDITIONAL HELP TOPICS
+
+       ccdred - CCD image reduction package
+     ccdtypes - Description of the CCD image types
+   flatfields - Discussion of CCD flat field calibrations
+        guide - Introductory guide to using the CCDRED package
+  instruments - Instrument specific data files
+      subsets - Description of CCD subsets
+.ft R
+.fi
+
+Printed copies of the on-line help documentation may be made with the
+command
+
+.ft L
+    cl> help \fItopic\fL | lprint
+.ft R
+
+     In addition to the package documentation for \fBccdred\fR,
+\fBlongslit\fR, and \fBapextract\fR there may be specific guides for
+certain instruments.  These specific guides, called "cookbooks", give
+specific examples and parameter values for the CCD data.
diff --git a/noao/imred/ccdred/doc/instruments.hlp b/noao/imred/ccdred/doc/instruments.hlp
new file mode 100644
index 00000000..95baff37
--- /dev/null
+++ b/noao/imred/ccdred/doc/instruments.hlp
@@ -0,0 +1,256 @@
+.help instruments Dec93 noao.imred.ccdred
+
+.ih
+NAME
+instruments -- Instrument specific data files
+.ih
+DESCRIPTION
+The \fBccdred\fR package has been designed to accommodate many different
+instruments, detectors, and observatories.  This is done by having
+instrument specific data files.  Note that by instrument we mean a
+combination of detector, instrument, application, and observatory, so
+there might be several "instruments" associated with a particular CCD
+detector.  Creating and maintaining the instrument files is generally
+the responsibility of the support staff, though the user may create or
+copy and modify his/her own instrument/application specific files.  The
+task \fBsetinstrument\fR makes this information available to the user
+and package easily.
+
+There are three instrument data files, all of which are optional.  The
+package may be used without the instrument files but much of the
+convenience of the package, particularly with respect to using the CCD
+image types, will be lost.  The three files are an instrument image
+header translation file, an initialization task which mainly sets
+default task parameters, and a bad pixel file identifying the cosmic
+bad pixels in the detector.  These files are generally stored in a
+system data directory which is a subdirectory of the logical
+directory "ccddb$".  Each file has a root name which identifies the
+instrument.
+.sh
+1. Instrument Translation File
+The instrument translation file translates the parameter names used by
+the \fBccdred\fR pacakge into instrument specific parameters and also
+supplies instrument specific default values.  The package parameter
+\fIccdred.instrument\fR specifies this file to the package.  The task
+\fBsetinstrument\fR sets this parameter, though it can be set
+explicitly like any other parameter.  For the standard instrument
+translation file the root name is the instrument identification and the
+extension is "dat" ("*.dat" files are protected from being removed in a
+"stripped" system, i.e. when all nonessential files are removed).
+Private instrument files may be given any name desired.
+
+The instrument translation proceeds as follows.  When a package task needs
+a parameter for an image, for example "imagetyp", it looks in the instrument
+translation file.  If the file is not found or none is specified then the
+image header keyword that is requested has the same name.  If an
+instrument translation file is defined then the requested
+parameter is translated to an image header keyword, provided a translation
+entry is given.  If no translation is given the package name is used.  For
+example the package parameter "imagetyp" might be translated to "data-typ"
+(the old NOAO CCD keyword).  If the parameter is not found then the default
+value specified in the translation file, if present, is returned.  For recording
+parameter information in the header, such as processing flags, the
+translation is also used.  The default value has no meaning in this case.
+For example, if the flag specifying that the image has been corrected
+by a flat field is to be set then the package parameter name "flatcor"
+might be translated to "ff-flag".  If no translation is given then the
+new image header parameter is entered as "flatcor".
+
+The format of the translation file are lines consisting of the package
+parameter name, followed by the image header keyword, followed by the
+default value.  The first two fields are parameter names.  The fields
+are separated by whitespace (blanks and tabs).  String  default values
+containing blanks must be quoted.  An example is given below.
+
+.nf
+    # Sample translation file.
+    exptime     itime
+    darktime    itime
+    imagetyp    data-typ
+    subset      f1pos
+    biassec     biassec    [411:431,2:573]
+    datasec     datasec    [14:385,2:573]
+
+    fixpix      bp-flag    0
+    overscan    bt-flag    0
+    zerocor     bi-flag    0
+    darkcor     dk-flag    0
+    flatcor     ff-flag    0
+    fringcor    fr-flag    0 
+.fi
+
+The first comment line is ignored as are blank lines.
+The first two lines translate the CCD image type, and the subset parameter
+without default values (see \fBccdtypes\fR and \fBsubsets\fR for more
+information).  The next two lines give the overscan bias strip
+section and the data section with default values for the instrument.
+Note that these parameters may be overridden in the task \fBccdproc\fR.
+
+The next set of translations requires further discussion.  For processing
+flags the package assumes that the absence of a keyword means that the
+processing has not been done.  If processing is always to be done with
+the \fBCCDRED\fR package and no processing keywords are recorded in the raw data
+then these parameters should be absent (unless you don't like the names
+used by the package).  However, for compatibility with the original NOAO
+CCD images, which may be processed outside of IRAF and which use 0 as the
+no processing value, the processing flags are translated and the false values
+are indicated by the default values.
+
+If there is more than one translation for the same CCDRED parameter,
+for example more than one exptime, then the last one is used.
+
+In addition to the parameter name translations the translation file
+contains translations between the value of the image type parameter
+and the image types used by the package.  These lines
+consist of the image header type string as the first field (with quotes
+if there are blanks) and the image type as recognized by the package.  The
+following example will make this clearer.
+
+.nf
+	'OBJECT (0)'		object
+	'DARK (1)'		dark
+	'PROJECTOR FLAT (2)'	flat
+	'SKY FLAT (3)'		other
+	'COMPARISON LAMP (4)'	other
+	'BIAS (5)'		zero
+	'DOME FLAT (6)'		flat
+.fi
+
+The values of the image type strings in the header contain blanks so they
+are quoted.  Also the case of the strings is important.  Note that there
+are two types of flat field images and three types of object images.
+
+The CCD image types recognized by the package are:
+
+.nf
+	zero   - zero level image such as a bias or preflash
+	dark   - dark count image
+	flat   - flat field image
+	illum  - iillumination image such as a sky image
+	fringe - fringe correction image
+	object - object image
+.fi
+
+There may be more than one image type that maps to the same package
+type.  In particular other standard CCD image types, such as comparison
+spectra, multiple exposure, standard star, etc., should be mapped to
+object or other.  There may also be more than one type of flat field,
+i.e. dome flat, sky flat, and lamp flat.  For more on the CCD image
+types see \fBccdtypes\fR.
+
+The complete set of package parameters are given below.
+The package parameter names are generally the same as the
+standard image header keywords being adopted by NOAO.
+
+.nf
+	General Image Header and Default Parameters
+    ccdmean		darktime	exptime		fixfile
+    imagetyp		ncombine	biassec		subset
+    title		datasec         nscanrow
+
+	       CCDRED Processing Flags
+    ccdproc		darkcor		fixpix		flatcor
+    fringcor		illumcor	overscan	trim
+    zerocor
+
+	       CCDRED CCD Image Types
+    dark		flat		fringe		illum
+    none		object		unknown		zero
+.fi
+
+The translation mechanism described here may become more
+sophisticated in the future and a general IRAF system facility may be
+implemented eventually.  For the present the translation mechanism is
+quite simple.
+.sh
+2. Instrument Setup Script
+The task \fBsetinstrument\fR translates an instrument ID into a
+CL script in the instrument directory.  This script is then executed.
+Generally this script simply sets the task parameters for an
+instrument/application.  However, it could do anything else the support
+staff desires.  Below are the first few lines of a typical instrument setup
+script.
+
+.nf
+	ccdred.instrument = "ccddb$kpno/example.dat"
+	ccdred.pixeltype = "real"
+	ccdproc.fixpix = yes
+	ccdproc.overscan = yes
+	ccdproc.trim = yes
+	ccdproc.zerocor = no
+	ccdproc.darkcor = no
+	ccdproc.flatcor = yes
+	ccdproc.biassec = "[411:431,2:573]"
+	ccdproc.datasec = "[14:385,2:573]"
+.fi
+
+The instrument parameter should always be set unless there is no
+translation file for the instrument.  The \fBccdproc\fR parameters
+illustrate setting the appropriate processing flags for the
+instrument.  The overscan bias and trim data sections show an alternate
+method of setting these instrument specific parameters.  They may be
+set in the setup script in which case they are given explicitly in the
+user parameter list for \fBccdproc\fR.  If the value is "image" then
+the parameters may be determined either through the default value in
+the instrument translation file, as illustrated in the previous
+section, or from the image header itself.
+
+The instrument setup script for setting default task parameters may be
+easily created by the support person as follows.  Set the package
+parameters using \fBeparam\fR or with CL statements.  Setting the
+parameters might involve testing.  When satisfied with the way the
+package is set then the parameters may be dumped to a setup script
+using the task \fBdparam\fR.  The final step is editing this script to
+delete unimportant and query parameters.  For example,
+
+.nf
+	cl> dparam ccdred >> file.cl
+	cl> dparam ccdproc >> file.cl
+	cl> dparam combine >> file.cl
+		...
+	cl> ed file.cl
+.fi
+.sh
+3. Instrument Bad Pixel File
+The bad pixel file describes the bad pixels, columns, and lines in the
+detector which are to be replaced by interpolation when processing the
+images.  This file is clearly detector specific.  The file consists of
+lines describing rectangular regions of the image.
+The regions are specified by four numbers giving the starting and ending
+columns followed by the starting and ending lines.  The starting and
+ending points may be the same to specify a single column or line.  The
+example below illustrates a bad pixel file.
+
+.nf
+	# RCA1 CCD untrimmed
+	25 25 1 512
+	108 108 1 512
+	302 302 403 512
+	1 512 70 70
+	245 246 312 315
+.fi
+
+If there is a comment line in the file containing the word "untrimmed"
+then the coordinates of the bad pixel regions apply to the original CCD
+detector coordinates.
+If the image has been trimmed and the bad pixels are replaced at a later
+stage then this word indicates that the trim region be determined from the
+image header and the necessary coordinate conversion made to the original
+CCD pixel coordinates.  Note that if a subraster readout is used the
+coordinates must still refer to the original CCD coordinates and
+not the raw, untrimmed readout image.  If the word
+"untrimmed" does not appear then the coordinates are assumed to apply to
+the image directly; i.e. the trimmed coordinates if the image has been
+trimmed or the original coordinates if the image has not been trimmed.
+The standard bad pixel files should always refer to the original, untrimmed
+coordinates.
+
+The first two bad pixel regions are complete bad columns (the image
+is 512 x 512), the next line is a partial bad column, the next line is
+a bad line, and the last line is a small bad region.  These files are
+easy to create, provided you have a good image to work from and a way
+to measure the positions with an image or graphics display.
+.ih
+SEE ALSO
+ccdtypes, subsets, setinstrument
+.endhelp
diff --git a/noao/imred/ccdred/doc/mkfringecor.hlp b/noao/imred/ccdred/doc/mkfringecor.hlp
new file mode 100644
index 00000000..797f4d11
--- /dev/null
+++ b/noao/imred/ccdred/doc/mkfringecor.hlp
@@ -0,0 +1,90 @@
+.help mkfringecor Feb88 noao.imred.ccdred
+.ih
+NAME
+mkfringecor -- Make fringe correction images from sky images
+.ih
+USAGE
+mkfringecor input output
+.ih
+PARAMETERS
+.ls input
+List of input images for making fringe correction images.
+.le
+.ls output
+List of output fringe correction images.  If none is
+specified or if the name is the same as the input image then the output
+image replaces the input image.
+.le
+.ls ccdtype = ""
+CCD image type to select from the input images.  If none is specified
+then all types are used.
+.le
+.ls xboxmin = 5, xboxmax = 0.25, yboxmin = 5, yboxmax = 0.25
+Minimum and maximum smoothing box size along the x and y axes.  The
+minimum box size is used at the edges and grows to the maximum size in
+the middle of the image.  This allows the smoothed image to better
+represent gradients at the edge of the image.  If a size is less then 1
+then it is interpreted as a fraction of the image size.  If a size is
+greater than or equal to 1 then it is the box size in pixels.  A size
+greater than the size of image selects a box equal to the size of the
+image.
+.le
+.ls clip = yes
+Clean the input images of objects?  If yes then a clipping algorithm is
+used to detect and exclude objects from the smoothing.
+.le
+.ls lowsigma = 2.5, highsigma = 2.5
+Sigma clipping thresholds above and below the smoothed background.
+.le
+.ls ccdproc (parameter set)
+CCD processing parameters.
+.le
+.ih
+DESCRIPTION
+The input blank sky images are automatically processed up through the
+iillumination correction before computing the fringe correction images.
+The fringe corrections are subset dependent.
+The slowly varying background is determined and subtracted leaving only
+the fringe pattern caused by the sky emission lines.  These fringe images
+are then scaled and subtracted from the observations by \fBccdproc\fR.
+The background is determined by heavily smoothing the image using a
+moving "boxcar" average.  The effects of the objects and fringes in the
+image is minimized by using a sigma clipping algorithm to detect and
+exclude them from the average.  Note, however, that objects left in the
+fringe image will affect the fringe corrected observations.  Any objects
+in the sky image should be removed using \fBskyreplace\fR (not yet
+available).
+
+The smoothing algorithm is a moving average over a two dimensional
+box.  The algorithm is unconvential in that the box size is not fixed.
+The box size is increased from the specified minimum at the edges to
+the maximum in the middle of the image.  This permits a better estimate
+of the background at the edges, while retaining the very large scale
+smoothing in the center of the image.  Note that the sophisticated
+tools of the \fBimages\fR package may be used for smoothing but this
+requires more of the user and, for the more sophisticated smoothing
+algorithms such as surface fitting, more processing time.
+
+To minimize the effects of the fringes and any objects in the blank sky
+calibration images a sigma clipping algorithm is used to detect and
+exclude features from the background.  This is done by computing the
+rms of the image lines relative to the smoothed background and
+excluding points exceeding the specified threshold factors times the
+rms.  This is done before each image line is added to the moving
+average, except for the first few lines where an iterative process is
+used.
+.ih
+EXAMPLES
+1. The two examples below make an fringe correction image from a blank
+sky image, "sky017".  In the first example a separate fringe
+image is created and in the second the fringe image replaces the
+sky image.
+
+.nf
+    cl> mkskycor sky017 Fringe
+    cl> mkskycor sky017 frg017
+.fi
+.ih
+SEE ALSO
+ccdproc
+.endhelp
diff --git a/noao/imred/ccdred/doc/mkillumcor.hlp b/noao/imred/ccdred/doc/mkillumcor.hlp
new file mode 100644
index 00000000..0effd7a2
--- /dev/null
+++ b/noao/imred/ccdred/doc/mkillumcor.hlp
@@ -0,0 +1,92 @@
+.help mkillumcor Oct88 noao.imred.ccdred
+.ih
+NAME
+mkillumcor -- Make flat field iillumination correction images
+.ih
+USAGE
+mkillumcor input output
+.ih
+PARAMETERS
+.ls input
+List of input images for making flat field iillumination correction images.
+.le
+.ls output
+List of output flat field iillumination correction images.  If none is
+specified or if the name is the same as the input image then the output
+image replaces the input image.
+.le
+.ls ccdtype = "flat"
+CCD image type to select from the input images.  If none is specified
+then all types are used.
+.le
+.ls xboxmin = 5, xboxmax = 0.25, yboxmin = 5, yboxmax = 0.25
+Minimum and maximum smoothing box size along the x and y axes.  The
+minimum box size is used at the edges and grows to the maximum size in
+the middle of the image.  This allows the smoothed image to better
+represent gradients at the edge of the image.  If a size is less then 1
+then it is interpreted as a fraction of the image size.  If a size is
+greater than or equal to 1 then it is the box size in pixels.  A size
+greater than the size of image selects a box equal to the size of the
+image.
+.le
+.ls clip = yes
+Clean the input images of objects?  If yes then a clipping algorithm is
+used to detect and exclude deviant points from the smoothing.
+.le
+.ls lowsigma = 2.5, highsigma = 2.5
+Sigma clipping thresholds above and below the smoothed iillumination.
+.le
+.ls divbyzero = 1.
+The iillumination correction is the inverse of the smoothed flat field.
+This may produce division by zero.  A warning is given if division
+by zero takes place and the result (the iillumination correction value)
+is replaced by the value of this parameter.
+.le
+.ls ccdproc (parameter set)
+CCD processing parameters.
+.le
+.ih
+DESCRIPTION
+First, the input flat field images are automatically processed if
+needed.  Then, the large scale iillumination pattern of the images is
+determined by heavily smoothing them using a moving "boxcar" average.
+The iillumination correction, the inverse of the iillumination pattern,
+is applied by \fBccdproc\fR to CCD images to remove the iillumination
+pattern introduced by the flat field.  The combination of the flat
+field calibration and the iillumination correction based on the flat
+field is equivalent to removing the iillumination from the flat field
+(see \fBmkillumflat\fR).  This two step calibration is generally used
+when the observations have been previously flat field calibrated.  This
+task is closely related to \fBmkskycor\fR which determines the
+iillumination correction from a blank sky image; this is preferable to
+using the iillumination from the flat field as it corrects for the
+residual iillumination error.  For a general discussion of the options
+for flat fields and iillumination corrections see \fBflatfields\fR.
+
+The smoothing algorithm is a moving average over a two dimensional
+box.  The algorithm is unconvential in that the box size is not fixed.
+The box size is increased from the specified minimum at the edges to
+the maximum in the middle of the image.  This permits a better estimate
+of the background at the edges, while retaining the very large scale
+smoothing in the center of the image.  Note that the sophisticated
+tools of the \fBimages\fR package may be used for smoothing but this
+requires more of the user and, for the more sophisticated smoothing
+algorithms such as surface fitting, more processing time.
+
+To minimize the effects of bad pixels a sigma clipping algorithm is
+used to detect and reject these pixels from the iillumination.  This is
+done by computing the rms of the image lines relative to the smoothed
+iillumination and excluding points exceeding the specified threshold
+factors times the rms.  This is done before each image line is added to
+the moving average, except for the first few lines where an iterative
+process is used.
+.ih
+EXAMPLES
+1. The example below makes an iillumination correction image from the
+flat field image, "flat017".
+
+    cl> mkillumcor flat017 Illum
+.ih
+SEE ALSO
+ccdproc, flatfields, mkillumflat, mkskycor, mkskyflat
+.endhelp
diff --git a/noao/imred/ccdred/doc/mkillumflat.hlp b/noao/imred/ccdred/doc/mkillumflat.hlp
new file mode 100644
index 00000000..8288fb85
--- /dev/null
+++ b/noao/imred/ccdred/doc/mkillumflat.hlp
@@ -0,0 +1,101 @@
+.help mkillumflat Oct88 noao.imred.ccdred
+.ih
+NAME
+mkillumflat -- Make illumination corrected flat fields
+.ih
+USAGE
+mkillumflat input output
+.ih
+PARAMETERS
+.ls input
+List of input flat field images to be illumination corrected.
+.le
+.ls output
+List of output illumination corrected flat field images.
+If none is specified or if the name is the same as the
+input image then the output image replaces the input image.
+.le
+.ls ccdtype = "flat"
+CCD image type to select from the input images.
+.le
+.ls xboxmin = 5, xboxmax = 0.25, yboxmin = 5, yboxmax = 0.25
+Minimum and maximum smoothing box size along the x and y axes.  The
+minimum box size is used at the edges and grows to the maximum size in
+the middle of the image.  This allows the smoothed image to better
+represent gradients at the edge of the image.  If a size is less then 1
+then it is interpreted as a fraction of the image size.  If a size is
+greater than or equal to 1 then it is the box size in pixels.  A size
+greater than the size of image selects a box equal to the size of the
+image.
+.le
+.ls clip = yes
+Clean the input images of objects?  If yes then a clipping algorithm is
+used to detect and exclude objects from the smoothing.
+.le
+.ls lowsigma = 2.5, highsigma = 2.5
+Sigma clipping thresholds above and below the smoothed illumination.
+.le
+.ls divbyzero = 1.
+The illumination flat field is the ratio of the flat field to a
+smoothed flat field.  This may produce division by zero.  A warning is
+given if division by zero takes place and the result (the illumination
+corrected flat field value) is replaced by the value of this
+parameter.
+.le
+.ls ccdproc (parameter set)
+CCD processing parameters.
+.le
+.ih
+DESCRIPTION
+First, the input flat field images are processed as needed.  Then the
+large scale illumination pattern of the images is removed.  The
+illumination pattern is determined by heavily smoothing the image using
+a moving "boxcar" average.  The output image is the ratio of the input
+image to the illumination pattern.  The illumination pattern is
+normalized by its mean to preserve the mean level of the input image.
+
+When this task is applied to flat field images only the small scale
+response effects are retained.  This is appropriate if the flat field
+images have illumination effects which differ from the astronomical
+images and blank sky images are not available for creating sky
+corrected flat fields.  When a high quality blank sky image is
+available the related task \fBmkskyflat\fR should be used.  Note that
+the illumination correction, whether from the flat field or a sky
+image, may be applied as a separate step by using the task
+\fBmkillumcor\fR or \fBmkskycor\fR and applying the illumination
+correction as a separate operation in \fBccdproc\fR.  However, creating
+an illumination corrected flat field image before processing is more
+efficient since one less operation per image processed is needed.  For
+more discussion about flat fields and illumination corrections see
+\fBflatfields\fR.
+
+The smoothing algorithm is a moving average over a two dimensional
+box.  The algorithm is unconvential in that the box size is not fixed.
+The box size is increased from the specified minimum at the edges to
+the maximum in the middle of the image.  This permits a better estimate
+of the background at the edges, while retaining the very large scale
+smoothing in the center of the image.  Note that the sophisticated
+tools of the \fBimages\fR package may be used for smoothing but this
+requires more of the user and, for the more sophisticated smoothing
+algorithms such as surface fitting, more processing time.
+
+To minimize the effects of bad pixels a sigma clipping algorithm is
+used to detect and reject these pixels from the illumination.  This is
+done by computing the rms of the image lines relative to the smoothed
+illumination and excluding points exceeding the specified threshold
+factors times the rms.  This is done before each image line is added to
+the moving average, except for the first few lines where an iterative
+process is used.
+.ih
+EXAMPLES
+1. Two examples in which a new image is created and in which the
+input flat fields are corrected in place are:
+
+.nf
+    cl> mkllumflat flat004 FlatV
+    cl> mkillumflat flat* ""
+.fi
+.ih
+SEE ALSO
+ccdproc, flatfields, mkfringecor, mkillumcor, mkskycor, mkskyflat
+.endhelp
diff --git a/noao/imred/ccdred/doc/mkskycor.hlp b/noao/imred/ccdred/doc/mkskycor.hlp
new file mode 100644
index 00000000..15cfacf6
--- /dev/null
+++ b/noao/imred/ccdred/doc/mkskycor.hlp
@@ -0,0 +1,103 @@
+.help mkskycor Feb88 noao.imred.ccdred
+.ih
+NAME
+mkskycor -- Make sky iillumination correction images
+.ih
+USAGE
+mkskycor input output
+.ih
+PARAMETERS
+.ls input
+List of input images for making sky iillumination correction images.
+.le
+.ls output
+List of output flat field iillumination correction images.  If none is
+specified or if the name is the same as the input image then the output
+image replaces the input image.
+.le
+.ls ccdtype = ""
+CCD image type to select from the input images.  If none is specified
+then all types are used.
+.le
+.ls xboxmin = 5, xboxmax = 0.25, yboxmin = 5, yboxmax = 0.25
+Minimum and maximum smoothing box size along the x and y axes.  The
+minimum box size is used at the edges and grows to the maximum size in
+the middle of the image.  This allows the smoothed image to better
+represent gradients at the edge of the image.  If a size is less then 1
+then it is interpreted as a fraction of the image size.  If a size is
+greater than or equal to 1 then it is the box size in pixels.  A size
+greater than the size of image selects a box equal to the size of the
+image.
+.le
+.ls clip = yes
+Clean the input images of objects?  If yes then a clipping algorithm is
+used to detect and exclude objects from the smoothing.
+.le
+.ls lowsigma = 2.5, highsigma = 2.5
+Sigma clipping thresholds above and below the smoothed iillumination.
+.le
+.ls ccdproc (parameter set)
+CCD processing parameters.
+.le
+.ih
+DESCRIPTION
+The large scale iillumination pattern of the input images, generally
+blank sky calibration images, is determined by heavily smoothing
+the image using a moving "boxcar" average.  The effects of objects in
+the image may be minimized by using a sigma clipping algorithm to
+detect and exclude the objects from the average.  This
+iillumination image is applied by \fBccdproc\fR to CCD images to remove
+the iillumination pattern.
+
+The input images are automatically processed up through flat field
+calibration before computing the iillumination.  The iillumination
+correction is that needed to make the processed images flat
+over large scales.  The input images are generally blank sky calibration
+images which have the same iillumination and instrumental effects
+as the object observations.  Object images may be used but removal
+of the objects may not be very good; particularly large, bright objects.
+For further discussion of flat fields and iillumination corrections
+see \fBflatfields\fR.
+
+You will notice that when you process images with an iillumination
+correction you are dividing each image by a flat field calibration and
+an iillumination correction.  If the iillumination corrections are not
+done as a later step but at the same time as the rest of the processing
+one will get the same calibration by multiplying the flat field by the
+iillumination correction and using this product alone as the flat
+field.  This approach has the advantage of one less calibration image
+and two less computations (scaling and dividing the iillumination
+correction).  Such an image, called a \fIsky flat\fR, may be created by
+\fBmkskyflat\fR as an alternative to this task.
+
+The smoothing algorithm is a moving average over a two dimensional
+box.  The algorithm is unconvential in that the box size is not fixed.
+The box size is increased from the specified minimum at the edges to
+the maximum in the middle of the image.  This permits a better estimate
+of the background at the edges, while retaining the very large scale
+smoothing in the center of the image.  Note that the sophisticated
+tools of the \fBimages\fR package may be used for smoothing but this
+requires more of the user and, for the more sophisticated smoothing
+algorithms such as surface fitting, more processing time.
+
+Blank sky images may not be completely blank so a sigma clipping
+algorithm may be used to detect and exclude objects from the
+iillumination pattern.  This is done by computing the rms of the image
+lines relative to the smoothed background and excluding points
+exceeding the specified threshold factors times the rms.  This is done
+before each image line is added to the moving average, except for the
+first few lines where an iterative process is used.
+.ih
+EXAMPLES
+1. The two examples below make an iillumination image from a blank sky image,
+"sky017".  In the first example a separate iillumination image is created
+and in the second the iillumination image replaces the sky image.
+
+.nf
+    cl> mkskycor sky017 Illum
+    cl> mkskycor sky017 sky017
+.fi
+.ih
+SEE ALSO
+ccdproc, flatfields, mkillumcor, mkillumflat, mkskyflat
+.endhelp
diff --git a/noao/imred/ccdred/doc/mkskyflat.hlp b/noao/imred/ccdred/doc/mkskyflat.hlp
new file mode 100644
index 00000000..d28e2301
--- /dev/null
+++ b/noao/imred/ccdred/doc/mkskyflat.hlp
@@ -0,0 +1,110 @@
+.help mkskyflat Feb88 noao.imred.ccdred
+.ih
+NAME
+mkskyflat -- Make sky corrected flat field images
+.ih
+USAGE
+mkskyflat input output
+.ih
+PARAMETERS
+.ls input
+List of blank sky images to be used to create sky corrected flat field
+calibration images.
+.le
+.ls output
+List of output sky corrected flat field calibration images (called
+sky flats).  If none is specified or if the name is the same as the
+input image then the output image replaces the input image.
+.le
+.ls ccdtype = ""
+CCD image type to select from the input images.
+.le
+.ls xboxmin = 5, xboxmax = 0.25, yboxmin = 5, yboxmax = 0.25
+Minimum and maximum smoothing box size along the x and y axes.  The
+minimum box size is used at the edges and grows to the maximum size in
+the middle of the image.  This allows the smoothed image to better
+represent gradients at the edge of the image.  If a size is less then 1
+then it is interpreted as a fraction of the image size.  If a size is
+greater than or equal to 1 then it is the box size in pixels.  A size
+greater than the size of image selects a box equal to the size of the
+image.
+.le
+.ls clip = yes
+Clean the input images of objects?  If yes then a clipping algorithm is
+used to detect and exclude objects from the smoothing.
+.le
+.ls lowsigma = 2.5, highsigma = 2.5
+Sigma clipping thresholds above and below the smoothed iillumination.
+.le
+.ls ccdproc (pset)
+CCD processing parameter set.
+.le
+.ih
+DESCRIPTION
+A sky corrected flat field calibration image, called a sky flat, is a
+flat field that when applied to observations of the sky have no large
+scale gradients.  Flat field images are generally obtained by exposures
+to lamps either illuminating the telescope field or a surface in the dome
+at which the telescope is pointed.  Because the detector is not illuminated
+in the same way as an observation of the sky there may be large
+scale iillumination patterns introduced into the observations with such
+a flat field.  To correct this type of flat field a blank sky observation
+(which has been divided by the original flat field) is heavily smoothed
+to remove the noise leaving only the residual large scale iillumination
+pattern.  This iillumination pattern is divided into the original flat
+field to remove this residual.
+
+The advantage of creating a sky flat field is that when processing
+the observations no additional operations are required.  However,
+if the observations have already been processed with the original
+flat field then the residual iillumination pattern of blank sky
+calibration images may be created as an iillumination correction
+to be applied by \fBccdproc\fR.  Such a correction is created by the
+task \fBmkskycor\fR.  If a good blank sky image is not
+available then it may be desirable to remove the iillumination pattern
+of the flat field image using \fBmkillumflat\fR or \fBmkillumcor\fR
+provided the sky observations are truly uniformly illuminated.
+For more on flat fields and iillumination corrections see \fBflatfields\fR.
+
+The input, blank sky images are first processed, based on the
+\fBccdproc\fR parameters, if needed.  These parameters also determine
+the flat field image to be used in making the sky flat.  The residual
+iillumination pattern is determined by heavily smoothing the image using
+a moving "boxcar" average.  The effects of objects in the input image
+may be minimized by using a sigma clipping algorithm to detect and
+exclude the objects from the average.  The output image is ratio of the
+flat field image, for the same subset as the input image, to the
+residual iillumination pattern determined from the processed blank sky
+input image.  The iillumination pattern is normalized by its mean to
+preserve the mean level of the flat field image.
+
+The smoothing algorithm is a moving average over a two dimensional
+box.  The algorithm is unconvential in that the box size is not fixed.
+The box size is increased from the specified minimum at the edges to
+the maximum in the middle of the image.  This permits a better estimate
+of the background at the edges, while retaining the very large scale
+smoothing in the center of the image.  Note that the sophisticated
+tools of the \fBimages\fR package may be used for smoothing but this
+requires more of the user and, for the more sophisticated smoothing
+algorithms such as surface fitting, more processing time.
+
+Blank sky images may not be completely blank so a sigma clipping
+algorithm may be used to detect and exclude objects from the
+iillumination pattern.  This is done by computing the rms of the image
+lines relative to the smoothed background and excluding points
+exceeding the specified threshold factors times the rms.  This is done
+before each image line is added to the moving average, except for the
+first few lines where an iterative process is used.
+.ih
+EXAMPLES
+1. Two examples in which a new image is created and in which the
+input sky images are converted to sky flats are:
+
+.nf
+    cl> mkskyflat sky004 Skyflat
+    cl> mkskyflat sky* ""
+.fi
+.ih
+SEE ALSO
+ccdproc, flatfields, mkfringecor, mkillumcor, mkillumflat, mkskycor
+.endhelp
diff --git a/noao/imred/ccdred/doc/setinstrument.hlp b/noao/imred/ccdred/doc/setinstrument.hlp
new file mode 100644
index 00000000..410dd20f
--- /dev/null
+++ b/noao/imred/ccdred/doc/setinstrument.hlp
@@ -0,0 +1,97 @@
+.help setinstrument Oct87 noao.imred.ccdred
+.ih
+NAME
+setinstrument -- Set instrument parameters
+.ih
+USAGE	
+setinstrument instrument
+.ih
+PARAMETERS
+.ls instrument
+Instrument identification for instrument parameters to be set.  If '?'
+then a list of the instrument identifiers is printed.
+.le
+.ls site = "kpno"
+Site ID.
+.le
+.ls directory = "ccddb$"
+Instrument directory containing instrument files.  The instrument files
+are found in the subdirectory given by the site ID. 
+.le
+.ls review = yes
+Review the instrument parameters?  If yes then \fBeparam\fR is run for
+the parameters of \fBccdred\fR and \fBccdproc\fR.
+.le
+.ls query
+Parameter query if initial instrument is not found.
+.le
+.ih
+DESCRIPTION
+The purpose of the task is to allow the user to easily set default
+parameters for a new instrument.  The default parameters are generally
+defined by support personal in an instrument directory for a particular
+site.  The instrument directory is the concatenation of the specified
+directory and the site.  For example if the directory is "ccddb$" and
+the site is "kpno" then the instrument directory is "ccddb$kpno/".
+The user may have his own set of instrument files in a local directory.
+The current directory is used by setting the directory and site to the
+null string ("").
+
+The user specifies an instrument identifier.  This instrument may
+be specific to a particular observatory, telescope, instrument, and
+detector.  If the character '?' is specified or the instrument file is
+not found then a list of instruments
+in the instrument directory is produced by paging the file "instruments.men".
+The task then performs the following operations:
+.ls (1)
+If an instrument translation file with the name given by the instrument
+ID and the extension ".dat" is found then the instrument translation
+file parameter, \fIccdred.instrument\fR, is set to this file.
+If it does not exist then the user is queried again.  Note that a
+null instrument, "", is allowed to set no translation file.
+.le
+.ls (2)
+If an instrument setup script with the name given by the instrument ID
+and the extension ".cl" is found then the commands in the file are
+executed (using the command \fIcl < script\fR.  This script generally
+sets default parameters.
+.le
+.ls (3)
+If the review flag is set the task \fBeparam\fR is run to allow the user
+to examine and modify the parameters for the package \fBccdred\fR and task
+\fBccdproc\fR.
+.le
+.ih
+EXAMPLES
+1. To get a list of the instruments;
+
+.nf
+	cl> setinstrument ?
+	[List of instruments]
+
+2. To set the instrument and edit the processing parameters:
+
+	cl> setinstrument ccdlink
+	[Edit CCDRED parameters]
+	[Edit CCDPROC parameters]
+
+3. To use your own instrument translation file and/or setup script in
+your working directory.
+
+	cl> setinst.site=""
+	cl> setinst.dir=""
+	cl> setinst myinstrument
+
+To make these files see help under \fBinstruments\fR.  Copying and modifying
+system files is also straightforward.
+
+	cl> copy ccddb$kpno/fits.dat .
+	cl> edit fits.dat
+	cl> setinst.site=""
+	cl> setinst.dir=""
+	cl> setinst fits
+.fi
+.ih
+SEE ALSO
+instruments, ccdred, ccdproc
+.endhelp
diff --git a/noao/imred/ccdred/doc/subsets.hlp b/noao/imred/ccdred/doc/subsets.hlp
new file mode 100644
index 00000000..78aafb01
--- /dev/null
+++ b/noao/imred/ccdred/doc/subsets.hlp
@@ -0,0 +1,99 @@
+.help subsets Jun87 noao.imred.ccdred
+.ih
+NAME
+subsets -- Description of CCD subsets
+.ih
+DESCRIPTION
+The \fBccdred\fR package groups observation into subsets.
+The image header parameter used to identify the subsets is defined
+in the instrument translation file (see help for \fBinstruments\fR).
+For example to select subsets by the header parameter "filters" the
+instrument translation file would contain the line:
+
+	subset	filters
+
+Observations are generally grouped into subsets based on a common
+instrument configuration such as a filter, aperture mask,
+grating setting, etc.  This allows combining images from several
+different subsets automatically and applying the appropriate
+flat field image when processing the observations.  For example
+if the subsets are by filter then \fBflatcombine\fR will search
+through all the images, find the flat field images (based on the
+CCD type parameter), and combine the flat field images from
+each filter separately.  Then when processing the images the
+flat field with the same filter as the observation is used.
+
+Each subset is assigned a short identifier.  This is listed when
+using \fBccdlist\fR and is appended to a root name when combining
+images.  Because the subset parameter in the image header may be
+any string there must be a mapping applied to generate unique
+identifiers.  This mapping is defined in the file given by
+the package parameter \fIccdred.ssfile\fR.  The file consists of
+lines with two fields (except that comment lines may be included
+as a line by itself or following the second field):
+
+	'subset string'	subset_id
+
+where the subset string is the image header string and the subset_id is
+the identifier.  A field must be quoted if it contains blanks.  The
+user may create this file but generally it is created by the tasks.  The
+tasks use the first word of the subset string as the default identifier
+and a number is appended if the first word is not unique.  The
+following steps define the subset identifier:
+
+.ls (1)
+Search the subset file, if present, for a matching subset string and
+use the defined subset identifier.
+.le
+.ls (2)
+If there is no matching subset string use the first word of the
+image header subset string and, if it is not unique,
+add successive integers until it is unique.
+.le
+.ls (3)
+If the identifier is not in the subset file create the file and add an
+entry if necessary.
+.le
+.ih
+EXAMPLES
+1. The subset file is "subsets" (the default).  The subset parameter is
+translated to "f1pos" in the image header (the old NOAO CCD parameter)
+which is an integer filter position.  After running a task, say
+"ccdlist *.imh" to cause all filters to be checked, the subset file contains:
+
+.nf
+	'2'	2
+	'5'	5
+	'3'	3
+.fi
+
+The order reflects the order in which the filters were encountered.
+Suppose the user wants to have more descriptive names then the subset
+file can be created or edited to the form:
+
+.nf
+	# Sample translation file.
+	'2'	U
+	'3'	B
+	'4'	V
+.fi
+
+(This is only an example and does not mean these are standard filters.)
+
+2. As another example suppose the image header parameter is "filter" and
+contains more descriptive strings.  The subset file might become:
+
+.nf
+	'GG 385 Filter'	GG
+	'GG 495 Filter'	GG1
+	'RG 610 Filter'	RG
+	'H-ALPHA'	H_ALPHA
+.fi
+
+In this case use of the first word was not very good but it is unique.
+It is better if the filters are encoded with the thought that the first
+word will be used by \fBccdred\fR; it should be short and unique.
+.ih
+SEE ALSO
+instruments
+.endhelp
diff --git a/noao/imred/ccdred/doc/zerocombine.hlp b/noao/imred/ccdred/doc/zerocombine.hlp
new file mode 100644
index 00000000..1646ea9c
--- /dev/null
+++ b/noao/imred/ccdred/doc/zerocombine.hlp
@@ -0,0 +1,121 @@
+.help zerocombine Aug91 noao.imred.ccdred
+.ih
+NAME
+zerocombine -- Combine and process zero level images
+.ih
+USAGE
+zerocombine input
+.ih
+PARAMETERS
+.ls input
+List of zero level images to combine.  The \fIccdtype\fR parameter
+may be used to select the zero level images from a list containing all
+types of data.
+.le
+.ls output = "Zero"
+Output zero level root image name.
+.le
+.ls combine = "average" (average|median)
+Type of combining operation performed on the final set of pixels (after
+rejection).  The choices are
+"average" or "median".  The median uses the average of the two central
+values when the number of pixels is even.
+.le
+.ls reject = "minmax" (none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip)
+Type of rejection operation.  See \fBcombine\fR for details.
+.le
+.ls ccdtype = "zero"
+CCD image type to combine.  If no image type is given then all input images
+are combined.
+.le
+.ls process = no
+Process the input images before combining?
+.le
+.ls delete = no
+Delete input images after combining?  Only those images combined are deleted.
+.le
+.ls clobber = no
+Clobber existing output images?
+.le
+.ls scale = "none" (none|mode|median|mean|exposure)
+Multiplicative image scaling to be applied.  The choices are none, scale
+by the mode, median, or mean of the specified statistics section, or scale
+by the exposure time given in the image header.
+.le
+.ls statsec = ""
+Section of images to use in computing image statistics for scaling.
+If no section is given then the entire region of the image is
+sampled (for efficiency the images are sampled if they are big enough).
+.le
+
+.ce
+Algorithm Parameters
+.ls nlow = 0,  nhigh = 1 (minmax)
+The number of low and high pixels to be rejected by the "minmax" algorithm.
+.le
+.ls nkeep = 1
+The minimum number of pixels to retain or the maximum number to reject
+when using the clipping algorithms (ccdclip, crreject, sigclip,
+avsigclip, or pclip).  When given as a positive value this is the minimum
+number to keep.  When given as a negative value the absolute value is
+the maximum number to reject.  This is actually converted to a number
+to keep by adding it to the number of images.
+.le
+.ls mclip = yes (ccdclip, crreject, sigclip, avsigcliip)
+Use the median as the estimate for the true intensity rather than the
+average with high and low values excluded in the "ccdclip", "crreject",
+"sigclip", and "avsigclip" algorithms?  The median is a better estimator
+in the presence of data which one wants to reject than the average.
+However, computing the median is slower than the average.
+.le
+.ls lsigma = 3., hsigma = 3. (ccdclip, crreject, sigclip, avsigclip, pclip)
+Low and high sigma clipping factors for the "ccdclip", "crreject", "sigclip",
+"avsigclip", and "pclip" algorithms.  They multiply a "sigma" factor
+produced by the algorithm to select a point below and above the average or
+median value for rejecting pixels.  The lower sigma is ignored for the
+"crreject" algorithm.
+.le
+.ls rdnoise = "0.", gain = "1.", snoise = "0." (ccdclip, crreject)
+CCD readout noise in electrons, gain in electrons/DN, and sensitivity noise
+as a fraction.  These parameters are used with the "ccdclip" and "crreject"
+algorithms.  The values may be either numeric or an image header keyword
+which contains the value.
+.le
+.ls pclip = -0.5 (pclip)
+Percentile clipping algorithm parameter.  If greater than
+one in absolute value then it specifies a number of pixels above or
+below the median to use for computing the clipping sigma.  If less
+than one in absolute value then it specifies the fraction of the pixels
+above or below the median to use.  A positive value selects a point
+above the median and a negative value selects a point below the median.
+The default of -0.5 selects approximately the quartile point.
+See \fBcombine\fR for further details.
+.le
+.ls blank = 0.
+Output value to be used when there are no pixels.
+.le
+.ih
+DESCRIPTION
+The zero level images in the input image list are combined.
+The input images may be processed first if desired.
+The original images may be deleted automatically if desired.
+The output pixel datatype will be real.
+
+This task is a script which applies \fBccdproc\fR and \fBcombine\fR.  The
+parameters and combining algorithms are described in detail in the help for
+\fBcombine\fR.  This script has default parameters specifically set for
+zero level images and simplifies the combining parameters.  There are other
+combining options not included in this task.  For these additional
+features, such as thresholding, offseting, masking, and projecting, use
+\fBcombine\fR.
+.ih
+EXAMPLES
+1. The image data contains four zero level images.
+To automatically select them and combine them as a background job
+using the default combining algorithm:
+
+    cl> zerocombine ccd*.imh&
+.ih
+SEE ALSO
+ccdproc, combine
+.endhelp
diff --git a/noao/imred/ccdred/flatcombine.cl b/noao/imred/ccdred/flatcombine.cl
new file mode 100644
index 00000000..78bd1e80
--- /dev/null
+++ b/noao/imred/ccdred/flatcombine.cl
@@ -0,0 +1,49 @@
+# FLATCOMBINE -- Process and combine flat field CCD images.
+
+procedure flatcombine (input)
+
+string	input			{prompt="List of flat field images to combine"}
+file	output="Flat"		{prompt="Output flat field root name"}
+string	combine="average"	{prompt="Type of combine operation",
+				 enum="average|median"}
+string	reject="avsigclip"	{prompt="Type of rejection",
+		enum="none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip"}
+string	ccdtype="flat"	{prompt="CCD image type to combine"}
+bool	process=yes	{prompt="Process images before combining?"}
+bool	subsets=yes	{prompt="Combine images by subset parameter?"}
+bool	delete=no	{prompt="Delete input images after combining?"}
+bool	clobber=no	{prompt="Clobber existing output image?"}
+string	scale="mode"	{prompt="Image scaling",
+			 enum="none|mode|median|mean|exposure"}
+string	statsec=""	{prompt="Image section for computing statistics"}
+int	nlow=1		{prompt="minmax: Number of low pixels to reject"}
+int	nhigh=1		{prompt="minmax: Number of high pixels to reject"}
+int	nkeep=1		{prompt="Minimum to keep (pos) or maximum to reject (neg)"}
+bool	mclip=yes	{prompt="Use median in sigma clipping algorithms?"}
+real	lsigma=3.	{prompt="Lower sigma clipping factor"}
+real	hsigma=3.	{prompt="Upper sigma clipping factor"}
+string	rdnoise="0."	{prompt="ccdclip: CCD readout noise (electrons)"}
+string	gain="1."	{prompt="ccdclip: CCD gain (electrons/DN)"}
+string	snoise="0."	{prompt="ccdclip: Sensitivity noise (fraction)"}
+real	pclip=-0.5	{prompt="pclip: Percentile clipping parameter"}
+real	blank=1.	{prompt="Value if there are no pixels"}
+
+begin
+	string	ims
+
+	ims = input
+
+	# Process images first if desired.
+	if (process == YES)
+	    ccdproc (ims, output="", ccdtype=ccdtype, noproc=no)
+
+	# Combine the flat field images.
+	combine (ims, output=output, plfile="", sigma="", combine=combine,
+	    reject=reject, ccdtype=ccdtype, subsets=subsets, delete=delete,
+	    clobber=clobber, project=no, outtype="real", offsets="none",
+	    masktype="none", blank=blank, scale=scale, zero="none", weight=no,
+	    statsec=statsec, lthreshold=INDEF, hthreshold=INDEF, nlow=nlow,
+	    nhigh=nhigh, nkeep=nkeep, mclip=mclip, lsigma=lsigma, hsigma=hsigma,
+	    rdnoise=rdnoise, gain=gain, snoise=snoise, sigscale=0.1,
+	    pclip=pclip, grow=0)
+end
diff --git a/noao/imred/ccdred/mkfringecor.par b/noao/imred/ccdred/mkfringecor.par
new file mode 100644
index 00000000..c088fe8b
--- /dev/null
+++ b/noao/imred/ccdred/mkfringecor.par
@@ -0,0 +1,11 @@
+input,s,a,,,,Input CCD images
+output,s,h,"",,,Output fringe images (same as input if none given)
+ccdtype,s,h,"",,,CCD image type to select
+xboxmin,r,h,5,0.,,Minimum smoothing box size in x at edges
+xboxmax,r,h,0.25,0.,,Maximum smoothing box size in x
+yboxmin,r,h,5,0.,,Minimum moothing box size in y at edges
+yboxmax,r,h,0.25,0.,,Maximum moothing box size in y
+clip,b,h,yes,,,Clip input pixels?
+lowsigma,r,h,2.5,0.,,Low clipping sigma
+highsigma,r,h,2.5,0.,,High clipping sigma
+ccdproc,pset,h,,,,CCD processing parameters
diff --git a/noao/imred/ccdred/mkillumcor.par b/noao/imred/ccdred/mkillumcor.par
new file mode 100644
index 00000000..cda8eb54
--- /dev/null
+++ b/noao/imred/ccdred/mkillumcor.par
@@ -0,0 +1,12 @@
+input,s,a,,,,Input CCD images
+output,s,a,,,,Output images (same as input if none given)
+ccdtype,s,h,"flat",,,CCD image type to select
+xboxmin,r,h,5,0.,,Minimum smoothing box size in x at edges
+xboxmax,r,h,0.25,0.,,Maximum smoothing box size in x
+yboxmin,r,h,5,0.,,Minimum smoothing box size in y at edges
+yboxmax,r,h,0.25,0.,,Maximum smoothing box size in y
+clip,b,h,yes,,,Clip input pixels?
+lowsigma,r,h,2.5,0.,,Low clipping sigma
+highsigma,r,h,2.5,0.,,High clipping sigma
+divbyzero,r,h,1.,,,Result for division by zero
+ccdproc,pset,h,,,,CCD processing parameters
diff --git a/noao/imred/ccdred/mkillumflat.par b/noao/imred/ccdred/mkillumflat.par
new file mode 100644
index 00000000..67897f46
--- /dev/null
+++ b/noao/imred/ccdred/mkillumflat.par
@@ -0,0 +1,12 @@
+input,s,a,,,,Input CCD flat field images
+output,s,a,,,,Output images (same as input if none given)
+ccdtype,s,h,"flat",,,CCD image type to select
+xboxmin,r,h,5,0.,,Minimum smoothing box size in x at edges
+xboxmax,r,h,0.25,0.,,Maximum smoothing box size in x
+yboxmin,r,h,5,0.,,Minimum moothing box size in y at edges
+yboxmax,r,h,0.25,0.,,Maximum moothing box size in y
+clip,b,h,yes,,,Clip input pixels?
+lowsigma,r,h,2.5,0.,,Low clipping sigma
+highsigma,r,h,2.5,0.,,High clipping sigma
+divbyzero,r,h,1.,,,Result for division by zero
+ccdproc,pset,h,,,,CCD processing parameters
diff --git a/noao/imred/ccdred/mkpkg b/noao/imred/ccdred/mkpkg
new file mode 100644
index 00000000..dab87bc3
--- /dev/null
+++ b/noao/imred/ccdred/mkpkg
@@ -0,0 +1,29 @@
+# Make CCDRED Package.
+
+$call	relink
+$exit
+
+update:
+	$call	relink
+	$call	install
+	;
+
+relink:
+	$update	libpkg.a
+	$call	ccdred
+	;
+
+install:
+	$move	xx_ccdred.e noaobin$x_ccdred.e
+	;
+
+ccdred:
+	$omake	x_ccdred.x
+	$link	x_ccdred.o libpkg.a -lxtools -lcurfit -lgsurfit -lncar -lgks\
+		-o xx_ccdred.e
+	;
+
+libpkg.a:
+	@src
+	@ccdtest
+	;
diff --git a/noao/imred/ccdred/mkskycor.par b/noao/imred/ccdred/mkskycor.par
new file mode 100644
index 00000000..e719dfa0
--- /dev/null
+++ b/noao/imred/ccdred/mkskycor.par
@@ -0,0 +1,11 @@
+input,s,a,,,,Input CCD images
+output,s,a,,,,Output images (same as input if none given)
+ccdtype,s,h,"",,,CCD image type to select
+xboxmin,r,h,5,0.,,Minimum smoothing box size in x at edges
+xboxmax,r,h,0.25,0.,,Maximum smoothing box size in x
+yboxmin,r,h,5,0.,,Minimum moothing box size in y at edges
+yboxmax,r,h,0.25,0.,,Maximum moothing box size in y
+clip,b,h,yes,,,Clip input pixels?
+lowsigma,r,h,2.5,0.,,Low clipping sigma
+highsigma,r,h,2.5,0.,,High clipping sigma
+ccdproc,pset,h,,,,CCD processing parameters
diff --git a/noao/imred/ccdred/mkskyflat.par b/noao/imred/ccdred/mkskyflat.par
new file mode 100644
index 00000000..e719dfa0
--- /dev/null
+++ b/noao/imred/ccdred/mkskyflat.par
@@ -0,0 +1,11 @@
+input,s,a,,,,Input CCD images
+output,s,a,,,,Output images (same as input if none given)
+ccdtype,s,h,"",,,CCD image type to select
+xboxmin,r,h,5,0.,,Minimum smoothing box size in x at edges
+xboxmax,r,h,0.25,0.,,Maximum smoothing box size in x
+yboxmin,r,h,5,0.,,Minimum moothing box size in y at edges
+yboxmax,r,h,0.25,0.,,Maximum moothing box size in y
+clip,b,h,yes,,,Clip input pixels?
+lowsigma,r,h,2.5,0.,,Low clipping sigma
+highsigma,r,h,2.5,0.,,High clipping sigma
+ccdproc,pset,h,,,,CCD processing parameters
diff --git a/noao/imred/ccdred/setinstrument.cl b/noao/imred/ccdred/setinstrument.cl
new file mode 100644
index 00000000..c10a7427
--- /dev/null
+++ b/noao/imred/ccdred/setinstrument.cl
@@ -0,0 +1,57 @@
+# SETINSTRUMENT -- Set up instrument parameters for the CCD reduction tasks.
+#
+# This task sets default parameters based on an instrument ID.
+
+procedure setinstrument (instrument)
+
+char	instrument		{prompt="Instrument ID (type ? for a list)"}
+char	site="kpno"		{prompt="Site ID"}
+char	directory="ccddb$"	{prompt="Instrument directory"}
+bool	review=yes		{prompt="Review instrument parameters?"}
+char	query			{prompt="Instrument ID (type q to quit)",
+				 mode="q"}
+
+begin
+	string	inst, instdir, instmen, instfile
+
+	# Define instrument directory, menu, and file
+	instdir = directory
+	if (site != "")
+	    instdir = instdir // site // "/"
+	instmen = instdir // "instruments.men"
+	inst = instrument
+	instfile = instdir // inst // ".dat"
+
+	# Loop until a valid instrument file is given.
+	while (inst != "" && !access (instfile)) {
+	    if (access (instmen))
+		page (instmen)
+	    else if (inst == "?")
+		print ("Instrument list ", instmen, " not found")
+	    else
+	        print ("Instrument file ", instfile, " not found")
+	    print ("")
+	    inst = query
+	    if (inst == "q")
+		return
+	    instrument = inst
+	    instfile = instdir // inst // ".dat"
+	}
+
+	# Set instrument parameter.
+	if (access (instfile))
+	    ccdred.instrument = instfile
+	else
+	    ccdred.instrument = ""
+
+	# Run instrument setup script.
+	instfile = instdir // inst // ".cl"
+	if (access (instfile))
+	    cl (< instfile)
+
+	# Review parameters if desired.
+	if (review) {
+	    eparam ("ccdred")
+	    eparam ("ccdproc")
+	}
+end
diff --git a/noao/imred/ccdred/skyreplace.par b/noao/imred/ccdred/skyreplace.par
new file mode 100644
index 00000000..b611c30d
--- /dev/null
+++ b/noao/imred/ccdred/skyreplace.par
@@ -0,0 +1,3 @@
+image,f,a,,,,Image to be modified
+frame,i,h,1,,,Image display frame
+cursor,*gcur,h,,,,Cursor
diff --git a/noao/imred/ccdred/src/calimage.x b/noao/imred/ccdred/src/calimage.x
new file mode 100644
index 00000000..82efdf54
--- /dev/null
+++ b/noao/imred/ccdred/src/calimage.x
@@ -0,0 +1,367 @@
+include	<error.h>
+include	<imset.h>
+include	"ccdtypes.h"
+
+define	SZ_SUBSET	16			# Maximum size of subset string
+define	IMAGE	Memc[$1+($2-1)*SZ_FNAME]	# Image string
+define	SUBSET	Memc[$1+($2-1)*(SZ_SUBSET+1)]	# Subset string
+
+# CAL_IMAGE -- Return a calibration image for a specified input image.
+# CAL_OPEN  -- Open the calibration image list.
+# CAL_CLOSE -- Close the calibration image list.
+# CAL_LIST  -- Add images to the calibration image list.
+#
+# The open procedure is called first to get the calibration image
+# lists and add them to an internal list.  Calibration images from the
+# input list are also added so that calibration images may be specified
+# either from the calibration image list parameters or in the input image list.
+# Existence errors and duplicate calibration images are ignored.
+# Validity checks are made when the calibration images are requested.
+#
+# During processing the calibration image names are requested for each input
+# image.  The calibration image list is searched for a calibration image of
+# the right type and subset.  If more than one is found the first one is
+# returned and a warning given for the others.  The warning is only issued
+# once.  If no calibration image is found then an error is returned.
+#
+# The calibration image list must be closed at the end of processing the
+# input images.
+
+
+# CAL_IMAGE -- Return a calibration image of a particular type.
+# Search the calibration list for the first calibration image of the desired
+# type and subset.  Print a warning if there  is more than one possible
+# calibration image and return an error if there is no calibration image. 
+
+procedure cal_image (im, ccdtype, nscan, image, maxchars)
+
+pointer	im		# Image to be processed
+int	ccdtype		# Callibration CCD image type desired
+int	nscan		# Number of scan rows desired
+char	image[maxchars]	# Calibration image (returned)
+int	maxchars	# Maximum number chars in image name
+
+int	i, m, n
+pointer	sp, subset, str
+bool	strne(), ccd_cmp()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subsets
+pointer	nscans		# Pointer to array of calibration nscan values
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, nscans, images, nimages
+
+begin
+	call smark (sp)
+	call salloc (subset, SZ_SUBSET, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	m = 0
+	n = 0
+	switch (ccdtype) {
+	case ZERO, DARK:
+	    do i = 1, nimages {
+		if (Memi[ccdtypes+i-1] != ccdtype)
+		    next
+		n = n + 1
+		if (n == 1) {
+		    m = i
+		} else {
+		    if (Memi[nscans+i-1] == Memi[nscans+m-1]) {
+#			call eprintf (
+#			    "Warning: Extra calibration image %s ignored\n")
+#			    call pargstr (IMAGE(images,i))
+
+			# Reset the image type to eliminate further warnings.
+			Memi[ccdtypes+i-1] = UNKNOWN
+		    } else if (Memi[nscans+m-1] != nscan &&
+			       (Memi[nscans+i-1] == nscan ||
+			       Memi[nscans+i-1] == 1)) {
+			m = i
+		    }
+		}
+	    }
+	case FLAT, ILLUM, FRINGE:
+	    call ccdsubset (im, Memc[subset], SZ_SUBSET)
+
+	    do i = 1, nimages {
+		if (Memi[ccdtypes+i-1] != ccdtype)
+		    next
+		if (strne (SUBSET(subsets,i), Memc[subset]))
+		    next
+		n = n + 1
+		if (n == 1) {
+		    m = i
+		} else {
+		    if (Memi[nscans+i-1] == Memi[nscans+m-1]) {
+#			call eprintf (
+#			    "Warning: Extra calibration image %s ignored\n")
+#			    call pargstr (IMAGE(images,i))
+
+			# Reset the image type to eliminate further warnings.
+			Memi[ccdtypes+i-1] = UNKNOWN
+		    } else if (Memi[nscans+m-1] != nscan &&
+			       (Memi[nscans+i-1] == nscan ||
+			       Memi[nscans+i-1] == 1)) {
+			m = i
+		    }
+		}
+	    }
+	}
+
+	# If no calibration image is found then it is an error.
+	if (m == 0) {
+	    switch (ccdtype) {
+	    case ZERO:
+	        call error (0, "No zero level calibration image found")
+	    case DARK:
+	        call error (0, "No dark count calibration image found")
+	    case FLAT:
+		call sprintf (Memc[str], SZ_LINE,
+	             "No flat field calibration image of subset %s found")
+		     call pargstr (Memc[subset])
+	        call error (0, Memc[str])
+	    case ILLUM:
+		call sprintf (Memc[str], SZ_LINE,
+	             "No illumination calibration image of subset %s found")
+		     call pargstr (Memc[subset])
+	        call error (0, Memc[str])
+	    case FRINGE:
+		call sprintf (Memc[str], SZ_LINE,
+	             "No fringe calibration image of subset %s found")
+		     call pargstr (Memc[subset])
+	        call error (0, Memc[str])
+	    }
+	}
+
+	call strcpy (IMAGE(images,m), image, maxchars)
+	if (nscan != Memi[nscans+m-1]) {
+	    if (nscan != 1 && Memi[nscans+m-1] == 1)
+		call cal_scan (nscan, image, maxchars)
+	    else {
+		call sprintf (Memc[str], SZ_LINE,
+	             "Cannot find or create calibration with nscan of %d")
+		     call pargi (nscan)
+	        call error (0, Memc[str])
+	    }
+	}
+
+	# Check that the input image is not the same as the calibration image.
+	call imstats (im, IM_IMAGENAME, Memc[str], SZ_LINE)
+	if (ccd_cmp (Memc[str], IMAGE(images,m))) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Calibration image %s is the same as the input image")
+		call pargstr (image)
+	    call error (0, Memc[str])
+	}
+
+	call sfree (sp)
+end
+
+
+# CAL_OPEN -- Create a list of calibration images from the input image list
+# and the calibration image lists.
+
+procedure cal_open (list)
+
+int	list		# List of input images
+int	list1		# List of calibration images
+
+pointer	sp, str
+int	ccdtype, strdic(), imtopenp()
+bool	clgetb()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subset numbers
+pointer	nscans		# Pointer to array of calibration nscan values
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, nscans, images, nimages
+
+errchk	cal_list
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	call clgstr ("ccdtype", Memc[str], SZ_LINE)
+	call xt_stripwhite (Memc[str])
+	if (Memc[str] == EOS)
+	    ccdtype = NONE
+	else
+	    ccdtype = strdic (Memc[str], Memc[str], SZ_LINE, CCDTYPES)
+
+	# Add calibration images to list.
+	nimages = 0
+	if (ccdtype != ZERO && clgetb ("zerocor")) {
+	    list1 = imtopenp ("zero")
+	    call cal_list (list1, ZERO)
+	    call imtclose (list1)
+	}
+	if (ccdtype != ZERO && ccdtype != DARK && clgetb ("darkcor")) {
+	    list1 = imtopenp ("dark")
+	    call cal_list (list1, DARK)
+	    call imtclose (list1)
+	}
+	if (ccdtype != ZERO && ccdtype != DARK && ccdtype != FLAT &&
+	    clgetb ("flatcor")) {
+	    list1 = imtopenp ("flat")
+	    call cal_list (list1, FLAT)
+	    call imtclose (list1)
+	}
+	if (ccdtype != ZERO && ccdtype != DARK && ccdtype != FLAT &&
+	    ccdtype != ILLUM && clgetb ("illumcor")) {
+	    list1 = imtopenp ("illum")
+	    call cal_list (list1, ILLUM)
+	    call imtclose (list1)
+	}
+	if (ccdtype != ZERO && ccdtype != DARK && ccdtype != FLAT &&
+	    ccdtype != FRINGE && clgetb ("fringecor")) {
+	    list1 = imtopenp ("fringe")
+	    call cal_list (list1, FRINGE)
+	    call imtclose (list1)
+	}
+	if (list != NULL) {
+	    call cal_list (list, UNKNOWN)
+	    call imtrew (list)
+	}
+
+	call sfree (sp)
+end
+
+
+# CAL_CLOSE -- Free memory from the internal calibration image list.
+
+procedure cal_close ()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subset
+pointer	nscans		# Pointer to array of calibration nscan values
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, nscans, images, nimages
+
+begin
+	if (nimages > 0) {
+	    call mfree (ccdtypes, TY_INT)
+	    call mfree (subsets, TY_CHAR)
+	    call mfree (nscans, TY_INT)
+	    call mfree (images, TY_CHAR)
+	}
+end
+
+
+# CAL_LIST -- Add calibration images to an internal list.
+# Map each image and get the CCD image type and subset.
+# If the ccdtype is given as a procedure argument this overrides the
+# image header type.  For the calibration images add the type, subset,
+# and image name to dynamic arrays.  Ignore duplicate names.
+
+procedure cal_list (list, listtype)
+
+pointer	list		# Image list
+int	listtype	# CCD type of image in list.
+			# Overrides header type if not UNKNOWN.
+
+int	i, ccdtype, ccdtypei(), ccdnscan(), imtgetim()
+pointer	sp, image, im, immap()
+bool	streq()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subsets
+pointer	nscans		# Pointer to array of calibration nscan values
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, nscans, images, nimages
+
+begin
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+
+	while (imtgetim (list, Memc[image], SZ_FNAME) != EOF) {
+	    # Open the image.  If an explicit type is given it is an
+	    # error if the image can't be opened.
+	    iferr (im = immap (Memc[image], READ_ONLY, 0)) {
+		if (listtype == UNKNOWN)
+		    next
+		else
+		    call erract (EA_ERROR)
+	    }
+
+	    # Override image header CCD type if a list type is given.
+	    if (listtype == UNKNOWN)
+	        ccdtype = ccdtypei (im)
+	    else
+		ccdtype = listtype
+		
+	    switch (ccdtype) {
+	    case ZERO, DARK, FLAT, ILLUM, FRINGE:
+		# Check for duplication.
+		for (i=1; i<=nimages; i=i+1)
+		    if (streq (Memc[image], IMAGE(images,i)))
+			break
+		if (i <= nimages)
+		    break
+
+		# Allocate memory for a new image.
+		if (i == 1) {
+		    call malloc (ccdtypes, i, TY_INT)
+		    call malloc (subsets, i * (SZ_SUBSET+1), TY_CHAR)
+		    call malloc (nscans, i, TY_INT)
+		    call malloc (images, i * SZ_FNAME, TY_CHAR)
+		} else {
+		    call realloc (ccdtypes, i, TY_INT)
+		    call realloc (subsets, i * SZ_FNAME, TY_CHAR)
+		    call realloc (nscans, i, TY_INT)
+		    call realloc (images, i * SZ_FNAME, TY_CHAR)
+		}
+
+		# Enter the ccdtype, subset, and image name.
+		Memi[ccdtypes+i-1] = ccdtype
+		Memi[nscans+i-1] = ccdnscan (im, ccdtype)
+		call ccdsubset (im, SUBSET(subsets,i), SZ_SUBSET)
+		call strcpy (Memc[image], IMAGE(images,i), SZ_FNAME-1)
+		nimages = i
+	    }
+	    call imunmap (im)
+	}
+	call sfree (sp)
+end
+
+
+# CAL_SCAN -- Generate name for scan corrected calibration image.
+
+procedure cal_scan (nscan, image, maxchar)
+
+int	nscan			#I Number of scan lines
+char	image[maxchar]		#U Input root name, output scan name
+int	maxchar			#I Maximum number of chars in image name
+
+bool	clgetb()
+pointer	sp, root, ext
+
+begin
+	# Check if this operation is desired.
+	if (!clgetb ("scancor") || nscan == 1)
+	    return
+
+	call smark (sp)
+	call salloc (root, SZ_FNAME, TY_CHAR)
+	call salloc (ext, SZ_FNAME, TY_CHAR)
+
+	call xt_imroot (image, Memc[root], SZ_FNAME)
+	call xt_imext (image, Memc[ext], SZ_FNAME)
+	if (IS_INDEFI (nscan)) {
+	    call sprintf (image, maxchar, "%s.1d%s")
+		call pargstr (Memc[root])
+		call pargstr (Memc[ext])
+	} else {
+	    call sprintf (image, maxchar, "%s.%d%s")
+		call pargstr (Memc[root])
+		call pargi (nscan)
+		call pargstr (Memc[ext])
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/ccdcache.com b/noao/imred/ccdred/src/ccdcache.com
new file mode 100644
index 00000000..91ffae12
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdcache.com
@@ -0,0 +1,10 @@
+# Common data defining the cached images and data.
+
+int	ccd_ncache		# Number of images cached
+int	ccd_maxcache		# Maximum size of cache
+int	ccd_szcache		# Current size of cache
+int	ccd_oldsize		# Original memory size
+int	ccd_pcache		# Pointer to image cache structures
+
+common	/ccdcache_com/ ccd_ncache, ccd_maxcache, ccd_szcache, ccd_oldsize,
+	ccd_pcache
diff --git a/noao/imred/ccdred/src/ccdcache.h b/noao/imred/ccdred/src/ccdcache.h
new file mode 100644
index 00000000..f7de3a2c
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdcache.h
@@ -0,0 +1,10 @@
+# Definition for image cache structure.
+
+define	CCD_LENCACHE		6
+
+define	CCD_IM		Memi[$1]	# IMIO pointer
+define	CCD_NACCESS	Memi[$1+1]	# Number of accesses requested
+define	CCD_SZDATA	Memi[$1+2]	# Size of data in cache in chars
+define	CCD_DATA	Memi[$1+3]	# Pointer to data cache
+define	CCD_BUFR	Memi[$1+4]	# Pointer to real image line
+define	CCD_BUFS	Memi[$1+5]	# Pointer to short image line
diff --git a/noao/imred/ccdred/src/ccdcache.x b/noao/imred/ccdred/src/ccdcache.x
new file mode 100644
index 00000000..78f84ace
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdcache.x
@@ -0,0 +1,381 @@
+include	<imhdr.h>
+include	<imset.h>
+include	<mach.h>
+include	"ccdcache.h"
+
+.help ccdcache Jun87
+.nf ---------------------------------------------------------------------
+The purpose of the CCD image caching package is to minimize image mapping
+time, to prevent multiple mapping of the same image, and to keep entire
+calibration images in memory for extended periods to minimize disk
+I/O.  It is selected by specifying a maximum caching size based on the
+available memory.  When there is not enough memory for caching (or by
+setting the size to 0) then standard IMIO is used.  When there is
+enough memory then as many images as will fit into the specified cache
+size are kept in memory.  Images are also kept mapped until explicitly
+flushed or the entire package is closed.
+
+This is a special purpose interface intended only for the CCDRED package.
+It has the following restrictions.
+
+    1.  Images must be processed to be cached.
+    2.  Images must be 2 dimensional to be cached
+    3.  Images must be real or short to be cached.
+    4.  Images must be read_only to be cached.
+    5.  Cached images remain in memory until they are displaced,
+	flushed, or the package is closed.
+
+The package consists of the following procedures.
+
+	      ccd_open ()
+	 im = ccd_cache (image)
+	ptr = ccd_glr (im, col1, col2, line)
+	ptr = ccd_gls (im, col1, col2, line)
+	      ccd_unmap (im)
+	      ccd_flush (im)
+	      ccd_close ()
+
+
+CCD_OPEN:   Initialize the image cache.  Called at the beginning.
+CCD_CLOSE:  Flush the image cache and restore memory.  Called at the end.
+
+CCD_CACHE:  Open an image and save the IMIO pointer.  If the image has been
+opened previously it need not be opened again.  If image data caching
+is specified the image data may be read it into memory.  In order for
+image data caching to occur the the image has to have been processed,
+be two dimensional, be real or short, and the total cache memory not
+be exceeded.  If an error occurs in reading the image into memory
+the data is not cached.
+
+CCD_UNMAP:  The image access number is decremented but the image
+is not closed against the event it will be used again.
+
+CCD_FLUSH:  The image is closed and flushed from the cache.
+
+CCD_GLR, CCD_GLS: Get a real or short image line.  If the image data is cached
+then a pointer to the line is quickly returned.  If the data is not cached then
+IMIO is used to get the pointer.
+.endhelp ---------------------------------------------------------------------
+
+
+
+# CCD_CACHE -- Open an image and possibly cache it in memory.
+
+pointer procedure ccd_cache (image, ccdtype)
+
+char	image[ARB]		# Image to be opened
+int	ccdtype			# Image type
+
+int	i, nc, nl, nbytes
+pointer	sp, str, pcache, pcache1, im
+
+int	sizeof()
+pointer	immap(), imgs2r(), imgs2s()
+bool	streq(), ccdcheck()
+errchk	immap, imgs2r, imgs2s
+
+include	"ccdcache.com"
+
+define	done_		99
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Check if the image is cached.
+	for (i=1; i<=ccd_ncache; i=i+1) {
+	    pcache = Memi[ccd_pcache+i-1]
+	    im = CCD_IM(pcache)
+	    call imstats (im, IM_IMAGENAME, Memc[str], SZ_LINE)
+	    if (streq (image, Memc[str]))
+		break
+	}
+
+	# If the image is not cached open it and allocate memory.
+	if (i > ccd_ncache) {
+	    im = immap (image, READ_ONLY, 0)
+	    ccd_ncache = i
+	    call realloc (ccd_pcache, ccd_ncache, TY_INT)
+	    call malloc (pcache, CCD_LENCACHE, TY_STRUCT)
+	    Memi[ccd_pcache+i-1] = pcache
+	    CCD_IM(pcache) = im
+	    CCD_NACCESS(pcache) = 0
+	    CCD_SZDATA(pcache) = 0
+	    CCD_DATA(pcache) = NULL
+	    CCD_BUFR(pcache) = NULL
+	    CCD_BUFS(pcache) = NULL
+	}
+
+	# If not caching the image data or if the image data has already
+	# been cached we are done.
+	if ((ccd_maxcache == 0) || (CCD_SZDATA(pcache) > 0))
+	    goto done_
+
+	# Don't cache unprocessed calibration image data.
+	# This is the only really CCDRED specific code.
+	if (ccdcheck (im, ccdtype))
+	    goto done_
+
+	# Check image is 2D and a supported pixel type.
+	if (IM_NDIM(im) != 2)
+	    goto done_
+	if ((IM_PIXTYPE(im) != TY_REAL) && (IM_PIXTYPE(im) !=TY_SHORT))
+	    goto done_
+
+	# Compute the size of the image data.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	nbytes = nc * nl * sizeof (IM_PIXTYPE(im)) * SZB_CHAR
+
+	# Free memory not in use.
+	if (ccd_szcache + nbytes > ccd_maxcache) {
+	    for (i=1; i<=ccd_ncache; i=i+1) {
+	        pcache1 = Memi[ccd_pcache+i-1]
+	        if (CCD_NACCESS(pcache1) == 0) {
+		    if (CCD_SZDATA(pcache1) > 0) {
+		        ccd_szcache = ccd_szcache - CCD_SZDATA(pcache1)
+		        CCD_SZDATA(pcache1) = 0
+		        CCD_DATA(pcache1) = NULL
+			call mfree (CCD_BUFR(pcache1), TY_REAL)
+			call mfree (CCD_BUFS(pcache1), TY_SHORT)
+		        call imseti (CCD_IM(pcache1), IM_CANCEL, YES)
+		        if (ccd_szcache + nbytes > ccd_maxcache)
+		            break
+		    }
+	        }
+	    }
+	}
+	if (ccd_szcache + nbytes > ccd_maxcache)
+	    goto done_
+
+	# Cache the image data
+	iferr {
+	    switch (IM_PIXTYPE (im)) {
+	    case TY_SHORT:
+	        CCD_DATA(pcache) = imgs2s (im, 1, nc, 1, nl)
+	    case TY_REAL:
+	        CCD_DATA(pcache) = imgs2r (im, 1, nc, 1, nl)
+	    }
+	    ccd_szcache = ccd_szcache + nbytes
+	    CCD_SZDATA(pcache) = nbytes
+	} then {
+	    call imunmap (im)
+	    im = immap (image, READ_ONLY, 0)
+	    CCD_IM(pcache) = im
+	    CCD_SZDATA(pcache) = 0
+	}
+
+done_
+	CCD_NACCESS(pcache) = CCD_NACCESS(pcache) + 1
+	call sfree (sp)
+	return (im)
+end
+
+
+# CCD_OPEN -- Initialize the CCD image cache.
+
+procedure ccd_open (max_cache)
+
+int	max_cache	# Maximum cache size in bytes
+
+int	max_size, begmem()
+include	"ccdcache.com"
+
+begin
+	ccd_ncache = 0
+	ccd_maxcache = max_cache
+	ccd_szcache = 0
+	call malloc (ccd_pcache, 1, TY_INT)
+
+	# Ask for the maximum physical memory.
+	if (ccd_maxcache > 0) {
+	    ccd_oldsize = begmem (0, ccd_oldsize, max_size)
+	    call fixmem (max_size)
+	}
+end
+
+
+# CCD_UNMAP -- Unmap an image.
+# Don't actually unmap the image since it may be opened again.
+
+procedure ccd_unmap (im)
+
+pointer	im			# IMIO pointer
+
+int	i
+pointer	pcache
+include	"ccdcache.com"
+
+begin
+	for (i=1; i<=ccd_ncache; i=i+1) {
+	    pcache = Memi[ccd_pcache+i-1]
+	    if (CCD_IM(pcache) == im) {
+		CCD_NACCESS(pcache) = CCD_NACCESS(pcache) - 1
+		return
+	    }
+	}
+
+	call imunmap (im)
+end
+
+
+# CCD_FLUSH -- Close image and flush from cache.
+
+procedure ccd_flush (im)
+
+pointer	im			# IMIO pointer
+
+int	i
+pointer	pcache
+include "ccdcache.com"
+
+begin
+	for (i=1; i<=ccd_ncache; i=i+1) {
+	    pcache = Memi[ccd_pcache+i-1]
+	    if (CCD_IM(pcache) == im) {
+		ccd_ncache = ccd_ncache - 1
+	        ccd_szcache = ccd_szcache - CCD_SZDATA(pcache)
+	        call mfree (CCD_BUFR(pcache), TY_REAL)
+	        call mfree (CCD_BUFS(pcache), TY_SHORT)
+		call mfree (pcache, TY_STRUCT)
+		for (; i<=ccd_ncache; i=i+1)
+		    Memi[ccd_pcache+i-1] = Memi[ccd_pcache+i]
+		break
+	    }
+	}
+
+	call imunmap (im)
+end
+
+
+# CCD_CLOSE -- Close the image cache.
+
+procedure ccd_close ()
+
+int	i
+pointer	pcache
+include "ccdcache.com"
+
+begin
+	for (i=1; i<=ccd_ncache; i=i+1) {
+	    pcache = Memi[ccd_pcache+i-1]
+	    call imunmap (CCD_IM(pcache))
+	    call mfree (CCD_BUFR(pcache), TY_REAL)
+	    call mfree (CCD_BUFS(pcache), TY_SHORT)
+	    call mfree (pcache, TY_STRUCT)
+	}
+	call mfree (ccd_pcache, TY_INT)
+
+	# Restore memory.
+	call fixmem (ccd_oldsize)
+end
+
+
+# CCD_GLR -- Get a line of real data from the image.
+# If the image data is cached this is fast (particularly if the datatype
+# matches).  If the image data is not cached then use IMIO.
+
+pointer procedure ccd_glr (im, col1, col2, line)
+
+pointer	im			# IMIO pointer
+int	col1, col2		# Columns
+int	line			# Line
+
+int	i
+pointer	pcache, data, bufr, imgs2r()
+errchk	malloc
+include "ccdcache.com"
+
+begin
+	# Quick test for cached data.
+	if (ccd_maxcache == 0)
+	    return (imgs2r (im, col1, col2, line, line))
+
+	# Return cached data.
+	if (IM_PIXTYPE(im) == TY_REAL) {
+	    for (i=1; i<=ccd_ncache; i=i+1) {
+		pcache = Memi[ccd_pcache+i-1]
+		if (CCD_IM(pcache) == im) {
+		    if (CCD_SZDATA(pcache) > 0)
+		        return (CCD_DATA(pcache)+(line-1)*IM_LEN(im,1)+col1-1)
+		    else
+			break
+		}
+	    }
+	} else {
+	    for (i=1; i<=ccd_ncache; i=i+1) {
+		pcache = Memi[ccd_pcache+i-1]
+		if (CCD_IM(pcache) == im) {
+		    if (CCD_SZDATA(pcache) > 0) {
+		        data = CCD_DATA(pcache)+(line-1)*IM_LEN(im,1)+col1-1
+		        bufr = CCD_BUFR(pcache)
+		        if (bufr == NULL) {
+			    call malloc (bufr, IM_LEN(im,1), TY_REAL)
+			    CCD_BUFR(pcache) = bufr
+			}
+		        call achtsr (Mems[data], Memr[bufr], IM_LEN(im,1))
+		        return (bufr)
+		    } else
+			break
+		}
+	    }
+	}
+
+	# Return uncached data.
+	return (imgs2r (im, col1, col2, line, line))
+end
+
+
+# CCD_GLS -- Get a line of short data from the image.
+# If the image data is cached this is fast (particularly if the datatype
+# matches).  If the image data is not cached then use IMIO.
+
+pointer procedure ccd_gls (im, col1, col2, line)
+
+pointer	im			# IMIO pointer
+int	col1, col2		# Columns
+int	line			# Line
+
+int	i
+pointer	pcache, data, bufs, imgs2s()
+errchk	malloc
+include "ccdcache.com"
+
+begin
+	# Quick test for cached data.
+	if (ccd_maxcache == 0)
+	    return (imgs2s (im, col1, col2, line, line))
+
+	# Return cached data.
+	if (IM_PIXTYPE(im) == TY_SHORT) {
+	    for (i=1; i<=ccd_ncache; i=i+1) {
+		pcache = Memi[ccd_pcache+i-1]
+		if (CCD_IM(pcache) == im) {
+		    if (CCD_SZDATA(pcache) > 0)
+		        return (CCD_DATA(pcache)+(line-1)*IM_LEN(im,1)+col1-1)
+		    else
+			break
+		}
+	    }
+	} else {
+	    for (i=1; i<=ccd_ncache; i=i+1) {
+		pcache = Memi[ccd_pcache+i-1]
+		if (CCD_IM(pcache) == im) {
+		    if (CCD_SZDATA(pcache) > 0) {
+		        data = CCD_DATA(pcache)+(line-1)*IM_LEN(im,1)+col1-1
+		        bufs = CCD_BUFS(pcache)
+		        if (bufs == NULL) {
+			    call malloc (bufs, IM_LEN(im,1), TY_SHORT)
+			    CCD_BUFS(pcache) = bufs
+		        }
+		        call achtrs (Memr[data], Mems[bufs], IM_LEN(im,1))
+		        return (bufs)
+		    } else
+			break
+		}
+	    }
+	}
+
+	# Return uncached data.
+	return (imgs2s (im, col1, col2, line, line))
+end
diff --git a/noao/imred/ccdred/src/ccdcheck.x b/noao/imred/ccdred/src/ccdcheck.x
new file mode 100644
index 00000000..0dde14f9
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdcheck.x
@@ -0,0 +1,67 @@
+include	<imhdr.h>
+include	"ccdtypes.h"
+
+# CCDCHECK -- Check processing status.
+
+bool procedure ccdcheck (im, ccdtype)
+
+pointer	im			# IMIO pointer
+int	ccdtype			# CCD type
+
+real	ccdmean, hdmgetr()
+bool	clgetb(), ccdflag()
+long	time
+int	hdmgeti()
+
+begin
+	if (clgetb ("trim") && !ccdflag (im, "trim"))
+	    return (true)
+	if (clgetb ("fixpix") && !ccdflag (im, "fixpix"))
+	    return (true)
+	if (clgetb ("overscan") && !ccdflag (im, "overscan"))
+	    return (true)
+
+	switch (ccdtype) {
+	case ZERO:
+	    if (clgetb ("readcor") && !ccdflag (im, "readcor"))
+	        return (true)
+	case DARK:
+	    if (clgetb ("zerocor") && !ccdflag (im, "zerocor"))
+	        return (true)
+	case FLAT:
+	    if (clgetb ("zerocor") && !ccdflag (im, "zerocor"))
+	        return (true)
+	    if (clgetb ("darkcor") && !ccdflag (im, "darkcor"))
+	        return (true)
+	    if (clgetb ("scancor") && !ccdflag (im, "scancor"))
+	        return (true)
+	    iferr (ccdmean = hdmgetr (im, "ccdmean"))
+		    return (true)
+	    iferr (time = hdmgeti (im, "ccdmeant"))
+		time = IM_MTIME(im)
+	    if (time < IM_MTIME(im))
+		return (true)
+	case ILLUM:
+	    if (clgetb ("zerocor") && !ccdflag (im, "zerocor"))
+	        return (true)
+	    if (clgetb ("darkcor") && !ccdflag (im, "darkcor"))
+	        return (true)
+	    if (clgetb ("flatcor") && !ccdflag (im, "flatcor"))
+	        return (true)
+	    iferr (ccdmean = hdmgetr (im, "ccdmean"))
+		return (true)
+	default:
+	    if (clgetb ("zerocor") && !ccdflag (im, "zerocor"))
+	        return (true)
+	    if (clgetb ("darkcor") && !ccdflag (im, "darkcor"))
+	        return (true)
+	    if (clgetb ("flatcor") && !ccdflag (im, "flatcor"))
+	        return (true)
+	    if (clgetb ("illumcor") && !ccdflag (im, "illumcor"))
+	        return (true)
+	    if (clgetb ("fringecor") && !ccdflag (im, "fringcor"))
+	        return (true)
+	}
+
+	return (false)
+end
diff --git a/noao/imred/ccdred/src/ccdcmp.x b/noao/imred/ccdred/src/ccdcmp.x
new file mode 100644
index 00000000..a2687934
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdcmp.x
@@ -0,0 +1,23 @@
+# CCD_CMP -- Compare two image names with extensions ignored.
+
+bool procedure ccd_cmp (image1, image2)
+
+char	image1[ARB]		# First image
+char	image2[ARB]		# Second image
+
+int	i, j, strmatch(), strlen(), strncmp()
+bool	streq()
+
+begin
+	if (streq (image1, image2))
+	    return (true)
+
+	i = max (strmatch (image1, ".imh"), strmatch (image1, ".hhh"))
+	if (i == 0)
+	    i = strlen (image1)
+	j = max (strmatch (image2, ".imh"), strmatch (image2, ".hhh"))
+	if (j == 0)
+	    j = strlen (image2)
+
+	return (strncmp (image1, image2, max (i, j)) == 0)
+end
diff --git a/noao/imred/ccdred/src/ccdcopy.x b/noao/imred/ccdred/src/ccdcopy.x
new file mode 100644
index 00000000..a12b2123
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdcopy.x
@@ -0,0 +1,31 @@
+include	<imhdr.h>
+
+# CCDCOPY -- Copy an image.  This should be done with an IMIO procedure
+# but there isn't one yet.
+
+procedure ccdcopy (old, new)
+
+char	old[ARB]		# Image to be copied
+char	new[ARB]		# New copy
+
+int	i, nc, nl
+pointer	in, out, immap(), imgl2s(), impl2s(), imgl2r(), impl2r()
+
+begin
+	in = immap (old, READ_ONLY, 0)
+	out = immap (new, NEW_COPY, in)
+
+	nc = IM_LEN(in,1)
+	nl = IM_LEN(in,2)
+	switch (IM_PIXTYPE(in)) {
+	case TY_SHORT:
+	    do i = 1, nl
+		call amovs (Mems[imgl2s(in,i)], Mems[impl2s(out,i)], nc)
+	default:
+	    do i = 1, nl
+		call amovr (Memr[imgl2r(in,i)], Memr[impl2r(out,i)], nc)
+	}
+
+	call imunmap (in)
+	call imunmap (out)
+end
diff --git a/noao/imred/ccdred/src/ccddelete.x b/noao/imred/ccdred/src/ccddelete.x
new file mode 100644
index 00000000..90931135
--- /dev/null
+++ b/noao/imred/ccdred/src/ccddelete.x
@@ -0,0 +1,55 @@
+# CCDDELETE -- Delete an image by renaming it to a backup image.
+#
+#   1.	Get the backup prefix which may be a path name.
+#   2.  If no prefix is specified then delete the image without a backup.
+#   3.  If there is a prefix then make a backup image name.
+#       Rename the image to the backup image name.
+#
+#   The backup image name is formed by prepending the backup prefix to the
+#   image name.  If a previous backup exist append integers to the backup
+#   prefix until a nonexistant image name is created.
+
+procedure ccddelete (image)
+
+char	image[ARB]		# Image to delete (backup)
+
+int	i, imaccess()
+pointer	sp, prefix, backup
+errchk	imdelete, imrename
+
+begin
+	call smark (sp)
+	call salloc (prefix, SZ_FNAME, TY_CHAR)
+	call salloc (backup, SZ_FNAME, TY_CHAR)
+
+	# Get the backup prefix.
+	call clgstr ("backup", Memc[prefix], SZ_FNAME)
+	call xt_stripwhite (Memc[prefix])
+
+	# If there is no prefix then simply delete the image.
+	if (Memc[prefix] == EOS)
+	    call imdelete (image)
+
+	# Otherwise create a backup image name which does not exist and
+	# rename the image to the backup image.
+
+	else {
+	    i = 0
+	    repeat {
+		if (i == 0) {
+	    	    call sprintf (Memc[backup], SZ_FNAME, "%s%s")
+		        call pargstr (Memc[prefix])
+		        call pargstr (image)
+		} else {
+	            call sprintf (Memc[backup], SZ_FNAME, "%s%d%s")
+			call pargstr (Memc[prefix])
+			call pargi (i)
+			call pargstr (image)
+		}
+	        i = i + 1
+	    } until (imaccess (Memc[backup], READ_ONLY) == NO)
+	    call imrename (image, Memc[backup])
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/ccdflag.x b/noao/imred/ccdred/src/ccdflag.x
new file mode 100644
index 00000000..427365d2
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdflag.x
@@ -0,0 +1,27 @@
+# CCDFLAG -- Determine if a CCD processing flag is set.  This is less than
+# obvious because of the need to use the default value to indicate a
+# false flag.
+
+bool procedure ccdflag (im, name)
+
+pointer	im		# IMIO pointer
+char	name[ARB]	# CCD flag name
+
+bool	flag, strne()
+pointer	sp, str1, str2
+
+begin
+	call smark (sp)
+	call salloc (str1, SZ_LINE, TY_CHAR)
+	call salloc (str2, SZ_LINE, TY_CHAR)
+
+	# Get the flag string value and the default value.
+	# The flag is true if the value and the default do not match.
+
+	call hdmgstr (im, name, Memc[str1], SZ_LINE)
+	call hdmgdef (name, Memc[str2], SZ_LINE)
+	flag = strne (Memc[str1], Memc[str2])
+
+	call sfree (sp)
+	return (flag)
+end
diff --git a/noao/imred/ccdred/src/ccdinst1.key b/noao/imred/ccdred/src/ccdinst1.key
new file mode 100644
index 00000000..2a3ef1d4
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdinst1.key
@@ -0,0 +1,27 @@
+			CCDINSTRUMENT COMMANDS
+
+?		Print command summary
+help		Print command summary
+imheader	Page image header
+instrument	Print current instrument translation file
+next		Next image
+newimage	Select a new image
+quit		Quit
+read		Read instrument translation file
+show		Show current translations
+write		Write instrument translation file
+
+translate	Translate image string selected by the imagetyp parameter
+		to one of the CCDRED types given as an argument or queried:
+		    object, zero, dark, flat, comp, illum, fringe, other
+
+The following are CCDRED parameters which may be translated.  You are
+queried for the image keyword to use or it may be typed after the command.
+An optional default value (returned if the image does not contain the
+keyword) may be typed as the second argument of the command.
+
+	BASIC PARAMETERS
+imagetyp	Image type parameter (see also translate)
+subset		Subset or filter parameter
+exptime		Exposure time
+darktime	Dark time (may be same as the exposure time)
diff --git a/noao/imred/ccdred/src/ccdinst2.key b/noao/imred/ccdred/src/ccdinst2.key
new file mode 100644
index 00000000..bd909433
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdinst2.key
@@ -0,0 +1,39 @@
+			CCDINSTRUMENT COMMANDS
+
+?		Print command summary
+help		Print command summary
+imheader	Page image header
+instrument	Print current instrument translation file
+next		Next image
+newimage	Select a new image
+quit		Quit
+read		Read instrument translation file
+show		Show current translations
+write		Write instrument translation file
+
+translate	Translate image string selected by the imagetyp parameter
+		to one of the CCDRED types given as an argument or queried:
+		    object, zero, dark, flat, comp, illum, fringe, other
+
+The following are CCDRED parameters which may be translated.  You are
+queried for the image keyword to use or it may be typed after the command.
+An optional default value (returned if the image does not contain the
+keyword) may be typed as the second argument of the command.
+
+	BASIC PARAMETERS
+imagetyp	Image type parameter (see also translate)
+subset		Subset or filter parameter
+exptime		Exposure time
+darktime	Dark time (may be same as the exposure time)
+	
+	USEFUL DEFAULT GEOMETRY PARAMETERS
+biassec		Bias section (often has a default value)
+trimsec		Trim section (often has a default value)
+
+	COMMON PROCESSING FLAGS
+fixpix		Bad pixel replacement flag
+overscan	Overscan correction flag
+trim		Trim flag
+zerocor		Zero level correction flag
+darkcor		Dark count correction flag
+flatcor		Flat field correction flag
diff --git a/noao/imred/ccdred/src/ccdinst3.key b/noao/imred/ccdred/src/ccdinst3.key
new file mode 100644
index 00000000..7215aa67
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdinst3.key
@@ -0,0 +1,62 @@
+			CCDINSTRUMENT COMMANDS
+
+?		Print command summary
+help		Print command summary
+imheader	Page image header
+instrument	Print current instrument translation file
+next		Next image
+newimage	Select a new image
+quit		Quit
+read		Read instrument translation file
+show		Show current translations
+write		Write instrument translation file
+
+translate	Translate image string selected by the imagetyp parameter
+		to one of the CCDRED types given as an argument or queried:
+		    object, zero, dark, flat, comp, illum, fringe, other
+
+The following are CCDRED parameters which may be translated.  You are
+queried for the image keyword to use or it may be typed after the command.
+An optional default value (returned if the image does not contain the
+keyword) may be typed as the second argument of the command.
+
+	BASIC PARAMETERS
+imagetyp	Image type parameter (see also translate)
+subset		Subset or filter parameter
+exptime		Exposure time
+darktime	Dark time (may be same as the exposure time)
+	
+	USEFUL DEFAULT GEOMETRY PARAMETERS
+biassec		Bias section (often has a default value)
+trimsec		Trim section (often has a default value)
+
+	COMMON PROCESSING FLAGS
+fixpix		Bad pixel replacement flag
+overscan	Overscan correction flag
+trim		Trim flag
+zerocor		Zero level correction flag
+darkcor		Dark count correction flag
+flatcor		Flat field correction flag
+
+	RARELY TRANSLATED PARAMETERS
+ccdsec		CCD section
+datasec		Data section
+fixfile		Bad pixel file
+
+fringcor	Fringe correction flag
+illumcor	Ilumination correction flag
+readcor		One dimensional zero level read out correction flag
+scancor		Scan mode correction flag
+
+illumflt	Ilumination flat image
+mkfringe	Fringe image
+mkillum		Illumination image
+skyflat		Sky flat image
+
+ccdmean		Mean value
+fringscl	Fringe scale factor
+ncombine	Number of images combined
+date-obs	Date of observations
+dec		Declination
+ra		Right Ascension
+title		Image title
diff --git a/noao/imred/ccdred/src/ccdlog.x b/noao/imred/ccdred/src/ccdlog.x
new file mode 100644
index 00000000..48453704
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdlog.x
@@ -0,0 +1,46 @@
+include	<imhdr.h>
+include	<imset.h>
+
+# CCDLOG -- Log information about the processing with the image name.
+#
+#   1.  If the package "verbose" parameter is set print the string preceded
+#	by the image name.
+#   2.  If the package "logfile" parameter is not null append the string,
+#	preceded by the image name, to the file.
+
+procedure ccdlog (im, str)
+
+pointer	im			# IMIO pointer
+char	str[ARB]		# Log string
+
+int	fd, open()
+bool	clgetb()
+pointer	sp, fname
+errchk	open
+
+begin
+	call smark (sp)
+	call salloc (fname, SZ_FNAME, TY_CHAR)
+
+	# Write to the standard error output if "verbose".
+	if (clgetb ("verbose")) {
+	    call imstats (im, IM_IMAGENAME, Memc[fname], SZ_FNAME)
+	    call eprintf ("%s: %s\n")
+		call pargstr (Memc[fname])
+		call pargstr (str)
+	}
+
+	# Append to the "logfile" if not null.
+	call clgstr ("logfile", Memc[fname], SZ_FNAME)
+	call xt_stripwhite (Memc[fname])
+	if (Memc[fname] != EOS) {
+	    fd = open (Memc[fname], APPEND, TEXT_FILE)
+	    call imstats (im, IM_IMAGENAME, Memc[fname], SZ_FNAME)
+	    call fprintf (fd, "%s: %s\n")
+		call pargstr (Memc[fname])
+		call pargstr (str)
+	    call close (fd)
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/ccdmean.x b/noao/imred/ccdred/src/ccdmean.x
new file mode 100644
index 00000000..d38ea97b
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdmean.x
@@ -0,0 +1,50 @@
+include	<imhdr.h>
+
+
+# CCDMEAN -- Compute mean and add to header if needed.
+
+procedure ccdmean (input)
+
+char	input[ARB]		# Input image
+
+int	i, nc, nl, hdmgeti()
+long	time, clktime()
+bool	clgetb()
+real	mean, hdmgetr(), asumr()
+pointer	in, immap(), imgl2r()
+errchk	immap
+
+begin
+	# Check if this operation has been done.
+
+	in = immap (input, READ_WRITE, 0)
+	ifnoerr (mean = hdmgetr (in, "ccdmean")) {
+	    iferr (time = hdmgeti (in, "ccdmeant"))
+		time = IM_MTIME(in)
+	    if (time >= IM_MTIME(in)) {
+		call imunmap (in)
+		return
+	    }
+	}
+
+	if (clgetb ("noproc")) {
+	    call eprintf (
+		"  [TO BE DONE] Compute mean of image\n")
+		call pargstr (input)
+	    call imunmap (in)
+	    return
+	}
+
+	# Compute and record the mean.
+	nc = IM_LEN(in,1)
+	nl = IM_LEN(in,2)
+	mean = 0.
+	do i = 1, nl
+	    mean = mean + asumr (Memr[imgl2r(in,i)], nc)
+	mean = mean / (nc * nl)
+	time = clktime (long(0))
+	call hdmputr (in, "ccdmean", mean)
+	call hdmputi (in, "ccdmeant", int (time))
+
+	call imunmap (in)
+end
diff --git a/noao/imred/ccdred/src/ccdnscan.x b/noao/imred/ccdred/src/ccdnscan.x
new file mode 100644
index 00000000..3a9fbeba
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdnscan.x
@@ -0,0 +1,38 @@
+include	"ccdtypes.h"
+
+
+# CCDNSCAN -- Return the number CCD scan rows.
+#
+# If not found in the header return the "nscan" parameter for objects and
+# 1 for calibration images.
+
+int procedure ccdnscan (im, ccdtype)
+
+pointer	im			#I Image
+int	ccdtype			#I CCD type
+int	nscan			#O Number of scan lines
+
+bool	clgetb()
+char	type, clgetc()
+int	hdmgeti(), clgeti()
+
+begin
+	iferr (nscan = hdmgeti (im, "nscanrow")) {
+	    switch (ccdtype) {
+	    case ZERO, DARK, FLAT, ILLUM, FRINGE:
+		nscan = 1
+	    default:
+		type = clgetc ("scantype")
+		if (type == 's')
+		    nscan = clgeti ("nscan")
+		else {
+		    if (clgetb ("scancor"))
+			nscan = INDEFI
+		    else
+			nscan = 1
+		}
+	    }
+	}
+
+	return (nscan)
+end
diff --git a/noao/imred/ccdred/src/ccdproc.x b/noao/imred/ccdred/src/ccdproc.x
new file mode 100644
index 00000000..1b2a133c
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdproc.x
@@ -0,0 +1,106 @@
+include	<error.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+# CCDPROC -- Process a CCD image of a specified CCD image type.
+#
+# The input image is corrected for bad pixels, overscan levels, zero
+# levels, dark counts, flat field, illumination, and fringing.  It may also
+# be trimmed.  The checking of whether to apply each correction, getting the
+# required parameters, and logging the operations is left to separate
+# procedures, one for each correction.  The actual processing is done by
+# a specialized procedure designed to be very efficient.  These
+# procedures may also process calibration images if necessary.
+# The specified image type overrides the image type in the image header.
+# There are two data type paths; one for short data types and one for
+# all other data types (usually real).
+
+procedure ccdproc (input, ccdtype)
+
+char	input[ARB]		# CCD image to process
+int	ccdtype			# CCD type of image (independent of header).
+
+pointer	sp, output, str, in, out, ccd, immap()
+errchk	immap, set_output, ccddelete
+errchk	set_fixpix, set_zero, set_dark, set_flat, set_illum, set_fringe
+
+begin
+	call smark (sp)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Map the image, make a working output image and set the processing
+	# parameters.
+
+	in = immap (input, READ_ONLY, 0)
+	call mktemp ("tmp", Memc[output], SZ_FNAME)
+	call set_output (in, out, Memc[output])
+	call set_proc (in, out, ccd)
+	call set_sections (ccd)
+	call set_trim (ccd)
+	call set_fixpix (ccd)
+	call set_overscan (ccd)
+
+	# Set processing appropriate for the various image types.
+	switch (ccdtype) {
+	case ZERO:
+	case DARK:
+	    call set_zero (ccd)
+	case FLAT:
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+	    CORS(ccd, FINDMEAN) = YES
+	    CORS(ccd, MINREP) = YES
+	case ILLUM:
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+	    call set_flat (ccd)
+	case OBJECT, COMP:
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+	    call set_flat (ccd)
+	    call set_illum (ccd)
+	    call set_fringe (ccd)
+	default:
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+	    call set_flat (ccd)
+	    call set_illum (ccd)
+	    call set_fringe (ccd)
+	    CORS(ccd, FINDMEAN) = YES
+	}
+
+	# Do the processing if the COR flag is set.
+	if (COR(ccd) == YES) {
+	    call doproc (ccd)
+	    call set_header (ccd)
+
+	    # Replace the input by the output image.
+	    call imunmap (in)
+	    call imunmap (out)
+	    iferr (call ccddelete (input)) {
+		call imdelete (Memc[output])
+		call error (1,
+		    "Can't delete or make backup of original image")
+	    }
+	    call imrename (Memc[output], input)
+	} else {
+	    # Delete the temporary output image leaving the input unchanged.
+	    call imunmap (in)
+	    iferr (call imunmap (out))
+		;
+	    iferr (call imdelete (Memc[output]))
+		;
+	}
+	call free_proc (ccd)
+
+	# Do special processing for calibration images.
+	switch (ccdtype) {
+	case ZERO:
+	    call readcor (input)
+	case FLAT:
+	    call ccdmean (input)
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/ccdred.h b/noao/imred/ccdred/src/ccdred.h
new file mode 100644
index 00000000..2d370d86
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdred.h
@@ -0,0 +1,150 @@
+# CCDRED Data Structures and Definitions
+
+# The CCD structure:  This structure is used to communicate processing
+# parameters between the package procedures.  It contains pointers to
+# data, calibration image IMIO pointers, scaling parameters, and the
+# correction flags.  The corrections flags indicate which processing
+# operations are to be performed.  The subsection parameters do not
+# include a step size.  A step size is assumed.  If arbitrary subsampling
+# is desired this would be the next generalization.
+
+define	LEN_CCD		131		# Length of CCD structure
+
+# CCD data coordinates
+define	CCD_C1		Memi[$1]	# CCD starting column
+define	CCD_C2		Memi[$1+1]	# CCD ending column
+define	CCD_L1		Memi[$1+2]	# CCD starting line
+define	CCD_L2		Memi[$1+3]	# CCD ending line
+
+# Input data
+define	IN_IM		Memi[$1+10]	# Input image pointer
+define	IN_C1		Memi[$1+11]	# Input data starting column
+define	IN_C2		Memi[$1+12]	# Input data ending column
+define	IN_L1		Memi[$1+13]	# Input data starting line
+define	IN_L2		Memi[$1+14]	# Input data ending line
+
+# Output data
+define	OUT_IM		Memi[$1+20]	# Output image pointer
+define	OUT_C1		Memi[$1+21]	# Output data starting column
+define	OUT_C2		Memi[$1+22]	# Output data ending column
+define	OUT_L1		Memi[$1+23]	# Output data starting line
+define	OUT_L2		Memi[$1+24]	# Output data ending line
+
+# Mask data
+define  MASK_IM         Memi[$1+30]     # Mask image pointer
+define  MASK_C1         Memi[$1+31]     # Mask data starting column
+define  MASK_C2         Memi[$1+32]     # Mask data ending column
+define  MASK_L1         Memi[$1+33]     # Mask data starting line
+define  MASK_L2         Memi[$1+34]     # Mask data ending line
+define  MASK_PM         Memi[$1+35]     # Mask pointer
+define  MASK_FP         Memi[$1+36]     # Mask fixpix data
+
+# Zero level data
+define	ZERO_IM		Memi[$1+40]	# Zero level image pointer
+define	ZERO_C1		Memi[$1+41]	# Zero level data starting column
+define	ZERO_C2		Memi[$1+42]	# Zero level data ending column
+define	ZERO_L1		Memi[$1+43]	# Zero level data starting line
+define	ZERO_L2		Memi[$1+44]	# Zero level data ending line
+
+# Dark count data
+define	DARK_IM		Memi[$1+50]	# Dark count image pointer
+define	DARK_C1		Memi[$1+51]	# Dark count data starting column
+define	DARK_C2		Memi[$1+52]	# Dark count data ending column
+define	DARK_L1		Memi[$1+53]	# Dark count data starting line
+define	DARK_L2		Memi[$1+54]	# Dark count data ending line
+
+# Flat field data
+define	FLAT_IM		Memi[$1+60]	# Flat field image pointer
+define	FLAT_C1		Memi[$1+61]	# Flat field data starting column
+define	FLAT_C2		Memi[$1+62]	# Flat field data ending column
+define	FLAT_L1		Memi[$1+63]	# Flat field data starting line
+define	FLAT_L2		Memi[$1+64]	# Flat field data ending line
+
+# Illumination data
+define	ILLUM_IM	Memi[$1+70]	# Illumination image pointer
+define	ILLUM_C1	Memi[$1+71]	# Illumination data starting column
+define	ILLUM_C2	Memi[$1+72]	# Illumination data ending column
+define	ILLUM_L1	Memi[$1+73]	# Illumination data starting line
+define	ILLUM_L2	Memi[$1+74]	# Illumination data ending line
+
+# Fringe data
+define	FRINGE_IM	Memi[$1+80]	# Fringe image pointer
+define	FRINGE_C1	Memi[$1+81]	# Fringe data starting column
+define	FRINGE_C2	Memi[$1+82]	# Fringe data ending column
+define	FRINGE_L1	Memi[$1+83]	# Fringe data starting line
+define	FRINGE_L2	Memi[$1+84]	# Fringe data ending line
+
+# Trim section
+define	TRIM_C1		Memi[$1+90]	# Trim starting column
+define	TRIM_C2		Memi[$1+91]	# Trim ending column
+define	TRIM_L1		Memi[$1+92]	# Trim starting line
+define	TRIM_L2		Memi[$1+93]	# Trim ending line
+
+# Bias section
+define	BIAS_C1		Memi[$1+100]	# Bias starting column
+define	BIAS_C2		Memi[$1+101]	# Bias ending column
+define	BIAS_L1		Memi[$1+102]	# Bias starting line
+define	BIAS_L2		Memi[$1+103]	# Bias ending line
+
+define	READAXIS	Memi[$1+110]	# Read out axis (1=cols, 2=lines)
+define	CALCTYPE	Memi[$1+111]	# Calculation data type
+define	OVERSCAN_TYPE	Memi[$1+112]	# Overscan type
+define	OVERSCAN_VEC	Memi[$1+113]	# Pointer to overscan vector
+define	DARKSCALE	Memr[P2R($1+114)]	# Dark count scale factor
+define	FRINGESCALE	Memr[P2R($1+115)]	# Fringe scale factor
+define	FLATSCALE	Memr[P2R($1+116)]	# Flat field scale factor
+define	ILLUMSCALE	Memr[P2R($1+117)]	# Illumination scale factor
+define	MINREPLACE	Memr[P2R($1+118)]	# Minimum replacement value
+define	MEAN		Memr[P2R($1+119)]	# Mean of output image
+define	COR		Memi[$1+120]	# Overall correction flag
+define	CORS		Memi[$1+121+($2-1)]  # Individual correction flags
+
+# The correction array contains the following elements with array indices
+# given by the macro definitions.
+
+define	NCORS		10		# Number of corrections
+
+define	FIXPIX		1		# Fix bad pixels
+define	TRIM		2		# Trim image
+define	OVERSCAN	3		# Apply overscan correction
+define	ZEROCOR		4		# Apply zero level correction
+define	DARKCOR		5		# Apply dark count correction
+define	FLATCOR		6		# Apply flat field correction
+define	ILLUMCOR	7		# Apply illumination correction
+define	FRINGECOR	8		# Apply fringe correction
+define	FINDMEAN	9		# Find the mean of the output image
+define	MINREP		10		# Check and replace minimum value
+
+# The following definitions identify the correction values in the correction
+# array.  They are defined in terms of bit fields so that it is possible to
+# add corrections to form unique combination corrections.  Some of
+# these combinations are implemented as compound operations for efficiency.
+
+define	O	001B	# overscan
+define	Z	002B	# zero level
+define	D	004B	# dark count
+define	F	010B	# flat field
+define	I	020B	# Illumination
+define	Q	040B	# Fringe
+
+# The following correction combinations are recognized.
+
+define	ZO	003B	# zero level + overscan
+define	DO	005B	# dark count + overscan
+define	DZ	006B	# dark count + zero level
+define	DZO	007B	# dark count + zero level + overscan
+define	FO	011B	# flat field + overscan
+define	FZ	012B	# flat field + zero level
+define	FZO	013B	# flat field + zero level + overscan
+define	FD	014B	# flat field + dark count
+define	FDO	015B	# flat field + dark count + overscan
+define	FDZ	016B	# flat field + dark count + zero level
+define	FDZO	017B	# flat field + dark count + zero level + overscan
+define	QI	060B	# fringe + illumination
+
+# The following overscan functions are recognized.
+define  OVERSCAN_TYPES "|mean|median|minmax|chebyshev|legendre|spline3|spline1|"
+define  OVERSCAN_MEAN   1               # Mean of overscan
+define  OVERSCAN_MEDIAN 2               # Median of overscan
+define  OVERSCAN_MINMAX 3               # Minmax of overscan
+define  OVERSCAN_FIT    4               # Following codes are function fits
diff --git a/noao/imred/ccdred/src/ccdsection.x b/noao/imred/ccdred/src/ccdsection.x
new file mode 100644
index 00000000..aced216a
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdsection.x
@@ -0,0 +1,100 @@
+include	<ctype.h>
+
+# CCD_SECTION -- Parse a 2D image section into its elements.
+# 1. The default values must be set by the caller.
+# 2. A null image section is OK.
+# 3. The first nonwhitespace character must be '['.
+# 4. The last interpreted character must be ']'.
+#
+# This procedure should be replaced with an IMIO procedure at some
+# point.
+
+procedure ccd_section (section, x1, x2, xstep, y1, y2, ystep)
+
+char	section[ARB]		# Image section
+int	x1, x2, xstep		# X image section parameters
+int	y1, y2, ystep		# X image section parameters
+
+int	i, ip, a, b, c, temp, ctoi()
+define	error_	99
+
+begin
+	# Decode the section string.
+	ip = 1
+	while (IS_WHITE(section[ip]))
+	    ip = ip + 1
+	if (section[ip] == '[')
+	    ip = ip + 1
+	else if (section[ip] == EOS)
+	    return
+	else
+	    goto error_
+
+	do i = 1, 2 {
+	    while (IS_WHITE(section[ip]))
+	        ip = ip + 1
+
+	    # Default values
+	    if (i == 1) {
+	        a = x1
+	        b = x2
+	        c = xstep
+	    } else {
+	        a = y1
+	        b = y2
+	        c = ystep
+	    }
+
+	    # Get a:b:c.  Allow notation such as "-*:c"
+	    # (or even "-:c") where the step is obviously negative.
+
+	    if (ctoi (section, ip, temp) > 0) {			# a
+		a = temp
+	        if (section[ip] == ':') {	
+		    ip = ip + 1
+		    if (ctoi (section, ip, b) == 0)		# a:b
+		        goto error_
+	        } else
+		    b = a
+	    } else if (section[ip] == '-') {			# -*
+		temp = a
+		a = b
+		b = temp
+	        ip = ip + 1
+	        if (section[ip] == '*')
+		    ip = ip + 1
+	    } else if (section[ip] == '*')			# *
+	        ip = ip + 1
+	    if (section[ip] == ':') {				# ..:step
+	        ip = ip + 1
+	        if (ctoi (section, ip, c) == 0)
+		    goto error_
+	        else if (c == 0)
+		    goto error_
+	    }
+	    if (a > b && c > 0)
+	        c = -c
+
+	    if (i == 1) {
+		x1 = a
+		x2 = b
+		xstep = c
+	    } else {
+		y1 = a
+		y2 = b
+		ystep = c
+	    }
+
+	    while (IS_WHITE(section[ip]))
+	        ip = ip + 1
+	    if (section[ip] == ',')
+		ip = ip + 1
+	}
+
+	if (section[ip] != ']')
+	    goto error_
+
+	return
+error_
+	call error (0, "Error in image section specification")
+end
diff --git a/noao/imred/ccdred/src/ccdsubsets.x b/noao/imred/ccdred/src/ccdsubsets.x
new file mode 100644
index 00000000..528b0223
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdsubsets.x
@@ -0,0 +1,93 @@
+include	<ctype.h>
+
+
+# CCDSUBSET -- Return the CCD subset identifier.
+#
+# 1. Get the subset string and search the subset record file for the ID string.
+# 2. If the subset string is not in the record file define a default ID string
+#    based on the first word of the subset string.  If the first word is not
+#    unique append a integer to the first word until it is unique.
+# 3. Add the new subset string and identifier to the record file.
+# 4. Since the ID string is used to generate image names replace all
+#    nonimage name characters with '_'.
+#
+# It is an error if the record file cannot be created or written when needed.
+
+procedure ccdsubset (im, subset, sz_name)
+
+pointer	im			# Image
+char	subset[sz_name]		# CCD subset identifier
+int	sz_name			# Size of subset string
+
+bool	streq()
+int	i, fd, ctowrd(), open(), fscan()
+pointer	sp, fname, str1, str2, subset1, subset2, subset3
+errchk	open
+
+begin
+	call smark (sp)
+	call salloc (fname, SZ_FNAME, TY_CHAR)
+	call salloc (str1, SZ_LINE, TY_CHAR)
+	call salloc (str2, SZ_LINE, TY_CHAR)
+	call salloc (subset1, SZ_LINE, TY_CHAR)
+	call salloc (subset2, SZ_LINE, TY_CHAR)
+	call salloc (subset3, SZ_LINE, TY_CHAR)
+
+	# Get the subset record file and the subset string.
+	call clgstr ("ssfile", Memc[fname], SZ_LINE)
+	call hdmgstr (im, "subset", Memc[str1], SZ_LINE)
+
+	# The default subset identifier is the first word of the subset string.
+	i = 1
+	i = ctowrd (Memc[str1], i, Memc[subset1], SZ_LINE)
+
+	# A null subset string is ok.  If not null check for conflict
+	# with previous subset IDs.
+	if (Memc[str1] != EOS) {
+	    call strcpy (Memc[subset1], Memc[subset3], SZ_LINE)
+
+	    # Search the subset record file for the same subset string.
+	    # If found use the ID string.  If the subset ID has been
+	    # used for another subset string then increment an integer
+	    # suffix to the default ID and check the list again.
+
+	    i = 1
+	    ifnoerr (fd = open (Memc[fname], READ_ONLY, TEXT_FILE)) {
+		while (fscan (fd) != EOF) {
+		    call gargwrd (Memc[str2], SZ_LINE)
+		    call gargwrd (Memc[subset2], SZ_LINE)
+		    if (streq (Memc[str1], Memc[str2])) {
+			i = 0
+			call strcpy (Memc[subset2], Memc[subset1], SZ_LINE)
+			break
+		    } if (streq (Memc[subset1], Memc[subset2])) {
+			call sprintf (Memc[subset1], SZ_LINE, "%s%d")
+			    call pargstr (Memc[subset3])
+			    call pargi (i)
+			i = i + 1
+			call seek (fd, BOF)
+		    }
+		}
+		call close (fd)
+	    }
+
+	    # If the subset is not in the record file add it.
+	    if (i > 0) {
+		fd = open (Memc[fname], APPEND, TEXT_FILE)
+		call fprintf (fd, "'%s'\t%s\n")
+		    call pargstr (Memc[str1])
+		    call pargstr (Memc[subset1])
+		call close (fd)
+	    }
+	}
+
+	# Set the subset ID string and replace magic characters by '_'
+	# since the subset ID is used in forming image names.
+
+	call strcpy (Memc[subset1], subset, sz_name)
+	for (i=1; subset[i]!=EOS; i=i+1)
+	    if (!(IS_ALNUM(subset[i])||subset[i]=='.'))
+		subset[i] = '_'
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/ccdtypes.h b/noao/imred/ccdred/src/ccdtypes.h
new file mode 100644
index 00000000..0d5d4caf
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdtypes.h
@@ -0,0 +1,14 @@
+# Standard CCD image types.
+
+define	CCDTYPES "|object|zero|dark|flat|illum|fringe|other|comp|"
+
+define	NONE		-1
+define	UNKNOWN		0
+define	OBJECT		1
+define	ZERO		2
+define	DARK		3
+define	FLAT		4
+define	ILLUM		5
+define	FRINGE		6
+define	OTHER		7
+define	COMP		8
diff --git a/noao/imred/ccdred/src/ccdtypes.x b/noao/imred/ccdred/src/ccdtypes.x
new file mode 100644
index 00000000..bf6d29e2
--- /dev/null
+++ b/noao/imred/ccdred/src/ccdtypes.x
@@ -0,0 +1,72 @@
+include	"ccdtypes.h"
+
+# CCDTYPES -- Return the CCD type name string.
+# CCDTYPEI -- Return the CCD type code.
+
+
+# CCDTYPES -- Return the CCD type name string.
+
+procedure ccdtypes (im, name, sz_name)
+
+pointer	im			# Image
+char	name[sz_name]		# CCD type name
+int	sz_name			# Size of name string
+
+int	strdic()
+pointer	sp, str
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the image type string.  If none then return "none".
+	# Otherwise get the corresponding package image type string.
+	# If the image type is unknown return "unknown" otherwise return
+	# the package name.
+
+	call hdmgstr (im, "imagetyp", Memc[str], SZ_LINE)
+	if (Memc[str] == EOS) {
+	    call strcpy ("none", name, sz_name)
+	} else {
+	    call hdmname (Memc[str], name, sz_name)
+	    if (name[1] == EOS)
+		call strcpy (Memc[str], name, sz_name)
+	    if (strdic (name, name, sz_name, CCDTYPES) == UNKNOWN)
+	    	call strcpy ("unknown", name, sz_name)
+	}
+
+	call sfree (sp)
+end
+
+
+# CCDTYPEI -- Return the CCD type code.
+
+int procedure ccdtypei (im)
+
+pointer	im			# Image
+int	ccdtype			# CCD type (returned)
+
+pointer	sp, str1, str2
+int	strdic()
+
+begin
+	call smark (sp)
+	call salloc (str1, SZ_LINE, TY_CHAR)
+	call salloc (str2, SZ_LINE, TY_CHAR)
+
+	# Get the image type and if there is none then return the NONE code.
+	call hdmgstr (im, "imagetyp", Memc[str1], SZ_LINE)
+	if (Memc[str1] == EOS) {
+	    ccdtype = NONE
+
+	# Otherwise get the package type and convert to an image type code.
+	} else {
+	    call hdmname (Memc[str1], Memc[str2], SZ_LINE)
+	    if (Memc[str2] == EOS)
+		call strcpy (Memc[str1], Memc[str2], SZ_LINE)
+	    ccdtype = strdic (Memc[str2], Memc[str2], SZ_LINE, CCDTYPES)
+	}
+
+	call sfree (sp)
+	return (ccdtype)
+end
diff --git a/noao/imred/ccdred/src/combine/generic/icaclip.x b/noao/imred/ccdred/src/combine/generic/icaclip.x
new file mode 100644
index 00000000..1530145c
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/icaclip.x
@@ -0,0 +1,1102 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		3	# Minimum number of images for this algorithm
+
+
+# IC_AAVSIGCLIP -- Reject pixels using an average sigma about the average
+# The average sigma is normalized by the expected poisson sigma.
+
+procedure ic_aavsigclips (d, m, n, scales, zeros, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+real	d1, low, high, sum, a, s, s1, r, one
+data	one /1.0/
+pointer	sp, sums, resid, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (sums, npts, TY_REAL)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Since the unweighted average is computed here possibly skip combining
+	if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	# Compute the unweighted average with the high and low rejected and
+	# the poisson scaled average sigma.  There must be at least three
+	# pixels at each point to define the average and contributions to
+	# the mean sigma.  Corrections for differences in the image
+	# scale factors are selected by the doscale1 flag.
+
+	nin = n[1]
+	s = 0.
+	n2 = 0
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (n1 < 3)
+		next
+
+	    # Unweighted average with the high and low rejected
+	    low = Mems[d[1]+k]
+	    high = Mems[d[2]+k]
+	    if (low > high) {
+		d1 = low
+		low = high
+		high = d1
+	    }
+	    sum = 0.
+	    do j = 3, n1 {
+	       d1 = Mems[d[j]+k]
+	       if (d1 < low) {
+		   sum = sum + low
+		   low = d1
+		} else if (d1 > high) {
+		    sum = sum + high
+		    high = d1
+		} else
+		    sum = sum + d1
+	    }
+	    a = sum / (n1 - 2)
+	    sum = sum + low + high
+
+	    # Poisson scaled sigma accumulation
+	    if (doscale1) {
+		do j = 1, n1 {
+		    dp1 = d[j] + k
+		    mp1 = m[j] + k
+
+		    d1 = Mems[dp1]
+		    l = Memi[mp1]
+		    s1 = max (one, (a + zeros[l]) /  scales[l])
+		    s = s + (d1 - a) ** 2 / s1
+		}
+	    } else {
+		s1 = max (one, a)
+		do j = 1, n1
+		    s = s + (Mems[d[j]+k] - a) ** 2 / s1
+	    }
+	    n2 = n2 + n1
+
+	    # Save the average and sum for later.
+	    average[i] = a
+	    Memr[sums+k] = sum
+	}
+
+	# Here is the final sigma.
+	if (n2 > 1)
+	    s = sqrt (s / (n2 - 1))
+
+	# Reject pixels and compute the final average (if needed).
+	# There must be at least three pixels at each point for rejection.
+	# Iteratively scale the mean sigma and reject pixels
+	# Compact the data and keep track of the image IDs if needed.
+
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 <= max (2, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Mems[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Mems[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    a = average[i]
+	    sum = Memr[sums+k]
+
+	    repeat {
+		n2 = n1
+		if (s > 0.) {
+		    if (doscale1) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    mp1 = m[j] + k
+
+			    d1 = Mems[dp1]
+			    l = Memi[mp1]
+			    s1 = s * sqrt (max (one, (a+zeros[l]) /  scales[l]))
+			    r = (d1 - a) / s1
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs(r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    mp2 = m[n1] + k
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    } else {
+			s1 = s * sqrt (max (one, a))
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    d1 = Mems[dp1]
+			    r = (d1 - a) / s1
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs(r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[n1] + k
+					l = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = l
+				    }
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+		if (n1 > 1)
+		    a = sum / n1
+	    } until (n1 == n2 || n1 <= max (2, maxkeep))
+
+	    # If too many are rejected add some back in.
+	    # Pixels with equal residuals are added together.
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mems[dp1]
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Mems[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mems[dp1]
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Mems[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+		if (n1 > 1)
+		    a = sum / n1
+	    }
+
+	    # Save the average if needed.
+	    n[i] = n1
+	    if (!docombine) {
+		if (n1 > 0)
+		    average[i] = a
+		else
+		    average[i] = blank
+	    }
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_MAVSIGCLIP -- Reject pixels using an average sigma about the median
+# The average sigma is normalized by the expected poisson sigma.
+
+procedure ic_mavsigclips (d, m, n, scales, zeros, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+pointer	sp, resid, mp1, mp2
+real	med, low, high, r, s, s1, one
+data	one /1.0/
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Compute the poisson scaled average sigma about the median.
+	# There must be at least three pixels at each point to define
+	# the mean sigma.  Corrections for differences in the image
+	# scale factors are selected by the doscale1 flag.
+
+	s = 0.
+	n2 = 0
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (n1 < 3) {
+		if (n1 == 0)
+		    median[i] = blank
+		else if (n1 == 1)
+		    median[i] = Mems[d[1]+k]
+		else {
+		    low = Mems[d[1]+k]
+		    high = Mems[d[2]+k]
+		    median[i] = (low + high) / 2.
+		}
+		next
+	    }
+
+	    # Median
+	    n3 = 1 + n1 / 2
+	    if (mod (n1, 2) == 0) {
+		low = Mems[d[n3-1]+k]
+		high = Mems[d[n3]+k]
+		med = (low + high) / 2.
+	    } else
+		med = Mems[d[n3]+k]
+
+	    # Poisson scaled sigma accumulation
+	    if (doscale1) {
+		do j = 1, n1 {
+		    l = Memi[m[j]+k]
+		    s1 = max (one, (med + zeros[l]) /  scales[l])
+		    s = s + (Mems[d[j]+k] - med) ** 2 / s1
+		}
+	    } else {
+		s1 = max (one, med)
+		do j = 1, n1
+		    s = s + (Mems[d[j]+k] - med) ** 2 / s1
+	    }
+	    n2 = n2 + n1
+
+	    # Save the median for later.
+	    median[i] = med
+	}
+
+	# Here is the final sigma.
+	if (n2 > 1)
+	    s = sqrt (s / (n2 - 1))
+	else
+	    return
+
+	# Compute individual sigmas and iteratively clip.
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 < max (3, maxkeep+1))
+		next
+	    nl = 1
+	    nh = n1
+	    med = median[i]
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 >= max (MINCLIP, maxkeep+1) && s > 0.) {
+		    if (doscale1) {
+			for (; nl <= n2; nl = nl + 1) {
+			    l = Memi[m[nl]+k]
+			    s1 = s * sqrt (max (one, (med+zeros[l])/scales[l]))
+			    r = (med - Mems[d[nl]+k]) / s1
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    l = Memi[m[nh]+k]
+			    s1 = s * sqrt (max (one, (med+zeros[l])/scales[l]))
+			    r = (Mems[d[nh]+k] - med) / s1
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    } else {
+			s1 = s * sqrt (max (one, med))
+			for (; nl <= n2; nl = nl + 1) {
+			    r = (med - Mems[d[nl]+k]) / s1
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    r = (Mems[d[nh]+k] - med) / s1
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    }
+
+		    # Recompute median
+		    if (n1 < n2) {
+			if (n1 > 0) {
+			    n3 = nl + n1 / 2
+			    if (mod (n1, 2) == 0) {
+				low = Mems[d[n3-1]+k]
+				high = Mems[d[n3]+k]
+				med = (low + high) / 2.
+			    } else
+				med = Mems[d[n3]+k]
+			} else
+			    med = blank
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    # If too many are rejected add some back in.
+	    # Pixels with equal residuals are added together.
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+
+		# Recompute median
+		if (n1 < n2) {
+		    if (n1 > 0) {
+			n3 = nl + n1 / 2
+			if (mod (n1, 2) == 0) {
+			    low = Mems[d[n3-1]+k]
+			    high = Mems[d[n3]+k]
+			    med = (low + high) / 2.
+			} else
+			    med = Mems[d[n3]+k]
+		    } else
+			med = blank
+		}
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mems[d[l]+k] = Mems[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mems[d[l]+k] = Mems[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median is computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+
+# IC_AAVSIGCLIP -- Reject pixels using an average sigma about the average
+# The average sigma is normalized by the expected poisson sigma.
+
+procedure ic_aavsigclipr (d, m, n, scales, zeros, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+real	d1, low, high, sum, a, s, s1, r, one
+data	one /1.0/
+pointer	sp, sums, resid, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (sums, npts, TY_REAL)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Since the unweighted average is computed here possibly skip combining
+	if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	# Compute the unweighted average with the high and low rejected and
+	# the poisson scaled average sigma.  There must be at least three
+	# pixels at each point to define the average and contributions to
+	# the mean sigma.  Corrections for differences in the image
+	# scale factors are selected by the doscale1 flag.
+
+	nin = n[1]
+	s = 0.
+	n2 = 0
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (n1 < 3)
+		next
+
+	    # Unweighted average with the high and low rejected
+	    low = Memr[d[1]+k]
+	    high = Memr[d[2]+k]
+	    if (low > high) {
+		d1 = low
+		low = high
+		high = d1
+	    }
+	    sum = 0.
+	    do j = 3, n1 {
+	       d1 = Memr[d[j]+k]
+	       if (d1 < low) {
+		   sum = sum + low
+		   low = d1
+		} else if (d1 > high) {
+		    sum = sum + high
+		    high = d1
+		} else
+		    sum = sum + d1
+	    }
+	    a = sum / (n1 - 2)
+	    sum = sum + low + high
+
+	    # Poisson scaled sigma accumulation
+	    if (doscale1) {
+		do j = 1, n1 {
+		    dp1 = d[j] + k
+		    mp1 = m[j] + k
+
+		    d1 = Memr[dp1]
+		    l = Memi[mp1]
+		    s1 = max (one, (a + zeros[l]) /  scales[l])
+		    s = s + (d1 - a) ** 2 / s1
+		}
+	    } else {
+		s1 = max (one, a)
+		do j = 1, n1
+		    s = s + (Memr[d[j]+k] - a) ** 2 / s1
+	    }
+	    n2 = n2 + n1
+
+	    # Save the average and sum for later.
+	    average[i] = a
+	    Memr[sums+k] = sum
+	}
+
+	# Here is the final sigma.
+	if (n2 > 1)
+	    s = sqrt (s / (n2 - 1))
+
+	# Reject pixels and compute the final average (if needed).
+	# There must be at least three pixels at each point for rejection.
+	# Iteratively scale the mean sigma and reject pixels
+	# Compact the data and keep track of the image IDs if needed.
+
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 <= max (2, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Memr[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Memr[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    a = average[i]
+	    sum = Memr[sums+k]
+
+	    repeat {
+		n2 = n1
+		if (s > 0.) {
+		    if (doscale1) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    mp1 = m[j] + k
+
+			    d1 = Memr[dp1]
+			    l = Memi[mp1]
+			    s1 = s * sqrt (max (one, (a+zeros[l]) /  scales[l]))
+			    r = (d1 - a) / s1
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs(r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    mp2 = m[n1] + k
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    } else {
+			s1 = s * sqrt (max (one, a))
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    d1 = Memr[dp1]
+			    r = (d1 - a) / s1
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs(r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[n1] + k
+					l = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = l
+				    }
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+		if (n1 > 1)
+		    a = sum / n1
+	    } until (n1 == n2 || n1 <= max (2, maxkeep))
+
+	    # If too many are rejected add some back in.
+	    # Pixels with equal residuals are added together.
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Memr[dp1]
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Memr[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Memr[dp1]
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Memr[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+		if (n1 > 1)
+		    a = sum / n1
+	    }
+
+	    # Save the average if needed.
+	    n[i] = n1
+	    if (!docombine) {
+		if (n1 > 0)
+		    average[i] = a
+		else
+		    average[i] = blank
+	    }
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_MAVSIGCLIP -- Reject pixels using an average sigma about the median
+# The average sigma is normalized by the expected poisson sigma.
+
+procedure ic_mavsigclipr (d, m, n, scales, zeros, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+pointer	sp, resid, mp1, mp2
+real	med, low, high, r, s, s1, one
+data	one /1.0/
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Compute the poisson scaled average sigma about the median.
+	# There must be at least three pixels at each point to define
+	# the mean sigma.  Corrections for differences in the image
+	# scale factors are selected by the doscale1 flag.
+
+	s = 0.
+	n2 = 0
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (n1 < 3) {
+		if (n1 == 0)
+		    median[i] = blank
+		else if (n1 == 1)
+		    median[i] = Memr[d[1]+k]
+		else {
+		    low = Memr[d[1]+k]
+		    high = Memr[d[2]+k]
+		    median[i] = (low + high) / 2.
+		}
+		next
+	    }
+
+	    # Median
+	    n3 = 1 + n1 / 2
+	    if (mod (n1, 2) == 0) {
+		low = Memr[d[n3-1]+k]
+		high = Memr[d[n3]+k]
+		med = (low + high) / 2.
+	    } else
+		med = Memr[d[n3]+k]
+
+	    # Poisson scaled sigma accumulation
+	    if (doscale1) {
+		do j = 1, n1 {
+		    l = Memi[m[j]+k]
+		    s1 = max (one, (med + zeros[l]) /  scales[l])
+		    s = s + (Memr[d[j]+k] - med) ** 2 / s1
+		}
+	    } else {
+		s1 = max (one, med)
+		do j = 1, n1
+		    s = s + (Memr[d[j]+k] - med) ** 2 / s1
+	    }
+	    n2 = n2 + n1
+
+	    # Save the median for later.
+	    median[i] = med
+	}
+
+	# Here is the final sigma.
+	if (n2 > 1)
+	    s = sqrt (s / (n2 - 1))
+	else
+	    return
+
+	# Compute individual sigmas and iteratively clip.
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 < max (3, maxkeep+1))
+		next
+	    nl = 1
+	    nh = n1
+	    med = median[i]
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 >= max (MINCLIP, maxkeep+1) && s > 0.) {
+		    if (doscale1) {
+			for (; nl <= n2; nl = nl + 1) {
+			    l = Memi[m[nl]+k]
+			    s1 = s * sqrt (max (one, (med+zeros[l])/scales[l]))
+			    r = (med - Memr[d[nl]+k]) / s1
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    l = Memi[m[nh]+k]
+			    s1 = s * sqrt (max (one, (med+zeros[l])/scales[l]))
+			    r = (Memr[d[nh]+k] - med) / s1
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    } else {
+			s1 = s * sqrt (max (one, med))
+			for (; nl <= n2; nl = nl + 1) {
+			    r = (med - Memr[d[nl]+k]) / s1
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    r = (Memr[d[nh]+k] - med) / s1
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    }
+
+		    # Recompute median
+		    if (n1 < n2) {
+			if (n1 > 0) {
+			    n3 = nl + n1 / 2
+			    if (mod (n1, 2) == 0) {
+				low = Memr[d[n3-1]+k]
+				high = Memr[d[n3]+k]
+				med = (low + high) / 2.
+			    } else
+				med = Memr[d[n3]+k]
+			} else
+			    med = blank
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    # If too many are rejected add some back in.
+	    # Pixels with equal residuals are added together.
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+
+		# Recompute median
+		if (n1 < n2) {
+		    if (n1 > 0) {
+			n3 = nl + n1 / 2
+			if (mod (n1, 2) == 0) {
+			    low = Memr[d[n3-1]+k]
+			    high = Memr[d[n3]+k]
+			    med = (low + high) / 2.
+			} else
+			    med = Memr[d[n3]+k]
+		    } else
+			med = blank
+		}
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Memr[d[l]+k] = Memr[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Memr[d[l]+k] = Memr[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median is computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/combine/generic/icaverage.x b/noao/imred/ccdred/src/combine/generic/icaverage.x
new file mode 100644
index 00000000..3646b725
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/icaverage.x
@@ -0,0 +1,163 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"../icombine.h"
+
+
+# IC_AVERAGE -- Compute the average image line.
+# Options include a weight average.
+
+procedure ic_averages (d, m, n, wts, npts, average)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image ID pointers
+int	n[npts]			# Number of points
+real	wts[ARB]		# Weights
+int	npts			# Number of output points per line
+real	average[npts]		# Average (returned)
+
+int	i, j, k
+real	sumwt, wt
+real	sum
+
+include	"../icombine.com"
+
+begin
+	# If no data has been excluded do the average without checking the
+	# number of points and using the fact that the weights are normalized.
+	# If all the data has been excluded set the average to the blank value.
+
+	if (dflag == D_ALL) {
+	    if (dowts) {
+		do i = 1, npts {
+		    k = i - 1
+		    wt = wts[Memi[m[1]+k]]
+		    sum = Mems[d[1]+k] * wt
+		    do j = 2, n[i] {
+			wt = wts[Memi[m[j]+k]]
+			sum = sum + Mems[d[j]+k] * wt
+		    }
+		    average[i] = sum
+		}
+	    } else {
+		do i = 1, npts {
+		    k = i - 1
+		    sum = Mems[d[1]+k]
+		    do j = 2, n[i]
+			sum = sum + Mems[d[j]+k]
+		    average[i] = sum / n[i]
+		}
+	    }
+	} else if (dflag == D_NONE) {
+	    do i = 1, npts
+		average[i] = blank
+	} else {
+	    if (dowts) {
+		do i = 1, npts {
+		    if (n[i] > 0) {
+			k = i - 1
+			wt = wts[Memi[m[1]+k]]
+			sum = Mems[d[1]+k] * wt
+			sumwt = wt
+			do j = 2, n[i] {
+			    wt = wts[Memi[m[j]+k]]
+			    sum = sum + Mems[d[j]+k] * wt
+			    sumwt = sumwt + wt
+			}
+			average[i] = sum / sumwt
+		    } else
+			average[i] = blank
+		}
+	    } else {
+		do i = 1, npts {
+		    if (n[i] > 0) {
+			k = i - 1
+			sum = Mems[d[1]+k]
+			do j = 2, n[i]
+			    sum = sum + Mems[d[j]+k]
+			average[i] = sum / n[i]
+		    } else
+			average[i] = blank
+		}
+	    }
+	}
+end
+
+# IC_AVERAGE -- Compute the average image line.
+# Options include a weight average.
+
+procedure ic_averager (d, m, n, wts, npts, average)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image ID pointers
+int	n[npts]			# Number of points
+real	wts[ARB]		# Weights
+int	npts			# Number of output points per line
+real	average[npts]		# Average (returned)
+
+int	i, j, k
+real	sumwt, wt
+real	sum
+
+include	"../icombine.com"
+
+begin
+	# If no data has been excluded do the average without checking the
+	# number of points and using the fact that the weights are normalized.
+	# If all the data has been excluded set the average to the blank value.
+
+	if (dflag == D_ALL) {
+	    if (dowts) {
+		do i = 1, npts {
+		    k = i - 1
+		    wt = wts[Memi[m[1]+k]]
+		    sum = Memr[d[1]+k] * wt
+		    do j = 2, n[i] {
+			wt = wts[Memi[m[j]+k]]
+			sum = sum + Memr[d[j]+k] * wt
+		    }
+		    average[i] = sum
+		}
+	    } else {
+		do i = 1, npts {
+		    k = i - 1
+		    sum = Memr[d[1]+k]
+		    do j = 2, n[i]
+			sum = sum + Memr[d[j]+k]
+		    average[i] = sum / n[i]
+		}
+	    }
+	} else if (dflag == D_NONE) {
+	    do i = 1, npts
+		average[i] = blank
+	} else {
+	    if (dowts) {
+		do i = 1, npts {
+		    if (n[i] > 0) {
+			k = i - 1
+			wt = wts[Memi[m[1]+k]]
+			sum = Memr[d[1]+k] * wt
+			sumwt = wt
+			do j = 2, n[i] {
+			    wt = wts[Memi[m[j]+k]]
+			    sum = sum + Memr[d[j]+k] * wt
+			    sumwt = sumwt + wt
+			}
+			average[i] = sum / sumwt
+		    } else
+			average[i] = blank
+		}
+	    } else {
+		do i = 1, npts {
+		    if (n[i] > 0) {
+			k = i - 1
+			sum = Memr[d[1]+k]
+			do j = 2, n[i]
+			    sum = sum + Memr[d[j]+k]
+			average[i] = sum / n[i]
+		    } else
+			average[i] = blank
+		}
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/src/combine/generic/iccclip.x b/noao/imred/ccdred/src/combine/generic/iccclip.x
new file mode 100644
index 00000000..57709064
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/iccclip.x
@@ -0,0 +1,898 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		2	# Mininum number of images for algorithm
+
+
+# IC_ACCDCLIP -- Reject pixels using CCD noise parameters about the average
+
+procedure ic_accdclips (d, m, n, scales, zeros, nm, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+real	nm[3,nimages]		# Noise model parameters
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+real	d1, low, high, sum, a, s, r, zero
+data	zero /0.0/
+pointer	sp, resid, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are no pixels go on to the combining.  Since the unweighted
+	# average is computed here possibly skip the combining later.
+
+	# There must be at least max (1, nkeep) pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	} else if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# There must be at least two pixels for rejection.  The initial
+	# average is the low/high rejected average except in the case of
+	# just two pixels.  The rejections are iterated and the average
+	# is recomputed.  Corrections for scaling may be performed.
+	# Depending on other flags the image IDs may also need to be adjusted.
+
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 <= max (MINCLIP-1, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Mems[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Mems[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    repeat {
+		if (n1 == 2) {
+		    sum = Mems[d[1]+k]
+		    sum = sum + Mems[d[2]+k]
+		    a = sum / 2
+		} else {
+		    low = Mems[d[1]+k]
+		    high = Mems[d[2]+k]
+		    if (low > high) {
+			d1 = low
+			low = high
+			high = d1
+		    }
+		    sum = 0.
+		    do j = 3, n1 {
+		       d1 = Mems[d[j]+k]
+		       if (d1 < low) {
+			   sum = sum + low
+			   low = d1
+			} else if (d1 > high) {
+			    sum = sum + high
+			    high = d1
+			} else
+			    sum = sum + d1
+		    }
+		    a = sum / (n1 - 2)
+		    sum = sum + low + high
+		}
+		n2 = n1
+		if (doscale1) {
+		    for (j=1; j<=n1; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+
+			l = Memi[mp1]
+			s = scales[l]
+			d1 = max (zero, s * (a + zeros[l]))
+			s = sqrt (nm[1,l] + d1/nm[2,l] + (d1*nm[3,l])**2) / s
+
+			d1 = Mems[dp1]
+			r = (d1 - a) / s
+			if (r < -lsigma || r > hsigma) {
+			    Memr[resid+n1] = abs(r)
+			    if (j < n1) {
+				dp2 = d[n1] + k
+				Mems[dp1] = Mems[dp2]
+				Mems[dp2] = d1
+				mp2 = m[n1] + k
+				Memi[mp1] = Memi[mp2]
+				Memi[mp2] = l
+				j = j - 1
+			    }
+			    sum = sum - d1
+			    n1 = n1 - 1
+			}
+		    }
+		} else {
+		    if (!keepids) {
+			s = max (zero, a)
+			s = sqrt (nm[1,1] + s/nm[2,1] + (s*nm[3,1])**2)
+		    }
+		    for (j=1; j<=n1; j=j+1) {
+			if (keepids) {
+			    l = Memi[m[j]+k]
+			    s = max (zero, a)
+			    s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			}
+			dp1 = d[j] + k
+			d1 = Mems[dp1]
+			r = (d1 - a) / s
+			if (r < -lsigma || r > hsigma) {
+			    Memr[resid+n1] = abs(r)
+			    if (j < n1) {
+				dp2 = d[n1] + k
+				Mems[dp1] = Mems[dp2]
+				Mems[dp2] = d1
+				if (keepids) {
+				    mp1 = m[j] + k
+				    mp2 = m[n1] + k
+				    l = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				}
+				j = j - 1
+			    }
+			    sum = sum - d1
+			    n1 = n1 - 1
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mems[dp1]
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Mems[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mems[dp1]
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Mems[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+	    }
+
+	    n[i] = n1
+	    if (!docombine)
+		if (n1 > 0)
+		    average[i] = sum / n1
+		else
+		    average[i] = blank
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_CCDCLIP -- Reject pixels using CCD noise parameters about the median
+
+procedure ic_mccdclips (d, m, n, scales, zeros, nm, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+real	nm[3,nimages]		# Noise model
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+real	r, s
+pointer	sp, resid, mp1, mp2
+real	med, zero
+data	zero /0.0/
+
+include	"../icombine.com"
+
+begin
+	# There must be at least max (MINCLIP, nkeep+1) pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Compute median and sigma and iteratively clip.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    nl = 1
+	    nh = n1
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 == 0)
+		    med = blank
+		else if (mod (n1, 2) == 0) {
+		    med = Mems[d[n3-1]+k]
+		    med = (med + Mems[d[n3]+k]) / 2.
+		} else
+		    med = Mems[d[n3]+k]
+
+		if (n1 >= max (MINCLIP, maxkeep+1)) {
+		    if (doscale1) {
+			for (; nl <= n2; nl = nl + 1) {
+			    l = Memi[m[nl]+k]
+			    s = scales[l]
+			    r = max (zero, s * (med + zeros[l]))
+			    s = sqrt (nm[1,l] + r/nm[2,l] + (r*nm[3,l])**2) / s
+			    r = (med - Mems[d[nl]+k]) / s
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    l = Memi[m[nh]+k]
+			    s = scales[l]
+			    r = max (zero, s * (med + zeros[l]))
+			    s = sqrt (nm[1,l] + r/nm[2,l] + (r*nm[3,l])**2) / s
+			    r = (Mems[d[nh]+k] - med) / s
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    } else {
+			if (!keepids) {
+			    s = max (zero, med)
+			    s = sqrt (nm[1,1] + s/nm[2,1] + (s*nm[3,1])**2)
+			}
+			for (; nl <= n2; nl = nl + 1) {
+			    if (keepids) {
+				l = Memi[m[nl]+k]
+				s = max (zero, med)
+				s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			    }
+			    r = (med - Mems[d[nl]+k]) / s
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    if (keepids) {
+				l = Memi[m[nh]+k]
+				s = max (zero, med)
+				s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			    }
+			    r = (Mems[d[nh]+k] -  med) / s
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mems[d[l]+k] = Mems[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mems[d[l]+k] = Mems[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median is computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+
+# IC_ACCDCLIP -- Reject pixels using CCD noise parameters about the average
+
+procedure ic_accdclipr (d, m, n, scales, zeros, nm, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+real	nm[3,nimages]		# Noise model parameters
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+real	d1, low, high, sum, a, s, r, zero
+data	zero /0.0/
+pointer	sp, resid, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are no pixels go on to the combining.  Since the unweighted
+	# average is computed here possibly skip the combining later.
+
+	# There must be at least max (1, nkeep) pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	} else if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# There must be at least two pixels for rejection.  The initial
+	# average is the low/high rejected average except in the case of
+	# just two pixels.  The rejections are iterated and the average
+	# is recomputed.  Corrections for scaling may be performed.
+	# Depending on other flags the image IDs may also need to be adjusted.
+
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 <= max (MINCLIP-1, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Memr[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Memr[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    repeat {
+		if (n1 == 2) {
+		    sum = Memr[d[1]+k]
+		    sum = sum + Memr[d[2]+k]
+		    a = sum / 2
+		} else {
+		    low = Memr[d[1]+k]
+		    high = Memr[d[2]+k]
+		    if (low > high) {
+			d1 = low
+			low = high
+			high = d1
+		    }
+		    sum = 0.
+		    do j = 3, n1 {
+		       d1 = Memr[d[j]+k]
+		       if (d1 < low) {
+			   sum = sum + low
+			   low = d1
+			} else if (d1 > high) {
+			    sum = sum + high
+			    high = d1
+			} else
+			    sum = sum + d1
+		    }
+		    a = sum / (n1 - 2)
+		    sum = sum + low + high
+		}
+		n2 = n1
+		if (doscale1) {
+		    for (j=1; j<=n1; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+
+			l = Memi[mp1]
+			s = scales[l]
+			d1 = max (zero, s * (a + zeros[l]))
+			s = sqrt (nm[1,l] + d1/nm[2,l] + (d1*nm[3,l])**2) / s
+
+			d1 = Memr[dp1]
+			r = (d1 - a) / s
+			if (r < -lsigma || r > hsigma) {
+			    Memr[resid+n1] = abs(r)
+			    if (j < n1) {
+				dp2 = d[n1] + k
+				Memr[dp1] = Memr[dp2]
+				Memr[dp2] = d1
+				mp2 = m[n1] + k
+				Memi[mp1] = Memi[mp2]
+				Memi[mp2] = l
+				j = j - 1
+			    }
+			    sum = sum - d1
+			    n1 = n1 - 1
+			}
+		    }
+		} else {
+		    if (!keepids) {
+			s = max (zero, a)
+			s = sqrt (nm[1,1] + s/nm[2,1] + (s*nm[3,1])**2)
+		    }
+		    for (j=1; j<=n1; j=j+1) {
+			if (keepids) {
+			    l = Memi[m[j]+k]
+			    s = max (zero, a)
+			    s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			}
+			dp1 = d[j] + k
+			d1 = Memr[dp1]
+			r = (d1 - a) / s
+			if (r < -lsigma || r > hsigma) {
+			    Memr[resid+n1] = abs(r)
+			    if (j < n1) {
+				dp2 = d[n1] + k
+				Memr[dp1] = Memr[dp2]
+				Memr[dp2] = d1
+				if (keepids) {
+				    mp1 = m[j] + k
+				    mp2 = m[n1] + k
+				    l = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				}
+				j = j - 1
+			    }
+			    sum = sum - d1
+			    n1 = n1 - 1
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Memr[dp1]
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Memr[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Memr[dp1]
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Memr[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+	    }
+
+	    n[i] = n1
+	    if (!docombine)
+		if (n1 > 0)
+		    average[i] = sum / n1
+		else
+		    average[i] = blank
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_CCDCLIP -- Reject pixels using CCD noise parameters about the median
+
+procedure ic_mccdclipr (d, m, n, scales, zeros, nm, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+real	nm[3,nimages]		# Noise model
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+real	r, s
+pointer	sp, resid, mp1, mp2
+real	med, zero
+data	zero /0.0/
+
+include	"../icombine.com"
+
+begin
+	# There must be at least max (MINCLIP, nkeep+1) pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Compute median and sigma and iteratively clip.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    nl = 1
+	    nh = n1
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 == 0)
+		    med = blank
+		else if (mod (n1, 2) == 0) {
+		    med = Memr[d[n3-1]+k]
+		    med = (med + Memr[d[n3]+k]) / 2.
+		} else
+		    med = Memr[d[n3]+k]
+
+		if (n1 >= max (MINCLIP, maxkeep+1)) {
+		    if (doscale1) {
+			for (; nl <= n2; nl = nl + 1) {
+			    l = Memi[m[nl]+k]
+			    s = scales[l]
+			    r = max (zero, s * (med + zeros[l]))
+			    s = sqrt (nm[1,l] + r/nm[2,l] + (r*nm[3,l])**2) / s
+			    r = (med - Memr[d[nl]+k]) / s
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    l = Memi[m[nh]+k]
+			    s = scales[l]
+			    r = max (zero, s * (med + zeros[l]))
+			    s = sqrt (nm[1,l] + r/nm[2,l] + (r*nm[3,l])**2) / s
+			    r = (Memr[d[nh]+k] - med) / s
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    } else {
+			if (!keepids) {
+			    s = max (zero, med)
+			    s = sqrt (nm[1,1] + s/nm[2,1] + (s*nm[3,1])**2)
+			}
+			for (; nl <= n2; nl = nl + 1) {
+			    if (keepids) {
+				l = Memi[m[nl]+k]
+				s = max (zero, med)
+				s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			    }
+			    r = (med - Memr[d[nl]+k]) / s
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    if (keepids) {
+				l = Memi[m[nh]+k]
+				s = max (zero, med)
+				s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			    }
+			    r = (Memr[d[nh]+k] -  med) / s
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Memr[d[l]+k] = Memr[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Memr[d[l]+k] = Memr[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median is computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/combine/generic/icgdata.x b/noao/imred/ccdred/src/combine/generic/icgdata.x
new file mode 100644
index 00000000..5c6ac18c
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/icgdata.x
@@ -0,0 +1,459 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	<mach.h>
+include	"../icombine.h"
+
+
+# IC_GDATA -- Get line of image and mask data and apply threshold and scaling.
+# Entirely empty lines are excluded.  The data are compacted within the
+# input data buffers.  If it is required, the connection to the original
+# image index is keeped in the returned m data pointers.
+
+procedure ic_gdatas (in, out, dbuf, d, id, n, m, lflag, offsets, scales,
+	zeros, nimages, npts, v1, v2)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+pointer	dbuf[nimages]		# Data buffers for nonaligned images
+pointer	d[nimages]		# Data pointers
+pointer	id[nimages]		# ID pointers
+int	n[npts]			# Number of good pixels
+pointer	m[nimages]		# Mask pointers
+int	lflag[nimages]		# Empty mask flags
+int	offsets[nimages,ARB]	# Image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero offset factors
+int	nimages			# Number of input images
+int	npts			# NUmber of output points per line
+long	v1[ARB], v2[ARB]	# Line vectors
+
+int	i, j, k, l, ndim, nused
+real	a, b
+pointer	buf, dp, ip, mp, imgnls()
+
+include	"../icombine.com"
+
+begin
+	# Get masks and return if there is no data
+	call ic_mget (in, out, offsets, v1, v2, m, lflag, nimages)
+	if (dflag == D_NONE)
+	    return
+
+	# Get data and fill data buffers.  Correct for offsets if needed.
+	ndim = IM_NDIM(out[1])
+	do i = 1, nimages {
+	    if (lflag[i] == D_NONE)
+		next
+	    if (aligned) {
+		call amovl (v1, v2, IM_MAXDIM)
+		if (project)
+		    v2[ndim+1] = i
+		j = imgnls (in[i], d[i], v2)
+	    } else {
+		v2[1] = v1[1]
+		do j = 2, ndim
+		    v2[j] = v1[j] - offsets[i,j]
+		if (project)
+		    v2[ndim+1] = i
+		j = imgnls (in[i], buf, v2)
+		call amovs (Mems[buf], Mems[dbuf[i]+offsets[i,1]],
+		    IM_LEN(in[i],1))
+		d[i] = dbuf[i]
+	    }
+	}
+
+	# Apply threshold if needed
+	if (dothresh) {
+	    do i = 1, nimages {
+		dp = d[i]
+		if (lflag[i] == D_ALL) {
+		    do j = 1, npts {
+			a = Mems[dp]
+			if (a < lthresh || a > hthresh) {
+			    Memi[m[i]+j-1] = 1
+			    lflag[i] = D_MIX
+			    dflag = D_MIX
+			}
+			dp = dp + 1
+		    }
+		} else if (lflag[i] == D_MIX) {
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    a = Mems[dp]
+			    if (a < lthresh || a > hthresh) {
+				Memi[m[i]+j-1] = 1
+				dflag = D_MIX
+			    }
+			}
+			dp = dp + 1
+			mp = mp + 1
+		    }
+		}
+
+		# Check for completely empty lines
+		if (lflag[i] == D_MIX) {
+		    lflag[i] = D_NONE
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    lflag[i] = D_MIX
+			    break
+			}
+			mp = mp + 1
+		    }
+		}
+	    }
+	}
+
+	# Apply scaling (avoiding masked pixels which might overflow?)
+	if (doscale) {
+	    if (dflag == D_ALL) {
+		do i = 1, nimages {
+		    dp = d[i]
+		    a = scales[i]
+		    b = -zeros[i]
+		    do j = 1, npts {
+			Mems[dp] = Mems[dp] / a + b
+			dp = dp + 1
+		    }
+		}
+	    } else if (dflag == D_MIX) {
+		do i = 1, nimages {
+		    dp = d[i]
+		    a = scales[i]
+		    b = -zeros[i]
+		    if (lflag[i] == D_ALL) {
+			do j = 1, npts {
+			    Mems[dp] = Mems[dp] / a + b
+			    dp = dp + 1
+			}
+		    } else if (lflag[i] == D_MIX) {
+			mp = m[i]
+			do j = 1, npts {
+			    if (Memi[mp] == 0)
+				Mems[dp] = Mems[dp] / a + b
+			    dp = dp + 1
+			    mp = mp + 1
+			}
+		    }
+		}
+	    }
+	}
+
+	# Sort pointers to exclude unused images.
+	# Use the lflag array to keep track of the image index.
+
+	if (dflag == D_ALL)
+	    nused = nimages
+	else {
+	    nused = 0
+	    do i = 1, nimages
+		if (lflag[i] != D_NONE) {
+		    nused = nused + 1
+		    d[nused] = d[i]
+		    m[nused] = m[i]
+		    lflag[nused] = i
+		}
+	    if (nused == 0)
+		dflag = D_NONE
+	}
+
+	# Compact data to remove bad pixels
+	# Keep track of the image indices if needed
+	# If growing mark the end of the included image indices with zero
+
+	if (dflag == D_ALL) {
+	    call amovki (nused, n, npts)
+	    if (keepids)
+		do i = 1, nimages
+		    call amovki (i, Memi[id[i]], npts)
+	} else if (dflag == D_NONE)
+	    call aclri (n, npts)
+	else {
+	    call aclri (n, npts)
+	    if (keepids) {
+		do i = 1, nused {
+		    l = lflag[i]
+		    dp = d[i]
+		    ip = id[i]
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    n[j] = n[j] + 1
+			    k = n[j]
+			    if (k < i) {
+				Mems[d[k]+j-1] = Mems[dp]
+				Memi[id[k]+j-1] = l
+			    } else
+				Memi[ip] = l
+			}
+			dp = dp + 1
+			ip = ip + 1
+			mp = mp + 1
+		    }
+		}
+		if (grow > 0) {
+		    do j = 1, npts {
+			do i = n[j]+1, nimages
+			    Memi[id[i]+j-1] = 0
+		    }
+		}
+	    } else {
+		do i = 1, nused {
+		    dp = d[i]
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    n[j] = n[j] + 1
+			    k = n[j]
+			    if (k < i)
+				Mems[d[k]+j-1] = Mems[dp]
+			}
+			dp = dp + 1
+			mp = mp + 1
+		    }
+		}
+	    }
+	}
+
+	# Sort the pixels and IDs if needed
+	if (mclip) {
+	    call malloc (dp, nimages, TY_SHORT)
+	    if (keepids) {
+		call malloc (ip, nimages, TY_INT)
+		call ic_2sorts (d, Mems[dp], id, Memi[ip], n, npts)
+		call mfree (ip, TY_INT)
+	    } else
+		call ic_sorts (d, Mems[dp], n, npts)
+	    call mfree (dp, TY_SHORT)
+	}
+end
+
+# IC_GDATA -- Get line of image and mask data and apply threshold and scaling.
+# Entirely empty lines are excluded.  The data are compacted within the
+# input data buffers.  If it is required, the connection to the original
+# image index is keeped in the returned m data pointers.
+
+procedure ic_gdatar (in, out, dbuf, d, id, n, m, lflag, offsets, scales,
+	zeros, nimages, npts, v1, v2)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+pointer	dbuf[nimages]		# Data buffers for nonaligned images
+pointer	d[nimages]		# Data pointers
+pointer	id[nimages]		# ID pointers
+int	n[npts]			# Number of good pixels
+pointer	m[nimages]		# Mask pointers
+int	lflag[nimages]		# Empty mask flags
+int	offsets[nimages,ARB]	# Image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero offset factors
+int	nimages			# Number of input images
+int	npts			# NUmber of output points per line
+long	v1[ARB], v2[ARB]	# Line vectors
+
+int	i, j, k, l, ndim, nused
+real	a, b
+pointer	buf, dp, ip, mp, imgnlr()
+
+include	"../icombine.com"
+
+begin
+	# Get masks and return if there is no data
+	call ic_mget (in, out, offsets, v1, v2, m, lflag, nimages)
+	if (dflag == D_NONE)
+	    return
+
+	# Get data and fill data buffers.  Correct for offsets if needed.
+	ndim = IM_NDIM(out[1])
+	do i = 1, nimages {
+	    if (lflag[i] == D_NONE)
+		next
+	    if (aligned) {
+		call amovl (v1, v2, IM_MAXDIM)
+		if (project)
+		    v2[ndim+1] = i
+		j = imgnlr (in[i], d[i], v2)
+	    } else {
+		v2[1] = v1[1]
+		do j = 2, ndim
+		    v2[j] = v1[j] - offsets[i,j]
+		if (project)
+		    v2[ndim+1] = i
+		j = imgnlr (in[i], buf, v2)
+		call amovr (Memr[buf], Memr[dbuf[i]+offsets[i,1]],
+		    IM_LEN(in[i],1))
+		d[i] = dbuf[i]
+	    }
+	}
+
+	# Apply threshold if needed
+	if (dothresh) {
+	    do i = 1, nimages {
+		dp = d[i]
+		if (lflag[i] == D_ALL) {
+		    do j = 1, npts {
+			a = Memr[dp]
+			if (a < lthresh || a > hthresh) {
+			    Memi[m[i]+j-1] = 1
+			    lflag[i] = D_MIX
+			    dflag = D_MIX
+			}
+			dp = dp + 1
+		    }
+		} else if (lflag[i] == D_MIX) {
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    a = Memr[dp]
+			    if (a < lthresh || a > hthresh) {
+				Memi[m[i]+j-1] = 1
+				dflag = D_MIX
+			    }
+			}
+			dp = dp + 1
+			mp = mp + 1
+		    }
+		}
+
+		# Check for completely empty lines
+		if (lflag[i] == D_MIX) {
+		    lflag[i] = D_NONE
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    lflag[i] = D_MIX
+			    break
+			}
+			mp = mp + 1
+		    }
+		}
+	    }
+	}
+
+	# Apply scaling (avoiding masked pixels which might overflow?)
+	if (doscale) {
+	    if (dflag == D_ALL) {
+		do i = 1, nimages {
+		    dp = d[i]
+		    a = scales[i]
+		    b = -zeros[i]
+		    do j = 1, npts {
+			Memr[dp] = Memr[dp] / a + b
+			dp = dp + 1
+		    }
+		}
+	    } else if (dflag == D_MIX) {
+		do i = 1, nimages {
+		    dp = d[i]
+		    a = scales[i]
+		    b = -zeros[i]
+		    if (lflag[i] == D_ALL) {
+			do j = 1, npts {
+			    Memr[dp] = Memr[dp] / a + b
+			    dp = dp + 1
+			}
+		    } else if (lflag[i] == D_MIX) {
+			mp = m[i]
+			do j = 1, npts {
+			    if (Memi[mp] == 0)
+				Memr[dp] = Memr[dp] / a + b
+			    dp = dp + 1
+			    mp = mp + 1
+			}
+		    }
+		}
+	    }
+	}
+
+	# Sort pointers to exclude unused images.
+	# Use the lflag array to keep track of the image index.
+
+	if (dflag == D_ALL)
+	    nused = nimages
+	else {
+	    nused = 0
+	    do i = 1, nimages
+		if (lflag[i] != D_NONE) {
+		    nused = nused + 1
+		    d[nused] = d[i]
+		    m[nused] = m[i]
+		    lflag[nused] = i
+		}
+	    if (nused == 0)
+		dflag = D_NONE
+	}
+
+	# Compact data to remove bad pixels
+	# Keep track of the image indices if needed
+	# If growing mark the end of the included image indices with zero
+
+	if (dflag == D_ALL) {
+	    call amovki (nused, n, npts)
+	    if (keepids)
+		do i = 1, nimages
+		    call amovki (i, Memi[id[i]], npts)
+	} else if (dflag == D_NONE)
+	    call aclri (n, npts)
+	else {
+	    call aclri (n, npts)
+	    if (keepids) {
+		do i = 1, nused {
+		    l = lflag[i]
+		    dp = d[i]
+		    ip = id[i]
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    n[j] = n[j] + 1
+			    k = n[j]
+			    if (k < i) {
+				Memr[d[k]+j-1] = Memr[dp]
+				Memi[id[k]+j-1] = l
+			    } else
+				Memi[ip] = l
+			}
+			dp = dp + 1
+			ip = ip + 1
+			mp = mp + 1
+		    }
+		}
+		if (grow > 0) {
+		    do j = 1, npts {
+			do i = n[j]+1, nimages
+			    Memi[id[i]+j-1] = 0
+		    }
+		}
+	    } else {
+		do i = 1, nused {
+		    dp = d[i]
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    n[j] = n[j] + 1
+			    k = n[j]
+			    if (k < i)
+				Memr[d[k]+j-1] = Memr[dp]
+			}
+			dp = dp + 1
+			mp = mp + 1
+		    }
+		}
+	    }
+	}
+
+	# Sort the pixels and IDs if needed
+	if (mclip) {
+	    call malloc (dp, nimages, TY_REAL)
+	    if (keepids) {
+		call malloc (ip, nimages, TY_INT)
+		call ic_2sortr (d, Memr[dp], id, Memi[ip], n, npts)
+		call mfree (ip, TY_INT)
+	    } else
+		call ic_sortr (d, Memr[dp], n, npts)
+	    call mfree (dp, TY_REAL)
+	}
+end
+
diff --git a/noao/imred/ccdred/src/combine/generic/icgrow.x b/noao/imred/ccdred/src/combine/generic/icgrow.x
new file mode 100644
index 00000000..b94e1cbc
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/icgrow.x
@@ -0,0 +1,148 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+
+# IC_GROW --  Reject neigbors of rejected pixels.
+# The rejected pixels are marked by having nonzero ids beyond the number
+# of included pixels.  The pixels rejected here are given zero ids
+# to avoid growing of the pixels rejected here.  The unweighted average
+# can be updated but any rejected pixels requires the median to be
+# recomputed.  When the number of pixels at a grow point reaches nkeep 
+# no further pixels are rejected.  Note that the rejection order is not
+# based on the magnitude of the residuals and so a grow from a weakly
+# rejected image pixel may take precedence over a grow from a strongly
+# rejected image pixel.
+
+procedure ic_grows (d, m, n, nimages, npts, average)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image id pointers
+int	n[npts]			# Number of good pixels
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i1, i2, j1, j2, k1, k2, l, is, ie, n2, maxkeep
+pointer	mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_NONE)
+	    return
+
+	do i1 = 1, npts {
+	    k1 = i1 - 1
+	    is = max (1, i1 - grow)
+	    ie = min (npts, i1 + grow)
+	    do j1 = n[i1]+1, nimages {
+		l = Memi[m[j1]+k1]
+		if (l == 0)
+		    next
+		if (combine == MEDIAN)
+		    docombine = true
+
+		do i2 = is, ie {
+		    if (i2 == i1)
+			next
+		    k2 = i2 - 1
+		    n2 = n[i2]
+		    if (nkeep < 0)
+			maxkeep = max (0, n2 + nkeep)
+		    else
+			maxkeep = min (n2, nkeep)
+		    if (n2 <= maxkeep)
+			next
+		    do j2 = 1, n2 {
+			mp1 = m[j2] + k2
+			if (Memi[mp1] == l) {
+			    if (!docombine && n2 > 1)
+				average[i2] =
+				    (n2*average[i2] - Mems[d[j2]+k2]) / (n2-1)
+			    mp2 = m[n2] + k2
+			    if (j2 < n2) {
+				Mems[d[j2]+k2] = Mems[d[n2]+k2]
+				Memi[mp1] = Memi[mp2]
+			    }
+			    Memi[mp2] = 0
+			    n[i2] = n2 - 1
+			    break
+			}
+		    }
+		}
+	    }
+	}
+end
+
+# IC_GROW --  Reject neigbors of rejected pixels.
+# The rejected pixels are marked by having nonzero ids beyond the number
+# of included pixels.  The pixels rejected here are given zero ids
+# to avoid growing of the pixels rejected here.  The unweighted average
+# can be updated but any rejected pixels requires the median to be
+# recomputed.  When the number of pixels at a grow point reaches nkeep 
+# no further pixels are rejected.  Note that the rejection order is not
+# based on the magnitude of the residuals and so a grow from a weakly
+# rejected image pixel may take precedence over a grow from a strongly
+# rejected image pixel.
+
+procedure ic_growr (d, m, n, nimages, npts, average)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image id pointers
+int	n[npts]			# Number of good pixels
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i1, i2, j1, j2, k1, k2, l, is, ie, n2, maxkeep
+pointer	mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_NONE)
+	    return
+
+	do i1 = 1, npts {
+	    k1 = i1 - 1
+	    is = max (1, i1 - grow)
+	    ie = min (npts, i1 + grow)
+	    do j1 = n[i1]+1, nimages {
+		l = Memi[m[j1]+k1]
+		if (l == 0)
+		    next
+		if (combine == MEDIAN)
+		    docombine = true
+
+		do i2 = is, ie {
+		    if (i2 == i1)
+			next
+		    k2 = i2 - 1
+		    n2 = n[i2]
+		    if (nkeep < 0)
+			maxkeep = max (0, n2 + nkeep)
+		    else
+			maxkeep = min (n2, nkeep)
+		    if (n2 <= maxkeep)
+			next
+		    do j2 = 1, n2 {
+			mp1 = m[j2] + k2
+			if (Memi[mp1] == l) {
+			    if (!docombine && n2 > 1)
+				average[i2] =
+				    (n2*average[i2] - Memr[d[j2]+k2]) / (n2-1)
+			    mp2 = m[n2] + k2
+			    if (j2 < n2) {
+				Memr[d[j2]+k2] = Memr[d[n2]+k2]
+				Memi[mp1] = Memi[mp2]
+			    }
+			    Memi[mp2] = 0
+			    n[i2] = n2 - 1
+			    break
+			}
+		    }
+		}
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/src/combine/generic/icmedian.x b/noao/imred/ccdred/src/combine/generic/icmedian.x
new file mode 100644
index 00000000..ec0166ba
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/icmedian.x
@@ -0,0 +1,343 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+
+# IC_MEDIAN -- Median of lines
+
+procedure ic_medians (d, n, npts, median)
+
+pointer	d[ARB]			# Input data line pointers
+int	n[npts]			# Number of good pixels
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, j1, j2, n1, lo, up, lo1, up1
+bool	even
+real	val1, val2, val3
+short	temp, wtemp
+
+include	"../icombine.com"
+
+begin
+	# If no data return after possibly setting blank values.
+	if (dflag == D_NONE) {
+	    do i = 1, npts
+		median[i]= blank
+	    return
+	}
+
+	# If the data were previously sorted then directly compute the median.
+	if (mclip) {
+	    if (dflag == D_ALL) {
+		n1 = n[1]
+		even = (mod (n1, 2) == 0)
+		j1 = n1 / 2 + 1
+		j2 = n1 / 2
+		do i = 1, npts {
+		    k = i - 1
+		    if (even) {
+			val1 = Mems[d[j1]+k]
+			val2 = Mems[d[j2]+k]
+			median[i] = (val1 + val2) / 2.
+		    } else
+			median[i] = Mems[d[j1]+k]
+		}
+	    } else {
+		do i = 1, npts {
+		    k = i - 1
+		    n1 = n[i]
+		    if (n1 > 0) {
+			j1 = n1 / 2 + 1
+			if (mod (n1, 2) == 0) {
+			    j2 = n1 / 2
+			    val1 = Mems[d[j1]+k]
+			    val2 = Mems[d[j2]+k]
+			    median[i] = (val1 + val2) / 2.
+			} else
+			    median[i] = Mems[d[j1]+k]
+		    } else
+			median[i] = blank
+		}
+	    }
+	    return
+	}
+
+	# Compute the median.
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+
+	    # If there are more than 3 points use Wirth algorithm.  This
+	    # is the same as vops$amed.gx except for an even number of
+	    # points it selects the middle two and averages.
+	    if (n1 > 3) {
+		lo = 1
+		up = n1
+		j  = max (lo, min (up, (up+1)/2))
+
+		while (lo < up) {
+		    if (! (lo < up))
+			break
+
+		    temp = Mems[d[j]+k];  lo1 = lo;  up1 = up
+
+		    repeat {
+			while (Mems[d[lo1]+k] < temp)
+			    lo1 = lo1 + 1
+			while (temp < Mems[d[up1]+k])
+			    up1 = up1 - 1
+			if (lo1 <= up1) {
+			    wtemp = Mems[d[lo1]+k]
+			    Mems[d[lo1]+k] = Mems[d[up1]+k]
+			    Mems[d[up1]+k] = wtemp
+			    lo1 = lo1 + 1;  up1 = up1 - 1
+			}
+		    } until (lo1 > up1)
+
+		    if (up1 < j)
+			lo = lo1
+		    if (j < lo1)
+			up = up1
+		}
+
+		median[i] = Mems[d[j]+k]
+
+		if (mod (n1,2) == 0) {
+		    lo = 1
+		    up = n1
+		    j  = max (lo, min (up, (up+1)/2)+1)
+
+		    while (lo < up) {
+			if (! (lo < up))
+			    break
+
+			temp = Mems[d[j]+k];  lo1 = lo;  up1 = up
+
+			repeat {
+			    while (Mems[d[lo1]+k] < temp)
+				lo1 = lo1 + 1
+			    while (temp < Mems[d[up1]+k])
+				up1 = up1 - 1
+			    if (lo1 <= up1) {
+				wtemp = Mems[d[lo1]+k]
+				Mems[d[lo1]+k] = Mems[d[up1]+k]
+				Mems[d[up1]+k] = wtemp
+				lo1 = lo1 + 1;  up1 = up1 - 1
+			    }
+			} until (lo1 > up1)
+
+			if (up1 < j)
+			    lo = lo1
+			if (j < lo1)
+			    up = up1
+		    }
+		    median[i] = (median[i] + Mems[d[j]+k]) / 2
+		}
+
+	    # If 3 points find the median directly.
+	    } else if (n1 == 3) {
+	        val1 = Mems[d[1]+k]
+	        val2 = Mems[d[2]+k]
+	        val3 = Mems[d[3]+k]
+	        if (val1 < val2) {
+		    if (val2 < val3)		# abc
+		        median[i] = val2
+		    else if (val1 < val3)	# acb
+		        median[i] = val3
+		    else			# cab
+		        median[i] = val1
+	        } else {
+		    if (val2 > val3)		# cba
+		        median[i] = val2
+		    else if (val1 > val3)	# bca
+		        median[i] = val3
+		    else			# bac
+		        median[i] = val1
+	        }
+
+	    # If 2 points average.
+	    } else if (n1 == 2) {
+		val1 = Mems[d[1]+k]
+		val2 = Mems[d[2]+k]
+		median[i] = (val1 + val2) / 2
+
+	    # If 1 point return the value.
+	    } else if (n1 == 1)
+		median[i] = Mems[d[1]+k]
+
+	    # If no points return with a possibly blank value.
+	    else
+		median[i] = blank
+	}
+end
+
+# IC_MEDIAN -- Median of lines
+
+procedure ic_medianr (d, n, npts, median)
+
+pointer	d[ARB]			# Input data line pointers
+int	n[npts]			# Number of good pixels
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, j1, j2, n1, lo, up, lo1, up1
+bool	even
+real	val1, val2, val3
+real	temp, wtemp
+
+include	"../icombine.com"
+
+begin
+	# If no data return after possibly setting blank values.
+	if (dflag == D_NONE) {
+	    do i = 1, npts
+		median[i]= blank
+	    return
+	}
+
+	# If the data were previously sorted then directly compute the median.
+	if (mclip) {
+	    if (dflag == D_ALL) {
+		n1 = n[1]
+		even = (mod (n1, 2) == 0)
+		j1 = n1 / 2 + 1
+		j2 = n1 / 2
+		do i = 1, npts {
+		    k = i - 1
+		    if (even) {
+			val1 = Memr[d[j1]+k]
+			val2 = Memr[d[j2]+k]
+			median[i] = (val1 + val2) / 2.
+		    } else
+			median[i] = Memr[d[j1]+k]
+		}
+	    } else {
+		do i = 1, npts {
+		    k = i - 1
+		    n1 = n[i]
+		    if (n1 > 0) {
+			j1 = n1 / 2 + 1
+			if (mod (n1, 2) == 0) {
+			    j2 = n1 / 2
+			    val1 = Memr[d[j1]+k]
+			    val2 = Memr[d[j2]+k]
+			    median[i] = (val1 + val2) / 2.
+			} else
+			    median[i] = Memr[d[j1]+k]
+		    } else
+			median[i] = blank
+		}
+	    }
+	    return
+	}
+
+	# Compute the median.
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+
+	    # If there are more than 3 points use Wirth algorithm.  This
+	    # is the same as vops$amed.gx except for an even number of
+	    # points it selects the middle two and averages.
+	    if (n1 > 3) {
+		lo = 1
+		up = n1
+		j  = max (lo, min (up, (up+1)/2))
+
+		while (lo < up) {
+		    if (! (lo < up))
+			break
+
+		    temp = Memr[d[j]+k];  lo1 = lo;  up1 = up
+
+		    repeat {
+			while (Memr[d[lo1]+k] < temp)
+			    lo1 = lo1 + 1
+			while (temp < Memr[d[up1]+k])
+			    up1 = up1 - 1
+			if (lo1 <= up1) {
+			    wtemp = Memr[d[lo1]+k]
+			    Memr[d[lo1]+k] = Memr[d[up1]+k]
+			    Memr[d[up1]+k] = wtemp
+			    lo1 = lo1 + 1;  up1 = up1 - 1
+			}
+		    } until (lo1 > up1)
+
+		    if (up1 < j)
+			lo = lo1
+		    if (j < lo1)
+			up = up1
+		}
+
+		median[i] = Memr[d[j]+k]
+
+		if (mod (n1,2) == 0) {
+		    lo = 1
+		    up = n1
+		    j  = max (lo, min (up, (up+1)/2)+1)
+
+		    while (lo < up) {
+			if (! (lo < up))
+			    break
+
+			temp = Memr[d[j]+k];  lo1 = lo;  up1 = up
+
+			repeat {
+			    while (Memr[d[lo1]+k] < temp)
+				lo1 = lo1 + 1
+			    while (temp < Memr[d[up1]+k])
+				up1 = up1 - 1
+			    if (lo1 <= up1) {
+				wtemp = Memr[d[lo1]+k]
+				Memr[d[lo1]+k] = Memr[d[up1]+k]
+				Memr[d[up1]+k] = wtemp
+				lo1 = lo1 + 1;  up1 = up1 - 1
+			    }
+			} until (lo1 > up1)
+
+			if (up1 < j)
+			    lo = lo1
+			if (j < lo1)
+			    up = up1
+		    }
+		    median[i] = (median[i] + Memr[d[j]+k]) / 2
+		}
+
+	    # If 3 points find the median directly.
+	    } else if (n1 == 3) {
+	        val1 = Memr[d[1]+k]
+	        val2 = Memr[d[2]+k]
+	        val3 = Memr[d[3]+k]
+	        if (val1 < val2) {
+		    if (val2 < val3)		# abc
+		        median[i] = val2
+		    else if (val1 < val3)	# acb
+		        median[i] = val3
+		    else			# cab
+		        median[i] = val1
+	        } else {
+		    if (val2 > val3)		# cba
+		        median[i] = val2
+		    else if (val1 > val3)	# bca
+		        median[i] = val3
+		    else			# bac
+		        median[i] = val1
+	        }
+
+	    # If 2 points average.
+	    } else if (n1 == 2) {
+		val1 = Memr[d[1]+k]
+		val2 = Memr[d[2]+k]
+		median[i] = (val1 + val2) / 2
+
+	    # If 1 point return the value.
+	    } else if (n1 == 1)
+		median[i] = Memr[d[1]+k]
+
+	    # If no points return with a possibly blank value.
+	    else
+		median[i] = blank
+	}
+end
+
diff --git a/noao/imred/ccdred/src/combine/generic/icmm.x b/noao/imred/ccdred/src/combine/generic/icmm.x
new file mode 100644
index 00000000..259759bd
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/icmm.x
@@ -0,0 +1,300 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+
+# IC_MM --  Reject a specified number of high and low pixels
+
+procedure ic_mms (d, m, n, npts)
+
+pointer	d[ARB]		# Data pointers
+pointer	m[ARB]		# Image ID pointers
+int	n[npts]			# Number of good pixels
+int	npts			# Number of output points per line
+
+int	n1, ncombine, npairs, nlow, nhigh, np
+int	i, i1, j, jmax, jmin
+pointer	k, kmax, kmin
+short	d1, d2, dmin, dmax
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_NONE)
+	    return
+
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    nlow = flow * n1 + 0.001
+	    nhigh = fhigh * n1 + 0.001
+	    ncombine = n1 - nlow -  nhigh
+	    npairs = min (nlow, nhigh)
+	    nlow = nlow - npairs
+	    nhigh = nhigh - npairs
+	}
+
+	do i = 1, npts {
+	    i1 = i - 1
+	    n1 = n[i]
+	    if (dflag == D_MIX) {
+		nlow = flow * n1 + 0.001
+		nhigh = fhigh * n1 + 0.001
+		ncombine = max (ncombine, n1 - nlow - nhigh)
+		npairs = min (nlow, nhigh)
+		nlow = nlow - npairs
+		nhigh = nhigh - npairs
+	    }
+
+	    # Reject the npairs low and high points.
+	    do np = 1, npairs {
+		k = d[1] + i1
+		d1 = Mems[k]
+		dmax = d1; dmin = d1; jmax = 1; jmin = 1; kmax = k; kmin = k
+		do j = 2, n1 {
+		    d2 = d1
+		    k = d[j] + i1
+		    d1 = Mems[k]
+		    if (d1 > dmax) {
+			dmax = d1; jmax = j; kmax = k
+		    } else if (d1 < dmin) {
+			dmin = d1; jmin = j; kmin = k
+		    }
+		}
+		j = n1 - 1
+		if (keepids) {
+		    if (jmax < j) {
+			if (jmin != j) {
+			    Mems[kmax] = d2
+			    Memi[m[jmax]+i1] = Memi[m[j]+i1]
+			} else {
+			    Mems[kmax] = d1
+			    Memi[m[jmax]+i1] = Memi[m[n1]+i1]
+			}
+		    }
+		    if (jmin < j) {
+			if (jmax != n1) {
+			    Mems[kmin] = d1
+			    Memi[m[jmin]+i1] = Memi[m[n1]+i1]
+			} else {
+			    Mems[kmin] = d2
+			    Memi[m[jmin]+i1] = Memi[m[j]+i1]
+			}
+		    }
+		} else {
+		    if (jmax < j) {
+			if (jmin != j)
+			    Mems[kmax] = d2
+			else
+			    Mems[kmax] = d1
+		    }
+		    if (jmin < j) {
+			if (jmax != n1)
+			    Mems[kmin] = d1
+			else
+			    Mems[kmin] = d2
+		    }
+		}
+		n1 = n1 - 2
+	    }
+
+	    # Reject the excess low points.
+	    do np = 1, nlow {
+		k = d[1] + i1
+		d1 = Mems[k]
+		dmin = d1; jmin = 1; kmin = k
+		do j = 2, n1 {
+		    k = d[j] + i1
+		    d1 = Mems[k]
+		    if (d1 < dmin) {
+			dmin = d1; jmin = j; kmin = k
+		    }
+		}
+		if (keepids) {
+		    if (jmin < n1) {
+			Mems[kmin] = d1
+			Memi[m[jmin]+i1] = Memi[m[n1]+i1]
+		    }
+		} else {
+		    if (jmin < n1)
+			Mems[kmin] = d1
+		}
+		n1 = n1 - 1 
+	    }
+
+	    # Reject the excess high points.
+	    do np = 1, nhigh {
+		k = d[1] + i1
+		d1 = Mems[k]
+		dmax = d1; jmax = 1; kmax = k
+		do j = 2, n1 {
+		    k = d[j] + i1
+		    d1 = Mems[k]
+		    if (d1 > dmax) {
+			dmax = d1; jmax = j; kmax = k
+		    }
+		}
+		if (keepids) {
+		    if (jmax < n1) {
+			Mems[kmax] = d1
+			Memi[m[jmax]+i1] = Memi[m[n1]+i1]
+		    }
+		} else {
+		    if (jmax < n1)
+			Mems[kmax] = d1
+		}
+		n1 = n1 - 1 
+	    }
+	    n[i] = n1
+	}
+
+	if (dflag == D_ALL && npairs + nlow + nhigh > 0)
+		dflag = D_MIX
+end
+
+# IC_MM --  Reject a specified number of high and low pixels
+
+procedure ic_mmr (d, m, n, npts)
+
+pointer	d[ARB]		# Data pointers
+pointer	m[ARB]		# Image ID pointers
+int	n[npts]			# Number of good pixels
+int	npts			# Number of output points per line
+
+int	n1, ncombine, npairs, nlow, nhigh, np
+int	i, i1, j, jmax, jmin
+pointer	k, kmax, kmin
+real	d1, d2, dmin, dmax
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_NONE)
+	    return
+
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    nlow = flow * n1 + 0.001
+	    nhigh = fhigh * n1 + 0.001
+	    ncombine = n1 - nlow -  nhigh
+	    npairs = min (nlow, nhigh)
+	    nlow = nlow - npairs
+	    nhigh = nhigh - npairs
+	}
+
+	do i = 1, npts {
+	    i1 = i - 1
+	    n1 = n[i]
+	    if (dflag == D_MIX) {
+		nlow = flow * n1 + 0.001
+		nhigh = fhigh * n1 + 0.001
+		ncombine = max (ncombine, n1 - nlow - nhigh)
+		npairs = min (nlow, nhigh)
+		nlow = nlow - npairs
+		nhigh = nhigh - npairs
+	    }
+
+	    # Reject the npairs low and high points.
+	    do np = 1, npairs {
+		k = d[1] + i1
+		d1 = Memr[k]
+		dmax = d1; dmin = d1; jmax = 1; jmin = 1; kmax = k; kmin = k
+		do j = 2, n1 {
+		    d2 = d1
+		    k = d[j] + i1
+		    d1 = Memr[k]
+		    if (d1 > dmax) {
+			dmax = d1; jmax = j; kmax = k
+		    } else if (d1 < dmin) {
+			dmin = d1; jmin = j; kmin = k
+		    }
+		}
+		j = n1 - 1
+		if (keepids) {
+		    if (jmax < j) {
+			if (jmin != j) {
+			    Memr[kmax] = d2
+			    Memi[m[jmax]+i1] = Memi[m[j]+i1]
+			} else {
+			    Memr[kmax] = d1
+			    Memi[m[jmax]+i1] = Memi[m[n1]+i1]
+			}
+		    }
+		    if (jmin < j) {
+			if (jmax != n1) {
+			    Memr[kmin] = d1
+			    Memi[m[jmin]+i1] = Memi[m[n1]+i1]
+			} else {
+			    Memr[kmin] = d2
+			    Memi[m[jmin]+i1] = Memi[m[j]+i1]
+			}
+		    }
+		} else {
+		    if (jmax < j) {
+			if (jmin != j)
+			    Memr[kmax] = d2
+			else
+			    Memr[kmax] = d1
+		    }
+		    if (jmin < j) {
+			if (jmax != n1)
+			    Memr[kmin] = d1
+			else
+			    Memr[kmin] = d2
+		    }
+		}
+		n1 = n1 - 2
+	    }
+
+	    # Reject the excess low points.
+	    do np = 1, nlow {
+		k = d[1] + i1
+		d1 = Memr[k]
+		dmin = d1; jmin = 1; kmin = k
+		do j = 2, n1 {
+		    k = d[j] + i1
+		    d1 = Memr[k]
+		    if (d1 < dmin) {
+			dmin = d1; jmin = j; kmin = k
+		    }
+		}
+		if (keepids) {
+		    if (jmin < n1) {
+			Memr[kmin] = d1
+			Memi[m[jmin]+i1] = Memi[m[n1]+i1]
+		    }
+		} else {
+		    if (jmin < n1)
+			Memr[kmin] = d1
+		}
+		n1 = n1 - 1 
+	    }
+
+	    # Reject the excess high points.
+	    do np = 1, nhigh {
+		k = d[1] + i1
+		d1 = Memr[k]
+		dmax = d1; jmax = 1; kmax = k
+		do j = 2, n1 {
+		    k = d[j] + i1
+		    d1 = Memr[k]
+		    if (d1 > dmax) {
+			dmax = d1; jmax = j; kmax = k
+		    }
+		}
+		if (keepids) {
+		    if (jmax < n1) {
+			Memr[kmax] = d1
+			Memi[m[jmax]+i1] = Memi[m[n1]+i1]
+		    }
+		} else {
+		    if (jmax < n1)
+			Memr[kmax] = d1
+		}
+		n1 = n1 - 1 
+	    }
+	    n[i] = n1
+	}
+
+	if (dflag == D_ALL && npairs + nlow + nhigh > 0)
+		dflag = D_MIX
+end
diff --git a/noao/imred/ccdred/src/combine/generic/icombine.x b/noao/imred/ccdred/src/combine/generic/icombine.x
new file mode 100644
index 00000000..b4ff60be
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/icombine.x
@@ -0,0 +1,607 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	<imset.h>
+include	<error.h>
+include	<syserr.h>
+include	<mach.h>
+include	"../icombine.h"
+
+
+# ICOMBINE -- Combine images
+#
+# The memory and open file descriptor limits are checked and an attempt
+# to recover is made either by setting the image pixel files to be
+# closed after I/O or by notifying the calling program that memory
+# ran out and the IMIO buffer size should be reduced.  After the checks
+# a procedure for the selected combine option is called.
+# Because there may be several failure modes when reaching the file
+# limits we first assume an error is due to the file limit, except for
+# out of memory, and close some pixel files.  If the error then repeats
+# on accessing the pixels the error is passed back.
+
+
+procedure icombines (in, out, offsets, nimages, bufsize)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+int	offsets[nimages,ARB]	# Input image offsets
+int	nimages			# Number of input images
+int	bufsize			# IMIO buffer size
+
+char	str[1]
+int	i, j, npts, fd, stropen(), errcode(), imstati()
+pointer	sp, d, id, n, m, lflag, scales, zeros, wts, dbuf
+pointer	buf, imgl1s(), impl1i()
+errchk	stropen, imgl1s, impl1i
+pointer	impl1r()
+errchk	impl1r
+
+include	"../icombine.com"
+
+begin
+	npts = IM_LEN(out[1],1)
+
+	# Allocate memory.
+	call smark (sp)
+	call salloc (d, nimages, TY_POINTER)
+	call salloc (id, nimages, TY_POINTER)
+	call salloc (n, npts, TY_INT)
+	call salloc (m, nimages, TY_POINTER)
+	call salloc (lflag, nimages, TY_INT)
+	call salloc (scales, nimages, TY_REAL)
+	call salloc (zeros, nimages, TY_REAL)
+	call salloc (wts, nimages, TY_REAL)
+	call amovki (D_ALL, Memi[lflag], nimages)
+
+	# If aligned use the IMIO buffer otherwise we need vectors of
+	# output length.
+
+	if (!aligned) {
+	    call salloc (dbuf, nimages, TY_POINTER)
+	    do i = 1, nimages
+		call salloc (Memi[dbuf+i-1], npts, TY_SHORT)
+	}
+
+	if (project) {
+	    call imseti (in[1], IM_NBUFS, nimages)
+	    call imseti (in[1], IM_BUFSIZE, bufsize)
+	    do i = 1, 3 {
+		if (out[i] != NULL)
+		    call imseti (out[i], IM_BUFSIZE, bufsize)
+	    }
+	} else {
+	    # Reserve FD for string operations.
+	    fd = stropen (str, 1, NEW_FILE)
+
+	    # Do I/O to the images.
+	    do i = 1, 3 {
+		if (out[i] != NULL)
+		    call imseti (out[i], IM_BUFSIZE, bufsize)
+	    }
+	    buf = impl1r (out[1])
+	    call aclrr (Memr[buf], npts)
+	    if (out[3] != NULL) {
+		buf = impl1r (out[3])
+		call aclrr (Memr[buf], npts)
+	    }
+	    if (out[2] != NULL) {
+		buf = impl1i (out[2])
+		call aclri (Memi[buf], npts)
+	    }
+
+	    do i = 1, nimages {
+		call imseti (in[i], IM_BUFSIZE, bufsize)
+		iferr (buf = imgl1s (in[i])) {
+		    switch (errcode()) {
+		    case SYS_MFULL:
+			call sfree (sp)
+			call strclose (fd)
+			call erract (EA_ERROR)
+		    case SYS_FTOOMANYFILES, SYS_IKIOPIX:
+			if (imstati (in[i], IM_CLOSEFD) == YES) {
+			    call sfree (sp)
+			    call strclose (fd)
+			    call erract (EA_ERROR)
+			}
+			do j = i-2, nimages
+			    call imseti (in[j], IM_CLOSEFD, YES)
+			buf = imgl1s (in[i])
+		    default:
+			call sfree (sp)
+			call strclose (fd)
+			call erract (EA_ERROR)
+		    }
+		}
+	    }
+
+	    call strclose (fd)
+	}
+
+	call ic_combines (in, out, Memi[dbuf], Memi[d], Memi[id], Memi[n],
+	    Memi[m], Memi[lflag], offsets, Memr[scales], Memr[zeros],
+	    Memr[wts], nimages, npts)
+end
+
+
+# IC_COMBINE -- Combine images.
+
+procedure ic_combines (in, out, dbuf, d, id, n, m, lflag, offsets,
+	scales, zeros, wts, nimages, npts)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output image
+pointer	dbuf[nimages]		# Data buffers for nonaligned images
+pointer	d[nimages]		# Data pointers
+pointer	id[nimages]		# Image index ID pointers
+int	n[npts]			# Number of good pixels
+pointer	m[nimages]		# Mask pointers
+int	lflag[nimages]		# Line flags
+int	offsets[nimages,ARB]	# Input image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero offset factors
+real	wts[nimages]		# Combining weights
+int	nimages			# Number of input images
+int	npts			# Number of points per output line
+
+int	i, ctor()
+real	r, imgetr()
+pointer	sp, v1, v2, v3, outdata, buf, nm, impnli()
+pointer	impnlr()
+errchk	ic_scale, imgetr
+
+include	"../icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (v1, IM_MAXDIM, TY_LONG)
+	call salloc (v2, IM_MAXDIM, TY_LONG)
+	call salloc (v3, IM_MAXDIM, TY_LONG)
+	call amovkl (long(1), Meml[v1], IM_MAXDIM)
+	call amovkl (long(1), Meml[v2], IM_MAXDIM)
+	call amovkl (long(1), Meml[v3], IM_MAXDIM)
+
+	call ic_scale (in, out, offsets, scales, zeros, wts, nimages)
+
+	# Set combine parameters
+	switch (combine) {
+	case AVERAGE:
+	    if (dowts)
+		keepids = true
+	    else
+		keepids = false
+	case MEDIAN:
+	    dowts = false
+	    keepids = false
+	}
+	docombine = true
+
+	# Set rejection algorithm specific parameters
+	switch (reject) {
+	case CCDCLIP, CRREJECT:
+	    call salloc (nm, 3*nimages, TY_REAL)
+	    i = 1
+	    if (ctor (Memc[rdnoise], i, r) > 0) {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)] = r
+	    } else {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)] = imgetr (in[i], Memc[rdnoise])
+	    }
+	    i = 1
+	    if (ctor (Memc[gain], i, r) > 0) {
+		do i = 1, nimages {
+		    Memr[nm+3*(i-1)+1] = r
+		    Memr[nm+3*(i-1)] =
+			max ((Memr[nm+3*(i-1)] / r) ** 2, 1e4 / MAX_REAL)
+		}
+	    } else {
+		do i = 1, nimages {
+		    r = imgetr (in[i], Memc[gain])
+		    Memr[nm+3*(i-1)+1] = r
+		    Memr[nm+3*(i-1)] =
+			max ((Memr[nm+3*(i-1)] / r) ** 2, 1e4 / MAX_REAL)
+		}
+	    }
+	    i = 1
+	    if (ctor (Memc[snoise], i, r) > 0) {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)+2] = r
+	    } else {
+		do i = 1, nimages {
+		    r = imgetr (in[i], Memc[snoise])
+		    Memr[nm+3*(i-1)+2] = r
+		}
+	    }
+	    if (!keepids) {
+		if (doscale1 || grow > 0)
+		    keepids = true
+		else {
+		    do i = 2, nimages {
+			if (Memr[nm+3*(i-1)] != Memr[nm] ||
+			    Memr[nm+3*(i-1)+1] != Memr[nm+1] ||
+			    Memr[nm+3*(i-1)+2] != Memr[nm+2]) {
+			    keepids = true
+			    break
+			}
+		    }
+		}
+	    }
+	    if (reject == CRREJECT)
+		lsigma = MAX_REAL
+	case MINMAX:
+	    mclip = false
+	    if (grow > 0)
+		keepids = true
+	case PCLIP:
+	    mclip = true
+	    if (grow > 0)
+		keepids = true
+	case AVSIGCLIP, SIGCLIP:
+	    if (doscale1 || grow > 0)
+		keepids = true
+	case NONE:
+	    mclip = false
+	    grow = 0
+	}
+
+	if (keepids) {
+	    do i = 1, nimages
+		call salloc (id[i], npts, TY_INT)
+	}
+
+	while (impnlr (out[1], outdata, Meml[v1]) != EOF) {
+	    call ic_gdatas (in, out, dbuf, d, id, n, m, lflag, offsets,
+		scales, zeros, nimages, npts, Meml[v2], Meml[v3])
+
+	    switch (reject) {
+	    case CCDCLIP, CRREJECT:
+		if (mclip)
+		    call ic_mccdclips (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Memr[outdata])
+		else
+		    call ic_accdclips (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Memr[outdata])
+	    case MINMAX:
+		call ic_mms (d, id, n, npts)
+	    case PCLIP:
+		call ic_pclips (d, id, n, nimages, npts, Memr[outdata])
+	    case SIGCLIP:
+		if (mclip)
+		    call ic_msigclips (d, id, n, scales, zeros, nimages, npts,
+			Memr[outdata])
+		else
+		    call ic_asigclips (d, id, n, scales, zeros, nimages, npts,
+			Memr[outdata])
+	    case AVSIGCLIP:
+		if (mclip)
+		    call ic_mavsigclips (d, id, n, scales, zeros, nimages,
+			npts, Memr[outdata])
+		else
+		    call ic_aavsigclips (d, id, n, scales, zeros, nimages,
+			npts, Memr[outdata])
+	    }
+
+	    if (grow > 0)
+		call ic_grows (d, id, n, nimages, npts, Memr[outdata])
+
+	    if (docombine) {
+		switch (combine) {
+		case AVERAGE:
+		    call ic_averages (d, id, n, wts, npts, Memr[outdata])
+		case MEDIAN:
+		    call ic_medians (d, n, npts, Memr[outdata])
+		}
+	    }
+
+	    if (out[2] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnli (out[2], buf, Meml[v1])
+		call amovki (nimages, Memi[buf], npts)
+		call asubi (Memi[buf], n, Memi[buf], npts)
+	    }
+		    
+	    if (out[3] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnlr (out[3], buf, Meml[v1])
+		call ic_sigmas (d, id, n, wts, npts, Memr[outdata],
+		    Memr[buf])
+	    }
+	    call amovl (Meml[v1], Meml[v2], IM_MAXDIM)
+	}
+
+	call sfree (sp)
+end
+
+procedure icombiner (in, out, offsets, nimages, bufsize)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+int	offsets[nimages,ARB]	# Input image offsets
+int	nimages			# Number of input images
+int	bufsize			# IMIO buffer size
+
+char	str[1]
+int	i, j, npts, fd, stropen(), errcode(), imstati()
+pointer	sp, d, id, n, m, lflag, scales, zeros, wts, dbuf
+pointer	buf, imgl1r(), impl1i()
+errchk	stropen, imgl1r, impl1i
+pointer	impl1r()
+errchk	impl1r
+
+include	"../icombine.com"
+
+begin
+	npts = IM_LEN(out[1],1)
+
+	# Allocate memory.
+	call smark (sp)
+	call salloc (d, nimages, TY_POINTER)
+	call salloc (id, nimages, TY_POINTER)
+	call salloc (n, npts, TY_INT)
+	call salloc (m, nimages, TY_POINTER)
+	call salloc (lflag, nimages, TY_INT)
+	call salloc (scales, nimages, TY_REAL)
+	call salloc (zeros, nimages, TY_REAL)
+	call salloc (wts, nimages, TY_REAL)
+	call amovki (D_ALL, Memi[lflag], nimages)
+
+	# If aligned use the IMIO buffer otherwise we need vectors of
+	# output length.
+
+	if (!aligned) {
+	    call salloc (dbuf, nimages, TY_POINTER)
+	    do i = 1, nimages
+		call salloc (Memi[dbuf+i-1], npts, TY_REAL)
+	}
+
+	if (project) {
+	    call imseti (in[1], IM_NBUFS, nimages)
+	    call imseti (in[1], IM_BUFSIZE, bufsize)
+	    do i = 1, 3 {
+		if (out[i] != NULL)
+		    call imseti (out[i], IM_BUFSIZE, bufsize)
+	    }
+	} else {
+	    # Reserve FD for string operations.
+	    fd = stropen (str, 1, NEW_FILE)
+
+	    # Do I/O to the images.
+	    do i = 1, 3 {
+		if (out[i] != NULL)
+		    call imseti (out[i], IM_BUFSIZE, bufsize)
+	    }
+	    buf = impl1r (out[1])
+	    call aclrr (Memr[buf], npts)
+	    if (out[3] != NULL) {
+		buf = impl1r (out[3])
+		call aclrr (Memr[buf], npts)
+	    }
+	    if (out[2] != NULL) {
+		buf = impl1i (out[2])
+		call aclri (Memi[buf], npts)
+	    }
+
+	    do i = 1, nimages {
+		call imseti (in[i], IM_BUFSIZE, bufsize)
+		iferr (buf = imgl1r (in[i])) {
+		    switch (errcode()) {
+		    case SYS_MFULL:
+			call sfree (sp)
+			call strclose (fd)
+			call erract (EA_ERROR)
+		    case SYS_FTOOMANYFILES, SYS_IKIOPIX:
+			if (imstati (in[i], IM_CLOSEFD) == YES) {
+			    call sfree (sp)
+			    call strclose (fd)
+			    call erract (EA_ERROR)
+			}
+			do j = i-2, nimages
+			    call imseti (in[j], IM_CLOSEFD, YES)
+			buf = imgl1r (in[i])
+		    default:
+			call sfree (sp)
+			call strclose (fd)
+			call erract (EA_ERROR)
+		    }
+		}
+	    }
+
+	    call strclose (fd)
+	}
+
+	call ic_combiner (in, out, Memi[dbuf], Memi[d], Memi[id], Memi[n],
+	    Memi[m], Memi[lflag], offsets, Memr[scales], Memr[zeros],
+	    Memr[wts], nimages, npts)
+end
+
+
+# IC_COMBINE -- Combine images.
+
+procedure ic_combiner (in, out, dbuf, d, id, n, m, lflag, offsets,
+	scales, zeros, wts, nimages, npts)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output image
+pointer	dbuf[nimages]		# Data buffers for nonaligned images
+pointer	d[nimages]		# Data pointers
+pointer	id[nimages]		# Image index ID pointers
+int	n[npts]			# Number of good pixels
+pointer	m[nimages]		# Mask pointers
+int	lflag[nimages]		# Line flags
+int	offsets[nimages,ARB]	# Input image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero offset factors
+real	wts[nimages]		# Combining weights
+int	nimages			# Number of input images
+int	npts			# Number of points per output line
+
+int	i, ctor()
+real	r, imgetr()
+pointer	sp, v1, v2, v3, outdata, buf, nm, impnli()
+pointer	impnlr()
+errchk	ic_scale, imgetr
+
+include	"../icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (v1, IM_MAXDIM, TY_LONG)
+	call salloc (v2, IM_MAXDIM, TY_LONG)
+	call salloc (v3, IM_MAXDIM, TY_LONG)
+	call amovkl (long(1), Meml[v1], IM_MAXDIM)
+	call amovkl (long(1), Meml[v2], IM_MAXDIM)
+	call amovkl (long(1), Meml[v3], IM_MAXDIM)
+
+	call ic_scale (in, out, offsets, scales, zeros, wts, nimages)
+
+	# Set combine parameters
+	switch (combine) {
+	case AVERAGE:
+	    if (dowts)
+		keepids = true
+	    else
+		keepids = false
+	case MEDIAN:
+	    dowts = false
+	    keepids = false
+	}
+	docombine = true
+
+	# Set rejection algorithm specific parameters
+	switch (reject) {
+	case CCDCLIP, CRREJECT:
+	    call salloc (nm, 3*nimages, TY_REAL)
+	    i = 1
+	    if (ctor (Memc[rdnoise], i, r) > 0) {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)] = r
+	    } else {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)] = imgetr (in[i], Memc[rdnoise])
+	    }
+	    i = 1
+	    if (ctor (Memc[gain], i, r) > 0) {
+		do i = 1, nimages {
+		    Memr[nm+3*(i-1)+1] = r
+		    Memr[nm+3*(i-1)] =
+			max ((Memr[nm+3*(i-1)] / r) ** 2, 1e4 / MAX_REAL)
+		}
+	    } else {
+		do i = 1, nimages {
+		    r = imgetr (in[i], Memc[gain])
+		    Memr[nm+3*(i-1)+1] = r
+		    Memr[nm+3*(i-1)] =
+			max ((Memr[nm+3*(i-1)] / r) ** 2, 1e4 / MAX_REAL)
+		}
+	    }
+	    i = 1
+	    if (ctor (Memc[snoise], i, r) > 0) {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)+2] = r
+	    } else {
+		do i = 1, nimages {
+		    r = imgetr (in[i], Memc[snoise])
+		    Memr[nm+3*(i-1)+2] = r
+		}
+	    }
+	    if (!keepids) {
+		if (doscale1 || grow > 0)
+		    keepids = true
+		else {
+		    do i = 2, nimages {
+			if (Memr[nm+3*(i-1)] != Memr[nm] ||
+			    Memr[nm+3*(i-1)+1] != Memr[nm+1] ||
+			    Memr[nm+3*(i-1)+2] != Memr[nm+2]) {
+			    keepids = true
+			    break
+			}
+		    }
+		}
+	    }
+	    if (reject == CRREJECT)
+		lsigma = MAX_REAL
+	case MINMAX:
+	    mclip = false
+	    if (grow > 0)
+		keepids = true
+	case PCLIP:
+	    mclip = true
+	    if (grow > 0)
+		keepids = true
+	case AVSIGCLIP, SIGCLIP:
+	    if (doscale1 || grow > 0)
+		keepids = true
+	case NONE:
+	    mclip = false
+	    grow = 0
+	}
+
+	if (keepids) {
+	    do i = 1, nimages
+		call salloc (id[i], npts, TY_INT)
+	}
+
+	while (impnlr (out[1], outdata, Meml[v1]) != EOF) {
+	    call ic_gdatar (in, out, dbuf, d, id, n, m, lflag, offsets,
+		scales, zeros, nimages, npts, Meml[v2], Meml[v3])
+
+	    switch (reject) {
+	    case CCDCLIP, CRREJECT:
+		if (mclip)
+		    call ic_mccdclipr (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Memr[outdata])
+		else
+		    call ic_accdclipr (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Memr[outdata])
+	    case MINMAX:
+		call ic_mmr (d, id, n, npts)
+	    case PCLIP:
+		call ic_pclipr (d, id, n, nimages, npts, Memr[outdata])
+	    case SIGCLIP:
+		if (mclip)
+		    call ic_msigclipr (d, id, n, scales, zeros, nimages, npts,
+			Memr[outdata])
+		else
+		    call ic_asigclipr (d, id, n, scales, zeros, nimages, npts,
+			Memr[outdata])
+	    case AVSIGCLIP:
+		if (mclip)
+		    call ic_mavsigclipr (d, id, n, scales, zeros, nimages,
+			npts, Memr[outdata])
+		else
+		    call ic_aavsigclipr (d, id, n, scales, zeros, nimages,
+			npts, Memr[outdata])
+	    }
+
+	    if (grow > 0)
+		call ic_growr (d, id, n, nimages, npts, Memr[outdata])
+
+	    if (docombine) {
+		switch (combine) {
+		case AVERAGE:
+		    call ic_averager (d, id, n, wts, npts, Memr[outdata])
+		case MEDIAN:
+		    call ic_medianr (d, n, npts, Memr[outdata])
+		}
+	    }
+
+	    if (out[2] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnli (out[2], buf, Meml[v1])
+		call amovki (nimages, Memi[buf], npts)
+		call asubi (Memi[buf], n, Memi[buf], npts)
+	    }
+		    
+	    if (out[3] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnlr (out[3], buf, Meml[v1])
+		call ic_sigmar (d, id, n, wts, npts, Memr[outdata],
+		    Memr[buf])
+	    }
+	    call amovl (Meml[v1], Meml[v2], IM_MAXDIM)
+	}
+
+	call sfree (sp)
+end
+
diff --git a/noao/imred/ccdred/src/combine/generic/icpclip.x b/noao/imred/ccdred/src/combine/generic/icpclip.x
new file mode 100644
index 00000000..da09bb75
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/icpclip.x
@@ -0,0 +1,442 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		3	# Minimum number for clipping
+
+
+# IC_PCLIP -- Percentile clip
+#
+# 1) Find the median
+# 2) Find the pixel which is the specified order index away
+# 3) Use the data value difference as a sigma and apply clipping
+# 4) Since the median is known return it so it does not have to be recomputed
+
+procedure ic_pclips (d, m, n, nimages, npts, median)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image id pointers
+int	n[npts]			# Number of good pixels
+int	nimages			# Number of input images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, n4, n5, nl, nh, nin, maxkeep
+bool	even, fp_equalr()
+real	sigma, r, s, t
+pointer	sp, resid, mp1, mp2
+real	med
+
+include	"../icombine.com"
+
+begin
+	# There must be at least MINCLIP and more than nkeep pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Set sign of pclip parameter
+	if (pclip < 0)
+	    t = -1.
+	else
+	    t = 1.
+
+	# If there are no rejected pixels compute certain parameters once.
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    n2 = 1 + n1 / 2
+	    even = (mod (n1, 2) == 0)
+	    if (pclip < 0.) {
+		if (even)
+		    n3 = max (1, nint (n2 - 1 + pclip))
+		else
+		    n3 = max (1, nint (n2 + pclip))
+	    } else
+		n3 = min (n1, nint (n2 + pclip))
+	    nin = n1
+	}
+
+	# Now apply clipping.
+	do i = 1, npts {
+	    # Compute median.
+	    if (dflag == D_MIX) {
+		n1 = n[i]
+		if (nkeep < 0)
+		    maxkeep = max (0, n1 + nkeep)
+		else
+		    maxkeep = min (n1, nkeep)
+		if (n1 == 0) {
+		    if (combine == MEDIAN)
+			median[i] = blank
+		    next
+		}
+		n2 = 1 + n1 / 2
+		even = (mod (n1, 2) == 0)
+		if (pclip < 0) {
+		    if (even)
+			n3 = max (1, nint (n2 - 1 + pclip))
+		    else
+			n3 = max (1, nint (n2 + pclip))
+		} else
+		    n3 = min (n1, nint (n2 + pclip))
+	    }
+
+	    j = i - 1 
+	    if (even) {
+		med = Mems[d[n2-1]+j]
+		med = (med + Mems[d[n2]+j]) / 2.
+	    } else
+		med = Mems[d[n2]+j]
+
+	    if (n1 < max (MINCLIP, maxkeep+1)) {
+		if (combine == MEDIAN)
+		    median[i] = med
+		next
+	    }
+
+	    # Define sigma for clipping
+	    sigma = t * (Mems[d[n3]+j] - med)
+	    if (fp_equalr (sigma, 0.)) {
+		if (combine == MEDIAN)
+		    median[i] = med
+		next
+	    }
+
+	    # Reject pixels and save residuals.
+	    # Check if any pixels are clipped.
+	    # If so recompute the median and reset the number of good pixels.
+	    # Only reorder if needed.
+
+	    for (nl=1; nl<=n1; nl=nl+1) {
+		r = (med - Mems[d[nl]+j]) / sigma
+		if (r < lsigma)
+		    break
+		Memr[resid+nl] = r
+	    }
+	    for (nh=n1; nh>=1; nh=nh-1) {
+		r = (Mems[d[nh]+j] -  med) / sigma
+		if (r < hsigma)
+		    break
+		Memr[resid+nh] = r
+	    }
+	    n4 = nh - nl + 1
+
+	    # If too many pixels are rejected add some back in.
+	    # All pixels with the same residual are added.
+	    while (n4 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n4 = nh - nl + 1
+	    }
+
+	    # If any pixels are rejected recompute the median.
+	    if (nl > 1 || nh < n1) {
+		n5 = nl + n4 / 2
+		if (mod (n4, 2) == 0) {
+		    med = Mems[d[n5-1]+j]
+		    med = (med + Mems[d[n5]+j]) / 2.
+		} else
+		    med = Mems[d[n5]+j]
+		n[i] = n4
+	    }
+	    if (combine == MEDIAN)
+		median[i] = med
+
+	    # Reorder if pixels only if necessary.
+	    if (nl > 1 && (combine != MEDIAN || grow > 0)) {
+		k = max (nl, n4 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mems[d[l]+j] = Mems[d[k]+j]
+			if (grow > 0) {
+			    mp1 = m[l] + j
+			    mp2 = m[k] + j
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+j] = Memi[m[k]+j]
+			k = k + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mems[d[l]+j] = Mems[d[k]+j]
+			k = k + 1
+		    }
+		}
+	    }
+	}
+
+	# Check if data flag needs to be reset for rejected pixels.
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag whether the median has been computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+
+# IC_PCLIP -- Percentile clip
+#
+# 1) Find the median
+# 2) Find the pixel which is the specified order index away
+# 3) Use the data value difference as a sigma and apply clipping
+# 4) Since the median is known return it so it does not have to be recomputed
+
+procedure ic_pclipr (d, m, n, nimages, npts, median)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image id pointers
+int	n[npts]			# Number of good pixels
+int	nimages			# Number of input images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, n4, n5, nl, nh, nin, maxkeep
+bool	even, fp_equalr()
+real	sigma, r, s, t
+pointer	sp, resid, mp1, mp2
+real	med
+
+include	"../icombine.com"
+
+begin
+	# There must be at least MINCLIP and more than nkeep pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Set sign of pclip parameter
+	if (pclip < 0)
+	    t = -1.
+	else
+	    t = 1.
+
+	# If there are no rejected pixels compute certain parameters once.
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    n2 = 1 + n1 / 2
+	    even = (mod (n1, 2) == 0)
+	    if (pclip < 0.) {
+		if (even)
+		    n3 = max (1, nint (n2 - 1 + pclip))
+		else
+		    n3 = max (1, nint (n2 + pclip))
+	    } else
+		n3 = min (n1, nint (n2 + pclip))
+	    nin = n1
+	}
+
+	# Now apply clipping.
+	do i = 1, npts {
+	    # Compute median.
+	    if (dflag == D_MIX) {
+		n1 = n[i]
+		if (nkeep < 0)
+		    maxkeep = max (0, n1 + nkeep)
+		else
+		    maxkeep = min (n1, nkeep)
+		if (n1 == 0) {
+		    if (combine == MEDIAN)
+			median[i] = blank
+		    next
+		}
+		n2 = 1 + n1 / 2
+		even = (mod (n1, 2) == 0)
+		if (pclip < 0) {
+		    if (even)
+			n3 = max (1, nint (n2 - 1 + pclip))
+		    else
+			n3 = max (1, nint (n2 + pclip))
+		} else
+		    n3 = min (n1, nint (n2 + pclip))
+	    }
+
+	    j = i - 1 
+	    if (even) {
+		med = Memr[d[n2-1]+j]
+		med = (med + Memr[d[n2]+j]) / 2.
+	    } else
+		med = Memr[d[n2]+j]
+
+	    if (n1 < max (MINCLIP, maxkeep+1)) {
+		if (combine == MEDIAN)
+		    median[i] = med
+		next
+	    }
+
+	    # Define sigma for clipping
+	    sigma = t * (Memr[d[n3]+j] - med)
+	    if (fp_equalr (sigma, 0.)) {
+		if (combine == MEDIAN)
+		    median[i] = med
+		next
+	    }
+
+	    # Reject pixels and save residuals.
+	    # Check if any pixels are clipped.
+	    # If so recompute the median and reset the number of good pixels.
+	    # Only reorder if needed.
+
+	    for (nl=1; nl<=n1; nl=nl+1) {
+		r = (med - Memr[d[nl]+j]) / sigma
+		if (r < lsigma)
+		    break
+		Memr[resid+nl] = r
+	    }
+	    for (nh=n1; nh>=1; nh=nh-1) {
+		r = (Memr[d[nh]+j] -  med) / sigma
+		if (r < hsigma)
+		    break
+		Memr[resid+nh] = r
+	    }
+	    n4 = nh - nl + 1
+
+	    # If too many pixels are rejected add some back in.
+	    # All pixels with the same residual are added.
+	    while (n4 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n4 = nh - nl + 1
+	    }
+
+	    # If any pixels are rejected recompute the median.
+	    if (nl > 1 || nh < n1) {
+		n5 = nl + n4 / 2
+		if (mod (n4, 2) == 0) {
+		    med = Memr[d[n5-1]+j]
+		    med = (med + Memr[d[n5]+j]) / 2.
+		} else
+		    med = Memr[d[n5]+j]
+		n[i] = n4
+	    }
+	    if (combine == MEDIAN)
+		median[i] = med
+
+	    # Reorder if pixels only if necessary.
+	    if (nl > 1 && (combine != MEDIAN || grow > 0)) {
+		k = max (nl, n4 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Memr[d[l]+j] = Memr[d[k]+j]
+			if (grow > 0) {
+			    mp1 = m[l] + j
+			    mp2 = m[k] + j
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+j] = Memi[m[k]+j]
+			k = k + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Memr[d[l]+j] = Memr[d[k]+j]
+			k = k + 1
+		    }
+		}
+	    }
+	}
+
+	# Check if data flag needs to be reset for rejected pixels.
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag whether the median has been computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/combine/generic/icsclip.x b/noao/imred/ccdred/src/combine/generic/icsclip.x
new file mode 100644
index 00000000..d7ccfd84
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/icsclip.x
@@ -0,0 +1,964 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		3	# Mininum number of images for algorithm
+
+
+# IC_ASIGCLIP -- Reject pixels using sigma clipping about the average
+# The initial average rejects the high and low pixels.  A correction for
+# different scalings of the images may be made.  Weights are not used.
+
+procedure ic_asigclips (d, m, n, scales, zeros, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+real	d1, low, high, sum, a, s, r, one
+data	one /1.0/
+pointer	sp, resid, w, wp, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	} 
+	
+	# Flag whether returned average needs to be recomputed.
+	if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	# Save the residuals and the sigma scaling corrections if needed.
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+	if (doscale1)
+	    call salloc (w, nimages, TY_REAL)
+
+	# Do sigma clipping.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+
+	    # If there are not enough pixels simply compute the average.
+	    if (n1 < max (3, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Mems[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Mems[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    # Compute average with the high and low rejected.
+	    low = Mems[d[1]+k]
+	    high = Mems[d[2]+k]
+	    if (low > high) {
+		d1 = low
+		low = high
+		high = d1
+	    }
+	    sum = 0.
+	    do j = 3, n1 {
+	       d1 = Mems[d[j]+k]
+	       if (d1 < low) {
+		   sum = sum + low
+		   low = d1
+		} else if (d1 > high) {
+		    sum = sum + high
+		    high = d1
+		} else
+		    sum = sum + d1
+	    }
+	    a = sum / (n1 - 2)
+	    sum = sum + low + high
+
+	    # Iteratively reject pixels and compute the final average if needed.
+	    # Compact the data and keep track of the image IDs if needed.
+
+	    repeat {
+		n2 = n1
+		if (doscale1) {
+		    # Compute sigma corrected for scaling.
+		    s = 0.
+		    wp = w - 1
+		    do j = 1, n1 {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			wp = wp + 1
+
+			d1 = Mems[dp1]
+			l = Memi[mp1]
+			r = sqrt (max (one, (a + zeros[l]) / scales[l]))
+			s = s + ((d1 - a) / r) ** 2
+			Memr[wp] = r
+		    }
+		    s = sqrt (s / (n1 - 1))
+
+		    # Reject pixels.  Save the residuals and data values.
+		    wp = w - 1
+		    if (s > 0.) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    mp1 = m[j] + k
+			    wp = wp + 1
+
+			    d1 = Mems[dp1]
+			    r = (d1 - a) / (s * Memr[wp])
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs (r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    Memr[wp] = Memr[w+n1-1]
+				    mp2 = m[n1] + k
+				    l = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		} else {
+		    # Compute the sigma without scale correction.
+		    s = 0.
+		    do j = 1, n1
+			s = s + (Mems[d[j]+k] - a) ** 2
+		    s = sqrt (s / (n1 - 1))
+
+		    # Reject pixels.  Save the residuals and data values.
+		    if (s > 0.) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    d1 = Mems[dp1]
+			    r = (d1 - a) / s
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs (r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[n1] + k
+					l = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = l
+				    }
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+
+		# Recompute the average.
+		if (n1 > 1)
+		    a = sum / n1
+	    } until (n1 == n2 || n1 <= max (2, maxkeep))
+
+	    # If too many pixels are rejected add some back.
+	    # All pixels with equal residuals are added back.
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mems[dp1]
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Mems[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mems[dp1]
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Mems[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+
+		# Recompute the average.
+		if (n1 > 1)
+		    a = sum / n1
+	    }
+
+	    # Save the average if needed.
+	    n[i] = n1
+	    if (!docombine) {
+		if (n1 > 0)
+		    average[i] = a
+		else
+		    average[i] = blank
+	    }
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_MSIGCLIP -- Reject pixels using sigma clipping about the median
+
+procedure ic_msigclips (d, m, n, scales, zeros, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+real	r, s
+pointer	sp, resid, w, mp1, mp2
+real	med, one
+data	one /1.0/
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	# Save the residuals and sigma scaling corrections if needed.
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+	if (doscale1)
+	    call salloc (w, nimages, TY_REAL)
+
+	# Compute median and sigma and iteratively clip.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    nl = 1
+	    nh = n1
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 == 0)
+		    med = blank
+		else if (mod (n1, 2) == 0)
+		    med = (Mems[d[n3-1]+k] + Mems[d[n3]+k]) / 2.
+		else
+		    med = Mems[d[n3]+k]
+
+		if (n1 >= max (MINCLIP, maxkeep+1)) {
+		    if (doscale1) {
+			# Compute the sigma with scaling correction.
+			s = 0.
+			do j = nl, nh {
+			    l = Memi[m[j]+k]
+			    r = sqrt (max (one, (med + zeros[l]) / scales[l]))
+			    s = s + ((Mems[d[j]+k] - med) / r) ** 2
+			    Memr[w+j-1] = r
+			}
+			s = sqrt (s / (n1 - 1))
+
+			# Reject pixels and save the residuals.
+			if (s > 0.) {
+			    for (; nl <= n2; nl = nl + 1) {
+				r = (med - Mems[d[nl]+k]) / (s * Memr[w+nl-1])
+				if (r <= lsigma)
+				    break
+				Memr[resid+nl] = r
+				n1 = n1 - 1
+			    }
+			    for (; nh >= nl; nh = nh - 1) {
+				r = (Mems[d[nh]+k] - med) / (s * Memr[w+nh-1])
+				if (r <= hsigma)
+				    break
+				Memr[resid+nh] = r
+				n1 = n1 - 1
+			    }
+			}
+		    } else {
+			# Compute the sigma without scaling correction.
+			s = 0.
+			do j = nl, nh
+			    s = s + (Mems[d[j]+k] - med) ** 2
+			s = sqrt (s / (n1 - 1))
+
+			# Reject pixels and save the residuals.
+			if (s > 0.) {
+			    for (; nl <= n2; nl = nl + 1) {
+				r = (med - Mems[d[nl]+k]) / s
+				if (r <= lsigma)
+				    break
+				Memr[resid+nl] = r
+				n1 = n1 - 1
+			    }
+			    for (; nh >= nl; nh = nh - 1) {
+				r = (Mems[d[nh]+k] -  med) / s
+				if (r <= hsigma)
+				    break
+				Memr[resid+nh] = r
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    # If too many pixels are rejected add some back.
+	    # All pixels with equal residuals are added back.
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mems[d[l]+k] = Mems[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mems[d[l]+k] = Mems[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median has been computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+
+# IC_ASIGCLIP -- Reject pixels using sigma clipping about the average
+# The initial average rejects the high and low pixels.  A correction for
+# different scalings of the images may be made.  Weights are not used.
+
+procedure ic_asigclipr (d, m, n, scales, zeros, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+real	d1, low, high, sum, a, s, r, one
+data	one /1.0/
+pointer	sp, resid, w, wp, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	} 
+	
+	# Flag whether returned average needs to be recomputed.
+	if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	# Save the residuals and the sigma scaling corrections if needed.
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+	if (doscale1)
+	    call salloc (w, nimages, TY_REAL)
+
+	# Do sigma clipping.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+
+	    # If there are not enough pixels simply compute the average.
+	    if (n1 < max (3, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Memr[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Memr[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    # Compute average with the high and low rejected.
+	    low = Memr[d[1]+k]
+	    high = Memr[d[2]+k]
+	    if (low > high) {
+		d1 = low
+		low = high
+		high = d1
+	    }
+	    sum = 0.
+	    do j = 3, n1 {
+	       d1 = Memr[d[j]+k]
+	       if (d1 < low) {
+		   sum = sum + low
+		   low = d1
+		} else if (d1 > high) {
+		    sum = sum + high
+		    high = d1
+		} else
+		    sum = sum + d1
+	    }
+	    a = sum / (n1 - 2)
+	    sum = sum + low + high
+
+	    # Iteratively reject pixels and compute the final average if needed.
+	    # Compact the data and keep track of the image IDs if needed.
+
+	    repeat {
+		n2 = n1
+		if (doscale1) {
+		    # Compute sigma corrected for scaling.
+		    s = 0.
+		    wp = w - 1
+		    do j = 1, n1 {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			wp = wp + 1
+
+			d1 = Memr[dp1]
+			l = Memi[mp1]
+			r = sqrt (max (one, (a + zeros[l]) / scales[l]))
+			s = s + ((d1 - a) / r) ** 2
+			Memr[wp] = r
+		    }
+		    s = sqrt (s / (n1 - 1))
+
+		    # Reject pixels.  Save the residuals and data values.
+		    wp = w - 1
+		    if (s > 0.) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    mp1 = m[j] + k
+			    wp = wp + 1
+
+			    d1 = Memr[dp1]
+			    r = (d1 - a) / (s * Memr[wp])
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs (r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    Memr[wp] = Memr[w+n1-1]
+				    mp2 = m[n1] + k
+				    l = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		} else {
+		    # Compute the sigma without scale correction.
+		    s = 0.
+		    do j = 1, n1
+			s = s + (Memr[d[j]+k] - a) ** 2
+		    s = sqrt (s / (n1 - 1))
+
+		    # Reject pixels.  Save the residuals and data values.
+		    if (s > 0.) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    d1 = Memr[dp1]
+			    r = (d1 - a) / s
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs (r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[n1] + k
+					l = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = l
+				    }
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+
+		# Recompute the average.
+		if (n1 > 1)
+		    a = sum / n1
+	    } until (n1 == n2 || n1 <= max (2, maxkeep))
+
+	    # If too many pixels are rejected add some back.
+	    # All pixels with equal residuals are added back.
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Memr[dp1]
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Memr[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Memr[dp1]
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Memr[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+
+		# Recompute the average.
+		if (n1 > 1)
+		    a = sum / n1
+	    }
+
+	    # Save the average if needed.
+	    n[i] = n1
+	    if (!docombine) {
+		if (n1 > 0)
+		    average[i] = a
+		else
+		    average[i] = blank
+	    }
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_MSIGCLIP -- Reject pixels using sigma clipping about the median
+
+procedure ic_msigclipr (d, m, n, scales, zeros, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+real	r, s
+pointer	sp, resid, w, mp1, mp2
+real	med, one
+data	one /1.0/
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	# Save the residuals and sigma scaling corrections if needed.
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+	if (doscale1)
+	    call salloc (w, nimages, TY_REAL)
+
+	# Compute median and sigma and iteratively clip.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    nl = 1
+	    nh = n1
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 == 0)
+		    med = blank
+		else if (mod (n1, 2) == 0)
+		    med = (Memr[d[n3-1]+k] + Memr[d[n3]+k]) / 2.
+		else
+		    med = Memr[d[n3]+k]
+
+		if (n1 >= max (MINCLIP, maxkeep+1)) {
+		    if (doscale1) {
+			# Compute the sigma with scaling correction.
+			s = 0.
+			do j = nl, nh {
+			    l = Memi[m[j]+k]
+			    r = sqrt (max (one, (med + zeros[l]) / scales[l]))
+			    s = s + ((Memr[d[j]+k] - med) / r) ** 2
+			    Memr[w+j-1] = r
+			}
+			s = sqrt (s / (n1 - 1))
+
+			# Reject pixels and save the residuals.
+			if (s > 0.) {
+			    for (; nl <= n2; nl = nl + 1) {
+				r = (med - Memr[d[nl]+k]) / (s * Memr[w+nl-1])
+				if (r <= lsigma)
+				    break
+				Memr[resid+nl] = r
+				n1 = n1 - 1
+			    }
+			    for (; nh >= nl; nh = nh - 1) {
+				r = (Memr[d[nh]+k] - med) / (s * Memr[w+nh-1])
+				if (r <= hsigma)
+				    break
+				Memr[resid+nh] = r
+				n1 = n1 - 1
+			    }
+			}
+		    } else {
+			# Compute the sigma without scaling correction.
+			s = 0.
+			do j = nl, nh
+			    s = s + (Memr[d[j]+k] - med) ** 2
+			s = sqrt (s / (n1 - 1))
+
+			# Reject pixels and save the residuals.
+			if (s > 0.) {
+			    for (; nl <= n2; nl = nl + 1) {
+				r = (med - Memr[d[nl]+k]) / s
+				if (r <= lsigma)
+				    break
+				Memr[resid+nl] = r
+				n1 = n1 - 1
+			    }
+			    for (; nh >= nl; nh = nh - 1) {
+				r = (Memr[d[nh]+k] -  med) / s
+				if (r <= hsigma)
+				    break
+				Memr[resid+nh] = r
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    # If too many pixels are rejected add some back.
+	    # All pixels with equal residuals are added back.
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Memr[d[l]+k] = Memr[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Memr[d[l]+k] = Memr[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median has been computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/combine/generic/icsigma.x b/noao/imred/ccdred/src/combine/generic/icsigma.x
new file mode 100644
index 00000000..bc0d9788
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/icsigma.x
@@ -0,0 +1,205 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"../icombine.h"
+
+
+# IC_SIGMA -- Compute the sigma image line.
+# The estimated sigma includes a correction for the finite population.
+# Weights are used if desired.
+
+procedure ic_sigmas (d, m, n, wts, npts, average, sigma)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image ID pointers
+int	n[npts]			# Number of points
+real	wts[ARB]		# Weights
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+real	sigma[npts]		# Sigma line (returned)
+
+int	i, j, k, n1
+real	wt, sigcor, sumwt
+real	a, sum
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    if (dowts) {
+		if (n1 > 1)
+		    sigcor = real (n1) / real (n1 - 1)
+		else
+		    sigcor = 1.
+		do i = 1, npts {
+		    k = i - 1
+		    a = average[i]
+		    wt = wts[Memi[m[1]+k]]
+		    sum = (Mems[d[1]+k] - a) ** 2 * wt
+		    do j = 2, n1 {
+			wt = wts[Memi[m[j]+k]]
+			sum = sum + (Mems[d[j]+k] - a) ** 2 * wt
+		    }
+		    sigma[i] = sqrt (sum * sigcor)
+		}
+	    } else {
+		if (n1 > 1)
+		    sigcor = 1. / real (n1 - 1)
+		else
+		    sigcor = 1.
+		do i = 1, npts {
+		    k = i - 1
+		    a = average[i]
+		    sum = (Mems[d[1]+k] - a) ** 2
+		    do j = 2, n1
+			sum = sum + (Mems[d[j]+k] - a) ** 2
+		    sigma[i] = sqrt (sum * sigcor)
+		}
+	    }
+	} else if (dflag == D_NONE) {
+	    do i = 1, npts
+		sigma[i] = blank
+	} else {
+	    if (dowts) {
+		do i = 1, npts {
+		    n1 = n[i]
+		    if (n1 > 0) {
+			k = i - 1
+			if (n1 > 1)
+			    sigcor = real (n1) / real (n1 -1)
+			else
+			    sigcor = 1
+			a = average[i]
+			wt = wts[Memi[m[1]+k]]
+			sum = (Mems[d[1]+k] - a) ** 2 * wt
+			sumwt = wt
+			do j = 2, n1 {
+			    wt = wts[Memi[m[j]+k]]
+			    sum = sum + (Mems[d[j]+k] - a) ** 2 * wt
+			    sumwt = sumwt + wt
+			}
+			sigma[i] = sqrt (sum / sumwt * sigcor)
+		    } else
+			sigma[i] = blank
+		}
+	    } else {
+		do i = 1, npts {
+		    n1 = n[i]
+		    if (n1 > 0) {
+			k = i - 1
+			if (n1 > 1)
+			    sigcor = 1. / real (n1 - 1)
+			else
+			    sigcor = 1.
+			a = average[i]
+			sum = (Mems[d[1]+k] - a) ** 2
+			do j = 2, n1
+			    sum = sum + (Mems[d[j]+k] - a) ** 2
+			sigma[i] = sqrt (sum * sigcor)
+		    } else
+			sigma[i] = blank
+		}
+	    }
+	}
+end
+
+# IC_SIGMA -- Compute the sigma image line.
+# The estimated sigma includes a correction for the finite population.
+# Weights are used if desired.
+
+procedure ic_sigmar (d, m, n, wts, npts, average, sigma)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image ID pointers
+int	n[npts]			# Number of points
+real	wts[ARB]		# Weights
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+real	sigma[npts]		# Sigma line (returned)
+
+int	i, j, k, n1
+real	wt, sigcor, sumwt
+real	a, sum
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    if (dowts) {
+		if (n1 > 1)
+		    sigcor = real (n1) / real (n1 - 1)
+		else
+		    sigcor = 1.
+		do i = 1, npts {
+		    k = i - 1
+		    a = average[i]
+		    wt = wts[Memi[m[1]+k]]
+		    sum = (Memr[d[1]+k] - a) ** 2 * wt
+		    do j = 2, n1 {
+			wt = wts[Memi[m[j]+k]]
+			sum = sum + (Memr[d[j]+k] - a) ** 2 * wt
+		    }
+		    sigma[i] = sqrt (sum * sigcor)
+		}
+	    } else {
+		if (n1 > 1)
+		    sigcor = 1. / real (n1 - 1)
+		else
+		    sigcor = 1.
+		do i = 1, npts {
+		    k = i - 1
+		    a = average[i]
+		    sum = (Memr[d[1]+k] - a) ** 2
+		    do j = 2, n1
+			sum = sum + (Memr[d[j]+k] - a) ** 2
+		    sigma[i] = sqrt (sum * sigcor)
+		}
+	    }
+	} else if (dflag == D_NONE) {
+	    do i = 1, npts
+		sigma[i] = blank
+	} else {
+	    if (dowts) {
+		do i = 1, npts {
+		    n1 = n[i]
+		    if (n1 > 0) {
+			k = i - 1
+			if (n1 > 1)
+			    sigcor = real (n1) / real (n1 -1)
+			else
+			    sigcor = 1
+			a = average[i]
+			wt = wts[Memi[m[1]+k]]
+			sum = (Memr[d[1]+k] - a) ** 2 * wt
+			sumwt = wt
+			do j = 2, n1 {
+			    wt = wts[Memi[m[j]+k]]
+			    sum = sum + (Memr[d[j]+k] - a) ** 2 * wt
+			    sumwt = sumwt + wt
+			}
+			sigma[i] = sqrt (sum / sumwt * sigcor)
+		    } else
+			sigma[i] = blank
+		}
+	    } else {
+		do i = 1, npts {
+		    n1 = n[i]
+		    if (n1 > 0) {
+			k = i - 1
+			if (n1 > 1)
+			    sigcor = 1. / real (n1 - 1)
+			else
+			    sigcor = 1.
+			a = average[i]
+			sum = (Memr[d[1]+k] - a) ** 2
+			do j = 2, n1
+			    sum = sum + (Memr[d[j]+k] - a) ** 2
+			sigma[i] = sqrt (sum * sigcor)
+		    } else
+			sigma[i] = blank
+		}
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/src/combine/generic/icsort.x b/noao/imred/ccdred/src/combine/generic/icsort.x
new file mode 100644
index 00000000..a39b68e2
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/icsort.x
@@ -0,0 +1,550 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+define	LOGPTR	32			# log2(maxpts) (4e9)
+
+
+# IC_SORT -- Quicksort.  This is based on the VOPS asrt except that
+# the input is an array of pointers to image lines and the sort is done
+# across the image lines at each point along the lines.  The number of
+# valid pixels at each point is allowed to vary.  The cases of 1, 2, and 3
+# pixels per point are treated specially.
+
+procedure ic_sorts (a, b, nvecs, npts)
+
+pointer	a[ARB]			# pointer to input vectors
+short	b[ARB]			# work array
+int	nvecs[npts]		# number of vectors
+int	npts			# number of points in vectors
+
+short	pivot, temp, temp3
+int	i, j, k, l, p, npix, lv[LOGPTR], uv[LOGPTR]
+define	swap {temp=$1;$1=$2;$2=temp}
+define	copy_	10
+
+begin
+	do l = 0, npts-1 {
+	    npix = nvecs[l+1]
+	    if (npix <= 1)
+		next
+
+	    do i = 1, npix
+		b[i] = Mems[a[i]+l]
+
+	    # Special cases
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (temp < pivot) {
+			b[1] = temp
+			b[2] = pivot
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (temp < pivot) {				# bac|bca|cba
+			if (temp < temp3) {			# bac|bca
+			    b[1] = temp
+			    if (pivot < temp3)			# bac
+				b[2] = pivot
+			    else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			}
+		    } else if (temp3 < temp) {			# acb|cab
+			b[3] = temp
+			if (pivot < temp3)			# acb
+			    b[2] = temp3
+			else {					# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+
+	    # General case
+	    do i = 1, npix
+		b[i] = Mems[a[i]+l]
+
+	    lv[1] = 1
+	    uv[1] = npix
+	    p = 1
+
+	    while (p > 0) {
+		if (lv[p] >= uv[p])		# only one elem in this subset
+		    p = p - 1			# pop stack
+		else {
+		    # Dummy do loop to trigger the Fortran optimizer.
+		    do p = p, ARB {
+			i = lv[p] - 1
+			j = uv[p]
+
+			# Select as the pivot the element at the center of the
+			# array, to avoid quadratic behavior on an already
+			# sorted array.
+
+			k = (lv[p] + uv[p]) / 2
+			swap (b[j], b[k])
+			pivot = b[j]		   # pivot line
+
+			while (i < j) {
+			    for (i=i+1;  b[i] < pivot;  i=i+1)
+				;
+			    for (j=j-1;  j > i;  j=j-1)
+				if (b[j] <= pivot)
+				    break
+			    if (i < j)		   # out of order pair
+				swap (b[i], b[j])  # interchange elements
+			}
+
+			j = uv[p]		   # move pivot to position i
+			swap (b[i], b[j])	   # interchange elements
+
+			if (i-lv[p] < uv[p] - i) { # stack so shorter done first
+			    lv[p+1] = lv[p]
+			    uv[p+1] = i - 1
+			    lv[p] = i + 1
+			} else {
+			    lv[p+1] = i + 1
+			    uv[p+1] = uv[p]
+			    uv[p] = i - 1
+			}
+
+			break
+		    }
+		    p = p + 1			   # push onto stack
+		}
+	    }
+
+copy_
+	    do i = 1, npix
+		Mems[a[i]+l] = b[i]
+	}
+end
+
+
+# IC_2SORT -- Quicksort.  This is based on the VOPS asrt except that
+# the input is an array of pointers to image lines and the sort is done
+# across the image lines at each point along the lines.  The number of
+# valid pixels at each point is allowed to vary.  The cases of 1, 2, and 3
+# pixels per point are treated specially.  A second integer set of
+# vectors is sorted.
+
+procedure ic_2sorts (a, b, c, d, nvecs, npts)
+
+pointer	a[ARB]			# pointer to input vectors
+short	b[ARB]			# work array
+pointer	c[ARB]			# pointer to associated integer vectors
+int	d[ARB]			# work array
+int	nvecs[npts]		# number of vectors
+int	npts			# number of points in vectors
+
+short	pivot, temp, temp3
+int	i, j, k, l, p, npix, lv[LOGPTR], uv[LOGPTR], itemp
+define	swap {temp=$1;$1=$2;$2=temp}
+define	iswap {itemp=$1;$1=$2;$2=itemp}
+define	copy_	10
+
+begin
+	do l = 0, npts-1 {
+	    npix = nvecs[l+1]
+	    if (npix <= 1)
+		next
+
+	    do i = 1, npix {
+		b[i] = Mems[a[i]+l]
+		d[i] = Memi[c[i]+l]
+	    }
+
+	    # Special cases
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (temp < pivot) {
+			b[1] = temp
+			b[2] = pivot
+			iswap (d[1], d[2])
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (temp < pivot) {				# bac|bca|cba
+			if (temp < temp3) {			# bac|bca
+			    b[1] = temp
+			    if (pivot < temp3) {		# bac
+				b[2] = pivot
+				iswap (d[1], d[2])
+			    } else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+				itemp = d[2]
+				d[2] = d[3]
+				d[3] = d[1]
+				d[1] = itemp
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			    iswap (d[1], d[3])
+			}
+		    } else if (temp3 < temp) {			# acb|cab
+			b[3] = temp
+			if (pivot < temp3) {			# acb
+			    b[2] = temp3
+			    iswap (d[2], d[3])
+			} else {				# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			    itemp = d[2]
+			    d[2] = d[1]
+			    d[1] = d[3]
+			    d[3] = itemp
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+
+	    # General case
+	    lv[1] = 1
+	    uv[1] = npix
+	    p = 1
+
+	    while (p > 0) {
+		if (lv[p] >= uv[p])		# only one elem in this subset
+		    p = p - 1			# pop stack
+		else {
+		    # Dummy do loop to trigger the Fortran optimizer.
+		    do p = p, ARB {
+			i = lv[p] - 1
+			j = uv[p]
+
+			# Select as the pivot the element at the center of the
+			# array, to avoid quadratic behavior on an already
+			# sorted array.
+
+			k = (lv[p] + uv[p]) / 2
+			swap (b[j], b[k]); swap (d[j], d[k])
+			pivot = b[j]		   # pivot line
+
+			while (i < j) {
+			    for (i=i+1;  b[i] < pivot;  i=i+1)
+				;
+			    for (j=j-1;  j > i;  j=j-1)
+				if (b[j] <= pivot)
+				    break
+			    if (i < j) {	   # out of order pair
+				swap (b[i], b[j])  # interchange elements
+				swap (d[i], d[j])
+			    }
+			}
+
+			j = uv[p]		   # move pivot to position i
+			swap (b[i], b[j])	   # interchange elements
+			swap (d[i], d[j])
+
+			if (i-lv[p] < uv[p] - i) { # stack so shorter done first
+			    lv[p+1] = lv[p]
+			    uv[p+1] = i - 1
+			    lv[p] = i + 1
+			} else {
+			    lv[p+1] = i + 1
+			    uv[p+1] = uv[p]
+			    uv[p] = i - 1
+			}
+
+			break
+		    }
+		    p = p + 1			   # push onto stack
+		}
+	    }
+
+copy_	   
+	    do i = 1, npix {
+		Mems[a[i]+l] = b[i]
+		Memi[c[i]+l] = d[i]
+	    }
+	}
+end
+
+# IC_SORT -- Quicksort.  This is based on the VOPS asrt except that
+# the input is an array of pointers to image lines and the sort is done
+# across the image lines at each point along the lines.  The number of
+# valid pixels at each point is allowed to vary.  The cases of 1, 2, and 3
+# pixels per point are treated specially.
+
+procedure ic_sortr (a, b, nvecs, npts)
+
+pointer	a[ARB]			# pointer to input vectors
+real	b[ARB]			# work array
+int	nvecs[npts]		# number of vectors
+int	npts			# number of points in vectors
+
+real	pivot, temp, temp3
+int	i, j, k, l, p, npix, lv[LOGPTR], uv[LOGPTR]
+define	swap {temp=$1;$1=$2;$2=temp}
+define	copy_	10
+
+begin
+	do l = 0, npts-1 {
+	    npix = nvecs[l+1]
+	    if (npix <= 1)
+		next
+
+	    do i = 1, npix
+		b[i] = Memr[a[i]+l]
+
+	    # Special cases
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (temp < pivot) {
+			b[1] = temp
+			b[2] = pivot
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (temp < pivot) {				# bac|bca|cba
+			if (temp < temp3) {			# bac|bca
+			    b[1] = temp
+			    if (pivot < temp3)			# bac
+				b[2] = pivot
+			    else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			}
+		    } else if (temp3 < temp) {			# acb|cab
+			b[3] = temp
+			if (pivot < temp3)			# acb
+			    b[2] = temp3
+			else {					# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+
+	    # General case
+	    do i = 1, npix
+		b[i] = Memr[a[i]+l]
+
+	    lv[1] = 1
+	    uv[1] = npix
+	    p = 1
+
+	    while (p > 0) {
+		if (lv[p] >= uv[p])		# only one elem in this subset
+		    p = p - 1			# pop stack
+		else {
+		    # Dummy do loop to trigger the Fortran optimizer.
+		    do p = p, ARB {
+			i = lv[p] - 1
+			j = uv[p]
+
+			# Select as the pivot the element at the center of the
+			# array, to avoid quadratic behavior on an already
+			# sorted array.
+
+			k = (lv[p] + uv[p]) / 2
+			swap (b[j], b[k])
+			pivot = b[j]		   # pivot line
+
+			while (i < j) {
+			    for (i=i+1;  b[i] < pivot;  i=i+1)
+				;
+			    for (j=j-1;  j > i;  j=j-1)
+				if (b[j] <= pivot)
+				    break
+			    if (i < j)		   # out of order pair
+				swap (b[i], b[j])  # interchange elements
+			}
+
+			j = uv[p]		   # move pivot to position i
+			swap (b[i], b[j])	   # interchange elements
+
+			if (i-lv[p] < uv[p] - i) { # stack so shorter done first
+			    lv[p+1] = lv[p]
+			    uv[p+1] = i - 1
+			    lv[p] = i + 1
+			} else {
+			    lv[p+1] = i + 1
+			    uv[p+1] = uv[p]
+			    uv[p] = i - 1
+			}
+
+			break
+		    }
+		    p = p + 1			   # push onto stack
+		}
+	    }
+
+copy_
+	    do i = 1, npix
+		Memr[a[i]+l] = b[i]
+	}
+end
+
+
+# IC_2SORT -- Quicksort.  This is based on the VOPS asrt except that
+# the input is an array of pointers to image lines and the sort is done
+# across the image lines at each point along the lines.  The number of
+# valid pixels at each point is allowed to vary.  The cases of 1, 2, and 3
+# pixels per point are treated specially.  A second integer set of
+# vectors is sorted.
+
+procedure ic_2sortr (a, b, c, d, nvecs, npts)
+
+pointer	a[ARB]			# pointer to input vectors
+real	b[ARB]			# work array
+pointer	c[ARB]			# pointer to associated integer vectors
+int	d[ARB]			# work array
+int	nvecs[npts]		# number of vectors
+int	npts			# number of points in vectors
+
+real	pivot, temp, temp3
+int	i, j, k, l, p, npix, lv[LOGPTR], uv[LOGPTR], itemp
+define	swap {temp=$1;$1=$2;$2=temp}
+define	iswap {itemp=$1;$1=$2;$2=itemp}
+define	copy_	10
+
+begin
+	do l = 0, npts-1 {
+	    npix = nvecs[l+1]
+	    if (npix <= 1)
+		next
+
+	    do i = 1, npix {
+		b[i] = Memr[a[i]+l]
+		d[i] = Memi[c[i]+l]
+	    }
+
+	    # Special cases
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (temp < pivot) {
+			b[1] = temp
+			b[2] = pivot
+			iswap (d[1], d[2])
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (temp < pivot) {				# bac|bca|cba
+			if (temp < temp3) {			# bac|bca
+			    b[1] = temp
+			    if (pivot < temp3) {		# bac
+				b[2] = pivot
+				iswap (d[1], d[2])
+			    } else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+				itemp = d[2]
+				d[2] = d[3]
+				d[3] = d[1]
+				d[1] = itemp
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			    iswap (d[1], d[3])
+			}
+		    } else if (temp3 < temp) {			# acb|cab
+			b[3] = temp
+			if (pivot < temp3) {			# acb
+			    b[2] = temp3
+			    iswap (d[2], d[3])
+			} else {				# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			    itemp = d[2]
+			    d[2] = d[1]
+			    d[1] = d[3]
+			    d[3] = itemp
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+
+	    # General case
+	    lv[1] = 1
+	    uv[1] = npix
+	    p = 1
+
+	    while (p > 0) {
+		if (lv[p] >= uv[p])		# only one elem in this subset
+		    p = p - 1			# pop stack
+		else {
+		    # Dummy do loop to trigger the Fortran optimizer.
+		    do p = p, ARB {
+			i = lv[p] - 1
+			j = uv[p]
+
+			# Select as the pivot the element at the center of the
+			# array, to avoid quadratic behavior on an already
+			# sorted array.
+
+			k = (lv[p] + uv[p]) / 2
+			swap (b[j], b[k]); swap (d[j], d[k])
+			pivot = b[j]		   # pivot line
+
+			while (i < j) {
+			    for (i=i+1;  b[i] < pivot;  i=i+1)
+				;
+			    for (j=j-1;  j > i;  j=j-1)
+				if (b[j] <= pivot)
+				    break
+			    if (i < j) {	   # out of order pair
+				swap (b[i], b[j])  # interchange elements
+				swap (d[i], d[j])
+			    }
+			}
+
+			j = uv[p]		   # move pivot to position i
+			swap (b[i], b[j])	   # interchange elements
+			swap (d[i], d[j])
+
+			if (i-lv[p] < uv[p] - i) { # stack so shorter done first
+			    lv[p+1] = lv[p]
+			    uv[p+1] = i - 1
+			    lv[p] = i + 1
+			} else {
+			    lv[p+1] = i + 1
+			    uv[p+1] = uv[p]
+			    uv[p] = i - 1
+			}
+
+			break
+		    }
+		    p = p + 1			   # push onto stack
+		}
+	    }
+
+copy_	   
+	    do i = 1, npix {
+		Memr[a[i]+l] = b[i]
+		Memi[c[i]+l] = d[i]
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/src/combine/generic/icstat.x b/noao/imred/ccdred/src/combine/generic/icstat.x
new file mode 100644
index 00000000..41512ccb
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/icstat.x
@@ -0,0 +1,444 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"../icombine.h"
+
+define	NMAX	10000	# Maximum number of pixels to sample
+
+
+# IC_STAT -- Compute image statistics within specified section.
+# The image section is relative to a reference image which may be
+# different than the input image and may have an offset.  Only a
+# subsample of pixels is used.  Masked and thresholded pixels are
+# ignored.  Only the desired statistics are computed to increase
+# efficiency.
+
+procedure ic_stats (im, imref, section, offsets, image, nimages,
+	domode, domedian, domean, mode, median, mean)
+
+pointer	im			 # Data image
+pointer	imref			 # Reference image for image section
+char	section[ARB]		 # Image section
+int	offsets[nimages,ARB]	 # Image section offset from data to reference
+int	image			 # Image index (for mask I/O)
+int	nimages			 # Number of images in  offsets.
+bool	domode, domedian, domean # Statistics to compute
+real	mode, median, mean	 # Statistics
+
+int	i, j, ndim, n, nv
+real	a
+pointer	sp, v1, v2, dv, va, vb
+pointer	data, mask, dp, lp, mp, imgnls()
+short	ic_modes()
+real    asums()
+
+
+include	"../icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (v1, IM_MAXDIM, TY_LONG)
+	call salloc (v2, IM_MAXDIM, TY_LONG)
+	call salloc (dv, IM_MAXDIM, TY_LONG)
+	call salloc (va, IM_MAXDIM, TY_LONG)
+	call salloc (vb, IM_MAXDIM, TY_LONG)
+
+	# Determine the image section parameters.  This must be in terms of
+	# the data image pixel coordinates though the section may be specified
+	# in terms of the reference image coordinates.  Limit the number of
+	# pixels in each dimension to a maximum.
+
+	ndim = IM_NDIM(im)
+	if (project)
+	    ndim = ndim - 1
+	call amovki (1, Memi[v1], IM_MAXDIM)
+	call amovki (1, Memi[va], IM_MAXDIM)
+	call amovki (1, Memi[dv], IM_MAXDIM)
+	call amovi (IM_LEN(imref,1), Memi[vb], ndim)
+	call ic_section (section, Memi[va], Memi[vb], Memi[dv], ndim)
+	if (im != imref)
+	    do i = 1, ndim {
+		Memi[va+i-1] = Memi[va+i-1] - offsets[image,i]
+		Memi[vb+i-1] = Memi[vb+i-1] - offsets[image,i]
+	    }
+
+	do j = 1, 10 {
+	    n = 1
+	    do i = 0, ndim-1 {
+		Memi[v1+i] = max (1, min (Memi[va+i], Memi[vb+i]))
+		Memi[v2+i] = min (IM_LEN(im,i+1), max (Memi[va+i], Memi[vb+i]))
+		Memi[dv+i] = j
+		nv = max (1, (Memi[v2+i] - Memi[v1+i]) / Memi[dv+i] + 1)
+		Memi[v2+i] = Memi[v1+i] + (nv - 1) * Memi[dv+i]
+		n = n * nv
+	    }
+	    if (n < NMAX)
+		break
+	}
+
+	call amovl (Memi[v1], Memi[va], IM_MAXDIM)
+	Memi[va] = 1
+	if (project)
+	   Memi[va+ndim] = image
+	call amovl (Memi[va], Memi[vb], IM_MAXDIM)
+
+	# Accumulate the pixel values within the section.  Masked pixels and
+	# thresholded pixels are ignored.
+
+	call salloc (data, n, TY_SHORT)
+	dp = data
+	while (imgnls (im, lp, Memi[vb]) != EOF) {
+	    call ic_mget1 (im, image, offsets[image,1], Memi[va], mask)
+	    lp = lp + Memi[v1] - 1
+	    if (dflag == D_ALL) {
+		if (dothresh) {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			a = Mems[lp]
+			if (a >= lthresh && a <= hthresh) {
+			    Mems[dp] = a
+			    dp = dp + 1
+			}
+			lp = lp + Memi[dv]
+		    }
+		} else {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			Mems[dp] = Mems[lp]
+			dp = dp + 1
+			lp = lp + Memi[dv]
+		    }
+		}
+	    } else if (dflag == D_MIX) {
+		mp = mask + Memi[v1] - 1
+		if (dothresh) {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			if (Memi[mp] == 0) {
+			    a = Mems[lp]
+			    if (a >= lthresh && a <= hthresh) {
+				Mems[dp] = a
+				dp = dp + 1
+			    }
+			}
+			mp = mp + Memi[dv]
+			lp = lp + Memi[dv]
+		    }
+		} else {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			if (Memi[mp] == 0) {
+			    Mems[dp] = Mems[lp]
+			    dp = dp + 1
+			}
+			mp = mp + Memi[dv]
+			lp = lp + Memi[dv]
+		    }
+		}
+	    }
+	    for (i=2; i<=ndim; i=i+1) {
+		Memi[va+i-1] = Memi[va+i-1] + Memi[dv+i-1]
+		if (Memi[va+i-1] <= Memi[v2+i-1])
+		    break
+		Memi[va+i-1] = Memi[v1+i-1]
+	    }
+	    if (i > ndim)
+		break
+	    call amovl (Memi[va], Memi[vb], IM_MAXDIM)
+	}
+
+	n = dp - data
+	if (n < 1) {
+	    call sfree (sp)
+	    call error (1, "Image section contains no pixels")
+	}
+
+	# Compute only statistics needed.
+	if (domode || domedian) {
+	    call asrts (Mems[data], Mems[data], n)
+	    mode = ic_modes (Mems[data], n)
+	    median = Mems[data+n/2-1]
+	}
+	if (domean)
+	    mean = asums (Mems[data], n) / n
+
+	call sfree (sp)
+end
+
+
+define	NMIN	10	# Minimum number of pixels for mode calculation
+define	ZRANGE	0.8	# Fraction of pixels about median to use
+define	ZSTEP	0.01	# Step size for search for mode
+define	ZBIN	0.1	# Bin size for mode.
+
+# IC_MODE -- Compute mode of an array.  The mode is found by binning
+# with a bin size based on the data range over a fraction of the
+# pixels about the median and a bin step which may be smaller than the
+# bin size.  If there are too few points the median is returned.
+# The input array must be sorted.
+
+short procedure ic_modes (a, n)
+
+short	a[n]			# Data array
+int	n			# Number of points
+
+int	i, j, k, nmax
+real	z1, z2, zstep, zbin
+short	mode
+bool	fp_equalr()
+
+begin
+	if (n < NMIN)
+	    return (a[n/2])
+
+	# Compute the mode.  The array must be sorted.  Consider a
+	# range of values about the median point.  Use a bin size which
+	# is ZBIN of the range.  Step the bin limits in ZSTEP fraction of
+	# the bin size.
+
+	i = 1 + n * (1. - ZRANGE) / 2.
+	j = 1 + n * (1. + ZRANGE) / 2.
+	z1 = a[i]
+	z2 = a[j]
+	if (fp_equalr (z1, z2)) {
+	    mode = z1
+	    return (mode)
+	}
+
+	zstep = ZSTEP * (z2 - z1)
+	zbin = ZBIN * (z2 - z1)
+	zstep = max (1., zstep)
+	zbin = max (1., zbin)
+
+	z1 = z1 - zstep
+	k = i
+	nmax = 0
+	repeat {
+	    z1 = z1 + zstep
+	    z2 = z1 + zbin
+	    for (; i < j && a[i] < z1; i=i+1)
+		;
+	    for (; k < j && a[k] < z2; k=k+1)
+		;
+	    if (k - i > nmax) {
+	        nmax = k - i
+	        mode = a[(i+k)/2]
+	    }
+	} until (k >= j)
+
+	return (mode)
+end
+
+# IC_STAT -- Compute image statistics within specified section.
+# The image section is relative to a reference image which may be
+# different than the input image and may have an offset.  Only a
+# subsample of pixels is used.  Masked and thresholded pixels are
+# ignored.  Only the desired statistics are computed to increase
+# efficiency.
+
+procedure ic_statr (im, imref, section, offsets, image, nimages,
+	domode, domedian, domean, mode, median, mean)
+
+pointer	im			 # Data image
+pointer	imref			 # Reference image for image section
+char	section[ARB]		 # Image section
+int	offsets[nimages,ARB]	 # Image section offset from data to reference
+int	image			 # Image index (for mask I/O)
+int	nimages			 # Number of images in  offsets.
+bool	domode, domedian, domean # Statistics to compute
+real	mode, median, mean	 # Statistics
+
+int	i, j, ndim, n, nv
+real	a
+pointer	sp, v1, v2, dv, va, vb
+pointer	data, mask, dp, lp, mp, imgnlr()
+real	ic_moder()
+real    asumr()
+
+
+include	"../icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (v1, IM_MAXDIM, TY_LONG)
+	call salloc (v2, IM_MAXDIM, TY_LONG)
+	call salloc (dv, IM_MAXDIM, TY_LONG)
+	call salloc (va, IM_MAXDIM, TY_LONG)
+	call salloc (vb, IM_MAXDIM, TY_LONG)
+
+	# Determine the image section parameters.  This must be in terms of
+	# the data image pixel coordinates though the section may be specified
+	# in terms of the reference image coordinates.  Limit the number of
+	# pixels in each dimension to a maximum.
+
+	ndim = IM_NDIM(im)
+	if (project)
+	    ndim = ndim - 1
+	call amovki (1, Memi[v1], IM_MAXDIM)
+	call amovki (1, Memi[va], IM_MAXDIM)
+	call amovki (1, Memi[dv], IM_MAXDIM)
+	call amovi (IM_LEN(imref,1), Memi[vb], ndim)
+	call ic_section (section, Memi[va], Memi[vb], Memi[dv], ndim)
+	if (im != imref)
+	    do i = 1, ndim {
+		Memi[va+i-1] = Memi[va+i-1] - offsets[image,i]
+		Memi[vb+i-1] = Memi[vb+i-1] - offsets[image,i]
+	    }
+
+	do j = 1, 10 {
+	    n = 1
+	    do i = 0, ndim-1 {
+		Memi[v1+i] = max (1, min (Memi[va+i], Memi[vb+i]))
+		Memi[v2+i] = min (IM_LEN(im,i+1), max (Memi[va+i], Memi[vb+i]))
+		Memi[dv+i] = j
+		nv = max (1, (Memi[v2+i] - Memi[v1+i]) / Memi[dv+i] + 1)
+		Memi[v2+i] = Memi[v1+i] + (nv - 1) * Memi[dv+i]
+		n = n * nv
+	    }
+	    if (n < NMAX)
+		break
+	}
+
+	call amovl (Memi[v1], Memi[va], IM_MAXDIM)
+	Memi[va] = 1
+	if (project)
+	   Memi[va+ndim] = image
+	call amovl (Memi[va], Memi[vb], IM_MAXDIM)
+
+	# Accumulate the pixel values within the section.  Masked pixels and
+	# thresholded pixels are ignored.
+
+	call salloc (data, n, TY_REAL)
+	dp = data
+	while (imgnlr (im, lp, Memi[vb]) != EOF) {
+	    call ic_mget1 (im, image, offsets[image,1], Memi[va], mask)
+	    lp = lp + Memi[v1] - 1
+	    if (dflag == D_ALL) {
+		if (dothresh) {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			a = Memr[lp]
+			if (a >= lthresh && a <= hthresh) {
+			    Memr[dp] = a
+			    dp = dp + 1
+			}
+			lp = lp + Memi[dv]
+		    }
+		} else {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			Memr[dp] = Memr[lp]
+			dp = dp + 1
+			lp = lp + Memi[dv]
+		    }
+		}
+	    } else if (dflag == D_MIX) {
+		mp = mask + Memi[v1] - 1
+		if (dothresh) {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			if (Memi[mp] == 0) {
+			    a = Memr[lp]
+			    if (a >= lthresh && a <= hthresh) {
+				Memr[dp] = a
+				dp = dp + 1
+			    }
+			}
+			mp = mp + Memi[dv]
+			lp = lp + Memi[dv]
+		    }
+		} else {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			if (Memi[mp] == 0) {
+			    Memr[dp] = Memr[lp]
+			    dp = dp + 1
+			}
+			mp = mp + Memi[dv]
+			lp = lp + Memi[dv]
+		    }
+		}
+	    }
+	    for (i=2; i<=ndim; i=i+1) {
+		Memi[va+i-1] = Memi[va+i-1] + Memi[dv+i-1]
+		if (Memi[va+i-1] <= Memi[v2+i-1])
+		    break
+		Memi[va+i-1] = Memi[v1+i-1]
+	    }
+	    if (i > ndim)
+		break
+	    call amovl (Memi[va], Memi[vb], IM_MAXDIM)
+	}
+
+	n = dp - data
+	if (n < 1) {
+	    call sfree (sp)
+	    call error (1, "Image section contains no pixels")
+	}
+
+	# Compute only statistics needed.
+	if (domode || domedian) {
+	    call asrtr (Memr[data], Memr[data], n)
+	    mode = ic_moder (Memr[data], n)
+	    median = Memr[data+n/2-1]
+	}
+	if (domean)
+	    mean = asumr (Memr[data], n) / n
+
+	call sfree (sp)
+end
+
+
+define	NMIN	10	# Minimum number of pixels for mode calculation
+define	ZRANGE	0.8	# Fraction of pixels about median to use
+define	ZSTEP	0.01	# Step size for search for mode
+define	ZBIN	0.1	# Bin size for mode.
+
+# IC_MODE -- Compute mode of an array.  The mode is found by binning
+# with a bin size based on the data range over a fraction of the
+# pixels about the median and a bin step which may be smaller than the
+# bin size.  If there are too few points the median is returned.
+# The input array must be sorted.
+
+real procedure ic_moder (a, n)
+
+real	a[n]			# Data array
+int	n			# Number of points
+
+int	i, j, k, nmax
+real	z1, z2, zstep, zbin
+real	mode
+bool	fp_equalr()
+
+begin
+	if (n < NMIN)
+	    return (a[n/2])
+
+	# Compute the mode.  The array must be sorted.  Consider a
+	# range of values about the median point.  Use a bin size which
+	# is ZBIN of the range.  Step the bin limits in ZSTEP fraction of
+	# the bin size.
+
+	i = 1 + n * (1. - ZRANGE) / 2.
+	j = 1 + n * (1. + ZRANGE) / 2.
+	z1 = a[i]
+	z2 = a[j]
+	if (fp_equalr (z1, z2)) {
+	    mode = z1
+	    return (mode)
+	}
+
+	zstep = ZSTEP * (z2 - z1)
+	zbin = ZBIN * (z2 - z1)
+
+	z1 = z1 - zstep
+	k = i
+	nmax = 0
+	repeat {
+	    z1 = z1 + zstep
+	    z2 = z1 + zbin
+	    for (; i < j && a[i] < z1; i=i+1)
+		;
+	    for (; k < j && a[k] < z2; k=k+1)
+		;
+	    if (k - i > nmax) {
+	        nmax = k - i
+	        mode = a[(i+k)/2]
+	    }
+	} until (k >= j)
+
+	return (mode)
+end
+
diff --git a/noao/imred/ccdred/src/combine/generic/mkpkg b/noao/imred/ccdred/src/combine/generic/mkpkg
new file mode 100644
index 00000000..63695459
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/generic/mkpkg
@@ -0,0 +1,23 @@
+# Make CCDRED Package.
+
+$checkout libpkg.a ../../..
+$update   libpkg.a
+$checkin  libpkg.a ../../..
+$exit
+
+libpkg.a:
+	icaclip.x	../icombine.com ../icombine.h
+	icaverage.x	../icombine.com ../icombine.h <imhdr.h>
+	iccclip.x	../icombine.com ../icombine.h
+	icgdata.x	../icombine.com ../icombine.h <imhdr.h> <mach.h>
+	icgrow.x	../icombine.com ../icombine.h
+	icmedian.x	../icombine.com ../icombine.h
+	icmm.x		../icombine.com ../icombine.h
+	icombine.x	../icombine.com ../icombine.h <error.h> <syserr.h>\
+			<imhdr.h> <imset.h> <mach.h>
+	icpclip.x	../icombine.com ../icombine.h
+	icsclip.x	../icombine.com ../icombine.h
+	icsigma.x	../icombine.com ../icombine.h <imhdr.h>
+	icsort.x	
+	icstat.x	../icombine.com ../icombine.h <imhdr.h>
+	;
diff --git a/noao/imred/ccdred/src/combine/icaclip.gx b/noao/imred/ccdred/src/combine/icaclip.gx
new file mode 100644
index 00000000..bb592542
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icaclip.gx
@@ -0,0 +1,573 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		3	# Minimum number of images for this algorithm
+
+$for (sr)
+# IC_AAVSIGCLIP -- Reject pixels using an average sigma about the average
+# The average sigma is normalized by the expected poisson sigma.
+
+procedure ic_aavsigclip$t (d, m, n, scales, zeros, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	average[npts]		# Average
+$else
+PIXEL	average[npts]		# Average
+$endif
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+$if (datatype == sil)
+real	d1, low, high, sum, a, s, s1, r, one
+data	one /1.0/
+$else
+PIXEL	d1, low, high, sum, a, s, s1, r, one
+data	one /1$f/
+$endif
+pointer	sp, sums, resid, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (sums, npts, TY_REAL)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Since the unweighted average is computed here possibly skip combining
+	if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	# Compute the unweighted average with the high and low rejected and
+	# the poisson scaled average sigma.  There must be at least three
+	# pixels at each point to define the average and contributions to
+	# the mean sigma.  Corrections for differences in the image
+	# scale factors are selected by the doscale1 flag.
+
+	nin = n[1]
+	s = 0.
+	n2 = 0
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (n1 < 3)
+		next
+
+	    # Unweighted average with the high and low rejected
+	    low = Mem$t[d[1]+k]
+	    high = Mem$t[d[2]+k]
+	    if (low > high) {
+		d1 = low
+		low = high
+		high = d1
+	    }
+	    sum = 0.
+	    do j = 3, n1 {
+	       d1 = Mem$t[d[j]+k]
+	       if (d1 < low) {
+		   sum = sum + low
+		   low = d1
+		} else if (d1 > high) {
+		    sum = sum + high
+		    high = d1
+		} else
+		    sum = sum + d1
+	    }
+	    a = sum / (n1 - 2)
+	    sum = sum + low + high
+
+	    # Poisson scaled sigma accumulation
+	    if (doscale1) {
+		do j = 1, n1 {
+		    dp1 = d[j] + k
+		    mp1 = m[j] + k
+
+		    d1 = Mem$t[dp1]
+		    l = Memi[mp1]
+		    s1 = max (one, (a + zeros[l]) /  scales[l])
+		    s = s + (d1 - a) ** 2 / s1
+		}
+	    } else {
+		s1 = max (one, a)
+		do j = 1, n1
+		    s = s + (Mem$t[d[j]+k] - a) ** 2 / s1
+	    }
+	    n2 = n2 + n1
+
+	    # Save the average and sum for later.
+	    average[i] = a
+	    Memr[sums+k] = sum
+	}
+
+	# Here is the final sigma.
+	if (n2 > 1)
+	    s = sqrt (s / (n2 - 1))
+
+	# Reject pixels and compute the final average (if needed).
+	# There must be at least three pixels at each point for rejection.
+	# Iteratively scale the mean sigma and reject pixels
+	# Compact the data and keep track of the image IDs if needed.
+
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 <= max (2, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Mem$t[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Mem$t[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    a = average[i]
+	    sum = Memr[sums+k]
+
+	    repeat {
+		n2 = n1
+		if (s > 0.) {
+		    if (doscale1) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    mp1 = m[j] + k
+
+			    d1 = Mem$t[dp1]
+			    l = Memi[mp1]
+			    s1 = s * sqrt (max (one, (a+zeros[l]) /  scales[l]))
+			    r = (d1 - a) / s1
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs(r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    mp2 = m[n1] + k
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    } else {
+			s1 = s * sqrt (max (one, a))
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    d1 = Mem$t[dp1]
+			    r = (d1 - a) / s1
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs(r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[n1] + k
+					l = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = l
+				    }
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+		if (n1 > 1)
+		    a = sum / n1
+	    } until (n1 == n2 || n1 <= max (2, maxkeep))
+
+	    # If too many are rejected add some back in.
+	    # Pixels with equal residuals are added together.
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mem$t[dp1]
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Mem$t[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mem$t[dp1]
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Mem$t[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+		if (n1 > 1)
+		    a = sum / n1
+	    }
+
+	    # Save the average if needed.
+	    n[i] = n1
+	    if (!docombine) {
+		if (n1 > 0)
+		    average[i] = a
+		else
+		    average[i] = blank
+	    }
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_MAVSIGCLIP -- Reject pixels using an average sigma about the median
+# The average sigma is normalized by the expected poisson sigma.
+
+procedure ic_mavsigclip$t (d, m, n, scales, zeros, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	median[npts]		# Median
+$else
+PIXEL	median[npts]		# Median
+$endif
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+pointer	sp, resid, mp1, mp2
+$if (datatype == sil)
+real	med, low, high, r, s, s1, one
+data	one /1.0/
+$else
+PIXEL	med, low, high, r, s, s1, one
+data	one /1$f/
+$endif
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Compute the poisson scaled average sigma about the median.
+	# There must be at least three pixels at each point to define
+	# the mean sigma.  Corrections for differences in the image
+	# scale factors are selected by the doscale1 flag.
+
+	s = 0.
+	n2 = 0
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (n1 < 3) {
+		if (n1 == 0)
+		    median[i] = blank
+		else if (n1 == 1)
+		    median[i] = Mem$t[d[1]+k]
+		else {
+		    low = Mem$t[d[1]+k]
+		    high = Mem$t[d[2]+k]
+		    median[i] = (low + high) / 2.
+		}
+		next
+	    }
+
+	    # Median
+	    n3 = 1 + n1 / 2
+	    if (mod (n1, 2) == 0) {
+		low = Mem$t[d[n3-1]+k]
+		high = Mem$t[d[n3]+k]
+		med = (low + high) / 2.
+	    } else
+		med = Mem$t[d[n3]+k]
+
+	    # Poisson scaled sigma accumulation
+	    if (doscale1) {
+		do j = 1, n1 {
+		    l = Memi[m[j]+k]
+		    s1 = max (one, (med + zeros[l]) /  scales[l])
+		    s = s + (Mem$t[d[j]+k] - med) ** 2 / s1
+		}
+	    } else {
+		s1 = max (one, med)
+		do j = 1, n1
+		    s = s + (Mem$t[d[j]+k] - med) ** 2 / s1
+	    }
+	    n2 = n2 + n1
+
+	    # Save the median for later.
+	    median[i] = med
+	}
+
+	# Here is the final sigma.
+	if (n2 > 1)
+	    s = sqrt (s / (n2 - 1))
+	else
+	    return
+
+	# Compute individual sigmas and iteratively clip.
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 < max (3, maxkeep+1))
+		next
+	    nl = 1
+	    nh = n1
+	    med = median[i]
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 >= max (MINCLIP, maxkeep+1) && s > 0.) {
+		    if (doscale1) {
+			for (; nl <= n2; nl = nl + 1) {
+			    l = Memi[m[nl]+k]
+			    s1 = s * sqrt (max (one, (med+zeros[l])/scales[l]))
+			    r = (med - Mem$t[d[nl]+k]) / s1
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    l = Memi[m[nh]+k]
+			    s1 = s * sqrt (max (one, (med+zeros[l])/scales[l]))
+			    r = (Mem$t[d[nh]+k] - med) / s1
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    } else {
+			s1 = s * sqrt (max (one, med))
+			for (; nl <= n2; nl = nl + 1) {
+			    r = (med - Mem$t[d[nl]+k]) / s1
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    r = (Mem$t[d[nh]+k] - med) / s1
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    }
+
+		    # Recompute median
+		    if (n1 < n2) {
+			if (n1 > 0) {
+			    n3 = nl + n1 / 2
+			    if (mod (n1, 2) == 0) {
+				low = Mem$t[d[n3-1]+k]
+				high = Mem$t[d[n3]+k]
+				med = (low + high) / 2.
+			    } else
+				med = Mem$t[d[n3]+k]
+			} else
+			    med = blank
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    # If too many are rejected add some back in.
+	    # Pixels with equal residuals are added together.
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+
+		# Recompute median
+		if (n1 < n2) {
+		    if (n1 > 0) {
+			n3 = nl + n1 / 2
+			if (mod (n1, 2) == 0) {
+			    low = Mem$t[d[n3-1]+k]
+			    high = Mem$t[d[n3]+k]
+			    med = (low + high) / 2.
+			} else
+			    med = Mem$t[d[n3]+k]
+		    } else
+			med = blank
+		}
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mem$t[d[l]+k] = Mem$t[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mem$t[d[l]+k] = Mem$t[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median is computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/icaverage.gx b/noao/imred/ccdred/src/combine/icaverage.gx
new file mode 100644
index 00000000..c145bb33
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icaverage.gx
@@ -0,0 +1,93 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"../icombine.h"
+
+$for (sr)
+# IC_AVERAGE -- Compute the average image line.
+# Options include a weight average.
+
+procedure ic_average$t (d, m, n, wts, npts, average)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image ID pointers
+int	n[npts]			# Number of points
+real	wts[ARB]		# Weights
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	average[npts]		# Average (returned)
+$else
+PIXEL	average[npts]		# Average (returned)
+$endif
+
+int	i, j, k
+real	sumwt, wt
+$if (datatype == sil)
+real	sum
+$else
+PIXEL	sum
+$endif
+
+include	"../icombine.com"
+
+begin
+	# If no data has been excluded do the average without checking the
+	# number of points and using the fact that the weights are normalized.
+	# If all the data has been excluded set the average to the blank value.
+
+	if (dflag == D_ALL) {
+	    if (dowts) {
+		do i = 1, npts {
+		    k = i - 1
+		    wt = wts[Memi[m[1]+k]]
+		    sum = Mem$t[d[1]+k] * wt
+		    do j = 2, n[i] {
+			wt = wts[Memi[m[j]+k]]
+			sum = sum + Mem$t[d[j]+k] * wt
+		    }
+		    average[i] = sum
+		}
+	    } else {
+		do i = 1, npts {
+		    k = i - 1
+		    sum = Mem$t[d[1]+k]
+		    do j = 2, n[i]
+			sum = sum + Mem$t[d[j]+k]
+		    average[i] = sum / n[i]
+		}
+	    }
+	} else if (dflag == D_NONE) {
+	    do i = 1, npts
+		average[i] = blank
+	} else {
+	    if (dowts) {
+		do i = 1, npts {
+		    if (n[i] > 0) {
+			k = i - 1
+			wt = wts[Memi[m[1]+k]]
+			sum = Mem$t[d[1]+k] * wt
+			sumwt = wt
+			do j = 2, n[i] {
+			    wt = wts[Memi[m[j]+k]]
+			    sum = sum + Mem$t[d[j]+k] * wt
+			    sumwt = sumwt + wt
+			}
+			average[i] = sum / sumwt
+		    } else
+			average[i] = blank
+		}
+	    } else {
+		do i = 1, npts {
+		    if (n[i] > 0) {
+			k = i - 1
+			sum = Mem$t[d[1]+k]
+			do j = 2, n[i]
+			    sum = sum + Mem$t[d[j]+k]
+			average[i] = sum / n[i]
+		    } else
+			average[i] = blank
+		}
+	    }
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/iccclip.gx b/noao/imred/ccdred/src/combine/iccclip.gx
new file mode 100644
index 00000000..69df984c
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/iccclip.gx
@@ -0,0 +1,471 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		2	# Mininum number of images for algorithm
+
+$for (sr)
+# IC_ACCDCLIP -- Reject pixels using CCD noise parameters about the average
+
+procedure ic_accdclip$t (d, m, n, scales, zeros, nm, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+real	nm[3,nimages]		# Noise model parameters
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	average[npts]		# Average
+$else
+PIXEL	average[npts]		# Average
+$endif
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+$if (datatype == sil)
+real	d1, low, high, sum, a, s, r, zero
+data	zero /0.0/
+$else
+PIXEL	d1, low, high, sum, a, s, r, zero
+data	zero /0$f/
+$endif
+pointer	sp, resid, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are no pixels go on to the combining.  Since the unweighted
+	# average is computed here possibly skip the combining later.
+
+	# There must be at least max (1, nkeep) pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	} else if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# There must be at least two pixels for rejection.  The initial
+	# average is the low/high rejected average except in the case of
+	# just two pixels.  The rejections are iterated and the average
+	# is recomputed.  Corrections for scaling may be performed.
+	# Depending on other flags the image IDs may also need to be adjusted.
+
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 <= max (MINCLIP-1, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Mem$t[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Mem$t[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    repeat {
+		if (n1 == 2) {
+		    sum = Mem$t[d[1]+k]
+		    sum = sum + Mem$t[d[2]+k]
+		    a = sum / 2
+		} else {
+		    low = Mem$t[d[1]+k]
+		    high = Mem$t[d[2]+k]
+		    if (low > high) {
+			d1 = low
+			low = high
+			high = d1
+		    }
+		    sum = 0.
+		    do j = 3, n1 {
+		       d1 = Mem$t[d[j]+k]
+		       if (d1 < low) {
+			   sum = sum + low
+			   low = d1
+			} else if (d1 > high) {
+			    sum = sum + high
+			    high = d1
+			} else
+			    sum = sum + d1
+		    }
+		    a = sum / (n1 - 2)
+		    sum = sum + low + high
+		}
+		n2 = n1
+		if (doscale1) {
+		    for (j=1; j<=n1; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+
+			l = Memi[mp1]
+			s = scales[l]
+			d1 = max (zero, s * (a + zeros[l]))
+			s = sqrt (nm[1,l] + d1/nm[2,l] + (d1*nm[3,l])**2) / s
+
+			d1 = Mem$t[dp1]
+			r = (d1 - a) / s
+			if (r < -lsigma || r > hsigma) {
+			    Memr[resid+n1] = abs(r)
+			    if (j < n1) {
+				dp2 = d[n1] + k
+				Mem$t[dp1] = Mem$t[dp2]
+				Mem$t[dp2] = d1
+				mp2 = m[n1] + k
+				Memi[mp1] = Memi[mp2]
+				Memi[mp2] = l
+				j = j - 1
+			    }
+			    sum = sum - d1
+			    n1 = n1 - 1
+			}
+		    }
+		} else {
+		    if (!keepids) {
+			s = max (zero, a)
+			s = sqrt (nm[1,1] + s/nm[2,1] + (s*nm[3,1])**2)
+		    }
+		    for (j=1; j<=n1; j=j+1) {
+			if (keepids) {
+			    l = Memi[m[j]+k]
+			    s = max (zero, a)
+			    s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			}
+			dp1 = d[j] + k
+			d1 = Mem$t[dp1]
+			r = (d1 - a) / s
+			if (r < -lsigma || r > hsigma) {
+			    Memr[resid+n1] = abs(r)
+			    if (j < n1) {
+				dp2 = d[n1] + k
+				Mem$t[dp1] = Mem$t[dp2]
+				Mem$t[dp2] = d1
+				if (keepids) {
+				    mp1 = m[j] + k
+				    mp2 = m[n1] + k
+				    l = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				}
+				j = j - 1
+			    }
+			    sum = sum - d1
+			    n1 = n1 - 1
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mem$t[dp1]
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Mem$t[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mem$t[dp1]
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Mem$t[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+	    }
+
+	    n[i] = n1
+	    if (!docombine)
+		if (n1 > 0)
+		    average[i] = sum / n1
+		else
+		    average[i] = blank
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_CCDCLIP -- Reject pixels using CCD noise parameters about the median
+
+procedure ic_mccdclip$t (d, m, n, scales, zeros, nm, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+real	nm[3,nimages]		# Noise model
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	median[npts]		# Median
+$else
+PIXEL	median[npts]		# Median
+$endif
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+real	r, s
+pointer	sp, resid, mp1, mp2
+$if (datatype == sil)
+real	med, zero
+data	zero /0.0/
+$else
+PIXEL	med, zero
+data	zero /0$f/
+$endif
+
+include	"../icombine.com"
+
+begin
+	# There must be at least max (MINCLIP, nkeep+1) pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Compute median and sigma and iteratively clip.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    nl = 1
+	    nh = n1
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 == 0)
+		    med = blank
+		else if (mod (n1, 2) == 0) {
+		    med = Mem$t[d[n3-1]+k]
+		    med = (med + Mem$t[d[n3]+k]) / 2.
+		} else
+		    med = Mem$t[d[n3]+k]
+
+		if (n1 >= max (MINCLIP, maxkeep+1)) {
+		    if (doscale1) {
+			for (; nl <= n2; nl = nl + 1) {
+			    l = Memi[m[nl]+k]
+			    s = scales[l]
+			    r = max (zero, s * (med + zeros[l]))
+			    s = sqrt (nm[1,l] + r/nm[2,l] + (r*nm[3,l])**2) / s
+			    r = (med - Mem$t[d[nl]+k]) / s
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    l = Memi[m[nh]+k]
+			    s = scales[l]
+			    r = max (zero, s * (med + zeros[l]))
+			    s = sqrt (nm[1,l] + r/nm[2,l] + (r*nm[3,l])**2) / s
+			    r = (Mem$t[d[nh]+k] - med) / s
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    } else {
+			if (!keepids) {
+			    s = max (zero, med)
+			    s = sqrt (nm[1,1] + s/nm[2,1] + (s*nm[3,1])**2)
+			}
+			for (; nl <= n2; nl = nl + 1) {
+			    if (keepids) {
+				l = Memi[m[nl]+k]
+				s = max (zero, med)
+				s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			    }
+			    r = (med - Mem$t[d[nl]+k]) / s
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    if (keepids) {
+				l = Memi[m[nh]+k]
+				s = max (zero, med)
+				s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			    }
+			    r = (Mem$t[d[nh]+k] -  med) / s
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mem$t[d[l]+k] = Mem$t[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mem$t[d[l]+k] = Mem$t[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median is computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/icgdata.gx b/noao/imred/ccdred/src/combine/icgdata.gx
new file mode 100644
index 00000000..41cf5810
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icgdata.gx
@@ -0,0 +1,233 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	<mach.h>
+include	"../icombine.h"
+
+$for (sr)
+# IC_GDATA -- Get line of image and mask data and apply threshold and scaling.
+# Entirely empty lines are excluded.  The data are compacted within the
+# input data buffers.  If it is required, the connection to the original
+# image index is keeped in the returned m data pointers.
+
+procedure ic_gdata$t (in, out, dbuf, d, id, n, m, lflag, offsets, scales,
+	zeros, nimages, npts, v1, v2)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+pointer	dbuf[nimages]		# Data buffers for nonaligned images
+pointer	d[nimages]		# Data pointers
+pointer	id[nimages]		# ID pointers
+int	n[npts]			# Number of good pixels
+pointer	m[nimages]		# Mask pointers
+int	lflag[nimages]		# Empty mask flags
+int	offsets[nimages,ARB]	# Image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero offset factors
+int	nimages			# Number of input images
+int	npts			# NUmber of output points per line
+long	v1[ARB], v2[ARB]	# Line vectors
+
+int	i, j, k, l, ndim, nused
+real	a, b
+pointer	buf, dp, ip, mp, imgnl$t()
+
+include	"../icombine.com"
+
+begin
+	# Get masks and return if there is no data
+	call ic_mget (in, out, offsets, v1, v2, m, lflag, nimages)
+	if (dflag == D_NONE)
+	    return
+
+	# Get data and fill data buffers.  Correct for offsets if needed.
+	ndim = IM_NDIM(out[1])
+	do i = 1, nimages {
+	    if (lflag[i] == D_NONE)
+		next
+	    if (aligned) {
+		call amovl (v1, v2, IM_MAXDIM)
+		if (project)
+		    v2[ndim+1] = i
+		j = imgnl$t (in[i], d[i], v2)
+	    } else {
+		v2[1] = v1[1]
+		do j = 2, ndim
+		    v2[j] = v1[j] - offsets[i,j]
+		if (project)
+		    v2[ndim+1] = i
+		j = imgnl$t (in[i], buf, v2)
+		call amov$t (Mem$t[buf], Mem$t[dbuf[i]+offsets[i,1]],
+		    IM_LEN(in[i],1))
+		d[i] = dbuf[i]
+	    }
+	}
+
+	# Apply threshold if needed
+	if (dothresh) {
+	    do i = 1, nimages {
+		dp = d[i]
+		if (lflag[i] == D_ALL) {
+		    do j = 1, npts {
+			a = Mem$t[dp]
+			if (a < lthresh || a > hthresh) {
+			    Memi[m[i]+j-1] = 1
+			    lflag[i] = D_MIX
+			    dflag = D_MIX
+			}
+			dp = dp + 1
+		    }
+		} else if (lflag[i] == D_MIX) {
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    a = Mem$t[dp]
+			    if (a < lthresh || a > hthresh) {
+				Memi[m[i]+j-1] = 1
+				dflag = D_MIX
+			    }
+			}
+			dp = dp + 1
+			mp = mp + 1
+		    }
+		}
+
+		# Check for completely empty lines
+		if (lflag[i] == D_MIX) {
+		    lflag[i] = D_NONE
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    lflag[i] = D_MIX
+			    break
+			}
+			mp = mp + 1
+		    }
+		}
+	    }
+	}
+
+	# Apply scaling (avoiding masked pixels which might overflow?)
+	if (doscale) {
+	    if (dflag == D_ALL) {
+		do i = 1, nimages {
+		    dp = d[i]
+		    a = scales[i]
+		    b = -zeros[i]
+		    do j = 1, npts {
+			Mem$t[dp] = Mem$t[dp] / a + b
+			dp = dp + 1
+		    }
+		}
+	    } else if (dflag == D_MIX) {
+		do i = 1, nimages {
+		    dp = d[i]
+		    a = scales[i]
+		    b = -zeros[i]
+		    if (lflag[i] == D_ALL) {
+			do j = 1, npts {
+			    Mem$t[dp] = Mem$t[dp] / a + b
+			    dp = dp + 1
+			}
+		    } else if (lflag[i] == D_MIX) {
+			mp = m[i]
+			do j = 1, npts {
+			    if (Memi[mp] == 0)
+				Mem$t[dp] = Mem$t[dp] / a + b
+			    dp = dp + 1
+			    mp = mp + 1
+			}
+		    }
+		}
+	    }
+	}
+
+	# Sort pointers to exclude unused images.
+	# Use the lflag array to keep track of the image index.
+
+	if (dflag == D_ALL)
+	    nused = nimages
+	else {
+	    nused = 0
+	    do i = 1, nimages
+		if (lflag[i] != D_NONE) {
+		    nused = nused + 1
+		    d[nused] = d[i]
+		    m[nused] = m[i]
+		    lflag[nused] = i
+		}
+	    if (nused == 0)
+		dflag = D_NONE
+	}
+
+	# Compact data to remove bad pixels
+	# Keep track of the image indices if needed
+	# If growing mark the end of the included image indices with zero
+
+	if (dflag == D_ALL) {
+	    call amovki (nused, n, npts)
+	    if (keepids)
+		do i = 1, nimages
+		    call amovki (i, Memi[id[i]], npts)
+	} else if (dflag == D_NONE)
+	    call aclri (n, npts)
+	else {
+	    call aclri (n, npts)
+	    if (keepids) {
+		do i = 1, nused {
+		    l = lflag[i]
+		    dp = d[i]
+		    ip = id[i]
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    n[j] = n[j] + 1
+			    k = n[j]
+			    if (k < i) {
+				Mem$t[d[k]+j-1] = Mem$t[dp]
+				Memi[id[k]+j-1] = l
+			    } else
+				Memi[ip] = l
+			}
+			dp = dp + 1
+			ip = ip + 1
+			mp = mp + 1
+		    }
+		}
+		if (grow > 0) {
+		    do j = 1, npts {
+			do i = n[j]+1, nimages
+			    Memi[id[i]+j-1] = 0
+		    }
+		}
+	    } else {
+		do i = 1, nused {
+		    dp = d[i]
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    n[j] = n[j] + 1
+			    k = n[j]
+			    if (k < i)
+				Mem$t[d[k]+j-1] = Mem$t[dp]
+			}
+			dp = dp + 1
+			mp = mp + 1
+		    }
+		}
+	    }
+	}
+
+	# Sort the pixels and IDs if needed
+	if (mclip) {
+	    call malloc (dp, nimages, TY_PIXEL)
+	    if (keepids) {
+		call malloc (ip, nimages, TY_INT)
+		call ic_2sort$t (d, Mem$t[dp], id, Memi[ip], n, npts)
+		call mfree (ip, TY_INT)
+	    } else
+		call ic_sort$t (d, Mem$t[dp], n, npts)
+	    call mfree (dp, TY_PIXEL)
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/icgrow.gx b/noao/imred/ccdred/src/combine/icgrow.gx
new file mode 100644
index 00000000..e3cf6228
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icgrow.gx
@@ -0,0 +1,81 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+$for (sr)
+# IC_GROW --  Reject neigbors of rejected pixels.
+# The rejected pixels are marked by having nonzero ids beyond the number
+# of included pixels.  The pixels rejected here are given zero ids
+# to avoid growing of the pixels rejected here.  The unweighted average
+# can be updated but any rejected pixels requires the median to be
+# recomputed.  When the number of pixels at a grow point reaches nkeep 
+# no further pixels are rejected.  Note that the rejection order is not
+# based on the magnitude of the residuals and so a grow from a weakly
+# rejected image pixel may take precedence over a grow from a strongly
+# rejected image pixel.
+
+procedure ic_grow$t (d, m, n, nimages, npts, average)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image id pointers
+int	n[npts]			# Number of good pixels
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	average[npts]		# Average
+$else
+PIXEL	average[npts]		# Average
+$endif
+
+int	i1, i2, j1, j2, k1, k2, l, is, ie, n2, maxkeep
+pointer	mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_NONE)
+	    return
+
+	do i1 = 1, npts {
+	    k1 = i1 - 1
+	    is = max (1, i1 - grow)
+	    ie = min (npts, i1 + grow)
+	    do j1 = n[i1]+1, nimages {
+		l = Memi[m[j1]+k1]
+		if (l == 0)
+		    next
+		if (combine == MEDIAN)
+		    docombine = true
+
+		do i2 = is, ie {
+		    if (i2 == i1)
+			next
+		    k2 = i2 - 1
+		    n2 = n[i2]
+		    if (nkeep < 0)
+			maxkeep = max (0, n2 + nkeep)
+		    else
+			maxkeep = min (n2, nkeep)
+		    if (n2 <= maxkeep)
+			next
+		    do j2 = 1, n2 {
+			mp1 = m[j2] + k2
+			if (Memi[mp1] == l) {
+			    if (!docombine && n2 > 1)
+				average[i2] =
+				    (n2*average[i2] - Mem$t[d[j2]+k2]) / (n2-1)
+			    mp2 = m[n2] + k2
+			    if (j2 < n2) {
+				Mem$t[d[j2]+k2] = Mem$t[d[n2]+k2]
+				Memi[mp1] = Memi[mp2]
+			    }
+			    Memi[mp2] = 0
+			    n[i2] = n2 - 1
+			    break
+			}
+		    }
+		}
+	    }
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/icimstack.x b/noao/imred/ccdred/src/combine/icimstack.x
new file mode 100644
index 00000000..2a19751d
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icimstack.x
@@ -0,0 +1,125 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<error.h>
+include	<imhdr.h>
+
+
+# IC_IMSTACK -- Stack images into a single image of higher dimension.
+
+procedure ic_imstack (images, nimages, output)
+
+char	images[SZ_FNAME-1, nimages]	#I Input images
+int	nimages				#I Number of images
+char	output				#I Name of output image
+
+int	i, j, npix
+long	line_in[IM_MAXDIM], line_out[IM_MAXDIM]
+pointer	sp, key, in, out, buf_in, buf_out, ptr
+
+int	imgnls(), imgnli(), imgnll(), imgnlr(), imgnld(), imgnlx()
+int	impnls(), impnli(), impnll(), impnlr(), impnld(), impnlx()
+pointer	immap()
+errchk	immap
+
+begin
+	call smark (sp)
+	call salloc (key, SZ_FNAME, TY_CHAR)
+
+	iferr {
+	    # Add each input image to the output image.
+	    out = NULL
+	    do i = 1, nimages {
+		in = NULL
+		ptr = immap (images[1,i], READ_ONLY, 0)
+		in = ptr
+
+		# For the first input image map the output image as a copy
+		# and increment the dimension.  Set the output line counter.
+
+		if (i == 1) {
+		    ptr = immap (output, NEW_COPY, in)
+		    out = ptr
+		    IM_NDIM(out) = IM_NDIM(out) + 1
+		    IM_LEN(out, IM_NDIM(out)) = nimages
+		    npix = IM_LEN(out, 1)
+		    call amovkl (long(1), line_out, IM_MAXDIM)
+		}
+
+		# Check next input image for consistency with the output image.
+		if (IM_NDIM(in) != IM_NDIM(out) - 1)
+		    call error (0, "Input images not consistent")
+		do j = 1, IM_NDIM(in) {
+		    if (IM_LEN(in, j) != IM_LEN(out, j))
+			call error (0, "Input images not consistent")
+		}
+
+		call sprintf (Memc[key], SZ_FNAME, "stck%04d")
+		    call pargi (i)
+		call imastr (out, Memc[key], images[1,i])
+
+		# Copy the input lines from the image to the next lines of
+		# the output image.  Switch on the output data type to optimize
+		# IMIO.
+
+		call amovkl (long(1), line_in, IM_MAXDIM)
+		switch (IM_PIXTYPE (out)) {
+		case TY_SHORT:
+		    while (imgnls (in, buf_in, line_in) != EOF) {
+			if (impnls (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovs (Mems[buf_in], Mems[buf_out], npix)
+		    }
+		case TY_INT:
+		    while (imgnli (in, buf_in, line_in) != EOF) {
+			if (impnli (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovi (Memi[buf_in], Memi[buf_out], npix)
+		    }
+		case TY_USHORT, TY_LONG:
+		    while (imgnll (in, buf_in, line_in) != EOF) {
+			if (impnll (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovl (Meml[buf_in], Meml[buf_out], npix)
+		    }
+		case TY_REAL:
+		    while (imgnlr (in, buf_in, line_in) != EOF) {
+			if (impnlr (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovr (Memr[buf_in], Memr[buf_out], npix)
+		    }
+		case TY_DOUBLE:
+		    while (imgnld (in, buf_in, line_in) != EOF) {
+			if (impnld (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovd (Memd[buf_in], Memd[buf_out], npix)
+		    }
+		case TY_COMPLEX:
+		    while (imgnlx (in, buf_in, line_in) != EOF) {
+			if (impnlx (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovx (Memx[buf_in], Memx[buf_out], npix)
+		    }
+		default:
+		    while (imgnlr (in, buf_in, line_in) != EOF) {
+			if (impnlr (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovr (Memr[buf_in], Memr[buf_out], npix)
+		    }
+		}
+		call imunmap (in)
+	    }
+	} then {
+	    if (out != NULL) {
+		call imunmap (out)
+		call imdelete (out)
+	    }
+	    if (in != NULL)
+		call imunmap (in)
+	    call sfree (sp)
+	    call erract (EA_ERROR)
+	}
+
+	# Finish up.
+	call imunmap (out)
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/combine/iclog.x b/noao/imred/ccdred/src/combine/iclog.x
new file mode 100644
index 00000000..82135866
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/iclog.x
@@ -0,0 +1,378 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	<imset.h>
+include	<mach.h>
+include	"icombine.h"
+include	"icmask.h"
+
+# IC_LOG -- Output log information is a log file has been specfied.
+
+procedure ic_log (in, out, ncombine, exptime, sname, zname, wname,
+	mode, median, mean, scales, zeros, wts, offsets, nimages,
+	dozero, nout, expname, exposure)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+int	ncombine[nimages]	# Number of previous combined images
+real	exptime[nimages]	# Exposure times
+char	sname[ARB]		# Scale name
+char	zname[ARB]		# Zero name
+char	wname[ARB]		# Weight name
+real	mode[nimages]		# Modes
+real	median[nimages]		# Medians
+real	mean[nimages]		# Means
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero or sky levels
+real	wts[nimages]		# Weights
+int	offsets[nimages,ARB]	# Image offsets
+int	nimages			# Number of images
+bool	dozero			# Zero flag
+int	nout			# Number of images combined in output
+char	expname[ARB]		# Exposure name
+real	exposure		# Output exposure
+
+int	i, j, stack, ctor()
+real	rval, imgetr()
+long	clktime()
+bool	prncombine, prexptime, prmode, prmedian, prmean, prmask
+bool	prrdn, prgain, prsn
+pointer	sp, fname, key
+errchk	imgetr
+
+include	"icombine.com"
+
+begin
+	if (logfd == NULL)
+	    return
+
+	call smark (sp)
+	call salloc (fname, SZ_LINE, TY_CHAR)
+
+	stack = NO
+	if (project) {
+	    ifnoerr (call imgstr (in[1], "stck0001", Memc[fname], SZ_LINE))
+	        stack = YES
+	}
+	if (stack == YES)
+	    call salloc (key, SZ_FNAME, TY_CHAR)
+
+	# Time stamp the log and print parameter information.
+
+	call cnvdate (clktime(0), Memc[fname], SZ_LINE)
+	call fprintf (logfd, "\n%s: IMCOMBINE\n")
+	    call pargstr (Memc[fname])
+	switch (combine) {
+	case  AVERAGE:
+	    call fprintf (logfd, "  combine = average, ")
+	case  MEDIAN:
+	    call fprintf (logfd, "  combine = median, ")
+	}
+	call fprintf (logfd, "scale = %s, zero = %s, weight = %s\n")
+	    call pargstr (sname)
+	    call pargstr (zname)
+	    call pargstr (wname)
+
+	switch (reject) {
+	case MINMAX:
+	    call fprintf (logfd, "  reject = minmax, nlow = %d, nhigh = %d\n")
+		call pargi (nint (flow * nimages))
+		call pargi (nint (fhigh * nimages))
+	case CCDCLIP:
+	    call fprintf (logfd, "  reject = ccdclip, mclip = %b, nkeep = %d\n")
+		call pargb (mclip)
+		call pargi (nkeep)
+	    call fprintf (logfd,
+	    "  rdnoise = %s, gain = %s, snoise = %s, sigma = %g, hsigma = %g\n")
+		call pargstr (Memc[rdnoise])
+		call pargstr (Memc[gain])
+		call pargstr (Memc[snoise])
+		call pargr (lsigma)
+		call pargr (hsigma)
+	case CRREJECT:
+	    call fprintf (logfd,
+		"  reject = crreject, mclip = %b, nkeep = %d\n")
+		call pargb (mclip)
+		call pargi (nkeep)
+	    call fprintf (logfd,
+		"  rdnoise = %s, gain = %s, snoise = %s, hsigma = %g\n")
+		call pargstr (Memc[rdnoise])
+		call pargstr (Memc[gain])
+		call pargstr (Memc[snoise])
+		call pargr (hsigma)
+	case PCLIP:
+	    call fprintf (logfd, "  reject = pclip, nkeep = %d\n")
+		call pargi (nkeep)
+	    call fprintf (logfd, "  pclip = %g, lsigma = %g, hsigma = %g\n")
+		call pargr (pclip)
+		call pargr (lsigma)
+		call pargr (hsigma)
+	case SIGCLIP:
+	    call fprintf (logfd, "  reject = sigclip, mclip = %b, nkeep = %d\n")
+		call pargb (mclip)
+		call pargi (nkeep)
+	    call fprintf (logfd, "  lsigma = %g, hsigma = %g\n")
+		call pargr (lsigma)
+		call pargr (hsigma)
+	case AVSIGCLIP:
+	    call fprintf (logfd,
+		"  reject = avsigclip, mclip = %b, nkeep = %d\n")
+		call pargb (mclip)
+		call pargi (nkeep)
+	    call fprintf (logfd, "  lsigma = %g, hsigma = %g\n")
+		call pargr (lsigma)
+		call pargr (hsigma)
+	}
+	if (reject != NONE && grow > 0) {
+	    call fprintf (logfd, "  grow = %d\n")
+		call pargi (grow)
+	}
+	if (dothresh) {
+	    if (lthresh > -MAX_REAL && hthresh < MAX_REAL) {
+		call fprintf (logfd, "  lthreshold = %g, hthreshold = %g\n")
+		    call pargr (lthresh)
+		    call pargr (hthresh)
+	    } else if (lthresh > -MAX_REAL) {
+		call fprintf (logfd, "  lthreshold = %g\n")
+		    call pargr (lthresh)
+	    } else {
+		call fprintf (logfd, "  hthreshold = %g\n")
+		    call pargr (hthresh)
+	    }
+	}
+	call fprintf (logfd, "  blank = %g\n")
+	    call pargr (blank)
+	call clgstr ("statsec", Memc[fname], SZ_LINE)
+	if (Memc[fname] != EOS) {
+	    call fprintf (logfd, "  statsec = %s\n")
+		call pargstr (Memc[fname])
+	}
+
+	if (ICM_TYPE(icm) != M_NONE) {
+	    switch (ICM_TYPE(icm)) {
+	    case M_BOOLEAN, M_GOODVAL:
+		call fprintf (logfd, "  masktype = goodval, maskval = %d\n")
+		    call pargi (ICM_VALUE(icm))
+	    case M_BADVAL:
+		call fprintf (logfd, "  masktype = badval, maskval = %d\n")
+		    call pargi (ICM_VALUE(icm))
+	    case M_GOODBITS:
+		call fprintf (logfd, "  masktype = goodbits, maskval = %d\n")
+		    call pargi (ICM_VALUE(icm))
+	    case M_BADBITS:
+		call fprintf (logfd, "  masktype = badbits, maskval = %d\n")
+		    call pargi (ICM_VALUE(icm))
+	    }
+	}
+
+	# Print information pertaining to individual images as a set of
+	# columns with the image name being the first column.  Determine
+	# what information is relevant and print the appropriate header.
+
+	prncombine = false
+	prexptime = false
+	prmode = false
+	prmedian = false
+	prmean = false
+	prmask = false
+	prrdn = false
+	prgain = false
+	prsn = false
+	do i = 1, nimages {
+	    if (ncombine[i] != ncombine[1])
+		prncombine = true
+	    if (exptime[i] != exptime[1])
+		prexptime = true
+	    if (mode[i] != mode[1])
+		prmode = true
+	    if (median[i] != median[1])
+		prmedian = true
+	    if (mean[i] != mean[1])
+		prmean = true
+	    if (ICM_TYPE(icm) != M_NONE && Memi[ICM_PMS(icm)+i-1] != NULL)
+		prmask = true
+	    if (reject == CCDCLIP || reject == CRREJECT) {
+		j = 1
+		if (ctor (Memc[rdnoise], j, rval) == 0)
+		    prrdn = true
+		j = 1
+		if (ctor (Memc[gain], j, rval) == 0)
+		    prgain = true
+		j = 1
+		if (ctor (Memc[snoise], j, rval) == 0)
+		    prsn = true
+	    }
+	}
+
+	call fprintf (logfd, "  %20s ")
+	    call pargstr ("Images")
+	if (prncombine) {
+	    call fprintf (logfd, " %6s")
+		call pargstr ("N")
+	}
+	if (prexptime) {
+	    call fprintf (logfd, " %6s")
+		call pargstr ("Exp")
+	}
+	if (prmode) {
+	    call fprintf (logfd, " %7s")
+		call pargstr ("Mode")
+	}
+	if (prmedian) {
+	    call fprintf (logfd, " %7s")
+		call pargstr ("Median")
+	}
+	if (prmean) {
+	    call fprintf (logfd, " %7s")
+		call pargstr ("Mean")
+	}
+	if (prrdn) {
+	    call fprintf (logfd, " %7s")
+		call pargstr ("Rdnoise")
+	}
+	if (prgain) {
+	    call fprintf (logfd, " %6s")
+		call pargstr ("Gain")
+	}
+	if (prsn) {
+	    call fprintf (logfd, " %6s")
+		call pargstr ("Snoise")
+	}
+	if (doscale) {
+	    call fprintf (logfd, " %6s")
+		call pargstr ("Scale")
+	}
+	if (dozero) {
+	    call fprintf (logfd, " %7s")
+		call pargstr ("Zero")
+	}
+	if (dowts) {
+	    call fprintf (logfd, " %6s")
+		call pargstr ("Weight")
+	}
+	if (!aligned) {
+	    call fprintf (logfd, " %9s")
+		call pargstr ("Offsets")
+	}
+	if (prmask) {
+	    call fprintf (logfd, " %s")
+		call pargstr ("Maskfile")
+	}
+	call fprintf (logfd, "\n")
+
+	do i = 1, nimages {
+	    if (stack == YES) {
+		call sprintf (Memc[key], SZ_FNAME, "stck%04d")
+		    call pargi (i)
+		ifnoerr (call imgstr (in[i], Memc[key], Memc[fname], SZ_LINE)) {
+		    call fprintf (logfd, "  %21s")
+			call pargstr (Memc[fname])
+		} else {
+		    call imstats (in[i], IM_IMAGENAME, Memc[fname], SZ_LINE)
+		    call fprintf (logfd, "  %16s[%3d]")
+			call pargstr (Memc[fname])
+			call pargi (i)
+		}
+	    } else if (project) {
+		call imstats (in[i], IM_IMAGENAME, Memc[fname], SZ_LINE)
+		call fprintf (logfd, "  %16s[%3d]")
+		    call pargstr (Memc[fname])
+		    call pargi (i)
+	    } else  {
+		call imstats (in[i], IM_IMAGENAME, Memc[fname], SZ_LINE)
+		call fprintf (logfd, "  %21s")
+		    call pargstr (Memc[fname])
+	    }
+	    if (prncombine) {
+		call fprintf (logfd, " %6d")
+		    call pargi (ncombine[i])
+	    }
+	    if (prexptime) {
+		call fprintf (logfd, " %6.1f")
+		    call pargr (exptime[i])
+	    }
+	    if (prmode) {
+		call fprintf (logfd, " %7.5g")
+		    call pargr (mode[i])
+	    }
+	    if (prmedian) {
+		call fprintf (logfd, " %7.5g")
+		    call pargr (median[i])
+	    }
+	    if (prmean) {
+		call fprintf (logfd, " %7.5g")
+		    call pargr (mean[i])
+	    }
+	    if (prrdn) {
+		rval = imgetr (in[i], Memc[rdnoise])
+		call fprintf (logfd, " %7g")
+		    call pargr (rval)
+	    }
+	    if (prgain) {
+		rval = imgetr (in[i], Memc[gain])
+		call fprintf (logfd, " %6g")
+		    call pargr (rval)
+	    }
+	    if (prsn) {
+		rval = imgetr (in[i], Memc[snoise])
+		call fprintf (logfd, " %6g")
+		    call pargr (rval)
+	    }
+	    if (doscale) {
+		call fprintf (logfd, " %6.3f")
+		    call pargr (1./scales[i])
+	    }
+	    if (dozero) {
+		call fprintf (logfd, " %7.5g")
+		    call pargr (-zeros[i])
+	    }
+	    if (dowts) {
+		call fprintf (logfd, " %6.3f")
+		    call pargr (wts[i])
+	    }
+	    if (!aligned) {
+		if (IM_NDIM(out[1]) == 1) {
+		    call fprintf (logfd, " %9d")
+			call pargi (offsets[i,1])
+		} else {
+		    do  j = 1, IM_NDIM(out[1]) {
+			call fprintf (logfd, " %4d")
+			    call pargi (offsets[i,j])
+		    }
+		}
+	    }
+	    if (prmask && Memi[ICM_PMS(icm)+i-1] != NULL) {
+		call imgstr (in[i], "BPM", Memc[fname], SZ_LINE)
+		call fprintf (logfd, " %s")
+		    call pargstr (Memc[fname])
+	    }
+	    call fprintf (logfd, "\n")
+	}
+
+	# Log information about the output images.
+ 	call imstats (out[1], IM_IMAGENAME, Memc[fname], SZ_LINE)
+	call fprintf (logfd, "\n  Output image = %s, ncombine = %d")
+	    call pargstr (Memc[fname])
+	    call pargi (nout)
+	if (expname[1] != EOS) {
+	    call fprintf (logfd, ", %s = %g")
+		call pargstr (expname)
+		call pargr (exposure)
+	}
+	call fprintf (logfd, "\n")
+
+	if (out[2] != NULL) {
+	    call imstats (out[2], IM_IMAGENAME, Memc[fname], SZ_LINE)
+	    call fprintf (logfd, "  Pixel list image = %s\n")
+		call pargstr (Memc[fname])
+	}
+
+	if (out[3] != NULL) {
+	    call imstats (out[3], IM_IMAGENAME, Memc[fname], SZ_LINE)
+	    call fprintf (logfd, "  Sigma image = %s\n")
+		call pargstr (Memc[fname])
+	}
+
+	call flush (logfd)
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/combine/icmask.com b/noao/imred/ccdred/src/combine/icmask.com
new file mode 100644
index 00000000..baba6f6a
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icmask.com
@@ -0,0 +1,8 @@
+# IMCMASK -- Common for IMCOMBINE mask interface.
+
+int	mtype		# Mask type
+int	mvalue		# Mask value
+pointer	bufs		# Pointer to data line buffers
+pointer	pms		# Pointer to array of PMIO pointers
+
+common	/imcmask/ mtype, mvalue, bufs, pms
diff --git a/noao/imred/ccdred/src/combine/icmask.h b/noao/imred/ccdred/src/combine/icmask.h
new file mode 100644
index 00000000..b2d30530
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icmask.h
@@ -0,0 +1,7 @@
+# ICMASK -- Data structure for IMCOMBINE mask interface.
+
+define	ICM_LEN		4		# Structure length
+define	ICM_TYPE	Memi[$1]	# Mask type
+define	ICM_VALUE	Memi[$1+1]	# Mask value
+define	ICM_BUFS	Memi[$1+2]	# Pointer to data line buffers
+define	ICM_PMS		Memi[$1+3]	# Pointer to array of PMIO pointers
diff --git a/noao/imred/ccdred/src/combine/icmask.x b/noao/imred/ccdred/src/combine/icmask.x
new file mode 100644
index 00000000..ba448b68
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icmask.x
@@ -0,0 +1,354 @@
+include	<imhdr.h>
+include	<pmset.h>
+include	"icombine.h"
+include	"icmask.h"
+
+# IC_MASK   -- ICOMBINE mask interface
+#
+# IC_MOPEN  -- Open masks
+# IC_MCLOSE -- Close the mask interface
+# IC_MGET   -- Get lines of mask pixels for all the images
+# IC_MGET1  -- Get a line of mask pixels for the specified image
+
+
+# IC_MOPEN -- Open masks.
+# Parse and interpret the mask selection parameters.
+
+procedure ic_mopen (in, out, nimages)
+
+pointer	in[nimages]		#I Input images
+pointer	out[ARB]		#I Output images
+int	nimages			#I Number of images
+
+int	mtype			# Mask type
+int	mvalue			# Mask value
+pointer	bufs			# Pointer to data line buffers
+pointer	pms			# Pointer to array of PMIO pointers
+
+int	i, npix, npms, clgwrd()
+real	clgetr()
+pointer	sp, fname, title, pm, pm_open()
+bool	invert, pm_empty()
+errchk	calloc, pm_open, pm_loadf
+
+include "icombine.com"
+
+begin
+	icm = NULL
+	if (IM_NDIM(out[1]) == 0)
+	    return
+
+	call smark (sp)
+	call salloc (fname, SZ_FNAME, TY_CHAR)
+	call salloc (title, SZ_FNAME, TY_CHAR)
+
+	# Determine the mask parameters and allocate memory.
+	# The mask buffers are initialize to all excluded so that
+	# output points outside the input data are always excluded
+	# and don't need to be set on a line-by-line basis.
+
+	mtype = clgwrd ("masktype", Memc[title], SZ_FNAME, MASKTYPES)
+	mvalue = clgetr ("maskvalue")
+	npix = IM_LEN(out[1],1)
+	call calloc (pms, nimages, TY_POINTER)
+	call calloc (bufs, nimages, TY_POINTER)
+	do i = 1, nimages {
+	    call malloc (Memi[bufs+i-1], npix, TY_INT)
+	    call amovki (1, Memi[Memi[bufs+i-1]], npix)
+	}
+
+	# Check for special cases.  The BOOLEAN type is used when only
+	# zero and nonzero are significant; i.e. the actual mask values are
+	# not important.  The invert flag is used to indicate that
+	# empty masks are all bad rather the all good.
+
+	if (mtype == 0)
+	    mtype = M_NONE
+	if (mtype == M_BADBITS && mvalue == 0) 
+	    mtype = M_NONE
+	if (mvalue == 0 && (mtype == M_GOODVAL || mtype == M_GOODBITS))
+	    mtype = M_BOOLEAN
+	if ((mtype == M_BADVAL && mvalue == 0) ||
+	    (mtype == M_GOODVAL && mvalue != 0) ||
+	    (mtype == M_GOODBITS && mvalue == 0))
+	    invert = true 
+	else
+	    invert = false 
+
+	# If mask images are to be used, get the mask name from the image
+	# header and open it saving the descriptor in the pms array.
+	# Empty masks (all good) are treated as if there was no mask image.
+
+	npms = 0
+	do i = 1, nimages {
+	    if (mtype != M_NONE) {
+		ifnoerr (call imgstr (in[i], "BPM", Memc[fname], SZ_FNAME)) {
+		    pm = pm_open (NULL)
+		    call pm_loadf (pm, Memc[fname], Memc[title], SZ_FNAME)
+		    call pm_seti (pm, P_REFIM, in[i])
+		    if (pm_empty (pm) && !invert)
+			call pm_close (pm)
+		    else {
+			if (project) {
+			    npms = nimages
+			    call amovki (pm, Memi[pms], nimages)
+			} else {
+			    npms = npms + 1
+			    Memi[pms+i-1] = pm
+			}
+		    }
+		    if (project)
+			break
+		}
+	    }
+	}
+
+	# If no mask images are found and the mask parameters imply that
+	# good values are 0 then use the special case of no masks.
+
+	if (npms == 0) {
+	    if (!invert)
+		mtype = M_NONE
+	}
+
+	# Set up mask structure.
+	call calloc (icm, ICM_LEN, TY_STRUCT)
+	ICM_TYPE(icm) = mtype
+	ICM_VALUE(icm) = mvalue
+	ICM_BUFS(icm) = bufs
+	ICM_PMS(icm) = pms
+
+	call sfree (sp)
+end
+
+
+# IC_MCLOSE -- Close the mask interface.
+
+procedure ic_mclose (nimages)
+
+int	nimages			# Number of images
+
+int	i
+include	"icombine.com"
+
+begin
+	if (icm == NULL)
+	    return
+
+	do i = 1, nimages
+	    call mfree (Memi[ICM_BUFS(icm)+i-1], TY_INT)
+	do i = 1, nimages {
+	    if (Memi[ICM_PMS(icm)+i-1] != NULL)
+		call pm_close (Memi[ICM_PMS(icm)+i-1])
+	    if (project)
+		break
+	}
+	call mfree (ICM_BUFS(icm), TY_POINTER)
+	call mfree (ICM_PMS(icm), TY_POINTER)
+	call mfree (icm, TY_STRUCT)
+end
+
+
+# IC_MGET -- Get lines of mask pixels in the output coordinate system.
+# This converts the mask format to an array where zero is good and nonzero
+# is bad.  This has special cases for optimization.
+
+procedure ic_mget (in, out, offsets, v1, v2, m, lflag, nimages)
+
+pointer	in[nimages]		# Input image pointers
+pointer	out[ARB]		# Output image pointer
+int	offsets[nimages,ARB]	# Offsets to  output image
+long	v1[IM_MAXDIM]		# Data vector desired in output image
+long	v2[IM_MAXDIM]		# Data vector in input image
+pointer	m[nimages]		# Pointer to mask pointers
+int	lflag[nimages]		# Line flags
+int	nimages			# Number of images
+
+int	mtype			# Mask type
+int	mvalue			# Mask value
+pointer	bufs			# Pointer to data line buffers
+pointer	pms			# Pointer to array of PMIO pointers
+
+int	i, j, ndim, nout, npix
+pointer	buf, pm
+bool	pm_linenotempty()
+errchk	pm_glpi
+
+include	"icombine.com"
+
+begin
+	# Determine if masks are needed at all.  Note that the threshold
+	# is applied by simulating mask values so the mask pointers have to
+	# be set.
+
+	dflag = D_ALL
+	if (icm == NULL)
+	    return
+	if (ICM_TYPE(icm) == M_NONE && aligned && !dothresh)
+	    return
+
+	mtype = ICM_TYPE(icm)
+	mvalue = ICM_VALUE(icm)
+	bufs = ICM_BUFS(icm)
+	pms = ICM_PMS(icm)
+
+	# Set the mask pointers and line flags and apply offsets if needed.
+
+	ndim = IM_NDIM(out[1])
+	nout = IM_LEN(out[1],1)
+	do i = 1, nimages {
+	    npix = IM_LEN(in[i],1)
+	    j = offsets[i,1]
+	    m[i] = Memi[bufs+i-1]
+	    buf = Memi[bufs+i-1] + j
+	    pm =  Memi[pms+i-1]
+	    if (npix == nout)
+	        lflag[i] = D_ALL
+	    else
+	        lflag[i] = D_MIX
+
+	    v2[1] = v1[1]
+	    do j = 2, ndim {
+		v2[j] = v1[j] - offsets[i,j]
+		if (v2[j] < 1 || v2[j] > IM_LEN(in[i],j)) {
+		    lflag[i] = D_NONE
+		    break
+		}
+	    }
+	    if (project)
+		v2[ndim+1] = i
+
+	    if (lflag[i] == D_NONE)
+		next
+
+	    if (pm == NULL) {
+		call aclri (Memi[buf], npix)
+		next
+	    }
+
+	    # Do mask I/O and convert to appropriate values in order of
+	    # expected usage.
+
+	    if (pm_linenotempty (pm, v2)) {
+		call pm_glpi (pm, v2, Memi[buf], 32, npix, 0)
+
+		if (mtype == M_BOOLEAN)
+		    ;
+		else if (mtype == M_BADBITS)
+		    call aandki (Memi[buf], mvalue, Memi[buf], npix)
+		else if (mtype == M_BADVAL)
+		    call abeqki (Memi[buf], mvalue, Memi[buf], npix)
+		else if (mtype == M_GOODBITS) {
+		    call aandki (Memi[buf], mvalue, Memi[buf], npix)
+		    call abeqki (Memi[buf], 0, Memi[buf], npix)
+		} else if (mtype == M_GOODVAL)
+		    call abneki (Memi[buf], mvalue, Memi[buf], npix)
+
+		lflag[i] = D_NONE
+		do j = 1, npix
+		    if (Memi[buf+j-1] == 0) {
+			lflag[i] = D_MIX
+			break
+		    }
+	    } else {
+		if (mtype == M_BOOLEAN || mtype == M_BADBITS) {
+		    call aclri (Memi[buf], npix)
+		} else if ((mtype == M_BADVAL && mvalue != 0) ||
+		    (mtype == M_GOODVAL && mvalue == 0)) {
+		    call aclri (Memi[buf], npix)
+		} else {
+		    call amovki (1, Memi[buf], npix)
+		    lflag[i] = D_NONE
+		}
+	    }
+	}
+
+	# Set overall data flag
+	dflag = lflag[1]
+	do i = 2, nimages  {
+	    if (lflag[i] != dflag) {
+		dflag = D_MIX
+		break
+	    }
+	}
+end
+
+
+# IC_MGET1 -- Get line of mask pixels from a specified image.
+# This is used by the IC_STAT procedure. This procedure  converts the
+# stored mask format to an array where zero is good and nonzero is bad.
+# The data vector and returned mask array are in the input image pixel system.
+
+procedure ic_mget1 (in, image, offset, v, m)
+
+pointer	in			# Input image pointer
+int	image			# Image index
+int	offset			# Column offset
+long	v[IM_MAXDIM]		# Data vector desired
+pointer	m			# Pointer to mask
+
+int	mtype			# Mask type
+int	mvalue			# Mask value
+pointer	bufs			# Pointer to data line buffers
+pointer	pms			# Pointer to array of PMIO pointers
+
+int	i, npix
+pointer	buf, pm
+bool	pm_linenotempty()
+errchk	pm_glpi
+
+include	"icombine.com"
+
+begin
+	dflag = D_ALL
+	if (icm == NULL)
+	    return
+	if (ICM_TYPE(icm) == M_NONE)
+	    return
+
+	mtype = ICM_TYPE(icm)
+	mvalue = ICM_VALUE(icm)
+	bufs = ICM_BUFS(icm)
+	pms = ICM_PMS(icm)
+
+	npix = IM_LEN(in,1)
+	m = Memi[bufs+image-1] + offset
+	pm =  Memi[pms+image-1]
+	if (pm == NULL)
+	    return
+
+	# Do mask I/O and convert to appropriate values in order of
+	# expected usage.
+
+	buf = m
+	if (pm_linenotempty (pm, v)) {
+	    call pm_glpi (pm, v, Memi[buf], 32, npix, 0)
+
+	    if (mtype == M_BOOLEAN)
+		;
+	    else if (mtype == M_BADBITS)
+		call aandki (Memi[buf], mvalue, Memi[buf], npix)
+	    else if (mtype == M_BADVAL)
+		call abeqki (Memi[buf], mvalue, Memi[buf], npix)
+	    else if (mtype == M_GOODBITS) {
+		call aandki (Memi[buf], mvalue, Memi[buf], npix)
+		call abeqki (Memi[buf], 0, Memi[buf], npix)
+	    } else if (mtype == M_GOODVAL)
+		call abneki (Memi[buf], mvalue, Memi[buf], npix)
+
+	    dflag = D_NONE
+	    do i = 1, npix
+		if (Memi[buf+i-1] == 0) {
+		    dflag = D_MIX
+		    break
+		}
+	} else {
+	    if (mtype == M_BOOLEAN || mtype == M_BADBITS) {
+		;
+	    } else if ((mtype == M_BADVAL && mvalue != 0) ||
+		(mtype == M_GOODVAL && mvalue == 0)) {
+		;
+	    } else
+		dflag = D_NONE
+	}
+end
diff --git a/noao/imred/ccdred/src/combine/icmedian.gx b/noao/imred/ccdred/src/combine/icmedian.gx
new file mode 100644
index 00000000..dc8488d9
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icmedian.gx
@@ -0,0 +1,228 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+$for (sr)
+# IC_MEDIAN -- Median of lines
+
+procedure ic_median$t (d, n, npts, median)
+
+pointer	d[ARB]			# Input data line pointers
+int	n[npts]			# Number of good pixels
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	median[npts]		# Median
+$else
+PIXEL	median[npts]		# Median
+$endif
+
+int	i, j, k, j1, j2, n1, lo, up, lo1, up1
+bool	even
+$if (datatype == silx)
+real	val1, val2, val3
+$else
+PIXEL	val1, val2, val3
+$endif
+PIXEL	temp, wtemp
+$if (datatype == x)
+real	abs_temp
+$endif
+
+include	"../icombine.com"
+
+begin
+	# If no data return after possibly setting blank values.
+	if (dflag == D_NONE) {
+	    do i = 1, npts
+		median[i]= blank
+	    return
+	}
+
+	# If the data were previously sorted then directly compute the median.
+	if (mclip) {
+	    if (dflag == D_ALL) {
+		n1 = n[1]
+		even = (mod (n1, 2) == 0)
+		j1 = n1 / 2 + 1
+		j2 = n1 / 2
+		do i = 1, npts {
+		    k = i - 1
+		    if (even) {
+			val1 = Mem$t[d[j1]+k]
+			val2 = Mem$t[d[j2]+k]
+			median[i] = (val1 + val2) / 2.
+		    } else
+			median[i] = Mem$t[d[j1]+k]
+		}
+	    } else {
+		do i = 1, npts {
+		    k = i - 1
+		    n1 = n[i]
+		    if (n1 > 0) {
+			j1 = n1 / 2 + 1
+			if (mod (n1, 2) == 0) {
+			    j2 = n1 / 2
+			    val1 = Mem$t[d[j1]+k]
+			    val2 = Mem$t[d[j2]+k]
+			    median[i] = (val1 + val2) / 2.
+			} else
+			    median[i] = Mem$t[d[j1]+k]
+		    } else
+			median[i] = blank
+		}
+	    }
+	    return
+	}
+
+	# Compute the median.
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+
+	    # If there are more than 3 points use Wirth algorithm.  This
+	    # is the same as vops$amed.gx except for an even number of
+	    # points it selects the middle two and averages.
+	    if (n1 > 3) {
+		lo = 1
+		up = n1
+		j  = max (lo, min (up, (up+1)/2))
+
+		while (lo < up) {
+		    if (! (lo < up))
+			break
+
+		    temp = Mem$t[d[j]+k];  lo1 = lo;  up1 = up
+		    $if (datatype == x)
+		    abs_temp = abs (temp)
+		    $endif
+
+		    repeat {
+			$if (datatype == x)
+			while (abs (Mem$t[d[lo1]+k]) < abs_temp)
+			$else
+			while (Mem$t[d[lo1]+k] < temp)
+			$endif
+			    lo1 = lo1 + 1
+			$if (datatype == x)
+			while (abs_temp < abs (Mem$t[d[up1]+k]))
+			$else
+			while (temp < Mem$t[d[up1]+k])
+			$endif
+			    up1 = up1 - 1
+			if (lo1 <= up1) {
+			    wtemp = Mem$t[d[lo1]+k]
+			    Mem$t[d[lo1]+k] = Mem$t[d[up1]+k]
+			    Mem$t[d[up1]+k] = wtemp
+			    lo1 = lo1 + 1;  up1 = up1 - 1
+			}
+		    } until (lo1 > up1)
+
+		    if (up1 < j)
+			lo = lo1
+		    if (j < lo1)
+			up = up1
+		}
+
+		median[i] = Mem$t[d[j]+k]
+
+		if (mod (n1,2) == 0) {
+		    lo = 1
+		    up = n1
+		    j  = max (lo, min (up, (up+1)/2)+1)
+
+		    while (lo < up) {
+			if (! (lo < up))
+			    break
+
+			temp = Mem$t[d[j]+k];  lo1 = lo;  up1 = up
+			$if (datatype == x)
+			abs_temp = abs (temp)
+			$endif
+
+			repeat {
+			    $if (datatype == x)
+			    while (abs (Mem$t[d[lo1]+k]) < abs_temp)
+			    $else
+			    while (Mem$t[d[lo1]+k] < temp)
+			    $endif
+				lo1 = lo1 + 1
+			    $if (datatype == x)
+			    while (abs_temp < abs (Mem$t[d[up1]+k]))
+			    $else
+			    while (temp < Mem$t[d[up1]+k])
+			    $endif
+				up1 = up1 - 1
+			    if (lo1 <= up1) {
+				wtemp = Mem$t[d[lo1]+k]
+				Mem$t[d[lo1]+k] = Mem$t[d[up1]+k]
+				Mem$t[d[up1]+k] = wtemp
+				lo1 = lo1 + 1;  up1 = up1 - 1
+			    }
+			} until (lo1 > up1)
+
+			if (up1 < j)
+			    lo = lo1
+			if (j < lo1)
+			    up = up1
+		    }
+		    median[i] = (median[i] + Mem$t[d[j]+k]) / 2
+		}
+
+	    # If 3 points find the median directly.
+	    } else if (n1 == 3) {
+		$if (datatype == x)
+	        val1 = abs (Mem$t[d[1]+k])
+	        val2 = abs (Mem$t[d[2]+k])
+	        val3 = abs (Mem$t[d[3]+k])
+	        if (val1 < val2) {
+		    if (val2 < val3)		# abc
+		        median[i] = Mem$t[d[2]+k]
+		    else if (val1 < val3)	# acb
+		        median[i] = Mem$t[d[3]+k]
+		    else			# cab
+		        median[i] = Mem$t[d[1]+k]
+	        } else {
+		    if (val2 > val3)		# cba
+		        median[i] = Mem$t[d[2]+k]
+		    else if (val1 > val3)	# bca
+		        median[i] = Mem$t[d[3]+k]
+		    else			# bac
+		        median[i] = Mem$t[d[1]+k]
+	        }
+		$else
+	        val1 = Mem$t[d[1]+k]
+	        val2 = Mem$t[d[2]+k]
+	        val3 = Mem$t[d[3]+k]
+	        if (val1 < val2) {
+		    if (val2 < val3)		# abc
+		        median[i] = val2
+		    else if (val1 < val3)	# acb
+		        median[i] = val3
+		    else			# cab
+		        median[i] = val1
+	        } else {
+		    if (val2 > val3)		# cba
+		        median[i] = val2
+		    else if (val1 > val3)	# bca
+		        median[i] = val3
+		    else			# bac
+		        median[i] = val1
+	        }
+		$endif
+
+	    # If 2 points average.
+	    } else if (n1 == 2) {
+		val1 = Mem$t[d[1]+k]
+		val2 = Mem$t[d[2]+k]
+		median[i] = (val1 + val2) / 2
+
+	    # If 1 point return the value.
+	    } else if (n1 == 1)
+		median[i] = Mem$t[d[1]+k]
+
+	    # If no points return with a possibly blank value.
+	    else
+		median[i] = blank
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/icmm.gx b/noao/imred/ccdred/src/combine/icmm.gx
new file mode 100644
index 00000000..90837ae5
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icmm.gx
@@ -0,0 +1,177 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+$for (sr)
+# IC_MM --  Reject a specified number of high and low pixels
+
+procedure ic_mm$t (d, m, n, npts)
+
+pointer	d[ARB]		# Data pointers
+pointer	m[ARB]		# Image ID pointers
+int	n[npts]			# Number of good pixels
+int	npts			# Number of output points per line
+
+int	n1, ncombine, npairs, nlow, nhigh, np
+int	i, i1, j, jmax, jmin
+pointer	k, kmax, kmin
+PIXEL	d1, d2, dmin, dmax
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_NONE)
+	    return
+
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    nlow = flow * n1 + 0.001
+	    nhigh = fhigh * n1 + 0.001
+	    ncombine = n1 - nlow -  nhigh
+	    npairs = min (nlow, nhigh)
+	    nlow = nlow - npairs
+	    nhigh = nhigh - npairs
+	}
+
+	do i = 1, npts {
+	    i1 = i - 1
+	    n1 = n[i]
+	    if (dflag == D_MIX) {
+		nlow = flow * n1 + 0.001
+		nhigh = fhigh * n1 + 0.001
+		ncombine = max (ncombine, n1 - nlow - nhigh)
+		npairs = min (nlow, nhigh)
+		nlow = nlow - npairs
+		nhigh = nhigh - npairs
+	    }
+
+	    # Reject the npairs low and high points.
+	    do np = 1, npairs {
+		k = d[1] + i1
+		$if (datatype == x)
+		d1 = abs (Mem$t[k])
+		$else
+		d1 = Mem$t[k]
+		$endif
+		dmax = d1; dmin = d1; jmax = 1; jmin = 1; kmax = k; kmin = k
+		do j = 2, n1 {
+		    d2 = d1
+		    k = d[j] + i1
+		    $if (datatype == x)
+		    d1 = abs (Mem$t[k])
+		    $else
+		    d1 = Mem$t[k]
+		    $endif
+		    if (d1 > dmax) {
+			dmax = d1; jmax = j; kmax = k
+		    } else if (d1 < dmin) {
+			dmin = d1; jmin = j; kmin = k
+		    }
+		}
+		j = n1 - 1
+		if (keepids) {
+		    if (jmax < j) {
+			if (jmin != j) {
+			    Mem$t[kmax] = d2
+			    Memi[m[jmax]+i1] = Memi[m[j]+i1]
+			} else {
+			    Mem$t[kmax] = d1
+			    Memi[m[jmax]+i1] = Memi[m[n1]+i1]
+			}
+		    }
+		    if (jmin < j) {
+			if (jmax != n1) {
+			    Mem$t[kmin] = d1
+			    Memi[m[jmin]+i1] = Memi[m[n1]+i1]
+			} else {
+			    Mem$t[kmin] = d2
+			    Memi[m[jmin]+i1] = Memi[m[j]+i1]
+			}
+		    }
+		} else {
+		    if (jmax < j) {
+			if (jmin != j)
+			    Mem$t[kmax] = d2
+			else
+			    Mem$t[kmax] = d1
+		    }
+		    if (jmin < j) {
+			if (jmax != n1)
+			    Mem$t[kmin] = d1
+			else
+			    Mem$t[kmin] = d2
+		    }
+		}
+		n1 = n1 - 2
+	    }
+
+	    # Reject the excess low points.
+	    do np = 1, nlow {
+		k = d[1] + i1
+		$if (datatype == x)
+		d1 = abs (Mem$t[k])
+		$else
+		d1 = Mem$t[k]
+		$endif
+		dmin = d1; jmin = 1; kmin = k
+		do j = 2, n1 {
+		    k = d[j] + i1
+		    $if (datatype == x)
+		    d1 = abs (Mem$t[k])
+		    $else
+		    d1 = Mem$t[k]
+		    $endif
+		    if (d1 < dmin) {
+			dmin = d1; jmin = j; kmin = k
+		    }
+		}
+		if (keepids) {
+		    if (jmin < n1) {
+			Mem$t[kmin] = d1
+			Memi[m[jmin]+i1] = Memi[m[n1]+i1]
+		    }
+		} else {
+		    if (jmin < n1)
+			Mem$t[kmin] = d1
+		}
+		n1 = n1 - 1 
+	    }
+
+	    # Reject the excess high points.
+	    do np = 1, nhigh {
+		k = d[1] + i1
+		$if (datatype == x)
+		d1 = abs (Mem$t[k])
+		$else
+		d1 = Mem$t[k]
+		$endif
+		dmax = d1; jmax = 1; kmax = k
+		do j = 2, n1 {
+		    k = d[j] + i1
+		    $if (datatype == x)
+		    d1 = abs (Mem$t[k])
+		    $else
+		    d1 = Mem$t[k]
+		    $endif
+		    if (d1 > dmax) {
+			dmax = d1; jmax = j; kmax = k
+		    }
+		}
+		if (keepids) {
+		    if (jmax < n1) {
+			Mem$t[kmax] = d1
+			Memi[m[jmax]+i1] = Memi[m[n1]+i1]
+		    }
+		} else {
+		    if (jmax < n1)
+			Mem$t[kmax] = d1
+		}
+		n1 = n1 - 1 
+	    }
+	    n[i] = n1
+	}
+
+	if (dflag == D_ALL && npairs + nlow + nhigh > 0)
+		dflag = D_MIX
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/icombine.com b/noao/imred/ccdred/src/combine/icombine.com
new file mode 100644
index 00000000..cb826d58
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icombine.com
@@ -0,0 +1,40 @@
+# ICOMBINE Common
+
+int	combine			# Combine algorithm
+int	reject			# Rejection algorithm
+bool	project			# Combine across the highest dimension?
+real	blank			# Blank value
+pointer	rdnoise			# CCD read noise
+pointer	gain			# CCD gain
+pointer	snoise			# CCD sensitivity noise
+real	lthresh			# Low threshold
+real	hthresh			# High threshold
+int	nkeep			# Minimum to keep
+real	lsigma			# Low sigma cutoff
+real	hsigma			# High sigma cutoff
+real	pclip			# Number or fraction of pixels from median
+real	flow			# Fraction of low pixels to reject
+real	fhigh			# Fraction of high pixels to reject
+int	grow			# Grow radius
+bool	mclip			# Use median in sigma clipping?
+real	sigscale		# Sigma scaling tolerance
+int	logfd			# Log file descriptor
+
+# These flags allow special conditions to be optimized.
+
+int	dflag			# Data flag (D_ALL, D_NONE, D_MIX)
+bool	aligned			# Are the images aligned?
+bool	doscale			# Do the images have to be scaled?
+bool	doscale1		# Do the sigma calculations have to be scaled?
+bool	dothresh		# Check pixels outside specified thresholds?
+bool	dowts			# Does the final average have to be weighted?
+bool	keepids			# Keep track of the image indices?
+bool	docombine		# Call the combine procedure?
+bool	sort			# Sort data?
+
+pointer	icm			# Mask data structure
+
+common	/imccom/ combine, reject, blank, rdnoise, gain, snoise, lsigma, hsigma,
+		 lthresh, hthresh, nkeep, pclip, flow, fhigh, grow, logfd,
+		 dflag, sigscale, project, mclip, aligned, doscale, doscale1,
+		 dothresh, dowts, keepids, docombine, sort, icm
diff --git a/noao/imred/ccdred/src/combine/icombine.gx b/noao/imred/ccdred/src/combine/icombine.gx
new file mode 100644
index 00000000..d6e93ef0
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icombine.gx
@@ -0,0 +1,395 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	<imset.h>
+include	<error.h>
+include	<syserr.h>
+include	<mach.h>
+include	"../icombine.h"
+
+
+# ICOMBINE -- Combine images
+#
+# The memory and open file descriptor limits are checked and an attempt
+# to recover is made either by setting the image pixel files to be
+# closed after I/O or by notifying the calling program that memory
+# ran out and the IMIO buffer size should be reduced.  After the checks
+# a procedure for the selected combine option is called.
+# Because there may be several failure modes when reaching the file
+# limits we first assume an error is due to the file limit, except for
+# out of memory, and close some pixel files.  If the error then repeats
+# on accessing the pixels the error is passed back.
+
+$for (sr)
+procedure icombine$t (in, out, offsets, nimages, bufsize)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+int	offsets[nimages,ARB]	# Input image offsets
+int	nimages			# Number of input images
+int	bufsize			# IMIO buffer size
+
+char	str[1]
+int	i, j, npts, fd, stropen(), errcode(), imstati()
+pointer	sp, d, id, n, m, lflag, scales, zeros, wts, dbuf
+pointer	buf, imgl1$t(), impl1i()
+errchk	stropen, imgl1$t, impl1i
+$if (datatype == sil)
+pointer	impl1r()
+errchk	impl1r
+$else
+pointer	impl1$t()
+errchk	impl1$t
+$endif
+
+include	"../icombine.com"
+
+begin
+	npts = IM_LEN(out[1],1)
+
+	# Allocate memory.
+	call smark (sp)
+	call salloc (d, nimages, TY_POINTER)
+	call salloc (id, nimages, TY_POINTER)
+	call salloc (n, npts, TY_INT)
+	call salloc (m, nimages, TY_POINTER)
+	call salloc (lflag, nimages, TY_INT)
+	call salloc (scales, nimages, TY_REAL)
+	call salloc (zeros, nimages, TY_REAL)
+	call salloc (wts, nimages, TY_REAL)
+	call amovki (D_ALL, Memi[lflag], nimages)
+
+	# If aligned use the IMIO buffer otherwise we need vectors of
+	# output length.
+
+	if (!aligned) {
+	    call salloc (dbuf, nimages, TY_POINTER)
+	    do i = 1, nimages
+		call salloc (Memi[dbuf+i-1], npts, TY_PIXEL)
+	}
+
+	if (project) {
+	    call imseti (in[1], IM_NBUFS, nimages)
+	    call imseti (in[1], IM_BUFSIZE, bufsize)
+	    do i = 1, 3 {
+		if (out[i] != NULL)
+		    call imseti (out[i], IM_BUFSIZE, bufsize)
+	    }
+	} else {
+	    # Reserve FD for string operations.
+	    fd = stropen (str, 1, NEW_FILE)
+
+	    # Do I/O to the images.
+	    do i = 1, 3 {
+		if (out[i] != NULL)
+		    call imseti (out[i], IM_BUFSIZE, bufsize)
+	    }
+	    $if (datatype == sil)
+	    buf = impl1r (out[1])
+	    call aclrr (Memr[buf], npts)
+	    if (out[3] != NULL) {
+		buf = impl1r (out[3])
+		call aclrr (Memr[buf], npts)
+	    }
+	    $else
+	    buf = impl1$t (out[1])
+	    call aclr$t (Mem$t[buf], npts)
+	    if (out[3] != NULL) {
+		buf = impl1$t (out[3])
+		call aclr$t (Mem$t[buf], npts)
+	    }
+	    $endif
+	    if (out[2] != NULL) {
+		buf = impl1i (out[2])
+		call aclri (Memi[buf], npts)
+	    }
+
+	    do i = 1, nimages {
+		call imseti (in[i], IM_BUFSIZE, bufsize)
+		iferr (buf = imgl1$t (in[i])) {
+		    switch (errcode()) {
+		    case SYS_MFULL:
+			call sfree (sp)
+			call strclose (fd)
+			call erract (EA_ERROR)
+		    case SYS_FTOOMANYFILES, SYS_IKIOPIX:
+			if (imstati (in[i], IM_CLOSEFD) == YES) {
+			    call sfree (sp)
+			    call strclose (fd)
+			    call erract (EA_ERROR)
+			}
+			do j = i-2, nimages
+			    call imseti (in[j], IM_CLOSEFD, YES)
+			buf = imgl1$t (in[i])
+		    default:
+			call sfree (sp)
+			call strclose (fd)
+			call erract (EA_ERROR)
+		    }
+		}
+	    }
+
+	    call strclose (fd)
+	}
+
+	call ic_combine$t (in, out, Memi[dbuf], Memi[d], Memi[id], Memi[n],
+	    Memi[m], Memi[lflag], offsets, Memr[scales], Memr[zeros],
+	    Memr[wts], nimages, npts)
+end
+
+
+# IC_COMBINE -- Combine images.
+
+procedure ic_combine$t (in, out, dbuf, d, id, n, m, lflag, offsets,
+	scales, zeros, wts, nimages, npts)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output image
+pointer	dbuf[nimages]		# Data buffers for nonaligned images
+pointer	d[nimages]		# Data pointers
+pointer	id[nimages]		# Image index ID pointers
+int	n[npts]			# Number of good pixels
+pointer	m[nimages]		# Mask pointers
+int	lflag[nimages]		# Line flags
+int	offsets[nimages,ARB]	# Input image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero offset factors
+real	wts[nimages]		# Combining weights
+int	nimages			# Number of input images
+int	npts			# Number of points per output line
+
+int	i, ctor()
+real	r, imgetr()
+pointer	sp, v1, v2, v3, outdata, buf, nm, impnli()
+$if (datatype == sil)
+pointer	impnlr()
+$else
+pointer	impnl$t()
+$endif
+errchk	ic_scale, imgetr
+
+include	"../icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (v1, IM_MAXDIM, TY_LONG)
+	call salloc (v2, IM_MAXDIM, TY_LONG)
+	call salloc (v3, IM_MAXDIM, TY_LONG)
+	call amovkl (long(1), Meml[v1], IM_MAXDIM)
+	call amovkl (long(1), Meml[v2], IM_MAXDIM)
+	call amovkl (long(1), Meml[v3], IM_MAXDIM)
+
+	call ic_scale (in, out, offsets, scales, zeros, wts, nimages)
+
+	# Set combine parameters
+	switch (combine) {
+	case AVERAGE:
+	    if (dowts)
+		keepids = true
+	    else
+		keepids = false
+	case MEDIAN:
+	    dowts = false
+	    keepids = false
+	}
+	docombine = true
+
+	# Set rejection algorithm specific parameters
+	switch (reject) {
+	case CCDCLIP, CRREJECT:
+	    call salloc (nm, 3*nimages, TY_REAL)
+	    i = 1
+	    if (ctor (Memc[rdnoise], i, r) > 0) {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)] = r
+	    } else {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)] = imgetr (in[i], Memc[rdnoise])
+	    }
+	    i = 1
+	    if (ctor (Memc[gain], i, r) > 0) {
+		do i = 1, nimages {
+		    Memr[nm+3*(i-1)+1] = r
+		    Memr[nm+3*(i-1)] =
+			max ((Memr[nm+3*(i-1)] / r) ** 2, 1e4 / MAX_REAL)
+		}
+	    } else {
+		do i = 1, nimages {
+		    r = imgetr (in[i], Memc[gain])
+		    Memr[nm+3*(i-1)+1] = r
+		    Memr[nm+3*(i-1)] =
+			max ((Memr[nm+3*(i-1)] / r) ** 2, 1e4 / MAX_REAL)
+		}
+	    }
+	    i = 1
+	    if (ctor (Memc[snoise], i, r) > 0) {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)+2] = r
+	    } else {
+		do i = 1, nimages {
+		    r = imgetr (in[i], Memc[snoise])
+		    Memr[nm+3*(i-1)+2] = r
+		}
+	    }
+	    if (!keepids) {
+		if (doscale1 || grow > 0)
+		    keepids = true
+		else {
+		    do i = 2, nimages {
+			if (Memr[nm+3*(i-1)] != Memr[nm] ||
+			    Memr[nm+3*(i-1)+1] != Memr[nm+1] ||
+			    Memr[nm+3*(i-1)+2] != Memr[nm+2]) {
+			    keepids = true
+			    break
+			}
+		    }
+		}
+	    }
+	    if (reject == CRREJECT)
+		lsigma = MAX_REAL
+	case MINMAX:
+	    mclip = false
+	    if (grow > 0)
+		keepids = true
+	case PCLIP:
+	    mclip = true
+	    if (grow > 0)
+		keepids = true
+	case AVSIGCLIP, SIGCLIP:
+	    if (doscale1 || grow > 0)
+		keepids = true
+	case NONE:
+	    mclip = false
+	    grow = 0
+	}
+
+	if (keepids) {
+	    do i = 1, nimages
+		call salloc (id[i], npts, TY_INT)
+	}
+
+	$if (datatype == sil)
+	while (impnlr (out[1], outdata, Meml[v1]) != EOF) {
+	    call ic_gdata$t (in, out, dbuf, d, id, n, m, lflag, offsets,
+		scales, zeros, nimages, npts, Meml[v2], Meml[v3])
+
+	    switch (reject) {
+	    case CCDCLIP, CRREJECT:
+		if (mclip)
+		    call ic_mccdclip$t (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Memr[outdata])
+		else
+		    call ic_accdclip$t (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Memr[outdata])
+	    case MINMAX:
+		call ic_mm$t (d, id, n, npts)
+	    case PCLIP:
+		call ic_pclip$t (d, id, n, nimages, npts, Memr[outdata])
+	    case SIGCLIP:
+		if (mclip)
+		    call ic_msigclip$t (d, id, n, scales, zeros, nimages, npts,
+			Memr[outdata])
+		else
+		    call ic_asigclip$t (d, id, n, scales, zeros, nimages, npts,
+			Memr[outdata])
+	    case AVSIGCLIP:
+		if (mclip)
+		    call ic_mavsigclip$t (d, id, n, scales, zeros, nimages,
+			npts, Memr[outdata])
+		else
+		    call ic_aavsigclip$t (d, id, n, scales, zeros, nimages,
+			npts, Memr[outdata])
+	    }
+
+	    if (grow > 0)
+		call ic_grow$t (d, id, n, nimages, npts, Memr[outdata])
+
+	    if (docombine) {
+		switch (combine) {
+		case AVERAGE:
+		    call ic_average$t (d, id, n, wts, npts, Memr[outdata])
+		case MEDIAN:
+		    call ic_median$t (d, n, npts, Memr[outdata])
+		}
+	    }
+
+	    if (out[2] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnli (out[2], buf, Meml[v1])
+		call amovki (nimages, Memi[buf], npts)
+		call asubi (Memi[buf], n, Memi[buf], npts)
+	    }
+		    
+	    if (out[3] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnlr (out[3], buf, Meml[v1])
+		call ic_sigma$t (d, id, n, wts, npts, Memr[outdata],
+		    Memr[buf])
+	    }
+	    call amovl (Meml[v1], Meml[v2], IM_MAXDIM)
+	}
+	$else
+	while (impnl$t (out[1], outdata, Meml[v1]) != EOF) {
+	    call ic_gdata$t (in, out, dbuf, d, id, n, m, lflag, offsets,
+		scales, zeros, nimages, npts, Meml[v2], Meml[v3])
+
+	    switch (reject) {
+	    case CCDCLIP, CRREJECT:
+		if (mclip)
+		    call ic_mccdclip$t (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Mem$t[outdata])
+		else
+		    call ic_accdclip$t (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Mem$t[outdata])
+	    case MINMAX:
+		call ic_mm$t (d, id, n, npts)
+	    case PCLIP:
+		call ic_pclip$t (d, id, n, nimages, npts, Mem$t[outdata])
+	    case SIGCLIP:
+		if (mclip)
+		    call ic_msigclip$t (d, id, n, scales, zeros, nimages, npts,
+			Mem$t[outdata])
+		else
+		    call ic_asigclip$t (d, id, n, scales, zeros, nimages, npts,
+			Mem$t[outdata])
+	    case AVSIGCLIP:
+		if (mclip)
+		    call ic_mavsigclip$t (d, id, n, scales, zeros, nimages,
+			npts, Mem$t[outdata])
+		else
+		    call ic_aavsigclip$t (d, id, n, scales, zeros, nimages,
+			npts, Mem$t[outdata])
+	    }
+
+	    if (grow > 0)
+		call ic_grow$t (d, id, n, nimages, npts, Mem$t[outdata])
+
+	    if (docombine) {
+		switch (combine) {
+		case AVERAGE:
+		    call ic_average$t (d, id, n, wts, npts, Mem$t[outdata])
+		case MEDIAN:
+		    call ic_median$t (d, n, npts, Mem$t[outdata])
+		}
+	    }
+
+	    if (out[2] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnli (out[2], buf, Meml[v1])
+		call amovki (nimages, Memi[buf], npts)
+		call asubi (Memi[buf], n, Memi[buf], npts)
+	    }
+		    
+	    if (out[3] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnl$t (out[3], buf, Meml[v1])
+		call ic_sigma$t (d, id, n, wts, npts, Mem$t[outdata],
+		    Mem$t[buf])
+	    }
+	    call amovl (Meml[v1], Meml[v2], IM_MAXDIM)
+	}
+	$endif
+
+	call sfree (sp)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/icombine.h b/noao/imred/ccdred/src/combine/icombine.h
new file mode 100644
index 00000000..13b77117
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icombine.h
@@ -0,0 +1,52 @@
+# ICOMBINE Definitions
+
+# Memory management parameters;
+define	DEFBUFSIZE		65536		# default IMIO buffer size
+define	FUDGE			0.8		# fudge factor
+
+# Rejection options:
+define	REJECT	"|none|ccdclip|crreject|minmax|pclip|sigclip|avsigclip|"
+define	NONE		1	# No rejection algorithm
+define	CCDCLIP		2	# CCD noise function clipping
+define	CRREJECT	3	# CCD noise function clipping
+define	MINMAX		4	# Minmax rejection
+define	PCLIP		5	# Percentile clip
+define	SIGCLIP		6	# Sigma clip
+define	AVSIGCLIP	7	# Sigma clip with average poisson sigma
+
+# Combine options:
+define	COMBINE	"|average|median|"
+define	AVERAGE		1
+define	MEDIAN		2
+
+# Scaling options:
+define	STYPES		"|none|mode|median|mean|exposure|"
+define	ZTYPES		"|none|mode|median|mean|"
+define	WTYPES		"|none|mode|median|mean|exposure|"
+define	S_NONE		1
+define	S_MODE		2
+define	S_MEDIAN	3
+define	S_MEAN		4
+define	S_EXPOSURE	5
+define	S_FILE		6
+define	S_KEYWORD	7
+define	S_SECTION	"|input|output|overlap|"
+define	S_INPUT		1
+define	S_OUTPUT	2
+define	S_OVERLAP	3
+
+# Mask options
+define	MASKTYPES	"|none|goodvalue|badvalue|goodbits|badbits|"
+define	M_NONE		1	# Don't use mask images
+define	M_GOODVAL	2	# Value selecting good pixels
+define	M_BADVAL	3	# Value selecting bad pixels
+define	M_GOODBITS	4	# Bits selecting good pixels
+define	M_BADBITS	5	# Bits selecting bad pixels
+define	M_BOOLEAN	-1	# Ignore mask values
+
+# Data flag
+define	D_ALL		0	# All pixels are good
+define	D_NONE		1	# All pixels are bad or rejected
+define	D_MIX		2	# Mixture of good and bad pixels
+
+define	TOL		0.001	# Tolerance for equal residuals
diff --git a/noao/imred/ccdred/src/combine/icpclip.gx b/noao/imred/ccdred/src/combine/icpclip.gx
new file mode 100644
index 00000000..223396c3
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icpclip.gx
@@ -0,0 +1,233 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		3	# Minimum number for clipping
+
+$for (sr)
+# IC_PCLIP -- Percentile clip
+#
+# 1) Find the median
+# 2) Find the pixel which is the specified order index away
+# 3) Use the data value difference as a sigma and apply clipping
+# 4) Since the median is known return it so it does not have to be recomputed
+
+procedure ic_pclip$t (d, m, n, nimages, npts, median)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image id pointers
+int	n[npts]			# Number of good pixels
+int	nimages			# Number of input images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	median[npts]		# Median
+$else
+PIXEL	median[npts]		# Median
+$endif
+
+int	i, j, k, l, id, n1, n2, n3, n4, n5, nl, nh, nin, maxkeep
+bool	even, fp_equalr()
+real	sigma, r, s, t
+pointer	sp, resid, mp1, mp2
+$if (datatype == sil)
+real	med
+$else
+PIXEL	med
+$endif
+
+include	"../icombine.com"
+
+begin
+	# There must be at least MINCLIP and more than nkeep pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Set sign of pclip parameter
+	if (pclip < 0)
+	    t = -1.
+	else
+	    t = 1.
+
+	# If there are no rejected pixels compute certain parameters once.
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    n2 = 1 + n1 / 2
+	    even = (mod (n1, 2) == 0)
+	    if (pclip < 0.) {
+		if (even)
+		    n3 = max (1, nint (n2 - 1 + pclip))
+		else
+		    n3 = max (1, nint (n2 + pclip))
+	    } else
+		n3 = min (n1, nint (n2 + pclip))
+	    nin = n1
+	}
+
+	# Now apply clipping.
+	do i = 1, npts {
+	    # Compute median.
+	    if (dflag == D_MIX) {
+		n1 = n[i]
+		if (nkeep < 0)
+		    maxkeep = max (0, n1 + nkeep)
+		else
+		    maxkeep = min (n1, nkeep)
+		if (n1 == 0) {
+		    if (combine == MEDIAN)
+			median[i] = blank
+		    next
+		}
+		n2 = 1 + n1 / 2
+		even = (mod (n1, 2) == 0)
+		if (pclip < 0) {
+		    if (even)
+			n3 = max (1, nint (n2 - 1 + pclip))
+		    else
+			n3 = max (1, nint (n2 + pclip))
+		} else
+		    n3 = min (n1, nint (n2 + pclip))
+	    }
+
+	    j = i - 1 
+	    if (even) {
+		med = Mem$t[d[n2-1]+j]
+		med = (med + Mem$t[d[n2]+j]) / 2.
+	    } else
+		med = Mem$t[d[n2]+j]
+
+	    if (n1 < max (MINCLIP, maxkeep+1)) {
+		if (combine == MEDIAN)
+		    median[i] = med
+		next
+	    }
+
+	    # Define sigma for clipping
+	    sigma = t * (Mem$t[d[n3]+j] - med)
+	    if (fp_equalr (sigma, 0.)) {
+		if (combine == MEDIAN)
+		    median[i] = med
+		next
+	    }
+
+	    # Reject pixels and save residuals.
+	    # Check if any pixels are clipped.
+	    # If so recompute the median and reset the number of good pixels.
+	    # Only reorder if needed.
+
+	    for (nl=1; nl<=n1; nl=nl+1) {
+		r = (med - Mem$t[d[nl]+j]) / sigma
+		if (r < lsigma)
+		    break
+		Memr[resid+nl] = r
+	    }
+	    for (nh=n1; nh>=1; nh=nh-1) {
+		r = (Mem$t[d[nh]+j] -  med) / sigma
+		if (r < hsigma)
+		    break
+		Memr[resid+nh] = r
+	    }
+	    n4 = nh - nl + 1
+
+	    # If too many pixels are rejected add some back in.
+	    # All pixels with the same residual are added.
+	    while (n4 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n4 = nh - nl + 1
+	    }
+
+	    # If any pixels are rejected recompute the median.
+	    if (nl > 1 || nh < n1) {
+		n5 = nl + n4 / 2
+		if (mod (n4, 2) == 0) {
+		    med = Mem$t[d[n5-1]+j]
+		    med = (med + Mem$t[d[n5]+j]) / 2.
+		} else
+		    med = Mem$t[d[n5]+j]
+		n[i] = n4
+	    }
+	    if (combine == MEDIAN)
+		median[i] = med
+
+	    # Reorder if pixels only if necessary.
+	    if (nl > 1 && (combine != MEDIAN || grow > 0)) {
+		k = max (nl, n4 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mem$t[d[l]+j] = Mem$t[d[k]+j]
+			if (grow > 0) {
+			    mp1 = m[l] + j
+			    mp2 = m[k] + j
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+j] = Memi[m[k]+j]
+			k = k + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mem$t[d[l]+j] = Mem$t[d[k]+j]
+			k = k + 1
+		    }
+		}
+	    }
+	}
+
+	# Check if data flag needs to be reset for rejected pixels.
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag whether the median has been computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/icscale.x b/noao/imred/ccdred/src/combine/icscale.x
new file mode 100644
index 00000000..fc4efb2f
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icscale.x
@@ -0,0 +1,376 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	<imset.h>
+include	<error.h>
+include	"icombine.h"
+
+# IC_SCALE -- Get the scale factors for the images.
+# 1. This procedure does CLIO to determine the type of scaling desired.
+# 2. The output header parameters for exposure time and NCOMBINE are set.
+
+procedure ic_scale (in, out, offsets, scales, zeros, wts, nimages)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+int	offsets[nimages,ARB]	# Image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero or sky levels
+real	wts[nimages]		# Weights
+int	nimages			# Number of images
+
+int	stype, ztype, wtype
+int	i, j, k, l, nout
+real	mode, median, mean, exposure, zmean, darktime, dark
+pointer	sp, ncombine, exptime, modes, medians, means
+pointer	section, str, sname, zname, wname, imref
+bool	domode, domedian, domean, dozero, snorm, znorm, wflag
+
+bool	clgetb()
+int	hdmgeti(), strdic(), ic_gscale()
+real	hdmgetr(), asumr(), asumi()
+errchk	ic_gscale, ic_statr
+
+include	"icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (ncombine, nimages, TY_INT)
+	call salloc (exptime, nimages, TY_REAL)
+	call salloc (modes, nimages, TY_REAL)
+	call salloc (medians, nimages, TY_REAL)
+	call salloc (means, nimages, TY_REAL)
+	call salloc (section, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+	call salloc (sname, SZ_FNAME, TY_CHAR)
+	call salloc (zname, SZ_FNAME, TY_CHAR)
+	call salloc (wname, SZ_FNAME, TY_CHAR)
+
+	# Set the defaults.
+	call amovki (1, Memi[ncombine], nimages)
+	call amovkr (0., Memr[exptime], nimages)
+	call amovkr (INDEF, Memr[modes], nimages)
+	call amovkr (INDEF, Memr[medians], nimages)
+	call amovkr (INDEF, Memr[means], nimages)
+	call amovkr (1., scales, nimages)
+	call amovkr (0., zeros, nimages)
+	call amovkr (1., wts, nimages)
+
+	# Get the number of images previously combined and the exposure times.
+	# The default combine number is 1 and the default exposure is 0.
+
+	do i = 1, nimages {
+	    iferr (Memi[ncombine+i-1] = hdmgeti (in[i], "ncombine"))
+		Memi[ncombine+i-1] = 1
+	    iferr (Memr[exptime+i-1] = hdmgetr (in[i], "exptime"))
+		Memr[exptime+i-1] = 0.
+	    if (project) {
+		call amovki (Memi[ncombine], Memi[ncombine], nimages)
+		call amovkr (Memr[exptime], Memr[exptime], nimages)
+		break
+	    }
+	}
+
+	# Set scaling factors.
+
+	stype = ic_gscale ("scale", Memc[sname], STYPES, in, Memr[exptime],
+	    scales, nimages)
+	ztype = ic_gscale ("zero", Memc[zname], ZTYPES, in, Memr[exptime],
+	    zeros, nimages)
+	wtype = ic_gscale ("weight", Memc[wname], WTYPES, in, Memr[exptime],
+	    wts, nimages)
+
+	# Get image statistics only if needed.
+	domode = ((stype==S_MODE)||(ztype==S_MODE)||(wtype==S_MODE))
+	domedian = ((stype==S_MEDIAN)||(ztype==S_MEDIAN)||(wtype==S_MEDIAN))
+	domean = ((stype==S_MEAN)||(ztype==S_MEAN)||(wtype==S_MEAN))
+	if (domode || domedian || domean) {
+	    Memc[section] = EOS
+	    Memc[str] = EOS
+	    call clgstr ("statsec", Memc[section], SZ_FNAME)
+	    call sscan (Memc[section])
+	    call gargwrd (Memc[section], SZ_FNAME)
+	    call  gargwrd (Memc[str], SZ_LINE)
+
+	    i = strdic (Memc[section], Memc[section], SZ_FNAME, S_SECTION)
+	    switch (i) {
+	    case S_INPUT:
+		call strcpy (Memc[str], Memc[section], SZ_FNAME)
+		imref = NULL
+	    case S_OUTPUT:
+		call strcpy (Memc[str], Memc[section], SZ_FNAME)
+		imref = out[1]
+	    case S_OVERLAP:
+		call strcpy ("[", Memc[section], SZ_FNAME)
+		do i = 1, IM_NDIM(out[1]) {
+		    k = offsets[1,i] + 1
+		    l = offsets[1,i] + IM_LEN(in[1],i)
+		    do j = 2, nimages {
+			k = max (k, offsets[j,i]+1)
+			l = min (l, offsets[j,i]+IM_LEN(in[j],i))
+		    }
+		    if (i < IM_NDIM(out[1]))
+			call sprintf (Memc[str], SZ_LINE, "%d:%d,")
+		    else
+			call sprintf (Memc[str], SZ_LINE, "%d:%d]")
+			    call pargi (k)
+			    call pargi (l)
+		    call strcat (Memc[str], Memc[section], SZ_FNAME)
+		}
+		imref = out[1]
+	    default:
+		imref = NULL
+	    }
+
+	    do i = 1, nimages {
+		if (imref != out[1])
+		    imref = in[i]
+		call ic_statr (in[i], imref, Memc[section], offsets,
+		    i, nimages, domode, domedian, domean, mode, median, mean)
+		if (domode) {
+		    Memr[modes+i-1] = mode
+		    if (stype == S_MODE)
+			scales[i] = mode
+		    if (ztype == S_MODE)
+			zeros[i] = mode
+		    if (wtype == S_MODE)
+			wts[i] = mode
+		}
+		if (domedian) {
+		    Memr[medians+i-1] = median
+		    if (stype == S_MEDIAN)
+			scales[i] = median
+		    if (ztype == S_MEDIAN)
+			zeros[i] = median
+		    if (wtype == S_MEDIAN)
+			wts[i] = median
+		}
+		if (domean) {
+		    Memr[means+i-1] = mean
+		    if (stype == S_MEAN)
+			scales[i] = mean
+		    if (ztype == S_MEAN)
+			zeros[i] = mean
+		    if (wtype == S_MEAN)
+			wts[i] = mean
+		}
+	    }
+	}
+
+	do i = 1, nimages
+	    if (scales[i] <= 0.) {
+		call eprintf ("WARNING: Negative scale factors")
+		call eprintf (" -- ignoring scaling\n")
+		call amovkr (1., scales, nimages)
+		break
+	    }
+
+	# Convert to relative factors if needed.
+	snorm = (stype == S_FILE || stype == S_KEYWORD)
+	znorm = (ztype == S_FILE || ztype == S_KEYWORD)
+	wflag = (wtype == S_FILE || wtype == S_KEYWORD)
+	if (snorm)
+	    call arcpr (1., scales, scales, nimages)
+	else {
+	    mean = asumr (scales, nimages) / nimages
+	    call adivkr (scales, mean, scales, nimages)
+	}
+	call adivr (zeros, scales, zeros, nimages)
+	zmean = asumr (zeros, nimages) / nimages
+
+	if (wtype != S_NONE) {
+	    do i = 1, nimages {
+		if (wts[i] <= 0.) {
+		    call eprintf ("WARNING: Negative weights")
+		    call eprintf (" -- using only NCOMBINE weights\n")
+		    do j = 1, nimages
+			wts[j] = Memi[ncombine+j-1]
+		    break
+		}
+		if (ztype == S_NONE || znorm || wflag)
+	            wts[i] = Memi[ncombine+i-1] * wts[i]
+		else {
+		    if (zeros[i] <= 0.) {
+			call eprintf ("WARNING: Negative zero offsets")
+			call eprintf (" -- ignoring zero weight adjustments\n")
+			do j = 1, nimages
+			    wts[j] = Memi[ncombine+j-1] * wts[j]
+			break
+		    }
+		    wts[i] = Memi[ncombine+i-1] * wts[i] * zmean / zeros[i]
+		}
+	    }
+	}
+
+	if (znorm)
+	    call anegr (zeros, zeros, nimages)
+	else {
+	    # Because of finite arithmetic it is possible for the zero offsets
+	    # to be nonzero even when they are all equal.  Just for the sake of
+	    # a nice log set the zero offsets in this case.
+
+	    call asubkr (zeros, zmean, zeros, nimages)
+	    for (i=2; (i<=nimages)&&(zeros[i]==zeros[1]); i=i+1)
+		;
+	    if (i > nimages)
+		call aclrr (zeros, nimages)
+	}
+	mean = asumr (wts, nimages)
+	call adivkr (wts, mean, wts, nimages)
+
+	# Set flags for scaling, zero offsets, sigma scaling, weights.
+	# Sigma scaling may be suppressed if the scales or zeros are
+	# different by a specified tolerance.
+
+	doscale = false
+	dozero = false
+	doscale1 = false
+	dowts = false
+	do i = 2, nimages {
+	    if (snorm || scales[i] != scales[1])
+		doscale = true
+	    if (znorm || zeros[i] != zeros[1])
+		dozero = true
+	    if (wts[i] != wts[1])
+		dowts = true
+	}
+	if (doscale && sigscale != 0.) {
+	    do i = 1, nimages {
+		if (abs (scales[i] - 1) > sigscale) {
+		    doscale1 = true
+		    break
+		}
+	    }
+	    if (!doscale1 && zmean > 0.) {
+		do i = 1, nimages {
+		    if (abs (zeros[i] / zmean) > sigscale) {
+			doscale1 = true
+			break
+		    }
+		}
+	    }
+	}
+		    
+	# Set the output header parameters.
+	nout = asumi (Memi[ncombine], nimages)
+	call hdmputi (out[1], "ncombine", nout)
+	exposure = 0.
+	darktime = 0.
+	mean = 0.
+	do i = 1, nimages {
+	    exposure = exposure + wts[i] * Memr[exptime+i-1] / scales[i]
+	    ifnoerr (dark = hdmgetr (in[i], "darktime"))
+		darktime = darktime + wts[i] * dark / scales[i]
+	    else
+		darktime = darktime + wts[i] * Memr[exptime+i-1] / scales[i]
+	    ifnoerr (mode = hdmgetr (in[i], "ccdmean"))
+		mean = mean + wts[i] * mode / scales[i]
+	}
+	call hdmputr (out[1], "exptime", exposure)
+	call hdmputr (out[1], "darktime", darktime)
+	ifnoerr (mode = hdmgetr (out[1], "ccdmean")) {
+	    call hdmputr (out[1], "ccdmean", mean)
+	    iferr (call imdelf (out[1], "ccdmeant"))
+		;
+	}
+	if (out[2] != NULL) {
+	    call imstats (out[2], IM_IMAGENAME, Memc[str], SZ_FNAME)
+	    call imastr (out[1], "BPM", Memc[str])
+	}
+
+	# Start the log here since much of the info is only available here.
+	if (clgetb ("verbose")) {
+	    i = logfd
+	    logfd = STDOUT
+	    call ic_log (in, out, Memi[ncombine], Memr[exptime], Memc[sname],
+		Memc[zname], Memc[wname], Memr[modes], Memr[medians],
+		Memr[means], scales, zeros, wts, offsets, nimages, dozero,
+		nout, "", exposure)
+
+	    logfd = i
+	}
+	call ic_log (in, out, Memi[ncombine], Memr[exptime], Memc[sname],
+	    Memc[zname], Memc[wname], Memr[modes], Memr[medians], Memr[means],
+	    scales, zeros, wts, offsets, nimages, dozero, nout,
+	    "", exposure)
+
+	doscale = (doscale || dozero)
+
+	call sfree (sp)
+end
+
+
+# IC_GSCALE -- Get scale values as directed by CL parameter
+# The values can be one of those in the dictionary, from a file specified
+# with a @ prefix, or from an image header keyword specified by a ! prefix.
+
+int procedure ic_gscale (param, name, dic, in, exptime, values, nimages)
+
+char	param[ARB]		#I CL parameter name
+char	name[SZ_FNAME]		#O Parameter value
+char	dic[ARB]		#I Dictionary string
+pointer	in[nimages]		#I IMIO pointers
+real	exptime[nimages]	#I Exposure times
+real	values[nimages]		#O Values
+int	nimages			#I Number of images
+
+int	type			#O Type of value
+
+int	fd, i, nowhite(), open(), fscan(), nscan(), strdic()
+real	rval, hdmgetr()
+pointer	errstr
+errchk	open, hdmgetr()
+
+include	"icombine.com"
+
+begin
+	call clgstr (param, name, SZ_FNAME)
+	if (nowhite (name, name, SZ_FNAME) == 0)
+	    type = S_NONE
+	else if (name[1] == '@') {
+	    type = S_FILE
+	    fd = open (name[2], READ_ONLY, TEXT_FILE)
+	    i = 0
+	    while (fscan (fd) != EOF) {
+		call gargr (rval)
+		if (nscan() != 1)
+		    next
+		if (i == nimages) {
+		   call eprintf (
+		       "Warning: Ignoring additional %s values in %s\n")
+		       call pargstr (param)
+		       call pargstr (name[2])
+		   break
+		}
+		i = i + 1
+		values[i] = rval
+	    }
+	    call close (fd)
+	    if (i < nimages) {
+		call salloc (errstr, SZ_LINE, TY_CHAR)
+		call sprintf (Memc[errstr], SZ_FNAME,
+		    "Insufficient %s values in %s")
+		    call pargstr (param)
+		    call pargstr (name[2])
+		call error (1, Memc[errstr])
+	    }
+	} else if (name[1] == '!') {
+	    type = S_KEYWORD
+	    do i = 1, nimages {
+		values[i] = hdmgetr (in[i], name[2])
+		if (project) {
+		    call amovkr (values, values, nimages)
+		    break
+		}
+	    }
+	} else {
+	    type = strdic (name, name, SZ_FNAME, dic)
+	    if (type == 0)
+		call error (1, "Unknown scale, zero, or weight type")
+	    if (type==S_EXPOSURE)
+		do i = 1, nimages
+		    values[i] = max (0.001, exptime[i])
+	}
+
+	return (type)
+end
diff --git a/noao/imred/ccdred/src/combine/icsclip.gx b/noao/imred/ccdred/src/combine/icsclip.gx
new file mode 100644
index 00000000..f70611aa
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icsclip.gx
@@ -0,0 +1,504 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		3	# Mininum number of images for algorithm
+
+$for (sr)
+# IC_ASIGCLIP -- Reject pixels using sigma clipping about the average
+# The initial average rejects the high and low pixels.  A correction for
+# different scalings of the images may be made.  Weights are not used.
+
+procedure ic_asigclip$t (d, m, n, scales, zeros, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	average[npts]		# Average
+$else
+PIXEL	average[npts]		# Average
+$endif
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+$if (datatype == sil)
+real	d1, low, high, sum, a, s, r, one
+data	one /1.0/
+$else
+PIXEL	d1, low, high, sum, a, s, r, one
+data	one /1$f/
+$endif
+pointer	sp, resid, w, wp, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	} 
+	
+	# Flag whether returned average needs to be recomputed.
+	if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	# Save the residuals and the sigma scaling corrections if needed.
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+	if (doscale1)
+	    call salloc (w, nimages, TY_REAL)
+
+	# Do sigma clipping.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+
+	    # If there are not enough pixels simply compute the average.
+	    if (n1 < max (3, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Mem$t[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Mem$t[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    # Compute average with the high and low rejected.
+	    low = Mem$t[d[1]+k]
+	    high = Mem$t[d[2]+k]
+	    if (low > high) {
+		d1 = low
+		low = high
+		high = d1
+	    }
+	    sum = 0.
+	    do j = 3, n1 {
+	       d1 = Mem$t[d[j]+k]
+	       if (d1 < low) {
+		   sum = sum + low
+		   low = d1
+		} else if (d1 > high) {
+		    sum = sum + high
+		    high = d1
+		} else
+		    sum = sum + d1
+	    }
+	    a = sum / (n1 - 2)
+	    sum = sum + low + high
+
+	    # Iteratively reject pixels and compute the final average if needed.
+	    # Compact the data and keep track of the image IDs if needed.
+
+	    repeat {
+		n2 = n1
+		if (doscale1) {
+		    # Compute sigma corrected for scaling.
+		    s = 0.
+		    wp = w - 1
+		    do j = 1, n1 {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			wp = wp + 1
+
+			d1 = Mem$t[dp1]
+			l = Memi[mp1]
+			r = sqrt (max (one, (a + zeros[l]) / scales[l]))
+			s = s + ((d1 - a) / r) ** 2
+			Memr[wp] = r
+		    }
+		    s = sqrt (s / (n1 - 1))
+
+		    # Reject pixels.  Save the residuals and data values.
+		    wp = w - 1
+		    if (s > 0.) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    mp1 = m[j] + k
+			    wp = wp + 1
+
+			    d1 = Mem$t[dp1]
+			    r = (d1 - a) / (s * Memr[wp])
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs (r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    Memr[wp] = Memr[w+n1-1]
+				    mp2 = m[n1] + k
+				    l = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		} else {
+		    # Compute the sigma without scale correction.
+		    s = 0.
+		    do j = 1, n1
+			s = s + (Mem$t[d[j]+k] - a) ** 2
+		    s = sqrt (s / (n1 - 1))
+
+		    # Reject pixels.  Save the residuals and data values.
+		    if (s > 0.) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    d1 = Mem$t[dp1]
+			    r = (d1 - a) / s
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs (r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[n1] + k
+					l = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = l
+				    }
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+
+		# Recompute the average.
+		if (n1 > 1)
+		    a = sum / n1
+	    } until (n1 == n2 || n1 <= max (2, maxkeep))
+
+	    # If too many pixels are rejected add some back.
+	    # All pixels with equal residuals are added back.
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mem$t[dp1]
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Mem$t[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mem$t[dp1]
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Mem$t[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+
+		# Recompute the average.
+		if (n1 > 1)
+		    a = sum / n1
+	    }
+
+	    # Save the average if needed.
+	    n[i] = n1
+	    if (!docombine) {
+		if (n1 > 0)
+		    average[i] = a
+		else
+		    average[i] = blank
+	    }
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_MSIGCLIP -- Reject pixels using sigma clipping about the median
+
+procedure ic_msigclip$t (d, m, n, scales, zeros, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	median[npts]		# Median
+$else
+PIXEL	median[npts]		# Median
+$endif
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+real	r, s
+pointer	sp, resid, w, mp1, mp2
+$if (datatype == sil)
+real	med, one
+data	one /1.0/
+$else
+PIXEL	med, one
+data	one /1$f/
+$endif
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	# Save the residuals and sigma scaling corrections if needed.
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+	if (doscale1)
+	    call salloc (w, nimages, TY_REAL)
+
+	# Compute median and sigma and iteratively clip.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    nl = 1
+	    nh = n1
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 == 0)
+		    med = blank
+		else if (mod (n1, 2) == 0)
+		    med = (Mem$t[d[n3-1]+k] + Mem$t[d[n3]+k]) / 2.
+		else
+		    med = Mem$t[d[n3]+k]
+
+		if (n1 >= max (MINCLIP, maxkeep+1)) {
+		    if (doscale1) {
+			# Compute the sigma with scaling correction.
+			s = 0.
+			do j = nl, nh {
+			    l = Memi[m[j]+k]
+			    r = sqrt (max (one, (med + zeros[l]) / scales[l]))
+			    s = s + ((Mem$t[d[j]+k] - med) / r) ** 2
+			    Memr[w+j-1] = r
+			}
+			s = sqrt (s / (n1 - 1))
+
+			# Reject pixels and save the residuals.
+			if (s > 0.) {
+			    for (; nl <= n2; nl = nl + 1) {
+				r = (med - Mem$t[d[nl]+k]) / (s * Memr[w+nl-1])
+				if (r <= lsigma)
+				    break
+				Memr[resid+nl] = r
+				n1 = n1 - 1
+			    }
+			    for (; nh >= nl; nh = nh - 1) {
+				r = (Mem$t[d[nh]+k] - med) / (s * Memr[w+nh-1])
+				if (r <= hsigma)
+				    break
+				Memr[resid+nh] = r
+				n1 = n1 - 1
+			    }
+			}
+		    } else {
+			# Compute the sigma without scaling correction.
+			s = 0.
+			do j = nl, nh
+			    s = s + (Mem$t[d[j]+k] - med) ** 2
+			s = sqrt (s / (n1 - 1))
+
+			# Reject pixels and save the residuals.
+			if (s > 0.) {
+			    for (; nl <= n2; nl = nl + 1) {
+				r = (med - Mem$t[d[nl]+k]) / s
+				if (r <= lsigma)
+				    break
+				Memr[resid+nl] = r
+				n1 = n1 - 1
+			    }
+			    for (; nh >= nl; nh = nh - 1) {
+				r = (Mem$t[d[nh]+k] -  med) / s
+				if (r <= hsigma)
+				    break
+				Memr[resid+nh] = r
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    # If too many pixels are rejected add some back.
+	    # All pixels with equal residuals are added back.
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mem$t[d[l]+k] = Mem$t[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mem$t[d[l]+k] = Mem$t[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median has been computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/icsection.x b/noao/imred/ccdred/src/combine/icsection.x
new file mode 100644
index 00000000..746c1f51
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icsection.x
@@ -0,0 +1,94 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<ctype.h>
+
+# IC_SECTION -- Parse an image section into its elements.
+# 1. The default values must be set by the caller.
+# 2. A null image section is OK.
+# 3. The first nonwhitespace character must be '['.
+# 4. The last interpreted character must be ']'.
+#
+# This procedure should be replaced with an IMIO procedure at some
+# point.
+
+procedure ic_section (section, x1, x2, xs, ndim)
+
+char	section[ARB]		# Image section
+int	x1[ndim]		# Starting pixel
+int	x2[ndim]		# Ending pixel
+int	xs[ndim]		# Step
+int	ndim			# Number of dimensions
+
+int	i, ip, a, b, c, temp, ctoi()
+define	error_	99
+
+begin
+	# Decode the section string.
+	ip = 1
+	while (IS_WHITE(section[ip]))
+	    ip = ip + 1
+	if (section[ip] == '[')
+	    ip = ip + 1
+	else if (section[ip] == EOS)
+	    return
+	else
+	    goto error_
+
+	do i = 1, ndim {
+	    while (IS_WHITE(section[ip]))
+	        ip = ip + 1
+	    if (section[ip] == ']')
+		break
+
+	    # Default values
+	    a = x1[i]
+	    b = x2[i]
+	    c = xs[i]
+
+	    # Get a:b:c.  Allow notation such as "-*:c"
+	    # (or even "-:c") where the step is obviously negative.
+
+	    if (ctoi (section, ip, temp) > 0) {			# a
+		a = temp
+	        if (section[ip] == ':') {	
+		    ip = ip + 1
+		    if (ctoi (section, ip, b) == 0)		# a:b
+		        goto error_
+	        } else
+		    b = a
+	    } else if (section[ip] == '-') {			# -*
+		temp = a
+		a = b
+		b = temp
+	        ip = ip + 1
+	        if (section[ip] == '*')
+		    ip = ip + 1
+	    } else if (section[ip] == '*')			# *
+	        ip = ip + 1
+	    if (section[ip] == ':') {				# ..:step
+	        ip = ip + 1
+	        if (ctoi (section, ip, c) == 0)
+		    goto error_
+	        else if (c == 0)
+		    goto error_
+	    }
+	    if (a > b && c > 0)
+	        c = -c
+
+	    x1[i] = a
+	    x2[i] = b
+	    xs[i] = c
+
+	    while (IS_WHITE(section[ip]))
+	        ip = ip + 1
+	    if (section[ip] == ',')
+		ip = ip + 1
+	}
+
+	if (section[ip] != ']')
+	    goto error_
+
+	return
+error_
+	call error (0, "Error in image section specification")
+end
diff --git a/noao/imred/ccdred/src/combine/icsetout.x b/noao/imred/ccdred/src/combine/icsetout.x
new file mode 100644
index 00000000..bd1d75ec
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icsetout.x
@@ -0,0 +1,193 @@
+include	<imhdr.h>
+include <mwset.h>
+
+# IC_SETOUT -- Set output image size and offsets of input images.
+
+procedure ic_setout (in, out, offsets, nimages)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+int	offsets[nimages,ARB]	# Offsets
+int	nimages			# Number of images
+
+int	i, j, indim, outdim, mwdim, a, b, amin, bmax, fd
+real	val
+bool	reloff, streq()
+pointer	sp, fname, lref, wref, cd, coord, shift, axno, axval
+pointer	mw, ct, mw_openim(), mw_sctran()
+int	open(), fscan(), nscan(), mw_stati()
+errchk	mw_openim, mw_gwtermd, mw_gltermd, mw_gaxmap
+errchk	mw_sctran, mw_ctrand, open
+
+include	"icombine.com"
+define	newscan_ 10
+
+begin
+	call smark (sp)
+	call salloc (fname, SZ_FNAME, TY_CHAR)
+	call salloc (lref, IM_MAXDIM, TY_DOUBLE)
+	call salloc (wref, IM_MAXDIM, TY_DOUBLE)
+	call salloc (cd, IM_MAXDIM*IM_MAXDIM, TY_DOUBLE)
+	call salloc (coord, IM_MAXDIM, TY_DOUBLE)
+	call salloc (shift, IM_MAXDIM, TY_REAL)
+	call salloc (axno, IM_MAXDIM, TY_INT)
+	call salloc (axval, IM_MAXDIM, TY_INT)
+
+	# Check and set the image dimensionality.
+	indim = IM_NDIM(in[1])
+	outdim = IM_NDIM(out[1])
+	if (project) {
+	    outdim = indim - 1
+	    IM_NDIM(out[1]) = outdim
+	} else {
+	    do i = 1, nimages
+		if (IM_NDIM(in[i]) != outdim) {
+		    call sfree (sp)
+		    call error (1, "Image dimensions are not the same")
+		}
+	}
+
+	# Set the reference point to that of the first image.
+	mw = mw_openim (in[1])
+	mwdim = mw_stati (mw, MW_NPHYSDIM)
+	call mw_gwtermd (mw, Memd[lref], Memd[wref], Memd[cd], mwdim)
+	ct = mw_sctran (mw, "world", "logical", 0)
+	call mw_ctrand (ct, Memd[wref], Memd[lref], mwdim)
+	call mw_ctfree (ct)
+	if (project)
+	    Memd[lref+outdim] = 1
+
+	# Parse the user offset string.  If "none" then there are no offsets.
+	# If "wcs" then set the offsets based on the image WCS.
+	# If "grid" then set the offsets based on the input grid parameters.
+	# If a file scan it.
+
+	call clgstr ("offsets", Memc[fname], SZ_FNAME)
+	call sscan (Memc[fname])
+	call gargwrd (Memc[fname], SZ_FNAME)
+	if (nscan() == 0 || streq (Memc[fname], "none")) {
+	    call aclri (offsets, outdim*nimages)
+	    reloff = true
+	} else if (streq (Memc[fname], "wcs")) {
+	    do j = 1, outdim
+		offsets[1,j] = 0
+	    if (project) {
+		ct = mw_sctran (mw, "world", "logical", 0)
+		do i = 2, nimages {
+		    Memd[wref+outdim] = i
+		    call mw_ctrand (ct, Memd[wref], Memd[coord], indim)
+		    do j = 1, outdim
+			offsets[i,j] = nint (Memd[lref+j-1] - Memd[coord+j-1])
+		}
+		call mw_ctfree (ct)
+		call mw_close (mw)
+	    } else {
+		do i = 2, nimages {
+		    call mw_close (mw)
+		    mw = mw_openim (in[i])
+		    ct = mw_sctran (mw, "world", "logical", 0)
+		    call mw_ctrand (ct, Memd[wref], Memd[coord], indim)
+		    do j = 1, outdim
+			offsets[i,j] = nint (Memd[lref+j-1] - Memd[coord+j-1])
+		    call mw_ctfree (ct)
+		}
+	    }
+	    reloff = true
+	} else if (streq (Memc[fname], "grid")) {
+	    amin = 1
+	    do j = 1, outdim {
+		call gargi (a)
+		call gargi (b)
+		if (nscan() < 1+2*j)
+		    break
+		do i = 1, nimages
+		    offsets[i,j] = mod ((i-1)/amin, a) * b 
+		amin = amin * a
+	    }
+	    reloff = true
+	} else {
+	    reloff = true
+	    fd = open (Memc[fname], READ_ONLY, TEXT_FILE)
+	    do i = 1, nimages {
+newscan_	if (fscan (fd) == EOF)
+		    call error (1, "IMCOMBINE: Offset list too short")
+		call gargwrd (Memc[fname], SZ_FNAME)
+		if (Memc[fname] == '#') {
+		    call gargwrd (Memc[fname], SZ_FNAME)
+		    call strlwr (Memc[fname])
+		    if (streq (Memc[fname], "absolute"))
+			reloff = false
+		    else if (streq (Memc[fname], "relative"))
+			reloff = true
+		    goto newscan_
+		}
+		call reset_scan ()
+		do j = 1, outdim {
+		    call gargr (val)
+		    offsets[i,j] = nint (val)
+		}
+		if (nscan() < outdim)
+		    call error (1, "IMCOMBINE: Error in offset list")
+	    }
+	    call close (fd)
+	}
+
+	# Set the output image size and the aligned flag 
+	aligned = true
+	do j = 1, outdim {
+	    a = offsets[1,j]
+	    b = IM_LEN(in[1],j) + a
+	    amin = a
+	    bmax = b
+	    do i = 2, nimages {
+		a = offsets[i,j]
+		b = IM_LEN(in[i],j) + a
+		if (a != amin || b != bmax || !reloff)
+		    aligned = false
+		amin = min (a, amin)
+		bmax = max (b, bmax)
+	    }
+	    IM_LEN(out[1],j) = bmax
+	    if (reloff || amin < 0) {
+		do i = 1, nimages
+		    offsets[i,j] = offsets[i,j] - amin
+		IM_LEN(out[1],j) = IM_LEN(out[1],j) - amin
+	    }
+	}
+
+	# Update the WCS.
+	if (project || !aligned || !reloff) {
+	    call mw_close (mw)
+	    mw = mw_openim (out[1])
+	    mwdim = mw_stati (mw, MW_NPHYSDIM)
+	    call mw_gaxmap (mw, Memi[axno], Memi[axval], mwdim)
+	    if (!aligned || !reloff) {
+		call mw_gltermd (mw, Memd[cd], Memd[lref], mwdim)
+		do i = 1, mwdim {
+		    j = Memi[axno+i-1]
+		    if (j > 0 && j <= indim)
+			Memd[lref+i-1] = Memd[lref+i-1] + offsets[1,j]
+		}
+		call mw_sltermd (mw, Memd[cd], Memd[lref], mwdim)
+	    }
+	    if (project) {
+		# Apply dimensional reduction.
+		do i = 1, mwdim {
+		    j = Memi[axno+i-1]
+		    if (j <= outdim)
+			next
+		    else if (j > outdim+1)
+			Memi[axno+i-1] = j - 1
+		    else {
+			Memi[axno+i-1] = 0
+			Memi[axval+i-1] = 0
+		    }
+		}
+		call mw_saxmap (mw, Memi[axno], Memi[axval], mwdim)
+	    }
+	    call mw_saveim (mw, out)
+	}
+	call mw_close (mw)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/combine/icsigma.gx b/noao/imred/ccdred/src/combine/icsigma.gx
new file mode 100644
index 00000000..d0ae28d4
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icsigma.gx
@@ -0,0 +1,115 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"../icombine.h"
+
+$for (sr)
+# IC_SIGMA -- Compute the sigma image line.
+# The estimated sigma includes a correction for the finite population.
+# Weights are used if desired.
+
+procedure ic_sigma$t (d, m, n, wts, npts, average, sigma)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image ID pointers
+int	n[npts]			# Number of points
+real	wts[ARB]		# Weights
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	average[npts]		# Average
+real	sigma[npts]		# Sigma line (returned)
+$else
+PIXEL	average[npts]		# Average
+PIXEL	sigma[npts]		# Sigma line (returned)
+$endif
+
+int	i, j, k, n1
+real	wt, sigcor, sumwt
+$if (datatype == sil)
+real	a, sum
+$else
+PIXEL	a, sum
+$endif
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    if (dowts) {
+		if (n1 > 1)
+		    sigcor = real (n1) / real (n1 - 1)
+		else
+		    sigcor = 1.
+		do i = 1, npts {
+		    k = i - 1
+		    a = average[i]
+		    wt = wts[Memi[m[1]+k]]
+		    sum = (Mem$t[d[1]+k] - a) ** 2 * wt
+		    do j = 2, n1 {
+			wt = wts[Memi[m[j]+k]]
+			sum = sum + (Mem$t[d[j]+k] - a) ** 2 * wt
+		    }
+		    sigma[i] = sqrt (sum * sigcor)
+		}
+	    } else {
+		if (n1 > 1)
+		    sigcor = 1. / real (n1 - 1)
+		else
+		    sigcor = 1.
+		do i = 1, npts {
+		    k = i - 1
+		    a = average[i]
+		    sum = (Mem$t[d[1]+k] - a) ** 2
+		    do j = 2, n1
+			sum = sum + (Mem$t[d[j]+k] - a) ** 2
+		    sigma[i] = sqrt (sum * sigcor)
+		}
+	    }
+	} else if (dflag == D_NONE) {
+	    do i = 1, npts
+		sigma[i] = blank
+	} else {
+	    if (dowts) {
+		do i = 1, npts {
+		    n1 = n[i]
+		    if (n1 > 0) {
+			k = i - 1
+			if (n1 > 1)
+			    sigcor = real (n1) / real (n1 -1)
+			else
+			    sigcor = 1
+			a = average[i]
+			wt = wts[Memi[m[1]+k]]
+			sum = (Mem$t[d[1]+k] - a) ** 2 * wt
+			sumwt = wt
+			do j = 2, n1 {
+			    wt = wts[Memi[m[j]+k]]
+			    sum = sum + (Mem$t[d[j]+k] - a) ** 2 * wt
+			    sumwt = sumwt + wt
+			}
+			sigma[i] = sqrt (sum / sumwt * sigcor)
+		    } else
+			sigma[i] = blank
+		}
+	    } else {
+		do i = 1, npts {
+		    n1 = n[i]
+		    if (n1 > 0) {
+			k = i - 1
+			if (n1 > 1)
+			    sigcor = 1. / real (n1 - 1)
+			else
+			    sigcor = 1.
+			a = average[i]
+			sum = (Mem$t[d[1]+k] - a) ** 2
+			do j = 2, n1
+			    sum = sum + (Mem$t[d[j]+k] - a) ** 2
+			sigma[i] = sqrt (sum * sigcor)
+		    } else
+			sigma[i] = blank
+		}
+	    }
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/icsort.gx b/noao/imred/ccdred/src/combine/icsort.gx
new file mode 100644
index 00000000..2235dbd0
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icsort.gx
@@ -0,0 +1,386 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+define	LOGPTR	32			# log2(maxpts) (4e9)
+
+$for (sr)
+# IC_SORT -- Quicksort.  This is based on the VOPS asrt except that
+# the input is an array of pointers to image lines and the sort is done
+# across the image lines at each point along the lines.  The number of
+# valid pixels at each point is allowed to vary.  The cases of 1, 2, and 3
+# pixels per point are treated specially.
+
+procedure ic_sort$t (a, b, nvecs, npts)
+
+pointer	a[ARB]			# pointer to input vectors
+PIXEL	b[ARB]			# work array
+int	nvecs[npts]		# number of vectors
+int	npts			# number of points in vectors
+
+PIXEL	pivot, temp, temp3
+int	i, j, k, l, p, npix, lv[LOGPTR], uv[LOGPTR]
+define	swap {temp=$1;$1=$2;$2=temp}
+define	copy_	10
+
+begin
+	do l = 0, npts-1 {
+	    npix = nvecs[l+1]
+	    if (npix <= 1)
+		next
+
+	    do i = 1, npix
+		b[i] = Mem$t[a[i]+l]
+
+	    # Special cases
+	    $if (datatype == x)
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (abs (temp) < abs (pivot)) {
+			b[1] = temp
+			b[2] = pivot
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (abs (temp) < abs (pivot)) {		# bac|bca|cba
+			if (abs (temp) < abs (temp3)) {		# bac|bca
+			    b[1] = temp
+			    if (abs (pivot) < abs (temp3))	# bac
+				b[2] = pivot
+			    else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			}
+		    } else if (abs (temp3) < abs (temp)) {	# acb|cab
+			b[3] = temp
+			if (abs (pivot) < abs (temp3))		# acb
+			    b[2] = temp3
+			else {					# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+	    $else
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (temp < pivot) {
+			b[1] = temp
+			b[2] = pivot
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (temp < pivot) {				# bac|bca|cba
+			if (temp < temp3) {			# bac|bca
+			    b[1] = temp
+			    if (pivot < temp3)			# bac
+				b[2] = pivot
+			    else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			}
+		    } else if (temp3 < temp) {			# acb|cab
+			b[3] = temp
+			if (pivot < temp3)			# acb
+			    b[2] = temp3
+			else {					# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+	    $endif
+
+	    # General case
+	    do i = 1, npix
+		b[i] = Mem$t[a[i]+l]
+
+	    lv[1] = 1
+	    uv[1] = npix
+	    p = 1
+
+	    while (p > 0) {
+		if (lv[p] >= uv[p])		# only one elem in this subset
+		    p = p - 1			# pop stack
+		else {
+		    # Dummy do loop to trigger the Fortran optimizer.
+		    do p = p, ARB {
+			i = lv[p] - 1
+			j = uv[p]
+
+			# Select as the pivot the element at the center of the
+			# array, to avoid quadratic behavior on an already
+			# sorted array.
+
+			k = (lv[p] + uv[p]) / 2
+			swap (b[j], b[k])
+			pivot = b[j]		   # pivot line
+
+			while (i < j) {
+			$if (datatype == x)
+			    for (i=i+1;  abs(b[i]) < abs(pivot);  i=i+1)
+			$else
+			    for (i=i+1;  b[i] < pivot;  i=i+1)
+			$endif
+				;
+			    for (j=j-1;  j > i;  j=j-1)
+			$if (datatype == x)
+				if (abs(b[j]) <= abs(pivot))
+			$else
+				if (b[j] <= pivot)
+			$endif
+				    break
+			    if (i < j)		   # out of order pair
+				swap (b[i], b[j])  # interchange elements
+			}
+
+			j = uv[p]		   # move pivot to position i
+			swap (b[i], b[j])	   # interchange elements
+
+			if (i-lv[p] < uv[p] - i) { # stack so shorter done first
+			    lv[p+1] = lv[p]
+			    uv[p+1] = i - 1
+			    lv[p] = i + 1
+			} else {
+			    lv[p+1] = i + 1
+			    uv[p+1] = uv[p]
+			    uv[p] = i - 1
+			}
+
+			break
+		    }
+		    p = p + 1			   # push onto stack
+		}
+	    }
+
+copy_
+	    do i = 1, npix
+		Mem$t[a[i]+l] = b[i]
+	}
+end
+
+
+# IC_2SORT -- Quicksort.  This is based on the VOPS asrt except that
+# the input is an array of pointers to image lines and the sort is done
+# across the image lines at each point along the lines.  The number of
+# valid pixels at each point is allowed to vary.  The cases of 1, 2, and 3
+# pixels per point are treated specially.  A second integer set of
+# vectors is sorted.
+
+procedure ic_2sort$t (a, b, c, d, nvecs, npts)
+
+pointer	a[ARB]			# pointer to input vectors
+PIXEL	b[ARB]			# work array
+pointer	c[ARB]			# pointer to associated integer vectors
+int	d[ARB]			# work array
+int	nvecs[npts]		# number of vectors
+int	npts			# number of points in vectors
+
+PIXEL	pivot, temp, temp3
+int	i, j, k, l, p, npix, lv[LOGPTR], uv[LOGPTR], itemp
+define	swap {temp=$1;$1=$2;$2=temp}
+define	iswap {itemp=$1;$1=$2;$2=itemp}
+define	copy_	10
+
+begin
+	do l = 0, npts-1 {
+	    npix = nvecs[l+1]
+	    if (npix <= 1)
+		next
+
+	    do i = 1, npix {
+		b[i] = Mem$t[a[i]+l]
+		d[i] = Memi[c[i]+l]
+	    }
+
+	    # Special cases
+	    $if (datatype == x)
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (abs (temp) < abs (pivot)) {
+			b[1] = temp
+			b[2] = pivot
+			iswap (d[1], d[2])
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (abs (temp) < abs (pivot)) {		# bac|bca|cba
+			if (abs (temp) < abs (temp3)) {		# bac|bca
+			    b[1] = temp
+			    if (abs (pivot) < abs (temp3)) {	# bac
+				b[2] = pivot
+				iswap (d[1], d[2])
+			    } else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+				itemp = d[2]
+				d[2] = d[3]
+				d[3] = d[1]
+				d[1] = itemp
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			    iswap (d[1], d[3])
+			}
+		    } else if (abs (temp3) < abs (temp)) {	# acb|cab
+			b[3] = temp
+			if (abs (pivot) < abs (temp3)) {	# acb
+			    b[2] = temp3
+			    iswap (d[2], d[3])
+			} else {				# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			    itemp = d[2]
+			    d[2] = d[1]
+			    d[1] = d[3]
+			    d[3] = itemp
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+	    $else
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (temp < pivot) {
+			b[1] = temp
+			b[2] = pivot
+			iswap (d[1], d[2])
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (temp < pivot) {				# bac|bca|cba
+			if (temp < temp3) {			# bac|bca
+			    b[1] = temp
+			    if (pivot < temp3) {		# bac
+				b[2] = pivot
+				iswap (d[1], d[2])
+			    } else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+				itemp = d[2]
+				d[2] = d[3]
+				d[3] = d[1]
+				d[1] = itemp
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			    iswap (d[1], d[3])
+			}
+		    } else if (temp3 < temp) {			# acb|cab
+			b[3] = temp
+			if (pivot < temp3) {			# acb
+			    b[2] = temp3
+			    iswap (d[2], d[3])
+			} else {				# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			    itemp = d[2]
+			    d[2] = d[1]
+			    d[1] = d[3]
+			    d[3] = itemp
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+	    $endif
+
+	    # General case
+	    lv[1] = 1
+	    uv[1] = npix
+	    p = 1
+
+	    while (p > 0) {
+		if (lv[p] >= uv[p])		# only one elem in this subset
+		    p = p - 1			# pop stack
+		else {
+		    # Dummy do loop to trigger the Fortran optimizer.
+		    do p = p, ARB {
+			i = lv[p] - 1
+			j = uv[p]
+
+			# Select as the pivot the element at the center of the
+			# array, to avoid quadratic behavior on an already
+			# sorted array.
+
+			k = (lv[p] + uv[p]) / 2
+			swap (b[j], b[k]); swap (d[j], d[k])
+			pivot = b[j]		   # pivot line
+
+			while (i < j) {
+			$if (datatype == x)
+			    for (i=i+1;  abs(b[i]) < abs(pivot);  i=i+1)
+			$else
+			    for (i=i+1;  b[i] < pivot;  i=i+1)
+			$endif
+				;
+			    for (j=j-1;  j > i;  j=j-1)
+			$if (datatype == x)
+				if (abs(b[j]) <= abs(pivot))
+			$else
+				if (b[j] <= pivot)
+			$endif
+				    break
+			    if (i < j) {	   # out of order pair
+				swap (b[i], b[j])  # interchange elements
+				swap (d[i], d[j])
+			    }
+			}
+
+			j = uv[p]		   # move pivot to position i
+			swap (b[i], b[j])	   # interchange elements
+			swap (d[i], d[j])
+
+			if (i-lv[p] < uv[p] - i) { # stack so shorter done first
+			    lv[p+1] = lv[p]
+			    uv[p+1] = i - 1
+			    lv[p] = i + 1
+			} else {
+			    lv[p+1] = i + 1
+			    uv[p+1] = uv[p]
+			    uv[p] = i - 1
+			}
+
+			break
+		    }
+		    p = p + 1			   # push onto stack
+		}
+	    }
+
+copy_	   
+	    do i = 1, npix {
+		Mem$t[a[i]+l] = b[i]
+		Memi[c[i]+l] = d[i]
+	    }
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/icstat.gx b/noao/imred/ccdred/src/combine/icstat.gx
new file mode 100644
index 00000000..099ddf5e
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/icstat.gx
@@ -0,0 +1,237 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"../icombine.h"
+
+define	NMAX	10000	# Maximum number of pixels to sample
+
+$for (sr)
+# IC_STAT -- Compute image statistics within specified section.
+# The image section is relative to a reference image which may be
+# different than the input image and may have an offset.  Only a
+# subsample of pixels is used.  Masked and thresholded pixels are
+# ignored.  Only the desired statistics are computed to increase
+# efficiency.
+
+procedure ic_stat$t (im, imref, section, offsets, image, nimages,
+	domode, domedian, domean, mode, median, mean)
+
+pointer	im			 # Data image
+pointer	imref			 # Reference image for image section
+char	section[ARB]		 # Image section
+int	offsets[nimages,ARB]	 # Image section offset from data to reference
+int	image			 # Image index (for mask I/O)
+int	nimages			 # Number of images in  offsets.
+bool	domode, domedian, domean # Statistics to compute
+real	mode, median, mean	 # Statistics
+
+int	i, j, ndim, n, nv
+real	a
+pointer	sp, v1, v2, dv, va, vb
+pointer	data, mask, dp, lp, mp, imgnl$t()
+PIXEL	ic_mode$t()
+$if (datatype == irs)
+real    asum$t()
+$endif
+$if (datatype == dl)
+double  asum$t()
+$endif
+$if (datatype == x)
+complex asum$t()
+$endif
+
+
+include	"../icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (v1, IM_MAXDIM, TY_LONG)
+	call salloc (v2, IM_MAXDIM, TY_LONG)
+	call salloc (dv, IM_MAXDIM, TY_LONG)
+	call salloc (va, IM_MAXDIM, TY_LONG)
+	call salloc (vb, IM_MAXDIM, TY_LONG)
+
+	# Determine the image section parameters.  This must be in terms of
+	# the data image pixel coordinates though the section may be specified
+	# in terms of the reference image coordinates.  Limit the number of
+	# pixels in each dimension to a maximum.
+
+	ndim = IM_NDIM(im)
+	if (project)
+	    ndim = ndim - 1
+	call amovki (1, Memi[v1], IM_MAXDIM)
+	call amovki (1, Memi[va], IM_MAXDIM)
+	call amovki (1, Memi[dv], IM_MAXDIM)
+	call amovi (IM_LEN(imref,1), Memi[vb], ndim)
+	call ic_section (section, Memi[va], Memi[vb], Memi[dv], ndim)
+	if (im != imref)
+	    do i = 1, ndim {
+		Memi[va+i-1] = Memi[va+i-1] - offsets[image,i]
+		Memi[vb+i-1] = Memi[vb+i-1] - offsets[image,i]
+	    }
+
+	do j = 1, 10 {
+	    n = 1
+	    do i = 0, ndim-1 {
+		Memi[v1+i] = max (1, min (Memi[va+i], Memi[vb+i]))
+		Memi[v2+i] = min (IM_LEN(im,i+1), max (Memi[va+i], Memi[vb+i]))
+		Memi[dv+i] = j
+		nv = max (1, (Memi[v2+i] - Memi[v1+i]) / Memi[dv+i] + 1)
+		Memi[v2+i] = Memi[v1+i] + (nv - 1) * Memi[dv+i]
+		n = n * nv
+	    }
+	    if (n < NMAX)
+		break
+	}
+
+	call amovl (Memi[v1], Memi[va], IM_MAXDIM)
+	Memi[va] = 1
+	if (project)
+	   Memi[va+ndim] = image
+	call amovl (Memi[va], Memi[vb], IM_MAXDIM)
+
+	# Accumulate the pixel values within the section.  Masked pixels and
+	# thresholded pixels are ignored.
+
+	call salloc (data, n, TY_PIXEL)
+	dp = data
+	while (imgnl$t (im, lp, Memi[vb]) != EOF) {
+	    call ic_mget1 (im, image, offsets[image,1], Memi[va], mask)
+	    lp = lp + Memi[v1] - 1
+	    if (dflag == D_ALL) {
+		if (dothresh) {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			a = Mem$t[lp]
+			if (a >= lthresh && a <= hthresh) {
+			    Mem$t[dp] = a
+			    dp = dp + 1
+			}
+			lp = lp + Memi[dv]
+		    }
+		} else {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			Mem$t[dp] = Mem$t[lp]
+			dp = dp + 1
+			lp = lp + Memi[dv]
+		    }
+		}
+	    } else if (dflag == D_MIX) {
+		mp = mask + Memi[v1] - 1
+		if (dothresh) {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			if (Memi[mp] == 0) {
+			    a = Mem$t[lp]
+			    if (a >= lthresh && a <= hthresh) {
+				Mem$t[dp] = a
+				dp = dp + 1
+			    }
+			}
+			mp = mp + Memi[dv]
+			lp = lp + Memi[dv]
+		    }
+		} else {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			if (Memi[mp] == 0) {
+			    Mem$t[dp] = Mem$t[lp]
+			    dp = dp + 1
+			}
+			mp = mp + Memi[dv]
+			lp = lp + Memi[dv]
+		    }
+		}
+	    }
+	    for (i=2; i<=ndim; i=i+1) {
+		Memi[va+i-1] = Memi[va+i-1] + Memi[dv+i-1]
+		if (Memi[va+i-1] <= Memi[v2+i-1])
+		    break
+		Memi[va+i-1] = Memi[v1+i-1]
+	    }
+	    if (i > ndim)
+		break
+	    call amovl (Memi[va], Memi[vb], IM_MAXDIM)
+	}
+
+	n = dp - data
+	if (n < 1) {
+	    call sfree (sp)
+	    call error (1, "Image section contains no pixels")
+	}
+
+	# Compute only statistics needed.
+	if (domode || domedian) {
+	    call asrt$t (Mem$t[data], Mem$t[data], n)
+	    mode = ic_mode$t (Mem$t[data], n)
+	    median = Mem$t[data+n/2-1]
+	}
+	if (domean)
+	    mean = asum$t (Mem$t[data], n) / n
+
+	call sfree (sp)
+end
+
+
+define	NMIN	10	# Minimum number of pixels for mode calculation
+define	ZRANGE	0.8	# Fraction of pixels about median to use
+define	ZSTEP	0.01	# Step size for search for mode
+define	ZBIN	0.1	# Bin size for mode.
+
+# IC_MODE -- Compute mode of an array.  The mode is found by binning
+# with a bin size based on the data range over a fraction of the
+# pixels about the median and a bin step which may be smaller than the
+# bin size.  If there are too few points the median is returned.
+# The input array must be sorted.
+
+PIXEL procedure ic_mode$t (a, n)
+
+PIXEL	a[n]			# Data array
+int	n			# Number of points
+
+int	i, j, k, nmax
+real	z1, z2, zstep, zbin
+PIXEL	mode
+bool	fp_equalr()
+
+begin
+	if (n < NMIN)
+	    return (a[n/2])
+
+	# Compute the mode.  The array must be sorted.  Consider a
+	# range of values about the median point.  Use a bin size which
+	# is ZBIN of the range.  Step the bin limits in ZSTEP fraction of
+	# the bin size.
+
+	i = 1 + n * (1. - ZRANGE) / 2.
+	j = 1 + n * (1. + ZRANGE) / 2.
+	z1 = a[i]
+	z2 = a[j]
+	if (fp_equalr (z1, z2)) {
+	    mode = z1
+	    return (mode)
+	}
+
+	zstep = ZSTEP * (z2 - z1)
+	zbin = ZBIN * (z2 - z1)
+	$if (datatype == sil)
+	zstep = max (1., zstep)
+	zbin = max (1., zbin)
+	$endif
+
+	z1 = z1 - zstep
+	k = i
+	nmax = 0
+	repeat {
+	    z1 = z1 + zstep
+	    z2 = z1 + zbin
+	    for (; i < j && a[i] < z1; i=i+1)
+		;
+	    for (; k < j && a[k] < z2; k=k+1)
+		;
+	    if (k - i > nmax) {
+	        nmax = k - i
+	        mode = a[(i+k)/2]
+	    }
+	} until (k >= j)
+
+	return (mode)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/combine/mkpkg b/noao/imred/ccdred/src/combine/mkpkg
new file mode 100644
index 00000000..2c5c0795
--- /dev/null
+++ b/noao/imred/ccdred/src/combine/mkpkg
@@ -0,0 +1,51 @@
+# Make CCDRED Package.
+
+$checkout libpkg.a ../..
+$update   libpkg.a
+$checkin  libpkg.a ../..
+$exit
+
+generic:
+	$set	GEN = "$$generic -k"
+
+        $ifolder (generic/icaclip.x, icaclip.gx)
+	    $(GEN) icaclip.gx -o generic/icaclip.x $endif
+        $ifolder (generic/icaverage.x, icaverage.gx)
+	    $(GEN) icaverage.gx -o generic/icaverage.x $endif
+        $ifolder (generic/iccclip.x, iccclip.gx)
+	    $(GEN) iccclip.gx -o generic/iccclip.x $endif
+        $ifolder (generic/icgdata.x, icgdata.gx)
+	    $(GEN) icgdata.gx -o generic/icgdata.x $endif
+        $ifolder (generic/icgrow.x, icgrow.gx)
+	    $(GEN) icgrow.gx -o generic/icgrow.x $endif
+        $ifolder (generic/icmedian.x, icmedian.gx)
+	    $(GEN) icmedian.gx -o generic/icmedian.x $endif
+        $ifolder (generic/icmm.x, icmm.gx)
+	    $(GEN) icmm.gx -o generic/icmm.x $endif
+        $ifolder (generic/icombine.x, icombine.gx)
+	    $(GEN) icombine.gx -o generic/icombine.x $endif
+        $ifolder (generic/icpclip.x, icpclip.gx)
+	    $(GEN) icpclip.gx -o generic/icpclip.x $endif
+        $ifolder (generic/icsclip.x, icsclip.gx)
+	    $(GEN) icsclip.gx -o generic/icsclip.x $endif
+        $ifolder (generic/icsigma.x, icsigma.gx)
+	    $(GEN) icsigma.gx -o generic/icsigma.x $endif
+        $ifolder (generic/icsort.x, icsort.gx)
+	    $(GEN) icsort.gx -o generic/icsort.x $endif
+        $ifolder (generic/icstat.x, icstat.gx)
+	    $(GEN) icstat.gx -o generic/icstat.x $endif
+	;
+
+libpkg.a:
+	$ifeq (USE_GENERIC, yes) $call generic $endif
+	@generic
+
+	icimstack.x	<error.h> <imhdr.h>
+	iclog.x		icmask.h icombine.com icombine.h <imhdr.h> <imset.h>\
+			<mach.h>
+	icmask.x	icmask.h icombine.com icombine.h icombine.com <imhdr.h>\
+			<pmset.h>
+	icscale.x	icombine.com icombine.h <error.h> <imhdr.h> <imset.h>
+	icsection.x	<ctype.h>
+	icsetout.x	icombine.com <imhdr.h> <mwset.h>
+	;
diff --git a/noao/imred/ccdred/src/cor.gx b/noao/imred/ccdred/src/cor.gx
new file mode 100644
index 00000000..189f9437
--- /dev/null
+++ b/noao/imred/ccdred/src/cor.gx
@@ -0,0 +1,362 @@
+include	"ccdred.h"
+
+
+.help cor Feb87 noao.imred.ccdred
+.nf ----------------------------------------------------------------------------
+cor -- Process CCD image lines
+
+These procedures are the heart of the CCD processing.  They do the desired
+set of processing operations on the image line data as efficiently as
+possible.  They are called by the PROC procedures.  There are four procedures
+one for each readout axis and one for short and real image data.
+Some sets of operations are coded as single compound operations for efficiency.
+To keep the number of combinations managable only the most common
+combinations are coded as compound operations.  The combinations
+consist of any set of line overscan, column overscan, zero level, dark
+count, and flat field and any set of illumination and fringe
+correction.  The corrections are applied in place to the output vector.
+
+The column readout procedure is more complicated in order to handle
+zero level and flat field corrections specified as one dimensional
+readout corrections instead of two dimensional calibration images.
+Column readout format is probably extremely rare and the 1D readout
+corrections are used only for special types of data.
+.ih
+SEE ALSO
+proc, ccdred.h
+.endhelp -----------------------------------------------------------------------
+
+$for (sr)
+# COR1 -- Correct image lines with readout axis 1 (lines).
+
+procedure cor1$t (cors, out, overscan, zero, dark, flat, illum,
+	fringe, n, darkscale, flatscale, illumscale, frgscale)
+
+int	cors[ARB]	# Correction flags
+PIXEL	out[n]		# Output data
+real	overscan	# Overscan value
+PIXEL	zero[n]		# Zero level correction
+PIXEL	dark[n]		# Dark count correction
+PIXEL	flat[n]		# Flat field correction
+PIXEL	illum[n]	# Illumination correction
+PIXEL	fringe[n]	# Fringe correction
+int	n		# Number of pixels
+real	darkscale	# Dark count scale factor
+real	flatscale	# Flat field scale factor
+real	illumscale	# Illumination scale factor
+real	frgscale	# Fringe scale factor
+
+int	i, op
+
+begin
+	op = cors[OVERSCAN] + cors[ZEROCOR] + cors[DARKCOR] + cors[FLATCOR]
+	switch (op) {
+	case O: # overscan
+	    do i = 1, n
+	        out[i] = out[i] - overscan
+	case Z: # zero level
+	    do i = 1, n
+		out[i] = out[i] - zero[i]
+
+	case ZO: # zero level + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - zero[i]
+
+	case D: # dark count
+	    do i = 1, n
+		out[i] = out[i] - darkscale * dark[i]
+	case DO: # dark count + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - darkscale * dark[i]
+	case DZ: # dark count + zero level
+	    do i = 1, n
+		out[i] = out[i] - zero[i] - darkscale * dark[i]
+	case DZO: # dark count + zero level + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - zero[i] - darkscale * dark[i]
+
+	case F: # flat field
+	    do i = 1, n
+		out[i] = out[i] * flatscale / flat[i]
+	case FO: # flat field + overscan
+	    do i = 1, n
+	        out[i] = (out[i] - overscan) * flatscale / flat[i]
+	case FZ: # flat field + zero level
+	    do i = 1, n
+		out[i] = (out[i] - zero[i]) * flatscale / flat[i]
+	case FZO: # flat field + zero level + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - zero[i]) * flatscale /
+		    flat[i]
+	case FD: # flat field + dark count
+	    do i = 1, n
+		out[i] = (out[i] - darkscale * dark[i]) * flatscale / flat[i]
+	case FDO: # flat field + dark count + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - darkscale * dark[i]) *
+		    flatscale / flat[i]
+	case FDZ: # flat field + dark count + zero level
+	    do i = 1, n
+		out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+		    flatscale / flat[i]
+	case FDZO: # flat field + dark count + zero level + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - zero[i] -
+		    darkscale * dark[i]) * flatscale / flat[i]
+	}
+
+	# Often these operations will not be performed so test for no
+	# correction rather than go through the switch.
+
+	op = cors[ILLUMCOR] + cors[FRINGECOR]
+	if (op != 0) {
+	    switch (op) {
+	    case I: # illumination
+	        do i = 1, n
+		    out[i] = out[i] * illumscale / illum[i]
+	    case Q: # fringe
+	        do i = 1, n
+		    out[i] = out[i] - frgscale * fringe[i]
+	    case QI: # fringe + illumination
+	        do i = 1, n
+		    out[i] = out[i]*illumscale/illum[i] - frgscale*fringe[i]
+	    }
+	}
+end
+
+
+# COR2 -- Correct lines for readout axis 2 (columns).  This procedure is
+# more complex than when the readout is along the image lines because the
+# zero level and/or flat field corrections may be single readout column
+# vectors.
+
+procedure cor2$t (line, cors, out, overscan, zero, dark, flat, illum,
+	fringe, n, zeroim, flatim, darkscale, flatscale, illumscale, frgscale)
+
+int	line		# Line to be corrected
+int	cors[ARB]	# Correction flags
+PIXEL	out[n]		# Output data
+real	overscan[n]	# Overscan value
+PIXEL	zero[n]		# Zero level correction
+PIXEL	dark[n]		# Dark count correction
+PIXEL	flat[n]		# Flat field correction
+PIXEL	illum[n]	# Illumination correction
+PIXEL	fringe[n]	# Fringe correction
+int	n		# Number of pixels
+pointer	zeroim		# Zero level IMIO pointer (NULL if 1D vector)
+pointer	flatim		# Flat field IMIO pointer (NULL if 1D vector)
+real	darkscale	# Dark count scale factor
+real	flatscale	# Flat field scale factor
+real	illumscale	# Illumination scale factor
+real	frgscale	# Fringe scale factor
+
+PIXEL	zeroval
+real	flatval
+int	i, op
+
+begin
+	op = cors[OVERSCAN] + cors[ZEROCOR] + cors[DARKCOR] + cors[FLATCOR]
+	switch (op) {
+	case O: # overscan
+	    do i = 1, n
+	        out[i] = out[i] - overscan[i]
+	case Z: # zero level
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - zero[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - zeroval
+	    }
+
+	case ZO: # zero level + overscan
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zero[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zeroval
+	    }
+
+	case D: # dark count
+	    do i = 1, n
+		out[i] = out[i] - darkscale * dark[i]
+	case DO: # dark count + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan[i] - darkscale * dark[i]
+	case DZ: # dark count + zero level
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - zero[i] - darkscale * dark[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - zeroval - darkscale * dark[i]
+	    }
+	case DZO: # dark count + zero level + overscan
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zero[i] -
+			darkscale * dark[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zeroval -
+			darkscale * dark[i]
+	    }
+
+	case F: # flat field
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = out[i] * flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = out[i] * flatval
+	    }
+	case FO: # flat field + overscan
+	    if (flatim != NULL) {
+	        do i = 1, n
+	            out[i] = (out[i] - overscan[i]) * flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+	            out[i] = (out[i] - overscan[i]) * flatval
+	    }
+	case FZ: # flat field + zero level
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i]) * flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval) * flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval) * flatval
+		}
+	    }
+	case FZO: # flat field + zero level + overscan
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i]) *
+			    flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval) *
+			    flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval) * flatval
+		}
+	    }
+	case FD: # flat field + dark count
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = (out[i] - darkscale * dark[i]) * flatscale/flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = (out[i] - darkscale * dark[i]) * flatval
+	    }
+	case FDO: # flat field + dark count + overscan
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = (out[i] - overscan[i] - darkscale * dark[i]) *
+		        flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = (out[i] - overscan[i] - darkscale * dark[i]) *
+		        flatval
+	    }
+	case FDZ: # flat field + dark count + zero level
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+			    flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval - darkscale * dark[i]) *
+			    flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+			    flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval - darkscale * dark[i]) *
+			    flatval
+		}
+	    }
+	case FDZO: # flat field + dark count + zero level + overscan
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i] -
+			    darkscale * dark[i]) * flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval -
+			    darkscale * dark[i]) * flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i] -
+			    darkscale * dark[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval -
+			    darkscale * dark[i]) * flatval
+		}
+	    }
+	}
+
+	# Often these operations will not be performed so test for no
+	# correction rather than go through the switch.
+
+	op = cors[ILLUMCOR] + cors[FRINGECOR]
+	if (op != 0) {
+	    switch (op) {
+	    case I: # illumination
+	        do i = 1, n
+		    out[i] = out[i] * illumscale / illum[i]
+	    case Q: # fringe
+	        do i = 1, n
+		    out[i] = out[i] - frgscale * fringe[i]
+	    case QI: # fringe + illumination
+	        do i = 1, n
+		    out[i] = out[i]*illumscale/illum[i] - frgscale*fringe[i]
+	    }
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/cosmic/cosmicrays.hlp b/noao/imred/ccdred/src/cosmic/cosmicrays.hlp
new file mode 100644
index 00000000..bfb56e9c
--- /dev/null
+++ b/noao/imred/ccdred/src/cosmic/cosmicrays.hlp
@@ -0,0 +1,338 @@
+.help cosmicrays Dec87 noao.imred.ccdred
+.ih
+NAME
+cosmicrays -- Detect and replace cosmic rays
+.ih
+USAGE
+cosmicrays input output
+.ih
+PARAMETERS
+.ls input
+List of input images in which to detect cosmic rays.
+.le
+.ls output
+List of output images in which the detected cosmic rays will be replaced
+by an average of neighboring pixels.  If the output image name differs
+from the input image name then a copy of the input image is made with
+the detected cosmic rays replaced.  If no output images are specified
+then the input images are modified in place.  In place modification of
+an input image also occurs when the output image name is the same as
+the input image name.
+.le
+.ls badpix = ""
+List of bad pixel files to be created, one for each input image.  If no
+file names are given then no bad pixel file is created.  The bad pixel 
+file is a simple list of pixel coordinates for each replaced cosmic ray.
+This file may be used in conjunction with \fBbadpixelimage\fR to create
+a mask image.
+.le
+
+.ls ccdtype = ""
+If specified only the input images of the desired CCD image type will be
+selected.
+.le
+.ls threshold = 25.
+Detection threshold above the mean of the surrounding pixels for cosmic
+rays.  The threshold will depend on the noise characteristics of the
+image and how weak the cosmic rays may be for detection.  A typical value
+is 5 or more times the sigma of the background.
+.le
+.ls fluxratio = 2.
+The ratio (as a percent) of the mean neighboring pixel flux to the candidate
+cosmic ray pixel for rejection.  The value depends on the seeing and the
+characteristics of the cosmic rays.  Typical values are in the range
+2 to 10 percent.  This value may be reset interactively from a plot
+or defined by identifying selected objects as stars or cosmic rays.
+.le
+.ls npasses = 5
+Number of cosmic ray detection passes.  Since only the locally strongest
+pixel is considered a cosmic ray, multiple detection passes are needed to
+detect and replace multiple pixel cosmic ray events.
+.le
+.ls window = 5
+Size of cosmic ray detection window.  A square window of either 5 by 5 or
+7 by 7 is used to detect cosmic rays.  The smaller window allows detection
+in the presence of greater background gradients but is less sensitive at
+discriminating multiple event cosmic rays from stars.  It is also marginally
+faster.
+.le
+.ls interactive = yes
+Examine parameters interactively?  A plot of the mean flux within the
+detection window (x100) vs the flux ratio (x100) is plotted and the user may
+set the flux ratio threshold, delete and undelete specific events, and
+examine specific events.  This is useful for new data in which one is
+uncertain of an appropriate flux ratio threshold.  Once determined the
+task need not be used interactively.
+.le
+.ls train = no
+Define the flux ratio threshold by using a set of objects identified
+as stars (or other astronomical objects) or cosmic rays?
+.le
+.ls objects = ""
+Cursor list of coordinates of training objects.  If null (the null string "")
+then the image display cursor will be read.  The user is responsible for first
+displaying the image.  Otherwise a file containing cursor coordinates
+may be given.  The format of the cursor file is "x y wcs key" where
+x and y are the pixel coordinates, wcs is an arbitrary number such as 1,
+and key may be 's' for star or 'c' for cosmic ray.
+.le
+.ls savefile = ""
+File to save (by appending) the training object coordinates.  This is of
+use when the objects are identified using the image display cursor.  The
+saved file can then be input as the object cursor list for repeating the
+execution.
+.le
+.ls answer
+This parameter is used for interactive queries when processing a list of
+images.  The responses may be "no", "yes", "NO", or "YES".  The upper case
+responses permanently enable or disable the interactive review while
+the lower case reponses allow selective examination of certain input
+images.  \fIThis parameter should not be specified on the command line.
+If it is then the value will be ignored and the task will act as if
+the answer "yes" is given for each image; i.e. it will enter the interactive
+phase without prompting.\fR
+.le
+.ih
+OTHER PARAMETERS
+There are other parameters which may be defined by the package, as is the
+case with \fBccdred\fR, or as part of the task, as is the case with
+standalone version in the \fBgeneric\fR package.
+
+.ls verbose
+If yes then a time stamped log of the operation is printed on the standard
+output.
+.le
+.ls logfile
+If a log file is specified then a time stamped log of the operation is
+recorded.
+.le
+.ls plotfile
+If a plot file is specified then the graph of the flux ratio (x100) vs
+the mean flux (x100) is recorded as metacode.  This may be spooled or examined
+later.
+.le
+.ls graphics = "stdgraph"
+Interactive graphic output device for interactive examination of the
+detection parameters.
+.le
+.ls cursor = ""
+Interactive graphics cursor input.  If null the graphics display cursor
+is used, otherwise a file containing cursor input may be specified.
+.le
+.ls instrument
+The \fBccdred\fR instrument file is used for mapping header keywords and
+CCD image types.
+.le
+.ih
+IMAGE CURSOR COMMANDS
+
+.nf
+?	Help
+c	Identify the object as a cosmic ray
+s	Identify the object as a star
+g	Switch to the graphics plot
+q	Quit and continue with the cleaning
+.fi
+
+GRAPHICS CURSOR COMMANDS
+
+.nf
+?	Help
+a	Toggle between showing all candidates and only the training points
+d	Mark candidate for replacement (applys to '+' points)
+q	Quit and return to image cursor or replace the selected pixels
+r	Redraw the graph
+s	Make a surface plot for the candidate nearest the cursor
+t	Set the flux ratio threshold at the y cursor position
+u	Mark candidate to not be replaced (applys to 'x' points)
+w	Adjust the graph window (see \fBgtools\fR)
+<space>	Print the pixel coordinates
+.fi
+
+There are no colon commands except those for the windowing options (type
+:\help or see \fBgtools\fR).
+.ih
+DESCRIPTION
+Cosmic ray events in each input image are detected and replaced by the
+average of the four neighbors.  The replacement may be performed
+directly on the input image if no output image is specified or if the
+output image name is the same as the input image name.  If a new image
+is created it is a copy of the input image except for the replaced
+pixels.  The processing keyword CRCOR is added to the output image
+header.  Optional output includes a log file to which a processing log
+is appended, a verbose log output to the standard output (the same as
+that in the log file), a plot file showing the parameters of the
+detected cosmic ray candidates and the flux ratio threshold used, a
+bad pixel file containing the coordinates of the replaced pixels, and
+a file of training objects marked with the image display cursor.  The
+bad pixel file may be used for plotting purposes or to create a mask
+image for display and analysis using the task \fBbadpiximage\fR.  This
+bad pixel file will be replaced by the IRAF bad pixel facility when it
+becomes available.  If one wants more than a simple mask image then by
+creating a different output image a difference image between the
+original and the modified image may be made using \fBimarith\fR.
+
+This task may be applied to an image previously processed to detect
+additional cosmic rays.  A warning will be given (because of the
+CRCOR header parameter) and the previous processing header keyword will
+be overwritten.
+
+The cosmic ray detection algorithm consists of the following steps.
+First a pixel must be the brightest pixel within the specified
+detection window (either 5x5 or 7x7).  The mean flux in the surrounding
+pixels with the second brightest pixel excluded (which may also be a
+cosmic ray event) is computed and the candidate pixel must exceed this
+mean by the amount specified by the parameter \fIthreshold\fR.  A plane
+is fit to the border pixels of the window and the fitted background is
+subtracted.  The mean flux (now background subtracted) and the ratio of
+this mean to the cosmic ray candidate (the brightest pixel) are
+computed.  The mean flux (x100) and the ratio (x100) are recorded for
+interactive examination if desired.
+
+Once the list of cosmic ray candidates has been created and a threshold for
+the flux ratio established (by the parameter \fIfluxratio\fR, by the
+"training" method, or by using the graphics cursor in the interactive plot)
+the pixels with ratios below the threshold are replaced in the output by
+the average of the four neighboring pixels (with the second strongest pixel
+in the detection window excluded if it is one of these pixels).  Additonal
+pixels may then be detected and replaced in further passes as specified by
+the parameter \fInpasses\fR.  Note that only pixels in the vicinity of
+replaced pixels need be considered in further passes.
+
+The division between the peaks of real objects and cosmic rays is made
+based on the flux ratio between the mean flux (excluding the center
+pixel and the second strongest pixel) and the candidate pixel.  This
+threshold depends on the point spread function and the distribution of
+multiple cosmic ray events and any additional neighboring light caused
+by the events.  This threshold is not strongly coupled to small changes
+in the data so that once it is set for a new type of image data it may
+be used for similar images.  To set it initially one may examine the
+scatter plot of the flux ratio as a function of the mean flux.  This
+may be done interactively or from the optional plot file produced.
+
+After the initial list of cosmic ray candidates has been created and before
+the final replacing cosmic rays there are two optional steps to allow
+examining the candidates and setting the flux ratio threshold dividing
+cosmic rays from real objects.  The first optional step is define the flux
+ratio boundary by reference to user specified classifications; that is
+"training".  To do this step the \fItrain\fR parameter must be set to yes.
+The user classified objects are specified by a cursor input list.  This
+list can be an actual file or the image display cursor as defined by the
+\fIobjects\fR parameter.  The \fIsavefile\fR parameter is also used during
+the training to record the objects specified.  The parameter specifies a
+file to append the objects selected.  This is useful when the objects are
+defined by interactive image cursor and does not make much sense when using
+an input list.
+
+If the \fIobjects\fR parameter is specified as a null string then
+the image display cursor will be repeatedly read until a 'q' is
+entered.  The user first displays the image and then when the task
+reads the display cursor the cursor shape will change.  The user
+points at objects and types 's' for a star (or other astronomical
+object) and 'c' for a cosmic ray.  Note that this input is used
+to search for the matching object in the cosmic ray candidate list
+and so it is possible the selected object is not in the list though
+it is unlikely.  The selection will be quietly ignored in that case.
+To exit the interactive selection of training objects type 'q'.
+
+If 'g' is typed a graph of all the candidates is drawn showing
+"flux" vs. "flux ratio" (see below for more).  Training objects will
+be shown with a box and the currently set flux ratio threshold will
+also be shown.  Exiting the plot will return to entering more training
+objects.  The plot will remain and additional objects will immediately
+be shown with a new box.  Thus, if one wants to see the training
+objects identified in the plot as one selects them from the image
+display first type a 'g' to draw the initial plot.  Also by switching
+to the plot with 'g' allows you to draw surface plots (with 's') or
+get the pixel coordinates of a candidate (the space key) to be
+found in the display using the coordinate readout of the display.
+Note that the display interaction is simpler than might be desired
+because this task does not directly connect to the display.
+
+The most likely use for training is with the interactive image display.
+However one may prepare an input list by other means, one example
+is with \fBrimcursor\fR, and then specify the file name.  The savefile
+may also be used a cursor input to repeat the cosmic ray operation
+(but be careful not to have the cursor input and save file be the
+same file!).
+
+The flux ratio threshold is determined from the training objects by
+finding the point with the minimum number of misclassifications
+(stars as cosmic rays or cosmic rays as stars).  The threshold is
+set at the lowest value so that it will always go through one of
+the cosmic ray objects.  There should be at least one of each type
+of object defined for this to work.  The following option of
+examining the cosmic ray candidates and parameters may still be
+used to modify the derived flux ratio threshold.  One last point
+about the training objects is that even if some of the points
+lie on the wrong side of the threshold they will remain classified
+as cosmic ray or non-cosmic ray.  In other words, any object
+classified by the user will remain in that classification regardless
+of the final flux ratio threshold.
+
+After the training step the user will be queried to examine the candidates
+in the flux vs flux ratio plane if the \fIinteractive\fR flag is set.
+Responses may be made for specific images or for all images by using
+lower or upper case answers respectively.  When the parameters are
+examined interactively the user may change the flux ratio threshold
+('t' key).  Changes made are stored in the parameter file and, thus,
+learned for further images.  Pixels to be deleted are marked by crosses
+and pixels which are peaks of objects are marked by pluses.  The user
+may explicitly delete or undelete any point if desired but this is only
+for special cases near the threshold.  In the future keys for
+interactive display of the specific detections will be added.
+Currently a surface plot of any candidate may be displayed graphically
+in four 90 degree rotated views using the 's' key.  Note that the
+initial graph does not show all the points some of which are clearly
+cosmic rays because they have negative mean flux or flux ratio.  To
+view all data one must rewindow the graph with the 'w' key or ":/"
+commands (see \fBgtools\fR).
+.ih
+EXAMPLES
+1. To replace cosmic rays in a set of images ccd* without training:
+
+.nf
+    cl> cosmicrays ccd* new//ccd*
+    ccd001: Examine parameters interactively? (yes):
+    [A scatter plot graph is made.  One can adjust the threshold.]
+    [Looking at a few points using the 's' key can be instructive.]
+    [When done type 'q'.]
+    ccd002: Examine parameters interactively? (yes): NO
+    [No further interactive examination is done.]
+.fi
+
+After cleaning one typically displays the images and  possibly blinks them.
+A difference image or mask image may also be created.
+
+2. To use the interactive training method for setting the flux ratio threshold:
+
+.nf
+    # First display the image.
+    cl> display ccd001 1
+    z1 = 123.45 z2= 543.21
+    cl> cosmicrays ccd001 ccd001cr train+
+    [After the cosmic ray candidates are found the image display
+    [cursor will be activated.  Mark a cosmic ray with 'c' and
+    [a star with 's'.  Type 'g' to get a plot showing the two
+    [points with boxes.  Type 'q' to go back to the image display.
+    [As each new object is marked a box will appear in the plot and
+    [the threshold may change.  To find the location of an object
+    [seen in the plot use 'g' to go to the graph, space key to find
+    [the pixel coordinates, 'q' to go back to the image display,
+    [and the image display coordinate box to find the object.
+    [When done with the training type 'q'.
+    ccd001: Examine parameters interactively? (yes): no
+.fi
+
+3.  To create a mask image a bad pixel file must be specified.  In the
+following we replace the cosmic rays in place and create a bad pixel
+file and mask image:
+
+.nf
+    cl> cosmicrays ccd001 ccd001 badpix=ccd001.bp
+    cl> badpiximage ccd001.bp ccd001 ccd001bp
+.fi
+.ih
+SEE ALSO
+badpixelimage gtools imedit rimcursor
+.endhelp
diff --git a/noao/imred/ccdred/src/cosmic/crexamine.x b/noao/imred/ccdred/src/cosmic/crexamine.x
new file mode 100644
index 00000000..d84961bc
--- /dev/null
+++ b/noao/imred/ccdred/src/cosmic/crexamine.x
@@ -0,0 +1,486 @@
+include	<error.h>
+include	<syserr.h>
+include <imhdr.h>
+include	<gset.h>
+include	<mach.h>
+include	<pkg/gtools.h>
+include	"crlist.h"
+
+# CR_EXAMINE  -- Examine cosmic ray candidates interactively.
+# CR_GRAPH    -- Make a graph
+# CR_NEAREST  -- Find the nearest cosmic ray to the cursor.
+# CR_DELETE   -- Set replace flag for cosmic ray candidate nearest cursor.
+# CR_UNDELETE -- Set no replace flag for cosmic ray candidate nearest cursor.
+# CR_UPDATE   -- Change replacement flags, thresholds, and graphs.
+# CR_PLOT     -- Make log plot
+
+define	HELP	"noao$lib/scr/cosmicrays.key"
+define	PROMPT	"cosmic ray options"
+
+# CR_EXAMINE -- Examine cosmic ray candidates interactively.
+
+procedure cr_examine (cr, gp, gt, im, fluxratio, first)
+
+pointer	cr			# Cosmic ray list
+pointer	gp			# GIO pointer
+pointer	gt			# GTOOLS pointer
+pointer	im			# Image pointer
+real	fluxratio		# Flux ratio threshold
+int	first			# Initial key
+
+char	cmd[SZ_LINE]
+int	i, newgraph, wcs, key, nc, nl, c1, c2, l1, l2, show
+real	wx, wy
+pointer	data
+
+int	clgcur()
+pointer	imgs2r()
+
+begin
+	# Set up the graphics.
+	call gt_sets (gt, GTPARAMS, IM_TITLE(im))
+
+	# Set image limits
+	nc = IM_LEN(im, 1)
+	nl = IM_LEN(im, 2)
+
+	# Enter cursor loop.
+	key = first
+	repeat {
+	    switch (key) {
+	    case '?': # Print help text.
+		call gpagefile (gp, HELP, PROMPT)
+	    case ':': # Colon commands.
+		switch (cmd[1]) {
+		case '/':
+		    call gt_colon (cmd, gp, gt, newgraph)
+		default:
+		    call printf ("\007")
+		}
+	    case 'a': # Toggle show all
+		if (show == 0)
+		    show = 1
+		else
+		    show = 0
+		newgraph = YES
+	    case 'd': # Delete candidate
+		call cr_delete (gp, wx, wy, cr, i, show)
+	    case 'q': # Quit
+		break
+	    case 'r': # Redraw the graph.
+		newgraph = YES
+	    case 's': # Make surface plots
+		call cr_nearest (gp, wx, wy, cr, i, show)
+		c1 = max (1, int (Memr[CR_COL(cr)+i-1]) - 5)
+		c2 = min (nc, int (Memr[CR_COL(cr)+i-1]) + 5)
+		l1 = max (1, int (Memr[CR_LINE(cr)+i-1]) - 5)
+		l2 = min (nl, int (Memr[CR_LINE(cr)+i-1]) + 5)
+		data = imgs2r (im, c1, c2, l1, l2)
+		call gclear (gp)
+		call gsview (gp, 0.03, 0.48, 0.53, 0.98)
+		call cr_surface (gp, Memr[data], c2-c1+1, l2-l1+1, -33., 25.)
+		call gsview (gp, 0.53, 0.98, 0.53, 0.98)
+		call cr_surface (gp, Memr[data], c2-c1+1, l2-l1+1, -123., 25.)
+		call gsview (gp, 0.03, 0.48, 0.03, 0.48)
+		call cr_surface (gp, Memr[data], c2-c1+1, l2-l1+1, 57., 25.)
+		call gsview (gp, 0.53, 0.98, 0.03, 0.48)
+		call cr_surface (gp, Memr[data], c2-c1+1, l2-l1+1, 147., 25.)
+		call fprintf (STDERR, "[Type any key to continue]")
+		i = clgcur ("cursor", wx, wy, wcs, key, cmd, SZ_LINE)
+		newgraph = YES
+	    case 't': # Set threshold
+		call cr_update (gp, wy, cr, fluxratio, show)
+		call clputr ("fluxratio", fluxratio)
+	    case 'u': # Undelete candidate
+		call cr_undelete (gp, wx, wy, cr, i, show)
+	    case 'w':# Window the graph.
+		call gt_window (gt, gp, "cursor", newgraph)
+	    case ' ': # Print info
+		call cr_nearest (gp, wx, wy, cr, i, show)
+		call printf ("%d %d\n")
+		    call pargr (Memr[CR_COL(cr)+i-1])
+		    call pargr (Memr[CR_LINE(cr)+i-1])
+	    case 'z': # NOP
+		newgraph = NO
+	    default: # Ring bell for unrecognized commands.
+		call printf ("\007")
+	    }
+
+	    # Update the graph if needed.
+	    if (newgraph == YES) {
+		call cr_graph (gp, gt, cr, fluxratio, show)
+	        newgraph = NO
+	    }
+	} until (clgcur ("cursor", wx, wy, wcs, key, cmd, SZ_LINE) == EOF)
+end
+
+
+# CR_GRAPH -- Make a graph
+
+procedure cr_graph (gp, gt, cr, fluxratio, show)
+
+pointer	gp		# GIO pointer
+pointer	gt		# GTOOLS pointers
+pointer	cr		# Cosmic ray list
+real	fluxratio	# Flux ratio threshold
+int	show		# Show (0=all, 1=train)
+
+int	i, ncr
+real	x1, x2, y1, y2
+pointer	sp, x, y, w, flag, index
+
+begin
+	call smark (sp)
+
+	call cr_show (show, cr, x, y, w, flag, index, ncr)
+	if (ncr == 0) {
+	    call sfree (sp)
+	    return
+	}
+
+	call gclear (gp)
+	call gt_ascale (gp, gt, Memr[x+1], Memr[y+1], ncr)
+	call gt_swind (gp, gt)
+	call gt_labax (gp, gt)
+
+	do i = 1, ncr {
+	    if ((Memi[flag+i] == NO) || (Memi[flag+i] == ALWAYSNO))
+		call gmark (gp, Memr[x+i], Memr[y+i], GM_PLUS, 2., 2.)
+	    else
+		call gmark (gp, Memr[x+i], Memr[y+i], GM_CROSS, 2., 2.)
+	    if (Memr[w+i] != 0.)
+		call gmark (gp, Memr[x+i], Memr[y+i], GM_BOX, 2., 2.)
+	}
+
+	call ggwind (gp, x1, x2, y1, y2)
+	call gseti (gp, G_PLTYPE, 2)
+	call gline (gp, x1, fluxratio, x2, fluxratio)
+
+	call sfree (sp)
+end
+
+
+# CR_NEAREST -- Find the nearest cosmic ray to the cursor.
+
+procedure cr_nearest (gp, wx, wy, cr, nearest, show)
+
+pointer	gp		# GIO pointer
+real	wx, wy		# Cursor position
+pointer	cr		# Cosmic ray list
+int	nearest		# Index of nearest point (returned)
+int	show		# Show (0=all, 1=train)
+
+int	i, ncr
+real	x0, y0, x1, y1, x2, y2, r2, r2min
+pointer	sp, x, y, w, flag, index
+
+begin
+	call smark (sp)
+
+	call cr_show (show, cr, x, y, w, flag, index, ncr)
+	if (ncr == 0) {
+	    call sfree (sp)
+	    return
+	}
+
+	# Search for nearest point in NDC.
+	r2min = MAX_REAL
+	call gctran (gp, wx, wy, wx, wy, 1, 0)
+	do i = 1, ncr {
+	    x1 = Memr[x+i]
+	    y1 = Memr[y+i]
+	    call gctran (gp, x1, y1, x0, y0, 1, 0)
+	    r2 = (x0 - wx) ** 2 + (y0 - wy) ** 2
+	    if (r2 < r2min) {
+		r2min = r2
+		x2 = x1
+		y2 = y1
+		nearest = i
+	    }
+	}
+	if (index != NULL)
+	    nearest = Memi[index+nearest]
+
+	# Move the cursor to the selected point.
+	call gscur (gp, x2, y2)
+
+	call sfree (sp)
+end
+
+
+# CR_DELETE -- Set replace flag for cosmic ray candidate nearest cursor.
+
+procedure cr_delete (gp, wx, wy, cr, nearest, show)
+
+pointer	gp		# GIO pointer
+real	wx, wy		# Cursor position
+pointer	cr		# Cosmic ray list
+int	nearest		# Index of nearest point (returned)
+int	show		# Show (0=all, 1=train)
+
+int	i, ncr
+real	x0, y0, x1, y1, x2, y2, r2, r2min
+pointer	sp, x, y, w, flag, index
+
+begin
+	call smark (sp)
+
+	call cr_show (show, cr, x, y, w, flag, index, ncr)
+	if (ncr == 0) {
+	    call sfree (sp)
+	    return
+	}
+
+	# Search for nearest point in NDC.
+	nearest = 0
+	r2min = MAX_REAL
+	call gctran (gp, wx, wy, wx, wy, 1, 0)
+	do i = 1, ncr {
+	    if ((Memi[flag+i] == YES) || (Memi[flag+i] == ALWAYSYES))
+		next
+	    x1 = Memr[x+i]
+	    y1 = Memr[y+i]
+	    call gctran (gp, x1, y1, x0, y0, 1, 0)
+	    r2 = (x0 - wx) ** 2 + (y0 - wy) ** 2
+	    if (r2 < r2min) {
+		r2min = r2
+		x2 = x1
+		y2 = y1
+		nearest = i
+	    }
+	}
+
+	# Move the cursor to the selected point and mark the deleted point.
+	if (nearest > 0) {
+	    if (index != NULL)
+		nearest = Memi[index+nearest]
+	    Memi[CR_FLAG(cr)+nearest-1] = ALWAYSYES
+	    Memi[CR_WT(cr)+nearest-1] = -1
+	    call gscur (gp, x2, y2)
+	    call gseti (gp, G_PMLTYPE, 0)
+	    y2 = Memr[CR_RATIO(cr)+nearest-1]
+	    call gmark (gp, x2, y2, GM_PLUS, 2., 2.)
+	    call gseti (gp, G_PMLTYPE, 1)
+	    call gmark (gp, x2, y2, GM_CROSS, 2., 2.)
+	}
+
+	call sfree (sp)
+end
+
+
+# CR_UNDELETE -- Set no replace flag for cosmic ray candidate nearest cursor.
+
+procedure cr_undelete (gp, wx, wy, cr, nearest, show)
+
+pointer	gp		# GIO pointer
+real	wx, wy		# Cursor position
+pointer	cr		# Cosmic ray list
+int	nearest		# Index of nearest point (returned)
+int	show		# Show (0=all, 1=train)
+
+int	i, ncr
+real	x0, y0, x1, y1, x2, y2, r2, r2min
+pointer	sp, x, y, w, flag, index
+
+begin
+	call smark (sp)
+
+	call cr_show (show, cr, x, y, w, flag, index, ncr)
+	if (ncr == 0) {
+	    call sfree (sp)
+	    return
+	}
+
+	# Search for nearest point in NDC.
+	nearest = 0
+	r2min = MAX_REAL
+	call gctran (gp, wx, wy, wx, wy, 1, 0)
+	do i = 1, ncr {
+	    if ((Memi[flag+i] == NO) || (Memi[flag+i] == ALWAYSNO))
+		next
+	    x1 = Memr[x+i]
+	    y1 = Memr[y+i]
+	    call gctran (gp, x1, y1, x0, y0, 1, 0)
+	    r2 = (x0 - wx) ** 2 + (y0 - wy) ** 2
+	    if (r2 < r2min) {
+		r2min = r2
+		x2 = x1
+		y2 = y1
+		nearest = i
+	    }
+	}
+
+	# Move the cursor to the selected point and mark the delete point.
+	if (nearest > 0) {
+	    if (index != NULL)
+		nearest = Memi[index+nearest]
+	    Memi[CR_FLAG(cr)+nearest-1] = ALWAYSNO
+	    Memi[CR_WT(cr)+nearest-1] = 1
+	    call gscur (gp, x2, y2)
+
+	    call gseti (gp, G_PMLTYPE, 0)
+	    y2 = Memr[CR_RATIO(cr)+nearest-1]
+	    call gmark (gp, x2, y2, GM_CROSS, 2., 2.)
+	    call gseti (gp, G_PMLTYPE, 1)
+	    call gmark (gp, x2, y2, GM_PLUS, 2., 2.)
+	}
+
+	call sfree (sp)
+end
+
+
+# CR_UPDATE -- Change replacement flags, thresholds, and graphs.
+
+procedure cr_update (gp, wy, cr, fluxratio, show)
+
+pointer	gp		# GIO pointer
+real	wy		# Y cursor position
+pointer	cr		# Cosmic ray list
+real	fluxratio	# Flux ratio threshold
+int	show		# Show (0=all, 1=train)
+
+int	i, ncr, flag
+real	x1, x2, y1, y2
+pointer	x, y, f
+
+begin
+	call gseti (gp, G_PLTYPE, 0)
+	call ggwind (gp, x1, x2, y1, y2)
+	call gline (gp, x1, fluxratio, x2, fluxratio)
+	fluxratio = wy
+	call gseti (gp, G_PLTYPE, 2)
+	call gline (gp, x1, fluxratio, x2, fluxratio)
+
+	if (show == 1)
+	    return
+
+	ncr = CR_NCR(cr)
+	x = CR_FLUX(cr) - 1
+	y = CR_RATIO(cr) - 1
+	f = CR_FLAG(cr) - 1
+
+	do i = 1, ncr {
+	    flag = Memi[f+i]
+	    if ((flag == ALWAYSYES) || (flag == ALWAYSNO))
+		next
+	    x1 = Memr[x+i]
+	    y1 = Memr[y+i]
+	    if (flag == NO) {
+	        if (y1 < fluxratio) {
+		    Memi[f+i] = YES
+		    call gseti (gp, G_PMLTYPE, 0)
+		    call gmark (gp, x1, y1, GM_PLUS, 2., 2.)
+		    call gseti (gp, G_PMLTYPE, 1)
+		    call gmark (gp, x1, y1, GM_CROSS, 2., 2.)
+		}
+	    } else {
+	        if (y1 >= fluxratio) {
+		    Memi[f+i] = NO
+		    call gseti (gp, G_PMLTYPE, 0)
+		    call gmark (gp, x1, y1, GM_CROSS, 2., 2.)
+		    call gseti (gp, G_PMLTYPE, 1)
+		    call gmark (gp, x1, y1, GM_PLUS, 2., 2.)
+		}
+	    }
+	}
+end
+
+
+# CR_PLOT -- Make log plot
+
+procedure cr_plot (cr, im, fluxratio)
+
+pointer	cr			# Cosmic ray list
+pointer	im			# Image pointer
+real	fluxratio		# Flux ratio threshold
+
+int	fd, open(), errcode()
+pointer	sp, fname, gp, gt, gopen(), gt_init()
+errchk	gopen
+
+begin
+	call smark (sp)
+	call salloc (fname, SZ_FNAME, TY_CHAR)
+
+	# Open the plotfile.
+	call clgstr ("plotfile", Memc[fname], SZ_FNAME)
+	iferr (fd = open (Memc[fname], APPEND, BINARY_FILE)) {
+	    if (errcode() != SYS_FNOFNAME)
+		call erract (EA_WARN)
+	    return
+	}
+
+	# Set up the graphics.
+	gp = gopen ("stdplot", NEW_FILE, fd)
+	gt = gt_init()
+	call gt_sets (gt, GTTYPE, "mark")
+	call gt_sets (gt, GTXTRAN, "log")
+	call gt_setr (gt, GTXMIN, 10.)
+	call gt_setr (gt, GTYMIN, 0.)
+	call gt_sets (gt, GTTITLE, "Parameters of cosmic rays candidates")
+	call gt_sets (gt, GTPARAMS, IM_TITLE(im))
+	call gt_sets (gt, GTXLABEL, "Flux")
+	call gt_sets (gt, GTYLABEL, "Flux Ratio")
+
+	call cr_graph (gp, gt, cr, fluxratio, 'r')
+
+	call gt_free (gt)
+	call gclose (gp)
+	call close (fd)
+	call sfree (sp)
+end
+
+
+# CR_SHOW -- Select data to show.
+# This returns pointers to the data.  Note the pointers are salloc from
+# the last smark which is done by the calling program.
+
+procedure cr_show (show, cr, x, y, w, flag, index, ncr)
+
+int	show		#I Data to show (0=all, 1=train)
+pointer	cr		#I CR data
+pointer	x		#O Fluxes
+pointer	y		#O Ratios
+pointer	w		#O Weights
+pointer	flag		#O Flags
+pointer	index		#O Index into CR data (if not null)
+int	ncr		#O Number of selected data points
+
+int	i
+
+begin
+	switch (show) {
+	case 0:
+	    ncr = CR_NCR(cr)
+	    x = CR_FLUX(cr) - 1
+	    y = CR_RATIO(cr) - 1
+	    w = CR_WT(cr) - 1
+	    flag = CR_FLAG(cr) - 1
+	    index = NULL
+	case 1:
+	    ncr = CR_NCR(cr)
+	    call salloc (x, ncr, TY_REAL)
+	    call salloc (y, ncr, TY_REAL)
+	    call salloc (w, ncr, TY_REAL)
+	    call salloc (flag, ncr, TY_INT)
+	    call salloc (index, ncr, TY_INT)
+
+	    ncr = 0
+	    x = x - 1
+	    y = y - 1
+	    w = w - 1
+	    flag = flag - 1
+	    index = index - 1
+
+	    do i = 1, CR_NCR(cr) {
+		if (Memr[CR_WT(cr)+i-1] == 0.)
+		    next
+		ncr = ncr + 1
+		Memr[x+ncr] = Memr[CR_FLUX(cr)+i-1]
+		Memr[y+ncr] = Memr[CR_RATIO(cr)+i-1]
+		Memr[w+ncr] = Memr[CR_WT(cr)+i-1]
+		Memi[flag+ncr] = Memi[CR_FLAG(cr)+i-1]
+		Memi[index+ncr] = i
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/src/cosmic/crfind.x b/noao/imred/ccdred/src/cosmic/crfind.x
new file mode 100644
index 00000000..58850940
--- /dev/null
+++ b/noao/imred/ccdred/src/cosmic/crfind.x
@@ -0,0 +1,305 @@
+include	<math/gsurfit.h>
+
+# CR_FIND -- Find cosmic ray candidates.
+# This procedure is an interface to special procedures specific to a given
+# window size.
+
+procedure cr_find (cr, threshold, data, nc, nl, col, line,
+    sf1, sf2, x, y, z, w)
+
+pointer	cr						# Cosmic ray list
+real	threshold					# Detection threshold
+pointer	data[ARB]					# Data lines
+int	nc						# Number of columns
+int	nl						# Number of lines
+int	col						# First column
+int	line						# Center line
+pointer	sf1, sf2					# Surface fitting
+real	x[ARB], y[ARB], z[ARB], w[ARB]			# Surface arrays
+
+pointer	a, b, c, d, e, f, g
+
+begin
+	switch (nl) {
+	case 5:
+	    a = data[1]
+	    b = data[2]
+	    c = data[3]
+	    d = data[4]
+	    e = data[5]
+	    call cr_find5 (cr, threshold,  col, line, Memr[a], Memr[b],
+		Memr[c], Memr[d], Memr[e], nc, sf1, sf2, x, y, z, w)
+	case 7:
+	    a = data[1]
+	    b = data[2]
+	    c = data[3]
+	    d = data[4]
+	    e = data[5]
+	    f = data[6]
+	    g = data[7]
+	    call cr_find7 (cr, threshold,  col, line, Memr[a], Memr[b],
+		Memr[c], Memr[d], Memr[e], Memr[f], Memr[g], nc,
+		sf1, sf2, x, y, z, w)
+	}
+end
+
+
+# CR_FIND7 -- Find cosmic rays candidates in 7x7 window.
+# This routine finds cosmic rays candidates with the following algorithm.
+#    1. If the pixel is not a local maximum relative to it's 48 neighbors
+#	go on to the next pixel.
+#    2. Identify the next strongest pixel in the 7x7 region.
+#	This suspect pixel is excluded in the following.
+#    2. Compute the flux of the 7x7 region excluding the cosmic ray
+#	candidate and the suspect pixel.
+#    3. The candidate must exceed the average flux per pixel by a specified
+#	threshold.  If not go on to the next pixel.
+#    4. Fit a plane to the border pixels (excluding the suspect pixel).
+#    5. Subtract the background defined by the plane.
+#    6. Determine a replacement value as the average of the four adjacent
+#	pixels (excluding the suspect pixels).
+#    7. Add the pixel to the cosmic ray candidate list.
+
+procedure cr_find7 (cr, threshold, col, line, a, b, c, d, e, f, g, n,
+	sf1, sf2, x, y, z, w)
+
+pointer	cr						# Cosmic ray list
+real	threshold					# Detection threshold
+int	col						# First column
+int	line						# Line
+real	a[ARB], b[ARB], c[ARB], d[ARB]			# Image lines
+real	e[ARB], f[ARB], g[ARB]				# Image lines
+int	n						# Number of columns
+pointer	sf1, sf2					# Surface fitting
+real	x[49], y[49], z[49], w[49]			# Surface arrays
+
+real	bkgd[49] 
+int	i1, i2, i3, i4, i5, i6, i7, j, j1, j2
+real	p, flux, replace, asumr()
+pointer	sf
+
+begin
+	for (i4=4; i4<=n-3; i4=i4+1) {
+	    # Must be local maxima.
+	    p = d[i4]
+	    if (p<a[i4]||p<b[i4]||p<c[i4]||p<e[i4]||p<f[i4]||p<g[i4])
+		next
+	    i1 = i4 - 3
+	    if (p<a[i1]||p<b[i1]||p<c[i1]||p<d[i1]||p<e[i1]||p<f[i1]||p<g[i1])
+		next
+	    i2 = i4 - 2
+	    if (p<a[i2]||p<b[i2]||p<c[i2]||p<d[i2]||p<e[i2]||p<f[i2]||p<g[i2])
+		next
+	    i3 = i4 - 1
+	    if (p<a[i3]||p<b[i3]||p<c[i3]||p<d[i3]||p<e[i3]||p<f[i3]||p<g[i3])
+		next
+	    i5 = i4 + 1
+	    if (p<a[i5]||p<b[i5]||p<c[i5]||p<d[i5]||p<e[i5]||p<f[i5]||p<g[i5])
+		next
+	    i6 = i4 + 2
+	    if (p<a[i6]||p<b[i6]||p<c[i6]||p<d[i6]||p<e[i6]||p<f[i6]||p<g[i6])
+		next
+	    i7 = i4 + 3
+	    if (p<a[i7]||p<b[i7]||p<c[i7]||p<d[i7]||p<e[i7]||p<f[i7]||p<g[i7])
+		next
+
+	    # Convert to a single array in surface fitting order. 
+	    call amovr (a[i1], z[1], 7)
+	    z[8] = b[i7]; z[9] = c[i7]; z[10] = d[i7]; z[11] = e[i7]
+	    z[12] = f[i7]; z[13] = g[i7]; z[14] = g[i6]; z[15] = g[i5]
+	    z[16] = f[i4]; z[17] = g[i3]; z[18] = g[i2]; z[19] = g[i1]
+	    z[20] = f[i1]; z[21] = e[i1]; z[22] = d[i1]; z[23] = c[i1]
+	    z[24] = b[i1]
+	    call amovr (b[i2], z[25], 5)
+	    call amovr (c[i2], z[30], 5)
+	    call amovr (d[i2], z[35], 5)
+	    call amovr (e[i2], z[40], 5)
+	    call amovr (f[i2], z[45], 5)
+
+	    # Find the highest point excluding the center.
+	    j1 = 37; j2 = 1
+	    do j = 2, 49 {
+		if (j == j1)
+		    next
+		if (z[j] > z[j2])
+		    j2 = j 
+	    }
+
+	    # Compute the flux excluding the extreme points.
+	    flux = (asumr (z, 49) - z[j1] - z[j2]) / 47
+
+	    # Pixel must be exceed specified threshold.
+	    if (p < flux + threshold)
+		next
+
+	    # Fit and subtract the background.
+	    if (j2 < 25) {
+	        w[j2] = 0
+		sf = sf2
+	        call gsfit (sf, x, y, z, w, 24, WTS_USER, j)
+		w[j2] = 1
+	    } else {
+		sf = sf1
+	        call gsrefit (sf, x, y, z, w, j)
+	    }
+
+	    call gsvector (sf, x, y, bkgd, 49)
+	    call asubr (z, bkgd, z, 49)
+	    p = z[j1]
+
+	    # Compute the flux excluding the extreme points.
+	    flux = (asumr (z, 49) - z[j1] - z[j2]) / 47
+
+	    # Determine replacement value from four nearest neighbors again
+	    # excluding the most deviant pixels.
+	    replace = 0
+	    j = 0
+	    if (j2 != 32) {
+		replace = replace + c[i4]
+		j = j + 1
+	    }
+	    if (j2 != 36) {
+		replace = replace + d[i3]
+		j = j + 1
+	    }
+	    if (j2 != 38) {
+		replace = replace + d[i5]
+		j = j + 1
+	    }
+	    if (j2 != 42) {
+		replace = replace + e[i4]
+		j = j + 1
+	    }
+	    replace = replace / j
+
+	    # Add pixel to cosmic ray list.
+	    flux = 100. * flux
+	    call cr_add (cr, col+i4-1, line, flux, flux/p, 0., replace, 0)
+	    i4 = i7
+	}
+end
+
+
+# CR_FIND5 -- Find cosmic rays candidates in 5x5 window.
+# This routine finds cosmic rays candidates with the following algorithm.
+#    1. If the pixel is not a local maximum relative to it's 24 neighbors
+#	go on to the next pixel.
+#    2. Identify the next strongest pixel in the 5x5 region.
+#	This suspect pixel is excluded in the following.
+#    2. Compute the flux of the 5x5 region excluding the cosmic ray
+#	candidate and the suspect pixel.
+#    3. The candidate must exceed the average flux per pixel by a specified
+#	threshold.  If not go on to the next pixel.
+#    4. Fit a plane to the border pixels (excluding the suspect pixel).
+#    5. Subtract the background defined by the plane.
+#    6. Determine a replacement value as the average of the four adjacent
+#	pixels (excluding the suspect pixels).
+#    7. Add the pixel to the cosmic ray candidate list.
+
+procedure cr_find5 (cr, threshold, col, line, a, b, c, d, e, n,
+	sf1, sf2, x, y, z, w)
+
+pointer	cr						# Cosmic ray list
+real	threshold					# Detection threshold
+int	col						# First column
+int	line						# Line
+real	a[ARB], b[ARB], c[ARB], d[ARB], e[ARB]		# Image lines
+int	n						# Number of columns
+pointer	sf1, sf2					# Surface fitting
+real	x[25], y[25], z[25], w[25]			# Surface arrays
+
+real	bkgd[25] 
+int	i1, i2, i3, i4, i5, j, j1, j2
+real	p, flux, replace, asumr()
+pointer	sf
+
+begin
+	for (i3=3; i3<=n-2; i3=i3+1) {
+	    # Must be local maxima.
+	    p = c[i3]
+	    if (p<a[i3]||p<b[i3]||p<d[i3]||p<e[i3])
+		next
+	    i1 = i3 - 2
+	    if (p<a[i1]||p<b[i1]||p<c[i1]||p<d[i1]||p<e[i1])
+		next
+	    i2 = i3 - 1
+	    if (p<a[i2]||p<b[i2]||p<c[i2]||p<d[i2]||p<e[i2])
+		next
+	    i4 = i3 + 1
+	    if (p<a[i4]||p<b[i4]||p<c[i4]||p<d[i4]||p<e[i4])
+		next
+	    i5 = i3 + 2
+	    if (p<a[i5]||p<b[i5]||p<c[i5]||p<d[i5]||p<e[i5])
+		next
+
+	    # Convert to a single array in surface fitting order. 
+	    call amovr (a[i1], z[1], 5)
+	    z[6] = b[i5]; z[7] = c[i5]; z[8] = d[i5]; z[9] = e[i5]
+	    z[10] = e[i4]; z[11] = e[i3]; z[12] = e[i2]; z[13] = e[i1]
+	    z[14] = d[i1]; z[15] = c[i1]; z[16] = b[i1]
+	    call amovr (b[i2], z[17], 3)
+	    call amovr (c[i2], z[20], 3)
+	    call amovr (d[i2], z[23], 3)
+
+	    # Find the highest point excluding the center.
+	    j1 = 21; j2 = 1
+	    do j = 2, 25 {
+		if (j == j1)
+		    next
+		if (z[j] > z[j2])
+		    j2 = j 
+	    }
+
+	    # Compute the flux excluding the extreme points.
+	    flux = (asumr (z, 25) - z[j1] - z[j2]) / 23
+
+	    # Pixel must be exceed specified threshold.
+	    if (p < flux + threshold)
+		next
+
+	    # Fit and subtract the background.
+	    if (j2 < 17) {
+	        w[j2] = 0
+		sf = sf2
+	        call gsfit (sf, x, y, z, w, 16, WTS_USER, j)
+		w[j2] = 1
+	    } else {
+		sf = sf1
+	        call gsrefit (sf, x, y, z, w, j)
+	    }
+
+	    call gsvector (sf, x, y, bkgd, 25)
+	    call asubr (z, bkgd, z, 25)
+	    p = z[j1]
+
+	    # Compute the flux excluding the extreme points.
+	    flux = (asumr (z, 25) - z[j1] - z[j2]) / 23
+
+	    # Determine replacement value from four nearest neighbors again
+	    # excluding the most deviant pixels.
+	    replace = 0
+	    j = 0
+	    if (j2 != 18) {
+		replace = replace + b[i3]
+		j = j + 1
+	    }
+	    if (j2 != 20) {
+		replace = replace + c[i2]
+		j = j + 1
+	    }
+	    if (j2 != 22) {
+		replace = replace + c[i4]
+		j = j + 1
+	    }
+	    if (j2 != 24) {
+		replace = replace + d[i3]
+		j = j + 1
+	    }
+	    replace = replace / j
+
+	    # Add pixel to cosmic ray list.
+	    flux = 100. * flux
+	    call cr_add (cr, col+i3-1, line, flux, flux/p, 0., replace, 0)
+	    i3 = i5
+	}
+end
diff --git a/noao/imred/ccdred/src/cosmic/crlist.h b/noao/imred/ccdred/src/cosmic/crlist.h
new file mode 100644
index 00000000..1ed498a7
--- /dev/null
+++ b/noao/imred/ccdred/src/cosmic/crlist.h
@@ -0,0 +1,17 @@
+define	CR_ALLOC	100		# Allocation block size
+define	CR_LENSTRUCT	9		# Length of structure
+
+define	CR_NCR		Memi[$1]	# Number of cosmic rays
+define	CR_NALLOC	Memi[$1+1]	# Length of cosmic ray list
+define	CR_COL		Memi[$1+2]	# Pointer to columns
+define	CR_LINE		Memi[$1+3]	# Pointer to lines
+define	CR_FLUX		Memi[$1+4]	# Pointer to fluxes
+define	CR_RATIO	Memi[$1+5]	# Pointer to flux ratios
+define	CR_WT		Memi[$1+6]	# Pointer to training weights
+define	CR_REPLACE	Memi[$1+7]	# Pointer to replacement values
+define	CR_FLAG		Memi[$1+8]	# Pointer to rejection flag
+
+define	ALWAYSNO	3
+define	ALWAYSYES	4
+
+define	CR_RMAX		3.		# Maximum radius for matching
diff --git a/noao/imred/ccdred/src/cosmic/crlist.x b/noao/imred/ccdred/src/cosmic/crlist.x
new file mode 100644
index 00000000..e0a8fd5c
--- /dev/null
+++ b/noao/imred/ccdred/src/cosmic/crlist.x
@@ -0,0 +1,366 @@
+include	<error.h>
+include	<syserr.h>
+include	<gset.h>
+include	"crlist.h"
+
+define	HELP	"noao$lib/scr/cosmicrays.key"
+define	PROMPT	"cosmic ray options"
+
+# CR_OPEN    -- Open cosmic ray list
+# CR_CLOSE   -- Close cosmic ray list
+# CR_ADD     -- Add a cosmic ray candidate to cosmic ray list.
+# CR_TRAIN   -- Set flux ratio threshold from a training set.
+# CR_FINDTHRESH -- Find flux ratio.
+# CR_WEIGHT  -- Compute the training weight at a particular flux ratio.
+# CR_FLAGS   -- Set cosmic ray reject flags.
+# CR_BADPIX  -- Store cosmic rays in bad pixel list.
+# CR_REPLACE -- Replace cosmic rays in image with replacement values.
+
+# CR_OPEN -- Open cosmic ray list
+
+procedure cr_open (cr)
+
+pointer	cr		# Cosmic ray list pointer
+errchk	malloc
+
+begin
+	call malloc (cr, CR_LENSTRUCT, TY_STRUCT)
+	call malloc (CR_COL(cr), CR_ALLOC, TY_REAL)
+	call malloc (CR_LINE(cr), CR_ALLOC, TY_REAL)
+	call malloc (CR_FLUX(cr), CR_ALLOC, TY_REAL)
+	call malloc (CR_RATIO(cr), CR_ALLOC, TY_REAL)
+	call malloc (CR_WT(cr), CR_ALLOC, TY_REAL)
+	call malloc (CR_REPLACE(cr), CR_ALLOC, TY_REAL)
+	call malloc (CR_FLAG(cr), CR_ALLOC, TY_INT)
+	CR_NCR(cr) = 0
+	CR_NALLOC(cr) = CR_ALLOC
+end
+
+
+# CR_CLOSE -- Close cosmic ray list
+
+procedure cr_close (cr)
+
+pointer	cr		# Cosmic ray list pointer
+
+begin
+	call mfree (CR_COL(cr), TY_REAL)
+	call mfree (CR_LINE(cr), TY_REAL)
+	call mfree (CR_FLUX(cr), TY_REAL)
+	call mfree (CR_RATIO(cr), TY_REAL)
+	call mfree (CR_WT(cr), TY_REAL)
+	call mfree (CR_REPLACE(cr), TY_REAL)
+	call mfree (CR_FLAG(cr), TY_INT)
+	call mfree (cr, TY_STRUCT)
+end
+
+# CR_ADD -- Add a cosmic ray candidate to cosmic ray list.
+
+procedure cr_add (cr, col, line, flux, ratio, wt, replace, flag)
+
+pointer	cr		# Cosmic ray list pointer
+int	col		# Cofluxn
+int	line		# Line
+real	flux		# Luminosity
+real	ratio		# Ratio
+real	wt		# Weight
+real	replace		# Sky value
+int	flag		# Flag value
+
+int	ncr
+errchk	realloc
+
+begin
+	if (CR_NCR(cr) == CR_NALLOC(cr)) {
+	    CR_NALLOC(cr) = CR_NALLOC(cr) + CR_ALLOC
+	    call realloc (CR_COL(cr), CR_NALLOC(cr), TY_REAL)
+	    call realloc (CR_LINE(cr), CR_NALLOC(cr), TY_REAL)
+	    call realloc (CR_FLUX(cr), CR_NALLOC(cr), TY_REAL)
+	    call realloc (CR_RATIO(cr), CR_NALLOC(cr), TY_REAL)
+	    call realloc (CR_WT(cr), CR_NALLOC(cr), TY_REAL)
+	    call realloc (CR_REPLACE(cr), CR_NALLOC(cr), TY_REAL)
+	    call realloc (CR_FLAG(cr), CR_NALLOC(cr), TY_INT)
+	}
+
+	ncr = CR_NCR(cr)
+	CR_NCR(cr) = ncr + 1
+	Memr[CR_COL(cr)+ncr] = col
+	Memr[CR_LINE(cr)+ncr] = line
+	Memr[CR_FLUX(cr)+ncr] = flux
+	Memr[CR_RATIO(cr)+ncr] = ratio
+	Memr[CR_WT(cr)+ncr] = wt
+	Memr[CR_REPLACE(cr)+ncr] = replace
+	Memi[CR_FLAG(cr)+ncr] = flag
+end
+
+
+# CR_TRAIN -- Set flux ratio threshold from a training set.
+
+procedure cr_train (cr, gp, gt, im, fluxratio, fname)
+
+pointer	cr		#I Cosmic ray list
+pointer	gp		#I GIO pointer
+pointer	gt		#I GTOOLS pointer
+pointer	im		#I IMIO pointer
+real	fluxratio	#O Flux ratio threshold
+char	fname[ARB]	#I Save file name
+
+char	cmd[10]
+bool	gflag
+real	x, y, y1, y2, w, r, rmin
+int	i, j, n, f, ncr, wcs, key, fd, clgcur(), open(), errcode()
+pointer	col, line, ratio, flux, wt, flag
+
+begin
+	# Open save file
+	iferr (fd = open (fname, APPEND, TEXT_FILE)) {
+	    if (errcode() != SYS_FNOFNAME)
+		call erract (EA_WARN)
+	    fd = 0
+	}
+
+	ncr = CR_NCR(cr)
+	col = CR_COL(cr) - 1
+	line = CR_LINE(cr) - 1
+	flux = CR_FLUX(cr) - 1
+	ratio = CR_RATIO(cr) - 1
+	wt = CR_WT(cr) - 1
+	flag = CR_FLAG(cr) - 1
+
+	gflag = false
+	n = 0
+	while (clgcur ("objects", x, y, wcs, key, cmd, 10) != EOF) {
+	    switch (key) {
+	    case '?':
+		call gpagefile (gp, HELP, PROMPT)
+		next
+	    case 'q':
+		break
+	    case 's':
+		w = 1
+		f = ALWAYSNO
+	    case 'c':
+		w = -1
+		f = ALWAYSYES
+	    case 'g':
+		if (gflag)
+		    call cr_examine (cr, gp, gt, im, fluxratio, 'z')
+		else {
+		    if (n > 1)
+			call cr_findthresh (cr, fluxratio)
+		    call cr_flags (cr, fluxratio)
+		    call cr_examine (cr, gp, gt, im, fluxratio, 'r')
+		    gflag = true
+		}
+		next
+	    default:
+		next
+	    }
+
+	    y1 = y - CR_RMAX
+	    y2 = y + CR_RMAX
+	    for (i=10; i<ncr && y1>Memr[line+i]; i=i+10)
+		;
+	    j = i - 9
+	    rmin = (Memr[col+j] - x) ** 2 + (Memr[line+j] - y) ** 2
+	    for (i=j+1; i<ncr && y2>Memr[line+i]; i=i+1) {
+		r = (Memr[col+i] - x) ** 2 + (Memr[line+i] - y) ** 2
+		if (r < rmin) {
+		    rmin = r
+		    j = i
+		}
+	    }
+	    if (sqrt (rmin) > CR_RMAX)
+		next
+
+	    Memr[wt+j] = w
+	    Memi[flag+j] = f
+	    n = n + 1
+
+	    if (gflag) {
+		if (n > 1) {
+		    call cr_findthresh (cr, r)
+		    call cr_update (gp, r, cr, fluxratio, 0)
+		}
+		call gmark (gp, Memr[flux+j], Memr[ratio+j], GM_BOX, 2., 2.)
+	    }
+	    if (fd > 0) {
+		call fprintf (fd, "%g %g %d %c\n")
+		    call pargr (x)
+		    call pargr (y)
+		    call pargi (wcs)
+		    call pargi (key)
+	    }
+	}
+
+	if (fd > 0)
+	    call close (fd)
+end
+
+
+# CR_FINDTHRESH -- Find flux ratio.
+
+procedure cr_findthresh (cr, fluxratio)
+
+pointer	cr		#I Cosmic ray list
+real	fluxratio	#O Flux ratio threshold
+
+real	w, r, rmin, cr_weight()
+int	i, ncr
+pointer	ratio, wt
+
+begin
+	ncr = CR_NCR(cr)
+	ratio = CR_RATIO(cr) - 1
+	wt = CR_WT(cr) - 1
+
+	fluxratio = Memr[ratio+1]
+	rmin = cr_weight (fluxratio, Memr[ratio+1], Memr[wt+1], ncr)
+	do i = 2, ncr {
+	    if (Memr[wt+i] == 0.)
+		next
+	    r = Memr[ratio+i]
+	    w = cr_weight (r, Memr[ratio+1], Memr[wt+1], ncr)
+	    if (w <= rmin) {
+		if (w == rmin)
+		    fluxratio = min (fluxratio, r)
+		else {
+		    rmin = w
+		    fluxratio = r
+		}
+	    }
+	}
+end
+
+
+# CR_WEIGHT -- Compute the training weight at a particular flux ratio.
+
+real procedure cr_weight (fluxratio, ratio, wts, ncr)
+
+real	fluxratio		#I Flux ratio
+real	ratio[ARB]		#I Ratio Values
+real	wts[ARB]		#I Weights
+int	ncr			#I Number of ratio values
+real	wt			#O Sum of weights
+
+int	i
+
+begin
+	wt = 0.
+	do i = 1, ncr {
+	    if (ratio[i] > fluxratio) {
+		if (wts[i] < 0.)
+		    wt = wt - wts[i]
+	    } else {
+		if (wts[i] > 0.)
+		    wt = wt + wts[i]
+	    }
+	}
+	return (wt)
+end
+
+
+# CR_FLAGS -- Set cosmic ray reject flags.
+
+procedure cr_flags (cr, fluxratio)
+
+pointer	cr			# Cosmic ray candidate list
+real	fluxratio		# Rejection limits
+
+int	i, ncr
+pointer	ratio, flag
+
+begin
+	ncr = CR_NCR(cr)
+	ratio = CR_RATIO(cr) - 1
+	flag = CR_FLAG(cr) - 1
+
+	do i = 1, ncr {
+	    if ((Memi[flag+i] == ALWAYSYES) || (Memi[flag+i] == ALWAYSNO))
+		next
+	    if (Memr[ratio+i] > fluxratio)
+		Memi[flag+i] = NO
+	    else
+		Memi[flag+i] = YES
+	}
+end
+
+
+# CR_BADPIX -- Store cosmic rays in bad pixel list.
+# This is currently a temporary measure until a real bad pixel list is
+# implemented.
+
+procedure cr_badpix (cr, fname)
+
+pointer	cr		# Cosmic ray list
+char	fname[ARB]	# Bad pixel file name
+
+int	i, ncr, c, l, f, fd, open(), errcode()
+pointer	col, line, ratio, flux, flag
+errchk	open
+
+begin
+	# Open bad pixel file
+	iferr (fd = open (fname, APPEND, TEXT_FILE)) {
+	    if (errcode() != SYS_FNOFNAME)
+		call erract (EA_WARN)
+	    return
+	}
+
+	ncr = CR_NCR(cr)
+	col = CR_COL(cr) - 1
+	line = CR_LINE(cr) - 1
+	flux = CR_FLUX(cr) - 1
+	ratio = CR_RATIO(cr) - 1
+	flag = CR_FLAG(cr) - 1
+
+	do i = 1, ncr {
+	    f = Memi[flag+i]
+	    if ((f == NO) || (f == ALWAYSNO))
+		next
+
+	    c = Memr[col+i]
+	    l = Memr[line+i]
+	    call fprintf (fd, "%d %d\n")
+	        call pargi (c)
+	        call pargi (l)
+	}
+	call close (fd)
+end
+
+
+# CR_REPLACE -- Replace cosmic rays in image with replacement values.
+
+procedure cr_replace (cr, offset, im, nreplaced)
+
+pointer	cr		# Cosmic ray list
+int	offset		# Offset in list
+pointer	im		# IMIO pointer of output image
+int	nreplaced	# Number replaced (for log)
+
+int	i, ncr, c, l, f
+real	r
+pointer	col, line, replace, flag, imps2r()
+
+begin
+	ncr = CR_NCR(cr)
+	if (ncr <= offset)
+	    return
+
+	col = CR_COL(cr) - 1
+	line = CR_LINE(cr) - 1
+	replace = CR_REPLACE(cr) - 1
+	flag = CR_FLAG(cr) - 1
+
+	do i = offset+1, ncr {
+	    f = Memi[flag+i]
+	    if ((f == NO) || (f == ALWAYSNO))
+		next
+
+	    c = Memr[col+i]
+	    l = Memr[line+i]
+	    r = Memr[replace+i]
+	    Memr[imps2r (im, c, c, l, l)] = r
+	    nreplaced = nreplaced + 1
+	}
+end
diff --git a/noao/imred/ccdred/src/cosmic/crsurface.x b/noao/imred/ccdred/src/cosmic/crsurface.x
new file mode 100644
index 00000000..32645ff4
--- /dev/null
+++ b/noao/imred/ccdred/src/cosmic/crsurface.x
@@ -0,0 +1,46 @@
+define	DUMMY	6
+
+# CR_SURFACE -- Draw a perspective view of a surface.  The altitude
+# and azimuth of the viewing angle are variable.
+
+procedure cr_surface(gp, data, ncols, nlines, angh, angv)
+
+pointer	gp			# GIO pointer
+real	data[ncols,nlines]	# Surface data to be plotted
+int	ncols, nlines		# Dimensions of surface
+real	angh, angv		# Orientation of surface (degrees)
+
+int	wkid
+pointer	sp, work
+
+int	first
+real	vpx1, vpx2, vpy1, vpy2
+common  /frstfg/ first
+common  /noaovp/ vpx1, vpx2, vpy1, vpy2
+
+begin
+	call smark (sp)
+	call salloc (work, 2 * (2 * ncols * nlines + ncols + nlines), TY_REAL)
+
+	# Initialize surface common blocks
+	first = 1
+	call srfabd()
+
+	# Define viewport.
+	call ggview (gp, vpx1, vpx2, vpy1, vpy2) 
+
+	# Link GKS to GIO
+	wkid = 1
+	call gopks (STDERR)
+	call gopwk (wkid, DUMMY, gp)
+	call gacwk (wkid)
+
+	call ezsrfc (data, ncols, nlines, angh, angv, Memr[work])
+
+	call gdawk (wkid)
+	# We don't want to close the GIO pointer.
+	#call gclwk (wkid)
+	call gclks ()
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/cosmic/mkpkg b/noao/imred/ccdred/src/cosmic/mkpkg
new file mode 100644
index 00000000..d63d9c2c
--- /dev/null
+++ b/noao/imred/ccdred/src/cosmic/mkpkg
@@ -0,0 +1,16 @@
+# COSMIC RAY CLEANING
+
+$checkout libpkg.a ../..
+$update   libpkg.a
+$checkin  libpkg.a ../..
+$exit
+
+libpkg.a:
+	crexamine.x	crlist.h <error.h> <gset.h> <mach.h> <pkg/gtools.h>\
+			<imhdr.h> <syserr.h>
+	crfind.x	<math/gsurfit.h>
+	crlist.x	crlist.h <error.h> <gset.h> <syserr.h>
+	crsurface.x	
+	t_cosmicrays.x	crlist.h <error.h> <gset.h> <math/gsurfit.h>\
+			<pkg/gtools.h> <imhdr.h> <imset.h>
+	;
diff --git a/noao/imred/ccdred/src/cosmic/t_cosmicrays.x b/noao/imred/ccdred/src/cosmic/t_cosmicrays.x
new file mode 100644
index 00000000..8640b639
--- /dev/null
+++ b/noao/imred/ccdred/src/cosmic/t_cosmicrays.x
@@ -0,0 +1,348 @@
+include	<error.h>
+include <imhdr.h>
+include <imset.h>
+include	<math/gsurfit.h>
+include	<gset.h>
+include	<pkg/gtools.h>
+include	"crlist.h"
+
+# T_COSMICRAYS -- Detect and remove cosmic rays in images.
+# A list of images is examined for cosmic rays which are then replaced
+# by values from neighboring pixels.  The output image may be the same
+# as the input image.  This is the top level procedure which manages
+# the input and output image data.  The actual algorithm for detecting
+# cosmic rays is in CR_FIND.
+
+procedure t_cosmicrays ()
+
+int	list1			# List of input images to be cleaned
+int	list2			# List of output images
+int	list3			# List of output bad pixel files
+real	threshold		# Detection threshold
+real	fluxratio		# Luminosity boundary for stars
+int	npasses			# Number of cleaning passes
+int	szwin			# Size of detection window
+bool	train			# Use training objects?
+pointer	savefile		# Save file for training objects
+bool	interactive		# Examine cosmic ray parameters?
+char	ans			# Answer to interactive query
+
+int	nc, nl, c, c1, c2, l, l1, l2, szhwin, szwin2
+int	i, j, k, m, ncr, ncrlast, nreplaced, flag
+pointer	sp, input, output, badpix, str, gp, gt, im, in, out
+pointer	x, y, z, w, sf1, sf2, cr, data, ptr
+
+bool	clgetb(), ccdflag(), streq(), strne()
+char	clgetc()
+int	imtopenp(), imtlen(), imtgetim(), clpopnu(), clgfil(), clgeti()
+real	clgetr()
+pointer	immap(), impl2r(), imgs2r(), gopen(), gt_init()
+errchk	immap, impl2r, imgs2r
+errchk	cr_find, cr_examine, cr_replace, cr_plot, cr_badpix
+
+begin
+	call smark (sp)
+	call salloc (input, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (badpix, SZ_FNAME, TY_CHAR)
+	call salloc (savefile, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the task parameters.  Check that the number of output images
+	# is either zero, in which case the cosmic rays will be removed
+	# in place, or equal to the number of input images.
+
+	list1 = imtopenp ("input")
+	list2 = imtopenp ("output")
+	i = imtlen (list1)
+	j = imtlen (list2)
+	if (j > 0 && j != i)
+	    call error (0, "Input and output image lists do not match")
+
+	list3 = clpopnu ("badpix")
+	threshold = clgetr ("threshold")
+	fluxratio = clgetr ("fluxratio")
+	npasses = clgeti ("npasses")
+	szwin = clgeti ("window")
+	train = clgetb ("train")
+	call clgstr ("savefile", Memc[savefile], SZ_FNAME)
+	interactive = clgetb ("interactive")
+	call clpstr ("answer", "yes")
+	ans = 'y'
+
+	# Set up the graphics.
+	call clgstr ("graphics", Memc[str], SZ_LINE)
+	if (interactive) {
+	    gp = gopen (Memc[str], NEW_FILE+AW_DEFER, STDGRAPH)
+	    gt = gt_init()
+	    call gt_sets (gt, GTTYPE, "mark")
+	    call gt_sets (gt, GTXTRAN, "log")
+	    call gt_setr (gt, GTXMIN, 10.)
+	    call gt_setr (gt, GTYMIN, 0.)
+	    call gt_sets (gt, GTTITLE, "Parameters of cosmic rays candidates")
+	    call gt_sets (gt, GTXLABEL, "Flux")
+	    call gt_sets (gt, GTYLABEL, "Flux Ratio")
+	}
+
+	# Use image header translation file.
+	call clgstr ("instrument", Memc[input], SZ_FNAME)
+	call hdmopen (Memc[input])
+
+	# Set up surface fitting.  The background points are placed together
+	# at the beginning of the arrays.  There are two surface pointers,
+	# one for using the fast refit if there are no points excluded and
+	# one for doing a full fit with points excluded.
+
+	szhwin = szwin / 2
+	szwin2 = szwin * szwin
+	call salloc (data, szwin, TY_INT)
+	call salloc (x, szwin2, TY_REAL)
+	call salloc (y, szwin2, TY_REAL)
+	call salloc (z, szwin2, TY_REAL)
+	call salloc (w, szwin2, TY_REAL)
+
+	k = 0
+	do i = 1, szwin {
+	    Memr[x+k] = i
+	    Memr[y+k] = 1
+	    k = k + 1
+	}
+	do i = 2, szwin {
+	    Memr[x+k] = szwin
+	    Memr[y+k] = i
+	    k = k + 1
+	}
+	do i = szwin-1, 1, -1 {
+	    Memr[x+k] = i
+	    Memr[y+k] = szwin
+	    k = k + 1
+	}
+	do i = szwin-1, 2, -1 {
+	    Memr[x+k] = 1
+	    Memr[y+k] = i
+	    k = k + 1
+	}
+	do i = 2, szwin-1 {
+	    do j = 2, szwin-1 {
+	        Memr[x+k] = j
+	        Memr[y+k] = i
+	        k = k + 1
+	    }
+	}
+	call aclrr (Memr[z], szwin2)
+	call amovkr (1., Memr[w], 4*szwin-4)
+	call gsinit (sf1, GS_POLYNOMIAL, 2, 2, NO, 1., real(szwin),
+	    1., real(szwin))
+	call gsinit (sf2, GS_POLYNOMIAL, 2, 2, NO, 1., real(szwin),
+	    1., real(szwin))
+	call gsfit (sf1, Memr[x], Memr[y], Memr[z], Memr[w], 4*szwin-4,
+	    WTS_USER, j)
+
+	# Process each input image.  Either work in place or create a
+	# new output image.  If an error mapping the images occurs
+	# issue a warning and go on to the next input image.
+
+	while (imtgetim (list1, Memc[input], SZ_FNAME) != EOF) {
+	    if (imtgetim (list2, Memc[output], SZ_FNAME) == EOF)
+		call strcpy (Memc[input], Memc[output], SZ_FNAME)
+	    if (clgfil (list3, Memc[badpix], SZ_FNAME) == EOF)
+		Memc[badpix] = EOS
+
+	    iferr {
+		in = NULL
+		out = NULL
+		cr = NULL
+
+		# Map the input image and check for image type and
+		# previous correction flag.  If the output image is
+		# the same as the input image work in place.
+		# Initialize IMIO to use a scrolling buffer of lines.
+
+		call set_input (Memc[input], im, i)
+		if (im == NULL)
+		    call error (1, "Skipping input image")
+
+		if (ccdflag (im, "crcor")) {
+		    call eprintf ("WARNING: %s previously corrected\n")
+			call pargstr (Memc[input])
+		    #call imunmap (im)
+		    #next
+		}
+
+	        if (streq (Memc[input], Memc[output])) {
+		    call imunmap (im)
+	            im = immap (Memc[input], READ_WRITE, 0)
+		}
+		in = im
+
+	        nc = IM_LEN(in,1)
+	        nl = IM_LEN(in,2)
+	        if ((nl < szwin) || (nc < szwin))
+	            call error (0, "Image size is too small")
+	        call imseti (in, IM_NBUFS, szwin)
+	        call imseti (in, IM_TYBNDRY, BT_NEAREST)
+	        call imseti (in, IM_NBNDRYPIX, szhwin)
+
+		# Open the output image if needed.
+	        if (strne (Memc[input], Memc[output]))
+		    im = immap (Memc[output], NEW_COPY, in)
+		out = im
+
+		# Open a cosmic ray list structure.
+	        call cr_open (cr)
+		ncrlast = 0
+		nreplaced = 0
+
+		# Now proceed through the image line by line, scrolling
+		# the line buffers at each step.  If creating a new image
+		# also write out each line as it is read.  A procedure is
+		# called to find the cosmic ray candidates in the line
+		# and add them to the list maintained by CRLIST.
+		# Note that cosmic rays are not replaced at this point
+		# in order to allow the user to modify the criteria for
+		# a cosmic ray and review the results.
+
+	        c1 = 1-szhwin
+	        c2 = nc+szhwin
+		do i = 1, szwin-1 
+		    Memi[data+i] =
+			imgs2r (in, c1, c2, i-szhwin, i-szhwin)
+
+	        do l = 1, nl {
+		    do i = 1, szwin-1
+			Memi[data+i-1] = Memi[data+i]
+		    Memi[data+szwin-1] =
+			imgs2r (in, c1, c2, l+szhwin, l+szhwin)
+		    if (out != in)
+		        call amovr (Memr[Memi[data+szhwin]+szhwin],
+			    Memr[impl2r(out,l)], nc)
+
+	            call cr_find (cr, threshold, Memi[data],
+		        c2-c1+1, szwin, c1, l,
+		        sf1, sf2, Memr[x], Memr[y], Memr[z], Memr[w])
+	        }
+		if (interactive && train) {
+		    call cr_train (cr, gp, gt, in, fluxratio, Memc[savefile])
+		    train = false
+		}
+	        call cr_flags (cr, fluxratio)
+
+		# If desired examine the cosmic ray list interactively.
+	        if (interactive && ans != 'N') {
+		    if (ans != 'Y') {
+		        call eprintf ("%s - ")
+		            call pargstr (Memc[input])
+		        call flush (STDERR)
+		        ans = clgetc ("answer")
+		    }
+		    if ((ans == 'Y') || (ans == 'y'))
+	                call cr_examine (cr, gp, gt, in, fluxratio, 'r')
+	        }
+
+		# Now replace the selected cosmic rays in the output image.
+
+		call imflush (out)
+		call imseti (out, IM_ADVICE, RANDOM)
+	        call cr_replace (cr, ncrlast, out, nreplaced)
+
+		# Do additional passes through the data.  We work in place
+		# in the output image.  Note that we only have to look in
+		# the vicinity of replaced cosmic rays for secondary
+		# events since we've already looked at every pixel once.
+		# Instead of scrolling through the image we will extract
+		# subrasters around each replaced cosmic ray.  However,
+		# we use pointers into the subraster to maintain the same
+		# format expected by CR_FIND.
+
+	        if (npasses > 1) {
+	            if (out != in)
+	                call imunmap (out)
+	            call imunmap (in)
+		    im = immap (Memc[output], READ_WRITE, 0)
+		    in = im
+		    out = im
+	            call imseti (in, IM_TYBNDRY, BT_NEAREST)
+	            call imseti (in, IM_NBNDRYPIX, szhwin)
+
+	            for (i=2; i<=npasses; i=i+1) {
+			# Loop through each cosmic ray in the previous pass.
+		        ncr = CR_NCR(cr)
+		        do j = ncrlast+1, ncr {
+			    flag = Memi[CR_FLAG(cr)+j-1]
+			    if (flag==NO || flag==ALWAYSNO)
+			        next
+			    c = Memr[CR_COL(cr)+j-1]
+			    l = Memr[CR_LINE(cr)+j-1]
+			    c1 = max (1-szhwin, c - (szwin-1))
+			    c2 = min (nc+szhwin, c + (szwin-1))
+			    k = c2 - c1 + 1
+			    l1 = max (1-szhwin, l - (szwin-1))
+			    l2 = min (nl+szhwin, l + (szwin-1))
+
+			    # Set the line pointers off an image section
+			    # centered on a previously replaced cosmic ray.
+
+			    ptr = imgs2r (in, c1, c2, l1, l2) - k
+
+			    l1 = max (1, l - szhwin)
+			    l2 = min (nl, l + szhwin)
+			    do l = l1, l2 {
+				do m = 1, szwin
+				    Memi[data+m-1] = ptr + m * k
+				ptr = ptr + k
+
+	                        call cr_find ( cr, threshold, Memi[data],
+				    k, szwin, c1, l, sf1, sf2,
+				    Memr[x], Memr[y], Memr[z], Memr[w])
+			    }
+	                }
+		        call cr_flags (cr, fluxratio)
+
+			# Replace any new cosmic rays found.
+	                call cr_replace (cr, ncr, in, nreplaced)
+			ncrlast = ncr
+		    }
+	        }
+
+		# Output header log, log, plot, and bad pixels.
+		call sprintf (Memc[str], SZ_LINE,
+		    "Threshold=%5.1f, fluxratio=%6.2f, removed=%d")
+		    call pargr (threshold)
+		    call pargr (fluxratio)
+		    call pargi (nreplaced)
+		call timelog (Memc[str], SZ_LINE)
+		call ccdlog (out, Memc[str])
+		call hdmpstr (out, "crcor", Memc[str])
+
+		call cr_plot (cr, in, fluxratio)
+		call cr_badpix (cr, Memc[badpix])
+
+	        call cr_close (cr)
+	        if (out != in)
+	            call imunmap (out)
+	        call imunmap (in)
+	    } then {
+		# In case of error clean up and go on to the next image.
+		if (in != NULL) {
+		    if (out != NULL && out != in)
+			call imunmap (out)
+		    call imunmap (in)
+		}
+		if (cr != NULL)
+		    call cr_close (cr)
+		call erract (EA_WARN)
+	    }
+	}
+
+	if (interactive) {
+	    call gt_free (gt)
+	    call gclose (gp)
+	}
+	call imtclose (list1)
+	call imtclose (list2)
+	call clpcls (list3)
+	call hdmclose ()
+	call gsfree (sf1)
+	call gsfree (sf2)
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/doproc.x b/noao/imred/ccdred/src/doproc.x
new file mode 100644
index 00000000..909c6f12
--- /dev/null
+++ b/noao/imred/ccdred/src/doproc.x
@@ -0,0 +1,29 @@
+include	"ccdred.h"
+
+# DOPROC -- Call the appropriate processing procedure.
+#
+# There are four data type paths depending on the readout axis and
+# the calculation data type.
+
+procedure doproc (ccd)
+
+pointer	ccd		# CCD processing structure
+
+begin
+	switch (READAXIS (ccd)) {
+	case 1:
+	    switch (CALCTYPE (ccd)) {
+	    case TY_SHORT:
+	        call proc1s (ccd)
+	    default:
+	        call proc1r (ccd)
+	    }
+	case 2:
+	    switch (CALCTYPE (ccd)) {
+	    case TY_SHORT:
+	        call proc2s (ccd)
+	    default:
+	        call proc2r (ccd)
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/src/generic/ccdred.h b/noao/imred/ccdred/src/generic/ccdred.h
new file mode 100644
index 00000000..2d370d86
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/ccdred.h
@@ -0,0 +1,150 @@
+# CCDRED Data Structures and Definitions
+
+# The CCD structure:  This structure is used to communicate processing
+# parameters between the package procedures.  It contains pointers to
+# data, calibration image IMIO pointers, scaling parameters, and the
+# correction flags.  The corrections flags indicate which processing
+# operations are to be performed.  The subsection parameters do not
+# include a step size.  A step size is assumed.  If arbitrary subsampling
+# is desired this would be the next generalization.
+
+define	LEN_CCD		131		# Length of CCD structure
+
+# CCD data coordinates
+define	CCD_C1		Memi[$1]	# CCD starting column
+define	CCD_C2		Memi[$1+1]	# CCD ending column
+define	CCD_L1		Memi[$1+2]	# CCD starting line
+define	CCD_L2		Memi[$1+3]	# CCD ending line
+
+# Input data
+define	IN_IM		Memi[$1+10]	# Input image pointer
+define	IN_C1		Memi[$1+11]	# Input data starting column
+define	IN_C2		Memi[$1+12]	# Input data ending column
+define	IN_L1		Memi[$1+13]	# Input data starting line
+define	IN_L2		Memi[$1+14]	# Input data ending line
+
+# Output data
+define	OUT_IM		Memi[$1+20]	# Output image pointer
+define	OUT_C1		Memi[$1+21]	# Output data starting column
+define	OUT_C2		Memi[$1+22]	# Output data ending column
+define	OUT_L1		Memi[$1+23]	# Output data starting line
+define	OUT_L2		Memi[$1+24]	# Output data ending line
+
+# Mask data
+define  MASK_IM         Memi[$1+30]     # Mask image pointer
+define  MASK_C1         Memi[$1+31]     # Mask data starting column
+define  MASK_C2         Memi[$1+32]     # Mask data ending column
+define  MASK_L1         Memi[$1+33]     # Mask data starting line
+define  MASK_L2         Memi[$1+34]     # Mask data ending line
+define  MASK_PM         Memi[$1+35]     # Mask pointer
+define  MASK_FP         Memi[$1+36]     # Mask fixpix data
+
+# Zero level data
+define	ZERO_IM		Memi[$1+40]	# Zero level image pointer
+define	ZERO_C1		Memi[$1+41]	# Zero level data starting column
+define	ZERO_C2		Memi[$1+42]	# Zero level data ending column
+define	ZERO_L1		Memi[$1+43]	# Zero level data starting line
+define	ZERO_L2		Memi[$1+44]	# Zero level data ending line
+
+# Dark count data
+define	DARK_IM		Memi[$1+50]	# Dark count image pointer
+define	DARK_C1		Memi[$1+51]	# Dark count data starting column
+define	DARK_C2		Memi[$1+52]	# Dark count data ending column
+define	DARK_L1		Memi[$1+53]	# Dark count data starting line
+define	DARK_L2		Memi[$1+54]	# Dark count data ending line
+
+# Flat field data
+define	FLAT_IM		Memi[$1+60]	# Flat field image pointer
+define	FLAT_C1		Memi[$1+61]	# Flat field data starting column
+define	FLAT_C2		Memi[$1+62]	# Flat field data ending column
+define	FLAT_L1		Memi[$1+63]	# Flat field data starting line
+define	FLAT_L2		Memi[$1+64]	# Flat field data ending line
+
+# Illumination data
+define	ILLUM_IM	Memi[$1+70]	# Illumination image pointer
+define	ILLUM_C1	Memi[$1+71]	# Illumination data starting column
+define	ILLUM_C2	Memi[$1+72]	# Illumination data ending column
+define	ILLUM_L1	Memi[$1+73]	# Illumination data starting line
+define	ILLUM_L2	Memi[$1+74]	# Illumination data ending line
+
+# Fringe data
+define	FRINGE_IM	Memi[$1+80]	# Fringe image pointer
+define	FRINGE_C1	Memi[$1+81]	# Fringe data starting column
+define	FRINGE_C2	Memi[$1+82]	# Fringe data ending column
+define	FRINGE_L1	Memi[$1+83]	# Fringe data starting line
+define	FRINGE_L2	Memi[$1+84]	# Fringe data ending line
+
+# Trim section
+define	TRIM_C1		Memi[$1+90]	# Trim starting column
+define	TRIM_C2		Memi[$1+91]	# Trim ending column
+define	TRIM_L1		Memi[$1+92]	# Trim starting line
+define	TRIM_L2		Memi[$1+93]	# Trim ending line
+
+# Bias section
+define	BIAS_C1		Memi[$1+100]	# Bias starting column
+define	BIAS_C2		Memi[$1+101]	# Bias ending column
+define	BIAS_L1		Memi[$1+102]	# Bias starting line
+define	BIAS_L2		Memi[$1+103]	# Bias ending line
+
+define	READAXIS	Memi[$1+110]	# Read out axis (1=cols, 2=lines)
+define	CALCTYPE	Memi[$1+111]	# Calculation data type
+define	OVERSCAN_TYPE	Memi[$1+112]	# Overscan type
+define	OVERSCAN_VEC	Memi[$1+113]	# Pointer to overscan vector
+define	DARKSCALE	Memr[P2R($1+114)]	# Dark count scale factor
+define	FRINGESCALE	Memr[P2R($1+115)]	# Fringe scale factor
+define	FLATSCALE	Memr[P2R($1+116)]	# Flat field scale factor
+define	ILLUMSCALE	Memr[P2R($1+117)]	# Illumination scale factor
+define	MINREPLACE	Memr[P2R($1+118)]	# Minimum replacement value
+define	MEAN		Memr[P2R($1+119)]	# Mean of output image
+define	COR		Memi[$1+120]	# Overall correction flag
+define	CORS		Memi[$1+121+($2-1)]  # Individual correction flags
+
+# The correction array contains the following elements with array indices
+# given by the macro definitions.
+
+define	NCORS		10		# Number of corrections
+
+define	FIXPIX		1		# Fix bad pixels
+define	TRIM		2		# Trim image
+define	OVERSCAN	3		# Apply overscan correction
+define	ZEROCOR		4		# Apply zero level correction
+define	DARKCOR		5		# Apply dark count correction
+define	FLATCOR		6		# Apply flat field correction
+define	ILLUMCOR	7		# Apply illumination correction
+define	FRINGECOR	8		# Apply fringe correction
+define	FINDMEAN	9		# Find the mean of the output image
+define	MINREP		10		# Check and replace minimum value
+
+# The following definitions identify the correction values in the correction
+# array.  They are defined in terms of bit fields so that it is possible to
+# add corrections to form unique combination corrections.  Some of
+# these combinations are implemented as compound operations for efficiency.
+
+define	O	001B	# overscan
+define	Z	002B	# zero level
+define	D	004B	# dark count
+define	F	010B	# flat field
+define	I	020B	# Illumination
+define	Q	040B	# Fringe
+
+# The following correction combinations are recognized.
+
+define	ZO	003B	# zero level + overscan
+define	DO	005B	# dark count + overscan
+define	DZ	006B	# dark count + zero level
+define	DZO	007B	# dark count + zero level + overscan
+define	FO	011B	# flat field + overscan
+define	FZ	012B	# flat field + zero level
+define	FZO	013B	# flat field + zero level + overscan
+define	FD	014B	# flat field + dark count
+define	FDO	015B	# flat field + dark count + overscan
+define	FDZ	016B	# flat field + dark count + zero level
+define	FDZO	017B	# flat field + dark count + zero level + overscan
+define	QI	060B	# fringe + illumination
+
+# The following overscan functions are recognized.
+define  OVERSCAN_TYPES "|mean|median|minmax|chebyshev|legendre|spline3|spline1|"
+define  OVERSCAN_MEAN   1               # Mean of overscan
+define  OVERSCAN_MEDIAN 2               # Median of overscan
+define  OVERSCAN_MINMAX 3               # Minmax of overscan
+define  OVERSCAN_FIT    4               # Following codes are function fits
diff --git a/noao/imred/ccdred/src/generic/cor.x b/noao/imred/ccdred/src/generic/cor.x
new file mode 100644
index 00000000..fd2a8d6b
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/cor.x
@@ -0,0 +1,694 @@
+include	"ccdred.h"
+
+
+.help cor Feb87 noao.imred.ccdred
+.nf ----------------------------------------------------------------------------
+cor -- Process CCD image lines
+
+These procedures are the heart of the CCD processing.  They do the desired
+set of processing operations on the image line data as efficiently as
+possible.  They are called by the PROC procedures.  There are four procedures
+one for each readout axis and one for short and real image data.
+Some sets of operations are coded as single compound operations for efficiency.
+To keep the number of combinations managable only the most common
+combinations are coded as compound operations.  The combinations
+consist of any set of line overscan, column overscan, zero level, dark
+count, and flat field and any set of illumination and fringe
+correction.  The corrections are applied in place to the output vector.
+
+The column readout procedure is more complicated in order to handle
+zero level and flat field corrections specified as one dimensional
+readout corrections instead of two dimensional calibration images.
+Column readout format is probably extremely rare and the 1D readout
+corrections are used only for special types of data.
+.ih
+SEE ALSO
+proc, ccdred.h
+.endhelp -----------------------------------------------------------------------
+
+
+# COR1 -- Correct image lines with readout axis 1 (lines).
+
+procedure cor1s (cors, out, overscan, zero, dark, flat, illum,
+	fringe, n, darkscale, flatscale, illumscale, frgscale)
+
+int	cors[ARB]	# Correction flags
+short	out[n]		# Output data
+real	overscan	# Overscan value
+short	zero[n]		# Zero level correction
+short	dark[n]		# Dark count correction
+short	flat[n]		# Flat field correction
+short	illum[n]	# Illumination correction
+short	fringe[n]	# Fringe correction
+int	n		# Number of pixels
+real	darkscale	# Dark count scale factor
+real	flatscale	# Flat field scale factor
+real	illumscale	# Illumination scale factor
+real	frgscale	# Fringe scale factor
+
+int	i, op
+
+begin
+	op = cors[OVERSCAN] + cors[ZEROCOR] + cors[DARKCOR] + cors[FLATCOR]
+	switch (op) {
+	case O: # overscan
+	    do i = 1, n
+	        out[i] = out[i] - overscan
+	case Z: # zero level
+	    do i = 1, n
+		out[i] = out[i] - zero[i]
+
+	case ZO: # zero level + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - zero[i]
+
+	case D: # dark count
+	    do i = 1, n
+		out[i] = out[i] - darkscale * dark[i]
+	case DO: # dark count + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - darkscale * dark[i]
+	case DZ: # dark count + zero level
+	    do i = 1, n
+		out[i] = out[i] - zero[i] - darkscale * dark[i]
+	case DZO: # dark count + zero level + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - zero[i] - darkscale * dark[i]
+
+	case F: # flat field
+	    do i = 1, n
+		out[i] = out[i] * flatscale / flat[i]
+	case FO: # flat field + overscan
+	    do i = 1, n
+	        out[i] = (out[i] - overscan) * flatscale / flat[i]
+	case FZ: # flat field + zero level
+	    do i = 1, n
+		out[i] = (out[i] - zero[i]) * flatscale / flat[i]
+	case FZO: # flat field + zero level + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - zero[i]) * flatscale /
+		    flat[i]
+	case FD: # flat field + dark count
+	    do i = 1, n
+		out[i] = (out[i] - darkscale * dark[i]) * flatscale / flat[i]
+	case FDO: # flat field + dark count + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - darkscale * dark[i]) *
+		    flatscale / flat[i]
+	case FDZ: # flat field + dark count + zero level
+	    do i = 1, n
+		out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+		    flatscale / flat[i]
+	case FDZO: # flat field + dark count + zero level + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - zero[i] -
+		    darkscale * dark[i]) * flatscale / flat[i]
+	}
+
+	# Often these operations will not be performed so test for no
+	# correction rather than go through the switch.
+
+	op = cors[ILLUMCOR] + cors[FRINGECOR]
+	if (op != 0) {
+	    switch (op) {
+	    case I: # illumination
+	        do i = 1, n
+		    out[i] = out[i] * illumscale / illum[i]
+	    case Q: # fringe
+	        do i = 1, n
+		    out[i] = out[i] - frgscale * fringe[i]
+	    case QI: # fringe + illumination
+	        do i = 1, n
+		    out[i] = out[i]*illumscale/illum[i] - frgscale*fringe[i]
+	    }
+	}
+end
+
+
+# COR2 -- Correct lines for readout axis 2 (columns).  This procedure is
+# more complex than when the readout is along the image lines because the
+# zero level and/or flat field corrections may be single readout column
+# vectors.
+
+procedure cor2s (line, cors, out, overscan, zero, dark, flat, illum,
+	fringe, n, zeroim, flatim, darkscale, flatscale, illumscale, frgscale)
+
+int	line		# Line to be corrected
+int	cors[ARB]	# Correction flags
+short	out[n]		# Output data
+real	overscan[n]	# Overscan value
+short	zero[n]		# Zero level correction
+short	dark[n]		# Dark count correction
+short	flat[n]		# Flat field correction
+short	illum[n]	# Illumination correction
+short	fringe[n]	# Fringe correction
+int	n		# Number of pixels
+pointer	zeroim		# Zero level IMIO pointer (NULL if 1D vector)
+pointer	flatim		# Flat field IMIO pointer (NULL if 1D vector)
+real	darkscale	# Dark count scale factor
+real	flatscale	# Flat field scale factor
+real	illumscale	# Illumination scale factor
+real	frgscale	# Fringe scale factor
+
+short	zeroval
+real	flatval
+int	i, op
+
+begin
+	op = cors[OVERSCAN] + cors[ZEROCOR] + cors[DARKCOR] + cors[FLATCOR]
+	switch (op) {
+	case O: # overscan
+	    do i = 1, n
+	        out[i] = out[i] - overscan[i]
+	case Z: # zero level
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - zero[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - zeroval
+	    }
+
+	case ZO: # zero level + overscan
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zero[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zeroval
+	    }
+
+	case D: # dark count
+	    do i = 1, n
+		out[i] = out[i] - darkscale * dark[i]
+	case DO: # dark count + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan[i] - darkscale * dark[i]
+	case DZ: # dark count + zero level
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - zero[i] - darkscale * dark[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - zeroval - darkscale * dark[i]
+	    }
+	case DZO: # dark count + zero level + overscan
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zero[i] -
+			darkscale * dark[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zeroval -
+			darkscale * dark[i]
+	    }
+
+	case F: # flat field
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = out[i] * flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = out[i] * flatval
+	    }
+	case FO: # flat field + overscan
+	    if (flatim != NULL) {
+	        do i = 1, n
+	            out[i] = (out[i] - overscan[i]) * flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+	            out[i] = (out[i] - overscan[i]) * flatval
+	    }
+	case FZ: # flat field + zero level
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i]) * flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval) * flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval) * flatval
+		}
+	    }
+	case FZO: # flat field + zero level + overscan
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i]) *
+			    flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval) *
+			    flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval) * flatval
+		}
+	    }
+	case FD: # flat field + dark count
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = (out[i] - darkscale * dark[i]) * flatscale/flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = (out[i] - darkscale * dark[i]) * flatval
+	    }
+	case FDO: # flat field + dark count + overscan
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = (out[i] - overscan[i] - darkscale * dark[i]) *
+		        flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = (out[i] - overscan[i] - darkscale * dark[i]) *
+		        flatval
+	    }
+	case FDZ: # flat field + dark count + zero level
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+			    flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval - darkscale * dark[i]) *
+			    flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+			    flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval - darkscale * dark[i]) *
+			    flatval
+		}
+	    }
+	case FDZO: # flat field + dark count + zero level + overscan
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i] -
+			    darkscale * dark[i]) * flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval -
+			    darkscale * dark[i]) * flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i] -
+			    darkscale * dark[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval -
+			    darkscale * dark[i]) * flatval
+		}
+	    }
+	}
+
+	# Often these operations will not be performed so test for no
+	# correction rather than go through the switch.
+
+	op = cors[ILLUMCOR] + cors[FRINGECOR]
+	if (op != 0) {
+	    switch (op) {
+	    case I: # illumination
+	        do i = 1, n
+		    out[i] = out[i] * illumscale / illum[i]
+	    case Q: # fringe
+	        do i = 1, n
+		    out[i] = out[i] - frgscale * fringe[i]
+	    case QI: # fringe + illumination
+	        do i = 1, n
+		    out[i] = out[i]*illumscale/illum[i] - frgscale*fringe[i]
+	    }
+	}
+end
+
+# COR1 -- Correct image lines with readout axis 1 (lines).
+
+procedure cor1r (cors, out, overscan, zero, dark, flat, illum,
+	fringe, n, darkscale, flatscale, illumscale, frgscale)
+
+int	cors[ARB]	# Correction flags
+real	out[n]		# Output data
+real	overscan	# Overscan value
+real	zero[n]		# Zero level correction
+real	dark[n]		# Dark count correction
+real	flat[n]		# Flat field correction
+real	illum[n]	# Illumination correction
+real	fringe[n]	# Fringe correction
+int	n		# Number of pixels
+real	darkscale	# Dark count scale factor
+real	flatscale	# Flat field scale factor
+real	illumscale	# Illumination scale factor
+real	frgscale	# Fringe scale factor
+
+int	i, op
+
+begin
+	op = cors[OVERSCAN] + cors[ZEROCOR] + cors[DARKCOR] + cors[FLATCOR]
+	switch (op) {
+	case O: # overscan
+	    do i = 1, n
+	        out[i] = out[i] - overscan
+	case Z: # zero level
+	    do i = 1, n
+		out[i] = out[i] - zero[i]
+
+	case ZO: # zero level + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - zero[i]
+
+	case D: # dark count
+	    do i = 1, n
+		out[i] = out[i] - darkscale * dark[i]
+	case DO: # dark count + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - darkscale * dark[i]
+	case DZ: # dark count + zero level
+	    do i = 1, n
+		out[i] = out[i] - zero[i] - darkscale * dark[i]
+	case DZO: # dark count + zero level + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - zero[i] - darkscale * dark[i]
+
+	case F: # flat field
+	    do i = 1, n
+		out[i] = out[i] * flatscale / flat[i]
+	case FO: # flat field + overscan
+	    do i = 1, n
+	        out[i] = (out[i] - overscan) * flatscale / flat[i]
+	case FZ: # flat field + zero level
+	    do i = 1, n
+		out[i] = (out[i] - zero[i]) * flatscale / flat[i]
+	case FZO: # flat field + zero level + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - zero[i]) * flatscale /
+		    flat[i]
+	case FD: # flat field + dark count
+	    do i = 1, n
+		out[i] = (out[i] - darkscale * dark[i]) * flatscale / flat[i]
+	case FDO: # flat field + dark count + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - darkscale * dark[i]) *
+		    flatscale / flat[i]
+	case FDZ: # flat field + dark count + zero level
+	    do i = 1, n
+		out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+		    flatscale / flat[i]
+	case FDZO: # flat field + dark count + zero level + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - zero[i] -
+		    darkscale * dark[i]) * flatscale / flat[i]
+	}
+
+	# Often these operations will not be performed so test for no
+	# correction rather than go through the switch.
+
+	op = cors[ILLUMCOR] + cors[FRINGECOR]
+	if (op != 0) {
+	    switch (op) {
+	    case I: # illumination
+	        do i = 1, n
+		    out[i] = out[i] * illumscale / illum[i]
+	    case Q: # fringe
+	        do i = 1, n
+		    out[i] = out[i] - frgscale * fringe[i]
+	    case QI: # fringe + illumination
+	        do i = 1, n
+		    out[i] = out[i]*illumscale/illum[i] - frgscale*fringe[i]
+	    }
+	}
+end
+
+
+# COR2 -- Correct lines for readout axis 2 (columns).  This procedure is
+# more complex than when the readout is along the image lines because the
+# zero level and/or flat field corrections may be single readout column
+# vectors.
+
+procedure cor2r (line, cors, out, overscan, zero, dark, flat, illum,
+	fringe, n, zeroim, flatim, darkscale, flatscale, illumscale, frgscale)
+
+int	line		# Line to be corrected
+int	cors[ARB]	# Correction flags
+real	out[n]		# Output data
+real	overscan[n]	# Overscan value
+real	zero[n]		# Zero level correction
+real	dark[n]		# Dark count correction
+real	flat[n]		# Flat field correction
+real	illum[n]	# Illumination correction
+real	fringe[n]	# Fringe correction
+int	n		# Number of pixels
+pointer	zeroim		# Zero level IMIO pointer (NULL if 1D vector)
+pointer	flatim		# Flat field IMIO pointer (NULL if 1D vector)
+real	darkscale	# Dark count scale factor
+real	flatscale	# Flat field scale factor
+real	illumscale	# Illumination scale factor
+real	frgscale	# Fringe scale factor
+
+real	zeroval
+real	flatval
+int	i, op
+
+begin
+	op = cors[OVERSCAN] + cors[ZEROCOR] + cors[DARKCOR] + cors[FLATCOR]
+	switch (op) {
+	case O: # overscan
+	    do i = 1, n
+	        out[i] = out[i] - overscan[i]
+	case Z: # zero level
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - zero[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - zeroval
+	    }
+
+	case ZO: # zero level + overscan
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zero[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zeroval
+	    }
+
+	case D: # dark count
+	    do i = 1, n
+		out[i] = out[i] - darkscale * dark[i]
+	case DO: # dark count + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan[i] - darkscale * dark[i]
+	case DZ: # dark count + zero level
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - zero[i] - darkscale * dark[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - zeroval - darkscale * dark[i]
+	    }
+	case DZO: # dark count + zero level + overscan
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zero[i] -
+			darkscale * dark[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zeroval -
+			darkscale * dark[i]
+	    }
+
+	case F: # flat field
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = out[i] * flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = out[i] * flatval
+	    }
+	case FO: # flat field + overscan
+	    if (flatim != NULL) {
+	        do i = 1, n
+	            out[i] = (out[i] - overscan[i]) * flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+	            out[i] = (out[i] - overscan[i]) * flatval
+	    }
+	case FZ: # flat field + zero level
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i]) * flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval) * flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval) * flatval
+		}
+	    }
+	case FZO: # flat field + zero level + overscan
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i]) *
+			    flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval) *
+			    flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval) * flatval
+		}
+	    }
+	case FD: # flat field + dark count
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = (out[i] - darkscale * dark[i]) * flatscale/flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = (out[i] - darkscale * dark[i]) * flatval
+	    }
+	case FDO: # flat field + dark count + overscan
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = (out[i] - overscan[i] - darkscale * dark[i]) *
+		        flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = (out[i] - overscan[i] - darkscale * dark[i]) *
+		        flatval
+	    }
+	case FDZ: # flat field + dark count + zero level
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+			    flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval - darkscale * dark[i]) *
+			    flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+			    flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval - darkscale * dark[i]) *
+			    flatval
+		}
+	    }
+	case FDZO: # flat field + dark count + zero level + overscan
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i] -
+			    darkscale * dark[i]) * flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval -
+			    darkscale * dark[i]) * flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i] -
+			    darkscale * dark[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval -
+			    darkscale * dark[i]) * flatval
+		}
+	    }
+	}
+
+	# Often these operations will not be performed so test for no
+	# correction rather than go through the switch.
+
+	op = cors[ILLUMCOR] + cors[FRINGECOR]
+	if (op != 0) {
+	    switch (op) {
+	    case I: # illumination
+	        do i = 1, n
+		    out[i] = out[i] * illumscale / illum[i]
+	    case Q: # fringe
+	        do i = 1, n
+		    out[i] = out[i] - frgscale * fringe[i]
+	    case QI: # fringe + illumination
+	        do i = 1, n
+		    out[i] = out[i]*illumscale/illum[i] - frgscale*fringe[i]
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/src/generic/icaclip.x b/noao/imred/ccdred/src/generic/icaclip.x
new file mode 100644
index 00000000..1530145c
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/icaclip.x
@@ -0,0 +1,1102 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		3	# Minimum number of images for this algorithm
+
+
+# IC_AAVSIGCLIP -- Reject pixels using an average sigma about the average
+# The average sigma is normalized by the expected poisson sigma.
+
+procedure ic_aavsigclips (d, m, n, scales, zeros, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+real	d1, low, high, sum, a, s, s1, r, one
+data	one /1.0/
+pointer	sp, sums, resid, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (sums, npts, TY_REAL)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Since the unweighted average is computed here possibly skip combining
+	if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	# Compute the unweighted average with the high and low rejected and
+	# the poisson scaled average sigma.  There must be at least three
+	# pixels at each point to define the average and contributions to
+	# the mean sigma.  Corrections for differences in the image
+	# scale factors are selected by the doscale1 flag.
+
+	nin = n[1]
+	s = 0.
+	n2 = 0
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (n1 < 3)
+		next
+
+	    # Unweighted average with the high and low rejected
+	    low = Mems[d[1]+k]
+	    high = Mems[d[2]+k]
+	    if (low > high) {
+		d1 = low
+		low = high
+		high = d1
+	    }
+	    sum = 0.
+	    do j = 3, n1 {
+	       d1 = Mems[d[j]+k]
+	       if (d1 < low) {
+		   sum = sum + low
+		   low = d1
+		} else if (d1 > high) {
+		    sum = sum + high
+		    high = d1
+		} else
+		    sum = sum + d1
+	    }
+	    a = sum / (n1 - 2)
+	    sum = sum + low + high
+
+	    # Poisson scaled sigma accumulation
+	    if (doscale1) {
+		do j = 1, n1 {
+		    dp1 = d[j] + k
+		    mp1 = m[j] + k
+
+		    d1 = Mems[dp1]
+		    l = Memi[mp1]
+		    s1 = max (one, (a + zeros[l]) /  scales[l])
+		    s = s + (d1 - a) ** 2 / s1
+		}
+	    } else {
+		s1 = max (one, a)
+		do j = 1, n1
+		    s = s + (Mems[d[j]+k] - a) ** 2 / s1
+	    }
+	    n2 = n2 + n1
+
+	    # Save the average and sum for later.
+	    average[i] = a
+	    Memr[sums+k] = sum
+	}
+
+	# Here is the final sigma.
+	if (n2 > 1)
+	    s = sqrt (s / (n2 - 1))
+
+	# Reject pixels and compute the final average (if needed).
+	# There must be at least three pixels at each point for rejection.
+	# Iteratively scale the mean sigma and reject pixels
+	# Compact the data and keep track of the image IDs if needed.
+
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 <= max (2, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Mems[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Mems[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    a = average[i]
+	    sum = Memr[sums+k]
+
+	    repeat {
+		n2 = n1
+		if (s > 0.) {
+		    if (doscale1) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    mp1 = m[j] + k
+
+			    d1 = Mems[dp1]
+			    l = Memi[mp1]
+			    s1 = s * sqrt (max (one, (a+zeros[l]) /  scales[l]))
+			    r = (d1 - a) / s1
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs(r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    mp2 = m[n1] + k
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    } else {
+			s1 = s * sqrt (max (one, a))
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    d1 = Mems[dp1]
+			    r = (d1 - a) / s1
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs(r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[n1] + k
+					l = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = l
+				    }
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+		if (n1 > 1)
+		    a = sum / n1
+	    } until (n1 == n2 || n1 <= max (2, maxkeep))
+
+	    # If too many are rejected add some back in.
+	    # Pixels with equal residuals are added together.
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mems[dp1]
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Mems[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mems[dp1]
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Mems[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+		if (n1 > 1)
+		    a = sum / n1
+	    }
+
+	    # Save the average if needed.
+	    n[i] = n1
+	    if (!docombine) {
+		if (n1 > 0)
+		    average[i] = a
+		else
+		    average[i] = blank
+	    }
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_MAVSIGCLIP -- Reject pixels using an average sigma about the median
+# The average sigma is normalized by the expected poisson sigma.
+
+procedure ic_mavsigclips (d, m, n, scales, zeros, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+pointer	sp, resid, mp1, mp2
+real	med, low, high, r, s, s1, one
+data	one /1.0/
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Compute the poisson scaled average sigma about the median.
+	# There must be at least three pixels at each point to define
+	# the mean sigma.  Corrections for differences in the image
+	# scale factors are selected by the doscale1 flag.
+
+	s = 0.
+	n2 = 0
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (n1 < 3) {
+		if (n1 == 0)
+		    median[i] = blank
+		else if (n1 == 1)
+		    median[i] = Mems[d[1]+k]
+		else {
+		    low = Mems[d[1]+k]
+		    high = Mems[d[2]+k]
+		    median[i] = (low + high) / 2.
+		}
+		next
+	    }
+
+	    # Median
+	    n3 = 1 + n1 / 2
+	    if (mod (n1, 2) == 0) {
+		low = Mems[d[n3-1]+k]
+		high = Mems[d[n3]+k]
+		med = (low + high) / 2.
+	    } else
+		med = Mems[d[n3]+k]
+
+	    # Poisson scaled sigma accumulation
+	    if (doscale1) {
+		do j = 1, n1 {
+		    l = Memi[m[j]+k]
+		    s1 = max (one, (med + zeros[l]) /  scales[l])
+		    s = s + (Mems[d[j]+k] - med) ** 2 / s1
+		}
+	    } else {
+		s1 = max (one, med)
+		do j = 1, n1
+		    s = s + (Mems[d[j]+k] - med) ** 2 / s1
+	    }
+	    n2 = n2 + n1
+
+	    # Save the median for later.
+	    median[i] = med
+	}
+
+	# Here is the final sigma.
+	if (n2 > 1)
+	    s = sqrt (s / (n2 - 1))
+	else
+	    return
+
+	# Compute individual sigmas and iteratively clip.
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 < max (3, maxkeep+1))
+		next
+	    nl = 1
+	    nh = n1
+	    med = median[i]
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 >= max (MINCLIP, maxkeep+1) && s > 0.) {
+		    if (doscale1) {
+			for (; nl <= n2; nl = nl + 1) {
+			    l = Memi[m[nl]+k]
+			    s1 = s * sqrt (max (one, (med+zeros[l])/scales[l]))
+			    r = (med - Mems[d[nl]+k]) / s1
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    l = Memi[m[nh]+k]
+			    s1 = s * sqrt (max (one, (med+zeros[l])/scales[l]))
+			    r = (Mems[d[nh]+k] - med) / s1
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    } else {
+			s1 = s * sqrt (max (one, med))
+			for (; nl <= n2; nl = nl + 1) {
+			    r = (med - Mems[d[nl]+k]) / s1
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    r = (Mems[d[nh]+k] - med) / s1
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    }
+
+		    # Recompute median
+		    if (n1 < n2) {
+			if (n1 > 0) {
+			    n3 = nl + n1 / 2
+			    if (mod (n1, 2) == 0) {
+				low = Mems[d[n3-1]+k]
+				high = Mems[d[n3]+k]
+				med = (low + high) / 2.
+			    } else
+				med = Mems[d[n3]+k]
+			} else
+			    med = blank
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    # If too many are rejected add some back in.
+	    # Pixels with equal residuals are added together.
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+
+		# Recompute median
+		if (n1 < n2) {
+		    if (n1 > 0) {
+			n3 = nl + n1 / 2
+			if (mod (n1, 2) == 0) {
+			    low = Mems[d[n3-1]+k]
+			    high = Mems[d[n3]+k]
+			    med = (low + high) / 2.
+			} else
+			    med = Mems[d[n3]+k]
+		    } else
+			med = blank
+		}
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mems[d[l]+k] = Mems[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mems[d[l]+k] = Mems[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median is computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+
+# IC_AAVSIGCLIP -- Reject pixels using an average sigma about the average
+# The average sigma is normalized by the expected poisson sigma.
+
+procedure ic_aavsigclipr (d, m, n, scales, zeros, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+real	d1, low, high, sum, a, s, s1, r, one
+data	one /1.0/
+pointer	sp, sums, resid, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (sums, npts, TY_REAL)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Since the unweighted average is computed here possibly skip combining
+	if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	# Compute the unweighted average with the high and low rejected and
+	# the poisson scaled average sigma.  There must be at least three
+	# pixels at each point to define the average and contributions to
+	# the mean sigma.  Corrections for differences in the image
+	# scale factors are selected by the doscale1 flag.
+
+	nin = n[1]
+	s = 0.
+	n2 = 0
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (n1 < 3)
+		next
+
+	    # Unweighted average with the high and low rejected
+	    low = Memr[d[1]+k]
+	    high = Memr[d[2]+k]
+	    if (low > high) {
+		d1 = low
+		low = high
+		high = d1
+	    }
+	    sum = 0.
+	    do j = 3, n1 {
+	       d1 = Memr[d[j]+k]
+	       if (d1 < low) {
+		   sum = sum + low
+		   low = d1
+		} else if (d1 > high) {
+		    sum = sum + high
+		    high = d1
+		} else
+		    sum = sum + d1
+	    }
+	    a = sum / (n1 - 2)
+	    sum = sum + low + high
+
+	    # Poisson scaled sigma accumulation
+	    if (doscale1) {
+		do j = 1, n1 {
+		    dp1 = d[j] + k
+		    mp1 = m[j] + k
+
+		    d1 = Memr[dp1]
+		    l = Memi[mp1]
+		    s1 = max (one, (a + zeros[l]) /  scales[l])
+		    s = s + (d1 - a) ** 2 / s1
+		}
+	    } else {
+		s1 = max (one, a)
+		do j = 1, n1
+		    s = s + (Memr[d[j]+k] - a) ** 2 / s1
+	    }
+	    n2 = n2 + n1
+
+	    # Save the average and sum for later.
+	    average[i] = a
+	    Memr[sums+k] = sum
+	}
+
+	# Here is the final sigma.
+	if (n2 > 1)
+	    s = sqrt (s / (n2 - 1))
+
+	# Reject pixels and compute the final average (if needed).
+	# There must be at least three pixels at each point for rejection.
+	# Iteratively scale the mean sigma and reject pixels
+	# Compact the data and keep track of the image IDs if needed.
+
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 <= max (2, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Memr[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Memr[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    a = average[i]
+	    sum = Memr[sums+k]
+
+	    repeat {
+		n2 = n1
+		if (s > 0.) {
+		    if (doscale1) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    mp1 = m[j] + k
+
+			    d1 = Memr[dp1]
+			    l = Memi[mp1]
+			    s1 = s * sqrt (max (one, (a+zeros[l]) /  scales[l]))
+			    r = (d1 - a) / s1
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs(r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    mp2 = m[n1] + k
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    } else {
+			s1 = s * sqrt (max (one, a))
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    d1 = Memr[dp1]
+			    r = (d1 - a) / s1
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs(r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[n1] + k
+					l = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = l
+				    }
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+		if (n1 > 1)
+		    a = sum / n1
+	    } until (n1 == n2 || n1 <= max (2, maxkeep))
+
+	    # If too many are rejected add some back in.
+	    # Pixels with equal residuals are added together.
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Memr[dp1]
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Memr[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Memr[dp1]
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Memr[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+		if (n1 > 1)
+		    a = sum / n1
+	    }
+
+	    # Save the average if needed.
+	    n[i] = n1
+	    if (!docombine) {
+		if (n1 > 0)
+		    average[i] = a
+		else
+		    average[i] = blank
+	    }
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_MAVSIGCLIP -- Reject pixels using an average sigma about the median
+# The average sigma is normalized by the expected poisson sigma.
+
+procedure ic_mavsigclipr (d, m, n, scales, zeros, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+pointer	sp, resid, mp1, mp2
+real	med, low, high, r, s, s1, one
+data	one /1.0/
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Compute the poisson scaled average sigma about the median.
+	# There must be at least three pixels at each point to define
+	# the mean sigma.  Corrections for differences in the image
+	# scale factors are selected by the doscale1 flag.
+
+	s = 0.
+	n2 = 0
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (n1 < 3) {
+		if (n1 == 0)
+		    median[i] = blank
+		else if (n1 == 1)
+		    median[i] = Memr[d[1]+k]
+		else {
+		    low = Memr[d[1]+k]
+		    high = Memr[d[2]+k]
+		    median[i] = (low + high) / 2.
+		}
+		next
+	    }
+
+	    # Median
+	    n3 = 1 + n1 / 2
+	    if (mod (n1, 2) == 0) {
+		low = Memr[d[n3-1]+k]
+		high = Memr[d[n3]+k]
+		med = (low + high) / 2.
+	    } else
+		med = Memr[d[n3]+k]
+
+	    # Poisson scaled sigma accumulation
+	    if (doscale1) {
+		do j = 1, n1 {
+		    l = Memi[m[j]+k]
+		    s1 = max (one, (med + zeros[l]) /  scales[l])
+		    s = s + (Memr[d[j]+k] - med) ** 2 / s1
+		}
+	    } else {
+		s1 = max (one, med)
+		do j = 1, n1
+		    s = s + (Memr[d[j]+k] - med) ** 2 / s1
+	    }
+	    n2 = n2 + n1
+
+	    # Save the median for later.
+	    median[i] = med
+	}
+
+	# Here is the final sigma.
+	if (n2 > 1)
+	    s = sqrt (s / (n2 - 1))
+	else
+	    return
+
+	# Compute individual sigmas and iteratively clip.
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 < max (3, maxkeep+1))
+		next
+	    nl = 1
+	    nh = n1
+	    med = median[i]
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 >= max (MINCLIP, maxkeep+1) && s > 0.) {
+		    if (doscale1) {
+			for (; nl <= n2; nl = nl + 1) {
+			    l = Memi[m[nl]+k]
+			    s1 = s * sqrt (max (one, (med+zeros[l])/scales[l]))
+			    r = (med - Memr[d[nl]+k]) / s1
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    l = Memi[m[nh]+k]
+			    s1 = s * sqrt (max (one, (med+zeros[l])/scales[l]))
+			    r = (Memr[d[nh]+k] - med) / s1
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    } else {
+			s1 = s * sqrt (max (one, med))
+			for (; nl <= n2; nl = nl + 1) {
+			    r = (med - Memr[d[nl]+k]) / s1
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    r = (Memr[d[nh]+k] - med) / s1
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    }
+
+		    # Recompute median
+		    if (n1 < n2) {
+			if (n1 > 0) {
+			    n3 = nl + n1 / 2
+			    if (mod (n1, 2) == 0) {
+				low = Memr[d[n3-1]+k]
+				high = Memr[d[n3]+k]
+				med = (low + high) / 2.
+			    } else
+				med = Memr[d[n3]+k]
+			} else
+			    med = blank
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    # If too many are rejected add some back in.
+	    # Pixels with equal residuals are added together.
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+
+		# Recompute median
+		if (n1 < n2) {
+		    if (n1 > 0) {
+			n3 = nl + n1 / 2
+			if (mod (n1, 2) == 0) {
+			    low = Memr[d[n3-1]+k]
+			    high = Memr[d[n3]+k]
+			    med = (low + high) / 2.
+			} else
+			    med = Memr[d[n3]+k]
+		    } else
+			med = blank
+		}
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Memr[d[l]+k] = Memr[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Memr[d[l]+k] = Memr[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median is computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/generic/icaverage.x b/noao/imred/ccdred/src/generic/icaverage.x
new file mode 100644
index 00000000..3646b725
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/icaverage.x
@@ -0,0 +1,163 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"../icombine.h"
+
+
+# IC_AVERAGE -- Compute the average image line.
+# Options include a weight average.
+
+procedure ic_averages (d, m, n, wts, npts, average)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image ID pointers
+int	n[npts]			# Number of points
+real	wts[ARB]		# Weights
+int	npts			# Number of output points per line
+real	average[npts]		# Average (returned)
+
+int	i, j, k
+real	sumwt, wt
+real	sum
+
+include	"../icombine.com"
+
+begin
+	# If no data has been excluded do the average without checking the
+	# number of points and using the fact that the weights are normalized.
+	# If all the data has been excluded set the average to the blank value.
+
+	if (dflag == D_ALL) {
+	    if (dowts) {
+		do i = 1, npts {
+		    k = i - 1
+		    wt = wts[Memi[m[1]+k]]
+		    sum = Mems[d[1]+k] * wt
+		    do j = 2, n[i] {
+			wt = wts[Memi[m[j]+k]]
+			sum = sum + Mems[d[j]+k] * wt
+		    }
+		    average[i] = sum
+		}
+	    } else {
+		do i = 1, npts {
+		    k = i - 1
+		    sum = Mems[d[1]+k]
+		    do j = 2, n[i]
+			sum = sum + Mems[d[j]+k]
+		    average[i] = sum / n[i]
+		}
+	    }
+	} else if (dflag == D_NONE) {
+	    do i = 1, npts
+		average[i] = blank
+	} else {
+	    if (dowts) {
+		do i = 1, npts {
+		    if (n[i] > 0) {
+			k = i - 1
+			wt = wts[Memi[m[1]+k]]
+			sum = Mems[d[1]+k] * wt
+			sumwt = wt
+			do j = 2, n[i] {
+			    wt = wts[Memi[m[j]+k]]
+			    sum = sum + Mems[d[j]+k] * wt
+			    sumwt = sumwt + wt
+			}
+			average[i] = sum / sumwt
+		    } else
+			average[i] = blank
+		}
+	    } else {
+		do i = 1, npts {
+		    if (n[i] > 0) {
+			k = i - 1
+			sum = Mems[d[1]+k]
+			do j = 2, n[i]
+			    sum = sum + Mems[d[j]+k]
+			average[i] = sum / n[i]
+		    } else
+			average[i] = blank
+		}
+	    }
+	}
+end
+
+# IC_AVERAGE -- Compute the average image line.
+# Options include a weight average.
+
+procedure ic_averager (d, m, n, wts, npts, average)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image ID pointers
+int	n[npts]			# Number of points
+real	wts[ARB]		# Weights
+int	npts			# Number of output points per line
+real	average[npts]		# Average (returned)
+
+int	i, j, k
+real	sumwt, wt
+real	sum
+
+include	"../icombine.com"
+
+begin
+	# If no data has been excluded do the average without checking the
+	# number of points and using the fact that the weights are normalized.
+	# If all the data has been excluded set the average to the blank value.
+
+	if (dflag == D_ALL) {
+	    if (dowts) {
+		do i = 1, npts {
+		    k = i - 1
+		    wt = wts[Memi[m[1]+k]]
+		    sum = Memr[d[1]+k] * wt
+		    do j = 2, n[i] {
+			wt = wts[Memi[m[j]+k]]
+			sum = sum + Memr[d[j]+k] * wt
+		    }
+		    average[i] = sum
+		}
+	    } else {
+		do i = 1, npts {
+		    k = i - 1
+		    sum = Memr[d[1]+k]
+		    do j = 2, n[i]
+			sum = sum + Memr[d[j]+k]
+		    average[i] = sum / n[i]
+		}
+	    }
+	} else if (dflag == D_NONE) {
+	    do i = 1, npts
+		average[i] = blank
+	} else {
+	    if (dowts) {
+		do i = 1, npts {
+		    if (n[i] > 0) {
+			k = i - 1
+			wt = wts[Memi[m[1]+k]]
+			sum = Memr[d[1]+k] * wt
+			sumwt = wt
+			do j = 2, n[i] {
+			    wt = wts[Memi[m[j]+k]]
+			    sum = sum + Memr[d[j]+k] * wt
+			    sumwt = sumwt + wt
+			}
+			average[i] = sum / sumwt
+		    } else
+			average[i] = blank
+		}
+	    } else {
+		do i = 1, npts {
+		    if (n[i] > 0) {
+			k = i - 1
+			sum = Memr[d[1]+k]
+			do j = 2, n[i]
+			    sum = sum + Memr[d[j]+k]
+			average[i] = sum / n[i]
+		    } else
+			average[i] = blank
+		}
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/src/generic/iccclip.x b/noao/imred/ccdred/src/generic/iccclip.x
new file mode 100644
index 00000000..57709064
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/iccclip.x
@@ -0,0 +1,898 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		2	# Mininum number of images for algorithm
+
+
+# IC_ACCDCLIP -- Reject pixels using CCD noise parameters about the average
+
+procedure ic_accdclips (d, m, n, scales, zeros, nm, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+real	nm[3,nimages]		# Noise model parameters
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+real	d1, low, high, sum, a, s, r, zero
+data	zero /0.0/
+pointer	sp, resid, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are no pixels go on to the combining.  Since the unweighted
+	# average is computed here possibly skip the combining later.
+
+	# There must be at least max (1, nkeep) pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	} else if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# There must be at least two pixels for rejection.  The initial
+	# average is the low/high rejected average except in the case of
+	# just two pixels.  The rejections are iterated and the average
+	# is recomputed.  Corrections for scaling may be performed.
+	# Depending on other flags the image IDs may also need to be adjusted.
+
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 <= max (MINCLIP-1, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Mems[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Mems[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    repeat {
+		if (n1 == 2) {
+		    sum = Mems[d[1]+k]
+		    sum = sum + Mems[d[2]+k]
+		    a = sum / 2
+		} else {
+		    low = Mems[d[1]+k]
+		    high = Mems[d[2]+k]
+		    if (low > high) {
+			d1 = low
+			low = high
+			high = d1
+		    }
+		    sum = 0.
+		    do j = 3, n1 {
+		       d1 = Mems[d[j]+k]
+		       if (d1 < low) {
+			   sum = sum + low
+			   low = d1
+			} else if (d1 > high) {
+			    sum = sum + high
+			    high = d1
+			} else
+			    sum = sum + d1
+		    }
+		    a = sum / (n1 - 2)
+		    sum = sum + low + high
+		}
+		n2 = n1
+		if (doscale1) {
+		    for (j=1; j<=n1; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+
+			l = Memi[mp1]
+			s = scales[l]
+			d1 = max (zero, s * (a + zeros[l]))
+			s = sqrt (nm[1,l] + d1/nm[2,l] + (d1*nm[3,l])**2) / s
+
+			d1 = Mems[dp1]
+			r = (d1 - a) / s
+			if (r < -lsigma || r > hsigma) {
+			    Memr[resid+n1] = abs(r)
+			    if (j < n1) {
+				dp2 = d[n1] + k
+				Mems[dp1] = Mems[dp2]
+				Mems[dp2] = d1
+				mp2 = m[n1] + k
+				Memi[mp1] = Memi[mp2]
+				Memi[mp2] = l
+				j = j - 1
+			    }
+			    sum = sum - d1
+			    n1 = n1 - 1
+			}
+		    }
+		} else {
+		    if (!keepids) {
+			s = max (zero, a)
+			s = sqrt (nm[1,1] + s/nm[2,1] + (s*nm[3,1])**2)
+		    }
+		    for (j=1; j<=n1; j=j+1) {
+			if (keepids) {
+			    l = Memi[m[j]+k]
+			    s = max (zero, a)
+			    s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			}
+			dp1 = d[j] + k
+			d1 = Mems[dp1]
+			r = (d1 - a) / s
+			if (r < -lsigma || r > hsigma) {
+			    Memr[resid+n1] = abs(r)
+			    if (j < n1) {
+				dp2 = d[n1] + k
+				Mems[dp1] = Mems[dp2]
+				Mems[dp2] = d1
+				if (keepids) {
+				    mp1 = m[j] + k
+				    mp2 = m[n1] + k
+				    l = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				}
+				j = j - 1
+			    }
+			    sum = sum - d1
+			    n1 = n1 - 1
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mems[dp1]
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Mems[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mems[dp1]
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Mems[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+	    }
+
+	    n[i] = n1
+	    if (!docombine)
+		if (n1 > 0)
+		    average[i] = sum / n1
+		else
+		    average[i] = blank
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_CCDCLIP -- Reject pixels using CCD noise parameters about the median
+
+procedure ic_mccdclips (d, m, n, scales, zeros, nm, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+real	nm[3,nimages]		# Noise model
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+real	r, s
+pointer	sp, resid, mp1, mp2
+real	med, zero
+data	zero /0.0/
+
+include	"../icombine.com"
+
+begin
+	# There must be at least max (MINCLIP, nkeep+1) pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Compute median and sigma and iteratively clip.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    nl = 1
+	    nh = n1
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 == 0)
+		    med = blank
+		else if (mod (n1, 2) == 0) {
+		    med = Mems[d[n3-1]+k]
+		    med = (med + Mems[d[n3]+k]) / 2.
+		} else
+		    med = Mems[d[n3]+k]
+
+		if (n1 >= max (MINCLIP, maxkeep+1)) {
+		    if (doscale1) {
+			for (; nl <= n2; nl = nl + 1) {
+			    l = Memi[m[nl]+k]
+			    s = scales[l]
+			    r = max (zero, s * (med + zeros[l]))
+			    s = sqrt (nm[1,l] + r/nm[2,l] + (r*nm[3,l])**2) / s
+			    r = (med - Mems[d[nl]+k]) / s
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    l = Memi[m[nh]+k]
+			    s = scales[l]
+			    r = max (zero, s * (med + zeros[l]))
+			    s = sqrt (nm[1,l] + r/nm[2,l] + (r*nm[3,l])**2) / s
+			    r = (Mems[d[nh]+k] - med) / s
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    } else {
+			if (!keepids) {
+			    s = max (zero, med)
+			    s = sqrt (nm[1,1] + s/nm[2,1] + (s*nm[3,1])**2)
+			}
+			for (; nl <= n2; nl = nl + 1) {
+			    if (keepids) {
+				l = Memi[m[nl]+k]
+				s = max (zero, med)
+				s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			    }
+			    r = (med - Mems[d[nl]+k]) / s
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    if (keepids) {
+				l = Memi[m[nh]+k]
+				s = max (zero, med)
+				s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			    }
+			    r = (Mems[d[nh]+k] -  med) / s
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mems[d[l]+k] = Mems[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mems[d[l]+k] = Mems[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median is computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+
+# IC_ACCDCLIP -- Reject pixels using CCD noise parameters about the average
+
+procedure ic_accdclipr (d, m, n, scales, zeros, nm, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+real	nm[3,nimages]		# Noise model parameters
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+real	d1, low, high, sum, a, s, r, zero
+data	zero /0.0/
+pointer	sp, resid, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are no pixels go on to the combining.  Since the unweighted
+	# average is computed here possibly skip the combining later.
+
+	# There must be at least max (1, nkeep) pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	} else if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# There must be at least two pixels for rejection.  The initial
+	# average is the low/high rejected average except in the case of
+	# just two pixels.  The rejections are iterated and the average
+	# is recomputed.  Corrections for scaling may be performed.
+	# Depending on other flags the image IDs may also need to be adjusted.
+
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 <= max (MINCLIP-1, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Memr[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Memr[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    repeat {
+		if (n1 == 2) {
+		    sum = Memr[d[1]+k]
+		    sum = sum + Memr[d[2]+k]
+		    a = sum / 2
+		} else {
+		    low = Memr[d[1]+k]
+		    high = Memr[d[2]+k]
+		    if (low > high) {
+			d1 = low
+			low = high
+			high = d1
+		    }
+		    sum = 0.
+		    do j = 3, n1 {
+		       d1 = Memr[d[j]+k]
+		       if (d1 < low) {
+			   sum = sum + low
+			   low = d1
+			} else if (d1 > high) {
+			    sum = sum + high
+			    high = d1
+			} else
+			    sum = sum + d1
+		    }
+		    a = sum / (n1 - 2)
+		    sum = sum + low + high
+		}
+		n2 = n1
+		if (doscale1) {
+		    for (j=1; j<=n1; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+
+			l = Memi[mp1]
+			s = scales[l]
+			d1 = max (zero, s * (a + zeros[l]))
+			s = sqrt (nm[1,l] + d1/nm[2,l] + (d1*nm[3,l])**2) / s
+
+			d1 = Memr[dp1]
+			r = (d1 - a) / s
+			if (r < -lsigma || r > hsigma) {
+			    Memr[resid+n1] = abs(r)
+			    if (j < n1) {
+				dp2 = d[n1] + k
+				Memr[dp1] = Memr[dp2]
+				Memr[dp2] = d1
+				mp2 = m[n1] + k
+				Memi[mp1] = Memi[mp2]
+				Memi[mp2] = l
+				j = j - 1
+			    }
+			    sum = sum - d1
+			    n1 = n1 - 1
+			}
+		    }
+		} else {
+		    if (!keepids) {
+			s = max (zero, a)
+			s = sqrt (nm[1,1] + s/nm[2,1] + (s*nm[3,1])**2)
+		    }
+		    for (j=1; j<=n1; j=j+1) {
+			if (keepids) {
+			    l = Memi[m[j]+k]
+			    s = max (zero, a)
+			    s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			}
+			dp1 = d[j] + k
+			d1 = Memr[dp1]
+			r = (d1 - a) / s
+			if (r < -lsigma || r > hsigma) {
+			    Memr[resid+n1] = abs(r)
+			    if (j < n1) {
+				dp2 = d[n1] + k
+				Memr[dp1] = Memr[dp2]
+				Memr[dp2] = d1
+				if (keepids) {
+				    mp1 = m[j] + k
+				    mp2 = m[n1] + k
+				    l = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				}
+				j = j - 1
+			    }
+			    sum = sum - d1
+			    n1 = n1 - 1
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Memr[dp1]
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Memr[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Memr[dp1]
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Memr[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+	    }
+
+	    n[i] = n1
+	    if (!docombine)
+		if (n1 > 0)
+		    average[i] = sum / n1
+		else
+		    average[i] = blank
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_CCDCLIP -- Reject pixels using CCD noise parameters about the median
+
+procedure ic_mccdclipr (d, m, n, scales, zeros, nm, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+real	nm[3,nimages]		# Noise model
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+real	r, s
+pointer	sp, resid, mp1, mp2
+real	med, zero
+data	zero /0.0/
+
+include	"../icombine.com"
+
+begin
+	# There must be at least max (MINCLIP, nkeep+1) pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Compute median and sigma and iteratively clip.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    nl = 1
+	    nh = n1
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 == 0)
+		    med = blank
+		else if (mod (n1, 2) == 0) {
+		    med = Memr[d[n3-1]+k]
+		    med = (med + Memr[d[n3]+k]) / 2.
+		} else
+		    med = Memr[d[n3]+k]
+
+		if (n1 >= max (MINCLIP, maxkeep+1)) {
+		    if (doscale1) {
+			for (; nl <= n2; nl = nl + 1) {
+			    l = Memi[m[nl]+k]
+			    s = scales[l]
+			    r = max (zero, s * (med + zeros[l]))
+			    s = sqrt (nm[1,l] + r/nm[2,l] + (r*nm[3,l])**2) / s
+			    r = (med - Memr[d[nl]+k]) / s
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    l = Memi[m[nh]+k]
+			    s = scales[l]
+			    r = max (zero, s * (med + zeros[l]))
+			    s = sqrt (nm[1,l] + r/nm[2,l] + (r*nm[3,l])**2) / s
+			    r = (Memr[d[nh]+k] - med) / s
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    } else {
+			if (!keepids) {
+			    s = max (zero, med)
+			    s = sqrt (nm[1,1] + s/nm[2,1] + (s*nm[3,1])**2)
+			}
+			for (; nl <= n2; nl = nl + 1) {
+			    if (keepids) {
+				l = Memi[m[nl]+k]
+				s = max (zero, med)
+				s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			    }
+			    r = (med - Memr[d[nl]+k]) / s
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    if (keepids) {
+				l = Memi[m[nh]+k]
+				s = max (zero, med)
+				s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			    }
+			    r = (Memr[d[nh]+k] -  med) / s
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Memr[d[l]+k] = Memr[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Memr[d[l]+k] = Memr[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median is computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/generic/icgdata.x b/noao/imred/ccdred/src/generic/icgdata.x
new file mode 100644
index 00000000..5c6ac18c
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/icgdata.x
@@ -0,0 +1,459 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	<mach.h>
+include	"../icombine.h"
+
+
+# IC_GDATA -- Get line of image and mask data and apply threshold and scaling.
+# Entirely empty lines are excluded.  The data are compacted within the
+# input data buffers.  If it is required, the connection to the original
+# image index is keeped in the returned m data pointers.
+
+procedure ic_gdatas (in, out, dbuf, d, id, n, m, lflag, offsets, scales,
+	zeros, nimages, npts, v1, v2)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+pointer	dbuf[nimages]		# Data buffers for nonaligned images
+pointer	d[nimages]		# Data pointers
+pointer	id[nimages]		# ID pointers
+int	n[npts]			# Number of good pixels
+pointer	m[nimages]		# Mask pointers
+int	lflag[nimages]		# Empty mask flags
+int	offsets[nimages,ARB]	# Image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero offset factors
+int	nimages			# Number of input images
+int	npts			# NUmber of output points per line
+long	v1[ARB], v2[ARB]	# Line vectors
+
+int	i, j, k, l, ndim, nused
+real	a, b
+pointer	buf, dp, ip, mp, imgnls()
+
+include	"../icombine.com"
+
+begin
+	# Get masks and return if there is no data
+	call ic_mget (in, out, offsets, v1, v2, m, lflag, nimages)
+	if (dflag == D_NONE)
+	    return
+
+	# Get data and fill data buffers.  Correct for offsets if needed.
+	ndim = IM_NDIM(out[1])
+	do i = 1, nimages {
+	    if (lflag[i] == D_NONE)
+		next
+	    if (aligned) {
+		call amovl (v1, v2, IM_MAXDIM)
+		if (project)
+		    v2[ndim+1] = i
+		j = imgnls (in[i], d[i], v2)
+	    } else {
+		v2[1] = v1[1]
+		do j = 2, ndim
+		    v2[j] = v1[j] - offsets[i,j]
+		if (project)
+		    v2[ndim+1] = i
+		j = imgnls (in[i], buf, v2)
+		call amovs (Mems[buf], Mems[dbuf[i]+offsets[i,1]],
+		    IM_LEN(in[i],1))
+		d[i] = dbuf[i]
+	    }
+	}
+
+	# Apply threshold if needed
+	if (dothresh) {
+	    do i = 1, nimages {
+		dp = d[i]
+		if (lflag[i] == D_ALL) {
+		    do j = 1, npts {
+			a = Mems[dp]
+			if (a < lthresh || a > hthresh) {
+			    Memi[m[i]+j-1] = 1
+			    lflag[i] = D_MIX
+			    dflag = D_MIX
+			}
+			dp = dp + 1
+		    }
+		} else if (lflag[i] == D_MIX) {
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    a = Mems[dp]
+			    if (a < lthresh || a > hthresh) {
+				Memi[m[i]+j-1] = 1
+				dflag = D_MIX
+			    }
+			}
+			dp = dp + 1
+			mp = mp + 1
+		    }
+		}
+
+		# Check for completely empty lines
+		if (lflag[i] == D_MIX) {
+		    lflag[i] = D_NONE
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    lflag[i] = D_MIX
+			    break
+			}
+			mp = mp + 1
+		    }
+		}
+	    }
+	}
+
+	# Apply scaling (avoiding masked pixels which might overflow?)
+	if (doscale) {
+	    if (dflag == D_ALL) {
+		do i = 1, nimages {
+		    dp = d[i]
+		    a = scales[i]
+		    b = -zeros[i]
+		    do j = 1, npts {
+			Mems[dp] = Mems[dp] / a + b
+			dp = dp + 1
+		    }
+		}
+	    } else if (dflag == D_MIX) {
+		do i = 1, nimages {
+		    dp = d[i]
+		    a = scales[i]
+		    b = -zeros[i]
+		    if (lflag[i] == D_ALL) {
+			do j = 1, npts {
+			    Mems[dp] = Mems[dp] / a + b
+			    dp = dp + 1
+			}
+		    } else if (lflag[i] == D_MIX) {
+			mp = m[i]
+			do j = 1, npts {
+			    if (Memi[mp] == 0)
+				Mems[dp] = Mems[dp] / a + b
+			    dp = dp + 1
+			    mp = mp + 1
+			}
+		    }
+		}
+	    }
+	}
+
+	# Sort pointers to exclude unused images.
+	# Use the lflag array to keep track of the image index.
+
+	if (dflag == D_ALL)
+	    nused = nimages
+	else {
+	    nused = 0
+	    do i = 1, nimages
+		if (lflag[i] != D_NONE) {
+		    nused = nused + 1
+		    d[nused] = d[i]
+		    m[nused] = m[i]
+		    lflag[nused] = i
+		}
+	    if (nused == 0)
+		dflag = D_NONE
+	}
+
+	# Compact data to remove bad pixels
+	# Keep track of the image indices if needed
+	# If growing mark the end of the included image indices with zero
+
+	if (dflag == D_ALL) {
+	    call amovki (nused, n, npts)
+	    if (keepids)
+		do i = 1, nimages
+		    call amovki (i, Memi[id[i]], npts)
+	} else if (dflag == D_NONE)
+	    call aclri (n, npts)
+	else {
+	    call aclri (n, npts)
+	    if (keepids) {
+		do i = 1, nused {
+		    l = lflag[i]
+		    dp = d[i]
+		    ip = id[i]
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    n[j] = n[j] + 1
+			    k = n[j]
+			    if (k < i) {
+				Mems[d[k]+j-1] = Mems[dp]
+				Memi[id[k]+j-1] = l
+			    } else
+				Memi[ip] = l
+			}
+			dp = dp + 1
+			ip = ip + 1
+			mp = mp + 1
+		    }
+		}
+		if (grow > 0) {
+		    do j = 1, npts {
+			do i = n[j]+1, nimages
+			    Memi[id[i]+j-1] = 0
+		    }
+		}
+	    } else {
+		do i = 1, nused {
+		    dp = d[i]
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    n[j] = n[j] + 1
+			    k = n[j]
+			    if (k < i)
+				Mems[d[k]+j-1] = Mems[dp]
+			}
+			dp = dp + 1
+			mp = mp + 1
+		    }
+		}
+	    }
+	}
+
+	# Sort the pixels and IDs if needed
+	if (mclip) {
+	    call malloc (dp, nimages, TY_SHORT)
+	    if (keepids) {
+		call malloc (ip, nimages, TY_INT)
+		call ic_2sorts (d, Mems[dp], id, Memi[ip], n, npts)
+		call mfree (ip, TY_INT)
+	    } else
+		call ic_sorts (d, Mems[dp], n, npts)
+	    call mfree (dp, TY_SHORT)
+	}
+end
+
+# IC_GDATA -- Get line of image and mask data and apply threshold and scaling.
+# Entirely empty lines are excluded.  The data are compacted within the
+# input data buffers.  If it is required, the connection to the original
+# image index is keeped in the returned m data pointers.
+
+procedure ic_gdatar (in, out, dbuf, d, id, n, m, lflag, offsets, scales,
+	zeros, nimages, npts, v1, v2)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+pointer	dbuf[nimages]		# Data buffers for nonaligned images
+pointer	d[nimages]		# Data pointers
+pointer	id[nimages]		# ID pointers
+int	n[npts]			# Number of good pixels
+pointer	m[nimages]		# Mask pointers
+int	lflag[nimages]		# Empty mask flags
+int	offsets[nimages,ARB]	# Image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero offset factors
+int	nimages			# Number of input images
+int	npts			# NUmber of output points per line
+long	v1[ARB], v2[ARB]	# Line vectors
+
+int	i, j, k, l, ndim, nused
+real	a, b
+pointer	buf, dp, ip, mp, imgnlr()
+
+include	"../icombine.com"
+
+begin
+	# Get masks and return if there is no data
+	call ic_mget (in, out, offsets, v1, v2, m, lflag, nimages)
+	if (dflag == D_NONE)
+	    return
+
+	# Get data and fill data buffers.  Correct for offsets if needed.
+	ndim = IM_NDIM(out[1])
+	do i = 1, nimages {
+	    if (lflag[i] == D_NONE)
+		next
+	    if (aligned) {
+		call amovl (v1, v2, IM_MAXDIM)
+		if (project)
+		    v2[ndim+1] = i
+		j = imgnlr (in[i], d[i], v2)
+	    } else {
+		v2[1] = v1[1]
+		do j = 2, ndim
+		    v2[j] = v1[j] - offsets[i,j]
+		if (project)
+		    v2[ndim+1] = i
+		j = imgnlr (in[i], buf, v2)
+		call amovr (Memr[buf], Memr[dbuf[i]+offsets[i,1]],
+		    IM_LEN(in[i],1))
+		d[i] = dbuf[i]
+	    }
+	}
+
+	# Apply threshold if needed
+	if (dothresh) {
+	    do i = 1, nimages {
+		dp = d[i]
+		if (lflag[i] == D_ALL) {
+		    do j = 1, npts {
+			a = Memr[dp]
+			if (a < lthresh || a > hthresh) {
+			    Memi[m[i]+j-1] = 1
+			    lflag[i] = D_MIX
+			    dflag = D_MIX
+			}
+			dp = dp + 1
+		    }
+		} else if (lflag[i] == D_MIX) {
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    a = Memr[dp]
+			    if (a < lthresh || a > hthresh) {
+				Memi[m[i]+j-1] = 1
+				dflag = D_MIX
+			    }
+			}
+			dp = dp + 1
+			mp = mp + 1
+		    }
+		}
+
+		# Check for completely empty lines
+		if (lflag[i] == D_MIX) {
+		    lflag[i] = D_NONE
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    lflag[i] = D_MIX
+			    break
+			}
+			mp = mp + 1
+		    }
+		}
+	    }
+	}
+
+	# Apply scaling (avoiding masked pixels which might overflow?)
+	if (doscale) {
+	    if (dflag == D_ALL) {
+		do i = 1, nimages {
+		    dp = d[i]
+		    a = scales[i]
+		    b = -zeros[i]
+		    do j = 1, npts {
+			Memr[dp] = Memr[dp] / a + b
+			dp = dp + 1
+		    }
+		}
+	    } else if (dflag == D_MIX) {
+		do i = 1, nimages {
+		    dp = d[i]
+		    a = scales[i]
+		    b = -zeros[i]
+		    if (lflag[i] == D_ALL) {
+			do j = 1, npts {
+			    Memr[dp] = Memr[dp] / a + b
+			    dp = dp + 1
+			}
+		    } else if (lflag[i] == D_MIX) {
+			mp = m[i]
+			do j = 1, npts {
+			    if (Memi[mp] == 0)
+				Memr[dp] = Memr[dp] / a + b
+			    dp = dp + 1
+			    mp = mp + 1
+			}
+		    }
+		}
+	    }
+	}
+
+	# Sort pointers to exclude unused images.
+	# Use the lflag array to keep track of the image index.
+
+	if (dflag == D_ALL)
+	    nused = nimages
+	else {
+	    nused = 0
+	    do i = 1, nimages
+		if (lflag[i] != D_NONE) {
+		    nused = nused + 1
+		    d[nused] = d[i]
+		    m[nused] = m[i]
+		    lflag[nused] = i
+		}
+	    if (nused == 0)
+		dflag = D_NONE
+	}
+
+	# Compact data to remove bad pixels
+	# Keep track of the image indices if needed
+	# If growing mark the end of the included image indices with zero
+
+	if (dflag == D_ALL) {
+	    call amovki (nused, n, npts)
+	    if (keepids)
+		do i = 1, nimages
+		    call amovki (i, Memi[id[i]], npts)
+	} else if (dflag == D_NONE)
+	    call aclri (n, npts)
+	else {
+	    call aclri (n, npts)
+	    if (keepids) {
+		do i = 1, nused {
+		    l = lflag[i]
+		    dp = d[i]
+		    ip = id[i]
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    n[j] = n[j] + 1
+			    k = n[j]
+			    if (k < i) {
+				Memr[d[k]+j-1] = Memr[dp]
+				Memi[id[k]+j-1] = l
+			    } else
+				Memi[ip] = l
+			}
+			dp = dp + 1
+			ip = ip + 1
+			mp = mp + 1
+		    }
+		}
+		if (grow > 0) {
+		    do j = 1, npts {
+			do i = n[j]+1, nimages
+			    Memi[id[i]+j-1] = 0
+		    }
+		}
+	    } else {
+		do i = 1, nused {
+		    dp = d[i]
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    n[j] = n[j] + 1
+			    k = n[j]
+			    if (k < i)
+				Memr[d[k]+j-1] = Memr[dp]
+			}
+			dp = dp + 1
+			mp = mp + 1
+		    }
+		}
+	    }
+	}
+
+	# Sort the pixels and IDs if needed
+	if (mclip) {
+	    call malloc (dp, nimages, TY_REAL)
+	    if (keepids) {
+		call malloc (ip, nimages, TY_INT)
+		call ic_2sortr (d, Memr[dp], id, Memi[ip], n, npts)
+		call mfree (ip, TY_INT)
+	    } else
+		call ic_sortr (d, Memr[dp], n, npts)
+	    call mfree (dp, TY_REAL)
+	}
+end
+
diff --git a/noao/imred/ccdred/src/generic/icgrow.x b/noao/imred/ccdred/src/generic/icgrow.x
new file mode 100644
index 00000000..b94e1cbc
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/icgrow.x
@@ -0,0 +1,148 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+
+# IC_GROW --  Reject neigbors of rejected pixels.
+# The rejected pixels are marked by having nonzero ids beyond the number
+# of included pixels.  The pixels rejected here are given zero ids
+# to avoid growing of the pixels rejected here.  The unweighted average
+# can be updated but any rejected pixels requires the median to be
+# recomputed.  When the number of pixels at a grow point reaches nkeep 
+# no further pixels are rejected.  Note that the rejection order is not
+# based on the magnitude of the residuals and so a grow from a weakly
+# rejected image pixel may take precedence over a grow from a strongly
+# rejected image pixel.
+
+procedure ic_grows (d, m, n, nimages, npts, average)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image id pointers
+int	n[npts]			# Number of good pixels
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i1, i2, j1, j2, k1, k2, l, is, ie, n2, maxkeep
+pointer	mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_NONE)
+	    return
+
+	do i1 = 1, npts {
+	    k1 = i1 - 1
+	    is = max (1, i1 - grow)
+	    ie = min (npts, i1 + grow)
+	    do j1 = n[i1]+1, nimages {
+		l = Memi[m[j1]+k1]
+		if (l == 0)
+		    next
+		if (combine == MEDIAN)
+		    docombine = true
+
+		do i2 = is, ie {
+		    if (i2 == i1)
+			next
+		    k2 = i2 - 1
+		    n2 = n[i2]
+		    if (nkeep < 0)
+			maxkeep = max (0, n2 + nkeep)
+		    else
+			maxkeep = min (n2, nkeep)
+		    if (n2 <= maxkeep)
+			next
+		    do j2 = 1, n2 {
+			mp1 = m[j2] + k2
+			if (Memi[mp1] == l) {
+			    if (!docombine && n2 > 1)
+				average[i2] =
+				    (n2*average[i2] - Mems[d[j2]+k2]) / (n2-1)
+			    mp2 = m[n2] + k2
+			    if (j2 < n2) {
+				Mems[d[j2]+k2] = Mems[d[n2]+k2]
+				Memi[mp1] = Memi[mp2]
+			    }
+			    Memi[mp2] = 0
+			    n[i2] = n2 - 1
+			    break
+			}
+		    }
+		}
+	    }
+	}
+end
+
+# IC_GROW --  Reject neigbors of rejected pixels.
+# The rejected pixels are marked by having nonzero ids beyond the number
+# of included pixels.  The pixels rejected here are given zero ids
+# to avoid growing of the pixels rejected here.  The unweighted average
+# can be updated but any rejected pixels requires the median to be
+# recomputed.  When the number of pixels at a grow point reaches nkeep 
+# no further pixels are rejected.  Note that the rejection order is not
+# based on the magnitude of the residuals and so a grow from a weakly
+# rejected image pixel may take precedence over a grow from a strongly
+# rejected image pixel.
+
+procedure ic_growr (d, m, n, nimages, npts, average)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image id pointers
+int	n[npts]			# Number of good pixels
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i1, i2, j1, j2, k1, k2, l, is, ie, n2, maxkeep
+pointer	mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_NONE)
+	    return
+
+	do i1 = 1, npts {
+	    k1 = i1 - 1
+	    is = max (1, i1 - grow)
+	    ie = min (npts, i1 + grow)
+	    do j1 = n[i1]+1, nimages {
+		l = Memi[m[j1]+k1]
+		if (l == 0)
+		    next
+		if (combine == MEDIAN)
+		    docombine = true
+
+		do i2 = is, ie {
+		    if (i2 == i1)
+			next
+		    k2 = i2 - 1
+		    n2 = n[i2]
+		    if (nkeep < 0)
+			maxkeep = max (0, n2 + nkeep)
+		    else
+			maxkeep = min (n2, nkeep)
+		    if (n2 <= maxkeep)
+			next
+		    do j2 = 1, n2 {
+			mp1 = m[j2] + k2
+			if (Memi[mp1] == l) {
+			    if (!docombine && n2 > 1)
+				average[i2] =
+				    (n2*average[i2] - Memr[d[j2]+k2]) / (n2-1)
+			    mp2 = m[n2] + k2
+			    if (j2 < n2) {
+				Memr[d[j2]+k2] = Memr[d[n2]+k2]
+				Memi[mp1] = Memi[mp2]
+			    }
+			    Memi[mp2] = 0
+			    n[i2] = n2 - 1
+			    break
+			}
+		    }
+		}
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/src/generic/icmedian.x b/noao/imred/ccdred/src/generic/icmedian.x
new file mode 100644
index 00000000..ec0166ba
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/icmedian.x
@@ -0,0 +1,343 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+
+# IC_MEDIAN -- Median of lines
+
+procedure ic_medians (d, n, npts, median)
+
+pointer	d[ARB]			# Input data line pointers
+int	n[npts]			# Number of good pixels
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, j1, j2, n1, lo, up, lo1, up1
+bool	even
+real	val1, val2, val3
+short	temp, wtemp
+
+include	"../icombine.com"
+
+begin
+	# If no data return after possibly setting blank values.
+	if (dflag == D_NONE) {
+	    do i = 1, npts
+		median[i]= blank
+	    return
+	}
+
+	# If the data were previously sorted then directly compute the median.
+	if (mclip) {
+	    if (dflag == D_ALL) {
+		n1 = n[1]
+		even = (mod (n1, 2) == 0)
+		j1 = n1 / 2 + 1
+		j2 = n1 / 2
+		do i = 1, npts {
+		    k = i - 1
+		    if (even) {
+			val1 = Mems[d[j1]+k]
+			val2 = Mems[d[j2]+k]
+			median[i] = (val1 + val2) / 2.
+		    } else
+			median[i] = Mems[d[j1]+k]
+		}
+	    } else {
+		do i = 1, npts {
+		    k = i - 1
+		    n1 = n[i]
+		    if (n1 > 0) {
+			j1 = n1 / 2 + 1
+			if (mod (n1, 2) == 0) {
+			    j2 = n1 / 2
+			    val1 = Mems[d[j1]+k]
+			    val2 = Mems[d[j2]+k]
+			    median[i] = (val1 + val2) / 2.
+			} else
+			    median[i] = Mems[d[j1]+k]
+		    } else
+			median[i] = blank
+		}
+	    }
+	    return
+	}
+
+	# Compute the median.
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+
+	    # If there are more than 3 points use Wirth algorithm.  This
+	    # is the same as vops$amed.gx except for an even number of
+	    # points it selects the middle two and averages.
+	    if (n1 > 3) {
+		lo = 1
+		up = n1
+		j  = max (lo, min (up, (up+1)/2))
+
+		while (lo < up) {
+		    if (! (lo < up))
+			break
+
+		    temp = Mems[d[j]+k];  lo1 = lo;  up1 = up
+
+		    repeat {
+			while (Mems[d[lo1]+k] < temp)
+			    lo1 = lo1 + 1
+			while (temp < Mems[d[up1]+k])
+			    up1 = up1 - 1
+			if (lo1 <= up1) {
+			    wtemp = Mems[d[lo1]+k]
+			    Mems[d[lo1]+k] = Mems[d[up1]+k]
+			    Mems[d[up1]+k] = wtemp
+			    lo1 = lo1 + 1;  up1 = up1 - 1
+			}
+		    } until (lo1 > up1)
+
+		    if (up1 < j)
+			lo = lo1
+		    if (j < lo1)
+			up = up1
+		}
+
+		median[i] = Mems[d[j]+k]
+
+		if (mod (n1,2) == 0) {
+		    lo = 1
+		    up = n1
+		    j  = max (lo, min (up, (up+1)/2)+1)
+
+		    while (lo < up) {
+			if (! (lo < up))
+			    break
+
+			temp = Mems[d[j]+k];  lo1 = lo;  up1 = up
+
+			repeat {
+			    while (Mems[d[lo1]+k] < temp)
+				lo1 = lo1 + 1
+			    while (temp < Mems[d[up1]+k])
+				up1 = up1 - 1
+			    if (lo1 <= up1) {
+				wtemp = Mems[d[lo1]+k]
+				Mems[d[lo1]+k] = Mems[d[up1]+k]
+				Mems[d[up1]+k] = wtemp
+				lo1 = lo1 + 1;  up1 = up1 - 1
+			    }
+			} until (lo1 > up1)
+
+			if (up1 < j)
+			    lo = lo1
+			if (j < lo1)
+			    up = up1
+		    }
+		    median[i] = (median[i] + Mems[d[j]+k]) / 2
+		}
+
+	    # If 3 points find the median directly.
+	    } else if (n1 == 3) {
+	        val1 = Mems[d[1]+k]
+	        val2 = Mems[d[2]+k]
+	        val3 = Mems[d[3]+k]
+	        if (val1 < val2) {
+		    if (val2 < val3)		# abc
+		        median[i] = val2
+		    else if (val1 < val3)	# acb
+		        median[i] = val3
+		    else			# cab
+		        median[i] = val1
+	        } else {
+		    if (val2 > val3)		# cba
+		        median[i] = val2
+		    else if (val1 > val3)	# bca
+		        median[i] = val3
+		    else			# bac
+		        median[i] = val1
+	        }
+
+	    # If 2 points average.
+	    } else if (n1 == 2) {
+		val1 = Mems[d[1]+k]
+		val2 = Mems[d[2]+k]
+		median[i] = (val1 + val2) / 2
+
+	    # If 1 point return the value.
+	    } else if (n1 == 1)
+		median[i] = Mems[d[1]+k]
+
+	    # If no points return with a possibly blank value.
+	    else
+		median[i] = blank
+	}
+end
+
+# IC_MEDIAN -- Median of lines
+
+procedure ic_medianr (d, n, npts, median)
+
+pointer	d[ARB]			# Input data line pointers
+int	n[npts]			# Number of good pixels
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, j1, j2, n1, lo, up, lo1, up1
+bool	even
+real	val1, val2, val3
+real	temp, wtemp
+
+include	"../icombine.com"
+
+begin
+	# If no data return after possibly setting blank values.
+	if (dflag == D_NONE) {
+	    do i = 1, npts
+		median[i]= blank
+	    return
+	}
+
+	# If the data were previously sorted then directly compute the median.
+	if (mclip) {
+	    if (dflag == D_ALL) {
+		n1 = n[1]
+		even = (mod (n1, 2) == 0)
+		j1 = n1 / 2 + 1
+		j2 = n1 / 2
+		do i = 1, npts {
+		    k = i - 1
+		    if (even) {
+			val1 = Memr[d[j1]+k]
+			val2 = Memr[d[j2]+k]
+			median[i] = (val1 + val2) / 2.
+		    } else
+			median[i] = Memr[d[j1]+k]
+		}
+	    } else {
+		do i = 1, npts {
+		    k = i - 1
+		    n1 = n[i]
+		    if (n1 > 0) {
+			j1 = n1 / 2 + 1
+			if (mod (n1, 2) == 0) {
+			    j2 = n1 / 2
+			    val1 = Memr[d[j1]+k]
+			    val2 = Memr[d[j2]+k]
+			    median[i] = (val1 + val2) / 2.
+			} else
+			    median[i] = Memr[d[j1]+k]
+		    } else
+			median[i] = blank
+		}
+	    }
+	    return
+	}
+
+	# Compute the median.
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+
+	    # If there are more than 3 points use Wirth algorithm.  This
+	    # is the same as vops$amed.gx except for an even number of
+	    # points it selects the middle two and averages.
+	    if (n1 > 3) {
+		lo = 1
+		up = n1
+		j  = max (lo, min (up, (up+1)/2))
+
+		while (lo < up) {
+		    if (! (lo < up))
+			break
+
+		    temp = Memr[d[j]+k];  lo1 = lo;  up1 = up
+
+		    repeat {
+			while (Memr[d[lo1]+k] < temp)
+			    lo1 = lo1 + 1
+			while (temp < Memr[d[up1]+k])
+			    up1 = up1 - 1
+			if (lo1 <= up1) {
+			    wtemp = Memr[d[lo1]+k]
+			    Memr[d[lo1]+k] = Memr[d[up1]+k]
+			    Memr[d[up1]+k] = wtemp
+			    lo1 = lo1 + 1;  up1 = up1 - 1
+			}
+		    } until (lo1 > up1)
+
+		    if (up1 < j)
+			lo = lo1
+		    if (j < lo1)
+			up = up1
+		}
+
+		median[i] = Memr[d[j]+k]
+
+		if (mod (n1,2) == 0) {
+		    lo = 1
+		    up = n1
+		    j  = max (lo, min (up, (up+1)/2)+1)
+
+		    while (lo < up) {
+			if (! (lo < up))
+			    break
+
+			temp = Memr[d[j]+k];  lo1 = lo;  up1 = up
+
+			repeat {
+			    while (Memr[d[lo1]+k] < temp)
+				lo1 = lo1 + 1
+			    while (temp < Memr[d[up1]+k])
+				up1 = up1 - 1
+			    if (lo1 <= up1) {
+				wtemp = Memr[d[lo1]+k]
+				Memr[d[lo1]+k] = Memr[d[up1]+k]
+				Memr[d[up1]+k] = wtemp
+				lo1 = lo1 + 1;  up1 = up1 - 1
+			    }
+			} until (lo1 > up1)
+
+			if (up1 < j)
+			    lo = lo1
+			if (j < lo1)
+			    up = up1
+		    }
+		    median[i] = (median[i] + Memr[d[j]+k]) / 2
+		}
+
+	    # If 3 points find the median directly.
+	    } else if (n1 == 3) {
+	        val1 = Memr[d[1]+k]
+	        val2 = Memr[d[2]+k]
+	        val3 = Memr[d[3]+k]
+	        if (val1 < val2) {
+		    if (val2 < val3)		# abc
+		        median[i] = val2
+		    else if (val1 < val3)	# acb
+		        median[i] = val3
+		    else			# cab
+		        median[i] = val1
+	        } else {
+		    if (val2 > val3)		# cba
+		        median[i] = val2
+		    else if (val1 > val3)	# bca
+		        median[i] = val3
+		    else			# bac
+		        median[i] = val1
+	        }
+
+	    # If 2 points average.
+	    } else if (n1 == 2) {
+		val1 = Memr[d[1]+k]
+		val2 = Memr[d[2]+k]
+		median[i] = (val1 + val2) / 2
+
+	    # If 1 point return the value.
+	    } else if (n1 == 1)
+		median[i] = Memr[d[1]+k]
+
+	    # If no points return with a possibly blank value.
+	    else
+		median[i] = blank
+	}
+end
+
diff --git a/noao/imred/ccdred/src/generic/icmm.x b/noao/imred/ccdred/src/generic/icmm.x
new file mode 100644
index 00000000..259759bd
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/icmm.x
@@ -0,0 +1,300 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+
+# IC_MM --  Reject a specified number of high and low pixels
+
+procedure ic_mms (d, m, n, npts)
+
+pointer	d[ARB]		# Data pointers
+pointer	m[ARB]		# Image ID pointers
+int	n[npts]			# Number of good pixels
+int	npts			# Number of output points per line
+
+int	n1, ncombine, npairs, nlow, nhigh, np
+int	i, i1, j, jmax, jmin
+pointer	k, kmax, kmin
+short	d1, d2, dmin, dmax
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_NONE)
+	    return
+
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    nlow = flow * n1 + 0.001
+	    nhigh = fhigh * n1 + 0.001
+	    ncombine = n1 - nlow -  nhigh
+	    npairs = min (nlow, nhigh)
+	    nlow = nlow - npairs
+	    nhigh = nhigh - npairs
+	}
+
+	do i = 1, npts {
+	    i1 = i - 1
+	    n1 = n[i]
+	    if (dflag == D_MIX) {
+		nlow = flow * n1 + 0.001
+		nhigh = fhigh * n1 + 0.001
+		ncombine = max (ncombine, n1 - nlow - nhigh)
+		npairs = min (nlow, nhigh)
+		nlow = nlow - npairs
+		nhigh = nhigh - npairs
+	    }
+
+	    # Reject the npairs low and high points.
+	    do np = 1, npairs {
+		k = d[1] + i1
+		d1 = Mems[k]
+		dmax = d1; dmin = d1; jmax = 1; jmin = 1; kmax = k; kmin = k
+		do j = 2, n1 {
+		    d2 = d1
+		    k = d[j] + i1
+		    d1 = Mems[k]
+		    if (d1 > dmax) {
+			dmax = d1; jmax = j; kmax = k
+		    } else if (d1 < dmin) {
+			dmin = d1; jmin = j; kmin = k
+		    }
+		}
+		j = n1 - 1
+		if (keepids) {
+		    if (jmax < j) {
+			if (jmin != j) {
+			    Mems[kmax] = d2
+			    Memi[m[jmax]+i1] = Memi[m[j]+i1]
+			} else {
+			    Mems[kmax] = d1
+			    Memi[m[jmax]+i1] = Memi[m[n1]+i1]
+			}
+		    }
+		    if (jmin < j) {
+			if (jmax != n1) {
+			    Mems[kmin] = d1
+			    Memi[m[jmin]+i1] = Memi[m[n1]+i1]
+			} else {
+			    Mems[kmin] = d2
+			    Memi[m[jmin]+i1] = Memi[m[j]+i1]
+			}
+		    }
+		} else {
+		    if (jmax < j) {
+			if (jmin != j)
+			    Mems[kmax] = d2
+			else
+			    Mems[kmax] = d1
+		    }
+		    if (jmin < j) {
+			if (jmax != n1)
+			    Mems[kmin] = d1
+			else
+			    Mems[kmin] = d2
+		    }
+		}
+		n1 = n1 - 2
+	    }
+
+	    # Reject the excess low points.
+	    do np = 1, nlow {
+		k = d[1] + i1
+		d1 = Mems[k]
+		dmin = d1; jmin = 1; kmin = k
+		do j = 2, n1 {
+		    k = d[j] + i1
+		    d1 = Mems[k]
+		    if (d1 < dmin) {
+			dmin = d1; jmin = j; kmin = k
+		    }
+		}
+		if (keepids) {
+		    if (jmin < n1) {
+			Mems[kmin] = d1
+			Memi[m[jmin]+i1] = Memi[m[n1]+i1]
+		    }
+		} else {
+		    if (jmin < n1)
+			Mems[kmin] = d1
+		}
+		n1 = n1 - 1 
+	    }
+
+	    # Reject the excess high points.
+	    do np = 1, nhigh {
+		k = d[1] + i1
+		d1 = Mems[k]
+		dmax = d1; jmax = 1; kmax = k
+		do j = 2, n1 {
+		    k = d[j] + i1
+		    d1 = Mems[k]
+		    if (d1 > dmax) {
+			dmax = d1; jmax = j; kmax = k
+		    }
+		}
+		if (keepids) {
+		    if (jmax < n1) {
+			Mems[kmax] = d1
+			Memi[m[jmax]+i1] = Memi[m[n1]+i1]
+		    }
+		} else {
+		    if (jmax < n1)
+			Mems[kmax] = d1
+		}
+		n1 = n1 - 1 
+	    }
+	    n[i] = n1
+	}
+
+	if (dflag == D_ALL && npairs + nlow + nhigh > 0)
+		dflag = D_MIX
+end
+
+# IC_MM --  Reject a specified number of high and low pixels
+
+procedure ic_mmr (d, m, n, npts)
+
+pointer	d[ARB]		# Data pointers
+pointer	m[ARB]		# Image ID pointers
+int	n[npts]			# Number of good pixels
+int	npts			# Number of output points per line
+
+int	n1, ncombine, npairs, nlow, nhigh, np
+int	i, i1, j, jmax, jmin
+pointer	k, kmax, kmin
+real	d1, d2, dmin, dmax
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_NONE)
+	    return
+
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    nlow = flow * n1 + 0.001
+	    nhigh = fhigh * n1 + 0.001
+	    ncombine = n1 - nlow -  nhigh
+	    npairs = min (nlow, nhigh)
+	    nlow = nlow - npairs
+	    nhigh = nhigh - npairs
+	}
+
+	do i = 1, npts {
+	    i1 = i - 1
+	    n1 = n[i]
+	    if (dflag == D_MIX) {
+		nlow = flow * n1 + 0.001
+		nhigh = fhigh * n1 + 0.001
+		ncombine = max (ncombine, n1 - nlow - nhigh)
+		npairs = min (nlow, nhigh)
+		nlow = nlow - npairs
+		nhigh = nhigh - npairs
+	    }
+
+	    # Reject the npairs low and high points.
+	    do np = 1, npairs {
+		k = d[1] + i1
+		d1 = Memr[k]
+		dmax = d1; dmin = d1; jmax = 1; jmin = 1; kmax = k; kmin = k
+		do j = 2, n1 {
+		    d2 = d1
+		    k = d[j] + i1
+		    d1 = Memr[k]
+		    if (d1 > dmax) {
+			dmax = d1; jmax = j; kmax = k
+		    } else if (d1 < dmin) {
+			dmin = d1; jmin = j; kmin = k
+		    }
+		}
+		j = n1 - 1
+		if (keepids) {
+		    if (jmax < j) {
+			if (jmin != j) {
+			    Memr[kmax] = d2
+			    Memi[m[jmax]+i1] = Memi[m[j]+i1]
+			} else {
+			    Memr[kmax] = d1
+			    Memi[m[jmax]+i1] = Memi[m[n1]+i1]
+			}
+		    }
+		    if (jmin < j) {
+			if (jmax != n1) {
+			    Memr[kmin] = d1
+			    Memi[m[jmin]+i1] = Memi[m[n1]+i1]
+			} else {
+			    Memr[kmin] = d2
+			    Memi[m[jmin]+i1] = Memi[m[j]+i1]
+			}
+		    }
+		} else {
+		    if (jmax < j) {
+			if (jmin != j)
+			    Memr[kmax] = d2
+			else
+			    Memr[kmax] = d1
+		    }
+		    if (jmin < j) {
+			if (jmax != n1)
+			    Memr[kmin] = d1
+			else
+			    Memr[kmin] = d2
+		    }
+		}
+		n1 = n1 - 2
+	    }
+
+	    # Reject the excess low points.
+	    do np = 1, nlow {
+		k = d[1] + i1
+		d1 = Memr[k]
+		dmin = d1; jmin = 1; kmin = k
+		do j = 2, n1 {
+		    k = d[j] + i1
+		    d1 = Memr[k]
+		    if (d1 < dmin) {
+			dmin = d1; jmin = j; kmin = k
+		    }
+		}
+		if (keepids) {
+		    if (jmin < n1) {
+			Memr[kmin] = d1
+			Memi[m[jmin]+i1] = Memi[m[n1]+i1]
+		    }
+		} else {
+		    if (jmin < n1)
+			Memr[kmin] = d1
+		}
+		n1 = n1 - 1 
+	    }
+
+	    # Reject the excess high points.
+	    do np = 1, nhigh {
+		k = d[1] + i1
+		d1 = Memr[k]
+		dmax = d1; jmax = 1; kmax = k
+		do j = 2, n1 {
+		    k = d[j] + i1
+		    d1 = Memr[k]
+		    if (d1 > dmax) {
+			dmax = d1; jmax = j; kmax = k
+		    }
+		}
+		if (keepids) {
+		    if (jmax < n1) {
+			Memr[kmax] = d1
+			Memi[m[jmax]+i1] = Memi[m[n1]+i1]
+		    }
+		} else {
+		    if (jmax < n1)
+			Memr[kmax] = d1
+		}
+		n1 = n1 - 1 
+	    }
+	    n[i] = n1
+	}
+
+	if (dflag == D_ALL && npairs + nlow + nhigh > 0)
+		dflag = D_MIX
+end
diff --git a/noao/imred/ccdred/src/generic/icombine.x b/noao/imred/ccdred/src/generic/icombine.x
new file mode 100644
index 00000000..b4ff60be
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/icombine.x
@@ -0,0 +1,607 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	<imset.h>
+include	<error.h>
+include	<syserr.h>
+include	<mach.h>
+include	"../icombine.h"
+
+
+# ICOMBINE -- Combine images
+#
+# The memory and open file descriptor limits are checked and an attempt
+# to recover is made either by setting the image pixel files to be
+# closed after I/O or by notifying the calling program that memory
+# ran out and the IMIO buffer size should be reduced.  After the checks
+# a procedure for the selected combine option is called.
+# Because there may be several failure modes when reaching the file
+# limits we first assume an error is due to the file limit, except for
+# out of memory, and close some pixel files.  If the error then repeats
+# on accessing the pixels the error is passed back.
+
+
+procedure icombines (in, out, offsets, nimages, bufsize)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+int	offsets[nimages,ARB]	# Input image offsets
+int	nimages			# Number of input images
+int	bufsize			# IMIO buffer size
+
+char	str[1]
+int	i, j, npts, fd, stropen(), errcode(), imstati()
+pointer	sp, d, id, n, m, lflag, scales, zeros, wts, dbuf
+pointer	buf, imgl1s(), impl1i()
+errchk	stropen, imgl1s, impl1i
+pointer	impl1r()
+errchk	impl1r
+
+include	"../icombine.com"
+
+begin
+	npts = IM_LEN(out[1],1)
+
+	# Allocate memory.
+	call smark (sp)
+	call salloc (d, nimages, TY_POINTER)
+	call salloc (id, nimages, TY_POINTER)
+	call salloc (n, npts, TY_INT)
+	call salloc (m, nimages, TY_POINTER)
+	call salloc (lflag, nimages, TY_INT)
+	call salloc (scales, nimages, TY_REAL)
+	call salloc (zeros, nimages, TY_REAL)
+	call salloc (wts, nimages, TY_REAL)
+	call amovki (D_ALL, Memi[lflag], nimages)
+
+	# If aligned use the IMIO buffer otherwise we need vectors of
+	# output length.
+
+	if (!aligned) {
+	    call salloc (dbuf, nimages, TY_POINTER)
+	    do i = 1, nimages
+		call salloc (Memi[dbuf+i-1], npts, TY_SHORT)
+	}
+
+	if (project) {
+	    call imseti (in[1], IM_NBUFS, nimages)
+	    call imseti (in[1], IM_BUFSIZE, bufsize)
+	    do i = 1, 3 {
+		if (out[i] != NULL)
+		    call imseti (out[i], IM_BUFSIZE, bufsize)
+	    }
+	} else {
+	    # Reserve FD for string operations.
+	    fd = stropen (str, 1, NEW_FILE)
+
+	    # Do I/O to the images.
+	    do i = 1, 3 {
+		if (out[i] != NULL)
+		    call imseti (out[i], IM_BUFSIZE, bufsize)
+	    }
+	    buf = impl1r (out[1])
+	    call aclrr (Memr[buf], npts)
+	    if (out[3] != NULL) {
+		buf = impl1r (out[3])
+		call aclrr (Memr[buf], npts)
+	    }
+	    if (out[2] != NULL) {
+		buf = impl1i (out[2])
+		call aclri (Memi[buf], npts)
+	    }
+
+	    do i = 1, nimages {
+		call imseti (in[i], IM_BUFSIZE, bufsize)
+		iferr (buf = imgl1s (in[i])) {
+		    switch (errcode()) {
+		    case SYS_MFULL:
+			call sfree (sp)
+			call strclose (fd)
+			call erract (EA_ERROR)
+		    case SYS_FTOOMANYFILES, SYS_IKIOPIX:
+			if (imstati (in[i], IM_CLOSEFD) == YES) {
+			    call sfree (sp)
+			    call strclose (fd)
+			    call erract (EA_ERROR)
+			}
+			do j = i-2, nimages
+			    call imseti (in[j], IM_CLOSEFD, YES)
+			buf = imgl1s (in[i])
+		    default:
+			call sfree (sp)
+			call strclose (fd)
+			call erract (EA_ERROR)
+		    }
+		}
+	    }
+
+	    call strclose (fd)
+	}
+
+	call ic_combines (in, out, Memi[dbuf], Memi[d], Memi[id], Memi[n],
+	    Memi[m], Memi[lflag], offsets, Memr[scales], Memr[zeros],
+	    Memr[wts], nimages, npts)
+end
+
+
+# IC_COMBINE -- Combine images.
+
+procedure ic_combines (in, out, dbuf, d, id, n, m, lflag, offsets,
+	scales, zeros, wts, nimages, npts)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output image
+pointer	dbuf[nimages]		# Data buffers for nonaligned images
+pointer	d[nimages]		# Data pointers
+pointer	id[nimages]		# Image index ID pointers
+int	n[npts]			# Number of good pixels
+pointer	m[nimages]		# Mask pointers
+int	lflag[nimages]		# Line flags
+int	offsets[nimages,ARB]	# Input image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero offset factors
+real	wts[nimages]		# Combining weights
+int	nimages			# Number of input images
+int	npts			# Number of points per output line
+
+int	i, ctor()
+real	r, imgetr()
+pointer	sp, v1, v2, v3, outdata, buf, nm, impnli()
+pointer	impnlr()
+errchk	ic_scale, imgetr
+
+include	"../icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (v1, IM_MAXDIM, TY_LONG)
+	call salloc (v2, IM_MAXDIM, TY_LONG)
+	call salloc (v3, IM_MAXDIM, TY_LONG)
+	call amovkl (long(1), Meml[v1], IM_MAXDIM)
+	call amovkl (long(1), Meml[v2], IM_MAXDIM)
+	call amovkl (long(1), Meml[v3], IM_MAXDIM)
+
+	call ic_scale (in, out, offsets, scales, zeros, wts, nimages)
+
+	# Set combine parameters
+	switch (combine) {
+	case AVERAGE:
+	    if (dowts)
+		keepids = true
+	    else
+		keepids = false
+	case MEDIAN:
+	    dowts = false
+	    keepids = false
+	}
+	docombine = true
+
+	# Set rejection algorithm specific parameters
+	switch (reject) {
+	case CCDCLIP, CRREJECT:
+	    call salloc (nm, 3*nimages, TY_REAL)
+	    i = 1
+	    if (ctor (Memc[rdnoise], i, r) > 0) {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)] = r
+	    } else {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)] = imgetr (in[i], Memc[rdnoise])
+	    }
+	    i = 1
+	    if (ctor (Memc[gain], i, r) > 0) {
+		do i = 1, nimages {
+		    Memr[nm+3*(i-1)+1] = r
+		    Memr[nm+3*(i-1)] =
+			max ((Memr[nm+3*(i-1)] / r) ** 2, 1e4 / MAX_REAL)
+		}
+	    } else {
+		do i = 1, nimages {
+		    r = imgetr (in[i], Memc[gain])
+		    Memr[nm+3*(i-1)+1] = r
+		    Memr[nm+3*(i-1)] =
+			max ((Memr[nm+3*(i-1)] / r) ** 2, 1e4 / MAX_REAL)
+		}
+	    }
+	    i = 1
+	    if (ctor (Memc[snoise], i, r) > 0) {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)+2] = r
+	    } else {
+		do i = 1, nimages {
+		    r = imgetr (in[i], Memc[snoise])
+		    Memr[nm+3*(i-1)+2] = r
+		}
+	    }
+	    if (!keepids) {
+		if (doscale1 || grow > 0)
+		    keepids = true
+		else {
+		    do i = 2, nimages {
+			if (Memr[nm+3*(i-1)] != Memr[nm] ||
+			    Memr[nm+3*(i-1)+1] != Memr[nm+1] ||
+			    Memr[nm+3*(i-1)+2] != Memr[nm+2]) {
+			    keepids = true
+			    break
+			}
+		    }
+		}
+	    }
+	    if (reject == CRREJECT)
+		lsigma = MAX_REAL
+	case MINMAX:
+	    mclip = false
+	    if (grow > 0)
+		keepids = true
+	case PCLIP:
+	    mclip = true
+	    if (grow > 0)
+		keepids = true
+	case AVSIGCLIP, SIGCLIP:
+	    if (doscale1 || grow > 0)
+		keepids = true
+	case NONE:
+	    mclip = false
+	    grow = 0
+	}
+
+	if (keepids) {
+	    do i = 1, nimages
+		call salloc (id[i], npts, TY_INT)
+	}
+
+	while (impnlr (out[1], outdata, Meml[v1]) != EOF) {
+	    call ic_gdatas (in, out, dbuf, d, id, n, m, lflag, offsets,
+		scales, zeros, nimages, npts, Meml[v2], Meml[v3])
+
+	    switch (reject) {
+	    case CCDCLIP, CRREJECT:
+		if (mclip)
+		    call ic_mccdclips (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Memr[outdata])
+		else
+		    call ic_accdclips (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Memr[outdata])
+	    case MINMAX:
+		call ic_mms (d, id, n, npts)
+	    case PCLIP:
+		call ic_pclips (d, id, n, nimages, npts, Memr[outdata])
+	    case SIGCLIP:
+		if (mclip)
+		    call ic_msigclips (d, id, n, scales, zeros, nimages, npts,
+			Memr[outdata])
+		else
+		    call ic_asigclips (d, id, n, scales, zeros, nimages, npts,
+			Memr[outdata])
+	    case AVSIGCLIP:
+		if (mclip)
+		    call ic_mavsigclips (d, id, n, scales, zeros, nimages,
+			npts, Memr[outdata])
+		else
+		    call ic_aavsigclips (d, id, n, scales, zeros, nimages,
+			npts, Memr[outdata])
+	    }
+
+	    if (grow > 0)
+		call ic_grows (d, id, n, nimages, npts, Memr[outdata])
+
+	    if (docombine) {
+		switch (combine) {
+		case AVERAGE:
+		    call ic_averages (d, id, n, wts, npts, Memr[outdata])
+		case MEDIAN:
+		    call ic_medians (d, n, npts, Memr[outdata])
+		}
+	    }
+
+	    if (out[2] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnli (out[2], buf, Meml[v1])
+		call amovki (nimages, Memi[buf], npts)
+		call asubi (Memi[buf], n, Memi[buf], npts)
+	    }
+		    
+	    if (out[3] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnlr (out[3], buf, Meml[v1])
+		call ic_sigmas (d, id, n, wts, npts, Memr[outdata],
+		    Memr[buf])
+	    }
+	    call amovl (Meml[v1], Meml[v2], IM_MAXDIM)
+	}
+
+	call sfree (sp)
+end
+
+procedure icombiner (in, out, offsets, nimages, bufsize)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+int	offsets[nimages,ARB]	# Input image offsets
+int	nimages			# Number of input images
+int	bufsize			# IMIO buffer size
+
+char	str[1]
+int	i, j, npts, fd, stropen(), errcode(), imstati()
+pointer	sp, d, id, n, m, lflag, scales, zeros, wts, dbuf
+pointer	buf, imgl1r(), impl1i()
+errchk	stropen, imgl1r, impl1i
+pointer	impl1r()
+errchk	impl1r
+
+include	"../icombine.com"
+
+begin
+	npts = IM_LEN(out[1],1)
+
+	# Allocate memory.
+	call smark (sp)
+	call salloc (d, nimages, TY_POINTER)
+	call salloc (id, nimages, TY_POINTER)
+	call salloc (n, npts, TY_INT)
+	call salloc (m, nimages, TY_POINTER)
+	call salloc (lflag, nimages, TY_INT)
+	call salloc (scales, nimages, TY_REAL)
+	call salloc (zeros, nimages, TY_REAL)
+	call salloc (wts, nimages, TY_REAL)
+	call amovki (D_ALL, Memi[lflag], nimages)
+
+	# If aligned use the IMIO buffer otherwise we need vectors of
+	# output length.
+
+	if (!aligned) {
+	    call salloc (dbuf, nimages, TY_POINTER)
+	    do i = 1, nimages
+		call salloc (Memi[dbuf+i-1], npts, TY_REAL)
+	}
+
+	if (project) {
+	    call imseti (in[1], IM_NBUFS, nimages)
+	    call imseti (in[1], IM_BUFSIZE, bufsize)
+	    do i = 1, 3 {
+		if (out[i] != NULL)
+		    call imseti (out[i], IM_BUFSIZE, bufsize)
+	    }
+	} else {
+	    # Reserve FD for string operations.
+	    fd = stropen (str, 1, NEW_FILE)
+
+	    # Do I/O to the images.
+	    do i = 1, 3 {
+		if (out[i] != NULL)
+		    call imseti (out[i], IM_BUFSIZE, bufsize)
+	    }
+	    buf = impl1r (out[1])
+	    call aclrr (Memr[buf], npts)
+	    if (out[3] != NULL) {
+		buf = impl1r (out[3])
+		call aclrr (Memr[buf], npts)
+	    }
+	    if (out[2] != NULL) {
+		buf = impl1i (out[2])
+		call aclri (Memi[buf], npts)
+	    }
+
+	    do i = 1, nimages {
+		call imseti (in[i], IM_BUFSIZE, bufsize)
+		iferr (buf = imgl1r (in[i])) {
+		    switch (errcode()) {
+		    case SYS_MFULL:
+			call sfree (sp)
+			call strclose (fd)
+			call erract (EA_ERROR)
+		    case SYS_FTOOMANYFILES, SYS_IKIOPIX:
+			if (imstati (in[i], IM_CLOSEFD) == YES) {
+			    call sfree (sp)
+			    call strclose (fd)
+			    call erract (EA_ERROR)
+			}
+			do j = i-2, nimages
+			    call imseti (in[j], IM_CLOSEFD, YES)
+			buf = imgl1r (in[i])
+		    default:
+			call sfree (sp)
+			call strclose (fd)
+			call erract (EA_ERROR)
+		    }
+		}
+	    }
+
+	    call strclose (fd)
+	}
+
+	call ic_combiner (in, out, Memi[dbuf], Memi[d], Memi[id], Memi[n],
+	    Memi[m], Memi[lflag], offsets, Memr[scales], Memr[zeros],
+	    Memr[wts], nimages, npts)
+end
+
+
+# IC_COMBINE -- Combine images.
+
+procedure ic_combiner (in, out, dbuf, d, id, n, m, lflag, offsets,
+	scales, zeros, wts, nimages, npts)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output image
+pointer	dbuf[nimages]		# Data buffers for nonaligned images
+pointer	d[nimages]		# Data pointers
+pointer	id[nimages]		# Image index ID pointers
+int	n[npts]			# Number of good pixels
+pointer	m[nimages]		# Mask pointers
+int	lflag[nimages]		# Line flags
+int	offsets[nimages,ARB]	# Input image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero offset factors
+real	wts[nimages]		# Combining weights
+int	nimages			# Number of input images
+int	npts			# Number of points per output line
+
+int	i, ctor()
+real	r, imgetr()
+pointer	sp, v1, v2, v3, outdata, buf, nm, impnli()
+pointer	impnlr()
+errchk	ic_scale, imgetr
+
+include	"../icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (v1, IM_MAXDIM, TY_LONG)
+	call salloc (v2, IM_MAXDIM, TY_LONG)
+	call salloc (v3, IM_MAXDIM, TY_LONG)
+	call amovkl (long(1), Meml[v1], IM_MAXDIM)
+	call amovkl (long(1), Meml[v2], IM_MAXDIM)
+	call amovkl (long(1), Meml[v3], IM_MAXDIM)
+
+	call ic_scale (in, out, offsets, scales, zeros, wts, nimages)
+
+	# Set combine parameters
+	switch (combine) {
+	case AVERAGE:
+	    if (dowts)
+		keepids = true
+	    else
+		keepids = false
+	case MEDIAN:
+	    dowts = false
+	    keepids = false
+	}
+	docombine = true
+
+	# Set rejection algorithm specific parameters
+	switch (reject) {
+	case CCDCLIP, CRREJECT:
+	    call salloc (nm, 3*nimages, TY_REAL)
+	    i = 1
+	    if (ctor (Memc[rdnoise], i, r) > 0) {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)] = r
+	    } else {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)] = imgetr (in[i], Memc[rdnoise])
+	    }
+	    i = 1
+	    if (ctor (Memc[gain], i, r) > 0) {
+		do i = 1, nimages {
+		    Memr[nm+3*(i-1)+1] = r
+		    Memr[nm+3*(i-1)] =
+			max ((Memr[nm+3*(i-1)] / r) ** 2, 1e4 / MAX_REAL)
+		}
+	    } else {
+		do i = 1, nimages {
+		    r = imgetr (in[i], Memc[gain])
+		    Memr[nm+3*(i-1)+1] = r
+		    Memr[nm+3*(i-1)] =
+			max ((Memr[nm+3*(i-1)] / r) ** 2, 1e4 / MAX_REAL)
+		}
+	    }
+	    i = 1
+	    if (ctor (Memc[snoise], i, r) > 0) {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)+2] = r
+	    } else {
+		do i = 1, nimages {
+		    r = imgetr (in[i], Memc[snoise])
+		    Memr[nm+3*(i-1)+2] = r
+		}
+	    }
+	    if (!keepids) {
+		if (doscale1 || grow > 0)
+		    keepids = true
+		else {
+		    do i = 2, nimages {
+			if (Memr[nm+3*(i-1)] != Memr[nm] ||
+			    Memr[nm+3*(i-1)+1] != Memr[nm+1] ||
+			    Memr[nm+3*(i-1)+2] != Memr[nm+2]) {
+			    keepids = true
+			    break
+			}
+		    }
+		}
+	    }
+	    if (reject == CRREJECT)
+		lsigma = MAX_REAL
+	case MINMAX:
+	    mclip = false
+	    if (grow > 0)
+		keepids = true
+	case PCLIP:
+	    mclip = true
+	    if (grow > 0)
+		keepids = true
+	case AVSIGCLIP, SIGCLIP:
+	    if (doscale1 || grow > 0)
+		keepids = true
+	case NONE:
+	    mclip = false
+	    grow = 0
+	}
+
+	if (keepids) {
+	    do i = 1, nimages
+		call salloc (id[i], npts, TY_INT)
+	}
+
+	while (impnlr (out[1], outdata, Meml[v1]) != EOF) {
+	    call ic_gdatar (in, out, dbuf, d, id, n, m, lflag, offsets,
+		scales, zeros, nimages, npts, Meml[v2], Meml[v3])
+
+	    switch (reject) {
+	    case CCDCLIP, CRREJECT:
+		if (mclip)
+		    call ic_mccdclipr (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Memr[outdata])
+		else
+		    call ic_accdclipr (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Memr[outdata])
+	    case MINMAX:
+		call ic_mmr (d, id, n, npts)
+	    case PCLIP:
+		call ic_pclipr (d, id, n, nimages, npts, Memr[outdata])
+	    case SIGCLIP:
+		if (mclip)
+		    call ic_msigclipr (d, id, n, scales, zeros, nimages, npts,
+			Memr[outdata])
+		else
+		    call ic_asigclipr (d, id, n, scales, zeros, nimages, npts,
+			Memr[outdata])
+	    case AVSIGCLIP:
+		if (mclip)
+		    call ic_mavsigclipr (d, id, n, scales, zeros, nimages,
+			npts, Memr[outdata])
+		else
+		    call ic_aavsigclipr (d, id, n, scales, zeros, nimages,
+			npts, Memr[outdata])
+	    }
+
+	    if (grow > 0)
+		call ic_growr (d, id, n, nimages, npts, Memr[outdata])
+
+	    if (docombine) {
+		switch (combine) {
+		case AVERAGE:
+		    call ic_averager (d, id, n, wts, npts, Memr[outdata])
+		case MEDIAN:
+		    call ic_medianr (d, n, npts, Memr[outdata])
+		}
+	    }
+
+	    if (out[2] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnli (out[2], buf, Meml[v1])
+		call amovki (nimages, Memi[buf], npts)
+		call asubi (Memi[buf], n, Memi[buf], npts)
+	    }
+		    
+	    if (out[3] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnlr (out[3], buf, Meml[v1])
+		call ic_sigmar (d, id, n, wts, npts, Memr[outdata],
+		    Memr[buf])
+	    }
+	    call amovl (Meml[v1], Meml[v2], IM_MAXDIM)
+	}
+
+	call sfree (sp)
+end
+
diff --git a/noao/imred/ccdred/src/generic/icpclip.x b/noao/imred/ccdred/src/generic/icpclip.x
new file mode 100644
index 00000000..da09bb75
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/icpclip.x
@@ -0,0 +1,442 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		3	# Minimum number for clipping
+
+
+# IC_PCLIP -- Percentile clip
+#
+# 1) Find the median
+# 2) Find the pixel which is the specified order index away
+# 3) Use the data value difference as a sigma and apply clipping
+# 4) Since the median is known return it so it does not have to be recomputed
+
+procedure ic_pclips (d, m, n, nimages, npts, median)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image id pointers
+int	n[npts]			# Number of good pixels
+int	nimages			# Number of input images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, n4, n5, nl, nh, nin, maxkeep
+bool	even, fp_equalr()
+real	sigma, r, s, t
+pointer	sp, resid, mp1, mp2
+real	med
+
+include	"../icombine.com"
+
+begin
+	# There must be at least MINCLIP and more than nkeep pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Set sign of pclip parameter
+	if (pclip < 0)
+	    t = -1.
+	else
+	    t = 1.
+
+	# If there are no rejected pixels compute certain parameters once.
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    n2 = 1 + n1 / 2
+	    even = (mod (n1, 2) == 0)
+	    if (pclip < 0.) {
+		if (even)
+		    n3 = max (1, nint (n2 - 1 + pclip))
+		else
+		    n3 = max (1, nint (n2 + pclip))
+	    } else
+		n3 = min (n1, nint (n2 + pclip))
+	    nin = n1
+	}
+
+	# Now apply clipping.
+	do i = 1, npts {
+	    # Compute median.
+	    if (dflag == D_MIX) {
+		n1 = n[i]
+		if (nkeep < 0)
+		    maxkeep = max (0, n1 + nkeep)
+		else
+		    maxkeep = min (n1, nkeep)
+		if (n1 == 0) {
+		    if (combine == MEDIAN)
+			median[i] = blank
+		    next
+		}
+		n2 = 1 + n1 / 2
+		even = (mod (n1, 2) == 0)
+		if (pclip < 0) {
+		    if (even)
+			n3 = max (1, nint (n2 - 1 + pclip))
+		    else
+			n3 = max (1, nint (n2 + pclip))
+		} else
+		    n3 = min (n1, nint (n2 + pclip))
+	    }
+
+	    j = i - 1 
+	    if (even) {
+		med = Mems[d[n2-1]+j]
+		med = (med + Mems[d[n2]+j]) / 2.
+	    } else
+		med = Mems[d[n2]+j]
+
+	    if (n1 < max (MINCLIP, maxkeep+1)) {
+		if (combine == MEDIAN)
+		    median[i] = med
+		next
+	    }
+
+	    # Define sigma for clipping
+	    sigma = t * (Mems[d[n3]+j] - med)
+	    if (fp_equalr (sigma, 0.)) {
+		if (combine == MEDIAN)
+		    median[i] = med
+		next
+	    }
+
+	    # Reject pixels and save residuals.
+	    # Check if any pixels are clipped.
+	    # If so recompute the median and reset the number of good pixels.
+	    # Only reorder if needed.
+
+	    for (nl=1; nl<=n1; nl=nl+1) {
+		r = (med - Mems[d[nl]+j]) / sigma
+		if (r < lsigma)
+		    break
+		Memr[resid+nl] = r
+	    }
+	    for (nh=n1; nh>=1; nh=nh-1) {
+		r = (Mems[d[nh]+j] -  med) / sigma
+		if (r < hsigma)
+		    break
+		Memr[resid+nh] = r
+	    }
+	    n4 = nh - nl + 1
+
+	    # If too many pixels are rejected add some back in.
+	    # All pixels with the same residual are added.
+	    while (n4 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n4 = nh - nl + 1
+	    }
+
+	    # If any pixels are rejected recompute the median.
+	    if (nl > 1 || nh < n1) {
+		n5 = nl + n4 / 2
+		if (mod (n4, 2) == 0) {
+		    med = Mems[d[n5-1]+j]
+		    med = (med + Mems[d[n5]+j]) / 2.
+		} else
+		    med = Mems[d[n5]+j]
+		n[i] = n4
+	    }
+	    if (combine == MEDIAN)
+		median[i] = med
+
+	    # Reorder if pixels only if necessary.
+	    if (nl > 1 && (combine != MEDIAN || grow > 0)) {
+		k = max (nl, n4 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mems[d[l]+j] = Mems[d[k]+j]
+			if (grow > 0) {
+			    mp1 = m[l] + j
+			    mp2 = m[k] + j
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+j] = Memi[m[k]+j]
+			k = k + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mems[d[l]+j] = Mems[d[k]+j]
+			k = k + 1
+		    }
+		}
+	    }
+	}
+
+	# Check if data flag needs to be reset for rejected pixels.
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag whether the median has been computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+
+# IC_PCLIP -- Percentile clip
+#
+# 1) Find the median
+# 2) Find the pixel which is the specified order index away
+# 3) Use the data value difference as a sigma and apply clipping
+# 4) Since the median is known return it so it does not have to be recomputed
+
+procedure ic_pclipr (d, m, n, nimages, npts, median)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image id pointers
+int	n[npts]			# Number of good pixels
+int	nimages			# Number of input images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, n4, n5, nl, nh, nin, maxkeep
+bool	even, fp_equalr()
+real	sigma, r, s, t
+pointer	sp, resid, mp1, mp2
+real	med
+
+include	"../icombine.com"
+
+begin
+	# There must be at least MINCLIP and more than nkeep pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Set sign of pclip parameter
+	if (pclip < 0)
+	    t = -1.
+	else
+	    t = 1.
+
+	# If there are no rejected pixels compute certain parameters once.
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    n2 = 1 + n1 / 2
+	    even = (mod (n1, 2) == 0)
+	    if (pclip < 0.) {
+		if (even)
+		    n3 = max (1, nint (n2 - 1 + pclip))
+		else
+		    n3 = max (1, nint (n2 + pclip))
+	    } else
+		n3 = min (n1, nint (n2 + pclip))
+	    nin = n1
+	}
+
+	# Now apply clipping.
+	do i = 1, npts {
+	    # Compute median.
+	    if (dflag == D_MIX) {
+		n1 = n[i]
+		if (nkeep < 0)
+		    maxkeep = max (0, n1 + nkeep)
+		else
+		    maxkeep = min (n1, nkeep)
+		if (n1 == 0) {
+		    if (combine == MEDIAN)
+			median[i] = blank
+		    next
+		}
+		n2 = 1 + n1 / 2
+		even = (mod (n1, 2) == 0)
+		if (pclip < 0) {
+		    if (even)
+			n3 = max (1, nint (n2 - 1 + pclip))
+		    else
+			n3 = max (1, nint (n2 + pclip))
+		} else
+		    n3 = min (n1, nint (n2 + pclip))
+	    }
+
+	    j = i - 1 
+	    if (even) {
+		med = Memr[d[n2-1]+j]
+		med = (med + Memr[d[n2]+j]) / 2.
+	    } else
+		med = Memr[d[n2]+j]
+
+	    if (n1 < max (MINCLIP, maxkeep+1)) {
+		if (combine == MEDIAN)
+		    median[i] = med
+		next
+	    }
+
+	    # Define sigma for clipping
+	    sigma = t * (Memr[d[n3]+j] - med)
+	    if (fp_equalr (sigma, 0.)) {
+		if (combine == MEDIAN)
+		    median[i] = med
+		next
+	    }
+
+	    # Reject pixels and save residuals.
+	    # Check if any pixels are clipped.
+	    # If so recompute the median and reset the number of good pixels.
+	    # Only reorder if needed.
+
+	    for (nl=1; nl<=n1; nl=nl+1) {
+		r = (med - Memr[d[nl]+j]) / sigma
+		if (r < lsigma)
+		    break
+		Memr[resid+nl] = r
+	    }
+	    for (nh=n1; nh>=1; nh=nh-1) {
+		r = (Memr[d[nh]+j] -  med) / sigma
+		if (r < hsigma)
+		    break
+		Memr[resid+nh] = r
+	    }
+	    n4 = nh - nl + 1
+
+	    # If too many pixels are rejected add some back in.
+	    # All pixels with the same residual are added.
+	    while (n4 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n4 = nh - nl + 1
+	    }
+
+	    # If any pixels are rejected recompute the median.
+	    if (nl > 1 || nh < n1) {
+		n5 = nl + n4 / 2
+		if (mod (n4, 2) == 0) {
+		    med = Memr[d[n5-1]+j]
+		    med = (med + Memr[d[n5]+j]) / 2.
+		} else
+		    med = Memr[d[n5]+j]
+		n[i] = n4
+	    }
+	    if (combine == MEDIAN)
+		median[i] = med
+
+	    # Reorder if pixels only if necessary.
+	    if (nl > 1 && (combine != MEDIAN || grow > 0)) {
+		k = max (nl, n4 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Memr[d[l]+j] = Memr[d[k]+j]
+			if (grow > 0) {
+			    mp1 = m[l] + j
+			    mp2 = m[k] + j
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+j] = Memi[m[k]+j]
+			k = k + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Memr[d[l]+j] = Memr[d[k]+j]
+			k = k + 1
+		    }
+		}
+	    }
+	}
+
+	# Check if data flag needs to be reset for rejected pixels.
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag whether the median has been computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/generic/icsclip.x b/noao/imred/ccdred/src/generic/icsclip.x
new file mode 100644
index 00000000..d7ccfd84
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/icsclip.x
@@ -0,0 +1,964 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		3	# Mininum number of images for algorithm
+
+
+# IC_ASIGCLIP -- Reject pixels using sigma clipping about the average
+# The initial average rejects the high and low pixels.  A correction for
+# different scalings of the images may be made.  Weights are not used.
+
+procedure ic_asigclips (d, m, n, scales, zeros, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+real	d1, low, high, sum, a, s, r, one
+data	one /1.0/
+pointer	sp, resid, w, wp, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	} 
+	
+	# Flag whether returned average needs to be recomputed.
+	if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	# Save the residuals and the sigma scaling corrections if needed.
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+	if (doscale1)
+	    call salloc (w, nimages, TY_REAL)
+
+	# Do sigma clipping.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+
+	    # If there are not enough pixels simply compute the average.
+	    if (n1 < max (3, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Mems[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Mems[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    # Compute average with the high and low rejected.
+	    low = Mems[d[1]+k]
+	    high = Mems[d[2]+k]
+	    if (low > high) {
+		d1 = low
+		low = high
+		high = d1
+	    }
+	    sum = 0.
+	    do j = 3, n1 {
+	       d1 = Mems[d[j]+k]
+	       if (d1 < low) {
+		   sum = sum + low
+		   low = d1
+		} else if (d1 > high) {
+		    sum = sum + high
+		    high = d1
+		} else
+		    sum = sum + d1
+	    }
+	    a = sum / (n1 - 2)
+	    sum = sum + low + high
+
+	    # Iteratively reject pixels and compute the final average if needed.
+	    # Compact the data and keep track of the image IDs if needed.
+
+	    repeat {
+		n2 = n1
+		if (doscale1) {
+		    # Compute sigma corrected for scaling.
+		    s = 0.
+		    wp = w - 1
+		    do j = 1, n1 {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			wp = wp + 1
+
+			d1 = Mems[dp1]
+			l = Memi[mp1]
+			r = sqrt (max (one, (a + zeros[l]) / scales[l]))
+			s = s + ((d1 - a) / r) ** 2
+			Memr[wp] = r
+		    }
+		    s = sqrt (s / (n1 - 1))
+
+		    # Reject pixels.  Save the residuals and data values.
+		    wp = w - 1
+		    if (s > 0.) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    mp1 = m[j] + k
+			    wp = wp + 1
+
+			    d1 = Mems[dp1]
+			    r = (d1 - a) / (s * Memr[wp])
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs (r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    Memr[wp] = Memr[w+n1-1]
+				    mp2 = m[n1] + k
+				    l = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		} else {
+		    # Compute the sigma without scale correction.
+		    s = 0.
+		    do j = 1, n1
+			s = s + (Mems[d[j]+k] - a) ** 2
+		    s = sqrt (s / (n1 - 1))
+
+		    # Reject pixels.  Save the residuals and data values.
+		    if (s > 0.) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    d1 = Mems[dp1]
+			    r = (d1 - a) / s
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs (r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[n1] + k
+					l = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = l
+				    }
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+
+		# Recompute the average.
+		if (n1 > 1)
+		    a = sum / n1
+	    } until (n1 == n2 || n1 <= max (2, maxkeep))
+
+	    # If too many pixels are rejected add some back.
+	    # All pixels with equal residuals are added back.
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mems[dp1]
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Mems[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mems[dp1]
+				    Mems[dp1] = Mems[dp2]
+				    Mems[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Mems[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+
+		# Recompute the average.
+		if (n1 > 1)
+		    a = sum / n1
+	    }
+
+	    # Save the average if needed.
+	    n[i] = n1
+	    if (!docombine) {
+		if (n1 > 0)
+		    average[i] = a
+		else
+		    average[i] = blank
+	    }
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_MSIGCLIP -- Reject pixels using sigma clipping about the median
+
+procedure ic_msigclips (d, m, n, scales, zeros, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+real	r, s
+pointer	sp, resid, w, mp1, mp2
+real	med, one
+data	one /1.0/
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	# Save the residuals and sigma scaling corrections if needed.
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+	if (doscale1)
+	    call salloc (w, nimages, TY_REAL)
+
+	# Compute median and sigma and iteratively clip.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    nl = 1
+	    nh = n1
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 == 0)
+		    med = blank
+		else if (mod (n1, 2) == 0)
+		    med = (Mems[d[n3-1]+k] + Mems[d[n3]+k]) / 2.
+		else
+		    med = Mems[d[n3]+k]
+
+		if (n1 >= max (MINCLIP, maxkeep+1)) {
+		    if (doscale1) {
+			# Compute the sigma with scaling correction.
+			s = 0.
+			do j = nl, nh {
+			    l = Memi[m[j]+k]
+			    r = sqrt (max (one, (med + zeros[l]) / scales[l]))
+			    s = s + ((Mems[d[j]+k] - med) / r) ** 2
+			    Memr[w+j-1] = r
+			}
+			s = sqrt (s / (n1 - 1))
+
+			# Reject pixels and save the residuals.
+			if (s > 0.) {
+			    for (; nl <= n2; nl = nl + 1) {
+				r = (med - Mems[d[nl]+k]) / (s * Memr[w+nl-1])
+				if (r <= lsigma)
+				    break
+				Memr[resid+nl] = r
+				n1 = n1 - 1
+			    }
+			    for (; nh >= nl; nh = nh - 1) {
+				r = (Mems[d[nh]+k] - med) / (s * Memr[w+nh-1])
+				if (r <= hsigma)
+				    break
+				Memr[resid+nh] = r
+				n1 = n1 - 1
+			    }
+			}
+		    } else {
+			# Compute the sigma without scaling correction.
+			s = 0.
+			do j = nl, nh
+			    s = s + (Mems[d[j]+k] - med) ** 2
+			s = sqrt (s / (n1 - 1))
+
+			# Reject pixels and save the residuals.
+			if (s > 0.) {
+			    for (; nl <= n2; nl = nl + 1) {
+				r = (med - Mems[d[nl]+k]) / s
+				if (r <= lsigma)
+				    break
+				Memr[resid+nl] = r
+				n1 = n1 - 1
+			    }
+			    for (; nh >= nl; nh = nh - 1) {
+				r = (Mems[d[nh]+k] -  med) / s
+				if (r <= hsigma)
+				    break
+				Memr[resid+nh] = r
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    # If too many pixels are rejected add some back.
+	    # All pixels with equal residuals are added back.
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mems[d[l]+k] = Mems[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mems[d[l]+k] = Mems[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median has been computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+
+# IC_ASIGCLIP -- Reject pixels using sigma clipping about the average
+# The initial average rejects the high and low pixels.  A correction for
+# different scalings of the images may be made.  Weights are not used.
+
+procedure ic_asigclipr (d, m, n, scales, zeros, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+real	d1, low, high, sum, a, s, r, one
+data	one /1.0/
+pointer	sp, resid, w, wp, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	} 
+	
+	# Flag whether returned average needs to be recomputed.
+	if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	# Save the residuals and the sigma scaling corrections if needed.
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+	if (doscale1)
+	    call salloc (w, nimages, TY_REAL)
+
+	# Do sigma clipping.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+
+	    # If there are not enough pixels simply compute the average.
+	    if (n1 < max (3, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Memr[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Memr[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    # Compute average with the high and low rejected.
+	    low = Memr[d[1]+k]
+	    high = Memr[d[2]+k]
+	    if (low > high) {
+		d1 = low
+		low = high
+		high = d1
+	    }
+	    sum = 0.
+	    do j = 3, n1 {
+	       d1 = Memr[d[j]+k]
+	       if (d1 < low) {
+		   sum = sum + low
+		   low = d1
+		} else if (d1 > high) {
+		    sum = sum + high
+		    high = d1
+		} else
+		    sum = sum + d1
+	    }
+	    a = sum / (n1 - 2)
+	    sum = sum + low + high
+
+	    # Iteratively reject pixels and compute the final average if needed.
+	    # Compact the data and keep track of the image IDs if needed.
+
+	    repeat {
+		n2 = n1
+		if (doscale1) {
+		    # Compute sigma corrected for scaling.
+		    s = 0.
+		    wp = w - 1
+		    do j = 1, n1 {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			wp = wp + 1
+
+			d1 = Memr[dp1]
+			l = Memi[mp1]
+			r = sqrt (max (one, (a + zeros[l]) / scales[l]))
+			s = s + ((d1 - a) / r) ** 2
+			Memr[wp] = r
+		    }
+		    s = sqrt (s / (n1 - 1))
+
+		    # Reject pixels.  Save the residuals and data values.
+		    wp = w - 1
+		    if (s > 0.) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    mp1 = m[j] + k
+			    wp = wp + 1
+
+			    d1 = Memr[dp1]
+			    r = (d1 - a) / (s * Memr[wp])
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs (r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    Memr[wp] = Memr[w+n1-1]
+				    mp2 = m[n1] + k
+				    l = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		} else {
+		    # Compute the sigma without scale correction.
+		    s = 0.
+		    do j = 1, n1
+			s = s + (Memr[d[j]+k] - a) ** 2
+		    s = sqrt (s / (n1 - 1))
+
+		    # Reject pixels.  Save the residuals and data values.
+		    if (s > 0.) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    d1 = Memr[dp1]
+			    r = (d1 - a) / s
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs (r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[n1] + k
+					l = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = l
+				    }
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+
+		# Recompute the average.
+		if (n1 > 1)
+		    a = sum / n1
+	    } until (n1 == n2 || n1 <= max (2, maxkeep))
+
+	    # If too many pixels are rejected add some back.
+	    # All pixels with equal residuals are added back.
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Memr[dp1]
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Memr[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Memr[dp1]
+				    Memr[dp1] = Memr[dp2]
+				    Memr[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Memr[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+
+		# Recompute the average.
+		if (n1 > 1)
+		    a = sum / n1
+	    }
+
+	    # Save the average if needed.
+	    n[i] = n1
+	    if (!docombine) {
+		if (n1 > 0)
+		    average[i] = a
+		else
+		    average[i] = blank
+	    }
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_MSIGCLIP -- Reject pixels using sigma clipping about the median
+
+procedure ic_msigclipr (d, m, n, scales, zeros, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+real	median[npts]		# Median
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+real	r, s
+pointer	sp, resid, w, mp1, mp2
+real	med, one
+data	one /1.0/
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	# Save the residuals and sigma scaling corrections if needed.
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+	if (doscale1)
+	    call salloc (w, nimages, TY_REAL)
+
+	# Compute median and sigma and iteratively clip.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    nl = 1
+	    nh = n1
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 == 0)
+		    med = blank
+		else if (mod (n1, 2) == 0)
+		    med = (Memr[d[n3-1]+k] + Memr[d[n3]+k]) / 2.
+		else
+		    med = Memr[d[n3]+k]
+
+		if (n1 >= max (MINCLIP, maxkeep+1)) {
+		    if (doscale1) {
+			# Compute the sigma with scaling correction.
+			s = 0.
+			do j = nl, nh {
+			    l = Memi[m[j]+k]
+			    r = sqrt (max (one, (med + zeros[l]) / scales[l]))
+			    s = s + ((Memr[d[j]+k] - med) / r) ** 2
+			    Memr[w+j-1] = r
+			}
+			s = sqrt (s / (n1 - 1))
+
+			# Reject pixels and save the residuals.
+			if (s > 0.) {
+			    for (; nl <= n2; nl = nl + 1) {
+				r = (med - Memr[d[nl]+k]) / (s * Memr[w+nl-1])
+				if (r <= lsigma)
+				    break
+				Memr[resid+nl] = r
+				n1 = n1 - 1
+			    }
+			    for (; nh >= nl; nh = nh - 1) {
+				r = (Memr[d[nh]+k] - med) / (s * Memr[w+nh-1])
+				if (r <= hsigma)
+				    break
+				Memr[resid+nh] = r
+				n1 = n1 - 1
+			    }
+			}
+		    } else {
+			# Compute the sigma without scaling correction.
+			s = 0.
+			do j = nl, nh
+			    s = s + (Memr[d[j]+k] - med) ** 2
+			s = sqrt (s / (n1 - 1))
+
+			# Reject pixels and save the residuals.
+			if (s > 0.) {
+			    for (; nl <= n2; nl = nl + 1) {
+				r = (med - Memr[d[nl]+k]) / s
+				if (r <= lsigma)
+				    break
+				Memr[resid+nl] = r
+				n1 = n1 - 1
+			    }
+			    for (; nh >= nl; nh = nh - 1) {
+				r = (Memr[d[nh]+k] -  med) / s
+				if (r <= hsigma)
+				    break
+				Memr[resid+nh] = r
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    # If too many pixels are rejected add some back.
+	    # All pixels with equal residuals are added back.
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Memr[d[l]+k] = Memr[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Memr[d[l]+k] = Memr[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median has been computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/generic/icsigma.x b/noao/imred/ccdred/src/generic/icsigma.x
new file mode 100644
index 00000000..bc0d9788
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/icsigma.x
@@ -0,0 +1,205 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"../icombine.h"
+
+
+# IC_SIGMA -- Compute the sigma image line.
+# The estimated sigma includes a correction for the finite population.
+# Weights are used if desired.
+
+procedure ic_sigmas (d, m, n, wts, npts, average, sigma)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image ID pointers
+int	n[npts]			# Number of points
+real	wts[ARB]		# Weights
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+real	sigma[npts]		# Sigma line (returned)
+
+int	i, j, k, n1
+real	wt, sigcor, sumwt
+real	a, sum
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    if (dowts) {
+		if (n1 > 1)
+		    sigcor = real (n1) / real (n1 - 1)
+		else
+		    sigcor = 1.
+		do i = 1, npts {
+		    k = i - 1
+		    a = average[i]
+		    wt = wts[Memi[m[1]+k]]
+		    sum = (Mems[d[1]+k] - a) ** 2 * wt
+		    do j = 2, n1 {
+			wt = wts[Memi[m[j]+k]]
+			sum = sum + (Mems[d[j]+k] - a) ** 2 * wt
+		    }
+		    sigma[i] = sqrt (sum * sigcor)
+		}
+	    } else {
+		if (n1 > 1)
+		    sigcor = 1. / real (n1 - 1)
+		else
+		    sigcor = 1.
+		do i = 1, npts {
+		    k = i - 1
+		    a = average[i]
+		    sum = (Mems[d[1]+k] - a) ** 2
+		    do j = 2, n1
+			sum = sum + (Mems[d[j]+k] - a) ** 2
+		    sigma[i] = sqrt (sum * sigcor)
+		}
+	    }
+	} else if (dflag == D_NONE) {
+	    do i = 1, npts
+		sigma[i] = blank
+	} else {
+	    if (dowts) {
+		do i = 1, npts {
+		    n1 = n[i]
+		    if (n1 > 0) {
+			k = i - 1
+			if (n1 > 1)
+			    sigcor = real (n1) / real (n1 -1)
+			else
+			    sigcor = 1
+			a = average[i]
+			wt = wts[Memi[m[1]+k]]
+			sum = (Mems[d[1]+k] - a) ** 2 * wt
+			sumwt = wt
+			do j = 2, n1 {
+			    wt = wts[Memi[m[j]+k]]
+			    sum = sum + (Mems[d[j]+k] - a) ** 2 * wt
+			    sumwt = sumwt + wt
+			}
+			sigma[i] = sqrt (sum / sumwt * sigcor)
+		    } else
+			sigma[i] = blank
+		}
+	    } else {
+		do i = 1, npts {
+		    n1 = n[i]
+		    if (n1 > 0) {
+			k = i - 1
+			if (n1 > 1)
+			    sigcor = 1. / real (n1 - 1)
+			else
+			    sigcor = 1.
+			a = average[i]
+			sum = (Mems[d[1]+k] - a) ** 2
+			do j = 2, n1
+			    sum = sum + (Mems[d[j]+k] - a) ** 2
+			sigma[i] = sqrt (sum * sigcor)
+		    } else
+			sigma[i] = blank
+		}
+	    }
+	}
+end
+
+# IC_SIGMA -- Compute the sigma image line.
+# The estimated sigma includes a correction for the finite population.
+# Weights are used if desired.
+
+procedure ic_sigmar (d, m, n, wts, npts, average, sigma)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image ID pointers
+int	n[npts]			# Number of points
+real	wts[ARB]		# Weights
+int	npts			# Number of output points per line
+real	average[npts]		# Average
+real	sigma[npts]		# Sigma line (returned)
+
+int	i, j, k, n1
+real	wt, sigcor, sumwt
+real	a, sum
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    if (dowts) {
+		if (n1 > 1)
+		    sigcor = real (n1) / real (n1 - 1)
+		else
+		    sigcor = 1.
+		do i = 1, npts {
+		    k = i - 1
+		    a = average[i]
+		    wt = wts[Memi[m[1]+k]]
+		    sum = (Memr[d[1]+k] - a) ** 2 * wt
+		    do j = 2, n1 {
+			wt = wts[Memi[m[j]+k]]
+			sum = sum + (Memr[d[j]+k] - a) ** 2 * wt
+		    }
+		    sigma[i] = sqrt (sum * sigcor)
+		}
+	    } else {
+		if (n1 > 1)
+		    sigcor = 1. / real (n1 - 1)
+		else
+		    sigcor = 1.
+		do i = 1, npts {
+		    k = i - 1
+		    a = average[i]
+		    sum = (Memr[d[1]+k] - a) ** 2
+		    do j = 2, n1
+			sum = sum + (Memr[d[j]+k] - a) ** 2
+		    sigma[i] = sqrt (sum * sigcor)
+		}
+	    }
+	} else if (dflag == D_NONE) {
+	    do i = 1, npts
+		sigma[i] = blank
+	} else {
+	    if (dowts) {
+		do i = 1, npts {
+		    n1 = n[i]
+		    if (n1 > 0) {
+			k = i - 1
+			if (n1 > 1)
+			    sigcor = real (n1) / real (n1 -1)
+			else
+			    sigcor = 1
+			a = average[i]
+			wt = wts[Memi[m[1]+k]]
+			sum = (Memr[d[1]+k] - a) ** 2 * wt
+			sumwt = wt
+			do j = 2, n1 {
+			    wt = wts[Memi[m[j]+k]]
+			    sum = sum + (Memr[d[j]+k] - a) ** 2 * wt
+			    sumwt = sumwt + wt
+			}
+			sigma[i] = sqrt (sum / sumwt * sigcor)
+		    } else
+			sigma[i] = blank
+		}
+	    } else {
+		do i = 1, npts {
+		    n1 = n[i]
+		    if (n1 > 0) {
+			k = i - 1
+			if (n1 > 1)
+			    sigcor = 1. / real (n1 - 1)
+			else
+			    sigcor = 1.
+			a = average[i]
+			sum = (Memr[d[1]+k] - a) ** 2
+			do j = 2, n1
+			    sum = sum + (Memr[d[j]+k] - a) ** 2
+			sigma[i] = sqrt (sum * sigcor)
+		    } else
+			sigma[i] = blank
+		}
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/src/generic/icsort.x b/noao/imred/ccdred/src/generic/icsort.x
new file mode 100644
index 00000000..a39b68e2
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/icsort.x
@@ -0,0 +1,550 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+define	LOGPTR	32			# log2(maxpts) (4e9)
+
+
+# IC_SORT -- Quicksort.  This is based on the VOPS asrt except that
+# the input is an array of pointers to image lines and the sort is done
+# across the image lines at each point along the lines.  The number of
+# valid pixels at each point is allowed to vary.  The cases of 1, 2, and 3
+# pixels per point are treated specially.
+
+procedure ic_sorts (a, b, nvecs, npts)
+
+pointer	a[ARB]			# pointer to input vectors
+short	b[ARB]			# work array
+int	nvecs[npts]		# number of vectors
+int	npts			# number of points in vectors
+
+short	pivot, temp, temp3
+int	i, j, k, l, p, npix, lv[LOGPTR], uv[LOGPTR]
+define	swap {temp=$1;$1=$2;$2=temp}
+define	copy_	10
+
+begin
+	do l = 0, npts-1 {
+	    npix = nvecs[l+1]
+	    if (npix <= 1)
+		next
+
+	    do i = 1, npix
+		b[i] = Mems[a[i]+l]
+
+	    # Special cases
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (temp < pivot) {
+			b[1] = temp
+			b[2] = pivot
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (temp < pivot) {				# bac|bca|cba
+			if (temp < temp3) {			# bac|bca
+			    b[1] = temp
+			    if (pivot < temp3)			# bac
+				b[2] = pivot
+			    else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			}
+		    } else if (temp3 < temp) {			# acb|cab
+			b[3] = temp
+			if (pivot < temp3)			# acb
+			    b[2] = temp3
+			else {					# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+
+	    # General case
+	    do i = 1, npix
+		b[i] = Mems[a[i]+l]
+
+	    lv[1] = 1
+	    uv[1] = npix
+	    p = 1
+
+	    while (p > 0) {
+		if (lv[p] >= uv[p])		# only one elem in this subset
+		    p = p - 1			# pop stack
+		else {
+		    # Dummy do loop to trigger the Fortran optimizer.
+		    do p = p, ARB {
+			i = lv[p] - 1
+			j = uv[p]
+
+			# Select as the pivot the element at the center of the
+			# array, to avoid quadratic behavior on an already
+			# sorted array.
+
+			k = (lv[p] + uv[p]) / 2
+			swap (b[j], b[k])
+			pivot = b[j]		   # pivot line
+
+			while (i < j) {
+			    for (i=i+1;  b[i] < pivot;  i=i+1)
+				;
+			    for (j=j-1;  j > i;  j=j-1)
+				if (b[j] <= pivot)
+				    break
+			    if (i < j)		   # out of order pair
+				swap (b[i], b[j])  # interchange elements
+			}
+
+			j = uv[p]		   # move pivot to position i
+			swap (b[i], b[j])	   # interchange elements
+
+			if (i-lv[p] < uv[p] - i) { # stack so shorter done first
+			    lv[p+1] = lv[p]
+			    uv[p+1] = i - 1
+			    lv[p] = i + 1
+			} else {
+			    lv[p+1] = i + 1
+			    uv[p+1] = uv[p]
+			    uv[p] = i - 1
+			}
+
+			break
+		    }
+		    p = p + 1			   # push onto stack
+		}
+	    }
+
+copy_
+	    do i = 1, npix
+		Mems[a[i]+l] = b[i]
+	}
+end
+
+
+# IC_2SORT -- Quicksort.  This is based on the VOPS asrt except that
+# the input is an array of pointers to image lines and the sort is done
+# across the image lines at each point along the lines.  The number of
+# valid pixels at each point is allowed to vary.  The cases of 1, 2, and 3
+# pixels per point are treated specially.  A second integer set of
+# vectors is sorted.
+
+procedure ic_2sorts (a, b, c, d, nvecs, npts)
+
+pointer	a[ARB]			# pointer to input vectors
+short	b[ARB]			# work array
+pointer	c[ARB]			# pointer to associated integer vectors
+int	d[ARB]			# work array
+int	nvecs[npts]		# number of vectors
+int	npts			# number of points in vectors
+
+short	pivot, temp, temp3
+int	i, j, k, l, p, npix, lv[LOGPTR], uv[LOGPTR], itemp
+define	swap {temp=$1;$1=$2;$2=temp}
+define	iswap {itemp=$1;$1=$2;$2=itemp}
+define	copy_	10
+
+begin
+	do l = 0, npts-1 {
+	    npix = nvecs[l+1]
+	    if (npix <= 1)
+		next
+
+	    do i = 1, npix {
+		b[i] = Mems[a[i]+l]
+		d[i] = Memi[c[i]+l]
+	    }
+
+	    # Special cases
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (temp < pivot) {
+			b[1] = temp
+			b[2] = pivot
+			iswap (d[1], d[2])
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (temp < pivot) {				# bac|bca|cba
+			if (temp < temp3) {			# bac|bca
+			    b[1] = temp
+			    if (pivot < temp3) {		# bac
+				b[2] = pivot
+				iswap (d[1], d[2])
+			    } else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+				itemp = d[2]
+				d[2] = d[3]
+				d[3] = d[1]
+				d[1] = itemp
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			    iswap (d[1], d[3])
+			}
+		    } else if (temp3 < temp) {			# acb|cab
+			b[3] = temp
+			if (pivot < temp3) {			# acb
+			    b[2] = temp3
+			    iswap (d[2], d[3])
+			} else {				# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			    itemp = d[2]
+			    d[2] = d[1]
+			    d[1] = d[3]
+			    d[3] = itemp
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+
+	    # General case
+	    lv[1] = 1
+	    uv[1] = npix
+	    p = 1
+
+	    while (p > 0) {
+		if (lv[p] >= uv[p])		# only one elem in this subset
+		    p = p - 1			# pop stack
+		else {
+		    # Dummy do loop to trigger the Fortran optimizer.
+		    do p = p, ARB {
+			i = lv[p] - 1
+			j = uv[p]
+
+			# Select as the pivot the element at the center of the
+			# array, to avoid quadratic behavior on an already
+			# sorted array.
+
+			k = (lv[p] + uv[p]) / 2
+			swap (b[j], b[k]); swap (d[j], d[k])
+			pivot = b[j]		   # pivot line
+
+			while (i < j) {
+			    for (i=i+1;  b[i] < pivot;  i=i+1)
+				;
+			    for (j=j-1;  j > i;  j=j-1)
+				if (b[j] <= pivot)
+				    break
+			    if (i < j) {	   # out of order pair
+				swap (b[i], b[j])  # interchange elements
+				swap (d[i], d[j])
+			    }
+			}
+
+			j = uv[p]		   # move pivot to position i
+			swap (b[i], b[j])	   # interchange elements
+			swap (d[i], d[j])
+
+			if (i-lv[p] < uv[p] - i) { # stack so shorter done first
+			    lv[p+1] = lv[p]
+			    uv[p+1] = i - 1
+			    lv[p] = i + 1
+			} else {
+			    lv[p+1] = i + 1
+			    uv[p+1] = uv[p]
+			    uv[p] = i - 1
+			}
+
+			break
+		    }
+		    p = p + 1			   # push onto stack
+		}
+	    }
+
+copy_	   
+	    do i = 1, npix {
+		Mems[a[i]+l] = b[i]
+		Memi[c[i]+l] = d[i]
+	    }
+	}
+end
+
+# IC_SORT -- Quicksort.  This is based on the VOPS asrt except that
+# the input is an array of pointers to image lines and the sort is done
+# across the image lines at each point along the lines.  The number of
+# valid pixels at each point is allowed to vary.  The cases of 1, 2, and 3
+# pixels per point are treated specially.
+
+procedure ic_sortr (a, b, nvecs, npts)
+
+pointer	a[ARB]			# pointer to input vectors
+real	b[ARB]			# work array
+int	nvecs[npts]		# number of vectors
+int	npts			# number of points in vectors
+
+real	pivot, temp, temp3
+int	i, j, k, l, p, npix, lv[LOGPTR], uv[LOGPTR]
+define	swap {temp=$1;$1=$2;$2=temp}
+define	copy_	10
+
+begin
+	do l = 0, npts-1 {
+	    npix = nvecs[l+1]
+	    if (npix <= 1)
+		next
+
+	    do i = 1, npix
+		b[i] = Memr[a[i]+l]
+
+	    # Special cases
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (temp < pivot) {
+			b[1] = temp
+			b[2] = pivot
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (temp < pivot) {				# bac|bca|cba
+			if (temp < temp3) {			# bac|bca
+			    b[1] = temp
+			    if (pivot < temp3)			# bac
+				b[2] = pivot
+			    else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			}
+		    } else if (temp3 < temp) {			# acb|cab
+			b[3] = temp
+			if (pivot < temp3)			# acb
+			    b[2] = temp3
+			else {					# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+
+	    # General case
+	    do i = 1, npix
+		b[i] = Memr[a[i]+l]
+
+	    lv[1] = 1
+	    uv[1] = npix
+	    p = 1
+
+	    while (p > 0) {
+		if (lv[p] >= uv[p])		# only one elem in this subset
+		    p = p - 1			# pop stack
+		else {
+		    # Dummy do loop to trigger the Fortran optimizer.
+		    do p = p, ARB {
+			i = lv[p] - 1
+			j = uv[p]
+
+			# Select as the pivot the element at the center of the
+			# array, to avoid quadratic behavior on an already
+			# sorted array.
+
+			k = (lv[p] + uv[p]) / 2
+			swap (b[j], b[k])
+			pivot = b[j]		   # pivot line
+
+			while (i < j) {
+			    for (i=i+1;  b[i] < pivot;  i=i+1)
+				;
+			    for (j=j-1;  j > i;  j=j-1)
+				if (b[j] <= pivot)
+				    break
+			    if (i < j)		   # out of order pair
+				swap (b[i], b[j])  # interchange elements
+			}
+
+			j = uv[p]		   # move pivot to position i
+			swap (b[i], b[j])	   # interchange elements
+
+			if (i-lv[p] < uv[p] - i) { # stack so shorter done first
+			    lv[p+1] = lv[p]
+			    uv[p+1] = i - 1
+			    lv[p] = i + 1
+			} else {
+			    lv[p+1] = i + 1
+			    uv[p+1] = uv[p]
+			    uv[p] = i - 1
+			}
+
+			break
+		    }
+		    p = p + 1			   # push onto stack
+		}
+	    }
+
+copy_
+	    do i = 1, npix
+		Memr[a[i]+l] = b[i]
+	}
+end
+
+
+# IC_2SORT -- Quicksort.  This is based on the VOPS asrt except that
+# the input is an array of pointers to image lines and the sort is done
+# across the image lines at each point along the lines.  The number of
+# valid pixels at each point is allowed to vary.  The cases of 1, 2, and 3
+# pixels per point are treated specially.  A second integer set of
+# vectors is sorted.
+
+procedure ic_2sortr (a, b, c, d, nvecs, npts)
+
+pointer	a[ARB]			# pointer to input vectors
+real	b[ARB]			# work array
+pointer	c[ARB]			# pointer to associated integer vectors
+int	d[ARB]			# work array
+int	nvecs[npts]		# number of vectors
+int	npts			# number of points in vectors
+
+real	pivot, temp, temp3
+int	i, j, k, l, p, npix, lv[LOGPTR], uv[LOGPTR], itemp
+define	swap {temp=$1;$1=$2;$2=temp}
+define	iswap {itemp=$1;$1=$2;$2=itemp}
+define	copy_	10
+
+begin
+	do l = 0, npts-1 {
+	    npix = nvecs[l+1]
+	    if (npix <= 1)
+		next
+
+	    do i = 1, npix {
+		b[i] = Memr[a[i]+l]
+		d[i] = Memi[c[i]+l]
+	    }
+
+	    # Special cases
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (temp < pivot) {
+			b[1] = temp
+			b[2] = pivot
+			iswap (d[1], d[2])
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (temp < pivot) {				# bac|bca|cba
+			if (temp < temp3) {			# bac|bca
+			    b[1] = temp
+			    if (pivot < temp3) {		# bac
+				b[2] = pivot
+				iswap (d[1], d[2])
+			    } else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+				itemp = d[2]
+				d[2] = d[3]
+				d[3] = d[1]
+				d[1] = itemp
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			    iswap (d[1], d[3])
+			}
+		    } else if (temp3 < temp) {			# acb|cab
+			b[3] = temp
+			if (pivot < temp3) {			# acb
+			    b[2] = temp3
+			    iswap (d[2], d[3])
+			} else {				# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			    itemp = d[2]
+			    d[2] = d[1]
+			    d[1] = d[3]
+			    d[3] = itemp
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+
+	    # General case
+	    lv[1] = 1
+	    uv[1] = npix
+	    p = 1
+
+	    while (p > 0) {
+		if (lv[p] >= uv[p])		# only one elem in this subset
+		    p = p - 1			# pop stack
+		else {
+		    # Dummy do loop to trigger the Fortran optimizer.
+		    do p = p, ARB {
+			i = lv[p] - 1
+			j = uv[p]
+
+			# Select as the pivot the element at the center of the
+			# array, to avoid quadratic behavior on an already
+			# sorted array.
+
+			k = (lv[p] + uv[p]) / 2
+			swap (b[j], b[k]); swap (d[j], d[k])
+			pivot = b[j]		   # pivot line
+
+			while (i < j) {
+			    for (i=i+1;  b[i] < pivot;  i=i+1)
+				;
+			    for (j=j-1;  j > i;  j=j-1)
+				if (b[j] <= pivot)
+				    break
+			    if (i < j) {	   # out of order pair
+				swap (b[i], b[j])  # interchange elements
+				swap (d[i], d[j])
+			    }
+			}
+
+			j = uv[p]		   # move pivot to position i
+			swap (b[i], b[j])	   # interchange elements
+			swap (d[i], d[j])
+
+			if (i-lv[p] < uv[p] - i) { # stack so shorter done first
+			    lv[p+1] = lv[p]
+			    uv[p+1] = i - 1
+			    lv[p] = i + 1
+			} else {
+			    lv[p+1] = i + 1
+			    uv[p+1] = uv[p]
+			    uv[p] = i - 1
+			}
+
+			break
+		    }
+		    p = p + 1			   # push onto stack
+		}
+	    }
+
+copy_	   
+	    do i = 1, npix {
+		Memr[a[i]+l] = b[i]
+		Memi[c[i]+l] = d[i]
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/src/generic/icstat.x b/noao/imred/ccdred/src/generic/icstat.x
new file mode 100644
index 00000000..41512ccb
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/icstat.x
@@ -0,0 +1,444 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"../icombine.h"
+
+define	NMAX	10000	# Maximum number of pixels to sample
+
+
+# IC_STAT -- Compute image statistics within specified section.
+# The image section is relative to a reference image which may be
+# different than the input image and may have an offset.  Only a
+# subsample of pixels is used.  Masked and thresholded pixels are
+# ignored.  Only the desired statistics are computed to increase
+# efficiency.
+
+procedure ic_stats (im, imref, section, offsets, image, nimages,
+	domode, domedian, domean, mode, median, mean)
+
+pointer	im			 # Data image
+pointer	imref			 # Reference image for image section
+char	section[ARB]		 # Image section
+int	offsets[nimages,ARB]	 # Image section offset from data to reference
+int	image			 # Image index (for mask I/O)
+int	nimages			 # Number of images in  offsets.
+bool	domode, domedian, domean # Statistics to compute
+real	mode, median, mean	 # Statistics
+
+int	i, j, ndim, n, nv
+real	a
+pointer	sp, v1, v2, dv, va, vb
+pointer	data, mask, dp, lp, mp, imgnls()
+short	ic_modes()
+real    asums()
+
+
+include	"../icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (v1, IM_MAXDIM, TY_LONG)
+	call salloc (v2, IM_MAXDIM, TY_LONG)
+	call salloc (dv, IM_MAXDIM, TY_LONG)
+	call salloc (va, IM_MAXDIM, TY_LONG)
+	call salloc (vb, IM_MAXDIM, TY_LONG)
+
+	# Determine the image section parameters.  This must be in terms of
+	# the data image pixel coordinates though the section may be specified
+	# in terms of the reference image coordinates.  Limit the number of
+	# pixels in each dimension to a maximum.
+
+	ndim = IM_NDIM(im)
+	if (project)
+	    ndim = ndim - 1
+	call amovki (1, Memi[v1], IM_MAXDIM)
+	call amovki (1, Memi[va], IM_MAXDIM)
+	call amovki (1, Memi[dv], IM_MAXDIM)
+	call amovi (IM_LEN(imref,1), Memi[vb], ndim)
+	call ic_section (section, Memi[va], Memi[vb], Memi[dv], ndim)
+	if (im != imref)
+	    do i = 1, ndim {
+		Memi[va+i-1] = Memi[va+i-1] - offsets[image,i]
+		Memi[vb+i-1] = Memi[vb+i-1] - offsets[image,i]
+	    }
+
+	do j = 1, 10 {
+	    n = 1
+	    do i = 0, ndim-1 {
+		Memi[v1+i] = max (1, min (Memi[va+i], Memi[vb+i]))
+		Memi[v2+i] = min (IM_LEN(im,i+1), max (Memi[va+i], Memi[vb+i]))
+		Memi[dv+i] = j
+		nv = max (1, (Memi[v2+i] - Memi[v1+i]) / Memi[dv+i] + 1)
+		Memi[v2+i] = Memi[v1+i] + (nv - 1) * Memi[dv+i]
+		n = n * nv
+	    }
+	    if (n < NMAX)
+		break
+	}
+
+	call amovl (Memi[v1], Memi[va], IM_MAXDIM)
+	Memi[va] = 1
+	if (project)
+	   Memi[va+ndim] = image
+	call amovl (Memi[va], Memi[vb], IM_MAXDIM)
+
+	# Accumulate the pixel values within the section.  Masked pixels and
+	# thresholded pixels are ignored.
+
+	call salloc (data, n, TY_SHORT)
+	dp = data
+	while (imgnls (im, lp, Memi[vb]) != EOF) {
+	    call ic_mget1 (im, image, offsets[image,1], Memi[va], mask)
+	    lp = lp + Memi[v1] - 1
+	    if (dflag == D_ALL) {
+		if (dothresh) {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			a = Mems[lp]
+			if (a >= lthresh && a <= hthresh) {
+			    Mems[dp] = a
+			    dp = dp + 1
+			}
+			lp = lp + Memi[dv]
+		    }
+		} else {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			Mems[dp] = Mems[lp]
+			dp = dp + 1
+			lp = lp + Memi[dv]
+		    }
+		}
+	    } else if (dflag == D_MIX) {
+		mp = mask + Memi[v1] - 1
+		if (dothresh) {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			if (Memi[mp] == 0) {
+			    a = Mems[lp]
+			    if (a >= lthresh && a <= hthresh) {
+				Mems[dp] = a
+				dp = dp + 1
+			    }
+			}
+			mp = mp + Memi[dv]
+			lp = lp + Memi[dv]
+		    }
+		} else {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			if (Memi[mp] == 0) {
+			    Mems[dp] = Mems[lp]
+			    dp = dp + 1
+			}
+			mp = mp + Memi[dv]
+			lp = lp + Memi[dv]
+		    }
+		}
+	    }
+	    for (i=2; i<=ndim; i=i+1) {
+		Memi[va+i-1] = Memi[va+i-1] + Memi[dv+i-1]
+		if (Memi[va+i-1] <= Memi[v2+i-1])
+		    break
+		Memi[va+i-1] = Memi[v1+i-1]
+	    }
+	    if (i > ndim)
+		break
+	    call amovl (Memi[va], Memi[vb], IM_MAXDIM)
+	}
+
+	n = dp - data
+	if (n < 1) {
+	    call sfree (sp)
+	    call error (1, "Image section contains no pixels")
+	}
+
+	# Compute only statistics needed.
+	if (domode || domedian) {
+	    call asrts (Mems[data], Mems[data], n)
+	    mode = ic_modes (Mems[data], n)
+	    median = Mems[data+n/2-1]
+	}
+	if (domean)
+	    mean = asums (Mems[data], n) / n
+
+	call sfree (sp)
+end
+
+
+define	NMIN	10	# Minimum number of pixels for mode calculation
+define	ZRANGE	0.8	# Fraction of pixels about median to use
+define	ZSTEP	0.01	# Step size for search for mode
+define	ZBIN	0.1	# Bin size for mode.
+
+# IC_MODE -- Compute mode of an array.  The mode is found by binning
+# with a bin size based on the data range over a fraction of the
+# pixels about the median and a bin step which may be smaller than the
+# bin size.  If there are too few points the median is returned.
+# The input array must be sorted.
+
+short procedure ic_modes (a, n)
+
+short	a[n]			# Data array
+int	n			# Number of points
+
+int	i, j, k, nmax
+real	z1, z2, zstep, zbin
+short	mode
+bool	fp_equalr()
+
+begin
+	if (n < NMIN)
+	    return (a[n/2])
+
+	# Compute the mode.  The array must be sorted.  Consider a
+	# range of values about the median point.  Use a bin size which
+	# is ZBIN of the range.  Step the bin limits in ZSTEP fraction of
+	# the bin size.
+
+	i = 1 + n * (1. - ZRANGE) / 2.
+	j = 1 + n * (1. + ZRANGE) / 2.
+	z1 = a[i]
+	z2 = a[j]
+	if (fp_equalr (z1, z2)) {
+	    mode = z1
+	    return (mode)
+	}
+
+	zstep = ZSTEP * (z2 - z1)
+	zbin = ZBIN * (z2 - z1)
+	zstep = max (1., zstep)
+	zbin = max (1., zbin)
+
+	z1 = z1 - zstep
+	k = i
+	nmax = 0
+	repeat {
+	    z1 = z1 + zstep
+	    z2 = z1 + zbin
+	    for (; i < j && a[i] < z1; i=i+1)
+		;
+	    for (; k < j && a[k] < z2; k=k+1)
+		;
+	    if (k - i > nmax) {
+	        nmax = k - i
+	        mode = a[(i+k)/2]
+	    }
+	} until (k >= j)
+
+	return (mode)
+end
+
+# IC_STAT -- Compute image statistics within specified section.
+# The image section is relative to a reference image which may be
+# different than the input image and may have an offset.  Only a
+# subsample of pixels is used.  Masked and thresholded pixels are
+# ignored.  Only the desired statistics are computed to increase
+# efficiency.
+
+procedure ic_statr (im, imref, section, offsets, image, nimages,
+	domode, domedian, domean, mode, median, mean)
+
+pointer	im			 # Data image
+pointer	imref			 # Reference image for image section
+char	section[ARB]		 # Image section
+int	offsets[nimages,ARB]	 # Image section offset from data to reference
+int	image			 # Image index (for mask I/O)
+int	nimages			 # Number of images in  offsets.
+bool	domode, domedian, domean # Statistics to compute
+real	mode, median, mean	 # Statistics
+
+int	i, j, ndim, n, nv
+real	a
+pointer	sp, v1, v2, dv, va, vb
+pointer	data, mask, dp, lp, mp, imgnlr()
+real	ic_moder()
+real    asumr()
+
+
+include	"../icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (v1, IM_MAXDIM, TY_LONG)
+	call salloc (v2, IM_MAXDIM, TY_LONG)
+	call salloc (dv, IM_MAXDIM, TY_LONG)
+	call salloc (va, IM_MAXDIM, TY_LONG)
+	call salloc (vb, IM_MAXDIM, TY_LONG)
+
+	# Determine the image section parameters.  This must be in terms of
+	# the data image pixel coordinates though the section may be specified
+	# in terms of the reference image coordinates.  Limit the number of
+	# pixels in each dimension to a maximum.
+
+	ndim = IM_NDIM(im)
+	if (project)
+	    ndim = ndim - 1
+	call amovki (1, Memi[v1], IM_MAXDIM)
+	call amovki (1, Memi[va], IM_MAXDIM)
+	call amovki (1, Memi[dv], IM_MAXDIM)
+	call amovi (IM_LEN(imref,1), Memi[vb], ndim)
+	call ic_section (section, Memi[va], Memi[vb], Memi[dv], ndim)
+	if (im != imref)
+	    do i = 1, ndim {
+		Memi[va+i-1] = Memi[va+i-1] - offsets[image,i]
+		Memi[vb+i-1] = Memi[vb+i-1] - offsets[image,i]
+	    }
+
+	do j = 1, 10 {
+	    n = 1
+	    do i = 0, ndim-1 {
+		Memi[v1+i] = max (1, min (Memi[va+i], Memi[vb+i]))
+		Memi[v2+i] = min (IM_LEN(im,i+1), max (Memi[va+i], Memi[vb+i]))
+		Memi[dv+i] = j
+		nv = max (1, (Memi[v2+i] - Memi[v1+i]) / Memi[dv+i] + 1)
+		Memi[v2+i] = Memi[v1+i] + (nv - 1) * Memi[dv+i]
+		n = n * nv
+	    }
+	    if (n < NMAX)
+		break
+	}
+
+	call amovl (Memi[v1], Memi[va], IM_MAXDIM)
+	Memi[va] = 1
+	if (project)
+	   Memi[va+ndim] = image
+	call amovl (Memi[va], Memi[vb], IM_MAXDIM)
+
+	# Accumulate the pixel values within the section.  Masked pixels and
+	# thresholded pixels are ignored.
+
+	call salloc (data, n, TY_REAL)
+	dp = data
+	while (imgnlr (im, lp, Memi[vb]) != EOF) {
+	    call ic_mget1 (im, image, offsets[image,1], Memi[va], mask)
+	    lp = lp + Memi[v1] - 1
+	    if (dflag == D_ALL) {
+		if (dothresh) {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			a = Memr[lp]
+			if (a >= lthresh && a <= hthresh) {
+			    Memr[dp] = a
+			    dp = dp + 1
+			}
+			lp = lp + Memi[dv]
+		    }
+		} else {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			Memr[dp] = Memr[lp]
+			dp = dp + 1
+			lp = lp + Memi[dv]
+		    }
+		}
+	    } else if (dflag == D_MIX) {
+		mp = mask + Memi[v1] - 1
+		if (dothresh) {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			if (Memi[mp] == 0) {
+			    a = Memr[lp]
+			    if (a >= lthresh && a <= hthresh) {
+				Memr[dp] = a
+				dp = dp + 1
+			    }
+			}
+			mp = mp + Memi[dv]
+			lp = lp + Memi[dv]
+		    }
+		} else {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			if (Memi[mp] == 0) {
+			    Memr[dp] = Memr[lp]
+			    dp = dp + 1
+			}
+			mp = mp + Memi[dv]
+			lp = lp + Memi[dv]
+		    }
+		}
+	    }
+	    for (i=2; i<=ndim; i=i+1) {
+		Memi[va+i-1] = Memi[va+i-1] + Memi[dv+i-1]
+		if (Memi[va+i-1] <= Memi[v2+i-1])
+		    break
+		Memi[va+i-1] = Memi[v1+i-1]
+	    }
+	    if (i > ndim)
+		break
+	    call amovl (Memi[va], Memi[vb], IM_MAXDIM)
+	}
+
+	n = dp - data
+	if (n < 1) {
+	    call sfree (sp)
+	    call error (1, "Image section contains no pixels")
+	}
+
+	# Compute only statistics needed.
+	if (domode || domedian) {
+	    call asrtr (Memr[data], Memr[data], n)
+	    mode = ic_moder (Memr[data], n)
+	    median = Memr[data+n/2-1]
+	}
+	if (domean)
+	    mean = asumr (Memr[data], n) / n
+
+	call sfree (sp)
+end
+
+
+define	NMIN	10	# Minimum number of pixels for mode calculation
+define	ZRANGE	0.8	# Fraction of pixels about median to use
+define	ZSTEP	0.01	# Step size for search for mode
+define	ZBIN	0.1	# Bin size for mode.
+
+# IC_MODE -- Compute mode of an array.  The mode is found by binning
+# with a bin size based on the data range over a fraction of the
+# pixels about the median and a bin step which may be smaller than the
+# bin size.  If there are too few points the median is returned.
+# The input array must be sorted.
+
+real procedure ic_moder (a, n)
+
+real	a[n]			# Data array
+int	n			# Number of points
+
+int	i, j, k, nmax
+real	z1, z2, zstep, zbin
+real	mode
+bool	fp_equalr()
+
+begin
+	if (n < NMIN)
+	    return (a[n/2])
+
+	# Compute the mode.  The array must be sorted.  Consider a
+	# range of values about the median point.  Use a bin size which
+	# is ZBIN of the range.  Step the bin limits in ZSTEP fraction of
+	# the bin size.
+
+	i = 1 + n * (1. - ZRANGE) / 2.
+	j = 1 + n * (1. + ZRANGE) / 2.
+	z1 = a[i]
+	z2 = a[j]
+	if (fp_equalr (z1, z2)) {
+	    mode = z1
+	    return (mode)
+	}
+
+	zstep = ZSTEP * (z2 - z1)
+	zbin = ZBIN * (z2 - z1)
+
+	z1 = z1 - zstep
+	k = i
+	nmax = 0
+	repeat {
+	    z1 = z1 + zstep
+	    z2 = z1 + zbin
+	    for (; i < j && a[i] < z1; i=i+1)
+		;
+	    for (; k < j && a[k] < z2; k=k+1)
+		;
+	    if (k - i > nmax) {
+	        nmax = k - i
+	        mode = a[(i+k)/2]
+	    }
+	} until (k >= j)
+
+	return (mode)
+end
+
diff --git a/noao/imred/ccdred/src/generic/mkpkg b/noao/imred/ccdred/src/generic/mkpkg
new file mode 100644
index 00000000..3d841680
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/mkpkg
@@ -0,0 +1,11 @@
+# Make CCDRED Package.
+
+$checkout libpkg.a ../..
+$update   libpkg.a
+$checkin  libpkg.a ../..
+$exit
+
+libpkg.a:
+	cor.x		ccdred.h
+	proc.x		ccdred.h <imhdr.h>
+	;
diff --git a/noao/imred/ccdred/src/generic/proc.x b/noao/imred/ccdred/src/generic/proc.x
new file mode 100644
index 00000000..242da9c9
--- /dev/null
+++ b/noao/imred/ccdred/src/generic/proc.x
@@ -0,0 +1,735 @@
+include	<imhdr.h>
+include	"ccdred.h"
+
+
+.help proc Feb87 noao.imred.ccdred
+.nf ----------------------------------------------------------------------------
+proc -- Process CCD images
+
+These are the main CCD reduction procedures.  There is one for each
+readout axis (lines or columns) and one for short and real image data.
+They apply corrections for bad pixels, overscan levels, zero levels,
+dark counts, flat field response, illumination response, and fringe
+effects.  The image is also trimmed if it was mapped with an image
+section.  The mean value for the output image is computed when the flat
+field or illumination image is processed to form the scale factor for
+these calibrations in order to avoid reading through these image a
+second time.
+
+The processing information and parameters are specified in the CCD
+structure. The processing operations to be performed are specified by
+the correction array CORS in the ccd structure.  There is one array
+element for each operation with indices defined symbolically by macro
+definitions (see ccdred.h); i.e.  FLATCOR.  The value of the array
+element is an integer bit field in which the bit set is the same as the
+array index; i.e element 3 will have the third bit set for an operation
+with array value 2**(3-1)=4.  If an operation is not to be performed
+the bit is not set and the array element has the numeric value zero.
+Note that the addition of several correction elements gives a unique
+bit field describing a combination of operations.  For efficiency the
+most common combinations are implemented as separate units.
+
+The CCD structure also contains the correction or calibration data
+consisting either pointers to data, IMIO pointers for the calibration
+images, and scale factors.
+
+The processing is performed line-by-line.  The procedure CORINPUT is
+called to get an input line.  This procedure trims and fixes bad pixels by
+interpolation.  The output line and lines from the various calibration
+images are read.  The image vectors as well as the overscan vector and
+the scale factors are passed to the procedure COR (which also
+dereferences the pointer data into simple arrays and variables).  That
+procedure does the actual corrections apart from bad pixel
+corrections.
+
+The final optional step is to add each corrected output line to form a
+mean.  This adds efficiency since the operation is done only if desired
+and the output image data is already in memory so there is no I/O
+penalty.
+
+SEE ALSO
+    ccdred.h, cor, fixpix, setfixpix, setoverscan, settrim,
+    setzero, setdark, setflat, setillum, setfringe
+.endhelp ----------------------------------------------------------------------
+
+
+
+# PROC1 -- Process CCD images with readout axis 1 (lines).
+
+procedure proc1s (ccd)
+
+pointer	ccd		# CCD structure
+
+int	line, ncols, nlines, findmean, rep
+int	overscan_type, overscan_c1, noverscan
+real	overscan, darkscale, flatscale, illumscale, frgscale, mean
+short	minrep
+pointer	in, out, zeroim, darkim, flatim, illumim, fringeim, overscan_vec
+pointer	inbuf, outbuf, zerobuf, darkbuf, flatbuf, illumbuf, fringebuf
+
+real	asums()
+real	find_overscans()
+pointer	imgl2s(), impl2s(), ccd_gls(), xt_fpss()
+
+begin
+	# Initialize.  If the correction image is 1D then just get the
+	# data once.
+
+	in = IN_IM(ccd)
+	out = OUT_IM(ccd)
+	ncols = OUT_C2(ccd) - OUT_C1(ccd) + 1
+	nlines = OUT_L2(ccd) - OUT_L1(ccd) + 1
+
+	findmean = CORS(ccd, FINDMEAN)
+	if (findmean == YES)
+	    mean = 0.
+	rep = CORS(ccd, MINREP)
+	if (rep == YES)
+	    minrep = MINREPLACE(ccd)
+
+	if (CORS(ccd, OVERSCAN) == 0)
+	    overscan_type = 0
+	else {
+	    overscan_type = OVERSCAN_TYPE(ccd)
+	    overscan_vec = OVERSCAN_VEC(ccd)
+	    overscan_c1 = BIAS_C1(ccd) - 1
+	    noverscan = BIAS_C2(ccd) - overscan_c1
+	}
+
+	if (CORS(ccd, ZEROCOR) == 0) {
+	    zeroim = NULL
+	    zerobuf = 1
+	} else if (IM_LEN(ZERO_IM(ccd),2) == 1) {
+	    zeroim = NULL
+	    zerobuf = ccd_gls (ZERO_IM(ccd), ZERO_C1(ccd), ZERO_C2(ccd), 1)
+	} else
+	    zeroim = ZERO_IM(ccd)
+
+	if (CORS(ccd, DARKCOR) == 0) {
+	    darkim = NULL
+	    darkbuf = 1
+	} else if (IM_LEN(DARK_IM(ccd),2) == 1) {
+	    darkim = NULL
+	    darkbuf = ccd_gls (DARK_IM(ccd), DARK_C1(ccd), DARK_C2(ccd), 1)
+	    darkscale = FLATSCALE(ccd)
+	} else {
+	    darkim = DARK_IM(ccd)
+	    darkscale = DARKSCALE(ccd)
+	}
+
+	if (CORS(ccd, FLATCOR) == 0) {
+	    flatim = NULL
+	    flatbuf = 1
+	} else if (IM_LEN(FLAT_IM(ccd),2) == 1) {
+	    flatim = NULL
+	    flatbuf = ccd_gls (FLAT_IM(ccd), FLAT_C1(ccd), FLAT_C2(ccd), 1)
+	    flatscale = FLATSCALE(ccd)
+	} else {
+	    flatim = FLAT_IM(ccd)
+	    flatscale = FLATSCALE(ccd)
+	}
+
+	if (CORS(ccd, ILLUMCOR) == 0) {
+	    illumim = NULL
+	    illumbuf = 1
+	} else {
+	    illumim = ILLUM_IM(ccd)
+	    illumscale = ILLUMSCALE(ccd)
+	}
+
+	if (CORS(ccd, FRINGECOR) == 0) {
+	    fringeim = NULL
+	    fringebuf = 1
+	} else {
+	    fringeim = FRINGE_IM(ccd)
+	    frgscale = FRINGESCALE(ccd)
+	}
+
+	# For each line read lines from the input.  Procedure XT_FPS replaces
+	# bad pixels by interpolation.  The trimmed region is copied to the
+	# output.  Get lines from the output image and from the zero level,
+	# dark count, flat field, illumination, and fringe images.  Call COR1
+	# to do the actual pixel corrections.  Finally, add the output pixels
+	# to a sum for computing the mean.  We must copy data outside of the
+	# output data section.
+
+	do line = 2 - OUT_L1(ccd), 0
+	    call amovs (
+		Mems[imgl2s(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mems[impl2s(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	do line = 1, nlines {
+	    outbuf = impl2s (out, OUT_L1(ccd)+line-1)
+
+	    inbuf = xt_fpss (MASK_FP(ccd), in, IN_L1(ccd)+line-1, IN_C1(ccd),
+		IN_C2(ccd), IN_L1(ccd), IN_L2(ccd), NULL)
+	    call amovs (Mems[inbuf+IN_C1(ccd)-OUT_C1(ccd)], Mems[outbuf],
+		IM_LEN(out,1))
+
+	    outbuf = outbuf + OUT_C1(ccd) - 1
+	    if (overscan_type != 0) {
+		if (overscan_type < OVERSCAN_FIT)
+		    overscan = find_overscans (Mems[inbuf+overscan_c1],
+			noverscan, overscan_type)
+		else
+		    overscan = Memr[overscan_vec+line-1]
+	    }
+	    if (zeroim != NULL)
+		zerobuf = ccd_gls (zeroim, ZERO_C1(ccd), ZERO_C2(ccd),
+		    ZERO_L1(ccd)+line-1)
+	    if (darkim != NULL)
+		darkbuf = ccd_gls (darkim, DARK_C1(ccd), DARK_C2(ccd),
+		    DARK_L1(ccd)+line-1)
+	    if (flatim != NULL)
+		flatbuf = ccd_gls (flatim, FLAT_C1(ccd), FLAT_C2(ccd),
+		    FLAT_L1(ccd)+line-1)
+	    if (illumim != NULL)
+		illumbuf = ccd_gls (illumim, ILLUM_C1(ccd), ILLUM_C2(ccd),
+		    ILLUM_L1(ccd)+line-1)
+	    if (fringeim != NULL)
+		fringebuf = ccd_gls (fringeim, FRINGE_C1(ccd), FRINGE_C2(ccd),
+		    FRINGE_L1(ccd)+line-1)
+
+	    call cor1s (CORS(ccd,1), Mems[outbuf],
+		overscan, Mems[zerobuf], Mems[darkbuf],
+		Mems[flatbuf], Mems[illumbuf], Mems[fringebuf], ncols,
+		darkscale, flatscale, illumscale, frgscale)
+
+	    if (rep == YES)
+		call amaxks (Mems[outbuf], minrep, Mems[outbuf], ncols)
+	    if (findmean == YES)
+		mean = mean + asums (Mems[outbuf], ncols)
+	}
+
+	do line = nlines+1, IM_LEN(out,2)-OUT_L1(ccd)+1
+	    call amovs (
+		Mems[imgl2s(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mems[impl2s(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	# Compute the mean from the sum of the output pixels.
+	if (findmean == YES)
+	    MEAN(ccd) = mean / ncols / nlines
+end
+
+
+# PROC2 -- Process CCD images with readout axis 2 (columns).
+
+procedure proc2s (ccd)
+
+pointer	ccd		# CCD structure
+
+int	line, ncols, nlines, findmean, rep
+real	darkscale, flatscale, illumscale, frgscale, mean
+short	minrep
+pointer	in, out, zeroim, darkim, flatim, illumim, fringeim, overscan_vec
+pointer	inbuf, outbuf, zerobuf, darkbuf, flatbuf, illumbuf, fringebuf
+
+real	asums()
+pointer	imgl2s(), impl2s(), imgs2s(), ccd_gls(), xt_fpss()
+
+begin
+	# Initialize.  If the correction image is 1D then just get the
+	# data once.
+
+	in = IN_IM(ccd)
+	out = OUT_IM(ccd)
+	ncols = OUT_C2(ccd) - OUT_C1(ccd) + 1
+	nlines = OUT_L2(ccd) - OUT_L1(ccd) + 1
+
+	findmean = CORS(ccd, FINDMEAN)
+	if (findmean == YES)
+	    mean = 0.
+	rep = CORS(ccd, MINREP)
+	if (rep == YES)
+	    minrep = MINREPLACE(ccd)
+
+	overscan_vec = OVERSCAN_VEC(ccd)
+
+	if (CORS(ccd, ZEROCOR) == 0) {
+	    zeroim = NULL
+	    zerobuf = 1
+	} else if (IM_LEN(ZERO_IM(ccd),1) == 1) {
+	    zeroim = NULL
+	    zerobuf = imgs2s (ZERO_IM(ccd), 1, 1, ZERO_L1(ccd), ZERO_L2(ccd))
+	} else
+	    zeroim = ZERO_IM(ccd)
+
+	if (CORS(ccd, DARKCOR) == 0) {
+	    darkim = NULL
+	    darkbuf = 1
+	} else if (IM_LEN(DARK_IM(ccd),1) == 1) {
+	    darkim = NULL
+	    darkbuf = imgs2s (DARK_IM(ccd), 1, 1, DARK_L1(ccd), DARK_L2(ccd))
+	    darkscale = DARKSCALE(ccd)
+	} else {
+	    darkim = DARK_IM(ccd)
+	    darkscale = DARKSCALE(ccd)
+	}
+
+	if (CORS(ccd, FLATCOR) == 0) {
+	    flatim = NULL
+	    flatbuf = 1
+	} else if (IM_LEN(FLAT_IM(ccd),1) == 1) {
+	    flatim = NULL
+	    flatbuf = imgs2s (FLAT_IM(ccd), 1, 1, FLAT_L1(ccd), FLAT_L2(ccd))
+	    flatscale = FLATSCALE(ccd)
+	} else {
+	    flatim = FLAT_IM(ccd)
+	    flatscale = FLATSCALE(ccd)
+	}
+
+	if (CORS(ccd, ILLUMCOR) == 0) {
+	    illumim = NULL
+	    illumbuf = 1
+	} else {
+	    illumim = ILLUM_IM(ccd)
+	    illumscale = ILLUMSCALE(ccd)
+	}
+
+	if (CORS(ccd, FRINGECOR) == 0) {
+	    fringeim = NULL
+	    fringebuf = 1
+	} else {
+	    fringeim = FRINGE_IM(ccd)
+	    frgscale = FRINGESCALE(ccd)
+	}
+
+	# For each line read lines from the input.  Procedure CORINPUT
+	# replaces bad pixels by interpolation and applies a trim to the
+	# input.  Get lines from the output image and from the zero level,
+	# dark count, flat field, illumination, and fringe images.
+	# Call COR2 to do the actual pixel corrections.  Finally, add the
+	# output pixels to a sum for computing the mean.
+	# We must copy data outside of the output data section.
+
+	do line = 2 - OUT_L1(ccd), 0
+	    call amovs (
+		Mems[imgl2s(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mems[impl2s(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	do line = 1, nlines {
+	    outbuf = impl2s (out, OUT_L1(ccd)+line-1)
+
+	    inbuf = xt_fpss (MASK_FP(ccd), in, IN_L1(ccd)+line-1, IN_C1(ccd),
+		IN_C2(ccd), IN_L1(ccd), IN_L2(ccd), NULL)
+	    call amovs (Mems[inbuf+IN_C1(ccd)-OUT_C1(ccd)], Mems[outbuf],
+		IM_LEN(out,1))
+
+	    outbuf = outbuf + OUT_C1(ccd) - 1
+	    if (zeroim != NULL)
+		zerobuf = ccd_gls (zeroim, ZERO_C1(ccd), ZERO_C2(ccd),
+		    ZERO_L1(ccd)+line-1)
+	    if (darkim != NULL)
+		darkbuf = ccd_gls (darkim, DARK_C1(ccd), DARK_C2(ccd),
+		    DARK_L1(ccd)+line-1)
+	    if (flatim != NULL)
+		flatbuf = ccd_gls (flatim, FLAT_C1(ccd), FLAT_C2(ccd),
+		    FLAT_L1(ccd)+line-1)
+	    if (illumim != NULL)
+		illumbuf = ccd_gls (illumim, ILLUM_C1(ccd), ILLUM_C2(ccd),
+		    ILLUM_L1(ccd)+line-1)
+	    if (fringeim != NULL)
+		fringebuf = ccd_gls (fringeim, FRINGE_C1(ccd), FRINGE_C2(ccd),
+		    FRINGE_L1(ccd)+line-1)
+
+	    call cor2s (line, CORS(ccd,1), Mems[outbuf],
+		Memr[overscan_vec], Mems[zerobuf], Mems[darkbuf],
+		Mems[flatbuf], Mems[illumbuf], Mems[fringebuf], ncols,
+		zeroim, flatim, darkscale, flatscale, illumscale, frgscale)
+
+	    if (rep == YES)
+		call amaxks (Mems[outbuf], minrep, Mems[outbuf], ncols)
+	    if (findmean == YES)
+		mean = mean + asums (Mems[outbuf], ncols)
+	}
+
+	do line = nlines+1, IM_LEN(out,2)-OUT_L1(ccd)+1
+	    call amovs (
+		Mems[imgl2s(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mems[impl2s(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	# Compute the mean from the sum of the output pixels.
+	if (findmean == YES)
+	    MEAN(ccd) = mean / ncols / nlines
+end
+
+
+# FIND_OVERSCAN -- Find the overscan value for a line.
+# No check is made on the number of pixels.
+# The median is the (npix+1)/2 element.
+
+real procedure find_overscans (data, npix, type)
+
+short	data[npix]	#I Overscan data
+int	npix		#I Number of overscan points
+int	type		#I Type of overscan calculation
+
+int	i
+real	overscan, d, dmin, dmax
+short	asoks()
+
+begin
+	if (type == OVERSCAN_MINMAX) {
+	    overscan = data[1]
+	    dmin = data[1]
+	    dmax = data[1]
+	    do i = 2, npix {
+		d = data[i]
+		overscan = overscan + d
+		if (d < dmin)
+		    dmin = d
+		else if (d > dmax)
+		    dmax = d
+	    }
+	    overscan = (overscan - dmin - dmax) / (npix - 2)
+	} else if (type == OVERSCAN_MEDIAN)
+	    overscan = asoks (data, npix, (npix + 1) / 2)
+	else {
+	    overscan = data[1]
+	    do i = 2, npix
+		overscan = overscan + data[i]
+	    overscan = overscan / npix
+	}
+
+	return (overscan)
+end
+
+# PROC1 -- Process CCD images with readout axis 1 (lines).
+
+procedure proc1r (ccd)
+
+pointer	ccd		# CCD structure
+
+int	line, ncols, nlines, findmean, rep
+int	overscan_type, overscan_c1, noverscan
+real	overscan, darkscale, flatscale, illumscale, frgscale, mean
+real	minrep
+pointer	in, out, zeroim, darkim, flatim, illumim, fringeim, overscan_vec
+pointer	inbuf, outbuf, zerobuf, darkbuf, flatbuf, illumbuf, fringebuf
+
+real	asumr()
+real	find_overscanr()
+pointer	imgl2r(), impl2r(), ccd_glr(), xt_fpsr()
+
+begin
+	# Initialize.  If the correction image is 1D then just get the
+	# data once.
+
+	in = IN_IM(ccd)
+	out = OUT_IM(ccd)
+	ncols = OUT_C2(ccd) - OUT_C1(ccd) + 1
+	nlines = OUT_L2(ccd) - OUT_L1(ccd) + 1
+
+	findmean = CORS(ccd, FINDMEAN)
+	if (findmean == YES)
+	    mean = 0.
+	rep = CORS(ccd, MINREP)
+	if (rep == YES)
+	    minrep = MINREPLACE(ccd)
+
+	if (CORS(ccd, OVERSCAN) == 0)
+	    overscan_type = 0
+	else {
+	    overscan_type = OVERSCAN_TYPE(ccd)
+	    overscan_vec = OVERSCAN_VEC(ccd)
+	    overscan_c1 = BIAS_C1(ccd) - 1
+	    noverscan = BIAS_C2(ccd) - overscan_c1
+	}
+
+	if (CORS(ccd, ZEROCOR) == 0) {
+	    zeroim = NULL
+	    zerobuf = 1
+	} else if (IM_LEN(ZERO_IM(ccd),2) == 1) {
+	    zeroim = NULL
+	    zerobuf = ccd_glr (ZERO_IM(ccd), ZERO_C1(ccd), ZERO_C2(ccd), 1)
+	} else
+	    zeroim = ZERO_IM(ccd)
+
+	if (CORS(ccd, DARKCOR) == 0) {
+	    darkim = NULL
+	    darkbuf = 1
+	} else if (IM_LEN(DARK_IM(ccd),2) == 1) {
+	    darkim = NULL
+	    darkbuf = ccd_glr (DARK_IM(ccd), DARK_C1(ccd), DARK_C2(ccd), 1)
+	    darkscale = FLATSCALE(ccd)
+	} else {
+	    darkim = DARK_IM(ccd)
+	    darkscale = DARKSCALE(ccd)
+	}
+
+	if (CORS(ccd, FLATCOR) == 0) {
+	    flatim = NULL
+	    flatbuf = 1
+	} else if (IM_LEN(FLAT_IM(ccd),2) == 1) {
+	    flatim = NULL
+	    flatbuf = ccd_glr (FLAT_IM(ccd), FLAT_C1(ccd), FLAT_C2(ccd), 1)
+	    flatscale = FLATSCALE(ccd)
+	} else {
+	    flatim = FLAT_IM(ccd)
+	    flatscale = FLATSCALE(ccd)
+	}
+
+	if (CORS(ccd, ILLUMCOR) == 0) {
+	    illumim = NULL
+	    illumbuf = 1
+	} else {
+	    illumim = ILLUM_IM(ccd)
+	    illumscale = ILLUMSCALE(ccd)
+	}
+
+	if (CORS(ccd, FRINGECOR) == 0) {
+	    fringeim = NULL
+	    fringebuf = 1
+	} else {
+	    fringeim = FRINGE_IM(ccd)
+	    frgscale = FRINGESCALE(ccd)
+	}
+
+	# For each line read lines from the input.  Procedure XT_FPS replaces
+	# bad pixels by interpolation.  The trimmed region is copied to the
+	# output.  Get lines from the output image and from the zero level,
+	# dark count, flat field, illumination, and fringe images.  Call COR1
+	# to do the actual pixel corrections.  Finally, add the output pixels
+	# to a sum for computing the mean.  We must copy data outside of the
+	# output data section.
+
+	do line = 2 - OUT_L1(ccd), 0
+	    call amovr (
+		Memr[imgl2r(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Memr[impl2r(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	do line = 1, nlines {
+	    outbuf = impl2r (out, OUT_L1(ccd)+line-1)
+
+	    inbuf = xt_fpsr (MASK_FP(ccd), in, IN_L1(ccd)+line-1, IN_C1(ccd),
+		IN_C2(ccd), IN_L1(ccd), IN_L2(ccd), NULL)
+	    call amovr (Memr[inbuf+IN_C1(ccd)-OUT_C1(ccd)], Memr[outbuf],
+		IM_LEN(out,1))
+
+	    outbuf = outbuf + OUT_C1(ccd) - 1
+	    if (overscan_type != 0) {
+		if (overscan_type < OVERSCAN_FIT)
+		    overscan = find_overscanr (Memr[inbuf+overscan_c1],
+			noverscan, overscan_type)
+		else
+		    overscan = Memr[overscan_vec+line-1]
+	    }
+	    if (zeroim != NULL)
+		zerobuf = ccd_glr (zeroim, ZERO_C1(ccd), ZERO_C2(ccd),
+		    ZERO_L1(ccd)+line-1)
+	    if (darkim != NULL)
+		darkbuf = ccd_glr (darkim, DARK_C1(ccd), DARK_C2(ccd),
+		    DARK_L1(ccd)+line-1)
+	    if (flatim != NULL)
+		flatbuf = ccd_glr (flatim, FLAT_C1(ccd), FLAT_C2(ccd),
+		    FLAT_L1(ccd)+line-1)
+	    if (illumim != NULL)
+		illumbuf = ccd_glr (illumim, ILLUM_C1(ccd), ILLUM_C2(ccd),
+		    ILLUM_L1(ccd)+line-1)
+	    if (fringeim != NULL)
+		fringebuf = ccd_glr (fringeim, FRINGE_C1(ccd), FRINGE_C2(ccd),
+		    FRINGE_L1(ccd)+line-1)
+
+	    call cor1r (CORS(ccd,1), Memr[outbuf],
+		overscan, Memr[zerobuf], Memr[darkbuf],
+		Memr[flatbuf], Memr[illumbuf], Memr[fringebuf], ncols,
+		darkscale, flatscale, illumscale, frgscale)
+
+	    if (rep == YES)
+		call amaxkr (Memr[outbuf], minrep, Memr[outbuf], ncols)
+	    if (findmean == YES)
+		mean = mean + asumr (Memr[outbuf], ncols)
+	}
+
+	do line = nlines+1, IM_LEN(out,2)-OUT_L1(ccd)+1
+	    call amovr (
+		Memr[imgl2r(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Memr[impl2r(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	# Compute the mean from the sum of the output pixels.
+	if (findmean == YES)
+	    MEAN(ccd) = mean / ncols / nlines
+end
+
+
+# PROC2 -- Process CCD images with readout axis 2 (columns).
+
+procedure proc2r (ccd)
+
+pointer	ccd		# CCD structure
+
+int	line, ncols, nlines, findmean, rep
+real	darkscale, flatscale, illumscale, frgscale, mean
+real	minrep
+pointer	in, out, zeroim, darkim, flatim, illumim, fringeim, overscan_vec
+pointer	inbuf, outbuf, zerobuf, darkbuf, flatbuf, illumbuf, fringebuf
+
+real	asumr()
+pointer	imgl2r(), impl2r(), imgs2r(), ccd_glr(), xt_fpsr()
+
+begin
+	# Initialize.  If the correction image is 1D then just get the
+	# data once.
+
+	in = IN_IM(ccd)
+	out = OUT_IM(ccd)
+	ncols = OUT_C2(ccd) - OUT_C1(ccd) + 1
+	nlines = OUT_L2(ccd) - OUT_L1(ccd) + 1
+
+	findmean = CORS(ccd, FINDMEAN)
+	if (findmean == YES)
+	    mean = 0.
+	rep = CORS(ccd, MINREP)
+	if (rep == YES)
+	    minrep = MINREPLACE(ccd)
+
+	overscan_vec = OVERSCAN_VEC(ccd)
+
+	if (CORS(ccd, ZEROCOR) == 0) {
+	    zeroim = NULL
+	    zerobuf = 1
+	} else if (IM_LEN(ZERO_IM(ccd),1) == 1) {
+	    zeroim = NULL
+	    zerobuf = imgs2r (ZERO_IM(ccd), 1, 1, ZERO_L1(ccd), ZERO_L2(ccd))
+	} else
+	    zeroim = ZERO_IM(ccd)
+
+	if (CORS(ccd, DARKCOR) == 0) {
+	    darkim = NULL
+	    darkbuf = 1
+	} else if (IM_LEN(DARK_IM(ccd),1) == 1) {
+	    darkim = NULL
+	    darkbuf = imgs2r (DARK_IM(ccd), 1, 1, DARK_L1(ccd), DARK_L2(ccd))
+	    darkscale = DARKSCALE(ccd)
+	} else {
+	    darkim = DARK_IM(ccd)
+	    darkscale = DARKSCALE(ccd)
+	}
+
+	if (CORS(ccd, FLATCOR) == 0) {
+	    flatim = NULL
+	    flatbuf = 1
+	} else if (IM_LEN(FLAT_IM(ccd),1) == 1) {
+	    flatim = NULL
+	    flatbuf = imgs2r (FLAT_IM(ccd), 1, 1, FLAT_L1(ccd), FLAT_L2(ccd))
+	    flatscale = FLATSCALE(ccd)
+	} else {
+	    flatim = FLAT_IM(ccd)
+	    flatscale = FLATSCALE(ccd)
+	}
+
+	if (CORS(ccd, ILLUMCOR) == 0) {
+	    illumim = NULL
+	    illumbuf = 1
+	} else {
+	    illumim = ILLUM_IM(ccd)
+	    illumscale = ILLUMSCALE(ccd)
+	}
+
+	if (CORS(ccd, FRINGECOR) == 0) {
+	    fringeim = NULL
+	    fringebuf = 1
+	} else {
+	    fringeim = FRINGE_IM(ccd)
+	    frgscale = FRINGESCALE(ccd)
+	}
+
+	# For each line read lines from the input.  Procedure CORINPUT
+	# replaces bad pixels by interpolation and applies a trim to the
+	# input.  Get lines from the output image and from the zero level,
+	# dark count, flat field, illumination, and fringe images.
+	# Call COR2 to do the actual pixel corrections.  Finally, add the
+	# output pixels to a sum for computing the mean.
+	# We must copy data outside of the output data section.
+
+	do line = 2 - OUT_L1(ccd), 0
+	    call amovr (
+		Memr[imgl2r(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Memr[impl2r(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	do line = 1, nlines {
+	    outbuf = impl2r (out, OUT_L1(ccd)+line-1)
+
+	    inbuf = xt_fpsr (MASK_FP(ccd), in, IN_L1(ccd)+line-1, IN_C1(ccd),
+		IN_C2(ccd), IN_L1(ccd), IN_L2(ccd), NULL)
+	    call amovr (Memr[inbuf+IN_C1(ccd)-OUT_C1(ccd)], Memr[outbuf],
+		IM_LEN(out,1))
+
+	    outbuf = outbuf + OUT_C1(ccd) - 1
+	    if (zeroim != NULL)
+		zerobuf = ccd_glr (zeroim, ZERO_C1(ccd), ZERO_C2(ccd),
+		    ZERO_L1(ccd)+line-1)
+	    if (darkim != NULL)
+		darkbuf = ccd_glr (darkim, DARK_C1(ccd), DARK_C2(ccd),
+		    DARK_L1(ccd)+line-1)
+	    if (flatim != NULL)
+		flatbuf = ccd_glr (flatim, FLAT_C1(ccd), FLAT_C2(ccd),
+		    FLAT_L1(ccd)+line-1)
+	    if (illumim != NULL)
+		illumbuf = ccd_glr (illumim, ILLUM_C1(ccd), ILLUM_C2(ccd),
+		    ILLUM_L1(ccd)+line-1)
+	    if (fringeim != NULL)
+		fringebuf = ccd_glr (fringeim, FRINGE_C1(ccd), FRINGE_C2(ccd),
+		    FRINGE_L1(ccd)+line-1)
+
+	    call cor2r (line, CORS(ccd,1), Memr[outbuf],
+		Memr[overscan_vec], Memr[zerobuf], Memr[darkbuf],
+		Memr[flatbuf], Memr[illumbuf], Memr[fringebuf], ncols,
+		zeroim, flatim, darkscale, flatscale, illumscale, frgscale)
+
+	    if (rep == YES)
+		call amaxkr (Memr[outbuf], minrep, Memr[outbuf], ncols)
+	    if (findmean == YES)
+		mean = mean + asumr (Memr[outbuf], ncols)
+	}
+
+	do line = nlines+1, IM_LEN(out,2)-OUT_L1(ccd)+1
+	    call amovr (
+		Memr[imgl2r(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Memr[impl2r(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	# Compute the mean from the sum of the output pixels.
+	if (findmean == YES)
+	    MEAN(ccd) = mean / ncols / nlines
+end
+
+
+# FIND_OVERSCAN -- Find the overscan value for a line.
+# No check is made on the number of pixels.
+# The median is the (npix+1)/2 element.
+
+real procedure find_overscanr (data, npix, type)
+
+real	data[npix]	#I Overscan data
+int	npix		#I Number of overscan points
+int	type		#I Type of overscan calculation
+
+int	i
+real	overscan, d, dmin, dmax
+real	asokr()
+
+begin
+	if (type == OVERSCAN_MINMAX) {
+	    overscan = data[1]
+	    dmin = data[1]
+	    dmax = data[1]
+	    do i = 2, npix {
+		d = data[i]
+		overscan = overscan + d
+		if (d < dmin)
+		    dmin = d
+		else if (d > dmax)
+		    dmax = d
+	    }
+	    overscan = (overscan - dmin - dmax) / (npix - 2)
+	} else if (type == OVERSCAN_MEDIAN)
+	    overscan = asokr (data, npix, (npix + 1) / 2)
+	else {
+	    overscan = data[1]
+	    do i = 2, npix
+		overscan = overscan + data[i]
+	    overscan = overscan / npix
+	}
+
+	return (overscan)
+end
diff --git a/noao/imred/ccdred/src/hdrmap.com b/noao/imred/ccdred/src/hdrmap.com
new file mode 100644
index 00000000..5aa74185
--- /dev/null
+++ b/noao/imred/ccdred/src/hdrmap.com
@@ -0,0 +1,4 @@
+# Common for HDRMAP package.
+
+pointer	stp			# Symbol table pointer
+common	/hdmcom/ stp
diff --git a/noao/imred/ccdred/src/hdrmap.x b/noao/imred/ccdred/src/hdrmap.x
new file mode 100644
index 00000000..ebcb253e
--- /dev/null
+++ b/noao/imred/ccdred/src/hdrmap.x
@@ -0,0 +1,544 @@
+include	<error.h>
+include	<syserr.h>
+
+.help hdrmap
+.nf-----------------------------------------------------------------------------
+HDRMAP -- Map translation between task parameters and image header parameters.
+
+In order for tasks to be partially independent of the image header
+parameter names used by different instruments and observatories a
+translation is made between task parameters and image header
+parameters.  This translation is given in a file consisting of the task
+parameter name, the image header parameter name, and an optional
+default value.  This file is turned into a symbol table.  If the
+translation file is not found a null pointer is returned.  The package will
+then use the task parameter names directly.  Also if there is no
+translation given in the file for a particular parameter it is passed
+on directly.  If a parameter is not in the image header then the symbol
+table default value, if given, is returned.  This package is layered on
+the IMIO header package.
+
+	        hdmopen (fname)
+		hdmclose ()
+		hdmwrite (fname, mode)
+		hdmname (parameter, str, max_char)
+		hdmgdef (parameter, str, max_char)
+		hdmpdef (parameter, str, max_char)
+	  y/n = hdmaccf (im, parameter)
+		hdmgstr (im, parameter, str, max_char)
+	 ival = hdmgeti (im, parameter)
+	 rval = hdmgetr (im, parameter)
+		hdmpstr (im, parameter, str)
+		hdmputi (im, parameter, value)
+		hdmputr (im, parameter, value)
+		hdmgstp (stp)
+		hdmpstp (stp)
+		hdmdelf (im, parameter)
+		hdmparm (name, parameter, max_char)
+
+hdmopen  -- Open the translation file and map it into a symbol table pointer.
+hdmclose -- Close the symbol table pointer.
+hdmwrite -- Write out translation file.
+hdmname  -- Return the image header parameter name.
+hdmpname -- Put the image header parameter name.
+hdmgdef  -- Get the default value as a string (null if none).
+hdmpdef  -- Put the default value as a string.
+hdmaccf  -- Return whether the image header parameter exists (regardless of
+	    whether there is a default value).
+hdmgstr  -- Get a string valued parameter.  Return default value if not in the
+	    image header.  Return null string if no default or image value.
+hdmgeti  -- Get an integer valued parameter.  Return default value if not in
+	    the image header and error condition if no default or image value.
+hdmgetr  -- Get a real valued parameter.  Return default value if not in
+	    the image header or error condition if no default or image value.
+hdmpstr  -- Put a string valued parameter in the image header.
+hdmputi  -- Put an integer valued parameter in the image header.
+hdmputr  -- Put a real valued parameter in the image header.
+hdmgstp  -- Get the symbol table pointer to save it while another map is used.
+hdmpstp  -- Put the symbol table pointer to restore a map.
+hdmdelf  -- Delete a field.
+hdmparm  -- Return the parameter name corresponding to an image header name.
+.endhelp -----------------------------------------------------------------------
+
+# Symbol table definitions.
+define	LEN_INDEX	32		# Length of symtab index
+define	LEN_STAB	1024		# Length of symtab string buffer
+define	SZ_SBUF		128		# Size of symtab string buffer
+
+define	SZ_NAME		79		# Size of translation symbol name
+define	SZ_DEFAULT	79		# Size of default string
+define	SYMLEN		80		# Length of symbol structure
+
+# Symbol table structure
+define	NAME		Memc[P2C($1)]		# Translation name for symbol
+define	DEFAULT		Memc[P2C($1+40)]	# Default value of parameter
+
+
+# HDMOPEN -- Open the translation file and map it into a symbol table pointer.
+
+procedure hdmopen (fname)
+
+char	fname[ARB]		# Image header map file
+
+int	fd, open(), fscan(), nscan(), errcode()
+pointer	sp, parameter, sym, stopen(), stenter()
+include	"hdrmap.com"
+
+begin
+	# Create an empty symbol table.
+	stp = stopen (fname, LEN_INDEX, LEN_STAB, SZ_SBUF)
+
+	# Return if file not found.
+	iferr (fd = open (fname, READ_ONLY, TEXT_FILE)) {
+	    if (errcode () != SYS_FNOFNAME)
+		call erract (EA_WARN)
+	    return
+	}
+
+	call smark (sp)
+	call salloc (parameter, SZ_NAME, TY_CHAR)
+
+	# Read the file an enter the translations in the symbol table.
+	while (fscan(fd) != EOF) {
+	    call gargwrd (Memc[parameter], SZ_NAME)
+	    if ((nscan() == 0) || (Memc[parameter] == '#'))
+		next
+	    sym = stenter (stp, Memc[parameter], SYMLEN)
+	    call gargwrd (NAME(sym), SZ_NAME)
+	    call gargwrd (DEFAULT(sym), SZ_DEFAULT)
+	}
+
+	call close (fd)
+	call sfree (sp)
+end
+
+
+# HDMCLOSE -- Close the symbol table pointer.
+
+procedure hdmclose ()
+
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    call stclose (stp)
+end
+
+
+# HDMWRITE -- Write out translation file.
+
+procedure hdmwrite (fname, mode)
+
+char	fname[ARB]		# Image header map file
+int	mode			# Access mode (APPEND, NEW_FILE)
+
+int	fd, open(), stridxs()
+pointer	sym, sthead(), stnext(), stname()
+errchk	open
+include	"hdrmap.com"
+
+begin
+	# If there is no symbol table do nothing.
+	if (stp == NULL)
+	    return
+
+	fd = open (fname, mode, TEXT_FILE)
+
+	sym = sthead (stp)
+	for (sym = sthead (stp); sym != NULL; sym = stnext (stp, sym)) {
+	    if (stridxs (" 	", Memc[stname (stp, sym)]) > 0)
+		call fprintf (fd, "'%s'%30t")
+	    else
+		call fprintf (fd, "%s%30t")
+	    call pargstr (Memc[stname (stp, sym)])
+	    if (stridxs (" 	", NAME(sym)) > 0)
+		call fprintf (fd, " '%s'%10t")
+	    else
+		call fprintf (fd, " %s%10t")
+	    call pargstr (NAME(sym))
+	    if (DEFAULT(sym) != EOS) {
+		if (stridxs (" 	", DEFAULT(sym)) > 0)
+		    call fprintf (fd, " '%s'")
+		else
+		    call fprintf (fd, " %s")
+		call pargstr (DEFAULT(sym))
+	    }
+	    call fprintf (fd, "\n")
+	}
+
+	call close (fd)
+end
+
+
+# HDMNAME -- Return the image header parameter name
+
+procedure hdmname (parameter, str, max_char)
+
+char	parameter[ARB]		# Parameter name
+char	str[max_char]		# String containing mapped parameter name
+int	max_char		# Maximum characters in string
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call strcpy (NAME(sym), str, max_char)
+	else
+	    call strcpy (parameter, str, max_char)
+end
+
+
+# HDMPNAME -- Put the image header parameter name
+
+procedure hdmpname (parameter, str)
+
+char	parameter[ARB]		# Parameter name
+char	str[ARB]		# String containing mapped parameter name
+
+pointer	sym, stfind(), stenter()
+include	"hdrmap.com"
+
+begin
+	if (stp == NULL)
+	    return
+
+	sym = stfind (stp, parameter)
+	if (sym == NULL) {
+	    sym = stenter (stp, parameter, SYMLEN)
+	    DEFAULT(sym) = EOS
+	}
+
+	call strcpy (str, NAME(sym), SZ_NAME)
+end
+
+
+# HDMGDEF -- Get the default value as a string (null string if none).
+
+procedure hdmgdef (parameter, str, max_char)
+
+char	parameter[ARB]		# Parameter name
+char	str[max_char]		# String containing default value
+int	max_char		# Maximum characters in string
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call strcpy (DEFAULT(sym), str, max_char)
+	else
+	    str[1] = EOS
+end
+
+
+# HDMPDEF -- PUt the default value as a string.
+
+procedure hdmpdef (parameter, str)
+
+char	parameter[ARB]		# Parameter name
+char	str[ARB]		# String containing default value
+
+pointer	sym, stfind(), stenter()
+include	"hdrmap.com"
+
+begin
+	if (stp == NULL)
+	    return
+
+	sym = stfind (stp, parameter)
+	if (sym == NULL) {
+	    sym = stenter (stp, parameter, SYMLEN)
+	    call strcpy (parameter, NAME(sym), SZ_NAME)
+	}
+
+	call strcpy (str, DEFAULT(sym), SZ_DEFAULT)
+end
+
+
+# HDMACCF -- Return whether the image header parameter exists (regardless of
+# whether there is a default value).
+
+int procedure hdmaccf (im, parameter)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+
+int	imaccf()
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    return (imaccf (im, NAME(sym)))
+	else
+	    return (imaccf (im, parameter))
+end
+
+
+# HDMGSTR -- Get a string valued parameter.  Return default value if not in
+# the image header.  Return null string if no default or image value.
+
+procedure hdmgstr (im, parameter, str, max_char)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+char	str[max_char]		# String value to return
+int	max_char		# Maximum characters in returned string
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL) {
+	    iferr (call imgstr (im, NAME(sym), str, max_char))
+		call strcpy (DEFAULT(sym), str, max_char)
+	} else {
+	    iferr (call imgstr (im, parameter, str, max_char))
+		str[1] = EOS
+	}
+end
+
+
+# HDMGETR -- Get a real valued parameter.  Return default value if not in
+# the image header.  Return error condition if no default or image value.
+
+real procedure hdmgetr (im, parameter)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+
+int	ip, ctor()
+real	value, imgetr()
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL) {
+	    iferr (value = imgetr (im, NAME(sym))) {
+		ip = 1
+		if (ctor (DEFAULT(sym), ip, value) == 0)
+		    call error (0, "HDMGETR: No value found")
+	    }
+	} else
+	    value = imgetr (im, parameter)
+
+	return (value)
+end
+
+
+# HDMGETI -- Get an integer valued parameter.  Return default value if not in
+# the image header.  Return error condition if no default or image value.
+
+int procedure hdmgeti (im, parameter)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+
+int	ip, ctoi()
+int	value, imgeti()
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL) {
+	    iferr (value = imgeti (im, NAME(sym))) {
+		ip = 1
+		if (ctoi (DEFAULT(sym), ip, value) == 0)
+		    call error (0, "HDMGETI: No value found")
+	    }
+	} else
+	    value = imgeti (im, parameter)
+
+	return (value)
+end
+
+
+# HDMPSTR -- Put a string valued parameter in the image header.
+
+procedure hdmpstr (im, parameter, str)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+char	str[ARB]		# String value
+
+int	imaccf(), imgftype()
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL) {
+	    if (imaccf (im, NAME(sym)) == YES)
+	        if (imgftype (im, NAME(sym)) != TY_CHAR)
+		    call imdelf (im, NAME(sym))
+	    call imastr (im, NAME(sym), str)
+	} else {
+	    if (imaccf (im, parameter) == YES)
+	        if (imgftype (im, parameter) != TY_CHAR)
+		    call imdelf (im, parameter)
+	    call imastr (im, parameter, str)
+	}
+end
+
+
+# HDMPUTI -- Put an integer valued parameter in the image header.
+
+procedure hdmputi (im, parameter, value)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+int	value			# Integer value to put
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call imaddi (im, NAME(sym), value)
+	else
+	    call imaddi (im, parameter, value)
+end
+
+
+# HDMPUTR -- Put a real valued parameter in the image header.
+
+procedure hdmputr (im, parameter, value)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+real	value			# Real value to put
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call imaddr (im, NAME(sym), value)
+	else
+	    call imaddr (im, parameter, value)
+end
+
+
+# HDMGSTP -- Get the symbol table pointer to save a translation map.
+# The symbol table is restored with HDMPSTP.
+
+procedure hdmgstp (ptr)
+
+pointer	ptr		# Symbol table pointer to return
+
+include	"hdrmap.com"
+
+begin
+	ptr = stp
+end
+
+
+# HDMPSTP -- Put a symbol table pointer to restore a header map.
+# The symbol table is optained with HDMGSTP.
+
+procedure hdmpstp (ptr)
+
+pointer	ptr		# Symbol table pointer to restore
+
+include	"hdrmap.com"
+
+begin
+	stp = ptr
+end
+
+
+# HDMDELF -- Delete a field.  It is an error if the field does not exist.
+
+procedure hdmdelf (im, parameter)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call imdelf (im, NAME(sym))
+	else
+	    call imdelf (im, parameter)
+end
+
+
+# HDMPARAM -- Get parameter given the image header name.
+
+procedure hdmparam (name, parameter, max_char)
+
+char	name[ARB]		# Image header name
+char	parameter[max_char]	# Parameter
+int	max_char		# Maximum size of parameter string
+
+bool	streq()
+pointer	sym, sthead(), stname(), stnext()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = sthead (stp)
+	else
+	    sym = NULL
+
+	while (sym != NULL) {
+	    if (streq (NAME(sym), name)) {
+		call strcpy (Memc[stname(stp, sym)], parameter, max_char)
+		return
+	    }
+	    sym = stnext (stp, sym)
+	}
+	call strcpy (name, parameter, max_char)
+end
diff --git a/noao/imred/ccdred/src/icaclip.gx b/noao/imred/ccdred/src/icaclip.gx
new file mode 100644
index 00000000..bb592542
--- /dev/null
+++ b/noao/imred/ccdred/src/icaclip.gx
@@ -0,0 +1,573 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		3	# Minimum number of images for this algorithm
+
+$for (sr)
+# IC_AAVSIGCLIP -- Reject pixels using an average sigma about the average
+# The average sigma is normalized by the expected poisson sigma.
+
+procedure ic_aavsigclip$t (d, m, n, scales, zeros, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	average[npts]		# Average
+$else
+PIXEL	average[npts]		# Average
+$endif
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+$if (datatype == sil)
+real	d1, low, high, sum, a, s, s1, r, one
+data	one /1.0/
+$else
+PIXEL	d1, low, high, sum, a, s, s1, r, one
+data	one /1$f/
+$endif
+pointer	sp, sums, resid, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (sums, npts, TY_REAL)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Since the unweighted average is computed here possibly skip combining
+	if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	# Compute the unweighted average with the high and low rejected and
+	# the poisson scaled average sigma.  There must be at least three
+	# pixels at each point to define the average and contributions to
+	# the mean sigma.  Corrections for differences in the image
+	# scale factors are selected by the doscale1 flag.
+
+	nin = n[1]
+	s = 0.
+	n2 = 0
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (n1 < 3)
+		next
+
+	    # Unweighted average with the high and low rejected
+	    low = Mem$t[d[1]+k]
+	    high = Mem$t[d[2]+k]
+	    if (low > high) {
+		d1 = low
+		low = high
+		high = d1
+	    }
+	    sum = 0.
+	    do j = 3, n1 {
+	       d1 = Mem$t[d[j]+k]
+	       if (d1 < low) {
+		   sum = sum + low
+		   low = d1
+		} else if (d1 > high) {
+		    sum = sum + high
+		    high = d1
+		} else
+		    sum = sum + d1
+	    }
+	    a = sum / (n1 - 2)
+	    sum = sum + low + high
+
+	    # Poisson scaled sigma accumulation
+	    if (doscale1) {
+		do j = 1, n1 {
+		    dp1 = d[j] + k
+		    mp1 = m[j] + k
+
+		    d1 = Mem$t[dp1]
+		    l = Memi[mp1]
+		    s1 = max (one, (a + zeros[l]) /  scales[l])
+		    s = s + (d1 - a) ** 2 / s1
+		}
+	    } else {
+		s1 = max (one, a)
+		do j = 1, n1
+		    s = s + (Mem$t[d[j]+k] - a) ** 2 / s1
+	    }
+	    n2 = n2 + n1
+
+	    # Save the average and sum for later.
+	    average[i] = a
+	    Memr[sums+k] = sum
+	}
+
+	# Here is the final sigma.
+	if (n2 > 1)
+	    s = sqrt (s / (n2 - 1))
+
+	# Reject pixels and compute the final average (if needed).
+	# There must be at least three pixels at each point for rejection.
+	# Iteratively scale the mean sigma and reject pixels
+	# Compact the data and keep track of the image IDs if needed.
+
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 <= max (2, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Mem$t[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Mem$t[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    a = average[i]
+	    sum = Memr[sums+k]
+
+	    repeat {
+		n2 = n1
+		if (s > 0.) {
+		    if (doscale1) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    mp1 = m[j] + k
+
+			    d1 = Mem$t[dp1]
+			    l = Memi[mp1]
+			    s1 = s * sqrt (max (one, (a+zeros[l]) /  scales[l]))
+			    r = (d1 - a) / s1
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs(r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    mp2 = m[n1] + k
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    } else {
+			s1 = s * sqrt (max (one, a))
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    d1 = Mem$t[dp1]
+			    r = (d1 - a) / s1
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs(r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[n1] + k
+					l = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = l
+				    }
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+		if (n1 > 1)
+		    a = sum / n1
+	    } until (n1 == n2 || n1 <= max (2, maxkeep))
+
+	    # If too many are rejected add some back in.
+	    # Pixels with equal residuals are added together.
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mem$t[dp1]
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Mem$t[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mem$t[dp1]
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Mem$t[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+		if (n1 > 1)
+		    a = sum / n1
+	    }
+
+	    # Save the average if needed.
+	    n[i] = n1
+	    if (!docombine) {
+		if (n1 > 0)
+		    average[i] = a
+		else
+		    average[i] = blank
+	    }
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_MAVSIGCLIP -- Reject pixels using an average sigma about the median
+# The average sigma is normalized by the expected poisson sigma.
+
+procedure ic_mavsigclip$t (d, m, n, scales, zeros, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	median[npts]		# Median
+$else
+PIXEL	median[npts]		# Median
+$endif
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+pointer	sp, resid, mp1, mp2
+$if (datatype == sil)
+real	med, low, high, r, s, s1, one
+data	one /1.0/
+$else
+PIXEL	med, low, high, r, s, s1, one
+data	one /1$f/
+$endif
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Compute the poisson scaled average sigma about the median.
+	# There must be at least three pixels at each point to define
+	# the mean sigma.  Corrections for differences in the image
+	# scale factors are selected by the doscale1 flag.
+
+	s = 0.
+	n2 = 0
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (n1 < 3) {
+		if (n1 == 0)
+		    median[i] = blank
+		else if (n1 == 1)
+		    median[i] = Mem$t[d[1]+k]
+		else {
+		    low = Mem$t[d[1]+k]
+		    high = Mem$t[d[2]+k]
+		    median[i] = (low + high) / 2.
+		}
+		next
+	    }
+
+	    # Median
+	    n3 = 1 + n1 / 2
+	    if (mod (n1, 2) == 0) {
+		low = Mem$t[d[n3-1]+k]
+		high = Mem$t[d[n3]+k]
+		med = (low + high) / 2.
+	    } else
+		med = Mem$t[d[n3]+k]
+
+	    # Poisson scaled sigma accumulation
+	    if (doscale1) {
+		do j = 1, n1 {
+		    l = Memi[m[j]+k]
+		    s1 = max (one, (med + zeros[l]) /  scales[l])
+		    s = s + (Mem$t[d[j]+k] - med) ** 2 / s1
+		}
+	    } else {
+		s1 = max (one, med)
+		do j = 1, n1
+		    s = s + (Mem$t[d[j]+k] - med) ** 2 / s1
+	    }
+	    n2 = n2 + n1
+
+	    # Save the median for later.
+	    median[i] = med
+	}
+
+	# Here is the final sigma.
+	if (n2 > 1)
+	    s = sqrt (s / (n2 - 1))
+	else
+	    return
+
+	# Compute individual sigmas and iteratively clip.
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 < max (3, maxkeep+1))
+		next
+	    nl = 1
+	    nh = n1
+	    med = median[i]
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 >= max (MINCLIP, maxkeep+1) && s > 0.) {
+		    if (doscale1) {
+			for (; nl <= n2; nl = nl + 1) {
+			    l = Memi[m[nl]+k]
+			    s1 = s * sqrt (max (one, (med+zeros[l])/scales[l]))
+			    r = (med - Mem$t[d[nl]+k]) / s1
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    l = Memi[m[nh]+k]
+			    s1 = s * sqrt (max (one, (med+zeros[l])/scales[l]))
+			    r = (Mem$t[d[nh]+k] - med) / s1
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    } else {
+			s1 = s * sqrt (max (one, med))
+			for (; nl <= n2; nl = nl + 1) {
+			    r = (med - Mem$t[d[nl]+k]) / s1
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    r = (Mem$t[d[nh]+k] - med) / s1
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    }
+
+		    # Recompute median
+		    if (n1 < n2) {
+			if (n1 > 0) {
+			    n3 = nl + n1 / 2
+			    if (mod (n1, 2) == 0) {
+				low = Mem$t[d[n3-1]+k]
+				high = Mem$t[d[n3]+k]
+				med = (low + high) / 2.
+			    } else
+				med = Mem$t[d[n3]+k]
+			} else
+			    med = blank
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    # If too many are rejected add some back in.
+	    # Pixels with equal residuals are added together.
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+
+		# Recompute median
+		if (n1 < n2) {
+		    if (n1 > 0) {
+			n3 = nl + n1 / 2
+			if (mod (n1, 2) == 0) {
+			    low = Mem$t[d[n3-1]+k]
+			    high = Mem$t[d[n3]+k]
+			    med = (low + high) / 2.
+			} else
+			    med = Mem$t[d[n3]+k]
+		    } else
+			med = blank
+		}
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mem$t[d[l]+k] = Mem$t[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mem$t[d[l]+k] = Mem$t[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median is computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/icaverage.gx b/noao/imred/ccdred/src/icaverage.gx
new file mode 100644
index 00000000..c145bb33
--- /dev/null
+++ b/noao/imred/ccdred/src/icaverage.gx
@@ -0,0 +1,93 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"../icombine.h"
+
+$for (sr)
+# IC_AVERAGE -- Compute the average image line.
+# Options include a weight average.
+
+procedure ic_average$t (d, m, n, wts, npts, average)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image ID pointers
+int	n[npts]			# Number of points
+real	wts[ARB]		# Weights
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	average[npts]		# Average (returned)
+$else
+PIXEL	average[npts]		# Average (returned)
+$endif
+
+int	i, j, k
+real	sumwt, wt
+$if (datatype == sil)
+real	sum
+$else
+PIXEL	sum
+$endif
+
+include	"../icombine.com"
+
+begin
+	# If no data has been excluded do the average without checking the
+	# number of points and using the fact that the weights are normalized.
+	# If all the data has been excluded set the average to the blank value.
+
+	if (dflag == D_ALL) {
+	    if (dowts) {
+		do i = 1, npts {
+		    k = i - 1
+		    wt = wts[Memi[m[1]+k]]
+		    sum = Mem$t[d[1]+k] * wt
+		    do j = 2, n[i] {
+			wt = wts[Memi[m[j]+k]]
+			sum = sum + Mem$t[d[j]+k] * wt
+		    }
+		    average[i] = sum
+		}
+	    } else {
+		do i = 1, npts {
+		    k = i - 1
+		    sum = Mem$t[d[1]+k]
+		    do j = 2, n[i]
+			sum = sum + Mem$t[d[j]+k]
+		    average[i] = sum / n[i]
+		}
+	    }
+	} else if (dflag == D_NONE) {
+	    do i = 1, npts
+		average[i] = blank
+	} else {
+	    if (dowts) {
+		do i = 1, npts {
+		    if (n[i] > 0) {
+			k = i - 1
+			wt = wts[Memi[m[1]+k]]
+			sum = Mem$t[d[1]+k] * wt
+			sumwt = wt
+			do j = 2, n[i] {
+			    wt = wts[Memi[m[j]+k]]
+			    sum = sum + Mem$t[d[j]+k] * wt
+			    sumwt = sumwt + wt
+			}
+			average[i] = sum / sumwt
+		    } else
+			average[i] = blank
+		}
+	    } else {
+		do i = 1, npts {
+		    if (n[i] > 0) {
+			k = i - 1
+			sum = Mem$t[d[1]+k]
+			do j = 2, n[i]
+			    sum = sum + Mem$t[d[j]+k]
+			average[i] = sum / n[i]
+		    } else
+			average[i] = blank
+		}
+	    }
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/iccclip.gx b/noao/imred/ccdred/src/iccclip.gx
new file mode 100644
index 00000000..69df984c
--- /dev/null
+++ b/noao/imred/ccdred/src/iccclip.gx
@@ -0,0 +1,471 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		2	# Mininum number of images for algorithm
+
+$for (sr)
+# IC_ACCDCLIP -- Reject pixels using CCD noise parameters about the average
+
+procedure ic_accdclip$t (d, m, n, scales, zeros, nm, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+real	nm[3,nimages]		# Noise model parameters
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	average[npts]		# Average
+$else
+PIXEL	average[npts]		# Average
+$endif
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+$if (datatype == sil)
+real	d1, low, high, sum, a, s, r, zero
+data	zero /0.0/
+$else
+PIXEL	d1, low, high, sum, a, s, r, zero
+data	zero /0$f/
+$endif
+pointer	sp, resid, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are no pixels go on to the combining.  Since the unweighted
+	# average is computed here possibly skip the combining later.
+
+	# There must be at least max (1, nkeep) pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	} else if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# There must be at least two pixels for rejection.  The initial
+	# average is the low/high rejected average except in the case of
+	# just two pixels.  The rejections are iterated and the average
+	# is recomputed.  Corrections for scaling may be performed.
+	# Depending on other flags the image IDs may also need to be adjusted.
+
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    if (n1 <= max (MINCLIP-1, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Mem$t[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Mem$t[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    repeat {
+		if (n1 == 2) {
+		    sum = Mem$t[d[1]+k]
+		    sum = sum + Mem$t[d[2]+k]
+		    a = sum / 2
+		} else {
+		    low = Mem$t[d[1]+k]
+		    high = Mem$t[d[2]+k]
+		    if (low > high) {
+			d1 = low
+			low = high
+			high = d1
+		    }
+		    sum = 0.
+		    do j = 3, n1 {
+		       d1 = Mem$t[d[j]+k]
+		       if (d1 < low) {
+			   sum = sum + low
+			   low = d1
+			} else if (d1 > high) {
+			    sum = sum + high
+			    high = d1
+			} else
+			    sum = sum + d1
+		    }
+		    a = sum / (n1 - 2)
+		    sum = sum + low + high
+		}
+		n2 = n1
+		if (doscale1) {
+		    for (j=1; j<=n1; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+
+			l = Memi[mp1]
+			s = scales[l]
+			d1 = max (zero, s * (a + zeros[l]))
+			s = sqrt (nm[1,l] + d1/nm[2,l] + (d1*nm[3,l])**2) / s
+
+			d1 = Mem$t[dp1]
+			r = (d1 - a) / s
+			if (r < -lsigma || r > hsigma) {
+			    Memr[resid+n1] = abs(r)
+			    if (j < n1) {
+				dp2 = d[n1] + k
+				Mem$t[dp1] = Mem$t[dp2]
+				Mem$t[dp2] = d1
+				mp2 = m[n1] + k
+				Memi[mp1] = Memi[mp2]
+				Memi[mp2] = l
+				j = j - 1
+			    }
+			    sum = sum - d1
+			    n1 = n1 - 1
+			}
+		    }
+		} else {
+		    if (!keepids) {
+			s = max (zero, a)
+			s = sqrt (nm[1,1] + s/nm[2,1] + (s*nm[3,1])**2)
+		    }
+		    for (j=1; j<=n1; j=j+1) {
+			if (keepids) {
+			    l = Memi[m[j]+k]
+			    s = max (zero, a)
+			    s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			}
+			dp1 = d[j] + k
+			d1 = Mem$t[dp1]
+			r = (d1 - a) / s
+			if (r < -lsigma || r > hsigma) {
+			    Memr[resid+n1] = abs(r)
+			    if (j < n1) {
+				dp2 = d[n1] + k
+				Mem$t[dp1] = Mem$t[dp2]
+				Mem$t[dp2] = d1
+				if (keepids) {
+				    mp1 = m[j] + k
+				    mp2 = m[n1] + k
+				    l = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				}
+				j = j - 1
+			    }
+			    sum = sum - d1
+			    n1 = n1 - 1
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mem$t[dp1]
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Mem$t[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mem$t[dp1]
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Mem$t[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+	    }
+
+	    n[i] = n1
+	    if (!docombine)
+		if (n1 > 0)
+		    average[i] = sum / n1
+		else
+		    average[i] = blank
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_CCDCLIP -- Reject pixels using CCD noise parameters about the median
+
+procedure ic_mccdclip$t (d, m, n, scales, zeros, nm, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+real	nm[3,nimages]		# Noise model
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	median[npts]		# Median
+$else
+PIXEL	median[npts]		# Median
+$endif
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+real	r, s
+pointer	sp, resid, mp1, mp2
+$if (datatype == sil)
+real	med, zero
+data	zero /0.0/
+$else
+PIXEL	med, zero
+data	zero /0$f/
+$endif
+
+include	"../icombine.com"
+
+begin
+	# There must be at least max (MINCLIP, nkeep+1) pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Compute median and sigma and iteratively clip.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    nl = 1
+	    nh = n1
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 == 0)
+		    med = blank
+		else if (mod (n1, 2) == 0) {
+		    med = Mem$t[d[n3-1]+k]
+		    med = (med + Mem$t[d[n3]+k]) / 2.
+		} else
+		    med = Mem$t[d[n3]+k]
+
+		if (n1 >= max (MINCLIP, maxkeep+1)) {
+		    if (doscale1) {
+			for (; nl <= n2; nl = nl + 1) {
+			    l = Memi[m[nl]+k]
+			    s = scales[l]
+			    r = max (zero, s * (med + zeros[l]))
+			    s = sqrt (nm[1,l] + r/nm[2,l] + (r*nm[3,l])**2) / s
+			    r = (med - Mem$t[d[nl]+k]) / s
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    l = Memi[m[nh]+k]
+			    s = scales[l]
+			    r = max (zero, s * (med + zeros[l]))
+			    s = sqrt (nm[1,l] + r/nm[2,l] + (r*nm[3,l])**2) / s
+			    r = (Mem$t[d[nh]+k] - med) / s
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    } else {
+			if (!keepids) {
+			    s = max (zero, med)
+			    s = sqrt (nm[1,1] + s/nm[2,1] + (s*nm[3,1])**2)
+			}
+			for (; nl <= n2; nl = nl + 1) {
+			    if (keepids) {
+				l = Memi[m[nl]+k]
+				s = max (zero, med)
+				s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			    }
+			    r = (med - Mem$t[d[nl]+k]) / s
+			    if (r <= lsigma)
+				break
+			    Memr[resid+nl] = r
+			    n1 = n1 - 1
+			}
+			for (; nh >= nl; nh = nh - 1) {
+			    if (keepids) {
+				l = Memi[m[nh]+k]
+				s = max (zero, med)
+				s = sqrt (nm[1,l] + s/nm[2,l] + (s*nm[3,l])**2)
+			    }
+			    r = (Mem$t[d[nh]+k] -  med) / s
+			    if (r <= hsigma)
+				break
+			    Memr[resid+nh] = r
+			    n1 = n1 - 1
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mem$t[d[l]+k] = Mem$t[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mem$t[d[l]+k] = Mem$t[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median is computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/icgdata.gx b/noao/imred/ccdred/src/icgdata.gx
new file mode 100644
index 00000000..41cf5810
--- /dev/null
+++ b/noao/imred/ccdred/src/icgdata.gx
@@ -0,0 +1,233 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	<mach.h>
+include	"../icombine.h"
+
+$for (sr)
+# IC_GDATA -- Get line of image and mask data and apply threshold and scaling.
+# Entirely empty lines are excluded.  The data are compacted within the
+# input data buffers.  If it is required, the connection to the original
+# image index is keeped in the returned m data pointers.
+
+procedure ic_gdata$t (in, out, dbuf, d, id, n, m, lflag, offsets, scales,
+	zeros, nimages, npts, v1, v2)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+pointer	dbuf[nimages]		# Data buffers for nonaligned images
+pointer	d[nimages]		# Data pointers
+pointer	id[nimages]		# ID pointers
+int	n[npts]			# Number of good pixels
+pointer	m[nimages]		# Mask pointers
+int	lflag[nimages]		# Empty mask flags
+int	offsets[nimages,ARB]	# Image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero offset factors
+int	nimages			# Number of input images
+int	npts			# NUmber of output points per line
+long	v1[ARB], v2[ARB]	# Line vectors
+
+int	i, j, k, l, ndim, nused
+real	a, b
+pointer	buf, dp, ip, mp, imgnl$t()
+
+include	"../icombine.com"
+
+begin
+	# Get masks and return if there is no data
+	call ic_mget (in, out, offsets, v1, v2, m, lflag, nimages)
+	if (dflag == D_NONE)
+	    return
+
+	# Get data and fill data buffers.  Correct for offsets if needed.
+	ndim = IM_NDIM(out[1])
+	do i = 1, nimages {
+	    if (lflag[i] == D_NONE)
+		next
+	    if (aligned) {
+		call amovl (v1, v2, IM_MAXDIM)
+		if (project)
+		    v2[ndim+1] = i
+		j = imgnl$t (in[i], d[i], v2)
+	    } else {
+		v2[1] = v1[1]
+		do j = 2, ndim
+		    v2[j] = v1[j] - offsets[i,j]
+		if (project)
+		    v2[ndim+1] = i
+		j = imgnl$t (in[i], buf, v2)
+		call amov$t (Mem$t[buf], Mem$t[dbuf[i]+offsets[i,1]],
+		    IM_LEN(in[i],1))
+		d[i] = dbuf[i]
+	    }
+	}
+
+	# Apply threshold if needed
+	if (dothresh) {
+	    do i = 1, nimages {
+		dp = d[i]
+		if (lflag[i] == D_ALL) {
+		    do j = 1, npts {
+			a = Mem$t[dp]
+			if (a < lthresh || a > hthresh) {
+			    Memi[m[i]+j-1] = 1
+			    lflag[i] = D_MIX
+			    dflag = D_MIX
+			}
+			dp = dp + 1
+		    }
+		} else if (lflag[i] == D_MIX) {
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    a = Mem$t[dp]
+			    if (a < lthresh || a > hthresh) {
+				Memi[m[i]+j-1] = 1
+				dflag = D_MIX
+			    }
+			}
+			dp = dp + 1
+			mp = mp + 1
+		    }
+		}
+
+		# Check for completely empty lines
+		if (lflag[i] == D_MIX) {
+		    lflag[i] = D_NONE
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    lflag[i] = D_MIX
+			    break
+			}
+			mp = mp + 1
+		    }
+		}
+	    }
+	}
+
+	# Apply scaling (avoiding masked pixels which might overflow?)
+	if (doscale) {
+	    if (dflag == D_ALL) {
+		do i = 1, nimages {
+		    dp = d[i]
+		    a = scales[i]
+		    b = -zeros[i]
+		    do j = 1, npts {
+			Mem$t[dp] = Mem$t[dp] / a + b
+			dp = dp + 1
+		    }
+		}
+	    } else if (dflag == D_MIX) {
+		do i = 1, nimages {
+		    dp = d[i]
+		    a = scales[i]
+		    b = -zeros[i]
+		    if (lflag[i] == D_ALL) {
+			do j = 1, npts {
+			    Mem$t[dp] = Mem$t[dp] / a + b
+			    dp = dp + 1
+			}
+		    } else if (lflag[i] == D_MIX) {
+			mp = m[i]
+			do j = 1, npts {
+			    if (Memi[mp] == 0)
+				Mem$t[dp] = Mem$t[dp] / a + b
+			    dp = dp + 1
+			    mp = mp + 1
+			}
+		    }
+		}
+	    }
+	}
+
+	# Sort pointers to exclude unused images.
+	# Use the lflag array to keep track of the image index.
+
+	if (dflag == D_ALL)
+	    nused = nimages
+	else {
+	    nused = 0
+	    do i = 1, nimages
+		if (lflag[i] != D_NONE) {
+		    nused = nused + 1
+		    d[nused] = d[i]
+		    m[nused] = m[i]
+		    lflag[nused] = i
+		}
+	    if (nused == 0)
+		dflag = D_NONE
+	}
+
+	# Compact data to remove bad pixels
+	# Keep track of the image indices if needed
+	# If growing mark the end of the included image indices with zero
+
+	if (dflag == D_ALL) {
+	    call amovki (nused, n, npts)
+	    if (keepids)
+		do i = 1, nimages
+		    call amovki (i, Memi[id[i]], npts)
+	} else if (dflag == D_NONE)
+	    call aclri (n, npts)
+	else {
+	    call aclri (n, npts)
+	    if (keepids) {
+		do i = 1, nused {
+		    l = lflag[i]
+		    dp = d[i]
+		    ip = id[i]
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    n[j] = n[j] + 1
+			    k = n[j]
+			    if (k < i) {
+				Mem$t[d[k]+j-1] = Mem$t[dp]
+				Memi[id[k]+j-1] = l
+			    } else
+				Memi[ip] = l
+			}
+			dp = dp + 1
+			ip = ip + 1
+			mp = mp + 1
+		    }
+		}
+		if (grow > 0) {
+		    do j = 1, npts {
+			do i = n[j]+1, nimages
+			    Memi[id[i]+j-1] = 0
+		    }
+		}
+	    } else {
+		do i = 1, nused {
+		    dp = d[i]
+		    mp = m[i]
+		    do j = 1, npts {
+			if (Memi[mp] == 0) {
+			    n[j] = n[j] + 1
+			    k = n[j]
+			    if (k < i)
+				Mem$t[d[k]+j-1] = Mem$t[dp]
+			}
+			dp = dp + 1
+			mp = mp + 1
+		    }
+		}
+	    }
+	}
+
+	# Sort the pixels and IDs if needed
+	if (mclip) {
+	    call malloc (dp, nimages, TY_PIXEL)
+	    if (keepids) {
+		call malloc (ip, nimages, TY_INT)
+		call ic_2sort$t (d, Mem$t[dp], id, Memi[ip], n, npts)
+		call mfree (ip, TY_INT)
+	    } else
+		call ic_sort$t (d, Mem$t[dp], n, npts)
+	    call mfree (dp, TY_PIXEL)
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/icgrow.gx b/noao/imred/ccdred/src/icgrow.gx
new file mode 100644
index 00000000..e3cf6228
--- /dev/null
+++ b/noao/imred/ccdred/src/icgrow.gx
@@ -0,0 +1,81 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+$for (sr)
+# IC_GROW --  Reject neigbors of rejected pixels.
+# The rejected pixels are marked by having nonzero ids beyond the number
+# of included pixels.  The pixels rejected here are given zero ids
+# to avoid growing of the pixels rejected here.  The unweighted average
+# can be updated but any rejected pixels requires the median to be
+# recomputed.  When the number of pixels at a grow point reaches nkeep 
+# no further pixels are rejected.  Note that the rejection order is not
+# based on the magnitude of the residuals and so a grow from a weakly
+# rejected image pixel may take precedence over a grow from a strongly
+# rejected image pixel.
+
+procedure ic_grow$t (d, m, n, nimages, npts, average)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image id pointers
+int	n[npts]			# Number of good pixels
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	average[npts]		# Average
+$else
+PIXEL	average[npts]		# Average
+$endif
+
+int	i1, i2, j1, j2, k1, k2, l, is, ie, n2, maxkeep
+pointer	mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_NONE)
+	    return
+
+	do i1 = 1, npts {
+	    k1 = i1 - 1
+	    is = max (1, i1 - grow)
+	    ie = min (npts, i1 + grow)
+	    do j1 = n[i1]+1, nimages {
+		l = Memi[m[j1]+k1]
+		if (l == 0)
+		    next
+		if (combine == MEDIAN)
+		    docombine = true
+
+		do i2 = is, ie {
+		    if (i2 == i1)
+			next
+		    k2 = i2 - 1
+		    n2 = n[i2]
+		    if (nkeep < 0)
+			maxkeep = max (0, n2 + nkeep)
+		    else
+			maxkeep = min (n2, nkeep)
+		    if (n2 <= maxkeep)
+			next
+		    do j2 = 1, n2 {
+			mp1 = m[j2] + k2
+			if (Memi[mp1] == l) {
+			    if (!docombine && n2 > 1)
+				average[i2] =
+				    (n2*average[i2] - Mem$t[d[j2]+k2]) / (n2-1)
+			    mp2 = m[n2] + k2
+			    if (j2 < n2) {
+				Mem$t[d[j2]+k2] = Mem$t[d[n2]+k2]
+				Memi[mp1] = Memi[mp2]
+			    }
+			    Memi[mp2] = 0
+			    n[i2] = n2 - 1
+			    break
+			}
+		    }
+		}
+	    }
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/icimstack.x b/noao/imred/ccdred/src/icimstack.x
new file mode 100644
index 00000000..2a19751d
--- /dev/null
+++ b/noao/imred/ccdred/src/icimstack.x
@@ -0,0 +1,125 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<error.h>
+include	<imhdr.h>
+
+
+# IC_IMSTACK -- Stack images into a single image of higher dimension.
+
+procedure ic_imstack (images, nimages, output)
+
+char	images[SZ_FNAME-1, nimages]	#I Input images
+int	nimages				#I Number of images
+char	output				#I Name of output image
+
+int	i, j, npix
+long	line_in[IM_MAXDIM], line_out[IM_MAXDIM]
+pointer	sp, key, in, out, buf_in, buf_out, ptr
+
+int	imgnls(), imgnli(), imgnll(), imgnlr(), imgnld(), imgnlx()
+int	impnls(), impnli(), impnll(), impnlr(), impnld(), impnlx()
+pointer	immap()
+errchk	immap
+
+begin
+	call smark (sp)
+	call salloc (key, SZ_FNAME, TY_CHAR)
+
+	iferr {
+	    # Add each input image to the output image.
+	    out = NULL
+	    do i = 1, nimages {
+		in = NULL
+		ptr = immap (images[1,i], READ_ONLY, 0)
+		in = ptr
+
+		# For the first input image map the output image as a copy
+		# and increment the dimension.  Set the output line counter.
+
+		if (i == 1) {
+		    ptr = immap (output, NEW_COPY, in)
+		    out = ptr
+		    IM_NDIM(out) = IM_NDIM(out) + 1
+		    IM_LEN(out, IM_NDIM(out)) = nimages
+		    npix = IM_LEN(out, 1)
+		    call amovkl (long(1), line_out, IM_MAXDIM)
+		}
+
+		# Check next input image for consistency with the output image.
+		if (IM_NDIM(in) != IM_NDIM(out) - 1)
+		    call error (0, "Input images not consistent")
+		do j = 1, IM_NDIM(in) {
+		    if (IM_LEN(in, j) != IM_LEN(out, j))
+			call error (0, "Input images not consistent")
+		}
+
+		call sprintf (Memc[key], SZ_FNAME, "stck%04d")
+		    call pargi (i)
+		call imastr (out, Memc[key], images[1,i])
+
+		# Copy the input lines from the image to the next lines of
+		# the output image.  Switch on the output data type to optimize
+		# IMIO.
+
+		call amovkl (long(1), line_in, IM_MAXDIM)
+		switch (IM_PIXTYPE (out)) {
+		case TY_SHORT:
+		    while (imgnls (in, buf_in, line_in) != EOF) {
+			if (impnls (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovs (Mems[buf_in], Mems[buf_out], npix)
+		    }
+		case TY_INT:
+		    while (imgnli (in, buf_in, line_in) != EOF) {
+			if (impnli (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovi (Memi[buf_in], Memi[buf_out], npix)
+		    }
+		case TY_USHORT, TY_LONG:
+		    while (imgnll (in, buf_in, line_in) != EOF) {
+			if (impnll (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovl (Meml[buf_in], Meml[buf_out], npix)
+		    }
+		case TY_REAL:
+		    while (imgnlr (in, buf_in, line_in) != EOF) {
+			if (impnlr (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovr (Memr[buf_in], Memr[buf_out], npix)
+		    }
+		case TY_DOUBLE:
+		    while (imgnld (in, buf_in, line_in) != EOF) {
+			if (impnld (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovd (Memd[buf_in], Memd[buf_out], npix)
+		    }
+		case TY_COMPLEX:
+		    while (imgnlx (in, buf_in, line_in) != EOF) {
+			if (impnlx (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovx (Memx[buf_in], Memx[buf_out], npix)
+		    }
+		default:
+		    while (imgnlr (in, buf_in, line_in) != EOF) {
+			if (impnlr (out, buf_out, line_out) == EOF)
+			    call error (0, "Error writing output image")
+			call amovr (Memr[buf_in], Memr[buf_out], npix)
+		    }
+		}
+		call imunmap (in)
+	    }
+	} then {
+	    if (out != NULL) {
+		call imunmap (out)
+		call imdelete (out)
+	    }
+	    if (in != NULL)
+		call imunmap (in)
+	    call sfree (sp)
+	    call erract (EA_ERROR)
+	}
+
+	# Finish up.
+	call imunmap (out)
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/iclog.x b/noao/imred/ccdred/src/iclog.x
new file mode 100644
index 00000000..82135866
--- /dev/null
+++ b/noao/imred/ccdred/src/iclog.x
@@ -0,0 +1,378 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	<imset.h>
+include	<mach.h>
+include	"icombine.h"
+include	"icmask.h"
+
+# IC_LOG -- Output log information is a log file has been specfied.
+
+procedure ic_log (in, out, ncombine, exptime, sname, zname, wname,
+	mode, median, mean, scales, zeros, wts, offsets, nimages,
+	dozero, nout, expname, exposure)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+int	ncombine[nimages]	# Number of previous combined images
+real	exptime[nimages]	# Exposure times
+char	sname[ARB]		# Scale name
+char	zname[ARB]		# Zero name
+char	wname[ARB]		# Weight name
+real	mode[nimages]		# Modes
+real	median[nimages]		# Medians
+real	mean[nimages]		# Means
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero or sky levels
+real	wts[nimages]		# Weights
+int	offsets[nimages,ARB]	# Image offsets
+int	nimages			# Number of images
+bool	dozero			# Zero flag
+int	nout			# Number of images combined in output
+char	expname[ARB]		# Exposure name
+real	exposure		# Output exposure
+
+int	i, j, stack, ctor()
+real	rval, imgetr()
+long	clktime()
+bool	prncombine, prexptime, prmode, prmedian, prmean, prmask
+bool	prrdn, prgain, prsn
+pointer	sp, fname, key
+errchk	imgetr
+
+include	"icombine.com"
+
+begin
+	if (logfd == NULL)
+	    return
+
+	call smark (sp)
+	call salloc (fname, SZ_LINE, TY_CHAR)
+
+	stack = NO
+	if (project) {
+	    ifnoerr (call imgstr (in[1], "stck0001", Memc[fname], SZ_LINE))
+	        stack = YES
+	}
+	if (stack == YES)
+	    call salloc (key, SZ_FNAME, TY_CHAR)
+
+	# Time stamp the log and print parameter information.
+
+	call cnvdate (clktime(0), Memc[fname], SZ_LINE)
+	call fprintf (logfd, "\n%s: IMCOMBINE\n")
+	    call pargstr (Memc[fname])
+	switch (combine) {
+	case  AVERAGE:
+	    call fprintf (logfd, "  combine = average, ")
+	case  MEDIAN:
+	    call fprintf (logfd, "  combine = median, ")
+	}
+	call fprintf (logfd, "scale = %s, zero = %s, weight = %s\n")
+	    call pargstr (sname)
+	    call pargstr (zname)
+	    call pargstr (wname)
+
+	switch (reject) {
+	case MINMAX:
+	    call fprintf (logfd, "  reject = minmax, nlow = %d, nhigh = %d\n")
+		call pargi (nint (flow * nimages))
+		call pargi (nint (fhigh * nimages))
+	case CCDCLIP:
+	    call fprintf (logfd, "  reject = ccdclip, mclip = %b, nkeep = %d\n")
+		call pargb (mclip)
+		call pargi (nkeep)
+	    call fprintf (logfd,
+	    "  rdnoise = %s, gain = %s, snoise = %s, sigma = %g, hsigma = %g\n")
+		call pargstr (Memc[rdnoise])
+		call pargstr (Memc[gain])
+		call pargstr (Memc[snoise])
+		call pargr (lsigma)
+		call pargr (hsigma)
+	case CRREJECT:
+	    call fprintf (logfd,
+		"  reject = crreject, mclip = %b, nkeep = %d\n")
+		call pargb (mclip)
+		call pargi (nkeep)
+	    call fprintf (logfd,
+		"  rdnoise = %s, gain = %s, snoise = %s, hsigma = %g\n")
+		call pargstr (Memc[rdnoise])
+		call pargstr (Memc[gain])
+		call pargstr (Memc[snoise])
+		call pargr (hsigma)
+	case PCLIP:
+	    call fprintf (logfd, "  reject = pclip, nkeep = %d\n")
+		call pargi (nkeep)
+	    call fprintf (logfd, "  pclip = %g, lsigma = %g, hsigma = %g\n")
+		call pargr (pclip)
+		call pargr (lsigma)
+		call pargr (hsigma)
+	case SIGCLIP:
+	    call fprintf (logfd, "  reject = sigclip, mclip = %b, nkeep = %d\n")
+		call pargb (mclip)
+		call pargi (nkeep)
+	    call fprintf (logfd, "  lsigma = %g, hsigma = %g\n")
+		call pargr (lsigma)
+		call pargr (hsigma)
+	case AVSIGCLIP:
+	    call fprintf (logfd,
+		"  reject = avsigclip, mclip = %b, nkeep = %d\n")
+		call pargb (mclip)
+		call pargi (nkeep)
+	    call fprintf (logfd, "  lsigma = %g, hsigma = %g\n")
+		call pargr (lsigma)
+		call pargr (hsigma)
+	}
+	if (reject != NONE && grow > 0) {
+	    call fprintf (logfd, "  grow = %d\n")
+		call pargi (grow)
+	}
+	if (dothresh) {
+	    if (lthresh > -MAX_REAL && hthresh < MAX_REAL) {
+		call fprintf (logfd, "  lthreshold = %g, hthreshold = %g\n")
+		    call pargr (lthresh)
+		    call pargr (hthresh)
+	    } else if (lthresh > -MAX_REAL) {
+		call fprintf (logfd, "  lthreshold = %g\n")
+		    call pargr (lthresh)
+	    } else {
+		call fprintf (logfd, "  hthreshold = %g\n")
+		    call pargr (hthresh)
+	    }
+	}
+	call fprintf (logfd, "  blank = %g\n")
+	    call pargr (blank)
+	call clgstr ("statsec", Memc[fname], SZ_LINE)
+	if (Memc[fname] != EOS) {
+	    call fprintf (logfd, "  statsec = %s\n")
+		call pargstr (Memc[fname])
+	}
+
+	if (ICM_TYPE(icm) != M_NONE) {
+	    switch (ICM_TYPE(icm)) {
+	    case M_BOOLEAN, M_GOODVAL:
+		call fprintf (logfd, "  masktype = goodval, maskval = %d\n")
+		    call pargi (ICM_VALUE(icm))
+	    case M_BADVAL:
+		call fprintf (logfd, "  masktype = badval, maskval = %d\n")
+		    call pargi (ICM_VALUE(icm))
+	    case M_GOODBITS:
+		call fprintf (logfd, "  masktype = goodbits, maskval = %d\n")
+		    call pargi (ICM_VALUE(icm))
+	    case M_BADBITS:
+		call fprintf (logfd, "  masktype = badbits, maskval = %d\n")
+		    call pargi (ICM_VALUE(icm))
+	    }
+	}
+
+	# Print information pertaining to individual images as a set of
+	# columns with the image name being the first column.  Determine
+	# what information is relevant and print the appropriate header.
+
+	prncombine = false
+	prexptime = false
+	prmode = false
+	prmedian = false
+	prmean = false
+	prmask = false
+	prrdn = false
+	prgain = false
+	prsn = false
+	do i = 1, nimages {
+	    if (ncombine[i] != ncombine[1])
+		prncombine = true
+	    if (exptime[i] != exptime[1])
+		prexptime = true
+	    if (mode[i] != mode[1])
+		prmode = true
+	    if (median[i] != median[1])
+		prmedian = true
+	    if (mean[i] != mean[1])
+		prmean = true
+	    if (ICM_TYPE(icm) != M_NONE && Memi[ICM_PMS(icm)+i-1] != NULL)
+		prmask = true
+	    if (reject == CCDCLIP || reject == CRREJECT) {
+		j = 1
+		if (ctor (Memc[rdnoise], j, rval) == 0)
+		    prrdn = true
+		j = 1
+		if (ctor (Memc[gain], j, rval) == 0)
+		    prgain = true
+		j = 1
+		if (ctor (Memc[snoise], j, rval) == 0)
+		    prsn = true
+	    }
+	}
+
+	call fprintf (logfd, "  %20s ")
+	    call pargstr ("Images")
+	if (prncombine) {
+	    call fprintf (logfd, " %6s")
+		call pargstr ("N")
+	}
+	if (prexptime) {
+	    call fprintf (logfd, " %6s")
+		call pargstr ("Exp")
+	}
+	if (prmode) {
+	    call fprintf (logfd, " %7s")
+		call pargstr ("Mode")
+	}
+	if (prmedian) {
+	    call fprintf (logfd, " %7s")
+		call pargstr ("Median")
+	}
+	if (prmean) {
+	    call fprintf (logfd, " %7s")
+		call pargstr ("Mean")
+	}
+	if (prrdn) {
+	    call fprintf (logfd, " %7s")
+		call pargstr ("Rdnoise")
+	}
+	if (prgain) {
+	    call fprintf (logfd, " %6s")
+		call pargstr ("Gain")
+	}
+	if (prsn) {
+	    call fprintf (logfd, " %6s")
+		call pargstr ("Snoise")
+	}
+	if (doscale) {
+	    call fprintf (logfd, " %6s")
+		call pargstr ("Scale")
+	}
+	if (dozero) {
+	    call fprintf (logfd, " %7s")
+		call pargstr ("Zero")
+	}
+	if (dowts) {
+	    call fprintf (logfd, " %6s")
+		call pargstr ("Weight")
+	}
+	if (!aligned) {
+	    call fprintf (logfd, " %9s")
+		call pargstr ("Offsets")
+	}
+	if (prmask) {
+	    call fprintf (logfd, " %s")
+		call pargstr ("Maskfile")
+	}
+	call fprintf (logfd, "\n")
+
+	do i = 1, nimages {
+	    if (stack == YES) {
+		call sprintf (Memc[key], SZ_FNAME, "stck%04d")
+		    call pargi (i)
+		ifnoerr (call imgstr (in[i], Memc[key], Memc[fname], SZ_LINE)) {
+		    call fprintf (logfd, "  %21s")
+			call pargstr (Memc[fname])
+		} else {
+		    call imstats (in[i], IM_IMAGENAME, Memc[fname], SZ_LINE)
+		    call fprintf (logfd, "  %16s[%3d]")
+			call pargstr (Memc[fname])
+			call pargi (i)
+		}
+	    } else if (project) {
+		call imstats (in[i], IM_IMAGENAME, Memc[fname], SZ_LINE)
+		call fprintf (logfd, "  %16s[%3d]")
+		    call pargstr (Memc[fname])
+		    call pargi (i)
+	    } else  {
+		call imstats (in[i], IM_IMAGENAME, Memc[fname], SZ_LINE)
+		call fprintf (logfd, "  %21s")
+		    call pargstr (Memc[fname])
+	    }
+	    if (prncombine) {
+		call fprintf (logfd, " %6d")
+		    call pargi (ncombine[i])
+	    }
+	    if (prexptime) {
+		call fprintf (logfd, " %6.1f")
+		    call pargr (exptime[i])
+	    }
+	    if (prmode) {
+		call fprintf (logfd, " %7.5g")
+		    call pargr (mode[i])
+	    }
+	    if (prmedian) {
+		call fprintf (logfd, " %7.5g")
+		    call pargr (median[i])
+	    }
+	    if (prmean) {
+		call fprintf (logfd, " %7.5g")
+		    call pargr (mean[i])
+	    }
+	    if (prrdn) {
+		rval = imgetr (in[i], Memc[rdnoise])
+		call fprintf (logfd, " %7g")
+		    call pargr (rval)
+	    }
+	    if (prgain) {
+		rval = imgetr (in[i], Memc[gain])
+		call fprintf (logfd, " %6g")
+		    call pargr (rval)
+	    }
+	    if (prsn) {
+		rval = imgetr (in[i], Memc[snoise])
+		call fprintf (logfd, " %6g")
+		    call pargr (rval)
+	    }
+	    if (doscale) {
+		call fprintf (logfd, " %6.3f")
+		    call pargr (1./scales[i])
+	    }
+	    if (dozero) {
+		call fprintf (logfd, " %7.5g")
+		    call pargr (-zeros[i])
+	    }
+	    if (dowts) {
+		call fprintf (logfd, " %6.3f")
+		    call pargr (wts[i])
+	    }
+	    if (!aligned) {
+		if (IM_NDIM(out[1]) == 1) {
+		    call fprintf (logfd, " %9d")
+			call pargi (offsets[i,1])
+		} else {
+		    do  j = 1, IM_NDIM(out[1]) {
+			call fprintf (logfd, " %4d")
+			    call pargi (offsets[i,j])
+		    }
+		}
+	    }
+	    if (prmask && Memi[ICM_PMS(icm)+i-1] != NULL) {
+		call imgstr (in[i], "BPM", Memc[fname], SZ_LINE)
+		call fprintf (logfd, " %s")
+		    call pargstr (Memc[fname])
+	    }
+	    call fprintf (logfd, "\n")
+	}
+
+	# Log information about the output images.
+ 	call imstats (out[1], IM_IMAGENAME, Memc[fname], SZ_LINE)
+	call fprintf (logfd, "\n  Output image = %s, ncombine = %d")
+	    call pargstr (Memc[fname])
+	    call pargi (nout)
+	if (expname[1] != EOS) {
+	    call fprintf (logfd, ", %s = %g")
+		call pargstr (expname)
+		call pargr (exposure)
+	}
+	call fprintf (logfd, "\n")
+
+	if (out[2] != NULL) {
+	    call imstats (out[2], IM_IMAGENAME, Memc[fname], SZ_LINE)
+	    call fprintf (logfd, "  Pixel list image = %s\n")
+		call pargstr (Memc[fname])
+	}
+
+	if (out[3] != NULL) {
+	    call imstats (out[3], IM_IMAGENAME, Memc[fname], SZ_LINE)
+	    call fprintf (logfd, "  Sigma image = %s\n")
+		call pargstr (Memc[fname])
+	}
+
+	call flush (logfd)
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/icmask.com b/noao/imred/ccdred/src/icmask.com
new file mode 100644
index 00000000..baba6f6a
--- /dev/null
+++ b/noao/imred/ccdred/src/icmask.com
@@ -0,0 +1,8 @@
+# IMCMASK -- Common for IMCOMBINE mask interface.
+
+int	mtype		# Mask type
+int	mvalue		# Mask value
+pointer	bufs		# Pointer to data line buffers
+pointer	pms		# Pointer to array of PMIO pointers
+
+common	/imcmask/ mtype, mvalue, bufs, pms
diff --git a/noao/imred/ccdred/src/icmask.h b/noao/imred/ccdred/src/icmask.h
new file mode 100644
index 00000000..b2d30530
--- /dev/null
+++ b/noao/imred/ccdred/src/icmask.h
@@ -0,0 +1,7 @@
+# ICMASK -- Data structure for IMCOMBINE mask interface.
+
+define	ICM_LEN		4		# Structure length
+define	ICM_TYPE	Memi[$1]	# Mask type
+define	ICM_VALUE	Memi[$1+1]	# Mask value
+define	ICM_BUFS	Memi[$1+2]	# Pointer to data line buffers
+define	ICM_PMS		Memi[$1+3]	# Pointer to array of PMIO pointers
diff --git a/noao/imred/ccdred/src/icmask.x b/noao/imred/ccdred/src/icmask.x
new file mode 100644
index 00000000..ba448b68
--- /dev/null
+++ b/noao/imred/ccdred/src/icmask.x
@@ -0,0 +1,354 @@
+include	<imhdr.h>
+include	<pmset.h>
+include	"icombine.h"
+include	"icmask.h"
+
+# IC_MASK   -- ICOMBINE mask interface
+#
+# IC_MOPEN  -- Open masks
+# IC_MCLOSE -- Close the mask interface
+# IC_MGET   -- Get lines of mask pixels for all the images
+# IC_MGET1  -- Get a line of mask pixels for the specified image
+
+
+# IC_MOPEN -- Open masks.
+# Parse and interpret the mask selection parameters.
+
+procedure ic_mopen (in, out, nimages)
+
+pointer	in[nimages]		#I Input images
+pointer	out[ARB]		#I Output images
+int	nimages			#I Number of images
+
+int	mtype			# Mask type
+int	mvalue			# Mask value
+pointer	bufs			# Pointer to data line buffers
+pointer	pms			# Pointer to array of PMIO pointers
+
+int	i, npix, npms, clgwrd()
+real	clgetr()
+pointer	sp, fname, title, pm, pm_open()
+bool	invert, pm_empty()
+errchk	calloc, pm_open, pm_loadf
+
+include "icombine.com"
+
+begin
+	icm = NULL
+	if (IM_NDIM(out[1]) == 0)
+	    return
+
+	call smark (sp)
+	call salloc (fname, SZ_FNAME, TY_CHAR)
+	call salloc (title, SZ_FNAME, TY_CHAR)
+
+	# Determine the mask parameters and allocate memory.
+	# The mask buffers are initialize to all excluded so that
+	# output points outside the input data are always excluded
+	# and don't need to be set on a line-by-line basis.
+
+	mtype = clgwrd ("masktype", Memc[title], SZ_FNAME, MASKTYPES)
+	mvalue = clgetr ("maskvalue")
+	npix = IM_LEN(out[1],1)
+	call calloc (pms, nimages, TY_POINTER)
+	call calloc (bufs, nimages, TY_POINTER)
+	do i = 1, nimages {
+	    call malloc (Memi[bufs+i-1], npix, TY_INT)
+	    call amovki (1, Memi[Memi[bufs+i-1]], npix)
+	}
+
+	# Check for special cases.  The BOOLEAN type is used when only
+	# zero and nonzero are significant; i.e. the actual mask values are
+	# not important.  The invert flag is used to indicate that
+	# empty masks are all bad rather the all good.
+
+	if (mtype == 0)
+	    mtype = M_NONE
+	if (mtype == M_BADBITS && mvalue == 0) 
+	    mtype = M_NONE
+	if (mvalue == 0 && (mtype == M_GOODVAL || mtype == M_GOODBITS))
+	    mtype = M_BOOLEAN
+	if ((mtype == M_BADVAL && mvalue == 0) ||
+	    (mtype == M_GOODVAL && mvalue != 0) ||
+	    (mtype == M_GOODBITS && mvalue == 0))
+	    invert = true 
+	else
+	    invert = false 
+
+	# If mask images are to be used, get the mask name from the image
+	# header and open it saving the descriptor in the pms array.
+	# Empty masks (all good) are treated as if there was no mask image.
+
+	npms = 0
+	do i = 1, nimages {
+	    if (mtype != M_NONE) {
+		ifnoerr (call imgstr (in[i], "BPM", Memc[fname], SZ_FNAME)) {
+		    pm = pm_open (NULL)
+		    call pm_loadf (pm, Memc[fname], Memc[title], SZ_FNAME)
+		    call pm_seti (pm, P_REFIM, in[i])
+		    if (pm_empty (pm) && !invert)
+			call pm_close (pm)
+		    else {
+			if (project) {
+			    npms = nimages
+			    call amovki (pm, Memi[pms], nimages)
+			} else {
+			    npms = npms + 1
+			    Memi[pms+i-1] = pm
+			}
+		    }
+		    if (project)
+			break
+		}
+	    }
+	}
+
+	# If no mask images are found and the mask parameters imply that
+	# good values are 0 then use the special case of no masks.
+
+	if (npms == 0) {
+	    if (!invert)
+		mtype = M_NONE
+	}
+
+	# Set up mask structure.
+	call calloc (icm, ICM_LEN, TY_STRUCT)
+	ICM_TYPE(icm) = mtype
+	ICM_VALUE(icm) = mvalue
+	ICM_BUFS(icm) = bufs
+	ICM_PMS(icm) = pms
+
+	call sfree (sp)
+end
+
+
+# IC_MCLOSE -- Close the mask interface.
+
+procedure ic_mclose (nimages)
+
+int	nimages			# Number of images
+
+int	i
+include	"icombine.com"
+
+begin
+	if (icm == NULL)
+	    return
+
+	do i = 1, nimages
+	    call mfree (Memi[ICM_BUFS(icm)+i-1], TY_INT)
+	do i = 1, nimages {
+	    if (Memi[ICM_PMS(icm)+i-1] != NULL)
+		call pm_close (Memi[ICM_PMS(icm)+i-1])
+	    if (project)
+		break
+	}
+	call mfree (ICM_BUFS(icm), TY_POINTER)
+	call mfree (ICM_PMS(icm), TY_POINTER)
+	call mfree (icm, TY_STRUCT)
+end
+
+
+# IC_MGET -- Get lines of mask pixels in the output coordinate system.
+# This converts the mask format to an array where zero is good and nonzero
+# is bad.  This has special cases for optimization.
+
+procedure ic_mget (in, out, offsets, v1, v2, m, lflag, nimages)
+
+pointer	in[nimages]		# Input image pointers
+pointer	out[ARB]		# Output image pointer
+int	offsets[nimages,ARB]	# Offsets to  output image
+long	v1[IM_MAXDIM]		# Data vector desired in output image
+long	v2[IM_MAXDIM]		# Data vector in input image
+pointer	m[nimages]		# Pointer to mask pointers
+int	lflag[nimages]		# Line flags
+int	nimages			# Number of images
+
+int	mtype			# Mask type
+int	mvalue			# Mask value
+pointer	bufs			# Pointer to data line buffers
+pointer	pms			# Pointer to array of PMIO pointers
+
+int	i, j, ndim, nout, npix
+pointer	buf, pm
+bool	pm_linenotempty()
+errchk	pm_glpi
+
+include	"icombine.com"
+
+begin
+	# Determine if masks are needed at all.  Note that the threshold
+	# is applied by simulating mask values so the mask pointers have to
+	# be set.
+
+	dflag = D_ALL
+	if (icm == NULL)
+	    return
+	if (ICM_TYPE(icm) == M_NONE && aligned && !dothresh)
+	    return
+
+	mtype = ICM_TYPE(icm)
+	mvalue = ICM_VALUE(icm)
+	bufs = ICM_BUFS(icm)
+	pms = ICM_PMS(icm)
+
+	# Set the mask pointers and line flags and apply offsets if needed.
+
+	ndim = IM_NDIM(out[1])
+	nout = IM_LEN(out[1],1)
+	do i = 1, nimages {
+	    npix = IM_LEN(in[i],1)
+	    j = offsets[i,1]
+	    m[i] = Memi[bufs+i-1]
+	    buf = Memi[bufs+i-1] + j
+	    pm =  Memi[pms+i-1]
+	    if (npix == nout)
+	        lflag[i] = D_ALL
+	    else
+	        lflag[i] = D_MIX
+
+	    v2[1] = v1[1]
+	    do j = 2, ndim {
+		v2[j] = v1[j] - offsets[i,j]
+		if (v2[j] < 1 || v2[j] > IM_LEN(in[i],j)) {
+		    lflag[i] = D_NONE
+		    break
+		}
+	    }
+	    if (project)
+		v2[ndim+1] = i
+
+	    if (lflag[i] == D_NONE)
+		next
+
+	    if (pm == NULL) {
+		call aclri (Memi[buf], npix)
+		next
+	    }
+
+	    # Do mask I/O and convert to appropriate values in order of
+	    # expected usage.
+
+	    if (pm_linenotempty (pm, v2)) {
+		call pm_glpi (pm, v2, Memi[buf], 32, npix, 0)
+
+		if (mtype == M_BOOLEAN)
+		    ;
+		else if (mtype == M_BADBITS)
+		    call aandki (Memi[buf], mvalue, Memi[buf], npix)
+		else if (mtype == M_BADVAL)
+		    call abeqki (Memi[buf], mvalue, Memi[buf], npix)
+		else if (mtype == M_GOODBITS) {
+		    call aandki (Memi[buf], mvalue, Memi[buf], npix)
+		    call abeqki (Memi[buf], 0, Memi[buf], npix)
+		} else if (mtype == M_GOODVAL)
+		    call abneki (Memi[buf], mvalue, Memi[buf], npix)
+
+		lflag[i] = D_NONE
+		do j = 1, npix
+		    if (Memi[buf+j-1] == 0) {
+			lflag[i] = D_MIX
+			break
+		    }
+	    } else {
+		if (mtype == M_BOOLEAN || mtype == M_BADBITS) {
+		    call aclri (Memi[buf], npix)
+		} else if ((mtype == M_BADVAL && mvalue != 0) ||
+		    (mtype == M_GOODVAL && mvalue == 0)) {
+		    call aclri (Memi[buf], npix)
+		} else {
+		    call amovki (1, Memi[buf], npix)
+		    lflag[i] = D_NONE
+		}
+	    }
+	}
+
+	# Set overall data flag
+	dflag = lflag[1]
+	do i = 2, nimages  {
+	    if (lflag[i] != dflag) {
+		dflag = D_MIX
+		break
+	    }
+	}
+end
+
+
+# IC_MGET1 -- Get line of mask pixels from a specified image.
+# This is used by the IC_STAT procedure. This procedure  converts the
+# stored mask format to an array where zero is good and nonzero is bad.
+# The data vector and returned mask array are in the input image pixel system.
+
+procedure ic_mget1 (in, image, offset, v, m)
+
+pointer	in			# Input image pointer
+int	image			# Image index
+int	offset			# Column offset
+long	v[IM_MAXDIM]		# Data vector desired
+pointer	m			# Pointer to mask
+
+int	mtype			# Mask type
+int	mvalue			# Mask value
+pointer	bufs			# Pointer to data line buffers
+pointer	pms			# Pointer to array of PMIO pointers
+
+int	i, npix
+pointer	buf, pm
+bool	pm_linenotempty()
+errchk	pm_glpi
+
+include	"icombine.com"
+
+begin
+	dflag = D_ALL
+	if (icm == NULL)
+	    return
+	if (ICM_TYPE(icm) == M_NONE)
+	    return
+
+	mtype = ICM_TYPE(icm)
+	mvalue = ICM_VALUE(icm)
+	bufs = ICM_BUFS(icm)
+	pms = ICM_PMS(icm)
+
+	npix = IM_LEN(in,1)
+	m = Memi[bufs+image-1] + offset
+	pm =  Memi[pms+image-1]
+	if (pm == NULL)
+	    return
+
+	# Do mask I/O and convert to appropriate values in order of
+	# expected usage.
+
+	buf = m
+	if (pm_linenotempty (pm, v)) {
+	    call pm_glpi (pm, v, Memi[buf], 32, npix, 0)
+
+	    if (mtype == M_BOOLEAN)
+		;
+	    else if (mtype == M_BADBITS)
+		call aandki (Memi[buf], mvalue, Memi[buf], npix)
+	    else if (mtype == M_BADVAL)
+		call abeqki (Memi[buf], mvalue, Memi[buf], npix)
+	    else if (mtype == M_GOODBITS) {
+		call aandki (Memi[buf], mvalue, Memi[buf], npix)
+		call abeqki (Memi[buf], 0, Memi[buf], npix)
+	    } else if (mtype == M_GOODVAL)
+		call abneki (Memi[buf], mvalue, Memi[buf], npix)
+
+	    dflag = D_NONE
+	    do i = 1, npix
+		if (Memi[buf+i-1] == 0) {
+		    dflag = D_MIX
+		    break
+		}
+	} else {
+	    if (mtype == M_BOOLEAN || mtype == M_BADBITS) {
+		;
+	    } else if ((mtype == M_BADVAL && mvalue != 0) ||
+		(mtype == M_GOODVAL && mvalue == 0)) {
+		;
+	    } else
+		dflag = D_NONE
+	}
+end
diff --git a/noao/imred/ccdred/src/icmedian.gx b/noao/imred/ccdred/src/icmedian.gx
new file mode 100644
index 00000000..dc8488d9
--- /dev/null
+++ b/noao/imred/ccdred/src/icmedian.gx
@@ -0,0 +1,228 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+$for (sr)
+# IC_MEDIAN -- Median of lines
+
+procedure ic_median$t (d, n, npts, median)
+
+pointer	d[ARB]			# Input data line pointers
+int	n[npts]			# Number of good pixels
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	median[npts]		# Median
+$else
+PIXEL	median[npts]		# Median
+$endif
+
+int	i, j, k, j1, j2, n1, lo, up, lo1, up1
+bool	even
+$if (datatype == silx)
+real	val1, val2, val3
+$else
+PIXEL	val1, val2, val3
+$endif
+PIXEL	temp, wtemp
+$if (datatype == x)
+real	abs_temp
+$endif
+
+include	"../icombine.com"
+
+begin
+	# If no data return after possibly setting blank values.
+	if (dflag == D_NONE) {
+	    do i = 1, npts
+		median[i]= blank
+	    return
+	}
+
+	# If the data were previously sorted then directly compute the median.
+	if (mclip) {
+	    if (dflag == D_ALL) {
+		n1 = n[1]
+		even = (mod (n1, 2) == 0)
+		j1 = n1 / 2 + 1
+		j2 = n1 / 2
+		do i = 1, npts {
+		    k = i - 1
+		    if (even) {
+			val1 = Mem$t[d[j1]+k]
+			val2 = Mem$t[d[j2]+k]
+			median[i] = (val1 + val2) / 2.
+		    } else
+			median[i] = Mem$t[d[j1]+k]
+		}
+	    } else {
+		do i = 1, npts {
+		    k = i - 1
+		    n1 = n[i]
+		    if (n1 > 0) {
+			j1 = n1 / 2 + 1
+			if (mod (n1, 2) == 0) {
+			    j2 = n1 / 2
+			    val1 = Mem$t[d[j1]+k]
+			    val2 = Mem$t[d[j2]+k]
+			    median[i] = (val1 + val2) / 2.
+			} else
+			    median[i] = Mem$t[d[j1]+k]
+		    } else
+			median[i] = blank
+		}
+	    }
+	    return
+	}
+
+	# Compute the median.
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+
+	    # If there are more than 3 points use Wirth algorithm.  This
+	    # is the same as vops$amed.gx except for an even number of
+	    # points it selects the middle two and averages.
+	    if (n1 > 3) {
+		lo = 1
+		up = n1
+		j  = max (lo, min (up, (up+1)/2))
+
+		while (lo < up) {
+		    if (! (lo < up))
+			break
+
+		    temp = Mem$t[d[j]+k];  lo1 = lo;  up1 = up
+		    $if (datatype == x)
+		    abs_temp = abs (temp)
+		    $endif
+
+		    repeat {
+			$if (datatype == x)
+			while (abs (Mem$t[d[lo1]+k]) < abs_temp)
+			$else
+			while (Mem$t[d[lo1]+k] < temp)
+			$endif
+			    lo1 = lo1 + 1
+			$if (datatype == x)
+			while (abs_temp < abs (Mem$t[d[up1]+k]))
+			$else
+			while (temp < Mem$t[d[up1]+k])
+			$endif
+			    up1 = up1 - 1
+			if (lo1 <= up1) {
+			    wtemp = Mem$t[d[lo1]+k]
+			    Mem$t[d[lo1]+k] = Mem$t[d[up1]+k]
+			    Mem$t[d[up1]+k] = wtemp
+			    lo1 = lo1 + 1;  up1 = up1 - 1
+			}
+		    } until (lo1 > up1)
+
+		    if (up1 < j)
+			lo = lo1
+		    if (j < lo1)
+			up = up1
+		}
+
+		median[i] = Mem$t[d[j]+k]
+
+		if (mod (n1,2) == 0) {
+		    lo = 1
+		    up = n1
+		    j  = max (lo, min (up, (up+1)/2)+1)
+
+		    while (lo < up) {
+			if (! (lo < up))
+			    break
+
+			temp = Mem$t[d[j]+k];  lo1 = lo;  up1 = up
+			$if (datatype == x)
+			abs_temp = abs (temp)
+			$endif
+
+			repeat {
+			    $if (datatype == x)
+			    while (abs (Mem$t[d[lo1]+k]) < abs_temp)
+			    $else
+			    while (Mem$t[d[lo1]+k] < temp)
+			    $endif
+				lo1 = lo1 + 1
+			    $if (datatype == x)
+			    while (abs_temp < abs (Mem$t[d[up1]+k]))
+			    $else
+			    while (temp < Mem$t[d[up1]+k])
+			    $endif
+				up1 = up1 - 1
+			    if (lo1 <= up1) {
+				wtemp = Mem$t[d[lo1]+k]
+				Mem$t[d[lo1]+k] = Mem$t[d[up1]+k]
+				Mem$t[d[up1]+k] = wtemp
+				lo1 = lo1 + 1;  up1 = up1 - 1
+			    }
+			} until (lo1 > up1)
+
+			if (up1 < j)
+			    lo = lo1
+			if (j < lo1)
+			    up = up1
+		    }
+		    median[i] = (median[i] + Mem$t[d[j]+k]) / 2
+		}
+
+	    # If 3 points find the median directly.
+	    } else if (n1 == 3) {
+		$if (datatype == x)
+	        val1 = abs (Mem$t[d[1]+k])
+	        val2 = abs (Mem$t[d[2]+k])
+	        val3 = abs (Mem$t[d[3]+k])
+	        if (val1 < val2) {
+		    if (val2 < val3)		# abc
+		        median[i] = Mem$t[d[2]+k]
+		    else if (val1 < val3)	# acb
+		        median[i] = Mem$t[d[3]+k]
+		    else			# cab
+		        median[i] = Mem$t[d[1]+k]
+	        } else {
+		    if (val2 > val3)		# cba
+		        median[i] = Mem$t[d[2]+k]
+		    else if (val1 > val3)	# bca
+		        median[i] = Mem$t[d[3]+k]
+		    else			# bac
+		        median[i] = Mem$t[d[1]+k]
+	        }
+		$else
+	        val1 = Mem$t[d[1]+k]
+	        val2 = Mem$t[d[2]+k]
+	        val3 = Mem$t[d[3]+k]
+	        if (val1 < val2) {
+		    if (val2 < val3)		# abc
+		        median[i] = val2
+		    else if (val1 < val3)	# acb
+		        median[i] = val3
+		    else			# cab
+		        median[i] = val1
+	        } else {
+		    if (val2 > val3)		# cba
+		        median[i] = val2
+		    else if (val1 > val3)	# bca
+		        median[i] = val3
+		    else			# bac
+		        median[i] = val1
+	        }
+		$endif
+
+	    # If 2 points average.
+	    } else if (n1 == 2) {
+		val1 = Mem$t[d[1]+k]
+		val2 = Mem$t[d[2]+k]
+		median[i] = (val1 + val2) / 2
+
+	    # If 1 point return the value.
+	    } else if (n1 == 1)
+		median[i] = Mem$t[d[1]+k]
+
+	    # If no points return with a possibly blank value.
+	    else
+		median[i] = blank
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/icmm.gx b/noao/imred/ccdred/src/icmm.gx
new file mode 100644
index 00000000..90837ae5
--- /dev/null
+++ b/noao/imred/ccdred/src/icmm.gx
@@ -0,0 +1,177 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+$for (sr)
+# IC_MM --  Reject a specified number of high and low pixels
+
+procedure ic_mm$t (d, m, n, npts)
+
+pointer	d[ARB]		# Data pointers
+pointer	m[ARB]		# Image ID pointers
+int	n[npts]			# Number of good pixels
+int	npts			# Number of output points per line
+
+int	n1, ncombine, npairs, nlow, nhigh, np
+int	i, i1, j, jmax, jmin
+pointer	k, kmax, kmin
+PIXEL	d1, d2, dmin, dmax
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_NONE)
+	    return
+
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    nlow = flow * n1 + 0.001
+	    nhigh = fhigh * n1 + 0.001
+	    ncombine = n1 - nlow -  nhigh
+	    npairs = min (nlow, nhigh)
+	    nlow = nlow - npairs
+	    nhigh = nhigh - npairs
+	}
+
+	do i = 1, npts {
+	    i1 = i - 1
+	    n1 = n[i]
+	    if (dflag == D_MIX) {
+		nlow = flow * n1 + 0.001
+		nhigh = fhigh * n1 + 0.001
+		ncombine = max (ncombine, n1 - nlow - nhigh)
+		npairs = min (nlow, nhigh)
+		nlow = nlow - npairs
+		nhigh = nhigh - npairs
+	    }
+
+	    # Reject the npairs low and high points.
+	    do np = 1, npairs {
+		k = d[1] + i1
+		$if (datatype == x)
+		d1 = abs (Mem$t[k])
+		$else
+		d1 = Mem$t[k]
+		$endif
+		dmax = d1; dmin = d1; jmax = 1; jmin = 1; kmax = k; kmin = k
+		do j = 2, n1 {
+		    d2 = d1
+		    k = d[j] + i1
+		    $if (datatype == x)
+		    d1 = abs (Mem$t[k])
+		    $else
+		    d1 = Mem$t[k]
+		    $endif
+		    if (d1 > dmax) {
+			dmax = d1; jmax = j; kmax = k
+		    } else if (d1 < dmin) {
+			dmin = d1; jmin = j; kmin = k
+		    }
+		}
+		j = n1 - 1
+		if (keepids) {
+		    if (jmax < j) {
+			if (jmin != j) {
+			    Mem$t[kmax] = d2
+			    Memi[m[jmax]+i1] = Memi[m[j]+i1]
+			} else {
+			    Mem$t[kmax] = d1
+			    Memi[m[jmax]+i1] = Memi[m[n1]+i1]
+			}
+		    }
+		    if (jmin < j) {
+			if (jmax != n1) {
+			    Mem$t[kmin] = d1
+			    Memi[m[jmin]+i1] = Memi[m[n1]+i1]
+			} else {
+			    Mem$t[kmin] = d2
+			    Memi[m[jmin]+i1] = Memi[m[j]+i1]
+			}
+		    }
+		} else {
+		    if (jmax < j) {
+			if (jmin != j)
+			    Mem$t[kmax] = d2
+			else
+			    Mem$t[kmax] = d1
+		    }
+		    if (jmin < j) {
+			if (jmax != n1)
+			    Mem$t[kmin] = d1
+			else
+			    Mem$t[kmin] = d2
+		    }
+		}
+		n1 = n1 - 2
+	    }
+
+	    # Reject the excess low points.
+	    do np = 1, nlow {
+		k = d[1] + i1
+		$if (datatype == x)
+		d1 = abs (Mem$t[k])
+		$else
+		d1 = Mem$t[k]
+		$endif
+		dmin = d1; jmin = 1; kmin = k
+		do j = 2, n1 {
+		    k = d[j] + i1
+		    $if (datatype == x)
+		    d1 = abs (Mem$t[k])
+		    $else
+		    d1 = Mem$t[k]
+		    $endif
+		    if (d1 < dmin) {
+			dmin = d1; jmin = j; kmin = k
+		    }
+		}
+		if (keepids) {
+		    if (jmin < n1) {
+			Mem$t[kmin] = d1
+			Memi[m[jmin]+i1] = Memi[m[n1]+i1]
+		    }
+		} else {
+		    if (jmin < n1)
+			Mem$t[kmin] = d1
+		}
+		n1 = n1 - 1 
+	    }
+
+	    # Reject the excess high points.
+	    do np = 1, nhigh {
+		k = d[1] + i1
+		$if (datatype == x)
+		d1 = abs (Mem$t[k])
+		$else
+		d1 = Mem$t[k]
+		$endif
+		dmax = d1; jmax = 1; kmax = k
+		do j = 2, n1 {
+		    k = d[j] + i1
+		    $if (datatype == x)
+		    d1 = abs (Mem$t[k])
+		    $else
+		    d1 = Mem$t[k]
+		    $endif
+		    if (d1 > dmax) {
+			dmax = d1; jmax = j; kmax = k
+		    }
+		}
+		if (keepids) {
+		    if (jmax < n1) {
+			Mem$t[kmax] = d1
+			Memi[m[jmax]+i1] = Memi[m[n1]+i1]
+		    }
+		} else {
+		    if (jmax < n1)
+			Mem$t[kmax] = d1
+		}
+		n1 = n1 - 1 
+	    }
+	    n[i] = n1
+	}
+
+	if (dflag == D_ALL && npairs + nlow + nhigh > 0)
+		dflag = D_MIX
+end
+$endfor
diff --git a/noao/imred/ccdred/src/icombine.com b/noao/imred/ccdred/src/icombine.com
new file mode 100644
index 00000000..cb826d58
--- /dev/null
+++ b/noao/imred/ccdred/src/icombine.com
@@ -0,0 +1,40 @@
+# ICOMBINE Common
+
+int	combine			# Combine algorithm
+int	reject			# Rejection algorithm
+bool	project			# Combine across the highest dimension?
+real	blank			# Blank value
+pointer	rdnoise			# CCD read noise
+pointer	gain			# CCD gain
+pointer	snoise			# CCD sensitivity noise
+real	lthresh			# Low threshold
+real	hthresh			# High threshold
+int	nkeep			# Minimum to keep
+real	lsigma			# Low sigma cutoff
+real	hsigma			# High sigma cutoff
+real	pclip			# Number or fraction of pixels from median
+real	flow			# Fraction of low pixels to reject
+real	fhigh			# Fraction of high pixels to reject
+int	grow			# Grow radius
+bool	mclip			# Use median in sigma clipping?
+real	sigscale		# Sigma scaling tolerance
+int	logfd			# Log file descriptor
+
+# These flags allow special conditions to be optimized.
+
+int	dflag			# Data flag (D_ALL, D_NONE, D_MIX)
+bool	aligned			# Are the images aligned?
+bool	doscale			# Do the images have to be scaled?
+bool	doscale1		# Do the sigma calculations have to be scaled?
+bool	dothresh		# Check pixels outside specified thresholds?
+bool	dowts			# Does the final average have to be weighted?
+bool	keepids			# Keep track of the image indices?
+bool	docombine		# Call the combine procedure?
+bool	sort			# Sort data?
+
+pointer	icm			# Mask data structure
+
+common	/imccom/ combine, reject, blank, rdnoise, gain, snoise, lsigma, hsigma,
+		 lthresh, hthresh, nkeep, pclip, flow, fhigh, grow, logfd,
+		 dflag, sigscale, project, mclip, aligned, doscale, doscale1,
+		 dothresh, dowts, keepids, docombine, sort, icm
diff --git a/noao/imred/ccdred/src/icombine.gx b/noao/imred/ccdred/src/icombine.gx
new file mode 100644
index 00000000..d6e93ef0
--- /dev/null
+++ b/noao/imred/ccdred/src/icombine.gx
@@ -0,0 +1,395 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	<imset.h>
+include	<error.h>
+include	<syserr.h>
+include	<mach.h>
+include	"../icombine.h"
+
+
+# ICOMBINE -- Combine images
+#
+# The memory and open file descriptor limits are checked and an attempt
+# to recover is made either by setting the image pixel files to be
+# closed after I/O or by notifying the calling program that memory
+# ran out and the IMIO buffer size should be reduced.  After the checks
+# a procedure for the selected combine option is called.
+# Because there may be several failure modes when reaching the file
+# limits we first assume an error is due to the file limit, except for
+# out of memory, and close some pixel files.  If the error then repeats
+# on accessing the pixels the error is passed back.
+
+$for (sr)
+procedure icombine$t (in, out, offsets, nimages, bufsize)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+int	offsets[nimages,ARB]	# Input image offsets
+int	nimages			# Number of input images
+int	bufsize			# IMIO buffer size
+
+char	str[1]
+int	i, j, npts, fd, stropen(), errcode(), imstati()
+pointer	sp, d, id, n, m, lflag, scales, zeros, wts, dbuf
+pointer	buf, imgl1$t(), impl1i()
+errchk	stropen, imgl1$t, impl1i
+$if (datatype == sil)
+pointer	impl1r()
+errchk	impl1r
+$else
+pointer	impl1$t()
+errchk	impl1$t
+$endif
+
+include	"../icombine.com"
+
+begin
+	npts = IM_LEN(out[1],1)
+
+	# Allocate memory.
+	call smark (sp)
+	call salloc (d, nimages, TY_POINTER)
+	call salloc (id, nimages, TY_POINTER)
+	call salloc (n, npts, TY_INT)
+	call salloc (m, nimages, TY_POINTER)
+	call salloc (lflag, nimages, TY_INT)
+	call salloc (scales, nimages, TY_REAL)
+	call salloc (zeros, nimages, TY_REAL)
+	call salloc (wts, nimages, TY_REAL)
+	call amovki (D_ALL, Memi[lflag], nimages)
+
+	# If aligned use the IMIO buffer otherwise we need vectors of
+	# output length.
+
+	if (!aligned) {
+	    call salloc (dbuf, nimages, TY_POINTER)
+	    do i = 1, nimages
+		call salloc (Memi[dbuf+i-1], npts, TY_PIXEL)
+	}
+
+	if (project) {
+	    call imseti (in[1], IM_NBUFS, nimages)
+	    call imseti (in[1], IM_BUFSIZE, bufsize)
+	    do i = 1, 3 {
+		if (out[i] != NULL)
+		    call imseti (out[i], IM_BUFSIZE, bufsize)
+	    }
+	} else {
+	    # Reserve FD for string operations.
+	    fd = stropen (str, 1, NEW_FILE)
+
+	    # Do I/O to the images.
+	    do i = 1, 3 {
+		if (out[i] != NULL)
+		    call imseti (out[i], IM_BUFSIZE, bufsize)
+	    }
+	    $if (datatype == sil)
+	    buf = impl1r (out[1])
+	    call aclrr (Memr[buf], npts)
+	    if (out[3] != NULL) {
+		buf = impl1r (out[3])
+		call aclrr (Memr[buf], npts)
+	    }
+	    $else
+	    buf = impl1$t (out[1])
+	    call aclr$t (Mem$t[buf], npts)
+	    if (out[3] != NULL) {
+		buf = impl1$t (out[3])
+		call aclr$t (Mem$t[buf], npts)
+	    }
+	    $endif
+	    if (out[2] != NULL) {
+		buf = impl1i (out[2])
+		call aclri (Memi[buf], npts)
+	    }
+
+	    do i = 1, nimages {
+		call imseti (in[i], IM_BUFSIZE, bufsize)
+		iferr (buf = imgl1$t (in[i])) {
+		    switch (errcode()) {
+		    case SYS_MFULL:
+			call sfree (sp)
+			call strclose (fd)
+			call erract (EA_ERROR)
+		    case SYS_FTOOMANYFILES, SYS_IKIOPIX:
+			if (imstati (in[i], IM_CLOSEFD) == YES) {
+			    call sfree (sp)
+			    call strclose (fd)
+			    call erract (EA_ERROR)
+			}
+			do j = i-2, nimages
+			    call imseti (in[j], IM_CLOSEFD, YES)
+			buf = imgl1$t (in[i])
+		    default:
+			call sfree (sp)
+			call strclose (fd)
+			call erract (EA_ERROR)
+		    }
+		}
+	    }
+
+	    call strclose (fd)
+	}
+
+	call ic_combine$t (in, out, Memi[dbuf], Memi[d], Memi[id], Memi[n],
+	    Memi[m], Memi[lflag], offsets, Memr[scales], Memr[zeros],
+	    Memr[wts], nimages, npts)
+end
+
+
+# IC_COMBINE -- Combine images.
+
+procedure ic_combine$t (in, out, dbuf, d, id, n, m, lflag, offsets,
+	scales, zeros, wts, nimages, npts)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output image
+pointer	dbuf[nimages]		# Data buffers for nonaligned images
+pointer	d[nimages]		# Data pointers
+pointer	id[nimages]		# Image index ID pointers
+int	n[npts]			# Number of good pixels
+pointer	m[nimages]		# Mask pointers
+int	lflag[nimages]		# Line flags
+int	offsets[nimages,ARB]	# Input image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero offset factors
+real	wts[nimages]		# Combining weights
+int	nimages			# Number of input images
+int	npts			# Number of points per output line
+
+int	i, ctor()
+real	r, imgetr()
+pointer	sp, v1, v2, v3, outdata, buf, nm, impnli()
+$if (datatype == sil)
+pointer	impnlr()
+$else
+pointer	impnl$t()
+$endif
+errchk	ic_scale, imgetr
+
+include	"../icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (v1, IM_MAXDIM, TY_LONG)
+	call salloc (v2, IM_MAXDIM, TY_LONG)
+	call salloc (v3, IM_MAXDIM, TY_LONG)
+	call amovkl (long(1), Meml[v1], IM_MAXDIM)
+	call amovkl (long(1), Meml[v2], IM_MAXDIM)
+	call amovkl (long(1), Meml[v3], IM_MAXDIM)
+
+	call ic_scale (in, out, offsets, scales, zeros, wts, nimages)
+
+	# Set combine parameters
+	switch (combine) {
+	case AVERAGE:
+	    if (dowts)
+		keepids = true
+	    else
+		keepids = false
+	case MEDIAN:
+	    dowts = false
+	    keepids = false
+	}
+	docombine = true
+
+	# Set rejection algorithm specific parameters
+	switch (reject) {
+	case CCDCLIP, CRREJECT:
+	    call salloc (nm, 3*nimages, TY_REAL)
+	    i = 1
+	    if (ctor (Memc[rdnoise], i, r) > 0) {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)] = r
+	    } else {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)] = imgetr (in[i], Memc[rdnoise])
+	    }
+	    i = 1
+	    if (ctor (Memc[gain], i, r) > 0) {
+		do i = 1, nimages {
+		    Memr[nm+3*(i-1)+1] = r
+		    Memr[nm+3*(i-1)] =
+			max ((Memr[nm+3*(i-1)] / r) ** 2, 1e4 / MAX_REAL)
+		}
+	    } else {
+		do i = 1, nimages {
+		    r = imgetr (in[i], Memc[gain])
+		    Memr[nm+3*(i-1)+1] = r
+		    Memr[nm+3*(i-1)] =
+			max ((Memr[nm+3*(i-1)] / r) ** 2, 1e4 / MAX_REAL)
+		}
+	    }
+	    i = 1
+	    if (ctor (Memc[snoise], i, r) > 0) {
+		do i = 1, nimages
+		    Memr[nm+3*(i-1)+2] = r
+	    } else {
+		do i = 1, nimages {
+		    r = imgetr (in[i], Memc[snoise])
+		    Memr[nm+3*(i-1)+2] = r
+		}
+	    }
+	    if (!keepids) {
+		if (doscale1 || grow > 0)
+		    keepids = true
+		else {
+		    do i = 2, nimages {
+			if (Memr[nm+3*(i-1)] != Memr[nm] ||
+			    Memr[nm+3*(i-1)+1] != Memr[nm+1] ||
+			    Memr[nm+3*(i-1)+2] != Memr[nm+2]) {
+			    keepids = true
+			    break
+			}
+		    }
+		}
+	    }
+	    if (reject == CRREJECT)
+		lsigma = MAX_REAL
+	case MINMAX:
+	    mclip = false
+	    if (grow > 0)
+		keepids = true
+	case PCLIP:
+	    mclip = true
+	    if (grow > 0)
+		keepids = true
+	case AVSIGCLIP, SIGCLIP:
+	    if (doscale1 || grow > 0)
+		keepids = true
+	case NONE:
+	    mclip = false
+	    grow = 0
+	}
+
+	if (keepids) {
+	    do i = 1, nimages
+		call salloc (id[i], npts, TY_INT)
+	}
+
+	$if (datatype == sil)
+	while (impnlr (out[1], outdata, Meml[v1]) != EOF) {
+	    call ic_gdata$t (in, out, dbuf, d, id, n, m, lflag, offsets,
+		scales, zeros, nimages, npts, Meml[v2], Meml[v3])
+
+	    switch (reject) {
+	    case CCDCLIP, CRREJECT:
+		if (mclip)
+		    call ic_mccdclip$t (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Memr[outdata])
+		else
+		    call ic_accdclip$t (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Memr[outdata])
+	    case MINMAX:
+		call ic_mm$t (d, id, n, npts)
+	    case PCLIP:
+		call ic_pclip$t (d, id, n, nimages, npts, Memr[outdata])
+	    case SIGCLIP:
+		if (mclip)
+		    call ic_msigclip$t (d, id, n, scales, zeros, nimages, npts,
+			Memr[outdata])
+		else
+		    call ic_asigclip$t (d, id, n, scales, zeros, nimages, npts,
+			Memr[outdata])
+	    case AVSIGCLIP:
+		if (mclip)
+		    call ic_mavsigclip$t (d, id, n, scales, zeros, nimages,
+			npts, Memr[outdata])
+		else
+		    call ic_aavsigclip$t (d, id, n, scales, zeros, nimages,
+			npts, Memr[outdata])
+	    }
+
+	    if (grow > 0)
+		call ic_grow$t (d, id, n, nimages, npts, Memr[outdata])
+
+	    if (docombine) {
+		switch (combine) {
+		case AVERAGE:
+		    call ic_average$t (d, id, n, wts, npts, Memr[outdata])
+		case MEDIAN:
+		    call ic_median$t (d, n, npts, Memr[outdata])
+		}
+	    }
+
+	    if (out[2] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnli (out[2], buf, Meml[v1])
+		call amovki (nimages, Memi[buf], npts)
+		call asubi (Memi[buf], n, Memi[buf], npts)
+	    }
+		    
+	    if (out[3] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnlr (out[3], buf, Meml[v1])
+		call ic_sigma$t (d, id, n, wts, npts, Memr[outdata],
+		    Memr[buf])
+	    }
+	    call amovl (Meml[v1], Meml[v2], IM_MAXDIM)
+	}
+	$else
+	while (impnl$t (out[1], outdata, Meml[v1]) != EOF) {
+	    call ic_gdata$t (in, out, dbuf, d, id, n, m, lflag, offsets,
+		scales, zeros, nimages, npts, Meml[v2], Meml[v3])
+
+	    switch (reject) {
+	    case CCDCLIP, CRREJECT:
+		if (mclip)
+		    call ic_mccdclip$t (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Mem$t[outdata])
+		else
+		    call ic_accdclip$t (d, id, n, scales, zeros, Memr[nm],
+			nimages, npts, Mem$t[outdata])
+	    case MINMAX:
+		call ic_mm$t (d, id, n, npts)
+	    case PCLIP:
+		call ic_pclip$t (d, id, n, nimages, npts, Mem$t[outdata])
+	    case SIGCLIP:
+		if (mclip)
+		    call ic_msigclip$t (d, id, n, scales, zeros, nimages, npts,
+			Mem$t[outdata])
+		else
+		    call ic_asigclip$t (d, id, n, scales, zeros, nimages, npts,
+			Mem$t[outdata])
+	    case AVSIGCLIP:
+		if (mclip)
+		    call ic_mavsigclip$t (d, id, n, scales, zeros, nimages,
+			npts, Mem$t[outdata])
+		else
+		    call ic_aavsigclip$t (d, id, n, scales, zeros, nimages,
+			npts, Mem$t[outdata])
+	    }
+
+	    if (grow > 0)
+		call ic_grow$t (d, id, n, nimages, npts, Mem$t[outdata])
+
+	    if (docombine) {
+		switch (combine) {
+		case AVERAGE:
+		    call ic_average$t (d, id, n, wts, npts, Mem$t[outdata])
+		case MEDIAN:
+		    call ic_median$t (d, n, npts, Mem$t[outdata])
+		}
+	    }
+
+	    if (out[2] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnli (out[2], buf, Meml[v1])
+		call amovki (nimages, Memi[buf], npts)
+		call asubi (Memi[buf], n, Memi[buf], npts)
+	    }
+		    
+	    if (out[3] != NULL) {
+		call amovl (Meml[v2], Meml[v1], IM_MAXDIM)
+		i = impnl$t (out[3], buf, Meml[v1])
+		call ic_sigma$t (d, id, n, wts, npts, Mem$t[outdata],
+		    Mem$t[buf])
+	    }
+	    call amovl (Meml[v1], Meml[v2], IM_MAXDIM)
+	}
+	$endif
+
+	call sfree (sp)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/icombine.h b/noao/imred/ccdred/src/icombine.h
new file mode 100644
index 00000000..13b77117
--- /dev/null
+++ b/noao/imred/ccdred/src/icombine.h
@@ -0,0 +1,52 @@
+# ICOMBINE Definitions
+
+# Memory management parameters;
+define	DEFBUFSIZE		65536		# default IMIO buffer size
+define	FUDGE			0.8		# fudge factor
+
+# Rejection options:
+define	REJECT	"|none|ccdclip|crreject|minmax|pclip|sigclip|avsigclip|"
+define	NONE		1	# No rejection algorithm
+define	CCDCLIP		2	# CCD noise function clipping
+define	CRREJECT	3	# CCD noise function clipping
+define	MINMAX		4	# Minmax rejection
+define	PCLIP		5	# Percentile clip
+define	SIGCLIP		6	# Sigma clip
+define	AVSIGCLIP	7	# Sigma clip with average poisson sigma
+
+# Combine options:
+define	COMBINE	"|average|median|"
+define	AVERAGE		1
+define	MEDIAN		2
+
+# Scaling options:
+define	STYPES		"|none|mode|median|mean|exposure|"
+define	ZTYPES		"|none|mode|median|mean|"
+define	WTYPES		"|none|mode|median|mean|exposure|"
+define	S_NONE		1
+define	S_MODE		2
+define	S_MEDIAN	3
+define	S_MEAN		4
+define	S_EXPOSURE	5
+define	S_FILE		6
+define	S_KEYWORD	7
+define	S_SECTION	"|input|output|overlap|"
+define	S_INPUT		1
+define	S_OUTPUT	2
+define	S_OVERLAP	3
+
+# Mask options
+define	MASKTYPES	"|none|goodvalue|badvalue|goodbits|badbits|"
+define	M_NONE		1	# Don't use mask images
+define	M_GOODVAL	2	# Value selecting good pixels
+define	M_BADVAL	3	# Value selecting bad pixels
+define	M_GOODBITS	4	# Bits selecting good pixels
+define	M_BADBITS	5	# Bits selecting bad pixels
+define	M_BOOLEAN	-1	# Ignore mask values
+
+# Data flag
+define	D_ALL		0	# All pixels are good
+define	D_NONE		1	# All pixels are bad or rejected
+define	D_MIX		2	# Mixture of good and bad pixels
+
+define	TOL		0.001	# Tolerance for equal residuals
diff --git a/noao/imred/ccdred/src/icpclip.gx b/noao/imred/ccdred/src/icpclip.gx
new file mode 100644
index 00000000..223396c3
--- /dev/null
+++ b/noao/imred/ccdred/src/icpclip.gx
@@ -0,0 +1,233 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		3	# Minimum number for clipping
+
+$for (sr)
+# IC_PCLIP -- Percentile clip
+#
+# 1) Find the median
+# 2) Find the pixel which is the specified order index away
+# 3) Use the data value difference as a sigma and apply clipping
+# 4) Since the median is known return it so it does not have to be recomputed
+
+procedure ic_pclip$t (d, m, n, nimages, npts, median)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image id pointers
+int	n[npts]			# Number of good pixels
+int	nimages			# Number of input images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	median[npts]		# Median
+$else
+PIXEL	median[npts]		# Median
+$endif
+
+int	i, j, k, l, id, n1, n2, n3, n4, n5, nl, nh, nin, maxkeep
+bool	even, fp_equalr()
+real	sigma, r, s, t
+pointer	sp, resid, mp1, mp2
+$if (datatype == sil)
+real	med
+$else
+PIXEL	med
+$endif
+
+include	"../icombine.com"
+
+begin
+	# There must be at least MINCLIP and more than nkeep pixels.
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+
+	# Set sign of pclip parameter
+	if (pclip < 0)
+	    t = -1.
+	else
+	    t = 1.
+
+	# If there are no rejected pixels compute certain parameters once.
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    n2 = 1 + n1 / 2
+	    even = (mod (n1, 2) == 0)
+	    if (pclip < 0.) {
+		if (even)
+		    n3 = max (1, nint (n2 - 1 + pclip))
+		else
+		    n3 = max (1, nint (n2 + pclip))
+	    } else
+		n3 = min (n1, nint (n2 + pclip))
+	    nin = n1
+	}
+
+	# Now apply clipping.
+	do i = 1, npts {
+	    # Compute median.
+	    if (dflag == D_MIX) {
+		n1 = n[i]
+		if (nkeep < 0)
+		    maxkeep = max (0, n1 + nkeep)
+		else
+		    maxkeep = min (n1, nkeep)
+		if (n1 == 0) {
+		    if (combine == MEDIAN)
+			median[i] = blank
+		    next
+		}
+		n2 = 1 + n1 / 2
+		even = (mod (n1, 2) == 0)
+		if (pclip < 0) {
+		    if (even)
+			n3 = max (1, nint (n2 - 1 + pclip))
+		    else
+			n3 = max (1, nint (n2 + pclip))
+		} else
+		    n3 = min (n1, nint (n2 + pclip))
+	    }
+
+	    j = i - 1 
+	    if (even) {
+		med = Mem$t[d[n2-1]+j]
+		med = (med + Mem$t[d[n2]+j]) / 2.
+	    } else
+		med = Mem$t[d[n2]+j]
+
+	    if (n1 < max (MINCLIP, maxkeep+1)) {
+		if (combine == MEDIAN)
+		    median[i] = med
+		next
+	    }
+
+	    # Define sigma for clipping
+	    sigma = t * (Mem$t[d[n3]+j] - med)
+	    if (fp_equalr (sigma, 0.)) {
+		if (combine == MEDIAN)
+		    median[i] = med
+		next
+	    }
+
+	    # Reject pixels and save residuals.
+	    # Check if any pixels are clipped.
+	    # If so recompute the median and reset the number of good pixels.
+	    # Only reorder if needed.
+
+	    for (nl=1; nl<=n1; nl=nl+1) {
+		r = (med - Mem$t[d[nl]+j]) / sigma
+		if (r < lsigma)
+		    break
+		Memr[resid+nl] = r
+	    }
+	    for (nh=n1; nh>=1; nh=nh-1) {
+		r = (Mem$t[d[nh]+j] -  med) / sigma
+		if (r < hsigma)
+		    break
+		Memr[resid+nh] = r
+	    }
+	    n4 = nh - nl + 1
+
+	    # If too many pixels are rejected add some back in.
+	    # All pixels with the same residual are added.
+	    while (n4 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n4 = nh - nl + 1
+	    }
+
+	    # If any pixels are rejected recompute the median.
+	    if (nl > 1 || nh < n1) {
+		n5 = nl + n4 / 2
+		if (mod (n4, 2) == 0) {
+		    med = Mem$t[d[n5-1]+j]
+		    med = (med + Mem$t[d[n5]+j]) / 2.
+		} else
+		    med = Mem$t[d[n5]+j]
+		n[i] = n4
+	    }
+	    if (combine == MEDIAN)
+		median[i] = med
+
+	    # Reorder if pixels only if necessary.
+	    if (nl > 1 && (combine != MEDIAN || grow > 0)) {
+		k = max (nl, n4 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mem$t[d[l]+j] = Mem$t[d[k]+j]
+			if (grow > 0) {
+			    mp1 = m[l] + j
+			    mp2 = m[k] + j
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+j] = Memi[m[k]+j]
+			k = k + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mem$t[d[l]+j] = Mem$t[d[k]+j]
+			k = k + 1
+		    }
+		}
+	    }
+	}
+
+	# Check if data flag needs to be reset for rejected pixels.
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag whether the median has been computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/icscale.x b/noao/imred/ccdred/src/icscale.x
new file mode 100644
index 00000000..fc4efb2f
--- /dev/null
+++ b/noao/imred/ccdred/src/icscale.x
@@ -0,0 +1,376 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	<imset.h>
+include	<error.h>
+include	"icombine.h"
+
+# IC_SCALE -- Get the scale factors for the images.
+# 1. This procedure does CLIO to determine the type of scaling desired.
+# 2. The output header parameters for exposure time and NCOMBINE are set.
+
+procedure ic_scale (in, out, offsets, scales, zeros, wts, nimages)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+int	offsets[nimages,ARB]	# Image offsets
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero or sky levels
+real	wts[nimages]		# Weights
+int	nimages			# Number of images
+
+int	stype, ztype, wtype
+int	i, j, k, l, nout
+real	mode, median, mean, exposure, zmean, darktime, dark
+pointer	sp, ncombine, exptime, modes, medians, means
+pointer	section, str, sname, zname, wname, imref
+bool	domode, domedian, domean, dozero, snorm, znorm, wflag
+
+bool	clgetb()
+int	hdmgeti(), strdic(), ic_gscale()
+real	hdmgetr(), asumr(), asumi()
+errchk	ic_gscale, ic_statr
+
+include	"icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (ncombine, nimages, TY_INT)
+	call salloc (exptime, nimages, TY_REAL)
+	call salloc (modes, nimages, TY_REAL)
+	call salloc (medians, nimages, TY_REAL)
+	call salloc (means, nimages, TY_REAL)
+	call salloc (section, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+	call salloc (sname, SZ_FNAME, TY_CHAR)
+	call salloc (zname, SZ_FNAME, TY_CHAR)
+	call salloc (wname, SZ_FNAME, TY_CHAR)
+
+	# Set the defaults.
+	call amovki (1, Memi[ncombine], nimages)
+	call amovkr (0., Memr[exptime], nimages)
+	call amovkr (INDEF, Memr[modes], nimages)
+	call amovkr (INDEF, Memr[medians], nimages)
+	call amovkr (INDEF, Memr[means], nimages)
+	call amovkr (1., scales, nimages)
+	call amovkr (0., zeros, nimages)
+	call amovkr (1., wts, nimages)
+
+	# Get the number of images previously combined and the exposure times.
+	# The default combine number is 1 and the default exposure is 0.
+
+	do i = 1, nimages {
+	    iferr (Memi[ncombine+i-1] = hdmgeti (in[i], "ncombine"))
+		Memi[ncombine+i-1] = 1
+	    iferr (Memr[exptime+i-1] = hdmgetr (in[i], "exptime"))
+		Memr[exptime+i-1] = 0.
+	    if (project) {
+		call amovki (Memi[ncombine], Memi[ncombine], nimages)
+		call amovkr (Memr[exptime], Memr[exptime], nimages)
+		break
+	    }
+	}
+
+	# Set scaling factors.
+
+	stype = ic_gscale ("scale", Memc[sname], STYPES, in, Memr[exptime],
+	    scales, nimages)
+	ztype = ic_gscale ("zero", Memc[zname], ZTYPES, in, Memr[exptime],
+	    zeros, nimages)
+	wtype = ic_gscale ("weight", Memc[wname], WTYPES, in, Memr[exptime],
+	    wts, nimages)
+
+	# Get image statistics only if needed.
+	domode = ((stype==S_MODE)||(ztype==S_MODE)||(wtype==S_MODE))
+	domedian = ((stype==S_MEDIAN)||(ztype==S_MEDIAN)||(wtype==S_MEDIAN))
+	domean = ((stype==S_MEAN)||(ztype==S_MEAN)||(wtype==S_MEAN))
+	if (domode || domedian || domean) {
+	    Memc[section] = EOS
+	    Memc[str] = EOS
+	    call clgstr ("statsec", Memc[section], SZ_FNAME)
+	    call sscan (Memc[section])
+	    call gargwrd (Memc[section], SZ_FNAME)
+	    call  gargwrd (Memc[str], SZ_LINE)
+
+	    i = strdic (Memc[section], Memc[section], SZ_FNAME, S_SECTION)
+	    switch (i) {
+	    case S_INPUT:
+		call strcpy (Memc[str], Memc[section], SZ_FNAME)
+		imref = NULL
+	    case S_OUTPUT:
+		call strcpy (Memc[str], Memc[section], SZ_FNAME)
+		imref = out[1]
+	    case S_OVERLAP:
+		call strcpy ("[", Memc[section], SZ_FNAME)
+		do i = 1, IM_NDIM(out[1]) {
+		    k = offsets[1,i] + 1
+		    l = offsets[1,i] + IM_LEN(in[1],i)
+		    do j = 2, nimages {
+			k = max (k, offsets[j,i]+1)
+			l = min (l, offsets[j,i]+IM_LEN(in[j],i))
+		    }
+		    if (i < IM_NDIM(out[1]))
+			call sprintf (Memc[str], SZ_LINE, "%d:%d,")
+		    else
+			call sprintf (Memc[str], SZ_LINE, "%d:%d]")
+			    call pargi (k)
+			    call pargi (l)
+		    call strcat (Memc[str], Memc[section], SZ_FNAME)
+		}
+		imref = out[1]
+	    default:
+		imref = NULL
+	    }
+
+	    do i = 1, nimages {
+		if (imref != out[1])
+		    imref = in[i]
+		call ic_statr (in[i], imref, Memc[section], offsets,
+		    i, nimages, domode, domedian, domean, mode, median, mean)
+		if (domode) {
+		    Memr[modes+i-1] = mode
+		    if (stype == S_MODE)
+			scales[i] = mode
+		    if (ztype == S_MODE)
+			zeros[i] = mode
+		    if (wtype == S_MODE)
+			wts[i] = mode
+		}
+		if (domedian) {
+		    Memr[medians+i-1] = median
+		    if (stype == S_MEDIAN)
+			scales[i] = median
+		    if (ztype == S_MEDIAN)
+			zeros[i] = median
+		    if (wtype == S_MEDIAN)
+			wts[i] = median
+		}
+		if (domean) {
+		    Memr[means+i-1] = mean
+		    if (stype == S_MEAN)
+			scales[i] = mean
+		    if (ztype == S_MEAN)
+			zeros[i] = mean
+		    if (wtype == S_MEAN)
+			wts[i] = mean
+		}
+	    }
+	}
+
+	do i = 1, nimages
+	    if (scales[i] <= 0.) {
+		call eprintf ("WARNING: Negative scale factors")
+		call eprintf (" -- ignoring scaling\n")
+		call amovkr (1., scales, nimages)
+		break
+	    }
+
+	# Convert to relative factors if needed.
+	snorm = (stype == S_FILE || stype == S_KEYWORD)
+	znorm = (ztype == S_FILE || ztype == S_KEYWORD)
+	wflag = (wtype == S_FILE || wtype == S_KEYWORD)
+	if (snorm)
+	    call arcpr (1., scales, scales, nimages)
+	else {
+	    mean = asumr (scales, nimages) / nimages
+	    call adivkr (scales, mean, scales, nimages)
+	}
+	call adivr (zeros, scales, zeros, nimages)
+	zmean = asumr (zeros, nimages) / nimages
+
+	if (wtype != S_NONE) {
+	    do i = 1, nimages {
+		if (wts[i] <= 0.) {
+		    call eprintf ("WARNING: Negative weights")
+		    call eprintf (" -- using only NCOMBINE weights\n")
+		    do j = 1, nimages
+			wts[j] = Memi[ncombine+j-1]
+		    break
+		}
+		if (ztype == S_NONE || znorm || wflag)
+	            wts[i] = Memi[ncombine+i-1] * wts[i]
+		else {
+		    if (zeros[i] <= 0.) {
+			call eprintf ("WARNING: Negative zero offsets")
+			call eprintf (" -- ignoring zero weight adjustments\n")
+			do j = 1, nimages
+			    wts[j] = Memi[ncombine+j-1] * wts[j]
+			break
+		    }
+		    wts[i] = Memi[ncombine+i-1] * wts[i] * zmean / zeros[i]
+		}
+	    }
+	}
+
+	if (znorm)
+	    call anegr (zeros, zeros, nimages)
+	else {
+	    # Because of finite arithmetic it is possible for the zero offsets
+	    # to be nonzero even when they are all equal.  Just for the sake of
+	    # a nice log set the zero offsets in this case.
+
+	    call asubkr (zeros, zmean, zeros, nimages)
+	    for (i=2; (i<=nimages)&&(zeros[i]==zeros[1]); i=i+1)
+		;
+	    if (i > nimages)
+		call aclrr (zeros, nimages)
+	}
+	mean = asumr (wts, nimages)
+	call adivkr (wts, mean, wts, nimages)
+
+	# Set flags for scaling, zero offsets, sigma scaling, weights.
+	# Sigma scaling may be suppressed if the scales or zeros are
+	# different by a specified tolerance.
+
+	doscale = false
+	dozero = false
+	doscale1 = false
+	dowts = false
+	do i = 2, nimages {
+	    if (snorm || scales[i] != scales[1])
+		doscale = true
+	    if (znorm || zeros[i] != zeros[1])
+		dozero = true
+	    if (wts[i] != wts[1])
+		dowts = true
+	}
+	if (doscale && sigscale != 0.) {
+	    do i = 1, nimages {
+		if (abs (scales[i] - 1) > sigscale) {
+		    doscale1 = true
+		    break
+		}
+	    }
+	    if (!doscale1 && zmean > 0.) {
+		do i = 1, nimages {
+		    if (abs (zeros[i] / zmean) > sigscale) {
+			doscale1 = true
+			break
+		    }
+		}
+	    }
+	}
+		    
+	# Set the output header parameters.
+	nout = asumi (Memi[ncombine], nimages)
+	call hdmputi (out[1], "ncombine", nout)
+	exposure = 0.
+	darktime = 0.
+	mean = 0.
+	do i = 1, nimages {
+	    exposure = exposure + wts[i] * Memr[exptime+i-1] / scales[i]
+	    ifnoerr (dark = hdmgetr (in[i], "darktime"))
+		darktime = darktime + wts[i] * dark / scales[i]
+	    else
+		darktime = darktime + wts[i] * Memr[exptime+i-1] / scales[i]
+	    ifnoerr (mode = hdmgetr (in[i], "ccdmean"))
+		mean = mean + wts[i] * mode / scales[i]
+	}
+	call hdmputr (out[1], "exptime", exposure)
+	call hdmputr (out[1], "darktime", darktime)
+	ifnoerr (mode = hdmgetr (out[1], "ccdmean")) {
+	    call hdmputr (out[1], "ccdmean", mean)
+	    iferr (call imdelf (out[1], "ccdmeant"))
+		;
+	}
+	if (out[2] != NULL) {
+	    call imstats (out[2], IM_IMAGENAME, Memc[str], SZ_FNAME)
+	    call imastr (out[1], "BPM", Memc[str])
+	}
+
+	# Start the log here since much of the info is only available here.
+	if (clgetb ("verbose")) {
+	    i = logfd
+	    logfd = STDOUT
+	    call ic_log (in, out, Memi[ncombine], Memr[exptime], Memc[sname],
+		Memc[zname], Memc[wname], Memr[modes], Memr[medians],
+		Memr[means], scales, zeros, wts, offsets, nimages, dozero,
+		nout, "", exposure)
+
+	    logfd = i
+	}
+	call ic_log (in, out, Memi[ncombine], Memr[exptime], Memc[sname],
+	    Memc[zname], Memc[wname], Memr[modes], Memr[medians], Memr[means],
+	    scales, zeros, wts, offsets, nimages, dozero, nout,
+	    "", exposure)
+
+	doscale = (doscale || dozero)
+
+	call sfree (sp)
+end
+
+
+# IC_GSCALE -- Get scale values as directed by CL parameter
+# The values can be one of those in the dictionary, from a file specified
+# with a @ prefix, or from an image header keyword specified by a ! prefix.
+
+int procedure ic_gscale (param, name, dic, in, exptime, values, nimages)
+
+char	param[ARB]		#I CL parameter name
+char	name[SZ_FNAME]		#O Parameter value
+char	dic[ARB]		#I Dictionary string
+pointer	in[nimages]		#I IMIO pointers
+real	exptime[nimages]	#I Exposure times
+real	values[nimages]		#O Values
+int	nimages			#I Number of images
+
+int	type			#O Type of value
+
+int	fd, i, nowhite(), open(), fscan(), nscan(), strdic()
+real	rval, hdmgetr()
+pointer	errstr
+errchk	open, hdmgetr()
+
+include	"icombine.com"
+
+begin
+	call clgstr (param, name, SZ_FNAME)
+	if (nowhite (name, name, SZ_FNAME) == 0)
+	    type = S_NONE
+	else if (name[1] == '@') {
+	    type = S_FILE
+	    fd = open (name[2], READ_ONLY, TEXT_FILE)
+	    i = 0
+	    while (fscan (fd) != EOF) {
+		call gargr (rval)
+		if (nscan() != 1)
+		    next
+		if (i == nimages) {
+		   call eprintf (
+		       "Warning: Ignoring additional %s values in %s\n")
+		       call pargstr (param)
+		       call pargstr (name[2])
+		   break
+		}
+		i = i + 1
+		values[i] = rval
+	    }
+	    call close (fd)
+	    if (i < nimages) {
+		call salloc (errstr, SZ_LINE, TY_CHAR)
+		call sprintf (Memc[errstr], SZ_FNAME,
+		    "Insufficient %s values in %s")
+		    call pargstr (param)
+		    call pargstr (name[2])
+		call error (1, Memc[errstr])
+	    }
+	} else if (name[1] == '!') {
+	    type = S_KEYWORD
+	    do i = 1, nimages {
+		values[i] = hdmgetr (in[i], name[2])
+		if (project) {
+		    call amovkr (values, values, nimages)
+		    break
+		}
+	    }
+	} else {
+	    type = strdic (name, name, SZ_FNAME, dic)
+	    if (type == 0)
+		call error (1, "Unknown scale, zero, or weight type")
+	    if (type==S_EXPOSURE)
+		do i = 1, nimages
+		    values[i] = max (0.001, exptime[i])
+	}
+
+	return (type)
+end
diff --git a/noao/imred/ccdred/src/icsclip.gx b/noao/imred/ccdred/src/icsclip.gx
new file mode 100644
index 00000000..f70611aa
--- /dev/null
+++ b/noao/imred/ccdred/src/icsclip.gx
@@ -0,0 +1,504 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	"../icombine.h"
+
+define	MINCLIP		3	# Mininum number of images for algorithm
+
+$for (sr)
+# IC_ASIGCLIP -- Reject pixels using sigma clipping about the average
+# The initial average rejects the high and low pixels.  A correction for
+# different scalings of the images may be made.  Weights are not used.
+
+procedure ic_asigclip$t (d, m, n, scales, zeros, nimages, npts, average)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	average[npts]		# Average
+$else
+PIXEL	average[npts]		# Average
+$endif
+
+int	i, j, k, l, jj, n1, n2, nin, nk, maxkeep
+$if (datatype == sil)
+real	d1, low, high, sum, a, s, r, one
+data	one /1.0/
+$else
+PIXEL	d1, low, high, sum, a, s, r, one
+data	one /1$f/
+$endif
+pointer	sp, resid, w, wp, dp1, dp2, mp1, mp2
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	} 
+	
+	# Flag whether returned average needs to be recomputed.
+	if (dowts || combine != AVERAGE)
+	    docombine = true
+	else
+	    docombine = false
+
+	# Save the residuals and the sigma scaling corrections if needed.
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+	if (doscale1)
+	    call salloc (w, nimages, TY_REAL)
+
+	# Do sigma clipping.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+
+	    # If there are not enough pixels simply compute the average.
+	    if (n1 < max (3, maxkeep)) {
+		if (!docombine) {
+		    if (n1 == 0)
+			average[i] = blank
+		    else {
+			sum = Mem$t[d[1]+k]
+			do j = 2, n1
+			    sum = sum + Mem$t[d[j]+k]
+			average[i] = sum / n1
+		    }
+		}
+		next
+	    }
+
+	    # Compute average with the high and low rejected.
+	    low = Mem$t[d[1]+k]
+	    high = Mem$t[d[2]+k]
+	    if (low > high) {
+		d1 = low
+		low = high
+		high = d1
+	    }
+	    sum = 0.
+	    do j = 3, n1 {
+	       d1 = Mem$t[d[j]+k]
+	       if (d1 < low) {
+		   sum = sum + low
+		   low = d1
+		} else if (d1 > high) {
+		    sum = sum + high
+		    high = d1
+		} else
+		    sum = sum + d1
+	    }
+	    a = sum / (n1 - 2)
+	    sum = sum + low + high
+
+	    # Iteratively reject pixels and compute the final average if needed.
+	    # Compact the data and keep track of the image IDs if needed.
+
+	    repeat {
+		n2 = n1
+		if (doscale1) {
+		    # Compute sigma corrected for scaling.
+		    s = 0.
+		    wp = w - 1
+		    do j = 1, n1 {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			wp = wp + 1
+
+			d1 = Mem$t[dp1]
+			l = Memi[mp1]
+			r = sqrt (max (one, (a + zeros[l]) / scales[l]))
+			s = s + ((d1 - a) / r) ** 2
+			Memr[wp] = r
+		    }
+		    s = sqrt (s / (n1 - 1))
+
+		    # Reject pixels.  Save the residuals and data values.
+		    wp = w - 1
+		    if (s > 0.) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    mp1 = m[j] + k
+			    wp = wp + 1
+
+			    d1 = Mem$t[dp1]
+			    r = (d1 - a) / (s * Memr[wp])
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs (r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    Memr[wp] = Memr[w+n1-1]
+				    mp2 = m[n1] + k
+				    l = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = l
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		} else {
+		    # Compute the sigma without scale correction.
+		    s = 0.
+		    do j = 1, n1
+			s = s + (Mem$t[d[j]+k] - a) ** 2
+		    s = sqrt (s / (n1 - 1))
+
+		    # Reject pixels.  Save the residuals and data values.
+		    if (s > 0.) {
+			for (j=1; j<=n1; j=j+1) {
+			    dp1 = d[j] + k
+			    d1 = Mem$t[dp1]
+			    r = (d1 - a) / s
+			    if (r < -lsigma || r > hsigma) {
+				Memr[resid+n1] = abs (r)
+				if (j < n1) {
+				    dp2 = d[n1] + k
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[n1] + k
+					l = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = l
+				    }
+				    j = j - 1
+				}
+				sum = sum - d1
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+
+		# Recompute the average.
+		if (n1 > 1)
+		    a = sum / n1
+	    } until (n1 == n2 || n1 <= max (2, maxkeep))
+
+	    # If too many pixels are rejected add some back.
+	    # All pixels with equal residuals are added back.
+	    if (n1 < maxkeep) {
+		nk = maxkeep
+		if (doscale1) {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			mp1 = m[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mem$t[dp1]
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    mp2 = m[l] + k
+				    s = Memi[mp1]
+				    Memi[mp1] = Memi[mp2]
+				    Memi[mp2] = s
+				}
+			    }
+			}
+			sum = sum + Mem$t[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		} else {
+		    for (j=n1+1; j<=nk; j=j+1) {
+			dp1 = d[j] + k
+			r = Memr[resid+j]
+			jj = 0
+			do l = j+1, n2 {
+			    s = Memr[resid+l]
+			    if (s < r + TOL) {
+				if (s > r - TOL)
+				    jj = jj + 1
+				else {
+				    jj = 0
+				    Memr[resid+l] = r
+				    r = s
+				    dp2 = d[l] + k
+				    d1 = Mem$t[dp1]
+				    Mem$t[dp1] = Mem$t[dp2]
+				    Mem$t[dp2] = d1
+				    if (keepids) {
+					mp1 = m[j] + k
+					mp2 = m[l] + k
+					s = Memi[mp1]
+					Memi[mp1] = Memi[mp2]
+					Memi[mp2] = s
+				    }
+				}
+			    }
+			}
+			sum = sum + Mem$t[dp1]
+			n1 = n1 + 1
+			nk = max (nk, j+jj)
+		    }
+		}
+
+		# Recompute the average.
+		if (n1 > 1)
+		    a = sum / n1
+	    }
+
+	    # Save the average if needed.
+	    n[i] = n1
+	    if (!docombine) {
+		if (n1 > 0)
+		    average[i] = a
+		else
+		    average[i] = blank
+	    }
+	}
+
+	# Check if the data flag has to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# IC_MSIGCLIP -- Reject pixels using sigma clipping about the median
+
+procedure ic_msigclip$t (d, m, n, scales, zeros, nimages, npts, median)
+
+pointer	d[nimages]		# Data pointers
+pointer	m[nimages]		# Image id pointers
+int	n[npts]			# Number of good pixels
+real	scales[nimages]		# Scales
+real	zeros[nimages]		# Zeros
+int	nimages			# Number of images
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	median[npts]		# Median
+$else
+PIXEL	median[npts]		# Median
+$endif
+
+int	i, j, k, l, id, n1, n2, n3, nl, nh, nin, maxkeep
+real	r, s
+pointer	sp, resid, w, mp1, mp2
+$if (datatype == sil)
+real	med, one
+data	one /1.0/
+$else
+PIXEL	med, one
+data	one /1$f/
+$endif
+
+include	"../icombine.com"
+
+begin
+	# If there are insufficient pixels go on to the combining
+	if (nkeep < 0)
+	    maxkeep = max (0, nimages + nkeep)
+	else
+	    maxkeep = min (nimages, nkeep)
+	if (nimages < max (MINCLIP, maxkeep+1) || dflag == D_NONE) {
+	    docombine = true
+	    return
+	}
+
+	# Save the residuals and sigma scaling corrections if needed.
+	call smark (sp)
+	call salloc (resid, nimages+1, TY_REAL)
+	if (doscale1)
+	    call salloc (w, nimages, TY_REAL)
+
+	# Compute median and sigma and iteratively clip.
+	nin = n[1]
+	do i = 1, npts {
+	    k = i - 1
+	    n1 = n[i]
+	    if (nkeep < 0)
+		maxkeep = max (0, n1 + nkeep)
+	    else
+		maxkeep = min (n1, nkeep)
+	    nl = 1
+	    nh = n1
+
+	    repeat {
+		n2 = n1
+		n3 = nl + n1 / 2
+
+		if (n1 == 0)
+		    med = blank
+		else if (mod (n1, 2) == 0)
+		    med = (Mem$t[d[n3-1]+k] + Mem$t[d[n3]+k]) / 2.
+		else
+		    med = Mem$t[d[n3]+k]
+
+		if (n1 >= max (MINCLIP, maxkeep+1)) {
+		    if (doscale1) {
+			# Compute the sigma with scaling correction.
+			s = 0.
+			do j = nl, nh {
+			    l = Memi[m[j]+k]
+			    r = sqrt (max (one, (med + zeros[l]) / scales[l]))
+			    s = s + ((Mem$t[d[j]+k] - med) / r) ** 2
+			    Memr[w+j-1] = r
+			}
+			s = sqrt (s / (n1 - 1))
+
+			# Reject pixels and save the residuals.
+			if (s > 0.) {
+			    for (; nl <= n2; nl = nl + 1) {
+				r = (med - Mem$t[d[nl]+k]) / (s * Memr[w+nl-1])
+				if (r <= lsigma)
+				    break
+				Memr[resid+nl] = r
+				n1 = n1 - 1
+			    }
+			    for (; nh >= nl; nh = nh - 1) {
+				r = (Mem$t[d[nh]+k] - med) / (s * Memr[w+nh-1])
+				if (r <= hsigma)
+				    break
+				Memr[resid+nh] = r
+				n1 = n1 - 1
+			    }
+			}
+		    } else {
+			# Compute the sigma without scaling correction.
+			s = 0.
+			do j = nl, nh
+			    s = s + (Mem$t[d[j]+k] - med) ** 2
+			s = sqrt (s / (n1 - 1))
+
+			# Reject pixels and save the residuals.
+			if (s > 0.) {
+			    for (; nl <= n2; nl = nl + 1) {
+				r = (med - Mem$t[d[nl]+k]) / s
+				if (r <= lsigma)
+				    break
+				Memr[resid+nl] = r
+				n1 = n1 - 1
+			    }
+			    for (; nh >= nl; nh = nh - 1) {
+				r = (Mem$t[d[nh]+k] -  med) / s
+				if (r <= hsigma)
+				    break
+				Memr[resid+nh] = r
+				n1 = n1 - 1
+			    }
+			}
+		    }
+		}
+	    } until (n1 == n2 || n1 < max (MINCLIP, maxkeep+1))
+
+	    # If too many pixels are rejected add some back.
+	    # All pixels with equal residuals are added back.
+	    while (n1 < maxkeep) {
+		if (nl == 1)
+		    nh = nh + 1
+		else if (nh == n[i])
+		    nl = nl - 1
+		else {
+		    r = Memr[resid+nl-1]
+		    s = Memr[resid+nh+1]
+		    if (r < s) {
+			nl = nl - 1
+			r = r + TOL
+			if (s <= r)
+			    nh = nh + 1
+			if (nl > 1) {
+			    if (Memr[resid+nl-1] <= r)
+				nl = nl - 1
+			}
+		    } else {
+			nh = nh + 1
+			s = s + TOL
+			if (r <= s)
+			    nl = nl - 1
+			if (nh < n2) {
+			    if (Memr[resid+nh+1] <= s)
+				nh = nh + 1
+			}
+		    }
+		}
+		n1 = nh - nl + 1
+	    }
+
+	    # Only set median and reorder if needed
+	    n[i] = n1
+	    if (n1 > 0 && nl > 1 && (combine != MEDIAN || grow > 0)) {
+		j = max (nl, n1 + 1)
+		if (keepids) {
+		    do l = 1, min (n1, nl-1) {
+			Mem$t[d[l]+k] = Mem$t[d[j]+k]
+			if (grow > 0) {
+			    mp1 = m[l] + k
+			    mp2 = m[j] + k
+			    id = Memi[mp1]
+			    Memi[mp1] = Memi[mp2]
+			    Memi[mp2] = id
+			} else
+			    Memi[m[l]+k] = Memi[m[j]+k]
+			j = j + 1
+		    }
+		} else {
+		    do l = 1, min (n1, nl - 1) {
+			Mem$t[d[l]+k] = Mem$t[d[j]+k]
+			j = j + 1
+		    }
+		}
+	    }
+
+	    if (combine == MEDIAN)
+		median[i] = med
+	}
+
+	# Check if data flag needs to be reset for rejected pixels
+	if (dflag == D_ALL) {
+	    do i = 1, npts {
+		if (n[i] != nin) {
+		    dflag = D_MIX
+		    break
+		}
+	    }
+	}
+
+	# Flag that the median has been computed.
+	if (combine == MEDIAN)
+	    docombine = false
+	else
+	    docombine = true
+
+	call sfree (sp)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/icsection.x b/noao/imred/ccdred/src/icsection.x
new file mode 100644
index 00000000..746c1f51
--- /dev/null
+++ b/noao/imred/ccdred/src/icsection.x
@@ -0,0 +1,94 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<ctype.h>
+
+# IC_SECTION -- Parse an image section into its elements.
+# 1. The default values must be set by the caller.
+# 2. A null image section is OK.
+# 3. The first nonwhitespace character must be '['.
+# 4. The last interpreted character must be ']'.
+#
+# This procedure should be replaced with an IMIO procedure at some
+# point.
+
+procedure ic_section (section, x1, x2, xs, ndim)
+
+char	section[ARB]		# Image section
+int	x1[ndim]		# Starting pixel
+int	x2[ndim]		# Ending pixel
+int	xs[ndim]		# Step
+int	ndim			# Number of dimensions
+
+int	i, ip, a, b, c, temp, ctoi()
+define	error_	99
+
+begin
+	# Decode the section string.
+	ip = 1
+	while (IS_WHITE(section[ip]))
+	    ip = ip + 1
+	if (section[ip] == '[')
+	    ip = ip + 1
+	else if (section[ip] == EOS)
+	    return
+	else
+	    goto error_
+
+	do i = 1, ndim {
+	    while (IS_WHITE(section[ip]))
+	        ip = ip + 1
+	    if (section[ip] == ']')
+		break
+
+	    # Default values
+	    a = x1[i]
+	    b = x2[i]
+	    c = xs[i]
+
+	    # Get a:b:c.  Allow notation such as "-*:c"
+	    # (or even "-:c") where the step is obviously negative.
+
+	    if (ctoi (section, ip, temp) > 0) {			# a
+		a = temp
+	        if (section[ip] == ':') {	
+		    ip = ip + 1
+		    if (ctoi (section, ip, b) == 0)		# a:b
+		        goto error_
+	        } else
+		    b = a
+	    } else if (section[ip] == '-') {			# -*
+		temp = a
+		a = b
+		b = temp
+	        ip = ip + 1
+	        if (section[ip] == '*')
+		    ip = ip + 1
+	    } else if (section[ip] == '*')			# *
+	        ip = ip + 1
+	    if (section[ip] == ':') {				# ..:step
+	        ip = ip + 1
+	        if (ctoi (section, ip, c) == 0)
+		    goto error_
+	        else if (c == 0)
+		    goto error_
+	    }
+	    if (a > b && c > 0)
+	        c = -c
+
+	    x1[i] = a
+	    x2[i] = b
+	    xs[i] = c
+
+	    while (IS_WHITE(section[ip]))
+	        ip = ip + 1
+	    if (section[ip] == ',')
+		ip = ip + 1
+	}
+
+	if (section[ip] != ']')
+	    goto error_
+
+	return
+error_
+	call error (0, "Error in image section specification")
+end
diff --git a/noao/imred/ccdred/src/icsetout.x b/noao/imred/ccdred/src/icsetout.x
new file mode 100644
index 00000000..bd1d75ec
--- /dev/null
+++ b/noao/imred/ccdred/src/icsetout.x
@@ -0,0 +1,193 @@
+include	<imhdr.h>
+include <mwset.h>
+
+# IC_SETOUT -- Set output image size and offsets of input images.
+
+procedure ic_setout (in, out, offsets, nimages)
+
+pointer	in[nimages]		# Input images
+pointer	out[ARB]		# Output images
+int	offsets[nimages,ARB]	# Offsets
+int	nimages			# Number of images
+
+int	i, j, indim, outdim, mwdim, a, b, amin, bmax, fd
+real	val
+bool	reloff, streq()
+pointer	sp, fname, lref, wref, cd, coord, shift, axno, axval
+pointer	mw, ct, mw_openim(), mw_sctran()
+int	open(), fscan(), nscan(), mw_stati()
+errchk	mw_openim, mw_gwtermd, mw_gltermd, mw_gaxmap
+errchk	mw_sctran, mw_ctrand, open
+
+include	"icombine.com"
+define	newscan_ 10
+
+begin
+	call smark (sp)
+	call salloc (fname, SZ_FNAME, TY_CHAR)
+	call salloc (lref, IM_MAXDIM, TY_DOUBLE)
+	call salloc (wref, IM_MAXDIM, TY_DOUBLE)
+	call salloc (cd, IM_MAXDIM*IM_MAXDIM, TY_DOUBLE)
+	call salloc (coord, IM_MAXDIM, TY_DOUBLE)
+	call salloc (shift, IM_MAXDIM, TY_REAL)
+	call salloc (axno, IM_MAXDIM, TY_INT)
+	call salloc (axval, IM_MAXDIM, TY_INT)
+
+	# Check and set the image dimensionality.
+	indim = IM_NDIM(in[1])
+	outdim = IM_NDIM(out[1])
+	if (project) {
+	    outdim = indim - 1
+	    IM_NDIM(out[1]) = outdim
+	} else {
+	    do i = 1, nimages
+		if (IM_NDIM(in[i]) != outdim) {
+		    call sfree (sp)
+		    call error (1, "Image dimensions are not the same")
+		}
+	}
+
+	# Set the reference point to that of the first image.
+	mw = mw_openim (in[1])
+	mwdim = mw_stati (mw, MW_NPHYSDIM)
+	call mw_gwtermd (mw, Memd[lref], Memd[wref], Memd[cd], mwdim)
+	ct = mw_sctran (mw, "world", "logical", 0)
+	call mw_ctrand (ct, Memd[wref], Memd[lref], mwdim)
+	call mw_ctfree (ct)
+	if (project)
+	    Memd[lref+outdim] = 1
+
+	# Parse the user offset string.  If "none" then there are no offsets.
+	# If "wcs" then set the offsets based on the image WCS.
+	# If "grid" then set the offsets based on the input grid parameters.
+	# If a file scan it.
+
+	call clgstr ("offsets", Memc[fname], SZ_FNAME)
+	call sscan (Memc[fname])
+	call gargwrd (Memc[fname], SZ_FNAME)
+	if (nscan() == 0 || streq (Memc[fname], "none")) {
+	    call aclri (offsets, outdim*nimages)
+	    reloff = true
+	} else if (streq (Memc[fname], "wcs")) {
+	    do j = 1, outdim
+		offsets[1,j] = 0
+	    if (project) {
+		ct = mw_sctran (mw, "world", "logical", 0)
+		do i = 2, nimages {
+		    Memd[wref+outdim] = i
+		    call mw_ctrand (ct, Memd[wref], Memd[coord], indim)
+		    do j = 1, outdim
+			offsets[i,j] = nint (Memd[lref+j-1] - Memd[coord+j-1])
+		}
+		call mw_ctfree (ct)
+		call mw_close (mw)
+	    } else {
+		do i = 2, nimages {
+		    call mw_close (mw)
+		    mw = mw_openim (in[i])
+		    ct = mw_sctran (mw, "world", "logical", 0)
+		    call mw_ctrand (ct, Memd[wref], Memd[coord], indim)
+		    do j = 1, outdim
+			offsets[i,j] = nint (Memd[lref+j-1] - Memd[coord+j-1])
+		    call mw_ctfree (ct)
+		}
+	    }
+	    reloff = true
+	} else if (streq (Memc[fname], "grid")) {
+	    amin = 1
+	    do j = 1, outdim {
+		call gargi (a)
+		call gargi (b)
+		if (nscan() < 1+2*j)
+		    break
+		do i = 1, nimages
+		    offsets[i,j] = mod ((i-1)/amin, a) * b 
+		amin = amin * a
+	    }
+	    reloff = true
+	} else {
+	    reloff = true
+	    fd = open (Memc[fname], READ_ONLY, TEXT_FILE)
+	    do i = 1, nimages {
+newscan_	if (fscan (fd) == EOF)
+		    call error (1, "IMCOMBINE: Offset list too short")
+		call gargwrd (Memc[fname], SZ_FNAME)
+		if (Memc[fname] == '#') {
+		    call gargwrd (Memc[fname], SZ_FNAME)
+		    call strlwr (Memc[fname])
+		    if (streq (Memc[fname], "absolute"))
+			reloff = false
+		    else if (streq (Memc[fname], "relative"))
+			reloff = true
+		    goto newscan_
+		}
+		call reset_scan ()
+		do j = 1, outdim {
+		    call gargr (val)
+		    offsets[i,j] = nint (val)
+		}
+		if (nscan() < outdim)
+		    call error (1, "IMCOMBINE: Error in offset list")
+	    }
+	    call close (fd)
+	}
+
+	# Set the output image size and the aligned flag 
+	aligned = true
+	do j = 1, outdim {
+	    a = offsets[1,j]
+	    b = IM_LEN(in[1],j) + a
+	    amin = a
+	    bmax = b
+	    do i = 2, nimages {
+		a = offsets[i,j]
+		b = IM_LEN(in[i],j) + a
+		if (a != amin || b != bmax || !reloff)
+		    aligned = false
+		amin = min (a, amin)
+		bmax = max (b, bmax)
+	    }
+	    IM_LEN(out[1],j) = bmax
+	    if (reloff || amin < 0) {
+		do i = 1, nimages
+		    offsets[i,j] = offsets[i,j] - amin
+		IM_LEN(out[1],j) = IM_LEN(out[1],j) - amin
+	    }
+	}
+
+	# Update the WCS.
+	if (project || !aligned || !reloff) {
+	    call mw_close (mw)
+	    mw = mw_openim (out[1])
+	    mwdim = mw_stati (mw, MW_NPHYSDIM)
+	    call mw_gaxmap (mw, Memi[axno], Memi[axval], mwdim)
+	    if (!aligned || !reloff) {
+		call mw_gltermd (mw, Memd[cd], Memd[lref], mwdim)
+		do i = 1, mwdim {
+		    j = Memi[axno+i-1]
+		    if (j > 0 && j <= indim)
+			Memd[lref+i-1] = Memd[lref+i-1] + offsets[1,j]
+		}
+		call mw_sltermd (mw, Memd[cd], Memd[lref], mwdim)
+	    }
+	    if (project) {
+		# Apply dimensional reduction.
+		do i = 1, mwdim {
+		    j = Memi[axno+i-1]
+		    if (j <= outdim)
+			next
+		    else if (j > outdim+1)
+			Memi[axno+i-1] = j - 1
+		    else {
+			Memi[axno+i-1] = 0
+			Memi[axval+i-1] = 0
+		    }
+		}
+		call mw_saxmap (mw, Memi[axno], Memi[axval], mwdim)
+	    }
+	    call mw_saveim (mw, out)
+	}
+	call mw_close (mw)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/icsigma.gx b/noao/imred/ccdred/src/icsigma.gx
new file mode 100644
index 00000000..d0ae28d4
--- /dev/null
+++ b/noao/imred/ccdred/src/icsigma.gx
@@ -0,0 +1,115 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"../icombine.h"
+
+$for (sr)
+# IC_SIGMA -- Compute the sigma image line.
+# The estimated sigma includes a correction for the finite population.
+# Weights are used if desired.
+
+procedure ic_sigma$t (d, m, n, wts, npts, average, sigma)
+
+pointer	d[ARB]			# Data pointers
+pointer	m[ARB]			# Image ID pointers
+int	n[npts]			# Number of points
+real	wts[ARB]		# Weights
+int	npts			# Number of output points per line
+$if (datatype == sil)
+real	average[npts]		# Average
+real	sigma[npts]		# Sigma line (returned)
+$else
+PIXEL	average[npts]		# Average
+PIXEL	sigma[npts]		# Sigma line (returned)
+$endif
+
+int	i, j, k, n1
+real	wt, sigcor, sumwt
+$if (datatype == sil)
+real	a, sum
+$else
+PIXEL	a, sum
+$endif
+
+include	"../icombine.com"
+
+begin
+	if (dflag == D_ALL) {
+	    n1 = n[1]
+	    if (dowts) {
+		if (n1 > 1)
+		    sigcor = real (n1) / real (n1 - 1)
+		else
+		    sigcor = 1.
+		do i = 1, npts {
+		    k = i - 1
+		    a = average[i]
+		    wt = wts[Memi[m[1]+k]]
+		    sum = (Mem$t[d[1]+k] - a) ** 2 * wt
+		    do j = 2, n1 {
+			wt = wts[Memi[m[j]+k]]
+			sum = sum + (Mem$t[d[j]+k] - a) ** 2 * wt
+		    }
+		    sigma[i] = sqrt (sum * sigcor)
+		}
+	    } else {
+		if (n1 > 1)
+		    sigcor = 1. / real (n1 - 1)
+		else
+		    sigcor = 1.
+		do i = 1, npts {
+		    k = i - 1
+		    a = average[i]
+		    sum = (Mem$t[d[1]+k] - a) ** 2
+		    do j = 2, n1
+			sum = sum + (Mem$t[d[j]+k] - a) ** 2
+		    sigma[i] = sqrt (sum * sigcor)
+		}
+	    }
+	} else if (dflag == D_NONE) {
+	    do i = 1, npts
+		sigma[i] = blank
+	} else {
+	    if (dowts) {
+		do i = 1, npts {
+		    n1 = n[i]
+		    if (n1 > 0) {
+			k = i - 1
+			if (n1 > 1)
+			    sigcor = real (n1) / real (n1 -1)
+			else
+			    sigcor = 1
+			a = average[i]
+			wt = wts[Memi[m[1]+k]]
+			sum = (Mem$t[d[1]+k] - a) ** 2 * wt
+			sumwt = wt
+			do j = 2, n1 {
+			    wt = wts[Memi[m[j]+k]]
+			    sum = sum + (Mem$t[d[j]+k] - a) ** 2 * wt
+			    sumwt = sumwt + wt
+			}
+			sigma[i] = sqrt (sum / sumwt * sigcor)
+		    } else
+			sigma[i] = blank
+		}
+	    } else {
+		do i = 1, npts {
+		    n1 = n[i]
+		    if (n1 > 0) {
+			k = i - 1
+			if (n1 > 1)
+			    sigcor = 1. / real (n1 - 1)
+			else
+			    sigcor = 1.
+			a = average[i]
+			sum = (Mem$t[d[1]+k] - a) ** 2
+			do j = 2, n1
+			    sum = sum + (Mem$t[d[j]+k] - a) ** 2
+			sigma[i] = sqrt (sum * sigcor)
+		    } else
+			sigma[i] = blank
+		}
+	    }
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/icsort.gx b/noao/imred/ccdred/src/icsort.gx
new file mode 100644
index 00000000..2235dbd0
--- /dev/null
+++ b/noao/imred/ccdred/src/icsort.gx
@@ -0,0 +1,386 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+define	LOGPTR	32			# log2(maxpts) (4e9)
+
+$for (sr)
+# IC_SORT -- Quicksort.  This is based on the VOPS asrt except that
+# the input is an array of pointers to image lines and the sort is done
+# across the image lines at each point along the lines.  The number of
+# valid pixels at each point is allowed to vary.  The cases of 1, 2, and 3
+# pixels per point are treated specially.
+
+procedure ic_sort$t (a, b, nvecs, npts)
+
+pointer	a[ARB]			# pointer to input vectors
+PIXEL	b[ARB]			# work array
+int	nvecs[npts]		# number of vectors
+int	npts			# number of points in vectors
+
+PIXEL	pivot, temp, temp3
+int	i, j, k, l, p, npix, lv[LOGPTR], uv[LOGPTR]
+define	swap {temp=$1;$1=$2;$2=temp}
+define	copy_	10
+
+begin
+	do l = 0, npts-1 {
+	    npix = nvecs[l+1]
+	    if (npix <= 1)
+		next
+
+	    do i = 1, npix
+		b[i] = Mem$t[a[i]+l]
+
+	    # Special cases
+	    $if (datatype == x)
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (abs (temp) < abs (pivot)) {
+			b[1] = temp
+			b[2] = pivot
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (abs (temp) < abs (pivot)) {		# bac|bca|cba
+			if (abs (temp) < abs (temp3)) {		# bac|bca
+			    b[1] = temp
+			    if (abs (pivot) < abs (temp3))	# bac
+				b[2] = pivot
+			    else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			}
+		    } else if (abs (temp3) < abs (temp)) {	# acb|cab
+			b[3] = temp
+			if (abs (pivot) < abs (temp3))		# acb
+			    b[2] = temp3
+			else {					# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+	    $else
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (temp < pivot) {
+			b[1] = temp
+			b[2] = pivot
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (temp < pivot) {				# bac|bca|cba
+			if (temp < temp3) {			# bac|bca
+			    b[1] = temp
+			    if (pivot < temp3)			# bac
+				b[2] = pivot
+			    else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			}
+		    } else if (temp3 < temp) {			# acb|cab
+			b[3] = temp
+			if (pivot < temp3)			# acb
+			    b[2] = temp3
+			else {					# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+	    $endif
+
+	    # General case
+	    do i = 1, npix
+		b[i] = Mem$t[a[i]+l]
+
+	    lv[1] = 1
+	    uv[1] = npix
+	    p = 1
+
+	    while (p > 0) {
+		if (lv[p] >= uv[p])		# only one elem in this subset
+		    p = p - 1			# pop stack
+		else {
+		    # Dummy do loop to trigger the Fortran optimizer.
+		    do p = p, ARB {
+			i = lv[p] - 1
+			j = uv[p]
+
+			# Select as the pivot the element at the center of the
+			# array, to avoid quadratic behavior on an already
+			# sorted array.
+
+			k = (lv[p] + uv[p]) / 2
+			swap (b[j], b[k])
+			pivot = b[j]		   # pivot line
+
+			while (i < j) {
+			$if (datatype == x)
+			    for (i=i+1;  abs(b[i]) < abs(pivot);  i=i+1)
+			$else
+			    for (i=i+1;  b[i] < pivot;  i=i+1)
+			$endif
+				;
+			    for (j=j-1;  j > i;  j=j-1)
+			$if (datatype == x)
+				if (abs(b[j]) <= abs(pivot))
+			$else
+				if (b[j] <= pivot)
+			$endif
+				    break
+			    if (i < j)		   # out of order pair
+				swap (b[i], b[j])  # interchange elements
+			}
+
+			j = uv[p]		   # move pivot to position i
+			swap (b[i], b[j])	   # interchange elements
+
+			if (i-lv[p] < uv[p] - i) { # stack so shorter done first
+			    lv[p+1] = lv[p]
+			    uv[p+1] = i - 1
+			    lv[p] = i + 1
+			} else {
+			    lv[p+1] = i + 1
+			    uv[p+1] = uv[p]
+			    uv[p] = i - 1
+			}
+
+			break
+		    }
+		    p = p + 1			   # push onto stack
+		}
+	    }
+
+copy_
+	    do i = 1, npix
+		Mem$t[a[i]+l] = b[i]
+	}
+end
+
+
+# IC_2SORT -- Quicksort.  This is based on the VOPS asrt except that
+# the input is an array of pointers to image lines and the sort is done
+# across the image lines at each point along the lines.  The number of
+# valid pixels at each point is allowed to vary.  The cases of 1, 2, and 3
+# pixels per point are treated specially.  A second integer set of
+# vectors is sorted.
+
+procedure ic_2sort$t (a, b, c, d, nvecs, npts)
+
+pointer	a[ARB]			# pointer to input vectors
+PIXEL	b[ARB]			# work array
+pointer	c[ARB]			# pointer to associated integer vectors
+int	d[ARB]			# work array
+int	nvecs[npts]		# number of vectors
+int	npts			# number of points in vectors
+
+PIXEL	pivot, temp, temp3
+int	i, j, k, l, p, npix, lv[LOGPTR], uv[LOGPTR], itemp
+define	swap {temp=$1;$1=$2;$2=temp}
+define	iswap {itemp=$1;$1=$2;$2=itemp}
+define	copy_	10
+
+begin
+	do l = 0, npts-1 {
+	    npix = nvecs[l+1]
+	    if (npix <= 1)
+		next
+
+	    do i = 1, npix {
+		b[i] = Mem$t[a[i]+l]
+		d[i] = Memi[c[i]+l]
+	    }
+
+	    # Special cases
+	    $if (datatype == x)
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (abs (temp) < abs (pivot)) {
+			b[1] = temp
+			b[2] = pivot
+			iswap (d[1], d[2])
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (abs (temp) < abs (pivot)) {		# bac|bca|cba
+			if (abs (temp) < abs (temp3)) {		# bac|bca
+			    b[1] = temp
+			    if (abs (pivot) < abs (temp3)) {	# bac
+				b[2] = pivot
+				iswap (d[1], d[2])
+			    } else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+				itemp = d[2]
+				d[2] = d[3]
+				d[3] = d[1]
+				d[1] = itemp
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			    iswap (d[1], d[3])
+			}
+		    } else if (abs (temp3) < abs (temp)) {	# acb|cab
+			b[3] = temp
+			if (abs (pivot) < abs (temp3)) {	# acb
+			    b[2] = temp3
+			    iswap (d[2], d[3])
+			} else {				# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			    itemp = d[2]
+			    d[2] = d[1]
+			    d[1] = d[3]
+			    d[3] = itemp
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+	    $else
+	    if (npix <= 3) {
+		pivot = b[1]
+		temp = b[2]
+		if (npix == 2) {
+		    if (temp < pivot) {
+			b[1] = temp
+			b[2] = pivot
+			iswap (d[1], d[2])
+		    } else
+			next
+		} else {
+		    temp3 = b[3]
+		    if (temp < pivot) {				# bac|bca|cba
+			if (temp < temp3) {			# bac|bca
+			    b[1] = temp
+			    if (pivot < temp3) {		# bac
+				b[2] = pivot
+				iswap (d[1], d[2])
+			    } else {				# bca
+				b[2] = temp3
+				b[3] = pivot
+				itemp = d[2]
+				d[2] = d[3]
+				d[3] = d[1]
+				d[1] = itemp
+			    }
+			} else {				# cba
+			    b[1] = temp3
+			    b[3] = pivot
+			    iswap (d[1], d[3])
+			}
+		    } else if (temp3 < temp) {			# acb|cab
+			b[3] = temp
+			if (pivot < temp3) {			# acb
+			    b[2] = temp3
+			    iswap (d[2], d[3])
+			} else {				# cab
+			    b[1] = temp3
+			    b[2] = pivot
+			    itemp = d[2]
+			    d[2] = d[1]
+			    d[1] = d[3]
+			    d[3] = itemp
+			}
+		    } else
+			next
+		}
+		goto copy_
+	    }
+	    $endif
+
+	    # General case
+	    lv[1] = 1
+	    uv[1] = npix
+	    p = 1
+
+	    while (p > 0) {
+		if (lv[p] >= uv[p])		# only one elem in this subset
+		    p = p - 1			# pop stack
+		else {
+		    # Dummy do loop to trigger the Fortran optimizer.
+		    do p = p, ARB {
+			i = lv[p] - 1
+			j = uv[p]
+
+			# Select as the pivot the element at the center of the
+			# array, to avoid quadratic behavior on an already
+			# sorted array.
+
+			k = (lv[p] + uv[p]) / 2
+			swap (b[j], b[k]); swap (d[j], d[k])
+			pivot = b[j]		   # pivot line
+
+			while (i < j) {
+			$if (datatype == x)
+			    for (i=i+1;  abs(b[i]) < abs(pivot);  i=i+1)
+			$else
+			    for (i=i+1;  b[i] < pivot;  i=i+1)
+			$endif
+				;
+			    for (j=j-1;  j > i;  j=j-1)
+			$if (datatype == x)
+				if (abs(b[j]) <= abs(pivot))
+			$else
+				if (b[j] <= pivot)
+			$endif
+				    break
+			    if (i < j) {	   # out of order pair
+				swap (b[i], b[j])  # interchange elements
+				swap (d[i], d[j])
+			    }
+			}
+
+			j = uv[p]		   # move pivot to position i
+			swap (b[i], b[j])	   # interchange elements
+			swap (d[i], d[j])
+
+			if (i-lv[p] < uv[p] - i) { # stack so shorter done first
+			    lv[p+1] = lv[p]
+			    uv[p+1] = i - 1
+			    lv[p] = i + 1
+			} else {
+			    lv[p+1] = i + 1
+			    uv[p+1] = uv[p]
+			    uv[p] = i - 1
+			}
+
+			break
+		    }
+		    p = p + 1			   # push onto stack
+		}
+	    }
+
+copy_	   
+	    do i = 1, npix {
+		Mem$t[a[i]+l] = b[i]
+		Memi[c[i]+l] = d[i]
+	    }
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/icstat.gx b/noao/imred/ccdred/src/icstat.gx
new file mode 100644
index 00000000..099ddf5e
--- /dev/null
+++ b/noao/imred/ccdred/src/icstat.gx
@@ -0,0 +1,237 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"../icombine.h"
+
+define	NMAX	10000	# Maximum number of pixels to sample
+
+$for (sr)
+# IC_STAT -- Compute image statistics within specified section.
+# The image section is relative to a reference image which may be
+# different than the input image and may have an offset.  Only a
+# subsample of pixels is used.  Masked and thresholded pixels are
+# ignored.  Only the desired statistics are computed to increase
+# efficiency.
+
+procedure ic_stat$t (im, imref, section, offsets, image, nimages,
+	domode, domedian, domean, mode, median, mean)
+
+pointer	im			 # Data image
+pointer	imref			 # Reference image for image section
+char	section[ARB]		 # Image section
+int	offsets[nimages,ARB]	 # Image section offset from data to reference
+int	image			 # Image index (for mask I/O)
+int	nimages			 # Number of images in  offsets.
+bool	domode, domedian, domean # Statistics to compute
+real	mode, median, mean	 # Statistics
+
+int	i, j, ndim, n, nv
+real	a
+pointer	sp, v1, v2, dv, va, vb
+pointer	data, mask, dp, lp, mp, imgnl$t()
+PIXEL	ic_mode$t()
+$if (datatype == irs)
+real    asum$t()
+$endif
+$if (datatype == dl)
+double  asum$t()
+$endif
+$if (datatype == x)
+complex asum$t()
+$endif
+
+
+include	"../icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (v1, IM_MAXDIM, TY_LONG)
+	call salloc (v2, IM_MAXDIM, TY_LONG)
+	call salloc (dv, IM_MAXDIM, TY_LONG)
+	call salloc (va, IM_MAXDIM, TY_LONG)
+	call salloc (vb, IM_MAXDIM, TY_LONG)
+
+	# Determine the image section parameters.  This must be in terms of
+	# the data image pixel coordinates though the section may be specified
+	# in terms of the reference image coordinates.  Limit the number of
+	# pixels in each dimension to a maximum.
+
+	ndim = IM_NDIM(im)
+	if (project)
+	    ndim = ndim - 1
+	call amovki (1, Memi[v1], IM_MAXDIM)
+	call amovki (1, Memi[va], IM_MAXDIM)
+	call amovki (1, Memi[dv], IM_MAXDIM)
+	call amovi (IM_LEN(imref,1), Memi[vb], ndim)
+	call ic_section (section, Memi[va], Memi[vb], Memi[dv], ndim)
+	if (im != imref)
+	    do i = 1, ndim {
+		Memi[va+i-1] = Memi[va+i-1] - offsets[image,i]
+		Memi[vb+i-1] = Memi[vb+i-1] - offsets[image,i]
+	    }
+
+	do j = 1, 10 {
+	    n = 1
+	    do i = 0, ndim-1 {
+		Memi[v1+i] = max (1, min (Memi[va+i], Memi[vb+i]))
+		Memi[v2+i] = min (IM_LEN(im,i+1), max (Memi[va+i], Memi[vb+i]))
+		Memi[dv+i] = j
+		nv = max (1, (Memi[v2+i] - Memi[v1+i]) / Memi[dv+i] + 1)
+		Memi[v2+i] = Memi[v1+i] + (nv - 1) * Memi[dv+i]
+		n = n * nv
+	    }
+	    if (n < NMAX)
+		break
+	}
+
+	call amovl (Memi[v1], Memi[va], IM_MAXDIM)
+	Memi[va] = 1
+	if (project)
+	   Memi[va+ndim] = image
+	call amovl (Memi[va], Memi[vb], IM_MAXDIM)
+
+	# Accumulate the pixel values within the section.  Masked pixels and
+	# thresholded pixels are ignored.
+
+	call salloc (data, n, TY_PIXEL)
+	dp = data
+	while (imgnl$t (im, lp, Memi[vb]) != EOF) {
+	    call ic_mget1 (im, image, offsets[image,1], Memi[va], mask)
+	    lp = lp + Memi[v1] - 1
+	    if (dflag == D_ALL) {
+		if (dothresh) {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			a = Mem$t[lp]
+			if (a >= lthresh && a <= hthresh) {
+			    Mem$t[dp] = a
+			    dp = dp + 1
+			}
+			lp = lp + Memi[dv]
+		    }
+		} else {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			Mem$t[dp] = Mem$t[lp]
+			dp = dp + 1
+			lp = lp + Memi[dv]
+		    }
+		}
+	    } else if (dflag == D_MIX) {
+		mp = mask + Memi[v1] - 1
+		if (dothresh) {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			if (Memi[mp] == 0) {
+			    a = Mem$t[lp]
+			    if (a >= lthresh && a <= hthresh) {
+				Mem$t[dp] = a
+				dp = dp + 1
+			    }
+			}
+			mp = mp + Memi[dv]
+			lp = lp + Memi[dv]
+		    }
+		} else {
+		    do i = Memi[v1], Memi[v2], Memi[dv] {
+			if (Memi[mp] == 0) {
+			    Mem$t[dp] = Mem$t[lp]
+			    dp = dp + 1
+			}
+			mp = mp + Memi[dv]
+			lp = lp + Memi[dv]
+		    }
+		}
+	    }
+	    for (i=2; i<=ndim; i=i+1) {
+		Memi[va+i-1] = Memi[va+i-1] + Memi[dv+i-1]
+		if (Memi[va+i-1] <= Memi[v2+i-1])
+		    break
+		Memi[va+i-1] = Memi[v1+i-1]
+	    }
+	    if (i > ndim)
+		break
+	    call amovl (Memi[va], Memi[vb], IM_MAXDIM)
+	}
+
+	n = dp - data
+	if (n < 1) {
+	    call sfree (sp)
+	    call error (1, "Image section contains no pixels")
+	}
+
+	# Compute only statistics needed.
+	if (domode || domedian) {
+	    call asrt$t (Mem$t[data], Mem$t[data], n)
+	    mode = ic_mode$t (Mem$t[data], n)
+	    median = Mem$t[data+n/2-1]
+	}
+	if (domean)
+	    mean = asum$t (Mem$t[data], n) / n
+
+	call sfree (sp)
+end
+
+
+define	NMIN	10	# Minimum number of pixels for mode calculation
+define	ZRANGE	0.8	# Fraction of pixels about median to use
+define	ZSTEP	0.01	# Step size for search for mode
+define	ZBIN	0.1	# Bin size for mode.
+
+# IC_MODE -- Compute mode of an array.  The mode is found by binning
+# with a bin size based on the data range over a fraction of the
+# pixels about the median and a bin step which may be smaller than the
+# bin size.  If there are too few points the median is returned.
+# The input array must be sorted.
+
+PIXEL procedure ic_mode$t (a, n)
+
+PIXEL	a[n]			# Data array
+int	n			# Number of points
+
+int	i, j, k, nmax
+real	z1, z2, zstep, zbin
+PIXEL	mode
+bool	fp_equalr()
+
+begin
+	if (n < NMIN)
+	    return (a[n/2])
+
+	# Compute the mode.  The array must be sorted.  Consider a
+	# range of values about the median point.  Use a bin size which
+	# is ZBIN of the range.  Step the bin limits in ZSTEP fraction of
+	# the bin size.
+
+	i = 1 + n * (1. - ZRANGE) / 2.
+	j = 1 + n * (1. + ZRANGE) / 2.
+	z1 = a[i]
+	z2 = a[j]
+	if (fp_equalr (z1, z2)) {
+	    mode = z1
+	    return (mode)
+	}
+
+	zstep = ZSTEP * (z2 - z1)
+	zbin = ZBIN * (z2 - z1)
+	$if (datatype == sil)
+	zstep = max (1., zstep)
+	zbin = max (1., zbin)
+	$endif
+
+	z1 = z1 - zstep
+	k = i
+	nmax = 0
+	repeat {
+	    z1 = z1 + zstep
+	    z2 = z1 + zbin
+	    for (; i < j && a[i] < z1; i=i+1)
+		;
+	    for (; k < j && a[k] < z2; k=k+1)
+		;
+	    if (k - i > nmax) {
+	        nmax = k - i
+	        mode = a[(i+k)/2]
+	    }
+	} until (k >= j)
+
+	return (mode)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/mkpkg b/noao/imred/ccdred/src/mkpkg
new file mode 100644
index 00000000..d2d46598
--- /dev/null
+++ b/noao/imred/ccdred/src/mkpkg
@@ -0,0 +1,75 @@
+# Make CCDRED Package.
+
+$checkout libpkg.a ..
+$update   libpkg.a
+$checkin  libpkg.a ..
+$exit
+
+generic:
+	$set	GEN = "$$generic -k"
+
+        $ifolder (generic/ccdred.h, ccdred.h)
+	    $copy ccdred.h generic/ccdred.h $endif
+        $ifolder (generic/proc.x,  proc.gx)
+	    $(GEN) proc.gx -o generic/proc.x $endif
+        $ifolder (generic/cor.x,  cor.gx)
+	    $(GEN) cor.gx -o generic/cor.x $endif
+	;
+
+libpkg.a:
+	$ifeq (USE_GENERIC, yes) $call generic $endif
+	@generic
+
+	@combine
+
+	calimage.x	ccdtypes.h <error.h> <imset.h>
+	ccdcache.x	ccdcache.com ccdcache.h ccdcache.com <imhdr.h>\
+			<imset.h> <mach.h>
+	ccdcheck.x	ccdtypes.h <imhdr.h>
+	ccdcmp.x	
+	ccdcopy.x	<imhdr.h>
+	ccddelete.x	
+	ccdflag.x	
+	ccdlog.x	<imhdr.h> <imset.h>
+	ccdmean.x	<imhdr.h>
+	ccdnscan.x	ccdtypes.h
+	ccdproc.x	ccdred.h ccdtypes.h <error.h>
+	ccdsection.x	<ctype.h>
+	ccdsubsets.x	<ctype.h>
+	ccdtypes.x	ccdtypes.h
+	doproc.x	ccdred.h
+	hdrmap.x	hdrmap.com <error.h> <syserr.h>
+	readcor.x	<imhdr.h>
+	scancor.x	<imhdr.h> <imset.h>
+	setdark.x	ccdred.h ccdtypes.h <imhdr.h>
+	setfixpix.x	ccdred.h <imhdr.h> <imset.h> <pmset.h>
+	setflat.x	ccdred.h ccdtypes.h <imhdr.h>
+	setfringe.x	ccdred.h ccdtypes.h <imhdr.h>
+	setheader.x	ccdred.h <imhdr.h>
+	setillum.x	ccdred.h ccdtypes.h <imhdr.h>
+	setinput.x	ccdtypes.h <error.h>
+	setinteract.x	<pkg/xtanswer.h>
+	setoutput.x	<imhdr.h> <imset.h>
+	setoverscan.x	ccdred.h <imhdr.h> <imset.h> <pkg/xtanswer.h>\
+			<pkg/gtools.h>
+	setproc.x	ccdred.h <imhdr.h>
+	setsections.x	ccdred.h <imhdr.h> <mwset.h>
+	settrim.x	ccdred.h <imhdr.h> <imset.h>
+	setzero.x	ccdred.h ccdtypes.h <imhdr.h>
+	t_badpixim.x	<imhdr.h>
+	t_ccdgroups.x	<error.h> <math.h>
+	t_ccdhedit.x	<error.h>
+	t_ccdinst.x	ccdtypes.h <error.h> <imhdr.h> <imio.h>
+	t_ccdlist.x	ccdtypes.h <error.h> <imhdr.h>
+	t_ccdmask.x	<imhdr.h>
+	t_ccdproc.x	ccdred.h ccdtypes.h <error.h> <imhdr.h>
+	t_combine.x	ccdred.h combine/icombine.com combine/icombine.h\
+			<error.h> <imhdr.h> <mach.h> <syserr.h>
+	t_mkfringe.x	ccdred.h <imhdr.h>
+	t_mkillumcor.x	ccdred.h
+	t_mkillumft.x	ccdred.h <imhdr.h>
+	t_mkskycor.x	ccdred.h <mach.h> <imhdr.h> <imset.h>
+	t_mkskyflat.x	ccdred.h ccdtypes.h <imhdr.h>
+	t_skyreplace.x	<imhdr.h>
+	timelog.x	<time.h>
+	;
diff --git a/noao/imred/ccdred/src/proc.gx b/noao/imred/ccdred/src/proc.gx
new file mode 100644
index 00000000..3161d2e6
--- /dev/null
+++ b/noao/imred/ccdred/src/proc.gx
@@ -0,0 +1,408 @@
+include	<imhdr.h>
+include	"ccdred.h"
+
+
+.help proc Feb87 noao.imred.ccdred
+.nf ----------------------------------------------------------------------------
+proc -- Process CCD images
+
+These are the main CCD reduction procedures.  There is one for each
+readout axis (lines or columns) and one for short and real image data.
+They apply corrections for bad pixels, overscan levels, zero levels,
+dark counts, flat field response, illumination response, and fringe
+effects.  The image is also trimmed if it was mapped with an image
+section.  The mean value for the output image is computed when the flat
+field or illumination image is processed to form the scale factor for
+these calibrations in order to avoid reading through these image a
+second time.
+
+The processing information and parameters are specified in the CCD
+structure. The processing operations to be performed are specified by
+the correction array CORS in the ccd structure.  There is one array
+element for each operation with indices defined symbolically by macro
+definitions (see ccdred.h); i.e.  FLATCOR.  The value of the array
+element is an integer bit field in which the bit set is the same as the
+array index; i.e element 3 will have the third bit set for an operation
+with array value 2**(3-1)=4.  If an operation is not to be performed
+the bit is not set and the array element has the numeric value zero.
+Note that the addition of several correction elements gives a unique
+bit field describing a combination of operations.  For efficiency the
+most common combinations are implemented as separate units.
+
+The CCD structure also contains the correction or calibration data
+consisting either pointers to data, IMIO pointers for the calibration
+images, and scale factors.
+
+The processing is performed line-by-line.  The procedure CORINPUT is
+called to get an input line.  This procedure trims and fixes bad pixels by
+interpolation.  The output line and lines from the various calibration
+images are read.  The image vectors as well as the overscan vector and
+the scale factors are passed to the procedure COR (which also
+dereferences the pointer data into simple arrays and variables).  That
+procedure does the actual corrections apart from bad pixel
+corrections.
+
+The final optional step is to add each corrected output line to form a
+mean.  This adds efficiency since the operation is done only if desired
+and the output image data is already in memory so there is no I/O
+penalty.
+
+SEE ALSO
+    ccdred.h, cor, fixpix, setfixpix, setoverscan, settrim,
+    setzero, setdark, setflat, setillum, setfringe
+.endhelp ----------------------------------------------------------------------
+
+
+$for (sr)
+# PROC1 -- Process CCD images with readout axis 1 (lines).
+
+procedure proc1$t (ccd)
+
+pointer	ccd		# CCD structure
+
+int	line, ncols, nlines, findmean, rep
+int	overscan_type, overscan_c1, noverscan
+real	overscan, darkscale, flatscale, illumscale, frgscale, mean
+PIXEL	minrep
+pointer	in, out, zeroim, darkim, flatim, illumim, fringeim, overscan_vec
+pointer	inbuf, outbuf, zerobuf, darkbuf, flatbuf, illumbuf, fringebuf
+
+$if (datatype == csir)
+real	asum$t()
+$else $if (datatype == ld)
+double	asum$t()
+$else
+PIXEL	asum$t()
+$endif $endif
+real	find_overscan$t()
+pointer	imgl2$t(), impl2$t(), ccd_gl$t(), xt_fps$t()
+
+begin
+	# Initialize.  If the correction image is 1D then just get the
+	# data once.
+
+	in = IN_IM(ccd)
+	out = OUT_IM(ccd)
+	ncols = OUT_C2(ccd) - OUT_C1(ccd) + 1
+	nlines = OUT_L2(ccd) - OUT_L1(ccd) + 1
+
+	findmean = CORS(ccd, FINDMEAN)
+	if (findmean == YES)
+	    mean = 0.
+	rep = CORS(ccd, MINREP)
+	if (rep == YES)
+	    minrep = MINREPLACE(ccd)
+
+	if (CORS(ccd, OVERSCAN) == 0)
+	    overscan_type = 0
+	else {
+	    overscan_type = OVERSCAN_TYPE(ccd)
+	    overscan_vec = OVERSCAN_VEC(ccd)
+	    overscan_c1 = BIAS_C1(ccd) - 1
+	    noverscan = BIAS_C2(ccd) - overscan_c1
+	}
+
+	if (CORS(ccd, ZEROCOR) == 0) {
+	    zeroim = NULL
+	    zerobuf = 1
+	} else if (IM_LEN(ZERO_IM(ccd),2) == 1) {
+	    zeroim = NULL
+	    zerobuf = ccd_gl$t (ZERO_IM(ccd), ZERO_C1(ccd), ZERO_C2(ccd), 1)
+	} else
+	    zeroim = ZERO_IM(ccd)
+
+	if (CORS(ccd, DARKCOR) == 0) {
+	    darkim = NULL
+	    darkbuf = 1
+	} else if (IM_LEN(DARK_IM(ccd),2) == 1) {
+	    darkim = NULL
+	    darkbuf = ccd_gl$t (DARK_IM(ccd), DARK_C1(ccd), DARK_C2(ccd), 1)
+	    darkscale = FLATSCALE(ccd)
+	} else {
+	    darkim = DARK_IM(ccd)
+	    darkscale = DARKSCALE(ccd)
+	}
+
+	if (CORS(ccd, FLATCOR) == 0) {
+	    flatim = NULL
+	    flatbuf = 1
+	} else if (IM_LEN(FLAT_IM(ccd),2) == 1) {
+	    flatim = NULL
+	    flatbuf = ccd_gl$t (FLAT_IM(ccd), FLAT_C1(ccd), FLAT_C2(ccd), 1)
+	    flatscale = FLATSCALE(ccd)
+	} else {
+	    flatim = FLAT_IM(ccd)
+	    flatscale = FLATSCALE(ccd)
+	}
+
+	if (CORS(ccd, ILLUMCOR) == 0) {
+	    illumim = NULL
+	    illumbuf = 1
+	} else {
+	    illumim = ILLUM_IM(ccd)
+	    illumscale = ILLUMSCALE(ccd)
+	}
+
+	if (CORS(ccd, FRINGECOR) == 0) {
+	    fringeim = NULL
+	    fringebuf = 1
+	} else {
+	    fringeim = FRINGE_IM(ccd)
+	    frgscale = FRINGESCALE(ccd)
+	}
+
+	# For each line read lines from the input.  Procedure XT_FPS replaces
+	# bad pixels by interpolation.  The trimmed region is copied to the
+	# output.  Get lines from the output image and from the zero level,
+	# dark count, flat field, illumination, and fringe images.  Call COR1
+	# to do the actual pixel corrections.  Finally, add the output pixels
+	# to a sum for computing the mean.  We must copy data outside of the
+	# output data section.
+
+	do line = 2 - OUT_L1(ccd), 0
+	    call amov$t (
+		Mem$t[imgl2$t(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mem$t[impl2$t(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	do line = 1, nlines {
+	    outbuf = impl2$t (out, OUT_L1(ccd)+line-1)
+
+	    inbuf = xt_fps$t (MASK_FP(ccd), in, IN_L1(ccd)+line-1, IN_C1(ccd),
+		IN_C2(ccd), IN_L1(ccd), IN_L2(ccd), NULL)
+	    call amov$t (Mem$t[inbuf+IN_C1(ccd)-OUT_C1(ccd)], Mem$t[outbuf],
+		IM_LEN(out,1))
+
+	    outbuf = outbuf + OUT_C1(ccd) - 1
+	    if (overscan_type != 0) {
+		if (overscan_type < OVERSCAN_FIT)
+		    overscan = find_overscan$t (Mem$t[inbuf+overscan_c1],
+			noverscan, overscan_type)
+		else
+		    overscan = Memr[overscan_vec+line-1]
+	    }
+	    if (zeroim != NULL)
+		zerobuf = ccd_gl$t (zeroim, ZERO_C1(ccd), ZERO_C2(ccd),
+		    ZERO_L1(ccd)+line-1)
+	    if (darkim != NULL)
+		darkbuf = ccd_gl$t (darkim, DARK_C1(ccd), DARK_C2(ccd),
+		    DARK_L1(ccd)+line-1)
+	    if (flatim != NULL)
+		flatbuf = ccd_gl$t (flatim, FLAT_C1(ccd), FLAT_C2(ccd),
+		    FLAT_L1(ccd)+line-1)
+	    if (illumim != NULL)
+		illumbuf = ccd_gl$t (illumim, ILLUM_C1(ccd), ILLUM_C2(ccd),
+		    ILLUM_L1(ccd)+line-1)
+	    if (fringeim != NULL)
+		fringebuf = ccd_gl$t (fringeim, FRINGE_C1(ccd), FRINGE_C2(ccd),
+		    FRINGE_L1(ccd)+line-1)
+
+	    call cor1$t (CORS(ccd,1), Mem$t[outbuf],
+		overscan, Mem$t[zerobuf], Mem$t[darkbuf],
+		Mem$t[flatbuf], Mem$t[illumbuf], Mem$t[fringebuf], ncols,
+		darkscale, flatscale, illumscale, frgscale)
+
+	    if (rep == YES)
+		call amaxk$t (Mem$t[outbuf], minrep, Mem$t[outbuf], ncols)
+	    if (findmean == YES)
+		mean = mean + asum$t (Mem$t[outbuf], ncols)
+	}
+
+	do line = nlines+1, IM_LEN(out,2)-OUT_L1(ccd)+1
+	    call amov$t (
+		Mem$t[imgl2$t(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mem$t[impl2$t(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	# Compute the mean from the sum of the output pixels.
+	if (findmean == YES)
+	    MEAN(ccd) = mean / ncols / nlines
+end
+
+
+# PROC2 -- Process CCD images with readout axis 2 (columns).
+
+procedure proc2$t (ccd)
+
+pointer	ccd		# CCD structure
+
+int	line, ncols, nlines, findmean, rep
+real	darkscale, flatscale, illumscale, frgscale, mean
+PIXEL	minrep
+pointer	in, out, zeroim, darkim, flatim, illumim, fringeim, overscan_vec
+pointer	inbuf, outbuf, zerobuf, darkbuf, flatbuf, illumbuf, fringebuf
+
+$if (datatype == csir)
+real	asum$t()
+$else $if (datatype == ld)
+double	asum$t()
+$else
+PIXEL	asum$t()
+$endif $endif
+pointer	imgl2$t(), impl2$t(), imgs2$t(), ccd_gl$t(), xt_fps$t()
+
+begin
+	# Initialize.  If the correction image is 1D then just get the
+	# data once.
+
+	in = IN_IM(ccd)
+	out = OUT_IM(ccd)
+	ncols = OUT_C2(ccd) - OUT_C1(ccd) + 1
+	nlines = OUT_L2(ccd) - OUT_L1(ccd) + 1
+
+	findmean = CORS(ccd, FINDMEAN)
+	if (findmean == YES)
+	    mean = 0.
+	rep = CORS(ccd, MINREP)
+	if (rep == YES)
+	    minrep = MINREPLACE(ccd)
+
+	overscan_vec = OVERSCAN_VEC(ccd)
+
+	if (CORS(ccd, ZEROCOR) == 0) {
+	    zeroim = NULL
+	    zerobuf = 1
+	} else if (IM_LEN(ZERO_IM(ccd),1) == 1) {
+	    zeroim = NULL
+	    zerobuf = imgs2$t (ZERO_IM(ccd), 1, 1, ZERO_L1(ccd), ZERO_L2(ccd))
+	} else
+	    zeroim = ZERO_IM(ccd)
+
+	if (CORS(ccd, DARKCOR) == 0) {
+	    darkim = NULL
+	    darkbuf = 1
+	} else if (IM_LEN(DARK_IM(ccd),1) == 1) {
+	    darkim = NULL
+	    darkbuf = imgs2$t (DARK_IM(ccd), 1, 1, DARK_L1(ccd), DARK_L2(ccd))
+	    darkscale = DARKSCALE(ccd)
+	} else {
+	    darkim = DARK_IM(ccd)
+	    darkscale = DARKSCALE(ccd)
+	}
+
+	if (CORS(ccd, FLATCOR) == 0) {
+	    flatim = NULL
+	    flatbuf = 1
+	} else if (IM_LEN(FLAT_IM(ccd),1) == 1) {
+	    flatim = NULL
+	    flatbuf = imgs2$t (FLAT_IM(ccd), 1, 1, FLAT_L1(ccd), FLAT_L2(ccd))
+	    flatscale = FLATSCALE(ccd)
+	} else {
+	    flatim = FLAT_IM(ccd)
+	    flatscale = FLATSCALE(ccd)
+	}
+
+	if (CORS(ccd, ILLUMCOR) == 0) {
+	    illumim = NULL
+	    illumbuf = 1
+	} else {
+	    illumim = ILLUM_IM(ccd)
+	    illumscale = ILLUMSCALE(ccd)
+	}
+
+	if (CORS(ccd, FRINGECOR) == 0) {
+	    fringeim = NULL
+	    fringebuf = 1
+	} else {
+	    fringeim = FRINGE_IM(ccd)
+	    frgscale = FRINGESCALE(ccd)
+	}
+
+	# For each line read lines from the input.  Procedure CORINPUT
+	# replaces bad pixels by interpolation and applies a trim to the
+	# input.  Get lines from the output image and from the zero level,
+	# dark count, flat field, illumination, and fringe images.
+	# Call COR2 to do the actual pixel corrections.  Finally, add the
+	# output pixels to a sum for computing the mean.
+	# We must copy data outside of the output data section.
+
+	do line = 2 - OUT_L1(ccd), 0
+	    call amov$t (
+		Mem$t[imgl2$t(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mem$t[impl2$t(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	do line = 1, nlines {
+	    outbuf = impl2$t (out, OUT_L1(ccd)+line-1)
+
+	    inbuf = xt_fps$t (MASK_FP(ccd), in, IN_L1(ccd)+line-1, IN_C1(ccd),
+		IN_C2(ccd), IN_L1(ccd), IN_L2(ccd), NULL)
+	    call amov$t (Mem$t[inbuf+IN_C1(ccd)-OUT_C1(ccd)], Mem$t[outbuf],
+		IM_LEN(out,1))
+
+	    outbuf = outbuf + OUT_C1(ccd) - 1
+	    if (zeroim != NULL)
+		zerobuf = ccd_gl$t (zeroim, ZERO_C1(ccd), ZERO_C2(ccd),
+		    ZERO_L1(ccd)+line-1)
+	    if (darkim != NULL)
+		darkbuf = ccd_gl$t (darkim, DARK_C1(ccd), DARK_C2(ccd),
+		    DARK_L1(ccd)+line-1)
+	    if (flatim != NULL)
+		flatbuf = ccd_gl$t (flatim, FLAT_C1(ccd), FLAT_C2(ccd),
+		    FLAT_L1(ccd)+line-1)
+	    if (illumim != NULL)
+		illumbuf = ccd_gl$t (illumim, ILLUM_C1(ccd), ILLUM_C2(ccd),
+		    ILLUM_L1(ccd)+line-1)
+	    if (fringeim != NULL)
+		fringebuf = ccd_gl$t (fringeim, FRINGE_C1(ccd), FRINGE_C2(ccd),
+		    FRINGE_L1(ccd)+line-1)
+
+	    call cor2$t (line, CORS(ccd,1), Mem$t[outbuf],
+		Memr[overscan_vec], Mem$t[zerobuf], Mem$t[darkbuf],
+		Mem$t[flatbuf], Mem$t[illumbuf], Mem$t[fringebuf], ncols,
+		zeroim, flatim, darkscale, flatscale, illumscale, frgscale)
+
+	    if (rep == YES)
+		call amaxk$t (Mem$t[outbuf], minrep, Mem$t[outbuf], ncols)
+	    if (findmean == YES)
+		mean = mean + asum$t (Mem$t[outbuf], ncols)
+	}
+
+	do line = nlines+1, IM_LEN(out,2)-OUT_L1(ccd)+1
+	    call amov$t (
+		Mem$t[imgl2$t(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mem$t[impl2$t(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	# Compute the mean from the sum of the output pixels.
+	if (findmean == YES)
+	    MEAN(ccd) = mean / ncols / nlines
+end
+
+
+# FIND_OVERSCAN -- Find the overscan value for a line.
+# No check is made on the number of pixels.
+# The median is the (npix+1)/2 element.
+
+real procedure find_overscan$t (data, npix, type)
+
+PIXEL	data[npix]	#I Overscan data
+int	npix		#I Number of overscan points
+int	type		#I Type of overscan calculation
+
+int	i
+real	overscan, d, dmin, dmax
+PIXEL	asok$t()
+
+begin
+	if (type == OVERSCAN_MINMAX) {
+	    overscan = data[1]
+	    dmin = data[1]
+	    dmax = data[1]
+	    do i = 2, npix {
+		d = data[i]
+		overscan = overscan + d
+		if (d < dmin)
+		    dmin = d
+		else if (d > dmax)
+		    dmax = d
+	    }
+	    overscan = (overscan - dmin - dmax) / (npix - 2)
+	} else if (type == OVERSCAN_MEDIAN)
+	    overscan = asok$t (data, npix, (npix + 1) / 2)
+	else {
+	    overscan = data[1]
+	    do i = 2, npix
+		overscan = overscan + data[i]
+	    overscan = overscan / npix
+	}
+
+	return (overscan)
+end
+$endfor
diff --git a/noao/imred/ccdred/src/readcor.x b/noao/imred/ccdred/src/readcor.x
new file mode 100644
index 00000000..61fbd836
--- /dev/null
+++ b/noao/imred/ccdred/src/readcor.x
@@ -0,0 +1,138 @@
+include	<imhdr.h>
+
+# READCOR -- Create a readout image.
+# Assume it is appropriate to perform this operation on the input image.
+# There is no CCD type checking.
+
+procedure readcor (input)
+
+char	input[ARB]		# Input image
+int	readaxis		# Readout axis
+
+int	i, nc, nl, c1, c2, cs, l1, l2, ls
+int	in_c1, in_c2, in_l1, in_l2, ccd_c1, ccd_c2, ccd_l1, ccd_l2
+pointer	sp, output, str, in, out, data
+
+real	asumr()
+int	clgwrd()
+bool	clgetb(), ccdflag()
+pointer	immap(), imgl2r(), impl2r(), imps2r()
+errchk	immap, ccddelete
+
+begin
+	# Check if this operation is desired.
+	if (!clgetb ("readcor"))
+	    return
+
+	# Check if this operation has been done.  Unfortunately this requires
+	# mapping the image.
+
+	in = immap (input, READ_ONLY, 0)
+	if (ccdflag (in, "readcor")) {
+	    call imunmap (in)
+	    return
+	}
+
+	if (clgetb ("noproc")) {
+	    call eprintf (
+		"  [TO BE DONE] Convert %s to readout correction\n")
+		call pargstr (input)
+	    call imunmap (in)
+	    return
+	}
+
+	call smark (sp)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# The default data section is the entire image.
+	nc = IM_LEN(in,1)
+	nl = IM_LEN(in,2)
+	c1 = 1
+	c2 = nc
+	cs = 1
+	l1 = 1
+	l2 = nl
+	ls = 1
+	call hdmgstr (in, "datasec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1))
+	    call error (0, "Error in DATASEC parameter")
+	in_c1 = c1
+	in_c2 = c2
+	in_l1 = l1
+	in_l2 = l2
+
+	# The default ccd section is the data section.
+	call hdmgstr (in, "ccdsec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((cs != 1) || (ls != 1))
+	    call error (0, "Error in CCDSEC parameter")
+	ccd_c1 = c1
+	ccd_c2 = c2
+	ccd_l1 = l1
+	ccd_l2 = l2
+	if ((in_c2-in_c1 != ccd_c2-ccd_c1) || (in_l2-in_l1 != ccd_l2-ccd_l1))
+	    call error (0, "Size of DATASEC and CCDSEC do not agree")
+
+	# Determine the readout axis.
+	readaxis = clgwrd ("readaxis", Memc[str], SZ_LINE, "|lines|columns|")
+
+	# Create output.
+	call mktemp ("tmp", Memc[output], SZ_FNAME)
+	call set_output (in, out, Memc[output])
+
+	# Average across the readout axis.
+	switch (readaxis) {
+	case 1:
+	    IM_LEN(out,2) = 1
+	    data = impl2r (out, 1)
+	    call aclrr (Memr[data], nc)
+	    nc = in_c2 - in_c1 + 1
+	    nl = in_l2 - in_l1 + 1
+	    data = data + in_c1 - 1
+	    do i = in_l1, in_l2
+		call aaddr (Memr[imgl2r(in,i)+in_c1-1], Memr[data],
+		    Memr[data], nc)
+	    call adivkr (Memr[data], real (nl), Memr[data], nc)
+	    call sprintf (Memc[str], SZ_LINE, "[%d:%d,1:1]")
+		call pargi (in_c1)
+		call pargi (in_c2)
+	    call hdmpstr (out, "datasec", Memc[str])
+	    call sprintf (Memc[str], SZ_LINE, "[%d:%d,*]")
+		call pargi (ccd_c1)
+		call pargi (ccd_c2)
+	    call hdmpstr (out, "ccdsec", Memc[str])
+	case 2:
+	    IM_LEN(out,1) = 1
+	    data = imps2r (out, 1, 1, 1, nl)
+	    call aclrr (Memr[data], nl)
+	    nc = in_c2 - in_c1 + 1
+	    nl = in_l2 - in_l1 + 1
+	    do i = in_l1, in_l2
+		Memr[data+i-1] = asumr (Memr[imgl2r(in,i)+in_c1-1], nc) / nc
+	    call sprintf (Memc[str], SZ_LINE, "[1:1,%d:%d]")
+		call pargi (in_l1)
+		call pargi (in_l2)
+	    call hdmpstr (out, "datasec", Memc[str])
+	    call sprintf (Memc[str], SZ_LINE, "[*,%d:%d]")
+		call pargi (ccd_l1)
+		call pargi (ccd_l2)
+	    call hdmpstr (out, "ccdsec", Memc[str])
+	}
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE,
+	    "Converted to readout format")
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (in, Memc[str])
+	call hdmpstr (out, "readcor", Memc[str])
+
+	# Replace the input image by the output image.
+	call imunmap (in)
+	call imunmap (out)
+	call ccddelete (input)
+	call imrename (Memc[output], input)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/scancor.x b/noao/imred/ccdred/src/scancor.x
new file mode 100644
index 00000000..6a5eb84c
--- /dev/null
+++ b/noao/imred/ccdred/src/scancor.x
@@ -0,0 +1,340 @@
+include	<imhdr.h>
+include	<imset.h>
+
+define	SCANTYPES	"|shortscan|longscan|"
+define	SHORTSCAN	1	# Short scan accumulation, normal readout
+define	LONGSCAN	2	# Long scan continuous readout
+
+# SCANCOR -- Create a scanned image from an unscanned image.
+
+procedure scancor (input, output, nscan, minreplace)
+
+char	input[ARB]		# Input image
+char	output[ARB]		# Output image (must be new image)
+int	nscan			# Number of scan lines
+real	minreplace		# Minmum value of output
+
+int	scantype		# Type of scan format
+int	readaxis		# Readout axis
+
+int	clgwrd()
+pointer	sp, str, in, out, immap()
+errchk	immap
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Determine readout axis and create the temporary output image.
+	scantype = clgwrd ("scantype", Memc[str], SZ_LINE, SCANTYPES)
+	readaxis = clgwrd ("readaxis", Memc[str], SZ_LINE, "|lines|columns|")
+
+	# Make the output scanned image.
+	in = immap (input, READ_ONLY, 0)
+	call set_output (in, out, output)
+
+	switch (scantype) {
+	case SHORTSCAN:
+	    call shortscan (in, out, nscan, minreplace, readaxis)
+	case LONGSCAN:
+	    call longscan (in, out, readaxis)
+	}
+		
+	# Log the operation.
+	switch (scantype) {
+	case SHORTSCAN:
+	    call sprintf (Memc[str], SZ_LINE,
+		"Converted to shortscan from %s with nscan=%d")
+	    call pargstr (input)
+	    call pargi (nscan)
+	    call hdmputi (out, "nscanrow", nscan)
+	case LONGSCAN:
+	    call sprintf (Memc[str], SZ_LINE, "Converted to longscan from %s")
+	    call pargstr (input)
+	}
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (out, Memc[str])
+	call hdmpstr (out, "scancor", Memc[str])
+
+	call imunmap (in)
+	call imunmap (out)
+
+	call sfree (sp)
+end
+
+
+# SHORTSCAN -- Make a shortscan mode image by using a moving average.
+#
+# NOTE!! The value of nscan used here is increased by 1 because the
+# current information in the image header is actually the number of
+# scan steps and NOT the number of rows.
+
+procedure shortscan (in, out, nscan, minreplace, readaxis)
+
+pointer	in		# Input image
+pointer	out		# Output image
+int	nscan		# Number of lines scanned before readout
+real	minreplace	# Minimum output value
+int	readaxis	# Readout axis
+
+bool	replace
+real	nscanr, sum, mean, asumr()
+int	i, j, k, l, len1, len2, nc, nl, nscani, c1, c2, cs, l1, l2, ls
+pointer	sp, str, bufs, datain, dataout, data, imgl2r(), impl2r()
+long	clktime()
+errchk	malloc, calloc
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# The default data section is the entire image.
+	len1 = IM_LEN(in,1)
+	len2 = IM_LEN(in,2)
+	c1 = 1
+	c2 = len1
+	cs = 1
+	l1 = 1
+	l2 = len2
+	ls = 1
+	call hdmgstr (in, "datasec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>len1)||(l1<1)||(l2>len2)||(cs!=1)||(ls!=1))
+	    call error (0, "Error in DATASEC parameter")
+	nc = c2 - c1 + 1
+	nl = l2 - l1 + 1
+
+	# Copy initial lines.
+	do i = 1, l1 - 1
+	    call amovr (Memr[imgl2r(in,i)], Memr[impl2r(out,i)], len1)
+
+	replace = !IS_INDEF(minreplace)
+	mean = 0.
+	switch (readaxis) {
+	case 1:
+	    nscani = max (1, min (nscan, nl) + 1)
+	    nscanr = nscani
+	    call imseti (in, IM_NBUFS, nscani)
+	    call malloc (bufs, nscani, TY_INT)
+	    call calloc (data, nc, TY_REAL)
+	    j = 1
+	    k = 1
+	    l = 1
+
+	    # Ramp up
+	    while (j <= nscani) {
+		i = j + l1 - 1
+		datain = imgl2r (in, i)
+		if (nc < len1)
+		    call amovr (Memr[datain], Memr[impl2r(out,i)], len1)
+		datain = datain + c1 - 1
+		Memi[bufs+mod(j,nscani)] = datain
+	        call aaddr (Memr[data], Memr[datain], Memr[data], nc)
+	        j = j + 1
+	    }
+	    dataout = impl2r (out, l+l1-1) + c1 - 1
+	    call adivkr (Memr[data], nscanr, Memr[dataout], nc)
+	    if (replace)
+		call amaxkr (Memr[dataout], minreplace, Memr[dataout], nc)
+	    mean = mean + asumr (Memr[dataout], nc)
+	    l = l + 1
+
+	    # Moving average
+	    while (j <= nl) {
+		datain = Memi[bufs+mod(k,nscani)]
+	        call asubr (Memr[data], Memr[datain], Memr[data], nc)
+		i = j + l1 - 1
+		datain = imgl2r (in, i)
+		if (nc < len1)
+		    call amovr (Memr[datain], Memr[impl2r(out,i)], len1)
+		datain = datain + c1 - 1
+		Memi[bufs+mod(j,nscani)] = datain
+	        call aaddr (Memr[data], Memr[datain], Memr[data], nc)
+		dataout = impl2r (out, l+l1-1) + c1 - 1
+		call adivkr (Memr[data], nscanr, Memr[dataout], nc)
+		if (replace)
+		    call amaxkr (Memr[dataout], minreplace, Memr[dataout], nc)
+		mean = mean + asumr (Memr[dataout], nc)
+
+	        j = j + 1
+	        k = k + 1
+	        l = l + 1
+	    }
+
+	    # Ramp down.
+	    while (l <= nl) {
+		datain = Memi[bufs+mod(k,nscani)]
+	        call asubr (Memr[data], Memr[datain], Memr[data], nc)
+		dataout = impl2r (out, l+l1-1) + c1 - 1
+		call adivkr (Memr[data], nscanr, Memr[dataout], nc)
+		if (replace)
+		    call amaxkr (Memr[dataout], minreplace, Memr[dataout], nc)
+		mean = mean + asumr (Memr[dataout], nc)
+
+	        k = k + 1
+	        l = l + 1
+	    }
+
+	    call mfree (bufs, TY_INT)
+	    call mfree (data, TY_REAL)
+
+	case 2:
+	    nscani = max (1, min (nscan, nc) + 1)
+	    nscanr = nscani
+	    do i = 1, nl {
+	        datain = imgl2r (in, i + l1 - 1)
+		datain = datain + c1 - 1
+	        data = impl2r (out, i + l1 - 1)
+		call amovr (Memr[datain], Memr[data], len1)
+		datain = datain + c1 - 1
+		data = data + c1 - 1
+		sum = 0
+		j = 0
+		k = 0
+		l = 0
+
+		# Ramp up
+		while (j < nscani) {
+		    sum = sum + Memr[datain+j]
+		    j = j + 1
+		}
+		if (replace)
+		    Memr[data] = max (minreplace, sum / nscani)
+		else
+		    Memr[data] = sum / nscani
+		mean = mean + Memr[data]
+		l = l + 1
+
+		# Moving average
+		while (j < nl) {
+		    sum = sum + Memr[datain+j] - Memr[datain+k]
+		    if (replace)
+			Memr[data+l] = max (minreplace, sum / nscani)
+		    else
+			Memr[data+l] = sum / nscani
+		    mean = mean + Memr[data+l]
+		    j = j + 1
+		    k = k + 1
+		    l = l + 1
+		}
+
+		# Ramp down
+		while (l < nl) {
+		    sum = sum - Memr[datain+k]
+		    if (replace)
+			Memr[data+l] = max (minreplace, sum / nscani)
+		    else
+			Memr[data+l] = sum / nscani
+		    mean = mean + Memr[data+l]
+		    k = k + 1
+		    l = l + 1
+		}
+	    }
+	}
+
+	# Copy final lines.
+	do i = l2+1, len2
+	    call amovr (Memr[imgl2r(in,i)], Memr[impl2r(out,i)], len1)
+
+	mean = mean / nc / nl
+	call hdmputr (out, "ccdmean", mean)
+	call hdmputi (out, "ccdmeant", int (clktime (long (0))))
+
+	call sfree (sp)
+end
+
+
+# LONGSCAN -- Make a longscan mode readout flat field correction by averaging
+# across the readout axis.
+
+procedure longscan (in, out, readaxis)
+
+pointer	in		# Input image
+pointer	out		# Output image
+int	readaxis	# Readout axis
+
+int	i, nc, nl, c1, c2, cs, l1, l2, ls
+int	in_c1, in_c2, in_l1, in_l2, ccd_c1, ccd_c2, ccd_l1, ccd_l2
+real	mean, asumr()
+long	clktime()
+pointer	sp, str, data, imgl2r(), impl2r(), imps2r()
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# The default data section is the entire image.
+	nc = IM_LEN(in,1)
+	nl = IM_LEN(in,2)
+	c1 = 1
+	c2 = nc
+	cs = 1
+	l1 = 1
+	l2 = nl
+	ls = 1
+	call hdmgstr (in, "datasec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1))
+	    call error (0, "Error in DATASEC parameter")
+	in_c1 = c1
+	in_c2 = c2
+	in_l1 = l1
+	in_l2 = l2
+
+	# The default ccd section is the data section.
+	call hdmgstr (in, "ccdsec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((cs != 1) || (ls != 1))
+	    call error (0, "Error in CCDSEC parameter")
+	ccd_c1 = c1
+	ccd_c2 = c2
+	ccd_l1 = l1
+	ccd_l2 = l2
+	if ((in_c2-in_c1 != ccd_c2-ccd_c1) || (in_l2-in_l1 != ccd_l2-ccd_l1))
+	    call error (0, "Size of DATASEC and CCDSEC do not agree")
+
+	switch (readaxis) {
+	case 1:
+	    IM_LEN(out,2) = 1
+	    data = impl2r (out, 1)
+	    call aclrr (Memr[data], nc)
+	    nc = in_c2 - in_c1 + 1
+	    nl = in_l2 - in_l1 + 1
+	    data = data + in_c1 - 1
+	    do i = in_l1, in_l2
+		call aaddr (Memr[imgl2r(in,i)+in_c1-1], Memr[data],
+		    Memr[data], nc)
+	    call adivkr (Memr[data], real (nl), Memr[data], nc)
+	    call sprintf (Memc[str], SZ_LINE, "[%d:%d,1:1]")
+		call pargi (in_c1)
+		call pargi (in_c2)
+	    call hdmpstr (out, "datasec", Memc[str])
+	    call sprintf (Memc[str], SZ_LINE, "[%d:%d,*]")
+		call pargi (ccd_c1)
+		call pargi (ccd_c2)
+	    call hdmpstr (out, "ccdsec", Memc[str])
+	    mean = asumr (Memr[data], nc) / nl
+	case 2:
+	    IM_LEN(out,1) = 1
+	    data = imps2r (out, 1, 1, 1, nl)
+	    call aclrr (Memr[data], nl)
+	    nc = in_c2 - in_c1 + 1
+	    nl = in_l2 - in_l1 + 1
+	    do i = in_l1, in_l2
+		Memr[data+i-1] = asumr (Memr[imgl2r(in,i)+in_c1-1], nc) / nc
+	    call sprintf (Memc[str], SZ_LINE, "[1:1,%d:%d]")
+		call pargi (in_l1)
+		call pargi (in_l2)
+	    call hdmpstr (out, "datasec", Memc[str])
+	    call sprintf (Memc[str], SZ_LINE, "[*,%d:%d]")
+		call pargi (ccd_l1)
+		call pargi (ccd_l2)
+	    call hdmpstr (out, "ccdsec", Memc[str])
+	    mean = asumr (Memr[data], nl) / nc
+	}
+
+	call hdmputr (out, "ccdmean", mean)
+	call hdmputi (out, "ccdmeant", int (clktime (long (0))))
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/setdark.x b/noao/imred/ccdred/src/setdark.x
new file mode 100644
index 00000000..c872aba4
--- /dev/null
+++ b/noao/imred/ccdred/src/setdark.x
@@ -0,0 +1,160 @@
+include	<imhdr.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+
+# SET_DARK -- Set parameters for dark count correction.
+#
+#   1.  Return immediately if the dark count correction is not requested or
+#	if the image has been previously corrected.
+#   2.  Get the dark count correction image and return an error if not found.
+#   3.  If the dark count image has not been processed call PROC.
+#   4.  Compute the dark count integration time scale factor.
+#   5.  Set the processing flags.
+#   6.  Log the operation (to user, logfile, and output image header).
+
+procedure set_dark (ccd)
+
+pointer	ccd			# CCD structure
+
+int	nscan, nc, nl, c1, c2, cs, l1, l2, ls, data_c1, ccd_c1, data_l1, ccd_l1
+real	darktime1, darktime2
+pointer	sp, image, str, im
+
+bool	clgetb(), ccdflag(), ccdcheck()
+int	ccdnscan(), ccdtypei()
+real	hdmgetr()
+pointer	ccd_cache()
+errchk	cal_image, ccd_cache, ccdproc, hdmgetr
+
+begin
+	# Check if the user wants this operation or it has already been done.
+	if (!clgetb ("darkcor") || ccdflag (IN_IM(ccd), "darkcor"))
+	    return
+
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the dark count correction image name.
+	if (clgetb ("scancor"))
+	    nscan = ccdnscan (IN_IM(ccd), ccdtypei(IN_IM(ccd)))
+	else
+	    nscan = 1
+	call cal_image (IN_IM(ccd), DARK, nscan, Memc[image], SZ_FNAME)
+
+	# If no processing is desired print dark count image and return.
+	if (clgetb ("noproc")) {
+	    call eprintf ("  [TO BE DONE] Dark count correction image is %s.\n")
+	        call pargstr (Memc[image])
+	    call sfree (sp)
+	    return
+	}
+
+	# Map the image and return on an error.
+	# Process the dark count image if necessary.
+	# If nscan > 1 then the dark may not yet exist so create it
+	# from the unscanned dark.
+
+	iferr (im = ccd_cache (Memc[image], DARK)) {
+	    call cal_image (IN_IM(ccd), DARK, 1, Memc[str], SZ_LINE)
+	    im = ccd_cache (Memc[str], DARK)
+	    if (ccdcheck (im, DARK)) {
+		call ccd_flush (im)
+		call ccdproc (Memc[str], DARK)
+	    }
+	    call scancor (Memc[str], Memc[image], nscan, INDEF)
+	    im = ccd_cache (Memc[image], DARK)
+	}
+
+	if (ccdcheck (im, DARK)) {
+	    call ccd_flush (im)
+	    call ccdproc (Memc[image], DARK)
+	    im = ccd_cache (Memc[image], DARK)
+	}
+
+	# Set the processing parameters in the CCD structure.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	c1 = 1
+	c2 = nc
+	l1 = 1
+	l2 = nl
+	cs = 1
+	ls = 1
+	call hdmgstr (im, "datasec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1)) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Data section error: image=%s[%d,%d], datasec=[%d:%d,%d:%d]")
+		call pargstr (Memc[image])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+	data_c1 = c1
+	data_l1 = l1
+	call hdmgstr (im, "ccdsec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if (nc == 1) {
+	    c1 = CCD_C1(ccd)
+	    c2 = CCD_C2(ccd)
+	}
+	if (nl == 1) {
+	    l1 = CCD_L1(ccd)
+	    l2 = CCD_L2(ccd)
+	}
+	ccd_c1 = c1
+	ccd_l1 = l1
+	if ((c1 > CCD_C1(ccd)) || (c2 < CCD_C2(ccd)) ||
+	    (l1 > CCD_L1(ccd)) || (l2 < CCD_L2(ccd))) {
+	    call sprintf (Memc[str], SZ_LINE,
+	        "CCD section error: input=[%d:%d,%d:%d], %s=[%d:%d,%d:%d]")
+		call pargi (CCD_C1(ccd))
+		call pargi (CCD_C2(ccd))
+		call pargi (CCD_L1(ccd))
+		call pargi (CCD_L2(ccd))
+		call pargstr (Memc[image])
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+
+	DARK_IM(ccd) = im
+	DARK_C1(ccd) = CCD_C1(ccd) - ccd_c1 + data_c1
+	DARK_C2(ccd) = CCD_C2(ccd) - ccd_c1 + data_c1
+	DARK_L1(ccd) = CCD_L1(ccd) - ccd_l1 + data_l1
+	DARK_L2(ccd) = CCD_L2(ccd) - ccd_l1 + data_l1
+
+	# Get the dark count integration times.  Return an error if not found.
+	iferr (darktime1 = hdmgetr (IN_IM(ccd), "darktime"))
+	    darktime1 = hdmgetr (IN_IM(ccd), "exptime")
+	iferr (darktime2 = hdmgetr (im, "darktime"))
+	    darktime2 = hdmgetr (im, "exptime")
+	if (darktime2 <= 0.) {
+	    call sprintf (Memc[str], SZ_LINE, "Dark time is zero for `%s'")
+		call pargstr (Memc[image])
+	    call error (1, Memc[str])
+	}
+
+	DARKSCALE(ccd) = darktime1 / darktime2
+	CORS(ccd, DARKCOR) = D
+	COR(ccd) = YES
+
+	# Record the operation in the output image and write a log record.
+	call sprintf (Memc[str], SZ_LINE,
+	    "Dark count correction image is %s with scale=%g")
+	    call pargstr (Memc[image])
+	    call pargr (DARKSCALE(ccd))
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "darkcor", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/setfixpix.x b/noao/imred/ccdred/src/setfixpix.x
new file mode 100644
index 00000000..e6b96298
--- /dev/null
+++ b/noao/imred/ccdred/src/setfixpix.x
@@ -0,0 +1,74 @@
+include	<imhdr.h>
+include	<imset.h>
+include	<pmset.h>
+include	"ccdred.h"
+
+
+# SET_FIXPIX -- Set parameters for bad pixel correction.
+#   1.  Return immediately if the bad pixel correction is not requested or
+#	if the image has been previously corrected.
+#   2.	Get the bad pixel mask.  Return an error if not found.
+#   3.	If the bad pixel mask has not been processed call PROC.
+#   4.	Set the processing flag.
+#   5.  Log the operation (to user, logfile, and output image header).
+#
+# This routine relies on the physical coordinate system and assumes
+# XT_PMMAP has taken care of matching the pixel mask to the input image.
+
+procedure set_fixpix (ccd)
+
+pointer	ccd			# CCD structure
+
+pointer	sp, image, str, im
+
+int	imstati()
+bool	clgetb(), streq(), ccdflag()
+pointer	xt_pmmap(), xt_fpinit()
+errchk	xt_pmmap(), xt_fpinit()
+
+begin
+	# Check if the user wants this operation or it has been done.
+	if (!clgetb ("fixpix") || ccdflag (IN_IM(ccd), "fixpix"))
+	    return
+
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the bad pixel file.  If the name is "image" then get the file
+	# name from the image header or symbol table.
+
+	call clgstr ("fixfile", Memc[image], SZ_FNAME)
+	if (streq (Memc[image], "image"))
+	    call hdmgstr (IN_IM(ccd), "fixfile", Memc[image], SZ_FNAME)
+
+	# If no processing is desired print message and return.
+	if (clgetb ("noproc")) {
+	    call eprintf ("  [TO BE DONE] Bad pixel file is %s\n")
+		call pargstr (Memc[image])
+	    call sfree (sp)
+	    return
+	}
+
+	# Map the bad pixel image and return on an error.
+	im = xt_pmmap (Memc[image], IN_IM(ccd), Memc[image], SZ_FNAME)
+	if (Memc[image] == EOS)
+	    call error (1, "No bad pixel mask found")
+	if (im != NULL)  {
+	    MASK_IM(ccd) = im
+	    MASK_PM(ccd) = imstati (im, IM_PMDES)
+	    MASK_FP(ccd) = xt_fpinit (MASK_PM(ccd), 2, 3)
+
+	    CORS(ccd, FIXPIX) = YES
+	    COR(ccd) = YES
+	}
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE, "Bad pixel file is %s")
+	    call pargstr (Memc[image])
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "fixpix", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/setflat.x b/noao/imred/ccdred/src/setflat.x
new file mode 100644
index 00000000..87713404
--- /dev/null
+++ b/noao/imred/ccdred/src/setflat.x
@@ -0,0 +1,146 @@
+include	<imhdr.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+# SET_FLAT -- Set parameters for flat field correction.
+#
+#   1.  Return immediately if the flat field correction is not requested or
+#	if the image has been previously corrected.
+#   2.  Get the flat field image and return on an error.
+#   3.  If the flat field image has not been processed call PROC.
+#   4.  Set the processing flags and record the operation in the output
+#   	image and write a log record.
+
+procedure set_flat (ccd)
+
+pointer	ccd			# CCD structure
+
+int	nc, nl, c1, c2, cs, l1, l2, ls, data_c1, ccd_c1, data_l1, ccd_l1
+pointer	sp, str, image, im, ccd_cache()
+bool	clgetb(), ccdflag(), ccdcheck()
+int	nscan, ccdnscan(), ccdtypei()
+real	hdmgetr()
+errchk	cal_image, ccd_cache, ccdproc, hdmgetr
+
+begin
+	# Check if the user wants this operation or if it has been done.
+	if (!clgetb ("flatcor") || ccdflag (IN_IM(ccd), "flatcor"))
+	    return
+
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the flat field correction image.
+	if (clgetb ("scancor"))
+	    nscan = ccdnscan (IN_IM(ccd), ccdtypei(IN_IM(ccd)))
+	else
+	    nscan = 1
+	call cal_image (IN_IM(ccd), FLAT, nscan, Memc[image], SZ_FNAME)
+
+	# If no processing is desired print flat field image name and return.
+	if (clgetb ("noproc")) {
+	    call eprintf ("  [TO BE DONE] Flat correction image is %s.\n")
+		call pargstr (Memc[image])
+	    call sfree (sp)
+	    return
+	}
+
+	# Map the image and return on an error.
+	# Process the flat field image if necessary.
+	# If nscan > 1 then the flat field may not yet exist so create it
+	# from the unscanned flat field.
+
+	iferr (im = ccd_cache (Memc[image], FLAT)) {
+	    call cal_image (IN_IM(ccd), FLAT, 1, Memc[str], SZ_LINE)
+	    im = ccd_cache (Memc[str], FLAT)
+	    if (ccdcheck (im, FLAT)) {
+		call ccd_flush (im)
+		call ccdproc (Memc[str], FLAT)
+	    }
+	    call scancor (Memc[str], Memc[image], nscan, MINREPLACE(ccd))
+	    im = ccd_cache (Memc[image], FLAT)
+	}
+
+	if (ccdcheck (im, FLAT)) {
+	    call ccd_flush (im)
+	    call ccdproc (Memc[image], FLAT)
+	    im = ccd_cache (Memc[image], FLAT)
+	}
+
+	# Set the processing parameters in the CCD structure.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	c1 = 1
+	c2 = nc
+	l1 = 1
+	l2 = nl
+	cs = 1
+	ls = 1
+	call hdmgstr (im, "datasec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1)) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Data section error: image=%s[%d,%d], datasec=[%d:%d,%d:%d]")
+		call pargstr (Memc[image])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+	data_c1 = c1
+	data_l1 = l1
+	call hdmgstr (im, "ccdsec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if (nc == 1) {
+	    c1 = CCD_C1(ccd)
+	    c2 = CCD_C2(ccd)
+	}
+	if (nl == 1) {
+	    l1 = CCD_L1(ccd)
+	    l2 = CCD_L2(ccd)
+	}
+	ccd_c1 = c1
+	ccd_l1 = l1
+	if ((c1 > CCD_C1(ccd)) || (c2 < CCD_C2(ccd)) ||
+	    (l1 > CCD_L1(ccd)) || (l2 < CCD_L2(ccd))) {
+	    call sprintf (Memc[str], SZ_LINE,
+	        "CCD section error: input=[%d:%d,%d:%d], %s=[%d:%d,%d:%d]")
+		call pargi (CCD_C1(ccd))
+		call pargi (CCD_C2(ccd))
+		call pargi (CCD_L1(ccd))
+		call pargi (CCD_L2(ccd))
+		call pargstr (Memc[image])
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+
+	FLAT_IM(ccd) = im
+	FLAT_C1(ccd) = CCD_C1(ccd) - ccd_c1 + data_c1
+	FLAT_C2(ccd) = CCD_C2(ccd) - ccd_c1 + data_c1
+	FLAT_L1(ccd) = CCD_L1(ccd) - ccd_l1 + data_l1
+	FLAT_L2(ccd) = CCD_L2(ccd) - ccd_l1 + data_l1
+
+	# If no mean value use 1 as the scale factor.
+	iferr (FLATSCALE(ccd) = hdmgetr (im, "ccdmean"))
+	    FLATSCALE(ccd) = 1.
+	CORS(ccd, FLATCOR) = F
+	COR(ccd) = YES
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE,
+	    "Flat field image is %s with scale=%g")
+	    call pargstr (Memc[image])
+	    call pargr (FLATSCALE(ccd))
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "flatcor", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/setfringe.x b/noao/imred/ccdred/src/setfringe.x
new file mode 100644
index 00000000..7055f35f
--- /dev/null
+++ b/noao/imred/ccdred/src/setfringe.x
@@ -0,0 +1,123 @@
+include	<imhdr.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+# SET_FRINGE -- Set parameters for fringe correction.
+#
+#   1.  Return immediately if the fringe correction is not requested or
+#	if the image has been previously corrected.
+#   2.  Get the fringe image and return error if the mkfringe flag is missing.
+#   3.  Set the processing flags and record the operation in the output
+#   	image and write a log record.
+
+procedure set_fringe (ccd)
+
+pointer	ccd			# CCD structure
+
+int	nc, nl, c1, c2, cs, l1, l2, ls, data_c1, ccd_c1, data_l1, ccd_l1
+real	exptime1, exptime2, fringescale
+pointer	sp, str, image, im
+
+bool	clgetb(), ccdflag()
+real	hdmgetr()
+pointer	ccd_cache()
+errchk	cal_image, ccd_cache, ccdproc, hdmgetr
+
+begin
+	# Check if the user wants this operation or if it has been done.
+	if (!clgetb ("fringecor") || ccdflag (IN_IM(ccd), "fringcor"))
+	    return
+
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the fringe correction image.
+	call cal_image (IN_IM(ccd), FRINGE, 1, Memc[image], SZ_FNAME)
+
+	# If no processing is desired print fringe image name and return.
+	if (clgetb ("noproc")) {
+	    call eprintf (
+		"  [TO BE DONE] Fringe correction image is %s.\n")
+		call pargstr (Memc[image])
+	    call sfree (sp)
+	    return
+	}
+
+	# Return an error if the fringe flag is missing.
+	im = ccd_cache (Memc[image], FRINGE)
+	if (!ccdflag (im, "mkfringe"))
+	    call error (0, "MKFRINGE flag missing from fringe image.")
+
+	# Set the processing parameters in the CCD structure.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	c1 = 1
+	c2 = nc
+	l1 = 1
+	l2 = nl
+	cs = 1
+	ls = 1
+	call hdmgstr (im, "datasec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1)) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Data section error: image=%s[%d,%d], datasec=[%d:%d,%d:%d]")
+		call pargstr (Memc[image])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+	data_c1 = c1
+	data_l1 = l1
+	call hdmgstr (im, "ccdsec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	ccd_c1 = c1
+	ccd_l1 = l1
+	if ((c1 > CCD_C1(ccd)) || (c2 < CCD_C2(ccd)) ||
+	    (l1 > CCD_L1(ccd)) || (l2 < CCD_L2(ccd))) {
+	    call sprintf (Memc[str], SZ_LINE,
+	        "CCD section error: input=[%d:%d,%d:%d], %s=[%d:%d,%d:%d]")
+		call pargi (CCD_C1(ccd))
+		call pargi (CCD_C2(ccd))
+		call pargi (CCD_L1(ccd))
+		call pargi (CCD_L2(ccd))
+		call pargstr (Memc[image])
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+
+	FRINGE_IM(ccd) = im
+	FRINGE_C1(ccd) = CCD_C1(ccd) - ccd_c1 + data_c1
+	FRINGE_C2(ccd) = CCD_C2(ccd) - ccd_c1 + data_c1
+	FRINGE_L1(ccd) = CCD_L1(ccd) - ccd_l1 + data_l1
+	FRINGE_L2(ccd) = CCD_L2(ccd) - ccd_l1 + data_l1
+
+	# Get the scaling factors.  If no fringe scale factor assume 1.
+	exptime1 = hdmgetr (IN_IM(ccd), "exptime")
+	exptime2 = hdmgetr (im, "exptime")
+	iferr (fringescale = hdmgetr (im, "fringscl"))
+	    fringescale = 1.
+
+	FRINGESCALE(ccd) = exptime1 / exptime2 * fringescale
+	CORS(ccd, FRINGECOR) = Q
+	COR(ccd) = YES
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE,
+	    "Fringe image is %s with scale=%g")
+	    call pargstr (Memc[image])
+	    call pargr (FRINGESCALE(ccd))
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "fringcor", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/setheader.x b/noao/imred/ccdred/src/setheader.x
new file mode 100644
index 00000000..aa13730a
--- /dev/null
+++ b/noao/imred/ccdred/src/setheader.x
@@ -0,0 +1,83 @@
+include	<imhdr.h>
+include	"ccdred.h"
+
+# SET_HEADER -- Set the output image header.
+
+procedure set_header (ccd)
+
+pointer	ccd			# CCD structure
+
+int	nc, nl
+real	shift[2]
+pointer	sp, str, out, mw, mw_openim()
+long	clktime()
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	out = OUT_IM(ccd)
+	nc = IM_LEN(out,1)
+	nl = IM_LEN(out,2)
+
+	# Set the data section if it is not the whole image.
+	if ((OUT_C1(ccd) != 1) || (OUT_C2(ccd) != nc) ||
+	    (OUT_L1(ccd) != 1) || (OUT_L2(ccd) != nl)) {
+	    call sprintf (Memc[str], SZ_LINE, "[%d:%d,%d:%d]")
+	        call pargi (OUT_C1(ccd))
+	        call pargi (OUT_C2(ccd))
+	        call pargi (OUT_L1(ccd))
+	        call pargi (OUT_L2(ccd))
+	    call hdmpstr (out, "datasec", Memc[str])
+	} else {
+	    iferr (call hdmdelf (out, "datasec"))
+		;
+	}
+
+	# Set the CCD section.
+	call sprintf (Memc[str], SZ_LINE, "[%d:%d,%d:%d]")
+	    call pargi (CCD_C1(ccd))
+	    call pargi (CCD_C2(ccd))
+	    call pargi (CCD_L1(ccd))
+	    call pargi (CCD_L2(ccd))
+	call hdmpstr (out, "ccdsec", Memc[str])
+
+	# If trimming update the trim and bias section parameters.
+	if (CORS(ccd, TRIM) == YES) {
+	    iferr (call hdmdelf (out, "trimsec"))
+	        ;
+	    iferr (call hdmdelf (out, "biassec"))
+	        ;
+	    BIAS_C1(ccd) = max (1, BIAS_C1(ccd) - TRIM_C1(ccd) + 1)
+	    BIAS_C2(ccd) = min (nc, BIAS_C2(ccd) - TRIM_C1(ccd) + 1)
+	    BIAS_L1(ccd) = max (1, BIAS_L1(ccd) - TRIM_L1(ccd) + 1)
+	    BIAS_L2(ccd) = min (nl, BIAS_L2(ccd) - TRIM_L1(ccd) + 1)
+	    if ((BIAS_C1(ccd)<=BIAS_C2(ccd)) && (BIAS_L1(ccd)<=BIAS_L2(ccd))) {
+		call sprintf (Memc[str], SZ_LINE, "[%d:%d,%d:%d]")
+		    call pargi (BIAS_C1(ccd))
+		    call pargi (BIAS_C2(ccd))
+		    call pargi (BIAS_L1(ccd))
+		    call pargi (BIAS_L2(ccd))
+		call hdmpstr (out, "biassec", Memc[str])
+	    }
+
+	    mw = mw_openim (out)
+	    shift[1] = 1 - IN_C1(ccd)
+	    shift[2] = 1 - IN_L1(ccd)
+	    call mw_shift (mw, shift, 3)
+	    call mw_saveim (mw, out)
+	}
+
+	# Set mean value if desired.
+	if (CORS(ccd, FINDMEAN) == YES) {
+	    call hdmputr (out, "ccdmean", MEAN(ccd))
+	    call hdmputi (out, "ccdmeant", int (clktime (long (0))))
+	}
+
+	# Mark image as processed.
+	call sprintf (Memc[str], SZ_LINE, "CCD processing done")
+	call timelog (Memc[str], SZ_LINE)
+	call hdmpstr (out, "ccdproc", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/setillum.x b/noao/imred/ccdred/src/setillum.x
new file mode 100644
index 00000000..d1677301
--- /dev/null
+++ b/noao/imred/ccdred/src/setillum.x
@@ -0,0 +1,132 @@
+include	<imhdr.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+# SET_ILLUM -- Set parameters for illumination correction.
+#
+#   1.  Return immediately if the illumination correction is not requested or
+#	if the image has been previously corrected.
+#   2.  Get the illumination image and return error if mkillum flag missing.
+#   3.  Set the processing flags and record the operation in the output
+#   	image and write a log record.
+
+procedure set_illum (ccd)
+
+pointer	ccd			# CCD structure
+
+int	nc, nl, c1, c2, cs, l1, l2, ls, data_c1, ccd_c1, data_l1, ccd_l1
+long	time
+pointer	sp, str, image, im
+
+bool	clgetb(), ccdflag()
+long	hdmgeti()
+real	hdmgetr()
+pointer	ccd_cache()
+errchk	cal_image, ccd_cache, ccdproc, hdmgetr, hdmgeti
+
+begin
+	# Check if the user wants this operation or if it has been done.
+	if (!clgetb ("illumcor") || ccdflag (IN_IM(ccd), "illumcor"))
+	    return
+
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the illumcor correction image.
+	call cal_image (IN_IM(ccd), ILLUM, 1, Memc[image], SZ_FNAME)
+
+	# If no processing is desired print illumination image name and return.
+	if (clgetb ("noproc")) {
+	    call eprintf (
+		"  [TO BE DONE] Illumination correction image is %s.\n")
+		call pargstr (Memc[image])
+	    call sfree (sp)
+	    return
+	}
+
+	# Return a warning if the illumination flag is missing.
+	im = ccd_cache (Memc[image], ILLUM)
+	if (!ccdflag (im, "mkillum")) {
+	    call ccd_flush (im)
+	    call error (0, "MKILLUM flag missing from illumination image")
+	}
+
+	# If no mean value for the scale factor compute it.
+	iferr (ILLUMSCALE(ccd) = hdmgetr (im, "ccdmean"))
+	    ILLUMSCALE(ccd) = INDEF
+	iferr (time = hdmgeti (im, "ccdmeant"))
+	    time = IM_MTIME(im)
+	if (IS_INDEF(ILLUMSCALE(ccd)) || time < IM_MTIME(im)) {
+	    call ccd_flush (im)
+	    call ccdmean (Memc[image])
+	    im = ccd_cache (Memc[image], ILLUM)
+	}
+	iferr (ILLUMSCALE(ccd) = hdmgetr (im, "ccdmean"))
+	    ILLUMSCALE(ccd) = 1.
+ 
+	# Set the processing parameters in the CCD structure.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	c1 = 1
+	c2 = nc
+	l1 = 1
+	l2 = nl
+	cs = 1
+	ls = 1
+	call hdmgstr (im, "datasec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1)) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Data section error: image=%s[%d,%d], datasec=[%d:%d,%d:%d]")
+		call pargstr (Memc[image])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+	data_c1 = c1
+	data_l1 = l1
+	call hdmgstr (im, "ccdsec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	ccd_c1 = c1
+	ccd_l1 = l1
+	if ((c1 > CCD_C1(ccd)) || (c2 < CCD_C2(ccd)) ||
+	    (l1 > CCD_L1(ccd)) || (l2 < CCD_L2(ccd))) {
+	    call sprintf (Memc[str], SZ_LINE,
+	        "CCD section error: input=[%d:%d,%d:%d], %s=[%d:%d,%d:%d]")
+		call pargi (CCD_C1(ccd))
+		call pargi (CCD_C2(ccd))
+		call pargi (CCD_L1(ccd))
+		call pargi (CCD_L2(ccd))
+		call pargstr (Memc[image])
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+
+	ILLUM_IM(ccd) = im
+	ILLUM_C1(ccd) = CCD_C1(ccd) - ccd_c1 + data_c1
+	ILLUM_C2(ccd) = CCD_C2(ccd) - ccd_c1 + data_c1
+	ILLUM_L1(ccd) = CCD_L1(ccd) - ccd_l1 + data_l1
+	ILLUM_L2(ccd) = CCD_L2(ccd) - ccd_l1 + data_l1
+
+	CORS(ccd, ILLUMCOR) = I
+	COR(ccd) = YES
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE,
+	    "Illumination image is %s with scale=%g")
+	    call pargstr (Memc[image])
+	    call pargr (ILLUMSCALE(ccd))
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "illumcor", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/setinput.x b/noao/imred/ccdred/src/setinput.x
new file mode 100644
index 00000000..3d3170db
--- /dev/null
+++ b/noao/imred/ccdred/src/setinput.x
@@ -0,0 +1,48 @@
+include	<error.h>
+include	"ccdtypes.h"
+
+# SET_INPUT -- Set the input image and image type.
+#
+# 1.  Open the input image.  Return warning and NULL pointer for an error.
+# 2.  Get the requested CCD image type.
+#	a. If no type is requested then accept the image.
+#	b. If a type is requested then match against the image type.
+#	   Unmap the image if no match.
+# 3.  If the image is acceptable then get the CCD type code.
+
+procedure set_input (image, im, ccdtype)
+
+char	image[ARB]	# Input image name
+pointer	im		# IMIO pointer (returned)
+int	ccdtype		# CCD image type
+
+bool	strne()
+int	ccdtypei()
+pointer	sp, str1, str2, immap()
+
+begin
+	# Open the image.  Return a warning and NULL pointer for an error.
+	iferr (im = immap (image, READ_ONLY, 0)) {
+	    call erract (EA_WARN)
+	    im = NULL
+	    return
+	}
+
+	call smark (sp)
+	call salloc (str1, SZ_LINE, TY_CHAR)
+	call salloc (str2, SZ_LINE, TY_CHAR)
+
+	# Get the requested CCD type.
+	call clgstr ("ccdtype", Memc[str1], SZ_LINE)
+	call xt_stripwhite (Memc[str1])
+	if (Memc[str1] != EOS) {
+	    call ccdtypes (im, Memc[str2], SZ_LINE)
+	    if (strne (Memc[str1], Memc[str2]))
+		call imunmap (im)
+	}
+
+	if (im != NULL)
+	    ccdtype = ccdtypei (im)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/setinteract.x b/noao/imred/ccdred/src/setinteract.x
new file mode 100644
index 00000000..05bc0f71
--- /dev/null
+++ b/noao/imred/ccdred/src/setinteract.x
@@ -0,0 +1,31 @@
+include	<pkg/xtanswer.h>
+
+# SET_INTERACTIVE -- Set the interactive flag.  Query the user if necessary.
+#
+# This procedure initializes the interactive flag if there is no query.
+# If there is a query it is issued by XT_ANSWER.   The four valued
+# interactive flag is returned.
+
+procedure set_interactive (query, interactive)
+
+char	query[ARB]		# Query prompt
+int	interactive		# Fit overscan interactively?  (returned)
+
+int	interact		# Saves last value of interactive flag
+bool	clgetb()
+
+begin
+	# If the query is null then initialize from the CL otherwise
+	# query the user.  This response is four valued to allow the user
+	# to turn off the query when processing multiple images.
+
+	if (query[1] == EOS) {
+	    if (clgetb ("interactive"))
+	        interact = YES
+	    else
+	        interact = ALWAYSNO
+	} else
+	    call xt_answer (query, interact)
+
+	interactive = interact
+end
diff --git a/noao/imred/ccdred/src/setoutput.x b/noao/imred/ccdred/src/setoutput.x
new file mode 100644
index 00000000..b401b5aa
--- /dev/null
+++ b/noao/imred/ccdred/src/setoutput.x
@@ -0,0 +1,52 @@
+include	<imhdr.h>
+include	<imset.h>
+
+# SET_OUTPUT -- Setup the output image.
+# The output image is a NEW_COPY of the input image.
+# The user may select a pixel datatype with higher precision though not
+# lower.
+
+procedure set_output (in, out, output)
+
+pointer	in			# Input IMIO pointer to copy
+pointer	out			# Output IMIO pointer
+char	output[SZ_FNAME]	# Output image name
+
+int	i, clscan(), nscan()
+char	type[1]
+pointer	immap()
+errchk	immap
+
+begin
+	out = immap (output, NEW_COPY, in)
+	IM_PIXTYPE(out) = TY_REAL
+	if (clscan ("pixeltype")  != EOF) {
+	    call gargwrd (type, 1)
+	    if (nscan() == 1) {
+		i = IM_PIXTYPE(in)
+		IM_PIXTYPE(out) = i
+		switch (type[1]) {
+		case 's':
+		    if (i == TY_USHORT)
+			IM_PIXTYPE(out) = TY_SHORT
+		case 'u':
+		    if (i == TY_SHORT)
+			IM_PIXTYPE(out) = TY_USHORT
+		case 'i':
+		    if (i == TY_SHORT || i == TY_USHORT)
+			IM_PIXTYPE(out) = TY_INT
+		case 'l':
+		    if (i == TY_SHORT || i == TY_USHORT || i == TY_INT)
+			IM_PIXTYPE(out) = TY_LONG
+		case 'r':
+		    if (i != TY_DOUBLE)
+			IM_PIXTYPE(out) = TY_REAL
+		case 'd':
+		    IM_PIXTYPE(out) = TY_DOUBLE
+		default:
+		    call imunmap (out)
+		    call error (0, "Unknown pixel type")
+		}
+	    }
+	}
+end
diff --git a/noao/imred/ccdred/src/setoverscan.x b/noao/imred/ccdred/src/setoverscan.x
new file mode 100644
index 00000000..e344aa92
--- /dev/null
+++ b/noao/imred/ccdred/src/setoverscan.x
@@ -0,0 +1,310 @@
+include	<imhdr.h>
+include	<imset.h>
+include <pkg/gtools.h>
+include	<pkg/xtanswer.h>
+include	"ccdred.h"
+
+
+# SET_OVERSCAN -- Set the overscan vector.
+#
+#   1.  Return immediately if the overscan correction is not requested or
+#	if the image has been previously corrected.
+#   2.	Determine the overscan columns or lines.  This may be specifed
+#	directly or indirectly through the image header or symbol table.
+#   3.  Determine the type of overscan.
+#   4.	If fitting the overscan average the overscan columns or lines and
+#     	fit a function with the ICFIT routines to smooth the overscan vector.
+#   5.  Set the processing flag.
+#   6.  Log the operation (to user, logfile, and output image header).
+
+procedure set_overscan (ccd)
+
+pointer	ccd			# CCD structure pointer
+
+int	i, first, last, navg, npts, type
+int	nc, nl, c1, c2, l1, l2
+pointer	sp, str, errstr, func, buf, x, overscan
+
+int	clgwrd()
+real	asumr()
+bool	clgetb(), ccdflag()
+pointer	imgl2r(), imgs2r()
+errchk	imgl2r, imgs2r, fit_overscan
+
+begin
+	# Check if the user wants this operation or if it has been done.
+	if (!clgetb ("overscan") || ccdflag (IN_IM(ccd), "overscan"))
+	    return
+
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+	call salloc (errstr, SZ_LINE, TY_CHAR)
+	call salloc (func, SZ_LINE, TY_CHAR)
+	call imstats (IN_IM(ccd), IM_IMAGENAME, Memc[str], SZ_LINE)
+
+	# Check bias section.
+	nc = IM_LEN(IN_IM(ccd),1)
+	nl = IM_LEN(IN_IM(ccd),2)
+	c1 = BIAS_C1(ccd)
+	c2 = BIAS_C2(ccd)
+	l1 = BIAS_L1(ccd)
+	l2 = BIAS_L2(ccd)
+	if ((c1 < 1) || (c2 > nc) || (l1 < 1) || (l2 > nl)) {
+	    call sprintf (Memc[errstr], SZ_LINE,
+		"Error in bias section: image=%s[%d,%d], biassec=[%d:%d,%d:%d]")
+		call pargstr (Memc[str])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[errstr])
+	}
+	if ((c1 == 1) && (c2 == nc) && (l1 == 1) && (l2 == nl)) {
+	    call error (0, "Bias section not specified or given as full image")
+	}
+
+	# If no processing is desired then print overscan strip and return.
+	if (clgetb ("noproc")) {
+	    call eprintf ("  [TO BE DONE] Overscan section is [%d:%d,%d:%d].\n")
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+		call sfree (sp)
+		return
+	}
+
+	# Determine the overscan section parameters. The readout axis
+	# determines the type of overscan.  The step sizes are ignored.
+	# The limits in the long dimension are replaced by the trim limits.
+
+	type = clgwrd ("function", Memc[func], SZ_LINE, OVERSCAN_TYPES)
+	if (type < OVERSCAN_FIT) {
+	    overscan = NULL
+	    if (READAXIS(ccd) == 2)
+		call error (1,
+		    "Overscan function type not allowed with readaxis of 2")
+	} else {
+	    if (READAXIS(ccd) == 1) {
+		first = c1
+		last = c2
+		navg = last - first + 1
+		npts = nl
+		call salloc (buf, npts, TY_REAL)
+		do i = 1, npts
+		    Memr[buf+i-1] = asumr (Memr[imgs2r (IN_IM(ccd), first, last,
+			i, i)], navg)
+		if (navg > 1)
+		    call adivkr (Memr[buf], real (navg), Memr[buf], npts)
+
+		# Trim the overscan vector and set the pixel coordinate.
+		npts = CCD_L2(ccd) - CCD_L1(ccd) + 1
+		call malloc (overscan, npts, TY_REAL)
+		call salloc (x, npts, TY_REAL)
+		call trim_overscan (Memr[buf], npts, IN_L1(ccd), Memr[x],
+		    Memr[overscan])
+
+		call fit_overscan (Memc[str], c1, c2, l1, l2, Memr[x],
+		    Memr[overscan], npts)
+
+	    } else {
+		first = l1
+		last = l2
+		navg = last - first + 1
+		npts = nc
+		call salloc (buf, npts, TY_REAL)
+		call aclrr (Memr[buf], npts)
+		do i = first, last
+		    call aaddr (Memr[imgl2r(IN_IM(ccd),i)], Memr[buf],
+			Memr[buf], npts)
+		if (navg > 1)
+		    call adivkr (Memr[buf], real (navg), Memr[buf], npts)
+
+		# Trim the overscan vector and set the pixel coordinate.
+		npts = CCD_C2(ccd) - CCD_C1(ccd) + 1
+		call malloc (overscan, npts, TY_REAL)
+		call salloc (x, npts, TY_REAL)
+		call trim_overscan (Memr[buf], npts, IN_C1(ccd), Memr[x],
+		    Memr[overscan])
+
+		call fit_overscan (Memc[str], c1, c2, l1, l2, Memr[x],
+		    Memr[overscan], npts)
+	    }
+	}
+	
+	# Set the CCD structure overscan parameters.
+	CORS(ccd, OVERSCAN) = O
+	COR(ccd) = YES
+	OVERSCAN_TYPE(ccd) = type
+	OVERSCAN_VEC(ccd) = overscan
+
+	# Log the operation.
+	if (type < OVERSCAN_FIT) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Overscan section is [%d:%d,%d:%d] with function=%s")
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+		call pargstr (Memc[func])
+	} else {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Overscan section is [%d:%d,%d:%d] with mean=%g")
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+		call pargr (asumr (Memr[overscan], npts) / npts)
+	}
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "overscan", Memc[str])
+
+	call sfree (sp)
+end
+
+
+# FIT_OVERSCAN -- Fit a function to smooth the overscan vector.
+#   The fitting uses the ICFIT procedures which may be interactive.
+#   Changes to these parameters are "learned".  The user is queried with a four
+#   valued logical query (XT_ANSWER routine) which may be turned off when
+#   multiple images are processed.
+
+procedure fit_overscan (image, c1, c2, l1, l2, x, overscan, npts)
+
+char	image[ARB]		# Image name for query and title
+int	c1, c2, l1, l2		# Overscan strip
+real	x[npts]			# Pixel coordinates of overscan
+real	overscan[npts]		# Input overscan and output fitted overscan
+int	npts			# Number of data points
+
+int	interactive, fd
+pointer	sp, str, w, ic, cv, gp, gt
+
+int	clgeti(), ic_geti(), open()
+real	clgetr(), ic_getr()
+pointer	gopen(), gt_init()
+errchk	gopen, open
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+	call salloc (w, npts, TY_REAL)
+	call amovkr (1., Memr[w], npts)
+
+	# Open the ICFIT procedures, get the fitting parameters, and
+	# set the fitting limits.
+
+	call ic_open (ic)
+	call clgstr ("function", Memc[str], SZ_LINE)
+	call ic_pstr (ic, "function", Memc[str])
+	call ic_puti (ic, "order", clgeti ("order"))
+	call clgstr ("sample", Memc[str], SZ_LINE)
+	call ic_pstr (ic, "sample", Memc[str])
+	call ic_puti (ic, "naverage", clgeti ("naverage"))
+	call ic_puti (ic, "niterate", clgeti ("niterate"))
+	call ic_putr (ic, "low", clgetr ("low_reject"))
+	call ic_putr (ic, "high", clgetr ("high_reject"))
+	call ic_putr (ic, "grow", clgetr ("grow"))
+	call ic_putr (ic, "xmin", min (x[1], x[npts]))
+	call ic_putr (ic, "xmax", max (x[1], x[npts]))
+	call ic_pstr (ic, "xlabel", "Pixel")
+	call ic_pstr (ic, "ylabel", "Overscan")
+
+	# If the fitting is done interactively set the GTOOLS and GIO
+	# pointers.  Also "learn" the fitting parameters since they may
+	# be changed when fitting interactively.
+
+	call sprintf (Memc[str], SZ_LINE,
+	    "Fit overscan vector for %s interactively")
+	    call pargstr (image)
+	call set_interactive (Memc[str], interactive)
+	if ((interactive == YES) || (interactive == ALWAYSYES)) {
+	    gt = gt_init ()
+	    call sprintf (Memc[str], SZ_LINE,
+	        "Overscan vector for %s from section [%d:%d,%d:%d]\n")
+	        call pargstr (image)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call gt_sets (gt, GTTITLE, Memc[str])
+	    call gt_sets (gt, GTTYPE, "line")
+	    call gt_setr (gt, GTXMIN, x[1])
+	    call gt_setr (gt, GTXMAX, x[npts])
+	    call clgstr ("graphics", Memc[str], SZ_FNAME)
+	    gp = gopen (Memc[str], NEW_FILE, STDGRAPH)
+
+	    call icg_fit (ic, gp, "cursor", gt, cv, x, overscan, Memr[w], npts)
+
+	    call ic_gstr (ic, "function", Memc[str], SZ_LINE)
+	    call clpstr ("function", Memc[str])
+	    call clputi ("order", ic_geti (ic, "order"))
+	    call ic_gstr (ic, "sample", Memc[str], SZ_LINE)
+	    call clpstr ("sample", Memc[str])
+	    call clputi ("naverage", ic_geti (ic, "naverage"))
+	    call clputi ("niterate", ic_geti (ic, "niterate"))
+	    call clputr ("low_reject", ic_getr (ic, "low"))
+	    call clputr ("high_reject", ic_getr (ic, "high"))
+	    call clputr ("grow", ic_getr (ic, "grow"))
+
+	    call gclose (gp)
+	    call gt_free (gt)
+	} else
+	    call ic_fit (ic, cv, x, overscan, Memr[w], npts, YES, YES, YES, YES)
+
+	# Make a log of the fit in the plot file if given.
+	call clgstr ("plotfile", Memc[str], SZ_LINE)
+	call xt_stripwhite (Memc[str])
+	if (Memc[str] != EOS) {
+	    fd = open (Memc[str], APPEND, BINARY_FILE)
+	    gp = gopen ("stdvdm", NEW_FILE, fd)
+	    gt = gt_init ()
+	    call sprintf (Memc[str], SZ_LINE,
+	        "Overscan vector for %s from section [%d:%d,%d:%d]\n")
+	        call pargstr (image)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call gt_sets (gt, GTTITLE, Memc[str])
+	    call gt_sets (gt, GTTYPE, "line")
+	    call gt_setr (gt, GTXMIN, 1.)
+	    call gt_setr (gt, GTXMAX, real (npts))
+	    call icg_graphr (ic, gp, gt, cv, x, overscan, Memr[w], npts)
+	    call gclose (gp)
+	    call close (fd)
+	    call gt_free (gt)
+	}
+
+	# Replace the raw overscan vector with the smooth fit.
+	call cvvector (cv, x, overscan, npts)
+
+	# Finish up.
+	call ic_closer (ic)
+	call cvfree (cv)
+	call sfree (sp)
+end
+
+
+# TRIM_OVERSCAN -- Trim the overscan vector.
+
+procedure trim_overscan (data, npts, start, x, overscan)
+
+real	data[ARB]		# Full overscan vector
+int	npts			# Length of trimmed vector
+int	start			# Trim start
+real	x[npts]			# Trimmed pixel coordinates (returned)
+real	overscan[npts]		# Trimmed overscan vector (returned)
+
+int	i, j
+
+begin
+	do i = 1, npts {
+	    j = start + i - 1
+	    x[i] = j
+	    overscan[i] = data[j]
+	}
+end
diff --git a/noao/imred/ccdred/src/setproc.x b/noao/imred/ccdred/src/setproc.x
new file mode 100644
index 00000000..06c7977b
--- /dev/null
+++ b/noao/imred/ccdred/src/setproc.x
@@ -0,0 +1,77 @@
+include	<imhdr.h>
+include	"ccdred.h"
+
+# SET_PROC -- Set the processing parameter structure pointer.
+
+procedure set_proc (in, out, ccd)
+
+pointer	in			# Input IMIO pointer
+pointer	out			# Output IMIO pointer
+pointer	ccd			# CCD structure (returned)
+
+int	clgwrd(), clscan(), nscan()
+real	clgetr()
+pointer	sp, str
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Allocate the ccd structure.
+	call calloc (ccd, LEN_CCD, TY_STRUCT)
+
+	IN_IM(ccd) = in
+	OUT_IM(ccd) = out
+	COR(ccd) = NO
+	CORS(ccd, FIXPIX) = NO
+	CORS(ccd, OVERSCAN) = NO
+	CORS(ccd, TRIM) = NO
+	READAXIS(ccd) = clgwrd ("readaxis",Memc[str],SZ_LINE,"|line|columns|")
+	MINREPLACE(ccd) = clgetr ("minreplace")
+
+	CALCTYPE(ccd) = TY_REAL
+	if (clscan ("pixeltype") != EOF) {
+	    call gargwrd (Memc[str], SZ_LINE)
+	    call gargwrd (Memc[str], SZ_LINE)
+	    if (nscan() == 2) {
+	        if (Memc[str] == 'r')
+		    CALCTYPE(ccd) = TY_REAL
+		else if (Memc[str] == 's')
+		    CALCTYPE(ccd) = TY_SHORT
+		else
+		    call error (1, "Invalid calculation datatype")
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# FREE_PROC -- Free the processing structure pointer.
+
+procedure free_proc (ccd)
+
+pointer	ccd			# CCD structure
+
+begin
+	# Unmap calibration images.
+	if (MASK_IM(ccd) != NULL)
+	    call imunmap (MASK_IM(ccd))
+	if (ZERO_IM(ccd) != NULL)
+	    call ccd_unmap (ZERO_IM(ccd))
+	if (DARK_IM(ccd) != NULL)
+	    call ccd_unmap (DARK_IM(ccd))
+	if (FLAT_IM(ccd) != NULL)
+	    call ccd_unmap (FLAT_IM(ccd))
+	if (ILLUM_IM(ccd) != NULL)
+	    call ccd_unmap (ILLUM_IM(ccd))
+	if (FRINGE_IM(ccd) != NULL)
+	    call ccd_unmap (FRINGE_IM(ccd))
+
+	# Free memory
+	if (OVERSCAN_VEC(ccd) != NULL)
+	    call mfree (OVERSCAN_VEC(ccd), TY_REAL)
+	if (MASK_FP(ccd) != NULL)
+	    call xt_fpfree (MASK_FP(ccd))
+	call mfree (ccd, TY_STRUCT)
+end
diff --git a/noao/imred/ccdred/src/setsections.x b/noao/imred/ccdred/src/setsections.x
new file mode 100644
index 00000000..80e61e49
--- /dev/null
+++ b/noao/imred/ccdred/src/setsections.x
@@ -0,0 +1,113 @@
+include	<imhdr.h>
+include	<mwset.h>
+include	"ccdred.h"
+
+# SET_SECTIONS -- Set the data section, ccd section, trim section and
+# bias section.  Also set the WCS.
+
+procedure set_sections (ccd)
+
+pointer	ccd			# CCD structure (returned)
+
+pointer	sp, str, mw, lterm, mw_openim()
+int	nc, nl, c1, c2, cs, l1, l2, ls, ndim, mw_stati()
+bool	streq()
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	nc = IM_LEN(IN_IM(ccd),1)
+	nl = IM_LEN(IN_IM(ccd),2)
+
+	# The default data section is the entire image.
+	c1 = 1
+	c2 = nc
+	cs = 1
+	l1 = 1
+	l2 = nl
+	ls = 1
+	call hdmgstr (IN_IM(ccd), "datasec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1))
+	    call error (0, "Error in DATASEC parameter")
+	IN_C1(ccd) = c1
+	IN_C2(ccd) = c2
+	IN_L1(ccd) = l1
+	IN_L2(ccd) = l2
+
+	# The default trim section is the data section.
+	# Defer limit checking until actually used.
+	c1 = IN_C1(ccd)
+	c2 = IN_C2(ccd)
+	l1 = IN_L1(ccd)
+	l2 = IN_L2(ccd)
+	call clgstr ("trimsec", Memc[str], SZ_LINE)
+	if (streq (Memc[str], "image"))
+	    call hdmgstr (IN_IM(ccd), "trimsec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((cs!=1)||(ls!=1))
+	    call error (0, "Error in TRIMSEC parameter")
+	TRIM_C1(ccd) = c1
+	TRIM_C2(ccd) = c2
+	TRIM_L1(ccd) = l1
+	TRIM_L2(ccd) = l2
+
+	# The default bias section is the whole image.
+	# Defer limit checking until actually used.
+	c1 = 1
+	c2 = nc
+	l1 = 1
+	l2 = nl
+	call clgstr ("biassec", Memc[str], SZ_LINE)
+	if (streq (Memc[str], "image"))
+	    call hdmgstr (IN_IM(ccd), "biassec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((cs!=1)||(ls!=1))
+	    call error (0, "Error in BIASSEC parameter")
+	BIAS_C1(ccd) = c1
+	BIAS_C2(ccd) = c2
+	BIAS_L1(ccd) = l1
+	BIAS_L2(ccd) = l2
+
+	# The default ccd section is the size of the data section.
+	c1 = 1
+	c2 = IN_C2(ccd) - IN_C1(ccd) + 1
+	l1 = 1
+	l2 = IN_L2(ccd) - IN_L1(ccd) + 1
+	call hdmgstr (IN_IM(ccd), "ccdsec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((cs != 1) || (ls != 1))
+	    call error (0, "Error in CCDSEC parameter")
+	CCD_C1(ccd) = c1
+	CCD_C2(ccd) = c2
+	CCD_L1(ccd) = l1
+	CCD_L2(ccd) = l2
+	if ((IN_C2(ccd)-IN_C1(ccd) != CCD_C2(ccd)-CCD_C1(ccd)) ||
+	    (IN_L2(ccd)-IN_L1(ccd) != CCD_L2(ccd)-CCD_L1(ccd)))
+	    call error (0, "Size of DATASEC and CCDSEC do not agree")
+
+	# The default output data section is the input data section.
+	OUT_C1(ccd) = IN_C1(ccd)
+	OUT_C2(ccd) = IN_C2(ccd)
+	OUT_L1(ccd) = IN_L1(ccd)
+	OUT_L2(ccd) = IN_L2(ccd)
+
+	# Set the physical WCS to be CCD coordinates.
+	mw = mw_openim (IN_IM(ccd))
+	ndim = mw_stati (mw, MW_NPHYSDIM)
+	call salloc (lterm, ndim * (1 + ndim), TY_REAL)
+	call mw_gltermr (mw, Memr[lterm+ndim], Memr[lterm], ndim)
+	Memr[lterm] = IN_C1(ccd) - CCD_C1(ccd)
+	Memr[lterm+1] = IN_L1(ccd) - CCD_L1(ccd)
+	Memr[lterm+ndim] = 1. / cs
+	Memr[lterm+ndim+1] = 0.
+	Memr[lterm+ndim+ndim] = 0.
+	Memr[lterm+ndim+ndim+1] = 1. / ls
+	call mw_sltermr (mw, Memr[lterm+ndim], Memr[lterm], ndim)
+	call mw_saveim (mw, IN_IM(ccd))
+	call mw_saveim (mw, OUT_IM(ccd))
+	call mw_close (mw)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/settrim.x b/noao/imred/ccdred/src/settrim.x
new file mode 100644
index 00000000..65d5d09c
--- /dev/null
+++ b/noao/imred/ccdred/src/settrim.x
@@ -0,0 +1,99 @@
+include	<imhdr.h>
+include	<imset.h>
+include	"ccdred.h"
+
+# SET_TRIM -- Set the trim parameters.
+#
+#   1.  Return immediately if the trim correction is not requested or
+#	if the image has been previously corrected.
+#   2.	Determine the trim section.  This may be specifed directly or
+#	indirectly through the image header or symbol table.
+#   3.  Parse the trim section and apply it to the output image.
+#   4.  If the image is trimmed then log the operation and reset the output
+#	image size.
+
+procedure set_trim (ccd)
+
+pointer	ccd			# CCD structure
+
+int	xt1, xt2, yt1, yt2
+int	nc, nl, c1, c2, l1, l2
+pointer	sp, str, image
+bool	clgetb(), ccdflag()
+
+begin
+	# Check if the user wants this operation or it has been done.
+	if (!clgetb ("trim") || ccdflag (IN_IM(ccd), "trim"))
+	    return
+
+	# Check trim section.
+	nc = IM_LEN(IN_IM(ccd),1)
+	nl = IM_LEN(IN_IM(ccd),2)
+	c1 = TRIM_C1(ccd)
+	c2 = TRIM_C2(ccd)
+	l1 = TRIM_L1(ccd)
+	l2 = TRIM_L2(ccd)
+	if ((c1 < 1) || (c2 > nc) || (l1 < 1) || (l2 > nl)) {
+	    call smark (sp)
+	    call salloc (str, SZ_LINE, TY_CHAR)
+	    call salloc (image, SZ_LINE, TY_CHAR)
+	    call imstats (IN_IM(ccd), IM_IMAGENAME, Memc[image], SZ_FNAME)
+	    call sprintf (Memc[str], SZ_LINE,
+		"Error in trim section: image=%s[%d,%d], trimsec=[%d:%d,%d:%d]")
+		call pargstr (Memc[image])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+
+	# If no processing is desired print trim section and return.
+	if (clgetb ("noproc")) {
+	    call eprintf ("  [TO BE DONE] Trim section is [%d:%d,%d:%d].\n")
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    return
+	}
+
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	xt1 = max (0, c1 - IN_C1(ccd))
+	xt2 = min (0, c2 - IN_C2(ccd))
+	yt1 = max (0, l1 - IN_L1(ccd))
+	yt2 = min (0, l2 - IN_L2(ccd))
+
+	CCD_C1(ccd) = CCD_C1(ccd) + xt1
+	CCD_C2(ccd) = CCD_C2(ccd) + xt2
+	CCD_L1(ccd) = CCD_L1(ccd) + yt1
+	CCD_L2(ccd) = CCD_L2(ccd) + yt2
+	IN_C1(ccd) = IN_C1(ccd) + xt1
+	IN_C2(ccd) = IN_C2(ccd) + xt2
+	IN_L1(ccd) = IN_L1(ccd) + yt1
+	IN_L2(ccd) = IN_L2(ccd) + yt2
+	OUT_C1(ccd) = IN_C1(ccd) - c1 + 1
+	OUT_C2(ccd) = IN_C2(ccd) - c1 + 1
+	OUT_L1(ccd) = IN_L1(ccd) - l1 + 1
+	OUT_L2(ccd) = IN_L2(ccd) - l1 + 1
+	IM_LEN(OUT_IM(ccd),1) = c2 - c1 + 1
+	IM_LEN(OUT_IM(ccd),2) = l2 - l1 + 1
+
+	CORS(ccd, TRIM) = YES
+	COR(ccd) = YES
+
+	call sprintf (Memc[str], SZ_LINE, "Trim data section is [%d:%d,%d:%d]")
+	    call pargi (c1)
+	    call pargi (c2)
+	    call pargi (l1)
+	    call pargi (l2)
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "trim", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/setzero.x b/noao/imred/ccdred/src/setzero.x
new file mode 100644
index 00000000..610aeee7
--- /dev/null
+++ b/noao/imred/ccdred/src/setzero.x
@@ -0,0 +1,141 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+# SET_ZERO -- Set parameters for zero level correction.
+#   1.  Return immediately if the zero level correction is not requested or
+#	if the image has been previously corrected.
+#   2.	Get the zero level correction image.  Return an error if not found.
+#   3.	If the zero level image has not been processed call ZEROPROC.
+#   4.	Set the processing flag.
+#   5.  Log the operation (to user, logfile, and output image header).
+
+procedure set_zero (ccd)
+
+pointer	ccd			# CCD structure
+
+int	nscan, nc, nl, c1, c2, cs, l1, l2, ls, data_c1, ccd_c1, data_l1, ccd_l1
+pointer	sp, str, image, im, ccd_cache()
+bool	clgetb(), ccdflag(), ccdcheck()
+int	ccdtypei(), ccdnscan()
+errchk	cal_image, ccd_cache, ccdproc
+
+begin
+	# Check if the user wants this operation or it has been done.
+	if (!clgetb ("zerocor") || ccdflag (IN_IM(ccd), "zerocor"))
+	    return
+
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the zero level correction image.
+	if (clgetb ("scancor"))
+	    nscan = ccdnscan (IN_IM(ccd), ccdtypei(IN_IM(ccd)))
+	else
+	    nscan = 1
+	call cal_image (IN_IM(ccd), ZERO, nscan, Memc[image], SZ_FNAME)
+
+	# If no processing is desired print zero correction image and return.
+	if (clgetb ("noproc")) {
+	    call eprintf ("  [TO BE DONE] Zero level correction image is %s.\n")
+		call pargstr (Memc[image])
+	    call sfree (sp)
+	    return
+	}
+
+	# Map the image and return on an error.
+	# Process the zero image if necessary.
+	# If nscan > 1 then the zero may not yet exist so create it
+	# from the unscanned zero.
+
+	iferr (im = ccd_cache (Memc[image], ZERO)) {
+	    call cal_image (IN_IM(ccd), ZERO, 1, Memc[str], SZ_LINE)
+	    im = ccd_cache (Memc[str], ZERO)
+	    if (ccdcheck (im, ZERO)) {
+		call ccd_flush (im)
+		call ccdproc (Memc[str], ZERO)
+	    }
+	    call scancor (Memc[str], Memc[image], nscan, INDEF)
+	    im = ccd_cache (Memc[image], ZERO)
+	}
+
+	if (ccdcheck (im, ZERO)) {
+	    call ccd_flush (im)
+	    call ccdproc (Memc[image], ZERO)
+	    im = ccd_cache (Memc[image], ZERO)
+	}
+
+	# Set the processing parameters in the CCD structure.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	c1 = 1
+	c2 = nc
+	l1 = 1
+	l2 = nl
+	cs = 1
+	ls = 1
+	call hdmgstr (im, "datasec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1)) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Data section error: image=%s[%d,%d], datasec=[%d:%d,%d:%d]")
+		call pargstr (Memc[image])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+	data_c1 = c1
+	data_l1 = l1
+	call hdmgstr (im, "ccdsec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if (nc == 1) {
+	    c1 = CCD_C1(ccd)
+	    c2 = CCD_C2(ccd)
+	}
+	if (nl == 1) {
+	    l1 = CCD_L1(ccd)
+	    l2 = CCD_L2(ccd)
+	}
+	ccd_c1 = c1
+	ccd_l1 = l1
+	if ((c1 > CCD_C1(ccd)) || (c2 < CCD_C2(ccd)) ||
+	    (l1 > CCD_L1(ccd)) || (l2 < CCD_L2(ccd))) {
+	    call sprintf (Memc[str], SZ_LINE,
+	        "CCD section error: input=[%d:%d,%d:%d], %s=[%d:%d,%d:%d]")
+		call pargi (CCD_C1(ccd))
+		call pargi (CCD_C2(ccd))
+		call pargi (CCD_L1(ccd))
+		call pargi (CCD_L2(ccd))
+		call pargstr (Memc[image])
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+
+	ZERO_IM(ccd) = im
+	ZERO_C1(ccd) = CCD_C1(ccd) - ccd_c1 + data_c1
+	ZERO_C2(ccd) = CCD_C2(ccd) - ccd_c1 + data_c1
+	ZERO_L1(ccd) = CCD_L1(ccd) - ccd_l1 + data_l1
+	ZERO_L2(ccd) = CCD_L2(ccd) - ccd_l1 + data_l1
+
+	CORS(ccd, ZEROCOR) = Z
+	COR(ccd) = YES
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE, "Zero level correction image is %s")
+	    call pargstr (Memc[image])
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "zerocor", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/sigma.gx b/noao/imred/ccdred/src/sigma.gx
new file mode 100644
index 00000000..8b59f1f6
--- /dev/null
+++ b/noao/imred/ccdred/src/sigma.gx
@@ -0,0 +1,89 @@
+$for (sr)
+# SIGMA -- Compute sigma line from image lines with rejection.
+
+procedure sigma$t (data, nimages, mean, sigma, npts)
+
+pointer	data[nimages]		# Data vectors
+int	nimages			# Number of data vectors
+$if (datatype == sil)
+real	mean[npts]		# Mean vector
+real	sigma[npts]		# Sigma vector (returned)
+$else
+PIXEL	mean[npts]		# Mean vector
+PIXEL	sigma[npts]		# Sigma vector (returned)
+$endif
+int	npts			# Number of points in each vector
+
+$if (datatype == sil)
+real	val, sig, pixval
+$else
+PIXEL	val, sig, pixval
+$endif
+int	i, j, n, n1
+
+begin
+	n = nimages - 1
+	do i = 1, npts {
+	    val = mean[i]
+	    sig = 0.
+	    n1 = n
+	    do j = 1, nimages {
+		pixval = Mem$t[data[j]+i-1]
+		if (IS_INDEF (pixval))
+		    n1 = n1 - 1
+		else
+		    sig = sig + (pixval - val) ** 2
+	    }
+	    if (n1 > 0)
+	        sigma[i] = sqrt (sig / n1)
+	    else
+	        sigma[i] = 0.
+	}
+end
+
+
+# WTSIGMA -- Compute scaled and weighted sigma line from image lines with
+# rejection.
+
+procedure wtsigma$t (data, scales, zeros, wts, nimages, mean, sigma, npts)
+
+pointer	data[nimages]		# Data vectors
+real	scales[nimages]		# Scale factors
+real	zeros[nimages]		# Zero levels
+real	wts[nimages]		# Weights
+int	nimages			# Number of data vectors
+$if (datatype == sil)
+real	mean[npts]		# Mean vector
+real	sigma[npts]		# Sigma vector (returned)
+real	val, sig, pixval
+$else
+PIXEL	mean[npts]		# Mean vector
+PIXEL	sigma[npts]		# Sigma vector (returned)
+PIXEL	val, sig, pixval
+$endif
+int	npts			# Number of points in each vector
+
+int	i, j, n
+real	sumwts
+
+begin
+	do i = 1, npts {
+	    val = mean[i]
+	    n = 0
+	    sig = 0.
+	    sumwts = 0.
+	    do j = 1, nimages {
+		pixval = Mem$t[data[j]+i-1]
+		if (!IS_INDEF (pixval)) {
+		    n = n + 1
+		    sig = sig + wts[j]*(pixval/scales[j]-zeros[j]-val) ** 2
+		    sumwts = sumwts + wts[j]
+		}
+	    }
+	    if (n > 1)
+	        sigma[i] = sqrt (sig / sumwts * n / (n - 1))
+	    else
+	        sigma[i] = 0.
+	}
+end
+$endfor
diff --git a/noao/imred/ccdred/src/t_badpixim.x b/noao/imred/ccdred/src/t_badpixim.x
new file mode 100644
index 00000000..3a44dfa0
--- /dev/null
+++ b/noao/imred/ccdred/src/t_badpixim.x
@@ -0,0 +1,114 @@
+include	<imhdr.h>
+
+# T_BADPIXIMAGE -- Create a bad pixel image mask from a bad pixel file.
+
+procedure t_badpiximage ()
+
+pointer	bpfile			# Bad pixel file
+pointer	bpimage			# Bad pixel image
+pointer	template		# Template image
+short	goodval, badval		# Good and bad values
+
+int	i, nc, nl, c1, c2, l1, l2, fd, x1, x2, xstep, y1, y2, ystep
+pointer	sp, str, im, im1
+
+short	clgets()
+bool	ccdflag()
+pointer	immap(), impl2s(), imps2s()
+int	open(), fscan(), nscan(), stridxs(), strmatch()
+errchk	open, immap
+
+begin
+	call smark (sp)
+	call salloc (bpfile, SZ_FNAME, TY_CHAR)
+	call salloc (bpimage, SZ_FNAME, TY_CHAR)
+	call salloc (template, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get task parameters.
+	call clgstr ("fixfile", Memc[bpfile], SZ_FNAME)
+	call clgstr ("template", Memc[template], SZ_FNAME)
+	call clgstr ("image", Memc[bpimage], SZ_FNAME)
+	goodval = clgets ("goodvalue")
+	badval = clgets ("badvalue")
+
+	# Open the files and abort on an error.
+	fd = open (Memc[bpfile], READ_ONLY, TEXT_FILE)
+	im1 = immap (Memc[template], READ_ONLY, 0)
+	im = immap (Memc[bpimage], NEW_COPY, im1)
+
+	# Set the output image.
+	IM_PIXTYPE(im) = TY_SHORT
+	call sprintf (IM_TITLE(im), SZ_IMTITLE,
+	    "Bad pixel image from bad pixel file %s")
+	    call pargstr (Memc[bpfile])
+
+	# Set the good pixel values.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	do i = 1, nl
+	    call amovks (goodval, Mems[impl2s(im,i)], nc)
+
+	# Set the bad pixel values.  By default the bad pixel coordinates
+	# refer to the image directly but if the word "untrimmed" appears
+	# in a comment then the coordinates refer to the untrimmed image.
+	# This is the same algorithm as used in SETFIXPIX for CCDPROC.
+
+	x1 = 1
+	xstep = 1
+	y1 = 1
+	ystep = 1
+	while (fscan (fd) != EOF) {
+	    call gargwrd (Memc[str], SZ_LINE)
+	    if (Memc[str] == '#') {
+		call gargstr (Memc[str], SZ_LINE)
+		if (strmatch (Memc[str], "{untrimmed}") != 0) {
+		    if (ccdflag (im, "trim")) {
+	    		call hdmgstr (im, "trim", Memc[str], SZ_LINE)
+	    		x2 = stridxs ("[", Memc[str])
+	    		if (x2 != 0) {
+			    x1 = 1
+			    x2 = IM_LEN(im,1)
+			    xstep = 1
+			    y1 = 1
+			    y2 = IM_LEN(im,2)
+			    ystep = 1
+			    call ccd_section (Memc[str+x2-1], x1, x2, xstep,
+				y1, y2, ystep)
+			}
+		    }
+		}
+	        next
+	    }
+		    
+	    call reset_scan()
+	    call gargi (c1)
+	    call gargi (c2)
+	    call gargi (l1)
+	    call gargi (l2)
+	    if (nscan() != 4) {
+	        if (nscan() == 2) {
+		    l1 = c2
+		    c2 = c1
+		    l2 = l1
+		} else
+		    next
+	    }
+
+	    c1 = max (1, (c1 - x1 + xstep - 1) / xstep + 1)
+	    c2 = min (nc, (c2 - x1) / xstep + 1)
+	    l1 = max (1, (l1 - y1 + ystep - 1) / ystep + 1)
+	    l2 = min (nl, (l2 - y1) / ystep + 1)
+
+	    if ((c1 > c2) || (l1 > l2))
+		next
+
+	    i = (c2 - c1 + 1) * (l2 - l1 + 1)
+	    call amovks (badval, Mems[imps2s(im,c1,c2,l1,l2)], i)
+	}
+
+	# Finish up.
+	call imunmap (im)
+	call imunmap (im1)
+	call close (fd)
+end
diff --git a/noao/imred/ccdred/src/t_ccdgroups.x b/noao/imred/ccdred/src/t_ccdgroups.x
new file mode 100644
index 00000000..225589e5
--- /dev/null
+++ b/noao/imred/ccdred/src/t_ccdgroups.x
@@ -0,0 +1,258 @@
+include	<error.h>
+include	<math.h>
+
+# Group type definitions.
+define	GROUPS	"|position|title|date|ccdtype|subset|"
+define	POSITION	1	# Group by position
+define	TITLE		2	# Group by title
+define	DATE		3	# Group by date
+define	CCDTYPE		4	# Group by ccdtype
+define	SUBSET		5	# Group by subset
+
+define	NALLOC		10	# Allocate memory in this size block
+
+# T_CCDGROUPS -- Group images into files based on parameters with common values.
+# The output consists of files containing the image names of images from the
+# input image list which have the same group type such as position, date,
+# or title.
+
+procedure t_ccdgroups ()
+
+int	images			# List of images
+pointer	root			# Output group root name
+int	group			# Group type
+real	radius			# Position radius
+bool	verbose			# Verbose output (package parameter)
+
+int	ngroup, fd, ntitles, npositions, ndates, ccdtype
+pointer	im, sp, image, output, suffix, titles, positions, dates
+
+bool	clgetb()
+real	clgetr()
+int	position_group(), title_group(), date_group()
+int	imtopenp(), imtgetim(), open(), clgwrd()
+errchk	set_input, position_group, title_group, date_group, open
+
+begin
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (root, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (suffix, SZ_FNAME, TY_CHAR)
+
+	# Get the task parameters.
+	images = imtopenp ("images")
+	call clgstr ("output", Memc[root], SZ_FNAME)
+	group = clgwrd ("group", Memc[image], SZ_FNAME, GROUPS)
+	radius = clgetr ("radius")
+	call clgstr ("instrument", Memc[image], SZ_FNAME)
+        if (Memc[image] == EOS)
+            call error (1, "No 'instrument' translation file specified.")
+	call hdmopen (Memc[image])
+	verbose = clgetb ("verbose")
+
+	# Loop through the images and place them into groups.
+	positions = NULL
+	npositions = 0
+	titles = NULL
+	ntitles = 0
+	dates = NULL
+	ndates = 0
+	while (imtgetim (images, Memc[image], SZ_FNAME) != EOF) {
+	    call set_input (Memc[image], im, ccdtype)
+	    if (im == NULL)
+		next
+
+	    iferr {
+		switch (group) {
+	        case POSITION:
+		    ngroup = position_group (im, positions, npositions, radius)
+	        case TITLE:
+	            ngroup = title_group (im, titles, ntitles)
+	        case DATE:
+	            ngroup = date_group (im, dates, ndates)
+	        }
+
+		# Define the output group file.
+		switch (group) {
+		case POSITION, TITLE, DATE:
+	            call sprintf (Memc[output], SZ_FNAME, "%s%d")
+		        call pargstr (Memc[root])
+		        call pargi (ngroup)
+		case CCDTYPE:
+		    call ccdtypes (im, Memc[suffix], SZ_FNAME)
+		    call sprintf (Memc[output], SZ_FNAME, "%s%d")
+			call pargstr (Memc[root])
+			call pargstr (Memc[suffix])
+		case SUBSET:
+		    call ccdsubset (im, Memc[suffix], SZ_FNAME)
+		    call sprintf (Memc[output], SZ_FNAME, "%s%d")
+			call pargstr (Memc[root])
+			call pargstr (Memc[suffix])
+		}
+
+		# Print the operation if verbose.
+		if (verbose) {
+	            call printf ("%s --> %s\n")
+		        call pargstr (Memc[image])
+		        call pargstr (Memc[output])
+		}
+
+		# Enter the image in the appropriate group file.
+	        fd = open (Memc[output], APPEND, TEXT_FILE)
+	        call fprintf (fd, "%s\n")
+		    call pargstr (Memc[image])
+	        call close (fd)
+	    } then
+		 call erract (EA_WARN)
+
+	    call imunmap (im)
+	}
+
+	# Finish up.
+	call imtclose (images)
+	if (positions != NULL)
+	    call mfree (positions, TY_REAL)
+	if (titles != NULL)
+	    call mfree (titles, TY_CHAR)
+	if (dates != NULL)
+	    call mfree (dates, TY_CHAR)
+	call sfree (sp)
+end
+
+
+# TITLE_GROUP -- Group images by title.
+
+int procedure title_group (im, titles, ntitles)
+
+pointer	im			# Image
+pointer	titles			# Pointer to title strings
+int	ntitles			# Number of titles
+
+int	i, nalloc
+pointer	sp, title, ptr
+bool	streq()
+errchk	hdmgstr
+
+begin
+	call smark (sp)
+	call salloc (title, SZ_LINE, TY_CHAR)
+	call hdmgstr (im, "title", Memc[title], SZ_LINE)
+
+	for (i=1; i<=ntitles; i=i+1) {
+	    ptr = titles + (i - 1) * SZ_LINE
+	    if (streq (Memc[title], Memc[ptr]))
+		break
+	}
+	if (i > ntitles) {
+	    if (i == 1) {
+		nalloc = NALLOC
+		call malloc (titles, nalloc * SZ_LINE, TY_CHAR)
+	    } else if (i > nalloc) {
+		nalloc = nalloc + NALLOC
+		call realloc (titles, nalloc * SZ_LINE, TY_CHAR)
+	    }
+	    ptr = titles + (i - 1) * SZ_LINE
+	    call strcpy (Memc[title], Memc[ptr], SZ_LINE-1)
+	    ntitles = i
+	}
+
+	call sfree (sp)
+	return (i)
+end
+
+
+# POSITION_GROUP -- Group by RA and DEC position.  The RA is in hours and
+# the DEC is in degrees.  The radius is in seconds of arc.
+
+int procedure position_group (im, positions, npositions, radius)
+
+pointer	im			# Image
+pointer	positions		# Positions
+int	npositions		# Number of positions
+real	radius			# Matching radius
+
+real	ra, dec, dra, ddec, r, hdmgetr()
+int	i, nalloc
+pointer	ptr
+errchk	hdmgetr
+
+begin
+	ra = hdmgetr (im, "ra")
+	dec = hdmgetr (im, "dec")
+
+	for (i=1; i<=npositions; i=i+1) {
+	    ptr = positions + 2 * i - 2
+	    dra = ra - Memr[ptr]
+	    ddec = dec - Memr[ptr+1]
+	    if (dra > 12.)
+		dra = dra - 24.
+	    if (dra < -12.)
+		dra = dra + 24.
+	    dra = dra * cos (DEGTORAD (dec)) * 15.
+	    r = sqrt (dra ** 2 + ddec ** 2) * 3600.
+	    if (r < radius)
+		break
+	}
+	if (i > npositions) {
+	    if (i == 1) {
+		nalloc = NALLOC
+		call malloc (positions, nalloc * 2, TY_REAL)
+	    } else if (i > nalloc) {
+		nalloc = nalloc + NALLOC
+		call realloc (positions, nalloc * 2, TY_REAL)
+	    }
+	    ptr = positions + 2 * i - 2
+	    Memr[ptr] = ra
+	    Memr[ptr+1] = dec
+	    npositions = i
+	}
+
+	return (i)
+end
+
+
+# DATE_GROUP -- Group by date.
+
+int procedure date_group (im, dates, ndates)
+
+pointer	im			# Image
+pointer	dates			# Pointer to date strings
+int	ndates			# Number of dates
+
+int	i, nalloc, stridxs()
+pointer	sp, date, ptr
+bool	streq()
+errchk	hdmgstr
+
+begin
+	call smark (sp)
+	call salloc (date, SZ_LINE, TY_CHAR)
+	call hdmgstr (im, "date-obs", Memc[date], SZ_LINE)
+
+	# Strip time if present.
+	i = stridxs ("T", Memc[date])
+	if (i > 0)
+	    Memc[date+i-1] = EOS
+
+	for (i=1; i<=ndates; i=i+1) {
+	    ptr = dates + (i - 1) * SZ_LINE
+	    if (streq (Memc[date], Memc[ptr]))
+		break
+	}
+	if (i > ndates) {
+	    if (i == 1) {
+		nalloc = NALLOC
+		call malloc (dates, nalloc * SZ_LINE, TY_CHAR)
+	    } else if (i > nalloc) {
+		nalloc = nalloc + NALLOC
+		call realloc (dates, nalloc * SZ_LINE, TY_CHAR)
+	    }
+	    ptr = dates + (i - 1) * SZ_LINE
+	    call strcpy (Memc[date], Memc[ptr], SZ_LINE-1)
+	    ndates = i
+	}
+
+	call sfree (sp)
+	return (i)
+end
diff --git a/noao/imred/ccdred/src/t_ccdhedit.x b/noao/imred/ccdred/src/t_ccdhedit.x
new file mode 100644
index 00000000..a7fd9121
--- /dev/null
+++ b/noao/imred/ccdred/src/t_ccdhedit.x
@@ -0,0 +1,87 @@
+include	<error.h>
+
+define	TYPES	"|string|real|integer|"
+define	SVAL	1	# String value
+define	RVAL	2	# Real value
+define	IVAL	3	# Integer value
+
+# T_CCDHEDIT -- Add, delete, or change CCD image header parameters.
+# This task differs from HEDIT in that it uses the CCD instrument translation
+# file.
+
+procedure t_ccdhedit ()
+
+int	list			# List of CCD images
+pointer	param			# Parameter name
+int	type			# Parameter type
+pointer	sval			# Parameter value
+pointer	instrument		# Instrument file
+
+int	ip, ival, imtopenp(), imtgetim(), clgwrd(), ctoi(), ctor()
+real	rval
+bool	streq()
+pointer	sp, im, immap()
+errchk	hdmpstr, hdmputr, hdmputi
+
+begin
+	call smark (sp)
+	call salloc (param, SZ_LINE, TY_CHAR)
+	call salloc (sval, SZ_LINE, TY_CHAR)
+	call salloc (instrument, SZ_FNAME, TY_CHAR)
+
+	# Get the task parameters.
+	list = imtopenp ("images")
+	call clgstr ("parameter", Memc[param], SZ_LINE)
+	type = clgwrd ("type", Memc[sval], SZ_LINE, TYPES)
+	call clgstr ("value", Memc[sval], SZ_LINE)
+	call clgstr ("instrument", Memc[instrument], SZ_FNAME)
+	call xt_stripwhite (Memc[sval])
+
+	# Open the instrument translation file.
+	call hdmopen (Memc[instrument])
+
+	# If the parameter is IMAGETYP then change the parameter value from
+	# the package form to the image form using the inverse mapping in the
+	# translation file.
+
+	if (streq (Memc[param], "imagetyp"))
+	    call hdmparm (Memc[sval], Memc[sval], SZ_LINE)
+
+	# Edit each image in the input list.
+	while (imtgetim (list, Memc[instrument], SZ_FNAME) != EOF) {
+	    iferr (im = immap (Memc[instrument], READ_WRITE, 0)) {
+		call erract (EA_WARN)
+		next
+	    }
+
+	    # If the parameter value is null then delete the entry.
+	    if (Memc[sval] == EOS) {
+		iferr (call hdmdelf (im, Memc[param]))
+		    call erract (EA_WARN)
+
+	    # Otherwise add the parameter of the specified type.
+	    } else {
+	        switch (type) {
+	        case SVAL:
+	            call hdmpstr (im, Memc[param], Memc[sval])
+	        case RVAL:
+		    ip = 1
+		    if (ctor (Memc[sval], ip, rval) == 0)
+		        call error (0, "Parameter value is not a number")
+		    call hdmputr (im, Memc[param], rval)
+	        case IVAL:
+		    ip = 1
+		    if (ctoi (Memc[sval], ip, ival) == 0)
+		        call error (0, "Parameter value is not a number")
+		    call hdmputi (im, Memc[param], ival)
+	        }
+	    }
+
+	    call imunmap (im)
+	}
+
+	# Finish up.
+	call hdmclose ()
+	call imtclose (list)
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/t_ccdinst.x b/noao/imred/ccdred/src/t_ccdinst.x
new file mode 100644
index 00000000..e98763fd
--- /dev/null
+++ b/noao/imred/ccdred/src/t_ccdinst.x
@@ -0,0 +1,667 @@
+include	<imhdr.h>
+include	<imio.h>
+include	<error.h>
+include	"ccdtypes.h"
+
+define	HELP1	"noao$imred/ccdred/src/ccdinst1.key"
+define	HELP2	"noao$imred/ccdred/src/ccdinst2.key"
+define	HELP3	"noao$imred/ccdred/src/ccdinst3.key"
+
+define	LEVELS	"|basic|common|all|"
+
+define	CMDS	"|quit|?|help|show|instrument|imheader|read|write|newimage\
+		 |translate|imagetyp|subset|exptime|darktime|fixfile|biassec\
+		 |ccdsec|datasec|trimsec|darkcor|fixpix|flatcor|fringcor\
+		 |illumcor|overscan|readcor|scancor|trim|zerocor|ccdmean\
+		 |fringscl|illumflt|mkfringe|mkillum|skyflat|ncombine\
+		 |date-obs|dec|ra|title|next|nscanrow|"
+
+define	QUIT		1	# Quit
+define	QUESTION	2	# Help
+define	HELP		3	# Help
+define	SHOW		4	# Show current translations
+define	INST		5	# Show instrument file
+define	IMHEADER	6	# Print image header
+define	READ		7	# Read instrument file
+define	WRITE		8	# Write instrument file
+define	NEWIMAGE	9	# Change image
+define	TRANSLATE	10	# Translate image type
+define	IMAGETYPE	11	# Image type
+define	SUBSET		12	# Subset parameter
+define	EXPTIME		13	# Exposure time
+define	DARKTIME	14	# Dark time
+define	FIXFILE		15	# Bad pixel file
+define	BIASSEC		16	# Bias section
+define	CCDSEC		17	# CCD section
+define	DATASEC		18	# Data section
+define	TRIMSEC		19	# Trim section
+define	DARKCOR		20	# Dark count flag
+define	FIXPIX		21	# Bad pixel flag
+define	FLATCOR		22	# Flat field flag
+define	FRINGCOR	23	# Fringe flag
+define	ILLUMCOR	24	# Illumination flag
+define	OVERSCAN	25	# Overscan flag
+define	READCOR		26	# Readout flag
+define	SCANCOR		27	# Scan mode flag
+define	NSCANROW	42	# Number of scan rows
+define	TRIM		28	# Trim flag
+define	ZEROCOR		29	# Zero level flag
+define	CCDMEAN		30	# CCD mean value
+define	FRINGSCL	31	# Fringe scale value
+define	ILLUMFLT	32	# Illumination flat flag
+define	MKFRINGE	33	# Illumination flag
+define	MKILLUM		34	# Illumination flag
+define	SKYFLAT		35	# Sky flat flag
+define	NCOMBINE	36	# NCOMBINE parameter
+define	DATEOBS		37	# Date
+define	DEC		38	# Dec
+define	RA		39	# RA
+define	TITLE		40	# Title
+define	NEXT		41	# Next image
+
+# T_CCDINST -- Check and modify instrument translations
+
+procedure t_ccdinst ()
+
+int	list, level, ncmd, imtopenp(), imtgetim(), scan(), access(), clgwrd()
+pointer	sp, image, inst, ssfile, im, immap()
+bool	update, clgetb()
+errchk	delete, hdmwrite
+
+begin
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (inst, SZ_FNAME, TY_CHAR)
+	call salloc (ssfile, SZ_FNAME, TY_CHAR)
+
+	# Get the task parameters, open the translation file, set defaults.
+	list = imtopenp ("images")
+	call clgstr ("instrument", Memc[inst], SZ_FNAME)
+	call clgstr ("ssfile", Memc[ssfile], SZ_FNAME)
+	level = clgwrd ("parameters", Memc[image], SZ_FNAME, LEVELS)
+        if (Memc[image] == EOS)
+            call error (1, "No 'parameters' file value specified.")
+	call hdmopen (Memc[inst])
+	ncmd = NEXT
+	update = false
+
+	# Process each image.
+	while (imtgetim (list, Memc[image], SZ_FNAME) != EOF) {
+	    iferr (im = immap (Memc[image], READ_ONLY, 0)) {
+		call erract (EA_WARN)
+		next
+	    }
+
+	    if (clgetb ("edit"))
+	        call ccdinst_edit (im, Memc[image], Memc[inst], Memc[ssfile],
+		    level, ncmd, update)
+	    else
+		call ccdinst_hdr (im, Memc[image], Memc[inst], Memc[ssfile],
+		    level)
+	    call imunmap (im)
+	    if (ncmd == QUIT)
+		break
+	}
+
+	# Update instrument file if necessary.
+	if (update) {
+	    call printf ("Update instrument file %s (%b)? ")
+		call pargstr (Memc[inst])
+		call pargb (update)
+	    call flush (STDOUT)
+	    if (scan() != EOF)
+		call gargb (update)
+	    if (update) {
+		iferr {
+		    if (access (Memc[inst], 0, 0) == YES)
+		        call delete (Memc[inst])
+		    call hdmwrite (Memc[inst], NEW_FILE)
+		} then
+		    call erract (EA_WARN)
+	    }
+	}
+
+	# Finish up.
+	call hdmclose ()
+	call imtclose (list)
+	call sfree (sp)
+end
+
+
+# CCDINST_EDIT -- Main instrument file editor loop.
+# This returns the last command (quit or next) and the update flag.
+# The image name may also be changed.
+
+procedure ccdinst_edit (im, image, inst, ssfile, level, ncmd, update)
+
+pointer	im			# Image pointer
+char	image[SZ_FNAME]		# Image name
+char	inst[SZ_FNAME]		# Instrument file
+char	ssfile[SZ_FNAME]	# Subset file
+int	level			# Parameter level
+int	ncmd			# Last command
+bool	update			# Update?
+
+bool	strne()
+int	scan(), nscan(), strdic(), access()
+pointer	sp, cmd, key, def, imval, im1, immap()
+errchk	delete, hdmwrite
+
+begin
+	call smark (sp)
+	call salloc (cmd, SZ_LINE, TY_CHAR)
+	call salloc (key, SZ_FNAME, TY_CHAR)
+	call salloc (def, SZ_LINE, TY_CHAR)
+	call salloc (imval, SZ_LINE, TY_CHAR)
+
+	call sscan ("show")
+	repeat {
+	    call gargwrd (Memc[cmd], SZ_LINE)
+	    ncmd = strdic (Memc[cmd], Memc[cmd], SZ_LINE, CMDS)
+	    switch (ncmd) {
+	    case NEXT, QUIT:
+		break
+	    case QUESTION, HELP:
+		if (level == 1)
+		    call pagefile (HELP1, "ccdinstrument")
+		else if (level == 2)
+		    call pagefile (HELP2, "ccdinstrument")
+		else if (level == 3)
+		    call pagefile (HELP3, "ccdinstrument")
+	    case SHOW:
+		call ccdinst_hdr (im, image, inst, ssfile, level)
+	    case INST:
+		call hdmwrite ("STDOUT", APPEND)
+		call printf ("\n")
+	    case IMHEADER:
+		call ccdinst_i (im, image)
+	    case READ:
+		call gargwrd (Memc[imval], SZ_LINE)
+		if (nscan() < 2) 
+		    call ccdinst_g ("Instrument file", inst, Memc[imval])
+		if (update)
+		    call printf ("WARNING: Previous changes lost\n")
+		call hdmclose ()
+		update = false
+		if (strne (inst, Memc[imval])) {
+		    iferr (call hdmopen (Memc[imval])) {
+			call erract (EA_WARN)
+			call hdmopen (inst)
+		    } else {
+			call ccdinst_hdr (im, image, inst, ssfile, level)
+			update = true
+		    }
+		}
+	    case WRITE:
+		call gargwrd (Memc[imval], SZ_LINE)
+		if (nscan() < 2)
+		    call ccdinst_g ("Instrument file", inst, Memc[imval])
+		iferr {
+		    if (access (Memc[imval], 0, 0) == YES)
+		        call delete (Memc[imval])
+		    call hdmwrite (Memc[imval], NEW_FILE)
+		    update = false
+		} then
+		    call erract (EA_WARN)
+	    case NEWIMAGE:
+		call gargwrd (Memc[imval], SZ_LINE)
+		if (nscan() < 2)
+		    call ccdinst_g ("New image name", image, Memc[imval])
+		if (strne (image, Memc[imval])) {
+		    iferr (im1 = immap (Memc[imval], READ_ONLY, 0)) {
+			call erract (EA_WARN)
+			im1 = NULL
+		    }
+		    if (im1 != NULL) {
+			call imunmap (im)
+			im = im1
+			call strcpy (Memc[imval], image, SZ_FNAME)
+			call ccdinst_hdr (im, image, inst, ssfile, level)
+		    }
+		}
+	    case TRANSLATE:
+		call ccdtypes (im, Memc[cmd], SZ_LINE)
+		call hdmgstr (im, "imagetyp", Memc[imval], SZ_LINE)
+
+		call gargwrd (Memc[def], SZ_FNAME)
+		if (nscan() < 2) {
+		    call printf ("CCDRED image type for '%s' (%s): ")
+			call pargstr (Memc[imval])
+			call pargstr (Memc[cmd])
+		    call flush (STDOUT)
+		    if (scan() != EOF)
+			call gargwrd (Memc[def], SZ_FNAME)
+		    if (nscan() == 0)
+			call strcpy (Memc[cmd], Memc[def], SZ_LINE)
+		}
+		if (strdic (Memc[def], Memc[def], SZ_LINE, CCDTYPES) == 0) {
+		    call printf ("Unknown CCDRED image type\n")
+		    call strcpy (Memc[cmd], Memc[def], SZ_LINE)
+		}
+		if (strne (Memc[def], Memc[cmd])) {
+		    call hdmpname (Memc[imval], Memc[def])
+		    call ccdinst_p (im, "imagetyp",
+			Memc[key], Memc[def], Memc[imval])
+		    update = true
+		}
+	    case IMAGETYPE:
+		call ccdinst_e (im, "image type", "imagetyp",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case SUBSET:
+		call ccdinst_e (im, "subset parameter", "subset",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case EXPTIME:
+		call ccdinst_e (im, "exposure time", "exptime",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case DARKTIME:
+		call ccdinst_e (im, "dark time", "darktime",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case FIXFILE:
+		call ccdinst_e (im, "bad pixel file", "fixfile",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case BIASSEC:
+		call ccdinst_e (im, "bias section", "biassec",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case CCDSEC:
+		call ccdinst_e (im, "original CCD section", "ccdsec",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case DATASEC:
+		call ccdinst_e (im, "data section", "datasec",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case TRIMSEC:
+		call ccdinst_e (im, "trim section", "trimsec",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case DARKCOR:
+		call ccdinst_e (im, "dark count flag", "darkcor",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case FIXPIX:
+		call ccdinst_e (im, "bad pixel flag", "fixpix",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case FLATCOR:
+		call ccdinst_e (im, "flat field flag", "flatcor",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case FRINGCOR:
+		call ccdinst_e (im, "fringe flag", "fringcor",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case ILLUMCOR:
+		call ccdinst_e (im, "illumination flag", "illumcor",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case OVERSCAN:
+		call ccdinst_e (im, "overscan flag", "overscan",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case READCOR:
+		call ccdinst_e (im, "read correction flag", "readcor",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case SCANCOR:
+		call ccdinst_e (im, "scan mode flag", "scancor",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case NSCANROW:
+		call ccdinst_e (im, "scan mode rows", "nscanrow",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case TRIM:
+		call ccdinst_e (im, "trim flag", "trim",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case ZEROCOR:
+		call ccdinst_e (im, "zero level flag", "zerocor",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case CCDMEAN:
+		call ccdinst_e (im, "mean value", "ccdmean",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case FRINGSCL:
+		call ccdinst_e (im, "fringe scale", "fringscl",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case ILLUMFLT:
+		call ccdinst_e (im, "illumination flat image", "illumflt",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case MKFRINGE:
+		call ccdinst_e (im, "fringe image", "mkfringe",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case MKILLUM:
+		call ccdinst_e (im, "illumination image", "mkillum",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case SKYFLAT:
+		call ccdinst_e (im, "sky flat image", "skyflat",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case NCOMBINE:
+		call ccdinst_e (im, "number of images combined", "ncombine",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case DATEOBS:
+		call ccdinst_e (im, "date of observation", "date-obs",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case DEC:
+		call ccdinst_e (im, "declination", "dec",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case RA:
+		call ccdinst_e (im, "ra", "ra",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    case TITLE:
+		call ccdinst_e (im, "title", "title",
+		    Memc[key], Memc[def], Memc[imval], update)
+	    default:
+	        if (nscan() > 0)
+		    call eprintf ("Unrecognized or ambiguous command\007\n")
+	    }
+	    call printf ("ccdinstrument> ")
+	    call flush (STDOUT)
+	} until (scan() == EOF)
+
+	call sfree (sp)
+end
+
+
+# CCDINST_HDR -- Print the current instrument translations for an image.
+
+procedure ccdinst_hdr (im, image, inst, ssfile, level)
+
+pointer	im			# Image pointer
+char	image[SZ_FNAME]		# Image name
+char	inst[SZ_FNAME]		# Instrument file
+char	ssfile[SZ_FNAME]	# Subset file
+int	level			# Parameter level
+
+pointer	sp, key, def, ccdval, imval
+
+begin
+	call smark (sp)
+	call salloc (key, SZ_FNAME, TY_CHAR)
+	call salloc (def, SZ_LINE, TY_CHAR)
+	call salloc (ccdval, SZ_LINE, TY_CHAR)
+	call salloc (imval, SZ_LINE, TY_CHAR)
+
+	# General stuff
+	call printf ("Image: %s\n")
+	    call pargstr (image)
+	call printf ("Instrument file: %s\n")
+	    call pargstr (inst)
+	call printf ("Subset file: %s\n")
+	    call pargstr (ssfile)
+
+	# Table labels
+	call printf ("\n%-8s  %-8s  %-8s  %-8s  %-8s\n")
+	    call pargstr ("CCDRED")
+	    call pargstr ("IMAGE")
+	    call pargstr ("DEFAULT")
+	    call pargstr ("CCDRED")
+	    call pargstr ("IMAGE")
+	call printf ("%-8s  %-8s  %-8s  %-8s  %-8s\n")
+	    call pargstr ("PARAM")
+	    call pargstr ("KEYWORD")
+	    call pargstr ("VALUE")
+	    call pargstr ("VALUE")
+	    call pargstr ("VALUE")
+	call printf ("---------------------------------------")
+	call printf ("---------------------------------------\n")
+
+	# Print translations.  Select those printed only with the all parameter.
+	call ccdinst_p (im, "imagetyp", Memc[key], Memc[def], Memc[imval])
+	call ccdinst_p (im, "subset", Memc[key], Memc[def], Memc[imval])
+	call ccdinst_p (im, "exptime", Memc[key], Memc[def], Memc[imval])
+	call ccdinst_p (im, "darktime", Memc[key], Memc[def], Memc[imval])
+	if (level > 1) {
+	    call printf ("\n")
+	    call ccdinst_p (im, "biassec", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "trimsec", Memc[key], Memc[def], Memc[imval])
+	    call printf ("\n")
+	    call ccdinst_p (im, "fixpix", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "overscan", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "trim", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "zerocor", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "darkcor", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "flatcor", Memc[key], Memc[def], Memc[imval])
+	}
+	if (level > 2) {
+	    call ccdinst_p (im, "datasec", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "ccdsec", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "fixfile", Memc[key], Memc[def], Memc[imval])
+	    call printf ("\n")
+	    call ccdinst_p (im, "illumcor", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "fringcor", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "readcor", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "scancor", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "nscanrow", Memc[key], Memc[def], Memc[imval])
+	    call printf ("\n")
+	    call ccdinst_p (im, "illumflt", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "mkfringe", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "mkillum", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "skyflat", Memc[key], Memc[def], Memc[imval])
+	    call printf ("\n")
+	    call ccdinst_p (im, "ccdmean", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "fringscl", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "ncombine", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "date-obs", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "dec", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "ra", Memc[key], Memc[def], Memc[imval])
+	    call ccdinst_p (im, "title", Memc[key], Memc[def], Memc[imval])
+	}
+
+	call printf ("\n")
+	call flush (STDOUT)
+	call sfree (sp)
+end
+
+
+# CCDINST_P -- Print the translation for the specified translation name.
+
+procedure ccdinst_p (im, name, key, def, value)
+
+pointer	im			# Image pointer
+char	name[SZ_FNAME]		# CCDRED name
+char	key[SZ_FNAME]		# Image header keyword
+char	def[SZ_LINE]		# Default value
+char	value[SZ_LINE]		# Value
+
+int	i, strdic(), hdmaccf()
+bool	bval, ccdflag()
+
+begin
+	i = strdic (name, key, SZ_FNAME, CMDS)
+	if (i == 0)
+	    return
+
+	# Get translaltion image keyword, default, and image value.
+	call hdmname (name, key, SZ_FNAME)
+	call hdmgdef (name, def, SZ_LINE)
+	call hdmgstr (im, name, value, SZ_LINE)
+	if (value[1] == EOS)
+	    call strcpy ("?", value, SZ_LINE)
+
+	switch (i) {
+	case IMAGETYPE: 
+	    call printf ("%-8s  %-8s  %-8s")  
+		call pargstr (name)
+		call pargstr (key)
+		call pargstr (def)
+	    call ccdtypes (im, def, SZ_LINE)
+	    call printf ("  %-8s  %-.39s\n")  
+		call pargstr (def)
+		call pargstr (value)
+	case SUBSET: 
+	    call printf ("%-8s  %-8s  %-8s")  
+		call pargstr (name)
+		call pargstr (key)
+		call pargstr (def)
+	    call ccdsubset (im, def, SZ_LINE)
+	    call printf ("  %-8s  %-.39s\n")  
+		call pargstr (def)
+		call pargstr (value)
+	case FIXPIX, OVERSCAN, TRIM, ZEROCOR, DARKCOR, FLATCOR, ILLUMCOR,
+	     FRINGCOR, READCOR, SCANCOR, ILLUMFLT, MKFRINGE, MKILLUM,
+	     SKYFLAT:
+	    bval = ccdflag (im, name)
+	    if (hdmaccf (im, name) == NO)
+		call strcpy ("?", value, SZ_LINE)
+	    call printf ("%-8s  %-8s  %-8s  %-8b  %-.39s\n")  
+		call pargstr (name)
+		call pargstr (key)
+		call pargstr (def)
+		call pargb (bval)
+		call pargstr (value)
+	default:
+	    call printf ("%-8s  %-8s  %-8s  %-8s")  
+		call pargstr (name)
+		call pargstr (key)
+		call pargstr (def)
+		call pargstr (value)
+	    if (hdmaccf (im, name) == NO)
+		call strcpy ("?", value, SZ_LINE)
+	    call printf ("  %-.39s\n")  
+		call pargstr (value)
+	}
+end
+
+
+# CCDINST_E -- Edit a single translation entry.
+# This checks for parameters on the command line and if missing queries.
+# The default value may only be changed on the command line.
+
+procedure ccdinst_e (im, prompt, name, key, def, imval, update)
+
+pointer	im			# Image pointer
+char	prompt[ARB]		# Parameter prompt name
+char	name[SZ_FNAME]		# CCDRED name
+char	key[SZ_FNAME]		# Image header keyword
+char	def[SZ_LINE]		# Default value
+char	imval[SZ_LINE]		# Value
+bool	update			# Update translation file?
+
+bool	strne()
+int	i, scan(), nscan()
+pointer	sp, oldkey, olddef
+
+begin
+	    call smark (sp)
+	    call salloc (oldkey, SZ_FNAME, TY_CHAR)
+	    call salloc (olddef, SZ_LINE, TY_CHAR)
+
+	    # Get command line values
+	    call gargwrd (key, SZ_FNAME)
+	    call gargwrd (def, SZ_LINE)
+
+	    # Get current values
+	    call hdmname (name, Memc[oldkey], SZ_FNAME)
+	    call hdmgdef (name, Memc[olddef], SZ_LINE)
+
+	    # Query for keyword if needed.
+	    i = nscan()
+	    if (i < 2) {
+		call printf ("Image keyword for %s (%s): ")
+		    call pargstr (prompt)
+		    call pargstr (Memc[oldkey])
+		call flush (STDOUT)
+		if (scan() != EOF)
+		    call gargwrd (key, SZ_FNAME)
+		if (nscan() == 0)
+		    call strcpy (Memc[oldkey], key, SZ_FNAME)
+	    }
+	    if (i < 3) {
+		#call printf ("Default %s (%s): ")
+		#    call pargstr (prompt)
+		#    call pargstr (Memc[olddef])
+		#call flush (STDOUT)
+		#if (scan() != EOF)
+		#    call gargwrd (def, SZ_LINE)
+		#if (nscan() == 0)
+		    call strcpy (Memc[olddef], def, SZ_LINE)
+	    }
+
+	    # Update only if the new value is different from the old value.
+	    if (strne (key, Memc[oldkey])) { 
+	        call hdmpname (name, key)
+		update = true
+	    }
+	    if (strne (def, Memc[olddef])) {
+		call hdmpdef (name, def)
+		update = true
+	    }
+
+	    # Print the revised translation.
+	    call ccdinst_p (im, name, key, def, imval)
+	    call sfree (sp)
+end
+
+
+# CCDINST_G -- General procedure to prompt for value.
+
+procedure ccdinst_g (prompt, def, val)
+
+char	prompt[ARB]		# Prompt
+char	def[ARB]		# Default value
+char	val[SZ_LINE]		# Value
+
+int	scan(), nscan()
+
+begin
+	call printf ("%s (%s): ")
+	    call pargstr (prompt)
+	    call pargstr (def)
+	call flush (STDOUT)
+	if (scan() != EOF)
+	    call gargwrd (val, SZ_FNAME)
+	if (nscan() == 0)
+	    call strcpy (def, val, SZ_LINE)
+end
+
+
+define	USER_AREA	Memc[($1+IMU-1)*SZ_STRUCT + 1]
+
+# CCDINST_IMH -- Print the user area of the image, if nonzero length
+# and it contains only ascii values.  This copied from the code for
+# IMHEADER.  It differs in including the OBJECT keyword, using a temporary
+# file to page the header, and no leading blanks.
+
+procedure ccdinst_i (im, image)
+
+pointer	im			# image descriptor
+char	image[ARB]		# image name
+
+pointer	sp, tmp, lbuf, ip
+int	in, out, ncols, min_lenuserarea 
+int	open(), stropen(), getline(), envgeti()
+
+begin
+	call smark (sp)
+	call salloc (tmp, SZ_FNAME, TY_CHAR)
+	call salloc (lbuf, SZ_LINE, TY_CHAR)
+
+	# Open user area in header.
+	min_lenuserarea = (LEN_IMDES + IM_LENHDRMEM(im) - IMU) * SZ_STRUCT - 1
+	in = stropen (USER_AREA(im), min_lenuserarea, READ_ONLY)
+	ncols = envgeti ("ttyncols")
+
+	# Open temporary output file.
+	call mktemp ("tmp$", Memc[tmp], SZ_FNAME)
+	iferr (out = open (Memc[tmp], NEW_FILE, TEXT_FILE)) {
+	    call erract (EA_WARN)
+	    call sfree (sp)
+	    return
+	}
+
+	# Copy standard header records.
+	call fprintf (out, "OBJECT  = '%s'\n")
+	    call pargstr (IM_TITLE(im))
+
+	# Copy header records to the output, stripping any trailing
+	# whitespace and clipping at the right margin.
+
+	while (getline (in, Memc[lbuf]) != EOF) {
+	    for (ip=lbuf;  Memc[ip] != EOS && Memc[ip] != '\n';  ip=ip+1)
+		;
+	    while (ip > lbuf && Memc[ip-1] == ' ')
+		ip = ip - 1
+	    if (ip - lbuf > ncols)
+		ip = lbuf + ncols 
+	    Memc[ip] = '\n'
+	    Memc[ip+1] = EOS
+	    
+	    call putline (out, Memc[lbuf])
+	}
+	call putline (out, "\n")
+
+	call close (in)
+	call close (out)
+
+	call pagefile (Memc[tmp], image)
+	call delete (Memc[tmp])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/t_ccdlist.x b/noao/imred/ccdred/src/t_ccdlist.x
new file mode 100644
index 00000000..1b438b27
--- /dev/null
+++ b/noao/imred/ccdred/src/t_ccdlist.x
@@ -0,0 +1,325 @@
+include	<imhdr.h>
+include	<error.h>
+include	"ccdtypes.h"
+
+define	SZ_CCDLINE	80	# Size of line for output
+
+
+# T_CCDLIST -- List CCD image information and processing status.
+#
+# Each input image of the specified image type is listed in either a one
+# line short format, a name only format, or a longer format.  The image
+# name, size, pixel type, image type, subset ID, processing flags and
+# title are printed on one line.  For the long format image details of
+# the processing operations are printed.
+
+procedure t_ccdlist ()
+
+int	list, ccdtype
+bool	names, lformat
+pointer	sp, image, im
+
+bool	clgetb()
+int	imtopenp(), imtgetim()
+
+begin
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+
+	# Get the task parameters and open the translation file.
+	list = imtopenp ("images")
+	names = clgetb ("names")
+	lformat = clgetb ("long")
+	call clgstr ("instrument", Memc[image], SZ_FNAME)
+        if (Memc[image] == EOS)
+            call error (1, "No 'instrument' translation file specified.")
+	call hdmopen (Memc[image])
+
+	# List each iamge.
+	while (imtgetim (list, Memc[image], SZ_FNAME) != EOF) {
+	    # Map the image and the instrument header translation.
+	    # Check the image type.
+	    call set_input (Memc[image], im, ccdtype)
+	    if (im == NULL)
+		next
+
+	    # Select the output format.
+	    if (names) {
+		call printf ("%s\n")
+		    call pargstr (Memc[image])
+	    } else if (lformat) {
+	        call shortlist (Memc[image], ccdtype, im)
+		call longlist (im, ccdtype)
+	    } else
+	        call shortlist (Memc[image], ccdtype, im)
+	    call flush (STDOUT)
+
+	    call imunmap (im)
+	}
+
+	# Finish up.
+	call hdmclose ()
+	call imtclose (list)
+	call sfree (sp)
+end
+
+
+# SHORTLIST -- List the one line short format consisting of the image name,
+# iamge size, pixel type, image type, subset ID, processing flags, and
+# title.
+
+procedure shortlist (image, ccdtype, im)
+
+char	image			# Image name
+int	ccdtype			# CCD image type
+pointer	im			# IMIO pointer
+
+bool	ccdflag()
+pointer	sp, str, subset
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_CCDLINE, TY_CHAR)
+	call salloc (subset, SZ_CCDLINE, TY_CHAR)
+
+	# Get the image type and subset ID.
+	call ccdtypes (im, Memc[str], SZ_CCDLINE)
+	call ccdsubset (im, Memc[subset], SZ_CCDLINE)
+
+	# List the image name, size, pixel type, image type, and subset.
+	call printf ("%s[%d,%d][%s][%s][%d]")
+	    call pargstr (image)
+	    call pargi (IM_LEN(im,1))
+	    call pargi (IM_LEN(im,2))
+	    call pargtype1 (IM_PIXTYPE(im))
+	    call pargstr (Memc[str])
+	    call pargstr (Memc[subset])
+
+	# Format and list the processing flags.
+	Memc[str] = EOS
+	if (ccdflag (im, "fixpix"))
+	    call strcat ("B", Memc[str], SZ_CCDLINE)
+	if (ccdflag (im, "overscan"))
+	    call strcat ("O", Memc[str], SZ_CCDLINE)
+	if (ccdflag (im, "trim"))
+	    call strcat ("T", Memc[str], SZ_CCDLINE)
+	if (ccdflag (im, "zerocor"))
+	    call strcat ("Z", Memc[str], SZ_CCDLINE)
+	if (ccdflag (im, "darkcor"))
+	    call strcat ("D", Memc[str], SZ_CCDLINE)
+	if (ccdflag (im, "flatcor"))
+	    call strcat ("F", Memc[str], SZ_CCDLINE)
+	if (ccdflag (im, "illumcor"))
+	    call strcat ("I", Memc[str], SZ_CCDLINE)
+	if (ccdflag (im, "fringcor"))
+	    call strcat ("Q", Memc[str], SZ_CCDLINE)
+	if (Memc[str] != EOS) {
+	    call printf ("[%s]")
+		call pargstr (Memc[str])
+	}
+
+	# List the title.
+	call printf (":%s\n")
+	    call pargstr (IM_TITLE(im))
+
+	call sfree (sp)
+end
+
+
+# LONGLIST -- Add the long format listing.
+# List some instrument parameters and information about each processing
+# step indicated by the processing parameters.  If the processing step has
+# not been done yet indicate this and the parameters to be used.
+
+procedure longlist (im, ccdtype)
+
+pointer	im			# IMIO pointer
+int	ccdtype			# CCD image type
+
+real	rval, hdmgetr()
+pointer	sp, instr, outstr
+bool	clgetb(), ccdflag(), streq()
+define	done_	99
+
+begin
+	call smark (sp)
+	call salloc (instr, SZ_LINE, TY_CHAR)
+	call salloc (outstr, SZ_LINE, TY_CHAR)
+
+	# List some image parameters.
+	Memc[outstr] = EOS
+	ifnoerr (rval = hdmgetr (im, "exptime")) {
+	    call sprintf (Memc[instr], SZ_LINE, " exposure=%d")
+		call pargr (rval)
+	    call strcat (Memc[instr], Memc[outstr], SZ_LINE)
+	}
+	ifnoerr (rval = hdmgetr (im, "darktime")) {
+	    call sprintf (Memc[instr], SZ_LINE, " darktime=%d")
+		call pargr (rval)
+	    call strcat (Memc[instr], Memc[outstr], SZ_LINE)
+	}
+	call printf ("   %s\n")
+	    call pargstr (Memc[outstr])
+
+	# List the processing strings.
+	if (ccdflag (im, "fixpix")) {
+	    call hdmgstr (im, "fixpix", Memc[outstr], SZ_LINE)
+	    call printf ("    %s\n")
+		call pargstr (Memc[outstr])
+	} else if (clgetb ("fixpix")) {
+	    call clgstr ("fixfile", Memc[outstr], SZ_LINE)
+	    if (streq (Memc[outstr], "image"))
+		call hdmgstr (im, "fixfile", Memc[outstr], SZ_LINE)
+	    if (Memc[outstr] != EOS) {
+	        call printf ("    [TO BE DONE] Bad pixel file is %s\n")
+		    call pargstr (Memc[outstr])
+	    } else
+	        call printf (
+		    "    [TO BE DONE] Bad pixel file needs to be specified\n")
+	}
+
+	if (ccdflag (im, "overscan")) {
+	    call hdmgstr (im, "overscan", Memc[outstr], SZ_LINE)
+	    call printf ("    %s\n")
+		call pargstr (Memc[outstr])
+	} else if (clgetb ("overscan")) {
+	    call clgstr ("biassec", Memc[outstr], SZ_LINE)
+	    if (streq (Memc[outstr], "image"))
+		call hdmgstr (im, "biassec", Memc[outstr], SZ_LINE)
+	    call printf ("    [TO BE DONE] Overscan strip is %s\n")
+		call pargstr (Memc[outstr])
+	}
+
+	if (ccdflag (im, "trim")) {
+	    call hdmgstr (im, "trim", Memc[outstr], SZ_LINE)
+	    call printf ("    %s\n")
+		call pargstr (Memc[outstr])
+	} else if (clgetb ("trim")) {
+	    call clgstr ("trimsec", Memc[outstr], SZ_LINE)
+	    if (streq (Memc[outstr], "image"))
+		call hdmgstr (im, "trimsec", Memc[outstr], SZ_LINE)
+	    call printf ("    [TO BE DONE] Trim image section is %s\n")
+		call pargstr (Memc[outstr])
+	}
+
+	if (ccdtype == ZERO) {
+	    if (ccdflag (im, "readcor")) {
+		call hdmgstr (im, "readcor", Memc[outstr], SZ_LINE)
+	        call printf ("    %s\n")
+		    call pargstr (Memc[outstr])
+	    } else if (clgetb ("readcor"))
+	        call printf (
+		    "    [TO BE DONE] Convert to readout format\n")
+	    goto done_
+	}
+	if (ccdflag (im, "zerocor")) {
+	    call hdmgstr (im, "zerocor", Memc[outstr], SZ_LINE)
+	    call printf ("    %s\n")
+		call pargstr (Memc[outstr])
+	} else if (clgetb ("zerocor"))
+	    call printf ("    [TO BE DONE] Zero level correction\n")
+
+	if (ccdtype == DARK)
+	    goto done_
+	if (ccdflag (im, "darkcor")) {
+	    call hdmgstr (im, "darkcor", Memc[outstr], SZ_LINE)
+	    call printf ("    %s\n")
+		call pargstr (Memc[outstr])
+	} else if (clgetb ("darkcor"))
+	    call printf ("    [TO BE DONE] Dark count correction\n")
+
+	if (ccdtype == FLAT) {
+	    if (ccdflag (im, "scancor")) {
+		call hdmgstr (im, "scancor", Memc[outstr], SZ_LINE)
+	        call printf ("    %s\n")
+		    call pargstr (Memc[outstr])
+	    } else if (clgetb ("scancor"))
+	        call printf (
+		    "    [TO BE DONE] Convert to scan format\n")
+	    if (ccdflag (im, "skyflat")) {
+		call hdmgstr (im, "skyflat", Memc[outstr], SZ_LINE)
+	        call printf ("    %s\n")
+		    call pargstr (Memc[outstr])
+	    }
+	    if (ccdflag (im, "illumflt")) {
+		call hdmgstr (im, "illumflt", Memc[outstr], SZ_LINE)
+	        call printf ("    %s\n")
+		    call pargstr (Memc[outstr])
+	    }
+	    goto done_
+	}
+	if (ccdflag (im, "flatcor")) {
+	    call hdmgstr (im, "flatcor", Memc[outstr], SZ_LINE)
+	    call printf ("    %s\n")
+		call pargstr (Memc[outstr])
+	} else if (clgetb ("flatcor"))
+	    call printf ("    [TO BE DONE] Flat field correction\n")
+
+	if (ccdtype == ILLUM) {
+	    if (ccdflag (im, "mkillum")) {
+		call hdmgstr (im, "mkillum", Memc[outstr], SZ_LINE)
+	        call printf ("    %s\n")
+		    call pargstr (Memc[outstr])
+	    } else
+	        call printf (
+		    "    [TO BE DONE] Convert to illumination correction\n")
+	    goto done_
+	}
+	if (ccdflag (im, "illumcor")) {
+	    call hdmgstr (im, "illumcor", Memc[outstr], SZ_LINE)
+	    call printf ("    %s\n")
+		call pargstr (Memc[outstr])
+	} else if (clgetb ("illumcor"))
+	    call printf ("    [TO BE DONE] Illumination correction\n")
+
+	if (ccdtype == FRINGE)
+	    goto done_
+	if (ccdflag (im, "fringcor")) {
+	    call hdmgstr (im, "fringecor", Memc[outstr], SZ_LINE)
+	    call printf ("    %s\n")
+		call pargstr (Memc[outstr])
+	} else if (clgetb ("fringecor"))
+	    call printf ("    [TO BE DONE] Fringe correction\n")
+
+done_
+	call sfree (sp)
+end
+
+
+# PARGTYPE1 -- Convert an integer type code into a string, and output the
+# string with PARGSTR to FMTIO.  Taken from IMHEADER.
+
+procedure pargtype1 (dtype)
+
+int	dtype
+
+begin
+	switch (dtype) {
+	case TY_UBYTE:
+	    call pargstr ("ubyte")
+	case TY_BOOL:
+	    call pargstr ("bool")
+	case TY_CHAR:
+	    call pargstr ("char")
+	case TY_SHORT:
+	    call pargstr ("short")
+	case TY_USHORT:
+	    call pargstr ("ushort")
+	case TY_INT:
+	    call pargstr ("int")
+	case TY_LONG:
+	    call pargstr ("long")
+	case TY_REAL:
+	    call pargstr ("real")
+	case TY_DOUBLE:
+	    call pargstr ("double")
+	case TY_COMPLEX:
+	    call pargstr ("complex")
+	case TY_POINTER:
+	    call pargstr ("pointer")
+	case TY_STRUCT:
+	    call pargstr ("struct")
+	default:
+	    call pargstr ("unknown datatype")
+	}
+end
diff --git a/noao/imred/ccdred/src/t_ccdmask.x b/noao/imred/ccdred/src/t_ccdmask.x
new file mode 100644
index 00000000..d5d074cb
--- /dev/null
+++ b/noao/imred/ccdred/src/t_ccdmask.x
@@ -0,0 +1,384 @@
+include	<imhdr.h>
+
+
+define	MAXBUF		500000	# Maximum pixel buffer
+
+define	PLSIG		30.9	# Low percentile
+define	PHSIG		69.1	# High percentile
+
+
+# T_CCDMASK -- Create a bad pixel mask from CCD images.
+# Deviant pixels relative to a local median and sigma are detected and
+# written to a pixel mask file.  There is a special algorithm for detecting
+# long column oriented features typical of CCD defects.  This task
+# is intended for use on flat fields or, even better, the ratio of
+# two flat fields at different exposure levels.
+
+procedure t_ccdmask ()
+
+pointer	image			# Input image
+pointer	mask			# Output mask
+int	ncmed, nlmed		# Median box size
+int	ncsig, nlsig		# Sigma box size
+real	lsig, hsig		# Threshold sigmas
+int	ngood			# Minmum good pixel sequence
+short	linterp			# Mask value for line interpolation 
+short	cinterp			# Mask value for column interpolation 
+short	eqinterp		# Mask value for equal interpolation
+
+int	i, j, c1, c2, c3, c4, nc, nl, ncstep, nc1
+pointer	sp, in, out, inbuf, outbuf
+real	clgetr()
+int	clgeti(), nowhite(), strmatch()
+pointer	immap(), imgs2r(), imps2s(), imgl2s(), impl2s()
+errchk	immap, imgs2r, imps2r, imgl2s, impl2s, cm_mask
+
+begin
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (mask, SZ_FNAME, TY_CHAR)
+
+	# Get parameters.
+	call clgstr ("image", Memc[image], SZ_FNAME)
+	call clgstr ("mask", Memc[mask], SZ_FNAME)
+	ncmed = clgeti ("ncmed")
+	nlmed = clgeti ("nlmed")
+	ncsig = clgeti ("ncsig")
+	nlsig = clgeti ("nlsig")
+	lsig = clgetr ("lsigma")
+	hsig = clgetr ("hsigma")
+	ngood = clgeti ("ngood")
+	linterp = clgeti ("linterp")
+	cinterp = clgeti ("cinterp")
+	eqinterp = clgeti ("eqinterp")
+
+	# Force a pixel list format.
+	i = nowhite (Memc[mask], Memc[mask], SZ_FNAME)
+	if (strmatch (Memc[mask], ".pl$") == 0)
+	    call strcat (".pl", Memc[mask], SZ_FNAME)
+
+	# Map the input and output images.
+	in = immap (Memc[image], READ_ONLY, 0)
+	out = immap (Memc[mask], NEW_COPY, in)
+
+	# Go through the input in large blocks of columns.  If the
+	# block is smaller than the whole image overlap the blocks
+	# so the median only has boundaries at the ends of the image.
+	# Set the mask values based on the distances to the nearest
+	# good pixels.
+
+	nc = IM_LEN(in,1)
+	nl = IM_LEN(in,2)
+	ncstep = max (1, MAXBUF / nl - ncmed)
+
+	outbuf = NULL
+	do i = 1, nc, ncstep {
+	    c1 = i
+	    c2 = min (nc, i + ncstep - 1)
+	    c3 = max (1, c1 - ncmed / 2)
+	    c4 = min (nc, c2 + ncmed / 2)
+	    nc1 = c4 - c3 + 1
+	    inbuf = imgs2r (in, c3, c4, 1, nl)
+	    if (outbuf == NULL)
+		call malloc (outbuf, nc1*nl, TY_SHORT)
+	    else
+		call realloc (outbuf, nc1*nl, TY_SHORT)
+	    call aclrs (Memc[outbuf], nc1*nl)
+	    call cm_mask (Memr[inbuf], Mems[outbuf], nc1, nl, c1-c3+1,
+		c2-c3+1, ncmed, nlmed, ncsig, nlsig, lsig, hsig, ngood)
+	    call cm_interp (Mems[outbuf], nc1, nl, c1-c3+1, c2-c3+1, nc,
+		linterp, cinterp, eqinterp)
+	    do j = 1, nl
+		call amovs (Mems[outbuf+(j-1)*nc1+c1-c3],
+		    Mems[imps2s(out,c1,c2,j,j)], c2-c1+1)
+	}
+	call mfree (outbuf, TY_SHORT)
+
+	call imunmap (out)
+	call imunmap (in)
+
+	# If the image was searched in blocks we need another pass to find
+	# the lengths of bad pixel regions along lines since they may
+	# span the block edges.  Previously the mask values were set
+	# to the column lengths so in this pass we can just look at
+	# whole lines sequentially.
+
+	if (nc1 != nc) {
+	    out = immap (Memc[mask], READ_WRITE, 0)
+	    do i = 1, nl {
+		inbuf = imgl2s (out, i)
+		outbuf = impl2s (out, i)
+		call cm_interp1 (Mems[inbuf], Mems[outbuf], nc, nl,
+		    linterp, cinterp, eqinterp)
+	    }
+	    call imunmap (out)
+	}
+
+	call sfree (sp)
+end
+
+
+# CM_MASK -- Compute the mask image.
+# A local background is computed using moving box medians to avoid
+# contaminating bad pixels.  The local sigma is computed in blocks (it is not
+# a moving box for efficiency) by using a percentile point of the sorted
+# pixel values to estimate the width of the distribution uncontaminated by
+# bad pixels).  Once the background and sigma are known deviant pixels are
+# found by using sigma threshold factors.  Sums of pixels along columns are
+# checked at various scales from single pixels to whole columns with the
+# sigma level set appropriately.  The provides sensitivity to weaker column
+# features such as CCD traps.
+
+procedure cm_mask (data, bp, nc, nl, nc1, nc2, ncmed, nlmed, ncsig, nlsig,
+	lsig, hsig, ngood)
+
+real	data[nc,nl]		#I Pixel array
+short	bp[nc,nl]		#U Bad pixel array (0=good, 1=bad)
+int	nc, nl			#I Number of columns and lines
+int	nc1, nc2		#I Columns to compute
+int	ncmed, nlmed		#I Median box size
+int	ncsig, nlsig		#I Sigma box size
+real	lsig, hsig		#I Threshold sigmas
+int	ngood			#I Minimum good pixel sequence
+
+int	i, j, k, l, m, nsum, plsig, phsig, jsig
+real	back, sigma, sum1, sum2, low, high, amedr()
+pointer	sp, bkg, sig, work, bp1, ptr
+
+begin
+	call smark (sp)
+	call salloc (bkg, nl, TY_REAL)
+	call salloc (sig, nl/nlsig, TY_REAL)
+	call salloc (work, max (ncsig*nlsig, ncmed*nlmed), TY_REAL)
+	call salloc (bp1, nl, TY_SHORT)
+
+	bkg = bkg - 1
+	sig = sig - 1
+
+	i = nlsig * ncsig
+	plsig = nint (PLSIG*i/100.-1)
+	phsig = nint (PHSIG*i/100.-1)
+
+	do i = nc1, nc2 {
+
+	    # Compute median background.  This is a moving median.
+	    l = min (nc, i+ncmed/2)
+	    l = max (1, l-ncmed+1)
+	    do j = 1, nl {
+		k = min (nl, j+nlmed/2)
+		k = max (1, k-nlmed+1)
+		ptr = work
+		do m = k, k+nlmed-1 {
+		    call amovr (data[l,m], Memr[ptr], ncmed)
+		    ptr = ptr + ncmed
+		}
+		back = amedr (Memr[work], ncmed * nlmed)
+		Memr[bkg+j] = back
+	    }
+
+	    # Compute sigmas from percentiles.  This is done in blocks.
+	    if (mod (i-nc1, ncsig) == 0 && i<nc-ncsig+1) {
+		do j = 1, nl-nlsig+1, nlsig {
+		    ptr = work
+		    do k = j, j+nlsig-1 {
+			call amovr (data[i,k], Memr[ptr], ncsig)
+			ptr = ptr + ncsig
+		    }
+		    call asrtr (Memr[work], Memr[work], ncsig*nlsig)
+		    sigma = Memr[work+phsig] - Memr[work+plsig]
+		    jsig = (j+nlsig-1) / nlsig
+		    Memr[sig+jsig] = sigma**2
+		}
+	    }
+
+	    # Single pixel iterative rejection.
+	    k = 0
+	    do j = 1, nl {
+		if (bp[i,j] == 1)
+		    k = k + 1
+		else {
+		    jsig = min ((j+nlsig-1)/nlsig, nl/nlsig)
+		    back = Memr[bkg+j]
+		    sigma = sqrt (Memr[sig+jsig])
+		    low = back - lsig * sigma
+		    high = back + hsig * sigma
+		    if (data[i,j] < low || data[i,j] > high) {
+			bp[i,j] = 1
+			k = k + 1
+		    }
+		}
+	    }
+	    if (k == nl)
+		next
+
+	    # Reject over column sums at various scales.
+	    # Ignore previously rejected pixels.
+
+	    l = 2
+	    while (l <= nl) {
+		do j = 1, nl
+		    Mems[bp1+j-1] = bp[i,j]
+		sum1 = 0
+		sum2 = 0
+		nsum = 0
+		k = 1
+		do j = k, l-1 {
+		    if (bp[i,j] == 1)
+			next
+		    jsig = min ((j+nlsig-1)/nlsig, nl/nlsig)
+		    sum1 = sum1 + data[i,j] - Memr[bkg+j]
+		    sum2 = sum2 + Memr[sig+jsig]
+		    nsum = nsum + 1
+		}
+		do j = l, nl {
+		    if (bp[i,j] == 0) {
+			jsig = min ((j+nlsig-1)/nlsig, nl/nlsig)
+			sum1 = sum1 + data[i,j] - Memr[bkg+j]
+			sum2 = sum2 + Memr[sig+jsig]
+			nsum = nsum + 1
+		    }
+		    if (nsum > 0) {
+			sigma = sqrt (sum2)
+			low = -lsig * sigma
+			high = hsig * sigma
+			if (sum1 < low || sum1 > high)
+			    do m = k, j
+				bp[i,m] = 1
+		    }
+		    if (Mems[bp1+k-1] == 0) {
+			jsig = min ((k+nlsig-1)/nlsig, nl/nlsig)
+			sum1 = sum1 - data[i,k] + Memr[bkg+k]
+			sum2 = sum2 - Memr[sig+jsig]
+			nsum = nsum - 1
+		    }
+		    k = k + 1
+		}
+
+		if (l == nl)
+		    break
+		else if (l < 10)
+		    l = l + 1
+		else
+		    l = min (l * 2, nl)
+	    }
+
+	    # Coalesce small good regions along columns.
+	    if (ngood > 1) {
+		for (k=1; k<=nl && bp[i,k]!=0; k=k+1)
+		    ;
+		while (k < nl) {
+		    for (l=k+1; l<=nl && bp[i,l]==0; l=l+1)
+			;
+		    if (l-k < ngood)
+			do j = k, l-1
+			    bp[i,j] = 1
+		    for (k=l+1; k<=nl && bp[i,k]!=0; k=k+1)
+			;
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# CM_INTERP -- Compute the lengths of bad regions along columns and lines.
+# If only part of the image is buffered set the pixel mask values
+# to the column lengths so a later pass can compare these values against
+# the full line lengths.  If the whole image is buffered then both
+# the column and line lengths can be determined and the the mask values
+# set based on these lengths.
+
+procedure cm_interp (bp, nc, nl, nc1, nc2, ncimage, linterp, cinterp, eqinterp)
+
+short	bp[nc,nl]		#U Bad pixel array
+int	nc, nl			#I Number of columns and lines
+int	nc1, nc2		#I Columns to compute
+int	ncimage			#I Number of columns in image
+short	linterp			#I Mask value for line interpolation 
+short	cinterp			#I Mask value for column interpolation 
+short	eqinterp		#I Mask value for equal interpolation
+
+int	i, j, k, l, m, n
+
+begin
+	do i = nc1, nc2 {
+
+	    # Set values to column length.
+	    for (k=1; k<=nl && bp[i,k]==0; k=k+1)
+		;
+	    while (k <= nl) {
+		for (l=k+1; l<=nl && bp[i,l]!=0; l=l+1)
+		    ;
+		m = l - k
+		do j = k, l-1
+		    bp[i,j] = m
+		for (k=l+1; k<=nl && bp[i,k]==0; k=k+1)
+		    ;
+	    }
+	}
+
+	# Set values to minimum axis length for interpolation.
+	if (nc == ncimage) {
+	    do j = 1, nl {
+		for (k=1; k<=nc && bp[k,j]==0; k=k+1)
+		    ;
+		while (k <= nc) {
+		    for (l=k+1; l<=nc && bp[l,j]!=0; l=l+1)
+			;
+		    m = l - k
+		    do i = k, l-1 {
+			n = bp[i,j]
+			if (n > m || n == nl)
+			    bp[i,j] = linterp
+			else if (n < m)
+			    bp[i,j] = cinterp
+			else
+			    bp[i,j] = eqinterp
+		    }
+		    for (k=l+1; k<=nc && bp[k,j]==0; k=k+1)
+			;
+		}
+	    }
+	}
+end
+
+
+# CM_INTERP1 -- Set the mask values based on the column and line lengths
+# of the bad pixel regions.  If this routine is called the pixel mask
+# is open READ/WRITE and the pixel mask values have been previously set
+# to the column lengths.  So here we just need to compute the line
+# lengths across the entire image and reset the mask values to the
+# appropriate interpolation mask code.
+
+procedure cm_interp1 (in, out, nc, nl, linterp, cinterp, eqinterp)
+
+short	in[nc]			#I Bad pixel array with column length codes
+short	out[nc]			#O Bad pixel array with interp axis codes
+int	nc, nl			#I Image dimensions
+short	linterp			#I Mask value for line interpolation 
+short	cinterp			#I Mask value for column interpolation 
+short	eqinterp		#I Mask value for equal interpolation
+
+int	i, j, l, m, n
+
+begin
+	for (j=1; j<=nc && in[j]==0; j=j+1)
+	    out[j] = 0
+	while (j < nc) {
+	    for (l=j+1; l<=nc && in[l]!=0; l=l+1)
+		;
+	    m = l - j
+	    do i = j, l-1 {
+		n = in[i]
+		if (n > m || n == nl)
+		    out[i] = linterp
+		else if (n < m)
+		    out[i] = cinterp
+		else
+		    out[i] = eqinterp
+	    }
+	    for (j=l+1; j<=nc && in[j]==0; j=j+1)
+		out[j] = 0
+	}
+end
diff --git a/noao/imred/ccdred/src/t_ccdproc.x b/noao/imred/ccdred/src/t_ccdproc.x
new file mode 100644
index 00000000..31e9ae6e
--- /dev/null
+++ b/noao/imred/ccdred/src/t_ccdproc.x
@@ -0,0 +1,176 @@
+include	<imhdr.h>
+include	<error.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+define	CACHEUNIT	1000000.	# Units of max_cache parameter
+
+# T_CCDPROC -- Process CCD images
+#
+# This is the main procedure for processing CCD images.  The images are
+# corrected for bad pixels, overscan levels, zero levels, dark counts,
+# flat field response, illumination errors, and fringe response.  They
+# may also be trimmed.  The input is a list of images to be processed.
+# Each image must match any image type requested.  The checking of
+# whether to apply each correction, getting the required parameters, and
+# logging the operations is left to separate procedures, one for each
+# correction.  The actual processing is done by a specialized procedure
+# designed to be very efficient.  These procedures may also process
+# calibration images if necessary.  There are two data type paths; one
+# for short pixel types and one for all other pixel types (usually
+# real).
+
+procedure t_ccdproc ()
+
+int	list			# List of CCD images to process
+int	outlist			# LIst of output images
+int	ccdtype			# CCD image type
+int	interactive		# Fit overscan interactively?
+int	max_cache		# Maximum image cache size
+
+bool	clgetb()
+real	clgetr()
+int	imtopenp(), imtgetim(), imtlen()
+pointer	sp, input, output, str, in, out, ccd
+errchk	set_input, set_output, ccddelete, cal_open
+errchk	set_fixpix, set_zero, set_dark, set_flat, set_illum, set_fringe
+
+begin
+	call smark (sp)
+	call salloc (input, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get input and output lists and check they make sense.
+	list = imtopenp ("images")
+	outlist = imtopenp ("output")
+	if (imtlen (outlist) > 0 && imtlen (outlist) != imtlen (list))
+	    call error (1, "Input and output lists do not match")
+
+	# Get instrument translation file.  Open the translation
+	# file.  Initialize the interactive flag and the calibration images.
+
+	call clgstr ("instrument", Memc[input], SZ_FNAME)
+	if (Memc[input] == EOS)
+	    call error (1, "No 'instrument' translation file specified.")
+	call hdmopen (Memc[input])
+	call set_interactive ("", interactive)
+	call cal_open (list)
+	if (imtlen (list) < 3)
+	    max_cache = 0.
+	else
+	    max_cache = CACHEUNIT * clgetr ("max_cache")
+	call ccd_open (max_cache)
+
+	# Process each image.
+	while (imtgetim (list, Memc[input], SZ_FNAME) != EOF) {
+	    if (clgetb ("noproc")) {
+		call printf ("%s:\n")
+		    call pargstr (Memc[input])
+	    }
+	    call set_input (Memc[input], in, ccdtype)
+	    if (in == NULL)
+		next
+
+	    # Set output image.
+	    if (imtlen (outlist) == 0)
+		call mktemp ("tmp", Memc[output], SZ_FNAME)
+	    else if (imtgetim (outlist, Memc[output], SZ_FNAME) == EOF)
+		call error (1, "Premature end of output list")
+	    call set_output (in, out, Memc[output])
+
+	    # Set processing parameters applicable to all images.
+	    call set_proc (in, out, ccd)
+	    call set_sections (ccd)
+	    call set_trim (ccd)
+	    call set_fixpix (ccd)
+	    call set_overscan (ccd)
+
+	    # Set processing parameters for the standard CCD image types.
+	    switch (ccdtype) {
+	    case ZERO:
+	    case DARK:
+	        call set_zero (ccd)
+	    case FLAT:
+	        call set_zero (ccd)
+	        call set_dark (ccd)
+		CORS(ccd, FINDMEAN) = YES
+		CORS(ccd, MINREP) = YES
+	    case ILLUM:
+	        call set_zero (ccd)
+	        call set_dark (ccd)
+	        call set_flat (ccd)
+	    case OBJECT, COMP:
+	        call set_zero (ccd)
+	        call set_dark (ccd)
+	        call set_flat (ccd)
+		iferr {
+	            call set_illum (ccd)
+	            call set_fringe (ccd)
+		} then
+		    call erract (EA_WARN)
+	    default:
+	        call set_zero (ccd)
+	        call set_dark (ccd)
+	        call set_flat (ccd)
+		iferr {
+		    call set_illum (ccd)
+	            call set_fringe (ccd)
+	        } then
+		    call erract (EA_WARN)
+		CORS(ccd, FINDMEAN) = YES
+	    }
+
+	    # Do the processing if the COR flag is set.
+
+	    if (COR(ccd) == YES) {
+		call doproc (ccd)
+		call set_header (ccd)
+
+	        call imunmap (in)
+	        call imunmap (out)
+		if (imtlen (outlist) == 0) {
+		    # Replace the input image by the corrected image.
+		    iferr (call ccddelete (Memc[input])) {
+			call imdelete (Memc[output])
+			call error (1,
+			    "Can't delete or make backup of original image")
+		    }
+		    call imrename (Memc[output], Memc[input])
+		}
+	    } else {
+		# Delete the output image.
+	        call imunmap (in)
+	        iferr (call imunmap (out))
+		    ;
+		iferr (call imdelete (Memc[output]))
+		    ;
+	    }
+	    call free_proc (ccd)
+
+	    # Do special processing on certain image types.
+	    if (imtlen (outlist) == 0) {
+		switch (ccdtype) {
+		case ZERO:
+		    call readcor (Memc[input])
+		case FLAT:
+		    call ccdmean (Memc[input])
+		}
+	    } else {
+		switch (ccdtype) {
+		case ZERO:
+		    call readcor (Memc[output])
+		case FLAT:
+		    call ccdmean (Memc[output])
+		}
+	    }
+	}
+
+	# Finish up.
+	call hdmclose ()
+	call imtclose (list)
+	call imtclose (outlist)
+	call cal_close ()
+	call ccd_close ()
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/t_combine.x b/noao/imred/ccdred/src/t_combine.x
new file mode 100644
index 00000000..66c14089
--- /dev/null
+++ b/noao/imred/ccdred/src/t_combine.x
@@ -0,0 +1,653 @@
+include	<imhdr.h>
+include	<error.h>
+include	<syserr.h>
+include	<mach.h>
+include	"ccdred.h"
+include	"icombine.h"
+
+
+# T_COMBINE -- Combine CCD images.
+# This task is a copy of IMAGES.IMCOMBINE except that it recognizes the
+# CCD types and can group images by AMP and SUBSET.  It also uses header
+# keyword translation for the exposure times.
+
+procedure t_combine ()
+
+pointer	images			# Images
+pointer	extns			# Image extensions for each subset
+pointer	subsets			# Subsets
+pointer	nimages			# Number of images in each subset
+int	nsubsets		# Number of subsets
+pointer	outroot			# Output root image name
+pointer	plroot			# Output pixel list root name
+pointer	sigroot			# Output root sigma image name
+pointer	logfile			# Log filename
+bool	delete			# Delete input images?
+
+int	i
+pointer	sp, output, plfile, sigma
+
+bool	clgetb()
+int	clgeti(), clgwrd()
+real	clgetr()
+
+include	"icombine.com"
+
+begin
+	call smark (sp)
+	call salloc (outroot, SZ_FNAME, TY_CHAR)
+	call salloc (plroot, SZ_FNAME, TY_CHAR)
+	call salloc (sigroot, SZ_FNAME, TY_CHAR)
+	call salloc (logfile, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (plfile, SZ_FNAME, TY_CHAR)
+	call salloc (sigma, SZ_FNAME, TY_CHAR)
+	call salloc (gain, SZ_FNAME, TY_CHAR)
+	call salloc (snoise, SZ_FNAME, TY_CHAR)
+	call salloc (rdnoise, SZ_FNAME, TY_CHAR)
+	call salloc (logfile, SZ_FNAME, TY_CHAR)
+
+	# Open the header translation which is needed to determine the
+	# amps, subsets and ccdtypes.  Get the input images.
+	# There must be a least one image in order to continue.
+
+	call clgstr ("instrument", Memc[output], SZ_FNAME)
+        if (Memc[output] == EOS)
+            call error (1, "No 'instrument' translation file specified.")
+	call hdmopen (Memc[output])
+	call cmb_images (images, extns, subsets, nimages, nsubsets)
+	if (nsubsets == 0)
+	    call error (0, "No images to combine")
+
+	# Get task parameters.  Some additional parameters are obtained later.
+	call clgstr ("output", Memc[outroot], SZ_FNAME)
+	call clgstr ("plfile", Memc[plroot], SZ_FNAME)
+	call clgstr ("sigma", Memc[sigroot], SZ_FNAME)
+	call clgstr ("logfile", Memc[logfile], SZ_FNAME)
+	call xt_stripwhite (Memc[outroot])
+	call xt_stripwhite (Memc[sigroot])
+	call xt_stripwhite (Memc[logfile])
+
+	project = clgetb ("project")
+	combine = clgwrd ("combine", Memc[output], SZ_FNAME, COMBINE)
+        reject = clgwrd ("reject", Memc[output], SZ_FNAME, REJECT)
+        blank = clgetr ("blank")
+        call clgstr ("gain", Memc[gain], SZ_FNAME)
+        call clgstr ("rdnoise", Memc[rdnoise], SZ_FNAME)
+        call clgstr ("snoise", Memc[snoise], SZ_FNAME)
+        lthresh = clgetr ("lthreshold")
+        hthresh = clgetr ("hthreshold")
+        lsigma = clgetr ("lsigma")
+        hsigma = clgetr ("hsigma")
+        grow = clgeti ("grow")
+        mclip = clgetb ("mclip")
+        sigscale = clgetr ("sigscale")
+	delete = clgetb ("delete")
+
+        # Check parameters, map INDEFs, and set threshold flag
+        if (IS_INDEFR (blank))
+            blank = 0.
+        if (IS_INDEFR (lsigma))
+            lsigma = MAX_REAL
+        if (IS_INDEFR (hsigma))
+            hsigma = MAX_REAL
+        if (IS_INDEFI (grow))
+            grow = 0
+        if (IS_INDEF (sigscale))
+            sigscale = 0.
+
+        if (IS_INDEF(lthresh) && IS_INDEF(hthresh))
+            dothresh = false
+        else {
+            dothresh = true
+            if (IS_INDEF(lthresh))
+                lthresh = -MAX_REAL
+            if (IS_INDEF(hthresh))
+                hthresh = MAX_REAL
+        }
+
+	# This is here for backward compatibility.
+	if (clgetb ("clobber"))
+	    call error (1, "Clobber option is no longer supported")
+
+	# Combine each input subset.
+	do i = 1, nsubsets {
+	    # Set the output, pl, and sigma image names with subset extension.
+
+	    call strcpy (Memc[outroot], Memc[output], SZ_FNAME)
+	    call sprintf (Memc[output], SZ_FNAME, "%s%s")
+		call pargstr (Memc[outroot])
+		call pargstr (Memc[Memi[extns+i-1]])
+
+	    call strcpy (Memc[plroot], Memc[plfile], SZ_FNAME)
+	    if (Memc[plfile] != EOS) {
+		call sprintf (Memc[plfile], SZ_FNAME, "%s%s")
+		    call pargstr (Memc[plroot])
+		    # Use this if we can append pl files.
+		    #call pargstr (Memc[Memi[extns+i-1]])
+		    call pargstr (Memc[Memi[subsets+i-1]])
+	    }
+
+	    call strcpy (Memc[sigroot], Memc[sigma], SZ_FNAME)
+	    if (Memc[sigma] != EOS) {
+		call sprintf (Memc[sigma], SZ_FNAME, "%s%s")
+		    call pargstr (Memc[sigroot])
+		    call pargstr (Memc[Memi[extns+i-1]])
+	    }
+
+	    # Combine all images from the (subset) list.
+	    iferr (call icombine (Memc[Memi[images+i-1]], Memi[nimages+i-1],
+		Memc[output], Memc[plfile], Memc[sigma],
+		Memc[logfile], NO, delete)) {
+		call erract (EA_WARN)
+	    }
+	    call mfree (Memi[images+i-1], TY_CHAR)
+	    call mfree (Memi[extns+i-1], TY_CHAR)
+	    call mfree (Memi[subsets+i-1], TY_CHAR)
+	}
+
+	# Finish up.
+	call mfree (images, TY_POINTER)
+	call mfree (extns, TY_POINTER)
+	call mfree (subsets, TY_POINTER)
+	call mfree (nimages, TY_INT)
+	call hdmclose ()
+	call sfree (sp)
+end
+
+
+# CMB_IMAGES -- Get images from a list of images.
+# The images are filtered by ccdtype and sorted by amplifier and subset.
+# The allocated lists must be freed by the caller.
+
+procedure cmb_images (images, extns, subsets, nimages, nsubsets)
+
+pointer	images		# Pointer to lists of subsets (allocated)
+pointer	extns		# Image extensions for each subset (allocated)
+pointer	subsets		# Subset names (allocated)
+pointer	nimages		# Number of images in subset (allocated)
+int	nsubsets	# Number of subsets
+
+int	list		# List of input images
+bool	doamps		# Divide input into subsets by amplifier?
+bool	dosubsets	# Divide input into subsets by subset parameter?
+bool	extend		# Add extensions to output image names?
+
+int	i, nimage, ccdtype
+pointer	sp, type, image, extn, subset, str, ptr, im
+#int	imtopenp(), imtlen(), imtgetim(), ccdtypecl(), ccdtypes()
+int	imtopenp(), imtlen(), imtgetim()
+pointer	immap()
+bool	clgetb(), streq()
+
+begin
+	# Get the input image list and check that there is at least one image.
+	nsubsets = 0
+	list = imtopenp ("input")
+	nimage = imtlen (list)
+	if (nimage == 0) {
+	    call imtclose (list)
+	    return
+	}
+
+	# Determine whether to divide images into subsets and append extensions.
+	#doamps = clgetb ("amps")
+	doamps = false
+	dosubsets = clgetb ("subsets")
+	#extend = clgetb ("extensions")
+	extend = true
+
+	call smark (sp)
+	call salloc (type, SZ_FNAME, TY_CHAR)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (extn, SZ_FNAME, TY_CHAR)
+	call salloc (subset, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_FNAME, TY_CHAR)
+
+	# Go through the input list and eliminate images not satisfying the
+	# CCD image type.  Separate into subsets if desired.  Create image
+	# and subset lists.
+
+	#ccdtype = ccdtypecl ("ccdtype", Memc[type], SZ_FNAME)
+	ccdtype = 0
+	call clgstr ("ccdtype", Memc[type], SZ_FNAME)
+	call xt_stripwhite (Memc[type])
+
+	while (imtgetim (list, Memc[image], SZ_FNAME)!=EOF) {
+	    iferr (im = immap (Memc[image], READ_ONLY, 0)) {
+		call erract (EA_WARN)
+		next
+	    }
+	    #ccdtype = ccdtypes (im, Memc[str], SZ_FNAME)
+	    call ccdtypes (im, Memc[str], SZ_FNAME)
+	    if (Memc[type] != EOS && !streq (Memc[str], Memc[type]))
+		next
+	    
+	    Memc[extn] = EOS
+	    Memc[subset] = EOS
+	    if (doamps) {
+		#call ccdamp (im, Memc[str], SZ_FNAME)
+		Memc[str] = EOS
+		if (extend)
+		    call strcat (Memc[str], Memc[extn], SZ_FNAME)
+		call strcat (Memc[str], Memc[subset], SZ_FNAME)
+	    }
+	    if (dosubsets) {
+		call ccdsubset (im, Memc[str], SZ_FNAME)
+		call strcat (Memc[str], Memc[extn], SZ_FNAME)
+		call strcat (Memc[str], Memc[subset], SZ_FNAME)
+	    }
+	    for (i=1; i <= nsubsets; i=i+1)
+		if (streq (Memc[subset], Memc[Memi[subsets+i-1]]))
+		    break
+
+	    if (i > nsubsets) {
+		if (nsubsets == 0) {
+		    call malloc (images, nimage, TY_POINTER)
+		    call malloc (extns, nimage, TY_POINTER)
+		    call malloc (subsets, nimage, TY_POINTER)
+		    call malloc (nimages, nimage, TY_INT)
+		} else if (mod (nsubsets, nimage) == 0) {
+		    call realloc (images, nsubsets+nimage, TY_POINTER)
+		    call realloc (extns, nsubsets+nimage, TY_POINTER)
+		    call realloc (subsets, nsubsets+nimage, TY_POINTER)
+		    call realloc (nimages, nsubsets+nimage, TY_INT)
+		}
+		nsubsets = i
+		call malloc (ptr, SZ_FNAME, TY_CHAR)
+		call strcpy (Memc[image], Memc[ptr], SZ_FNAME-1)
+		Memi[images+i-1] = ptr
+		call malloc (ptr, SZ_FNAME, TY_CHAR)
+		call strcpy (Memc[extn], Memc[ptr], SZ_FNAME)
+		Memi[extns+i-1] = ptr
+		call malloc (ptr, SZ_FNAME, TY_CHAR)
+		call strcpy (Memc[subset], Memc[ptr], SZ_FNAME)
+		Memi[subsets+i-1] = ptr
+		Memi[nimages+i-1] = 1
+	    } else {
+		ptr = Memi[images+i-1]
+		nimage = Memi[nimages+i-1] + 1
+		call realloc (ptr, nimage * SZ_FNAME, TY_CHAR)
+		Memi[images+i-1] = ptr
+		Memi[nimages+i-1] = nimage
+		ptr = ptr + (nimage - 1) * SZ_FNAME
+		call strcpy (Memc[image], Memc[ptr], SZ_FNAME-1)
+	    }
+		    
+	    call imunmap (im)
+	}
+	call realloc (images, nsubsets, TY_POINTER)
+	call realloc (extns, nsubsets, TY_POINTER)
+	call realloc (subsets, nsubsets, TY_POINTER)
+	call realloc (nimages, nsubsets, TY_INT)
+	call imtclose (list)
+	call sfree (sp)
+end
+
+
+# ICOMBINE -- Combine the CCD images in a list.
+# This procedure maps the images, sets the output dimensions and datatype,
+# opens the logfile, and sets IMIO parameters.  It attempts to adjust
+# buffer sizes and memory requirements for maximum efficiency.
+
+procedure icombine (images, nims, output, plfile, sigma, logfile, stack,
+	delete)
+
+char	images[SZ_FNAME-1, nims]	# Input images
+int	nims				# Number of images in list
+char	output[ARB]			# Output image
+char	plfile[ARB]			# Pixel list file
+char	sigma[ARB]			# Output sigma image
+char	logfile[ARB]			# Log filename
+int	stack				# Stack input images?
+bool	delete				# Delete input images?
+
+char	errstr[SZ_LINE]
+int	i, j, nimages, intype, bufsize, maxsize, memory, oldsize, stack1, err
+pointer	sp, sp1, in, out[3], offsets, temp, key, tmp
+
+int	getdatatype()
+real	clgetr()
+char	clgetc()
+int	clgeti(), begmem(), errget(), open(), ty_max(), sizeof()
+pointer	immap(), ic_plfile()
+errchk	ic_imstack, immap, ic_plfile, ic_setout, ccddelete
+
+include	"icombine.com"
+
+define	retry_	98
+define	done_	99
+
+begin
+	call smark (sp)
+
+	# Set number of images to combine.
+	if (project) {
+	    if (nims > 1) {
+		call sfree (sp)
+		call error (1, "Cannot project combine a list of images")
+	    }
+	    tmp = immap (images[1,1], READ_ONLY, 0); out[1] = tmp
+	    if (IM_NDIM(out[1]) == 1)
+		call error (1, "Can't project one dimensional images")
+	    nimages = IM_LEN(out[1],IM_NDIM(out[1]))
+	    call imunmap (out[1])
+	} else
+	    nimages = nims
+
+	# Convert the nkeep parameter if needed.
+        # Convert the pclip parameter to a number of pixels rather than
+        # a fraction.  This number stays constant even if pixels are
+        # rejected.  The number of low and high pixel rejected, however,
+        # are converted to a fraction of the valid pixels.
+
+	nkeep = clgeti ("nkeep")
+	if (nkeep < 0)
+	    nkeep = max (0, nimages + nkeep)
+
+        if (reject == PCLIP) {
+	    pclip = clgetr ("pclip")
+	    if (pclip == 0.)
+		call error (1, "Pclip parameter may not be zero")
+	    if (IS_INDEFR (pclip))
+		pclip = -0.5
+
+            i = nimages / 2.
+            if (abs (pclip) < 1.)
+                pclip = pclip * i
+            if (pclip < 0.)
+                pclip = min (-1, max (-i, int (pclip)))
+            else
+                pclip = max (1, min (i, int (pclip)))
+        }
+
+        if (reject == MINMAX) {
+	    flow = clgetr ("nlow")
+	    fhigh = clgetr ("nhigh")
+	    if (IS_INDEFR (flow))
+		flow = 0
+	    if (IS_INDEFR (fhigh))
+		fhigh = 0
+
+            if (flow >= 1)
+                flow = flow / nimages
+            if (fhigh >= 1)
+                fhigh = fhigh / nimages
+            i = flow * nimages
+            j = fhigh * nimages
+            if (i + j == 0)
+                reject = NONE
+            else if (i + j >= nimages) {
+                call eprintf ("Bad minmax rejection parameters\n")
+		call sfree (sp)
+		return
+            }
+        }
+
+	# Map the input images.
+	bufsize = 0
+	stack1 = stack
+retry_
+	iferr {
+	    out[1] = NULL
+	    out[2] = NULL
+	    out[3] = NULL
+	    icm = NULL
+	    logfd = NULL
+
+	    call smark (sp1)
+	    if (stack1 == YES) {
+		call salloc (temp, SZ_FNAME, TY_CHAR)
+		call mktemp ("tmp", Memc[temp], SZ_FNAME)
+		call ic_imstack (images, nimages, Memc[temp])
+		project = true
+	    }
+
+	    # Map the input image(s).
+	    if (project) {
+		if (stack1 == YES) {
+		    tmp = immap (Memc[temp], READ_ONLY, 0); out[1] = tmp
+		} else {
+		    tmp = immap (images[1,1], READ_ONLY, 0); out[1] = tmp
+		}
+		nimages = IM_LEN(out[1],IM_NDIM(out[1]))
+		call calloc (in, nimages, TY_POINTER)
+		call amovki (out[1], Memi[in], nimages)
+	    } else {
+		call calloc (in, nimages, TY_POINTER)
+		do i = 1, nimages {
+		    tmp = immap (images[1,i], READ_ONLY, 0); Memi[in+i-1] = tmp
+		}
+	    }
+
+	    # Map the output image and set dimensions and offsets.
+	    tmp = immap (output, NEW_COPY, Memi[in]); out[1] = tmp
+	    if (stack1 == YES) {
+		call salloc (key, SZ_FNAME, TY_CHAR)
+		do i = 1, nimages {
+		    call sprintf (Memc[key], SZ_FNAME, "stck%04d")
+			call pargi (i)
+		    call imdelf (out[1], Memc[key])
+		}
+	    }
+	    call salloc (offsets, nimages*IM_NDIM(out[1]), TY_INT)
+	    call ic_setout (Memi[in], out, Memi[offsets], nimages)
+
+	    # Determine the highest precedence datatype and set output datatype.
+	    intype = IM_PIXTYPE(Memi[in])
+	    do i = 2, nimages
+		intype = ty_max (intype, IM_PIXTYPE(Memi[in+i-1]))
+	    IM_PIXTYPE(out[1]) = getdatatype (clgetc ("outtype"))
+	    if (IM_PIXTYPE(out[1]) == ERR)
+		IM_PIXTYPE(out[1]) = intype
+
+	    # Open pixel list file if given.
+	    if (plfile[1] != EOS) {
+		tmp = ic_plfile (plfile, NEW_COPY, out[1]); out[2] = tmp
+	    } else
+		out[2] = NULL
+
+	    # Open the sigma image if given.
+	    if (sigma[1] != EOS) {
+		tmp = immap (sigma, NEW_COPY, out[1]); out[3] = tmp
+		IM_PIXTYPE(out[3]) = ty_max (TY_REAL, IM_PIXTYPE(out[1]))
+		call sprintf (IM_TITLE(out[3]), SZ_IMTITLE,
+		    "Combine sigma images for %s")
+		    call pargstr (output)
+	    } else
+		out[3] = NULL
+
+	    # This is done here to work around problem adding a keyword to
+	    # an NEW_COPY header and then using that header in a NEW_COPY.
+
+	    # Open masks.
+	    call ic_mopen (Memi[in], out, nimages)
+
+	    # Open the log file.
+	    logfd = NULL
+	    if (logfile[1] != EOS) {
+		iferr (logfd = open (logfile, APPEND, TEXT_FILE)) {
+		    logfd = NULL
+		    call erract (EA_WARN)
+		}
+	    }
+
+	    if (bufsize == 0) {
+		# Set initial IMIO buffer size based on the number of images
+		# and maximum amount of working memory available.  The buffer
+		# size may be adjusted later if the task runs out of memory.
+		# The FUDGE factor is used to allow for the size of the
+		# program, memory allocator inefficiencies, and any other
+		# memory requirements besides IMIO.
+
+		bufsize = 1
+		do i = 1, IM_NDIM(out[1])
+		    bufsize = bufsize * IM_LEN(out[1],i)
+		bufsize = bufsize * sizeof (intype)
+		bufsize = min (bufsize, DEFBUFSIZE)
+		memory = begmem ((nimages + 1) * bufsize, oldsize, maxsize)
+		memory = min (memory, int (FUDGE * maxsize))
+		bufsize = memory / (nimages + 1)
+	    }
+
+	    # Combine the images.  If an out of memory error occurs close all
+	    # images and files, divide the IMIO buffer size in half and try
+	    # again.
+
+	    switch (intype) {
+	    case TY_SHORT:
+		call icombines (Memi[in], out, Memi[offsets], nimages,
+		    bufsize)
+	    default:
+		call icombiner (Memi[in], out, Memi[offsets], nimages,
+		    bufsize)
+	    }
+	} then {
+	    err = errget (errstr, SZ_LINE)
+	    if (icm != NULL)
+		call ic_mclose (nimages)
+	    if (!project) {
+		do j = 2, nimages
+		    if (Memi[in+j-1] != NULL)
+			call imunmap (Memi[in+j-1])
+	    }
+	    if (out[2] != NULL) {
+		call imunmap (out[2])
+		call imdelete (plfile)
+	    }
+	    if (out[3] != NULL) {
+		call imunmap (out[3])
+		call imdelete (sigma)
+	    }
+	    if (out[1] != NULL) {
+		call imunmap (out[1])
+		call imdelete (output)
+	    }
+	    if (Memi[in] != NULL)
+		call imunmap (Memi[in])
+	    if (logfd != NULL)
+		call close (logfd)
+
+	    switch (err) {
+	    case SYS_MFULL:
+		bufsize = bufsize / 2
+		call sfree (sp1)
+		goto retry_
+	    case SYS_FTOOMANYFILES, SYS_IKIOPIX:
+		if (!project) {
+		    stack1 = YES
+		    call sfree (sp1)
+		    goto retry_
+		}
+		if (stack1 == YES)
+		    call imdelete (Memc[temp])
+		call fixmem (oldsize)
+		call sfree (sp1)
+		call error (err, errstr)
+	    default:
+		if (stack1 == YES)
+		    call imdelete (Memc[temp])
+		call fixmem (oldsize)
+		call sfree (sp1)
+		call error (err, errstr)
+	    }
+	}
+
+        # Unmap all the images, close the log file, and restore memory.
+	# The input images must be unmapped first to insure that there
+	# is a FD for the output images since the headers are opened to
+	# update them.  However, the order of the NEW_COPY pointers must
+	# be preserved; i.e. the output depends on the first input image,
+	# and the extra output images depend on the output image.
+
+	if (!project) {
+	    do i = 2, nimages {
+		if (Memi[in+i-1] != NULL) {
+		    call imunmap (Memi[in+i-1])
+		    if (delete)
+			call ccddelete (images[1,i])
+		}
+	    }
+	}
+	if (out[2] != NULL)
+	    call imunmap (out[2])
+	if (out[3] != NULL)
+	    call imunmap (out[3])
+	if (out[1] != NULL)
+	    call imunmap (out[1])
+	if (Memi[in] != NULL)
+	    call imunmap (Memi[in])
+	if (stack1 == YES)
+	    call imdelete (Memc[temp])
+	if (delete)
+	    call ccddelete (images[1,1])
+	if (logfd != NULL)
+	    call close (logfd)
+	if (icm != NULL)
+	    call ic_mclose (nimages)
+
+	call fixmem (oldsize)
+	call sfree (sp)
+end
+
+
+# TY_MAX -- Return the datatype of highest precedence.
+
+int procedure ty_max (type1, type2)
+
+int	type1, type2		# Datatypes
+
+int	i, j, type, order[8]
+data	order/TY_SHORT,TY_USHORT,TY_INT,TY_LONG,TY_REAL,TY_DOUBLE,TY_COMPLEX,TY_REAL/
+
+begin
+	for (i=1; (i<=7) && (type1!=order[i]); i=i+1)
+	    ;
+	for (j=1; (j<=7) && (type2!=order[j]); j=j+1)
+	    ;
+	type = order[max(i,j)]
+
+	# Special case of mixing short and unsigned short.
+	if (type == TY_USHORT && type1 != type2)
+	    type = TY_INT
+
+	return (type)
+end
+
+
+# IC_PLFILE -- Map pixel list file
+# This routine strips any image extensions and then adds .pl.
+
+pointer procedure ic_plfile (plfile, mode, refim)
+
+char    plfile[ARB]             # Pixel list file name
+int     mode                    # Image mode
+pointer refim                   # Reference image
+pointer pl                      # IMIO pointer (returned)
+
+int     i, strlen()
+bool    streq
+pointer sp, str, immap()
+
+begin
+        call smark (sp)
+        call salloc (str, SZ_FNAME, TY_CHAR)
+
+        call imgimage (plfile, Memc[str], SZ_FNAME)
+
+        # Strip any existing extensions
+        i = strlen(Memc[str])
+        switch (Memc[str+i-1]) {
+        case 'h':
+            if (i > 3 && Memc[str+i-4] == '.')
+                Memc[str+i-4] = EOS
+        case 'l':
+            if (i > 2 && streq (Memc[str+i-3], ".pl"))
+                Memc[str+i-3] = EOS
+        }
+
+        call strcat (".pl", Memc[str], SZ_FNAME)
+        pl = immap (Memc[str], NEW_COPY, refim)
+        call sfree (sp)
+        return (pl)
+end
diff --git a/noao/imred/ccdred/src/t_mkfringe.x b/noao/imred/ccdred/src/t_mkfringe.x
new file mode 100644
index 00000000..d3e2e82d
--- /dev/null
+++ b/noao/imred/ccdred/src/t_mkfringe.x
@@ -0,0 +1,191 @@
+include <imhdr.h>
+include	"ccdred.h"
+
+
+# T_MKFRINGECOR -- CL task to make fringe correction image.  The large scale
+# background of the input images is subtracted from the input image to obtain
+# the output fringe correction image.  The image is first processed if needed.
+
+procedure t_mkfringecor()
+
+int	listin			# List of input CCD images
+int	listout			# List of output CCD images
+int	ccdtype			# CCD image type
+int	interactive		# Fit overscan interactively?
+
+bool	clgetb(), streq()
+int	imtopenp(), imtgetim()
+pointer	sp, input, output, tmp, str, in, out, ccd
+errchk	set_input, set_output, ccddelete
+
+begin
+	call smark (sp)
+	call salloc (input, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (tmp, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the lists and instrument translation file.  Open the translation
+	# file.  Initialize the interactive flag and the calibration images.
+
+	listin = imtopenp ("input")
+	listout = imtopenp ("mkfringecor.output")
+	call clgstr ("instrument", Memc[input], SZ_FNAME)
+        if (Memc[input] == EOS)
+            call error (1, "No 'instrument' translation file specified.")
+	call hdmopen (Memc[input])
+	call set_interactive ("", interactive)
+	call cal_open (NULL)
+	call ccd_open (0)
+
+	# Process each image.
+	while (imtgetim (listin, Memc[input], SZ_FNAME) != EOF) {
+	    if (clgetb ("noproc")) {
+		call printf ("%s: mkfringecor\n")
+		    call pargstr (Memc[input])
+	    }
+	    
+	    # Set input and output images.  Use temporary image if needed.
+	    call set_input (Memc[input], in, ccdtype)
+	    if (in == NULL)
+		next
+
+	    if (imtgetim (listout, Memc[output], SZ_FNAME) == EOF)
+		call strcpy (Memc[input], Memc[output], SZ_FNAME)
+	    if (Memc[output] == EOS)
+		call strcpy (Memc[input], Memc[output], SZ_FNAME)
+	    if (streq (Memc[input], Memc[output]))
+	        call mktemp ("tmp", Memc[tmp], SZ_FNAME)
+	    else
+		call strcpy (Memc[output], Memc[tmp], SZ_FNAME)
+	    call set_output (in, out, Memc[tmp])
+
+	    # Process image as a flat field image.
+	    call set_proc (in, out, ccd)
+	    call set_sections (ccd)
+	    call set_trim (ccd)
+	    call set_fixpix (ccd)
+	    call set_overscan (ccd)
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+	    call set_flat (ccd)
+	    call set_illum (ccd)
+
+	    # Do the processing.
+	    if (CORS(ccd) == YES) {
+	        call doproc (ccd)
+	        call set_header (ccd)
+
+	        # Finish up
+	        call imunmap (in)
+	        call imunmap (out)
+	        if (streq (Memc[input], Memc[output])) {
+		    call ccddelete (Memc[input])
+	            call imrename (Memc[tmp], Memc[input])
+		} else
+		    call strcpy (Memc[output], Memc[input], SZ_FNAME)
+	    } else {
+		# Delete the temporary output image.  Make a copy if needed.
+	        call imunmap (in)
+	        call imunmap (out)
+		call imdelete (Memc[tmp])
+	    }
+	    call free_proc (ccd)
+
+	    # Do special processing.
+	    call mkfringecor (Memc[input], Memc[output])
+	    if (!streq (Memc[input], Memc[output]))
+		call ccdcopy (Memc[input], Memc[output])
+	}
+
+	# Finish up.
+	call hdmclose ()
+	call imtclose (listin)
+	call imtclose (listout)
+	call cal_close ()
+	call ccd_close ()
+	call sfree (sp)
+end
+
+
+# MKFRINGECOR -- Given an input image which has been processed make the output
+# fringe correction image.
+
+procedure mkfringecor (input, output)
+
+char	input[SZ_FNAME]		# Input image
+char	output[SZ_FNAME]	# Output image
+
+int	i, nc, nl
+pointer	sp, str, illum, tmp, in, im, out, out1
+bool	clgetb(), ccdflag(), streq()
+pointer	immap(), imgl2r(), impl2r()
+errchk	immap, ccddelete
+
+begin
+	# Check if this operation has been done.
+	in = immap (input, READ_ONLY, 0)
+	if (ccdflag (in, "mkfringe")) {
+	    call imunmap (in)
+	    return
+	}
+
+	# Print operation if not processing.
+	if (clgetb ("noproc")) {
+	    call eprintf (
+		"  [TO BE DONE] Make fringe correction\n")
+		call pargstr (input)
+	    call imunmap (in)
+	    return
+	}
+
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+	call salloc (illum, SZ_FNAME, TY_CHAR)
+	call salloc (tmp, SZ_FNAME, TY_CHAR)
+
+	# Make the illumination image.
+	call imunmap (in)
+	call strcpy (input, Memc[tmp], SZ_FNAME)
+	call mktemp ("tmp", Memc[illum], SZ_FNAME)
+	call mkillumination (Memc[tmp], Memc[illum], NO, NO)
+
+	in = immap (input, READ_ONLY, 0)
+	im = immap (Memc[illum], READ_ONLY, 0)
+
+	# Create the temporary output.
+	if (streq (input, output)) {
+	    call mktemp ("tmp", Memc[tmp], SZ_FNAME)
+	    call set_output (in, out, Memc[tmp])
+	    out1 = in
+	} else {
+	    call set_output (in, out, output)
+	    out1 = out
+	}
+
+	# Subtract the illumination from input image.
+	nc = IM_LEN(out,1)
+	nl = IM_LEN(out,2)
+	do i = 1, nl
+	    call asubr (Memr[imgl2r(in,i)], Memr[imgl2r(im,i)],
+		Memr[impl2r(out,i)], nc)
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE, "Fringe correction created")
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (out1, Memc[str])
+	call hdmpstr (out, "mkfringe", Memc[str])
+	call hdmpstr (out, "imagetyp", "fringe")
+
+	# Finish up
+	call imunmap (in)
+	call imunmap (im)
+	call imunmap (out)
+	call imdelete (Memc[illum])
+	if (streq (input, output)) {
+	    call ccddelete (input)
+	    call imrename (Memc[tmp], input)
+	} else
+	    call strcpy (output, input, SZ_FNAME)
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/t_mkillumcor.x b/noao/imred/ccdred/src/t_mkillumcor.x
new file mode 100644
index 00000000..e9113f01
--- /dev/null
+++ b/noao/imred/ccdred/src/t_mkillumcor.x
@@ -0,0 +1,108 @@
+include	"ccdred.h"
+
+# T_MKILLUMCOR -- Make flat field illumination correction images.
+#
+# The input flat field images are processed and smoothed to obtain
+# illumination correction images.  These illumination correction images
+# are used to correct already processed images for illumination effects
+# introduced by the flat field.
+
+procedure t_mkillumcor()
+
+int	listin			# List of input CCD images
+int	listout			# List of output CCD images
+int	ccdtype			# CCD image type
+int	interactive		# Fit overscan interactively?
+
+bool	clgetb(), streq()
+int	imtopenp(), imtgetim()
+pointer	sp, input, output, tmp, str, in, out, ccd
+errchk	set_input, set_output, ccddelete
+
+begin
+	call smark (sp)
+	call salloc (input, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (tmp, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the lists and instrument translation file.  Open the translation
+	# file.  Initialize the interactive flag and the calibration images.
+
+	listin = imtopenp ("input")
+	listout = imtopenp ("mkillumcor.output")
+	call clgstr ("instrument", Memc[input], SZ_FNAME)
+        if (Memc[input] == EOS)
+            call error (1, "No 'instrument' translation file specified.")
+	call hdmopen (Memc[input])
+	call set_interactive ("", interactive)
+	call cal_open (NULL)
+	call ccd_open (0)
+
+	# Process each image.
+	while (imtgetim (listin, Memc[input], SZ_FNAME) != EOF) {
+	    if (clgetb ("noproc")) {
+		call printf ("%s: mkillumcor\n")
+		    call pargstr (Memc[input])
+	    }
+
+	    #  Set input and output images.
+	    call set_input (Memc[input], in, ccdtype)
+	    if (in == NULL)
+		next
+
+	    if (imtgetim (listout, Memc[output], SZ_FNAME) == EOF)
+		call strcpy (Memc[input], Memc[output], SZ_FNAME)
+	    if (Memc[output] == EOS)
+		call strcpy (Memc[input], Memc[output], SZ_FNAME)
+	    if (streq (Memc[input], Memc[output]))
+	        call mktemp ("tmp", Memc[tmp], SZ_FNAME)
+	    else
+		call strcpy (Memc[output], Memc[tmp], SZ_FNAME)
+	    call set_output (in, out, Memc[tmp])
+
+	    # Process image as an illumination image.
+	    call set_proc (in, out, ccd)
+	    call set_sections (ccd)
+	    call set_trim (ccd)
+	    call set_fixpix (ccd)
+	    call set_overscan (ccd)
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+	    CORS(ccd, FINDMEAN) = YES
+
+	    # Do the processing if the COR flag is set.
+	    if (COR(ccd) == YES) {
+	        call doproc (ccd)
+	        call set_header (ccd)
+
+		# Replace the input image by the corrected image.
+	        call imunmap (in)
+	        call imunmap (out)
+		if (streq (Memc[input], Memc[output])) {
+		    call ccddelete (Memc[input])
+	            call imrename (Memc[tmp], Memc[input])
+		} else
+		    call strcpy (Memc[output], Memc[input], SZ_FNAME)
+	    } else {
+		# Make a copy if necessary.
+	        call imunmap (in)
+	        call imunmap (out)
+		call imdelete (Memc[tmp])
+	    }
+	    call free_proc (ccd)
+
+	    # Do special processing.
+	    call mkillumination (Memc[input], Memc[output], YES, YES)
+	    if (!streq (Memc[input], Memc[output]))
+		call ccdcopy (Memc[input], Memc[output])
+	}
+
+	# Finish up.
+	call hdmclose ()
+	call imtclose (listin)
+	call imtclose (listout)
+	call cal_close ()
+	call ccd_close ()
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/t_mkillumft.x b/noao/imred/ccdred/src/t_mkillumft.x
new file mode 100644
index 00000000..ecb66a8e
--- /dev/null
+++ b/noao/imred/ccdred/src/t_mkillumft.x
@@ -0,0 +1,229 @@
+include <imhdr.h>
+include	"ccdred.h"
+
+
+# T_MKILLUMFLAT -- Make illumination corrected flat field images.
+#
+# The input flat field images are processed and smoothed to obtain
+# illumination pattern.  The illumination pattern is then divided out
+# of the input image to make the output illumination corrected flat field
+# image.
+
+procedure t_mkillumflat()
+
+int	listin			# List of input CCD images
+int	listout			# List of output CCD images
+int	ccdtype			# CCD image type
+int	interactive		# Fit overscan interactively?
+
+bool	clgetb(), streq()
+int	imtopenp(), imtgetim()
+pointer	sp, input, output, tmp, str, in, out, ccd
+errchk	set_input, set_output, ccddelete
+
+begin
+	call smark (sp)
+	call salloc (input, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (tmp, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the lists and instrument translation file.  Open the translation
+	# file.  Initialize the interactive flag and the calibration images.
+
+	listin = imtopenp ("input")
+	listout = imtopenp ("mkillumflat.output")
+	call clgstr ("instrument", Memc[input], SZ_FNAME)
+	call hdmopen (Memc[input])
+	call set_interactive ("", interactive)
+	call cal_open (NULL)
+	call ccd_open (0)
+
+	# Process each image.
+	while (imtgetim (listin, Memc[input], SZ_FNAME) != EOF) {
+	    if (clgetb ("noproc")) {
+		call printf ("%s: mkillumflat\n")
+		    call pargstr (Memc[input])
+	    }
+	    
+	    # Set input and output images.  Use temporary image if needed.
+	    call set_input (Memc[input], in, ccdtype)
+	    if (in == NULL)
+		next
+
+	    if (imtgetim (listout, Memc[output], SZ_FNAME) == EOF)
+		call strcpy (Memc[input], Memc[output], SZ_FNAME)
+	    if (Memc[output] == EOS)
+		call strcpy (Memc[input], Memc[output], SZ_FNAME)
+	    if (streq (Memc[input], Memc[output]))
+	        call mktemp ("tmp", Memc[tmp], SZ_FNAME)
+	    else
+		call strcpy (Memc[output], Memc[tmp], SZ_FNAME)
+	    call set_output (in, out, Memc[tmp])
+
+	    # Process image as a flat field image.
+	    call set_proc (in, out, ccd)
+	    call set_sections (ccd)
+	    call set_trim (ccd)
+	    call set_fixpix (ccd)
+	    call set_overscan (ccd)
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+
+	    # Do the processing.
+	    if (CORS(ccd) == YES) {
+	        call doproc (ccd)
+	        call set_header (ccd)
+
+	        # Finish up
+	        call imunmap (in)
+	        call imunmap (out)
+	        if (streq (Memc[input], Memc[output])) {
+		    call ccddelete (Memc[input])
+	            call imrename (Memc[tmp], Memc[input])
+		} else
+		    call strcpy (Memc[output], Memc[input], SZ_FNAME)
+	    } else {
+		# Delete the temporary output image.  Make a copy if needed.
+	        call imunmap (in)
+	        call imunmap (out)
+		call imdelete (Memc[tmp])
+	    }
+	    call free_proc (ccd)
+
+	    # Do special processing.
+	    call mkillumflat (Memc[input], Memc[output])
+	    if (!streq (Memc[input], Memc[output]))
+		call ccdcopy (Memc[input], Memc[output])
+	}
+
+	# Finish up.
+	call hdmclose ()
+	call imtclose (listin)
+	call imtclose (listout)
+	call cal_close ()
+	call ccd_close ()
+	call sfree (sp)
+end
+
+
+# MKILLUMFLAT -- Take the processed input image and make the illumination
+# corrected flat field output image.  The illumination pattern is created
+# as a temporary image and then the applied to the input flat field
+# image to make the final output flat field image.  If the input and
+# output names are the same the operation is done in place.
+
+procedure mkillumflat (input, output)
+
+char	input[SZ_FNAME]		# Input image
+char	output[SZ_FNAME]	# Output image
+
+int	i, nc, nl
+real	scale
+long	time
+pointer	sp, str, illum, tmp, in, im, out, out1, data
+
+bool	clgetb(), ccdflag(), streq()
+int	hdmgeti()
+real	hdmgetr(), clgetr(), divzero()
+pointer	immap(), imgl2r(), impl2r()
+errchk	immap, ccddelete
+extern	divzero()
+
+real	rdivzero	# Result for divion by zero
+int	ndivzero	# Number of zero divisions
+common	/cdivzero/ rdivzero, ndivzero
+
+begin
+	# Check if this operation has been done.
+	in = immap (input, READ_ONLY, 0)
+	if (ccdflag (in, "illumflt")) {
+	    call imunmap (in)
+	    return
+	}
+
+	# Print operation if not processing.
+	if (clgetb ("noproc")) {
+	    call eprintf (
+		"  [TO BE DONE] Remove illumination\n")
+		call pargstr (input)
+	    call imunmap (in)
+	    return
+	}
+
+	# Get and set task parameters for division by zero.
+	rdivzero = clgetr ("divbyzero")
+	ndivzero = 0
+
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+	call salloc (illum, SZ_FNAME, TY_CHAR)
+	call salloc (tmp, SZ_FNAME, TY_CHAR)
+
+	# Make the illumination image.
+	call imunmap (in)
+	call strcpy (input, Memc[tmp], SZ_FNAME)
+	call mktemp ("tmp", Memc[illum], SZ_FNAME)
+	call mkillumination (Memc[tmp], Memc[illum], NO, NO)
+
+	in = immap (input, READ_ONLY, 0)
+	im = immap (Memc[illum], READ_ONLY, 0)
+	iferr (scale = hdmgetr (im, "ccdmean"))
+	    scale = 1.
+	iferr (time = hdmgeti (im, "ccdmeant"))
+	    time = IM_MTIME(im)
+	if (time < IM_MTIME(im))
+	    scale = 1.
+
+	# Create the temporary output.
+	if (streq (input, output)) {
+	    call mktemp ("tmp", Memc[tmp], SZ_FNAME)
+	    call set_output (in, out, Memc[tmp])
+	    out1 = in
+	} else {
+	    call set_output (in, out, output)
+	    out1 = out
+	}
+
+	# Divide the illumination and flat field images with scaling.
+	nc = IM_LEN(out,1)
+	nl = IM_LEN(out,2)
+	do i = 1, nl {
+	    data = impl2r (out, i)
+	    call advzr (Memr[imgl2r(in,i)], Memr[imgl2r(im,i)],
+		Memr[data], nc, divzero)
+	    if (scale != 1.)
+	        call amulkr (Memr[data], scale, Memr[data], nc)
+	}
+
+	# Log the operation.
+	if (ndivzero > 0) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Warning: %d divisions by zero replaced by %g")
+		call pargi (ndivzero)
+		call pargr (rdivzero)
+	    call ccdlog (out1, Memc[str])
+	}
+	call sprintf (Memc[str], SZ_LINE, "Removed illumination from flat")
+	call sprintf (Memc[str], SZ_LINE,
+	    "Illumination flat created from %s")
+	    call pargstr (input)
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (out1, Memc[str])
+	call hdmpstr (out, "illumflt", Memc[str])
+	call hdmpstr (out, "imagetyp", "flat")
+
+	# Finish up
+	call imunmap (in)
+	call imunmap (im)
+	call imunmap (out)
+	call imdelete (Memc[illum])
+
+	# The input name is changed to the output name for further processing.
+	if (streq (input, output)) {
+	    call ccddelete (input)
+	    call imrename (Memc[tmp], input)
+	} else
+	    call strcpy (output, input, SZ_FNAME)
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/t_mkskycor.x b/noao/imred/ccdred/src/t_mkskycor.x
new file mode 100644
index 00000000..fa3f3cd4
--- /dev/null
+++ b/noao/imred/ccdred/src/t_mkskycor.x
@@ -0,0 +1,694 @@
+include <imhdr.h>
+include <imset.h>
+include	<mach.h>
+include	"ccdred.h"
+
+define	MINSIGMA	1.	# Minimum sigma
+define	NITERATE	10	# Maximum number of clipping iterations
+
+# T_MKSKYCOR -- Make sky illumination correction images.
+#
+# The input images processed and smoothed to obtain an illumination correction
+# image.  This task is a version of T_CCDPROC which treats the images as
+# illumination images regardless of there CCD image type.
+
+procedure t_mkskycor()
+
+int	listin			# List of input CCD images
+int	listout			# List of output CCD images
+int	ccdtype			# CCD image type
+int	interactive		# Fit overscan interactively?
+
+bool	flatcor, ccdflag(), clgetb(), streq()
+int	imtopenp(), imtgetim()
+pointer	sp, input, output, tmp, str, in, out, ccd
+errchk	set_input, set_output, ccddelete
+
+begin
+	call smark (sp)
+	call salloc (input, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (tmp, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the lists and instrument translation file.  Open the translation
+	# file.  Initialize the interactive flag and the calibration images.
+
+	listin = imtopenp ("input")
+	listout = imtopenp ("mkskycor.output")
+	call clgstr ("instrument", Memc[input], SZ_FNAME)
+        if (Memc[input] == EOS)
+            call error (1, "No 'instrument' translation file specified.")
+	call hdmopen (Memc[input])
+	call set_interactive ("", interactive)
+	call cal_open (NULL)
+	call ccd_open (0)
+
+	# Process each image.
+	while (imtgetim (listin, Memc[input], SZ_FNAME) != EOF) {
+	    if (clgetb ("noproc")) {
+		call printf ("%s: mkskycor\n")
+		    call pargstr (Memc[input])
+	    }
+
+	    #  Set input and output images.
+	    call set_input (Memc[input], in, ccdtype)
+	    if (in == NULL)
+		next
+
+	    if (imtgetim (listout, Memc[output], SZ_FNAME) == EOF)
+		call strcpy (Memc[input], Memc[output], SZ_FNAME)
+	    if (Memc[output] == EOS)
+		call strcpy (Memc[input], Memc[output], SZ_FNAME)
+	    if (streq (Memc[input], Memc[output]))
+	        call mktemp ("tmp", Memc[tmp], SZ_FNAME)
+	    else
+		call strcpy (Memc[output], Memc[tmp], SZ_FNAME)
+	    call set_output (in, out, Memc[tmp])
+
+	    # Process image as an illumination image.
+	    call set_proc (in, out, ccd)
+	    call set_sections (ccd)
+	    call set_trim (ccd)
+	    call set_fixpix (ccd)
+	    call set_overscan (ccd)
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+	    call set_flat (ccd)
+
+	    # Do the processing if the COR flag is set.
+	    if (COR(ccd) == YES) {
+	        call doproc (ccd)
+	        call set_header (ccd)
+
+		# Replace the input image by the corrected image.
+	        flatcor = ccdflag (out, "flatcor")
+	        call imunmap (in)
+	        call imunmap (out)
+		if (streq (Memc[input], Memc[output])) {
+		    call ccddelete (Memc[input])
+	            call imrename (Memc[tmp], Memc[input])
+		} else
+		    call strcpy (Memc[output], Memc[input], SZ_FNAME)
+	    } else {
+		# Make a copy if necessary.
+	        flatcor = ccdflag (out, "flatcor")
+	        call imunmap (in)
+	        call imunmap (out)
+		call imdelete (Memc[tmp])
+	    }
+	    call free_proc (ccd)
+
+	    # Do special processing.
+	    if (!flatcor) {
+	        call eprintf (
+		    "%s: WARNING - Image should be flat fielded first\n")
+		    call pargstr (Memc[input])
+	    }
+	    call mkillumination (Memc[input], Memc[output], NO, YES)
+	    if (!streq (Memc[input], Memc[output]))
+		call ccdcopy (Memc[input], Memc[output])
+	}
+
+	# Finish up.
+	call hdmclose ()
+	call imtclose (listin)
+	call imtclose (listout)
+	call cal_close ()
+	call ccd_close ()
+	call sfree (sp)
+end
+
+
+# MKILLUMINATION -- Make illumination images.
+#
+# The images are boxcar smoothed to obtain the large scale illumination.
+# Objects in the images are excluded from the average by sigma clipping.
+
+procedure mkillumination (input, output, inverse, log)
+
+char	input[SZ_FNAME]		# Input image
+char	output[SZ_FNAME]	# Output image
+int	inverse			# Return inverse of illumination
+int	log			# Add log info?
+
+real	xbminr			# Minimum size of X smoothing box
+real	ybminr			# Minimum size of Y smoothing box
+real	xbmaxr			# Maximum size of X smoothing box
+real	ybmaxr			# Maximum size of Y smoothing box
+bool	clip			# Sigma clip
+real	lowsigma		# Low sigma clip
+real	highsigma		# High sigma clip
+
+int	xbmin, ybmin, xbmax, ybmax
+pointer	sp, str, tmp, in, out, out1
+
+bool	clgetb(), ccdflag(), streq()
+real	clgetr()
+pointer	immap()
+errchk	immap, ccddelete
+
+real	rdivzero	# Result for divion by zero
+int	ndivzero	# Number of zero divisions
+common	/cdivzero/ rdivzero, ndivzero
+
+begin
+	# Check if this operation has been done.  Unfortunately this requires
+	# mapping the image.
+
+	in = immap (input, READ_ONLY, 0)
+	if (ccdflag (in, "mkillum")) {
+	    call imunmap (in)
+	    return
+	}
+
+	if (clgetb ("noproc")) {
+	    call eprintf (
+		"  [TO BE DONE] Convert %s to illumination correction\n")
+		call pargstr (input)
+	    call imunmap (in)
+	    return
+	}
+
+	# Get task parameters
+	xbminr = clgetr ("xboxmin")
+	ybminr = clgetr ("yboxmin")
+	xbmaxr = clgetr ("xboxmax")
+	ybmaxr = clgetr ("yboxmax")
+	clip = clgetb ("clip")
+	if (clip) {
+	    lowsigma = max (MINSIGMA, clgetr ("lowsigma"))
+	    highsigma = max (MINSIGMA, clgetr ("highsigma"))
+	}
+	if (inverse == YES)
+	    rdivzero = clgetr ("divbyzero")
+	ndivzero = 0
+
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+	call salloc (tmp, SZ_FNAME, TY_CHAR)
+
+	# Create output.
+	if (streq (input, output)) {
+	    call mktemp ("tmp", Memc[tmp], SZ_FNAME)
+	    call set_output (in, out, Memc[tmp])
+	    out1 = in
+	} else {
+	    call set_output (in, out, output)
+	    out1 = out
+	}
+
+	if (xbminr < 1.)
+	    xbminr = xbminr * IM_LEN(in,1)
+	if (ybminr < 1.)
+	    ybminr = ybminr * IM_LEN(in,2)
+	if (xbmaxr < 1.)
+	    xbmaxr = xbmaxr * IM_LEN(in,1)
+	if (ybmaxr < 1.)
+	    ybmaxr = ybmaxr * IM_LEN(in,2)
+
+	xbmin = max (1, min (IM_LEN(in,1), nint (min (xbminr, xbmaxr))))
+	xbmax = max (1, min (IM_LEN(in,1), nint (max (xbminr, xbmaxr))))
+	ybmin = max (1, min (IM_LEN(in,2), nint (min (ybminr, ybmaxr))))
+	ybmax = max (1, min (IM_LEN(in,2), nint (max (ybminr, ybmaxr))))
+
+	if (clip)
+	    call illumination (in, out, xbmin, ybmin, xbmax, ybmax,
+		lowsigma, highsigma, inverse)
+	else
+	    call qillumination (in, out, xbmin, ybmin, xbmax, ybmax, inverse)
+
+	# Log the operation.
+	if (log == YES) {
+	    if (ndivzero > 0) {
+		call sprintf (Memc[str], SZ_LINE,
+		    "Warning: %d divisions by zero replaced by %g")
+		    call pargi (ndivzero)
+		    call pargr (rdivzero)
+		call ccdlog (out1, Memc[str])
+	    }
+	    call sprintf (Memc[str], SZ_LINE,
+		"Illumination correction created from %s")
+		call pargstr (input)
+	    call timelog (Memc[str], SZ_LINE)
+	    call ccdlog (out1, Memc[str])
+	}
+	call hdmpstr (out, "mkillum", Memc[str])
+	call hdmpstr (out, "imagetyp", "illum")
+
+	# Finish up
+	call imunmap (in)
+	call imunmap (out)
+	if (streq (input, output)) {
+	    call ccddelete (input)
+	    call imrename (Memc[tmp], input)
+	} else
+	    call strcpy (output, input, SZ_FNAME)
+	call sfree (sp)
+end
+
+
+# ILLUMINATION -- Make illumination correction image with clipping.
+
+procedure illumination (in, out, xbmin, ybmin, xbmax, ybmax, low, high, inverse)
+
+pointer	in		# Pointer to the input image
+pointer	out		# Pointer to the output image
+int	xbmin, ybmin	# Minimum dimensions of the boxcar
+int	xbmax, ybmax	# Maximum dimensions of the boxcar
+real	low, high	# Clipping sigma thresholds
+int	inverse		# Return inverse of illumination?
+
+real	scale, ccdmean
+int	i, ncols, nlines, linein, lineout, ybox2, nrej
+pointer	sp, ptr, ptrs, data, sum, avg, output
+
+long	clktime()
+int	boxclean()
+real	asumr(), divzero()
+pointer	imgl2r(), impl2r()
+extern	divzero()
+
+begin
+	# Set up an array of linepointers and accumulators
+	ncols = IM_LEN(out,1)
+	nlines = IM_LEN(out,2)
+	call smark (sp)
+	call salloc (ptrs, ybmax, TY_POINTER)
+	call salloc (sum, ncols, TY_REAL)
+	call salloc (avg, ncols, TY_REAL)
+	if (inverse == YES)
+	    call salloc (output, ncols, TY_REAL)
+	else
+	    output = avg
+
+	# Set input buffers.
+	if (ybmax < nlines)
+	    call imseti (in, IM_NBUFS, ybmax)
+
+	# Get the first average over the minimum y box.
+	call aclrr (Memr[sum], ncols)
+	linein = 0
+	while (linein < ybmin) {
+	    linein = linein + 1
+	    data = imgl2r (in, linein)
+	    call aaddr (Memr[data], Memr[sum], Memr[sum], ncols)
+	    ptr = ptrs + mod (linein, ybmax)
+	    Memi[ptr] = data
+	}
+	ybox2 = ybmin
+	scale = ybmin
+	call agboxcar (Memr[sum], Memr[avg], ncols, xbmin, xbmax, scale)
+
+	# Iteratively clean the initial lines.
+	ptr = ptrs
+	if (ybox2 != ybmax)
+	    ptr = ptr + 1
+	do i = 1, NITERATE {
+	    nrej = 0
+	    do lineout = 1, linein {
+		data = Memi[ptr+lineout-1]
+		nrej = nrej + boxclean (Memr[data], Memr[avg], Memr[sum],
+		    ncols, low, high)
+	    }
+	    if (nrej > 0)
+		call agboxcar (Memr[sum], Memr[avg], ncols, xbmin, xbmax,
+		    scale)
+	    else
+		break
+	}
+
+	# Output the minimum smoothing y box.
+	if (inverse == YES)
+	    call arczr (1., Memr[avg], Memr[output], ncols, divzero)
+	ybox2 = (ybmin + 1) / 2
+	lineout = 0
+	while (lineout < ybox2) {
+	    lineout = lineout + 1
+	    call amovr (Memr[output], Memr[impl2r(out, lineout)], ncols)
+	}
+	ccdmean = ybox2 * asumr (Memr[output], ncols)
+
+	# Increase the y box size by factors of 2 until the maximum size.
+	while (linein < ybmax) {
+	    linein = linein + 1
+	    data = imgl2r (in, linein)
+	    call aaddr (Memr[sum], Memr[data], Memr[sum], ncols)
+	    ptr = ptrs + mod (linein, ybmax)
+	    Memi[ptr] = data
+	    scale = scale + 1
+
+	    nrej = boxclean (Memr[data], Memr[avg], Memr[sum], ncols,
+		low, high)
+	    call agboxcar (Memr[sum], Memr[avg], ncols, xbmin, xbmax, scale)
+
+	    linein = linein + 1
+	    data = imgl2r (in, linein)
+	    call aaddr (Memr[sum], Memr[data], Memr[sum], ncols)
+	    ptr = ptrs + mod (linein, ybmax)
+	    Memi[ptr] = data
+
+	    nrej = boxclean (Memr[data], Memr[avg], Memr[sum], ncols, low, high)
+	    scale = scale + 1
+	    call agboxcar (Memr[sum], Memr[avg], ncols, xbmin, xbmax, scale)
+
+	    lineout = lineout + 1
+	    data = impl2r (out, lineout)
+	    if (inverse == YES)
+	        call arczr (1., Memr[avg], Memr[data], ncols, divzero)
+	    else
+		call amovr (Memr[avg], Memr[data], ncols)
+	    ccdmean = ccdmean + asumr (Memr[data], ncols)
+	}
+
+	# For each line subtract the last line from the sum, add the
+	# next line to the sum, and output a line.
+
+	while (linein < nlines) {
+	    linein = linein + 1
+	    ptr = ptrs + mod (linein, ybmax)
+	    data = Memi[ptr]
+	    call asubr (Memr[sum], Memr[data], Memr[sum], ncols)
+	    data = imgl2r (in, linein)
+	    call aaddr (Memr[sum], Memr[data], Memr[sum], ncols)
+	    Memi[ptr] = data
+
+	    nrej = boxclean (Memr[data], Memr[avg], Memr[sum], ncols, low, high)
+
+	    lineout = lineout + 1
+	    data = impl2r (out, lineout)
+	    call agboxcar (Memr[sum], Memr[avg], ncols, xbmin, xbmax, scale)
+
+	    if (inverse == YES)
+	        call arczr (1., Memr[avg], Memr[data], ncols, divzero)
+	    else
+		call amovr (Memr[avg], Memr[data], ncols)
+	    ccdmean = ccdmean + asumr (Memr[data], ncols)
+	}
+
+	# Decrease the y box in factors of 2 until minimum y box.
+	while (lineout < nlines - ybox2) {
+	    linein = linein + 1
+	    ptr = ptrs + mod (linein, ybmax)
+	    data = Memi[ptr]
+	    call asubr (Memr[sum], Memr[data], Memr[sum], ncols)
+	    linein = linein + 1
+	    ptr = ptrs + mod (linein, ybmax)
+	    data = Memi[ptr]
+	    call asubr (Memr[sum], Memr[data], Memr[sum], ncols)
+	    scale = scale - 2
+
+	    lineout = lineout + 1
+	    data = impl2r (out, lineout)
+	    call agboxcar (Memr[sum], Memr[data], ncols, xbmin, xbmax, scale)
+	    if (inverse == YES)
+	        call arczr (1., Memr[data], Memr[data], ncols, divzero)
+	    ccdmean = ccdmean + asumr (Memr[data], ncols)
+	}
+
+	# Output the last lines of the minimum y box size.
+	call agboxcar (Memr[sum], Memr[avg], ncols, xbmin, xbmax, scale)
+	if (inverse == YES)
+	    call arczr (1., Memr[avg], Memr[output], ncols, divzero)
+	ybox2 = nlines - lineout
+	while (lineout < nlines) {
+	    lineout = lineout + 1
+	    data = impl2r (out, lineout)
+	    call amovr (Memr[output], Memr[data], ncols)
+	}
+	ccdmean = ccdmean + ybox2 * asumr (Memr[output], ncols)
+
+	# Write scale factor out.
+	ccdmean = ccdmean / (ncols * nlines)
+	call hdmputr (out, "ccdmean", ccdmean)
+	call hdmputi (out, "ccdmeant", int (clktime (long (0))))
+
+	# Free buffers
+	call sfree (sp)
+end
+
+
+# QILLUMCOR -- Quick (no clipping) illumination correction image.
+
+procedure qillumination (in, out, xbmin, ybmin, xbmax, ybmax, inverse)
+
+pointer	in		# pointer to the input image
+pointer	out		# pointer to the output image
+int	xbmin, ybmin	# Minimum dimensions of the boxcar
+int	xbmax, ybmax	# Maximum dimensions of the boxcar
+int	inverse		# return inverse of illumination
+
+real	scale, ccdmean
+int	ncols, nlines, linein, lineout, ybox1
+pointer	sp, ptr, ptrs, data, sum, output
+
+long	clktime()
+real	asumr(), divzero()
+pointer	imgl2r(), impl2r()
+extern	divzero()
+
+begin
+	# Set up an array of linepointers and accumulators
+	ncols = IM_LEN(out,1)
+	nlines = IM_LEN(out,2)
+
+	call smark (sp)
+	call salloc (ptrs, ybmax, TY_POINTER)
+	call salloc (sum, ncols, TY_REAL)
+	call salloc (output, ncols, TY_REAL)
+
+	# Set input buffers.
+	if (ybmax < nlines)
+	    call imseti (in, IM_NBUFS, ybmax)
+
+	# Accumulate the minimum y box.
+	call aclrr (Memr[sum], ncols)
+	linein = 0
+	while (linein < ybmin) {
+	    linein = linein + 1
+	    data = imgl2r (in, linein)
+	    call aaddr (Memr[data], Memr[sum], Memr[sum],  ncols)
+	    ptr = ptrs + mod (linein, ybmax)
+	    Memi[ptr] = data
+	}
+
+	# Output the minimum y box.
+	ybox1 = (ybmin + 1) / 2
+	scale = ybmin
+	call agboxcar (Memr[sum], Memr[output], ncols, xbmin, xbmax, scale)
+	if (inverse == YES)
+	    call arczr (1., Memr[output], Memr[output], ncols, divzero)
+	lineout = 0
+	while (lineout < ybox1) {
+	    lineout = lineout + 1
+	    data = impl2r (out, lineout)
+	    call amovr (Memr[output], Memr[data], ncols)
+	}
+	ccdmean = ybox1 * asumr (Memr[output], ncols)
+
+	# Increase the y box size by steps of 2 until the maximum size.
+	while (linein < ybmax) {
+	    linein = linein + 1
+	    data = imgl2r (in, linein)
+	    call aaddr (Memr[sum], Memr[data], Memr[sum], ncols)
+	    ptr = ptrs + mod (linein, ybmax)
+	    Memi[ptr] = data
+	    linein = linein + 1
+	    data = imgl2r (in, linein)
+	    call aaddr (Memr[sum], Memr[data], Memr[sum], ncols)
+	    ptr = ptrs + mod (linein, ybmax)
+	    Memi[ptr] = data
+
+	    scale = scale + 2
+	    lineout = lineout + 1
+	    data = impl2r (out, lineout)
+	    call agboxcar (Memr[sum], Memr[data], ncols, xbmin, xbmax, scale)
+	    if (inverse == YES)
+	        call arczr (1., Memr[data], Memr[data], ncols, divzero)
+	    ccdmean = ccdmean + asumr (Memr[data], ncols)
+	}
+
+	# For each line subtract the last line from the sum, add the
+	# next line to the sum, and output a line.
+
+	while (linein < nlines) {
+	    linein = linein + 1
+	    ptr = ptrs + mod (linein, ybmax)
+	    data = Memi[ptr]
+	    call asubr (Memr[sum], Memr[data], Memr[sum], ncols)
+	    data = imgl2r (in, linein)
+	    call aaddr (Memr[sum], Memr[data], Memr[sum], ncols)
+	    Memi[ptr] = data
+
+	    lineout = lineout + 1
+	    data = impl2r (out, lineout)
+	    call agboxcar (Memr[sum], Memr[data], ncols, xbmin, xbmax, scale)
+	    if (inverse == YES)
+		call arczr (1., Memr[data], Memr[data], ncols, divzero)
+	    ccdmean = ccdmean + asumr (Memr[data], ncols)
+	}
+
+	# Decrease the y box in steps of 2 until minimum y box.
+	while (lineout < nlines - ybox1) {
+	    linein = linein + 1
+	    ptr = ptrs + mod (linein, ybmax)
+	    data = Memi[ptr]
+	    call asubr (Memr[sum], Memr[data], Memr[sum], ncols)
+	    linein = linein + 1
+	    ptr = ptrs + mod (linein, ybmax)
+	    data = Memi[ptr]
+	    call asubr (Memr[sum], Memr[data], Memr[sum], ncols)
+
+	    lineout = lineout + 1
+	    scale = scale - 2
+	    data = impl2r (out, lineout)
+	    call agboxcar (Memr[sum], Memr[data], ncols, xbmin, xbmax, scale)
+	    if (inverse == YES)
+		call arczr (1., Memr[data], Memr[data], ncols, divzero)
+	    ccdmean = ccdmean + asumr (Memr[data], ncols)
+	}
+
+	# Output the last lines of the minimum y box size.
+	call agboxcar (Memr[sum], Memr[output], ncols, xbmin, xbmax, scale)
+	if (inverse == YES)
+	    call arczr (1., Memr[output], Memr[output], ncols, divzero)
+	ybox1 = nlines - lineout
+	while (lineout < nlines) {
+	    lineout = lineout + 1
+	    data = impl2r (out, lineout)
+	    call amovr (Memr[output], Memr[data], ncols)
+	}
+	ccdmean = ccdmean + ybox1 * asumr (Memr[output], ncols)
+
+	# Write scale factor out.
+	ccdmean = ccdmean / (ncols * nlines)
+	call hdmputr (out, "ccdmean", ccdmean)
+	call hdmputi (out, "ccdmeant", int (clktime (long (0))))
+
+	# Free buffers
+	call sfree (sp)
+end
+
+
+# AGBOXCAR -- Vector growing boxcar smooth.
+# This implements the growing box algorithm which differs from the
+# normal boxcar smoothing which uses a fixed size box.
+
+procedure agboxcar (in, out, ncols, xbmin, xbmax, ybox)
+
+real	in[ncols]		# Sum of ybox lines
+real	out[ncols]		# Boxcar smoothed output
+int	ncols			# Number of columns
+int	xbmin, xbmax		# Boxcar size in x
+real	ybox			# Boxcar size in y
+
+int	colin, colout, lastcol, npix, xbmin2
+real	sum, output
+
+begin
+	xbmin2 = (xbmin + 1) / 2
+	colin = 0
+	sum = 0.
+	while (colin < xbmin) {
+	    colin = colin + 1
+	    sum = sum + in[colin]
+	}
+
+	npix = xbmin * ybox
+	output = sum / npix
+	colout = 0
+	while (colout < xbmin2) {
+	    colout = colout + 1
+	    out[colout] = output
+	}
+
+	while (colin < xbmax) {
+	    colin = colin + 1
+	    sum = sum + in[colin]
+	    colin = colin + 1
+	    sum = sum + in[colin]
+	    npix = npix + 2 * ybox
+	    colout = colout + 1
+	    out[colout] = sum / npix
+	}
+
+	lastcol = 0
+	while (colin < ncols) {
+	    colin = colin + 1
+	    lastcol = lastcol + 1
+	    sum = sum + in[colin] - in[lastcol]
+	    colout = colout + 1
+	    out[colout] = sum / npix
+	}
+
+	while (colout < ncols - xbmin2) {
+	    lastcol = lastcol + 1
+	    sum = sum - in[lastcol]
+	    lastcol = lastcol + 1
+	    sum = sum - in[lastcol]
+	    npix = npix - 2 * ybox
+	    colout = colout + 1
+	    out[colout] = sum / npix
+	}
+
+	output = sum / npix
+	while (colout < ncols) {
+	    colout = colout + 1
+	    out[colout] = output
+	}
+end
+
+
+# BOXCLEAN -- Reject data values from the sum for the next boxcar average
+# which exceed the minimum and maximum residual values from the current
+# boxcar average.  This excludes data from the moving average before it
+# enters the average.
+
+int procedure boxclean (data, boxavg, sum, ncols, low, high)
+
+real	data[ncols]		# Data line
+real	boxavg[ncols]		# Box average line
+real	sum[ncols]		# Moving sum
+int	ncols			# Number of columns
+real	low			# Low clipping factor
+real	high			# High clipping factor
+
+int	i, nrej
+real	rms, resid, minresid, maxresid
+
+begin
+	rms = 0.
+	do i = 1, ncols
+	    rms = rms + (data[i] - boxavg[i]) ** 2
+	rms = sqrt (rms / ncols)
+	minresid = -low * rms
+	maxresid = high * rms
+
+	nrej = 0
+	do i = 1, ncols {
+	    resid = data[i] - boxavg[i]
+	    if ((resid < minresid) || (resid > maxresid)) {
+		data[i] = boxavg[i]
+		sum[i] = sum[i] - resid
+		nrej = nrej + 1
+	    }
+	}
+
+	return (nrej)
+end
+
+
+# DIVZERO -- Error action for division by zero.
+
+real procedure divzero (x)
+
+real	x		# Value to be inversed
+
+real	rdivzero	# Result for divion by zero
+int	ndivzero	# Number of zero divisions
+common	/cdivzero/ rdivzero, ndivzero
+
+begin
+	ndivzero = ndivzero + 1
+	return (rdivzero)
+end
diff --git a/noao/imred/ccdred/src/t_mkskyflat.x b/noao/imred/ccdred/src/t_mkskyflat.x
new file mode 100644
index 00000000..02696905
--- /dev/null
+++ b/noao/imred/ccdred/src/t_mkskyflat.x
@@ -0,0 +1,215 @@
+include <imhdr.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+
+# T_MKSKYFLAT -- Apply a sky observation to a flat field to remove the
+# residual illumination pattern.
+
+procedure t_mkskyflat()
+
+int	listin			# List of input CCD images
+int	listout			# List of output CCD images
+int	ccdtype			# CCD image type
+int	interactive		# Fit overscan interactively?
+
+bool	flatcor, ccdflag(), clgetb(), streq()
+int	imtopenp(), imtgetim()
+pointer	sp, input, output, tmp, str, in, out, ccd
+errchk	set_input, set_output, ccddelete
+
+begin
+	call smark (sp)
+	call salloc (input, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (tmp, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the lists and instrument translation file.  Open the translation
+	# file.  Initialize the interactive flag and the calibration images.
+
+	listin = imtopenp ("input")
+	listout = imtopenp ("mkskyflat.output")
+	call clgstr ("instrument", Memc[input], SZ_FNAME)
+        if (Memc[input] == EOS)
+            call error (1, "No 'instrument' translation file specified.")
+	call hdmopen (Memc[input])
+	call set_interactive ("", interactive)
+ 
+	# Force flat fields even if flatcor=no
+	flatcor = clgetb ("flatcor")
+	call clputb ("flatcor", true)
+	call cal_open (NULL)
+	call ccd_open (0)
+	call clputb ("flatcor", flatcor)
+
+	# Process each image.
+	while (imtgetim (listin, Memc[input], SZ_FNAME) != EOF) {
+	    if (clgetb ("noproc")) {
+		call printf ("%s: mkskyflat\n")
+		    call pargstr (Memc[input])
+	    }
+	    
+	    # Set input and output images.  Use temporary image if needed.
+	    call set_input (Memc[input], in, ccdtype)
+	    if (in == NULL)
+		next
+
+	    if (imtgetim (listout, Memc[output], SZ_FNAME) == EOF)
+		call strcpy (Memc[input], Memc[output], SZ_FNAME)
+	    if (Memc[output] == EOS)
+		call strcpy (Memc[input], Memc[output], SZ_FNAME)
+	    if (streq (Memc[input], Memc[output]))
+	        call mktemp ("tmp", Memc[tmp], SZ_FNAME)
+	    else
+		call strcpy (Memc[output], Memc[tmp], SZ_FNAME)
+	    call set_output (in, out, Memc[tmp])
+
+	    # Process image as an illumination image.
+	    call set_proc (in, out, ccd)
+	    call set_sections (ccd)
+	    call set_trim (ccd)
+	    call set_fixpix (ccd)
+	    call set_overscan (ccd)
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+	    call set_flat (ccd)
+
+	    # Do the processing.
+	    if (CORS(ccd) == YES) {
+	        call doproc (ccd)
+	        call set_header (ccd)
+
+	        # Finish up
+	        flatcor = ccdflag (out, "flatcor")
+	        call imunmap (in)
+	        call imunmap (out)
+	        if (streq (Memc[input], Memc[output])) {
+		    call ccddelete (Memc[input])
+	            call imrename (Memc[tmp], Memc[input])
+		} else
+		    call strcpy (Memc[output], Memc[input], SZ_FNAME)
+	    } else {
+		# Delete the temporary output image.  Make a copy if needed.
+	        flatcor = ccdflag (out, "flatcor")
+	        call imunmap (in)
+	        call imunmap (out)
+		call imdelete (Memc[tmp])
+	    }
+	    call free_proc (ccd)
+
+	    # Do special processing.
+	    if (!flatcor) {
+	        call eprintf (
+		    "%s: WARNING - Image should be flat fielded first\n")
+		    call pargstr (Memc[input])
+	    }
+	    call mkillumination (Memc[input], Memc[output], NO, YES)
+	    call mkskyflat (Memc[input], Memc[output])
+	    if (!streq (Memc[input], Memc[output]))
+		call ccdcopy (Memc[input], Memc[output])
+	}
+
+	# Finish up.
+	call hdmclose ()
+	call imtclose (listin)
+	call imtclose (listout)
+	call cal_close ()
+	call ccd_close ()
+	call sfree (sp)
+end
+
+
+# MKSKYFLAT -- Make a sky flat by dividing the input illumination image by
+# the flat field.
+
+procedure mkskyflat (input, output)
+
+char	input[SZ_FNAME]		# Input image
+char	output[SZ_FNAME]	# Output image
+
+int	i, nc, nl
+long	time
+real	scale
+pointer	sp, str, flat, tmp, in, im, out, out1, data
+
+int	hdmgeti()
+bool	clgetb(), ccdflag(), streq()
+real	hdmgetr()
+pointer	immap(), imgl2r(), impl2r()
+errchk	immap, ccddelete
+
+begin
+	# Check if this operation has been done.
+	in = immap (input, READ_ONLY, 0)
+	if (ccdflag (in, "skyflat")) {
+	    call imunmap (in)
+	    return
+	}
+
+	# Print operation if not processing.
+	if (clgetb ("noproc")) {
+	    call eprintf (
+		"  [TO BE DONE] Convert %s to sky flat\n")
+		call pargstr (input)
+	    call imunmap (in)
+	    return
+	}
+
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+	call salloc (flat, SZ_FNAME, TY_CHAR)
+	call salloc (tmp, SZ_FNAME, TY_CHAR)
+
+	# Get the flat field.
+	call cal_image (in, FLAT, 1, Memc[flat], SZ_FNAME)
+	im = immap (Memc[flat], READ_ONLY, 0)
+	iferr (scale = hdmgetr (im, "ccdmean"))
+	    scale = 1.
+	iferr (time = hdmgeti (im, "ccdmeant"))
+	    time = IM_MTIME(im)
+	if (time < IM_MTIME(im))
+	    scale = 1.
+
+	# Create the temporary output.
+	if (streq (input, output)) {
+	    call mktemp ("tmp", Memc[tmp], SZ_FNAME)
+	    call set_output (in, out, Memc[tmp])
+	    out1 = in
+	} else {
+	    call set_output (in, out, output)
+	    out1 = out
+	}
+
+	# Multiply the illumination and flat field images with scaling.
+	nc = IM_LEN(out,1)
+	nl = IM_LEN(out,2)
+	do i = 1, nl {
+	    data = impl2r (out, i)
+	    call amulr (Memr[imgl2r(in,i)], Memr[imgl2r(im,i)],
+		Memr[data], nc)
+	    if (scale != 1.)
+	        call adivkr (Memr[data], scale, Memr[data], nc)
+	}
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE,
+	    "Sky flat created from %s and %s")
+	    call pargstr (input)
+	    call pargstr (Memc[flat])
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (out1, Memc[str])
+	call hdmpstr (out, "skyflat", Memc[str])
+	call hdmpstr (out, "imagetyp", "flat")
+
+	# Finish up
+	call imunmap (in)
+	call imunmap (im)
+	call imunmap (out)
+	if (streq (input, output)) {
+	    call ccddelete (input)
+	    call imrename (Memc[tmp], input)
+	} else
+	    call strcpy (output, input, SZ_FNAME)
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/src/t_skyreplace.x b/noao/imred/ccdred/src/t_skyreplace.x
new file mode 100644
index 00000000..9bd2e9d0
--- /dev/null
+++ b/noao/imred/ccdred/src/t_skyreplace.x
@@ -0,0 +1,301 @@
+include	<imhdr.h>
+
+
+# T_SKYREPLACE -- Replace objects by sky.  This development code as is not
+# used in the package.  It is here to be worked on further when an image
+# display interface is added.
+
+procedure t_skyreplace ()
+
+char	image[SZ_FNAME]		# Image to be modified
+
+char	graph[SZ_LINE], display[SZ_LINE], cmd[SZ_LINE]
+pointer	im, immap()
+int	clgeti(), wcs, key, clgcur(), nrep, skyreplace()
+real	wx, wy, xc, yc, r, s
+
+begin
+	call clgstr ("image", image, SZ_FNAME)
+	call sprintf (graph, SZ_LINE, "contour %s")
+	    call pargstr (image)
+	call sprintf (display, SZ_LINE, "display %s %d")
+	    call pargstr (image)
+	    call pargi (clgeti ("frame"))
+
+	im = immap (image, READ_WRITE, 0)
+	while (clgcur ("cursor",wx, wy, wcs, key, cmd, SZ_LINE) != EOF) {
+	    switch (key) {
+	    case 'a':
+		r = sqrt ((wx - xc) ** 2 + (wy - yc) ** 2)
+		s = 2 * r
+	    case 'b':
+		nrep = skyreplace (im, xc, yc, r, s)
+	    case 'c':
+		xc = wx
+		yc = wy
+	    case 'd':
+		call imunmap (im)
+		call clcmdw (display)
+		im = immap (image, READ_WRITE, 0)
+	    case 'g':
+		call imunmap (im)
+		call clcmdw (graph)
+		im = immap (image, READ_WRITE, 0)
+	    case 'q':
+		break
+	    default:
+		call printf ("\007")
+	    }
+	}
+
+	call imunmap (im)
+end
+
+
+define	NSKY	100	# Minimum number of sky points
+
+int procedure skyreplace (im, xc, yc, r, s)
+
+pointer	im		# IMIO pointer
+real	xc, yc		# Object center
+real	r		# Object aperture radius
+real	s		# Sky aperture radius
+
+real	avg, sigma, urand(), mode, find_mode()
+long	seed
+int	xlen, ylen, nx, nx1, nx2, ny, ny1, ny2, ntotal, nobj, nallsky, nsky[4]
+int	i, j, x1, x2, x3, x4, y1, y2, y3, y4, y
+pointer	sp, allsky, sky[4], ptr1, ptr2
+pointer	datain, dataout, imgs2r(), imps2r()
+
+begin
+	xlen = IM_LEN(im,1)
+	ylen = IM_LEN(im,2)
+	x1 = max (1, int (xc - s))
+	x4 = min (xlen, int (xc + s + 0.5))
+	y1 = max (1, int (yc - s))
+	y4 = min (ylen, int (yc + s + 0.5))
+	nx = x4 - x1 + 1
+	ny = y4 - y1 + 1
+	ntotal = nx * ny
+
+	x2 = max (1, int (xc - r))
+	x3 = min (xlen, int (xc + r + 0.5))
+	y2 = max (1, int (yc - r))
+	y3 = min (xlen, int (yc + r + 0.5))
+	nx1 = (x3 - x2 + 1)
+	ny1 = (y3 - y2 + 1)
+	nobj = nx1 * ny1
+	nallsky = ntotal - nobj
+
+	if ((nallsky < NSKY) || (nobj < 1))
+	    return (0)
+
+	call smark (sp)
+	call salloc (allsky, nallsky, TY_REAL)
+	datain = imgs2r (im, x1, x4, y1, y4)
+	dataout = imps2r (im, x2, x3, y2, y3)
+	ptr2 = allsky
+
+	# First quadrant
+	x2 = max (1, int (xc - r))
+	x3 = min (xlen, int (xc + 0.5))
+	y2 = max (1, int (yc - r))
+	y3 = min (xlen, int (yc + 0.5))
+	nx1 = x3 - x1 + 1
+	nx2 = x3 - x2
+	ny1 = y2 - y1
+	ny2 = y3 - y2 + 1
+	nsky[1] = nx1 * ny1 + nx2 * ny2
+	sky[1] = ptr2
+
+	if (nsky[1] > 0) {
+	    ptr1 = datain
+	    for (y=y1; y<y2; y=y+1) {
+	        call amovr (Memr[ptr1], Memr[ptr2], nx1)
+	        ptr1 = ptr1 + nx
+	        ptr2 = ptr2 + nx1
+	    }
+	    for (; y<=y3; y=y+1) {
+	        call amovr (Memr[ptr1], Memr[ptr2], nx2)
+	        ptr1 = ptr1 + nx
+	        ptr2 = ptr2 + nx2
+	    }
+	}
+
+	# Second quadrant
+	x2 = max (1, int (xc + 1.5))
+	x3 = min (xlen, int (xc + r + 0.5))
+	y2 = max (1, int (yc - r))
+	y3 = min (xlen, int (yc + 0.5))
+	nx1 = x4 - x2 + 1
+	nx2 = x4 - x3
+	ny1 = y2 - y1
+	ny2 = y3 - y2 + 1
+	nsky[2] = nx1 * ny1 + nx2 * ny2
+	sky[2] = ptr2
+
+	if (nsky[2] > 0) {
+	    ptr1 = datain + x2 - x1
+	    for (y=y1; y<y2; y=y+1) {
+	        call amovr (Memr[ptr1], Memr[ptr2], nx1)
+	        ptr1 = ptr1 + nx
+	        ptr2 = ptr2 + nx1
+	    }
+	    ptr1 = ptr1 + x3 - x2 + 1
+	    for (; y<=y3; y=y+1) {
+	        call amovr (Memr[ptr1], Memr[ptr2], nx2)
+	        ptr1 = ptr1 + nx
+	        ptr2 = ptr2 + nx2
+	    }
+	}
+
+	# Third quadrant
+	x2 = max (1, int (xc - r))
+	x3 = min (xlen, int (xc + 0.5))
+	y2 = max (1, int (yc + 1.5))
+	y3 = min (xlen, int (yc + r + 0.5))
+	nx1 = x3 - x2
+	nx2 = x3 - x1 + 1
+	ny1 = y3 - y2 + 1
+	ny2 = y4 - y3
+	nsky[3] = nx1 * ny1 + nx2 * ny2
+	sky[3] = ptr2
+
+	if (nsky[3] > 0) {
+	    ptr1 = datain + (y2 - y1) * nx
+	    for (y=y2; y<=y3; y=y+1) {
+	        call amovr (Memr[ptr1], Memr[ptr2], nx1)
+	        ptr1 = ptr1 + nx
+	        ptr2 = ptr2 + nx1
+	    }
+	    for (; y<=y4; y=y+1) {
+	        call amovr (Memr[ptr1], Memr[ptr2], nx2)
+	        ptr1 = ptr1 + nx
+	        ptr2 = ptr2 + nx2
+	    }
+	}
+
+	# Fourth quadrant
+	x2 = max (1, int (xc + 1.5))
+	x3 = min (xlen, int (xc + r + 0.5))
+	y2 = max (1, int (yc + 1.5))
+	y3 = min (xlen, int (yc + r + 0.5))
+	nx1 = x4 - x3
+	nx2 = x4 - x2 + 1
+	ny1 = y3 - y2 + 1
+	ny2 = y4 - y3
+	nsky[4] = ny1 * nx1 + ny2 * nx2
+	sky[4] = ptr2
+
+	if (nsky[4] > 0) {
+	    ptr1 = datain + (y2 - y1) * nx + x3 - x1 + 1
+	    for (y=y2; y<=y3; y=y+1) {
+	        call amovr (Memr[ptr1], Memr[ptr2], nx1)
+	        ptr1 = ptr1 + nx
+	        ptr2 = ptr2 + nx1
+	    }
+	    ptr1 = ptr1 - (x3 - x2 + 1)
+	    for (; y<=y4; y=y+1) {
+	        call amovr (Memr[ptr1], Memr[ptr2], nx2)
+	        ptr1 = ptr1 + nx
+	        ptr2 = ptr2 + nx2
+	    }
+	}
+
+	# This part is for doing a gradient correction.  It is not implemented.
+#	if ((nsky[1]>NSKY)&&(nsky[2]>NSKY)&&(nsky[3]>NSKY)&&(nsky[4]>NSKY)) {
+#	    call asrtr (Memr[sky[1]], Memr[sky[1]], nsky[1])
+#	    call asrtr (Memr[sky[2]], Memr[sky[2]], nsky[2])
+#	    call asrtr (Memr[sky[3]], Memr[sky[3]], nsky[3])
+#	    call asrtr (Memr[sky[4]], Memr[sky[4]], nsky[4])
+
+	    # Add a gradient correction here.
+
+#	    seed = dataout
+#	    do i = dataout, dataout+nobj-1 {
+#	        j = 4 * urand (seed) + 1
+#	        k = 0.95 * nsky[j] * urand (seed)
+#	        Memr[i] = Memr[sky[j]+k]
+#	    }
+#	} else {
+	    call asrtr (Memr[allsky], Memr[allsky], nallsky)
+
+	    # Find the mean and sigma excluding the outer 20%
+	    x1 = 0.1 * nallsky
+	    x2 = 0.9 * nallsky
+	    call aavgr (Memr[allsky+x1-1], x2-x1+1, avg, sigma)
+	    mode = find_mode (Memr[allsky], nallsky, nallsky / 20)
+	    call printf ("Mean = %g,  Median = %g,  Mode = %g\n")
+		call pargr (avg)
+		call pargr (Memr[allsky+nallsky/2-1])
+		call pargr (mode)
+	    for (x1=0; (x1<nallsky)&&(Memr[allsky+x1]<avg-3*sigma); x1=x1+1)
+		;
+	    for (x2=nallsky-1; (x2>0)&&(Memr[allsky+x2]>avg+3*sigma); x2=x2-1)
+		;
+	    nx = x2 - x1 - 1
+
+	    seed = dataout
+	    do i = dataout, dataout+nobj-1 {
+	        j = nx * urand (seed) + x1
+	        Memr[i] = Memr[allsky+j]
+	    }
+#	}
+
+	call sfree (sp)
+	return (nobj)
+end
+
+real procedure find_mode (data, npts, n)
+
+real	data[npts]		# Data
+int	npts			# Number of data points
+int	n			# Bin size
+
+int	x, xlast, xmin
+real	sumx, sumy, sumxx, sumxy, a, amin
+pointer	sp, slope
+
+begin
+	call smark (sp)
+	call salloc (slope, npts - n, TY_REAL)
+
+	sumx = 0.
+	sumy = 0.
+	sumxx = 0.
+	sumxy = 0.
+
+	x = 0
+	xlast = 0
+	while (x < n) {
+	    x = x + 1
+	    sumx = sumx + x
+	    sumy = sumy + data[x]
+	    sumxx = sumxx + x ** 2
+	    sumxy = sumxy + x * data[x]
+	}
+	amin = (n * sumxy - sumx * sumy) / (n * sumxx - sumx ** 2)
+	xmin = (x + xlast) / 2
+	Memr[slope] = amin
+
+	while (x < npts - n) {
+	    x = x + 1
+	    xlast = xlast + 1
+	    sumx = sumx + x - xlast
+	    sumy = sumy + data[x] - data[xlast]
+	    sumxx = sumxx + x * x - xlast * xlast
+	    sumxy = sumxy + x * data[x] - xlast * data[xlast]
+
+	    a = (n * sumxy - sumx * sumy) / (n * sumxx - sumx ** 2)
+	    if (a < amin) {
+		amin = a
+		xmin = (x + xlast) / 2
+	    }
+	    Memr[slope+xlast] = a
+	}
+
+	call gplotv (Memr[slope+11], npts-2*n-22, 1., real (npts-2*n-22), "")
+	call sfree (sp)
+	return (data[xmin])
+end
diff --git a/noao/imred/ccdred/src/timelog.x b/noao/imred/ccdred/src/timelog.x
new file mode 100644
index 00000000..7a8d969f
--- /dev/null
+++ b/noao/imred/ccdred/src/timelog.x
@@ -0,0 +1,29 @@
+include	<time.h>
+
+
+# TIMELOG -- Prepend a time stamp to the given string.
+#
+# For the purpose of a history logging prepend a short time stamp to the
+# given string.  Note that the input string is modified.
+
+procedure timelog (str, max_char)
+
+char	str[max_char]		# String to be time stamped
+int	max_char		# Maximum characters in string
+
+pointer	sp, time, temp
+long	clktime()
+
+begin
+	call smark (sp)
+	call salloc (time, SZ_DATE, TY_CHAR)
+	call salloc (temp, max_char, TY_CHAR)
+
+	call cnvdate (clktime(0), Memc[time], SZ_DATE)
+	call sprintf (Memc[temp], max_char, "%s %s")
+	    call pargstr (Memc[time])
+	    call pargstr (str)
+	call strcpy (Memc[temp], str, max_char)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ccdred/x_ccdred.x b/noao/imred/ccdred/x_ccdred.x
new file mode 100644
index 00000000..f651b668
--- /dev/null
+++ b/noao/imred/ccdred/x_ccdred.x
@@ -0,0 +1,15 @@
+task	badpiximage	= t_badpiximage,
+	ccdgroups	= t_ccdgroups,
+	ccdhedit	= t_ccdhedit,
+	ccdinstrument	= t_ccdinst,
+	ccdlist		= t_ccdlist,
+	ccdmask		= t_ccdmask,
+	ccdproc		= t_ccdproc,
+	qccdproc	= t_ccdproc,
+	combine		= t_combine,
+	mkfringecor	= t_mkfringecor,
+	mkillumcor	= t_mkillumcor,
+	mkillumflat	= t_mkillumflat,
+	mkimage		= t_mkimage,
+	mkskycor	= t_mkskycor,
+	mkskyflat	= t_mkskyflat
diff --git a/noao/imred/ccdred/zerocombine.cl b/noao/imred/ccdred/zerocombine.cl
new file mode 100644
index 00000000..6fb9613b
--- /dev/null
+++ b/noao/imred/ccdred/zerocombine.cl
@@ -0,0 +1,48 @@
+# ZEROCOMBINE -- Process and combine zero level CCD images.
+
+procedure zerocombine (input)
+
+string	input			{prompt="List of zero level images to combine"}
+file	output="Zero"		{prompt="Output zero level name"}
+string	combine="average"	{prompt="Type of combine operation",
+				 enum="average|median"}
+string	reject="minmax"		{prompt="Type of rejection",
+		enum="none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip"}
+string	ccdtype="zero"	{prompt="CCD image type to combine"}
+bool	process=no	{prompt="Process images before combining?"}
+bool	delete=no	{prompt="Delete input images after combining?"}
+bool	clobber=no	{prompt="Clobber existing output image?"}
+string	scale="none"	{prompt="Image scaling",
+			 enum="none|mode|median|mean|exposure"}
+string	statsec=""	{prompt="Image section for computing statistics"}
+int	nlow=0		{prompt="minmax: Number of low pixels to reject"}
+int	nhigh=1		{prompt="minmax: Number of high pixels to reject"}
+int	nkeep=1		{prompt="Minimum to keep (pos) or maximum to reject (neg)"}
+bool	mclip=yes	{prompt="Use median in sigma clipping algorithms?"}
+real	lsigma=3.	{prompt="Lower sigma clipping factor"}
+real	hsigma=3.	{prompt="Upper sigma clipping factor"}
+string	rdnoise="0."	{prompt="ccdclip: CCD readout noise (electrons)"}
+string	gain="1."	{prompt="ccdclip: CCD gain (electrons/DN)"}
+string	snoise="0."	{prompt="ccdclip: Sensitivity noise (fraction)"}
+real	pclip=-0.5	{prompt="pclip: Percentile clipping parameter"}
+real	blank=0.	{prompt="Value if there are no pixels"}
+
+begin
+	string	ims
+
+	ims = input
+
+	# Process images first if desired.
+	if (process == YES)
+	    ccdproc (ims, output="", ccdtype=ccdtype, noproc=no)
+
+	# Combine the flat field images.
+	combine (ims, output=output, plfile="", sigma="", combine=combine,
+	    reject=reject, ccdtype=ccdtype, subsets=no, delete=delete,
+	    clobber=clobber, project=no, outtype="real", offsets="none",
+	    masktype="none", blank=blank, scale=scale, zero="none", weight=no,
+	    statsec=statsec, lthreshold=INDEF, hthreshold=INDEF, nlow=nlow,
+	    nhigh=nhigh, nkeep=nkeep, mclip=mclip, lsigma=lsigma, hsigma=hsigma,
+	    rdnoise=rdnoise, gain=gain, snoise=snoise, sigscale=0.1,
+	    pclip=pclip, grow=0)
+end
diff --git a/noao/imred/crutil/crutil.cl b/noao/imred/crutil/crutil.cl
new file mode 100644
index 00000000..89e7ff3e
--- /dev/null
+++ b/noao/imred/crutil/crutil.cl
@@ -0,0 +1,18 @@
+#{ CRUTIL -- Cosmic Ray Utility Package
+
+package crutil
+
+reset	crusrc			= "crutil$src/"
+
+task	crcombine	= crusrc$crcombine.cl
+task	crnebula	= crusrc$crnebula.cl
+task	crfix		= crusrc$crfix.cl
+task	credit		= crusrc$credit.cl
+
+task	cosmicrays,
+	craverage,
+	crgrow,
+	crmedian	= crusrc$x_crutil.e
+
+
+clbye()
diff --git a/noao/imred/crutil/crutil.hd b/noao/imred/crutil/crutil.hd
new file mode 100644
index 00000000..0b6ee225
--- /dev/null
+++ b/noao/imred/crutil/crutil.hd
@@ -0,0 +1,17 @@
+# Help directory for the CRUTIL package.
+
+$doc = "./doc/"
+$crusrc = "./src/"
+
+revisions	sys=crusrc$Revisions
+
+overview	hlp=doc$overview.hlp
+
+cosmicrays	hlp=doc$cosmicrays.hlp,		src=crusrc$t_cosmicrays.x
+craverage	hlp=doc$craverage.hlp,		src=crusrc$t_craverage.x
+crcombine	hlp=doc$crcombine.hlp,		src=crusrc$crcombine.cl
+credit		hlp=doc$credit.hlp,		src=crusrc$credit.cl
+crfix		hlp=doc$crfix.hlp,		src=crusrc$crfix.cl
+crgrow		hlp=doc$crgrow.hlp,		src=crusrc$t_crgrow.x
+crmedian	hlp=doc$crmedian.hlp,		src=crusrc$t_crmedian.x
+crnebula	hlp=doc$crnebula.hlp,		src=crusrc$crnebula.cl
diff --git a/noao/imred/crutil/crutil.men b/noao/imred/crutil/crutil.men
new file mode 100644
index 00000000..f6117e5f
--- /dev/null
+++ b/noao/imred/crutil/crutil.men
@@ -0,0 +1,10 @@
+     cosmicrays - Remove cosmic rays using flux ratio algorithm
+      craverage - Detect CRs against average and avoid objects
+      crcombine - Combine multiple exposures to eliminate cosmic rays
+	 credit - Interactively edit cosmic rays using an image display
+	  crfix - Fix cosmic rays in images using cosmic ray masks
+         crgrow - Grow cosmic rays in cosmic ray masks
+       crmedian - Detect and replace cosmic rays with median filter
+       crnebula - Detect and replace cosmic rays in nebular data
+
+       overview - Overview of the package
diff --git a/noao/imred/crutil/crutil.par b/noao/imred/crutil/crutil.par
new file mode 100644
index 00000000..6782c988
--- /dev/null
+++ b/noao/imred/crutil/crutil.par
@@ -0,0 +1,3 @@
+# CRUTIL package parameter file
+
+version,s,h,"V1.5: August 22, 2001"
diff --git a/noao/imred/crutil/doc/cosmicrays.hlp b/noao/imred/crutil/doc/cosmicrays.hlp
new file mode 100644
index 00000000..55a284da
--- /dev/null
+++ b/noao/imred/crutil/doc/cosmicrays.hlp
@@ -0,0 +1,306 @@
+.help cosmicrays Apr98 noao.imred.crutil
+.ih
+NAME
+cosmicrays -- detect and replace cosmic rays
+.ih
+USAGE
+cosmicrays input output
+.ih
+PARAMETERS
+.ls input
+List of input images in which to detect cosmic rays.
+.le
+.ls output
+List of output images in which the detected cosmic rays will be replaced
+by an average of neighboring pixels.  If the output image name differs
+from the input image name then a copy of the input image is made with
+the detected cosmic rays replaced.  If no output images are specified
+then the input images are modified in place.  In place modification of
+an input image also occurs when the output image name is the same as
+the input image name.
+.le
+.ls crmasks = ""
+List of cosmic ray mask files to be created; one for each input image.  If no
+file names are given then no cosmic ray mask is created.  If an existing
+mask is specified the newly detected cosmic rays will be added.
+.le
+
+.ls threshold = 25.
+Detection threshold above the mean of the surrounding pixels for cosmic
+rays.  The threshold will depend on the noise characteristics of the
+image and how weak the cosmic rays may be for detection.  A typical value
+is 5 or more times the sigma of the background.
+.le
+.ls fluxratio = 2.
+The ratio (as a percent) of the mean neighboring pixel flux to the candidate
+cosmic ray pixel for rejection.  The value depends on the seeing and the
+characteristics of the cosmic rays.  Typical values are in the range
+2 to 10 percent.  This value may be reset interactively from a plot
+or defined by identifying selected objects as stars or cosmic rays.
+.le
+.ls npasses = 5
+Number of cosmic ray detection passes.  Since only the locally strongest
+pixel is considered a cosmic ray, multiple detection passes are needed to
+detect and replace cosmic ray events with multiple neighboring pixels.
+.le
+.ls window = 5
+Size of cosmic ray detection window.  A square window of either 5 by 5 or
+7 by 7 is used to detect cosmic rays.  The smaller window allows detection
+in the presence of greater background gradients but is less sensitive at
+discriminating multiple event cosmic rays from stars.  It is also marginally
+faster.
+.le
+.ls interactive = yes
+Examine parameters interactively?  A plot of the mean flux within the
+detection window (x100) vs the flux ratio (x100) is plotted and the user may
+set the flux ratio threshold, delete and undelete specific events, and
+examine specific events.  This is useful for new data in which one is
+uncertain of an appropriate flux ratio threshold.  Once determined the
+task need not be used interactively.
+.le
+.ls train = no
+Define the flux ratio threshold by using a set of objects identified
+as stars (or other astronomical objects) or cosmic rays?
+.le
+.ls objects = ""
+Cursor list of coordinates of training objects.  If null (the null string "")
+then the image display cursor will be read.  The user is responsible for first
+displaying the image.  Otherwise a file containing cursor coordinates
+may be given.  The format of the cursor file is "x y wcs key" where
+x and y are the pixel coordinates, wcs is an arbitrary number such as 1,
+and key may be 's' for star or 'c' for cosmic ray.
+.le
+.ls savefile = ""
+File to save (by appending) the training object coordinates.  This is of
+use when the objects are identified using the image display cursor.  The
+saved file can then be input as the object cursor list for repeating the
+execution.
+.le
+.ls plotfile
+If a plot file is specified then the graph of the flux ratio (x100) vs
+the mean flux (x100) is recorded as metacode.  This may be spooled or examined
+later.
+.le
+.ls graphics = "stdgraph"
+Interactive graphic output device for interactive examination of the
+detection parameters.
+.le
+.ls cursor = ""
+Interactive graphics cursor input.  If null the graphics display cursor
+is used, otherwise a file containing cursor input may be specified.
+.le
+.ls answer
+This parameter is used for interactive queries when processing a list of
+images.  The responses may be "no", "yes", "NO", or "YES".  The upper case
+responses permanently enable or disable the interactive review while
+the lower case reponses allow selective examination of certain input
+images.  \fIThis parameter should not be specified on the command line.
+If it is then the value will be ignored and the task will act as if
+the answer "yes" is given for each image; i.e. it will enter the interactive
+phase without prompting.\fR
+.le
+.ih
+IMAGE CURSOR COMMANDS
+
+.nf
+?	Help
+c	Identify the object as a cosmic ray
+s	Identify the object as a star
+g	Switch to the graphics plot
+q	Quit and continue with the cleaning
+.fi
+
+GRAPHICS CURSOR COMMANDS
+
+.nf
+?	Help
+a	Toggle between showing all candidates and only the training points
+d	Mark candidate for replacement (applys to '+' points)
+e	Mark candidates in a region for replacement (applys to '+' points)
+q	Quit and return to image cursor or replace the selected pixels
+r	Redraw the graph
+s	Make a surface plot for the candidate nearest the cursor
+t	Set the flux ratio threshold at the y cursor position
+u	Mark candidate to not be replaced (applys to 'x' points)
+v	Mark candidates in a region to not be replaced (applys to 'x' points)
+w	Adjust the graph window (see \fBgtools\fR)
+<space>	Print the pixel coordinates
+.fi
+
+There are no colon commands except those for the windowing options (type
+:\help or see \fBgtools\fR).
+.ih
+DESCRIPTION
+Cosmic ray events in each input image are detected and replaced by the
+average of the four neighbors.  The replacement may be performed
+directly on the input image if no output image is specified or if the
+output image name is the same as the input image name.  If a new image
+is created it is a copy of the input image except for the replaced
+pixels.  
+Optional output includes
+a plot file showing the parameters of the
+detected cosmic ray candidates and the flux ratio threshold used, a
+cosmic ray mask identifying the cosmic rays found, and
+a file of training objects marked with the image display cursor.  The
+cosmic ray mask may be used for display purposes, combined with other
+masks, and with \fBcrfix\fR.
+
+This task may be applied to an image previously processed to detect
+additional cosmic rays.
+
+The cosmic ray detection algorithm consists of the following steps.
+First a pixel must be the brightest pixel within the specified
+detection window (either 5x5 or 7x7).  The mean flux in the surrounding
+pixels with the second brightest pixel excluded (which may also be a
+cosmic ray event) is computed and the candidate pixel must exceed this
+mean by the amount specified by the parameter \fIthreshold\fR.  A plane
+is fit to the border pixels of the window and the fitted background is
+subtracted.  The mean flux (now background subtracted) and the ratio of
+this mean to the cosmic ray candidate (the brightest pixel) are
+computed.  The mean flux (x100) and the ratio (x100) are recorded for
+interactive examination if desired.
+
+Once the list of cosmic ray candidates has been created and a threshold for
+the flux ratio established (by the parameter \fIfluxratio\fR, by the
+"training" method, or by using the graphics cursor in the interactive plot)
+the pixels with ratios below the threshold are replaced in the output by
+the average of the four neighboring pixels (with the second strongest pixel
+in the detection window excluded if it is one of these pixels).  Additonal
+pixels may then be detected and replaced in further passes as specified by
+the parameter \fInpasses\fR.  Note that only pixels in the vicinity of
+replaced pixels need be considered in further passes.
+
+The division between the peaks of real objects and cosmic rays is made
+based on the flux ratio between the mean flux (excluding the center
+pixel and the second strongest pixel) and the candidate pixel.  This
+threshold depends on the point spread function and the distribution of
+multiple cosmic ray events and any additional neighboring light caused
+by the events.  This threshold is not strongly coupled to small changes
+in the data so that once it is set for a new type of image data it may
+be used for similar images.  To set it initially one may examine the
+scatter plot of the flux ratio as a function of the mean flux.  This
+may be done interactively or from the optional plot file produced.
+
+After the initial list of cosmic ray candidates has been created and before
+the final replacing cosmic rays there are two optional steps to allow
+examining the candidates and setting the flux ratio threshold dividing
+cosmic rays from real objects.  The first optional step is define the flux
+ratio boundary by reference to user specified classifications; that is
+"training".  To do this step the \fItrain\fR parameter must be set to yes.
+The user classified objects are specified by a cursor input list.  This
+list can be an actual file or the image display cursor as defined by the
+\fIobjects\fR parameter.  The \fIsavefile\fR parameter is also used during
+the training to record the objects specified.  The parameter specifies a
+file to append the objects selected.  This is useful when the objects are
+defined by interactive image cursor and does not make much sense when using
+an input list.
+
+If the \fIobjects\fR parameter is specified as a null string then
+the image display cursor will be repeatedly read until a 'q' is
+entered.  The user first displays the image and then when the task
+reads the display cursor the cursor shape will change.  The user
+points at objects and types 's' for a star (or other astronomical
+object) and 'c' for a cosmic ray.  Note that this input is used
+to search for the matching object in the cosmic ray candidate list
+and so it is possible the selected object is not in the list though
+it is unlikely.  The selection will be quietly ignored in that case.
+To exit the interactive selection of training objects type 'q'.
+
+If 'g' is typed a graph of all the candidates is drawn showing
+"flux" vs. "flux ratio" (see below for more).  Training objects will
+be shown with a box and the currently set flux ratio threshold will
+also be shown.  Exiting the plot will return to entering more training
+objects.  The plot will remain and additional objects will immediately
+be shown with a new box.  Thus, if one wants to see the training
+objects identified in the plot as one selects them from the image
+display first type a 'g' to draw the initial plot.  Also by switching
+to the plot with 'g' allows you to draw surface plots (with 's') or
+get the pixel coordinates of a candidate (the space key) to be
+found in the display using the coordinate readout of the display.
+Note that the display interaction is simpler than might be desired
+because this task does not directly connect to the display.
+
+The most likely use for training is with the interactive image display.
+However one may prepare an input list by other means, one example
+is with \fBrimcursor\fR, and then specify the file name.  The savefile
+may also be used a cursor input to repeat the cosmic ray operation
+(but be careful not to have the cursor input and save file be the
+same file!).
+
+The flux ratio threshold is determined from the training objects by
+finding the point with the minimum number of misclassifications
+(stars as cosmic rays or cosmic rays as stars).  The threshold is
+set at the lowest value so that it will always go through one of
+the cosmic ray objects.  There should be at least one of each type
+of object defined for this to work.  The following option of
+examining the cosmic ray candidates and parameters may still be
+used to modify the derived flux ratio threshold.  One last point
+about the training objects is that even if some of the points
+lie on the wrong side of the threshold they will remain classified
+as cosmic ray or non-cosmic ray.  In other words, any object
+classified by the user will remain in that classification regardless
+of the final flux ratio threshold.
+
+After the training step the user will be queried to examine the candidates
+in the flux vs flux ratio plane if the \fIinteractive\fR flag is set.
+Responses may be made for specific images or for all images by using
+lower or upper case answers respectively.  When the parameters are
+examined interactively the user may change the flux ratio threshold
+('t' key).  Changes made are stored in the parameter file and, thus,
+learned for further images.  Pixels to be deleted are marked by crosses
+and pixels which are peaks of objects are marked by pluses.  The user
+may explicitly delete or undelete any point if desired but this is only
+for special cases near the threshold.  In the future keys for
+interactive display of the specific detections will be added.
+Currently a surface plot of any candidate may be displayed graphically
+in four 90 degree rotated views using the 's' key.  Note that the
+initial graph does not show all the points some of which are clearly
+cosmic rays because they have negative mean flux or flux ratio.  To
+view all data one must rewindow the graph with the 'w' key or ":/"
+commands (see \fBgtools\fR).
+.ih
+EXAMPLES
+1. To replace cosmic rays in a set of images ccd* without training:
+
+.nf
+    cl> cosmicrays ccd* new//ccd*
+    ccd001: Examine parameters interactively? (yes):
+    [A scatter plot graph is made.  One can adjust the threshold.]
+    [Looking at a few points using the 's' key can be instructive.]
+    [When done type 'q'.]
+    ccd002: Examine parameters interactively? (yes): NO
+    [No further interactive examination is done.]
+.fi
+
+After cleaning one typically displays the images and  possibly blinks them.
+A difference image or mask image may also be created.
+
+2. To use the interactive training method for setting the flux ratio threshold:
+
+.nf
+    # First display the image.
+    cl> display ccd001 1
+    z1 = 123.45 z2= 543.21
+    cl> cosmicrays ccd001 ccd001cr train+
+    [After the cosmic ray candidates are found the image display
+    [cursor will be activated.  Mark a cosmic ray with 'c' and
+    [a star with 's'.  Type 'g' to get a plot showing the two
+    [points with boxes.  Type 'q' to go back to the image display.
+    [As each new object is marked a box will appear in the plot and
+    [the threshold may change.  To find the location of an object
+    [seen in the plot use 'g' to go to the graph, space key to find
+    [the pixel coordinates, 'q' to go back to the image display,
+    [and the image display coordinate box to find the object.
+    [When done with the training type 'q'.
+    ccd001: Examine parameters interactively? (yes): no
+.fi
+
+3.  To create a mask image a bad pixel file must be specified.
+
+.nf
+    cl> cosmicrays ccd001 ccd001 crmask=crccd001
+.fi
+.ih
+SEE ALSO
+crmedian, crnebula, crgrow, crfix, credit, gtools, imedit, rimcursor
+.endhelp
diff --git a/noao/imred/crutil/doc/craverage.hlp b/noao/imred/crutil/doc/craverage.hlp
new file mode 100644
index 00000000..bd4ef7c9
--- /dev/null
+++ b/noao/imred/crutil/doc/craverage.hlp
@@ -0,0 +1,232 @@
+.help craverage Apr98 noao.imred.crutil
+.ih
+NAME
+craverage -- detect CRs and objects using average filter
+.ih
+SYNOPSIS
+\fBCraverage\fR detects cosmic rays and objects using a moving block
+average filter with the central pixel plus some number of additional high
+pixels  excluded and a median of an annulus around the block average box.
+It avoids identification of the cores of objects as cosmic rays by
+excluding pixels within the detected objects as cosmic ray candidates.
+.ih
+USAGE   
+.nf
+craverage input output
+.fi
+.ih
+PARAMETERS
+.ls input
+List of input images in which to detect cosmic rays and objects.
+.le
+.ls output
+List of output images in which cosmic rays are replaced by the block average
+value excluding the cosmic ray.  If no output image name is given then
+no output image will be created.
+.le
+.ls crmask = ""
+List of input and output cosmic ray and object masks.  If the mask exists
+then the mask values are used to exclude data pixels from the calculations
+and zero mask values are candidates for cosmic rays or objects.
+Detected cosmic rays and objects are identified in the mask with values
+given by the \fIcrval\fR and \fIobjval\fR parameters.  If no output cosmic
+ray mask is given then no mask will be created.
+.le
+.ls average = ""
+List of output block average filtered images.  If no image name is given
+then no image will be created.
+.le
+.ls sigma = ""
+List of output sigma images.  If no image name is given then no image
+will be created.
+.le
+
+.ls navg = 5 (minimum of 3)
+Square block average filter size given as the number of pixels along an
+edge.  The value will be rounded up to an odd value to be symmetrical
+around the center pixel excluded from the average.
+.le
+.ls nrej = 0 (minimum of 0)
+Number of additional highest pixels to exclude, in addition to the
+central pixel, in the block average.  The value should be small but it
+is needed to deal with cosmic rays that are bigger than a single pixel.
+.le
+.ls nbkg = 5 (minimum of 1)
+Background annulus width around the box average filter in pixels.  The
+median of the pixels in this annulus is used to estimate the background.
+.le
+.ls nsig = 25 (minimum of 10)
+Square box size for empirical sigma estimates given as the number of
+pixels along an edge.  The sigma is estimated using percentile points
+of the pixels in the box.  The size of the box should contain
+of order 100 pixels or more.
+.le
+.ls var0 = 0., var1 = 0., var2 = 0.
+Variance coefficients for the variance model.  The variance model is
+
+.nf
+    variance = var0 + var1 * data + var2 * data^2
+.fi
+
+where data is the maximum of zero and the average filtered pixel value and
+the variance is in data numbers.  All the coefficients must be positive or
+zero.  If they are all zero then empirical data sigmas are estimated by a
+percentile method in boxes of size given by \fInsig\fR.
+.le
+
+.ls crval = 1
+Mask value for detected cosmic rays.  It is legal for the value to be
+zero to not mark the cosmic rays in the output mask.
+.le
+.ls lcrsig = 10., hcrsig = 5.
+Low and high sigma factors for detecting cosmic rays.  These factors
+multiply the computed or estimated sigma at each pixel and these threshold
+values are compared to the difference between the candidate pixel and the
+block average filter value (average of box around the pixel).  This only
+applies to pixels where the block average filter value is within a
+specified threshold of the background estimate; i.e. the average value is
+not considered as part of an object.
+.le
+.ls crgrow = 0.
+Cosmic ray growing radius.  Pixels detected and marked in the output cosmic
+ray mask by the \fIcrval\fR value are increased in size in the mask (but
+not replaced in the output image) by also flagging all zero valued mask
+pixels within this specified radius with the cosmic ray mask value.  This
+is done after the detection phase is complete.  The separation between
+pixels is the distance between pixel centers computed as a real value.
+Note a value of at least one is required to affect other mask pixels.
+.le
+
+.ls objval = 0
+Mask value for detected objects.  It is legal for the value to be
+zero to not mark the objects in the output mask.
+.le
+.ls lobjsig = 10., hobjsig = 5.
+Low and high sigma factors for detecting objects.  These factors multiply
+the computed or estimated sigma at each pixel and these threshold values
+are compared to the difference between the block average filter value and
+the background annulus median.  If the values are made very large then
+object detection can be eliminated and cosmic rays will be detected
+everywhere.
+.le
+.ls objgrow = 0.
+Object detection growing radius.  Pixels detected and marked in the output
+mask by the \fIobjval\fR value are increased in size in the mask by also
+flagging all zero valued mask pixels within this specified radius with the
+cosmic ray mask value.  This is done after the detection phase is complete
+and so object grown pixels are not used in excluding cosmic ray
+candidates.  The separation between pixels is the distance between pixel
+centers computed as a real value.  Note a value of at least one is
+required to affect other mask pixels.
+.le
+.ih
+DESCRIPTION
+\fBCraverage\fR detects cosmic rays and objects using a moving block
+average filter with the central pixel and a specified number of additional
+highest pixels excluded and a median of an annulus around the block average
+box.  It avoids identification of the cores of objects as cosmic rays by
+excluding pixels within the detected objects as cosmic ray candidates.
+
+The block average filter computes the average of pixels in a box with the
+central or target pixel excluded.  In addition the \fInrej\fR parameter can
+be used to exclude that number of highest remaining pixels as possible
+contamination from cosmic rays which are larger than one pixel or possibly
+a very nearby additional cosmic ray.  The \fInrej\fR value should be kept
+small relative to the total number of pixels in the average so that the
+average will still be elevated over the median in real underlying objects.
+The resulting average is used as the prediction for the value of the target
+pixel.  The median of the pixels in a square background annulus around the
+block average box provides the prediction for the background at the target
+pixel.
+
+The target pixel is considered part of an object if the difference between
+the average value and the median background exceeds a specified threshold.
+If the pixel is NOT considered to be part of an object then if the
+difference between the pixel value and the average value exceeds a
+different specified threshold it is identified as a cosmic ray.
+
+The thresholds are defined in terms of sigma factors, which may be
+different for positive and negative deviations and for object and
+cosmic ray identification.  The sigma factors multiply an estimate
+for the statistical sigma of the target pixel.  The estimate is
+either based on a noise model or sigma of pixels in a box near the
+target pixel.
+
+The \fIcrmask\fR parameter specifies a pixel mask for the image.  If the
+mask exists then non-zero mask values will be used to exclude pixels from
+the average, background median, and empirical sigma estimates.  Also any
+pixels with non-zero mask values will not be altered either in the output
+image or in the final mask.  If the  mask does not exist then it behaves as
+if all mask values are zero.  If all pixels in the average box or median
+annulus are previously flagged then the estimates will be undefined and
+nothing will be done to the output image or mask.  Because the task can
+use an input mask to mark pixels not to be considered it can be used
+in an iterative fashion.
+
+The noise model is given by the formula
+
+.nf
+    variance = var0 + var1 * data + var2 * data^2
+.fi
+
+where data is the maximum of zero and the average estimate for the target
+pixel.  The coefficients are all given in terms of the data numbers.  This
+model can be related to common detector parameters.  For CCDs var0 is the
+readout noise expressed as a variance in data numbers and var1 is the
+inverse gain (DN/electrons).  The second order coefficient has the
+interpretation of flat field introduced variance.
+
+If all the coefficients are zero then an empirical sigma is estimated as
+follows.  The input image is divided into square blocks of size
+\fInsig\fR.  The (unmasked) pixel values in a block are sorted and the
+pixel values nearest the 15.9 and 84.1 percentiles are selected.  These are
+the one sigma points in a Gaussian distribution.  The sigma estimate is the
+difference of these two values divided by two.  This algorithm is used to
+avoid contamination of the sigma estimate by the bad pixel values.  The
+block size must be at least 10 pixels in each dimension to provide
+sufficient pixels for a good estimate of the percentile points.  The sigma
+estimate for a pixel is the sigma from the nearest block.  A moving box is
+not used for reasons of efficiency.
+
+If an output image name is specified then the output image is produced as a
+copy of the input image but with the identified cosmic ray pixels replaced
+by the average predicted value.  Other optional output images are
+the average filtered values and the sigma values.
+
+If a mask is specified the detected cosmic rays will be identified with
+values given by the \fIcrval\fR parameter and object pixels will be
+identified with values given by the \fIobjval\fR parameter.  Note that one
+does not need to use an output image and the cosmic rays can be replaced by
+interpolation in the data using the tasks \fIcrfix\fR, \fIfixpix\fR, or
+\fIccdproc\fR.
+
+One final step may be applied to the output mask.  The mask values
+identified with the \fIcrval\fR and \fIobjval\fR values may be grown
+by identifying pixel values within a specified radius with the same
+mask value.  Note that this step is done at the end and so any pixels
+in a preexisting input mask with the same values will also be grown.
+Also the grown pixels will not affect the output cosmic ray replaced
+image.  See \fIcrgrow\fR for a further discussion.
+.ih
+EXAMPLES
+This example illustrates using the \fBcraverage\fR task to
+create a mask with cosmic rays and objects identified and displayed.
+The image is a CCD image with a readout noise of 5 electrons
+and a gain of 3 electrons per data number.  This implies variance
+model coefficients of
+
+.nf
+    var0 = (5/3)^2 = 2.78
+    var1 = 1/3 = 0.34
+.fi
+
+.nf
+    cl> display obj001 1                  # Display in first frame
+    cl> craverage obj001 "" crmask=mask001 var0=2.78 var1=0.34\
+    >>> crval=1 objval=2
+    cl> display crobj001 2 overlay=mask001 ocol="1=green,2=red"
+.fi
+.ih
+SEE ALSO
+cosmicrays, crnebula, median, crfix, crgrow, crmedian
+.endhelp
diff --git a/noao/imred/crutil/doc/crcombine.hlp b/noao/imred/crutil/doc/crcombine.hlp
new file mode 100644
index 00000000..3dddaebe
--- /dev/null
+++ b/noao/imred/crutil/doc/crcombine.hlp
@@ -0,0 +1,35 @@
+.help crcombine Apr98 noao.imred.crutil
+.ih
+NAME
+crcombine -- combine multiple exposures to eliminate cosmic rays
+.ih
+USAGE	
+.nf
+crcombine input output
+.fi
+.ih
+PARAMETERS
+See parameters for \fBimcombine\fR.
+.ih
+DESCRIPTION
+This task is a version of \fBimcombine\fR.  See the help for that task
+for a description of the parameters and algorithms.
+
+For the purpose of removing cosmic rays the most useful options
+are the "crreject" algorithm and/or combining with a median.  Many other
+options may work as well.  The best use of this task depends on the
+number of images available.  If there are more than a few images the
+images should be combined with an "average" and using a rejection
+algorithm.
+.ih
+EXAMPLES
+1.  To combine two images using the gain and read noise parameters in
+the image header:
+
+.nf
+    cl> crcombine obj012,obj013 abc gain=gain rdnoise=rdnoise 
+.fi
+.ih
+SEE ALSO
+imcombine
+.endhelp
diff --git a/noao/imred/crutil/doc/credit.hlp b/noao/imred/crutil/doc/credit.hlp
new file mode 100644
index 00000000..f038e5c1
--- /dev/null
+++ b/noao/imred/crutil/doc/credit.hlp
@@ -0,0 +1,39 @@
+.help credit Apr98 noao.imred.crutil
+.ih
+NAME
+credit -- interactively edit cosmic rays using an image display
+.ih
+USAGE	
+.nf
+credit input output
+.fi
+.ih
+PARAMETERS
+See parameters for \fBimedit\fR.
+.ih
+DESCRIPTION
+This task is a version of \fBimedit\fR.  See the help for that task
+for a description of the parameters and algorithms.
+
+For the purpose of editing cosmic rays the most useful editing option
+is 'b' to replace cosmic rays in a circular annulus using local sky
+values.  This can be done interactively or using a list of positions
+along with the \fIdefault\fR parameter value.
+.ih
+EXAMPLES
+1.  To replace cosmic rays interactively.
+
+.nf
+    cl> credit obj012 crobj012 crmask012
+.fi
+
+2.  To use a two column list of positions and remove the cosmic rays using
+the 'b' key algorithm.
+
+.nf
+    cl> credit obj012 crobj012 cursor=crlist.dat display-
+.fi
+.ih
+SEE ALSO
+imedit, epix
+.endhelp
diff --git a/noao/imred/crutil/doc/crfix.hlp b/noao/imred/crutil/doc/crfix.hlp
new file mode 100644
index 00000000..5794a001
--- /dev/null
+++ b/noao/imred/crutil/doc/crfix.hlp
@@ -0,0 +1,48 @@
+.help crfix Apr98 noao.imred.crutil
+.ih
+NAME
+crfix -- fix cosmic rays in images using cosmic ray masks
+.ih
+USAGE	
+.nf
+crfix input output masks
+.fi
+.ih
+PARAMETERS
+.ls input
+Input two dimensional image to be "fixed" (modified) by linear interpolation.
+.le
+.ls output
+Output image.  If the output image name exactly matches the input
+image name (including extensions) then the image will be modified in place.
+.le
+.ls crmask
+Cosmic ray mask identifying the cosmic rays to be fixed.  The mask
+values are zero for good data and non-zero for cosmic rays.
+.le
+.ih
+DESCRIPTION
+The input and output images are specified by the \fIinput\fR and
+\fIoutput\fR parameters.  If the input and output image names are
+identifical (including extensions) then image is modified in place.  Cosmic
+rays, identified in a cosmic ray mask specified by the \fIcrmask\fR
+parameter, are replaced in the output image by linear interpolation along
+lines or columns using the nearest good pixels.  The special mask name
+"BPM" may be used to select a mask name given in the input image header
+under the keyword "BPM".
+
+Cosmic ray pixels are "fixed" by replacing them with values
+by linear interpolation to the nearest pixels not identified as bad.
+The interpolation direction is the shortest length between good pixels
+along columns or lines.
+.ih
+EXAMPLES
+1.  To replace cosmic rays in an image:
+
+.nf
+    cl> crfix obj012 crobj012 crmask012
+.fi
+.ih
+SEE ALSO
+fixpix, crmedian, crnebula, cosmicrays, credit, epix
+.endhelp
diff --git a/noao/imred/crutil/doc/crgrow.hlp b/noao/imred/crutil/doc/crgrow.hlp
new file mode 100644
index 00000000..f3a1ff5c
--- /dev/null
+++ b/noao/imred/crutil/doc/crgrow.hlp
@@ -0,0 +1,55 @@
+.help crgrow Apr98 noao.imred.crutil
+.ih
+NAME
+crgrow -- grow cosmic rays in cosmic ray masks
+.ih
+USAGE	
+crgrow input output radius
+.ih
+PARAMETERS
+.ls input
+List of cosmic ray masks to be modified.
+.le
+.ls output
+List of output modified cosmic ray masks.  The input and output lists must
+match.  If the input and output cosmic ray masks are specified as the same
+then the input mask will be modified in place.
+.le
+.ls radius = 1.
+Replacement radius around cosmic rays.
+If a pixel is within this distance of a cosmic ray pixel
+it is identified by a value of 1 in the output cosmic ray mask.  Distances are
+measured between pixel centers which are have integer coordinates.
+.le
+.ls inval = INDEF
+Mask value to be grown.  A value of INDEF will grow all non-zero values.
+.le
+.ls outval = INDEF
+Mask value for grown pixels.  A value of INDEF will use the value of the
+pixel being grown for the grown pixel value.
+.le
+.ih
+DESCRIPTION
+The cosmic ray pixels, identified by the "inval" parameter, in the input
+mask are located and all unmasked (zero valued) pixels within the specified
+grow radius are set to a value given by the "outval" parameter. The
+distance between pixels is measured as a cartisian logical pixel coordinate
+distance.
+.ih
+EXAMPLES
+1.  A radius of 1 will grow cosmic rays in a "plus" pattern.
+
+.nf
+    cl> crgrow crmask1 crmask2 1
+.fi
+
+2.  A radius of 1.5 will grow cosmic rays in a box pattern.  The following
+will modify the input mask.
+
+.nf
+    cl> crgrow crmask crmask 1.5
+.fi
+.ih
+SEE ALSO
+imreplace
+.endhelp
diff --git a/noao/imred/crutil/doc/crmedian.hlp b/noao/imred/crutil/doc/crmedian.hlp
new file mode 100644
index 00000000..3147b676
--- /dev/null
+++ b/noao/imred/crutil/doc/crmedian.hlp
@@ -0,0 +1,157 @@
+.help crmedian Apr98 noao.imred.crutil
+.ih
+NAME
+crmedian -- detect, fix, and flag cosmic rays using median filtering
+.ih
+USAGE   
+.nf
+crmedian input output
+.fi
+.ih
+PARAMETERS
+.ls input
+Input image in which to detect cosmic rays.
+.le
+.ls output
+Output image in which cosmic rays are replaced by the median value.
+If no output image name is given then no output image will be created.
+.le
+.ls crmask = ""
+Output cosmic ray mask.  Detected cosmic rays (and other deviant pixels)
+are identified in the mask with values of one and good pixels with a values
+of zero.  If no output cosmic ray mask is given then no mask will be
+created.
+.le
+.ls median = ""
+Output median filtered image.  If no image name is given then no output will be
+created.
+.le
+.ls sigma = ""
+Output sigma image.  If no image name is given then no output will be
+created.
+.le
+.ls residual = ""
+Output residual image.  This is the input image minus the median filtered
+image divided by the sigma image.  Thresholds in this image determine the
+cosmic rays detected.  If no image name is given then no output will be
+created.
+.le
+.ls var0 = 0., var1 = 0., var2 = 0.
+Variance coefficients for the variance model.  The variance model is
+
+.nf
+    variance = var0 + var1 * data + var2 * data^2
+.fi
+
+where data is the maximum of zero and median pixel value and the variance
+is in data numbers.  All the coefficients must be positive or zero.  If
+they are all zero then empirical data sigmas are estimated by a percentile
+method in boxes of size given by \fIncsig\fR and \fInlsig\fR.
+.le
+.ls lsigma = 10, hsigma = 3
+Positive sigma factors to use for selecting pixels below and above
+the median level based on the local percentile sigma.  Cosmic rays will
+appear above the median level.
+.le
+.ls ncmed = 5, nlmed = 5
+The column and line size of a moving median rectangle used to estimate the
+uncontaminated local image.
+.le
+.ls ncsig = 25, nlsig = 25
+The column and line size of regions used to estimate the uncontaminated
+local sigma using a percentile.  The size of the box should contain
+of order 100 pixels or more.
+.le
+.ih
+DESCRIPTION
+\fBCrmedian\fR detects cosmic rays from pixels deviating by a specified
+statistical amount from the median at each pixel.  It outputs and set of
+the following: a copy of the input image with cosmic rays replaced by the
+median value, a cosmic ray mask identifying the cosmic rays, the median
+filtered image, a sigma image where each pixel has the estimated sigma, and
+the residual image used in detecting the cosmic rays.
+
+The residual image is computed by subtracting a median filtered version
+of the input data from the unfiltered input data and dividing by an
+estimate of the pixel sigmas.  The median filter
+box size is given by the \fIncmed\fR and \fInlmed\fR parameters.
+If a name for the median image is specified the median filtered image
+will be output.  The variance at each pixel is determined either from
+a variance model or empirically.  If a name for the sigma image is specified
+then the sigma values (the square root of the variance) will be output.
+If a name for the residual image is given then the residual image
+will be output.
+
+The empirical variance model is given by the formula
+
+.nf
+    variance = var0 + var1 * data + var2 * data^2
+.fi
+
+where data is the maximum of zero and median pixel value and the variance
+is in data numbers.  This model can be related to common detector
+parameters.  For CCDs var0 is the readout noise expressed as a variance in
+data numbers and var1 is the inverse gain (DN/electrons).  The second order
+coefficient has the interpretation of flat field introduced variance.
+
+If all the coefficients are zero then an empirical sigma is estimated
+as follows.  The input image is divided into blocks of size
+\fIncsig\fR and \fInlsig\fR.  The pixel values in a block are sorted
+and the pixel values nearest the 15.9 and 84.1 percentiles are
+selected.  These are the one sigma points in a Gaussian distribution.
+The sigma estimate is the difference of these two values divided by
+two.  This algorithm is used to avoid contamination of the sigma
+estimate by the bad pixel values.  The block size must be at least 10
+pixels in each dimension to provide sufficient pixels for a good estimate
+of the percentile points.  The sigma estimate for a pixel is the sigma
+from the nearest block.  A moving box is not used for efficiency.
+
+The residual image is divided by the sigma estimate at each pixel.
+Cosmic rays are identified by finding those pixels in the
+residual image which have values greater than \fIhsigma\fR and bad
+pixels with values below \fIlsigma\fR are also identified.
+
+If an output image name is specified then the output image is produced as a
+copy of the input image but with the identified cosmic ray pixels replaced
+by the median value.  If an output cosmic ray mask is specified a cosmic
+ray mask will be produced with values of zero for good pixels and one for
+bad pixels.  The cosmic ray mask is used to display the cosmic ray
+positions found and the cosmic rays can be replaced by interpolation (as
+opposed to the median value) using the task \fIcrfix\fR.
+
+The \fBcrmedian\fR detections are very simple and do not take into account
+real structure with scales of a pixel.  Thus this may clip the cores of
+stars and narrow nebular features in the data.  More sophisticated
+algorithms are found in \fBcosmicrays\fR, \fIcraverage\fR, and
+\fBcrnebula\fR.  The median, sigma, and residual images are available as
+output to evaluate the various aspects of the algorithm.
+.ih
+EXAMPLES
+This example illustrates using the \fBcrmedian\fR task to
+give a cosmic ray removed image and examining the results with an image
+display.  The image is a CCD image with a readout noise of 5 electrons
+and a gain of 3 electrons per data number.  This implies variance
+model coefficients of
+
+.nf
+    var0 = (5/3)^2 = 2.78
+    var1 = 1/3 = 0.34
+.fi
+
+.nf
+    cl> display obj001 1                  # Display in first frame
+    cl> # Determine output image, cosmic ray mask, and residual image
+    cl> crmedian obj001 crobj001 crmask=mask001 resid=res001\
+    >>> var0=2.78 var1=0.34
+    cl> display crobj001 2                # Display final image
+    cl> display mask001 3 zs- zr- z1=-1 z2=2 # Display mask
+    cl> display res001 4 zs- zr- z1=-5 z2=5  # Display residuals
+.fi
+
+By looking at the residual image the sigma clippig threshold can be
+adjusted and the noise parameters can be tweaked to minimize clipping
+of real extended structure.
+.ih
+SEE ALSO
+cosmicrays, craverage, crnebula, median, crfix, crgrow
+.endhelp
diff --git a/noao/imred/crutil/doc/crnebula.hlp b/noao/imred/crutil/doc/crnebula.hlp
new file mode 100644
index 00000000..174a6771
--- /dev/null
+++ b/noao/imred/crutil/doc/crnebula.hlp
@@ -0,0 +1,139 @@
+.help crnebula Apr98 noao.imred.crutil
+.ih
+NAME
+crnebula -- create a cosmic ray mask from nebular images
+.ih
+USAGE	
+.nf
+crnebula input output
+.fi
+.ih
+PARAMETERS
+.ls input
+Input image in which cosmic rays are to be detected.
+.le
+.ls output
+Output image in which cosmic rays are to be replaced by the median.
+If no output image is given (specified as "") then no output image
+is created.
+.le
+.ls crmask = ""
+Output cosmic ray mask identifying the cosmic rays found.  The mask
+will have values of one for cosmic rays and zero for non-cosmic rays.
+If no output cosmic ray mask is given (specified as "") then no mask
+is created.
+.le
+.ls residual = ""
+Output residual image.  This is the input image minus the median filtered
+image divided by the estimated sigma at each pixel.  Thresholds in this
+image determine the cosmic rays detected.  If no image name is given then
+no output will be created.
+.le
+.ls rmedresid = ""
+Output image for the difference between the box median filter image and
+the ring median filtered image divided by the estimated sigma at each
+pixel.  If no image name is given then no output will be created.
+.le
+.ls var0 = 0., var1 = 0., var2 = 0.
+Variance coefficients for the variance model.  The variance model is
+
+.nf
+    variance = var0 + var1 * data + var2 * data^2
+.fi
+
+where data is the maximum of zero and median pixel value and the variance is in
+data numbers.  All the coefficients must be positive or zero.  If they are
+all zero then empirical data sigmas are estimated by a percentile method in
+boxes of size given by \fIncsig\fR and \fInlsig\fR.
+.le
+.ls sigmed = 3.
+Sigma clipping factor for the residual image.
+.le
+.ls sigdiff = 3.
+Sigma clipping factor for the residuals between the box median and ring median
+filtered images.
+.le
+.ls mbox = 5
+Box size, in pixels, for the box median filtering.
+.le
+.ls rin = 1.5, rout = 6.
+Inner and outer radii, in pixels, for the ring median filtering.
+.le
+.ls verbose = no
+Print some progress information?
+.le
+.ih
+DESCRIPTION
+This task uses a combination of box median filtering to detect cosmic rays
+and the difference between box and ring median filtering to identify
+regions of fine nebular structure which should not be treated as cosmic
+rays.  The output consists of some set of the input image with cosmic rays
+replaced by the median, a cosmic ray mask, the residual image used to
+detect the cosmic rays, and the residual image used to exclude cosmic rays
+in regions of nebular fine structure.  The cosmic ray mask may be used
+later with \fBcrgrow\fR and \fBcrfix\fR to grow and remove the cosmic rays
+from the data by interpolation rather than the median.
+
+The algorithm is as follows.  The input image is median filtered using a
+box of size given by \fImbox\fR.  The residual image between the unfiltered
+and filter data is computed.  The residuals are divided by the estimated
+sigma of the pixel.  Cosmic rays are those which are more than \fIsigmed\fR
+above zero in the residual image.  This residual image may be output if an
+output name is specified.  This part of the algorithm is identical to that
+of the task \fIcrmedian\fR and, in fact, that task is used.
+
+The median image not only enhances cosmic rays it also enhances narrow fine
+structure in the input image.  To avoid identifying this structure as
+cosmic rays a second filtered residual image is created which
+preferentially identifies this structure over the cosmic rays.  The input
+image is filtered using a ring median of specified inner and outer radius.
+The inner radius is slightly larger than the scale of the cosmic rays and
+the outer radius is comparable to the box size of the box median filter.  A
+ring filter replaces the center of the ring by the median of the ring.  The
+difference between the input and ring median filtered image divided by the
+estimated sigma will then be very similar to the box median residual image both
+where there are cosmic rays and where there is diffuse structure but will
+be different where there are linear fine structure patterns.  The
+difference between the median residual image and this ring median residual
+image highlights the regions of fine structure. If a image name is specified
+for the difference of the residual images it will be output.
+
+The difference of the median residual images is used to exclude any cosmic
+ray candidate pixels determined from sigma clipping the box median residual
+image which lie where the difference of the median residual images is
+greater than \fIsigdiff\fR different from zero (both positive or
+negative).
+
+To understand this algorithm it is recommended that the user save the
+residual and residual difference images and display them and blink against
+the original data.
+.ih
+EXAMPLES
+This example, the same as in \fBcrmedian\fR, illustrates using the
+\fBcrnebual\fR task to give a cosmic ray removed image and examining the
+results with an image display.  The image is a CCD image with a readout
+noise of 5 electrons and a gain of 3 electrons per data number.  This
+implies variance model coefficients of
+
+.nf
+    var0 = (5/3)^2 = 2.78
+    var1 = 1/3 = 0.34
+.fi
+
+.nf
+    cl> display obj001 1                  # Display in first frame
+    cl> # Determine output image, cosmic ray mask, and residual images
+    cl> crnebula obj001 crobj001 crmask=mask001 resid=res001\
+    >>> rmedresid=rmed001 var0=2.78 var1=0.34
+    cl> display crobj001 2                # Display final image
+    cl> display res001 3 zs- zr- z1=-5 z2=5  # Display residuals
+    cl> display rmed001 4 zs- zr- z1=-5 z2=5
+.fi
+
+By looking at the residual image the sigma clippig threshold can be
+adjusted and the noise parameters can be tweaked to minimize clipping
+of real extended structure.
+.ih
+SEE ALSO
+cosmicrays, crmedian, median, rmedian, crfix, crgrow
+.endhelp
diff --git a/noao/imred/crutil/doc/overview.hlp b/noao/imred/crutil/doc/overview.hlp
new file mode 100644
index 00000000..cb4dc3de
--- /dev/null
+++ b/noao/imred/crutil/doc/overview.hlp
@@ -0,0 +1,76 @@
+.help overview Apr98 noao.imred.crutil
+
+.ce
+\fBThe Cosmic Ray Package: CRUTIL\fR
+
+The cosmic ray package provides tools for identifying and removing cosmic
+rays in images.  The tasks are:
+
+.nf
+ cosmicrays - Remove cosmic rays using flux ratio algorithm
+  craverage - Detect CRs against average and avoid objects
+  crcombine - Combine multiple exposures to eliminate cosmic rays
+     credit - Interactively edit cosmic rays using an image display
+      crfix - Fix cosmic rays in images using cosmic ray masks
+     crgrow - Grow cosmic rays in cosmic ray masks
+   crmedian - Detect and replace cosmic rays with median filter
+   crnebula - Detect and replace cosmic rays in nebular data
+.fi
+
+The best way to remove cosmic rays is using multiple exposures of the same
+field.  When this is done the task \fBcrcombine\fR is used to combine the
+exposures into a final single image with cosmic rays removed.  The images
+are scaled (if necessary) to a common data level either by multiplicative
+scaling, an additive background offset, or some combination of both.
+Cosmic rays are then found as pixels which differ by some statistical
+amount away for the average or median of the data.
+
+A median is the simplest way to remove cosmic rays.  This is an option
+with \fBcrcombine\fR.  But this does not make optimal use of the data.
+An average of the pixels remaining after some rejection operation is better.
+If the noise characteristics of the data can be described by a gain and
+read noise then cosmic rays can be optimally rejected using the
+"crreject" algorithm.  This works on two or more images.  There are
+a number of other rejection algorithms which can be used as described in
+the task help.
+
+The rest of the tasks in the package are used when only a single exposure
+is available.  These include interactive editing with \fBcredit\fR.  The
+replacement algorithms in this task may also be used non-interactively if
+you have a list of pixel coordinates as input.  Other tasks automatically
+identifying pixels which are significantly higher than surrounding pixels.
+
+The simplest of these tasks is \fBcrmedian\fR.  This replaces
+cosmic rays with a median value and produces a cosmic ray
+mask which is a simple type of integer image where good pixels have a value
+of zero and bad pixels have a non-zero value.  The tasks \fBcrgrow\fR and
+\fBcrfix\fR are provided to use this type of cosmic ray mask.  The former
+will flag additional pixels within some radius of the flagged pixels in the
+mask.  The latter is the basic tool for replacing the identified pixels in
+the data by neighboring data.  It uses linear interpolation along lines or
+columns.  The median task is simple but it often will flag the cores of
+stars or other small but real features.
+
+The task \fBcraverage\fR is similar to \fBcrmedian\fR in that it compares
+the pixel values against a smoothed version.  Instead of a median it uses
+an average with the central pixel excluded.  It is more sophisticated
+in that it also compares the average against a larger median to see if
+the region corresponds to an object.  Thus it can detect objects and
+the task could be used as a simple object detection task in its own right.
+Because the hardest part of cosmic ray detection from a single image is
+avoiding truncation of the cores of stars this task does not allow cosmic
+rays to be detected where it thinks there is an object.  This task is
+also more versatile in allow separate mask values and works on a list
+of images.
+
+Somewhat more sophisticated algorithms are available in the tasks
+\fBcosmicrays\fR and \fBcrnebula\fR.  These attempt to determine if a
+deviant pixel is the core of a star or part of a linear nebular feature
+respectively.
+
+The best use of these tasks is to experiment and iterate.  In particular,
+one may want to iterate a task several times and use both \fBcosmicrays\fR
+and \fBcraverage\fR.
+
+Good hunting!
+.endhelp
diff --git a/noao/imred/crutil/mkpkg b/noao/imred/crutil/mkpkg
new file mode 100644
index 00000000..3a55a03a
--- /dev/null
+++ b/noao/imred/crutil/mkpkg
@@ -0,0 +1,8 @@
+# Make the package.
+
+$call	update@src
+$exit
+
+update:
+	$call update@src
+	;
diff --git a/noao/imred/crutil/src/Revisions b/noao/imred/crutil/src/Revisions
new file mode 100644
index 00000000..a5ef52f1
--- /dev/null
+++ b/noao/imred/crutil/src/Revisions
@@ -0,0 +1,151 @@
+.help revisions Nov99 crutil
+.nf
+t_cosmicrays.x
+    A pointer to a an array of pointers was used in one place as a real.  This
+    is an error when integer and real arrays are not of the same size; i.e.
+    on 64-bit architectures.  (8/2/12, Valdes)
+
+=======
+V2.16.1
+=======
+
+t_craverage.x
+    The pointer for the input mask buffer when using the same mask for both
+    input and output was not being read to include the edge lines which are
+    used during the computation resulting in a segmentation violation.
+    (11/24/04, Valdes)
+
+=======
+V2.12.2
+=======
+
+t_craverage.x
+    To grow an output mask create by the task requires closing the new mask
+    and reopening it READ_WRITE.  (10/23/02, Valdes)
+
+=======
+V2.12.1
+=======
+
+=====
+V2.12
+=====
+
+t_craverage.x
+t_crmedian.x
+    The mask name may be !<keyword>.  (3/22/02, Valdes)
+
+xtmaskname.x	+
+t_craverage.x
+t_crmedian.x
+t_crgrow.x
+mkpkg
+    Modified to allow FITS mask extensions.  (3/22/02, Valdes)
+    
+mkpkg
+    Added missing mkpkg depencies for several source files. (12/13/01, MJF)
+
+============================
+CRUTIL V1.5: August 22, 2001
+============================
+
+crcombine.cl
+crcombine.par
+../doc/crcombine.hlp
+    Modified to use new version of IMCOMBINE.  (8/22/01, Valdes)
+
+noao$imred/crutil/	+
+    Installed package into the NOAO.IMRED package.  (8/22/01, Valdes)
+
+t_craverage.x
+    The nrej features was done wrong for nrej of 1 or 2. (5/3/01, Valdes)
+
+t_craverage.x
+    1.  The amov and aclr calls were using the wrong buffer start.
+    2.  Added missing imtclose calls.
+    3.  The growing needed to be moved outside the block buffering.
+    (10/4/00, Valdes as diagnosed by Davis)
+
+t_craverage.x
+craverage.par
+../doc/craverage.hlp
+    Added an nrej parameter to excluded additional pixels from the average.
+    This is needed to deal with cosmic rays which are bigger than one
+    pixel or very nearby additional cosmic rays.  (9/13/00, Valdes)
+
+========================
+CRUTIL V1.4: Jan 6, 2000
+========================
+
+t_crmedian.x
+    The calculation of the sigma would reference uninitialized data if
+    the image size was not a multiple of the sigma block size.
+    (1/6/00, Valdes)
+
+t_craverage.x
+    The indexing of the pixels to use for the sigma calculation was wrong.
+    (1/6/00, Valdes)
+
+t_craverage.x	+
+craverage.par	+
+x_crutil.e
+mkpkg
+../crutil.cl
+../crutil.men
+../crutil.hd
+    New task that finds cosmic rays against an average excluding the candidate
+    pixel.  It also detects objects and prevents cosmic rays being detected
+    in them (i.e. the cores of stars).  (11/30/99, Valdes)
+
+t_crgrow.x
+crgrow.par
+    1.	Broke main grow loop into a subroutine that can be called by other
+	tasks.
+    2.  Added inval and outval parameters to allow selecting mask values.
+    (11/30/99, Valdes)
+
+========================
+CRUTIL V1.3: Oct 19, 1999
+========================
+
+crnebula.cl
+    The rin and rout parameters were not being used and instead
+    the default values were hardwired.  (10/19/99, Valdes)
+
+========================
+CRUTIL V1.2: Sep 4, 1998
+========================
+
+t_crmedian.x
+    On images with more than about 500K pixels the median operation is
+    done in overlapping blocks of lines.  The amount of overlap is
+    half of the line median size "lmed".  The bug is that on output
+    the overlap regions end up being zero.  The output i/o is now done
+    in non-overlapping blocks.  (9/4/98, Valdes)
+
+=====================
+CRUTIL V1.1: May 1998
+=====================
+
+crexamine.x
+cosmicrays.key	+
+cosmicrays.hlp
+    The graphical deletion and undeletion of candidates now includes the
+    keys 'e' and 'v' to delete and undelete from a marked rectangular
+    region.  Also the key file was moved to the source directory.
+    (Valdes/Shopbell 5/15/98)
+
+cosmicrays.par
+    Fixed type in "crmasks" parameter name.
+    (Valdes/Shopbell 5/15/98)
+
+===========
+CRUTIL V1.0
+===========
+    
+New package created April 24, 1998.
+
+=======
+V2.11.1
+=======
+.endhelp
diff --git a/noao/imred/crutil/src/cosmicrays.key b/noao/imred/crutil/src/cosmicrays.key
new file mode 100644
index 00000000..beac2835
--- /dev/null
+++ b/noao/imred/crutil/src/cosmicrays.key
@@ -0,0 +1,43 @@
+	   COSMIC RAY DETECTION AND REPLACEMENT
+
+   
+INTERACTIVE IMAGE CURSOR COMMANDS
+
+When using the image display cursor to define a list of training objects
+the following keystrokes may be given.
+
+?	Help
+c	Identify the object as a cosmic ray
+s	Identify the object as a star
+g	Switch to the graphics plot
+q	Quit and continue with the cleaning
+
+There are no colon commands.
+
+
+INTERACTIVE GRAPHICS CURSOR COMMANDS
+
+  The graph shows the ratio of the mean background subtracted flux within the
+detection window (excluding the candidate cosmic ray and the second brightest
+pixel) to the flux of the candidate cosmic ray pixel as a function of the
+mean flux.  Both coordinates have been multiplied by 100 so the ratio is in
+precent.  The peaks of extended objects have high flux ratios while true
+cosmic rays have low ratios.  The main purpose of this step is to set the
+flux ratio threshold for discriminating stars and galaxies.  The cursor
+keys are:
+
+?	Help
+a	Toggle between showing all objects and only the training objects
+d	Mark candidate for replacement (applys to '+' points)
+e	Mark candidates in a region for replacement (applys to '+' points)
+q	Quit.  Returns to training or to replace the selected pixels
+r	Redraw the graph
+s	Make a surface plot for the candidate nearest the cursor
+t	Set the flux ratio threshold at the y cursor position
+u	Mark candidate to not be replaced (applys to 'x' points)
+v	Mark candidates in a region to not be replaced (applys to 'x' points)
+w	Adjust the graph window (see GTOOLS)
+<space> Print the pixel coordinates for a candidate
+
+There are no colon commands except those for the windowing options (type
+:\help or see GTOOLS).
diff --git a/noao/imred/crutil/src/cosmicrays.par b/noao/imred/crutil/src/cosmicrays.par
new file mode 100644
index 00000000..9016d9f9
--- /dev/null
+++ b/noao/imred/crutil/src/cosmicrays.par
@@ -0,0 +1,17 @@
+input,s,a,,,,List of images in which to detect cosmic rays
+output,s,a,,,,List of cosmic ray replaced output images (optional)
+crmasks,s,h,"",,,"List of bad pixel masks (optional)
+"
+threshold,r,h,25.,,,Detection threshold above mean
+fluxratio,r,h,2.,,,Flux ratio threshold (in percent)
+npasses,i,h,5,1,,Number of detection passes
+window,s,h,"5","5|7",,"Size of detection window
+"
+interactive,b,h,yes,,,Examine parameters interactively?
+train,b,h,no,,,Use training objects?
+objects,*imcur,h,"",,,Cursor list of training objects
+savefile,f,h,"",,,File to save train objects
+plotfile,f,h,"",,,Plot file
+graphics,s,h,"stdgraph",,,Interactive graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+answer,s,q,,"no|yes|NO|YES",,Review parameters for a particular image?
diff --git a/noao/imred/crutil/src/craverage.par b/noao/imred/crutil/src/craverage.par
new file mode 100644
index 00000000..b67c4585
--- /dev/null
+++ b/noao/imred/crutil/src/craverage.par
@@ -0,0 +1,23 @@
+input,f,a,,,,List of input images
+output,f,a,,,,List of output images
+crmask,f,h,,,,List of output cosmic ray and object masks
+average,f,h,,,,List of output block average filtered images
+sigma,f,h,,,,"List of output sigma images
+"
+navg,i,h,5,3,,Block average box size
+nrej,i,h,0,0,,Number of high pixels to reject from the average
+nbkg,i,h,5,1,,Background annulus width
+nsig,i,h,25,10,,Box size for sigma calculation
+var0,r,h,0.,0.,,Variance coefficient for DN^0 term
+var1,r,h,0.,0.,,Variance coefficient for DN^1 term
+var2,r,h,0.,0.,,"Variance coefficient for DN^2 term
+"
+crval,i,h,1,0,,Mask value for cosmic rays
+lcrsig,r,h,10.,,,Low cosmic ray sigma outside object
+hcrsig,r,h,5.,,,High cosmic ray sigma outside object
+crgrow,r,h,0.,0.,,"Cosmic ray grow radius
+"
+objval,i,h,0,0,,Mask value for objects
+lobjsig,r,h,10.,,,Low object detection sigma
+hobjsig,r,h,5.,,,High object detection sigma
+objgrow,r,h,0.,0.,,Object grow radius
diff --git a/noao/imred/crutil/src/crcombine.cl b/noao/imred/crutil/src/crcombine.cl
new file mode 100644
index 00000000..7c6bdc77
--- /dev/null
+++ b/noao/imred/crutil/src/crcombine.cl
@@ -0,0 +1,17 @@
+# CRCOMBINE -- Reject cosmic rays by combining multiple exposures.
+
+procedure crcombine (input, output)
+
+begin
+	imcombine (input, output, logfile=logfile, combine=combine,
+	    reject=reject, scale=scale, zero=zero, statsec=statsec,
+	    lsigma=lsigma, hsigma=hsigma, rdnoise=rdnoise, gain=gain,
+	    grow=grow, headers=headers, bpmasks=bpmasks, rejmasks=rejmasks,
+	    nrejmasks=nrejmasks, expmasks=expmasks, sigmas=sigmas,
+	    project=project, outtype=outtype, outlimits=outlimits,
+	    offsets=offsets, masktype=masktype, maskvalue=maskvalue,
+	    blank=blank, weight=weight, expname=expname,
+	    lthreshold=lthreshold, hthreshold=hthreshold, nlow=nlow,
+	    nhigh=nhigh, nkeep=nkeep, mclip=mclip, snoise=snoise,
+	    sigscale=sigscale, pclip=pclip)
+end
diff --git a/noao/imred/crutil/src/crcombine.par b/noao/imred/crutil/src/crcombine.par
new file mode 100644
index 00000000..95ae95ae
--- /dev/null
+++ b/noao/imred/crutil/src/crcombine.par
@@ -0,0 +1,45 @@
+# CRCOMBINE -- Image combine parameters
+
+input,s,a,,,,List of images to combine
+output,s,a,,,,List of output images
+logfile,s,h,"STDOUT",,,"Log file
+
+# Cosmic ray rejection parameters"
+combine,s,h,"average","average|median|sum",,Type of combine operation
+reject,s,h,"crreject","none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip",,Type of rejection
+scale,s,h,"mode",,,Image scaling
+zero,s,h,"none",,,Image zero point offset
+statsec,s,h,"",,,Image section for computing statistics
+lsigma,r,h,10.,0.,,Lower sigma clipping factor
+hsigma,r,h,3.,0.,,Upper sigma clipping factor
+rdnoise,s,h,"0.",,,CCD readout noise (electrons)
+gain,s,h,"1.",,,CCD gain (electrons/DN)
+grow,r,h,0.,0.,,"Radius (pixels) for neighbor rejection
+
+# Additional output"
+headers,s,h,"",,,List of header files (optional)
+bpmasks,s,h,"",,,List of bad pixel masks (optional)
+rejmasks,s,h,"",,,List of rejection masks (optional)
+nrejmasks,s,h,"",,,List of number rejected masks (optional)
+expmasks,s,h,"",,,List of exposure masks (optional)
+sigmas,s,h,"",,,"List of sigma images (optional)
+
+# Additional parameters"
+project,b,h,no,,,Project highest dimension of input images?
+outtype,s,h,"real","short|ushort|integer|long|real|double",,Output image pixel datatype
+outlimits,s,h,"",,,Output limits (x1 x2 y1 y2 ...)
+offsets,f,h,"none",,,Input image offsets
+masktype,s,h,"none","none|goodvalue|badvalue|goodbits|badbits",,Mask type
+maskvalue,r,h,0,,,Mask value
+blank,r,h,0.,,,Value if there are no pixels
+weight,s,h,"none",,,Image weights
+expname,s,h,"",,,Image header exposure time keyword
+lthreshold,r,h,INDEF,,,Lower threshold
+hthreshold,r,h,INDEF,,,Upper threshold
+nlow,i,h,1,0,,minmax: Number of low pixels to reject
+nhigh,i,h,1,0,,minmax: Number of high pixels to reject
+nkeep,i,h,1,,,Minimum to keep (pos) or maximum to reject (neg)
+mclip,b,h,yes,,,Use median in sigma clipping algorithms?
+snoise,s,h,"0.",,,Sensitivity noise (fraction)
+sigscale,r,h,0.1,0.,,Tolerance for sigma clipping scaling corrections
+pclip,r,h,-0.5,,,pclip: Percentile clipping parameter
diff --git a/noao/imred/crutil/src/credit.cl b/noao/imred/crutil/src/credit.cl
new file mode 100644
index 00000000..8b844f33
--- /dev/null
+++ b/noao/imred/crutil/src/credit.cl
@@ -0,0 +1,13 @@
+# CREDIT -- Edit cosmic rays with an image display.
+
+procedure credit (input, output)
+
+begin
+	imedit (input, output, cursor=cursor, logfile=logfile,
+	    display=display, autodisplay=autodisplay,
+	    autosurface=autosurface, aperture=aperture, radius=radius,
+	    search=search, buffer=buffer, width=width, xorder=xorder,
+	    yorder=yorder, value=value, sigma=sigma, angh=angh, angv=angv,
+	    command=command, graphics=graphics, default=default,
+	    fixpix=fixpix)
+end
diff --git a/noao/imred/crutil/src/credit.par b/noao/imred/crutil/src/credit.par
new file mode 100644
index 00000000..a23e0d35
--- /dev/null
+++ b/noao/imred/crutil/src/credit.par
@@ -0,0 +1,22 @@
+input,s,a,,,,Images to be edited
+output,s,a,,,,Output images
+cursor,*imcur,h,"",,,Cursor input
+logfile,s,h,"",,,Logfile for record of cursor commands
+display,b,h,yes,,,Display images?
+autodisplay,b,h,yes,,,Automatic image display?
+autosurface,b,h,no,,,Automatic surface plots?
+aperture,s,h,"circular","|circular|square|",,Aperture type
+radius,r,h,2.,,,Substitution radius
+search,r,h,2.,,,Search radius
+buffer,r,h,1.,0.,,Background buffer width
+width,r,h,2.,1.,,Background width
+xorder,i,h,2,0,,Background x order
+yorder,i,h,2,0,,Background y order
+value,r,h,0.,,,Constant value substitution
+sigma,r,h,INDEF,,,Added noise sigma
+angh,r,h, -33.,,,Horizontal viewing angle (degrees)
+angv,r,h,25.,,,Vertical viewing angle (degrees)
+command,s,h,"display $image 1 erase=$erase fill=yes order=0 >& dev$null",,,Display command
+graphics,s,h,"stdgraph",,,Graphics device
+default,s,h,"b",,,Default option for x-y input
+fixpix,b,h,no,,,Fixpix style input?
diff --git a/noao/imred/crutil/src/crexamine.x b/noao/imred/crutil/src/crexamine.x
new file mode 100644
index 00000000..14e8d589
--- /dev/null
+++ b/noao/imred/crutil/src/crexamine.x
@@ -0,0 +1,626 @@
+include	<error.h>
+include	<syserr.h>
+include <imhdr.h>
+include	<gset.h>
+include	<mach.h>
+include	<pkg/gtools.h>
+include	"crlist.h"
+
+# CR_EXAMINE  -- Examine cosmic ray candidates interactively.
+# CR_GRAPH    -- Make a graph
+# CR_NEAREST  -- Find the nearest cosmic ray to the cursor.
+# CR_DELETE   -- Set replace flag for cosmic ray candidate nearest cursor.
+# CR_UNDELETE -- Set no replace flag for cosmic ray candidate nearest cursor.
+# CR_UPDATE   -- Change replacement flags, thresholds, and graphs.
+# CR_PLOT     -- Make log plot
+
+define	HELP	"crutil$src/cosmicrays.key"
+define	PROMPT	"cosmic ray options"
+
+# CR_EXAMINE -- Examine cosmic ray candidates interactively.
+
+procedure cr_examine (cr, gp, gt, im, fluxratio, first)
+
+pointer	cr			# Cosmic ray list
+pointer	gp			# GIO pointer
+pointer	gt			# GTOOLS pointer
+pointer	im			# Image pointer
+real	fluxratio		# Flux ratio threshold
+int	first			# Initial key
+
+char	cmd[SZ_LINE]
+int	i, newgraph, wcs, key, nc, nl, c1, c2, l1, l2, show
+real	wx, wy, x1, y1, x2, y2
+pointer	data
+
+int	clgcur()
+pointer	imgs2r()
+
+begin
+	# Set up the graphics.
+	call gt_sets (gt, GTPARAMS, IM_TITLE(im))
+
+	# Set image limits
+	nc = IM_LEN(im, 1)
+	nl = IM_LEN(im, 2)
+
+	# Enter cursor loop.
+	key = first
+	repeat {
+	    switch (key) {
+	    case '?': # Print help text.
+		call gpagefile (gp, HELP, PROMPT)
+	    case ':': # Colon commands.
+		switch (cmd[1]) {
+		case '/':
+		    call gt_colon (cmd, gp, gt, newgraph)
+		default:
+		    call printf ("\007")
+		}
+	    case 'a': # Toggle show all
+		if (show == 0)
+		    show = 1
+		else
+		    show = 0
+		newgraph = YES
+	    case 'd': # Delete candidate
+		call cr_delete (gp, wx, wy, cr, i, show)
+	    case 'e': # Delete candidates in region
+                x1 = wx; y1 = wy
+                call printf ("again:")
+                if (clgcur ("cursor", x2, y2, wcs, key, cmd, SZ_LINE) == EOF)
+                    return
+		call cr_delete_reg (gp, x1, y1, x2, y2, cr, show)
+	    case 'q': # Quit
+		break
+	    case 'r': # Redraw the graph.
+		newgraph = YES
+	    case 's': # Make surface plots
+		call cr_nearest (gp, wx, wy, cr, i, show)
+		c1 = max (1, int (Memr[CR_COL(cr)+i-1]) - 5)
+		c2 = min (nc, int (Memr[CR_COL(cr)+i-1]) + 5)
+		l1 = max (1, int (Memr[CR_LINE(cr)+i-1]) - 5)
+		l2 = min (nl, int (Memr[CR_LINE(cr)+i-1]) + 5)
+		data = imgs2r (im, c1, c2, l1, l2)
+		call gclear (gp)
+		call gsview (gp, 0.03, 0.48, 0.53, 0.98)
+		call cr_surface (gp, Memr[data], c2-c1+1, l2-l1+1, -33., 25.)
+		call gsview (gp, 0.53, 0.98, 0.53, 0.98)
+		call cr_surface (gp, Memr[data], c2-c1+1, l2-l1+1, -123., 25.)
+		call gsview (gp, 0.03, 0.48, 0.03, 0.48)
+		call cr_surface (gp, Memr[data], c2-c1+1, l2-l1+1, 57., 25.)
+		call gsview (gp, 0.53, 0.98, 0.03, 0.48)
+		call cr_surface (gp, Memr[data], c2-c1+1, l2-l1+1, 147., 25.)
+		call fprintf (STDERR, "[Type any key to continue]")
+		i = clgcur ("cursor", wx, wy, wcs, key, cmd, SZ_LINE)
+		newgraph = YES
+	    case 't': # Set threshold
+		call cr_update (gp, wy, cr, fluxratio, show)
+		call clputr ("fluxratio", fluxratio)
+	    case 'u': # Undelete candidate
+		call cr_undelete (gp, wx, wy, cr, i, show)
+	    case 'v': # Undelete candidates in region
+                x1 = wx; y1 = wy
+                call printf ("again:")
+                if (clgcur ("cursor", x2, y2, wcs, key, cmd, SZ_LINE) == EOF)
+                    return
+		call cr_undelete_reg (gp, x1, y1, x2, y2, cr, show)
+	    case 'w':# Window the graph.
+		call gt_window (gt, gp, "cursor", newgraph)
+	    case ' ': # Print info
+		call cr_nearest (gp, wx, wy, cr, i, show)
+		call printf ("%d %d\n")
+		    call pargr (Memr[CR_COL(cr)+i-1])
+		    call pargr (Memr[CR_LINE(cr)+i-1])
+	    case 'z': # NOP
+		newgraph = NO
+	    default: # Ring bell for unrecognized commands.
+		call printf ("\007")
+	    }
+
+	    # Update the graph if needed.
+	    if (newgraph == YES) {
+		call cr_graph (gp, gt, cr, fluxratio, show)
+	        newgraph = NO
+	    }
+	} until (clgcur ("cursor", wx, wy, wcs, key, cmd, SZ_LINE) == EOF)
+end
+
+
+# CR_GRAPH -- Make a graph
+
+procedure cr_graph (gp, gt, cr, fluxratio, show)
+
+pointer	gp		# GIO pointer
+pointer	gt		# GTOOLS pointers
+pointer	cr		# Cosmic ray list
+real	fluxratio	# Flux ratio threshold
+int	show		# Show (0=all, 1=train)
+
+int	i, ncr
+real	x1, x2, y1, y2
+pointer	sp, x, y, w, flag, index
+
+begin
+	call smark (sp)
+
+	call cr_show (show, cr, x, y, w, flag, index, ncr)
+	if (ncr == 0) {
+	    call sfree (sp)
+	    return
+	}
+
+	call gclear (gp)
+	call gt_ascale (gp, gt, Memr[x+1], Memr[y+1], ncr)
+	call gt_swind (gp, gt)
+	call gt_labax (gp, gt)
+
+	do i = 1, ncr {
+	    if ((Memi[flag+i] == NO) || (Memi[flag+i] == ALWAYSNO))
+		call gmark (gp, Memr[x+i], Memr[y+i], GM_PLUS, 2., 2.)
+	    else
+		call gmark (gp, Memr[x+i], Memr[y+i], GM_CROSS, 2., 2.)
+	    if (Memr[w+i] != 0.)
+		call gmark (gp, Memr[x+i], Memr[y+i], GM_BOX, 2., 2.)
+	}
+
+	call ggwind (gp, x1, x2, y1, y2)
+	call gseti (gp, G_PLTYPE, 2)
+	call gline (gp, x1, fluxratio, x2, fluxratio)
+
+	call sfree (sp)
+end
+
+
+# CR_NEAREST -- Find the nearest cosmic ray to the cursor.
+
+procedure cr_nearest (gp, wx, wy, cr, nearest, show)
+
+pointer	gp		# GIO pointer
+real	wx, wy		# Cursor position
+pointer	cr		# Cosmic ray list
+int	nearest		# Index of nearest point (returned)
+int	show		# Show (0=all, 1=train)
+
+int	i, ncr
+real	x0, y0, x1, y1, x2, y2, r2, r2min
+pointer	sp, x, y, w, flag, index
+
+begin
+	call smark (sp)
+
+	call cr_show (show, cr, x, y, w, flag, index, ncr)
+	if (ncr == 0) {
+	    call sfree (sp)
+	    return
+	}
+
+	# Search for nearest point in NDC.
+	r2min = MAX_REAL
+	call gctran (gp, wx, wy, wx, wy, 1, 0)
+	do i = 1, ncr {
+	    x1 = Memr[x+i]
+	    y1 = Memr[y+i]
+	    call gctran (gp, x1, y1, x0, y0, 1, 0)
+	    r2 = (x0 - wx) ** 2 + (y0 - wy) ** 2
+	    if (r2 < r2min) {
+		r2min = r2
+		x2 = x1
+		y2 = y1
+		nearest = i
+	    }
+	}
+	if (index != NULL)
+	    nearest = Memi[index+nearest]
+
+	# Move the cursor to the selected point.
+	call gscur (gp, x2, y2)
+
+	call sfree (sp)
+end
+
+
+# CR_DELETE -- Set replace flag for cosmic ray candidate nearest cursor.
+
+procedure cr_delete (gp, wx, wy, cr, nearest, show)
+
+pointer	gp		# GIO pointer
+real	wx, wy		# Cursor position
+pointer	cr		# Cosmic ray list
+int	nearest		# Index of nearest point (returned)
+int	show		# Show (0=all, 1=train)
+
+int	i, ncr
+real	x0, y0, x1, y1, x2, y2, r2, r2min
+pointer	sp, x, y, w, flag, index
+
+begin
+	call smark (sp)
+
+	call cr_show (show, cr, x, y, w, flag, index, ncr)
+	if (ncr == 0) {
+	    call sfree (sp)
+	    return
+	}
+
+	# Search for nearest point in NDC.
+	nearest = 0
+	r2min = MAX_REAL
+	call gctran (gp, wx, wy, wx, wy, 1, 0)
+	do i = 1, ncr {
+	    if ((Memi[flag+i] == YES) || (Memi[flag+i] == ALWAYSYES))
+		next
+	    x1 = Memr[x+i]
+	    y1 = Memr[y+i]
+	    call gctran (gp, x1, y1, x0, y0, 1, 0)
+	    r2 = (x0 - wx) ** 2 + (y0 - wy) ** 2
+	    if (r2 < r2min) {
+		r2min = r2
+		x2 = x1
+		y2 = y1
+		nearest = i
+	    }
+	}
+
+	# Move the cursor to the selected point and mark the deleted point.
+	if (nearest > 0) {
+	    if (index != NULL)
+		nearest = Memi[index+nearest]
+	    Memi[CR_FLAG(cr)+nearest-1] = ALWAYSYES
+	    Memi[CR_WT(cr)+nearest-1] = -1
+	    call gscur (gp, x2, y2)
+	    call gseti (gp, G_PMLTYPE, 0)
+	    y2 = Memr[CR_RATIO(cr)+nearest-1]
+	    call gmark (gp, x2, y2, GM_PLUS, 2., 2.)
+	    call gseti (gp, G_PMLTYPE, 1)
+	    call gmark (gp, x2, y2, GM_CROSS, 2., 2.)
+	}
+
+	call sfree (sp)
+end
+
+
+# CR_DELETE_REG -- Set replace flag for cosmic ray candidates in a region.
+
+procedure cr_delete_reg (gp, wx1, wy1, wx2, wy2, cr, show)
+
+pointer	gp			# GIO pointer
+real	wx1, wy1, wx2, wy2	# Cursor positions
+pointer	cr			# Cosmic ray list
+int	show			# Show (0=all, 1=train)
+
+int	i, j, ncr
+real	x0, y0, x1, y1
+pointer	sp, x, y, w, flag, index
+
+begin
+	call smark (sp)
+
+	call cr_show (show, cr, x, y, w, flag, index, ncr)
+	if (ncr == 0) {
+	    call sfree (sp)
+	    return
+	}
+
+	# Check order of region points.
+	if (wx1 > wx2) {
+	    x0 = wx1
+	    wx1 = wx2
+	    wx2 = x0
+	}
+	if (wy1 > wy2) {
+	    y0 = wy1
+	    wy1 = wy2
+	    wy2 = y0
+	}
+
+	# Check if point in region.
+	call gctran (gp, wx1, wy1, wx1, wy1, 1, 0)
+	call gctran (gp, wx2, wy2, wx2, wy2, 1, 0)
+	do i = 1, ncr {
+	    if ((Memi[flag+i] == YES) || (Memi[flag+i] == ALWAYSYES))
+		next
+	    x1 = Memr[x+i]
+	    y1 = Memr[y+i]
+	    call gctran (gp, x1, y1, x0, y0, 1, 0)
+
+	    # Mark the deleted points.
+	    if ((x0 > wx1) && (x0 < wx2) && (y0 > wy1) && (y0 < wy2)) {
+		if (index != NULL)
+		    j = Memi[index+i]
+		else
+		    j = i
+		Memi[CR_FLAG(cr)+j-1] = ALWAYSYES
+		Memi[CR_WT(cr)+j-1] = -1
+		call gscur (gp, x1, y1)
+		call gseti (gp, G_PMLTYPE, 0)
+		y1 = Memr[CR_RATIO(cr)+j-1]
+		call gmark (gp, x1, y1, GM_PLUS, 2., 2.)
+		call gseti (gp, G_PMLTYPE, 1)
+		call gmark (gp, x1, y1, GM_CROSS, 2., 2.)
+	    }
+	}
+	call sfree (sp)
+end
+
+
+# CR_UNDELETE -- Set no replace flag for cosmic ray candidate nearest cursor.
+
+procedure cr_undelete (gp, wx, wy, cr, nearest, show)
+
+pointer	gp		# GIO pointer
+real	wx, wy		# Cursor position
+pointer	cr		# Cosmic ray list
+int	nearest		# Index of nearest point (returned)
+int	show		# Show (0=all, 1=train)
+
+int	i, ncr
+real	x0, y0, x1, y1, x2, y2, r2, r2min
+pointer	sp, x, y, w, flag, index
+
+begin
+	call smark (sp)
+
+	call cr_show (show, cr, x, y, w, flag, index, ncr)
+	if (ncr == 0) {
+	    call sfree (sp)
+	    return
+	}
+
+	# Search for nearest point in NDC.
+	nearest = 0
+	r2min = MAX_REAL
+	call gctran (gp, wx, wy, wx, wy, 1, 0)
+	do i = 1, ncr {
+	    if ((Memi[flag+i] == NO) || (Memi[flag+i] == ALWAYSNO))
+		next
+	    x1 = Memr[x+i]
+	    y1 = Memr[y+i]
+	    call gctran (gp, x1, y1, x0, y0, 1, 0)
+	    r2 = (x0 - wx) ** 2 + (y0 - wy) ** 2
+	    if (r2 < r2min) {
+		r2min = r2
+		x2 = x1
+		y2 = y1
+		nearest = i
+	    }
+	}
+
+	# Move the cursor to the selected point and mark the delete point.
+	if (nearest > 0) {
+	    if (index != NULL)
+		nearest = Memi[index+nearest]
+	    Memi[CR_FLAG(cr)+nearest-1] = ALWAYSNO
+	    Memi[CR_WT(cr)+nearest-1] = 1
+	    call gscur (gp, x2, y2)
+
+	    call gseti (gp, G_PMLTYPE, 0)
+	    y2 = Memr[CR_RATIO(cr)+nearest-1]
+	    call gmark (gp, x2, y2, GM_CROSS, 2., 2.)
+	    call gseti (gp, G_PMLTYPE, 1)
+	    call gmark (gp, x2, y2, GM_PLUS, 2., 2.)
+	}
+
+	call sfree (sp)
+end
+
+
+# CR_UNDELETE_REG -- Set no replace flag for cosmic ray candidates in a region.
+
+procedure cr_undelete_reg (gp, wx1, wy1, wx2, wy2, cr, show)
+
+pointer	gp			# GIO pointer
+real	wx1, wy1, wx2, wy2	# Cursor positions
+pointer	cr			# Cosmic ray list
+int	show			# Show (0=all, 1=train)
+
+int	i, j, ncr
+real	x0, y0, x1, y1
+pointer	sp, x, y, w, flag, index
+
+begin
+	call smark (sp)
+
+	call cr_show (show, cr, x, y, w, flag, index, ncr)
+	if (ncr == 0) {
+	    call sfree (sp)
+	    return
+	}
+
+	# Check order of region points.
+	if (wx1 > wx2) {
+	    x0 = wx1
+	    wx1 = wx2
+	    wx2 = x0
+	}
+	if (wy1 > wy2) {
+	    y0 = wy1
+	    wy1 = wy2
+	    wy2 = y0
+	}
+
+	# Check if point in region.
+	call gctran (gp, wx1, wy1, wx1, wy1, 1, 0)
+	call gctran (gp, wx2, wy2, wx2, wy2, 1, 0)
+	do i = 1, ncr {
+	    if ((Memi[flag+i] == NO) || (Memi[flag+i] == ALWAYSNO))
+		next
+	    x1 = Memr[x+i]
+	    y1 = Memr[y+i]
+	    call gctran (gp, x1, y1, x0, y0, 1, 0)
+
+	    # Mark the deleted points.
+	    if ((x0 > wx1) && (x0 < wx2) && (y0 > wy1) && (y0 < wy2)) {
+		if (index != NULL)
+		    j = Memi[index+i]
+		else
+		    j = i
+		Memi[CR_FLAG(cr)+j-1] = ALWAYSNO
+		Memi[CR_WT(cr)+j-1] = 1
+		call gscur (gp, x1, y1)
+		call gseti (gp, G_PMLTYPE, 0)
+		y1 = Memr[CR_RATIO(cr)+j-1]
+		call gmark (gp, x1, y1, GM_CROSS, 2., 2.)
+		call gseti (gp, G_PMLTYPE, 1)
+		call gmark (gp, x1, y1, GM_PLUS, 2., 2.)
+	    }
+	}
+	call sfree (sp)
+end
+
+
+# CR_UPDATE -- Change replacement flags, thresholds, and graphs.
+
+procedure cr_update (gp, wy, cr, fluxratio, show)
+
+pointer	gp		# GIO pointer
+real	wy		# Y cursor position
+pointer	cr		# Cosmic ray list
+real	fluxratio	# Flux ratio threshold
+int	show		# Show (0=all, 1=train)
+
+int	i, ncr, flag
+real	x1, x2, y1, y2
+pointer	x, y, f
+
+begin
+	call gseti (gp, G_PLTYPE, 0)
+	call ggwind (gp, x1, x2, y1, y2)
+	call gline (gp, x1, fluxratio, x2, fluxratio)
+	fluxratio = wy
+	call gseti (gp, G_PLTYPE, 2)
+	call gline (gp, x1, fluxratio, x2, fluxratio)
+
+	if (show == 1)
+	    return
+
+	ncr = CR_NCR(cr)
+	x = CR_FLUX(cr) - 1
+	y = CR_RATIO(cr) - 1
+	f = CR_FLAG(cr) - 1
+
+	do i = 1, ncr {
+	    flag = Memi[f+i]
+	    if ((flag == ALWAYSYES) || (flag == ALWAYSNO))
+		next
+	    x1 = Memr[x+i]
+	    y1 = Memr[y+i]
+	    if (flag == NO) {
+	        if (y1 < fluxratio) {
+		    Memi[f+i] = YES
+		    call gseti (gp, G_PMLTYPE, 0)
+		    call gmark (gp, x1, y1, GM_PLUS, 2., 2.)
+		    call gseti (gp, G_PMLTYPE, 1)
+		    call gmark (gp, x1, y1, GM_CROSS, 2., 2.)
+		}
+	    } else {
+	        if (y1 >= fluxratio) {
+		    Memi[f+i] = NO
+		    call gseti (gp, G_PMLTYPE, 0)
+		    call gmark (gp, x1, y1, GM_CROSS, 2., 2.)
+		    call gseti (gp, G_PMLTYPE, 1)
+		    call gmark (gp, x1, y1, GM_PLUS, 2., 2.)
+		}
+	    }
+	}
+end
+
+
+# CR_PLOT -- Make log plot
+
+procedure cr_plot (cr, im, fluxratio)
+
+pointer	cr			# Cosmic ray list
+pointer	im			# Image pointer
+real	fluxratio		# Flux ratio threshold
+
+int	fd, open(), errcode()
+pointer	sp, fname, gp, gt, gopen(), gt_init()
+errchk	gopen
+
+begin
+	call smark (sp)
+	call salloc (fname, SZ_FNAME, TY_CHAR)
+
+	# Open the plotfile.
+	call clgstr ("plotfile", Memc[fname], SZ_FNAME)
+	iferr (fd = open (Memc[fname], APPEND, BINARY_FILE)) {
+	    if (errcode() != SYS_FNOFNAME)
+		call erract (EA_WARN)
+	    return
+	}
+
+	# Set up the graphics.
+	gp = gopen ("stdplot", NEW_FILE, fd)
+	gt = gt_init()
+	call gt_sets (gt, GTTYPE, "mark")
+	call gt_sets (gt, GTXTRAN, "log")
+	call gt_setr (gt, GTXMIN, 10.)
+	call gt_setr (gt, GTYMIN, 0.)
+	call gt_sets (gt, GTTITLE, "Parameters of cosmic rays candidates")
+	call gt_sets (gt, GTPARAMS, IM_TITLE(im))
+	call gt_sets (gt, GTXLABEL, "Flux")
+	call gt_sets (gt, GTYLABEL, "Flux Ratio")
+
+	call cr_graph (gp, gt, cr, fluxratio, 'r')
+
+	call gt_free (gt)
+	call gclose (gp)
+	call close (fd)
+	call sfree (sp)
+end
+
+
+# CR_SHOW -- Select data to show.
+# This returns pointers to the data.  Note the pointers are salloc from
+# the last smark which is done by the calling program.
+
+procedure cr_show (show, cr, x, y, w, flag, index, ncr)
+
+int	show		#I Data to show (0=all, 1=train)
+pointer	cr		#I CR data
+pointer	x		#O Fluxes
+pointer	y		#O Ratios
+pointer	w		#O Weights
+pointer	flag		#O Flags
+pointer	index		#O Index into CR data (if not null)
+int	ncr		#O Number of selected data points
+
+int	i
+
+begin
+	switch (show) {
+	case 0:
+	    ncr = CR_NCR(cr)
+	    x = CR_FLUX(cr) - 1
+	    y = CR_RATIO(cr) - 1
+	    w = CR_WT(cr) - 1
+	    flag = CR_FLAG(cr) - 1
+	    index = NULL
+	case 1:
+	    ncr = CR_NCR(cr)
+	    call salloc (x, ncr, TY_REAL)
+	    call salloc (y, ncr, TY_REAL)
+	    call salloc (w, ncr, TY_REAL)
+	    call salloc (flag, ncr, TY_INT)
+	    call salloc (index, ncr, TY_INT)
+
+	    ncr = 0
+	    x = x - 1
+	    y = y - 1
+	    w = w - 1
+	    flag = flag - 1
+	    index = index - 1
+
+	    do i = 1, CR_NCR(cr) {
+		if (Memr[CR_WT(cr)+i-1] == 0.)
+		    next
+		ncr = ncr + 1
+		Memr[x+ncr] = Memr[CR_FLUX(cr)+i-1]
+		Memr[y+ncr] = Memr[CR_RATIO(cr)+i-1]
+		Memr[w+ncr] = Memr[CR_WT(cr)+i-1]
+		Memi[flag+ncr] = Memi[CR_FLAG(cr)+i-1]
+		Memi[index+ncr] = i
+	    }
+	}
+end
diff --git a/noao/imred/crutil/src/crfind.x b/noao/imred/crutil/src/crfind.x
new file mode 100644
index 00000000..58850940
--- /dev/null
+++ b/noao/imred/crutil/src/crfind.x
@@ -0,0 +1,305 @@
+include	<math/gsurfit.h>
+
+# CR_FIND -- Find cosmic ray candidates.
+# This procedure is an interface to special procedures specific to a given
+# window size.
+
+procedure cr_find (cr, threshold, data, nc, nl, col, line,
+    sf1, sf2, x, y, z, w)
+
+pointer	cr						# Cosmic ray list
+real	threshold					# Detection threshold
+pointer	data[ARB]					# Data lines
+int	nc						# Number of columns
+int	nl						# Number of lines
+int	col						# First column
+int	line						# Center line
+pointer	sf1, sf2					# Surface fitting
+real	x[ARB], y[ARB], z[ARB], w[ARB]			# Surface arrays
+
+pointer	a, b, c, d, e, f, g
+
+begin
+	switch (nl) {
+	case 5:
+	    a = data[1]
+	    b = data[2]
+	    c = data[3]
+	    d = data[4]
+	    e = data[5]
+	    call cr_find5 (cr, threshold,  col, line, Memr[a], Memr[b],
+		Memr[c], Memr[d], Memr[e], nc, sf1, sf2, x, y, z, w)
+	case 7:
+	    a = data[1]
+	    b = data[2]
+	    c = data[3]
+	    d = data[4]
+	    e = data[5]
+	    f = data[6]
+	    g = data[7]
+	    call cr_find7 (cr, threshold,  col, line, Memr[a], Memr[b],
+		Memr[c], Memr[d], Memr[e], Memr[f], Memr[g], nc,
+		sf1, sf2, x, y, z, w)
+	}
+end
+
+
+# CR_FIND7 -- Find cosmic rays candidates in 7x7 window.
+# This routine finds cosmic rays candidates with the following algorithm.
+#    1. If the pixel is not a local maximum relative to it's 48 neighbors
+#	go on to the next pixel.
+#    2. Identify the next strongest pixel in the 7x7 region.
+#	This suspect pixel is excluded in the following.
+#    2. Compute the flux of the 7x7 region excluding the cosmic ray
+#	candidate and the suspect pixel.
+#    3. The candidate must exceed the average flux per pixel by a specified
+#	threshold.  If not go on to the next pixel.
+#    4. Fit a plane to the border pixels (excluding the suspect pixel).
+#    5. Subtract the background defined by the plane.
+#    6. Determine a replacement value as the average of the four adjacent
+#	pixels (excluding the suspect pixels).
+#    7. Add the pixel to the cosmic ray candidate list.
+
+procedure cr_find7 (cr, threshold, col, line, a, b, c, d, e, f, g, n,
+	sf1, sf2, x, y, z, w)
+
+pointer	cr						# Cosmic ray list
+real	threshold					# Detection threshold
+int	col						# First column
+int	line						# Line
+real	a[ARB], b[ARB], c[ARB], d[ARB]			# Image lines
+real	e[ARB], f[ARB], g[ARB]				# Image lines
+int	n						# Number of columns
+pointer	sf1, sf2					# Surface fitting
+real	x[49], y[49], z[49], w[49]			# Surface arrays
+
+real	bkgd[49] 
+int	i1, i2, i3, i4, i5, i6, i7, j, j1, j2
+real	p, flux, replace, asumr()
+pointer	sf
+
+begin
+	for (i4=4; i4<=n-3; i4=i4+1) {
+	    # Must be local maxima.
+	    p = d[i4]
+	    if (p<a[i4]||p<b[i4]||p<c[i4]||p<e[i4]||p<f[i4]||p<g[i4])
+		next
+	    i1 = i4 - 3
+	    if (p<a[i1]||p<b[i1]||p<c[i1]||p<d[i1]||p<e[i1]||p<f[i1]||p<g[i1])
+		next
+	    i2 = i4 - 2
+	    if (p<a[i2]||p<b[i2]||p<c[i2]||p<d[i2]||p<e[i2]||p<f[i2]||p<g[i2])
+		next
+	    i3 = i4 - 1
+	    if (p<a[i3]||p<b[i3]||p<c[i3]||p<d[i3]||p<e[i3]||p<f[i3]||p<g[i3])
+		next
+	    i5 = i4 + 1
+	    if (p<a[i5]||p<b[i5]||p<c[i5]||p<d[i5]||p<e[i5]||p<f[i5]||p<g[i5])
+		next
+	    i6 = i4 + 2
+	    if (p<a[i6]||p<b[i6]||p<c[i6]||p<d[i6]||p<e[i6]||p<f[i6]||p<g[i6])
+		next
+	    i7 = i4 + 3
+	    if (p<a[i7]||p<b[i7]||p<c[i7]||p<d[i7]||p<e[i7]||p<f[i7]||p<g[i7])
+		next
+
+	    # Convert to a single array in surface fitting order. 
+	    call amovr (a[i1], z[1], 7)
+	    z[8] = b[i7]; z[9] = c[i7]; z[10] = d[i7]; z[11] = e[i7]
+	    z[12] = f[i7]; z[13] = g[i7]; z[14] = g[i6]; z[15] = g[i5]
+	    z[16] = f[i4]; z[17] = g[i3]; z[18] = g[i2]; z[19] = g[i1]
+	    z[20] = f[i1]; z[21] = e[i1]; z[22] = d[i1]; z[23] = c[i1]
+	    z[24] = b[i1]
+	    call amovr (b[i2], z[25], 5)
+	    call amovr (c[i2], z[30], 5)
+	    call amovr (d[i2], z[35], 5)
+	    call amovr (e[i2], z[40], 5)
+	    call amovr (f[i2], z[45], 5)
+
+	    # Find the highest point excluding the center.
+	    j1 = 37; j2 = 1
+	    do j = 2, 49 {
+		if (j == j1)
+		    next
+		if (z[j] > z[j2])
+		    j2 = j 
+	    }
+
+	    # Compute the flux excluding the extreme points.
+	    flux = (asumr (z, 49) - z[j1] - z[j2]) / 47
+
+	    # Pixel must be exceed specified threshold.
+	    if (p < flux + threshold)
+		next
+
+	    # Fit and subtract the background.
+	    if (j2 < 25) {
+	        w[j2] = 0
+		sf = sf2
+	        call gsfit (sf, x, y, z, w, 24, WTS_USER, j)
+		w[j2] = 1
+	    } else {
+		sf = sf1
+	        call gsrefit (sf, x, y, z, w, j)
+	    }
+
+	    call gsvector (sf, x, y, bkgd, 49)
+	    call asubr (z, bkgd, z, 49)
+	    p = z[j1]
+
+	    # Compute the flux excluding the extreme points.
+	    flux = (asumr (z, 49) - z[j1] - z[j2]) / 47
+
+	    # Determine replacement value from four nearest neighbors again
+	    # excluding the most deviant pixels.
+	    replace = 0
+	    j = 0
+	    if (j2 != 32) {
+		replace = replace + c[i4]
+		j = j + 1
+	    }
+	    if (j2 != 36) {
+		replace = replace + d[i3]
+		j = j + 1
+	    }
+	    if (j2 != 38) {
+		replace = replace + d[i5]
+		j = j + 1
+	    }
+	    if (j2 != 42) {
+		replace = replace + e[i4]
+		j = j + 1
+	    }
+	    replace = replace / j
+
+	    # Add pixel to cosmic ray list.
+	    flux = 100. * flux
+	    call cr_add (cr, col+i4-1, line, flux, flux/p, 0., replace, 0)
+	    i4 = i7
+	}
+end
+
+
+# CR_FIND5 -- Find cosmic rays candidates in 5x5 window.
+# This routine finds cosmic rays candidates with the following algorithm.
+#    1. If the pixel is not a local maximum relative to it's 24 neighbors
+#	go on to the next pixel.
+#    2. Identify the next strongest pixel in the 5x5 region.
+#	This suspect pixel is excluded in the following.
+#    2. Compute the flux of the 5x5 region excluding the cosmic ray
+#	candidate and the suspect pixel.
+#    3. The candidate must exceed the average flux per pixel by a specified
+#	threshold.  If not go on to the next pixel.
+#    4. Fit a plane to the border pixels (excluding the suspect pixel).
+#    5. Subtract the background defined by the plane.
+#    6. Determine a replacement value as the average of the four adjacent
+#	pixels (excluding the suspect pixels).
+#    7. Add the pixel to the cosmic ray candidate list.
+
+procedure cr_find5 (cr, threshold, col, line, a, b, c, d, e, n,
+	sf1, sf2, x, y, z, w)
+
+pointer	cr						# Cosmic ray list
+real	threshold					# Detection threshold
+int	col						# First column
+int	line						# Line
+real	a[ARB], b[ARB], c[ARB], d[ARB], e[ARB]		# Image lines
+int	n						# Number of columns
+pointer	sf1, sf2					# Surface fitting
+real	x[25], y[25], z[25], w[25]			# Surface arrays
+
+real	bkgd[25] 
+int	i1, i2, i3, i4, i5, j, j1, j2
+real	p, flux, replace, asumr()
+pointer	sf
+
+begin
+	for (i3=3; i3<=n-2; i3=i3+1) {
+	    # Must be local maxima.
+	    p = c[i3]
+	    if (p<a[i3]||p<b[i3]||p<d[i3]||p<e[i3])
+		next
+	    i1 = i3 - 2
+	    if (p<a[i1]||p<b[i1]||p<c[i1]||p<d[i1]||p<e[i1])
+		next
+	    i2 = i3 - 1
+	    if (p<a[i2]||p<b[i2]||p<c[i2]||p<d[i2]||p<e[i2])
+		next
+	    i4 = i3 + 1
+	    if (p<a[i4]||p<b[i4]||p<c[i4]||p<d[i4]||p<e[i4])
+		next
+	    i5 = i3 + 2
+	    if (p<a[i5]||p<b[i5]||p<c[i5]||p<d[i5]||p<e[i5])
+		next
+
+	    # Convert to a single array in surface fitting order. 
+	    call amovr (a[i1], z[1], 5)
+	    z[6] = b[i5]; z[7] = c[i5]; z[8] = d[i5]; z[9] = e[i5]
+	    z[10] = e[i4]; z[11] = e[i3]; z[12] = e[i2]; z[13] = e[i1]
+	    z[14] = d[i1]; z[15] = c[i1]; z[16] = b[i1]
+	    call amovr (b[i2], z[17], 3)
+	    call amovr (c[i2], z[20], 3)
+	    call amovr (d[i2], z[23], 3)
+
+	    # Find the highest point excluding the center.
+	    j1 = 21; j2 = 1
+	    do j = 2, 25 {
+		if (j == j1)
+		    next
+		if (z[j] > z[j2])
+		    j2 = j 
+	    }
+
+	    # Compute the flux excluding the extreme points.
+	    flux = (asumr (z, 25) - z[j1] - z[j2]) / 23
+
+	    # Pixel must be exceed specified threshold.
+	    if (p < flux + threshold)
+		next
+
+	    # Fit and subtract the background.
+	    if (j2 < 17) {
+	        w[j2] = 0
+		sf = sf2
+	        call gsfit (sf, x, y, z, w, 16, WTS_USER, j)
+		w[j2] = 1
+	    } else {
+		sf = sf1
+	        call gsrefit (sf, x, y, z, w, j)
+	    }
+
+	    call gsvector (sf, x, y, bkgd, 25)
+	    call asubr (z, bkgd, z, 25)
+	    p = z[j1]
+
+	    # Compute the flux excluding the extreme points.
+	    flux = (asumr (z, 25) - z[j1] - z[j2]) / 23
+
+	    # Determine replacement value from four nearest neighbors again
+	    # excluding the most deviant pixels.
+	    replace = 0
+	    j = 0
+	    if (j2 != 18) {
+		replace = replace + b[i3]
+		j = j + 1
+	    }
+	    if (j2 != 20) {
+		replace = replace + c[i2]
+		j = j + 1
+	    }
+	    if (j2 != 22) {
+		replace = replace + c[i4]
+		j = j + 1
+	    }
+	    if (j2 != 24) {
+		replace = replace + d[i3]
+		j = j + 1
+	    }
+	    replace = replace / j
+
+	    # Add pixel to cosmic ray list.
+	    flux = 100. * flux
+	    call cr_add (cr, col+i3-1, line, flux, flux/p, 0., replace, 0)
+	    i3 = i5
+	}
+end
diff --git a/noao/imred/crutil/src/crfix.cl b/noao/imred/crutil/src/crfix.cl
new file mode 100644
index 00000000..68947c7a
--- /dev/null
+++ b/noao/imred/crutil/src/crfix.cl
@@ -0,0 +1,20 @@
+# CRFIX -- Replace cosmic rays in an image using a cosmic ray mask.
+
+procedure crfix (input, output, crmask)
+
+file	input 			{prompt="Input image"}
+file	output 			{prompt="Output image"}
+file	crmask 			{prompt="Cosmic ray mask"}
+
+begin
+	file	in, out, crm
+
+	in = input
+	out = output
+	crm = crmask
+
+	if (in != out)
+	    imcopy (in, out, verbose=no)
+	fixpix (out, crm, linterp="INDEF", cinterp="INDEF", verbose=no,
+	    pixels=no)
+end
diff --git a/noao/imred/crutil/src/crgrow.par b/noao/imred/crutil/src/crgrow.par
new file mode 100644
index 00000000..f57eb3cc
--- /dev/null
+++ b/noao/imred/crutil/src/crgrow.par
@@ -0,0 +1,7 @@
+# CRGROW
+
+input,s,a,,,,Input cosmic ray masks
+output,s,a,,,,Output cosmic ray masks
+radius,r,h,1.,,,Grow radius
+inval,i,h,INDEF,,,Input mask value to grow (INDEF for any)
+outval,i,h,INDEF,,,Output grown mask value (INDEF for any)
diff --git a/noao/imred/crutil/src/crlist.h b/noao/imred/crutil/src/crlist.h
new file mode 100644
index 00000000..1ed498a7
--- /dev/null
+++ b/noao/imred/crutil/src/crlist.h
@@ -0,0 +1,17 @@
+define	CR_ALLOC	100		# Allocation block size
+define	CR_LENSTRUCT	9		# Length of structure
+
+define	CR_NCR		Memi[$1]	# Number of cosmic rays
+define	CR_NALLOC	Memi[$1+1]	# Length of cosmic ray list
+define	CR_COL		Memi[$1+2]	# Pointer to columns
+define	CR_LINE		Memi[$1+3]	# Pointer to lines
+define	CR_FLUX		Memi[$1+4]	# Pointer to fluxes
+define	CR_RATIO	Memi[$1+5]	# Pointer to flux ratios
+define	CR_WT		Memi[$1+6]	# Pointer to training weights
+define	CR_REPLACE	Memi[$1+7]	# Pointer to replacement values
+define	CR_FLAG		Memi[$1+8]	# Pointer to rejection flag
+
+define	ALWAYSNO	3
+define	ALWAYSYES	4
+
+define	CR_RMAX		3.		# Maximum radius for matching
diff --git a/noao/imred/crutil/src/crlist.x b/noao/imred/crutil/src/crlist.x
new file mode 100644
index 00000000..bb49fb03
--- /dev/null
+++ b/noao/imred/crutil/src/crlist.x
@@ -0,0 +1,417 @@
+include	<error.h>
+include	<syserr.h>
+include	<gset.h>
+include	<pmset.h>
+include	"crlist.h"
+
+define	HELP	"noao$lib/scr/cosmicrays.key"
+define	PROMPT	"cosmic ray options"
+
+# CR_OPEN    -- Open cosmic ray list
+# CR_CLOSE   -- Close cosmic ray list
+# CR_ADD     -- Add a cosmic ray candidate to cosmic ray list.
+# CR_TRAIN   -- Set flux ratio threshold from a training set.
+# CR_FINDTHRESH -- Find flux ratio.
+# CR_WEIGHT  -- Compute the training weight at a particular flux ratio.
+# CR_FLAGS   -- Set cosmic ray reject flags.
+# CR_BADPIX  -- Store cosmic rays in bad pixel list.
+# CR_REPLACE -- Replace cosmic rays in image with replacement values.
+
+# CR_OPEN -- Open cosmic ray list
+
+procedure cr_open (cr)
+
+pointer	cr		# Cosmic ray list pointer
+errchk	malloc
+
+begin
+	call malloc (cr, CR_LENSTRUCT, TY_STRUCT)
+	call malloc (CR_COL(cr), CR_ALLOC, TY_REAL)
+	call malloc (CR_LINE(cr), CR_ALLOC, TY_REAL)
+	call malloc (CR_FLUX(cr), CR_ALLOC, TY_REAL)
+	call malloc (CR_RATIO(cr), CR_ALLOC, TY_REAL)
+	call malloc (CR_WT(cr), CR_ALLOC, TY_REAL)
+	call malloc (CR_REPLACE(cr), CR_ALLOC, TY_REAL)
+	call malloc (CR_FLAG(cr), CR_ALLOC, TY_INT)
+	CR_NCR(cr) = 0
+	CR_NALLOC(cr) = CR_ALLOC
+end
+
+
+# CR_CLOSE -- Close cosmic ray list
+
+procedure cr_close (cr)
+
+pointer	cr		# Cosmic ray list pointer
+
+begin
+	call mfree (CR_COL(cr), TY_REAL)
+	call mfree (CR_LINE(cr), TY_REAL)
+	call mfree (CR_FLUX(cr), TY_REAL)
+	call mfree (CR_RATIO(cr), TY_REAL)
+	call mfree (CR_WT(cr), TY_REAL)
+	call mfree (CR_REPLACE(cr), TY_REAL)
+	call mfree (CR_FLAG(cr), TY_INT)
+	call mfree (cr, TY_STRUCT)
+end
+
+# CR_ADD -- Add a cosmic ray candidate to cosmic ray list.
+
+procedure cr_add (cr, col, line, flux, ratio, wt, replace, flag)
+
+pointer	cr		# Cosmic ray list pointer
+int	col		# Cofluxn
+int	line		# Line
+real	flux		# Luminosity
+real	ratio		# Ratio
+real	wt		# Weight
+real	replace		# Sky value
+int	flag		# Flag value
+
+int	ncr
+errchk	realloc
+
+begin
+	if (CR_NCR(cr) == CR_NALLOC(cr)) {
+	    CR_NALLOC(cr) = CR_NALLOC(cr) + CR_ALLOC
+	    call realloc (CR_COL(cr), CR_NALLOC(cr), TY_REAL)
+	    call realloc (CR_LINE(cr), CR_NALLOC(cr), TY_REAL)
+	    call realloc (CR_FLUX(cr), CR_NALLOC(cr), TY_REAL)
+	    call realloc (CR_RATIO(cr), CR_NALLOC(cr), TY_REAL)
+	    call realloc (CR_WT(cr), CR_NALLOC(cr), TY_REAL)
+	    call realloc (CR_REPLACE(cr), CR_NALLOC(cr), TY_REAL)
+	    call realloc (CR_FLAG(cr), CR_NALLOC(cr), TY_INT)
+	}
+
+	ncr = CR_NCR(cr)
+	CR_NCR(cr) = ncr + 1
+	Memr[CR_COL(cr)+ncr] = col
+	Memr[CR_LINE(cr)+ncr] = line
+	Memr[CR_FLUX(cr)+ncr] = flux
+	Memr[CR_RATIO(cr)+ncr] = ratio
+	Memr[CR_WT(cr)+ncr] = wt
+	Memr[CR_REPLACE(cr)+ncr] = replace
+	Memi[CR_FLAG(cr)+ncr] = flag
+end
+
+
+# CR_TRAIN -- Set flux ratio threshold from a training set.
+
+procedure cr_train (cr, gp, gt, im, fluxratio, fname)
+
+pointer	cr		#I Cosmic ray list
+pointer	gp		#I GIO pointer
+pointer	gt		#I GTOOLS pointer
+pointer	im		#I IMIO pointer
+real	fluxratio	#O Flux ratio threshold
+char	fname[ARB]	#I Save file name
+
+char	cmd[10]
+bool	gflag
+real	x, y, y1, y2, w, r, rmin
+int	i, j, n, f, ncr, wcs, key, fd, clgcur(), open(), errcode()
+pointer	col, line, ratio, flux, wt, flag
+
+begin
+	# Open save file
+	iferr (fd = open (fname, APPEND, TEXT_FILE)) {
+	    if (errcode() != SYS_FNOFNAME)
+		call erract (EA_WARN)
+	    fd = 0
+	}
+
+	ncr = CR_NCR(cr)
+	col = CR_COL(cr) - 1
+	line = CR_LINE(cr) - 1
+	flux = CR_FLUX(cr) - 1
+	ratio = CR_RATIO(cr) - 1
+	wt = CR_WT(cr) - 1
+	flag = CR_FLAG(cr) - 1
+
+	gflag = false
+	n = 0
+	while (clgcur ("objects", x, y, wcs, key, cmd, 10) != EOF) {
+	    switch (key) {
+	    case '?':
+		call gpagefile (gp, HELP, PROMPT)
+		next
+	    case 'q':
+		break
+	    case 's':
+		w = 1
+		f = ALWAYSNO
+	    case 'c':
+		w = -1
+		f = ALWAYSYES
+	    case 'g':
+		if (gflag)
+		    call cr_examine (cr, gp, gt, im, fluxratio, 'z')
+		else {
+		    if (n > 1)
+			call cr_findthresh (cr, fluxratio)
+		    call cr_flags (cr, fluxratio)
+		    call cr_examine (cr, gp, gt, im, fluxratio, 'r')
+		    gflag = true
+		}
+		next
+	    default:
+		next
+	    }
+
+	    y1 = y - CR_RMAX
+	    y2 = y + CR_RMAX
+	    for (i=10; i<ncr && y1>Memr[line+i]; i=i+10)
+		;
+	    j = i - 9
+	    rmin = (Memr[col+j] - x) ** 2 + (Memr[line+j] - y) ** 2
+	    for (i=j+1; i<ncr && y2>Memr[line+i]; i=i+1) {
+		r = (Memr[col+i] - x) ** 2 + (Memr[line+i] - y) ** 2
+		if (r < rmin) {
+		    rmin = r
+		    j = i
+		}
+	    }
+	    if (sqrt (rmin) > CR_RMAX)
+		next
+
+	    Memr[wt+j] = w
+	    Memi[flag+j] = f
+	    n = n + 1
+
+	    if (gflag) {
+		if (n > 1) {
+		    call cr_findthresh (cr, r)
+		    call cr_update (gp, r, cr, fluxratio, 0)
+		}
+		call gmark (gp, Memr[flux+j], Memr[ratio+j], GM_BOX, 2., 2.)
+	    }
+	    if (fd > 0) {
+		call fprintf (fd, "%g %g %d %c\n")
+		    call pargr (x)
+		    call pargr (y)
+		    call pargi (wcs)
+		    call pargi (key)
+	    }
+	}
+
+	if (fd > 0)
+	    call close (fd)
+end
+
+
+# CR_FINDTHRESH -- Find flux ratio.
+
+procedure cr_findthresh (cr, fluxratio)
+
+pointer	cr		#I Cosmic ray list
+real	fluxratio	#O Flux ratio threshold
+
+real	w, r, rmin, cr_weight()
+int	i, ncr
+pointer	ratio, wt
+
+begin
+	ncr = CR_NCR(cr)
+	ratio = CR_RATIO(cr) - 1
+	wt = CR_WT(cr) - 1
+
+	fluxratio = Memr[ratio+1]
+	rmin = cr_weight (fluxratio, Memr[ratio+1], Memr[wt+1], ncr)
+	do i = 2, ncr {
+	    if (Memr[wt+i] == 0.)
+		next
+	    r = Memr[ratio+i]
+	    w = cr_weight (r, Memr[ratio+1], Memr[wt+1], ncr)
+	    if (w <= rmin) {
+		if (w == rmin)
+		    fluxratio = min (fluxratio, r)
+		else {
+		    rmin = w
+		    fluxratio = r
+		}
+	    }
+	}
+end
+
+
+# CR_WEIGHT -- Compute the training weight at a particular flux ratio.
+
+real procedure cr_weight (fluxratio, ratio, wts, ncr)
+
+real	fluxratio		#I Flux ratio
+real	ratio[ARB]		#I Ratio Values
+real	wts[ARB]		#I Weights
+int	ncr			#I Number of ratio values
+real	wt			#O Sum of weights
+
+int	i
+
+begin
+	wt = 0.
+	do i = 1, ncr {
+	    if (ratio[i] > fluxratio) {
+		if (wts[i] < 0.)
+		    wt = wt - wts[i]
+	    } else {
+		if (wts[i] > 0.)
+		    wt = wt + wts[i]
+	    }
+	}
+	return (wt)
+end
+
+
+# CR_FLAGS -- Set cosmic ray reject flags.
+
+procedure cr_flags (cr, fluxratio)
+
+pointer	cr			# Cosmic ray candidate list
+real	fluxratio		# Rejection limits
+
+int	i, ncr
+pointer	ratio, flag
+
+begin
+	ncr = CR_NCR(cr)
+	ratio = CR_RATIO(cr) - 1
+	flag = CR_FLAG(cr) - 1
+
+	do i = 1, ncr {
+	    if ((Memi[flag+i] == ALWAYSYES) || (Memi[flag+i] == ALWAYSNO))
+		next
+	    if (Memr[ratio+i] > fluxratio)
+		Memi[flag+i] = NO
+	    else
+		Memi[flag+i] = YES
+	}
+end
+
+
+# CR_BADPIX -- Store cosmic rays in bad pixel list.
+# This is currently a temporary measure until a real bad pixel list is
+# implemented.
+
+procedure cr_badpix (cr, fname)
+
+pointer	cr		# Cosmic ray list
+char	fname[ARB]	# Bad pixel file name
+
+int	i, ncr, c, l, f, fd, open(), errcode()
+pointer	col, line, ratio, flux, flag
+errchk	open
+
+begin
+	# Open bad pixel file
+	iferr (fd = open (fname, APPEND, TEXT_FILE)) {
+	    if (errcode() != SYS_FNOFNAME)
+		call erract (EA_WARN)
+	    return
+	}
+
+	ncr = CR_NCR(cr)
+	col = CR_COL(cr) - 1
+	line = CR_LINE(cr) - 1
+	flux = CR_FLUX(cr) - 1
+	ratio = CR_RATIO(cr) - 1
+	flag = CR_FLAG(cr) - 1
+
+	do i = 1, ncr {
+	    f = Memi[flag+i]
+	    if ((f == NO) || (f == ALWAYSNO))
+		next
+
+	    c = Memr[col+i]
+	    l = Memr[line+i]
+	    call fprintf (fd, "%d %d\n")
+	        call pargi (c)
+	        call pargi (l)
+	}
+	call close (fd)
+end
+
+
+# CR_CRMASK -- Store cosmic rays in cosmic ray mask.
+
+procedure cr_crmask (cr, fname, ref)
+
+pointer	cr		# Cosmic ray list
+char	fname[ARB]	# Cosmic ray mask
+pointer	ref		# Refrence image
+
+int	i, axlen[7], depth, ncr, f, rl[3,2]
+long	v[2]
+pointer	sp, title, pm, col, line, flag, pm_newmask()
+errchk	pm_loadf, pm_newmask, pm_savef
+
+begin
+	call smark (sp)
+	call salloc (title, SZ_LINE, TY_CHAR)
+
+	pm = pm_newmask (ref, 1)
+	iferr (call pm_loadf (pm, fname, Memc[title], SZ_LINE))
+	    ;
+	call pm_gsize (pm, i, axlen, depth)
+
+	ncr = CR_NCR(cr)
+	col = CR_COL(cr) - 1
+	line = CR_LINE(cr) - 1
+	flag = CR_FLAG(cr) - 1
+
+	RL_LEN(rl) = 2
+	RL_AXLEN(rl) = axlen[1]
+	RL_N(rl,2) = 1
+	RL_V(rl,2) = 1
+	RL_X(rl,2) = 1
+
+	do i = 1, ncr {
+	    f = Memi[flag+i]
+	    if ((f == NO) || (f == ALWAYSNO))
+		next
+
+	    v[1] = Memr[col+i]
+	    v[2] = Memr[line+i]
+	    call pmplri (pm, v, rl, depth, 1, PIX_SRC)
+	}
+
+	call strcpy ("Cosmic ray mask from COSMICRAYS", Memc[title], SZ_LINE)
+	call pm_savef (pm, fname, Memc[title], PM_UPDATE)
+	call pm_close (pm)
+	call sfree (sp)
+end
+
+
+# CR_REPLACE -- Replace cosmic rays in image with replacement values.
+
+procedure cr_replace (cr, offset, im, nreplaced)
+
+pointer	cr		# Cosmic ray list
+int	offset		# Offset in list
+pointer	im		# IMIO pointer of output image
+int	nreplaced	# Number replaced (for log)
+
+int	i, ncr, c, l, f
+real	r
+pointer	col, line, replace, flag, imps2r()
+
+begin
+	ncr = CR_NCR(cr)
+	if (ncr <= offset)
+	    return
+
+	col = CR_COL(cr) - 1
+	line = CR_LINE(cr) - 1
+	replace = CR_REPLACE(cr) - 1
+	flag = CR_FLAG(cr) - 1
+
+	do i = offset+1, ncr {
+	    f = Memi[flag+i]
+	    if ((f == NO) || (f == ALWAYSNO))
+		next
+
+	    c = Memr[col+i]
+	    l = Memr[line+i]
+	    r = Memr[replace+i]
+	    Memr[imps2r (im, c, c, l, l)] = r
+	    nreplaced = nreplaced + 1
+	}
+end
diff --git a/noao/imred/crutil/src/crmedian.par b/noao/imred/crutil/src/crmedian.par
new file mode 100644
index 00000000..2baccb05
--- /dev/null
+++ b/noao/imred/crutil/src/crmedian.par
@@ -0,0 +1,15 @@
+input,f,a,,,,Input image
+output,f,a,,,,Output image
+crmask,f,h,,,,Output cosmic ray mask
+median,f,h,,,,Output median image
+sigma,f,h,,,,Output sigma image
+residual,f,h,,,,Output residual image
+var0,r,h,0.,0.,,Variance coefficient for DN^0 term
+var1,r,h,0.,0.,,Variance coefficient for DN^1 term
+var2,r,h,0.,0.,,Variance coefficient for DN^2 term
+lsigma,r,h,10.,,,Low clipping sigma factor
+hsigma,r,h,3.,,,High clipping sigma factor
+ncmed,i,h,5,1,,Column box size for median level calculation
+nlmed,i,h,5,1,,Line box size for median level calculation
+ncsig,i,h,25,10,,Column box size for sigma calculation
+nlsig,i,h,25,10,,Line box size for sigma calculation
diff --git a/noao/imred/crutil/src/crnebula.cl b/noao/imred/crutil/src/crnebula.cl
new file mode 100644
index 00000000..c5f214f9
--- /dev/null
+++ b/noao/imred/crutil/src/crnebula.cl
@@ -0,0 +1,116 @@
+# CRNEBULA -- Cosmic ray cleaning for images with fine nebular structure.
+
+procedure crnebula (input, output)
+
+file    input           {prompt="Input image"}
+file	output		{prompt="Output image"}
+file    crmask          {prompt="Cosmic ray mask"}
+file	residual	{prompt="Residual median image"}
+file	rmedresid	{prompt="Residual ring median image"}
+real    var0 = 1.       {prompt="Variance coefficient for DN^0 term", min=0.}
+real	var1 = 0.	{prompt="Variance coefficient for DN^1 term", min=0.}
+real	var2 = 0.	{prompt="Variance coefficient for DN^2 term", min=0.}
+real    sigmed = 3      {prompt="Sigma clip factor for residual median"}
+real    sigrmed = 3     {prompt="Sigma clip factor for residual ring median"}
+
+int     mbox = 5        {prompt="Median box size"}
+real    rin = 1.5       {prompt="Inner radius for ring median"}
+real    rout = 6        {prompt="Outer radius for ring median"}
+bool    verbose = no    {prompt="Verbose"}
+
+begin
+        file    in, out, med, sig, resid, rmed
+        struct  expr
+
+        # Query once for query parameters.
+        in = input
+        out = output
+
+        # Check on output images.
+	if (out != "" && imaccess (out))
+            error (1, "Output image already exists ("//out//")")
+        if (crmask != "" && imaccess (crmask))
+            error (1, "Output mask already exists ("//crmask//")")
+	if (residual != "" && imaccess (residual))
+            error (1, "Output residual image already exists ("//residual//")")
+	if (rmedresid != "" && imaccess (rmedresid))
+            error (1,
+	       "Output ring median difference already exists ("//rmedresid//")")
+
+        # Create median results.
+	med = mktemp ("cr")
+	sig = mktemp ("cr")
+	resid = residual
+	if (resid == "")
+	    resid = mktemp ("cr")
+	if (verbose)
+	    printf ("Creating CRMEDIAN results\n")
+	crmedian (in, "", crmask="", median=med, sigma=sig, residual=resid,
+	    var0=var0, var1=var1, var2=var2, lsigma=100., hsigma=sigmed,
+	    ncmed=mbox, nlmed=mbox, ncsig=25, nlsig=25)
+
+        # Create ring median filtered image.
+        rmed = mktemp ("cr")
+	rmedian (in, rmed, rin, rout, ratio=1., theta=0., zloreject=INDEF,
+	    zhireject=INDEF, boundary="wrap", constant=0., verbose=verbose)
+
+	# Create output images.
+	if (rmedresid != "") {
+	    printf ("(a-b)/c\n") | scan (expr)
+	    imexpr (expr, rmedresid, med, rmed, sig, dims="auto",
+		intype="auto", outtype="real", refim="auto", bwidth=0,
+		btype="nearest", bpixval=0., rangecheck=yes, verbose=no,
+		exprdb="none")
+	    imdelete (rmed, verify-)
+	    imdelete (sig, verify-)
+	    if (out != "") {
+		if (verbose)
+		    printf ("Create output image %s\n", out)
+		printf ("((a<%.3g)||(abs(b)>%.3g)) ? c : d\n",
+		    sigmed, sigrmed) | scan (expr)
+		imexpr (expr, out, resid, rmedresid, in, med, dims="auto",
+		    intype="auto", outtype="auto", refim="auto", bwidth=0,
+		    btype="nearest", bpixval=0., rangecheck=yes, verbose=no,
+		    exprdb="none")
+	    }
+	    if (crmask != "") {
+		if (verbose)
+		    printf ("Create cosmic ray mask %s\n", crmask)
+		printf ("((a<%.3g)||(abs(b)>%.3g)) ? 0 : 1\n",
+		    sigmed, sigrmed) | scan (expr)
+		set imtype = "pl"
+		imexpr (expr, crmask, resid, rmedresid, dims="auto",
+		    intype="auto", outtype="short", refim="auto", bwidth=0,
+		    btype="nearest", bpixval=0., rangecheck=yes, verbose=no,
+		    exprdb="none")
+	    }
+	    imdelete (med, verify-)
+	} else {
+	    if (out != "") {
+		if (verbose)
+		    printf ("Create output image %s\n", out)
+		printf ("((a<%.3g)||(abs((b-c)/d)>%.3g)) ? e : b\n",
+		    sigmed, sigrmed) | scan (expr)
+		imexpr (expr, out, resid, med, rmed, sig, in, dims="auto",
+		    intype="auto", outtype="auto", refim="auto", bwidth=0,
+		    btype="nearest", bpixval=0., rangecheck=yes, verbose=no,
+		    exprdb="none")
+	    }
+	    if (crmask != "") {
+		if (verbose)
+		    printf ("Create cosmic ray mask %s\n", crmask)
+		printf ("((a<%.3g)||(abs((b-c)/d)>%.3g)) ? 0 : 1\n",
+		    sigmed, sigrmed) | scan (expr)
+		set imtype = "pl"
+		imexpr (expr, crmask, resid, med, rmed, sig, dims="auto",
+		    intype="auto", outtype="short", refim="auto", bwidth=0,
+		    btype="nearest", bpixval=0., rangecheck=yes, verbose=no,
+		    exprdb="none")
+	    }
+	    imdelete (med, verify-)
+	    imdelete (sig, verify-)
+	    imdelete (rmed, verify-)
+	}
+	if (residual == "")
+	    imdelete (resid, verify-)
+end
diff --git a/noao/imred/crutil/src/crsurface.x b/noao/imred/crutil/src/crsurface.x
new file mode 100644
index 00000000..32645ff4
--- /dev/null
+++ b/noao/imred/crutil/src/crsurface.x
@@ -0,0 +1,46 @@
+define	DUMMY	6
+
+# CR_SURFACE -- Draw a perspective view of a surface.  The altitude
+# and azimuth of the viewing angle are variable.
+
+procedure cr_surface(gp, data, ncols, nlines, angh, angv)
+
+pointer	gp			# GIO pointer
+real	data[ncols,nlines]	# Surface data to be plotted
+int	ncols, nlines		# Dimensions of surface
+real	angh, angv		# Orientation of surface (degrees)
+
+int	wkid
+pointer	sp, work
+
+int	first
+real	vpx1, vpx2, vpy1, vpy2
+common  /frstfg/ first
+common  /noaovp/ vpx1, vpx2, vpy1, vpy2
+
+begin
+	call smark (sp)
+	call salloc (work, 2 * (2 * ncols * nlines + ncols + nlines), TY_REAL)
+
+	# Initialize surface common blocks
+	first = 1
+	call srfabd()
+
+	# Define viewport.
+	call ggview (gp, vpx1, vpx2, vpy1, vpy2) 
+
+	# Link GKS to GIO
+	wkid = 1
+	call gopks (STDERR)
+	call gopwk (wkid, DUMMY, gp)
+	call gacwk (wkid)
+
+	call ezsrfc (data, ncols, nlines, angh, angv, Memr[work])
+
+	call gdawk (wkid)
+	# We don't want to close the GIO pointer.
+	#call gclwk (wkid)
+	call gclks ()
+
+	call sfree (sp)
+end
diff --git a/noao/imred/crutil/src/mkpkg b/noao/imred/crutil/src/mkpkg
new file mode 100644
index 00000000..1279b656
--- /dev/null
+++ b/noao/imred/crutil/src/mkpkg
@@ -0,0 +1,38 @@
+# COSMIC RAY CLEANING PACKAGE
+
+$call	relink
+$exit
+
+update:
+        $call   relink
+        $call   install
+        ;
+
+relink:
+        $update libpkg.a
+        $call   crutil
+        ;
+
+install:
+        $move   xx_crutil.e noaobin$x_crutil.e
+        ;
+
+crutil:
+        $omake  x_crutil.x
+        $link   x_crutil.o libpkg.a -lxtools -lcurfit -lgsurfit -lncar -lgks\
+                -o xx_crutil.e
+        ;
+
+libpkg.a:
+	crexamine.x	crlist.h <error.h> <gset.h> <mach.h> <pkg/gtools.h>\
+			<imhdr.h>
+	crfind.x	<math/gsurfit.h>
+	crlist.x	crlist.h <error.h> <gset.h> <pmset.h>
+	crsurface.x	
+	t_cosmicrays.x	crlist.h <error.h> <math/gsurfit.h> <imhdr.h> <gset.h>\
+			<pkg/gtools.h> <imset.h>
+	t_craverage.x	<imhdr.h> <error.h> <mach.h>
+	t_crgrow.x	<error.h> <imhdr.h>
+	t_crmedian.x	<imhdr.h> <mach.h>
+	xtmaskname.x
+	;
diff --git a/noao/imred/crutil/src/t_cosmicrays.x b/noao/imred/crutil/src/t_cosmicrays.x
new file mode 100644
index 00000000..fa68a39d
--- /dev/null
+++ b/noao/imred/crutil/src/t_cosmicrays.x
@@ -0,0 +1,329 @@
+include	<error.h>
+include <imhdr.h>
+include <imset.h>
+include	<math/gsurfit.h>
+include	<gset.h>
+include	<pkg/gtools.h>
+include	"crlist.h"
+
+# T_COSMICRAYS -- Detect and remove cosmic rays in images.
+# A list of images is examined for cosmic rays which are then replaced
+# by values from neighboring pixels.  The output image may be the same
+# as the input image.  This is the top level procedure which manages
+# the input and output image data.  The actual algorithm for detecting
+# cosmic rays is in CR_FIND.
+
+procedure t_cosmicrays ()
+
+int	list1			# List of input images to be cleaned
+int	list2			# List of output images
+int	list3			# List of output bad pixel files
+real	threshold		# Detection threshold
+real	fluxratio		# Luminosity boundary for stars
+int	npasses			# Number of cleaning passes
+int	szwin			# Size of detection window
+bool	train			# Use training objects?
+pointer	savefile		# Save file for training objects
+bool	interactive		# Examine cosmic ray parameters?
+char	ans			# Answer to interactive query
+
+int	nc, nl, c, c1, c2, l, l1, l2, szhwin, szwin2
+int	i, j, k, m, ncr, ncrlast, nreplaced, flag
+pointer	sp, input, output, badpix, str, gp, gt, im, in, out
+pointer	x, y, z, w, sf1, sf2, cr, data, ptr
+
+bool	clgetb(), streq(), strne()
+char	clgetc()
+int	imtopenp(), imtlen(), imtgetim(), clpopnu(), clgfil(), clgeti()
+real	clgetr()
+pointer	immap(), impl2r(), imgs2r(), gopen(), gt_init()
+errchk	immap, impl2r, imgs2r
+errchk	cr_find, cr_examine, cr_replace, cr_plot, cr_crmask
+
+begin
+	call smark (sp)
+	call salloc (input, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (badpix, SZ_FNAME, TY_CHAR)
+	call salloc (savefile, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the task parameters.  Check that the number of output images
+	# is either zero, in which case the cosmic rays will be removed
+	# in place, or equal to the number of input images.
+
+	list1 = imtopenp ("input")
+	list2 = imtopenp ("output")
+	i = imtlen (list1)
+	j = imtlen (list2)
+	if (j > 0 && j != i)
+	    call error (0, "Input and output image lists do not match")
+
+	list3 = clpopnu ("crmasks")
+	threshold = clgetr ("threshold")
+	fluxratio = clgetr ("fluxratio")
+	npasses = clgeti ("npasses")
+	szwin = clgeti ("window")
+	train = clgetb ("train")
+	call clgstr ("savefile", Memc[savefile], SZ_FNAME)
+	interactive = clgetb ("interactive")
+	call clpstr ("answer", "yes")
+	ans = 'y'
+
+	# Set up the graphics.
+	call clgstr ("graphics", Memc[str], SZ_LINE)
+	if (interactive) {
+	    gp = gopen (Memc[str], NEW_FILE+AW_DEFER, STDGRAPH)
+	    gt = gt_init()
+	    call gt_sets (gt, GTTYPE, "mark")
+	    call gt_sets (gt, GTXTRAN, "log")
+	    call gt_setr (gt, GTXMIN, 10.)
+	    call gt_setr (gt, GTYMIN, 0.)
+	    call gt_sets (gt, GTTITLE, "Parameters of cosmic rays candidates")
+	    call gt_sets (gt, GTXLABEL, "Flux")
+	    call gt_sets (gt, GTYLABEL, "Flux Ratio")
+	}
+
+	# Set up surface fitting.  The background points are placed together
+	# at the beginning of the arrays.  There are two surface pointers,
+	# one for using the fast refit if there are no points excluded and
+	# one for doing a full fit with points excluded.
+
+	szhwin = szwin / 2
+	szwin2 = szwin * szwin
+	call salloc (data, szwin, TY_INT)
+	call salloc (x, szwin2, TY_REAL)
+	call salloc (y, szwin2, TY_REAL)
+	call salloc (z, szwin2, TY_REAL)
+	call salloc (w, szwin2, TY_REAL)
+
+	k = 0
+	do i = 1, szwin {
+	    Memr[x+k] = i
+	    Memr[y+k] = 1
+	    k = k + 1
+	}
+	do i = 2, szwin {
+	    Memr[x+k] = szwin
+	    Memr[y+k] = i
+	    k = k + 1
+	}
+	do i = szwin-1, 1, -1 {
+	    Memr[x+k] = i
+	    Memr[y+k] = szwin
+	    k = k + 1
+	}
+	do i = szwin-1, 2, -1 {
+	    Memr[x+k] = 1
+	    Memr[y+k] = i
+	    k = k + 1
+	}
+	do i = 2, szwin-1 {
+	    do j = 2, szwin-1 {
+	        Memr[x+k] = j
+	        Memr[y+k] = i
+	        k = k + 1
+	    }
+	}
+	call aclrr (Memr[z], szwin2)
+	call amovkr (1., Memr[w], 4*szwin-4)
+	call gsinit (sf1, GS_POLYNOMIAL, 2, 2, NO, 1., real(szwin),
+	    1., real(szwin))
+	call gsinit (sf2, GS_POLYNOMIAL, 2, 2, NO, 1., real(szwin),
+	    1., real(szwin))
+	call gsfit (sf1, Memr[x], Memr[y], Memr[z], Memr[w], 4*szwin-4,
+	    WTS_USER, j)
+
+	# Process each input image.  Either work in place or create a
+	# new output image.  If an error mapping the images occurs
+	# issue a warning and go on to the next input image.
+
+	while (imtgetim (list1, Memc[input], SZ_FNAME) != EOF) {
+	    if (imtgetim (list2, Memc[output], SZ_FNAME) == EOF)
+		call strcpy (Memc[input], Memc[output], SZ_FNAME)
+	    if (clgfil (list3, Memc[badpix], SZ_FNAME) == EOF)
+		Memc[badpix] = EOS
+
+	    iferr {
+		in = NULL
+		out = NULL
+		cr = NULL
+
+		# Map the input image.  If the output image is
+		# the same as the input image work in place.
+		# Initialize IMIO to use a scrolling buffer of lines.
+
+	        if (streq (Memc[input], Memc[output])) {
+	            im = immap (Memc[input], READ_WRITE, 0)
+		} else
+		    im = immap (Memc[input], READ_ONLY, 0)
+		in = im
+
+	        nc = IM_LEN(in,1)
+	        nl = IM_LEN(in,2)
+	        if ((nl < szwin) || (nc < szwin))
+	            call error (0, "Image size is too small")
+	        call imseti (in, IM_NBUFS, szwin)
+	        call imseti (in, IM_TYBNDRY, BT_NEAREST)
+	        call imseti (in, IM_NBNDRYPIX, szhwin)
+
+		# Open the output image if needed.
+	        if (strne (Memc[input], Memc[output]))
+		    im = immap (Memc[output], NEW_COPY, in)
+		out = im
+
+		# Open a cosmic ray list structure.
+	        call cr_open (cr)
+		ncrlast = 0
+		nreplaced = 0
+
+		# Now proceed through the image line by line, scrolling
+		# the line buffers at each step.  If creating a new image
+		# also write out each line as it is read.  A procedure is
+		# called to find the cosmic ray candidates in the line
+		# and add them to the list maintained by CRLIST.
+		# Note that cosmic rays are not replaced at this point
+		# in order to allow the user to modify the criteria for
+		# a cosmic ray and review the results.
+
+	        c1 = 1-szhwin
+	        c2 = nc+szhwin
+		do i = 1, szwin-1 
+		    Memi[data+i] =
+			imgs2r (in, c1, c2, i-szhwin, i-szhwin)
+
+	        do l = 1, nl {
+		    do i = 1, szwin-1
+			Memi[data+i-1] = Memi[data+i]
+		    Memi[data+szwin-1] =
+			imgs2r (in, c1, c2, l+szhwin, l+szhwin)
+		    if (out != in)
+		        call amovr (Memr[Memi[data+szhwin]+szhwin],
+			    Memr[impl2r(out,l)], nc)
+
+	            call cr_find (cr, threshold, Memi[data],
+		        c2-c1+1, szwin, c1, l,
+		        sf1, sf2, Memr[x], Memr[y], Memr[z], Memr[w])
+	        }
+		if (interactive && train) {
+		    call cr_train (cr, gp, gt, in, fluxratio, Memc[savefile])
+		    train = false
+		}
+	        call cr_flags (cr, fluxratio)
+
+		# If desired examine the cosmic ray list interactively.
+	        if (interactive && ans != 'N') {
+		    if (ans != 'Y') {
+		        call eprintf ("%s - ")
+		            call pargstr (Memc[input])
+		        call flush (STDERR)
+		        ans = clgetc ("answer")
+		    }
+		    if ((ans == 'Y') || (ans == 'y'))
+	                call cr_examine (cr, gp, gt, in, fluxratio, 'r')
+	        }
+
+		# Now replace the selected cosmic rays in the output image.
+
+		call imflush (out)
+		call imseti (out, IM_ADVICE, RANDOM)
+	        call cr_replace (cr, ncrlast, out, nreplaced)
+
+		# Do additional passes through the data.  We work in place
+		# in the output image.  Note that we only have to look in
+		# the vicinity of replaced cosmic rays for secondary
+		# events since we've already looked at every pixel once.
+		# Instead of scrolling through the image we will extract
+		# subrasters around each replaced cosmic ray.  However,
+		# we use pointers into the subraster to maintain the same
+		# format expected by CR_FIND.
+
+	        if (npasses > 1) {
+	            if (out != in)
+	                call imunmap (out)
+	            call imunmap (in)
+		    im = immap (Memc[output], READ_WRITE, 0)
+		    in = im
+		    out = im
+	            call imseti (in, IM_TYBNDRY, BT_NEAREST)
+	            call imseti (in, IM_NBNDRYPIX, szhwin)
+
+	            for (i=2; i<=npasses; i=i+1) {
+			# Loop through each cosmic ray in the previous pass.
+		        ncr = CR_NCR(cr)
+		        do j = ncrlast+1, ncr {
+			    flag = Memi[CR_FLAG(cr)+j-1]
+			    if (flag==NO || flag==ALWAYSNO)
+			        next
+			    c = Memr[CR_COL(cr)+j-1]
+			    l = Memr[CR_LINE(cr)+j-1]
+			    c1 = max (1-szhwin, c - (szwin-1))
+			    c2 = min (nc+szhwin, c + (szwin-1))
+			    k = c2 - c1 + 1
+			    l1 = max (1-szhwin, l - (szwin-1))
+			    l2 = min (nl+szhwin, l + (szwin-1))
+
+			    # Set the line pointers off an image section
+			    # centered on a previously replaced cosmic ray.
+
+			    ptr = imgs2r (in, c1, c2, l1, l2) - k
+
+			    l1 = max (1, l - szhwin)
+			    l2 = min (nl, l + szhwin)
+			    do l = l1, l2 {
+				do m = 1, szwin
+				    Memi[data+m-1] = ptr + m * k
+				ptr = ptr + k
+
+	                        call cr_find ( cr, threshold, Memi[data],
+				    k, szwin, c1, l, sf1, sf2,
+				    Memr[x], Memr[y], Memr[z], Memr[w])
+			    }
+	                }
+		        call cr_flags (cr, fluxratio)
+
+			# Replace any new cosmic rays found.
+	                call cr_replace (cr, ncr, in, nreplaced)
+			ncrlast = ncr
+		    }
+	        }
+
+		# Output header log, log, plot, and bad pixels.
+		call sprintf (Memc[str], SZ_LINE,
+		    "Threshold=%5.1f, fluxratio=%6.2f, removed=%d")
+		    call pargr (threshold)
+		    call pargr (fluxratio)
+		    call pargi (nreplaced)
+		call imastr (out, "crcor", Memc[str])
+
+		call cr_plot (cr, in, fluxratio)
+		call cr_crmask (cr, Memc[badpix], in)
+
+	        call cr_close (cr)
+	        if (out != in)
+	            call imunmap (out)
+	        call imunmap (in)
+	    } then {
+		# In case of error clean up and go on to the next image.
+		if (in != NULL) {
+		    if (out != NULL && out != in)
+			call imunmap (out)
+		    call imunmap (in)
+		}
+		if (cr != NULL)
+		    call cr_close (cr)
+		call erract (EA_WARN)
+	    }
+	}
+
+	if (interactive) {
+	    call gt_free (gt)
+	    call gclose (gp)
+	}
+	call imtclose (list1)
+	call imtclose (list2)
+	call clpcls (list3)
+	call gsfree (sf1)
+	call gsfree (sf2)
+	call sfree (sp)
+end
diff --git a/noao/imred/crutil/src/t_craverage.x b/noao/imred/crutil/src/t_craverage.x
new file mode 100644
index 00000000..f7b82113
--- /dev/null
+++ b/noao/imred/crutil/src/t_craverage.x
@@ -0,0 +1,847 @@
+include	<error.h>
+include	<imhdr.h>
+include	<mach.h>
+
+define	MAXBUF		500000	# Maximum pixel buffer
+
+define	PLSIG		15.87	# Low percentile
+define	PHSIG		84.13	# High percentile
+
+
+# T_CRAVERAGE -- Detect, fix, and flag cosmic rays.  Also detect objects.
+# Deviant pixels relative to a local average with the candidate pixel
+# excluded and sigma are detected and replaced by the average value
+# and/or written to a cosmic ray mask.  Average values above a the median
+# of a background annulus are detected as objects and cosmic rays are
+# excluded.  The object positions may be output in the mask.
+
+procedure t_craverage ()
+
+int	inlist			# Input image list
+int	outlist			# Output image list
+int	crlist			# Output mask list
+int	avglist			# Output average list
+int	siglist			# Output sigma list
+int	crval			# Output cosmic ray mask value
+int	objval			# Output object mask value
+int	navg			# Averaging box size
+int	nrej			# Number of high pixels to reject from average
+int	nbkg			# Background width
+int	nsig			# Sigma box size
+real	lobjsig, hobjsig	# Object threshold sigmas
+real	lcrsig, hcrsig		# CR threshold sigmas outside of object
+real	var0			# Variance coefficient for DN^0 term
+real	var1			# Variance coefficient for DN^1 term
+real	var2			# Variance coefficient for DN^2 term
+real	crgrw			# Cosmic ray grow radius
+real	objgrw			# Object grow radius
+
+int	i, nc, nl, nlstep, nbox, l1, l2, l3, l4, nl1, pmmode
+pointer	sp, input, output, crmask, crmask1, extname, average, sigma
+pointer	in, out, pm, aim, sim
+pointer	inbuf, pinbuf, outbuf, pbuf, abuf, sbuf
+
+real	clgetr()
+int	clgeti(), imtopenp(), imtgetim()
+pointer	immap(), imgs2s(), imgs2r(), imps2r(), imps2s()
+errchk	immap, imgs2s, imgs2r, imps2r, imps2s, craverage, crgrow, imgstr
+
+begin
+	call smark (sp)
+	call salloc (input, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (crmask, SZ_FNAME, TY_CHAR)
+	call salloc (crmask1, SZ_FNAME, TY_CHAR)
+	call salloc (average, SZ_FNAME, TY_CHAR)
+	call salloc (sigma, SZ_FNAME, TY_CHAR)
+	call salloc (extname, SZ_FNAME, TY_CHAR)
+
+	# Get parameters.
+	inlist = imtopenp ("input")
+	outlist = imtopenp ("output")
+	crlist = imtopenp ("crmask")
+	avglist = imtopenp ("average")
+	siglist = imtopenp ("sigma")
+	crval = clgeti ("crval")
+	objval = clgeti ("objval")
+	navg = max (1, clgeti ("navg") / 2)
+	nrej = min (clgeti ("nrej"), navg-1)
+	nbkg = clgeti ("nbkg")
+	nsig = clgeti ("nsig")
+	lobjsig = clgetr ("lobjsig")
+	hobjsig = clgetr ("hobjsig")
+	lcrsig = clgetr ("lcrsig")
+	hcrsig = clgetr ("hcrsig")
+	nbox = 2 * (navg + nbkg) + 1
+	var0 = clgetr ("var0")
+	var1 = clgetr ("var1")
+	var2 = clgetr ("var2")
+	crgrw = clgetr ("crgrow")
+	objgrw = clgetr ("objgrow")
+
+	# Do the input images.
+	Memc[crmask1] = EOS
+	while (imtgetim (inlist, Memc[input], SZ_FNAME) != EOF) {
+	    if (imtgetim (outlist, Memc[output], SZ_FNAME) == EOF)
+		Memc[output] = EOS
+	    if (imtgetim (crlist, Memc[crmask], SZ_FNAME) == EOF)
+	        call strcpy (Memc[crmask1], Memc[crmask], SZ_FNAME)
+	    else if (Memc[crmask] == '!')
+	        call strcpy (Memc[crmask], Memc[crmask1], SZ_FNAME)
+	    if (imtgetim (avglist, Memc[average], SZ_FNAME) == EOF)
+		Memc[average] = EOS
+	    if (imtgetim (siglist, Memc[sigma], SZ_FNAME) == EOF)
+		Memc[sigma] = EOS
+
+	    # Map the input and output images.
+	    iferr {
+		in = NULL; out = NULL; pm = NULL; aim = NULL; sim = NULL
+		inbuf = NULL; pinbuf = NULL; outbuf = NULL; pbuf = NULL;
+		abuf = NULL; sbuf=NULL
+
+		in = immap (Memc[input], READ_ONLY, 0)
+		if (Memc[output] != EOS)
+		    out = immap (Memc[output], NEW_COPY, in)
+		if (Memc[crmask] != EOS) {
+		    if (Memc[crmask] == '!')
+			call imgstr (in, Memc[crmask+1], Memc[crmask], SZ_FNAME)
+		    pmmode = READ_WRITE
+		    iferr (call imgstr (in, "extname", Memc[extname], SZ_FNAME))
+			call strcpy ("pl", Memc[extname], SZ_FNAME)
+		    call xt_maskname (Memc[crmask], Memc[extname], pmmode,
+			Memc[crmask], SZ_FNAME)
+		    iferr (pm = immap (Memc[crmask], pmmode, 0)) {
+			pmmode = NEW_COPY
+			pm = immap (Memc[crmask], pmmode, in)
+		    }
+		}
+		if (Memc[average] != EOS)
+		    aim = immap (Memc[average], NEW_COPY, in)
+		if (Memc[sigma] != EOS)
+		    sim = immap (Memc[sigma], NEW_COPY, in)
+
+		# Go through the input in large blocks of lines.  If the
+		# block is smaller than the whole image overlap the blocks
+		# so the average only has boundaries at the ends of the image.
+		# However, the output is done in non-overlapping blocks with
+		# the pointers are adjusted so that addresses can be in the
+		# space of the input block.  CRAVERAGE does not address
+		# outside of the output data block.  Set the mask values
+		# based on the distances to the nearest good pixels.
+
+		nc = IM_LEN(in,1)
+		nl = IM_LEN(in,2)
+		nlstep = max (1, MAXBUF / nc - nbox)
+
+		do i = 1, nl, nlstep {
+		    l1 = i
+		    l2 = min (nl, i + nlstep - 1)
+		    l3 = max (1, l1 - nbox / 2)
+		    l4 = min (nl, l2 + nbox / 2)
+		    nl1 = l4 - l3 + 1
+		    inbuf = imgs2r (in, 1, nc, l3, l4)
+		    if (out != NULL)
+			outbuf = imps2r (out, 1, nc, l1, l2) - (l1 - l3) * nc
+		    if (pm != NULL) {
+			if (pmmode == READ_WRITE) {
+			    pinbuf = imgs2s (pm, 1, nc, l3, l4)
+			    pbuf = imps2s (pm, 1, nc, l1, l2)
+			    call amovs (Mems[pinbuf+(l1-l3)*nc],
+				Mems[pbuf], nc*(l2-l1+1))
+			    pbuf = pbuf - (l1 - l3) * nc
+			} else {
+			    pinbuf = NULL
+			    pbuf = imps2s (pm, 1, nc, l1, l2)
+			    call aclrs (Mems[pbuf], nc*(l2-l1+1))
+			    pbuf = pbuf - (l1 - l3) * nc
+			}
+		    }
+		    if (aim != NULL)
+			abuf = imps2r (aim, 1, nc, l1, l2) - (l1 - l3) * nc
+		    if (sim != NULL)
+			sbuf = imps2r (sim, 1, nc, l1, l2) - (l1 - l3) * nc
+		    if (pinbuf == NULL)
+			call craverage (inbuf, outbuf, pbuf, abuf, sbuf,
+			    nc, nl1, l1-l3+1, l2-l3+1, navg, nrej, nbkg,
+			    var0, var1, var2, nsig, lcrsig, hcrsig,
+			    lobjsig, hobjsig, crval, objval)
+		    else
+			call craverage1 (inbuf, pinbuf, outbuf, pbuf, abuf,
+			    sbuf, nc, nl1, l1-l3+1, l2-l3+1, navg, nrej, nbkg,
+			    var0, var1, var2, nsig, lcrsig, hcrsig,
+			    lobjsig, hobjsig, crval, objval)
+		}
+
+		# Grow regions if desired.  The routines are nops if the
+		# grow is zero.
+
+		if (pm != NULL) {
+		    if (pmmode != READ_WRITE) {
+			call imunmap (pm)
+			iferr (pm = immap (Memc[crmask], READ_WRITE, 0))
+			    call error (1, "Can't reopen mask for growing")
+		    }
+
+		    if (crval == objval)
+			call crgrow (pm, max (crgrw, objgrw), crval, crval)
+		    else {
+			call crgrow (pm, crgrw, crval, crval)
+			call crgrow (pm, objgrw, objval, objval)
+		    }
+		}
+	    } then
+		call erract (EA_WARN)
+
+	    if (sim != NULL)
+		call imunmap (sim)
+	    if (aim != NULL)
+		call imunmap (aim)
+	    if (pm != NULL)
+		call imunmap (pm)
+	    if (out != NULL)
+		call imunmap (out)
+	    call imunmap (in)
+	}
+
+	call imtclose (inlist)
+	call imtclose (outlist)
+	call imtclose (crlist)
+	call imtclose (avglist)
+	call imtclose (siglist)
+
+	call sfree (sp)
+end
+
+
+# CRAVERAGE -- Detect, replace, and flag cosmic rays.
+# A local background is computed using moving box averages to avoid
+# contaminating bad pixels.  If variance model is given then that is
+# used otherwise a local sigma is computed in blocks (it is not a moving box
+# for efficiency) by using a percentile point of the sorted pixel values to
+# estimate the width of the distribution uncontaminated by bad pixels).  Once
+# the background and sigma are known deviant pixels are found by using sigma
+# threshold factors.
+
+procedure craverage (in, out, pout, aout, sout, nc, nl, nl1, nl2,
+	navg, nrej, nbkg, var0, var1, var2, nsig, lcrsig, hcrsig,
+	lobjsig, hobjsig crval, objval)
+
+pointer	in			#I Input data
+pointer	out			#O Output data
+pointer	pout			#O Output mask (0=good, 1=bad)
+pointer	aout			#O Output averages
+pointer	sout			#O Output sigmas
+int	nc, nl			#I Number of columns and lines
+int	nl1, nl2		#I Lines to compute
+int	navg			#I Averaging box half-size
+int	nrej			#I Number of high pixels to reject from average
+int	nbkg			#I Median background width
+real	var0			#I Variance coefficient for DN^0 term
+real	var1			#I Variance coefficient for DN^1 term
+real	var2			#I Variance coefficient for DN^2 term
+int	nsig			#I Sigma box size
+real	lcrsig, hcrsig		#I Threshold sigmas outside of object
+real	lobjsig, hobjsig	#I Object threshold sigmas
+int	crval			#I CR mask value
+int	objval			#I Object mask value
+
+int	i, j, c, c1, c2, c3, c4, l, l1, l2, l3, l4, n1, n2
+int	navg2, nbkg2, nsig2, plsig, phsig
+real	data, avg, bkg, sigma, losig, hosig
+real	low, high, cravg(), amedr()
+pointer	stack, avgs, bkgs, sigs, work1, work2
+pointer	ptr1, ptr2, ip, op, pp, ap, sp
+
+begin
+	navg2 = (2 * navg + 1) ** 2
+	nbkg2 = (2 * (navg + nbkg) + 1) ** 2 - navg2
+	nsig2 = nsig * nsig
+
+	call smark (stack)
+	call salloc (avgs, nc, TY_REAL)
+	call salloc (bkgs, nc, TY_REAL)
+	call salloc (sigs, nc, TY_REAL)
+	call salloc (work1, navg2, TY_REAL)
+	call salloc (work2, max (nsig2, nbkg2), TY_REAL)
+
+	if (var0 != 0. && var1 == 0. && var2 ==0.)
+	    call amovkr (sqrt(var0), Memr[sigs], nc)
+
+	avgs = avgs - 1
+	sigs = sigs - 1
+	bkgs = bkgs - 1
+
+	plsig = nint (PLSIG*nsig2/100.-1)
+	phsig = nint (PHSIG*nsig2/100.-1)
+	losig = lobjsig / sqrt (real(navg2-1))
+	hosig = hobjsig / sqrt (real(navg2-1))
+
+	do l = nl1, nl2 {
+	    # Compute statistics.
+	    l1 = max (1, l-navg-nbkg)
+	    l2 = max (1, l-navg)
+	    l3 = min (nl, l+navg)
+	    l4 = min (nl, l+navg+nbkg)
+	    ap = aout + (l - 1) * nc
+	    do c = 1, nc {
+		c1 = max (1, c-navg-nbkg)
+		c2 = max (1, c-navg)
+		c3 = min (nc, c+navg)
+		c4 = min (nc, c+navg+nbkg)
+		ptr1 = work1
+		ptr2 = work2
+		n1 = 0
+		n2 = 0
+		do j = l1, l2-1 {
+		    ip = in + (j - 1) * nc + c1 - 1
+		    do i = c1, c4 {
+			Memr[ptr2] = Memr[ip]
+			n2 = n2 + 1
+			ptr2 = ptr2 + 1
+			ip = ip + 1
+		    }
+		}
+		do j = l2, l3 {
+		    ip = in + (j - 1) * nc + c1 - 1
+		    do i = c1, c2-1 {
+			Memr[ptr2] = Memr[ip]
+			n2 = n2 + 1
+			ptr2 = ptr2 + 1
+			ip = ip + 1
+		    }
+		    do i = c2, c3 {
+			if (j != l || i != c) {
+			    Memr[ptr1] = Memr[ip]
+			    n1 = n1 + 1
+			    ptr1 = ptr1 + 1
+			}
+			ip = ip + 1
+		    }
+		    do i = c3+1, c4 {
+			Memr[ptr2] = Memr[ip]
+			n2 = n2 + 1
+			ptr2 = ptr2 + 1
+			ip = ip + 1
+		    }
+		}
+		do j = l3+1, l4 {
+		    ip = in + (j - 1) * nc + c1 - 1
+		    do i = c1, c4 {
+			Memr[ptr2] = Memr[ip]
+			n2 = n2 + 1
+			ptr2 = ptr2 + 1
+			ip = ip + 1
+		    }
+		}
+		avg = cravg (Memr[work1], n1, nrej)
+		bkg = amedr (Memr[work2], n2)
+		Memr[bkgs+c] = bkg
+		Memr[avgs+c] = avg
+		if (aout != NULL) {
+		    Memr[ap] = avg - bkg
+		    ap = ap + 1
+		}
+	    }
+
+	    # Compute sigmas and output if desired.
+	    if (var0 != 0. || var1 != 0. || var2 != 0.) {
+		if (var1 != 0.) {
+		    if (var2 != 0.) {
+			do c = 1, nc {
+			    data = max (0., Memr[avgs+c])
+			    Memr[sigs+c] = sqrt (var0+var1*data+var2*data**2)
+			}
+		    } else {
+			do c = 1, nc {
+			    data = max (0., Memr[avgs+c])
+			    Memr[sigs+c] = sqrt (var0 + var1 * data)
+			}
+		    }
+		} else if (var2 != 0.) {
+		    do c = 1, nc {
+			data = max (0., Memr[avgs+c])
+			Memr[sigs+c] = sqrt (var0 + var2 * data**2)
+		    }
+		}
+	    } else {
+		# Compute sigmas from percentiles.  This is done in blocks.
+		if (mod (l-nl1, nsig) == 0 && l<nl-nsig+1) {
+		    do c = 1, nc-nsig+1, nsig {
+			ptr2 = work2
+			n2 = 0
+			do j = l, l+nsig-1 {
+			    ip = in + (j - 1) * nc + c - 1
+			    do i = 1, nsig {
+				Memr[ptr2] = Memr[ip]
+				n2 = n2 + 1
+				ptr2 = ptr2 + 1
+				ip = ip + 1
+			    }
+			}
+			call asrtr (Memr[work2], Memr[work2], n2)
+			sigma = (Memr[work2+phsig] - Memr[work2+plsig]) / 2.
+			call amovkr (sigma, Memr[sigs+c], nsig)
+		    }
+		    call amovkr (sigma, Memr[sigs+c], nc-c+1)
+		}
+	    }
+	    if (sout != NULL) {
+		sp = sout + (l - 1) * nc
+		do c = 1, nc {
+		    Memr[sp] = Memr[sigs+c]
+		    sp = sp + 1
+		}
+	    }
+
+	    # Detect, fix, and flag cosmic rays.
+	    if (pout == NULL && out == NULL)
+		;
+	    else if (pout == NULL) {
+		ip = in + (l - 1) * nc
+		op = out + (l - 1) * nc
+		do c = 1, nc {
+		    data = Memr[ip]
+		    avg = Memr[avgs+c]
+		    bkg = Memr[bkgs+c]
+		    sigma = Memr[sigs+c]
+		    low = bkg - losig * sigma
+		    high = bkg + hosig * sigma
+		    if (avg < low || avg > high) {
+			Memr[op] = data
+		    } else {
+			low = avg - lcrsig * sigma
+			high = avg + hcrsig * sigma
+			if (data < low || data > high)
+			    Memr[op] = avg
+			else
+			    Memr[op] = data
+		    }
+		    ip = ip + 1
+		    op = op + 1
+		}
+	    } else if (out == NULL) {
+		ip = in + (l - 1) * nc
+		pp = pout + (l - 1) * nc
+		do c = 1, nc {
+		    data = Memr[ip]
+		    avg = Memr[avgs+c]
+		    bkg = Memr[bkgs+c]
+		    sigma = Memr[sigs+c]
+		    low = bkg - losig * sigma
+		    high = bkg + hosig * sigma
+		    if (avg < low || avg > high)
+			Mems[pp] = objval
+		    else {
+			low = avg - lcrsig * sigma
+			high = avg + hcrsig * sigma
+			if (data < low || data > high)
+			    Mems[pp] = crval
+		    }
+		    ip = ip + 1
+		    pp = pp + 1
+		}
+	    } else {
+		ip = in + (l - 1) * nc
+		op = out + (l - 1) * nc
+		pp = pout + (l - 1) * nc
+		do c = 1, nc {
+		    data = Memr[ip]
+		    avg = Memr[avgs+c]
+		    bkg = Memr[bkgs+c]
+		    sigma = Memr[sigs+c]
+		    low = bkg - losig * sigma
+		    high = bkg + hosig * sigma
+		    if (avg < low || avg > high) {
+			Memr[op] = data
+			Mems[pp] = objval
+		    } else {
+			low = avg - lcrsig * sigma
+			high = avg + hcrsig * sigma
+			if (data < low || data > high) {
+			    Memr[op] = avg
+			    Mems[pp] = crval
+			} else
+			    Memr[op] = data
+		    }
+		    ip = ip + 1
+		    op = op + 1
+		    pp = pp + 1
+		}
+	    }
+	}
+
+	call sfree (stack)
+end
+
+
+# CRAVERAGE1 -- Detect, replace, and flag cosmic rays checking input mask.
+# A local background is computed using moving box averages to avoid
+# contaminating bad pixels.  If variance model is given then that is
+# used otherwise a local sigma is computed in blocks (it is not a moving box
+# for efficiency) by using a percentile point of the sorted pixel values to
+# estimate the width of the distribution uncontaminated by bad pixels).  Once
+# the background and sigma are known deviant pixels are found by using sigma
+# threshold factors.
+
+procedure craverage1 (in, pin, out, pout, aout, sout, nc, nl, nl1, nl2,
+	navg, nrej, nbkg, var0, var1, var2, nsig, lcrsig, hcrsig,
+	lobjsig, hobjsig crval, objval)
+
+pointer	in			#I Input data
+pointer	pin			#I Pixel mask data
+pointer	out			#O Output data
+pointer	pout			#O Output mask (0=good, 1=bad)
+pointer	aout			#O Output averages
+pointer	sout			#O Output sigmas
+int	nc, nl			#I Number of columns and lines
+int	nl1, nl2		#I Lines to compute
+int	navg			#I Averaging box half-size
+int	nrej			#I Number of high pixels to reject from average
+int	nbkg			#I Median background width
+real	var0			#I Variance coefficient for DN^0 term
+real	var1			#I Variance coefficient for DN^1 term
+real	var2			#I Variance coefficient for DN^2 term
+int	nsig			#I Sigma box size
+real	lcrsig, hcrsig		#I Threshold sigmas outside of object
+real	lobjsig, hobjsig	#I Object threshold sigmas
+int	crval			#I CR mask value
+int	objval			#I Object mask value
+
+int	i, j, c, c1, c2, c3, c4, l, l1, l2, l3, l4, n1, n2
+int	navg2, nbkg2, nsig2, plsig, phsig
+real	data, avg, bkg, sigma, losig, hosig
+real	low, high, cravg(), amedr()
+pointer	stack, avgs, bkgs, sigs, work1, work2
+pointer	ptr1, ptr2, ip, mp, op, pp, ap, sp
+
+begin
+	navg2 = (2 * navg + 1) ** 2
+	nbkg2 = (2 * (navg + nbkg) + 1) ** 2 - navg2
+	nsig2 = nsig * nsig
+
+	call smark (stack)
+	call salloc (avgs, nc, TY_REAL)
+	call salloc (bkgs, nc, TY_REAL)
+	call salloc (sigs, nc, TY_REAL)
+	call salloc (work1, navg2, TY_REAL)
+	call salloc (work2, max (nsig2, nbkg2), TY_REAL)
+
+	if (var0 != 0. && var1 == 0. && var2 ==0.)
+	    call amovkr (sqrt(var0), Memr[sigs], nc)
+
+	avgs = avgs - 1
+	sigs = sigs - 1
+	bkgs = bkgs - 1
+
+	losig = lobjsig / sqrt (real(navg2-1))
+	hosig = hobjsig / sqrt (real(navg2-1))
+
+	do l = nl1, nl2 {
+	    # Compute statistics.
+	    l1 = max (1, l-navg-nbkg)
+	    l2 = max (1, l-navg)
+	    l3 = min (nl, l+navg)
+	    l4 = min (nl, l+navg+nbkg)
+	    ap = aout + (l - 1) * nc
+	    do c = 1, nc {
+		c1 = max (1, c-navg-nbkg)
+		c2 = max (1, c-navg)
+		c3 = min (nc, c+navg)
+		c4 = min (nc, c+navg+nbkg)
+		ptr1 = work1
+		ptr2 = work2
+		n1 = 0
+		n2 = 0
+		do j = l1, l2-1 {
+		    ip = in + (j - 1) * nc + c1 - 1
+		    mp = pin + (j - 1) * nc + c1 - 1
+		    do i = c1, c4 {
+			if (Mems[mp] == 0) {
+			    Memr[ptr2] = Memr[ip]
+			    n2 = n2 + 1
+			    ptr2 = ptr2 + 1
+			}
+			ip = ip + 1
+			mp = mp + 1
+		    }
+		}
+		do j = l2, l3 {
+		    ip = in + (j - 1) * nc + c1 - 1
+		    mp = pin + (j - 1) * nc + c1 - 1
+		    do i = c1, c2-1 {
+			if (Mems[mp] == 0) {
+			    Memr[ptr2] = Memr[ip]
+			    n2 = n2 + 1
+			    ptr2 = ptr2 + 1
+			}
+			ip = ip + 1
+			mp = mp + 1
+		    }
+		    do i = c2, c3 {
+			if ((j != l || i != c) && Mems[mp] == 0) {
+			    Memr[ptr1] = Memr[ip]
+			    n1 = n1 + 1
+			    ptr1 = ptr1 + 1
+			}
+			ip = ip + 1
+			mp = mp + 1
+		    }
+		    do i = c3+1, c4 {
+			if (Mems[mp] == 0) {
+			    Memr[ptr2] = Memr[ip]
+			    n2 = n2 + 1
+			    ptr2 = ptr2 + 1
+			}
+			ip = ip + 1
+			mp = mp + 1
+		    }
+		}
+		do j = l3+1, l4 {
+		    ip = in + (j - 1) * nc + c1 - 1
+		    mp = pin + (j - 1) * nc + c1 - 1
+		    do i = c1, c4 {
+			if (Mems[mp] == 0) {
+			    Memr[ptr2] = Memr[ip]
+			    n2 = n2 + 1
+			    ptr2 = ptr2 + 1
+			}
+			ip = ip + 1
+		    }
+		}
+		if (n1 > 0)
+		    avg = cravg (Memr[work1], n1, nrej)
+		else
+		    avg = INDEFR
+		if (n2 > 0)
+		    bkg = amedr (Memr[work2], n2)
+		else
+		    bkg = INDEFR
+		Memr[bkgs+c] = bkg
+		Memr[avgs+c] = avg
+		if (aout != NULL) {
+		    if (IS_INDEFR(avg) || IS_INDEFR(bkg))
+			Memr[ap] = 0.
+		    else
+			Memr[ap] = avg - bkg
+		    ap = ap + 1
+		}
+	    }
+
+	    # Compute sigmas and output if desired.
+	    if (var0 != 0. || var1 != 0. || var2 != 0.) {
+		if (var1 != 0.) {
+		    if (var2 != 0.) {
+			do c = 1, nc {
+			    data = max (0., Memr[avgs+c])
+			    Memr[sigs+c] = sqrt (var0+var1*data+var2*data**2)
+			}
+		    } else {
+			do c = 1, nc {
+			    data = max (0., Memr[avgs+c])
+			    Memr[sigs+c] = sqrt (var0 + var1 * data)
+			}
+		    }
+		} else if (var2 != 0.) {
+		    do c = 1, nc {
+			data = max (0., Memr[avgs+c])
+			Memr[sigs+c] = sqrt (var0 + var2 * data**2)
+		    }
+		}
+	    } else {
+		# Compute sigmas from percentiles.  This is done in blocks.
+		if (mod (l-nl1, nsig) == 0 && l<nl-nsig+1) {
+		    do c = 1, nc-nsig+1, nsig {
+			ptr2 = work2
+			n2 = 0
+			do j = l, l+nsig-1 {
+			    ip = in + (j - 1) * nc + c - 1
+			    mp = pin + (j - 1) * nc + c - 1
+			    do i = 1, nsig {
+				if (Mems[mp] == 0) {
+				    Memr[ptr2] = Memr[ip]
+				    n2 = n2 + 1
+				    ptr2 = ptr2 + 1
+				}
+				ip = ip + 1
+				mp = mp + 1
+			    }
+			}
+			if (n2 > 10) {
+			    call asrtr (Memr[work2], Memr[work2], n2)
+			    plsig = nint (PLSIG*n2/100.-1)
+			    phsig = nint (PHSIG*n2/100.-1)
+			    sigma = (Memr[work2+phsig]-Memr[work2+plsig])/2.
+			} else
+			    sigma = INDEFR
+			call amovkr (sigma, Memr[sigs+c], nsig)
+		    }
+		    call amovkr (sigma, Memr[sigs+c], nc-c+1)
+		}
+	    }
+	    if (sout != NULL) {
+		sp = sout + (l - 1) * nc
+		do c = 1, nc {
+		    sigma = Memr[sigs+c]
+		    if (IS_INDEFR(sigma))
+			Memr[sp] = 0.
+		    else
+			Memr[sp] = sigma
+		    sp = sp + 1
+		}
+	    }
+
+	    # Detect, fix, and flag cosmic rays.
+	    if (pout == NULL && out == NULL)
+		;
+	    if (pout == NULL) {
+		ip = in + (l - 1) * nc
+		mp = pin + (l - 1) * nc
+		op = out + (l - 1) * nc
+		do c = 1, nc {
+		    data = Memr[ip]
+		    avg = Memr[avgs+c]
+		    bkg = Memr[bkgs+c]
+		    sigma = Memr[sigs+c]
+		    if (!(Mems[mp] != 0 || IS_INDEFR(avg) ||
+			IS_INDEFR(bkg) || IS_INDEFR(sigma))) {
+			low = bkg - losig * sigma
+			high = bkg + hosig * sigma
+			if (avg < low || avg > high) {
+			    Memr[op] = data
+			} else {
+			    low = avg - lcrsig * sigma
+			    high = avg + hcrsig * sigma
+			    if (data < low || data > high)
+				Memr[op] = avg
+			    else
+				Memr[op] = data
+			}
+		    } else
+			Memr[op] = data
+		    ip = ip + 1
+		    mp = mp + 1
+		    op = op + 1
+		}
+	    } else if (out == NULL) {
+		ip = in + (l - 1) * nc
+		mp = pin + (l - 1) * nc
+		pp = pout + (l - 1) * nc
+		do c = 1, nc {
+		    data = Memr[ip]
+		    avg = Memr[avgs+c]
+		    bkg = Memr[bkgs+c]
+		    sigma = Memr[sigs+c]
+		    if (!(Mems[mp] != 0 || IS_INDEFR(avg) ||
+			IS_INDEFR(bkg) || IS_INDEFR(sigma))) {
+			low = bkg - losig * sigma
+			high = bkg + hosig * sigma
+			if (avg < low || avg > high)
+			    Mems[pp] = objval
+			else {
+			    low = avg - lcrsig * sigma
+			    high = avg + hcrsig * sigma
+			    if (data < low || data > high)
+				Mems[pp] = crval
+			}
+		    }
+		    ip = ip + 1
+		    mp = mp + 1
+		    pp = pp + 1
+		}
+	    } else {
+		ip = in + (l - 1) * nc
+		mp = pin + (l - 1) * nc
+		op = out + (l - 1) * nc
+		pp = pout + (l - 1) * nc
+		do c = 1, nc {
+		    data = Memr[ip]
+		    avg = Memr[avgs+c]
+		    bkg = Memr[bkgs+c]
+		    sigma = Memr[sigs+c]
+		    if (!(Mems[mp] != 0 || IS_INDEFR(avg) ||
+			IS_INDEFR(bkg) || IS_INDEFR(sigma))) {
+			low = bkg - losig * sigma
+			high = bkg + hosig * sigma
+			if (avg < low || avg > high) {
+			    Memr[op] = data
+			    Mems[pp] = objval
+			} else {
+			    low = avg - lcrsig * sigma
+			    high = avg + hcrsig * sigma
+			    if (data < low || data > high) {
+				Memr[op] = avg
+				Mems[pp] = crval
+			    } else
+				Memr[op] = data
+			}
+		    } else
+			Memr[op] = data
+		    ip = ip + 1
+		    mp = mp + 1
+		    op = op + 1
+		    pp = pp + 1
+		}
+	    }
+	}
+
+	call sfree (stack)
+end
+
+
+# CRAVG -- Compute average with the highest nrej points excluded.
+# When nrej is greater than 2 the data array will be returned sorted.
+
+real procedure cravg (data, npts, nrej)
+
+real	data[npts]		#I Input data (will be sorted if nrej>2)
+int	npts			#I Number of data points
+int	nrej			#I Number of data points to reject
+
+int	i
+real	sum, max1, max2, val
+
+begin
+	if (npts <= nrej)
+	    return (INDEFR)
+
+	switch (nrej) {
+	case 0:
+	    sum = 0.
+	    do i = 1, npts
+		sum = sum + data[i]
+	case 1:
+	    sum = 0.
+	    max1 = data[1]
+	    do i = 2, npts {
+		val = data[i]
+		if (val > max1) {
+		    sum = sum + max1
+		    max1 = val
+		} else
+		    sum = sum + val
+	    }
+	case 2:
+	    sum = 0.
+	    max1 = min (data[1], data[2])
+	    max2 = max (data[1], data[2])
+	    do i = 3, npts {
+		val = data[i]
+		if (val > max1) {
+		    sum = sum + max1
+		    if (val > max2) {
+			max1 = max2
+			max2 = val
+		    } else
+			max1 = val
+		} else
+		    sum = sum + val
+	    }
+	default:
+	    call asrtr (data, data, npts)
+	    sum = 0.
+	    do i = 1, npts-nrej
+		sum = sum + data[i]
+	}
+
+	return (sum / (npts - nrej))
+end
diff --git a/noao/imred/crutil/src/t_crgrow.x b/noao/imred/crutil/src/t_crgrow.x
new file mode 100644
index 00000000..7316cc76
--- /dev/null
+++ b/noao/imred/crutil/src/t_crgrow.x
@@ -0,0 +1,182 @@
+include	<error.h>
+include	<imhdr.h>
+
+# T_CRGROW -- Grow cosmic ray mask identifications.
+
+procedure t_crgrow ()
+
+int	input				# Input masks
+int	output				# Output masks
+real	radius				# Radius
+int	inval				# Input mask value to grow
+int	outval				# Output grown mask value
+
+pointer	sp, inmask, outmask, temp1, temp2
+pointer	im, ptr
+
+int	imtopenp(), imtlen(), imtgetim()
+bool	strne()
+int	clgeti()
+real	clgetr()
+pointer	immap()
+errchk	immap, crgrow
+
+begin
+	call smark (sp)
+	call salloc (inmask, SZ_FNAME, TY_CHAR)
+	call salloc (outmask, SZ_FNAME, TY_CHAR)
+	call salloc (temp1, SZ_FNAME, TY_CHAR)
+	call salloc (temp2, SZ_FNAME, TY_CHAR)
+
+	# Task parameters.
+	input = imtopenp ("input")
+	output = imtopenp ("output")
+	radius = max (0., clgetr ("radius"))
+	inval = clgeti ("inval")
+	outval = clgeti ("outval")
+
+	if (imtlen (output) != imtlen (input))
+	    call error (1, "Input and output lists do not match")
+
+	# Grow the cosmic ray masks.
+	while (imtgetim (input, Memc[inmask], SZ_FNAME) != EOF) {
+	    call strcpy (Memc[inmask], Memc[outmask], SZ_FNAME)
+	    if (imtgetim (output, Memc[outmask], SZ_FNAME) == EOF)
+		call error (1, "Output list ended prematurely")
+	    if (strne (Memc[inmask], Memc[outmask])) {
+		call imgcluster (Memc[inmask], Memc[temp1], SZ_FNAME)
+		call imgcluster (Memc[outmask], Memc[temp2], SZ_FNAME)
+		iferr (call imcopy (Memc[temp1], Memc[temp2])) {
+		    call erract (EA_WARN)
+		    next
+		}
+		im = immap (Memc[inmask], READ_ONLY, TY_CHAR)
+		iferr (call imgstr (im, "extname", Memc[temp1], SZ_FNAME))
+		    call strcpy ("pl", Memc[temp1], SZ_FNAME)
+		call imunmap (im)
+	    }
+	    call xt_maskname (Memc[outmask], Memc[temp1], 0, Memc[outmask],
+		SZ_FNAME)
+
+	    if (radius < 1.)
+		next
+
+	    iferr {
+		im = NULL
+	        ptr = immap (Memc[outmask], READ_WRITE, 0); im = ptr
+		call crgrow (im, radius, inval, outval)
+	    } then {
+		call erract (EA_WARN)
+		if (strne (Memc[inmask], Memc[outmask])) {
+		    if (im != NULL) {
+			call imunmap (im)
+			iferr (call imdelete (Memc[outmask]))
+			    call erract (EA_WARN)
+		    }
+		}
+	    }
+
+	    if (im != NULL)
+		call imunmap (im)
+	}
+
+	call imtclose (output)
+	call imtclose (input)
+	call sfree (sp)
+end
+
+
+# CRGROW -- Grow cosmic rays.
+
+procedure crgrow (im, grow, inval, outval)
+
+pointer	im			# Mask pointer (Read/Write)
+real	grow			# Radius (pixels)
+int	inval			# Input mask value for pixels to grow
+int	outval			# Output mask value for grown pixels
+
+int	i, j, k, l, nc, nl, ngrow, nbufs, val1, val2
+long	v1[2], v2[2]
+real	grow2, y2
+pointer	, buf, buf1, buf2, ptr
+
+int	imgnli(), impnli()
+errchk	calloc, imgnli, impnli
+
+begin
+	if (grow < 1. || inval == 0)
+	    return
+
+	grow2 = grow * grow
+	ngrow = int (grow)
+	buf = NULL
+
+	iferr {
+	    if (IM_NDIM(im) > 2)
+		call error (1,
+		    "Only one or two dimensional masks are allowed")
+
+	    nc = IM_LEN(im, 1)
+	    if (IM_NDIM(im) > 1)
+		nl = IM_LEN(im,2)
+	    else
+		nl = 1
+
+	    # Initialize buffering.
+	    nbufs = min (1 + 2 * ngrow, nl)
+	    call calloc (buf, nc*nbufs, TY_INT)
+
+	    call amovkl (long(1), v1, IM_NDIM(im))
+	    call amovkl (long(1), v2, IM_NDIM(im))
+	    while (imgnli (im, buf1, v1) != EOF) {
+		j = v1[2] - 1
+		buf2 = buf + mod (j, nbufs) * nc
+		do i = 1, nc {
+		    val1 = Memi[buf1]
+		    val2 = Memi[buf2]
+		    if ((IS_INDEFI(inval) && val1 != 0) || val1 == inval) {
+			do k = max(1,j-ngrow), min (nl,j+ngrow) {
+			    ptr = buf + mod (k, nbufs) * nc - 1
+			    y2 = (k - j) ** 2
+			    do l = max(1,i-ngrow), min (nc,i+ngrow) {
+				if ((l-i)**2 + y2 > grow2)
+				    next
+				Memi[ptr+l] = -val1
+			    }
+			}
+		    } else {
+			if (val2 >= 0)
+			    Memi[buf2] = val1
+		    }
+		    buf1 = buf1 + 1
+		    buf2 = buf2 + 1
+		}
+
+		if (j > ngrow) {
+		    while (impnli (im, buf2, v2) != EOF) {
+			k = v2[2] - 1
+			buf1 = buf + mod (k, nbufs) * nc
+			do i = 1, nc {
+			    val1 = Memi[buf1]
+			    if (val1 < 0) {
+				if (IS_INDEFI(outval))
+				    Memi[buf2] = -val1
+				else 
+				    Memi[buf2] = outval
+			    } else
+				Memi[buf2] = val1
+			    Memi[buf1] = 0.
+			    buf1 = buf1 + 1
+			    buf2 = buf2 + 1
+			}
+			if (j != nl)
+			    break
+		    }
+		}
+	    }
+	} then
+	    call erract (EA_ERROR)
+
+	if (buf != NULL)
+	    call mfree (buf, TY_INT)
+end
diff --git a/noao/imred/crutil/src/t_crmedian.x b/noao/imred/crutil/src/t_crmedian.x
new file mode 100644
index 00000000..6c7d0fba
--- /dev/null
+++ b/noao/imred/crutil/src/t_crmedian.x
@@ -0,0 +1,417 @@
+include	<imhdr.h>
+include	<mach.h>
+
+define	MAXBUF		500000	# Maximum pixel buffer
+
+define	PLSIG		15.87	# Low percentile
+define	PHSIG		84.13	# High percentile
+
+
+# T_CRMEDIAN -- Detect, fix, and flag cosmic rays.
+# Deviant pixels relative to a local median and sigma are detected and
+# replaced by the median value and/or written to a cosmic ray mask.
+
+procedure t_crmedian ()
+
+pointer	input			# Input image
+pointer	output			# Output image
+pointer	crmask			# Output mask
+pointer	median			# Output median
+pointer	sigma			# Output sigma
+pointer	residual		# Output residual
+real	var0			# Variance coefficient for DN^0 term
+real	var1			# Variance coefficient for DN^1 term
+real	var2			# Variance coefficient for DN^2 term
+real	lsig, hsig		# Threshold sigmas
+int	ncmed, nlmed		# Median box size
+int	ncsig, nlsig		# Sigma box size
+
+int	i, nc, nl, nlstep, l1, l2, l3, l4, nl1
+pointer	sp, extname, in, out, pm, mim, sim, rim
+pointer	inbuf, outbuf, pmbuf, mbuf, sbuf, rbuf
+real	clgetr()
+int	clgeti(), nowhite()
+pointer	immap(), imgs2r(), imps2r(), imps2s()
+errchk	immap, imgs2r, imps2r, imps2s, crmedian, imgstr
+
+begin
+	call smark (sp)
+	call salloc (input, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (crmask, SZ_FNAME, TY_CHAR)
+	call salloc (residual, SZ_FNAME, TY_CHAR)
+	call salloc (median, SZ_FNAME, TY_CHAR)
+	call salloc (sigma, SZ_FNAME, TY_CHAR)
+	call salloc (extname, SZ_FNAME, TY_CHAR)
+
+	# Get parameters.
+	call clgstr ("input", Memc[input], SZ_FNAME)
+	call clgstr ("output", Memc[output], SZ_FNAME)
+	call clgstr ("crmask", Memc[crmask], SZ_FNAME)
+	call clgstr ("median", Memc[median], SZ_FNAME)
+	call clgstr ("sigma", Memc[sigma], SZ_FNAME)
+	call clgstr ("residual", Memc[residual], SZ_FNAME)
+	var0 = clgetr ("var0")
+	var1 = clgetr ("var1")
+	var2 = clgetr ("var2")
+	lsig = clgetr ("lsigma")
+	hsig = clgetr ("hsigma")
+	ncmed = clgeti ("ncmed")
+	nlmed = clgeti ("nlmed")
+	ncsig = clgeti ("ncsig")
+	nlsig = clgeti ("nlsig")
+
+	# Map the input and output images.
+	in = NULL; out = NULL; pm = NULL; mim = NULL; sim = NULL; rim = NULL
+	inbuf = NULL; outbuf = NULL; pmbuf = NULL
+	mbuf = NULL; sbuf=NULL; rbuf = NULL
+	in = immap (Memc[input], READ_ONLY, 0)
+	if (nowhite (Memc[output], Memc[output], SZ_FNAME) > 0)
+	    out = immap (Memc[output], NEW_COPY, in)
+	if (nowhite (Memc[crmask], Memc[crmask], SZ_FNAME) > 0) {
+	    if (Memc[crmask] == '!')
+		call imgstr (in, Memc[crmask+1], Memc[crmask], SZ_FNAME)
+	    iferr (call imgstr (in, "extname", Memc[extname], SZ_FNAME))
+		call strcpy ("pl", Memc[extname], SZ_FNAME)
+	    call xt_maskname (Memc[crmask], Memc[extname], 0, Memc[crmask],
+		SZ_FNAME)
+	    pm = immap (Memc[crmask], NEW_COPY, in)
+	}
+	if (nowhite (Memc[median], Memc[median], SZ_FNAME) > 0)
+	    mim = immap (Memc[median], NEW_COPY, in)
+	if (nowhite (Memc[sigma], Memc[sigma], SZ_FNAME) > 0)
+	    sim = immap (Memc[sigma], NEW_COPY, in)
+	if (nowhite (Memc[residual], Memc[residual], SZ_FNAME) > 0)
+	    rim = immap (Memc[residual], NEW_COPY, in)
+
+	# Go through the input in large blocks of lines.  If the
+	# block is smaller than the whole image overlap the blocks
+	# so the median only has boundaries at the ends of the image.
+	# However, the output is done in non-overlapping blocks with
+	# the pointers are adjusted so that addresses can be in the space
+	# of the input block.  CRMEDIAN does not address outside of
+	# the output data block.  Set the mask values based on the
+	# distances to the nearest good pixels.
+
+	nc = IM_LEN(in,1)
+	nl = IM_LEN(in,2)
+	nlstep = max (1, MAXBUF / nc - nlmed)
+
+	do i = 1, nl, nlstep {
+	    l1 = i
+	    l2 = min (nl, i + nlstep - 1)
+	    l3 = max (1, l1 - nlmed / 2)
+	    l4 = min (nl, l2 + nlmed / 2)
+	    nl1 = l4 - l3 + 1
+	    inbuf = imgs2r (in, 1, nc, l3, l4)
+	    if (out != NULL)
+		outbuf = imps2r (out, 1, nc, l1, l2) - (l1 - l3) * nc
+	    if (pm != NULL)
+		pmbuf = imps2s (pm, 1, nc, l1, l2) - (l1 - l3) * nc
+	    if (mim != NULL)
+		mbuf = imps2r (mim, 1, nc, l1, l2) - (l1 - l3) * nc
+	    if (sim != NULL)
+		sbuf = imps2r (sim, 1, nc, l1, l2) - (l1 - l3) * nc
+	    if (rim != NULL)
+		rbuf = imps2r (rim, 1, nc, l1, l2) - (l1 - l3) * nc
+	    call crmedian (inbuf, outbuf, pmbuf, mbuf, sbuf, rbuf,
+		nc, nl1, l1-l3+1, l2-l3+1, ncmed, nlmed, var0, var1, var2,
+		ncsig, nlsig, lsig, hsig)
+	}
+
+	if (rim != NULL)
+	    call imunmap (rim)
+	if (sim != NULL)
+	    call imunmap (sim)
+	if (mim != NULL)
+	    call imunmap (mim)
+	if (pm != NULL)
+	    call imunmap (pm)
+	if (out != NULL)
+	    call imunmap (out)
+	call imunmap (in)
+	call sfree (sp)
+end
+
+
+# CRMEDIAN -- Detect, replace, and flag cosmic rays.
+# A local background is computed using moving box medians to avoid
+# contaminating bad pixels.  If variance model is given then that is
+# used otherwise a local sigma is computed in blocks (it is not a moving box
+# for efficiency) by using a percentile point of the sorted pixel values to
+# estimate the width of the distribution uncontaminated by bad pixels).  Once
+# the background and sigma are known deviant pixels are found by using sigma
+# threshold factors.
+
+procedure crmedian (in, out, pout, mout, sout, rout, nc, nl, nl1, nl2,
+	ncmed, nlmed, var0, var1, var2, ncsig, nlsig, lsig, hsig)
+
+pointer	in			#I Input data
+pointer	out			#O Output data
+pointer	pout			#O Output mask (0=good, 1=bad)
+pointer	mout			#O Output medians
+pointer	sout			#O Output sigmas
+pointer	rout			#O Output residuals
+int	nc, nl			#I Number of columns and lines
+int	nl1, nl2		#I Lines to compute
+int	ncmed, nlmed		#I Median box size
+real	var0			# Variance coefficient for DN^0 term
+real	var1			# Variance coefficient for DN^1 term
+real	var2			# Variance coefficient for DN^2 term
+int	ncsig, nlsig		#I Sigma box size
+real	lsig, hsig		#I Threshold sigmas
+
+int	i, j, k, l, m, plsig, phsig
+real	data, med, sigma, low, high, amedr()
+pointer	stack, meds, sigs, work, ptr, ip, op, pp, mp, sp, rp
+
+begin
+	call smark (stack)
+	call salloc (meds, nc, TY_REAL)
+	call salloc (sigs, nc, TY_REAL)
+	call salloc (work, max (ncsig*nlsig, ncmed*nlmed), TY_REAL)
+
+	if (var0 != 0. && var1 == 0. && var2 ==0.)
+	    call amovkr (sqrt(var0), Memr[sigs], nc)
+
+	meds = meds - 1
+	sigs = sigs - 1
+
+	i = ncsig * nlsig
+	plsig = nint (PLSIG*i/100.-1)
+	phsig = nint (PHSIG*i/100.-1)
+
+	do i = nl1, nl2 {
+
+	    # Compute median and output if desired.  This is a moving median.
+	    l = min (nl, i+nlmed/2)
+	    l = max (1, l-nlmed+1)
+	    mp = mout + (i - 1) * nc 
+	    do j = 1, nc {
+		k = min (nc, j+ncmed/2)
+		k = max (1, k-ncmed+1)
+		ptr = work
+		ip = in + (l - 1) * nc + k - 1
+		do m = l, l+nlmed-1 {
+		    call amovr (Memr[ip], Memr[ptr], ncmed)
+		    ip = ip + nc
+		    ptr = ptr + ncmed
+		}
+		med = amedr (Memr[work], ncmed * nlmed)
+		Memr[meds+j] = med
+		if (mout != NULL) {
+		    Memr[mp] = med
+		    mp = mp + 1
+		}
+	    }
+
+	    # Compute sigmas and output if desired.
+	    if (var0 != 0. || var1 != 0. || var2 != 0.) {
+		if (var1 != 0.) {
+		    if (var2 != 0.) {
+			do j = 1, nc {
+			    data = max (0., Memr[meds+j])
+			    Memr[sigs+j] = sqrt (var0 + var1*data + var2*data**2)
+			}
+		    } else {
+			do j = 1, nc {
+			    data = max (0., Memr[meds+j])
+			    Memr[sigs+j] = sqrt (var0 + var1 * data)
+			}
+		    }
+		} else if (var2 != 0.) {
+		    do j = 1, nc {
+			data = max (0., Memr[meds+j])
+			Memr[sigs+j] = sqrt (var0 + var2 * data**2)
+		    }
+		}
+	    } else {
+		# Compute sigmas from percentiles.  This is done in blocks.
+		if (mod (i-nl1, nlsig) == 0 && i<nl-nlsig+1) {
+		    do j = 1, nc-ncsig+1, ncsig {
+			ptr = work
+			ip = in + (i - 1) * nc + j - 1
+			do k = i, i+nlsig-1 {
+			    call amovr (Memr[ip], Memr[ptr], ncsig)
+			    ip = ip + nc
+			    ptr = ptr + ncsig
+			}
+			call asrtr (Memr[work], Memr[work], ncsig*nlsig)
+			sigma = (Memr[work+phsig] - Memr[work+plsig]) / 2.
+			call amovkr (sigma, Memr[sigs+j], ncsig)
+		    }
+		    call amovkr (sigma, Memr[sigs+j], nc-j+1)
+		}
+	    }
+	    if (sout != NULL) {
+		sp = sout + (i - 1) * nc
+		do j = 1, nc {
+		    Memr[sp] = Memr[sigs+j]
+		    sp = sp + 1
+		}
+	    }
+
+	    # Detect, fix, and flag cosmic rays.
+	    if (rout == NULL) {
+		if (pout == NULL) {
+		    ip = in + (i - 1) * nc
+		    op = out + (i - 1) * nc
+		    do j = 1, nc {
+			data = Memr[ip]
+			med = Memr[meds+j]
+			sigma = Memr[sigs+j]
+			low = med - lsig * sigma
+			high = med + hsig * sigma
+			if (data < low || data > high)
+			    Memr[op] = med
+			else
+			    Memr[op] = data
+			ip = ip + 1
+			op = op + 1
+		    }
+		} else if (out == NULL) {
+		    ip = in + (i - 1) * nc
+		    pp = pout + (i - 1) * nc
+		    do j = 1, nc {
+			data = Memr[ip]
+			med = Memr[meds+j]
+			sigma = Memr[sigs+j]
+			low = med - lsig * sigma
+			high = med + hsig * sigma
+			if (data < low || data > high)
+			    Mems[pp] = 1
+			else
+			    Mems[pp] = 0
+			ip = ip + 1
+			pp = pp + 1
+		    }
+		} else {
+		    ip = in + (i - 1) * nc
+		    op = out + (i - 1) * nc
+		    pp = pout + (i - 1) * nc
+		    do j = 1, nc {
+			data = Memr[ip]
+			med = Memr[meds+j]
+			sigma = Memr[sigs+j]
+			low = med - lsig * sigma
+			high = med + hsig * sigma
+			if (data < low || data > high) {
+			    Memr[op] = med
+			    Mems[pp] = 1
+			} else {
+			    Memr[op] = data
+			    Mems[pp] = 0
+			}
+			ip = ip + 1
+			op = op + 1
+			pp = pp + 1
+		    }
+		}
+	    } else {
+		if (pout == NULL && out == NULL) {
+		    ip = in + (i - 1) * nc
+		    rp = rout + (i - 1) * nc
+		    do j = 1, nc {
+			data = Memr[ip]
+			med = Memr[meds+j]
+			sigma = Memr[sigs+j]
+			if (sigma > 0.)
+			    Memr[rp] = (data - med) / sigma
+			else {
+			    if ((data - med) < 0.)
+				Memr[rp] = -MAX_REAL
+			    else
+				Memr[rp] = MAX_REAL
+			}
+			ip = ip + 1
+			rp = rp + 1
+		    }
+		} else if (pout == NULL) {
+		    ip = in + (i - 1) * nc
+		    op = out + (i - 1) * nc
+		    rp = rout + (i - 1) * nc
+		    do j = 1, nc {
+			data = Memr[ip]
+			med = Memr[meds+j]
+			sigma = Memr[sigs+j]
+			low = med - lsig * sigma
+			high = med + hsig * sigma
+			if (data < low || data > high)
+			    Memr[op] = med
+			else
+			    Memr[op] = data
+			if (sigma > 0.)
+			    Memr[rp] = (data - med) / sigma
+			else {
+			    if ((data - med) < 0.)
+				Memr[rp] = -MAX_REAL
+			    else
+				Memr[rp] = MAX_REAL
+			}
+			ip = ip + 1
+			op = op + 1
+			rp = rp + 1
+		    }
+		} else if (out == NULL) {
+		    ip = in + (i - 1) * nc
+		    pp = pout + (i - 1) * nc
+		    rp = rout + (i - 1) * nc
+		    do j = 1, nc {
+			data = Memr[ip]
+			med = Memr[meds+j]
+			sigma = Memr[sigs+j]
+			low = med - lsig * sigma
+			high = med + hsig * sigma
+			if (data < low || data > high)
+			    Mems[pp] = 1
+			else
+			    Mems[pp] = 0
+			if (sigma > 0.)
+			    Memr[rp] = (data - med) / sigma
+			else {
+			    if ((data - med) < 0.)
+				Memr[rp] = -MAX_REAL
+			    else
+				Memr[rp] = MAX_REAL
+			}
+			ip = ip + 1
+			pp = pp + 1
+			rp = rp + 1
+		    }
+		} else {
+		    ip = in + (i - 1) * nc
+		    op = out + (i - 1) * nc
+		    pp = pout + (i - 1) * nc
+		    rp = rout + (i - 1) * nc
+		    do j = 1, nc {
+			data = Memr[ip]
+			med = Memr[meds+j]
+			sigma = Memr[sigs+j]
+			low = med - lsig * sigma
+			high = med + hsig * sigma
+			if (data < low || data > high) {
+			    Memr[op] = med
+			    Mems[pp] = 1
+			} else {
+			    Memr[op] = data
+			    Mems[pp] = 0
+			}
+			if (sigma > 0.)
+			    Memr[rp] = (data - med) / sigma
+			else {
+			    if ((data - med) < 0.)
+				Memr[rp] = -MAX_REAL
+			    else
+				Memr[rp] = MAX_REAL
+			}
+			ip = ip + 1
+			op = op + 1
+			pp = pp + 1
+			rp = rp + 1
+		    }
+		}
+	    }
+	}
+
+	call sfree (stack)
+end
diff --git a/noao/imred/crutil/src/x_crutil.x b/noao/imred/crutil/src/x_crutil.x
new file mode 100644
index 00000000..48408a9f
--- /dev/null
+++ b/noao/imred/crutil/src/x_crutil.x
@@ -0,0 +1,4 @@
+task	cosmicrays	= t_cosmicrays,
+	craverage	= t_craverage,
+	crgrow		= t_crgrow,
+	crmedian	= t_crmedian
diff --git a/noao/imred/crutil/src/xtmaskname.x b/noao/imred/crutil/src/xtmaskname.x
new file mode 100644
index 00000000..eb132e12
--- /dev/null
+++ b/noao/imred/crutil/src/xtmaskname.x
@@ -0,0 +1,125 @@
+# MASKNAME -- Make a mask name.  This creates a FITS mask extension if
+# possible, otherwise it creates a pixel list file.  To create a FITS
+# extension the filename must explicitly select the FITS kernel or the
+# default image type must be a FITS file.  The input and output strings
+# may be the same.
+
+procedure xt_maskname (fname, extname, mode, mname, maxchar)
+
+char	fname[ARB]			#I File name
+char	extname[ARB]			#I Default pixel mask extension name
+int	mode				#I Mode
+char	mname[maxchar]			#O Output mask name
+int	maxchar				#I Maximum characters in mask name
+
+int	i, fits
+pointer	sp, temp
+
+bool	streq()
+int	strmatch(), stridxs(), strldxs(), strncmp()
+int	envfind(), access(), imaccess()
+
+begin
+	call smark (sp)
+	call salloc (temp, maxchar, TY_CHAR)
+
+	# Determine whether to use FITS pixel mask extensions.  One may set
+	# fits=NO to force use of pl even when FITS mask extensions are
+	# supported.
+	fits = YES
+	if (fits == YES && envfind ("masktype", Memc[temp], maxchar) > 0) {
+	    if (streq (Memc[temp], "pl"))
+		fits = NO
+	}
+	i = strldxs ("]", fname)
+
+	# Check for explicit .pl extension.
+	if (strmatch (fname, ".pl$") > 0)
+	    call strcpy (fname, mname, maxchar)
+
+	# Check for explicit mask extension.
+	else if (strmatch (fname, "type=mask") > 0)
+	    call strcpy (fname, mname, maxchar)
+	else if (strmatch (fname, "type\\\=mask") > 0)
+	    call strcpy (fname, mname, maxchar)
+
+	# Add mask type.
+	else if (i > 0) {
+	    if (mode != READ_ONLY) {
+		call strcpy (fname[i], Memc[temp], maxchar)
+		call sprintf (mname[i], maxchar-i, ",type=mask%s")
+		    call pargstr (Memc[temp])
+	    }
+	    i = stridxs ("[", mname)
+	    if (i > 0) {
+		call strcpy (mname[i+1], Memc[temp], SZ_FNAME)
+		if (strncmp (mname[i+1], "append", 6)==0 ||
+		    strncmp (mname[i+1], "inherit", 7)==0) {
+		    call sprintf (mname[i+1], SZ_FNAME-i+1, "%s,%s")
+			call pargstr (extname)
+			call pargstr (Memc[temp])
+		}
+	    }
+
+	# Create output from rootname name.
+	} else if (fits == YES) {
+	    call strcpy (fname, Memc[temp], SZ_FNAME)
+	    if (mode == READ_ONLY) {
+		call sprintf (mname, maxchar, "%s[%s]")
+		    call pargstr (Memc[temp])
+		    call pargstr (extname)
+	    } else {
+		call sprintf (mname, maxchar, "%s[%s,type=mask]")
+		    call pargstr (Memc[temp])
+		    call pargstr (extname)
+	    }
+	} else
+	    call strcat (".pl", mname, maxchar)
+
+	# Check if extension name is actually given.
+	i = stridxs ("[", mname)
+	if (i > 0) {
+	    call strcpy (mname[i+1], Memc[temp], SZ_FNAME)
+	    if (strncmp (mname[i+1], "append", 6)==0 ||
+		strncmp (mname[i+1], "inherit", 7)==0) {
+		call sprintf (mname[i+1], SZ_FNAME-i+1, "%s,%s")
+		    call pargstr (extname)
+		    call pargstr (Memc[temp])
+	    }
+	}
+		
+	# Convert to pl form if required.
+	i = stridxs ("[", mname)
+	if (i > 0 && mode == READ_ONLY)
+	    fits = imaccess (mname, mode)
+	if (fits == NO && i > 0) {
+	    mname[i] = EOS
+	    if (mode == NEW_IMAGE) {
+		if (access (mname, 0, 0) == NO) {
+		    ifnoerr (call fmkdir (mname))
+			mname[i] =  '/'
+		    else
+			mname[i] = '.'
+		} else
+		    mname[i] =  '/'
+	    } else {
+		if (access (mname, 0, 0) == NO)
+		    mname[i] = '.'
+		else
+		    mname[i] =  '/'
+	    }
+	        
+	    if (strncmp (mname[i+1], "type", 4) == 0 ||
+	        strncmp (mname[i+1], "append", 6) == 0 ||
+	        strncmp (mname[i+1], "inherit", 7) == 0) {
+		mname[i+1] = EOS
+		call strcat (extname, mname, maxchar)
+	    } else {
+		i = stridxs (",]", mname)
+		mname[i] = EOS
+	    }
+	    call strcat (".pl", mname, maxchar)
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/ctioslit/Revisions b/noao/imred/ctioslit/Revisions
new file mode 100644
index 00000000..28f900fd
--- /dev/null
+++ b/noao/imred/ctioslit/Revisions
@@ -0,0 +1,26 @@
+.help revisions Dec94 noao.imred.ctioslit
+.nf
+
+=====
+V2.12
+=====
+
+imred$ctioslit/standard.par
+    Added blackbody query parameters.  (5/2/02, Valdes)
+
+========
+V2.11.3b
+========
+
+imred$ctioslit/demos/mkdoslit.cl
+    Made the ARTDATA package parameters explicit (4/15/97, Valdes)
+
+imred$ctioslit/sparams.par
+    Changed match from 10. to -3.  (4/5/96, Valdes)
+
+imred$ctioslit/ctioslit.cl
+imred$ctioslit/ctioslit.men
+    Added background, illumination, response, apflatten, apnormalize.
+    (12/29/94, Valdes)
+
+.endhelp
diff --git a/noao/imred/ctioslit/calibrate.par b/noao/imred/ctioslit/calibrate.par
new file mode 100644
index 00000000..e09457a2
--- /dev/null
+++ b/noao/imred/ctioslit/calibrate.par
@@ -0,0 +1,13 @@
+# CALIBRATE parameter file
+
+input,s,a,,,,Input spectra to calibrate
+output,s,a,,,,Output calibrated spectra
+extinct,b,h,yes,,,Apply extinction correction?
+flux,b,h,yes,,,Apply flux calibration?
+extinction,s,h,)_.extinction,,,Extinction file
+observatory,s,h,)_.observatory,,,Observatory of observation
+ignoreaps,b,h,yes,,,Ignore aperture numbers in flux calibration?
+sensitivity,s,h,"sens",,,Image root name for sensitivity spectra
+fnu,b,h,no,,,Create spectra having units of FNU?
+airmass,r,q,,1.,,Airmass
+exptime,r,q,,,,Exposure time (seconds)
diff --git a/noao/imred/ctioslit/ctioslit.cl b/noao/imred/ctioslit/ctioslit.cl
new file mode 100644
index 00000000..abc2a1f3
--- /dev/null
+++ b/noao/imred/ctioslit/ctioslit.cl
@@ -0,0 +1,69 @@
+#{ CTIOSLIT package definition
+
+# Define CTIOSLIT package
+package ctioslit
+
+set	demos		= "ctioslit$demos/"
+
+# Slitproc
+cl < doslit$doslittasks.cl
+task	sparams		= "ctioslit$sparams.par"
+
+# Onedspec tasks
+task	autoidentify,
+	continuum,
+	deredden,
+	dispcor,
+	dopcor,
+	identify,
+	refspectra,
+	reidentify,
+	sarith,
+	sflip,
+	slist,
+	splot,
+	specplot,
+	specshift	= "onedspec$x_onedspec.e"
+task	scombine	= "onedspec$scombine/x_scombine.e"
+task	aidpars		= "onedspec$aidpars.par"
+task	bplot		= "onedspec$bplot.cl"
+task	scopy		= "onedspec$scopy.cl"
+task	dispcor1	= "onedspec$dispcor1.par"
+
+# Different default parameters
+task	calibrate,
+	sensfunc,
+	standard	= "ctioslit$x_onedspec.e"
+
+# Apextract tasks
+task	apall,
+	apedit,
+	apfind,
+	apflatten,
+	apnormalize,
+	aprecenter,
+	apresize,
+	apsum,
+	aptrace		= "apextract$x_apextract.e"
+task	apdefault	= "apextract$apdefault.par"
+task	apparams	= "apextract$apparams.par"
+task	apall1		= "apextract$apall1.par"
+task	apflat1		= "apextract$apflat1.par"
+task	apnorm1		= "apextract$apflat1.par"
+
+# Longslit tasks
+task	illumination,
+	response	= "twodspec$longslit/x_longslit.e"
+task	background	= "generic$background.cl"
+
+# Astutil tasks
+task	setairmass,
+	setjd		= "astutil$x_astutil.e"
+
+# Demos
+task	demos		= "demos$demos.cl"
+
+# Hide tasks from the user
+hidetask apparams, apall1, apflat1, apnorm1, dispcor1, sparams
+
+clbye()
diff --git a/noao/imred/ctioslit/ctioslit.hd b/noao/imred/ctioslit/ctioslit.hd
new file mode 100644
index 00000000..3ce338e7
--- /dev/null
+++ b/noao/imred/ctioslit/ctioslit.hd
@@ -0,0 +1 @@
+# Help directory for the CTIOSLIT package.
diff --git a/noao/imred/ctioslit/ctioslit.men b/noao/imred/ctioslit/ctioslit.men
new file mode 100644
index 00000000..31c74dd0
--- /dev/null
+++ b/noao/imred/ctioslit/ctioslit.men
@@ -0,0 +1,38 @@
+          apall - Extract 1D spectra (all parameters in one task)
+      apdefault - Set the default aperture parameters
+         apedit - Edit apertures interactively
+	 apfind - Automatically find spectra and define apertures
+      apflatten - Remove overall spectral and profile shapes from flat fields
+    apnormalize - Normalize 2D apertures by 1D functions
+     aprecenter - Recenter apertures
+       apresize - Resize apertures
+          apsum - Extract 1D spectra
+	aptrace - Trace positions of spectra
+
+     background - Fit and subtract a line or column background
+	  bplot - Batch plot of spectra with SPLOT
+      calibrate - Apply extinction and flux calibrations to spectra
+      continuum - Fit and normalize the continuum of multispec spectra
+       deredden - Apply interstellar extinction corrections
+        dispcor - Dispersion correct spectra
+	 dopcor - Doppler correct spectra
+       identify - Identify arc lines and determine a dispersion function
+   illumination - Determine illumination calibration
+     refspectra - Assign reference spectra to observations
+     reidentify - Reidentify arc lines and determine new dispersion functions
+       response - Determine response calibration
+	 sarith - Spectrum arithmetic
+       scombine - Combine spectra
+          scopy - Copy spectra including aperture selection and format changes
+       sensfunc - Create sensitivity function
+     setairmass - Compute effective airmass and middle UT for an exposure
+          setjd - Compute and set Julian dates in images
+	  sflip - Flip data and/or dispersion coordinates in spectra
+          slist - List spectrum headers
+       specplot - Stack and plot multiple spectra
+      specshift - Shift spectral dispersion coordinate systems
+	  splot - Plot and analyze spectra
+       standard - Identify standard stars to be used in sensitivity calc
+
+         doslit - Process CTIO slit spectra
+	  demos - Demonstrations and tests
diff --git a/noao/imred/ctioslit/ctioslit.par b/noao/imred/ctioslit/ctioslit.par
new file mode 100644
index 00000000..4ed0fbf0
--- /dev/null
+++ b/noao/imred/ctioslit/ctioslit.par
@@ -0,0 +1,15 @@
+# CTIOSLIT parameter file
+extinction,s,h,onedstds$ctioextinct.dat,,,Extinction file
+caldir,s,h,onedstds$ctionewcal/,,,Standard star calibration directory
+observatory,s,h,"observatory",,,Observatory of data
+interp,s,h,"poly5","nearest|linear|poly3|poly5|spline3|sinc",,Interpolation type
+dispaxis,i,h,2,1,3,Image axis for 2D/3D images
+nsum,s,h,"1",,,"Number of lines/columns/bands to sum for 2D/3D images
+"
+database,f,h,"database",,,Database
+verbose,b,h,no,,,Verbose output?
+logfile,s,h,"logfile",,,Log file
+plotfile,s,h,"",,,"Plot file
+"
+records,s,h,"",,,Record number extensions
+version,s,h,"CTIOSLIT V3: January 1992"
diff --git a/noao/imred/ctioslit/demos/demoarc1.dat b/noao/imred/ctioslit/demos/demoarc1.dat
new file mode 100644
index 00000000..fa0a179d
--- /dev/null
+++ b/noao/imred/ctioslit/demos/demoarc1.dat
@@ -0,0 +1,38 @@
+    OBJECT  = 'First comp        '  /  object name
+    OBSERVAT= 'KPNO              '  /  observatory
+    OBSERVER= 'Massey            '  /  observers
+    COMMENTS= 'Final New Ice     '  /  comments
+    EXPTIME =                  60.  /  actual integration time
+    DARKTIME=                  60.  /  total elapsed time
+    IMAGETYP= 'comp              '  /  object, dark, bias, etc.
+    DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+    UT      = '12:11:30.00       '  /  universal time
+    ST      = '09:04:54.00       '  /  sidereal time
+    RA      = '06:37:02.00       '  /  right ascension
+    DEC     = '06:09:03.00       '  /  declination
+    EPOCH   =               1991.9  /  epoch of ra and dec
+    ZD      = '48.760            '  /  zenith distance
+    AIRMASS =                   0.  /  airmass
+    TELESCOP= 'kpcdf             '  /  telescope name
+    DETECTOR= 'te1k              '  /  detector
+    PREFLASH=                    0  /  preflash time, seconds
+    GAIN    =                  5.4  /  gain, electrons per adu
+    DWELL   =                    5  /  sample integration time
+    RDNOISE =                  3.5  /  read noise, electrons per adu
+    DELAY0  =                    0  /  time delay after each pixel
+    DELAY1  =                    0  /  time delay after each row
+    CAMTEMP =                 -111  /  camera temperature
+    DEWTEMP =                 -183  /  dewar temperature
+    CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+    ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+    CCDSUM  = '1 1               '  /  on chip summation
+    INSTRUME= 'test              '  /  instrument
+    APERTURE= '250micron slit    '  /  aperture
+    TVFILT  = '4-96              '  /  tv filter
+    DISPAXIS= '2                 '  /  dispersion axis
+    GRATPOS =               4624.3  /  grating position
+    TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+    OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+    ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+    CCDMEAN =              179.398
+    CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/ctioslit/demos/demoarc2.dat b/noao/imred/ctioslit/demos/demoarc2.dat
new file mode 100644
index 00000000..4cd9975d
--- /dev/null
+++ b/noao/imred/ctioslit/demos/demoarc2.dat
@@ -0,0 +1,38 @@
+    OBJECT  = 'Last comp         '  /  object name
+    OBSERVAT= 'KPNO              '  /  observatory
+    OBSERVER= 'Massey            '  /  observers
+    COMMENTS= 'Final New Ice     '  /  comments
+    EXPTIME =                  60.  /  actual integration time
+    DARKTIME=                  60.  /  total elapsed time
+    IMAGETYP= 'comp              '  /  object, dark, bias, etc.
+    DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+    UT      = '12:41:30.00       '  /  universal time
+    ST      = '09:34:54.00       '  /  sidereal time
+    RA      = '06:37:02.00       '  /  right ascension
+    DEC     = '06:09:03.00       '  /  declination
+    EPOCH   =               1991.9  /  epoch of ra and dec
+    ZD      = '48.760            '  /  zenith distance
+    AIRMASS =                   0.  /  airmass
+    TELESCOP= 'kpcdf             '  /  telescope name
+    DETECTOR= 'te1k              '  /  detector
+    PREFLASH=                    0  /  preflash time, seconds
+    GAIN    =                  5.4  /  gain, electrons per adu
+    DWELL   =                    5  /  sample integration time
+    RDNOISE =                  3.5  /  read noise, electrons per adu
+    DELAY0  =                    0  /  time delay after each pixel
+    DELAY1  =                    0  /  time delay after each row
+    CAMTEMP =                 -111  /  camera temperature
+    DEWTEMP =                 -183  /  dewar temperature
+    CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+    ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+    CCDSUM  = '1 1               '  /  on chip summation
+    INSTRUME= 'test              '  /  instrument
+    APERTURE= '250micron slit    '  /  aperture
+    TVFILT  = '4-96              '  /  tv filter
+    DISPAXIS= '2                 '  /  dispersion axis
+    GRATPOS =               4624.3  /  grating position
+    TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+    OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+    ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+    CCDMEAN =              179.398
+    CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/ctioslit/demos/demoobj1.dat b/noao/imred/ctioslit/demos/demoobj1.dat
new file mode 100644
index 00000000..78f3b9ad
--- /dev/null
+++ b/noao/imred/ctioslit/demos/demoobj1.dat
@@ -0,0 +1,37 @@
+    OBJECT  = 'V640Mon 4500      '  /  object name
+    OBSERVAT= 'KPNO              '  /  observatory
+    OBSERVER= 'Massey            '  /  observers
+    COMMENTS= 'Final New Ice     '  /  comments
+    EXPTIME =                1200.  /  actual integration time
+    DARKTIME=                1200.  /  total elapsed time
+    IMAGETYP= 'object            '  /  object, dark, bias, etc.
+    DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+    UT      = '12:19:55.00       '  /  universal time
+    ST      = '09:13:15.00       '  /  sidereal time
+    RA      = '06:37:02.00       '  /  right ascension
+    DEC     = '06:08:52.00       '  /  declination
+    EPOCH   =               1991.9  /  epoch of ra and dec
+    ZD      = '44.580            '  /  zenith distance
+    AIRMASS =                   0.  /  airmass
+    TELESCOP= 'kpcdf             '  /  telescope name
+    DETECTOR= 'te1k              '  /  detector
+    PREFLASH=                    0  /  preflash time, seconds
+    GAIN    =                  5.4  /  gain, electrons per adu
+    DWELL   =                    5  /  sample integration time
+    RDNOISE =                  3.5  /  read noise, electrons per adu
+    DELAY0  =                    0  /  time delay after each pixel
+    DELAY1  =                    0  /  time delay after each row
+    CAMTEMP =                 -111  /  camera temperature
+    DEWTEMP =                 -183  /  dewar temperature
+    CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+    ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+    CCDSUM  = '1 1               '  /  on chip summation
+    INSTRUME= 'test              '  /  instrument
+    APERTURE= '250micron slit    '  /  aperture
+    TVFILT  = '4-96              '  /  tv filter
+    DISPAXIS= '2                 '  /  dispersion axis
+    GRATPOS =               4624.3  /  grating position
+    TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+    OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+    ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+    CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/ctioslit/demos/demos.cl b/noao/imred/ctioslit/demos/demos.cl
new file mode 100644
index 00000000..5b065c51
--- /dev/null
+++ b/noao/imred/ctioslit/demos/demos.cl
@@ -0,0 +1,18 @@
+# DEMOS -- Run specified demo provided a demo file exists.
+
+procedure demos (demoname)
+
+file	demoname	{prompt="Demo name"}
+
+begin
+	file	demo, demofile
+
+	if ($nargs == 0 && mode != "h")
+	    type ("demos$demos.men")
+	demo = demoname
+	demofile = "demos$" // demo // ".cl"
+	if (access (demofile))
+	    cl (< demofile)
+	else
+	    error (1, "Unknown demo " // demo)
+end
diff --git a/noao/imred/ctioslit/demos/demos.men b/noao/imred/ctioslit/demos/demos.men
new file mode 100644
index 00000000..c6f83e09
--- /dev/null
+++ b/noao/imred/ctioslit/demos/demos.men
@@ -0,0 +1,4 @@
+	MENU of CTIOSLIT Demonstrations
+
+       doslit - Quick test of DOSLIT (no comments, no delays)
+     mkdoslit - Make DOSLIT test data
diff --git a/noao/imred/ctioslit/demos/demos.par b/noao/imred/ctioslit/demos/demos.par
new file mode 100644
index 00000000..4181ed59
--- /dev/null
+++ b/noao/imred/ctioslit/demos/demos.par
@@ -0,0 +1,2 @@
+demoname,f,a,"",,,"Demo name"
+mode,s,h,"ql",,,
diff --git a/noao/imred/ctioslit/demos/demostd1.dat b/noao/imred/ctioslit/demos/demostd1.dat
new file mode 100644
index 00000000..78f3b9ad
--- /dev/null
+++ b/noao/imred/ctioslit/demos/demostd1.dat
@@ -0,0 +1,37 @@
+    OBJECT  = 'V640Mon 4500      '  /  object name
+    OBSERVAT= 'KPNO              '  /  observatory
+    OBSERVER= 'Massey            '  /  observers
+    COMMENTS= 'Final New Ice     '  /  comments
+    EXPTIME =                1200.  /  actual integration time
+    DARKTIME=                1200.  /  total elapsed time
+    IMAGETYP= 'object            '  /  object, dark, bias, etc.
+    DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+    UT      = '12:19:55.00       '  /  universal time
+    ST      = '09:13:15.00       '  /  sidereal time
+    RA      = '06:37:02.00       '  /  right ascension
+    DEC     = '06:08:52.00       '  /  declination
+    EPOCH   =               1991.9  /  epoch of ra and dec
+    ZD      = '44.580            '  /  zenith distance
+    AIRMASS =                   0.  /  airmass
+    TELESCOP= 'kpcdf             '  /  telescope name
+    DETECTOR= 'te1k              '  /  detector
+    PREFLASH=                    0  /  preflash time, seconds
+    GAIN    =                  5.4  /  gain, electrons per adu
+    DWELL   =                    5  /  sample integration time
+    RDNOISE =                  3.5  /  read noise, electrons per adu
+    DELAY0  =                    0  /  time delay after each pixel
+    DELAY1  =                    0  /  time delay after each row
+    CAMTEMP =                 -111  /  camera temperature
+    DEWTEMP =                 -183  /  dewar temperature
+    CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+    ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+    CCDSUM  = '1 1               '  /  on chip summation
+    INSTRUME= 'test              '  /  instrument
+    APERTURE= '250micron slit    '  /  aperture
+    TVFILT  = '4-96              '  /  tv filter
+    DISPAXIS= '2                 '  /  dispersion axis
+    GRATPOS =               4624.3  /  grating position
+    TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+    OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+    ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+    CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/ctioslit/demos/doslit.cl b/noao/imred/ctioslit/demos/doslit.cl
new file mode 100644
index 00000000..b2ecbde2
--- /dev/null
+++ b/noao/imred/ctioslit/demos/doslit.cl
@@ -0,0 +1,14 @@
+# Create demo data if needed.
+
+cl (< "demos$mkdoslit.cl")
+
+unlearn doslit
+sparams.extras = no
+sparams.coordlist = "linelists$idhenear.dat"
+delete demologfile,demoplotfile verify=no >& dev$null
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgdoslit.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/ctioslit/demos/mkdoslit.cl b/noao/imred/ctioslit/demos/mkdoslit.cl
new file mode 100644
index 00000000..b76f467d
--- /dev/null
+++ b/noao/imred/ctioslit/demos/mkdoslit.cl
@@ -0,0 +1,25 @@
+# Create demo data if needed.
+
+artdata
+artdata.nxc = 5
+artdata.nyc = 5
+artdata.nxsub = 10
+artdata.nysub = 10
+artdata.nxgsub = 5
+artdata.nygsub = 5
+artdata.dynrange = 100000.
+artdata.psfrange = 10.
+artdata.ranbuf = 0
+
+mkexample ("longslit", "demoarc1", oseed=5,  nseed=1,
+    errors=no, verbose=yes, list=no)
+mkheader ("demoarc1", "demos$demoarc1.dat", append=no, verbose=no)
+mkexample ("longslit", "demoobj1", oseed=1,  nseed=1,
+    errors=no, verbose=yes, list=no)
+mkheader ("demoobj1", "demos$demoobj1.dat", append=no, verbose=no)
+mkexample ("longslit", "demostd1", oseed=2, nseed=2,
+    errors=no, verbose=yes, list=no)
+mkheader ("demostd1", "demos$demostd1.dat", append=no, verbose=no)
+mkexample ("longslit", "demoarc2", oseed=5,  nseed=2,
+    errors=no, verbose=yes, list=no)
+mkheader ("demoarc2", "demos$demoarc2.dat", append=no, verbose=no)
diff --git a/noao/imred/ctioslit/demos/xgdoslit.dat b/noao/imred/ctioslit/demos/xgdoslit.dat
new file mode 100644
index 00000000..eef7d9f2
--- /dev/null
+++ b/noao/imred/ctioslit/demos/xgdoslit.dat
@@ -0,0 +1,71 @@
+\O=NOAO/IRAF IRAFX valdes@puppis Mon 14:58:37 15-Nov-93
+\T=xgterm
+\G=xgterm
+epar\sctioslit\n
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+y\r
+demologfile\r
+demoplotfile\r
+^Z
+epar\sdoslit\n
+demoobj1\r
+demoarc1,demoarc2\r
+\r
+demostd1\r
+rdnoise\r
+gain\r
+\r
+\r
+5700\r
+6.2\r
+\r
+y\r
+y\r
+y\r
+y\r
+y\r
+^Z
+doslit\sredo+\n
+\n
+\n
+b/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+y\n
+4210\n
+7350\n
+6.2\n
+\n
+n\n
+\n
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\n
+f56\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+Y\n
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+gkimos\sdemoplotfile\snx=3\sny=3\sdev=stdgraph\n
+q/<-5\s\s\s\s/=(.\s=\r
diff --git a/noao/imred/ctioslit/sensfunc.par b/noao/imred/ctioslit/sensfunc.par
new file mode 100644
index 00000000..94f84f4a
--- /dev/null
+++ b/noao/imred/ctioslit/sensfunc.par
@@ -0,0 +1,17 @@
+standards,s,a,std,,,Input standard star data file (from STANDARD)
+sensitivity,s,a,"sens",,,Output root sensitivity function imagename
+apertures,s,h,"",,,Aperture selection list
+ignoreaps,b,h,yes,,,Ignore apertures and make one sensitivity function?
+logfile,f,h,"logfile",,,Output log for statistics information
+extinction,f,h,)_.extinction,,,Extinction file
+newextinction,f,h,"extinct.dat",,,Output revised extinction file
+observatory,s,h,)_.observatory,,,Observatory of data
+function,s,h,"spline3","chebyshev|legendre|spline3|spline1",,Fitting function
+order,i,h,6,1,,Order of fit
+interactive,b,h,yes,,,Determine sensitivity function interactively?
+graphs,s,h,"sr",,,Graphs per frame
+marks,s,h,"plus cross box",,,Data mark types (marks deleted added)
+colors,s,h,"2 1 3 4",,,Colors (lines marks deleted added)
+cursor,*gcur,h,"",,,Graphics cursor input
+device,s,h,"stdgraph",,,Graphics output device
+answer,s,q, yes,"no|yes|NO|YES",,"(no|yes|NO|YES)"
diff --git a/noao/imred/ctioslit/sparams.par b/noao/imred/ctioslit/sparams.par
new file mode 100644
index 00000000..cfdf1f4f
--- /dev/null
+++ b/noao/imred/ctioslit/sparams.par
@@ -0,0 +1,65 @@
+line,i,h,INDEF,,,"Default dispersion line"
+nsum,i,h,10,,,"Number of dispersion lines to sum or median"
+extras,b,h,no,,,"Extract sky, sigma, etc.?
+
+-- DEFAULT APERTURE PARAMETERS -- "
+lower,r,h,-3.,,,Lower aperture limit relative to center
+upper,r,h,3.,,,"Upper aperture limit relative to center
+
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --"
+ylevel,r,h,0.05,,,"Fraction of peak or intensity for resizing
+
+-- TRACE PARAMETERS --"
+t_step,i,h,10,,,"Tracing step"
+t_function,s,h,"spline3","chebyshev|legendre|spline1|spline3",,"Trace fitting function"
+t_order,i,h,1,,,"Trace fitting function order"
+t_niterate,i,h,1,0,,"Trace rejection iterations"
+t_low,r,h,3.,0.,,"Trace lower rejection sigma"
+t_high,r,h,3.,0.,,"Trace upper rejection sigma
+
+-- APERTURE EXTRACTION PARAMETERS --"
+weights,s,h,"none",,,Extraction weights (none|variance)
+pfit,s,h,"fit1d","fit1d|fit2d",,Profile fitting algorithm (fit1d|fit2d)
+lsigma,r,h,3.,,,Lower rejection threshold
+usigma,r,h,3.,,,"Upper rejection threshold
+
+-- BACKGROUND SUBTRACTION PARAMETERS --"
+background,s,h,"fit","none|average|median|minimum|fit",,Background to subtract
+b_function,s,h,"legendre","chebyshev|legendre|spline1|spline3",,"Background function"
+b_order,i,h,1,,,"Background function order"
+b_sample,s,h,"-10:-6,6:10",,,"Background sample regions"
+b_naverage,i,h,-100,,,"Background average or median"
+b_niterate,i,h,1,0,,"Background rejection iterations"
+b_low,r,h,3.,0.,,"Background lower rejection sigma"
+b_high,r,h,3.,0.,,"Background upper rejection sigma
+
+-- ARC DISPERSION FUNCTION PARAMETERS --"
+threshold,r,h,10.,0.,,"Minimum line contrast threshold"
+coordlist,f,h,linelists$idhenear.dat,,,"Line list"
+match,r,h,10.,,,"Line list matching limit in Angstroms"
+fwidth,r,h,4.,,,"Arc line widths in pixels"
+cradius,r,h,10.,,,Centering radius in pixels
+i_function,s,h,"spline3","legendre|chebyshev|spline1|spline3",,"Coordinate function"
+i_order,i,h,1,1,,"Order of dispersion function"
+i_niterate,i,h,1,0,,"Rejection iterations"
+i_low,r,h,3.,0.,,"Lower rejection sigma"
+i_high,r,h,3.,0.,,"Upper rejection sigma"
+refit,b,h,yes,,,"Refit coordinate function when reidentifying?"
+addfeatures,b,h,no,,,"Add features when reidentifying?
+
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --"
+select,s,h,"interp",,,"Selection method for reference spectra"
+sort,s,h,"jd",,,"Sort key"
+group,s,h,"ljd",,,"Group key"
+time,b,h,no,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting
+
+-- DISPERSION CORRECTION PARAMETERS --"
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+log,b,h,no,,,"Logarithmic wavelength scale?"
+flux,b,h,yes,,,"Conserve flux?
+
+-- SENSITIVITY CALIBRATION PARAMETERS --"
+s_function,s,h,"spline3","chebyshev|legendre|spline3|spline1",,"Fitting function"
+s_order,i,h,1,1,,"Order of sensitivity function"
+fnu,b,h,no,,,"Create spectra having units of FNU?"
diff --git a/noao/imred/ctioslit/standard.par b/noao/imred/ctioslit/standard.par
new file mode 100644
index 00000000..99b98877
--- /dev/null
+++ b/noao/imred/ctioslit/standard.par
@@ -0,0 +1,21 @@
+input,f,a,,,,Input image file root name
+output,s,a,std,,,Output flux file (used by SENSFUNC)
+samestar,b,h,yes,,,Same star in all apertures?
+beam_switch,b,h,no,,,Beam switch spectra?
+apertures,s,h,"",,,Aperture selection list
+bandwidth,r,h,INDEF,,,Bandpass widths
+bandsep,r,h,INDEF,,,Bandpass separation
+fnuzero,r,h,3.68e-20,,,Absolute flux zero point
+extinction,s,h,)_.extinction,,,Extinction file
+caldir,s,h,)_.caldir,,,Directory containing calibration data
+observatory,s,h,)_.observatory,,,Observatory for data
+interact,b,h,yes,,,Graphic interaction to define new bandpasses
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+star_name,s,q,,,,Star name in calibration list
+airmass,r,q,,1.,,Airmass
+exptime,r,q,,,,Exposure time (seconds)
+mag,r,q,,,,Magnitude of star
+magband,s,q,,"U|B|V|R|I|J|H|K|L|Lprime|M",,"Magnitude type"
+teff,s,q,,,,Effective temperature or spectral type
+answer,s,q,no,,,"(no|yes|NO|YES|NO!|YES!)"
diff --git a/noao/imred/doc/demos.hlp b/noao/imred/doc/demos.hlp
new file mode 100644
index 00000000..35a32b6e
--- /dev/null
+++ b/noao/imred/doc/demos.hlp
@@ -0,0 +1,77 @@
+.help demos Sep90
+.ih
+NAME
+demos -- Demonstration and Test Procedures
+.ih
+PACKAGES
+noao.imred.argus, noao.imred.goldcams, noao.imred.kpcoude.fiber
+noao.imred.kpcoude.slit, noao.imred.nessie, noao.imred.specred
+noao.twodspec.longslit
+.ih
+USAGE
+demos demoname
+.ih
+PARAMETERS
+.ls demoname
+Demonstration or test procedure name.  Each package may have a different
+set of demonstrations.  If the demo name is not specified on the command
+line a menu of names is printed and then the name is queried.
+.le
+.ih
+DESCRIPTION
+Many packages have demonstration and test procedures.  These are generally
+based on artificial data and use the \fIstty playback\fR (see \fBstty\fR)
+mechanism of the CL.  A playback replaces interactive terminal input 
+with previously stored input but otherwise is an actual execution of
+the entered commands.  This allows both demonstration of various types
+and an actual test of the software on a particular IRAF system.
+
+Generally the \fBdemos\fR procedures create their own data if not present
+from a previous execution.  After the procedure is completed the data,
+logfiles, etc. are left so that they may be examined further and
+the user may try some experiments.  Thus, it might be useful to create
+a new directory for the demo using \fBmkdir\fR and "cd" to it.
+
+Currently, most of the demos are test procedures which do not contain
+comments and suitable delays to act as a demonstration.  These will
+be added in time.  Also some of the demos just create the demo/test
+data if one just wants some relevant data for experimentation with
+the package.
+
+One should be aware that since the tasks are actually run parameters
+are sometimes changed.
+.ih
+EXAMPLES
+1.  From the \fBgoldcam\fR package list the menu and execute the
+qtest demo.
+
+.nf
+	go> mkdir demo
+	go> cd demo
+	go> demos
+		MENU of GOLDCAM Demonstrations
+
+		qtest - Quick test of GOLDCAM (no comments, no delays)
+
+	Demo name (qtest): 
+	<Demo follows>
+.fi
+
+2.  From the \fBnessie\fR package create some simple test data.
+
+.nf
+	ne> demos mkqdata
+	Creating image demoobj ...
+	Creating image demoflat ...
+	Creating image demoarc1 ...
+	Creating image demoarc2 ...
+	ne> demos mkqdata
+	ne>
+.fi
+
+Note that the second execution does not create the data again.
+
+.ih
+SEE ALSO
+artdata.mkexamples, ccdred.ccdtest.demo
+.endhelp
diff --git a/noao/imred/doc/revisions.v2.ms b/noao/imred/doc/revisions.v2.ms
new file mode 100644
index 00000000..50036911
--- /dev/null
+++ b/noao/imred/doc/revisions.v2.ms
@@ -0,0 +1,89 @@
+.nr PS 9
+.nr VS 11
+.RP
+.ND
+.TL
+IMRED Package Revisions Summary: IRAF Version 2.10
+.AU
+Francisco Valdes
+.AI
+IRAF Group - Central Computer Services
+.K2
+P.O. Box 26732, Tucson, Arizona 85726
+September 1990
+.AB
+This paper summarizes the changes in Version 2 of the IRAF \fBimred\fR
+package which is part of IRAF Version 2.10.  The major changes are:
+
+.IP \(bu
+New multifiber reduction packages \fBargus\fR, \fBnessie\fR, and
+\fBkpcoude.fiber\fR.
+.IP \(bu
+New spectrophotmetric slit spectra reduction packages \fBgoldcam\fR,
+\fBspecred\fR, and \fBkpcoude.slit\fR.
+.IP \(bu
+New versions of the \fBmsred\fR and \fBechelle\fR packages based on
+the new versions of \fBapextract\fR and \fBonedspec\fR.
+.AE
+.NH
+Introduction
+.PP
+A number of new specialized image reduction packages and new versions
+of the generic echelle and multiobject spectroscopy packages have been
+added to the \fBimred\fR package in IRAF Version 2.10.  The new
+subpackages will be made available as external packages prior to
+the release of V2.10.  The major changes are:
+
+.IP \(bu
+New multifiber reduction packages \fBargus\fR, \fBnessie\fR, and
+\fBkpcoude.fiber\fR.
+.IP \(bu
+New spectrophotmetric slit spectra reduction packages \fBgoldcam\fR,
+\fBspecred\fR, and \fBkpcoude.slit\fR.
+.IP \(bu
+New versions of the \fBmsred\fR and \fBechelle\fR packages based on
+the new versions of \fBapextract\fR and \fBonedspec\fR.
+
+.LP
+In additions there have been some minor changes in the other
+spectroscopy packages required by changes in the \fBonedspec\fR package.
+.PP
+The new packages are specialized to specific instruments or types of
+data.  They contain tasks collected from the various general spectroscopy
+packages which are appropriate for a particular type of data.
+However, the most important contribution of these packages are
+special reduction tasks which are streamlined to perform the complete
+calibration and reduction of the data in as simple and automated
+manner as possible.  The tasks combine operations from both two
+dimensional extraction and one dimensional spectral calibrations
+and collects all the useful parameters in two parameter sets while
+fixing and hiding parameters which are irrelevent.
+.PP
+The new packages are as follows.  The \fBargus\fR package is for the
+flat fielding, throughput correction, extraction, dispersion correction,
+and sky correction of data from the CTIO \fIArgus\fR multifiber instrument.
+The \fBnessie\fR package is similar and is for the KPNO \fINessie\fR
+multifiber plugboard instrument.  The \fBkpcoude.fiber\fR package is
+specialized for the three fiber (two arc and one object) instrument
+at the KPNO Coude.  It is similar to the other multifiber packages
+except there is no sky subtraction.
+.PP
+The other three packages are for sky subtracted extraction,
+dispersion correction, extinction correction, and flux calibration
+of slit instruments.  The packages are for the KPNO \fIGoldcam\fR,
+the KPNO Coude, and for the CTIO \fI2DFRUTTI\fR.  They are all
+fairly general and could be used for other instruments.  They are
+distinguished by choices of default parameters.
+.PP
+There are user's guides for the powerful new reduction tasks in
+the new packages.  These are available both as nicely typeset
+documents and as on-line IRAF manual pages.
+.PP
+Tasks from the revised \fBapextract\fR and \fBonedspec\fR packages
+appear in many of the \fBimred\fR packages.  In particular the
+\fBechelle\fR and \fBmsred\fR packages are now based on this new
+software.
+.PP
+Some minor changes are the replacement of the \fBspecphot\fR package
+by \fBspecred\fR and the renaming and reorganization of the
+\fBcoude\fR package.
diff --git a/noao/imred/doc/tutor.hlp b/noao/imred/doc/tutor.hlp
new file mode 100644
index 00000000..21684194
--- /dev/null
+++ b/noao/imred/doc/tutor.hlp
@@ -0,0 +1,64 @@
+.help tutor Aug86 noao.imred
+.ih
+NAME
+tutor -- Present tutorial help on a particular package
+.ih
+USAGE
+tutor topic
+.ih
+PARAMETERS
+.ls topic
+Topic for which help is desired.  If no topic is given then available
+topics are presented.  The topic "all" prints all the topics.
+.le
+.ls package = ""
+Package for which tutorial help is desired.  If null then the tutorial
+for the current package is presented.
+.le
+.ls tutordb = "helpdb"
+The filename of the tutorial database to be searched.  If the \fIvalue\fR of the
+parameter is the reserved string "helpdb", the actual filename is the value
+of the CL environment variable \fIhelpdb\fR.
+.le
+.ih
+DESCRIPTION
+This task provides a tutorial facility for some of the IRAF packages.
+The tutorial consists of a number of topics
+which are obtained by typing "tutor topic" where topic is one of the
+available topics.  If no topic is given then the available topics are
+presented.  The topic "all" presents all the topics.
+
+This task is implemented using the \fBhelp\fR task.  Therefore,
+modifying the \fBhelp\fR parameters dealing with the device and print
+format will also determine the output of \fBtutor\fR.  The tutorial
+topic material is contained in the file Tutorial.hlp for each package.
+The database containing the directory to the tutorial files may or may
+not be the same as the standard help database.
+.ih
+EXAMPLES
+To get started:
+
+	cl> tutor
+
+To get help on reading and writing data tapes:
+
+	cl> tutor dataio
+
+To read all the topics:
+
+	cl> tutor all
+.ih
+BUGS
+Piping the output of \fBtutor\fR to lprint does not work properly because
+\fBhelp\fR is contained in a script.
+.ih
+TUTORIALS
+Tutorials are currently available only for the \fBechelle\fR package.
+This tutorial is in the process of being developed.
+.ih
+SEE ALSO
+.nf
+help
+Individual help pages for all the tasks mentioned in the tutorial.
+.fi
+.endhelp
diff --git a/noao/imred/dtoi/README b/noao/imred/dtoi/README
new file mode 100644
index 00000000..e293c6c8
--- /dev/null
+++ b/noao/imred/dtoi/README
@@ -0,0 +1 @@
+DTOI -- Density to intensity transformation package.
diff --git a/noao/imred/dtoi/Revisions b/noao/imred/dtoi/Revisions
new file mode 100644
index 00000000..e6e955ff
--- /dev/null
+++ b/noao/imred/dtoi/Revisions
@@ -0,0 +1,144 @@
+.help revisions Jun88 noao.imred.dtoi
+.nf
+
+imred$dtoi/selftest.x
+	The 'lut' was declared as TY_INT instead of TY_REAL (5/4/13)
+
+imred$dtoi/spolist.x
+	A TY_INT pointer was being used with Memr[] (4/20/13)
+
+=======
+V2.16
+=======
+
+imred$dtoi/hdtoi.x
+	The hd_fogcalc() procedure was being called with too few arguments
+	(7/12/09, MJF)
+
+=======
+V2.14.1
+=======
+
+imred$dtoi/hdicfit/mkpkg
+	Added missing dependencies.  (12/13/01, MJF)
+
+imred$dtoi/mkpkg
+	Added missing dependencies.  (10/11/99, Valdes)
+
+=======
+V2.11.2
+=======
+
+imred$dtoi/doc/hdfit.hlp
+imred$dtoi/doc/hdshift.hlp
+imred$dtoi/doc/hdtoi.hlp
+imred$dtoi/doc/spotlist.hlp
+	Fixed minor formating problems.  (4/22/99, Valdes)
+
+imred$dtoi/hdicggraph.x
+imred$dtoi/hdicebars.x
+	Replace direct access to GTOOLS structure with GTOOLS interface.
+	(12/18/98, Valdes)
+
+=======
+V2.11.1
+=======
+
+imred$dtoi/spotlist.x	7 Sept, 1989 SRo
+	In Suzanne's absence, removed the divide by nfog fog images in
+	hd_fogcalc() after a bug report by Steve Majewski that when multiple
+	fog images are used, the resultant fog values are too low by 1/nfog.
+	The total_pix accumulator is already a total for all images.  Should
+	be verified by Suzanne on her return.
+
+imred$dtoi/hdicfit/hdicgdelte.x  17 April, 1989 ShJ
+	Procedure icg_dl1 was declared as an integer procedure, although
+	it does not return a function values and was not being called
+	as a function.  
+
+imred$dtoi/hdicfit/hdicgcolon.x  27 March, 1989 ShJ
+	Changed only a comment line, to point out that the :ebars command
+	switches the meaning of the error bars between representing 
+	standard deviations or weights.  
+
+imred$dtoi/spotlist.x 11 May, 1988 ShJ
+	Added parameter "option", which selects a mean or median calculation
+	of spot densities and the fog value.  Previously, only a mean 
+	calculation was available.  The choice of "option" is written to
+	the database.  
+
+imred$dtoi/hd_aravr.x  11 May, 1988 ShJ
+	This is a new file, modified from the vops version only in that it
+	puts an upper limit on the number of iterations allowed in the
+	procedure of 10.  This should avoid the problem reported by
+	Steve Majewski of nearly saturated pixels "hanging"; they actually
+	were oscillating endlessly in the mean rejection calculation.
+
+imred$dtoi/hdtoi.x 11 May, 1988 ShJ
+	Added parameter "option", which selects a mean or median calulcation
+	of the fog value, in those cases where the user supplies a fog 
+	image, rather than a fog value.  Previously, only a mean calculation
+	was available.  This newly calculated value of fog is now also
+	written to the database.
+
+imred$dtoi/hdtoi.x 5 April, 1988 ShJ
+	Modified the way in which hdtoi scales intensities to the "ceiling"
+	parameter.  A maximum intensity is calculated, using cveval to
+	evaluate the transformed value of the maximum density above fog.
+	The fog value subtracted is hdtoi.fog, which may or may not
+	equal the value of fog written by spotlist into the database.
+	Previously, the program was incorrectly subtracting the spotlist
+	fog value from the maximum density when calculating the maximum
+	intensity and so the scale factor to represent saturated intensities
+	as "ceiling". 
+
+imred$dtoi/hdicgundel.x	25 March, 1988  ShJ
+	Procedures icg_u1d and icg_undeleted in this source file were
+	declared as functions but not returning a value.  They were not
+	being called as functions, and are now not declared as functions.
+
+imred$dtoi/database.x	14 March, 1988	ShJ
+	Added procedure to put a double precision value:  ddb_putd().
+
+imred$dtoi/spotlist.x	14 March, 1988	ShJ
+	Added code for additional input parameter: "maxad", the maximum
+	allowed input value, i.e., the AD units in a saturated pixel.  From
+	this value and the "scale" parameter, spotlist calculates the
+	maximum permissable density, and writes this to the database as a
+	double precision value. 
+
+imred$dtoi/hdfit.x	14 March, 1988	ShJ
+	Parameter "maxden" was removed, as this value is now calculated
+	precisely by spotlist and can be read from the database.
+
+imred$dtoi/spotlist.par
+imred$dtoi/hdfit.par
+imred$dtoi/doc/spotlist.hlp
+imred$dtoi/doc/hdfit.hlp	14 March, 1988	ShJ
+	Modified help pages and parameter files for spotlist and hdfit to
+	support the above changes to the user interface.
+
+imred$dtoi/hdtoi.x	11 March, 1988	ShJ
+	Bug fixed in hd_aptrans().  The equations for the k75 and k50 
+	transformations were incorrect, having a '*' where a '+' should
+	have been.  Also, the strncmp procedure was only checking the first 
+	character to distinguish between transformation types, in which
+	case k75 and k50 would not be resolved.
+
+imred$dtoi/hdfit.x	10 March, 1988	ShJ
+	Repaired an error in incrementing an offset into the output
+	arrays in hd_rdloge.   This error was seen only when more than
+	two databases contributed input values to be fit.  This was
+	a trivial arithmetic error that had been overlooked due to
+	insufficient testing.  This bug would produce a memory error
+	as values were written into unallocated locations.
+
+imred$dtoi/hdicfit/hdic.com	9 March, 1988	ShJ
+	Reordered the values in the common block, as the largest double
+	precision value was following the integers.  The SUN-4 compiler
+	gave warning of this, then padded the double value.  Also at this
+	time file hdicgundelete.x was renamed to hdicgundel.x to avoid
+	problems associated with filenames longer than 14 characters.  The 
+	hdicfit library was completely rebuilt at this time, to insure the
+	new object module would be retrieved.
+.endhelp
diff --git a/noao/imred/dtoi/database.x b/noao/imred/dtoi/database.x
new file mode 100644
index 00000000..cb501472
--- /dev/null
+++ b/noao/imred/dtoi/database.x
@@ -0,0 +1,611 @@
+include	<time.h>
+include	<ctype.h>
+include	<ctotok.h>
+include	<finfo.h>
+
+# DATABASE.X -- This file contains source for the database utilities used by
+# the DTOI package.  They are based on Frank Valdes's dtext utilities.
+
+# Definition for dbtext structure.
+
+define	DT_LEN		5
+
+define	DT		Memi[$1]	# FIO channel
+define	DT_NRECS	Memi[$1+1]	# Number of records
+define	DT_OFFSETS	Memi[$1+2]	# Pointer to record offsets
+define	DT_NAMES	Memi[$1+3]	# Pointer to name indices
+define	DT_MAP		Memi[$1+4]	# Pointer to record names
+
+define	DT_OFFSET	Meml[DT_OFFSETS($1)+$2-1]
+define	DT_NAMEI	Memi[DT_NAMES($1)+$2-1]
+define	DT_NAME		Memc[DT_MAP($1)+DT_NAMEI($1,$2)]
+
+define	DT_ALLOC	20		# Allocation block size
+
+
+# DDB_MAP -- Map the database.
+
+pointer procedure ddb_map (database, mode)
+
+char	database[ARB]			# Database file
+int	mode				# FIO mode
+
+int	i, nrec
+int	dt_alloc1, dt_alloc2
+pointer	db, str
+
+int	open(), fscan(), strlen()
+bool	streq()
+long	note()
+errchk	delete, open
+
+begin
+	call calloc (db, DT_LEN, TY_STRUCT)
+
+	if (mode == NEW_FILE)
+	    iferr (call delete (database))
+		;
+
+	DT(db) = open (database, mode, TEXT_FILE)
+
+	if (mode != READ_ONLY)
+	    return (db)
+
+	dt_alloc1 = DT_ALLOC
+	dt_alloc2 = DT_ALLOC * SZ_LINE
+	call malloc (DT_OFFSETS(db), dt_alloc1, TY_LONG)
+	call malloc (DT_NAMES(db), dt_alloc1, TY_INT)
+	call malloc (DT_MAP(db), dt_alloc2, TY_CHAR)
+	call malloc (str, SZ_LINE, TY_CHAR)
+
+	nrec = 1
+	DT_NRECS(db) = 0
+	DT_NAMEI(db, nrec) = 0
+
+	while (fscan (DT(db)) != EOF) {
+	    call gargwrd (DT_NAME(db, nrec), SZ_LINE)
+
+	    if (streq (DT_NAME(db, nrec), "begin")) {
+		call gargstr (Memc[str], SZ_LINE)
+		for (i=str; IS_WHITE(Memc[i]); i=i+1)
+		    ;
+		call strcpy (Memc[i], DT_NAME(db, nrec), SZ_LINE)
+
+		for (i = 1; i < nrec; i = i + 1)
+		    if (streq (DT_NAME(db, i), DT_NAME(db, nrec)))
+			break
+
+		if (i < nrec)
+		    DT_OFFSET(db, i) = note (DT(db))
+		else {
+		    DT_NRECS(db) = nrec
+		    DT_OFFSET(db, nrec) = note (DT(db))
+		    DT_NAMEI(db, nrec+1) = DT_NAMEI(db, nrec) +
+		        strlen (DT_NAME(db, nrec)) + 1
+		    nrec = nrec + 1
+		}
+
+		if (nrec == dt_alloc1) {
+		    dt_alloc1 = dt_alloc1 + DT_ALLOC
+		    call realloc (DT_OFFSETS(db), dt_alloc1, TY_LONG)
+		    call realloc (DT_NAMES(db), dt_alloc1, TY_INT)
+	        }
+
+	        if (DT_NAMEI(db, nrec) + SZ_LINE >= dt_alloc2) {
+		    dt_alloc2 = dt_alloc2 + DT_ALLOC * SZ_LINE
+		    call realloc (DT_MAP(db), dt_alloc2, TY_CHAR)
+		}
+	    }
+	}
+
+	call realloc (DT_MAP(db), DT_NAMEI(db, nrec), TY_CHAR)
+	call realloc (DT_OFFSETS(db), DT_NRECS(db), TY_LONG)
+	call realloc (DT_NAMES(db), DT_NRECS(db), TY_INT)
+
+	return (db)
+end
+
+
+# DDB_UNMAP -- Unmap the database.
+
+procedure ddb_unmap (db)
+
+pointer	db				# Database file descriptor
+
+begin
+	call close (DT(db))
+	call mfree (DT_MAP(db), TY_CHAR)
+	call mfree (DT_OFFSETS(db), TY_LONG)
+	call mfree (DT_NAMES(db), TY_INT)
+	call mfree (db, TY_STRUCT)
+end
+
+
+# DDB_PREC -- Write a record to the database.
+
+procedure ddb_prec (db, record)
+
+pointer	db		# Pointer to database
+char	record[ARB]	# Name of record to enter
+
+pointer	sp, entry
+
+begin
+	call smark (sp)
+	call salloc (entry, SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[entry], SZ_LINE, "begin\t%s\n")
+	    call pargstr (record)
+
+	call fprintf (DT(db), Memc[entry])
+
+	call sfree (sp)
+end
+
+
+# DDB_PUTR -- Write a real valued field into the current record.
+
+procedure ddb_putr (db, field, value)
+
+pointer	db		# Pointer to database
+char	field[ARB]	# Format string
+real	value		# Real value to output
+
+pointer	sp, entry
+
+begin
+	call smark (sp)
+	call salloc (entry, SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[entry], SZ_LINE, "\t%s\t%g\n")
+	    call pargstr (field)
+	    call pargr (value)
+	
+	call fprintf (DT(db), Memc[entry])
+
+	call sfree (sp)
+end
+
+# DDB_PUTD -- Write a double valued field into the current record.
+
+procedure ddb_putd (db, field, value)
+
+pointer	db		# Pointer to database
+char	field[ARB]	# Format string
+double	value		# Real value to output
+
+pointer	sp, entry
+
+begin
+	call smark (sp)
+	call salloc (entry, SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[entry], SZ_LINE, "\t%s\t%g\n")
+	    call pargstr (field)
+	    call pargd (value)
+	
+	call fprintf (DT(db), Memc[entry])
+
+	call sfree (sp)
+end
+
+
+# DDB_PUTI -- Write an integer valued field into the current record.
+
+procedure ddb_puti (db, field, value)
+
+pointer	db		# Pointer to database
+char	field[ARB]	# Format string
+int	value		# Integer value to output
+
+pointer	sp, entry
+
+begin
+	call smark (sp)
+	call salloc (entry, SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[entry], SZ_LINE, "\t%s\t%d\n")
+	    call pargstr (field)
+	    call pargi (value)
+	
+	call fprintf (DT(db), Memc[entry])
+
+	call sfree (sp)
+end
+
+
+# DDB_PSTR -- Write a string valued field into the current record.
+
+procedure ddb_pstr (db, field, value)
+
+pointer	db		# Pointer to database
+char	field[ARB]	# Format string
+char	value[ARB]	# String field
+
+pointer	sp, entry
+
+begin
+	call smark (sp)
+	call salloc (entry, SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[entry], SZ_LINE, "\t%s\t%s\n")
+	    call pargstr (field)
+	    call pargstr (value)
+	
+	call fprintf (DT(db), Memc[entry])
+
+	call sfree (sp)
+end
+
+
+# DDB_PAR -- Put an array of real values into a field in the current record.
+
+procedure ddb_par (db, field, array, nvals)
+
+pointer	db		# Pointer to database structure
+char	field[ARB]	# Name of field to be added
+real	array[nvals]	# Array of real values 
+int	nvals		# Number of values in array
+
+pointer	sp, entry
+int	i
+
+begin
+	call smark (sp)
+	call salloc (entry, SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[entry], SZ_LINE, "\t%s\t%d\n")
+	    call pargstr (field)
+	    call pargi (nvals)
+
+	call fprintf (DT(db), Memc[entry])
+
+	do i = 1, nvals {
+	    call sprintf (Memc[entry], SZ_LINE, "\t\t%g\n")
+		call pargr (array[i])
+	    
+	    call fprintf (DT(db), Memc[entry])
+	}
+
+	call sfree (sp)
+end
+
+
+# DDB_PAD -- Put an array of double values into a field in the current record.
+
+procedure ddb_pad (db, field, array, nvals)
+
+pointer	db		# Pointer to database structure
+char	field[ARB]	# Name of field to be added
+double	array[nvals]	# Array of double values 
+int	nvals		# Number of values in array
+
+pointer	sp, entry
+int	i
+
+begin
+	call smark (sp)
+	call salloc (entry, SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[entry], SZ_LINE, "\t%s\t%d\n")
+	    call pargstr (field)
+	    call pargi (nvals)
+
+	call fprintf (DT(db), Memc[entry])
+
+	do i = 1, nvals {
+	    call sprintf (Memc[entry], SZ_LINE, "\t\t%g\n")
+		call pargd (array[i])
+	    
+	    call fprintf (DT(db), Memc[entry])
+	}
+
+	call sfree (sp)
+end
+
+
+# DDB_PAI -- Put an array of integer values into a field in the current 
+# record.
+
+procedure ddb_pai (db, field, array, nvals)
+
+pointer	db		# Pointer to database structure
+char	field[ARB]	# Name of field to be added
+int	array[nvals]	# Array of integer values 
+int	nvals		# Number of values in array
+
+pointer	sp, entry
+int	i
+
+begin
+	call smark (sp)
+	call salloc (entry, SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[entry], SZ_LINE, "\t%s\t%d\n")
+	    call pargstr (field)
+	    call pargi (nvals)
+
+	call fprintf (DT(db), Memc[entry])
+
+	do i = 1, nvals {
+	    call sprintf (Memc[entry], SZ_LINE, "\t\t%d\n")
+		call pargi (array[i])
+	    
+	    call fprintf (DT(db), Memc[entry])
+	}
+
+	call sfree (sp)
+end
+
+
+# DDB_LOCATE -- Locate a database record.
+
+int procedure ddb_locate (db, name)
+
+pointer	db				# DTTEXT pointer
+char	name[ARB]			# Record name
+
+int	i
+
+bool	streq()
+pointer	sp, err_string
+
+begin
+	do i = 1, DT_NRECS(db) {
+	    if (streq (name, DT_NAME(db, i)))
+		return (i)
+	}
+
+	# The record was not found
+
+	call smark (sp)
+	call salloc (err_string, SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[err_string], SZ_LINE, 
+	    "DDB_LOCATE: Database record '%s' not found")
+	        call pargstr (name)
+
+	call error (21, Memc[err_string])
+	call sfree (sp)
+end
+
+
+# DDB_GSTR -- Get a string field
+
+procedure ddb_gstr (db, record, field, str, maxchar)
+
+pointer	db				# Database file descriptor
+int	record				# Database index
+char	field[ARB]			# Database field
+char	str[maxchar]			# String value
+int	maxchar				# Maximum characters for string
+
+char	name[SZ_LINE]
+
+pointer	sp, esp
+int	i, fscan()
+bool	streq()
+
+begin
+	if ((record < 1) || (record > DT_NRECS(db)))
+	    call error (22, "Database record request out of bounds")
+
+	call seek (DT(db), DT_OFFSET(db, record))
+
+	while (fscan (DT(db)) != EOF) {
+	    call gargwrd (name, SZ_LINE)
+
+	    if (streq (name, "begin"))
+		break
+	    else if (streq (name, field)) {
+		call gargstr (str, maxchar)
+		for (i=1; IS_WHITE(str[i]); i=i+1)
+		    ;
+		if (i>1)
+		    call strcpy (str[i], str, maxchar)
+		return
+	    }
+	}
+
+	call smark (sp)
+	call salloc (esp, SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[esp], SZ_LINE, 
+	    "DDB_GSTR: Database field '%s' not found")
+		call pargstr (field)
+
+	call error (23, Memc[esp])
+	call sfree (sp)
+end
+
+
+# DDB_GETI -- Get an integer field.
+
+int procedure ddb_geti (db, record, field)
+
+pointer	db				# DTTEXT pointer
+int	record				# Database index
+char	field[ARB]			# Database field
+
+real	rval
+bool    fp_equalr()
+real	ddb_getr()
+
+errchk	ddb_getr
+
+begin
+	rval = ddb_getr (db, record, field)
+
+	if (fp_equalr (rval, INDEFR))
+	    return (INDEFI)
+	else 
+	    return (int (rval))
+end
+
+
+# DDB_GETR -- Get an real field
+
+real procedure ddb_getr (db, record, field)
+
+pointer	db				# DTTEXT pointer
+int	record				# Database index
+char	field[ARB]			# Database field
+
+pointer	sp, esp
+real	rval
+char	name[SZ_LINE]
+
+int	fscan(), nscan()
+bool	streq()
+
+begin
+	if ((record < 1) || (record > DT_NRECS(db)))
+	    call error (24, "Database record request out of bounds")
+
+	call seek (DT(db), DT_OFFSET(db, record))
+
+	while (fscan (DT(db)) != EOF) {
+	    call gargwrd (name, SZ_LINE)
+
+	    if (streq (name, "begin"))
+		break
+	    else if (streq (name, field)) {
+		call gargr (rval)
+		if (nscan() == 2)
+		   return (rval)
+		else
+		   call error (25, "Error in database field value")
+	    }
+	}
+
+	call smark (sp)
+	call salloc (esp, SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[esp], SZ_LINE, 
+	    "DDB_GET: Database field '%s' not found")
+		call pargstr (field)
+
+	call error (26, Memc[esp])
+	call sfree (sp)
+end
+
+
+# DDB_GAR -- Get a real array field
+
+procedure ddb_gar (db, record, field, array, len_array, npts)
+
+pointer	db				# DTTEXT pointer
+int	record				# Database index
+char	field[ARB]			# Database field
+real	array[len_array]		# Array values
+int	len_array			# Length of array
+int	npts				# Number of values in the field
+
+int	i
+double	tmp
+pointer	sp, dubble
+bool	fp_equald()
+
+begin
+	call smark (sp)
+	call salloc (dubble, npts, TY_DOUBLE)
+
+	call ddb_gad (db, record, field, Memd[dubble], len_array, npts)
+	do i = 1, npts {
+	    tmp = Memd[dubble+i-1]
+	    if (fp_equald (tmp, INDEFD))
+		array[i] = INDEFR
+	    else
+		array[i] = real (tmp)
+	}
+
+	call sfree (sp)
+end
+
+
+# DDB_GAD -- Get a double array field
+
+procedure ddb_gad (db, record, field, array, len_array, npts)
+
+pointer	db				# DTTEXT pointer
+int	record				# Database index
+char	field[ARB]			# Database field
+double	array[len_array]		# Array values
+int	len_array			# Length of array
+int	npts				# Number of points in the array
+
+pointer	sp, esp
+char	name[SZ_LINE]
+int	i
+
+int	fscan(), nscan()
+bool	streq()
+
+begin
+	if ((record < 1) || (record > DT_NRECS(db)))
+	    call error (27, "Database record request out of bounds")
+
+	call seek (DT(db), DT_OFFSET(db, record))
+
+	while (fscan (DT(db)) != EOF) {
+	    call gargwrd (name, SZ_LINE)
+
+	    if (streq (name, "begin"))
+		break
+	    else if (streq (name, field)) {
+		call gargi (npts)
+		if (nscan() != 2)
+		    call error (28, "Error in database field value")
+
+		npts = min (npts, len_array)
+		for (i = 1; i <= npts; i = i + 1) {
+		    if (fscan (DT(db)) == EOF)
+		        call error (29, "Error in database field value")
+
+		    call gargd (array[i])
+		    if (nscan() != 1)
+		        call error (30, "Error in database field value")
+		}
+		return
+	    }
+	}
+
+	call smark (sp)
+	call salloc (esp, SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[esp], SZ_LINE, 
+	    "DDB_GA: Database field '%s' not found")
+	        call pargstr (field)
+
+	call error (31, Memc[esp])
+	call sfree (sp)
+end
+
+
+# DDB_PTIME -- Put a time string with a comment
+
+procedure ddb_ptime (db)
+
+pointer	db				# DTTEXT pointer
+
+char	timestr[SZ_TIME]
+long	time, clktime()
+
+begin
+	time = clktime (0)
+	call cnvtime (time, timestr, SZ_TIME)
+	call fprintf (DT(db), "# %s\n")
+	    call pargstr (timestr)
+end
+
+
+# DDB_SCAN -- Scan a line from the database.
+
+int procedure ddb_scan (db)
+
+pointer	db			# DDB pointer
+int	fscan()
+
+begin
+	return (fscan (DT(db)))
+end
diff --git a/noao/imred/dtoi/dematch.par b/noao/imred/dtoi/dematch.par
new file mode 100644
index 00000000..cd7a5cfc
--- /dev/null
+++ b/noao/imred/dtoi/dematch.par
@@ -0,0 +1,8 @@
+# Cl parameters are:
+database,f,a,,,,Database of density information
+wedge,f,a,"",,,Wedge number used for calibration
+filter,f,a,"",,,Filter used for calibration
+emulsion,f,a,"",,,Emulsion used for calibration
+wedgefile,f,h,"noao$lib/hdwedge.dat",,,File containing exposure information
+nskip,i,h,0,,,Number of faint spots skipped
+verbose,b,h,yes,,,Print exposure record from wedgefile
diff --git a/noao/imred/dtoi/dematch.x b/noao/imred/dtoi/dematch.x
new file mode 100644
index 00000000..ff47e90f
--- /dev/null
+++ b/noao/imred/dtoi/dematch.x
@@ -0,0 +1,160 @@
+include	<error.h>
+
+# T_DEMATCH -- matches densities listed in the input database to
+# log exposure values retrieved from a system maintained or user
+# provided file.  The output matches are added to the input database.
+
+procedure t_dematch ()
+
+pointer	filter, emulsion, wedge_db, density_db, db, exp, den, sp
+pointer wedge, expo
+int	nskip, rec, nvalues
+
+pointer	ddb_map()
+bool	clgetb()
+int	ddb_locate(), ddb_geti(), clgeti()
+
+begin
+	call smark (sp)
+	call salloc (filter, SZ_FNAME, TY_CHAR)
+	call salloc (emulsion,  SZ_FNAME, TY_CHAR)
+	call salloc (wedge_db, SZ_FNAME, TY_CHAR)
+	call salloc (density_db, SZ_FNAME, TY_CHAR)
+	call salloc (wedge, SZ_FNAME, TY_CHAR)
+
+	# Get parameters
+	call clgstr ("database", Memc[density_db], SZ_FNAME)
+	call clgstr ("wedge", Memc[wedge], SZ_FNAME)
+	call clgstr ("filter", Memc[filter], SZ_FNAME)
+	call clgstr ("emulsion", Memc[emulsion], SZ_FNAME)
+	call clgstr ("wedgefile", Memc[wedge_db], SZ_FNAME)
+	nskip = clgeti ("nskip")
+
+	# Retrieve exposure information; one wedge per run
+	call hd_rwedge (Memc[wedge_db], exp, Memc[wedge], Memc[filter], 
+	    Memc[emulsion], clgetb("verbose"))
+
+	db = ddb_map (Memc[density_db], READ_ONLY)
+	iferr {
+	    rec = ddb_locate (db, "density")
+	    nvalues = ddb_geti (db, rec, "den_val")
+	} then
+	    call error (0, "Error locating density record in database")
+
+	call salloc (den, nvalues, TY_REAL)
+	iferr (call ddb_gar (db, rec, "den_val", Memr[den], nvalues, nvalues))
+	    call error (0, "Error reading density information")
+
+	# Close db file before reopening for append.
+	call ddb_unmap (db)
+
+	# Add fields for wedge, filter and plate as "calibrate" record
+	db = ddb_map (Memc[density_db], APPEND)
+	call ddb_prec (db, "calibrate")
+	call ddb_pstr (db, "wedge", Memc[wedge])
+	call ddb_pstr (db, "filter", Memc[filter])
+	call ddb_pstr (db, "emulsion", Memc[emulsion])
+
+	# Exposures are returned in increasing order.  Make sure the
+	# exposures are output in the same order as density values.
+
+	call salloc (expo, nvalues, TY_REAL)
+	call amovr (Memr[exp+nskip], Memr[expo], nvalues)
+
+	if (Memr[den] > Memr[den+nvalues-1])
+	    call hd_reorderr (Memr[expo], nvalues)
+
+	# Now add exposure values to database
+	call ddb_ptime (db)
+	call ddb_prec (db, "exposure")
+	call ddb_par (db, "log_exp", Memr[expo], nvalues)
+
+	call ddb_unmap (db)
+
+	call mfree (exp, TY_REAL)
+	call sfree (sp)
+end
+
+
+# HD_RWEDGE -- Read wedge information from database file for a given
+# wedge, filter, emulsion combination.  A pointer to the extracted
+# exposure values is returned as an argument.
+
+procedure hd_rwedge (db_file, exp, wedge, filter, emulsion, verbose)
+
+char	db_file[SZ_FNAME]	# Name of database with exposure information
+pointer	exp			# Pointer to array of exposure values - output
+char	wedge[SZ_FNAME]		# Wedge number
+char	filter[SZ_FNAME]	# Filter used
+char	emulsion[SZ_FNAME]	# Emulsion used
+bool	verbose			# Print record of exposure information?
+
+pointer	db
+char	wfe[SZ_FNAME]
+int	rec, nvalues, stat, i
+
+pointer ddb_map()
+int	ddb_locate(), ddb_geti(), ddb_scan()
+errchk	ddb_map, ddb_scan
+
+begin
+	# Convert strings to upper case for matching in database
+	call strupr (wedge)
+	call strupr (filter)
+	call strupr (emulsion)
+
+	db = ddb_map (db_file, READ_ONLY)
+	iferr (rec = ddb_locate (db, wedge))
+	    call erract (EA_FATAL)
+
+	# Construct field name of filter/emulsion combination in question
+	call sprintf (wfe, SZ_FNAME, "%s/%s")
+	    call pargstr (emulsion)
+	    call pargstr (filter)
+
+	# Retrieve exposure values from database file
+	iferr (nvalues = ddb_geti (db, rec, wfe))
+	    call erract (EA_FATAL)
+
+	call malloc (exp, nvalues, TY_REAL)
+	stat = ddb_scan (db)
+
+	do i = 1, nvalues {
+	    call gargr (Memr[exp+i-1])
+
+	    # Calibration values are stored 8 values per line
+	    if (mod (i, 8) == 0) {
+		if (nvalues > i)
+		    stat = ddb_scan (db)
+	    }
+	}
+	 
+	if (verbose) {
+	    call printf ("\nCalibration log exposure values for %s/%s: \n")
+	        call pargstr (wedge)
+	        call pargstr (wfe)
+	    
+	    do i = 1, nvalues {
+	        call printf ("%8g ")
+		    call pargr (Memr[exp+i-1])
+	        if (mod (i, 8) == 0)
+		    call printf ("\n")
+	    }
+
+	    # Need a newline if the last line didn't have 8 entries.
+	    if (mod (nvalues, 8) != 0)
+		call printf ("\n")
+
+	    call flush (STDOUT)
+	}
+
+	# Exposures are returned sorted in increasing order.  That is,
+	# the exposure for the lightest spot is element one, and the
+	# darkest spot's exposure value is the last array element.
+
+	if (Memr[exp] > Memr[exp+nvalues-1])
+	    # Out of order - flip elements
+	    call hd_reorderr (Memr[exp], nvalues)
+
+	call ddb_unmap (db)
+end
diff --git a/noao/imred/dtoi/doc/dematch.hlp b/noao/imred/dtoi/doc/dematch.hlp
new file mode 100644
index 00000000..7dffad26
--- /dev/null
+++ b/noao/imred/dtoi/doc/dematch.hlp
@@ -0,0 +1,51 @@
+.help dematch Feb87 imred.dtoi
+.ih
+NAME
+dematch -- match density to log exposure values
+.ih
+USAGE
+dematch database 
+.ih
+PARAMETERS
+.ls database
+Database containing density list, probably from \fIspotlist\fR.
+.le
+.ls wedge = "", filter = "", emulsion = ""
+Information used to retrieve log exposure values from \fBwedgefile\fR.
+.le
+.ls wedgefile = "noao$lib/hdwedge.dat"
+Name of file containing wedge intensity information.
+.le
+.ls nskip = 0
+Number of faint spots skipped, used as an offset into the list of
+log exposure values.
+.le
+.ls verbose = yes
+Print the log exposure information to STDOUT as well as to \fBdatabase\fR.
+.le
+.ih
+DESCRIPTION
+Task \fIdematch\fR matches density values to log exposure values.  A database
+of density values is input, as well as information needed to 
+retrieve log exposure values from a reference file.  The two sources of 
+information are matched, and the matching log exposure values are added 
+as a record in the database.
+
+Parameter \fBnskip\fR tells how many faint spots were not
+included in the density \fBdatabase\fR.  This information is
+used to align the density, exposure values.  It doesn't matter if the 
+densities are listed in a monotonically increasing or decreasing
+order, as long as no spots were omitted between the first and last
+measured.
+.ih
+EXAMPLES
+Match densities in db1 to log exposure values for wedge#117
+with a IIIAJ emulsion and a GG385 filter.
+.nf
+
+	cl> dematch db1 wedge=117 filt=gg385 emulsion=IIIAJ
+.fi
+.ih
+SEE ALSO
+spotlist, hdfit, hdtoi
+.endhelp
diff --git a/noao/imred/dtoi/doc/dtoi.ms b/noao/imred/dtoi/doc/dtoi.ms
new file mode 100644
index 00000000..4f999259
--- /dev/null
+++ b/noao/imred/dtoi/doc/dtoi.ms
@@ -0,0 +1,576 @@
+.RP
+.TL
+An Overview of the IRAF DTOI Package
+.AU
+Suzanne Hammond Jacoby
+.AI
+IRAF Group - Central Computer Services
+.K2 "" "" "*"
+February 1987
+.br
+Revised July 1988
+
+.AB
+This document describes the DTOI package, which contains tasks
+for determining and applying a density to intensity transformation to
+photographic data.  The transformation is determined from a set
+of calibration spots with known relative intensities.  A curve is
+interactively fit to the densities and intensities of the calibration
+spots.  The transformation is then applied and a new output image written.
+.AE
+
+.NH
+Introduction
+.PP
+The DTOI package contains tasks for computing and applying a density
+to intensity transformation to photographic data.  These tasks perform the
+standard steps in linearizing data: calculating HD data points from 
+calibration spots, fitting a curve to these points and applying the HD
+curve to the data.  It is also possible to combine related HD curves.
+Communication between the tasks is via text files which the user can 
+inspect or modify.  It is intended
+to be easy for users to introduce data from outside the DTOI package
+into the processing.
+.PP
+There are currently six tasks in the package.  They are:
+
+.ce
+The \fBDTOI\fR Package
+.TS
+center;
+n.
+spotlist \&- Calculate densities and weights of calibration spots.
+dematch \&- Match densities to log exposure values.
+hdfit \&- Fit characteristic curve to density, exposure data.
+hdtoi \&- Apply HD transformation to image data.
+hdshift \&- Align related characteristic curves.
+selftest \&- Test transformation algorithm.
+.TE
+.PP
+The DTOI package does not currently support the self calibration of images, 
+but the addition of this capability is planned.  This would involve
+determining the HD curve from the data itself, by assuming the point spread
+function scales linearly with intensity.
+.PP
+Upon entering the package, your calibration spots and images to be
+transformed should be on the disk in IRAF image format.
+
+.NH 
+Determining the HD Curve Data 
+.PP
+To determine the HD curve, you need two sets of data:  the
+measured photographic densities of a set of calibration spots and
+the log exposure values corresponding to these measurements.  The
+log exposure values must be known a priori.  Tasks \fIspotlist\fR and
+\fIdematch\fR are used to assemble these two data sets.
+.NH 2
+SPOTLIST
+.PP
+The first step is to calculate the density of
+the calibration spots, each of which is a separate IRAF image or image
+section.  The spot density is either the median of the spot pixels or
+the mean of the pixels when pixels more then a user specified number of
+standard deviations away from the mean have been rejected.  The numbers
+in the spot image must be scaled to density; parameter \fBspotlist.scale\fR
+is used such that density = input_value * scale.  Task \fIspotlist\fR also
+calculates the standard deviation of each spot and reports
+the number of good pixels, i.e., the number of pixels not rejected
+when determining the mean density.  
+The final product of this task is a record in the data base containing a
+density for each spot.  The scale factor used is also written to the data
+base; it will be read later in task \fIhdtoi\fR.
+.NH 2
+DEMATCH
+.PP
+Log exposure values must be matched to the measured density values.  These
+log exposure values must be known a priori and will be read from a file.
+Task \fIdematch\fR retrieves the proper exposure information by
+matching the wedge number, emulsion type and filter used.  Once a match
+has been made, the proper log exposure values are written to a record
+in the database.  
+.PP
+A database of log exposure values for the NOAO standard wedges is maintained 
+in a system file; the wedge/emulsion/filter combinations available are listed
+in last section of this document.  This file can be replaced with one specific 
+to any institution; the file name is supplied to task \fIdematch\fR as a 
+parameter.  In this way the wedge file can be personalized to any application 
+and not be lost when the system is updated.
+
+.NH
+Fitting the Curve
+.PP
+The HD curve, or characteristic curve, is a plot of density versus log 
+exposure.  This curve is determined from the data points generated by
+tasks \fIspotlist\fR and \fIdematch\fR.  The objective is to fit
+a curve to these points, such that Log exposure = F(Density).  The
+technique available in this package allows the independent variable of the
+fit to be a transformation of the density (log opacitance, for example).
+The log exposure and density values are
+read from the database.  If multiple entries for a particular record are 
+present in the database, the last one is used.
+.NH 2
+HDFIT
+.PP
+Task \fIhdfit\fR fits a characteristic curve to density and log exposure
+values in preparation for transforming an image from density to intensity.
+Five functional forms of the curve are available:
+.nf
+
+ 	  Power Series
+    	  Linear Spline
+    	  Cubic Spline
+    	  Legendre Polynomials
+    	  Chebyshev Polynomials
+ 	
+.fi
+.LP 
+It is possible to apply a transformation to the 
+independent variable (density above fog) prior to the fit.  The traditional 
+choice is to fit log exposure
+as a function of the log opacitance, rather than density directly.  This is
+sometimes referred to as the Baker, or Seidel, function.  Transforming
+the density has the effect of stretching the low density data points, which
+tend to be relatively oversampled. 
+In the DTOI package, four independendent variables are currently available:
+.nf
+
+ 	Density
+ 	Log Opacitance
+ 	K50 - (Kaiser* Transform with alpha = 0.50)
+ 	K75 - (Kaiser* Transform with alpha = 0.75)
+
+.fi
+.FS
+* Margoshes and Rasberry, Spectrochimica Acta, Vol 24B, p497, (1969)
+.FE
+Any combination of transformation type and fitting function can be used and
+changed interactively.  Two combinations of interest are discussed here.
+
+The default fit is a power series fit where the independent variable is 
+Log Opacitance.  That is:
+.LP
+.EQ
+
+	"Log Exposure = " sum from k=0 to {ncoeff - 1} {A sub k Y sup k}
+
+.EN
+.sp 1
+.EQ
+	"where Y = Log Opacitance = "Log sub 10 (10 sup Density - 1)
+.EN
+.LP
+A fit that is expected to best model a IIIA-J emulsion is a power series
+fit to a K75 transform of the density.  That is,
+.LP
+.EQ
+
+	"Log Exposure = "sum from k=0 to {ncoeff - 1} {A sub k Y sup k}
+
+.EN
+.sp 1
+.EQ
+"where Y = K75 transform = Density + 0.75 " Log sub 10 (1 - 10 sup -Density )
+.EN
+.LP
+Over the expected small dynamic range in variables of the fit, legendre
+and chebyshev functions offer no advantages over a simple power series
+functional form.  The cubic and linear spline fits may follow the data very
+closely, but with typically sparse data sets this is not desirable.  It
+is expected that power series fit will serve satisfactorily in all cases.
+
+.NH 3
+Interactive Curve Fitting
+.PP
+Task \fIhdfit\fR can be run interactively or not.  In interactive mode,
+points in the sample can be edited, added or deleted.  Weighting values
+can be changed as well as the fog value, the type of transformation
+and the fitting function chosen.  To obtain the best fit possible, interactive
+fitting is recommended.  A complete list of the available commands
+is printed here; this list is also available interactively with the 
+keystroke '\fL?\fR'.
+.TS
+center;
+c s s w(3.0i)
+c l s.
+
+	DTOI INTERACTIVE CURVE FITTING OPTIONS 
+
+\fL?\fR	Print options
+\fLa\fR	Add the point at the cursor position to the sample
+\fLc\fR	Print the coordinates and fit of point nearest the cursor
+\fLd\fR	Delete data point nearest the cursor
+\fLf\fR	Fit the data and redraw or overplot
+\fLg\fR	T{
+Redefine graph keys.  Any of the following data types may be along
+either axis:
+T}
+.T&
+l l l.
+ 	\fLx\fR  Independent variable	\fLy\fR  Dependent variable
+ 	\fLf\fR  Fitted value	\fLr\fR  Residual (y - f)
+ 	\fLd\fR  Ratio (y / f)	\fLn\fR  Nonlinear part of y
+ 	\fLu\fR  Density above fog
+
+Graph keys:	 	 
+.T&
+c l s.
+
+\fLh\fR	h = (x,y)  transformed density vs. log exposure
+\fLi\fR	i = (y,x)  log exposure vs. transformed density
+\fLj\fR	j = (x,r)  transformed density vs. residuals
+\fLk\fR	k = (x,d)  transformed density vs. the y(data)/y(fit) ratio
+\fLl\fR	l = (y,u)  log exposure vs. density above fog (HD Curve)
+
+\fLo\fR	Overplot the next graph
+\fLq\fR	T{
+Terminate the interactive curve fitting, updating the database file. 
+T}
+\fLr\fR	Redraw graph
+\fLu\fR	Undelete the deleted point nearest the cursor
+\fLw\fR	Set the graph window.  For help type 'w' followed by '?'.
+\fLx\fR	Change the x value of the point nearest the cursor
+\fLy\fR	Change the y value of the point nearest the cursor
+\fLz\fR	Change the weight of the point nearest the cursor
+
+.T&
+l s s w(3.0i).
+T{
+The parameters are listed or set with the following commands which may be
+abbreviated.  To list the value of a parameter type the command alone.
+T}
+
+.T&
+l l s.
+
+\fL:show \fR[\fIfile\fR]	Show the values of all the parameters
+\fL:vshow \fR[\fIfile\fR]	Show the values of all the parameters verbosely
+\fL:errors \fR[\fIfile\fR]	Print the errors of the fit (default STDOUT)
+\fL:reset \fR	T{
+Return to original conditions of x, y, wts and npts.
+T}
+\fL:ebars \fR[\fIerrors/weights\fR]	T{
+The size of marker type '[hv]ebars' can show either standard deviations or
+relative weights.
+T}
+\fL:function \fR[\fIvalue\fR]	T{
+Fitting function (power, chebyshev, legendre, spline3, or spline1)
+T}
+\fL:transform \fR[\fIvalue\fR]	Set the transform type (none, logo, k50, k75)
+\fL:fog \fR[\fIvalue\fR]	Change the fog level (or ":fog reset")
+\fL:order \fR[\fIvalue\fR]	Fitting function order
+\fL:quit \fR	Terminate HDFIT without updating database
+\fL:/mark \fRstring	T{
+Mark type (point, box, plus, cross, diamond, hline, vline, hebar, vebar, circle)
+T}
+
+.T&
+l s s.
+T{
+Additional commands are available for setting graph formats and manipulating
+the graphics.  Use the following commands for help.
+T}
+
+.T&
+l l s.
+\fL:/help\fR	Print help for graph formatting option
+\fL:.help\fR	Print cursor mode help
+
+.TE
+.PP
+The value of fog can be changed interactively if you have
+reason to override the value written in the database by \fIspotlist\fR.
+You can reset the fog to its original value with the command ":fog reset".
+A common problem with defining the HD curve is that some of 
+the calibration spot densities fall below fog.  This is caused by either
+the low signal to noise at low densities or by making a poor choice of 
+where to scan the fog level.  These points are rejected from the fit
+when a transformation of the density is being made, as the transform cannot
+be evaluated for negative density.  If the fog value or transformation 
+type is interactively changed so this problem no longer exists, 
+the spot densities are restored in the sample.
+
+The parameters of the final fit are written to a database which then
+contains the information
+necessary to reinitialize the curfit package for applying the transformation
+in \fIhdtoi\fR.  
+
+.NH
+Applying the Transform
+.PP
+.NH 2
+HDTOI
+.PP
+Once the HD curve has been defined, it is applied to a density image
+in task \fIhdtoi\fR.
+Here the transformation is applied, as described by the fit parameters
+stored in the database.  If more than one record of fit parameters is
+present, the last one is used.  This means task \fIhdfit\fR can be
+repeated until an acceptable solution is found; the last solution will
+be used by \fIhdtoi\fR.  On output, a new output image is written; the 
+input image is left intact.
+.PP
+The transformation is accomplished by using a look-up table.  All possible
+input values, from the minimum to maximum values found in the image, are
+converted to density using the scale value read from the database, and then 
+to intensity using the fit parameters determined by \fIhdfit\fR.  The input
+value is then the index into the intensity table: 
+intensity = look_up_table (input_value).
+.PP
+A scaling factor can be applied to the final intensities, as typically
+they will be < 1.0.  (The maximum log exposure in the NOAO wedge database
+is 0.0)  By default, a saturated density pixel will be assigned the "ceiling"
+intensity of 30000 and the other pixels are scaled accordingly.  
+The user is responsible for choosing a ceiling value
+that will avoid having significant digits truncated.
+The precision 
+of the transform is unaffected by scaling the
+final intensities, although caution must be used if the output image
+pixel type is an integer.  
+.PP
+The value of fog to be used is entered by the user, and can be either
+a number or a list of file names from which to calculate the fog value.
+The fog value is subtracted from the input image before the transformation
+takes place.
+Again, consider density values below fog.  Two choices are available for
+these densities: the calculated intensity can be equal to the constant 
+value 0.0 or equal -1.0 times the intensity determined for absolute (density).
+
+.NH
+Aligning Related HD curves
+.PP
+Calibration data sets from several plates can be combined once a shift
+particular to each set has been removed.  "Different spot exposures 
+define a series of HD curves which are parallel but mutually separated
+by arbitrary shifts in log exposure, produced by differing lamp intensities
+or exposure times.  Generally, Kodak spectroscopic plates can be
+averaged if [1] they come from the same emulsion batch and box, [2]
+they receive identical hypersensitizing, [3] they are exposed similarly and
+[4] they receive the same development." * 
+.FS
+* "Averaging Photographic Characteristic Curves", John Kormendy, from
+"ESO Workshop on Two Dimensional Photometry", Edited by P. Crane and
+K.Kjar, p 69, (1980), an ESO Publication.
+.FE
+.NH 2
+HDSHIFT
+.PP
+Procedure \fIhdshift\fR calculates and subtracts a zero point shift to 
+bring several related HD curves into alignment.  The individual shifts 
+are calculated by elimination of the first coefficient (Bevington, eqn 9-3):
+.EQ
+
+a0 = y bar - a sub 1 X bar - a sub 2 X bar sup 2 - ~ ...~ - a sub n X bar sup n
+
+.EN
+Here, the averages over y and X refer to individual calibration set averages; 
+the coefficients a1, ... an were previously calculated using data from all 
+calibration sets with task \fIhdfit\fR, and stored in the database.  The
+a0 term is calculated individually for each database; this term represents
+the zero point shift in log exposure and will be different for each database.
+
+On output, the log exposure values in each database have been 
+shifted to the zero point shift of the first database in the list.  The
+log exposure records are now aligned and it would be appropriate
+to run \fIhdfit\fR on the modified database list.
+.NH
+Testing the Transformation Algorithm
+.PP
+A test task is included to see if any numerical errors were introduced
+during the density to intensity transformation.  It also evaluates
+truncation errors produced when an output image with integer pixels,
+rather than reals, is written.
+.NH 2
+SELFTEST
+.PP
+An intensity vector is generated from a density vector in two different
+ways.  The first method uses the density vector and known coefficients
+to compute the intensity.  The second method uses the curfit package
+to generate a look up table of intensities as done in task \fIhdtoi\fR.  The
+residual of the two vectors is plotted; ideally the difference between
+the 'known' and 'calculated' intensity is zero.
+.PP
+Task \fIselftest\fR also plots intensity as a function of density for
+both integer and real output pixels.  The user should investigate the
+plot with the cursor zoom and expand capabilities to determine if
+truncation errors are significant.
+.NH
+The Wedgefile Database
+.PP
+Task \fIdematch\fR reads a database and retrieves log exposure information 
+for certain combinations of wedge number, photographic emulsion and filter.  
+Those combinations included in the NOAO database are listed in the next 
+section, although any calibration data can be included if the values are
+known.  To modify the database, it is recommended that
+you generate a new file rather than add records to the existing file.  This
+way, the modifications will not be lost when a new version of the IRAF
+system is released.  
+
+In the database, the information for each wedge makes up a separate record;
+each record starts with the word \fBbegin\fR.  Each record has a title field 
+and can have multiple emulsion/filter fields.  The number of log exposure
+values must be given, followed by the values written 8 per line.  The order 
+of the exposure data can be either monotonically increasing or decreasing.  
+Here is an example:
+.DS
+begin	115
+	title	MAYALL 4-M PF BEFORE 15APR74 (CHROME) [MP1-MP968]
+	IIIAJ/UG2	16
+		  0.000 -0.160 -0.419 -0.671 -0.872 -1.153 -1.471 -1.765
+		 -2.106 -2.342 -2.614 -2.876 -3.183 -3.555 -3.911 -4.058
+	IIAO/UG2	16
+		  0.000 -0.160 -0.418 -0.670 -0.871 -1.152 -1.468 -1.761
+		 -2.102 -2.338 -2.609 -2.870 -3.176 -3.547 -3.901 -4.047
+
+.DE
+.NH 2
+Contents of the NOAO Wedgefile
+.LP
+The following table lists the wedge/emulsion/filter combinations available in
+the NOAO wedgefile database.  
+.TS
+center;
+l l s s s
+l l l l l.
+
+\fBWedge  24 	CTIO SCHMIDT WESTON TUBE SENSITOMETER.            \fR
+ 	MONO/MONO					
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge  48 	PALOMAR 48-INCH SCHMIDT STEP WEDGE.               \fR
+ 	MONO/MONO			
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge  84 	OLD 84-INCH SPOT SENSITOMETER (1967)               \fR
+ 	MONO/MONO			
+
+.TE
+.TS
+l l s s s
+l l l l l.
+\fBWedge 101 	SPOT BOX 4, KEPT IN SCHOENING-S LAB.              \fR
+ 	IIIAJ/UG2	IIAO/UG2	IIIAJ/*5113	IIAO/*5113       
+ 	IIAO/GG385	IIIAJ/CLEAR	IIIAJ/GG385	IIAD/GG495       
+ 	127/GG495	098/RG610	127/RG610	IVN/RG695       
+ 	MONO/4363	MONO/4760	MONO/5200	MONO/5876        
+ 	MONO/6470			
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge 115 	MAYALL 4-M PF BEFORE 15APR74 (CHROME) [MP1-MP968] \fR
+ 	IIIAJ/UG2	IIAO/UG2	IIIAJ/*5113	IIAO/*5113       
+ 	IIAO/GG385	IIIAJ/CLEAR	IIIAJ/GG385	IIAD/GG495       
+ 	127/GG495	098/RG610	127/RG610	IVN/RG695       
+ 	MONO/4363	MONO/4770	MONO/5200	MONO/5876        
+ 	MONO/6470			
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge 117 	CTIO 4-METER P.F.                                 \fR
+ 	IIIAJ/UG2	IIAO/UG2	IIIAJ/*5113	IIAO/*5113       
+ 	IIAO/GG385	IIIAJ/CLEAR	IIIAJ/GG385	IIAD/GG495       
+ 	127/GG495	098/RG610	127/RG610	IVN/RG695       
+ 	MONO/4363	MONO/4770	MONO/5200	MONO/5876        
+ 	MONO/6470			
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge 118 	CTIO 4-METER CASSEGRAIN                           \fR
+ 	IIIAJ/UG2	IIAO/UG2	IIIAJ/*5113	IIAO/*5113       
+ 	IIAO/GG385	IIIAJ/CLEAR	IIIAJ/GG385	IIAD/GG495       
+ 	127/GG495	098/RG610	127/RG610	IVN/RG695       
+ 	MONO/4363	MONO/4760	MONO/5200	MONO/5876        
+ 	MONO/6470	MONO/6900		
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge 119	SPOT BOX 5, KEPT AT MAYALL 4-METER.               \fR
+ 	IIIAJ/UG2	IIAO/UG2	IIIAJ/*5113	IIAO/*5113       
+ 	IIAO/GG385	IIIAJ/CLEAR	IIIAJ/GG385	IIAD/GG495       
+ 	127/GG495	098/RG610	127/RG610	IVN/RG695       
+ 	MONO/4363	MONO/4760	MONO/5200	MONO/5876        
+ 	MONO/6470			
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge 120 	SPOT BOX 6, KEPT AT 2.1-METER.                    \fR
+ 	IIIAJ/UG2	IIAO/UG2	IIIAJ/*5113	IIAO/*5113       
+ 	IIAO/GG385	IIIAJ/CLEAR	IIIAJ/GG385	IIAD/GG495       
+ 	127/GG495	098/RG610	127/RG610	IVN/RG695       
+ 	MONO/4363	MONO/4760	MONO/5200	MONO/5876        
+ 	MONO/6470			
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge 121 	SPOT BOX 8, KEPT IN SCHOENING'S LAB.              \fR
+ 	IIIAJ/UG2	IIAO/UG2	IIIAJ/*5113	IIAO/*5113       
+ 	IIAO/GG385	IIIAJ/CLEAR	IIIAJ/GG385	IIAD/GG495       
+ 	127/GG495	098/RG610	127/RG610	IVN/RG695       
+ 	MONO/4363	MONO/4760	MONO/5200	MONO/5876        
+ 	MONO/6470        
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge 122 	SPOT BOX 7, AVAILABLE AT KPNO NIGHT ASST'S OFFICE \fR
+ 	IIIAJ/UG2	IIAO/UG2	IIIAJ/*5113	IIAO/*5113       
+ 	IIAO/GG385	IIIAJ/CLEAR	IIIAJ/GG385	IIAD/GG495       
+ 	127/GG495	098/RG610	127/RG610	IVN/RG695       
+ 	MONO/4363	MONO/4760	MONO/5200	MONO/5876        
+ 	MONO/6470C			
+.TE
+.TS
+l l s s s
+l l l l l.
+\fBWedge 123 	MAYALL 4-M P.F. 15APR74 TO 21MAY74 [MP969-MP1051] \fR
+ 	IIIAJ/UG2	IIAO/UG2	IIIAJ/*5113	IIAO/*5113       
+ 	IIAO/GG385	IIIAJ/CLEAR	IIIAJ/GG385	IIAD/GG495       
+ 	127/GG495	098/RG610	127/RG610	IVN/RG695       
+ 	MONO/4363	MONO/4770	MONO/5200	MONO/5876        
+ 	MONO/6470        
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge 129 	MAYALL 4-METER P.F. AFTER 21MAY74 [MP1052-->  ]   \fR
+ 	IIIAJ/UG2	IIAO/UG2	IIIAJ/*5113	IIAO/*5113       
+ 	IIAO/GG385	IIIAJ/CLEAR	IIIAJ/GG385	IIAD/GG495       
+ 	127/GG495	098/RG610	127/RG610	IVN/RG695       
+ 	MONO/4363	MONO/4760	MONO/5200	MONO/5876        
+ 	MONO/6470			
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge 130 	MAYALL 4-METER CASS CAMERA.                       \fR
+ 	IIIAJ/UG2	IIAO/UG2	IIIAJ/*5113	IIAO/*5113       
+ 	IIAO/GG385	IIIAJ/CLEAR	IIIAJ/GG385	IIAD/GG495       
+ 	127/GG495	098/RG610	127/RG610	IVN/RG695       
+ 	MONO/4363	MONO/4760	MONO/5200	MONO/5876        
+ 	MONO/6470			
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge 138 	TRAVELLING BOX AFTER 06JAN78.                    \fR
+ 	IIIAJ/UG2	IIAO/UG2	IIIAJ/*5113	IIAO/*5113       
+ 	IIAO/GG385	IIIAJ/CLEAR	IIIAJ/GG385	IIAD/GG495       
+ 	127/GG495	098/RG610	127/RG610	IVN/RG695       
+ 	MONO/4363	MONO/4770	MONO/5200	MONO/5876        
+ 	MONO/6470			
+
+.T&
+l l s s s
+l l l l l.
+\fBWedge 201 	TEN UCLA SPOTS (H. FORD, 10JAN78)                 \fR
+ 	MONO/MONO			
+.TE
diff --git a/noao/imred/dtoi/doc/dtoi.toc b/noao/imred/dtoi/doc/dtoi.toc
new file mode 100644
index 00000000..cd794321
--- /dev/null
+++ b/noao/imred/dtoi/doc/dtoi.toc
@@ -0,0 +1,34 @@
+.LP
+.DS C
+\fBTable of Contents\fR
+.DE
+.sp 3
+1.\h'|0.4i'\fBIntroduction\fP\l'|5.6i.'\0\01
+.sp
+2.\h'|0.4i'\fBDetermining the HD Curve Data \fP\l'|5.6i.'\0\01
+.br
+\h'|0.4i'2.1.\h'|0.9i'SPOTLIST\l'|5.6i.'\0\02
+.br
+\h'|0.4i'2.2.\h'|0.9i'DEMATCH\l'|5.6i.'\0\02
+.sp
+3.\h'|0.4i'\fBFitting the Curve\fP\l'|5.6i.'\0\02
+.br
+\h'|0.4i'3.1.\h'|0.9i'HDFIT\l'|5.6i.'\0\02
+.br
+\h'|0.9i'3.1.1.\h'|1.5i'Interactive Curve Fitting\l'|5.6i.'\0\03
+.sp
+4.\h'|0.4i'\fBApplying the Transform\fP\l'|5.6i.'\0\05
+.br
+\h'|0.4i'4.1.\h'|0.9i'HDTOI\l'|5.6i.'\0\05
+.sp
+5.\h'|0.4i'\fBAligning Related HD curves\fP\l'|5.6i.'\0\06
+.br
+\h'|0.4i'5.1.\h'|0.9i'HDSHIFT\l'|5.6i.'\0\06
+.sp
+6.\h'|0.4i'\fBTesting the Transformation Algorithm\fP\l'|5.6i.'\0\06
+.br
+\h'|0.4i'6.1.\h'|0.9i'SELFTEST\l'|5.6i.'\0\06
+.sp
+7.\h'|0.4i'\fBThe Wedgefile Database\fP\l'|5.6i.'\0\06
+.br
+\h'|0.4i'7.1.\h'|0.9i'Contents of the NOAO Wedgefile\l'|5.6i.'\0\07
diff --git a/noao/imred/dtoi/doc/hdfit.hlp b/noao/imred/dtoi/doc/hdfit.hlp
new file mode 100644
index 00000000..0b55137e
--- /dev/null
+++ b/noao/imred/dtoi/doc/hdfit.hlp
@@ -0,0 +1,79 @@
+.help hdfit Mar88 imred.dtoi
+.ih
+NAME
+hdfit -- fit characteristic curve to density, exposure data
+.ih
+USAGE
+hdfit database 
+.ih
+PARAMETERS
+.ls database
+Database[s] containing the density, log exposure information.
+.le
+.ls function = "power"
+Type of curve to fit; chosen from "power", "legendre", "chebyshev", 
+"spline1" or "spline3".  Abbreviations are permitted.
+.le
+.ls transform = "logopacitance"
+Transformation performed on the density prior to fitting.  Chosen from
+"none", "logopacitance", "k50" or "k75". 
+.le
+.ls weighting = "none"
+Weights can be assigned to the independent variable for fitting a curve.
+Choices are "none", "user" and "calculated".
+.le
+.ls order = 4
+Order of the fit.
+.le
+.ls interactive = yes
+Fit the data interactively?
+.le
+.ls device = "stdgraph"
+Interactive graphics device.
+.le
+.ls cursor = "stdgcur"
+Source of cursor input.
+.le
+.ih
+DESCRIPTION
+Task \fIhdfit\fR is used to fit a curve to density and log exposure
+values in preparation for transforming an image from density to intensity.
+The log exposure and density are read from \fBdatabase\fR.
+More than one database can be input,
+in which case one curve is fit to the combined data and the results
+written to each database in the list.
+
+Weights can be applied to the independent variable of the fit.
+Weights can be changed interactively, and are originally chosen from
+"none", "user" and "calculated".  A weights value can
+be calculated from the standard deviations, read from \fBdatabase\fR,
+as weight = (normalized density) / sdev.  If user weights are to be
+used, they are read from \fBdatabase\fR record "weights" as "wts_vals"
+entries.  
+
+When \fBinteractive\fR = yes, the HD curve is plotted and the cursor
+made available for interactively examining and altering the fit.
+The fitting function, transformation and order can be modified; data
+points can be added, deleted or edited.  Four choices of independent
+variable are available in \fBhdfit\fR by means of the parameter 
+\fBtransform\fR.  No transformation can take place, in which case
+the independent variable is the density.  Other choices are the log
+opacitance or a Kaiser transform with alpha = 0.50 or 0.75.  The
+default choice is to fit log exposure as a function of the log opacitance; 
+this is traditionally known as the Baker-Seidel function.
+.ih
+EXAMPLES
+.nf
+Using the defaults as starting parameters, interactively fit a curve to
+the data points in db1.
+
+	cl> hdfit db1 
+
+A sixth order power series function is fit in batch mode to the db1 data.
+
+	cl> hdfit db1 order=6 interactive-
+.fi
+.ih
+SEE ALSO
+spotlist, dematch, hdtoi
+.endhelp
diff --git a/noao/imred/dtoi/doc/hdshift.hlp b/noao/imred/dtoi/doc/hdshift.hlp
new file mode 100644
index 00000000..aaa59063
--- /dev/null
+++ b/noao/imred/dtoi/doc/hdshift.hlp
@@ -0,0 +1,50 @@
+.help hdshift Feb87 imred.dtoi
+.ih
+NAME
+hdshift - calculate and subtract zero point to align HD curves.
+.ih
+USAGE
+hdshift database
+.ih
+PARAMETERS
+.ls database
+Input list of databases containing density, exposure and fit information.
+.le
+.ih
+DESCRIPTION
+For each file in \fBdatabase\fR, procedure \fBhdshift\fR calculates and 
+subtracts a zero point shift to bring several related HD curves into
+alignment.  The individual shifts are calculated by elimination of the 
+first coefficient (Bevington, eqn 9-3):
+.nf
+                _      _      _               _
+           a0 = y - a1*X - a2*X**2 - ... - an*X**n
+
+.fi
+Here, the averages over y and X refer to individual \fBdatabase\fR averages; 
+the coefficients a1, ... an were previously calculated using data from all 
+\fBdatabase\fRs, in task \fIhdfit\fR, and stored in the database.  The
+a0 term is calculated individually for each database; this term represents
+the zero point shift in log exposure and will be different for each database.
+
+On output, the log exposure values in each \fBdatabase\fR have been 
+shifted to the zero point shift of the first database in the list.  The
+log exposure records are now aligned and it would be appropriate
+to run task \fIhdfit\fR on the modified \fBdatabase\fR list and
+determine the common solution.
+.ih
+EXAMPLES
+.nf
+
+Shift the curves in four databases to a common zero point.  
+
+	cl> hdshift db1,db2,db3,db4
+.fi
+.ih
+SEE ALSO
+hdfit, hdtoi
+.br
+"Averaging Photographic Characteristic Curves", John Kormendy, from
+"ESO Workshop on Two Dimensional Photometry", Edited by P. Crane and
+K.Kjar, p 69, (1980), an ESO Publication.
+.endhelp
diff --git a/noao/imred/dtoi/doc/hdtoi.hlp b/noao/imred/dtoi/doc/hdtoi.hlp
new file mode 100644
index 00000000..bf4355f0
--- /dev/null
+++ b/noao/imred/dtoi/doc/hdtoi.hlp
@@ -0,0 +1,88 @@
+.help hdtoi May88 imred.dtoi
+.ih
+NAME
+hdtoi -- transform images according to hd curve
+.ih
+USAGE
+hdtoi input output database
+.ih
+PARAMETERS
+.ls input
+List of images to be transformed.
+.le
+.ls output
+List of output image names.
+.le
+.ls database
+Name of text database describing HD curve.
+.le
+.ls fog = ""
+Value of fog level, read from database if unspecified.
+.le
+.ls option = "mean"
+Option for calculating fog density when \fBfog\fR is a file list, can be
+either "mean" or "median".
+.le
+.ls sigma = 3.0
+If \fBfog\fR is a file name, and \fBoption\fR = "mean", the mean fog density
+is iteratively calculated using this rejection criteria.
+.le
+.ls floor = 0.0
+Value assigned to levels below fog, can be either 0.0 or -1.0.  
+.le
+.ls ceiling = 30000.
+The final intensities are scaled to this value, such that a saturated
+input density equals \fBceiling\fR on output.
+.le
+.ls datatype = "r"
+Datatype of output image pixels.
+.le
+.ls verbose = yes
+Print log of processing to STDOUT.
+.le
+.ih
+DESCRIPTION
+Task \fIhdtoi\fR transforms one image to another as described by the 
+\fBdatabase\fR.  There is only one HD curve per run; the same 
+transformation is applied to all input images.
+
+The fog value can be obtained in three ways: read from the database, read
+as a floating point number, or calculated from a list of fog images.  If 
+parameter \fBfog\fR is not specified, the fog value is read from 
+\fBdatabase\fR.  If \fBfog\fR is specified, it can be entered
+as either a floating point number or as a list of file names.  If the
+value cannot be read as a number, it is assumed to be a file name.  In that
+case, the density of each file in the fog list is calculated and the 
+average of these values is subtracted from \fBinput\fR before processing.
+The algorithm used to calculate the fog density is selected by the
+\fBoption\fR parameter, and is either a "mean" or "median" calculation.
+The fog density can be the mean value after pixels more than the specified
+number of sigma have been rejected, or the median value of all the fog spot
+pixels.
+
+The fog value is subtracted from the input image before the transformation
+takes place.  It is possible that some density values will fall below
+the fog level; these values are handled in one of two ways.  Values
+below the fog value are set equal to 0.0 when \fBfloor\fR = 0.0.  If 
+\fBfloor\fR = -1.0, the resulting intensity = -1 * intensity (abs (value)).
+
+A scaling factor is applied to the final intensities, as typically
+they will be < 1.0.  The \fBceiling\fR parameter is used to specify what
+value a saturated density is transformed to; all intensities are scaled
+to this upper limit.  The precision of the transformation is unaffected by 
+this parameter, although caution must be used if the output image pixel
+type is an integer.  The user is responsible for choosing
+a \fBceiling\fR that avoids the truncation of significant digits.
+.ih
+EXAMPLES
+Convert three density images to intensity images as described in database db1.
+
+	cl> hdtoi denin* intim1,intim2,intim3 db1
+.ih
+TIME REQUIREMENTS
+Task \fBhdtoi\fR requires 20 cpu seconds to transform a 512 square image, with
+a 12 bit data range, on a VAX 750
+.ih
+SEE ALSO
+spotlist, dematch, hdfit
+.endhelp
diff --git a/noao/imred/dtoi/doc/selftest.hlp b/noao/imred/dtoi/doc/selftest.hlp
new file mode 100644
index 00000000..329c9099
--- /dev/null
+++ b/noao/imred/dtoi/doc/selftest.hlp
@@ -0,0 +1,81 @@
+.help selftest Feb87 imred.dtoi
+.ih
+NAME
+selftest -- test routine to verify \fIdtoi\fR transformation
+.ih
+USAGE
+selftest nbits
+.ih
+PARAMETERS
+.ls nbits = 12
+Dymanic range of data to test.
+.le
+.ls device = "stdgraph" 
+Plotting device for graphical output.
+.le
+.ls verbose = no
+A table of density, intensity values is printed if \fBverbose\fR = yes.
+.le
+.ls ceiling = 30000.
+Maximum intensity to output.
+.le
+.ls max_raw = 0
+The maximum raw data value.  Needed only if \fInbits\fR equals something
+other than 12, 15 or 0.
+.le
+.ls scale = 0.0
+The raw data value to density scale value.  Needed only if \fInbits\fR
+equals something other than 12, 15, or 0.
+.le
+
+.ih
+DESCRIPTION
+Task \fIselftest\fR is a test program for the \fIdtoi\fR package.  Its 
+output can be examined to see if numerical errors are introduced during
+the density to intensity transformation.  It also evaluates truncation
+errors produced when an output image with integer pixels is written.  
+
+Many different PDS setups can be investigated with task \fBselftest\fR.
+Setting parameter \fInbits\fR = 12
+indicates PDS format data, with data range 0 to 3071.  Setting \fInbits\fR = 15 
+indicates FITS format data, with data range 0 to 24575.  The special value of
+\fInbits\fR = 0 means a small test data range from 1 to 144 is investigated.
+If any other value of \fInbits\fR is entered, the user is queried for the
+max raw data values and the raw data to density scaling factor.
+
+An intensity vector is generated from a density vector in two different ways.  
+The first method uses the density vector and known coefficients to compute
+the intensity.  The second method uses the curfit package to generate a
+look up table of intensities as done in task \fBHDTOI\fR.  The residual
+of the two intensity vectors is plotted.  Ideally, the difference between
+the 'known' intensities and 'calculated' intensities is zero.
+
+The second plot output by \fBselftest\fR shows intensity as a function
+of density.  Two lines are overplotted; integer intensity versus density
+and real intensity versus density.  Because truncation errors are most
+pronounced at low density values, the plot covers only the lowest 5%
+of the density range.  The user should investigate the plot with the
+cursor zoom and expand capabilities to determine if truncation errors
+are significant.
+
+In verbose mode, \fBselftest\fR produced a three column table of raw
+data value, density and calculated intensity. 
+
+.ih
+EXAMPLES
+
+.nf
+Run task selftest for 12 bit data with plots appearing on the terminal.
+
+	cl> selftest
+
+.fi
+Run selftest in verbose mode, spooling the output to file 'ditable'.  This
+file is then run through the 'fields' task to extract the density and intensity
+columns which are piped to plot.  The results in a plot of the look up table.
+.nf
+
+	cl> selftest ver+ > ditable
+	cl> fields ditable 2,3 | graph xlab=Density ylab=Intensity
+.fi
+.endhelp
diff --git a/noao/imred/dtoi/doc/splotlist.hlp b/noao/imred/dtoi/doc/splotlist.hlp
new file mode 100644
index 00000000..43b3f223
--- /dev/null
+++ b/noao/imred/dtoi/doc/splotlist.hlp
@@ -0,0 +1,81 @@
+.help spotlist May88 imred.dtoi
+.ih
+NAME
+spotlist -- calculate densities of calibration spots 
+.ih
+USAGE
+spotlist spots fogs database
+.ih
+PARAMETERS
+.ls spots
+List of image files containing the calibration data.
+.le
+.ls fogs
+List of image files containing fog spots.
+.le
+.ls database
+Name for output database.
+.le
+.ls scale = 0.00151			# (4.65 / 3071.)
+The scale factor to convert values in the image files to densities, such
+that scale = density / input_value.
+.le
+.ls maxad = 3071
+The maximum A/D value, that is, the input value corresponding to a
+saturated pixel.
+.le
+.ls option= "mean"
+Option for calculating densities can be either "mean" or "median".
+.le
+.ls sigma = 3.0
+Rejection criteria for iteratively calculating mean density.
+.le
+.ih
+DESCRIPTION
+Task \fIspotlist\fR reads calibration spot images and calculates their
+density and standard deviation.  Three records are entered in the
+database: density, standard deviation and number of unrejected pixels.
+Each record contains as many entries as calibration spots.
+
+All input values are multiplied by the \fBscale\fR parameter to convert
+them to densities.  The value of \fBscale\fR is not critical to the 
+reductions, it is provided so that \fIspotlist\fR output can be in the 
+familiar units of density.  The default value of \fBscale\fR is correct
+for NOAO PDS data written to a PDS format tape.  If a FITS format tape was 
+written, \fBscale\fR = 0.0001893.  These values are appropriate for the PDS 
+with its new 15-bit logarithmic A to D converter.  The value of \fBscale\fR
+used is also entered in the database.
+
+Parameter \fBmaxad\fR is the integer input value that represents a
+saturated pixel.  This value is used by \fIspotlist\fR to accurately
+calculate the density of a saturated pixel, which is then entered in the
+database.  This value of "maxden" will later be used by task \fIhdfit\fR
+to normalize the independent variable vector, and by task \fIhdtoi\fR to
+scale the intensity range precisely to a user specified value.
+
+A fog level is calculated from image \fBfogs\fR, and entered into
+the database file.  If more than one image is given for \fBfogs\fR, 
+a single fog value is calculated from all fog pixels.  The fog level
+is calculated but not subtracted in this procedure.  The fog images to be 
+averaged should be the same size.  An entry for the fog level is made
+in the database.
+
+The \fBspots\fR files are assumed to be ordered such that they are either
+monotonically increasing or decreasing in density, with no omitted spots
+between the first and last measured.  The calculated density can be
+calculated two ways; the algorithm used is selected by the \fBoption\fR
+parameter.  The density is either the mean spot value after pixels more
+than the specified number of sigma from the mean value have been rejected,
+or the median value of all the spot pixels.  
+.ih
+EXAMPLES
+Calculate mean densities of calibration spots which had previously been
+read in from a FITS format tape.  The database "db1" will be created.
+
+.nf
+	cl> spotlist spots* fogspot db1 scale=1.893e-4
+.fi
+.ih
+SEE ALSO
+dematch, hdfit, hdtoi
+.endhelp
diff --git a/noao/imred/dtoi/dtoi.cl b/noao/imred/dtoi/dtoi.cl
new file mode 100644
index 00000000..3dd6c42b
--- /dev/null
+++ b/noao/imred/dtoi/dtoi.cl
@@ -0,0 +1,16 @@
+#{
+# DTOI package -- Density to Intensity Transformation Package.  (Feb87)
+
+set	dtoi		= "iraf$noao/imred/dtoi/"
+
+package	dtoi
+
+task	dematch,
+	hdfit,
+	hdtoi,
+	hdshift,
+	selftest,
+	spotlist	= "dtoi$x_dtoi.e"
+
+
+clbye()
diff --git a/noao/imred/dtoi/dtoi.hd b/noao/imred/dtoi/dtoi.hd
new file mode 100644
index 00000000..af554ac2
--- /dev/null
+++ b/noao/imred/dtoi/dtoi.hd
@@ -0,0 +1,11 @@
+# Help directory for the dtoi package.
+
+$doc		= "iraf$noao/imred/dtoi/doc/"
+
+dematch		hlp=doc$dematch.hlp,		src=dematch.x
+hdfit		hlp=doc$hdfit.hlp,		src=hdfit.x
+hdtoi		hlp=doc$hdtoi.hlp,		src=hdtoi.x
+hdshift		hlp=doc$hdshift.hlp,		src=hdshift.x
+spotlist	hlp=doc$spotlist.hlp,		src=spotlist.x
+selftest	hlp=doc$selftest.hlp,		src=selftest.x
+revisions	sys=Revisions
diff --git a/noao/imred/dtoi/dtoi.men b/noao/imred/dtoi/dtoi.men
new file mode 100644
index 00000000..f22d92eb
--- /dev/null
+++ b/noao/imred/dtoi/dtoi.men
@@ -0,0 +1,6 @@
+	dematch - Match a list of density values to exposure values
+	  hdfit - Fit a curve to density, log exposure values
+	hdshift - Align related HD curves
+          hdtoi - Apply DTOI transformation to density image
+       selftest - Self test program to check DTOI transformation
+       spotlist - Generate a list of calibration spot values
diff --git a/noao/imred/dtoi/dtoi.par b/noao/imred/dtoi/dtoi.par
new file mode 100644
index 00000000..494aa73c
--- /dev/null
+++ b/noao/imred/dtoi/dtoi.par
@@ -0,0 +1,2 @@
+version,s,h,"February 13, 1987"
+mode,s,h,ql
diff --git a/noao/imred/dtoi/hd_aravr.x b/noao/imred/dtoi/hd_aravr.x
new file mode 100644
index 00000000..3376264b
--- /dev/null
+++ b/noao/imred/dtoi/hd_aravr.x
@@ -0,0 +1,50 @@
+define	MAX_ITERATIONS	10
+include	<mach.h>
+
+# HD_ARAV -- Compute the mean and standard deviation of a sample array by
+# iteratively rejecting points further than KSIG from the mean.  If the
+# value of KSIG is given as 0.0, a cutoff value will be automatically
+# calculated from the standard deviation and number of points in the sample.
+# The number of pixels remaining in the sample upon termination is returned
+# as the function value.
+#
+# A max_iterations parameter was added to prevent the rejection scheme
+# from oscillating endlessly for nearly saturated pixels.  This is the
+# only difference between the vops procedure and hd_aravr.  (ShJ 5/88)
+
+int procedure hd_aravr (a, npix, mean, sigma, ksig)
+
+real	a[ARB]			# input data array
+real	mean, sigma, ksig, deviation, lcut, hcut, lgpx
+int	npix, niter, ngpix, old_ngpix, awvgr()
+
+begin
+	lcut = -MAX_REAL				# no rejection to start
+	hcut =  MAX_REAL
+	ngpix = 0
+	niter = 0
+
+	# Iteratively compute mean, sigma and reject outliers until no
+	# more pixels are rejected, or until there are no more pixels,
+	# or until the maximum iterations limit is exceeded.
+
+	repeat {
+	    niter = niter + 1
+	    old_ngpix = ngpix
+	    ngpix = awvgr (a, npix, mean, sigma, lcut, hcut)
+	    if (ngpix <= 1)
+		break
+
+	    if (ksig == 0.0) {				# Chauvenet's relation
+		lgpx = log10 (real(ngpix))
+		deviation = (lgpx * (-0.1042 * lgpx + 1.1695) + .8895) * sigma
+	    } else
+		deviation = sigma * abs(ksig)
+
+	    lcut = mean - deviation			# compute window
+	    hcut = mean + deviation
+
+	} until ((old_ngpix == ngpix) || (niter > MAX_ITERATIONS))
+
+	return (ngpix)
+end
diff --git a/noao/imred/dtoi/hdfit.par b/noao/imred/dtoi/hdfit.par
new file mode 100644
index 00000000..7f42aa2a
--- /dev/null
+++ b/noao/imred/dtoi/hdfit.par
@@ -0,0 +1,9 @@
+# Cl parameters for task hdfit are:
+database,f,a,,,,List of database names
+function,s,h,"power",,,Fitting function
+transform,s,h,"logopacitance",,,Independent variable transformation
+order,i,h,4,,,Initial order (ncoeff) of fit
+interactive,b,h,y,,,Interactive fitting flag
+device,s,h,"stdgraph",,,Name of interactive graphics device
+weighting,s,h,"none",,,Type of weighting
+cursor,*gcur,h,"",,,Source of cursor input
diff --git a/noao/imred/dtoi/hdfit.x b/noao/imred/dtoi/hdfit.x
new file mode 100644
index 00000000..04a82f6e
--- /dev/null
+++ b/noao/imred/dtoi/hdfit.x
@@ -0,0 +1,364 @@
+include	<math/curfit.h>
+include	<imhdr.h>
+include	<fset.h>
+include	<mach.h>
+include	<ctype.h>
+include	<error.h>
+include	<pkg/gtools.h>
+include	<pkg/xtanswer.h>
+include	"hdicfit/hdicfit.h"
+
+# T_HDFIT -- Fit a curve.  This task fits a characteristic
+# curve to density and log exposure data read from an input
+# database.  The interactive curve fitting package is used.
+# The database is updated to contain the values of the fit 
+# necessary to reinitialize the curfit package for performing 
+# the transformation in hdtoi. 
+
+procedure t_hdfit ()
+
+pointer	sp, fcn, device, db, gt, exp, wts, save, trans, weight
+pointer	dbfile, ic, den, errs
+int	db_list, order, interactive, nsave, nvals, wt_type, update
+real	ref_fog, real_fog
+double	fog, maxden
+
+pointer	ddb_map(), gt_init()
+bool	clgetb(), fp_equalr(), fp_equald()
+int	clpopni(), clgeti(), strncmp(), clgfil(), hd_fit()
+real	ic_getr()
+
+begin
+	call smark  (sp)
+	call salloc (fcn, SZ_FNAME, TY_CHAR)
+	call salloc (device, SZ_FNAME, TY_CHAR)
+	call salloc (trans, SZ_FNAME, TY_CHAR)
+	call salloc (weight,  SZ_FNAME, TY_CHAR)
+	call salloc (dbfile, SZ_FNAME, TY_CHAR)
+
+	# Get cl parameters
+	db_list = clpopni ("database")
+	call clgstr ("function", Memc[fcn], SZ_FNAME)
+	call clgstr ("transform", Memc[trans], SZ_FNAME)
+	order = clgeti ("order")
+
+	# Decide which type of weighting the user wants
+	call clgstr ("weighting", Memc[weight], SZ_FNAME)
+	if (strncmp (Memc[weight], "none", 1) == 0)
+	    wt_type = WT_NONE
+	else if (strncmp (Memc[weight], "user", 1) == 0)
+	    wt_type = WT_USER
+	else if (strncmp (Memc[weight], "calc", 1) == 0)
+	    wt_type = WT_CALC
+	else
+	    call error (0, "Unrecognized weighting type")
+
+	# Initialize interactive curve fitting package.
+	gt = gt_init ()
+	call ic_open (ic)
+	call ic_pstr (ic, "function", Memc[fcn])
+	call ic_pstr (ic, "transform", Memc[trans])
+	call ic_puti (ic, "order", order)
+	call ic_pstr (ic, "ylabel", "Log Exposure")
+	call ic_pkey (ic, 5, 'y', 'u')
+
+	if (clgetb ("interactive")) {
+	    interactive = YES
+	    call clgstr ("device", Memc[device], SZ_FNAME)
+	} else {
+	    interactive = NO
+	    call strcpy ("", Memc[device], SZ_FNAME)
+	}
+
+	# Read information from each dlog file; accumulate number of values.
+	# The density (not fog subtracted) is returned.  The density values
+	# are also sorted in increasing order.
+
+	call hd_rdloge (db_list, exp, den, wts, errs, nvals, fog, maxden,
+	    wt_type)
+	if (nvals == 0)
+	    call error (1, "T_HDFIT: No data values in sample")
+
+	call hd_sdloge (Memd[den], Memd[exp], Memd[wts], Memd[errs], nvals)
+	call ic_putr (ic, "fog", real(fog))
+	ref_fog = real (fog)
+	call ic_putr (ic, "rfog", ref_fog)
+
+	# Initialize the dtoi/icgfit interface.
+	if (fp_equald (maxden, 0.0D0))
+	    call error (1, "Saturated pixel density not initialized")
+	call hdic_init (Memd[den], nvals, maxden)
+
+	update = hd_fit (ic, gt, Memd[den], Memd[exp], Memd[wts], Memd[errs],
+	    nvals, save, nsave, Memc[device], interactive)
+	     
+	if (update == YES) {
+	    # Record fit information in (each) database
+	    call ic_gstr  (ic, "function", Memc[fcn], SZ_FNAME)
+	    call ic_gstr  (ic, "transform", Memc[trans], SZ_FNAME)
+	    real_fog = ic_getr (ic, "fog")
+
+	    while (clgfil (db_list, Memc[dbfile], SZ_FNAME) != EOF) {
+	        db = ddb_map (Memc[dbfile], APPEND)
+	        call ddb_ptime (db)
+	        # Add new fog record if it was changed interactively.
+	        if (!fp_equalr (real_fog, ref_fog)) {
+		    call ddb_prec (db, "fog")
+		    call ddb_putr (db, "density", real_fog)
+	        }
+
+	        call ddb_prec (db, "cv")
+	        call ddb_pad  (db, "save", Memd[save], nsave)
+	        call ddb_pstr (db, "function", Memc[fcn])
+	        call ddb_pstr (db, "transformation", Memc[trans])
+
+	        call ddb_unmap (db)
+	    }
+	}
+
+	call ic_closed (ic)
+	call mfree (save, TY_DOUBLE)
+	call mfree (den,  TY_DOUBLE)
+	call mfree (exp,  TY_DOUBLE)
+	call mfree (wts , TY_DOUBLE)
+	call mfree (errs, TY_DOUBLE)
+
+	call gt_free (gt)
+	call clpcls (db_list)
+	call sfree (sp)
+end
+
+
+# HD_RLOGE -- Read log exposure, density and weights from a single dloge
+# database file.  Pointers to the three arrays are returned as arguments.
+# The number of values accumulated is returned also; note that the value
+# of nvals is changed upon return; it should not be given as a constant.
+# If more than one database is being read (as in HDSHIFT applications),
+# the density ABOVE fog is returned, and the reference fog values set = 0.0
+# The maximum density, the density of a saturated pixel, is read from the
+# first databas and returned.
+
+procedure hd_rdloge (db_list, exp, den, wts, errs, nvals, fog, maxden, wt_type)
+
+int	db_list			# File descriptor for data base file
+pointer	exp			# Pointer to exposure array - returned
+pointer	den			# Pointer to density array - returned
+pointer	wts			# Pointer to weights array - returned
+pointer	errs			# Pointer to std deviation array - returned
+int	nvals			# Number of data pairs read - returned
+double	fog			# Value of fog read from database - returned
+double  maxden			# Maximum density, read from db - returned
+int	wt_type			# Type of weighting
+
+pointer	db
+bool	sdevrec
+int	buflen, off, rec
+int	nden, nexp, nwts, nspots, nerrs, nfiles
+char	dloge[SZ_FNAME]
+
+pointer	ddb_map()
+bool	fp_equald()
+int	ddb_locate(), ddb_geti(), clgfil(), imtlen()
+real	ddb_getr()
+errchk	ddb_locate, ddb_gad, malloc, ddb_map, ddb_unmap
+
+begin
+	nvals = 0
+	off = 0
+	buflen = NSPOTS
+	nfiles = imtlen (db_list)
+	maxden = 0.0D0
+
+	# Dynamically allocate memory for arrays; it can be increased later.
+	call malloc (exp, buflen, TY_DOUBLE)
+	call malloc (den, buflen, TY_DOUBLE)
+	call malloc (wts, buflen, TY_DOUBLE)
+	call malloc (errs, buflen, TY_DOUBLE)
+
+	while (clgfil (db_list, dloge, SZ_FNAME) != EOF) {
+	    iferr (db = ddb_map (dloge, READ_ONLY)) {
+		call erract (EA_WARN)
+		next
+	    }
+
+	    # Get fog value to be subtracted from density
+	    rec = ddb_locate (db, "fog")
+	    fog = double (ddb_getr (db, rec, "density"))
+
+	    # Get density array
+	    rec = ddb_locate (db, "density")
+	    nden = ddb_geti (db, rec, "den_val")
+
+	    call ddb_gad (db, rec, "den_val", Memd[den+off], nden, nden)
+	    if (nfiles > 1)
+		call asubkd (Memd[den+off], fog, Memd[den+off], nden)
+
+	    # Get log exposure array
+	    rec = ddb_locate (db, "exposure")
+	    nexp = ddb_geti (db, rec, "log_exp")
+	    call ddb_gad (db, rec, "log_exp", Memd[exp+off], nexp, nexp)
+
+	    # Get saturated pixel density if not already set
+	    if (fp_equald (maxden, 0.0D0)) {
+	        iferr (rec = ddb_locate (db, "common")){
+		    ;
+		} else
+	            maxden = double (ddb_getr (db, rec, "maxden"))
+	    }
+
+	    # Get std deviation array
+	    sdevrec = true
+	    iferr {
+	        rec = ddb_locate (db, "standard deviation")
+	        nerrs = ddb_geti (db, rec, "sdev_val")
+	        call ddb_gad (db, rec, "sdev_val", Memd[errs+off], nerrs, nerrs)
+	    } then {
+		call erract (EA_WARN)
+		call eprintf ("Marker type '[ve]bar' can only show weights\n")
+		call amovkd (0.0D0, Memd[errs+off], nden)
+		sdevrec = FALSE
+	    }
+
+	    if (wt_type == WT_CALC) {
+	        if (sdevrec) {
+		    iferr {
+                        nspots = min (nden, nexp, nerrs)
+                        call adivd (Memd[den+off], Memd[errs+off], 
+			    Memd[wts+off], nspots)
+	            } then {
+		        call erract (EA_WARN)
+		        call eprintf ("All weights set to 1.0\n")
+	                call amovkd (double (1.0), Memd[wts+off], nspots)
+	            }
+	        } else {
+		    nspots = min (nden, nexp)	
+		    call eprintf ("No sdev record; All weights set to 1.0\n")
+	            call amovkd (double (1.0), Memd[wts+off], nspots)
+	        }
+	    }
+
+	    if (wt_type == WT_USER) {
+	        # WT_USER: fill "user" weights array
+	        iferr {
+	            rec = ddb_locate (db, "weight")
+	            nwts = ddb_geti (db, rec, "wts_val")
+		    nspots = min (nden, nexp, nwts)
+	            call ddb_gad (db, rec, "wts_val", Memd[wts+off], nwts, nwts)
+	        } then {
+	            # Users weights can't be found. Set weights array to 1.0's.
+		    call erract (EA_WARN)
+		    call eprintf ("All weights set to 1.0\n")
+	            nspots = min (nden, nexp)
+	            call amovkd (double (1.0), Memd[wts+off], nspots)
+		}
+	    }
+
+	    if (wt_type == WT_NONE) {
+	        # WT_NONE: fill "none" weights array
+	        nspots = min (nden, nexp)
+		call amovkd (double (1.0), Memd[wts+off], nspots)
+	    }
+    
+	    # Increment number of counts; reallocate memory if necessary.
+	    nvals = nvals + nspots
+	    off = off + nspots
+
+	    if (nvals > buflen) {
+		buflen = buflen + NSPOTS
+		call realloc (exp, buflen, TY_DOUBLE)
+		call realloc (den, buflen, TY_DOUBLE)
+		call realloc (wts, buflen, TY_DOUBLE)
+		call realloc (errs, buflen, TY_DOUBLE)
+	    }
+
+	    call ddb_unmap (db)
+	}
+
+	if (nfiles > 1)
+	    fog = 0.0D0
+	call clprew (db_list)
+end
+
+
+# HD_SLOGE -- Sort the log exposure, density and weight information in order
+# of increasing exposure value.  The sorting is done is place.  The three
+# data values are assummed matched on input, that is, exposure[i] matches
+# density[i] with weight[i] for all array entries.
+
+procedure hd_sdloge (density, exposure, weights, errors,  nvals)
+
+double	density[nvals]		# Density array
+double	exposure[nvals]		# Exposure array
+double	weights[nvals]		# Weights array
+double	errors[nvals]		# Standard deviation array
+int	nvals			# Number of values in data arrays
+
+int	i, j
+double	temp
+define	swap	{temp=$1;$1=$2;$2=temp}
+
+begin
+	# Bubble sort - inefficient, but sorting is done only once on
+	# an expected small sample size (16 pts typically). 
+
+	for (i = nvals; i > 1; i = i - 1)
+	    for (j = 1; j < i; j = j + 1) 
+		if (density [j] > density [j+1]) {
+
+		    # Out of order; exchange values
+		    swap (exposure[j], exposure[j+1])
+		    swap ( density[j],  density[j+1])
+		    swap ( weights[j],  weights[j+1])
+		    swap (  errors[j],   errors[j+1])
+		}
+end
+
+
+# HD_FIT -- Fit the curve to input density, exposure and weight values.
+# The fit can be performed interactively or not. 
+
+int procedure hd_fit (ic,
+	gt, den, exp, wts, errs, nvals, save, nsave, dev, interact)
+
+pointer	ic
+pointer	gt			# Graphics tools pointer
+double	den[ARB]		# Density values
+double	exp[ARB]		# Exposure values
+double	wts[ARB]		# Weight array
+double	errs[ARB]		# Standard deviation array
+int	nvals			# Number of data pairs to fit
+pointer	save			# ??
+int	nsave			# ??
+char	dev[SZ_FNAME]		# Interactive graphics device
+int	interact		# Flag for interactive graphics
+
+pointer	gp, cv, sp, x, dum
+pointer	gopen()
+int	update, dcvstati()
+errchk	malloc, gopen
+
+begin
+	if (interact == YES) {
+	    gp = gopen (dev, NEW_FILE, STDGRAPH)
+	    call icg_fitd (ic, gp, "cursor", gt, cv, den, exp, wts, errs, nvals)
+	    call gclose (gp)
+	    update = IC_UPDATE(ic)
+
+	} else {
+	    # Do fit non-interactively
+	    call smark (sp)
+	    call salloc (x, nvals, TY_DOUBLE)
+	    call salloc (dum, nvals, TY_INT)
+	    call hdic_transform (ic, den, wts, Memd[x], wts, Memi[dum], nvals)
+	    call ic_fitd (ic, cv, Memd[x], exp, wts, nvals, YES, YES, YES, YES)
+	    call sfree (sp)
+	    update = YES
+	}
+
+	nsave = (dcvstati (cv, CVORDER)) + 7
+	call malloc (save, nsave, TY_DOUBLE)
+	call dcvsave (cv, Memd[save])
+	call dcvfree (cv)
+
+	return (update)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdic.com b/noao/imred/dtoi/hdicfit/hdic.com
new file mode 100644
index 00000000..959df10e
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdic.com
@@ -0,0 +1,6 @@
+# Common block for hdtoi package/ icgfit package interface.
+
+int	nraw
+double	maxden
+pointer	den, big_den
+common	/raw/maxden, den, big_den, nraw
diff --git a/noao/imred/dtoi/hdicfit/hdicadd.x b/noao/imred/dtoi/hdicfit/hdicadd.x
new file mode 100644
index 00000000..1fae152d
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicadd.x
@@ -0,0 +1,47 @@
+include	"hdicfit.h"
+
+# HDIC_ADDPOINT -- Add a density, exposure, weights point into the sample.
+
+procedure hdic_addpoint (ic,
+	nden, nexp, nwts, den, y, wts, userwts, x, wd, sdev, npts)
+
+pointer	ic		# Pointer to ic data structure
+real	nden		# New density value to be added
+real	nexp		# New exposure value to be added
+double	nwts		# New weight value to be added
+pointer	den		# Pointer to existing density array
+pointer	y		# Pointer to existing exposure array
+pointer	wts		# Pointer to existing wts array
+pointer	userwts		# Pointer to existing userwts array
+pointer	x		# Pointer to existing array of ind variables
+pointer	wd		# Pointer to flag array for deletion reasons
+pointer	sdev		# Pointer to standard deviation array
+int	npts		# Number of points, incremented on output
+
+begin
+	npts = npts + 1
+
+	call realloc (den,     npts, TY_DOUBLE)
+	call realloc (y,       npts, TY_DOUBLE)
+	call realloc (wts,     npts, TY_DOUBLE)
+	call realloc (userwts, npts, TY_DOUBLE)
+	call realloc (x,       npts, TY_DOUBLE)
+	call realloc (wd,      npts, TY_INT)
+	call realloc (sdev,    npts, TY_DOUBLE)
+
+	Memd[den+npts-1] = double (nden)
+	Memd[y  +npts-1] = double (nexp)
+	Memd[wts+npts-1] = double (nwts)
+	Memd[userwts+npts-1] = double (nwts)
+	Memi[wd +npts-1] = NDELETE
+	Memd[sdev+npts-1] = ADDED_PT
+
+	# Sort the data and then update the reference vector.
+	call hdic_sort (Memd[den], Memd[y], Memd[wts], Memd[userwts], 
+	    Memi[wd], Memd[sdev],  npts)
+	call hdic_init (Memd[den], npts, Memd[den+npts-1])
+
+	IC_NEWX(ic) = YES
+	IC_NEWY(ic) = YES
+	IC_NEWWTS(ic) = YES
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicclean.x b/noao/imred/dtoi/hdicfit/hdicclean.x
new file mode 100644
index 00000000..6c838123
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicclean.x
@@ -0,0 +1,94 @@
+include <pkg/rg.h>
+include	"hdicfit.h"
+
+# IC_CLEAN -- Replace rejected points by the fitted values.
+
+procedure ic_cleand (ic, cv, x, y, w, npts)
+
+pointer	ic				# ICFIT pointer
+pointer	cv				# Curfit pointer
+double	x[ARB]				# Ordinates
+double	y[ARB]				# Abscissas
+double	w[ARB]				# Weights
+int	npts				# Number of points
+
+int	i, nclean, newreject
+pointer	sp, xclean, yclean, wclean
+double	dcveval()
+
+begin
+	if ((IC_LOW(ic) == 0.) && (IC_HIGH(ic) == 0.))
+	    return
+
+	# If there has been no subsampling and no sample averaging then the
+	# IC_REJPTS(ic) array already contains the rejected points.
+
+	if (npts == IC_NFIT(ic)) {
+	    if (IC_NREJECT(ic) > 0) {
+	        do i = 1, npts {
+		    if (Memi[IC_REJPTS(ic)+i-1] == YES)
+		        y[i] = dcveval (cv, x[i])
+	        }
+	    }
+
+	# If there has been no sample averaging then the rejpts array already
+	# contains indices into the subsampled array.
+
+	} else if (abs(IC_NAVERAGE(ic)) == 1) {
+	    if (IC_NREJECT(ic) > 0) {
+	        do i = 1, npts {
+		    if (Memi[IC_REJPTS(ic)+i-1] == YES)
+			Memd[IC_YFIT(ic)+i-1] =
+			    dcveval (cv, Memd[IC_XFIT(ic)+i-1])
+		}
+	    }
+	    call rg_unpackd (IC_RG(ic), Memd[IC_YFIT(ic)], y)
+
+	# Because ic_fit rejects points from the fitting data which
+	# has been sample averaged the rejpts array refers to the wrong data.
+	# Do the cleaning using ic_deviant to find the points to reject.
+
+	} else if (RG_NPTS(IC_RG(ic)) == npts) {
+	    call amovki (NO, Memi[IC_REJPTS(ic)], npts)
+	    call ic_deviantd (cv, x, y, w, Memi[IC_REJPTS(ic)], npts,
+		IC_LOW(ic), IC_HIGH(ic), IC_GROW(ic), NO, IC_NREJECT(ic),
+		newreject)
+	    if (IC_NREJECT(ic) > 0) {
+	        do i = 1, npts {
+		    if (Memi[IC_REJPTS(ic)+i-1] == YES)
+			y[i] = dcveval (cv, x[i])
+		}
+	    }
+
+	# If there is subsampling then allocate temporary arrays for the
+	# subsample points.
+
+	} else {
+	    call smark (sp)
+
+	    nclean = RG_NPTS(IC_RG(ic))
+	    call salloc (xclean, nclean, TY_DOUBLE)
+	    call salloc (yclean, nclean, TY_DOUBLE)
+	    call salloc (wclean, nclean, TY_DOUBLE)
+
+	    call rg_packd (IC_RG(ic), x, Memd[xclean])
+	    call rg_packd (IC_RG(ic), y, Memd[yclean])
+	    call rg_packd (IC_RG(ic), w, Memd[wclean])
+	    call amovki (NO, Memi[IC_REJPTS(ic)], npts)
+
+	    call ic_deviantd (cv, Memd[xclean], Memd[yclean],
+		Memd[wclean], Memi[IC_REJPTS(ic)], nclean, IC_LOW(ic),
+		IC_HIGH(ic), IC_GROW(ic), NO, IC_NREJECT(ic), newreject)
+
+	    if (IC_NREJECT(ic) > 0) {
+	        do i = 1, npts {
+		    if (Memi[IC_REJPTS(ic)+i-1] == YES)
+			Memd[yclean+i-1] = dcveval (cv, Memd[xclean+i-1])
+		}
+	    }
+	    call rg_unpackd (IC_RG(ic), Memd[yclean], y)
+
+	    call sfree (sp)
+	}
+end
+
diff --git a/noao/imred/dtoi/hdicfit/hdicdeviant.x b/noao/imred/dtoi/hdicfit/hdicdeviant.x
new file mode 100644
index 00000000..0c6f8f75
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicdeviant.x
@@ -0,0 +1,116 @@
+include	<mach.h>
+include	<math/curfit.h>
+
+# IC_DEVIANT -- Find deviant points with large residuals from the fit
+# and reject from the fit.
+#
+# The sigma of the fit residuals is calculated.  The rejection thresholds
+# are set at +-reject*sigma.  Points outside the rejection threshold are
+# recorded in the reject array.
+
+procedure ic_deviantd (cv, x, y, w, rejpts, npts, low_reject, high_reject,
+	grow, refit, nreject, newreject)
+
+pointer	cv				# Curve descriptor
+double	x[ARB]				# Input ordinates
+double	y[ARB]				# Input data values
+double	w[ARB]				# Weights
+int	rejpts[ARB]			# Points rejected
+int	npts				# Number of input points
+real	low_reject, high_reject		# Rejection thresholds
+real	grow				# Rejection radius
+int	refit				# Refit the curve?
+int	nreject				# Number of points rejected
+int	newreject			# Number of new points rejected
+
+int	i, j, i_min, i_max, ilast
+double	sigma, low_cut, high_cut, residual
+pointer	sp, residuals
+
+begin
+	# If low_reject and high_reject are zero then simply return.
+	if ((low_reject == 0.) && (high_reject == 0.))
+	    return
+
+	# Allocate memory for the residuals.
+	call smark (sp)
+	call salloc (residuals, npts, TY_DOUBLE)
+
+	# Compute the residuals.
+	call dcvvector (cv, x, Memd[residuals], npts)
+	call asubd (y, Memd[residuals], Memd[residuals], npts)
+
+	# Compute the sigma of the residuals.  If there are less than
+	# 5 points return.
+
+	j = 0
+	nreject = 0
+	sigma = 0.
+
+	do i = 1, npts {
+	    if ((w[i] != 0.) && (rejpts[i] == NO)) {
+		sigma = sigma + Memd[residuals+i-1] ** 2
+		j = j + 1
+	    } else if (rejpts[i] == YES)
+		nreject = nreject + 1
+	}
+
+	if (j < 5) {
+	    call sfree (sp)
+	    return
+	} else
+	    sigma = sqrt (sigma / j)
+
+	if (low_reject > 0.)
+	    low_cut = -low_reject * sigma
+	else
+	    low_cut = -MAX_REAL
+	if (high_reject > 0.)
+	    high_cut = high_reject * sigma
+	else
+	    high_cut = MAX_REAL
+
+	# Reject the residuals exceeding the rejection limits.
+	# A for loop is used instead of do because with region growing we
+	# want to modify the loop index.
+
+	newreject = 0
+	for (i = 1; i <= npts; i = i + 1) {
+	    if ((w[i] == 0.) || (rejpts[i] == YES))
+		next
+
+	    residual = Memd[residuals + i - 1]
+	    if ((residual > high_cut) || (residual < low_cut)) {
+		i_min = max (1, int (i - grow))
+		i_max = min (npts, int (i + grow))
+
+		# Reject points from the fit and flag them.
+		do j = i_min, i_max {
+		    if ((abs (x[i] - x[j]) <= grow) && (w[j] != 0.) &&
+		        (rejpts[j] == NO)) {
+			if (refit == YES)
+	        	    call dcvrject (cv, x[j], y[j], w[j])
+			rejpts[j] = YES
+		        newreject = newreject + 1
+			ilast = j
+		    }
+		}
+		i = ilast
+	    }
+	}
+
+	if ((refit == YES) && (newreject > 0)) {
+	    call dcvsolve (cv, i)
+
+	    switch (i) {
+	    case SINGULAR:
+		call eprintf ("ic_reject: Singular solution\n")
+	    case NO_DEG_FREEDOM:
+		call eprintf ("ic_reject: No degrees of freedom\n")
+	    }
+	}
+
+	nreject = nreject + newreject
+
+	call sfree (sp)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicdosetup.x b/noao/imred/dtoi/hdicfit/hdicdosetup.x
new file mode 100644
index 00000000..c9e117ec
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicdosetup.x
@@ -0,0 +1,104 @@
+include	<math/curfit.h>
+include	"hdicfit.h"
+
+# IC_DOSETUP -- Setup the fit.  This is called at the start of each call
+# to ic_fit to update the fitting parameters if necessary.
+
+procedure ic_dosetupd (ic, cv, x, wts, npts, newx, newwts, newfunction, refit)
+
+pointer	ic				# ICFIT pointer
+pointer	cv				# Curfit pointer
+double	x[ARB]				# Ordinates of data
+double	wts[ARB]			# Weights
+int	npts				# Number of points in data
+int	newx				# New x points?
+int	newwts				# New weights?
+int	newfunction			# New function?
+int	refit				# Use cvrefit?
+
+int	ord
+pointer	rg_xrangesd()
+extern	hd_powerd()
+errchk	rg_xrangesd, malloc
+
+begin
+	# Set sample points.
+	if ((newx == YES) || (newwts == YES)) {
+	    if (npts == 0)
+		call error (0, "No data points for fit")
+
+	    call mfree (IC_XFIT(ic), TY_DOUBLE)
+	    call mfree (IC_YFIT(ic), TY_DOUBLE)
+	    call malloc (IC_XFIT(ic), npts, TY_DOUBLE)
+
+	    call mfree (IC_WTSFIT(ic), TY_DOUBLE)
+	    call malloc (IC_WTSFIT(ic), npts, TY_DOUBLE)
+
+	    call mfree (IC_REJPTS(ic), TY_INT)
+	    call malloc (IC_REJPTS(ic), npts, TY_INT)
+	    call amovki (NO, Memi[IC_REJPTS(ic)], npts)
+	    IC_NREJECT(ic) = 0
+
+	    # Set sample points.
+
+	    call rg_free (IC_RG(ic))
+	    IC_RG(ic) = rg_xrangesd (Memc[IC_SAMPLE(ic)], x, npts)
+	    call rg_order (IC_RG(ic))
+	    call rg_merge (IC_RG(ic))
+	    call rg_wtbind (IC_RG(ic), abs (IC_NAVERAGE(ic)), x, wts, npts,
+		Memd[IC_XFIT(ic)], Memd[IC_WTSFIT(ic)], IC_NFIT(ic))
+
+	    if (IC_NFIT(ic) == 0)
+		call error (0, "No sample points for fit")
+
+	    if (IC_NFIT(ic) == npts) {
+	        call rg_free (IC_RG(ic))
+	        call mfree (IC_XFIT(ic), TY_DOUBLE)
+	        call mfree (IC_WTSFIT(ic), TY_DOUBLE)
+	        IC_YFIT(ic) = NULL
+		IC_WTSFIT(ic) = NULL
+	    } else
+	        call malloc (IC_YFIT(ic), IC_NFIT(ic), TY_DOUBLE)
+
+	    refit = NO
+	}
+
+	# Set curve fitting parameters.
+
+	if ((newx == YES) || (newfunction == YES)) {
+	    if (cv != NULL)
+	        call dcvfree (cv)
+
+	    switch (IC_FUNCTION(ic)) {
+	    case LEGENDRE, CHEBYSHEV:
+		ord = min (IC_ORDER(ic), IC_NFIT(ic))
+	        call dcvinit (cv, IC_FUNCTION(ic), ord, double (IC_XMIN(ic)),
+		    double (IC_XMAX(ic)))
+	    case SPLINE1:
+		ord = min (IC_ORDER(ic), IC_NFIT(ic) - 1)
+		if (ord > 0)
+	            call dcvinit (cv, SPLINE1, ord, double (IC_XMIN(ic)),
+			double (IC_XMAX(ic)))
+		else
+	            call dcvinit (cv, LEGENDRE, IC_NFIT(ic),
+			double (IC_XMIN(ic)), double (IC_XMAX(ic)))
+	    case SPLINE3:
+		ord = min (IC_ORDER(ic), IC_NFIT(ic) - 3)
+		if (ord > 0)
+	            call dcvinit (cv, SPLINE3, ord, double (IC_XMIN(ic)),
+			double (IC_XMAX(ic)))
+		else
+	            call dcvinit (cv, LEGENDRE, IC_NFIT(ic),
+			double (IC_XMIN(ic)), double (IC_XMAX(ic)))
+ 	    case USERFNC:
+ 		ord = min (IC_ORDER(ic), IC_NFIT(ic))
+ 		call dcvinit (cv, USERFNC, ord, double (IC_XMIN(ic)),
+ 		    double (IC_XMAX(ic)))
+ 		call dcvuserfnc (cv, hd_powerd)
+	    default:
+		call error (0, "Unknown fitting function")
+	    }
+
+	    refit = NO
+	}
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicebars.x b/noao/imred/dtoi/hdicfit/hdicebars.x
new file mode 100644
index 00000000..335c161d
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicebars.x
@@ -0,0 +1,217 @@
+include	<gset.h>
+include	<mach.h>
+include	<pkg/gtools.h>
+include	"hdicfit.h"
+
+define	MSIZE	2.0
+
+# HDIC_EBARS -- Plot data points with their error bars as markers.  The
+# independent variable is fog subtracted transformed density.
+
+procedure hdic_ebars (ic, gp, gt, x, y, wts, ebw, npts)
+
+pointer	ic		# Pointer to ic structure
+pointer	gp		# Pointer to graphics stream
+pointer	gt		# Pointer to gtools structure
+double	x[ARB]		# Array of independent variables
+double	y[ARB]		# Array of dependent variables
+double	wts[ARB]	# Array of weights
+double	ebw[ARB]	# Error bar half width (positive number)
+int	npts		# Number of points
+
+pointer	sp, xr, yr, sz
+int	orig_mark, i, xaxis, yaxis, mark, added_mark
+real	size, dx, dy, szmk
+int	gt_geti()
+bool	fp_equald()
+include	"hdic.com"
+
+begin
+	call smark (sp)
+
+	xaxis = (IC_AXES (ic, IC_GKEY(ic), 1))
+	yaxis = (IC_AXES (ic, IC_GKEY(ic), 2))
+
+	if (xaxis == 'x' || xaxis == 'u')
+	    orig_mark = GM_HEBAR
+	else if (yaxis == 'x' || yaxis == 'u')
+	    orig_mark = GM_VEBAR
+	else {
+	    call eprintf ("Choose graph type with axes 'u' or 'x'\n")
+	    call sfree (sp)
+	    return
+	}
+
+	added_mark = GM_CIRCLE
+
+	call salloc (xr, npts, TY_REAL)
+	call salloc (yr, npts, TY_REAL)
+	call salloc (sz, npts, TY_REAL)
+
+	call achtdr (x, Memr[xr], npts)
+	call achtdr (y, Memr[yr], npts)
+	call achtdr (ebw, Memr[sz], npts)
+
+	if (IC_OVERPLOT(ic) == NO) {
+	    # Start a new plot
+	    call gclear (gp)
+
+	    # Set the graph scale and axes
+	    call gascale (gp, Memr[xr], npts, 1)
+	    call gascale (gp, Memr[yr], npts, 2)
+
+	    # If plotting HD curve, set wy2 to maxden, which may have
+	    # been updated if a new endpoint was added.
+
+	    if ((IC_AXES (ic, IC_GKEY(ic), 1) == 'y') &&
+		(IC_AXES (ic, IC_GKEY(ic), 2) == 'u')) 
+		call gswind (gp, INDEF, INDEF, INDEF, real (maxden))
+
+	    call gt_swind (gp, gt)
+	    call gt_labax (gp, gt)
+	}
+
+	call ggscale (gp, 0.0, 0.0, dx, dy)
+
+	do i = 1, npts {
+	    size = Memr[sz+i-1]		# Sizes are WCS units; transform them
+	    if (gt_geti (gt, GTTRANSPOSE) == NO) {
+	        size = size / dx
+		mark = orig_mark
+		szmk = size
+		# Check for added point
+		if (fp_equald (ebw[i], ADDED_PT)) {
+		    szmk = MSIZE
+		    mark = added_mark
+		}
+
+		# Check for deleted point
+		if (fp_equald (wts[i], 0.0D0)) {
+		    szmk = MSIZE
+		    mark = mark + GM_CROSS
+		}
+
+	        call gmark (gp, Memr[xr+i-1], Memr[yr+i-1], mark, szmk, szmk)
+
+	    } else {
+		size = size / dy
+		szmk = size
+		mark = orig_mark
+
+		# Check for added point
+		if (fp_equald (ebw[i], ADDED_PT)) {
+		    szmk = MSIZE
+		    mark = added_mark
+		}
+
+		# Check for deleted point
+		if (fp_equald (wts[i], 0.0D0)) {
+		    szmk = MSIZE
+		    mark = mark + GM_CROSS
+		}
+
+		call gmark (gp, Memr[yr+i-1], Memr[xr+i-1], mark, szmk, szmk)
+	    }
+	}
+	
+	IC_OVERPLOT(ic) = NO
+	call sfree (sp)
+end
+
+
+# HDIC_EBW -- Calculate error bar width for plotting points.  Width is
+# returned in NDC units.
+
+procedure hdic_ebw (ic, density, indv, sdev, ebw, npts)
+
+pointer	ic		# Pointer to ic structure
+double	density[ARB]	# Untransformed density NOT fog subtracted
+double	indv[ARB]	# Transformed density above fog
+double	sdev[ARB]	# Array of standard deviation values, density units
+double	ebw[ARB]	# Error bar half width (positive numbers)
+int	npts		# Number of data points
+
+double	fog
+pointer	sp, denaf, outwe
+int	xaxis, yaxis, i
+bool	fp_equald()
+real	ic_getr()
+
+begin
+	xaxis = (IC_AXES (ic, IC_GKEY(ic), 1))
+	yaxis = (IC_AXES (ic, IC_GKEY(ic), 2))
+
+	if (xaxis == 'u' || yaxis == 'u') {
+	    call amovd (sdev, ebw, npts) 
+	    return
+	}
+
+	call smark (sp)
+	call salloc (denaf, npts, TY_DOUBLE)
+	call salloc (outwe, npts, TY_DOUBLE)
+
+	fog = double (ic_getr (ic, "fog"))
+
+	call asubkd (density, fog, Memd[denaf], npts)
+	call aaddd  (Memd[denaf], sdev, Memd[denaf], npts)
+
+	call hdic_ebtran (Memd[denaf], Memd[outwe], npts, IC_TRANSFORM(ic))
+
+	# Subtract transformed values to get errors.  Then check for
+	# added points, which are flagged with ebw=ADDED_PT.
+
+	call asubd (Memd[outwe], indv, ebw, npts)
+	do i = 1, npts {
+	    if (fp_equald (sdev[i], ADDED_PT))
+		ebw[i] = ADDED_PT
+	}
+
+	call sfree (sp)
+end
+
+
+# HDIC_EBTRAN -- Apply transformation, generating a vector of independent
+# variables from a density vector.  The independent variable vector is the
+# standard deviation values and the output values are the errors.  This
+# routine checks for ADDED_PT valued standard deviation, which indicates an
+# added point.
+
+procedure hdic_ebtran (density, ind_var, npts, transform)
+
+double	density[npts]		# Density vector - input
+double	ind_var[npts]		# Ind variable vector - filled on output
+int	npts			# Length of data vectors
+int	transform		# Integer code for transform type
+
+int	i
+bool	fp_equald()
+
+begin
+	switch (transform) {
+	case HD_LOGO:
+	    do i = 1, npts {
+		if (fp_equald (density[i], 0.0))
+		    ind_var[i] = 0.0
+		else
+		    ind_var[i] = log10 ((10. ** density[i]) - 1.0)
+	    }
+	case HD_K75:
+	    do i = 1, npts {
+		if (fp_equald (density[i], 0.0))
+		    ind_var[i] = 0.0
+		else
+		    ind_var[i] = density[i] + 0.75*log10(1.- 10.**(-density[i]))
+	    }
+	case HD_K50:
+	    do i = 1, npts {
+		if (fp_equald (density[i], 0.0))
+		    ind_var[i] = 0.0
+		else
+		    ind_var[i] = density[i] + 0.50*log10(1.- 10.**(-density[i]))
+	    }
+	case HD_NONE:
+	    call amovd (density, ind_var, npts)
+	default:
+	    call error (0, "Unrecognized transformation in HDIC_EBTRAN")
+	}
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicerrors.x b/noao/imred/dtoi/hdicfit/hdicerrors.x
new file mode 100644
index 00000000..7722e5e2
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicerrors.x
@@ -0,0 +1,143 @@
+include	<math/curfit.h>
+include	"hdicfit.h"
+
+# IC_ERRORS -- Compute and error diagnositic information.
+
+procedure ic_errorsd (ic, file, cv, x, y, wts, npts)
+
+pointer	ic		# ICFIT pointer
+char	file[ARB]	# Output file
+pointer	cv		# Curfit pointer
+double	x[ARB]		# Ordinates
+double	y[ARB]		# Abscissas
+double	wts[ARB]	# Weights
+int	npts		# Number of data points
+
+int	i, n, deleted, ncoeffs, fd
+double	chisqr, rms
+pointer	sp, fit, wts1, coeffs, errors
+
+int	dcvstati(), open()
+double	ic_rmsd()
+errchk	open()
+
+begin
+	# Open the output file.
+	fd = open (file, APPEND, TEXT_FILE)
+
+	# Determine the number of coefficients and allocate memory.
+	ncoeffs = dcvstati (cv, CVNCOEFF)
+	call smark (sp)
+	call salloc (coeffs, ncoeffs, TY_DOUBLE)
+	call salloc (errors, ncoeffs, TY_DOUBLE)
+
+	if (npts == IC_NFIT(ic)) {
+	    # Allocate memory for the fit.
+	    n = npts
+	    call salloc (fit, n, TY_DOUBLE)
+	    call salloc (wts1, n, TY_DOUBLE)
+
+	    # Eliminate rejected points and count deleted points.
+	    call amovd (wts, Memd[wts1], n)
+	    if (IC_NREJECT(ic) > 0) {
+		do i = 1, npts {
+		    if (Memi[IC_REJPTS(ic)+i-1] == YES)
+			Memd[wts1+i-1] = 0.
+		}
+	    }
+	    deleted = 0
+	    do i = 1, n {
+		if (wts[i] == 0.)
+		    deleted = deleted + 1
+	    }
+
+	    # Get the coefficients and compute the errors.
+	    call dcvvector (cv, x, Memd[fit], n)
+	    call dcvcoeff (cv, Memd[coeffs], ncoeffs)
+	    call dcverrors (cv, y, Memd[wts1], Memd[fit], n, chisqr,
+		Memd[errors])
+	    rms = ic_rmsd (x, y, Memd[fit], Memd[wts1], n)
+
+	} else {
+	    # Allocate memory for the fit.
+	    n = IC_NFIT(ic)
+	    call salloc (fit, n, TY_DOUBLE)
+	    call salloc (wts1, n, TY_DOUBLE)
+
+	    # Eliminate rejected points and count deleted points.
+	    call amovd (Memd[IC_WTSFIT(ic)], Memd[wts1], n)
+	    if (IC_NREJECT(ic) > 0) {
+	        do i = 1, npts {
+		    if (Memi[IC_REJPTS(ic)+i-1] == YES)
+			Memd[wts1+i-1] = 0.
+		}
+	    }
+	    deleted = 0
+	    do i = 1, n {
+		if (wts[i] == 0.)
+		    deleted = deleted + 1
+	    }
+
+	    # Get the coefficients and compute the errors.
+	    call dcvvector (cv, Memd[IC_XFIT(ic)], Memd[fit], n)
+	    rms = ic_rmsd (Memd[IC_XFIT(ic)], Memd[IC_YFIT(ic)],
+		Memd[fit], Memd[wts1], n)
+	    call dcvcoeff (cv, Memd[coeffs], ncoeffs)
+	    call dcverrors (cv, Memd[IC_YFIT(ic)], Memd[wts1], Memd[fit],
+		n, chisqr, Memd[errors])
+	}
+
+	# Print the error analysis.
+	call fprintf (fd, "total points = %d\nsample points = %d\n")
+	    call pargi (npts)
+	    call pargi (n)
+	call fprintf (fd, "nrejected = %d\ndeleted = %d\n")
+	    call pargi (IC_NREJECT(ic))
+	    call pargi (deleted)
+	call fprintf (fd, "RMS = %7.4g\n")
+	    call pargd (rms)
+	call fprintf (fd, "square root of reduced chi square = %7.4g\n")
+	    call pargd (sqrt (chisqr))
+
+	#call fprintf (fd, "\tcoefficent\terror\n")
+	#do i = 1, ncoeffs {
+	#    call fprintf (fd, "\t%10.4e\t%10.4e\n")
+	#	call parg$t (Mem$t[coeffs+i-1])
+	#	call parg$t (Mem$t[errors+i-1])
+	#}
+
+	# Free allocated memory.
+	call sfree (sp)
+	call close (fd)
+end
+
+
+# IC_RMS -- Compute RMS of points which have not been deleted.
+
+double procedure ic_rmsd (x, y, fit, wts, npts)
+
+double	x[ARB]		# Ordinates
+double	y[ARB]		# Abscissas
+double	fit[ARB]	# Fit
+double	wts[ARB]	# Weights
+int	npts		# Number of data points
+
+int	i, n
+double	resid, rms
+
+begin
+	rms = 0.
+	n = 0
+	do i = 1, npts {
+	    if (wts[i] == 0.)
+		next
+	    resid = y[i] - fit[i]
+	    rms = rms + resid * resid
+	    n = n + 1
+	}
+
+	if (n > 0)
+	    rms = sqrt (rms / n)
+
+	return (rms)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicfit.h b/noao/imred/dtoi/hdicfit/hdicfit.h
new file mode 100644
index 00000000..89d9c73d
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicfit.h
@@ -0,0 +1,65 @@
+# Definition file for DTOI task hdfit which uses the hdicfit subdirectory.
+
+define	NSPOTS		64	   # Initially, max number of calibration spots
+define	NVALS_FIT	200	   # Number of points in vector of fitted points
+define	WT_NONE		0	   # No weighting used in fit
+define	WT_USER		1	   # User specifies weighting in fit
+define	WT_CALC		2	   # Weighting in fit calculated from std dev
+define	MIN_DEN		EPSILONR   # Density used for setting curfit minval
+define	HD_NONE		1	   # Ind var is density - no transformation
+define	HD_LOGO		2	   # Ind var is log opacitance
+define	HD_K50		3	   # Ind var is Kaiser transform w/ alpha=0.50
+define	HD_K75		4	   # Ind var is Kaiser transform w/ alpha=0.75
+define	UDELETE		100	   # Point deleted by user flag
+define	PDELETE		101	   # Point deleted by program
+define	NDELETE		102	   # Point not deleted 
+define	ADDED_PT	0.0	   # Indication of added point in sdev array
+
+# The ICFIT data structure - modified for use with the DTOI package.
+
+define	IC_NGKEYS	5		# Number of graph keys
+define	IC_LENSTRUCT	47		# Length of ICFIT structure
+
+# User fitting parameters
+define	IC_FUNCTION	Memi[$1]	# Function type
+define	IC_ORDER	Memi[$1+1]	# Order of function
+define	IC_SAMPLE	Memi[$1+2]	# Pointer to sample string
+define	IC_NAVERAGE	Memi[$1+3]	# Sampling averaging bin
+define	IC_NITERATE	Memi[$1+4]	# Number of rejection interation
+define	IC_TRANSFORM	Memi[$1+5]	# Type of transformation ** DTOI ONLY **
+define	IC_XMIN		Memr[P2R($1+6)]	# Minimum value for curve
+define	IC_XMAX		Memr[P2R($1+7)]	# Maximum value for curve
+define	IC_LOW		Memr[P2R($1+8)]	# Low rejection value
+define	IC_HIGH		Memr[P2R($1+9)]	# Low rejection value
+define	IC_GROW		Memr[P2R($1+10)]# Rejection growing radius
+
+# ICFIT parameters used for fitting
+define	IC_NFIT		Memi[$1+11]	# Number of fit points
+define	IC_NREJECT	Memi[$1+12]	# Number of rejected points
+define	IC_RG		Memi[$1+13]	# Pointer for ranges
+define	IC_XFIT		Memi[$1+14]	# Pointer to ordinates of fit points
+define	IC_YFIT		Memi[$1+15]	# Pointer to abscissas of fit points
+define	IC_WTSFIT	Memi[$1+16]	# Pointer to weights of fit points
+define	IC_REJPTS	Memi[$1+17]	# Pointer to rejected points
+
+# ICFIT parameters used for interactive graphics
+define	IC_NEWX		Memi[$1+18]	# New x fit points?
+define	IC_NEWY		Memi[$1+19]	# New y points?
+define	IC_NEWWTS	Memi[$1+20]	# New weights?
+define	IC_NEWFUNCTION	Memi[$1+21]	# New fitting function?
+define	IC_NEWTRANSFORM Memi[$1+22]	# New transform?  ** DTOI ONLY **
+define	IC_OVERPLOT	Memi[$1+23]	# Overplot next plot?
+define	IC_FITERROR	Memi[$1+24]	# Error in fit
+define	IC_LABELS	Memi[$1+25+$2-1]# Graph axis labels
+define	IC_UNITS	Memi[$1+27+$2-1]# Graph axis units
+
+define	IC_FOG		Memr[P2R($1+29)]# *** DTOI ONLY *** value of fog level
+define	IC_NEWFOG	Memi[$1+30]	# Flag for change in fog
+define	IC_RESET	Memi[$1+31]	# Flag for resetting variables
+define	IC_UPDATE	Memi[$1+32]
+define	IC_EBARS	Memi[$1+33]	# Flag for plotting error bars
+define	IC_RFOG		Memr[P2R($1+34)]# Reference value of fog for resetting
+
+# ICFIT key definitions
+define	IC_GKEY		Memi[$1+35]			# Graph key
+define	IC_AXES		Memi[$1+36+($2-1)*2+$3-1]	# Graph axis codes
diff --git a/noao/imred/dtoi/hdicfit/hdicfit.x b/noao/imred/dtoi/hdicfit/hdicfit.x
new file mode 100644
index 00000000..91e05f9d
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicfit.x
@@ -0,0 +1,80 @@
+include	<math/curfit.h>
+include	"hdicfit.h"
+
+# IC_FIT -- Fit a function.  This is the main fitting task.  It uses
+# flags to define changes since the last fit.  This allows the most
+# efficient use of the curfit and ranges packages.
+
+procedure ic_fitd (ic, cv, x, y, wts, npts, newx, newy, newwts, newfunction)
+
+pointer	ic				# ICFIT pointer
+pointer	cv				# Curfit pointer
+double	x[npts]				# Ordinates
+double	y[npts]				# Data to be fit
+double	wts[npts]			# Weights
+int	npts				# Number of points
+int	newx				# New x points?
+int	newy				# New y points?
+int	newwts				# New weights?
+int	newfunction			# New function?
+
+int	ier, refit
+errchk	ic_dosetupd
+
+begin
+	# Setup the new parameters.
+	call ic_dosetupd (ic, cv, x, wts, npts, newx, newwts, newfunction,
+	    refit)
+
+	if (npts == IC_NFIT(ic)) {
+	    # If not sampling use the data array directly.
+	    if (refit == NO) {
+	        call dcvfit (cv, x, y, wts, npts, WTS_USER, ier)
+	    } else if (newy == YES)
+	        call dcvrefit (cv, x, y, wts, ier)
+
+	} else {
+	    # If sampling first form the sample y values.
+	    if ((newx == YES) || (newy == YES) || (newwts == YES))
+	        call rg_wtbind (IC_RG(ic), IC_NAVERAGE(ic), y, wts, npts,
+		    Memd[IC_YFIT(ic)], Memd[IC_WTSFIT(ic)], IC_NFIT(ic))
+	    if (refit == NO) {
+	        call dcvfit (cv, Memd[IC_XFIT(ic)], Memd[IC_YFIT(ic)],
+		    Memd[IC_WTSFIT(ic)], IC_NFIT(ic), WTS_USER, ier)
+	    } else if (newy == YES)
+	        call dcvrefit (cv, Memd[IC_XFIT(ic)], Memd[IC_YFIT(ic)],
+		    Memd[IC_WTSFIT(ic)], ier)
+	}
+
+	# Check for an error in the fit.
+	switch (ier) {
+	case SINGULAR:
+	    call printf ("Singular solution")
+	    call flush (STDOUT)
+	case NO_DEG_FREEDOM:
+	    call printf ("No degrees of freedom")
+	    call flush (STDOUT)
+	    return
+	}
+
+	refit = YES
+
+	# Do pixel rejection if desired.
+	if ((IC_LOW(ic) > 0.) || (IC_HIGH(ic) > 0.)) {
+	    if (npts == IC_NFIT(ic)) {
+	        call ic_rejectd (cv, x, y, wts, Memi[IC_REJPTS(ic)],
+		    IC_NFIT(ic), IC_LOW(ic), IC_HIGH(ic), IC_NITERATE(ic),
+		    IC_GROW(ic), IC_NREJECT(ic))
+	    } else {
+	        call ic_rejectd (cv, Memd[IC_XFIT(ic)], Memd[IC_YFIT(ic)],
+		    Memd[IC_WTSFIT(ic)], Memi[IC_REJPTS(ic)], IC_NFIT(ic),
+		    IC_LOW(ic), IC_HIGH(ic), IC_NITERATE(ic), IC_GROW(ic),
+		    IC_NREJECT(ic))
+	    }
+
+	    if (IC_NREJECT(ic) > 0)
+		refit = NO
+	} else
+	    IC_NREJECT(ic) = 0
+end
+
diff --git a/noao/imred/dtoi/hdicfit/hdicgaxes.x b/noao/imred/dtoi/hdicfit/hdicgaxes.x
new file mode 100644
index 00000000..4f016c9d
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicgaxes.x
@@ -0,0 +1,101 @@
+include	<pkg/gtools.h>
+include	"hdicfit.h"
+
+# ICG_AXES -- Set axes data.
+# The applications program may set additional axes types.
+
+procedure icg_axesd (ic, gt, cv, axis, x, y, z, npts)
+
+pointer	ic				# ICFIT pointer
+pointer	gt				# GTOOLS pointer
+pointer	cv				# CURFIT pointer
+int	axis				# Output axis
+double	x[npts]				# Independent variable
+double	y[npts]				# Dependent variable
+double	z[npts]				# Output values
+int	npts				# Number of points
+
+int	i, axistype, gtlabel[2], gtunits[2]
+double 	a, b, xmin, xmax
+pointer	label, units
+
+double	dcveval(), icg_dvzd()
+errchk	adivd()
+extern	icg_dvzd()
+
+data	gtlabel/GTXLABEL, GTYLABEL/
+data	gtunits/GTXUNITS, GTYUNITS/
+
+begin
+	axistype = IC_AXES(ic, IC_GKEY(ic), axis)
+	switch (axistype) {
+	case 'x':	# Independent variable
+	    call gt_sets (gt, gtlabel[axis], Memc[IC_LABELS(ic,1)])
+	    call gt_sets (gt, gtunits[axis], Memc[IC_UNITS(ic,1)])
+	    call amovd (x, z, npts)
+	    call gt_sets (gt, GTSUBTITLE, "")
+	case 'y':	# Dependent variable
+	    call gt_sets (gt, gtlabel[axis], Memc[IC_LABELS(ic,2)])
+	    call gt_sets (gt, gtunits[axis], Memc[IC_UNITS(ic,2)])
+	    call amovd (y, z, npts)
+	    call gt_sets (gt, GTSUBTITLE, "")
+	case 'f':	# Fitted values
+	    call gt_sets (gt, gtlabel[axis], "fit")
+	    call gt_sets (gt, gtunits[axis], Memc[IC_UNITS(ic,2)])
+	    call dcvvector (cv, x, z, npts)
+	    call gt_sets (gt, GTSUBTITLE, "")
+	case 'r':	# Residuals
+	    call gt_sets (gt, gtlabel[axis], "residuals")
+	    call gt_sets (gt, gtunits[axis], Memc[IC_UNITS(ic,2)])
+	    call dcvvector (cv, x, z, npts)
+	    call asubd (y, z, z, npts)
+	    call gt_sets (gt, GTSUBTITLE, "")
+	case 'd':	# Ratio
+	    call gt_sets (gt, gtlabel[axis], "ratio")
+	    call gt_sets (gt, gtunits[axis], "")
+	    call dcvvector (cv, x, z, npts)
+#	    iferr (call adiv$t (y, z, z, npts))
+		call advzd (y, z, z, npts, icg_dvzd)
+	    call gt_sets (gt, GTSUBTITLE, "")
+	case 'n':	# Linear component removed
+	    call gt_sets (gt, gtlabel[axis], "non-linear component")
+	    call gt_sets (gt, gtunits[axis], Memc[IC_UNITS(ic,2)])
+	    xmin = IC_XMIN(ic)
+	    xmax = IC_XMAX(ic)
+	    a = dcveval (cv, double(xmin))
+	    b = (dcveval (cv, double(xmax)) - a) / (xmax - xmin)
+	    do i = 1, npts
+	        z[i] = y[i] - a - b * (x[i] - xmin)
+	    call gt_sets (gt, GTSUBTITLE, "")
+	default:	# User axes types.
+	    call malloc (label, SZ_LINE, TY_CHAR)
+	    call malloc (units, SZ_LINE, TY_CHAR)
+	    if (axis == 1) {
+		call strcpy (Memc[IC_LABELS(ic,1)], Memc[label], SZ_LINE)
+		call strcpy (Memc[IC_UNITS(ic,1)], Memc[units], SZ_LINE)
+	        call amovd (x, z, npts)
+	    } else {
+		call strcpy (Memc[IC_LABELS(ic,2)], Memc[label], SZ_LINE)
+		call strcpy (Memc[IC_UNITS(ic,2)], Memc[units], SZ_LINE)
+	        call amovd (y, z, npts)
+	    }
+	    call icg_uaxesd (ic, axistype, cv, x, y, z, npts, Memc[label], 
+		Memc[units], SZ_LINE)
+	    call gt_sets (gt, gtlabel[axis], Memc[label])
+	    call gt_sets (gt, gtunits[axis], Memc[units])
+	    call gt_sets (gt, GTSUBTITLE, "HD Curve")
+	    call mfree (label, TY_CHAR)
+	    call mfree (units, TY_CHAR)
+	}
+end
+
+
+# ICG_DVZ -- Error action to take on zero division.
+
+double procedure icg_dvzd (x)
+
+double	x			# Numerator
+
+begin
+	return (1.)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicgcolon.x b/noao/imred/dtoi/hdicfit/hdicgcolon.x
new file mode 100644
index 00000000..52299df7
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicgcolon.x
@@ -0,0 +1,284 @@
+include	<error.h>
+include	<gset.h>
+include	"hdicfit.h"
+
+define	EB_WTS	10
+define	EB_SDEV	11
+
+# List of colon commands.
+define	CMDS "|show|sample|naverage|function|order|low_reject|high_reject|\
+              |niterate|grow|errors|vshow|transform|fog|reset|quit|ebars|"
+
+define	SHOW		1	# Show values of parameters
+define	SAMPLE		2	# Set or show sample ranges
+define	NAVERAGE	3	# Set or show sample averaging or medianing
+define	FUNCTION	4	# Set or show function type
+define	ORDER		5	# Set or show order
+define	LOW_REJECT	6	# Set or show lower rejection factor
+define	HIGH_REJECT	7	# Set or show upper rejection factor
+# newline		8
+define	NITERATE	9	# Set or show rejection iterations
+define	GROW		10	# Set or show rejection growing radius
+define	ERRORS		11	# Show errors of fit
+define	VSHOW		12	# Show verbose information
+define	TRANSFORM	13	# Set or show transformation
+define	FOG		14	# Set or show value of fog
+define	RESET		15	# Reset x, y, wts, npts to original values
+define	QUIT		16	# Terminate without updating database
+define	EBARS		17	# Set error bars to represent weights or
+				#     standard deviations
+
+# ICG_COLON -- Processes colon commands.  
+
+procedure icg_colond (ic, cmdstr, gp, gt, cv, x, y, wts, npts)
+
+pointer	ic				# ICFIT pointer
+char	cmdstr[ARB]			# Command string
+pointer	gp				# GIO pointer
+pointer	gt				# GTOOLS pointer
+pointer	cv				# CURFIT pointer for error listing
+double	x[npts], y[npts], wts[npts]	# Data arrays for error listing
+int	npts				# Number of data points
+
+real	rval
+char	cmd[SZ_LINE]
+int	ncmd, ival, ip, junk
+
+int	nscan(), strdic(), strncmp(), ctor()
+string	funcs "|chebyshev|legendre|spline1|spline3|power|"
+string	tform "|none|logopacitance|k50|k75|"
+
+begin
+	# Use formated scan to parse the command string.
+	# The first word is the command and it may be minimum match
+	# abbreviated with the list of commands.
+
+	call sscan (cmdstr)
+	call gargwrd (cmd, SZ_LINE)
+	ncmd = strdic (cmd, cmd, SZ_LINE, CMDS)
+
+	switch (ncmd) {
+	case SHOW:
+	    # show: Show the values of the fitting parameters.  The terminal
+	    # is cleared and paged using the gtools paging procedures.
+
+	    call gargwrd (cmd, SZ_LINE)
+	    if (nscan() == 1) {
+	        call gdeactivate (gp, AW_CLEAR)
+		call ic_show (ic, "STDOUT", gt)
+	        call greactivate (gp, AW_PAUSE)
+	    } else {
+		iferr (call ic_show (ic, cmd, gt))
+		    call erract (EA_WARN)
+	    }
+
+	case SAMPLE:
+	    # sample: List or set the sample points.
+
+	    call gargwrd (cmd, SZ_LINE)
+	    if (cmd[1] == EOS) {
+	        call printf ("sample = %s\n")
+		    call pargstr (Memc[IC_SAMPLE(ic)])
+	    } else {
+		call strcpy (cmd, Memc[IC_SAMPLE(ic)], SZ_LINE)
+		IC_NEWX(ic) = YES
+	    }
+
+	case NAVERAGE:
+	    # naverage: List or set the sample averging.
+
+	    call gargi (ival)
+	    if (nscan() == 1) {
+		call printf ("naverage = %d\n")
+		    call pargi (IC_NAVERAGE(ic))
+	    } else {
+		IC_NAVERAGE(ic) = ival
+		IC_NEWX(ic) = YES
+	    }
+
+	case FUNCTION:
+	    # function: List or set the fitting function.
+
+	    call gargwrd (cmd, SZ_LINE)
+	    if (cmd[1] == EOS) {
+		call printf ("function = %s\n")
+		    call ic_gstr (ic, "function", cmd, SZ_LINE)
+		    call pargstr (cmd)
+	    } else {
+		if (strdic (cmd, cmd, SZ_LINE, funcs) > 0) {
+		    call ic_pstr (ic, "function", cmd)
+		    IC_NEWFUNCTION(ic) = YES
+		} else
+		    call printf ("Unknown or ambiguous function")
+	    }
+
+	case ORDER:
+	    # order: List or set the function order.
+
+	    call gargi (ival)
+	    if (nscan() == 1) {
+		call printf ("order = %d\n")
+		    call pargi (IC_ORDER(ic))
+	    } else {
+		IC_ORDER(ic) = ival
+		IC_NEWFUNCTION(ic) = YES
+	    }
+
+	case LOW_REJECT:
+	    # low_reject: List or set the lower rejection threshold.
+
+	    call gargr (rval)
+	    if (nscan() == 1) {
+		call printf ("low_reject = %g\n")
+		    call pargr (IC_LOW(ic))
+	    } else
+		IC_LOW(ic) = rval
+
+	case HIGH_REJECT:
+	    # high_reject: List or set the high rejection threshold.
+
+	    call gargr (rval)
+	    if (nscan() == 1) {
+		call printf ("high_reject = %g\n")
+		    call pargr (IC_HIGH(ic))
+	    } else
+		IC_HIGH(ic) = rval
+
+	case NITERATE:
+	    # niterate: List or set the number of rejection iterations.
+
+	    call gargi (ival)
+	    if (nscan() == 1) {
+		call printf ("niterate = %d\n")
+		    call pargi (IC_NITERATE(ic))
+	    } else
+		IC_NITERATE(ic) = ival
+
+	case GROW:
+	    # grow: List or set the rejection growing.
+
+	    call gargr (rval)
+	    if (nscan() == 1) {
+		call printf ("grow = %g\n")
+		    call pargr (IC_GROW(ic))
+	    } else
+		IC_GROW(ic) = rval
+
+	case ERRORS:
+	    call gargwrd (cmd, SZ_LINE)
+	    if (nscan() == 1) {
+	        call gdeactivate (gp, AW_CLEAR)
+		call ic_show (ic, "STDOUT", gt)
+		call ic_errorsd (ic, "STDOUT", cv, x, y, wts, npts)
+	        call greactivate (gp, AW_PAUSE)
+	    } else {
+		iferr {
+		    call ic_show (ic, cmd, gt)
+		    call ic_errorsd (ic, cmd, cv, x, y, wts, npts)
+		} then
+		    call erract (EA_WARN)
+	    }
+	case VSHOW:
+	    # verbose show:  Show the values of the fitting parameters. 
+	    # The terminal is paged using the gtools paging procedure. 
+
+	    call gargwrd (cmd, SZ_LINE)
+	    if (cmd[1] == EOS) {
+		call gdeactivate (gp, AW_CLEAR)
+		call ic_vshowd (ic, "STDOUT", cv, x, y, wts, npts, gt)
+		call greactivate (gp, AW_PAUSE)
+	    } else {
+		iferr {
+		    call ic_vshowd (ic, cmd, cv, x, y, wts, npts, gt)
+		} then 
+		    call erract (EA_WARN)
+	    }
+	case TRANSFORM:
+	    # transform: List or set the transformation type.  This
+	    # option applies to HDTOI procedures only.
+
+	    call gargwrd (cmd, SZ_LINE)
+	    if (cmd[1] == EOS) {
+		call printf ("transform = %s\n")
+		    call ic_gstr (ic, "transform", cmd, SZ_LINE)
+		    call pargstr (cmd)
+	    } else {
+		ival= strdic (cmd, cmd, SZ_LINE, tform) 
+		if (ival > 0) {
+		    call ic_pstr (ic, "transform", cmd)
+		    IC_NEWTRANSFORM(ic) = YES
+		    IC_NEWX(ic) = YES
+		    switch (IC_TRANSFORM(ic)) {
+		    case HD_NONE:
+	    		call ic_pstr (ic, "xlabel", "Density")
+		    case HD_LOGO:
+	    		call ic_pstr (ic, "xlabel", 
+			    "Log Opacitance: log (10**Den - 1)")
+		    case HD_K50:
+	    		call ic_pstr (ic, "xlabel", 
+		           "Den + 0.50 * Log (1 - (10 ** -Den))")
+		    case HD_K75:
+	    		call ic_pstr (ic, "xlabel", 
+			    "Den + 0.75 * Log (1 - (10 ** -Den))")
+		    }
+		} else
+		    call printf ("Unknown or ambiguous transform")
+	    }
+
+	case FOG:
+	    # fog: DTOI ONLY - change or reset the value of the fog level
+
+	    call gargwrd (cmd, SZ_LINE)
+	    if (cmd[1] == EOS) {
+		call printf ("fog = %g\n")
+		    call pargr (IC_FOG(ic))
+	    } else {
+		if (strncmp (cmd, "reset", 1) == 0)
+		    IC_FOG(ic) = IC_RFOG(ic)
+		else {
+		    ip = 1
+		    junk = ctor (cmd, ip, rval)
+		    IC_FOG(ic) = rval
+		}
+		IC_NEWFOG(ic) = YES
+		IC_NEWX(ic) = YES
+	    }
+
+	case RESET:
+	    # Set flag to reset x, y, wts and npts to original values.
+	    IC_RESET(ic) = YES
+	    IC_NEWX(ic) = YES
+	    IC_NEWY(ic) = YES
+	    IC_NEWWTS(ic) = YES
+	    IC_NEWFUNCTION(ic) = YES
+	    IC_NEWTRANSFORM(ic) = YES
+
+	case QUIT:
+	    # Set update flag to know
+	    IC_UPDATE(ic) = NO
+
+	case EBARS:
+	    # [HV]BAR marker can indicate either errors or weights
+	    call gargwrd (cmd, SZ_LINE)
+	    if (cmd[1] == EOS) {
+		if (IC_EBARS(ic) == EB_WTS)
+		    call printf ("ebars = Weights\n")
+		else if (IC_EBARS(ic) == EB_SDEV)
+		    call printf ("ebars = Errors\n")
+	    } else {
+		if (strncmp (cmd, "weights", 1) == 0 || 
+		    strncmp (cmd, "WEIGHTS", 1) == 0)
+		    IC_EBARS(ic) = EB_WTS
+		else if (strncmp (cmd, "errors", 1) == 0 || 
+		    strncmp (cmd, "ERRORS", 1) == 0)
+		    IC_EBARS(ic) = EB_SDEV
+		else
+		    call printf ("Unrecognized value for ebars '%s'\n")
+			call pargstr (cmd)
+	    }
+
+	default:
+	    call eprintf ("Unrecognized command '%s'\n")
+		call pargstr (cmd)
+	}
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicgdelete.x b/noao/imred/dtoi/hdicfit/hdicgdelete.x
new file mode 100644
index 00000000..82c61f70
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicgdelete.x
@@ -0,0 +1,81 @@
+include	<gset.h>
+include	<mach.h>
+include	<pkg/gtools.h>
+include	"hdicfit.h"
+
+define	MSIZE		2.		# Mark size
+
+# ICG_DELETE -- Delete data point nearest the cursor.
+# The nearest point to the cursor in NDC coordinates is determined.
+
+procedure icg_deleted (ic, gp, gt, cv, x, y, wts, npts, wx, wy)
+
+pointer	ic					# ICFIT pointer
+pointer	gp					# GIO pointer
+pointer	gt					# GTOOLS pointer
+pointer	cv					# CURFIT pointer
+double	x[npts], y[npts]			# Data points
+double	wts[npts]				# Weight array
+int	npts					# Number of points
+real	wx, wy					# Position to be nearest
+
+int	gt_geti()
+pointer	sp, xout, yout
+
+begin
+	call smark (sp)
+	call salloc (xout, npts, TY_DOUBLE)
+	call salloc (yout, npts, TY_DOUBLE)
+
+	call icg_axesd (ic, gt, cv, 1, x, y, Memd[xout], npts)
+	call icg_axesd (ic, gt, cv, 2, x, y, Memd[yout], npts)
+	if (gt_geti (gt, GTTRANSPOSE) == NO)
+	    call icg_d1d (ic, gp, Memd[xout], Memd[yout], wts, npts, wx, wy)
+	else
+	    call icg_d1d (ic, gp, Memd[yout], Memd[xout], wts, npts, wy, wx)
+
+	call sfree (sp)
+end
+
+
+# ICG_D1D - Do the actual delete.
+
+procedure icg_d1d (ic, gp, x, y, wts, npts, wx, wy)
+
+pointer	ic					# ICFIT pointer
+pointer	gp					# GIO pointer
+double	x[npts], y[npts]			# Data points
+double	wts[npts]				# Weight array
+int	npts					# Number of points
+real	wx, wy					# Position to be nearest
+
+int	i, j
+real	x0, y0, r2, r2min
+
+begin
+	# Transform world cursor coordinates to NDC.
+	call gctran (gp, wx, wy, wx, wy, 1, 0)
+
+	# Search for nearest point to a point with non-zero weight.
+	r2min = MAX_REAL
+	do i = 1, npts {
+	    if (wts[i] == 0.)
+		next
+
+	    call gctran (gp, real (x[i]), real (y[i]), x0, y0, 1, 0)
+		
+	    r2 = (x0 - wx) ** 2 + (y0 - wy) ** 2
+	    if (r2 < r2min) {
+		r2min = r2
+		j = i
+	    }
+	}
+
+	# Mark the deleted point with a cross and set the weight to zero.
+	if (j != 0) {
+	    call gscur (gp, real (x[j]), real (y[j]))
+	    call gmark (gp, real (x[j]), real (y[j]), GM_CROSS, MSIZE, MSIZE)
+	    wts[j] = 0.
+	    IC_NEWWTS(ic) = YES
+	}
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicgfit.x b/noao/imred/dtoi/hdicfit/hdicgfit.x
new file mode 100644
index 00000000..b50ed03c
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicgfit.x
@@ -0,0 +1,402 @@
+include	<error.h>
+include	<pkg/gtools.h>
+include	<mach.h>
+include	<gset.h>
+include	"hdicfit.h"
+
+define	HELP		"noao$lib/scr/hdicgfit.key"
+define	PROMPT		"hdicfit options"
+define	EB_WTS		10
+define	EB_SDEV		11
+
+# ICG_FIT -- Interactive curve fitting with graphics.  This is the main
+# entry point for the interactive graphics part of the icfit package.
+
+procedure icg_fitd (ic, gp, cursor, gt, cv, density, loge, owts, osdev, npts)
+
+pointer	ic			# ICFIT pointer
+pointer	gp			# GIO pointer
+char	cursor[ARB]		# GIO cursor input
+pointer	gt			# GTOOLS pointer
+pointer	cv			# CURFIT pointer
+double	density[npts]		# Original density, not fog subtracted
+double	loge[npts]		# Original log exposure values
+double	owts[npts]		# Original weights array
+double	osdev[npts]		# Original standard deviation array
+int	npts			# Number of points
+
+real	wx, wy, wwy, oldx, oldy
+int	wcs, key, nptso
+char	cmd[SZ_LINE]
+
+int	i, newgraph, axes[2], linetype
+double	x1, newwt
+pointer	userwts, x, y, wts, den, whydel, sdev, ebw
+
+int	clgcur(), stridxs(), scan(), nscan()
+int	icg_nearestd(), gstati()
+double	dcveval()
+errchk	ic_fitd, malloc
+define	redraw_ 91
+
+begin
+	# Allocate memory for the fit and a copy of the weights.
+	# The weights are copied because they are changed when points are
+	# deleted.  The input x is the untransformed density, and is used
+	# to generate other types of transforms.  Points can be added to
+	# the sample, so the y array and weights array can change as well.
+	# The original number of points is also remembered.
+
+	call malloc (userwts, npts, TY_DOUBLE)
+	call malloc (x,       npts, TY_DOUBLE)
+	call malloc (y,       npts, TY_DOUBLE)
+	call malloc (wts,     npts, TY_DOUBLE)
+	call malloc (den,     npts, TY_DOUBLE)
+	call malloc (whydel,  npts, TY_INT)
+	call malloc (sdev,    npts, TY_DOUBLE)
+	call malloc (ebw,     npts, TY_DOUBLE)
+
+	call amovd (owts,     Memd[userwts], npts)
+	call amovd (owts,     Memd[wts],     npts)
+	call amovd (loge,     Memd[y],       npts)
+	call amovd (density,  Memd[den],     npts)
+	call amovki (NDELETE, Memi[whydel],  npts)
+	call amovd (osdev,    Memd[sdev],    npts)
+	nptso = npts
+
+	# Initialize
+	IC_OVERPLOT(ic) = NO
+	IC_NEWX(ic) = YES
+	IC_NEWY(ic) = YES
+	IC_NEWWTS(ic) = YES
+	IC_NEWFUNCTION(ic) = YES
+	IC_NEWTRANSFORM(ic) = YES
+	IC_UPDATE(ic) = YES
+	IC_EBARS(ic) = EB_SDEV
+
+	# Read cursor commands.
+
+	key = 'f'
+	axes[1] = IC_AXES(ic, IC_GKEY(ic), 1)
+	axes[2] = IC_AXES(ic, IC_GKEY(ic), 2)
+
+	repeat {
+	    switch (key) {
+	    case '?': # Print help text.
+		call gpagefile (gp, HELP, PROMPT)
+
+	    case 'q': # Terminate cursor loop
+		break
+
+	    case ':': # List or set parameters
+		if (stridxs ("/", cmd) == 1)
+	            call gt_colon (cmd, gp, gt, newgraph)
+		else
+		    call icg_colond (ic, cmd, gp, gt, cv, Memd[x], 
+			Memd[y], Memd[wts], npts)
+
+		if (IC_RESET(ic) == YES) {
+		    npts = nptso
+		    call amovd (owts, Memd[userwts], npts)
+		    call amovd (owts, Memd[wts], npts)
+		    call amovd (loge, Memd[y], npts)
+		    call amovd (density, Memd[den], npts)
+		    call amovki (NDELETE, Memi[whydel], npts)
+		    call amovd (osdev, Memd[sdev], npts)
+		    call hdic_init (density, npts, 0.0)
+		}
+
+		# See if user wants to quit without updating
+		if (IC_UPDATE(ic) == NO) {
+		    call mfree (x, TY_DOUBLE)
+		    call mfree (y, TY_DOUBLE)
+		    call mfree (wts, TY_DOUBLE)
+		    call mfree (userwts, TY_DOUBLE)
+		    call mfree (den, TY_DOUBLE)
+		    call mfree (sdev, TY_DOUBLE)
+		    return
+		}
+
+	    case 'a': # Add data points to the sample.  This is only possible 
+		      # from an HD curve plot.
+
+		if ((IC_AXES (ic, IC_GKEY(ic), 1) == 'y') &&
+		    (IC_AXES (ic, IC_GKEY(ic), 2) == 'u')) {
+
+		    # Query for weight after plotting current location
+		    # call gt_plot (gp, gt, wx, wy, 1)
+		    call gmark (gp, wx, wy, GM_CIRCLE, 2.0, 2.0)
+		    newwt = 1.0D0
+		    call printf ("Enter weight of new point (%g): ")
+			call pargd (newwt)
+		    call flush (STDOUT)
+		    if (scan() != EOF) {
+		        call pargd (x1)
+		        if (nscan() == 1) {
+			    if (!IS_INDEFD (x1)) {
+			        newwt = x1
+			    }
+		        }
+		    }
+
+		} else {
+		    call eprintf ("Points can be added only from an HD Curve\n")
+		    next
+		}
+
+		# Add fog into "density above fog" value read from cursor
+		wwy = wy + IC_FOG (ic)
+		if (wwy < 0.0) {
+		    call eprintf (
+			"New density (%g) is below fog and will not be added\n")
+			    call pargr (wwy)
+		    next
+		}
+
+		# Add point into sample
+		call eprintf ("New Point: density above fog = %.4f, log ")
+		    call pargr (wwy)
+		call eprintf ("exposure = %.4f, weight = %.4f\n")
+		    call pargr (wx)
+		    call pargd (newwt)
+
+		call hdic_addpoint (ic, wwy, wx, newwt, den, y, wts, userwts, 
+		    x, whydel, sdev, npts)
+
+		call realloc (ebw, npts, TY_DOUBLE)
+
+		call hdic_transform (ic, Memd[den], Memd[userwts], Memd[x], 
+		    Memd[wts], Memi[whydel], npts)
+
+	    case 'c': # Print the positions of data points.
+		i = icg_nearestd (ic, gp, gt, cv, Memd[x], Memd[y], npts, 
+		    wx, wy)
+
+	    	if (i != 0) {
+		    call printf ("den= %7.4g x= %7.4g  exp= %7.4g  fit= %7.4g")
+			call pargd (Memd[den+i-1])
+			call pargd (Memd[x+i-1])
+			call pargd (Memd[y+i-1])
+			call pargd (dcveval (cv, Memd[x+i-1]))
+		}
+
+	    case 'd': # Delete data points.
+		call icg_deleted (ic, gp, gt, cv, Memd[x], Memd[y], Memd[wts], 
+		    npts, wx, wy)
+
+	    case 'f': # Fit the function and reset the flags.
+		iferr {
+		    # Copy new transformed vector, if necessary
+		    if (IC_NEWTRANSFORM(ic) == YES || IC_NEWFOG(ic) == YES) 
+			call hdic_transform (ic, Memd[den], Memd[userwts], 
+			    Memd[x], Memd[wts], Memi[whydel], npts)
+
+		    call ic_fitd (ic, cv, Memd[x], Memd[y], Memd[wts], npts, 
+			IC_NEWX(ic), IC_NEWY(ic), IC_NEWWTS(ic), 
+			    IC_NEWFUNCTION(ic))
+
+		    IC_NEWX(ic) = NO
+		    IC_NEWY(ic) = NO
+		    IC_NEWWTS(ic) = NO
+		    IC_NEWFUNCTION(ic) = NO
+		    IC_NEWTRANSFORM(ic) = NO
+		    IC_FITERROR(ic) = NO
+		    IC_NEWFOG(ic) = NO
+		    newgraph = YES
+		} then {
+		    IC_FITERROR(ic) = YES
+		    call erract (EA_WARN)
+		    newgraph = NO
+		}
+
+	    case 'g':	# Set graph axes types.
+		call printf ("Graph key to be defined: ")
+		call flush (STDOUT)
+		if (scan() == EOF)
+		    goto redraw_
+		call gargc (cmd[1])
+
+		switch (cmd[1]) {
+		case '\n':
+		case 'h', 'i', 'j', 'k', 'l':
+		    switch (cmd[1]) {
+		    case 'h':
+		        key = 1
+		    case 'i':
+		        key = 2
+		    case 'j':
+		        key = 3
+		    case 'k':
+		        key = 4
+		    case 'l':
+		        key = 5
+		    }
+
+		    call printf ("Set graph axes types (%c, %c): ")
+		        call pargc (IC_AXES(ic, key, 1))
+		        call pargc (IC_AXES(ic, key, 2))
+		    call flush (STDOUT)
+		    if (scan() == EOF)
+		        goto redraw_
+		    call gargc (cmd[1])
+
+		    switch (cmd[1]) {
+		    case '\n':
+		    default:
+		        call gargc (cmd[2])
+		        call gargc (cmd[2])
+		        if (cmd[2] != '\n') {
+			    IC_AXES(ic, key, 1) = cmd[1]
+			    IC_AXES(ic, key, 2) = cmd[2]
+		        }
+		    }
+		default:
+		    call printf ("Not a graph key")
+		}
+
+	    case 'h':
+		if (IC_GKEY(ic) != 1) {
+		    IC_GKEY(ic) = 1
+		    newgraph = YES
+		}
+
+	    case 'i':
+		if (IC_GKEY(ic) != 2) {
+		    IC_GKEY(ic) = 2
+		    newgraph = YES
+		}
+
+	    case 'j':
+		if (IC_GKEY(ic) != 3) {
+		    IC_GKEY(ic) = 3
+		    newgraph = YES
+		}
+
+	    case 'k':
+		if (IC_GKEY(ic) != 4) {
+		    IC_GKEY(ic) = 4
+		    newgraph = YES
+		}
+
+	    case 'l':
+		if (IC_GKEY(ic) != 5) {
+		    IC_GKEY(ic) = 5
+		    newgraph = YES
+		}
+
+	    case 'o': # Set overplot flag
+		IC_OVERPLOT(ic) = YES
+
+	    case 'r': # Redraw the graph
+		newgraph = YES
+
+	    case 'u': # Undelete data points.
+		call icg_undeleted (ic, gp, gt, cv, Memd[x], Memd[y], 
+		    Memd[wts], Memd[userwts], npts, wx, wy)
+
+	    case 'w':  # Window graph
+		call gt_window (gt, gp, cursor, newgraph)
+
+	    case 'x': # Reset the value of the x point.
+		i = icg_nearestd (ic, gp, gt, cv, Memd[x], Memd[y], npts, wx, 
+		    wy)
+
+	    	if (i != 0) {
+		    call printf ("Enter new x (%g): ")
+			call pargd (Memd[x+i-1])
+		    call flush (STDOUT)
+		    if (scan() != EOF) {
+		        call gargd (x1)
+		        if (nscan() == 1) {
+			    if (!IS_INDEF (x1)) {
+				oldx = Memd[x+i-1]
+				oldy = Memd[y+i-1]
+			        Memd[x+i-1] = x1
+				call hd_redraw (gp, oldx, oldy, x1, oldy)
+			        IC_NEWX(ic) = YES
+			    }
+			}
+		    }
+		}
+
+	    case 'y': # Reset the value of the y point.
+		i = icg_nearestd (ic, gp, gt, cv, Memd[x], Memd[y], npts, wx, 
+		    wy)
+
+	    	if (i != 0) {
+		    call printf ("Enter new y (%g): ")
+			call pargd (Memd[y+i-1])
+		    call flush (STDOUT)
+		    if (scan() != EOF) {
+		        call gargd (x1)
+		        if (nscan() == 1) {
+			    if (!IS_INDEF (x1)) {
+				oldx = Memd[x+i-1]
+				oldy = Memd[y+i-1]
+			        Memd[y+i-1] = x1
+				call hd_redraw (gp, oldx, oldy, oldx, x1)
+			        IC_NEWY(ic) = YES
+			    }
+			}
+		    }
+		}
+
+	    case 'z': # Reset the weight value of the nearest point
+		i = icg_nearestd (ic, gp, gt, cv, Memd[x], Memd[y], npts, wx, 
+		    wy)
+
+	    	if (i != 0) {
+		    call printf ("Enter new weight (%g): ")
+			call pargd (Memd[wts+i-1])
+		    call flush (STDOUT)
+		    if (scan() != EOF) {
+		        call gargd (x1)
+		        if (nscan() == 1) {
+			    if (!IS_INDEF (x1)) {
+			        Memd[wts+i-1] = x1
+			        IC_NEWWTS(ic) = YES
+			    }
+			}
+		    }
+		}
+
+	    default: # Let the user decide on any other keys.
+		call icg_user (ic, gp, gt, cv, wx, wy, wcs, key, cmd)
+	    }
+
+	    # Redraw the graph if necessary.
+redraw_	    if (newgraph == YES) {
+		if (IC_AXES(ic, IC_GKEY(ic), 1) != axes[1]) {
+		    axes[1] = IC_AXES(ic, IC_GKEY(ic), 1)
+		    call gt_setr (gt, GTXMIN, INDEF)
+		    call gt_setr (gt, GTXMAX, INDEF)
+		}
+		if (IC_AXES(ic, IC_GKEY(ic), 2) != axes[2]) {
+		    axes[2] = IC_AXES(ic, IC_GKEY(ic), 2)
+		    call gt_setr (gt, GTYMIN, INDEF)
+		    call gt_setr (gt, GTYMAX, INDEF)
+		}
+
+		# Overplot with a different line type
+		if (IC_OVERPLOT(ic) == YES)
+		    linetype = min ((gstati (gp, G_PLTYPE) + 1), 4)
+		else
+		    linetype = GL_SOLID
+		call gseti (gp, G_PLTYPE, linetype)
+
+		call hdic_ebw (ic, Memd[den], Memd[x], Memd[sdev], Memd[ebw], 
+		    npts)
+
+	    	call icg_graphd (ic, gp, gt, cv, Memd[x], Memd[y], Memd[wts], 
+		    Memd[ebw], npts)
+
+		newgraph = NO
+	    }
+	} until (clgcur (cursor, wx, wy, wcs, key, cmd, SZ_LINE) == EOF)
+
+	call mfree (x, TY_DOUBLE)
+	call mfree (y, TY_DOUBLE)
+	call mfree (wts, TY_DOUBLE)
+	call mfree (userwts, TY_DOUBLE)
+	call mfree (den, TY_DOUBLE)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicggraph.x b/noao/imred/dtoi/hdicfit/hdicggraph.x
new file mode 100644
index 00000000..dcd9ade3
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicggraph.x
@@ -0,0 +1,329 @@
+include	<mach.h>
+include	<gset.h>
+include	<pkg/gtools.h>
+include	"hdicfit.h"
+
+define	MSIZE		2.		# Mark size
+define	SZ_TPLOT	7		# String length for plot type
+define	EB_WTS		10
+define	EB_SDEV		11
+define	MAX_SZMARKER	4
+
+# ICG_GRAPH -- Graph data and fit.
+
+procedure icg_graphd (ic, gp, gt, cv, x, y, wts, ebw, npts)
+
+pointer	ic				# ICFIT pointer
+pointer	gp				# GIO pointer
+pointer	gt				# GTOOLS pointers
+pointer	cv				# Curfit pointer
+double	x[npts]				# Independent variable
+double	y[npts]				# Dependent variable
+double	wts[npts]			# Weights
+double	ebw[npts]			# Half the error bar width
+int	npts				# Number of points
+
+pointer	xout, yout
+int	nvalues
+errchk	malloc
+
+begin
+	call malloc (xout, npts, TY_DOUBLE)
+	call malloc (yout, npts, TY_DOUBLE)
+
+	call icg_axesd (ic, gt, cv, 1, x, y, Memd[xout], npts)
+	call icg_axesd (ic, gt, cv, 2, x, y, Memd[yout], npts)
+	call icg_paramsd (ic, cv, x, y, wts, npts, gt)
+	
+	call icg_g1d (ic, gp, gt, Memd[xout], Memd[yout], wts, ebw, npts)
+
+	if (npts != IC_NFIT(ic)) {
+	    if ((abs (IC_NAVERAGE(ic)) > 1) || (IC_NREJECT(ic) > 0)) {
+	        call realloc (xout, IC_NFIT(ic), TY_DOUBLE)
+		call realloc (yout, IC_NFIT(ic), TY_DOUBLE)
+		call icg_axesd (ic, gt, cv, 1, Memd[IC_XFIT(ic)],
+		    Memd[IC_YFIT(ic)], Memd[xout], IC_NFIT(ic))
+		call icg_axesd (ic, gt, cv, 2, Memd[IC_XFIT(ic)],
+		    Memd[IC_YFIT(ic)], Memd[yout], IC_NFIT(ic))
+		call icg_g2d (ic, gp, gt, Memd[xout], Memd[yout],
+		    IC_NFIT(ic))
+	    }
+
+	} else if (IC_NREJECT(ic) > 0)
+	    call icg_g2d (ic, gp, gt, Memd[xout], Memd[yout], npts)
+
+	nvalues = NVALS_FIT
+	call icg_gfd (ic, gp, gt, cv, nvalues)
+
+	# Mark the the sample regions.
+	call icg_sampled (ic, gp, gt, x, npts, 1)
+
+	call mfree (xout, TY_DOUBLE)
+	call mfree (yout, TY_DOUBLE)
+end
+
+
+# ICG_G1D -- Plot data vector.
+
+procedure icg_g1d (ic, gp, gt, x, y, wts, ebw, npts)
+
+pointer	ic		# Pointer to ic structure
+pointer	gp		# Pointer to graphics stream
+pointer	gt		# Pointer to gtools structure
+double	x[npts]		# Array of independent variables
+double	y[npts]		# Array of dependent variables
+double	wts[npts]	# Array of weights
+double	ebw[npts]	# Error bar half width in WCS (positive density)
+int	npts		# Number of points
+
+pointer	sp, xr, yr, sz, szmk, gt1, gt2
+char	tplot[SZ_TPLOT]
+int	i, xaxis, yaxis, symbols[3], markplot
+real	size, rmin, rmax, big
+bool	fp_equald(), streq(), fp_equalr()
+int	strncmp()
+data	symbols/GM_PLUS, GM_BOX, GM_CIRCLE/
+include	"hdic.com"
+
+begin
+	call smark (sp)
+	call salloc (xr,   npts, TY_REAL)
+	call salloc (yr,   npts, TY_REAL)
+	call salloc (sz,   npts, TY_REAL)
+	call salloc (szmk, npts, TY_REAL)
+
+	call achtdr (x, Memr[xr], npts)
+	call achtdr (y, Memr[yr], npts)
+
+	xaxis = (IC_AXES (ic, IC_GKEY(ic), 1))
+	yaxis = (IC_AXES (ic, IC_GKEY(ic), 2))
+
+	# Set up gtools structure for deleted (gt1) and added (gt2) points
+	call gt_copy (gt, gt1)
+	call gt_setr (gt1, GTXSIZE, MSIZE)
+	call gt_setr (gt1, GTYSIZE, MSIZE)
+	call gt_sets (gt1, GTMARK,  "cross")
+
+	call gt_copy (gt, gt2)
+	call gt_setr (gt2, GTXSIZE, MSIZE)
+	call gt_setr (gt2, GTYSIZE, MSIZE)
+	call gt_sets (gt2, GTMARK,  "circle")
+
+	markplot = NO
+	call gt_gets (gt, GTTYPE, tplot, SZ_TPLOT)
+	if (strncmp (tplot, "mark", 4) == 0)
+	    markplot = YES
+
+	if (IC_OVERPLOT(ic) == NO) {
+	    # Start a new plot
+	    call gclear (gp)
+
+	    # Set the graph scale and axes
+	    call gascale (gp, Memr[xr], npts, 1)
+	    call gascale (gp, Memr[yr], npts, 2)
+
+	    # If plotting HD curve, set wy2 to maxden, which may have
+	    # been updated if a new endpoint was added.
+
+	    if (xaxis == 'y' && yaxis == 'u')
+		call gswind (gp, INDEF, INDEF, INDEF, real (maxden))
+
+	    call gt_swind (gp, gt)
+	    call gt_labax (gp, gt)
+	}
+
+	# Calculate size of markers if error bars are being used.  If the
+	# weights are being used as the marker size, they are first scaled
+	# between 1.0 and the maximum marker size.
+
+	call gt_gets (gt, GTMARK, tplot, SZ_TPLOT)
+	if (streq (tplot, "hebar") || streq (tplot, "vebar")) {
+	    if (IC_EBARS(ic) == EB_WTS) {
+		call achtdr (wts, Memr[sz], npts)
+		call alimr  (Memr[sz], npts, rmin, rmax)
+		if (fp_equalr (rmin, rmax))
+		    call amovr (Memr[sz], Memr[szmk], npts)
+		else {
+		    big = real  (MAX_SZMARKER)
+		    call amapr  (Memr[sz], Memr[szmk], npts,rmin,rmax,1.0, big)
+		}
+	    } else {
+		call achtdr (ebw, Memr[sz], npts)
+		call hd_szmk (gp, gt, xaxis, yaxis, tplot, Memr[sz], 
+		    Memr[szmk], npts)
+	    }
+	} else
+	    call amovkr (MSIZE, Memr[szmk], npts)
+
+	do i = 1, npts {
+	    # Check for deleted point
+	    if (fp_equald (wts[i], 0.0D0))
+	        call gt_plot (gp, gt1, Memr[xr+i-1], Memr[yr+i-1], 1)
+
+	    # Check for added point
+	    else if (fp_equald (ebw[i], ADDED_PT))
+	        call gt_plot (gp, gt2, Memr[xr+i-1], Memr[yr+i-1], 1)
+
+	    else {
+	        size = Memr[szmk+i-1]
+	        call gt_setr (gt, GTXSIZE, size)
+	        call gt_setr (gt, GTYSIZE, size)
+                call gt_plot (gp, gt, Memr[xr+i-1], Memr[yr+i-1], 1)
+	    }
+	}
+	
+	IC_OVERPLOT(ic) = NO
+	call sfree (sp)
+end
+
+
+# HD_SZMK -- Calculate size of error bar markers.  This procedure is
+# called when the marker type is hebar or vebar and the marker size is
+# to be the error in the point, not its weight in the fit.
+
+procedure hd_szmk (gp, gt, xaxis, yaxis, mark, insz, outsz, npts)
+
+pointer	gp			# Pointer to gio structure
+pointer	gt			# Pointer to gtools structure
+int	xaxis, yaxis		# Codes for x and y axis types
+char	mark[SZ_TPLOT]		# Type of marker to use
+real	insz[npts]		# Standard deviations in WCS units
+real	outsz[npts]		# Output size array in NDC units
+int	npts			# Number of points in arrays
+
+int	gt_geti()
+char	tplot[SZ_TPLOT]
+real	dx, dy
+bool	streq()
+
+begin
+	# Check validity of axis types
+	if (xaxis != 'x' && xaxis != 'u' && yaxis != 'x' && yaxis != 'u') {
+	    call eprintf ("Choose graph type with axes 'u' or 'x'; ")
+	    call eprintf ("Using marker size 2.0\n")
+	    call amovkr (MSIZE, outsz, npts)
+	    return
+	}
+
+	call gt_gets (gt, GTMARK, tplot, SZ_TPLOT)
+	if (streq (tplot, "hebar")) {
+	    if (yaxis == 'x' || yaxis == 'u') {
+	        call gt_sets (gt, GTMARK, "vebar")
+	        call eprintf ("Marker switched to vebar\n")
+		# call flush (STDOUT)
+	    }
+	} else if (streq (tplot, "vebar")) {
+	    if (xaxis == 'x' || xaxis == 'u') {
+	        call gt_sets (gt, GTMARK, "hebar")
+	        call eprintf ("Marker switched to hebar\n")
+		# call flush (STDOUT)
+	    }
+	}
+
+	# Need to scale standard deviation from density to NDC units
+        call ggscale (gp, 0.0, 0.0, dx, dy)
+	if (gt_geti (gt, GTTRANSPOSE) == NO)
+	    call adivkr (insz, dx, outsz, npts)
+	else
+	    call adivkr (insz, dy, outsz, npts)
+end
+
+
+# ICG_G2D -- Show sample range and rejected data on plot.
+
+procedure icg_g2d (ic, gp, gt, x, y, npts)
+
+pointer	ic			# ICFIT pointer
+pointer	gp			# GIO pointer
+pointer	gt			# GTOOLS pointer
+double	x[npts], y[npts]	# Data points
+int	npts			# Number of data points
+
+int	i
+pointer	sp, xr, yr, gt1
+
+begin
+	call smark (sp)
+	call salloc (xr, npts, TY_REAL)
+	call salloc (yr, npts, TY_REAL)
+	call achtdr (x, Memr[xr], npts)
+	call achtdr (y, Memr[yr], npts)
+
+	call gt_copy (gt, gt1)
+	call gt_sets (gt1, GTTYPE, "mark")
+
+	# Mark the sample points.
+
+	if (abs (IC_NAVERAGE(ic)) > 1) {
+	    call gt_sets (gt1, GTMARK, "plus")
+	    call gt_setr (gt1, GTXSIZE, real (-abs (IC_NAVERAGE(ic))))
+	    call gt_setr (gt1, GTYSIZE, 1.)
+	    call gt_plot (gp, gt1, Memr[xr], Memr[yr], npts)
+	}
+
+	# Mark the rejected points.
+
+	if (IC_NREJECT(ic) > 0) {
+	    call gt_sets (gt1, GTMARK, "diamond")
+	    call gt_setr (gt1, GTXSIZE, MSIZE)
+	    call gt_setr (gt1, GTYSIZE, MSIZE)
+	    do i = 1, npts {
+		if (Memi[IC_REJPTS(ic)+i-1] == YES)
+	            call gt_plot (gp, gt1, Memr[xr+i-1], Memr[yr+i-1], 1)
+	    }
+	}
+
+	call gt_free (gt1)
+	call sfree (sp)
+end
+
+
+# ICG_GF[RD] -- Overplot the fit on a graph of the data points.  A vector
+# is constructed and evaluated, then plotted.
+
+procedure icg_gfd (ic, gp, gt, cv, npts)
+
+pointer	ic			# ICFIT pointer
+pointer	gp			# GIO pointer
+pointer	gt			# GTOOL pointer
+pointer	cv			# CURFIT pointer
+int	npts			# Number of points to plot
+
+pointer	sp, xr, yr, x, y, xo, yo, gt1
+int	gstati()
+
+begin
+	call smark (sp)
+
+	if (IC_FITERROR(ic) == YES)
+	    return
+
+	call salloc (xr, npts, TY_REAL)
+	call salloc (yr, npts, TY_REAL)
+	call salloc (x,  npts, TY_DOUBLE)
+	call salloc (y,  npts, TY_DOUBLE)
+	call salloc (xo, npts, TY_DOUBLE)
+	call salloc (yo, npts, TY_DOUBLE)
+
+	# Calculate big vector of independent variable values.  Note value
+	# of npts can change with this call.
+	call hdic_gvec (ic, Memd[x], npts, IC_TRANSFORM(ic))
+
+	# Calculate vector of fit values. 
+	call dcvvector (cv, Memd[x], Memd[y], npts)
+
+	# Convert to user function or transpose axes.  Change type to reals
+	# for plotting.
+	call icg_axesd (ic, gt, cv, 1, Memd[x], Memd[y], Memd[xo], npts)
+	call icg_axesd (ic, gt, cv, 2, Memd[x], Memd[y], Memd[yo], npts)
+	call achtdr (Memd[xo], Memr[xr], npts)
+	call achtdr (Memd[yo], Memr[yr], npts)
+
+	call gt_copy (gt, gt1)
+	call gt_sets (gt1, GTTYPE, "line")
+	call gt_seti (gt1, GTLINE, gstati (gp, G_PLTYPE))
+	call gt_plot (gp, gt1, Memr[xr], Memr[yr], npts)
+	call gt_free (gt1)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicgnearest.x b/noao/imred/dtoi/hdicfit/hdicgnearest.x
new file mode 100644
index 00000000..8d556273
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicgnearest.x
@@ -0,0 +1,72 @@
+include	<mach.h>
+include	<pkg/gtools.h>
+
+# ICG_NEAREST -- Find the nearest point to the cursor and return the index.
+# The nearest point to the cursor in NDC coordinates is determined.
+# The cursor is moved to the nearest point selected.
+
+int procedure icg_nearestd (ic, gp, gt, cv, x, y, npts, wx, wy)
+
+pointer	ic					# ICFIT pointer
+pointer	gp					# GIO pointer
+pointer	gt					# GTOOLS pointer
+pointer	cv					# CURFIT pointer
+double	x[npts], y[npts]			# Data points
+int	npts					# Number of points
+real	wx, wy					# Cursor position
+
+int	pt
+pointer	sp, xout, yout
+int	icg_nd(), gt_geti()
+
+begin
+	call smark (sp)
+	call salloc (xout, npts, TY_DOUBLE)
+	call salloc (yout, npts, TY_DOUBLE)
+
+	call icg_axesd (ic, gt, cv, 1, x, y, Memd[xout], npts)
+	call icg_axesd (ic, gt, cv, 2, x, y, Memd[yout], npts)
+
+	if (gt_geti (gt, GTTRANSPOSE) == NO)
+	    pt = icg_nd (gp, Memd[xout], Memd[yout], npts, wx, wy)
+	else
+	    pt = icg_nd (gp, Memd[yout], Memd[xout], npts, wy, wx)
+	call sfree (sp)
+	
+	return (pt)
+end
+
+
+# ICG_ND -- ??
+
+int procedure icg_nd (gp, x, y, npts, wx, wy)
+
+pointer	gp					# GIO pointer
+double	x[npts], y[npts]			# Data points
+int	npts					# Number of points
+real	wx, wy					# Cursor position
+
+int	i, j
+real	x0, y0, r2, r2min
+
+begin
+	# Transform world cursor coordinates to NDC.
+	call gctran (gp, wx, wy, wx, wy, 1, 0)
+
+	# Search for nearest point.
+	r2min = MAX_REAL
+	do i = 1, npts {
+	    call gctran (gp, real (x[i]), real (y[i]), x0, y0, 1, 0)
+	    r2 = (x0 - wx) ** 2 + (y0 - wy) ** 2
+	    if (r2 < r2min) {
+		r2min = r2
+		j = i
+	    }
+	}
+
+	# Move the cursor to the selected point and return the index.
+	if (j != 0)
+	    call gscur (gp, real (x[j]), real (y[j]))
+
+	return (j)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicgparams.x b/noao/imred/dtoi/hdicfit/hdicgparams.x
new file mode 100644
index 00000000..e502fba1
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicgparams.x
@@ -0,0 +1,94 @@
+include	<pkg/gtools.h>
+include	"hdicfit.h"
+
+# ICG_PARAMS -- Set parameter string.
+
+procedure icg_paramsd (ic, cv, x, y, wts, npts, gt)
+
+pointer	ic		# ICFIT pointer
+pointer	cv		# Curfit pointer
+double	x[ARB]		# Ordinates
+double	y[ARB]		# Abscissas
+double	wts[ARB]	# Weights
+int	npts		# Number of data points
+pointer	gt		# GTOOLS pointer
+
+double	rms
+int	i, n, deleted
+pointer	sp, fit, wts1, str, params
+double	ic_rmsd()
+
+begin
+	call smark (sp)
+
+	if (npts == IC_NFIT(ic)) {
+	    # Allocate memory for the fit.
+	    n = npts
+	    call salloc (fit, n, TY_DOUBLE)
+	    call salloc (wts1, n, TY_DOUBLE)
+
+	    # Eliminate rejected points and count deleted points.
+	    call amovd (wts, Memd[wts1], n)
+	    if (IC_NREJECT(ic) > 0) {
+		do i = 1, npts {
+		    if (Memi[IC_REJPTS(ic)+i-1] == YES)
+			Memd[wts1+i-1] = 0.
+		}
+	    }
+	    deleted = 0
+	    do i = 1, n {
+		if (wts[i] == 0.)
+		    deleted = deleted + 1
+	    }
+
+	    # Set the fit and compute the RMS error.
+	    call dcvvector (cv, x, Memd[fit], n)
+	    rms = ic_rmsd (x, y, Memd[fit], Memd[wts1], n)
+
+	} else {
+	    # Allocate memory for the fit.
+	    n = IC_NFIT(ic)
+	    call salloc (fit, n, TY_DOUBLE)
+	    call salloc (wts1, n, TY_DOUBLE)
+
+	    # Eliminate rejected points and count deleted points.
+	    call amovd (Memd[IC_WTSFIT(ic)], Memd[wts1], n)
+	    if (IC_NREJECT(ic) > 0) {
+	        do i = 1, npts {
+		    if (Memi[IC_REJPTS(ic)+i-1] == YES)
+			Memd[wts1+i-1] = 0.
+		}
+	    }
+	    deleted = 0
+	    do i = 1, n {
+		if (wts[i] == 0.)
+		    deleted = deleted + 1
+	    }
+
+	    # Set the fit and compute the rms error.
+	    call dcvvector (cv, Memd[IC_XFIT(ic)], Memd[fit], n)
+	    rms = ic_rmsd (Memd[IC_XFIT(ic)], Memd[IC_YFIT(ic)], Memd[fit],
+		Memd[wts1], n)
+	}
+
+	# Print the parameters and errors.
+	call salloc (str, SZ_LINE, TY_CHAR)
+	call salloc (params, 2*SZ_LINE, TY_CHAR)
+
+	call sprintf (Memc[str],SZ_LINE, "function=%s, order=%d, transform=%s")
+	    call ic_gstr (ic, "function", Memc[params], 2*SZ_LINE)
+	    call pargstr (Memc[params])
+	    call pargi (IC_ORDER(ic))
+	    call ic_gstr (ic, "transform", Memc[params], SZ_LINE)
+	    call pargstr (Memc[params])
+	call sprintf (Memc[params], 2*SZ_LINE,
+            "%s\nfog=%.5f,  total=%d, deleted=%d, RMS=%7.4g")
+	    call pargstr (Memc[str])
+	    call pargr (IC_FOG(ic))
+	    call pargi (npts)
+	    call pargi (deleted)
+	    call pargd (rms)
+	call gt_sets (gt, GTPARAMS, Memc[params])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicgredraw.x b/noao/imred/dtoi/hdicfit/hdicgredraw.x
new file mode 100644
index 00000000..d42a0740
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicgredraw.x
@@ -0,0 +1,22 @@
+include	<gset.h>
+
+define	MSIZE	2.0
+
+# HD_REDRAW -- Redraw a data point.  The old position marker is erased,
+# the new marker drawn, and the cursor moved to the new location.
+
+procedure hd_redraw (gp, oldx, oldy, newx, newy)
+
+pointer	gp		# Pointer to graphics stream
+real	oldx		# Old x coordinate
+real	oldy		# Old y coordinate
+real	newx		# New x coordinate
+real	newy		# New y coordinate
+
+begin
+	call gseti (gp, G_PMLTYPE, GL_CLEAR)
+	call gmark (gp, oldx, oldy, GM_PLUS, MSIZE, MSIZE)
+	call gseti (gp, G_PMLTYPE, GL_SOLID)
+	call gmark (gp, newx, newy, GM_PLUS, MSIZE, MSIZE)
+	call gscur (gp, newx, newy)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicgsample.x b/noao/imred/dtoi/hdicfit/hdicgsample.x
new file mode 100644
index 00000000..12eef158
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicgsample.x
@@ -0,0 +1,84 @@
+include	<gset.h>
+include	<pkg/rg.h>
+include	<pkg/gtools.h>
+include	"hdicfit.h"
+
+# ICG_SAMPLE -- Mark sample.
+
+procedure icg_sampled (ic, gp, gt, x, npts, pltype)
+
+pointer	ic				# ICFIT pointer
+pointer	gp				# GIO pointer
+pointer	gt				# GTOOLS pointer
+double	x[npts]				# Ordinates of graph
+int	npts				# Number of data points
+int	pltype				# Plot line type
+
+pointer	rg
+int	i, axis, pltype1
+real	xl, xr, yb, yt, dy
+real	x1, x2, y1, y2, y3
+
+int	gstati(), stridxs(), gt_geti()
+pointer	rg_xrangesd()
+
+begin
+	if (stridxs ("*", Memc[IC_SAMPLE(ic)]) > 0)
+	    return
+
+	# Find axis along which the independent data is plotted.
+	if (IC_AXES(ic,IC_GKEY(ic),1) == 'x')
+	    axis = 1
+	else if (IC_AXES(ic,IC_GKEY(ic),2) == 'x')
+	    axis = 2
+	else
+	    return
+
+	if (gt_geti (gt, GTTRANSPOSE) == YES)
+	    axis = mod (axis, 2) + 1
+
+	pltype1 = gstati (gp, G_PLTYPE)
+	call gseti (gp, G_PLTYPE, pltype)
+	rg = rg_xrangesd (Memc[IC_SAMPLE(ic)], x, npts)
+
+	switch (axis) {
+	case 1:
+	    call ggwind (gp, xl, xr, yb, yt)
+
+	    dy = yt - yb
+	    y1 = yb + dy / 100
+	    y2 = y1 + dy / 20
+	    y3 = (y1 + y2) / 2
+
+	    do i = 1, RG_NRGS(rg) {
+	        x1 = x[RG_X1(rg, i)]
+	        x2 = x[RG_X2(rg, i)]
+	        if ((x1 > xl) && (x1 < xr))
+	            call gline (gp, x1, y1, x1, y2)
+	        if ((x2 > xl) && (x2 < xr))
+	            call gline (gp, x2, y1, x2, y2)
+	        call gline (gp, x1, y3, x2, y3)
+	    }
+	case 2:
+	    call ggwind (gp, yb, yt, xl, xr)
+
+	    dy = yt - yb
+	    y1 = yb + dy / 100
+	    y2 = y1 + dy / 20
+	    y3 = (y1 + y2) / 2
+
+	    do i = 1, RG_NRGS(rg) {
+	        x1 = x[RG_X1(rg, i)]
+	        x2 = x[RG_X2(rg, i)]
+	        if ((x1 > xl) && (x1 < xr))
+	            call gline (gp, y1, x1, y2, x1)
+	        if ((x2 > xl) && (x2 < xr))
+	            call gline (gp, y1, x2, y2, x2)
+	        call gline (gp, y3, x1, y3, x2)
+	    }
+	}
+
+	call gseti (gp, G_PLTYPE, pltype1)
+	call rg_free (rg)
+end
+
diff --git a/noao/imred/dtoi/hdicfit/hdicguaxes.x b/noao/imred/dtoi/hdicfit/hdicguaxes.x
new file mode 100644
index 00000000..f8199c87
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicguaxes.x
@@ -0,0 +1,38 @@
+include	"hdicfit.h"
+
+# ICG_UAXIS -- Set user axis.
+
+procedure icg_uaxesd (ic, key, cv, x, y, z, npts, label, units, maxchars)
+
+pointer	ic				# Pointer to ic structure
+int	key				# Key for axes
+pointer	cv				# CURFIT pointer
+double	x[npts]				# Independent variable
+double	y[npts]				# Dependent variable
+double	z[npts]				# Output values
+int	npts				# Number of points
+char	label[maxchars]			# Axis label
+char	units[maxchars]			# Units for axis
+int	maxchars			# Maximum chars in label
+
+int	offset
+double	fog
+real	ic_getr()
+include	"hdic.com"
+
+begin
+	# Axis type 'u' returns the untransformed independent variable
+	# in the z array.  That is, the original density values after
+	# subtracting the current fog value.  Some density values could be
+	# below fog were excluded from the transformed vector. 
+
+	call strcpy ("Density above fog", label, maxchars)
+	fog = double (ic_getr (ic, "fog"))
+
+	if (npts == nraw)
+	    call asubkd (Memd[den], fog, z, npts)
+	else {
+	    offset = big_den + (NVALS_FIT - npts)
+	    call asubkd (Memd[offset], fog, z, npts)
+	}
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicgundel.x b/noao/imred/dtoi/hdicfit/hdicgundel.x
new file mode 100644
index 00000000..9a7c68a4
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicgundel.x
@@ -0,0 +1,87 @@
+include	<gset.h>
+include	<mach.h>
+include	<pkg/gtools.h>
+include	"hdicfit.h"
+
+define	MSIZE		2.		# Mark size
+
+# ICG_UNDELETE -- Undelete data point nearest the cursor.
+# The nearest point to the cursor in NDC coordinates is determined.
+
+procedure icg_undeleted (ic, gp, gt, cv, x, y, wts, userwts, npts, wx, wy)
+
+pointer	ic					# ICFIT pointer
+pointer	gp					# GIO pointer
+pointer	gt					# GTOOLS pointer
+pointer	cv					# CURFIT pointer
+double	x[npts], y[npts]			# Data points
+double	wts[npts], userwts[npts]		# Weight arrays
+int	npts					# Number of points
+real	wx, wy					# Position to be nearest
+
+pointer	sp, xout, yout
+int	gt_geti()
+
+begin
+	call smark (sp)
+	call salloc (xout, npts, TY_DOUBLE)
+	call salloc (yout, npts, TY_DOUBLE)
+
+	call icg_axesd (ic, gt, cv, 1, x, y, Memd[xout], npts)
+	call icg_axesd (ic, gt, cv, 2, x, y, Memd[yout], npts)
+	if (gt_geti (gt, GTTRANSPOSE) == NO) {
+	    call icg_u1d (ic, gp, Memd[xout], Memd[yout], wts, userwts,
+		npts, wx, wy)
+	} else {
+	    call icg_u1d (ic, gp, Memd[yout], Memd[xout], wts, userwts,
+		npts, wy, wx)
+	}
+
+	call sfree (sp)
+end
+
+
+# ICG_U1D -- Do the actual undelete.
+
+procedure icg_u1d (ic, gp, x, y, wts, userwts, npts, wx, wy)
+
+pointer	ic					# ICFIT pointer
+pointer	gp					# GIO pointer
+double	x[npts], y[npts]			# Data points
+double	wts[npts], userwts[npts]		# Weight arrays
+int	npts					# Number of points
+real	wx, wy					# Position to be nearest
+
+int	i, j
+real	x0, y0, r2, r2min
+
+begin
+	# Transform world cursor coordinates to NDC.
+	call gctran (gp, wx, wy, wx, wy, 1, 0)
+
+	# Search for nearest point to a point with zero weight.
+	r2min = MAX_REAL
+	do i = 1, npts {
+	    if (wts[i] != 0.)
+		next
+
+	    call gctran (gp, real (x[i]), real (y[i]), x0, y0, 1, 0)
+
+	    r2 = (x0 - wx) ** 2 + (y0 - wy) ** 2
+	    if (r2 < r2min) {
+		r2min = r2
+		j = i
+	    }
+	}
+
+	# Unmark the deleted point and reset the weight.
+	if (j != 0) {
+	    call gscur (gp, real (x[j]), real (y[j]))
+	    call gseti (gp, G_PMLTYPE, GL_CLEAR)
+	    call gmark (gp, real (x[j]), real (y[j]), GM_CROSS, MSIZE, MSIZE)
+	    call gseti (gp, G_PMLTYPE, GL_SOLID)
+	    call gmark (gp, real (x[j]), real (y[j]), GM_PLUS, MSIZE, MSIZE)
+	    wts[j] = userwts[j]
+	    IC_NEWWTS(ic) = YES
+	}
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicguser.x b/noao/imred/dtoi/hdicfit/hdicguser.x
new file mode 100644
index 00000000..5e070537
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicguser.x
@@ -0,0 +1,17 @@
+# ICG_USER -- User default action
+
+procedure icg_user (ic, gp, gt, cv, wx, wy, wcs, key, cmd)
+
+pointer	ic			# ICFIT pointer
+pointer	gp			# GIO pointer
+pointer	gt			# GTOOLS pointer
+pointer	cv			# CURFIT pointer
+real	wx, wy			# Cursor positions
+int	wcs			# GIO WCS
+int	key			# Cursor key
+char	cmd[ARB]		# Cursor command
+
+begin
+	# Ring bell
+	call printf ("\07")
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicgvec.x b/noao/imred/dtoi/hdicfit/hdicgvec.x
new file mode 100644
index 00000000..81909cb8
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicgvec.x
@@ -0,0 +1,74 @@
+include	<mach.h>
+include	"hdicfit.h"
+
+# HDIC_GVEC -- Get a vector of data to be plotted.  The raw density
+# values are stored in common.  From these values, all possible transforms
+# can be generated.
+
+procedure hdic_gvec (ic, xout, npts, transform)
+
+pointer	ic		# Pointer to ic structure
+double	xout[npts]	# Output vector
+int	npts		# Desired npoints to output - possibly changed on output
+int	transform	# Integer code for desired type of transform
+
+pointer	sp, bigdenaf
+int	i, j, npts_desired
+double	fog, dval
+real	ic_getr()
+include	"hdic.com"
+
+begin
+	npts_desired = npts
+	if (npts_desired != NVALS_FIT) 
+	    call error (0, "hdicgvec: nvals != NVALS_FIT")
+
+	call smark (sp)
+	call salloc (bigdenaf, npts, TY_DOUBLE)
+
+	j = 1
+
+	fog = double (ic_getr (ic, "fog"))
+	call asubkd (Memd[big_den], fog, Memd[bigdenaf], npts)
+
+	switch (transform) {
+	case HD_NONE:
+	    call amovd (Memd[bigdenaf], xout, NVALS_FIT)
+
+	case HD_LOGO:
+	    do i = 1, npts_desired {
+		dval = Memd[bigdenaf+i-1]
+		if (dval < 0.0D0)
+		    npts = npts - 1
+		else {
+		    xout[j] = log10 ((10.**dval) - 1.0)
+		    j = j + 1
+		}
+	    }
+
+	case HD_K75:
+	    do i = 1, npts_desired {
+		dval = Memd[bigdenaf+i-1]
+		if (dval < 0.0D0)
+		    npts = npts - 1
+		else {
+		    xout[j] = dval + 0.75 * log10 (1.0 - (10.** (-dval)))
+		    j = j + 1
+		}
+	    }
+
+	case HD_K50:
+	    do i = 1, npts_desired {
+		dval = Memd[bigdenaf+i-1]
+		if (dval < 0.0D0)
+		    npts = npts - 1
+		else {
+		    xout[j] = dval + 0.50 * log10 (1.0 - (10.** (-dval)))
+		    j = j + 1
+		}
+	    }
+
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicinit.x b/noao/imred/dtoi/hdicfit/hdicinit.x
new file mode 100644
index 00000000..d9730051
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicinit.x
@@ -0,0 +1,60 @@
+include	<mach.h>
+include	"hdicfit.h"
+
+# HDIC_INIT -- Initialize hdfit/icgfit interface.
+
+procedure hdic_init (density, nvalues, dmax)
+
+double	density[nvalues]	# Reference density above fog values
+int	nvalues			# Number of values in sample
+double	dmax			# Maximum possible density
+
+int	i
+pointer	sp, base
+double	xxmax, xxmin, delta_den
+bool	fp_equald()
+include	"hdic.com"
+errchk	malloc
+
+begin
+	call smark (sp)
+
+	if (den == NULL || big_den == NULL) {
+	    call malloc (den, nvalues, TY_DOUBLE)
+	    call malloc (big_den, NVALS_FIT, TY_DOUBLE)
+	} else if (nvalues != nraw) 
+	    call realloc (den, nvalues, TY_DOUBLE)
+
+	nraw = nvalues
+	call salloc (base, NVALS_FIT, TY_DOUBLE)
+
+	# Copy density array to pointer location
+	call amovd (density, Memd[den], nraw)
+
+	# Calculate big vector of density values.  The points are spaced 
+	# linear in log space, to yield adequate spacing at low density values.
+
+	call alimd (density, nraw, xxmin, xxmax)
+
+	# Put user value for maximum density in common block if it is valid.
+	if (! fp_equald (dmax, 0.0D0))
+	    maxden = dmax
+
+	# Make big_den go all the way to maxden, not just xxmax.  Make sure
+	# the value of xxmin won't cause the log function to blow up.
+
+	if (xxmin > 0.0D0)
+	    ;
+	else
+	    xxmin = 2.0 * EPSILOND
+
+	delta_den = (log10 (maxden) - log10 (xxmin)) / double (NVALS_FIT - 1)
+
+	do i = 1, NVALS_FIT
+	    Memd[big_den+i-1] = log10 (xxmin) + double (i-1) * delta_den
+
+	call amovkd (10.0D0, Memd[base], NVALS_FIT)
+	call aexpd (Memd[base], Memd[big_den], Memd[big_den], NVALS_FIT)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicparams.x b/noao/imred/dtoi/hdicfit/hdicparams.x
new file mode 100644
index 00000000..1840dccd
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicparams.x
@@ -0,0 +1,323 @@
+include "hdicfit.h"
+
+define	FUNCTIONS	"|chebyshev|legendre|spline3|spline1|power|"
+define	TRANSFORMS	"|none|logopacitance|k50|k75|"
+
+# IC_OPEN -- Open ICFIT parameter structure.
+
+procedure ic_open (ic)
+
+pointer	ic		# ICFIT pointer
+errchk	malloc
+
+begin
+	# Allocate memory for the package parameter structure.
+	call malloc (ic, IC_LENSTRUCT, TY_STRUCT)
+	call malloc (IC_SAMPLE(ic), SZ_LINE, TY_CHAR)
+	call malloc (IC_LABELS(ic,1), SZ_LINE, TY_CHAR)
+	call malloc (IC_LABELS(ic,2), SZ_LINE, TY_CHAR)
+	call malloc (IC_UNITS(ic,1), SZ_LINE, TY_CHAR)
+	call malloc (IC_UNITS(ic,2), SZ_LINE, TY_CHAR)
+
+	# Set defaults.
+	call ic_pstr (ic, "function", "spline3")
+	call ic_puti (ic, "order", 1)
+	call ic_pstr (ic, "sample", "*")
+	call ic_puti (ic, "naverage", 1)
+	call ic_puti (ic, "niterate", 0)
+	call ic_putr (ic, "low", 0.)
+	call ic_putr (ic, "high", 0.)
+	call ic_putr (ic, "grow", 0.)
+	call ic_pstr (ic, "xlabel", "X")
+	call ic_pstr (ic, "ylabel", "Y")
+	call ic_pstr (ic, "xunits", "")
+	call ic_pstr (ic, "yunits", "")
+	call ic_puti (ic, "key", 1)
+	call ic_pkey (ic, 1, 'x', 'y')
+	call ic_pkey (ic, 2, 'y', 'x')
+	call ic_pkey (ic, 3, 'x', 'r')
+	call ic_pkey (ic, 4, 'x', 'd')
+	call ic_pkey (ic, 5, 'x', 'n')
+
+	# Initialize other parameters
+	IC_RG(ic) = NULL
+	IC_XFIT(ic) = NULL
+	IC_YFIT(ic) = NULL
+	IC_WTSFIT(ic) = NULL
+	IC_REJPTS(ic) = NULL
+end
+
+
+# IC_CLOSER -- Close ICFIT parameter structure.
+
+procedure ic_closer (ic)
+
+pointer	ic		# ICFIT pointer
+
+begin
+	# Free memory for the package parameter structure.
+	call rg_free (IC_RG(ic))
+	call mfree (IC_XFIT(ic), TY_REAL)
+	call mfree (IC_YFIT(ic), TY_REAL)
+	call mfree (IC_WTSFIT(ic), TY_REAL)
+	call mfree (IC_REJPTS(ic), TY_INT)
+	call mfree (IC_SAMPLE(ic), TY_CHAR)
+	call mfree (IC_LABELS(ic,1), TY_CHAR)
+	call mfree (IC_LABELS(ic,2), TY_CHAR)
+	call mfree (IC_UNITS(ic,1), TY_CHAR)
+	call mfree (IC_UNITS(ic,2), TY_CHAR)
+	call mfree (ic, TY_STRUCT)
+end
+
+
+# IC_CLOSED -- Close ICFIT parameter structure.
+
+procedure ic_closed (ic)
+
+pointer	ic		# ICFIT pointer
+
+begin
+	# Free memory for the package parameter structure.
+	call rg_free (IC_RG(ic))
+	call mfree (IC_XFIT(ic), TY_DOUBLE)
+	call mfree (IC_YFIT(ic), TY_DOUBLE)
+	call mfree (IC_WTSFIT(ic), TY_DOUBLE)
+	call mfree (IC_REJPTS(ic), TY_INT)
+	call mfree (IC_SAMPLE(ic), TY_CHAR)
+	call mfree (IC_LABELS(ic,1), TY_CHAR)
+	call mfree (IC_LABELS(ic,2), TY_CHAR)
+	call mfree (IC_UNITS(ic,1), TY_CHAR)
+	call mfree (IC_UNITS(ic,2), TY_CHAR)
+	call mfree (ic, TY_STRUCT)
+end
+
+
+# IC_PSTR -- Put string valued parameters.
+
+procedure ic_pstr (ic, param, str)
+
+pointer	ic			# ICFIT pointer
+char	param[ARB]		# Parameter to be put
+char	str[ARB]		# String value
+
+int	i
+pointer	ptr
+int	strdic()
+bool	streq()
+
+begin
+	if (streq (param, "sample"))
+	    call strcpy (str, Memc[IC_SAMPLE(ic)], SZ_LINE)
+	else if (streq (param, "function")) {
+	    call malloc (ptr, SZ_LINE, TY_CHAR)
+	    i = strdic (str, Memc[ptr], SZ_LINE, FUNCTIONS)
+	    if (i > 0)
+		IC_FUNCTION(ic) = i
+	    call mfree (ptr, TY_CHAR)
+	} else if (streq (param, "transform")) {
+	    call malloc (ptr, SZ_LINE, TY_CHAR)
+	    i = strdic (str, Memc[ptr], SZ_LINE, TRANSFORMS)
+	    if (i > 0)
+		IC_TRANSFORM(ic) = i
+	    call mfree (ptr, TY_CHAR)
+	} else if (streq (param, "xlabel"))
+	    call strcpy (str, Memc[IC_LABELS(ic,1)], SZ_LINE)
+	else if (streq (param, "ylabel"))
+	    call strcpy (str, Memc[IC_LABELS(ic,2)], SZ_LINE)
+	else if (streq (param, "xunits"))
+	    call strcpy (str, Memc[IC_UNITS(ic,1)], SZ_LINE)
+	else if (streq (param, "yunits"))
+	    call strcpy (str, Memc[IC_UNITS(ic,2)], SZ_LINE)
+	else
+	    call error (0, "ICFIT: Unknown parameter")
+end
+
+
+# IC_PUTI -- Put integer valued parameters.
+
+procedure ic_puti (ic, param, ival)
+
+pointer	ic			# ICFIT pointer
+char	param[ARB]		# Parameter to be put
+int	ival			# Integer value
+
+bool	streq()
+
+begin
+	if (streq (param, "naverage"))
+	    IC_NAVERAGE(ic) = ival
+	else if (streq (param, "order"))
+	    IC_ORDER(ic) = ival
+	else if (streq (param, "niterate"))
+	    IC_NITERATE(ic) = ival
+	else if (streq (param, "key"))
+	    IC_GKEY(ic) = ival
+	else if (streq (param, "transform"))
+	    IC_TRANSFORM(ic) = ival
+	else
+	    call error (0, "ICFIT: Unknown parameter")
+end
+
+
+# IC_PKEY -- Put key parameters.
+# Note the key types must be integers not characters.
+
+procedure ic_pkey (ic, key, xaxis, yaxis)
+
+pointer	ic			# ICFIT pointer
+int	key			# Key to be defined
+int	xaxis			# X axis type
+int	yaxis			# Y axis type
+
+begin
+	IC_AXES(ic, key, 1) = xaxis
+	IC_AXES(ic, key, 2) = yaxis
+end
+
+
+# IC_GKEY -- Get key parameters.
+
+procedure ic_gkey (ic, key, xaxis, yaxis)
+
+pointer	ic			# ICFIT pointer
+int	key			# Key to be gotten
+int	xaxis			# X axis type
+int	yaxis			# Y axis type
+
+begin
+	xaxis = IC_AXES(ic, key, 1)
+	yaxis = IC_AXES(ic, key, 2)
+end
+
+
+# IC_PUTR -- Put real valued parameters.
+
+procedure ic_putr (ic, param, rval)
+
+pointer	ic			# ICFIT pointer
+char	param[ARB]		# Parameter to be put
+real	rval			# Real value
+
+bool	streq()
+
+begin
+	if (streq (param, "xmin"))
+	    IC_XMIN(ic) = rval
+	else if (streq (param, "xmax"))
+	    IC_XMAX(ic) = rval
+	else if (streq (param, "low"))
+	    IC_LOW(ic) = rval
+	else if (streq (param, "high"))
+	    IC_HIGH(ic) = rval
+	else if (streq (param, "grow"))
+	    IC_GROW(ic) = rval
+	else if (streq (param, "fog"))
+	    IC_FOG(ic) = rval
+	else if (streq (param, "rfog"))
+	    IC_RFOG(ic) = rval
+	else
+	    call error (0, "ICFIT: Unknown parameter")
+end
+
+
+# IC_GSTR -- Get string valued parameters.
+
+procedure ic_gstr (ic, param, str, maxchars)
+
+pointer	ic			# ICFIT pointer
+char	param[ARB]		# Parameter to be put
+char	str[maxchars]		# String value
+int	maxchars		# Maximum number of characters
+
+bool	streq()
+
+begin
+	if (streq (param, "sample"))
+	    call strcpy (Memc[IC_SAMPLE(ic)], str, maxchars)
+	else if (streq (param, "xlabel"))
+	    call strcpy (Memc[IC_LABELS(ic,1)], str, maxchars)
+	else if (streq (param, "ylabel"))
+	    call strcpy (Memc[IC_LABELS(ic,2)], str, maxchars)
+	else if (streq (param, "xunits"))
+	    call strcpy (Memc[IC_UNITS(ic,1)], str, maxchars)
+	else if (streq (param, "yunits"))
+	    call strcpy (Memc[IC_UNITS(ic,2)], str, maxchars)
+	else if (streq (param, "function")) {
+	    switch (IC_FUNCTION(ic)) {
+	    case 1:
+		call strcpy ("chebyshev", str, maxchars)
+	    case 2:
+		call strcpy ("legendre", str, maxchars)
+	    case 3:
+		call strcpy ("spline3", str, maxchars)
+	    case 4:
+		call strcpy ("spline1", str, maxchars)
+	    case 5:
+		call strcpy ("power", str, maxchars)
+	    }
+	} else if (streq (param, "transform")) {
+	    switch (IC_TRANSFORM(ic)) {
+	    case 1:
+		call strcpy ("none", str, maxchars)
+	    case 2:
+		call strcpy ("logopacitance", str, maxchars)
+	    case 3:
+		call strcpy ("k50", str, maxchars)
+	    case 4:
+		call strcpy ("k75", str, maxchars)
+	    }
+	} else
+	    call error (0, "ICFIT: Unknown parameter")
+end
+
+
+# IC_GETI -- Get integer valued parameters.
+
+int procedure ic_geti (ic, param)
+
+pointer	ic			# ICFIT pointer
+char	param[ARB]		# Parameter to be gotten
+
+bool	streq()
+
+begin
+	if (streq (param, "naverage"))
+	    return (IC_NAVERAGE(ic))
+	else if (streq (param, "order"))
+	    return (IC_ORDER(ic))
+	else if (streq (param, "niterate"))
+	    return (IC_NITERATE(ic))
+	else if (streq (param, "key"))
+	    return (IC_GKEY(ic))
+	else if (streq (param, "transform"))
+	    return (IC_TRANSFORM(ic))
+
+	call error (0, "ICFIT: Unknown parameter")
+end
+
+
+# IC_GETR -- Get real valued parameters.
+
+real procedure ic_getr (ic, param)
+
+pointer	ic			# ICFIT pointer
+char	param[ARB]		# Parameter to be put
+
+bool	streq()
+
+begin
+	if (streq (param, "xmin"))
+	    return (IC_XMIN(ic))
+	else if (streq (param, "xmax"))
+	    return (IC_XMAX(ic))
+	else if (streq (param, "low"))
+	    return (IC_LOW(ic))
+	else if (streq (param, "high"))
+	    return (IC_HIGH(ic))
+	else if (streq (param, "grow"))
+	    return (IC_GROW(ic))
+	else if (streq (param, "fog"))
+	    return (IC_FOG(ic))
+
+	call error (0, "ICFIT: Unknown parameter")
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicreject.x b/noao/imred/dtoi/hdicfit/hdicreject.x
new file mode 100644
index 00000000..82dd093c
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicreject.x
@@ -0,0 +1,39 @@
+# IC_REJECT -- Reject points with large residuals from the fit.
+#
+# The sigma of the fit residuals is calculated.  The rejection thresholds
+# are set at low_reject*sigma and high_reject*sigma.  Points outside the
+# rejection threshold are rejected from the fit and flagged in the rejpts
+# array.  Finally, the remaining points are refit.
+
+procedure ic_rejectd (cv, x, y, w, rejpts, npts, low_reject, high_reject,
+	niterate, grow, nreject)
+
+pointer	cv				# Curve descriptor
+double	x[npts]				# Input ordinates
+double	y[npts]				# Input data values
+double	w[npts]				# Weights
+int	rejpts[npts]			# Points rejected
+int	npts				# Number of input points
+real	low_reject, high_reject		# Rejection threshold
+int	niterate			# Number of rejection iterations
+real	grow				# Rejection radius
+int	nreject				# Number of points rejected
+
+int	i, newreject
+
+begin
+	# Initialize rejection.
+	nreject = 0
+	call amovki (NO, rejpts, npts)
+
+	if (niterate <= 0)
+	    return
+
+	# Find deviant points.
+	do i = 1, niterate {
+	    call ic_deviantd (cv, x, y, w, rejpts, npts, low_reject,
+		high_reject, grow, YES, nreject, newreject)
+	    if (newreject == 0)
+		break
+	}
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicshow.x b/noao/imred/dtoi/hdicfit/hdicshow.x
new file mode 100644
index 00000000..521f04d3
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicshow.x
@@ -0,0 +1,52 @@
+include	<pkg/gtools.h>
+include	"hdicfit.h"
+
+# IC_SHOW -- Show the values of the parameters.
+
+procedure ic_show (ic, file, gt)
+
+pointer	ic			# ICFIT pointer
+char	file[ARB]		# Output file
+pointer	gt			# GTOOLS pointer
+
+int	fd
+pointer	str
+int	open()
+long	clktime()
+errchk	open, malloc
+
+begin
+	fd = open (file, APPEND, TEXT_FILE)
+	call malloc (str, SZ_LINE, TY_CHAR)
+
+	call cnvtime (clktime(0), Memc[str], SZ_LINE)
+	call fprintf (fd, "\n# %s\n")
+	    call pargstr (Memc[str])
+
+	call gt_gets (gt, GTTITLE, Memc[str], SZ_LINE)
+	call fprintf (fd, "# %s\n")
+	    call pargstr (Memc[str])
+
+	call gt_gets (gt, GTYUNITS, Memc[str], SZ_LINE)
+	if (Memc[str] != EOS) {
+	    call fprintf (fd, "fit units = %s\n")
+	        call pargstr (Memc[str])
+	}
+
+	call ic_gstr (ic, "function", Memc[str], SZ_LINE)
+	call fprintf (fd, "function = %s\n")
+	    call pargstr (Memc[str])
+
+	call fprintf (fd, "order = %d\n")
+	    call pargi (IC_ORDER(ic))
+
+	call ic_gstr (ic, "transform", Memc[str], SZ_LINE)
+	call fprintf (fd, "transform = %s\n")
+	    call pargstr (Memc[str])
+
+	call fprintf (fd, "fog = %g\n")
+	    call pargr (IC_FOG(ic))
+
+	call mfree (str, TY_CHAR)
+	call close (fd)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicsort.x b/noao/imred/dtoi/hdicfit/hdicsort.x
new file mode 100644
index 00000000..16d6e0a6
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicsort.x
@@ -0,0 +1,38 @@
+# HDIC_SORT -- sort the log exposure, density and weight information in order
+# of increasing density value.  The sorting is done is place.  The four
+# data values are assummed matched on input, that is, exposure[i] matches
+# density[i] with weight[i] (and userwts[i]) for all array entries.
+
+procedure hdic_sort (density, exposure, weights, userwts, whydel, sdev, nvals)
+
+double	density[nvals]		# Density array
+double	exposure[nvals]		# Log exposure array
+double	weights[nvals]		# Weights array
+double	userwts[nvals]		# Reference weights array
+int	whydel[nvals]		# Flag array of reasons for deletion
+double	sdev[nvals]		# Array of standard deviations
+int	nvals			# Number of values to sort
+
+int	i, j
+double	temp
+define	swap	{temp=$1;$1=$2;$2=temp}
+int	itemp
+define	iswap   {itemp=$1;$1=$2;$2=itemp}
+
+begin
+	# Bubble sort - inefficient, but sorting is done infrequently
+	# an expected small sample size (16 pts typically). 
+
+	for (i = nvals; i > 1; i = i - 1)
+	    for (j = 1; j < i; j = j + 1) 
+		if (density [j] > density[j+1]) {
+
+		    # Out of order; exchange values
+		    swap (exposure[j], exposure[j+1])
+		    swap ( density[j],  density[j+1])
+		    swap ( weights[j],  weights[j+1])
+		    swap ( userwts[j],  userwts[j+1])
+		   iswap (  whydel[j],   whydel[j+1])
+		    swap (    sdev[j],     sdev[j+1])
+		}
+end
diff --git a/noao/imred/dtoi/hdicfit/hdictrans.x b/noao/imred/dtoi/hdicfit/hdictrans.x
new file mode 100644
index 00000000..0ee89037
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdictrans.x
@@ -0,0 +1,155 @@
+include	<mach.h>
+include	"hdicfit.h"
+
+# HDIC_TRANSFORM -- Transform density to independent variable of fit.  The
+# desired transform is stored in the ic structure.  A vector of x values
+# is returned, as is a possibly modified weights array.  The minimum and
+# maximum limits of the fit are updated in the ic structure; the labels
+# are set also when IC_NEWTRANSFORM = YES.  The fog value is subtracted
+# from the input density array and the transform performed. 
+
+procedure hdic_transform (ic, density, userwts, xout, wts, whydel, npts)
+
+pointer	ic		# Pointer to ic structure
+double	density[npts]	# Array of original density values
+double	userwts[npts]	# Array of original weights values
+double	xout[npts]	# Transformed density above fog (returned)
+double	wts[npts]	# Input weights array
+int	whydel[npts]	# Reason for deletion array 
+int	npts		# The number of density points - maybe changed on output
+
+int	i
+pointer	denaf, sp
+double	fog, xxmin, xxmax, dval
+bool	fp_equald()
+real	ic_getr()
+include	"hdic.com"
+
+begin
+	# Allocate space for density above fog array
+	call smark (sp)
+	call salloc (denaf, npts, TY_DOUBLE)
+
+	fog = double (ic_getr (ic, "fog"))
+	call asubkd (density, fog, Memd[denaf], npts)
+
+	switch (IC_TRANSFORM(ic)) {
+	case HD_NONE:
+	    do i = 1, npts {
+		xout[i] = Memd[denaf+i-1]
+		# In every case, if the point was deleted by the program, 
+		# restore it.
+		if (whydel[i] == PDELETE) {
+	            wts[i] = userwts[i]
+		    whydel[i] = NDELETE
+	        }
+	    }
+
+	    call ic_pstr (ic, "xlabel", "Density above Fog")
+	    xxmin = MIN_DEN - fog
+	    xxmax = maxden
+	    call ic_putr (ic, "xmin", real (xxmin))
+	    call ic_putr (ic, "xmax", real (xxmax))
+
+	case HD_LOGO:
+	    call ic_pstr (ic, "xlabel", "Log Opacitance: Log (10**Den - 1)")
+	    xxmin = log10 ((10. ** (MIN_DEN)) - 1.0)
+	    xxmax = log10 ((10. ** (maxden)) - 1.0)
+	    call ic_putr (ic, "xmin", real (xxmin))
+	    call ic_putr (ic, "xmax", real (xxmax))
+
+	    do i = 1, npts {
+		dval = Memd[denaf+i-1]
+		if (dval < 0.0D0 || (fp_equald (dval, 0.0D0))) {
+		    xout[i] = dval
+		    wts[i] = 0.0D0
+		    whydel[i] = PDELETE
+
+		} else {
+		    xout[i] = log10 ((10. ** (dval)) - 1.0)
+
+		    # If point had been deleted, find out why.  It affects the
+		    # weights value returned.  Only if the point was previously
+		    # deleted by the program, restore it; otherwise, leave it 
+		    # alone.
+
+		    if (fp_equald (wts[i], 0.0D0)) {
+		        if (whydel[i] == PDELETE) {
+		            wts[i] = userwts[i]
+			    whydel[i] = NDELETE
+			}
+		    } else
+			wts[i] = userwts[i]
+	    }
+	}
+
+	case HD_K75:
+	    call ic_pstr (ic, "xlabel", "Den + 0.75 * Log (1 - (10 ** -Den))")
+	    xxmin = MIN_DEN + 0.75 * log10 (1.0 - (10. ** (-MIN_DEN)))
+	    xxmax = maxden + 0.75 * log10 (1.0 - (10. ** (-maxden)))
+	    call ic_putr (ic, "xmin", real (xxmin))
+	    call ic_putr (ic, "xmax", real (xxmax))
+
+	    do i = 1, npts {
+		dval = Memd[denaf+i-1]
+		if (dval < 0.0D0 || (fp_equald (dval, 0.0D0))) {
+		    xout[i] = dval
+		    wts[i] = 0.0D0
+		    whydel[i] = PDELETE
+
+		} else {
+		    xout[i] = dval + 0.75 * log10 (1.0 - (10.** (-dval)))
+
+		    # If point had been deleted, find out why.  It affects the
+		    # weights value returned.  Only if the point was previously
+		    # deleted by the program, restore it; otherwise, leave it 
+		    # alone.
+
+		    if (fp_equald (wts[i], 0.0D0)) {
+		        if (wts[i] == PDELETE) {
+		            wts[i] = userwts[i]
+			    whydel[i] = NDELETE
+			}
+		    } else
+			wts[i] = userwts[i]
+	    }
+	}
+
+	case HD_K50:
+	    call ic_pstr (ic, "xlabel", "Den + 0.50 * Log (1 - (10 ** -Den))")
+	    xxmin = MIN_DEN + 0.50 * log10 (1.0 - (10. ** (-MIN_DEN)))
+	    xxmax = maxden + 0.50 * log10 (1.0 - (10. ** (-maxden)))
+	    call ic_putr (ic, "xmin", real (xxmin))
+	    call ic_putr (ic, "xmax", real (xxmax))
+
+	    do i = 1, npts {
+		dval = Memd[denaf+i-1]
+		if (dval < 0.0D0 || (fp_equald (dval, 0.0D0))) {
+		    xout[i] = dval
+		    wts[i] = 0.0D0
+		    whydel[i] = PDELETE
+
+		} else {
+		    xout[i] = dval + 0.50 * log10 (1.0 - (10.** (-dval)))
+
+		    # If point had been deleted, find out why.  It affects the
+		    # weights value returned.  Only if the point was previously
+		    # deleted by the program, restore it; otherwise, leave it 
+		    # alone.
+
+		    if (fp_equald (wts[i], 0.0D0)) {
+		        if (wts[i] == PDELETE) {
+		            wts[i] = userwts[i]
+			    whydel[i] = NDELETE
+			}
+		    } else
+			wts[i] = userwts[i]
+		}
+	    }
+
+	default:
+	    call eprintf ("Unrecognizable Transform\n")
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/dtoi/hdicfit/hdicvshow.x b/noao/imred/dtoi/hdicfit/hdicvshow.x
new file mode 100644
index 00000000..e62f6522
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/hdicvshow.x
@@ -0,0 +1,155 @@
+include	<math/curfit.h>
+include	"hdicfit.h"
+
+# IC_VSHOW -- Show fit parameters in verbose mode.
+
+procedure ic_vshowd (ic, file, cv, x, y, wts, npts, gt)
+
+pointer	ic		# ICFIT pointer
+char	file[ARB]	# Output file
+pointer	cv		# Curfit pointer
+double	x[ARB]		# Ordinates
+double	y[ARB]		# Abscissas
+double	wts[ARB]	# Weights
+int	npts		# Number of data points
+pointer	gt		# Graphics tools pointer
+
+double	chisqr, rms
+int	i, n, deleted, ncoeffs, fd
+pointer	sp, fit, wts1, coeffs, errors
+
+int	dcvstati(), open()
+double	ic_rmsd()
+errchk	open()
+
+begin
+	# Do the standard ic_show option, then add on the verbose part.
+	call ic_show (ic, file, gt)
+
+	if (npts == 0) {
+	    call eprintf ("Incomplete output - no data points for fit\n")
+	    return
+	}
+
+	# Open the output file.
+	fd = open (file, APPEND, TEXT_FILE)
+
+	# Determine the number of coefficients and allocate memory.
+	ncoeffs = dcvstati (cv, CVNCOEFF)
+
+	call smark (sp)
+	call salloc (coeffs, ncoeffs, TY_DOUBLE)
+	call salloc (errors, ncoeffs, TY_DOUBLE)
+
+	if (npts == IC_NFIT(ic)) {
+	    # Allocate memory for the fit.
+	    n = npts
+	    call salloc (fit, n, TY_DOUBLE)
+	    call salloc (wts1, n, TY_DOUBLE)
+
+	    # Eliminate rejected points and count deleted points.
+	    call amovd (wts, Memd[wts1], n)
+	    if (IC_NREJECT(ic) > 0) {
+		do i = 1, npts {
+		    if (Memi[IC_REJPTS(ic)+i-1] == YES)
+			Memd[wts1+i-1] = 0.
+		}
+	    }
+	    deleted = 0
+	    do i = 1, n {
+		if (wts[i] == 0.)
+		    deleted = deleted + 1
+	    }
+
+	    # Get the coefficients and compute the errors.
+	    call dcvvector (cv, x, Memd[fit], n)
+	    call dcvcoeff (cv, Memd[coeffs], ncoeffs)
+	    call dcverrors (cv, y, Memd[wts1], Memd[fit], n, chisqr,
+		Memd[errors])
+	    rms = ic_rmsd (x, y, Memd[fit], Memd[wts1], n)
+
+	} else {
+	    # Allocate memory for the fit.
+	    n = IC_NFIT(ic)
+	    call salloc (fit, n, TY_DOUBLE)
+	    call salloc (wts1, n, TY_DOUBLE)
+
+	    # Eliminate rejected points and count deleted points.
+	    call amovd (Memd[IC_WTSFIT(ic)], Memd[wts1], n)
+	    if (IC_NREJECT(ic) > 0) {
+	        do i = 1, npts {
+		    if (Memi[IC_REJPTS(ic)+i-1] == YES)
+			Memd[wts1+i-1] = 0.
+		}
+	    }
+	    deleted = 0
+	    do i = 1, n {
+		if (wts[i] == 0.)
+		    deleted = deleted + 1
+	    }
+
+	    # Get the coefficients and compute the errors.
+	    call dcvvector (cv, Memd[IC_XFIT(ic)], Memd[fit], n)
+	    rms = ic_rmsd (Memd[IC_XFIT(ic)], Memd[IC_YFIT(ic)],
+		Memd[fit], Memd[wts1], n)
+	    call dcvcoeff (cv, Memd[coeffs], ncoeffs)
+	    call dcverrors (cv, Memd[IC_YFIT(ic)], Memd[wts1], Memd[fit],
+		n, chisqr, Memd[errors])
+	}
+
+	# Print the error analysis.
+	call fprintf (fd, "total points = %d\n")
+	    call pargi (npts)
+	call fprintf (fd, "deleted = %d\n")
+	    call pargi (deleted)
+	call fprintf (fd, "RMS = %7.4g\n")
+	    call pargd (rms)
+	call fprintf (fd, "square root of reduced chi square = %7.4g\n")
+	    call pargd (sqrt (chisqr))
+
+	call fprintf (fd, "# \t  coefficent\t  error\n")
+	do i = 1, ncoeffs {
+	    call fprintf (fd, "\t%10.4e\t%10.4e\n")
+		call pargd (Memd[coeffs+i-1])
+	 	call pargd (Memd[errors+i-1])
+	}
+
+	# Print x,y pairs and weights
+	call ic_listxywd (fd, cv, x, y, wts, npts)
+
+	call sfree (sp)
+	call close (fd)
+end
+
+
+# IC_LISTXYW -- List data as x,y pairs on output with their weights.  Used 
+# for verbose show procedure.  The untransformed density is also output,
+# regardless of what transformation may have been applied.
+
+procedure ic_listxywd (fd, cv, xvals, yvals, weights, nvalues)
+
+int	fd			# File descriptor of output file
+pointer	cv			# Pointer to curfit structure
+int	nvalues			# Number of data values
+double	xvals[nvalues]		# Array of x data values
+double	yvals[nvalues]		# Array of y data values
+double	weights[nvalues]	# Array of weight values
+
+int	i
+double	dcveval()
+include	"hdic.com"
+
+begin
+	call fprintf (fd,"\n#%15t Density %27t X %39t Yfit %51t LogE %63tWts\n")
+
+	do i = 1, nvalues {
+	    call fprintf (fd, 
+	    "%2d %15t%-12.7f%27t%-12.7f%39t%-12.7f%51t%-12.7f%63t%-12.7f\n")
+		call pargi (i)
+		call pargd (Memd[den+i-1])
+		call pargd (xvals[i])
+		call pargd (dcveval (cv, xvals[i]))
+		call pargd (yvals[i])
+		call pargd (weights[i])
+	}
+end
diff --git a/noao/imred/dtoi/hdicfit/mkpkg b/noao/imred/dtoi/hdicfit/mkpkg
new file mode 100644
index 00000000..5fc5031f
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/mkpkg
@@ -0,0 +1,37 @@
+# HDICFIT package.  *** Modified from icgfit package for DTOI applications ***
+
+update:
+	$update libhdic.a
+
+libhdic.a:
+
+	hdicclean.x	hdicfit.h <pkg/rg.h>
+	hdicdeviant.x	<mach.h> <math/curfit.h>
+	hdicdosetup.x	hdicfit.h <math/curfit.h>
+	hdicerrors.x	hdicfit.h <math/curfit.h>
+	hdicfit.x	hdicfit.h <math/curfit.h>
+	hdicgaxes.x	hdicfit.h <pkg/gtools.h>
+	hdicgcolon.x	hdicfit.h <error.h> <gset.h>
+	hdicgdelete.x	hdicfit.h <gset.h> <mach.h> <pkg/gtools.h>
+	hdicgfit.x	hdicfit.h <error.h> <pkg/gtools.h> <mach.h> <gset.h>
+	hdicggraph.x	hdicfit.h hdic.com <gset.h> <pkg/gtools.h> <mach.h>
+	hdicgnearest.x	<mach.h> <pkg/gtools.h>
+	hdicgparams.x	hdicfit.h <pkg/gtools.h>
+	hdicgsample.x	hdicfit.h <gset.h> <pkg/gtools.h> <pkg/rg.h>
+	hdicguaxes.x	hdic.com hdicfit.h
+	hdicgundel.x	hdicfit.h <gset.h> <mach.h> <pkg/gtools.h>
+	hdicguser.x	
+	hdicparams.x	hdicfit.h
+	hdicreject.x	
+	hdicshow.x	hdicfit.h <pkg/gtools.h>
+	hdicvshow.x	hdicfit.h hdic.com <math/curfit.h>
+
+	hdictrans.x	hdicfit.h <mach.h> hdic.com
+	hdicgvec.x	hdicfit.h <mach.h> hdic.com
+	hdicadd.x	hdicfit.h
+	hdicinit.x 	hdic.com hdicfit.h <mach.h>
+	hdicsort.x
+	userfcn.x	<error.h>
+	hdicgredraw.x	<gset.h>
+	hdicebars.x	hdicfit.h hdic.com <pkg/gtools.h> <gset.h> <mach.h>
+	;
diff --git a/noao/imred/dtoi/hdicfit/userfcn.x b/noao/imred/dtoi/hdicfit/userfcn.x
new file mode 100644
index 00000000..d5dba4ed
--- /dev/null
+++ b/noao/imred/dtoi/hdicfit/userfcn.x
@@ -0,0 +1,37 @@
+include	<error.h>
+
+# HD_POWERR -- Construct the basis functions for a power series function.
+# Invoked from curfit as a user function.  Real version.
+
+procedure hd_powerr (x, order, k1, k2, basis)
+
+real	x		# array of data points
+int	order		# order of polynomial, order = 1, constant
+real	k1, k2		# normalizing constants - unused
+real	basis[ARB]	# basis functions
+
+int	i
+
+begin
+	do i = 1, order
+	    iferr (basis[i] = x ** (i-1))
+		call erract (EA_FATAL) 
+end
+
+
+# HD_POWERD -- Double version of above.
+
+procedure hd_powerd (x, order, k1, k2, basis)
+
+double	x		# array of data points
+int	order		# order of polynomial, order = 1, constant
+double	k1, k2		# normalizing constants - unused
+double	basis[ARB]	# basis functions
+
+int	i
+
+begin
+	do i = 1, order
+            iferr (basis[i] = x ** (i-1))
+	        call erract (EA_FATAL)
+end
diff --git a/noao/imred/dtoi/hdshift.par b/noao/imred/dtoi/hdshift.par
new file mode 100644
index 00000000..c1fdf5c9
--- /dev/null
+++ b/noao/imred/dtoi/hdshift.par
@@ -0,0 +1,2 @@
+# Cl parameters for task hdshift are:
+database,s,a,"",,,List of database file
diff --git a/noao/imred/dtoi/hdshift.x b/noao/imred/dtoi/hdshift.x
new file mode 100644
index 00000000..cde846ad
--- /dev/null
+++ b/noao/imred/dtoi/hdshift.x
@@ -0,0 +1,184 @@
+include	<math/curfit.h>
+
+# T_HDSHIFT -- Task hdshift in the dtoi package.  This task is provided
+# to support Kormendy's method of combining related characteristic curves.
+# A zero point shift in log exp unique to each set of spots is calculated and
+# subtracted.  A single curve is fit to the combined, shifted data in
+# a separate task (hdfit).
+
+procedure t_hdshift ()
+
+pointer	sp, de, fun, save, db, cv, ps_coeff, den, exp, cvf
+int	fd, rec, nsave, ncoeff, nvalues, i, nfile, junk
+real	a0, ref_a0
+
+pointer	ddb_map()
+int	clpopni(), ddb_locate(), ddb_geti(), cvstati(), strncmp(), clgfil()
+
+begin
+	# Allocate space on stack for string buffers
+	call smark (sp)
+	call salloc (de, SZ_FNAME, TY_CHAR)
+	call salloc (cvf, SZ_FNAME, TY_CHAR)
+	call salloc (fun, SZ_FNAME, TY_CHAR)
+
+	# Get list of the database names.  The curfit information is retrieved
+	# from the first file in the list, the list is then rewound.
+
+	fd = clpopni ("database")
+	junk = clgfil (fd, Memc[cvf], SZ_FNAME)
+	call clprew (fd)
+
+	# Get coefficients of common fit from cv_file
+	db = ddb_map (Memc[cvf], READ_ONLY)
+	rec = ddb_locate (db, "cv")
+	nsave = ddb_geti (db, rec, "save")
+	call salloc (save, nsave, TY_REAL)
+	call ddb_gar (db, rec, "save", Memr[save], nsave, nsave)
+	call ddb_gstr (db, rec, "function", Memc[fun], SZ_LINE)
+
+	call cvrestore (cv, Memr[save])
+	ncoeff = cvstati (cv, CVNCOEFF)
+	call salloc (ps_coeff, ncoeff, TY_REAL)
+
+	if (strncmp (Memc[fun], "power", 5) == 0)
+	    call cvcoeff (cv, Memr[ps_coeff], ncoeff)
+	else
+	    call cvpower (cv, Memr[ps_coeff], ncoeff)
+
+	do i = 1, ncoeff {
+	    call eprintf ("%d   %.7g\n")
+	        call pargi (i)
+	        call pargr (Memr[ps_coeff+i-1])
+	}
+
+	call ddb_unmap (db)
+
+	nfile = 0
+	while (clgfil (fd, Memc[de], SZ_FNAME) != EOF) {
+	    db = ddb_map (Memc[de], READ_ONLY)
+	    call hds_read (db, den, exp, nvalues)
+	    call hds_calc (den, exp, nvalues, Memr[ps_coeff], ncoeff, a0)
+	    nfile = nfile + 1
+	    if (nfile == 1)
+		ref_a0 = a0
+	    a0 = a0 - ref_a0
+
+	    call printf ("file %s: subtracting zero point a0 = %.7g\n")
+		call pargstr (Memc[de])
+		call pargr (a0)
+
+	    # Write new log exposure information to database
+	    db = ddb_map (Memc[de], APPEND)
+	    call hds_wdb  (db, exp, nvalues, a0)
+	    call mfree (den, TY_REAL)
+	    call mfree (exp, TY_REAL)
+	    call ddb_unmap (db)
+	}
+
+	call clpcls (fd)
+	call sfree (sp)
+end
+
+
+# HDS_READ -- Read the density and exposure values from the database file.
+# The density above fog and log exposure values are returned, as well as
+# the number of data pairs read.
+
+procedure hds_read (db, den, exp, nvalues)
+
+pointer	db			# Pointer to input database file
+pointer	den			# Pointer to density array - returned
+pointer	exp			# Pointer to exposure array - returned
+int	nvalues			# Number of data pairs read - returned
+
+real	fog
+int	nden, nexp, rec
+int	ddb_locate(), ddb_geti()
+real	ddb_getr()
+
+begin
+	# Get fog value to be subtracted from density
+	rec = ddb_locate (db, "fog")
+	fog = ddb_getr (db, rec, "density")
+
+	# Get density array
+	rec = ddb_locate (db, "density")
+	nden = ddb_geti (db, rec, "den_val")
+	call malloc (den, nden, TY_REAL)
+	call ddb_gar (db, rec, "den_val", Memr[den], nden, nden)
+	call asubkr (Memr[den], fog, Memr[den], nden)
+
+	# Get exposure array
+	rec = ddb_locate (db, "exposure")
+	nexp = ddb_geti (db, rec, "log_exp")
+	call malloc (exp, nexp, TY_REAL)
+	call ddb_gar (db, rec, "log_exp", Memr[exp], nexp, nexp)
+
+	nvalues = min (nden, nexp)
+end
+
+
+# HDS_CALC -- Calculate the individual shift, a0.
+
+procedure hds_calc (den, exp, nvalues, ps_coeff, ncoeff, a0)
+
+pointer	den
+pointer	exp
+int	nvalues
+real	ps_coeff[ARB]
+int	ncoeff
+real	a0
+
+int	i
+real	yavg, ycalc, xavg
+
+begin
+	# Calculate average density and log exposure values
+	xavg = 0.0
+	yavg = 0.0
+
+	do i = 1, nvalues {
+	    xavg = xavg + Memr[den+i-1]
+	    yavg = yavg + Memr[exp+i-1]
+	}
+
+	xavg = xavg / real (nvalues)
+	yavg = yavg / real (nvalues)
+
+	ycalc = 0.0
+	do i = 2, ncoeff
+	    ycalc = ycalc + ps_coeff[i] * (xavg ** real (i-1))
+
+	# Subtraction yields the zero point shift in question
+	a0 = yavg - ycalc
+end
+
+
+# HDS_WDB -- Write shifted log exposure values to database.
+
+procedure hds_wdb  (db, exp, nvalues, a0)
+
+pointer	db		# Pointer to database
+pointer	exp		# Pointer to array of exposure values
+int	nvalues		# Number of exposure values in sample
+real	a0		# Shift to be subtracted
+
+pointer	sp, expsub
+
+begin
+	call smark (sp)
+	call salloc (expsub, nvalues, TY_REAL)
+
+	call ddb_ptime (db)
+	call ddb_prec (db, "exposure")
+
+	call eprintf ("a0 = %g\n")
+	    call pargr (a0)
+
+	call asubkr (Memr[exp], a0, Memr[expsub], nvalues)
+	call ddb_par (db, "log_exp", Memr[expsub], nvalues)
+
+	call ddb_putr (db, "A0 shift", a0)
+	call sfree (sp)
+end
diff --git a/noao/imred/dtoi/hdtoi.par b/noao/imred/dtoi/hdtoi.par
new file mode 100644
index 00000000..e26cde83
--- /dev/null
+++ b/noao/imred/dtoi/hdtoi.par
@@ -0,0 +1,11 @@
+# Cl parameters are:
+input,f,a,,,,List of images to be transformed
+output,f,a,,,,List of output image names
+database,f,a,,,,Database containing fit parameters
+fog,s,h,"",,,Value of fog - read from database if unspecified
+sigma,r,h,3.0,,,Rejection criteria for determining mean fog
+floor,r,h,0.0,,,Value assigned to levels below fog
+ceiling,r,h,30000.,,,Scale highest density to this intensity value
+datatype,s,h,r,,,Pixel type of output image
+option,s,h,mean,"mean|median",,Choice of fog algorithm (mean or median)
+verbose,b,h,yes,,,Print log of processing to STDOUT
diff --git a/noao/imred/dtoi/hdtoi.x b/noao/imred/dtoi/hdtoi.x
new file mode 100644
index 00000000..5b550ea8
--- /dev/null
+++ b/noao/imred/dtoi/hdtoi.x
@@ -0,0 +1,407 @@
+include	<imhdr.h>
+include	<mach.h>
+include	<math/curfit.h>
+include	<error.h>
+include	"hdicfit/hdicfit.h"
+
+# T_HDTOI -- transform an image from density to intensity, according
+# to an hd curve described in an input database.  A look up table of
+# all possible values is generated with the curfit package, and
+# then the image is transformed line by line.  A fog value is subtracted
+# from the image prior to transformation, and it can be entered as either
+# a number or a list of fog images from which the fog value is calculated.
+# If a fog value has not been entered by the user, it is read from the database.
+
+procedure t_hdtoi ()
+
+pointer	sp, cv, fog, db, im_in, lut, im_out, imageout, imagein, option
+bool	verbose
+int	minval, maxval, in_list, rec, ip, out_list, fog_list, ngpix
+int	datatype, nluv, updatedb, nfpix
+real	sigma, floor, scale, fog_val, sdev
+
+char	clgetc()
+bool	streq(), clgetb()
+pointer	ddb_map(), immap()
+int	imtopenp(), ddb_locate(), ctor(), imtlen(), imtgetim()
+int	get_data_type(), imtopen()
+real	clgetr(), ddb_getr()
+
+begin
+	call smark (sp)
+	call salloc (cv,       SZ_FNAME, TY_CHAR)
+	call salloc (fog,      SZ_LINE,  TY_CHAR)
+	call salloc (imageout, SZ_FNAME, TY_CHAR)
+	call salloc (imagein,  SZ_FNAME, TY_CHAR)
+
+	# Get cl parameters
+	in_list = imtopenp ("input")
+	out_list = imtopenp ("output")
+	call clgstr ("database", Memc[cv], SZ_FNAME)
+	call clgstr ("fog", Memc[fog], SZ_LINE)
+	sigma = clgetr ("sigma")
+	floor = clgetr ("floor")
+	verbose = clgetb ("verbose")
+	updatedb = NO
+
+	datatype = get_data_type (clgetc ("datatype"))
+	if (datatype == ERR)
+	    call eprintf ("Using input pixel datatype for output\n")
+
+	db = ddb_map (Memc[cv], READ_ONLY)
+	rec = ddb_locate (db, "common")
+	scale = ddb_getr (db, rec, "scale")
+
+	# If not specified by user, get fog value from database.  User can
+	# specify fog as a real number or a list of fog file names.
+
+	if (streq (Memc[fog], "")) {
+	    rec = ddb_locate (db, "fog")
+	    fog_val = ddb_getr (db, rec, "density")
+	} else {
+	    ip = 1
+	    if (ctor (Memc[fog], ip, fog_val) == 0) {
+		if (verbose)
+		    call eprintf ("Calculating fog value ...\n")
+		fog_list = imtopen (Memc[fog])
+		call salloc (option, SZ_FNAME, TY_CHAR)
+		call clgstr ("option", Memc[option], SZ_FNAME)
+	        call hd_fogcalc (fog_list, fog_val, sdev, ngpix, scale, sigma,
+		    Memc[option], nfpix)
+
+		call eprintf ("Fog density = %f, sdev = %f, ngpix = %d\n")
+		    call pargr (fog_val)
+		    call pargr (sdev)
+		    call pargi (ngpix)
+
+		updatedb = YES
+	    }
+	}
+
+	# Generate look up table.  First, the range of input values to
+	# calculate output values for must be determined.  Arguments
+	# minval and maxval are integers because we assume all input
+	# images are short integers.
+
+	call hd_glimits (in_list, minval, maxval)
+	nluv = (maxval - minval) + 1
+	call salloc (lut, nluv, TY_REAL)
+
+	if (verbose)
+	    call eprintf ("Generating look up table ...\n")
+	call hd_wlut (db, Memr[lut], minval, maxval, fog_val, floor)
+
+	# Loop through input images, applying transform
+	if (imtlen (in_list) != imtlen (out_list)) {
+	    call imtclose (in_list)
+	    call imtclose (out_list)
+	    call error (0, "Number of input and output images not the same")
+	}
+
+	while ((imtgetim (in_list, Memc[imagein], SZ_FNAME) != EOF) &&
+	    (imtgetim (out_list, Memc[imageout], SZ_FNAME) != EOF)) {
+
+	    iferr (im_in = immap (Memc[imagein], READ_ONLY, 0)) {
+		call erract (EA_WARN)
+		next 
+	    }
+
+	    iferr (im_out = immap (Memc[imageout], NEW_COPY, im_in)) {
+		call imunmap (im_in)
+		call erract (EA_WARN)
+		next
+	    }
+
+	    if (verbose) {
+	        call eprintf ("Density to Intensity Transform: %s ===> %s\n")
+    		    call pargstr (Memc[imagein])
+    		    call pargstr (Memc[imageout])
+	    }
+
+	    call hd_transform (im_in, im_out, Memr[lut], nluv, minval, datatype)
+
+	    call imunmap (im_in)
+	    call imunmap (im_out)
+	}
+
+	call ddb_unmap (db)
+	call imtclose (in_list)
+	call imtclose (out_list)
+
+	if (updatedb == YES) {
+	    db = ddb_map (Memc[cv], APPEND)
+	    # Write fog information to database as single record
+	    call ddb_prec (db, "fog")
+	    call ddb_putr (db, "density", fog_val)
+	    call ddb_putr (db, "sdev", sdev)
+	    call ddb_puti (db, "ngpix", ngpix)
+	    call ddb_pstr (db, "option", Memc[option])
+	    call ddb_unmap (db)
+	}
+
+	call sfree (sp)
+end
+
+
+# HD_TRANSFORM -- Apply transformation to image.
+
+procedure hd_transform (im, im_out, lu_table, nvals, minval, datatype)
+
+pointer	im		# Input image header pointer
+pointer	im_out		# Transformed image header pointer
+real	lu_table[ARB]	# Array of intensity values
+int	nvals		# Number of values in the lut
+int	minval		# Offset to first value in look up table
+int	datatype	# Pixel type on output
+
+int	j, ncols
+pointer	ptr_in, ptr_out, sp, luti
+pointer	impl2r(), imgl2i(), impl2i()
+
+begin
+	if (datatype == ERR)
+	    IM_PIXTYPE(im_out) = IM_PIXTYPE(im)
+	else
+	    IM_PIXTYPE(im_out) = datatype
+
+	ncols = IM_LEN(im,1)
+
+	switch (datatype) {
+	case TY_REAL, TY_DOUBLE:
+	    # Loop over input image rows.  The look up table is left as
+	    # a real array and a floating point image is written out.
+
+	    do j = 1, IM_LEN(im,2) {
+	        ptr_in = imgl2i (im, j)
+	        ptr_out = impl2r (im_out, j)
+		call asubki (Memi[ptr_in], minval, Memi[ptr_in], ncols)
+		call alutr (Memi[ptr_in], Memr[ptr_out], ncols, lu_table)
+	    }
+
+	default:
+	    # Loop over input image rows. The look up table is truncated
+	    # to type integer.
+
+	    call smark (sp)
+	    call salloc (luti, nvals, TY_INT)
+	    call achtri (lu_table, Memi[luti], nvals)
+
+	    do j = 1, IM_LEN(im,2) {
+	        ptr_in = imgl2i (im, j)
+	        ptr_out = impl2i (im_out, j)
+		call asubki (Memi[ptr_in], minval, Memi[ptr_in], ncols)
+		call aluti (Memi[ptr_in], Memi[ptr_out], ncols, Memi[luti])
+	    }
+
+	    call sfree (sp)
+	}
+end
+
+
+# HD_WLUT -- write look up table, such that intensity = lut [a/d output].
+# An entry is made in the look up table for every possible input value,
+# from minval to maxval.
+
+procedure hd_wlut (db, lut, minval, maxval, fog_val, floor)
+
+pointer	db		# Pointer to database file
+real 	lut[ARB]	# Pointer to look up table, which gets filled here
+int	minval		# Minimum value to transform
+int	maxval		# Maximum value to transform
+real	fog_val		# Fog value to be subtracted from densities
+real	floor		# Value assigned to densities below fog
+
+bool	zerofloor
+pointer	sp, trans, fcn, save, cv, dens, ind_var, value
+int	rec, nsave, i, function, nneg, npos, nvalues
+real	scale, maxcvval, factor, maxexp, maxden, maxdenaf
+
+bool	fp_equalr()
+int	strncmp(), ddb_locate(), ddb_geti(), cvstati()
+real	ddb_getr(), clgetr(), cveval()
+extern	hd_powerr()
+
+begin
+	call smark (sp)
+	call salloc (trans, SZ_FNAME, TY_CHAR)
+	call salloc (fcn, SZ_FNAME, TY_CHAR)
+
+	nvalues = (maxval - minval) + 1
+	call salloc (ind_var, nvalues, TY_REAL)
+	call salloc (dens,    nvalues, TY_REAL)
+	call salloc (value,   nvalues, TY_REAL)
+
+	rec = ddb_locate (db, "common")
+	scale = ddb_getr (db, rec, "scale")
+	maxden = ddb_getr (db, rec, "maxden")
+
+	rec = ddb_locate (db, "cv")
+	nsave = ddb_geti (db, rec, "save")
+	call salloc (save, nsave, TY_REAL)
+	call ddb_gar (db, rec, "save", Memr[save], nsave, nsave)
+	call ddb_gstr (db, rec, "transformation", Memc[trans], SZ_LINE)
+
+	call cvrestore (cv, Memr[save])
+	function = cvstati (cv, CVTYPE)
+
+	if (function == USERFNC) {
+	    # Need to restablish choice of user function
+	    call ddb_gstr (db, rec, "function", Memc[fcn], SZ_FNAME)
+	    if (strncmp (Memc[fcn], "power", 1) == 0) 
+		call cvuserfnc (cv, hd_powerr)
+	    else
+		call error (0, "Unknown user function in database")
+	}
+
+	maxdenaf = maxden - fog_val
+	call hd_aptrans (maxdenaf, maxcvval, 1, Memc[trans])
+	maxcvval = 10.0 ** (cveval (cv, maxcvval))
+	factor = clgetr ("ceiling") / maxcvval
+	maxexp = real (MAX_EXPONENT) - (log10 (factor) + 1.0)
+
+	zerofloor = false
+	if (fp_equalr (0.0, floor))
+	    zerofloor = true
+
+	do i = 1, nvalues
+	    Memr[value+i-1] = real (minval + i - 1)
+
+	# Scale all posible voltage values to density above fog
+	call altmr (Memr[value], Memr[dens], nvalues, scale, -fog_val)
+
+	# Find index of first value greater than MIN_DEN.  Values less than 
+	# this must be handled as the user specified with the floor parameter.
+
+	for (nneg=0; Memr[dens+nneg] < MIN_DEN; nneg=nneg+1)
+	    ;
+	npos = nvalues - nneg
+	
+	# Generate independent variable vector and then lut values.  The
+	# logic is different if there are values below fog.  Evaluating 
+	# the polynomial fit with cvvector yields the log exposure.  This
+	# is then converted to intensity and scaled by a user supplied factor.
+
+	if (nneg > 0) {
+	    if (zerofloor) {
+		call amovkr (0.0, lut, nneg)
+		call hd_aptrans (Memr[dens+nneg],Memr[ind_var],npos,Memc[trans])
+		call cvvector (cv, Memr[ind_var], lut[nneg+1], npos)
+		call argtr (lut[nneg+1], npos, maxexp, maxexp)
+		do i = nneg+1, nvalues
+		    lut[i] = (10. ** lut[i]) * factor
+
+	    } else {
+		call amulkr (Memr[dens], -1.0, Memr[dens], nneg)
+
+		# Care must be taken so that no density of value 0.0 is 
+		# passed to hd_aptrans.  This would cause an overflow.
+
+		do i = 1, nneg {
+		    if (fp_equalr (Memr[dens], 0.0))
+			Memr[dens] = MIN_DEN
+		}
+
+		call hd_aptrans (Memr[dens],Memr[ind_var], nvalues, Memc[trans])
+		call cvvector (cv, Memr[ind_var], lut, nvalues)
+		call argtr (lut, nvalues, maxexp, maxexp)
+	        do i = 1, nvalues
+		    lut[i] = (10.0 ** lut[i]) * factor
+		call amulkr (lut, -1.0, lut, nneg)
+	    }
+		
+	} else {
+	    call hd_aptrans (Memr[dens], Memr[ind_var], nvalues, Memc[trans])
+	    call cvvector (cv, Memr[ind_var], lut, nvalues)
+	    call argtr (lut, nvalues, maxexp, maxexp)
+	    do i = 1, nvalues
+		lut[i] = (10.0 ** lut[i]) * factor
+	}
+
+	call cvfree (cv)
+	call sfree (sp)
+end
+
+
+# HD_APTRANS -- Apply transformation, generating a vector of independent
+# variables from a density vector.  It is assummed all values in the
+# input density vector are valid and will not cause arithmetic errors.
+# No checking for out of bounds values is performed.
+
+procedure hd_aptrans (density, ind_var, nvalues, transform)
+
+real	density[nvalues]	# Density vector - input
+real	ind_var[nvalues]	# Ind variable vector - filled on output
+int	nvalues			# Length of vectors
+char	transform[ARB]		# String containing transformation type
+
+int	i
+int	strncmp()
+
+begin
+	if (strncmp (transform, "logopacitance", 1) == 0) {
+	    do i = 1, nvalues
+	        ind_var[i] = log10 ((10. ** density[i]) - 1.0)
+
+	} else if (strncmp (transform, "k75", 2) == 0) {
+	    do i = 1, nvalues
+	        ind_var[i] = density[i] + .75 * log10(1. - 10. ** (-density[i]))
+
+	} else if (strncmp (transform, "k50", 2) == 0) {
+	    do i = 1, nvalues
+	        ind_var[i] = density[i] + .50 * log10(1. - 10. ** (-density[i]))
+
+	} else if (strncmp (transform, "none", 1) == 0) {
+	    do i = 1, nvalues
+	        ind_var[i] = density[i]
+
+	} else 
+	    call error (0, "Unrecognized transformation in database file")
+end
+
+
+# HD_GLIMITS -- Determinine the range of max and min values for a list
+# of images.
+
+procedure hd_glimits (in_list, minval, maxval)
+
+int	in_list		# File descriptor for list of images
+int	minval		# Smallest pixel value - returned
+int	maxval		# Largest  pixel value - returned
+
+pointer	im
+char	image[SZ_FNAME]
+real	current_min, current_max, min, max
+pointer	immap()
+int	imtgetim()
+errchk	imtgetim, im_minmax, imtrew
+
+begin
+	current_min = MAX_REAL
+	current_max = EPSILONR
+
+	while (imtgetim (in_list, image, SZ_FNAME) != EOF) {
+	    iferr (im = immap (image, READ_ONLY, 0))
+		# Just ignore it, warning will be printed by t_hdtoi
+		next
+
+	    # Update min max values if necessary
+	    if (IM_LIMTIME(im) < IM_MTIME(im))
+	        call im_minmax (im, IM_MIN(im), IM_MAX(im))
+
+	    min = IM_MIN(im)
+	    max = IM_MAX(im)
+
+	    if (min < current_min)
+		current_min = min
+
+	    if (max > current_max)
+		current_max = max
+	    
+	    call imunmap (im)
+	}
+
+	minval = int (current_min)
+	maxval = int (current_max)
+
+	call imtrew (in_list)
+end
diff --git a/noao/imred/dtoi/minmax.x b/noao/imred/dtoi/minmax.x
new file mode 100644
index 00000000..97d113f0
--- /dev/null
+++ b/noao/imred/dtoi/minmax.x
@@ -0,0 +1,73 @@
+include	<imhdr.h>
+
+# IM_MINMAX -- Compute the minimum and maximum pixel values of an image.
+# Works for images of any dimensionality, size, or datatype, although
+# the min and max values can currently only be stored in the image header
+# as real values.
+
+procedure im_minmax (im, min_value, max_value)
+
+pointer	im				# image descriptor
+real	min_value			# minimum pixel value in image (out)
+real	max_value			# maximum pixel value in image (out)
+
+pointer	buf
+bool	first_line
+long	v[IM_MAXDIM]
+short	minval_s, maxval_s
+long	minval_l, maxval_l
+real	minval_r, maxval_r
+int	imgnls(), imgnll(), imgnlr()
+errchk	amovkl, imgnls, imgnll, imgnlr, alims, aliml, alimr
+
+begin
+	call amovkl (long(1), v, IM_MAXDIM)		# start vector
+	first_line = true
+	min_value = INDEF
+	max_value = INDEF
+
+	switch (IM_PIXTYPE(im)) {
+	case TY_SHORT:
+	    while (imgnls (im, buf, v) != EOF) {
+		call alims (Mems[buf], IM_LEN(im,1), minval_s, maxval_s)
+		if (first_line) {
+		    min_value = minval_s
+		    max_value = maxval_s
+		    first_line = false
+		} else {
+		    if (minval_s < min_value)
+			min_value = minval_s
+		    if (maxval_s > max_value)
+			max_value = maxval_s
+		}
+	    }
+	case TY_USHORT, TY_INT, TY_LONG:
+	    while (imgnll (im, buf, v) != EOF) {
+		call aliml (Meml[buf], IM_LEN(im,1), minval_l, maxval_l)
+		if (first_line) {
+		    min_value = minval_s
+		    max_value = maxval_s
+		    first_line = false
+		} else {
+		    if (minval_l < min_value)
+			min_value = minval_l
+		    if (maxval_l > max_value)
+			max_value = maxval_l
+		}
+	    }
+	default:
+	    while (imgnlr (im, buf, v) != EOF) {
+		call alimr (Memr[buf], IM_LEN(im,1), minval_r, maxval_r)
+		if (first_line) {
+		    min_value = minval_r
+		    max_value = maxval_r
+		    first_line = false
+		} else {
+		    if (minval_r < min_value)
+			min_value = minval_r
+		    if (maxval_r > max_value)
+			max_value = maxval_r
+		}
+	    }
+	}
+end
diff --git a/noao/imred/dtoi/mkpkg b/noao/imred/dtoi/mkpkg
new file mode 100644
index 00000000..80d5b737
--- /dev/null
+++ b/noao/imred/dtoi/mkpkg
@@ -0,0 +1,40 @@
+# Make the DTOI package.
+
+$call	relink
+$exit
+
+update:
+	$call	relink
+	$call	install
+	;
+
+relink:
+	$call update@hdicfit
+	$update	libpkg.a
+	$call	dtoi
+	;
+
+install:
+	$move	xx_dtoi.e noaobin$x_dtoi.e
+	;
+
+dtoi:
+	$omake  x_dtoi.x
+	$link	x_dtoi.o libpkg.a hdicfit/libhdic.a -lxtools -lcurfit\
+		-o xx_dtoi.e
+	;
+
+libpkg.a:
+	database.x	<ctotok.h> <ctype.h> <finfo.h> <time.h>
+	dematch.x	<error.h>
+	hd_aravr.x	<mach.h>
+	hdfit.x		hdicfit/hdicfit.h <ctype.h> <error.h> <fset.h>\
+			<imhdr.h> <mach.h> <math/curfit.h> <pkg/gtools.h>\
+			<pkg/xtanswer.h>
+	hdshift.x	<math/curfit.h>
+	hdtoi.x		hdicfit/hdicfit.h <error.h> <imhdr.h> <mach.h>\
+			<math/curfit.h>
+	minmax.x	<imhdr.h>
+	selftest.x	<gio.h> <gset.h> <mach.h>
+	spotlist.x	<error.h> <fset.h> <imhdr.h> <mach.h>
+	;
diff --git a/noao/imred/dtoi/selftest.par b/noao/imred/dtoi/selftest.par
new file mode 100644
index 00000000..75445cf7
--- /dev/null
+++ b/noao/imred/dtoi/selftest.par
@@ -0,0 +1,8 @@
+# Parameters for task selftest
+nbits,i,q,12,,,Test data range
+device,s,h,"stdgraph",,,Output device
+verbose,b,h,no,,,"Print density, intensity values?"
+ceiling,r,h,30000.,,,Scale densest point to this intensity
+max_raw,i,q,0,,,Max raw data value
+scale,r,q,,0.0,,Raw value to density scale factor
+mode,s,h,ql
diff --git a/noao/imred/dtoi/selftest.x b/noao/imred/dtoi/selftest.x
new file mode 100644
index 00000000..3a7a4a4a
--- /dev/null
+++ b/noao/imred/dtoi/selftest.x
@@ -0,0 +1,290 @@
+include	<gio.h>
+include	<gset.h>
+include	<mach.h>
+
+define	A0	(-1.74743)
+define	A1	(0.73)
+define	A2	(-0.24)
+define	A3	(0.035)
+define	MAXDEN	6.0
+
+# T_SELFTEST -- a test procedure for the DTOI package.  Two intensity vectors
+# are calculated in different ways and compared.  A plot of the residuals is
+# shown.  A plot showing the extent of truncation errors is also drawn.  Two
+# standard ranges of data values are available: 12 bit, representing PDS
+# format data and 15 bit, representing the FITS data format available on the
+# PDS.  Any other choice results in a small test, ranging from 1 - 144.
+
+procedure t_selftest
+
+bool	verbose
+char	device[SZ_FNAME]
+pointer	sp, intk, intc, raw, den, gp
+int	min_raw, max_raw, nvalues, i, nbits
+real	scale, factor, ceiling
+
+bool	clgetb()
+pointer	gopen()
+int	clgeti()
+real	clgetr()
+
+begin
+	call smark (sp)
+
+	nbits = clgeti ("nbits")
+
+	switch (nbits) {
+	case 12:
+	    min_raw = 1
+	    max_raw = 3072
+	    scale   = 0.00151
+	case 15:
+	    min_raw = 1
+	    max_raw = 24576
+	    scale   = 4.65 / 24575. 
+	case 0:
+	    call eprintf ("Using test data range from 1 - 144\n")
+	    min_raw = 1
+	    max_raw = 144
+	    scale   = 0.0325
+	default:
+	    call eprintf ("Unknown case: nbits = '%d', Please supply values:\n")
+		call pargi (nbits)
+	    min_raw = 1
+	    max_raw = clgeti ("max_raw")
+	    # max density = 6.0.  Density = raw value * scale.
+	    call clputr ("scale.p_maximum", real (MAXDEN / max_raw))
+	    call clputr ("scale.p_default", real (4.65 / (max_raw - 1)))
+	    scale = clgetr ("scale")
+	}
+
+	call clgstr ("device", device, SZ_FNAME)
+	verbose = clgetb ("verbose")
+	ceiling = clgetr ("ceiling")
+
+	gp = gopen (device, NEW_FILE, STDGRAPH)
+
+	nvalues = max_raw - min_raw + 1
+	call salloc (intk, nvalues, TY_REAL)
+	call salloc (intc, nvalues, TY_REAL)
+	call salloc (den,  nvalues, TY_REAL)
+	call salloc (raw,  nvalues, TY_REAL)
+
+	do i = 1, nvalues
+	    Memr[raw+i-1] = min_raw + i - 1
+
+	call amulkr (Memr[raw], scale, Memr[den], nvalues)
+
+	call hd_known (min_raw, max_raw, scale, Memr[intk], nvalues)
+	call hd_calc  (min_raw, max_raw, scale, Memr[intc], nvalues)
+	 
+	if (verbose) {
+	    factor = ceiling / Memr[intc+nvalues-1]
+	    call printf ("# %20tRaw Value %40tDensity %60tIntensity\n\n")
+	    do i = 1, nvalues {
+	        call printf ("%20t%d %40t%g %60t%g\n")
+		    call pargi (i)
+		    call pargr (Memr[den+i-1])
+		    call pargr (Memr[intc+i-1] * factor)
+	    }
+	}
+
+	call hd_plotit (gp, Memr[den], Memr[intk], Memr[intc], nvalues)
+
+	call hd_trunc (gp, Memr[den], nvalues, ceiling, Memr[intc])
+
+	call gclose (gp)
+	call sfree (sp)
+end
+
+
+# HD_KNOWN -- Calculate vector of known intensity values.
+
+procedure hd_known (min_raw, max_raw, scale, intk, nvalues)
+
+int	min_raw			# Minimum raw data value
+int	max_raw			# Maximum raw data value
+real	scale			# Density = raw_value * scale
+real	intk[nvalues]		# Known intensities - filled on return
+int	nvalues			# Number of intensity values requested
+
+int	i
+real	density, logo
+real	exp
+
+begin
+	do i = min_raw, max_raw {
+	    density = max (EPSILONR, i * scale)
+	    logo = log10 ((10. ** density) - 1.0)
+	    exp  = A0 + A1 * logo + A2 * logo ** 2 + A3 * logo ** 3
+	    intk[i] = 10 ** (exp)
+	}
+end
+
+
+# HD_CALC -- Calcuate vector of intensity values as in HDTOI.
+
+procedure hd_calc (min, max, scale, intc, nvalues)
+
+int	min			# Minimum raw data value
+int	max			# Maximum raw data value
+real	scale			# Density = raw_value * scale
+real	intc[nvalues]		# Calculated intensity values - filled on return
+int	nvalues			# Number of intensity values requested
+
+real	cfit[9]
+pointer	sp, lut
+
+begin
+	call smark (sp)
+	call salloc (lut, nvalues, TY_REAL)
+
+	cfit[1] = 5.0
+	cfit[2] = 4.0
+	cfit[3] = -10.0
+	cfit[4] = MAXDEN
+	cfit[5] = 1.
+	cfit[6] = A0
+	cfit[7] = A1
+	cfit[8] = A2
+	cfit[9] = A3
+	call st_wlut (Memr[lut], min, max, scale, cfit)
+	call st_transform (min, max, Memr[lut], nvalues, intc)
+
+	call sfree (sp)
+end
+
+
+# HD_TRUNC -- Investigate truncation errors for real versus int output image.
+
+procedure hd_trunc (gp, density, nvalues, ceiling, intc)
+
+pointer	gp			# Pointer to graphics stream
+real	density[nvalues]	# Density array
+int	nvalues			# Number of density, intensity values
+real	ceiling			# Max intensity to output
+real	intc[nvalues]		# Calculated intensity values
+
+pointer	sp, yint, yreal
+int	npvals
+real	factor
+
+begin
+	call smark (sp)
+
+	# Only the lowest 5% of the data values are plotted
+	npvals = nvalues * 0.05
+
+	call salloc (yint, npvals, TY_INT)
+	call salloc (yreal, npvals, TY_REAL)
+
+	# Scale intensity vector to ceiling 
+	factor = ceiling / intc[nvalues]
+
+	call amulkr (intc, factor, intc, npvals)
+	call achtri (intc, Memi[yint], npvals)
+	call achtir (Memi[yint], Memr[yreal], npvals)
+
+	call gascale (gp, density,  npvals, 1)
+	call gascale (gp, Memr[yreal], npvals, 2)
+	call gsview  (gp, 0.2, 0.9, 0.1, 0.4)
+	call gseti (gp, G_ROUND, YES)
+	call glabax  (gp, 
+	    "Expand to see Truncation Errors\n (real=SOLID, integer=DASHED)", 
+	    "Density (Lowest 5% only)", "Intensity")
+
+	call gseti  (gp, G_PLTYPE, GL_SOLID)
+	call gpline (gp, density, intc, npvals)
+
+	call gseti  (gp, G_PLTYPE, GL_DASHED)
+	call gpline (gp, density, Memr[yreal], npvals)
+
+	call sfree (sp)
+end
+
+
+# HD_PLOTIT -- Plot residuals of calculated versus known itensity.
+
+procedure hd_plotit (gp, density, intk, intc, nvalues)
+
+pointer	gp			# Pointer to graphics stream
+real	density[nvalues]	# Density array
+real	intk[nvalues]		# Array of known intensities
+real	intc[nvalues]		# Array of calculated intensities
+int	nvalues			# Number of density, intensity values
+
+pointer	sp, resid
+
+begin
+	call smark (sp)
+	call salloc (resid, nvalues, TY_REAL)
+
+	call asubr (intk, intc, Memr[resid], nvalues)
+
+	call gascale (gp, density, nvalues, 1)
+	call gascale (gp, Memr[resid], nvalues, 2)
+	call gsview  (gp, 0.2, 0.9, 0.6, 0.9)
+	call gseti   (gp, G_ROUND, YES)
+
+	call glabax  (gp, "Residual Intensity\n (Known - Calculated)", 
+	    "Density", "")
+	call gpline  (gp, density, Memr[resid], nvalues)
+
+	call sfree (sp)
+end
+
+
+# ST_WLUT -- Generate look up table, using technique of HDTOI.
+
+procedure st_wlut (lut, min, max, scale, cfit)
+
+real	lut[ARB]	# Look up table of intensities
+int	min		# Minimum raw data value
+int	max		# Maximum raw data value
+real	scale		# Density = raw_value * scale
+real	cfit[ARB]	# Coefficient array for restoring curfit
+
+pointer	cv, sp, den, indv, kv
+int	nvalues, i
+extern	hd_powerr()
+
+begin
+	call smark (sp)
+	nvalues = max - min + 1
+	call salloc (den, nvalues, TY_REAL)
+	call salloc (indv, nvalues, TY_REAL)
+	call salloc (kv, nvalues, TY_REAL)
+	do i = 1, nvalues
+	    Memr[kv+i-1] = real (i)
+
+	call amulkr (Memr[kv], scale, Memr[den], nvalues)
+
+	call cvrestore (cv, cfit)
+	call cvuserfnc (cv, hd_powerr)
+
+	call hd_aptrans (Memr[den], Memr[indv], nvalues, "logo")
+	call cvvector (cv, Memr[indv], lut, nvalues)
+	do i = 1, nvalues
+	    lut[i] = 10.0 ** lut[i]
+
+	call cvfree (cv)
+	call sfree (sp)
+end
+
+
+# ST_TRANSFORM -- Apply transformation from look up table to input vector.
+
+procedure st_transform (min, max, lut, nvalues, intc)
+
+int	min		# Minimum raw data value
+int	max		# Maximum raw data value
+real	lut[ARB]	# Array of intensity values
+int	nvalues		# Number of density, intensity values
+real	intc[ARB]	# Calculated intensities - returned
+
+int	i
+
+begin
+	do i = 1, nvalues
+	    intc[i] = lut[i]
+end
diff --git a/noao/imred/dtoi/spotlist.par b/noao/imred/dtoi/spotlist.par
new file mode 100644
index 00000000..8134c8de
--- /dev/null
+++ b/noao/imred/dtoi/spotlist.par
@@ -0,0 +1,8 @@
+# The cl parameters for task spotlist in the dtoi package
+spots,f,a,,,,List of image files containing spot data
+fogs,f,a,,,,List of images containing fog spots
+database,f,a,,,,Name of output database file
+scale,r,h,0.00151,,,Input value to density scale factor
+maxad,i,h,3071,,,Integer A/D value of saturated pixel
+sigma,r,h,3.0,,,Rejection criteria when determining mean density
+option,s,h,mean,"mean|median",,Choice of algorithm (mean or median)
diff --git a/noao/imred/dtoi/spotlist.x b/noao/imred/dtoi/spotlist.x
new file mode 100644
index 00000000..8f4ffeee
--- /dev/null
+++ b/noao/imred/dtoi/spotlist.x
@@ -0,0 +1,395 @@
+include	<error.h>
+include	<imhdr.h>
+include	<mach.h>
+include	<fset.h>
+
+# T_SPOTLIST -- calculates the densities and standard deviations of calibration
+# spots read in as IRAF images.  Entries for density, sdev, spot number
+# and number of pixels used in the average are made in the output database.
+# These values are entered for all spots and the fog level.  The
+# fog level is calculated but not subtracted in this procedure.
+
+procedure t_spotlist ()
+
+pointer	db, sp, den, ngpix, sdev, dloge, option, npix
+int	spot_fd, fog_fd, fngpix, nspots, maxad, fnpix
+real	scale, sigma, fsdev, fog
+double	maxden
+
+pointer	ddb_map()
+int	imtopenp(), imtlen(), clgeti(), strncmp()
+real	clgetr()
+
+begin
+	call smark (sp)
+	call salloc (dloge, SZ_FNAME, TY_CHAR)
+	call salloc (option, SZ_FNAME, TY_CHAR)
+
+	# Get parameters and open file name templates
+	spot_fd = imtopenp ("spots")
+	fog_fd  = imtopenp ("fogs")
+	call clgstr ("database", Memc[dloge], SZ_FNAME)
+	scale = clgetr ("scale")
+	maxad = clgeti ("maxad")
+	sigma = clgetr ("sigma")
+	call clgstr ("option", Memc[option], SZ_FNAME)
+
+	maxden = maxad * double (scale)
+
+	# Allocate space for density, standard deviation and ngpix arrays
+	nspots = imtlen (spot_fd)
+	call salloc ( den,  nspots, TY_REAL)
+	call salloc (sdev,  nspots, TY_REAL)
+	call salloc (ngpix, nspots, TY_INT)
+	call salloc ( npix, nspots, TY_INT)
+
+	# Calculate densities depending on algorithm option.  The 
+	# number of saturated pixels per spot is also calculated now.
+
+	if (strncmp (Memc[option], "median", 3) == 0)
+	    call hd_median (spot_fd, Memr[den], Memr[sdev], Memi[ngpix],
+		nspots, scale, Memi[npix])
+	else
+	    call hd_mean (spot_fd, Memr[den], Memr[sdev], Memi[ngpix], 
+		nspots, scale, sigma, Memi[npix])
+
+	# Calculate fog level and count saturated pixels
+	call hd_fogcalc (fog_fd, fog, fsdev, fngpix, scale, sigma, 
+	    Memc[option], fnpix)
+
+	# Now print results to stdout
+	call hd_printit (Memr[den], Memr[sdev], Memi[npix], Memi[ngpix], 
+	    fog, fsdev, fnpix, fngpix, nspots)
+	    
+	# Open output database file and write spot information
+	db = ddb_map (Memc[dloge], APPEND)
+	call hd_wspotdb (db, Memr[den], Memr[sdev], Memi[ngpix], nspots)
+
+	# Write fog information to database as single record
+	call ddb_prec (db, "fog")
+	call ddb_putr (db, "density", fog)
+	call ddb_putr (db, "sdev", fsdev)
+	call ddb_puti (db, "ngpix", fngpix)
+
+	# Scale info gets written to database also (very precisely!)
+	call ddb_prec (db, "common")
+	call ddb_putr (db, "scale", scale)
+	call ddb_putd (db, "maxden", maxden)
+	call ddb_pstr (db, "option", Memc[option])
+
+	call ddb_unmap (db)
+
+	call imtclose (spot_fd)
+	call imtclose (fog_fd)
+	call sfree (sp)
+end
+
+
+# HD_MEAN -- Calculate mean density of calibration spots.
+
+procedure hd_mean (spot_fd, den, sdev, ngpix, nspots, scale, sigma, npix)
+
+int	spot_fd		# File descriptor for list of spots
+real	den[ARB]	# Mean density values - filled on return
+real	sdev[ARB]	# Standard deviation array - filled on return
+int	ngpix[ARB]	# Number of unrejected pixels - filled on return
+int	nspots		# Number of spots in list
+real	scale		# Scale for voltage to density conversion
+real	sigma		# Rejection criteria set by user
+int	npix[ARB]	# Number of pixels per spot
+
+pointer	im, spot, sp, pix
+int	i, junk, ncols, nlines
+pointer	immap(), imgs2r()
+int	imtgetim(), hd_aravr()
+errchk	imgs2r, amulkr, hd_aravr
+
+begin
+	call smark (sp)
+	call salloc (spot, SZ_FNAME, TY_CHAR)
+
+	# Loop over spot rasters.  Calculate density and standard deviation.
+	for (i = 1; i <= nspots; i = i + 1) {
+	    junk = imtgetim (spot_fd, Memc[spot], SZ_FNAME)
+	    iferr (im = immap (Memc[spot], READ_ONLY, 0)) {
+		call erract (EA_WARN)
+		next
+	    }
+
+	    ncols = IM_LEN(im,1)
+	    nlines = IM_LEN(im,2)
+	    npix[i] = ncols * nlines
+
+	    # For all pixels in the image, scale the a/d value to density and
+	    # calculate the mean value, using a mean rejection algorithm.
+
+	    pix = imgs2r (im, 1, ncols, 1, nlines)
+	    call amulkr (Memr[pix], scale, Memr[pix], npix[i])
+	    ngpix[i] = hd_aravr (Memr[pix], npix[i], den[i], sdev[i], sigma)
+	    call imunmap (im)
+	}
+
+	call sfree (sp)
+end
+
+
+# HD_MEDIAN -- Calculate median density of calibration spots.
+
+procedure hd_median (spot_fd, den, sdev, ngpix, nspots, scale, npix)
+
+int	spot_fd		# File descriptor for list of spots
+real	den[ARB]	# Mean density values - filled on return
+real	sdev[ARB]	# Standard deviation of input spots
+int	ngpix[ARB]	# Number of pixels not rejected
+int	nspots		# Number of spots in list
+real	scale		# Scale for voltage to density conversion
+int	npix[ARB]	# Number of pixels per spot
+
+pointer	im, spot, sp, pix
+int	i, junk, ncols, nlines
+real	junk_mean
+pointer	immap(), imgs2r()
+int	imtgetim()
+real	amedr()
+errchk	imgs2r, amulkr, amedr
+
+begin
+	call smark (sp)
+	call salloc (spot, SZ_FNAME, TY_CHAR)
+
+	# Loop over spot rasters.  Calculate density and standard deviation.
+	for (i = 1; i <= nspots; i = i + 1) {
+	    junk = imtgetim (spot_fd, Memc[spot], SZ_FNAME)
+	    iferr (im = immap (Memc[spot], READ_ONLY, 0)) {
+		call erract (EA_WARN)
+		next
+	    }
+
+	    ncols = IM_LEN(im,1)
+	    nlines = IM_LEN(im,2)
+	    npix[i] = ncols * nlines
+
+	    # For all pixels in the image, scale the a/d value to density and
+	    # calculate the median value.  For the user's information, the
+	    # sigma is also calculated in a call to aavgr.
+
+	    pix = imgs2r (im, 1, ncols, 1, nlines)
+	    call amulkr (Memr[pix], scale, Memr[pix], npix[i])
+	    den[i] = amedr (Memr[pix], npix[i])
+	    ngpix[i] = npix[i]
+	    call aavgr (Memr[pix], npix[i], junk_mean, sdev[i])
+	    call imunmap (im)
+	}
+
+	call sfree (sp)
+end
+
+
+# HD_FOGCALC -- Calculate fog density.
+
+procedure hd_fogcalc (fog_fd, fog, fsdev, fngpix, scale, sigma, option, nfpix)
+
+int	fog_fd		# File descriptor for list of fog spots
+real	fog		# Mean fog value - returned
+real	fsdev		# Standard deviation - returned
+int	fngpix		# Number of pixels used - returned
+real	scale		# Voltage to density scaling factor
+real	sigma		# Rejection criteria - set by user
+char	option[ARB]     # User's choice of mean/median algorithm
+int	nfpix		# Total number of fog pixels
+
+pointer	pix, im, sp, fogfile, ptr
+int	nfog, maxfog, i, junk, ncols, nlines, npix, total_pix, op
+real	junk_mean
+pointer	immap(), imgs2r()
+int	imtlen(), imtgetim(), hd_aravr(), strncmp()
+real	amedr()
+errchk	calloc, imgs2r, aaddr, amulkr, hd_aravr
+
+begin
+	call smark (sp)
+	call salloc (fogfile, SZ_FNAME, TY_CHAR)
+
+	pix = NULL
+	total_pix = 0
+	op = 0
+	nfog = imtlen (fog_fd)
+	maxfog = nfog
+	do i = 1, maxfog {
+	    junk = imtgetim (fog_fd, Memc[fogfile], SZ_FNAME)
+	    iferr (im = immap (Memc[fogfile], READ_ONLY, 0)) {
+		call erract (EA_WARN)
+		nfog = nfog - 1
+		next
+	    }
+
+	    ncols = IM_LEN(im,1)
+	    nlines = IM_LEN(im,2)
+	    npix = ncols * nlines
+	    total_pix = total_pix + npix
+
+	    if (pix == NULL)
+		# Initialize space for accumulating pixels
+		call calloc (pix, npix, TY_REAL)
+	    else
+	       # Increase space for accumulating pixels
+	       call realloc (pix, total_pix, TY_REAL)
+
+	    # Build up vector of fog pixels
+	    ptr = imgs2r (im, 1, ncols, 1, nlines)
+	    call amovr (Memr[ptr], Memr[pix+op], npix)
+	    op = op + npix
+
+	    call imunmap (im)
+	}
+
+	# Scale values to density and calculate fog and std deviation
+
+	if (nfog > 0) {
+# 7 Sept 1989, S. Rooke:  in Suzanne's absence, made following bugfix after
+# bug reported by Steve Majewski that fog values are off by 1/n images where
+# multiple fog images are used in a single run.  The total_pix already contains
+# the sum of all pixel values, so the fog pixel values should not be divided
+# by nfog.  This should be verified by Suzanne on her return, and these comments
+# removed.
+#	    call amulkr (Memr[pix], scale / real (nfog), Memr[pix], total_pix)
+	    call amulkr (Memr[pix], scale, Memr[pix], total_pix)
+	    if (strncmp (option, "median", 3) == 0) {
+		fog = amedr (Memr[pix], total_pix)
+		fngpix = total_pix
+		call aavgr (Memr[pix], total_pix, junk_mean, fsdev)
+	    } else
+	        fngpix = hd_aravr (Memr[pix], total_pix, fog, fsdev, sigma)
+	}  else {
+	    fog = 0.0
+	    fsdev = 0.0
+	    fngpix = 0
+	}
+	nfpix = total_pix
+
+	call mfree (pix, TY_REAL)
+	call sfree (sp)
+end
+
+
+# HD_WSPOTDB -- Write spot information to database file.  Values are first
+# sorted in order of increasing density.
+
+procedure hd_wspotdb (db, density, sdev, ngpix, nspots)
+
+pointer	db			# Pointer to database
+real	density[ARB]		# Array of densities
+real	sdev [ARB]		# Array of standard deviations
+int	ngpix [ARB]		# Array of npix used in calculations
+int	nspots			# Number of density spots
+
+begin
+	if (density[1] > density[nspots]) {
+	    # Need to reorder arrays
+	    call hd_reorderr (density, nspots)
+	    call hd_reorderr (   sdev, nspots)
+	    call hd_reorderi (  ngpix, nspots)
+	}
+
+	call ddb_ptime (db)
+
+	# Density record
+	call ddb_prec (db, "density")
+	call ddb_par (db, "den_val", density, nspots)
+
+	# Standard deviation of density is written to a record
+	call ddb_prec (db, "standard deviation")
+	call ddb_par (db, "sdev_val", sdev, nspots)
+
+	# Record for npix_used
+	call ddb_prec (db, "ngpix")
+	call ddb_pai (db, "npix_val", ngpix, nspots)
+end
+
+
+# HD_REORDERR - Flip order of real array in place.
+
+procedure hd_reorderr (array, nvals)
+
+real	array[ARB]		# Real array to be reordered
+int	nvals			# Number of elements in array
+
+pointer	sp, tmp
+int	i
+
+begin
+	call smark (sp)
+	call salloc (tmp, nvals, TY_REAL)
+
+	call amovr (array, Memr[tmp], nvals)
+	do i = 1, nvals
+	    array[i] = Memr[tmp+nvals-i]
+
+	call sfree (sp)
+end
+
+
+# HD_REORDERI -- Flip order of integer array in place.
+
+procedure hd_reorderi (array, nvals)
+
+int	array[ARB]		# Integer array to be ordered
+int	nvals			# Number of elements in array
+
+pointer	sp, tmp
+int	i
+
+begin
+	call smark (sp)
+	call salloc (tmp, nvals, TY_INT)
+
+	call amovi (array, Memi[tmp], nvals)
+	do i = 1, nvals
+	    array[i] = Memi[tmp+nvals-i]
+
+	call sfree (sp)
+end
+
+
+# HD_PRINTIT -- Neatly printout all the accumulated information.
+
+procedure hd_printit (den, sdev, npix, ngpix, fog, fsdev, fnpix, fngpix, nspots)
+
+real	  den[ARB]	# density array 
+real	 sdev[ARB]	# std deviation array 
+int	 npix[ARB]      # npix array
+int	ngpix[ARB]      # ngoodpix array
+real	fog		# fog value
+real	fsdev           # std deviation of fog
+int     fnpix		# npix in fog
+int	fngpix		# ngoodpix in fog
+int	nspots		# number of spots
+int	i
+
+begin
+
+	call fseti (STDOUT, F_FLUSHNL, YES)
+
+	call printf ("\n                                         # Number of P")
+	call printf ("ixels\n")
+	call printf ("# Spot Number  Density   Std Deviation  Total  Used  Rej")
+	call printf ("ected \n")
+
+	do i = 1, nspots {
+	    call printf ("    %d %17t%.4f %27t%.4f %43t%d %5d %6d \n")
+	        call pargi (i)
+	        call pargr (den[i])
+	        call pargr (sdev[i])
+	        call pargi (npix[i])
+	        call pargi (ngpix[i])
+	        call pargi (npix[i] - ngpix[i])
+	}
+
+	call printf ("   FOG %17t%.4f %27t%.4f %43t%d %5d %6d \n")
+	    call pargr (fog)
+	    call pargr (fsdev)
+	    call pargi (fnpix)
+	    call pargi (fngpix)
+	    call pargi (fnpix - fngpix)
+
+end
diff --git a/noao/imred/dtoi/x_dtoi.x b/noao/imred/dtoi/x_dtoi.x
new file mode 100644
index 00000000..5fd0cc72
--- /dev/null
+++ b/noao/imred/dtoi/x_dtoi.x
@@ -0,0 +1,6 @@
+task spotlist = t_spotlist,
+	hdfit = t_hdfit,
+      hdshift = t_hdshift,
+	hdtoi = t_hdtoi,
+      dematch = t_dematch,
+     selftest = t_selftest
diff --git a/noao/imred/echelle/Revisions b/noao/imred/echelle/Revisions
new file mode 100644
index 00000000..1ba3c451
--- /dev/null
+++ b/noao/imred/echelle/Revisions
@@ -0,0 +1,247 @@
+.help revisions Jun88 noao.imred.echelle
+.nf
+=======
+V2.12.3
+=======
+
+imred$echelle/echelle.cl
+    With the change of SCOMBINE to a separate executable the package
+    file needed to be updated.  (1/19/05)
+
+=======
+V2.12.2
+=======
+
+imred$echelle/doc/ecidentify.hlp
+    Fixed some minor typos in the function description section.
+    (8/26/03, Valdes)
+
+=======
+V2.12.1
+=======
+
+=====
+V2.12
+=====
+
+imred$echelle/standard.par
+    Added blackbody query parameters.  (5/2/02, Valdes)
+
+imred$echelle/doc/ecidentify.hlp
+    Added a description of how to evaluate the dispersion functions.
+    (4/20/01, Valdes)
+
+imred$echelle/doc/dofoe.hlp
+    Modified to explain that this task may be used with a single fiber.
+    (11/21/00, Valdes)
+
+========
+V2.11.3a
+========
+
+imred$echelle/doc/ecidentify.hlp
+    Fixed minor formating problem. (4/22/99, Valdes)
+
+=====
+V2.11
+=====
+
+imred$echelle/echelle.cl
+imred$echelle/echelle.men
+    Added sapertures to the pacakge.  (12/4/97, Valdes)
+
+=====
+V2.11
+=====
+
+imred$echelle/demos/mkdoecslit.cl
+imred$echelle/demos/mkdofoe.cl
+    Made the ARTDATA package parameters explicit (4/15/97, Valdes)
+
+imred$echelle/demos/xgdoecslit.dat
+    The test now includes batch processing.  (10/3/96, Valdes)
+
+imred$echelle/echelle.cl
+    Increased the minimum min_lenuserarea from 40000 to 100000.
+    (7/31/96, Valdes)
+
+imred$echelle/demos/mkdoecslit.cl
+    Added a flat field.  (11/6/94, Valdes)
+
+imred$echelle/*
+    Further updates for WCS version of ONEDSPEC. (7/24/91, Valdes)
+
+imred$echelle/echelle.cl
+imred$echelle/echelle.par
+imred$echelle/echelle.men
+imred$echelle/echelle.hd
+    The package was updated for V3 of APEXTRACT and ONEDSPEC.  All parameter
+    files are now part of those packages and now local copies are used.
+    Some tasks have disappeared such as APIO and ECSELECT and a number of
+    others have been added.
+
+imred$echelle/ecbplot.cl -
+imred$echelle/doc/ecbplot.hlp -
+imred$echelle/echelle.cl
+imred$echelle/echelle.hd
+imred$echelle/echelle.men
+    The generic task BPLOT replaces ECBPLOT.  (8/24/90, Valdes)
+
+============================
+V3 of APEXTRACT and ONEDSPEC
+============================
+
+imred$echelle/doc/ecreidentify.hlp
+    The refit option now maintains the order offset of the reference.
+    (6/12/90, Valdes)
+
+====
+V2.9
+====
+
+imred$echelle/ecbplot.cl
+    Added a missing parameter declaration for "cur".  (10/27/89, Valdes)
+
+====
+V2.8
+====
+
+imred$echelle/eccontinuum.par +
+imred$echelle/doc/eccontinuum.hlp +
+imred$echelle/echelle.cl
+imred$echelle/echelle.men
+imred$echelle/echelle.hd
+    Added the hooks for the new eccontinuum.  The executable is in
+    onedspec$t_ecctm.x.  (6/2/89, Seaman)
+
+imred$echelle/ecbplot.cl +
+imred$echelle/doc/ecbplot.hlp +
+imred$echelle/echelle.cl
+imred$echelle/echelle.men
+imred$echelle/echelle.hd
+    Added the new script and removed bplot.  (6/2/89, Seaman)
+
+imred$echelle/standard.par
+    Removed ennumerated list.  (4/10/89, Valdes)
+
+imred$echelle/echelle.cl
+imred$echelle/echelle.men
+imred$echelle/specplot.par+
+	Task SPECPLOT added.  (4/3/89 ShJ)
+
+imred$echelle/ecselect.par +
+imred$echelle/doc/ecselect.hlp +
+imred$echelle/echelle.cl
+imred$echelle/echelle.men
+imred$echelle/echelle.hd
+    Added a new task ECSELECT to select and extract apertures from
+    echelle format spectra.  (3/8/89, Valdes)
+
+imred$echelle/apscatter.par +
+imred$echelle/apscat1.par +
+imred$echelle/apscat2.par +
+imred$echelle/echelle.cl
+imred$echelle/echelle.men
+    Added a new task, APSCATTER, to fit and subtract scattered light.
+    It includes two hidden psets, APSCAT1 and APSCAT2.  (3/3/89, Valdes)
+
+imred$echelle/doc/ecidentify.hlp
+    Add a little discussion concerning the speed advantage of the 'o'
+    fit compared to the 'f' fit. (2/2/89, Valdes)
+
+noao$imred/echelle/
+    Davis, Oct 31, 1988
+    The tasks ecbplot and eccontinuum and the hidden task _enranges were
+    added to the echelle package. These tasks were written by Rob
+    Seaman.
+
+imred$echelle/echelle.cl
+imred$echelle/echelle.par
+imred$echelle/echelle.men
+imred$echelle/ecdispcor.par +
+imred$echelle/ecidentify.par +
+imred$echelle/ecreidentify.par +
+imred$echelle/refspectra.par +
+imred$echelle/dispcor.par -
+imred$echelle/identify.par -
+imred$echelle/reidentify.par -
+    New version of this package using new echelle tools instead of ONEDSPEC
+    tools.  (4/7/88 Valdes)
+
+================================================================================
+
+noao$imred/echelle/reidentify.par
+    Valdes, Jan 4, 1988
+    Updated parameter file for new REIDENTIFY parameter.
+
+noao$imred/echelle/echelle.cl
+noao$imred/echelle/echelle.men
+noao$imred/echelle/apnormalize.par +
+    Added the APNORMALIZE task to the package. (fv 7/1/87)
+
+noao$imred/echelle/dispcor.par
+    Valdes, March 5, 1987
+    1.  The DISPCOR default parameter file has been updated because of
+	changes to the task; most notable being that wstart and wpc are
+	list structured.
+
+noao$imred/echelle/echelle.cl
+noao$imred/echelle/echelle.men
+noao$imred/echelle/shedit.par +
+    Valdes, October 6, 1986
+    1.  Added new task SHEDIT.
+
+noao$imred/echelle/identify.par
+    Valdes, October 3, 1986
+    1.  Added new IDENTIFY parameter "threshold".
+
+noao$imred/echelle/echelle.cl
+noao$imred/echelle/echelle.men
+noao$imred/echelle/apdefine.par -
+noao$imred/echelle/extract.par -
+noao$imred/echelle/trace.par -
+    Valdes, September 16, 1986
+    1.  Package modified to use the new APEXTRACT package.
+    2.  Deleted obsolete files
+
+noao$imred/echelle/echelle.hd
+noao$imred/echelle/echelle.men
+noao$imred/echelle/doc/Tutorial.hlp +
+    Valdes, August 18, 1986:
+    1.  Added prototype tutorial document to the ECHELLE package.
+     
+====================================
+Version 2.3 Release, August 18, 1986
+====================================
+
+echelle:  Valdes, July 3, 1986:
+    1.  IDENTIFY parameter file updated to reflect new name for line list.
+
+=====================================
+STScI Pre-release and SUN 2.3 Release
+=====================================
+
+echelle:  Valdes, June 2, 1986:
+    1.  New APEXTRACT tasks defined in package.
+
+echelle:  Valdes, May 12, 1986:
+    1.  SPLOT updated.  New parameters XMIN, XMAX, YMIN, YMAX.
+
+echelle:  Valdes, April 7, 1986:
+    1.  Package parameter file changed to delete latitude.
+    2.  DISPCOR latitude parameter now obtained from OBSERVATORY.
+
+echelle:  Valdes, March 27, 1986:
+    1.  New task SETDISP added.
+    2.  APEXTRACT tasks defined in ECHELLE package instead of loaded from
+	TWODSPEC$APEXTRACT.
+
+===========
+Release 2.2
+===========
+From Valdes December 31, 1985:
+
+1.  Tasks FLATFIT, FLATDIV, and EXTRACT have been removed from the ECHELLE
+package.  The TWODSPEC package containing the task EXTRACT is loaded with
+the ECHELLE package.
+.endhelp
diff --git a/noao/imred/echelle/calibrate.par b/noao/imred/echelle/calibrate.par
new file mode 100644
index 00000000..532ca60e
--- /dev/null
+++ b/noao/imred/echelle/calibrate.par
@@ -0,0 +1,13 @@
+# CALIBRATE parameter file
+
+input,s,a,,,,Input spectra to calibrate
+output,s,a,,,,Output calibrated spectra
+extinct,b,h,yes,,,Apply extinction correction?
+flux,b,h,yes,,,Apply flux calibration?
+extinction,s,h,)_.extinction,,,Extinction file
+observatory,s,h,)_.observatory,,,Observatory of observation
+ignoreaps,b,h,no,,,Ignore aperture numbers in flux calibration?
+sensitivity,s,h,"sens",,,Image root name for sensitivity spectra
+fnu,b,h,no,,,Create spectra having units of FNU?
+airmass,r,q,,1.,,Airmass
+exptime,r,q,,,,Exposure time (seconds)
diff --git a/noao/imred/echelle/demos/demoarc.dat b/noao/imred/echelle/demos/demoarc.dat
new file mode 100644
index 00000000..fa0a179d
--- /dev/null
+++ b/noao/imred/echelle/demos/demoarc.dat
@@ -0,0 +1,38 @@
+    OBJECT  = 'First comp        '  /  object name
+    OBSERVAT= 'KPNO              '  /  observatory
+    OBSERVER= 'Massey            '  /  observers
+    COMMENTS= 'Final New Ice     '  /  comments
+    EXPTIME =                  60.  /  actual integration time
+    DARKTIME=                  60.  /  total elapsed time
+    IMAGETYP= 'comp              '  /  object, dark, bias, etc.
+    DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+    UT      = '12:11:30.00       '  /  universal time
+    ST      = '09:04:54.00       '  /  sidereal time
+    RA      = '06:37:02.00       '  /  right ascension
+    DEC     = '06:09:03.00       '  /  declination
+    EPOCH   =               1991.9  /  epoch of ra and dec
+    ZD      = '48.760            '  /  zenith distance
+    AIRMASS =                   0.  /  airmass
+    TELESCOP= 'kpcdf             '  /  telescope name
+    DETECTOR= 'te1k              '  /  detector
+    PREFLASH=                    0  /  preflash time, seconds
+    GAIN    =                  5.4  /  gain, electrons per adu
+    DWELL   =                    5  /  sample integration time
+    RDNOISE =                  3.5  /  read noise, electrons per adu
+    DELAY0  =                    0  /  time delay after each pixel
+    DELAY1  =                    0  /  time delay after each row
+    CAMTEMP =                 -111  /  camera temperature
+    DEWTEMP =                 -183  /  dewar temperature
+    CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+    ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+    CCDSUM  = '1 1               '  /  on chip summation
+    INSTRUME= 'test              '  /  instrument
+    APERTURE= '250micron slit    '  /  aperture
+    TVFILT  = '4-96              '  /  tv filter
+    DISPAXIS= '2                 '  /  dispersion axis
+    GRATPOS =               4624.3  /  grating position
+    TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+    OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+    ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+    CCDMEAN =              179.398
+    CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/echelle/demos/demoobj.dat b/noao/imred/echelle/demos/demoobj.dat
new file mode 100644
index 00000000..78f3b9ad
--- /dev/null
+++ b/noao/imred/echelle/demos/demoobj.dat
@@ -0,0 +1,37 @@
+    OBJECT  = 'V640Mon 4500      '  /  object name
+    OBSERVAT= 'KPNO              '  /  observatory
+    OBSERVER= 'Massey            '  /  observers
+    COMMENTS= 'Final New Ice     '  /  comments
+    EXPTIME =                1200.  /  actual integration time
+    DARKTIME=                1200.  /  total elapsed time
+    IMAGETYP= 'object            '  /  object, dark, bias, etc.
+    DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+    UT      = '12:19:55.00       '  /  universal time
+    ST      = '09:13:15.00       '  /  sidereal time
+    RA      = '06:37:02.00       '  /  right ascension
+    DEC     = '06:08:52.00       '  /  declination
+    EPOCH   =               1991.9  /  epoch of ra and dec
+    ZD      = '44.580            '  /  zenith distance
+    AIRMASS =                   0.  /  airmass
+    TELESCOP= 'kpcdf             '  /  telescope name
+    DETECTOR= 'te1k              '  /  detector
+    PREFLASH=                    0  /  preflash time, seconds
+    GAIN    =                  5.4  /  gain, electrons per adu
+    DWELL   =                    5  /  sample integration time
+    RDNOISE =                  3.5  /  read noise, electrons per adu
+    DELAY0  =                    0  /  time delay after each pixel
+    DELAY1  =                    0  /  time delay after each row
+    CAMTEMP =                 -111  /  camera temperature
+    DEWTEMP =                 -183  /  dewar temperature
+    CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+    ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+    CCDSUM  = '1 1               '  /  on chip summation
+    INSTRUME= 'test              '  /  instrument
+    APERTURE= '250micron slit    '  /  aperture
+    TVFILT  = '4-96              '  /  tv filter
+    DISPAXIS= '2                 '  /  dispersion axis
+    GRATPOS =               4624.3  /  grating position
+    TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+    OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+    ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+    CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/echelle/demos/demos.cl b/noao/imred/echelle/demos/demos.cl
new file mode 100644
index 00000000..00033829
--- /dev/null
+++ b/noao/imred/echelle/demos/demos.cl
@@ -0,0 +1,20 @@
+# DEMOS -- Run specified demo provided a demo file exists.
+
+procedure demos (demoname)
+
+file	demoname	{prompt="Demo name"}
+
+begin
+	file	demo, demofile
+
+	if ($nargs == 0 && mode != "h")
+	    type ("demos$demos.men")
+	demo = demoname
+	demofile = "demos$" // demo // ".cl"
+	if (access (demofile)) {
+	    task $demo=(demofile)
+	    demo
+#	    cl (< demofile)
+	} else
+	    error (1, "Unknown demo " // demo)
+end
diff --git a/noao/imred/echelle/demos/demos.men b/noao/imred/echelle/demos/demos.men
new file mode 100644
index 00000000..09d41022
--- /dev/null
+++ b/noao/imred/echelle/demos/demos.men
@@ -0,0 +1,7 @@
+	MENU of ECHELLE Demonstrations
+
+   mkdoecslit - Make test echelle slit data (3 orders, 100x256)
+     doecslit - Quick test of DOECSLIT (small images, no comments, no delays)
+
+      mkdofoe - Make test FOE data (3 orders, 100x256)
+        dofoe - Quick test of DOFOE (small images, no comments, no delays)
diff --git a/noao/imred/echelle/demos/demos.par b/noao/imred/echelle/demos/demos.par
new file mode 100644
index 00000000..4181ed59
--- /dev/null
+++ b/noao/imred/echelle/demos/demos.par
@@ -0,0 +1,2 @@
+demoname,f,a,"",,,"Demo name"
+mode,s,h,"ql",,,
diff --git a/noao/imred/echelle/demos/demostd.dat b/noao/imred/echelle/demos/demostd.dat
new file mode 100644
index 00000000..7588f3fa
--- /dev/null
+++ b/noao/imred/echelle/demos/demostd.dat
@@ -0,0 +1,36 @@
+    OBJECT  = 'V640Mon 4500      '  /  object name
+    OBSERVAT= 'KPNO              '  /  observatory
+    OBSERVER= 'Massey            '  /  observers
+    COMMENTS= 'Final New Ice     '  /  comments
+    EXPTIME =                1200.  /  actual integration time
+    DARKTIME=                1200.  /  total elapsed time
+    IMAGETYP= 'object            '  /  object, dark, bias, etc.
+    DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+    UT      = '12:19:55.00       '  /  universal time
+    ST      = '09:13:15.00       '  /  sidereal time
+    RA      = '06:37:02.00       '  /  right ascension
+    DEC     = '06:08:52.00       '  /  declination
+    EPOCH   =               1991.9  /  epoch of ra and dec
+    ZD      = '44.580            '  /  zenith distance
+    AIRMASS =                   0.  /  airmass
+    TELESCOP= 'kpcdf             '  /  telescope name
+    DETECTOR= 'te1k              '  /  detector
+    PREFLASH=                    0  /  preflash time, seconds
+    GAIN    =                  5.4  /  gain, electrons per adu
+    DWELL   =                    5  /  sample integration time
+    RDNOISE =                  3.5  /  read noise, electrons per adu
+    DELAY0  =                    0  /  time delay after each pixel
+    DELAY1  =                    0  /  time delay after each row
+    CAMTEMP =                 -111  /  camera temperature
+    DEWTEMP =                 -183  /  dewar temperature
+    CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+    ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+    CCDSUM  = '1 1               '  /  on chip summation
+    INSTRUME= 'test              '  /  instrument
+    APERTURE= '250micron slit    '  /  aperture
+    TVFILT  = '4-96              '  /  tv filter
+    GRATPOS =               4624.3  /  grating position
+    TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+    OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+    ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+    CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/echelle/demos/doecslit.cl b/noao/imred/echelle/demos/doecslit.cl
new file mode 100644
index 00000000..17483089
--- /dev/null
+++ b/noao/imred/echelle/demos/doecslit.cl
@@ -0,0 +1,21 @@
+# Create demo data if needed.
+
+task $mkdoecslit=demos$mkdoecslit.cl
+mkdoecslit
+imdel ("demo*.??h,sens*", verify=no, >& "dev$null")
+imcopy ("Bdemoobj1", "demoobj1", verbose=no)
+imcopy ("Bdemoobj2", "demoobj2", verbose=no)
+imcopy ("Bdemoarc", "demoarc", verbose=no)
+imcopy ("Bdemostd", "demostd", verbose=no)
+
+unlearn doecslit apscat1 apscat2
+sparams.extras = no
+sparams.bandwidth = 3
+sparams.bandsep = 3
+delete ("demologfile,demoplotfile,std", verify=no, >& "dev$null")
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgdoecslit.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/echelle/demos/dofoe.cl b/noao/imred/echelle/demos/dofoe.cl
new file mode 100644
index 00000000..9a7d0da3
--- /dev/null
+++ b/noao/imred/echelle/demos/dofoe.cl
@@ -0,0 +1,13 @@
+# Create demo data if needed.
+
+task $mkdofoe=demos$mkdofoe.cl
+mkdofoe
+
+unlearn dofoe params
+delete ("demologfile,demoplotfile", verify=no, >& "dev$null")
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgdofoe.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/echelle/demos/ecdofoe.dat b/noao/imred/echelle/demos/ecdofoe.dat
new file mode 100644
index 00000000..edaa050b
--- /dev/null
+++ b/noao/imred/echelle/demos/ecdofoe.dat
@@ -0,0 +1,33 @@
+# Tue 10:20:50 16-Nov-93
+begin	ecidentify demoarc.ec
+	id	demoarc.ec
+	task	ecidentify
+	image	demoarc.ec
+	features	8
+		  1  116    78.35   4965.0792   4965.0795   4.0  1  1
+		  2  115    77.21    5009.335   5009.3344   4.0  1  1
+		  2  115   227.04   5019.8062   5019.8062   4.0  1  1
+		  3  114    11.56   5049.8052    5049.796   4.0  1  1
+		  3  114    25.44   5050.7874   5050.7842   4.0  1  1
+		  3  114    89.66   5055.3289   5055.3473   4.0  1  1
+		  3  114   184.46   5062.0332   5062.0371   4.0  1  1
+		  3  114   225.77   5064.9549   5064.9454   4.0  1  1
+	offset	117
+	slope	-1
+	niterate 3
+	lowreject 3.
+	highreject 3.
+	coefficients	12
+		1.
+		2.
+		2.
+		1.
+		1.
+		256.
+		114.
+		116.
+		576485.7847819133
+		1024.71926036047
+		-134.8425017381852
+		-3.224100491592999
+
diff --git a/noao/imred/echelle/demos/mkdoecslit.cl b/noao/imred/echelle/demos/mkdoecslit.cl
new file mode 100644
index 00000000..1d5fa14b
--- /dev/null
+++ b/noao/imred/echelle/demos/mkdoecslit.cl
@@ -0,0 +1,137 @@
+# Create test data if needed.
+
+procedure mkdoecslit ()
+begin
+
+	artdata
+	artdata.nxc = 5
+	artdata.nyc = 5
+	artdata.nxsub = 10
+	artdata.nysub = 10
+	artdata.nxgsub = 5
+	artdata.nygsub = 5
+	artdata.dynrange = 100000.
+	artdata.psfrange = 10.
+	artdata.ranbuf = 0
+
+	if (!access ("Bdemoflat." // envget ("imtype"))) {
+	    print ("Creating example demoflat ...")
+	    mkechelle ("Bdemoflat", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demoobj.dat", list=no, make=yes,
+		comments=no, xc=INDEF, yc=INDEF, pixsize=0.027,
+		profile="slit", width=20., scattered=10., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=20000., temperature=5700., lines="",
+		nrandom=0, peak=5.0, sigma=0.1, seed=2, >& "dev$null")
+	    mknoise ("Bdemoflat", output="", ncols=512, nlines=512, title="",
+		header="", background=0., gain=1., rdnoise=10., poisson=no,
+		seed=5, cosrays="", ncosrays=0, energy=30000., radius=0.5,
+		ar=1., pa=0., comments=no)
+	}
+
+	if (!access ("Bdemoobj1." // envget ("imtype"))) {
+	    print ("Creating example demoobj1 ...")
+	    mkechelle ("Bdemoobj1", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demoobj.dat", list=no, make=yes,
+		comments=no, xc=INDEF, yc=INDEF, pixsize=0.027,
+		profile="gaussian", width=4., scattered=25., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=500., temperature=7700., lines="",
+		nrandom=100, peak=-0.2, sigma=0.3, seed=1, >& "dev$null")
+	    mkechelle ("Bdemoobj1", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demoobj.dat", list=no, make=yes,
+		comments=no, xc=INDEF, yc=INDEF, pixsize=0.027,
+		profile="slit", width=20., scattered=10., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=200., temperature=5700., lines="",
+		nrandom=20, peak=5.0, sigma=0.1, seed=2, >& "dev$null")
+	    mknoise ("Bdemoobj1", output="", ncols=512, nlines=512, title="",
+		header="", background=0., gain=1., rdnoise=10., poisson=yes,
+		seed=1, cosrays="", ncosrays=0, energy=30000., radius=0.5,
+		ar=1., pa=0., comments=no)
+	}
+
+	if (!access ("Bdemoobj2." // envget ("imtype"))) {
+	    print ("Creating example demoobj2 ...")
+	    mkechelle ("Bdemoobj2", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demoobj.dat", list=no, make=yes,
+		comments=no, xc=INDEF, yc=INDEF, pixsize=0.027,
+		profile="gaussian", width=4., scattered=25., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=10., z=no, continuum=500., temperature=7700., lines="",
+		nrandom=100, peak=-0.2, sigma=0.3, seed=1, >& "dev$null")
+	    mkechelle ("Bdemoobj2", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demoobj.dat", list=no, make=yes,
+		comments=no, xc=INDEF, yc=INDEF, pixsize=0.027,
+		profile="slit", width=20., scattered=10., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=200., temperature=5700., lines="",
+		nrandom=20, peak=5.0, sigma=0.1, seed=2, >& "dev$null")
+	    mknoise ("Bdemoobj2", output="", ncols=512, nlines=512, title="",
+		header="", background=0., gain=1., rdnoise=10., poisson=yes,
+		seed=4, cosrays="", ncosrays=0, energy=30000., radius=0.5,
+		ar=1., pa=0., comments=no)
+	}
+
+	if (!access ("Bdemostd." // envget ("imtype"))) {
+	    print ("Creating example demostd ...")
+	    mkechelle ("Bdemostd", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demostd.dat", list=no, make=yes,
+		comments=no, xc=INDEF, yc=INDEF, pixsize=0.027,
+		profile="gaussian", width=4., scattered=25., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=500., temperature=10000., lines="",
+		nrandom=0, peak=-0.5, sigma=0.5, seed=3, >& "dev$null")
+	    mkechelle ("Bdemostd", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demostd.dat", list=no, make=yes,
+		comments=no, xc=INDEF, yc=INDEF, pixsize=0.027,
+		profile="slit", width=20., scattered=10., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=200., temperature=5700., lines="",
+		nrandom=20, peak=5.0, sigma=0.1, seed=2, >& "dev$null")
+	    mknoise ("Bdemostd", output="", ncols=512, nlines=512, title="",
+		header="", background=0., gain=1., rdnoise=10., poisson=yes,
+		seed=2, cosrays="", ncosrays=0, energy=30000., radius=0.5,
+		ar=1., pa=0., comments=no)
+	}
+
+	if (!access ("Bdemoarc." // envget ("imtype"))) {
+	    print ("Creating example demoarc ...")
+	    mkechelle ("Bdemoarc", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demoarc.dat", list=no, make=yes,
+		comments=no, xc=INDEF, yc=INDEF, pixsize=0.027,
+		profile="slit", width=20., scattered=10., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=20., temperature=0.,
+		lines="mkexamples$ecthorium.dat", nrandom=0, peak=-0.5,
+		sigma=0.05, seed=1, >& "dev$null")
+	    mknoise ("Bdemoarc", output="", ncols=512, nlines=512, title="",
+		header="", background=0., gain=1., rdnoise=10., poisson=yes,
+		seed=3, cosrays="", ncosrays=0, energy=30000., radius=0.5,
+		ar=1., pa=0., comments=no)
+	}
+end
diff --git a/noao/imred/echelle/demos/mkdofoe.cl b/noao/imred/echelle/demos/mkdofoe.cl
new file mode 100644
index 00000000..6a18aaea
--- /dev/null
+++ b/noao/imred/echelle/demos/mkdofoe.cl
@@ -0,0 +1,103 @@
+# Create test data if needed.
+
+procedure mkdofoe ()
+begin
+
+	artdata
+	artdata.nxc = 5
+	artdata.nyc = 5
+	artdata.nxsub = 10
+	artdata.nysub = 10
+	artdata.nxgsub = 5
+	artdata.nygsub = 5
+	artdata.dynrange = 100000.
+	artdata.psfrange = 10.
+	artdata.ranbuf = 0
+
+	if (!access ("demoobj." // envget ("imtype"))) {
+	    print ("Creating example demoobj ...")
+	    mkechelle ("demoobj", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demoobj.dat", list=no, make=yes,
+		comments=no, xc=50, yc=50.1, pixsize=0.027,
+		profile="gaussian", width=4., scattered=25., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=500., temperature=7700., lines="",
+		nrandom=100, peak=-0.2, sigma=0.3, seed=1, >& "dev$null")
+	    mkechelle ("demoobj", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demoobj.dat", list=no, make=yes,
+		comments=no, xc=60, yc=51.6, pixsize=0.027,
+		profile="gaussian", width=4., scattered=0., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=4.95, temperature=0.,
+		lines="mkexamples$ecthorium.dat", nrandom=0, peak=-0.5,
+		sigma=0.05, seed=1, >& "dev$null")
+	    mknoise ("demoobj", output="", ncols=512, nlines=512, title="",
+		header="", background=0., gain=1., rdnoise=10., poisson=yes,
+		seed=1, cosrays="", ncosrays=0, energy=30000., radius=0.5,
+		ar=1., pa=0., comments=no)
+	}
+
+	if (!access ("demoflat." // envget ("imtype"))) {
+	    print ("Creating example demoflat ...")
+	    mkechelle ("demoflat", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demoobj.dat", list=no, make=yes,
+		comments=no, xc=50, yc=50.2, pixsize=0.027,
+		profile="gaussian", width=4., scattered=25., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=1000., temperature=5700., lines="",
+		nrandom=0, peak=-0.2, sigma=0.3, seed=1, >& "dev$null")
+	    mkechelle ("demoflat", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demoobj.dat", list=no, make=yes,
+		comments=no, xc=60, yc=51.7, pixsize=0.027,
+		profile="gaussian", width=4., scattered=25., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=990., temperature=7700., lines="",
+		nrandom=0, peak=-0.2, sigma=0.3, seed=1, >& "dev$null")
+	    mknoise ("demoflat", output="", ncols=512, nlines=512, title="",
+		header="", background=0., gain=1., rdnoise=10., poisson=yes,
+		seed=2, cosrays="", ncosrays=0, energy=30000., radius=0.5,
+		ar=1., pa=0., comments=no)
+	}
+
+	if (!access ("demoarc." // envget ("imtype"))) {
+	    print ("Creating example demoarc ...")
+	    mkechelle ("demoarc", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demoarc.dat", list=no, make=yes,
+		comments=no, xc=50, yc=50, pixsize=0.027,
+		profile="gaussian", width=4., scattered=0., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=10., temperature=0.,
+		lines="mkexamples$ecthorium.dat", nrandom=0, peak=-0.5,
+		sigma=0.05, seed=1, >& "dev$null")
+	    mkechelle ("demoarc", yes, ncols=100, nlines=256, norders=21,
+		title="Artificial Echelle Spectrum",
+		header="demos$demoarc.dat", list=no, make=yes,
+		comments=no, xc=60, yc=51.5, pixsize=0.027,
+		profile="gaussian", width=4., scattered=0., f=590., gmm=31.6,
+		blaze=63., theta=69., order=112, wavelength=5007.49,
+		dispersion=2.61, cf=590., cgmm=226., cblaze=4.53,
+		ctheta=-11.97, corder=1, cwavelength=6700., cdispersion=70.,
+		rv=0., z=no, continuum=9.9, temperature=0.,
+		lines="mkexamples$ecthorium.dat", nrandom=0, peak=-0.5,
+		sigma=0.05, seed=1, >& "dev$null")
+	    mknoise ("demoarc", output="", ncols=512, nlines=512, title="",
+		header="", background=0., gain=1., rdnoise=10., poisson=yes,
+		seed=3, cosrays="", ncosrays=0, energy=30000., radius=0.5,
+		ar=1., pa=0., comments=no)
+	}
+end
diff --git a/noao/imred/echelle/demos/xgdoecslit.dat b/noao/imred/echelle/demos/xgdoecslit.dat
new file mode 100644
index 00000000..3c59563a
--- /dev/null
+++ b/noao/imred/echelle/demos/xgdoecslit.dat
@@ -0,0 +1,105 @@
+\O=NOAO/IRAF IRAFX valdes@puppis Mon 14:58:37 15-Nov-93
+\T=xgterm
+\G=xgterm
+epar\sechel\n
+\r
+onedstds$spechayescal/\r
+\r
+\r
+\r
+\r
+\r
+y\r
+demologfile\r
+demoplotfile\r
+^Z
+epar\sdoecslit\n
+demoobj1,demoobj2\r
+demostd\r
+demoarc\r
+\r
+demostd\r
+rdnoise\r
+gain\r
+\r
+3\r
+\r
+\r
+y\r
+y\r
+y\r
+\r
+\r
+scat\r
+y\r
+^Z
+doecslit\sredo+\n
+\n
+\n
+b/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\r
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+N\r
+n\n
+n\n
+\n
+\n
+\n
+\n
+:/<-5\s\s\s\s/=(.\s=\r sample\s9:92\r
+f/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+i/<-5\s\s\s\s/=(.\s=\r
+m200.\s\s\s\s20=*,.\r 4965\r
+m3+0*\s\s\s\s3,&*1)\r 4966\r
+k/<-5\s\s\s\s/=(.\s=\r
+m(?3"\s\s\s\s(?+&<:\r 5002\r
+m+\s3$\s\s\s\s+\s:&:-\r 5003.6\r
+m2*3$\s\s\s\s2+.&:-\r 5009.3\r
+k/<-5\s\s\s\s/=(.\s=\r
+m%937\s\s\s\s%90&"$\r 5044.7\r
+m,,3&\s\s\s\s,,/&7?\r 5049.8\r
+m9,4'\s\s\s\s9,?%,)\r 5059.8\r
+m3-4"\s\s\s\s3.\s%32\r 5055.3\r
+f/<-5\s\s\s\s/=(.\s=\r
+:/<-5\s\s\s\s/=(.\s=\r xo\s4\r
+o/<-5\s\s\s\s/=(.\s=\r 114\r
+q/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+f/<-5\s\s\s\s/=(.\s=\r
+o/<-5\s\s\s\s/=(.\s=\r 114\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+hz14\n
+y\n
+q/<-5\s\s\s\s/=(.\s=\r
+NO!\r
+y\n
+q/<-5\s\s\s\s/=(.\s=\r
+N\r
+\n
+1\n
+q/<-5\s\s\s\s/=(.\s=\r
+\n
+2\n
+q/<-5\s\s\s\s/=(.\s=\r
+\n
+2\n
+q/<-5\s\s\s\s/=(.\s=\r
+imdel\sdemoobj1.ec\n
+del\sdatabase/apdemoobj1\n
+doecslit\squick+\n
+\n
+imdel\sdemoobj1.ec\n
+doecslit\sbatch+\ssplot-\n
+\n
diff --git a/noao/imred/echelle/demos/xgdofoe.dat b/noao/imred/echelle/demos/xgdofoe.dat
new file mode 100644
index 00000000..bd436909
--- /dev/null
+++ b/noao/imred/echelle/demos/xgdofoe.dat
@@ -0,0 +1,50 @@
+\O=NOAO/IRAF IRAFX valdes@puppis Mon 14:58:37 15-Nov-93
+\T=xgterm
+\G=xgterm
+epar\sechelle\n
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+y\r
+demologfile\r
+demoplotfile\r
+^Z
+epar\sdofoe\n
+demoobj\r
+demoflat\r
+demoflat\r
+demoarc\r
+\r
+rdnoise\r
+gain\r
+\r
+3\r
+5\r
+^Z
+dofoe\sredo+\n
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\r
+i/<-5\s\s\s\s/=(.\s=\r
+m++4'\s\s\s\s++8%,)\r 4965\r
+k/<-5\s\s\s\s/=(.\s=\r
+m+)4'\s\s\s\s+)=%,)\r 5009\r
+m9!4'\s\s\s\s9""%,)\r 5020\r
+k/<-5\s\s\s\s/=(.\s=\r
+m%'5'\s\s\s\s%'*$#!\r 5049.8\r
+m&15(\s\s\s\s&1%$\s4\r 5050.8\r
+m,.55\s\s\s\s,.)#/4\r 5055.3\r
+m5#7\s\s\s\s\s5$2!7:\r 5062\r
+m8=78\s\s\s\s8>.\s8)\r 5064.9\r
+f/<-5\s\s\s\s/=(.\s=\r
+o/<-5\s\s\s\s/=(.\s=\r 114\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
diff --git a/noao/imred/echelle/doc/Tutorial.hlp b/noao/imred/echelle/doc/Tutorial.hlp
new file mode 100644
index 00000000..655ca307
--- /dev/null
+++ b/noao/imred/echelle/doc/Tutorial.hlp
@@ -0,0 +1,184 @@
+.help Tutorial Aug86 "Echelle Tutorial"
+.ih
+TOPICS
+The echelle tutorial consists of a number of different topics.  To obtain help
+on a particular topic type "tutor topic" where the topic is one of the
+following:
+
+.nf
+			TOPICS
+
+         topics - List of topics
+       overview - An overview of the echelle reduction process
+	 dataio - Reading and writing data tapes
+        tracing - Tracing the positions of the orders
+     extraction - Extracting one or two dimensional spectra
+     references - Additional references
+	    all - Print all of the tutorial
+.fi
+
+The topics are kept brief and describe the simplest operations.  More
+sophisticated discussions are available for all the tasks in the printed
+documentation and through the on-line \fBhelp\fR facility; i.e. "help taskname".
+.ih
+OVERVIEW
+The \fBechelle\fR package provides for the extraction of the orders from
+two dimensional echelle images into one dimensional spectra.  After extraction
+the one dimensional spectra are wavelength and flux calibrated.  The usual
+flow of the reductions is
+.ls (1)
+Read data from tape.
+.le
+.ls (2)
+Set the dispersion axis in the image headers using the task \fBsetdisp\fR.
+This is required by many of the tasks which follow.
+.le
+.ls (3)
+Trace one or more images to define the positions of the orders within the
+two dimensional format.
+.le
+.ls (4)
+Extract the orders into one dimensional spectra.
+.le
+.ls (5)
+Use arc calibration spectra to determine wavelength solutions.
+.le
+.ls (6)
+Apply the wavelength solutions to the other spectra and rebin the spectra
+into linear or logarithmic wavelength intervals.
+.le
+.ls (7)
+Determine flux calibrations using standard star observations.
+.le
+.ls (8)
+Apply the flux calibrations to the other object spectra.
+.le
+.ls (9)
+Save the reductions as FITS images and make plots of the spectra.
+.le
+
+There are many variations on these steps possible with the great flexibility
+of the reduction tools at your disposal.  The most important one to mention
+is that the orders may be extracted as two dimensional strips in order to
+apply more complex geometric distortion corrections using the \fBlongslit\fR
+package.
+.ih
+DATAIO
+To read CCD Camera format tapes use \fBrcamera\fR from the \fBmtlocal\fR
+package.  FITS format tapes are read and written with \fBrfits\fR and
+\fBwfits\fR from the \fBdataio\fR package.  Remember you need to
+\fBallocate\fR the tape drive before you can read or write tapes and
+you should \fBdeallocate\fR the tapes when you are through with the
+tape drive.
+
+.nf
+	ec> allocate mta
+	ec> deallocate mta
+	ec> rcamera mta 1-99 ech datatype=r >rcam.log &
+	ec> rfits mta 1-99 ech datatype=r >rfits.log &
+	ec> wfits mta spectra*
+.fi
+.ih
+TRACING
+The positions of the orders across the image dispersion axis as a function
+of position along the dispersion axis are determined by the task \fBtrace\fR.
+There are three steps in tracing an image; defining the initial positions of
+the orders at one point along the dispersion, automatically determining
+the positions at other points in steps from the starting point, and fitting
+smooth curves to the positions as a function of dispersion position.  The
+first and last steps are interactive, at least initially.  After the first
+image other images may be traced noninteractively.
+
+Select an image with narrow, strong profiles and run trace:
+
+	ec> trace imagename
+
+When you are asked if you want to edit the apertures respond with "yes".
+The central cut across the dispersion is graphed.  Position the cursor
+over the first order to be traced and type 'm'.  Adjust the width of the
+extraction aperture with the 'l', 'u', or 'y' keys or specify the lower
+and upper widths explicitly with ":lower value" or ":upper value".
+If background subtraction is to be used type 'b' and set the background
+fitting parameters (see the \fBbackground\fR tutorial)
+Now mark the remaining orders with the 'm' key.  The widths of the
+previous aperture are preserved for each new aperture.  When you are
+satisfied with the marked apertures type 'q'.
+
+The positions of the orders are now traced in steps from the initial point.
+Once the positions have been traced you are asked whether to fit the
+traced apertures interactively.  Respond with "yes".  You will now be
+asked specifically if the first aperture is to be fit.  Respond with "yes"
+again.  The traced positions are graphed along with a fitted curve.  You now
+have many options for adjusting the fit.  The most important one is the
+order which is set by typing ":order value", where value is the desired
+order, and then 'f' to refit the data.  For full information of the
+options see the help for \fBicfit\fR.  When you are satisfied type 'q'.
+
+You are then prompted for the next order.  The previous fitting parameters
+will be used so at this point you may want to just answer "NO" to skip
+the interactive fitting of the other traced orders, though the graphs of the
+fit will still be displayed.
+
+You now have several options about how to define the positions of the
+orders in your other images.
+
+.ls (1)
+You may apply the tracing to all other observations with no
+further tracing.  This is done by specifying the traced image
+as the "reference" in the extraction process.
+.le
+.ls (2)
+You may maintain the same shape of the traces and correct for
+shifts in the positions of the orders across the dispersion
+by recentering each aperture.  This is done
+with the task \fBapedit\fR or the editing switch during extraction
+using the first traced image as the reference.  The apertures are
+recenter using the 'c' key.
+.le
+.ls (3)
+Finally, you may retrace other images either from scratch or
+using the first traced image as the initial reference.  In the latter
+case the tracing may be done noninteractively as a batch process.
+.le
+.ih
+EXTRACTION
+There are two types of extraction; to one dimensional spectra or
+to two dimensional strips.  The second type of extraction is accomplished
+by the task \fBstripextract\fR in the \fBtwodspec.apextract\fR package
+and is used if further reductions using the \fBlongslit\fR package are
+desired.  Normally, however, one ignores the small geometric distortion
+in which curves of constant wavelength differ slightly from the image
+dispersion axis.
+
+Extraction of the traced echelle orders is performed by the task
+\fBsumextract\fR.  The pixels within each aperture at each point along
+the dispersion axis are summed to produce one dimensional spectra, one
+for each order and each extracted image.  The sum may be weighted
+in two ways; "profile" or "variance" weighting.  The variance weighting
+may require that you know the CCD readout noise and photon/ADU conversion.
+For a description of the weights see the help for \fBsumextract\fR
+or the paper "The APEXTRACT Package".  The spectra may also be cleaned
+of cosmic rays and bad pixels at the same time and have a background
+subtracted.  The background subtraction parameters must be set when
+defining the apertures or later using the apedit mode in \fBapedit\fR,
+\fBtrace\fR, or \fBsumextract\fR.  See the tutorial on \fBbackground\fR
+for further information.
+
+Once the extraction parameters have been set simply type
+
+	ec> sumextract images
+
+where images is the list of images to be extracted.  If each image has
+not been traced then a traced reference image should be given.
+One may correct for shifts relative to the traced image by setting the
+switch to edit the apertures and then recentering each aperture before
+extracting.  If there is no aperture editing then the extractions may
+be done as a background or batch process.
+.ih
+REFERENCES
+.ls (1)
+Pilachowski, C. and J. V. Barnes, \fINotes on the IRAF for Reduction of
+Echelle/CCD Data\fR, NOAO Central Computer Services, 1986.  This document
+is also available in the \fBIRAF User Handbook , Vol. 2B -- NOAO Cookbooks\fR.
+.le
+.endhelp
diff --git a/noao/imred/echelle/doc/doecslit.hlp b/noao/imred/echelle/doc/doecslit.hlp
new file mode 100644
index 00000000..7bf69f00
--- /dev/null
+++ b/noao/imred/echelle/doc/doecslit.hlp
@@ -0,0 +1,1230 @@
+.help doecslit Feb93 noao.imred.echelle
+.ih
+NAME
+doecslit -- Echelle slit spectra reduction task
+.ih
+USAGE
+doecslit objects
+.ih
+SUMMARY
+\fBDoecslit\fR subtracts background sky or scattered light, extracts,
+wavelength calibrates, and flux calibrates multiorder echelle slit spectra
+which have been processed to remove the detector characteristics; i.e. CCD
+images have been bias, dark count, and flat field corrected.  The spectra
+should be oriented such that pixels of constant wavelength are aligned with
+the image columns or lines.  Small departures from this alignment are not
+critical resulting in only a small loss of resolution.  Single order
+observations should be reduced with \fBdoslit\fR.
+.ih
+PARAMETERS
+.ls objects
+List of object images to be processed.  Previously processed spectra are
+ignored unless the \fIredo\fR flag is set or the \fIupdate\fR flag is set
+and dependent calibration data has changed.  If the images contain the
+keyword IMAGETYP then only those with a value of "object" or "OBJECT"
+are used and those with a value of "comp" or "COMPARISON" are added
+to the list of arcs.  Extracted spectra are ignored.
+.le
+.ls apref = ""
+Aperture reference spectrum.  This spectrum is used to define the basic
+extraction apertures and is typically a bright star spectrum.
+.le
+.ls arcs = "" (at least one if dispersion correcting)
+List of arc calibration spectra.  These spectra are used to define
+the dispersion functions.  The first spectrum is used to mark lines
+and set the dispersion function interactively and dispersion functions
+for all other arc spectra are derived from it.  If the images contain
+the keyword IMAGETYP then only those with a value of "comp" or
+"COMPARISON" are used.  All others are ignored as are extracted spectra.
+.le
+.ls arctable = "" (optional) (refspectra)
+Table defining which arc spectra are to be assigned to which object
+spectra (see \fBrefspectra\fR).  If not specified an assignment based
+on a header parameter, \fIsparams.sort\fR, such as the Julian date
+is made.
+.le
+.ls standards = "" (at least one if flux calibrating)
+List of standard star spectra.  The standard stars must have entries in
+the calibration database (package parameter \fIechelle.caldir\fR).
+.le
+
+.ls readnoise = 0., gain = 1. (apsum)
+Read out noise in photons and detector gain in photons per data value.
+This parameter defines the minimum noise sigma and the conversion between
+photon Poisson statistics and the data number statistics.  Image header
+keywords (case insensitive) may be specified to obtain the values from the
+image header.
+.le
+.ls datamax = INDEF (apsum.saturation)
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the standard star or
+arc spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.le
+.ls norders = 10 (apfind)
+Number of orders to be found automatically.
+.le
+.ls width = 5. (apedit)
+Approximate full width of the spectrum profiles.  This parameter is used
+to define a width and error radius for the profile centering algorithm,
+and defaults for the aperture limits and background regions.
+.le
+
+.ls dispcor = yes
+Dispersion correct spectra?  This may involve either defining a nonlinear
+dispersion coordinate system in the image header or resampling the
+spectra to uniform linear wavelength coordinates as selected by
+the parameter \fIsparams.linearize\fR.
+.le
+.ls extcor = no
+Extinction correct the spectra?
+.le
+.ls fluxcal = no
+Flux calibrate the spectra using standard star observations?
+.le
+.ls resize = no (apresize)
+Resize the defaults apertures for each object based on the spectrum profile?
+.le
+.ls clean = no (apsum)
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction.  In addition the datamax parameters
+can be useful.
+.le
+.ls trace = yes (non-quicklook mode only) (aptrace)
+Allow tracing each object spectrum separately?  If not set then the trace
+from the aperture reference is used, with recentering to allow for shifts
+across the dispersion.  If set then each object and standard star
+image is retraced.  Retracing is NOT done in quicklook mode.
+.le
+.ls background = "none" (apsum, apscatter)
+Type of background light subtraction.  The choices are "none" for no
+background subtraction, "scattered" for a global scattered light
+subtraction, "average" to average the background within background regions,
+"median" to use the median in background regions, "minimum" to use the
+minimum in background regions, or "fit" to fit across the dispersion using
+the background within background regions.  The scattered light option fits
+and subtracts a smooth global background and modifies the input images.
+This is a slow operation and so is NOT performed in quicklook mode.  The
+other background options are local to each aperture.  The "fit" option uses
+additional fitting parameters from \fBsparams\fR and the "scattered" option
+uses parameters from \fBapscat1\fR and \fBapscat2\fR.
+.le
+.ls splot = no
+Plot the final spectra?  In quicklook mode a noninteractive, stacked plot
+is automatically produced using the task \fBspecplot\fR while in
+non-quicklook mode a query is given and the task \fBsplot\fR is used for
+interactive plotting.
+.le
+.ls redo = no
+Redo operations previously done?  If no then previously processed spectra
+in the objects list will not be processed unless required by the
+update option.
+.le
+.ls update = no
+Update processing of previously processed spectra if the aperture
+reference image, the dispersion reference image, or standard star
+calibration data are changed?
+.le
+.ls quicklook = no
+Extract and calibrate spectra with minimal interaction?  In quicklook mode
+only aperture reference definitions, the initial dispersion function
+solution, and the standard star setup are done interactively.  Scattered
+light subtraction and individual object tracing are not performed.
+Normally the \fIsplot\fR option is set in this mode to produce an automatic
+final spectrum plot for each object.  It is recommended that this mode not be
+used for final reductions.
+.le
+.ls batch = no
+Process spectra as a background or batch job provided there are no interactive
+steps remaining.
+.le
+.ls listonly = no
+List processing steps but don't process?
+.le
+
+.ls sparams = "" (pset)
+Name of parameter set containing additional processing parameters.  This
+parameter is only for indicating the link to the parameter set
+\fBsparams\fR and should not be given a value.  The parameter set may be
+examined and modified in the usual ways (typically with "epar
+sparams" or ":e sparams" from the parameter editor).  The parameters are
+described below.
+.le
+
+.ce
+-- GENERAL PARAMETERS --
+.ls line = INDEF, nsum = 10
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, recentering, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.le
+.ls extras = no (apsum)
+Include raw unweighted and uncleaned spectra, the background spectra, and
+the estimated sigma spectra in a three dimensional output image format.
+See the discussion in the \fBapextract\fR package for further information.
+.le
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+.ls ylevel = 0.05 (apresize)
+Fraction of the peak to set aperture limits during automatic resizing.
+.le
+
+.ce
+-- TRACE PARAMETERS --
+.ls t_step = 10 (aptrace)
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \fInsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.le
+.ls t_function = "spline3", t_order = 2 (aptrace)
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.le
+.ls t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+Default number of rejection iterations and rejection sigma thresholds.
+.le
+
+.ce
+-- BACKGROUND AND SCATTERED LIGHT PARAMETERS --
+.ls b_function = "legendre", b_order = 1 (apsum)
+Default background fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.le
+.ls b_naverage = -100 (apsum)
+Default number of points to average or median.  Positive numbers
+average that number of sequential points to form a fitting point.
+Negative numbers median that number, in absolute value, of sequential
+points.  A value of 1 does no averaging and each data point is used in the
+fit.
+.le
+.ls b_niterate = 0 (apsum)
+Default number of rejection iterations.  If greater than zero the fit is
+used to detect deviant fitting points and reject them before repeating the
+fit.  The number of iterations of this process is given by this parameter.
+.le
+.ls b_low_reject = 3., b_high_reject = 3. (apsum)
+Default background lower and upper rejection sigmas.  If greater than zero
+points deviating from the fit below and above the fit by more than this
+number of times the sigma of the residuals are rejected before refitting.
+.le
+.ls buffer = 1. (apscatter)
+Buffer distance from the edge of any aperture for data to be included
+in the scattered light determination.  This parameter may be modified
+interactively.
+.le
+.ls apscat1 = "", apscat2 = "" (apscatter)
+Parameter sets for the fitting functions across and along the dispersion.
+These parameters are those used by \fBicfit\fR.  These parameters are
+usually set interactively.
+.le
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+.ls weights = "none" (apsum) (none|variance)
+Type of extraction weighting.  Note that if the \fIclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+.ls "none"
+The pixels are summed without weights except for partial pixels at the
+ends.
+.le
+.ls "variance"
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \fIgain\fR and \fIreadnoise\fR
+parameters.
+.le
+.le
+.ls pfit = "fit1d" (apsum and approfile) (fit1d|fit2d)
+Type of profile fitting algorithm to use.  The "fit1d" algorithm is
+preferred except in cases of extreme tilt.
+.le
+.ls lsigma = 3., usigma = 3. (apsum)
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.le
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+.ls threshold = 10. (identify/reidentify)
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.le
+.ls coordlist = "linelist$thar.dat" (ecidentify)
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelist$".
+.le
+.ls match = 1. (ecidentify)
+The maximum difference for a match between the dispersion function computed
+value and a wavelength in the coordinate list.
+.le
+.ls fwidth = 4. (ecidentify)
+Approximate full base width (in pixels) of arc lines.
+.le
+.ls cradius = 10. (reidentify)
+Radius from previous position to reidentify arc line.
+.le
+.ls i_function = "legendre", i_xorder = 3, i_yorder = 3 (ecidentify)
+The default function, function order for the pixel position dependence, and
+function order for the aperture number dependence to be fit to the arc
+wavelengths.  The functions choices are "chebyshev" or "legendre".
+.le
+.ls i_niterate = 3, i_low = 3.0, i_high = 3.0 (ecidentify)
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.le
+.ls refit = yes (ecreidentify)
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.le
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+.ls select = "interp" (refspectra)
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+.ls average
+Average two reference spectra without regard to any sort parameter.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.
+This option is used to assign two reference spectra, with equal weights,
+independent of any sorting parameter.
+.le
+.ls following
+Select the nearest following spectrum in the reference list based on the
+sorting parameter.  If there is no following spectrum use the nearest preceding
+spectrum.
+.le
+.ls interp
+Interpolate between the preceding and following spectra in the reference
+list based on the sorting parameter.  If there is no preceding and following
+spectrum use the nearest spectrum.  The interpolation is weighted by the
+relative distances of the sorting parameter.
+.le
+.ls match
+Match each input spectrum with the reference spectrum list in order.
+This overrides the reference aperture check.
+.le
+.ls nearest
+Select the nearest spectrum in the reference list based on the sorting
+parameter.
+.le
+.ls preceding
+Select the nearest preceding spectrum in the reference list based on the
+sorting parameter.  If there is no preceding spectrum use the nearest following
+spectrum.
+.le
+.le
+.ls sort = "jd" (setjd and refspectra)
+Image header keyword to be used as the sorting parameter for selection
+based on order.  The header parameter must be numeric but otherwise may
+be anything.  Common sorting parameters are times or positions.
+.le
+.ls group = "ljd" (setjd and refspectra)
+Image header keyword to be used to group spectra.  For those selection
+methods which use the group parameter the reference and object
+spectra must have identical values for this keyword.  This can
+be anything but it must be constant within a group.  Common grouping
+parameters are the date of observation "date-obs" (provided it does not
+change over a night) or the local Julian day number.
+.le
+.ls time = no, timewrap = 17. (refspectra)
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.le
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+.ls linearize = yes (dispcor)
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling using
+the linear dispersion parameters specified by other parameters.  If
+no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data is not interpolated.  Note the interpolation
+function type is set by the package parameter \fIinterp\fR.
+.le
+.ls log = no (ecdispcor)
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.le
+.ls flux = yes (ecdispcor)
+Conserve the total flux during interpolation?  If \fIno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \fIyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.le
+
+.ce
+-- SENSITIVITY CALIBRATION PARAMETERS --
+.ls bandwidth = 10., bandsep = 10. (standard)
+Interpolated bandpass grid.  If INDEF then the same bandpasses as in the
+calibration files are used otherwise the calibration data is interpolated
+to the specified set of bandpasses.
+.le
+.ls s_interact = yes (standard)
+Display the bandpasses on the standard star data and allow interactive
+addition and deletion of bandpasses.
+.le
+.ls s_function = "spline3", s_order = 1 (sensfunc)
+Function and order used to fit the sensitivity data.  The function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline3" cubic spline,
+and "spline1" linear spline.
+Order of the sensitivity fitting function.  The value corresponds to the
+number of polynomial terms or the number of spline pieces.  The default
+values may be changed interactively.
+.le
+.ls fnu = no (calibrate)
+The default calibration is into units of F-lambda. If \fIfnu\fR = yes then
+the calibrated spectrum will be in units of F-nu.
+.le
+
+.ce
+PACKAGE PARAMETERS
+.ls dispaxis = 2
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.  The default value defers to the
+package parameter of the same name.
+.le
+.ls extinction = "onedstds$kpnoextinct.dat" (standard, sensfunc, calibrate)
+Extinction file for a site.  There are two extinction files in the
+NOAO standards library, onedstds$, for KPNO and CTIO.  These extinction
+files are used for extinction and flux calibration.
+.le
+.ls caldir (standard)
+Standard star calibration directory.  A directory containing standard
+star data files.  Note that the directory name must end with '/'.
+There are a number of standard star calibrations directories in the NOAO
+standards library, onedstds$.
+.le
+.ls observatory = "observatory" (observatory)
+The default observatory to use for latitude dependent computations.
+If the OBSERVAT keyword in the image header it takes precedence over
+this parameter.
+.le
+.ls interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc) (dispcor)
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.nf
+        nearest - nearest neighbor
+         linear - linear
+          poly3 - 3rd order polynomial
+          poly5 - 5th order polynomial
+        spline3 - cubic spline
+           sinc - sinc function
+.fi
+.le
+.ls database = "database"
+Database name used by various tasks.  This is a directory which is created
+if necessary.
+.le
+.ls verbose = no
+Verbose output?  If set then almost all the information written to the
+logfile is also written to the terminal except when the task is a
+background or batch process.
+.le
+.ls logfile = "logfile"
+If specified detailed text log information is written to this file.
+.le
+.ls plotfile = ""
+If specified metacode plots are recorded in this file for later review.
+Since plot information can become large this should be used only if
+really desired.
+.le
+.ih
+ENVIRONMENT PARAMETERS
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
+.ih
+DESCRIPTION
+\fBDoecslit\fR subtracts background sky or scattered light, extracts,
+wavelength calibrates, and flux calibrates multiorder echelle slit spectra
+which have been processed to remove the detector characteristics; i.e. CCD
+images have been bias, dark count, and flat field corrected.  The spectra
+should be oriented such that pixels of constant wavelength are aligned with
+the image columns or lines.  Small departures from this alignment are not
+critical resulting in only a small loss of resolution.  Single order
+observations should be reduced with \fBdoslit\fR.
+
+The task is a command language script which collects and combines the
+functions and parameters of many general purpose tasks to provide a single,
+complete data reduction path and a degree of guidance, automation, and
+record keeping.  In the following description and in the parameter section
+the various general tasks used are identified.  Further
+information about those tasks and their parameters may be found in their
+documentation.  \fBDoecslit\fR also simplifies and consolidates parameters
+from those tasks and keeps track of previous processing to avoid
+duplications.
+
+The general organization of the task is to do the interactive setup steps,
+such as the aperture definitions and reference dispersion function
+determination, first using representative calibration data and then perform
+the majority of the reductions automatically, possibly as a background
+process, with reference to the setup data.  In addition, the task
+determines which setup and processing operations have been completed in
+previous executions of the task and, contingent on the \fIredo\fR and
+\fIupdate\fR options, skip or repeat some or all the steps.
+
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage
+since there are many variations possible.
+
+\fBUsage Outline\fR
+
+.ls 6 [1]
+The images are first processed with \fBccdproc\fR for overscan,
+zero level, dark count, and flat field corrections.
+.le
+.ls [2]
+Set the \fBdoecslit\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed, an aperture reference image (usually a bright
+star spectrum) to use in finding the orders and defining the
+aperture parameters, one or more arc images, and one or more standard
+star images.  If there are many object, arc, or standard star images
+you might prepare "@ files".  Set the detector and data
+specific parameters.  Select the processing options desired.
+Finally you might wish to review the \fBsparams\fR algorithm parameters
+though the defaults are probably adequate.
+.le
+.ls [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the current execution and no further queries of that
+type will be made.
+.le
+.ls [4]
+The specified number of orders (ranked by peak strength) in the aperture
+reference image are located and default fixed width apertures are
+assigned.  If the resize option is set the apertures are resized by finding
+the level which is 5% (the default) of the peak above local background.
+You then have the option of entering the aperture editing loop to check the
+aperture positions, sizes, and background fitting parameters.  This is
+highly recommended.  Note that it is important that the aperture numbers be
+sequential with the orders and if any orders are skipped the aperture
+numbers should also skip.  It is also important to verify the background
+regions with the 'b' key.  Usually you want any changes made to the
+background definitions to apply to all apertures so use the 'a' key to
+select all apertures before modifying the background parameters.  To exit
+the background mode and then to exit the review mode use 'q'.
+.le
+.ls [5]
+The order positions at a series of points along the dispersion are measured
+and a function is fit to these positions.  This may be done interactively
+to examine the traced positions and adjust the fitting parameters.  To exit
+the interactive fitting type 'q'.  Not all orders need be examined and the
+"NO" response will quit the interactive fitting using the last defined
+fitting parameters on the remaining traces.
+.le
+.ls [6]
+Apertures are now defined for all standard and object images.  This is only
+done if there are no previous aperture definitions for the image.  The
+aperture references previously defined are used as the initial set of
+apertures for each image.  The apertures are then recentered by an average
+shift over all orders and resized if that option is selected.
+The apertures may also be retraced and interactively examined
+for each image if the tracing option is selected and quicklook mode is not.
+.le
+.ls [7]
+If scattered light subtraction is selected the scattered light parameters
+are set using the aperture reference image and the task \fBapscatter\fR.
+The purpose of this is to interactively define the aperture buffer distance
+for the scattered light and the cross and parallel dispersion fitting
+parameters.  The fitting parameters are taken from and recorded in the
+parameter sets \fBapscat1\fR and \fBapscat2\fR.  All other scattered light
+subtractions are done noninteractively with these parameters.  Note that
+the scattered light correction modifies the input images.  Scattered light
+subtraction is not done in quicklook mode.
+.le
+.ls [8]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  The dispersion function is defined using the task
+\fBecidentify\fR.  Identify a few arc lines in a few orders with 'm' and
+'o' and use the 'l' line list identification command to automatically add
+additional lines and fit the dispersion function.  Check the quality of the
+dispersion function fit with 'f'.  When satisfied exit with 'q'.
+.le
+.ls [9]
+If the flux calibration option is selected the standard star spectra are
+processed (if not done previously).  The images are background subtracted,
+extracted, and wavelength calibrated.  The appropriate arc
+calibration spectra are extracted and the dispersion function refit
+using the arc reference spectrum as a starting point.  The standard star
+fluxes through the calibration bandpasses are compiled.  You are queried
+for the name of the standard star calibration data file.  Because echelle
+spectra are often at much higher dispersion than the calibration data,
+interpolated bandpasses may be defined with the bandpass parameters in
+\fBsparams\fR and checked or modified interactively.
+
+After all the standard stars are processed a sensitivity function is
+determined using the interactive task \fBsensfunc\fR.  Finally, the
+standard star spectra are extinction corrected and flux calibrated
+using the derived sensitivity function.
+.le
+.ls [10]
+The object spectra are now automatically background subtracted
+(an alternative to scattered light subtraction),
+extracted, wavelength calibrated, and flux calibrated.
+.le
+.ls [11]
+The option to examine the final spectra with \fBsplot\fR may be given.
+To exit type 'q'.  In quicklook mode the spectra are plotted
+noninteractively with \fBspecplot\fR.
+.le
+.ls [12]
+The final spectra will have the same name as the original 2D images
+with a ".ec" extension added.
+.le
+
+\fBSpectra and Data Files\fR
+
+The basic input consists of echelle slit object, standard star, and arc
+calibration spectra stored as IRAF images.
+The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+The raw CCD images must be
+processed to remove overscan, bias, dark count, and flat field effects.
+This is generally done using the \fBccdred\fR package.  Flat fields which
+are not contaminated by low counts between the apertures may be prepared
+with the task \fBapflatten\fR (recommended) or \fBapnormalize\fR.  Lines of
+constant wavelength across the orders should be closely aligned with one of
+the image axes.  Sometimes the orders are aligned rather than the spectral
+features.  This will result in a small amount of resolution loss but is
+often acceptable.  In some cases one may correct for misalignment with the
+\fBrotate\fR task.  More complex geometric problems and observations of
+extended objects should be handled by the \fBlongslit\fR package and single
+order observations should be processed by \fBdoslit\fR.
+
+The aperture reference spectrum is generally a bright star.  The arc
+spectra are comparison arc lamp observations (they must all be of the same
+type).  The assignment of arc calibration exposures to object exposures is
+generally done by selecting the nearest in time and interpolating.
+However, the optional \fIarc assignment table\fR may be used to explicitly
+assign arc images to specific objects.  The format of this file is
+described in task \fBrefspectra\fR.
+
+The final reduced spectra are recorded in two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ec" extension.  Each line in the reduced image is a one dimensional
+spectrum with associated aperture, order, and wavelength
+information.  When the \fIextras\fR parameter is set the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tasks such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.  The special task \fBscopy\fR may be used to extract
+specific apertures or to change format to individual one dimensional
+images.  The task \fBscombine\fR is used to combine or merge orders into
+a single spectrum.
+
+\fBPackage Parameters\fR
+
+The \fBechelle\fR package parameters set parameters which change
+infrequently and define the standard I/O functions.  The extinction file
+is used for making extinction corrections and the standard star
+calibration directory is used for determining flux calibrations from
+standard star observations.  The calibration directories contain data files
+with standard star fluxes and band passes.  The available extinction
+files and flux calibration directories may be listed using the command:
+.nf
+
+	cl> page onedstds$README
+
+.fi
+The extinction correction requires computation of an air mass using the
+task \fBsetairmass\fR.  The air mass computation needs information
+about the observation and, in particular, the latitude of the observatory.
+This is determined using the OBSERVAT image header keyword.  If this
+keyword is not present the observatory parameter is used.  See the
+task \fBobservatory\fR for more on defining the observatory parameters.
+
+The spectrum interpolation type is used whenever a spectrum needs to be
+resampled for linearization or performing operations between spectra
+with different sampling.  The "sinc" interpolation may be of interest
+as an alternative but see the cautions given in \fBonedspec.package\fR.
+
+The verbose parameter selects whether to print everything which goes
+into the log file on the terminal.  It is useful for monitoring
+what the \fBdoecslit\fR task does.  The log and plot files are useful for
+keeping a record of the processing.  A log file is highly recommended.
+A plot file provides a record of the apertures, traces, and extracted
+spectra but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+
+\fBProcessing Parameters\fR
+
+The input images are specified by image lists.  The lists may be
+a list of explicit comma separate image names, @ files, or image
+templates using pattern matching against file names in the directory.
+To allow wildcard image lists to be used safely and conveniently the
+image lists are checked to remove extracted images (the .ec images)
+and to automatically identify object and arc spectra.  Object and arc
+images are identified by the keyword IMAGETYP with values of "object",
+"OBJECT", "comp", or "COMPARISON" (the current practice at NOAO).
+If arc images are found in the object list they are transferred to the
+arc list while if object images are found in the arc list they are ignored.
+All other image types, such as biases, darks, or flat fields, are
+ignored.  This behavior allows simply specifying all images with a wildcard
+in the object list with automatic selections of arc spectra or a
+wildcard in the arc list to automatically find the arc spectra.
+If the data lack the identifying information it is up to the user
+to explicitly set the proper lists.
+
+As mentioned earlier, all the arc images must be of the same type;
+that is taken with the same arc lamp.  The aperture reference parameter
+is a single image name which is usually a bright star.
+
+The next set of parameters describe the noise characteristics and the
+general layout of the orders.  The read out noise and gain are used when
+"cleaning" cosmic rays and when using variance or optimal weighting.  These
+parameters must be fairly accurate.  Note that these are the effective
+parameters and must be adjusted if previous processing has modified the
+pixel values; such as with an unnormalized flat field.
+
+The general direction in which the orders run is specified by the
+dispersion axis parameter.  Recall that ideally it is the direction
+of constant wavelength which should be aligned with an image axis and
+the dispersion direction will not be aligned because of the cross-dispersion.
+The \fInorders\fR parameter is used to automatically find the orders.  The
+specified number of the brightest peaks are found.  Generally after finding the
+orders the aperture definitions are reviewed and adjusted interactively.
+The profile width should be approximately the full width at the profile
+base.  The default aperture limits and background regions are all
+derived from this width parameter.
+
+The next set of parameters select the processing steps and options.  The
+various calibration steps may be done simultaneously, that is at the same
+time as the basic extractions, or in separate executions of the task.
+Typically, all the desired operations are done at the same time.
+Dispersion correction requires at least one arc spectrum and flux
+calibration requires dispersion correction and at least one standard star
+observation.
+
+The \fIresize\fR option resets the edges of the extraction apertures based
+on the profile for each object and standard star order.  The default
+resizing is to the 5% point relative to the peak measured above the
+background.  This allows following changes in the seeing.  However, one
+should consider the consequences of this if attempting to flux calibrate
+the observations.  Except in quicklook mode, the apertures for each object
+and standard star observation may be reviewed graphically and further
+adjustments made to the aperture width and background regions.
+
+The apertures for each observation are adjusted for small shifts relative
+to the reference aperture definitions.  If you think this is not sufficient,
+say to account for rotation of the detector or for differing atmospheric
+dispersion, the \fItrace\fR option allows redefining the aperture trace
+functions for each observation.  Note this is only allowed in non-quicklook
+mode.
+
+The \fIclean\fR option invokes a profile
+fitting and deviant point rejection algorithm as well as a variance weighting
+of points in the aperture.  See the next section for more about
+requirements to use this option.
+
+The \fIbackground\fR option selects a type of correction for background
+or scattered light.  If the type is "scattered" a global scattered light
+is fit to the data between the apertures  and subtracted from the images.
+\fINote that the input images are modified by this operation\fR.
+This option is slow and is not allowed in quicklook
+mode.  Alternatively, a local background may be subtracted using
+background regions defined for each aperture.  The background may be
+within the slit for a sky subtraction or outside of the slit for a
+local scattered light subtraction.  The data in the regions
+may be averaged, medianed, or the minimum value used.  Another choice
+is to fit the data in the background regions by a function and interpolate
+to the object aperture.
+
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\fIupdate\fR flag is set.  The changes which will cause an update are a new
+reference image, adding the scattered light subtraction option, a new arc
+reference image, and new standard stars.  If all input spectra are to be
+processed regardless of previous processing the \fIredo\fR flag may be
+used.  Note that reprocessing clobbers the previously processed output
+spectra.
+
+The final step is to plot the spectra if the \fIsplot\fR option is
+selected.  In non-quicklook mode there is a query which may be
+answered either in lower or upper case.  The plotting uses the interactive
+task \fBsplot\fR.  In quicklook mode the plot appears noninteractively
+using the task \fBspecplot\fR.  
+
+The \fIquicklook\fR option provides a simpler, less interactive, mode.
+The quicklook mode automatically assigns the reference apertures to
+the object and standard star observations without interactive review
+or tracing, does not do the time consuming scattered light correction,
+and the \fIsplot\fR option selects a noninteractive plot to be
+shown at the end of processing of each object and standard star
+spectrum.  While the algorithms used in quicklook mode are nearly the same
+as in non-quicklook mode and the final results may be the same it is
+recommended that the greater degree of monitoring and review in
+non-quicklook mode be used for careful final reductions.
+
+The batch processing option allows object spectra to be processed as a
+background or batch job.  This will occur only if the interactive
+\fIsplot\fR option is not active; either not set, turned off during
+processing with "NO", or in quicklook mode.  In batch processing the
+terminal output is suppressed.
+
+The \fIlistonly\fR option prints a summary of the processing steps
+which will be performed on the input spectra without actually doing
+anything.  This is useful for verifying which spectra will be affected
+if the input list contains previously processed spectra.  The listing
+does not include any arc spectra which may be extracted to dispersion
+calibrate an object spectrum.
+
+The last parameter (excluding the task mode parameter) points to
+another parameter set for the algorithm parameters.  The default
+parameter set is called \fBsparams\fR.  The algorithm parameters are
+discussed further in the next section.
+
+\fBAlgorithms and Algorithm Parameters\fR
+
+This section summarizes the various algorithms used by the
+\fBdoecslit\fR task and the parameters which control and modify the
+algorithms.  The algorithm parameters available to you are
+collected in the parameter set \fBsparams\fR.  These parameters are
+taken from the various general purpose tasks used by the \fBdoecslit\fR
+processing task.  Additional information about these parameters and
+algorithms may be found in the help for the actual
+task executed.  These tasks are identified below.  The aim of this
+parameter set organization is to collect all the algorithm parameters
+in one place separate from the processing parameters and include only
+those which are relevant for echelle slit data.  The parameter values
+can be changed from the defaults by using the parameter editor,
+.nf
+
+cl> epar sparams
+
+.fi
+or simple typing \fIsparams\fR.
+The parameter editor can also be entered when editing the \fBdoecslit\fR
+parameters by typing \fI:e\fR when positioned at the \fIsparams\fR
+parameter.
+
+\fBAperture Definitions\fR
+
+The first operation is to define the extraction apertures, which include the
+aperture width, background regions, and position dependence with
+wavelength, for the input echelle slit spectra and, if flux calibration is
+selected, the standard star spectra.  This is done only for spectra which
+do not have previously defined apertures unless the \fIredo\fR option is
+set to force all definitions to be redone.  Thus, apertures may be
+defined separately using the \fBapextract\fR tasks.  This is particularly
+useful if one needs to use reference images to define apertures for very
+weak spectra which are not well centered or traced by themselves.
+
+Initially apertures are defined for a specified \fIaperture reference\fR
+image.  The selected number of orders are found automatically by selecting
+the highest peaks in a cut across the dispersion.  Apertures are assigned
+with a width given by the \fIwidth\fR parameter and numbered sequentially.
+The background regions are also defined in terms of the width parameter
+starting at one width distance from the profile center and extending to two
+widths on both sides of the profile.  As an example, if the width parameter
+is 5 pixels the default aperture limits are +/- 2.5 pixels and the
+background sample regions will be "-10:-5,5:10".  If the \fIresize\fR
+parameter is set the aperture limits are adjusted to a specified point on
+the spectrum profile (see \fBapresize\fR).
+
+A query is then given allowing the aperture definitions to be reviewed and
+modified.  Queries made by \fBdoecslit\fR generally may be answered with either
+lower case "yes" or "no" or with upper case "YES" or "NO".  The upper
+case responses apply to all further queries and so are used to eliminate
+further queries of that kind.
+
+Reviewing the aperture definitions is highly recommended to check the
+aperture numbering, aperture limits, and background regions.  The aperture
+numbers must be linearly related, with a slope of +/- 1, to the true order
+numbers though absolute order numbers need not be known.  The key point is
+that if an order is skipped the aperture numbers must also skip.  The
+background regions are checked with the 'b' key.  Typically one adjusts all
+the background regions at the same time by selecting all apertures with
+the 'a' key first.  To exit the background and aperture editing steps type
+'q'.
+
+Next the positions of the orders at various points along the dispersion
+are measured and "trace functions" are fit.  The user is asked whether
+to fit each trace function interactively.  This is selected to adjust
+the fitting parameters such as function type and order.  When
+interactively fitting a query is given for each aperture.  After the
+first aperture one may skip reviewing the other traces.
+
+After the aperture reference image is done all the object and standard star
+images are checked for aperture definitions and those without definitions
+are assigned apertures.  The assignment consists of inheriting the aperture
+from the reference aperture image, recentering the apertures based on an
+average shift that best centers all the apertures, resizing the apertures
+if the resize option is selected, and retracing the spectral orders if the
+retracing option is selected.  Retracing is only allowed in non-quicklook
+mode (set by the \fIquicklook\fR parameter).  Also interactive review of
+the aperture definitions is only done in
+non-quicklook mode.  In quicklook mode the aperture definitions are all set
+noninteractively without retracing.  It is recommended that quicklook only
+be used for initial quick extractions and calibration and that for final
+reductions one at least review the aperture definitions and possibly
+retrace each observation.
+
+The above steps are all performed using tasks from the \fBapextract\fR
+package and parameters from the \fBsparams\fR parameters.  As a quick
+summary, the dispersion direction of the spectra are determined from the
+package \fBdispaxis\fR parameter if not defined in the image header.  The default
+line or column for finding the object position on the slit and the number
+of image lines or columns to sum are set by the \fIline\fR and \fInsum\fR
+parameters.  A line of INDEF (the default) selects the middle of the
+image.  The automatic finding algorithm is described for the task
+\fBapfind\fR and basically finds the strongest peaks.  The resizing is
+described in the task \fBapresize\fR and the parameters used are also
+described there.  The tracing is
+done as described in \fBaptrace\fR and consists of stepping along the image
+using the specified \fIt_step\fR parameter.  The function fitting uses the
+\fBicfit\fR commands with the other parameters from the tracing section.
+
+\fBBackground or Scattered Light Subtraction\fR
+
+In addition to not subtracting any sky or scattered light there are two
+approaches to subtracting background light.  The first is to determine
+a smooth global scattered light component.  The second is to subtract
+a locally determined background at each point along the dispersion and
+for each aperture.  This can be either for a sky subtraction if the
+background regions are within the slit or scattered light if the
+background regions are outside of the slit.  Note that background
+subtraction is only done for object and standard star images and not
+for arc spectra.  Also, the global scattered light option is not done
+in quicklook mode.
+
+The global scattered light fitting and subtraction is done with the task
+\fBapscatter\fR.  The function fitting parameters are set interactively
+using the aperture reference spectrum.  All other subtractions are done
+noninteractively with the same set of parameters.  The scattered light is
+subtracted from the input images, thus modifying them, and one might wish
+to first make backups of the original images.
+
+The scattered light is measured between the apertures using a specified
+buffer distance from the aperture edges.  The scattered light pixels are
+fit by a series of one dimensional functions across the dispersion.  The
+independent fits are then smoothed along the dispersion by again fitting
+low order functions.  These fits then define the smooth scattered light
+surface to be subtracted from the image.  The fitting parameters are
+defined and recorded in the two parameter sets \fIapscat1\fR and
+\fIapscat2\fR.  The scattered light algorithm is described more fully in
+\fBapscatter\fR.  This algorithm is relatively slow.
+
+Local background subtraction is done during extraction based on background
+regions and parameters defined by the default background parameters or
+changed during interactive review of the apertures.  The background
+subtraction options are to subtract the average, median, or minimum of the
+pixels in the background regions, or to fit a function and subtract the
+function from under the extracted object pixels.  The background regions
+are specified in pixels from the aperture center and follow changes in
+center of the spectrum along the dispersion.  The syntax is colon separated
+ranges with multiple ranges separated by a comma or space.  The background
+fitting uses the \fBicfit\fR routines which include medians, iterative
+rejection of deviant points, and a choice of function types and orders.
+Note that it is important to use a method which rejects cosmic rays such as
+using either medians over all the background regions (\fIbackground\fR =
+"median") or median samples during fitting (\fIb_naverage\fR < -1).  The
+background subtraction algorithm and options are described in greater
+detail in \fBapsum\fR and \fBapbackground\fR.
+
+\fBExtraction\fR
+
+The actual extraction of the spectra is done by summing across the
+fixed width apertures at each point along the dispersion.
+The default is to simply sum the pixels using
+partial pixels at the ends.  There is an option to weight the
+sum based on a Poisson variance model using the \fIreadnoise\fR and
+\fIgain\fR detector parameters.  Note that if the \fIclean\fR
+option is selected the variance weighted extraction is used regardless
+of the \fIweights\fR parameter.  The sigma thresholds for cleaning
+are also set in the \fBsparams\fR parameters.
+
+The cleaning and variance weighting options require knowing the effective
+(i.e. accounting for any image combining) read out noise and gain.
+These numbers need to be adjusted if the image has been processed
+such that the intensity scale has a different origin (such as
+a scattered light subtraction) or scaling (such as caused by unnormalized
+flat fielding).  These options also require using background subtraction
+if the profile does not go to zero.  For optimal extraction and
+cleaning to work it is recommended that any flat fielding be done
+using flat fields produced by \fBapflatten\fR, no scattered light
+correction, and using background subtraction if there is any
+appreciable sky or to compensate for scattered light.
+For further discussion of cleaning and variance weighted extraction see
+\fBapvariance\fR and \fBapprofiles\fR as well as  \fBapsum\fR.
+
+\fBDispersion Correction\fR
+
+If dispersion correction is not selected, \fIdispcor\fR=no, then the object
+spectra are simply extracted.  The extracted spectra may be plotted
+by setting the \fIsplot\fR option.  This produces a query and uses
+the interactive \fBsplot\fR task in non-quicklook mode and uses
+\fBspecplot\fR noninteractively in quicklook mode.
+
+Dispersion corrections are applied to the extracted spectra if the
+\fIdispcor\fR processing parameter is set.  There
+are three basic steps involved; determining the dispersion functions
+relating pixel position to wavelength, assigning the appropriate
+dispersion function to a particular observation, and either storing
+the nonlinear dispersion function in the image headers or resampling the
+spectra to evenly spaced pixels in wavelength.
+
+The first arc spectrum in the arc list is used to define the reference
+dispersion solution.  It is extracted using the reference aperture definition.
+Note extractions of arc spectra are not background or scattered light
+subtracted.  The interactive task \fBecidentify\fR is used to define the
+dispersion function.  The idea is to mark some lines in a few orders whose
+wavelengths are known (with the line list used to supply additional lines after
+the first few identifications define the approximate wavelengths) and to fit a
+function giving the wavelength from the aperture number and pixel position.
+
+The arc dispersion function parameters are for \fBecidentify\fR and it's
+related partner \fBecreidentify\fR.  The parameters define a line list for
+use in automatically assigning wavelengths to arc lines, a centering width
+(which should match the line widths at the base of the lines), the
+dispersion function type and orders, parameters to exclude bad lines from
+function fits, and defining whether to refit the dispersion function as
+opposed to simply determining a zero point shift.  The defaults should
+generally be adequate and the dispersion function fitting parameters may be
+altered interactively.  One should consult the help for the two tasks for
+additional details of these parameters and the interactive operation of
+\fBecidentify\fR.
+
+Once the reference dispersion function is defined other arc spectra are
+extracted as required by the object spectra.  The assignment of arcs is
+done either explicitly with an arc assignment table (parameter
+\fIarctable\fR) or based on a header parameter such as a time.
+This assignments are made by the task
+\fBrefspectra\fR.  When two arcs are assigned to an object spectrum an
+interpolation is done between the two dispersion functions.  This makes an
+approximate correction for steady drifts in the dispersion.
+
+The tasks \fBsetjd\fR and \fBsetairmass\fR are automatically run on all
+spectra.  This computes and adds the header parameters for the Julian date
+(JD), the local Julian day number (LJD), the universal time (UTMIDDLE), and
+the air mass at the middle of the exposure.  The default arc assignment is
+to use the Julian date grouped by the local Julian day number.  The
+grouping allows multiple nights of data to be correctly assigned at the
+same time.
+
+In non-quicklook mode the arc spectra assigned to each object are
+extracted using the same apertures as the object.  This accounts for
+changes in the recentering, aperture sizes, and tracing functions.
+In quicklook mode the arc spectra are extracted using the reference
+apertures.  When the same arc is used for several object images this
+allows the arc spectrum to only be extracted once.
+
+Defining the dispersion function for a new arc extraction is done with
+the task \fBecreidentify\fR.  This is done noninteractively with log
+information recorded about the line reidentifications and the fit.
+
+The last step of dispersion correction is setting the dispersion
+of the object image from the arc images.  There are two choices here.
+If the \fIlinearize\fR parameter is not set the nonlinear dispersion
+function is stored in the image header.  Other IRAF tasks interpret
+this information when dispersion coordinates are needed for plotting
+or analysis.  This has the advantage of not requiring the spectra
+to be interpolated and the disadvantage that the dispersion
+information is only understood by IRAF tasks and cannot be readily
+exported to other analysis software.
+
+If the \fIlinearize\fR parameter is set then the spectra are resampled to a
+linear dispersion relation either in wavelength or the log of the
+wavelength.  For echelle spectra each order is linearized independently so
+that the wavelength interval per pixel is different in different orders.
+This preserves most of the resolution and avoids over or under sampling of
+the highest or lowest dispersion orders.  The wavelength limits are
+taken from the limits determined from the arc reference spectrum and
+the number of pixels is the same as the original images.  The dispersion
+per pixel is then derived from these constraints.
+
+The linearization algorithm  parameters allow selecting the interpolation
+function type, whether to conserve flux per pixel by integrating across the
+extent of the final pixel, and whether to linearize to equal linear or
+logarithmic intervals.  The latter may be appropriate for radial velocity
+studies.  The default is to use a fifth order polynomial for interpolation,
+to conserve flux, and to not use logarithmic wavelength bins.  These
+parameters are described fully in the help for the task \fBdispcor\fR which
+performs the correction.
+
+\fBFlux Calibration\fR
+
+Flux calibration consists of an extinction correction and an instrumental
+sensitivity calibration.  The extinction correction only depends on the
+extinction function defined by the package parameter \fIextinct\fR and
+determination of the airmass from the header parameters (the air mass is
+computed by \fBsetairmass\fR as mentioned earlier).  The sensitivity
+calibration depends on a sensitivity calibration spectrum determined from
+standard star observations for which there are tabulated absolute fluxes.
+The task that applies both the extinction correction and sensitivity
+calibration to each extracted object spectrum is \fBcalibrate\fR.  Consult
+the manual page for this task for more information.
+
+Generation of the sensitivity calibration spectrum is done before
+processing any object spectra since it has two interactive steps and
+requires all the standard star observations.  The first step is tabulating
+the observed fluxes over the same bandpasses as the calibrated absolute
+fluxes.  For very high resolution it may be the case that the measured
+calibration bandpasses are too large or sparse.  In this case one must
+interpolate the calibration data to bandpasses appropriate for the data.
+If the bandpass widths and separations are given as INDEF then the same
+bandpasses as in the calibration file are used.  Otherwise a uniform grid
+of bandpasses is interpolated.  Using interpolated bandpasses is not
+rigorous but is sometimes the only choice for echelle spectra.
+
+The standard star tabulations are done after each standard star is
+extracted and dispersion corrected.  You are asked for the name of the
+standard star as tabulated in the absolute flux data files in the directory
+\fIcaldir\fR defined by the package parameters.  If the \fIinteract\fR
+parameter is yes the bandpasses can be displayed on the data and you can
+interactively add or delete bandpasses. The tabulation of the standard star
+observations over the standard bandpasses is done by the task
+\fBstandard\fR.  The tabulated data is stored in the file \fIstd\fR.  Note
+that if the \fIredo\fR flag is not set any new standard stars specified in
+subsequent executions of \fBdoecslit\fR are added to the previous data in
+the data file, otherwise the file is first deleted.  Modification of the
+tabulated standard star data, such as by adding new stars, will cause any
+spectra in the input list which have been previously calibrated to be
+reprocessed if the \fIupdate\fR flag is set.
+
+After the standard star calibration bandpass fluxes are tabulated the
+information from all the standard stars is combined to produce a
+sensitivity function for use by \fBcalibrate\fR.  The sensitivity function
+determination is interactive and uses the task \fBsensfunc\fR.  This task
+allows fitting a smooth sensitivity function to the ratio of the observed
+to calibrated fluxes verses wavelength.  The types of manipulations one
+needs to do include deleting bad observations, possibly removing variable
+extinction (for poor data), and possibly deriving a revised extinction
+function.  This is a complex operation and one should consult the manual
+page for \fBsensfunc\fR.  The sensitivity function is saved as one
+dimensional spectra (one per order) with the root name \fIsens\fR.
+Deletion of these images will also cause reprocessing to occur if the
+\fIupdate\fR flag is set.
+.ih
+EXAMPLES
+1.  The following example uses artificial data and may be executed
+at the terminal (with IRAF V2.10).  This is similar to the sequence
+performed by the test procedure "demos doecslit".
+
+.nf
+ec> demos mkecslit
+Creating example longslit in image demoobj ...
+Creating example longslit in image demostd ...
+Creating example longslit in image demoarc ...
+ec> echelle.verbose=no
+ec> echelle.caldir=onedstds$spechayescal/
+ec> doecslit Bdemoobj apref=Bdemostd arcs=Bdemoarc stand=Bdemostd \
+>>> norders=3 extcor+ fluxcal+ resize+ splot+
+Set reference aperture for Bdemostd
+Edit apertures for Bdemostd?  (yes):
+<Check background with 'b', exit background and review with 'q'>
+Fit traced positions for Bdemostd interactively?  (yes):  
+Fit curve to aperture 1 of Bdemostd interactively  (yes):
+<Exit with 'q'>
+Fit curve to aperture 2 of Bdemostd interactively  (yes): N
+Edit apertures for Bdemoobj?  (yes):
+<Check background with 'b', exit background and review with 'q'>
+Fit traced positions for Bdemoobj interactively?  (yes): N
+Extract arc reference image Bdemoarc
+Determine dispersion solution for Bdemoarc
+<Type 'm' at first strong line (pixel 156) and identify it as 4965>
+<Type 'k' to go to next order>
+<Mark 52->5002, 74->5003.6, 155->5009.3>
+<Type 'k' to go to next order and mark 18->5044.7, 231->5059.8>
+<Type 'f' to see the fit residuals>
+<Type 'q' to quit fit and then 'q' to exit>
+Extract standard star spectrum Bdemostd
+Assign arc spectra for Bdemostd
+Extract and reidentify arc spectrum Bdemoarc
+Dispersion correct Bdemostd
+B...ec.imh: ap = 1, w1 = 4953.9, w2 = 4972.2, dw = 0.071, nw = 256
+B...ec.imh: ap = 2, w1 = 4998.3, w2 = 5016.5, dw = 0.071, nw = 256
+B...ec.imh: ap = 3, w1 = 5043.5, w2 = 5061.6, dw = 0.070, nw = 256
+Compile standard star fluxes for Bdemostd
+Bdemostd.ec.imh[1]: Artificial Echelle Spectrum
+Star name in calibration list: hz14
+Bdemostd.ec.imh[1]: Edit bandpasses? (no|yes|NO|YES|NO!|YES!) (no): y
+<Exit with 'q'>
+Bdemostd.ec.imh[2]: Artificial Echelle Spectrum
+Bdemostd.ec.imh[2]: Edit bandpasses? (no|yes|NO|YES|NO!|YES!) (y): N
+Bdemostd.ec.imh[3]: Artificial Echelle Spectrum
+Bdemostd.ec.imh[3]: Edit bandpasses? (no|yes|NO|YES|NO!|YES!) (N):
+Compute sensitivity function
+Fit aperture 1 interactively? (no|yes|NO|YES) (no|yes|NO|YES) (yes):
+<Exit with 'q'>
+Sensitivity function for aperture  1 --> sens.0001
+Fit aperture 2 interactively? (no|yes|NO|YES) (no|yes|NO|YES) (yes): N
+Sensitivity function for aperture  2 --> sens.0002
+Sensitivity function for aperture  3 --> sens.0003
+Flux and/or extinction calibrate standard stars
+Standard stars:
+Splot spectrum? (no|yes|NO|YES) (yes):
+Image line/aperture to plot (0:) (1):
+<Exit with 'q'>
+Extract object spectrum Bdemoobj
+Assign arc spectra for Bdemoobj
+Extract and reidentify arc spectrum Bdemoarc
+Dispersion correct Bdemoobj
+B...ec.imh: ap = 1, w1 = 4953.9, w2 = 4972.2, dw = 0.071, nw = 256
+B...ec.imh: ap = 2, w1 = 4998.3, w2 = 5016.5, dw = 0.071, nw = 256
+B...ec.imh: ap = 3, w1 = 5043.5, w2 = 5061.6, dw = 0.070, nw = 256
+Extinction correct Bdemoobj
+Flux calibrate Bdemoobj
+Bdemoobj.ec.imh:
+Splot spectrum? (no|yes|NO|YES) (yes):
+Image line/aperture to plot (0:) (1):
+<Exit with 'q'>
+.fi
+.ih
+REVISIONS
+.ls DOECSLIT V2.10.3
+The image format type to be
+processed is selected with the \fIimtype\fR environment parameter.  The
+dispersion axis parameter is now a package parameter.  Images will only
+be processed if the have the CCDPROC keyword.  A \fIdatamax\fR parameter
+has been added to help improve cosmic ray rejection.  A bug which
+alphabetized the arc spectra was fixed.
+.le
+.ih
+SEE ALSO
+apbackground, apedit, apfind, approfiles, aprecenter, apresize, apsum, aptrace,
+apvariance, calibrate, ccdred, center1d, ctioslit, dispcor,
+echelle.doecslit, ecidentify, ecreidentify, icfit, kpnocoude, kpnoslit,
+msred, observatory, onedspec.package, refspectra, sensfunc, setairmass, setjd,
+splot, standard
+.endhelp
diff --git a/noao/imred/echelle/doc/doecslit.ms b/noao/imred/echelle/doc/doecslit.ms
new file mode 100644
index 00000000..a93f3e8b
--- /dev/null
+++ b/noao/imred/echelle/doc/doecslit.ms
@@ -0,0 +1,1479 @@
+.nr PS 9
+.nr VS 11
+.de V1
+.ft CW
+.nf
+..
+.de V2
+.fi
+.ft R
+..
+.de LS
+.br
+.in +2
+..
+.de LE
+.br
+.sp .5v
+.in -2
+..
+.ND February 1993
+.TL
+Guide to the Slit Spectra Reduction Task DOECSLIT
+.AU
+Francisco Valdes
+.AI
+IRAF Group - Central Computer Services
+.K2
+.DY
+
+.AB
+\fBDoecslit\fR subtracts background sky or scattered light, extracts,
+wavelength calibrates, and flux calibrates multiorder echelle slit spectra
+which have been processed to remove the detector characteristics; i.e. CCD
+images have been bias, dark count, and flat field corrected.  The spectra
+should be oriented such that pixels of constant wavelength are aligned with
+the image columns or lines.  Small departures from this alignment are not
+critical resulting in only a small loss of resolution.  Single order
+observations should be reduced with \fBdoslit\fR.
+.AE
+.NH
+Introduction
+.LP
+\fBDoecslit\fR subtracts background sky or scattered light, extracts,
+wavelength calibrates, and flux calibrates multiorder echelle slit spectra
+which have been processed to remove the detector characteristics; i.e. CCD
+images have been bias, dark count, and flat field corrected.  The spectra
+should be oriented such that pixels of constant wavelength are aligned with
+the image columns or lines.  Small departures from this alignment are not
+critical resulting in only a small loss of resolution.  Single order
+observations should be reduced with \fBdoslit\fR.
+.LP
+The task is a command language script which collects and combines the
+functions and parameters of many general purpose tasks to provide a single,
+complete data reduction path and a degree of guidance, automation, and
+record keeping.  In the following description and in the parameter section
+the various general tasks used are identified.  Further
+information about those tasks and their parameters may be found in their
+documentation.  \fBDoecslit\fR also simplifies and consolidates parameters
+from those tasks and keeps track of previous processing to avoid
+duplications.
+.LP
+The general organization of the task is to do the interactive setup steps,
+such as the aperture definitions and reference dispersion function
+determination, first using representative calibration data and then perform
+the majority of the reductions automatically, possibly as a background
+process, with reference to the setup data.  In addition, the task
+determines which setup and processing operations have been completed in
+previous executions of the task and, contingent on the \f(CWredo\fR and
+\f(CWupdate\fR options, skip or repeat some or all the steps.
+.LP
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage
+since there are many variations possible.
+.NH
+Usage Outline
+.LP
+.IP [1] 6
+The images are first processed with \fBccdproc\fR for overscan,
+zero level, dark count, and flat field corrections.
+.IP [2]
+Set the \fBdoecslit\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed, an aperture reference image (usually a bright
+star spectrum) to use in finding the orders and defining the
+aperture parameters, one or more arc images, and one or more standard
+star images.  If there are many object, arc, or standard star images
+you might prepare "@ files".  Set the detector and data
+specific parameters.  Select the processing options desired.
+Finally you might wish to review the \fBsparams\fR algorithm parameters
+though the defaults are probably adequate.
+.IP [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the current execution and no further queries of that
+type will be made.
+.IP [4]
+The specified number of orders (ranked by peak strength) in the aperture
+reference image are located and default fixed width apertures are
+assigned.  If the resize option is set the apertures are resized by finding
+the level which is 5% (the default) of the peak above local background.
+You then have the option of entering the aperture editing loop to check the
+aperture positions, sizes, and background fitting parameters.  This is
+highly recommended.  Note that it is important that the aperture numbers be
+sequential with the orders and if any orders are skipped the aperture
+numbers should also skip.  It is also important to verify the background
+regions with the 'b' key.  Usually you want any changes made to the
+background definitions to apply to all apertures so use the 'a' key to
+select all apertures before modifying the background parameters.  To exit
+the background mode and then to exit the review mode use 'q'.
+.IP [5]
+The order positions at a series of points along the dispersion are measured
+and a function is fit to these positions.  This may be done interactively
+to examine the traced positions and adjust the fitting parameters.  To exit
+the interactive fitting type 'q'.  Not all orders need be examined and the
+"NO" response will quit the interactive fitting using the last defined
+fitting parameters on the remaining traces.
+.IP [6]
+Apertures are now defined for all standard and object images.  This is only
+done if there are no previous aperture definitions for the image.  The
+aperture references previously defined are used as the initial set of
+apertures for each image.  The apertures are then recentered by an average
+shift over all orders and resized if that option is selected.
+The apertures may also be retraced and interactively examined
+for each image if the tracing option is selected and quicklook mode is not.
+.IP [7]
+If scattered light subtraction is selected the scattered light parameters
+are set using the aperture reference image and the task \fBapscatter\fR.
+The purpose of this is to interactively define the aperture buffer distance
+for the scattered light and the cross and parallel dispersion fitting
+parameters.  The fitting parameters are taken from and recorded in the
+parameter sets \fBapscat1\fR and \fBapscat2\fR.  All other scattered light
+subtractions are done noninteractively with these parameters.  Note that
+the scattered light correction modifies the input images.  Scattered light
+subtraction is not done in quicklook mode.
+.IP [8]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  The dispersion function is defined using the task
+\fBecidentify\fR.  Identify a few arc lines in a few orders with 'm' and 'o'
+and use the 'l' line list identification command to automatically add
+additional lines and fit the dispersion function.  Check the quality of the
+dispersion function fit with 'f'.  When satisfied exit with 'q'.
+.IP [9]
+If the flux calibration option is selected the standard star spectra are
+processed (if not done previously).  The images are background subtracted,
+extracted, and wavelength calibrated.  The appropriate arc
+calibration spectra are extracted and the dispersion function refit
+using the arc reference spectrum as a starting point.  The standard star
+fluxes through the calibration bandpasses are compiled.  You are queried
+for the name of the standard star calibration data file.  Because echelle
+spectra are often at much higher dispersion than the calibration data
+interpolated bandpasses may be defined with the bandpass parameters in
+\fBsparams\fR and checked or modified interactively.
+.IP
+After all the standard stars are processed a sensitivity function is
+determined using the interactive task \fBsensfunc\fR.  Finally, the
+standard star spectra are extinction corrected and flux calibrated
+using the derived sensitivity function.
+.IP [10]
+The object spectra are now automatically background subtracted
+(an alternative to scattered light subtraction),
+extracted, wavelength calibrated, and flux calibrated.
+.IP [11]
+The option to examine the final spectra with \fBsplot\fR may be given.
+To exit type 'q'.  In quicklook mode the spectra are plotted
+noninteractively with \fBspecplot\fR.
+.IP [12]
+The final spectra will have the same name as the original 2D images
+with a ".ec" extension added.
+.NH
+Spectra and Data Files
+.LP
+The basic input consists of echelle slit object, standard star, and arc
+calibration spectra stored as IRAF images.
+The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+The raw CCD images must be
+processed to remove overscan, bias, dark count, and flat field effects.
+This is generally done using the \fBccdred\fR package.  Flat fields which
+are not contaminated by low counts between the apertures may be prepared
+with the task \fBapflatten\fR (recommended) or \fBapnormalize\fR.  Lines of
+constant wavelength across the orders should be closely aligned with one of
+the image axes.  Sometimes the orders are aligned rather than the spectral
+features.  This will result in a small amount of resolution loss but is
+often acceptable.  In some cases one may correct for misalignment with the
+\fBrotate\fR task.  More complex geometric problems and observations of
+extended objects should be handled by the \fBlongslit\fR package and single
+order observations should be processed by \fBdoslit\fR.
+.LP
+The aperture reference spectrum is generally a bright star.  The arc
+spectra are comparison arc lamp observations (they must all be of the same
+type).  The assignment of arc calibration exposures to object exposures is
+generally done by selecting the nearest in time and interpolating.
+However, the optional \fIarc assignment table\fR may be used to explicitly
+assign arc images to specific objects.  The format of this file is
+described in task \fBrefspectra\fR.
+.LP
+The final reduced spectra are recorded in two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ec" extension.  Each line in the reduced image is a one dimensional
+spectrum with associated aperture, order, and wavelength
+information.  When the \f(CWextras\fR parameter is set the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tasks such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.  The special task \fBscopy\fR may be used to extract
+specific apertures or to change format to individual one dimensional
+images.  The task \fBscombine\fR is used to combine or merge orders into
+a single spectrum.
+.NH
+Package Parameters
+.LP
+The \fBechelle\fR package parameters, shown in Figure 1, set parameters
+which change infrequently and define the standard I/O functions.
+.KS
+
+.ce
+Figure 1: Package Parameter Set for the ECHELLE Package
+
+.V1
+cl> epar echelle
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = imred
+   TASK = echelle
+
+(extinct= onedstds$kpnoextinct.dat) Extinction file
+(caldir = onedstds$spechayescal/) Standard star calibration directory
+(observa=  observatory) Observatory of data
+(interp =        poly5) Interpolation type
+(dispaxi=            2) Image axis for 2D images
+(nsum   =            1) Number of lines/columns to sum for 2D images
+
+(databas=     database) Database
+(verbose=          no) Verbose output?
+(logfile=      logfile) Text log file
+(plotfil=             ) Plot file
+
+(records=                     ) Record number extensions
+(version= ECHELLE V3: July 1991)
+
+.KE
+.V2
+The extinction file
+is used for making extinction corrections and the standard star
+calibration directory is used for determining flux calibrations from
+standard star observations.  The calibration directories contain data files
+with standard star fluxes and band passes.  The available extinction
+files and flux calibration directories may be listed using the command:
+.V1
+
+	cl> page onedstds$README
+
+.V2
+The extinction correction requires computation of an air mass using the
+task \fBsetairmass\fR.  The air mass computation needs information
+about the observation and, in particular, the latitude of the observatory.
+This is determined using the OBSERVAT image header keyword.  If this
+keyword is not present the observatory parameter is used.  See the
+task \fBobservatory\fR for more on defining the observatory parameters.
+.LP
+The spectrum interpolation type is used whenever a spectrum needs to be
+resampled for linearization or performing operations between spectra
+with different sampling.  The "sinc" interpolation may be of interest
+as an alternative but see the cautions given in \fBonedspec.package\fR.
+.LP
+The verbose parameter selects whether to print everything which goes
+into the log file on the terminal.  It is useful for monitoring
+everything that the task does.  The log and plot files are useful for
+keeping a record of the processing.  A log file is highly recommended.
+A plot file provides a record of the apertures, traces, and extracted
+spectra but can become quite large.
+.NH
+Processing Parameters
+.LP
+The \fBdoecslit\fR parameters are shown in Figure 2.
+.KS
+
+.ce
+Figure 2: Parameter Set for DOECSLIT
+
+.V1
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = echelle
+   TASK = doecslit
+
+objects =               List of object spectra
+(apref  =             ) Aperture reference spectrum
+(arcs   =             ) List of arc spectra
+(arctabl=             ) Arc assignment table (optional)
+(standar=             ) List of standard star spectra
+.KE
+.V1
+
+(readnoi=           0.) Read out noise sigma (photons)
+(gain   =           1.) Photon gain (photons/data number)
+(datamax=        INDEF) Max data value / cosmic ray threshold
+(norders=           10) Number of orders
+(width  =           5.) Width of profiles (pixels)
+
+(dispcor=          yes) Dispersion correct spectra?
+(extcor =           no) Extinction correct spectra?
+(fluxcal=           no) Flux calibrate spectra?
+(resize =           no) Resize object apertures?
+(clean  =           no) Detect and replace bad pixels?
+(trace  =          yes) Trace object spectra?
+(backgro=         none) Background to subtract
+(splot  =           no) Plot the final spectra?
+(redo   =           no) Redo operations if previously done?
+(update =           no) Update spectra if cal data changes?
+(quicklo=           no) Approximate quicklook reductions?
+(batch  =           no) Extract objects in batch?
+(listonl=           no) List steps but don't process?
+
+(sparams=             ) Algorithm parameters
+
+.V2
+The input images are specified by image lists.  The lists may be
+a list of explicit comma separate image names, @ files, or image
+templates using pattern matching against file names in the directory.
+To allow wildcard image lists to be used safely and conveniently the
+image lists are checked to remove extracted images (the .ec images)
+and to automatically identify object and arc spectra.  Object and arc
+images are identified by the keyword IMAGETYP with values of "object",
+"OBJECT", "comp", or "COMPARISON" (the current practice at NOAO).
+If arc images are found in the object list they are transferred to the
+arc list while if object images are found in the arc list they are ignored.
+All other image types, such as biases, darks, or flat fields, are
+ignored.  This behavior allows simply specifying all images with a wildcard
+in the object list with automatic selections of arc spectra or a
+wildcard in the arc list to automatically find the arc spectra.
+If the data lack the identifying information it is up to the user
+to explicitly set the proper lists.
+.LP
+As mentioned earlier, all the arc images must be of the same type;
+that is taken with the same arc lamp.  The aperture reference parameter
+is a single image name which is usually a bright star.
+.LP
+The next set of parameters describe the noise characteristics and the
+general layout of the orders.  The read out noise and gain are used when
+"cleaning" cosmic rays and when using variance or optimal weighting.  These
+parameters must be fairly accurate.  Note that these are the effective
+parameters and must be adjusted if previous processing has modified the
+pixel values; such as with an unnormalized flat field.
+.LP
+The general direction in which the orders run is specified by the
+dispersion axis parameter.  Recall that ideally it is the direction
+of constant wavelength which should be aligned with an image axis and
+the dispersion direction will not be aligned because of the cross-dispersion.
+The \f(CWnorders\fR parameter is used to automatically find the orders.  The
+specified number of the brightest peaks are found.  Generally after finding the
+orders the aperture definitions are reviewed and adjusted interactively.
+The profile width should be approximately the full width at the profile
+base.  The default aperture limits and background regions are all
+derived from this width parameter.
+.LP
+The next set of parameters select the processing steps and options.  The
+various calibration steps may be done simultaneously, that is at the same
+time as the basic extractions, or in separate executions of the task.
+Typically, all the desired operations are done at the same time.
+Dispersion correction requires at least one arc spectrum and flux
+calibration requires dispersion correction and at least one standard star
+observation.
+.LP
+The \f(CWresize\fR option resets the edges of the extraction apertures based
+on the profile for each object and standard star order.  The default
+resizing is to the 5% point relative to the peak measured above the
+background.  This allows following changes in the seeing.  However, one
+should consider the consequences of this if attempting to flux calibrate
+the observations.  Except in quicklook mode, the apertures for each object
+and standard star observation may be reviewed graphically and further
+adjustments made to the aperture width and background regions.
+.LP
+The apertures for each observation are adjusted for small shifts relative
+to the reference aperture definitions.  If you think this is not sufficient,
+say to account for rotation of the detector or for differing atmospheric
+dispersion, the \f(CWtrace\fR option allows redefining the aperture trace
+functions for each observation.  Note this is only allowed in non-quicklook
+mode.
+.LP
+The \f(CWclean\fR option invokes a profile
+fitting and deviant point rejection algorithm as well as a variance weighting
+of points in the aperture.  See the next section for more about
+requirements to use this option.
+.LP
+The \f(CWbackground\fR option selects a type of correction for background
+or scattered light.  If the type is "scattered" a global scattered light
+is fit to the data between the apertures  and subtracted from the images.
+\fINote that the input images are modified by this operation\fR.
+This option is slow and is not allowed in quicklook
+mode.  Alternatively, a local background may be subtracted using
+background regions defined for each aperture.  The background may be
+within the slit for a sky subtraction or outside of the slit for a
+local scattered light subtraction.  The data in the regions
+may be averaged, medianed, or the minimum value used.  Another choice
+is to fit the data in the background regions by a function and interpolate
+to the object aperture.
+.LP
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\f(CWupdate\fR flag is set.  The changes which will cause an update are a new
+reference image, adding the scattered light subtraction option, a new arc
+reference image, and new standard stars.  If all input spectra are to be
+processed regardless of previous processing the \f(CWredo\fR flag may be
+used.  Note that reprocessing clobbers the previously processed output
+spectra.
+.LP
+The final step is to plot the spectra if the \f(CWsplot\fR option is
+selected.  In non-quicklook mode there is a query which may be
+answered either in lower or upper case.  The plotting uses the interactive
+task \fBsplot\fR.  In quicklook mode the plot appears noninteractively
+using the task \fBspecplot\fR.  
+.LP
+The \f(CWquicklook\fR option provides a simpler, less interactive, mode.
+The quicklook mode automatically assigns the reference apertures to
+the object and standard star observations without interactive review
+or tracing, does not do the time consuming scattered light correction,
+and the \f(CWsplot\fR option selects a noninteractive plot to be
+shown at the end of processing of each object and standard star
+spectrum.  While the algorithms used in quicklook mode are nearly the same
+as in non-quicklook mode and the final results may be the same it is
+recommended that the greater degree of monitoring and review in
+non-quicklook mode be used for careful final reductions.
+.LP
+The batch processing option allows object spectra to be processed as a
+background or batch job.  This will occur only if the interactive
+\f(CWsplot\fR option is not active; either not set, turned off during
+processing with "NO", or in quicklook mode.  In batch processing the
+terminal output is suppressed.
+.LP
+The \f(CWlistonly\fR option prints a summary of the processing steps
+which will be performed on the input spectra without actually doing
+anything.  This is useful for verifying which spectra will be affected
+if the input list contains previously processed spectra.  The listing
+does not include any arc spectra which may be extracted to dispersion
+calibrate an object spectrum.
+.LP
+The last parameter (excluding the task mode parameter) points to
+another parameter set for the algorithm parameters.  The default
+parameter set is called \fBsparams\fR.  The algorithm parameters are
+discussed further in the next section.
+.NH
+Algorithms and Algorithm Parameters
+.LP
+This section summarizes the various algorithms used by the
+\fBdoecslit\fR task and the parameters which control and modify the
+algorithms.  The algorithm parameters available to you are
+collected in the parameter set \fBsparams\fR.  These parameters are
+taken from the various general purpose tasks used by the \fBdoecslit\fR
+processing task.  Additional information about these parameters and
+algorithms may be found in the help for the actual
+task executed.  These tasks are identified below.  The aim of this
+parameter set organization is to collect all the algorithm parameters
+in one place separate from the processing parameters and include only
+those which are relevant for echelle slit data.  The parameter values
+can be changed from the defaults by using the parameter editor,
+.V1
+
+cl> epar sparams
+
+.V2
+or simple typing \f(CWsparams\fR.
+The parameter editor can also be entered when editing the \fBdoecslit\fR
+parameters by typing \f(CW:e\fR when positioned at the \f(CWsparams\fR
+parameter.  Figure 3 shows the parameter set.
+.KS
+
+.ce
+Figure 3: Algorithm Parameter Set
+
+.V1
+cl> epar sparams
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = echelle
+   TASK = sparams
+
+(line   =        INDEF) Default dispersion line
+(nsum   =           10) Number of dispersion lines to sum
+(extras =           no) Extract sky, sigma, etc.?
+
+                        -- AUTOMATIC APERTURE RESIZING PARAMETERS --
+(ylevel =         0.05) Fraction of peak or intensity for resizing
+.KE
+.V1
+
+                        -- TRACE PARAMETERS --
+(t_step =           10) Tracing step
+(t_funct=      spline3) Trace fitting function
+(t_order=            2) Trace fitting function order
+(t_niter=            1) Trace rejection iterations
+(t_low  =           3.) Trace lower rejection sigma
+(t_high =           3.) Trace upper rejection sigma
+
+                        -- BACKGROUND AND SCATTERED LIGHT PARAMETERS --
+(b_funct=     legendre) Background function
+(b_order=            1) Background function order
+(b_naver=         -100) Background average or median
+(b_niter=            0) Background rejection iterations
+(b_low  =           3.) Background lower rejection sigma
+(b_high =           3.) Background upper rejection sigma
+(buffer =           1.) Buffer distance from apertures
+(apscat1=             ) Fitting parameters across the dispersion
+(apscat2=             ) Fitting parameters along the dispersion
+
+                        -- APERTURE EXTRACTION PARAMETERS --
+(weights=         none) Extraction weights (none|variance)
+(pfit   =        fit1d) Profile fitting algorithm (fit1d|fit2d)
+(lsigma =           3.) Lower rejection threshold
+(usigma =           3.) Upper rejection threshold
+
+                                -- ARC DISPERSION FUNCTION PARAMETERS --
+(coordli= linelist$thar.dat) Line list
+(match  =           1.) Line list matching limit in Angstroms
+(fwidth =           4.) Arc line widths in pixels
+(cradius=          10.) Centering radius in pixels
+(i_funct=     legendre) Echelle coordinate function
+(i_xorde=            3) Order of coordinate function along dispersion
+(i_yorde=            3) Order of coordinate function across dispersion
+(i_niter=            3) Rejection iterations
+(i_low  =           3.) Lower rejection sigma
+(i_high =           3.) Upper rejection sigma
+(refit  =          yes) Refit coordinate function when reidentifying
+
+                        -- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+(select =       interp) Selection method for reference spectra
+(sort   =           jd) Sort key
+(group  =          ljd) Group key
+(time   =           no) Is sort key a time?
+(timewra=          17.) Time wrap point for time sorting
+
+                        -- DISPERSION CORRECTION PARAMETERS --
+(lineari=          yes) Linearize (interpolate) spectra?
+(log    =           no) Logarithmic wavelength scale?
+(flux   =          yes) Conserve flux?
+
+                        -- SENSITIVITY CALIBRATION PARAMETERS --
+(bandwid=          10.) Bandpass widths
+(bandsep=          10.) Bandpass separation
+(s_inter=          yes) Graphic interaction to examine/define bandpasses
+(s_funct=      spline3) Fitting function
+(s_order=            1) Order of sensitivity function
+(fnu    =           no) Create spectra having units of FNU?
+
+.V2
+.NH 2
+Aperture Definitions
+.LP
+The first operation is to define the extraction apertures, which include the
+aperture width, background regions, and position dependence with
+wavelength, for the input echelle slit spectra and, if flux calibration is
+selected, the standard star spectra.  This is done only for spectra which
+do not have previously defined apertures unless the \f(CWredo\fR option is
+set to force all definitions to be redone.  Thus, apertures may be
+defined separately using the \fBapextract\fR tasks.  This is particularly
+useful if one needs to use reference images to define apertures for very
+weak spectra which are not well centered or traced by themselves.
+.LP
+Initially apertures are defined for a specified \fIaperture reference\fR
+image.  The selected number of orders are found automatically by selecting
+the highest peaks in a cut across the dispersion.  Apertures are assigned
+with a width given by the \f(CWwidth\fR parameter and numbered sequentially.
+The background regions are also defined in terms of the width parameter
+starting at one width distance from the profile center and extending to two
+widths on both sides of the profile.  As an example, if the width parameter
+is 5 pixels the default aperture limits are +/- 2.5 pixels and the
+background sample regions will be "-10:-5,5:10".  If the \f(CWresize\fR
+parameter is set the aperture limits are adjusted to a specified point on
+the spectrum profile (see \fBapresize\fR).
+.LP
+A query is then given allowing the aperture definitions to be reviewed and
+modified.  Queries made by \fBdoecslit\fR generally may be answered with either
+lower case "yes" or "no" or with upper case "YES" or "NO".  The upper
+case responses apply to all further queries and so are used to eliminate
+further queries of that kind.
+.LP
+Reviewing the aperture definitions is highly recommended to check the
+aperture numbering, aperture limits, and background regions.  The aperture
+numbers must be linearly related, with a slope of +/- 1, to the true order
+numbers though absolute order numbers need not be known.  The key point is
+that if an order is skipped the aperture numbers must also skip.  The
+background regions are checked with the 'b' key.  Typically one adjusts all
+the background regions at the same time by selecting all apertures with
+the 'a' key first.  To exit the background and aperture editing steps type
+'q'.
+.LP
+Next the positions of the orders at various points along the dispersion
+are measured and "trace functions" are fit.  The user is asked whether
+to fit each trace function interactively.  This is selected to adjust
+the fitting parameters such as function type and order.  When
+interactively fitting a query is given for each aperture.  After the
+first aperture one may skip reviewing the other traces.
+.LP
+After the aperture reference image is done all the object and standard star
+images are checked for aperture definitions and those without definitions
+are assigned apertures.  The assignment consists of inheriting the aperture
+from the reference aperture image, recentering the apertures based on an
+average shift that best centers all the apertures, resizing the apertures
+if the resize option is selected, and retracing the spectral orders if the
+retracing option is selected.  Retracing is only allowed in non-quicklook
+mode (set by the \f(CWquicklook\fR parameter).  Also interactive review of
+the aperture definitions is only done in
+non-quicklook mode.  In quicklook mode the aperture definitions are all set
+noninteractively without retracing.  It is recommended that quicklook only
+be used for initial quick extractions and calibration and that for final
+reductions one at least review the aperture definitions and possibly
+retrace each observation.
+.LP
+The above steps are all performed using tasks from the \fBapextract\fR
+package and parameters from the \fBsparams\fR parameters.  As a quick
+summary, the dispersion direction of the spectra are determined from the
+package \fBdispaxis\fR parameter if not defined in the image header.  The default
+line or column for finding the object position on the slit and the number
+of image lines or columns to sum are set by the \f(CWline\fR and \f(CWnsum\fR
+parameters.  A line of INDEF (the default) selects the middle of the
+image.  The automatic finding algorithm is described for the task
+\fBapfind\fR and basically finds the strongest peaks.  The resizing is
+described in the task \fBapresize\fR and the parameters used are also
+described there.  The tracing is
+done as described in \fBaptrace\fR and consists of stepping along the image
+using the specified \f(CWt_step\fR parameter.  The function fitting uses the
+\fBicfit\fR commands with the other parameters from the tracing section.
+.NH 2
+Background or Scattered Light Subtraction
+.LP
+In addition to not subtracting any sky or scattered light there are two
+approaches to subtracting background light.  The first is to determine
+a smooth global scattered light component.  The second is to subtract
+a locally determined background at each point along the dispersion and
+for each aperture.  This can be either for a sky subtraction if the
+background regions are within the slit or scattered light if the
+background regions are outside of the slit.  Note that background
+subtraction is only done for object and standard star images and not
+for arc spectra.  Also, the global scattered light option is not done
+in quicklook mode.
+.LP
+The global scattered light fitting and subtraction is done with the task
+\fBapscatter\fR.  The function fitting parameters are set interactively
+using the aperture reference spectrum.  All other subtractions are done
+noninteractively with the same set of parameters.  The scattered light is
+subtracted from the input images, thus modifying them, and one might wish
+to first make backups of the original images.
+.LP
+The scattered light is measured between the apertures using a specified
+buffer distance from the aperture edges.  The scattered light pixels are
+fit by a series of one dimensional functions across the dispersion.  The
+independent fits are then smoothed along the dispersion by again fitting
+low order functions.  These fits then define the smooth scattered light
+surface to be subtracted from the image.  The fitting parameters are
+defined and recorded in the two parameter sets \f(CWapscat1\fR and
+\f(CWapscat2\fR.  The scattered light algorithm is described more fully in
+\fBapscatter\fR.  This algorithm is relatively slow.
+.LP
+Local background subtraction is done during extraction based on background
+regions and parameters defined by the default background parameters or
+changed during interactive review of the apertures.  The background
+subtraction options are to subtract the average, median, or minimum of the
+pixels in the background regions, or to fit a function and subtract the
+function from under the extracted object pixels.  The background regions
+are specified in pixels from the aperture center and follow changes in
+center of the spectrum along the dispersion.  The syntax is colon separated
+ranges with multiple ranges separated by a comma or space.  The background
+fitting uses the \fBicfit\fR routines which include medians, iterative
+rejection of deviant points, and a choice of function types and orders.
+Note that it is important to use a method which rejects cosmic rays such as
+using either medians over all the background regions (\f(CWbackground\fR =
+"median") or median samples during fitting (\f(CWb_naverage\fR < -1).  The
+background subtraction algorithm and options are described in greater
+detail in \fBapsum\fR and \fBapbackground\fR.
+.NH 2
+Extraction
+.LP
+The actual extraction of the spectra is done by summing across the
+fixed width apertures at each point along the dispersion.
+The default is to simply sum the pixels using
+partial pixels at the ends.  There is an option to weight the
+sum based on a Poisson variance model using the \f(CWreadnoise\fR and
+\f(CWgain\fR detector parameters.  Note that if the \f(CWclean\fR
+option is selected the variance weighted extraction is used regardless
+of the \f(CWweights\fR parameter.  The sigma thresholds for cleaning
+are also set in the \fBsparams\fR parameters.
+.LP
+The cleaning and variance weighting options require knowing the effective
+(i.e. accounting for any image combining) read out noise and gain.
+These numbers need to be adjusted if the image has been processed
+such that the intensity scale has a different origin (such as
+a scattered light subtraction) or scaling (such as caused by unnormalized
+flat fielding).  These options also require using background subtraction
+if the profile does not go to zero.  For optimal extraction and
+cleaning to work it is recommended that any flat fielding be done
+using flat fields produced by \fBapflatten\fR, no scattered light
+correction, and using background subtraction if there is any
+appreciable sky or to compensate for scattered light.
+For further discussion of cleaning and variance weighted extraction see
+\fBapvariance\fR and \fBapprofiles\fR as well as  \fBapsum\fR.
+.NH 2
+Dispersion Correction
+.LP
+If dispersion correction is not selected, \f(CWdispcor\fR=no, then the object
+spectra are simply extracted.  The extracted spectra may be plotted
+by setting the \f(CWsplot\fR option.  This produces a query and uses
+the interactive \fBsplot\fR task in non-quicklook mode and uses
+\fBspecplot\fR noninteractively in quicklook mode.
+.LP
+Dispersion corrections are applied to the extracted spectra if the
+\f(CWdispcor\fR processing parameter is set.  There
+are three basic steps involved; determining the dispersion functions
+relating pixel position to wavelength, assigning the appropriate
+dispersion function to a particular observation, and either storing
+the nonlinear dispersion function in the image headers or resampling the
+spectra to evenly spaced pixels in wavelength.
+.LP
+The first arc spectrum in the arc list is used to define the reference
+dispersion solution.  It is extracted using the reference aperture definition.
+Note extractions of arc spectra are not background or scattered light
+subtracted.  The interactive task \fBecidentify\fR is used to define the
+dispersion function.  The idea is to mark some lines in a few orders whose
+wavelengths are known (with the line list used to supply additional lines after
+the first few identifications define the approximate wavelengths) and to fit a
+function giving the wavelength from the aperture number and pixel position.
+.LP
+The arc dispersion function parameters are for \fBecidentify\fR and it's
+related partner \fBecreidentify\fR.  The parameters define a line list for
+use in automatically assigning wavelengths to arc lines, a centering width
+(which should match the line widths at the base of the lines), the
+dispersion function type and orders, parameters to exclude bad lines from
+function fits, and defining whether to refit the dispersion function as
+opposed to simply determining a zero point shift.  The defaults should
+generally be adequate and the dispersion function fitting parameters may be
+altered interactively.  One should consult the help for the two tasks for
+additional details of these parameters and the interactive operation of
+\fBecidentify\fR.
+.LP
+Once the reference dispersion function is defined other arc spectra are
+extracted as required by the object spectra.  The assignment of arcs is
+done either explicitly with an arc assignment table (parameter
+\f(CWarctable\fR) or based on a header parameter such as a time.
+This assignments are made by the task
+\fBrefspectra\fR.  When two arcs are assigned to an object spectrum an
+interpolation is done between the two dispersion functions.  This makes an
+approximate correction for steady drifts in the dispersion.
+.LP
+The tasks \fBsetjd\fR and \fBsetairmass\fR are automatically run on all
+spectra.  This computes and adds the header parameters for the Julian date
+(JD), the local Julian day number (LJD), the universal time (UTMIDDLE), and
+the air mass at the middle of the exposure.  The default arc assignment is
+to use the Julian date grouped by the local Julian day number.  The
+grouping allows multiple nights of data to be correctly assigned at the
+same time.
+.LP
+In non-quicklook mode the arc spectra assigned to each object are
+extracted using the same apertures as the object.  This accounts for
+changes in the recentering, aperture sizes, and tracing functions.
+In quicklook mode the arc spectra are extracted using the reference
+apertures.  When the same arc is used for several object images this
+allows the arc spectrum to only be extracted once.
+.LP
+Defining the dispersion function for a new arc extraction is done with
+the task \fBecreidentify\fR.  This is done noninteractively with log
+information recorded about the line reidentifications and the fit.
+.LP
+The last step of dispersion correction is setting the dispersion
+of the object image from the arc images.  There are two choices here.
+If the \f(CWlinearize\fR parameter is not set the nonlinear dispersion
+function is stored in the image header.  Other IRAF tasks interpret
+this information when dispersion coordinates are needed for plotting
+or analysis.  This has the advantage of not requiring the spectra
+to be interpolated and the disadvantage that the dispersion
+information is only understood by IRAF tasks and cannot be readily
+exported to other analysis software.
+.LP
+If the \f(CWlinearize\fR parameter is set then the spectra are resampled to a
+linear dispersion relation either in wavelength or the log of the
+wavelength.  For echelle spectra each order is linearized independently so
+that the wavelength interval per pixel is different in different orders.
+This preserves most of the resolution and avoids over or under sampling of
+the highest or lowest dispersion orders.  The wavelength limits are
+taken from the limits determined from the arc reference spectrum and
+the number of pixels is the same as the original images.  The dispersion
+per pixel is then derived from these constraints.
+.LP
+The linearization algorithm  parameters allow selecting the interpolation
+function type, whether to conserve flux per pixel by integrating across the
+extent of the final pixel, and whether to linearize to equal linear or
+logarithmic intervals.  The latter may be appropriate for radial velocity
+studies.  The default is to use a fifth order polynomial for interpolation,
+to conserve flux, and to not use logarithmic wavelength bins.  These
+parameters are described fully in the help for the task \fBdispcor\fR which
+performs the correction.
+.NH 2
+Flux Calibration
+.LP
+Flux calibration consists of an extinction correction and an instrumental
+sensitivity calibration.  The extinction correction only depends on the
+extinction function defined by the package parameter \f(CWextinct\fR and
+determination of the airmass from the header parameters (the air mass is
+computed by \fBsetairmass\fR as mentioned earlier).  The sensitivity
+calibration depends on a sensitivity calibration spectrum determined from
+standard star observations for which there are tabulated absolute fluxes.
+The task that applies both the extinction correction and sensitivity
+calibration to each extracted object spectrum is \fBcalibrate\fR.  Consult
+the manual page for this task for more information.
+.LP
+Generation of the sensitivity calibration spectrum is done before
+processing any object spectra since it has two interactive steps and
+requires all the standard star observations.  The first step is tabulating
+the observed fluxes over the same bandpasses as the calibrated absolute
+fluxes.  For very high resolution it may be the case that the measured
+calibration bandpasses are too large or sparse.  In this case one must
+interpolate the calibration data to bandpasses appropriate for the data.
+If the bandpass widths and separations are given as INDEF then the same
+bandpasses as in the calibration file are used.  Otherwise a uniform grid
+of bandpasses is interpolated.  Using interpolated bandpasses is not
+rigorous but is sometimes the only choice for echelle spectra.
+.LP
+The standard star tabulations are done after each standard star is
+extracted and dispersion corrected.  You are asked for the name of the
+standard star as tabulated in the absolute flux data files in the directory
+\f(CWcaldir\fR defined by the package parameters.  If the \f(CWinteract\fR
+parameter is yes the bandpasses can be displayed on the data and you can
+interactively add or delete bandpasses. The tabulation of the standard star
+observations over the standard bandpasses is done by the task
+\fBstandard\fR.  The tabulated data is stored in the file \f(CWstd\fR.  Note
+that if the \f(CWredo\fR flag is not set any new standard stars specified in
+subsequent executions of \fBdoecslit\fR are added to the previous data in
+the data file, otherwise the file is first deleted.  Modification of the
+tabulated standard star data, such as by adding new stars, will cause any
+spectra in the input list which have been previously calibrated to be
+reprocessed if the \f(CWupdate\fR flag is set.
+.LP
+After the standard star calibration bandpass fluxes are tabulated the
+information from all the standard stars is combined to produce a
+sensitivity function for use by \fBcalibrate\fR.  The sensitivity function
+determination is interactive and uses the task \fBsensfunc\fR.  This task
+allows fitting a smooth sensitivity function to the ratio of the observed
+to calibrated fluxes verses wavelength.  The types of manipulations one
+needs to do include deleting bad observations, possibly removing variable
+extinction (for poor data), and possibly deriving a revised extinction
+function.  This is a complex operation and one should consult the manual
+page for \fBsensfunc\fR.  The sensitivity function is saved as one
+dimensional spectra (one per order) with the root name \f(CWsens\fR.
+Deletion of these images will also cause reprocessing to occur if the
+\f(CWupdate\fR flag is set.
+.NH
+References
+.NH 2
+IRAF Introductory References
+.LP
+Work is underway on a new introductory guide to IRAF.  Currently, the
+work below is the primary introduction.
+.IP
+P. Shames and D. Tody, \fIA User's Introduction to the IRAF Command
+Language\fR, Central Computer Services, NOAO, 1986.
+.NH 2
+CCD Reductions
+.IP
+F. Valdes, \fIThe IRAF CCD Reduction Package -- CCDRED\fR, Central
+Computer Services, NOAO, 1987.
+.IP
+F. Valdes, \fIUser's Guide to the CCDRED Package\fR, Central
+Computer Services, NOAO, 1988.  Also on-line as \f(CWhelp ccdred.guide\fR.
+.IP
+P. Massey, \fIA User's Guide to CCD Reductions with IRAF\fR, Central
+Computer Services, NOAO, 1989.
+.NH 2
+Aperture Extraction Package
+.IP
+F. Valdes, \fIThe IRAF APEXTRACT Package\fR, Central Computer Services,
+NOAO, 1987 (out-of-date).
+.NH 2
+Task Help References
+.LP
+Each task in the \fBspecred\fR packages and tasks used by \fBdofibers\fR have
+help pages describing the parameters and task in some detail.  To get
+on-line help type
+.V1
+
+cl> help \fItaskname\fR
+
+.V2
+The output of this command can be piped to \fBlprint\fR to make a printed
+copy.
+
+.V1
+      apall - Extract 1D spectra (all parameters in one task)
+  apdefault - Set the default aperture parameters and apidtable
+     apedit - Edit apertures interactively
+     apfind - Automatically find spectra and define apertures
+      apfit - Fit 2D spectra and output the fit, difference, or ratio
+  apflatten - Remove overall spectral and profile shapes from flat fields
+     apmask - Create and IRAF pixel list mask of the apertures
+apnormalize - Normalize 2D apertures by 1D functions
+ aprecenter - Recenter apertures
+   apresize - Resize apertures
+  apscatter - Fit and subtract scattered light
+      apsum - Extract 1D spectra
+    aptrace - Trace positions of spectra
+
+      bplot - Batch plots of spectra
+  calibrate - Apply extinction and flux calibrations to spectra
+  continuum - Fit the continuum in spectra
+   deredden - Apply interstellar extinction corrections
+    dispcor - Dispersion correct spectra
+     dopcor - Doppler correct spectra
+ ecidentify - Identify features in spectrum for dispersion solution
+ecreidentify - Automatically identify features in spectra
+ refspectra - Assign wavelength reference spectra to other spectra
+     sarith - Spectrum arithmetic
+   scombine - Combine spectra
+      scopy - Select and copy apertures in different spectral formats
+   sensfunc - Create sensitivity function
+ setairmass - Compute effective airmass and middle UT for an exposure
+      setjd - Compute and set Julian dates in images
+      slist - List spectrum header parameters
+   specplot - Stack and plot multiple spectra
+      splot - Preliminary spectral plot/analysis
+   standard - Identify standard stars to be used in sensitivity calc
+
+   doecslit - Process Echelle slit spectra
+      demos - Demonstrations and tests
+
+            Additional help topics
+
+   onedspec.package - Package parameters and general description of package
+  apextract.package - Package parameters and general description of package
+ approfiles - Profile determination algorithms
+ apvariance - Extractions, variance weighting, cleaning, and noise model
+   center1d - One dimensional centering algorithm
+      icfit - Interactive one dimensional curve fitting
+
+.V2
+.SH
+Appendix A: DOECSLIT Parameters
+.LP
+.nr PS 8
+.nr VS 10
+objects
+.LS
+List of object images to be processed.  Previously processed spectra are
+ignored unless the \f(CWredo\fR flag is set or the \f(CWupdate\fR flag is set
+and dependent calibration data has changed.  If the images contain the
+keyword IMAGETYP then only those with a value of "object" or "OBJECT"
+are used and those with a value of "comp" or "COMPARISON" are added
+to the list of arcs.  Extracted spectra are ignored.
+.LE
+apref = ""
+.LS
+Aperture reference spectrum.  This spectrum is used to define the basic
+extraction apertures and is typically a bright star spectrum.
+.LE
+arcs = "" (at least one if dispersion correcting)
+.LS
+List of arc calibration spectra.  These spectra are used to define
+the dispersion functions.  The first spectrum is used to mark lines
+and set the dispersion function interactively and dispersion functions
+for all other arc spectra are derived from it.  If the images contain
+the keyword IMAGETYP then only those with a value of "comp" or
+"COMPARISON" are used.  All others are ignored as are extracted spectra.
+.LE
+arctable = "" (optional) (refspectra)
+.LS
+Table defining which arc spectra are to be assigned to which object
+spectra (see \fBrefspectra\fR).  If not specified an assignment based
+on a header parameter, \f(CWsparams.sort\fR, such as the Julian date
+is made.
+.LE
+standards = "" (at least one if flux calibrating)
+.LS
+List of standard star spectra.  The standard stars must have entries in
+the calibration database (package parameter \f(CWechelle.caldir\fR).
+.LE
+
+readnoise = 0., gain = 1. (apsum)
+.LS
+Read out noise in photons and detector gain in photons per data value.
+This parameter defines the minimum noise sigma and the conversion between
+photon Poisson statistics and the data number statistics.  Image header
+keywords (case insensitive) may be specified to obtain the values from the
+image header.
+.LE
+datamax = INDEF (apsum.saturation)
+.LS
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the standard star or
+arc spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.LE
+norders = 10 (apfind)
+.LS
+Number of orders to be found automatically.
+.LE
+width = 5. (apedit)
+.LS
+Approximate full width of the spectrum profiles.  This parameter is used
+to define a width and error radius for the profile centering algorithm,
+and defaults for the aperture limits and background regions.
+.LE
+
+dispcor = yes
+.LS
+Dispersion correct spectra?  This may involve either defining a nonlinear
+dispersion coordinate system in the image header or resampling the
+spectra to uniform linear wavelength coordinates as selected by
+the parameter \f(CWsparams.linearize\fR.
+.LE
+extcor = no
+.LS
+Extinction correct the spectra?
+.LE
+fluxcal = no
+.LS
+Flux calibrate the spectra using standard star observations?
+.LE
+resize = no (apresize)
+.LS
+Resize the default apertures for each object based on the spectrum profile?
+.LE
+clean = no (apsum)
+.LS
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction.  In addition the datamax parameters
+can be useful.
+.LE
+trace = yes (non-quicklook mode only) (aptrace)
+.LS
+Allow tracing each object spectrum separately?  If not set then the trace
+from the aperture reference is used, with recentering to allow for shifts
+across the dispersion.  If set then each object and standard star
+image is retraced.  Retracing is NOT done in quicklook mode.
+.LE
+background = "none" (apsum, apscatter)
+.LS
+Type of background light subtraction.  The choices are "none" for no
+background subtraction, "scattered" for a global scattered light
+subtraction, "average" to average the background within background regions,
+"median" to use the median in background regions, "minimum" to use the
+minimum in background regions, or "fit" to fit across the dispersion using
+the background within background regions.  The scattered light option fits
+and subtracts a smooth global background and modifies the input images.
+This is a slow operation and so is NOT performed in quicklook mode.  The
+other background options are local to each aperture.  The "fit" option uses
+additional fitting parameters from \fBsparams\fR and the "scattered" option
+uses parameters from \fBapscat1\fR and \fBapscat2\fR.
+.LE
+splot = no
+.LS
+Plot the final spectra?  In quicklook mode a noninteractive, stacked plot
+is automatically produced using the task \fBspecplot\fR while in
+non-quicklook mode a query is given and the task \fBsplot\fR is used for
+interactive plotting.
+.LE
+redo = no
+.LS
+Redo operations previously done?  If no then previously processed spectra
+in the objects list will not be processed unless required by the
+update option.
+.LE
+update = no
+.LS
+Update processing of previously processed spectra if the aperture
+reference image, the dispersion reference image, or standard star
+calibration data are changed?
+.LE
+quicklook = no
+.LS
+Extract and calibrate spectra with minimal interaction?  In quicklook mode
+only aperture reference definitions, the initial dispersion function
+solution, and the standard star setup are done interactively.  Scattered
+light subtraction and individual object tracing are not performed.
+Normally the \f(CWsplot\fR option is set in this mode to produce an automatic
+final spectrum plot for each object.  It is recommended that this mode not be
+used for final reductions.
+.LE
+batch = no
+.LS
+Process spectra as a background or batch job provided there are no interactive
+steps remaining.
+.LE
+listonly = no
+.LS
+List processing steps but don't process?
+.LE
+
+sparams = "" (pset)
+.LS
+Name of parameter set containing additional processing parameters.  This
+parameter is only for indicating the link to the parameter set
+\fBsparams\fR and should not be given a value.  The parameter set may be
+examined and modified in the usual ways (typically with "epar sparams"
+or ":e sparams" from the parameter editor).  The parameters are
+described below.
+.LE
+
+.ce
+-- GENERAL PARAMETERS --
+
+line = INDEF, nsum = 10
+.LS
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, recentering, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.LE
+extras = no (apsum)
+.LS
+Include raw unweighted and uncleaned spectra, the background spectra, and
+the estimated sigma spectra in a three dimensional output image format.
+See the discussion in the \fBapextract\fR package for further information.
+.LE
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+
+ylevel = 0.05 (apresize)
+.LS
+Fraction of the peak to set aperture limits during automatic resizing.
+.LE
+
+.ce
+-- TRACE PARAMETERS --
+
+t_step = 10 (aptrace)
+.LS
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \f(CWnsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.LE
+t_function = "spline3", t_order = 2 (aptrace)
+.LS
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.LE
+t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+.LS
+Default number of rejection iterations and rejection sigma thresholds.
+.LE
+
+.ce
+-- BACKGROUND AND SCATTERED LIGHT PARAMETERS --
+
+b_function = "legendre", b_order = 1 (apsum)
+.LS
+Default background fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.LE
+b_naverage = -100 (apsum)
+.LS
+Default number of points to average or median.  Positive numbers
+average that number of sequential points to form a fitting point.
+Negative numbers median that number, in absolute value, of sequential
+points.  A value of 1 does no averaging and each data point is used in the
+fit.
+.LE
+b_niterate = 0 (apsum)
+.LS
+Default number of rejection iterations.  If greater than zero the fit is
+used to detect deviant fitting points and reject them before repeating the
+fit.  The number of iterations of this process is given by this parameter.
+.LE
+b_low_reject = 3., b_high_reject = 3. (apsum)
+.LS
+Default background lower and upper rejection sigmas.  If greater than zero
+points deviating from the fit below and above the fit by more than this
+number of times the sigma of the residuals are rejected before refitting.
+.LE
+buffer = 1. (apscatter)
+.LS
+Buffer distance from the edge of any aperture for data to be included
+in the scattered light determination.  This parameter may be modified
+interactively.
+.LE
+apscat1 = "", apscat2 = "" (apscatter)
+.LS
+Parameter sets for the fitting functions across and along the dispersion.
+These parameters are those used by \fBicfit\fR.  These parameters are
+usually set interactively.
+.LE
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+
+weights = "none" (apsum) (none|variance)
+.LS
+Type of extraction weighting.  Note that if the \f(CWclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+
+"none"
+.LS
+The pixels are summed without weights except for partial pixels at the
+ends.
+.LE
+"variance"
+.LS
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \f(CWgain\fR and \f(CWreadnoise\fR
+parameters.
+.LE
+.LE
+pfit = "fit1d" (apsum and approfile) (fit1d|fit2d)
+.LS
+Type of profile fitting algorithm to use.  The "fit1d" algorithm is
+preferred except in cases of extreme tilt.
+.LE
+lsigma = 3., usigma = 3. (apsum)
+.LS
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.LE
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+
+threshold = 10. (identify/reidentify)
+.LS
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.LE
+coordlist = "linelist$thar.dat" (ecidentify)
+.LS
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelist$".
+.LE
+match = 1. (ecidentify)
+.LS
+The maximum difference for a match between the dispersion function computed
+value and a wavelength in the coordinate list.
+.LE
+fwidth = 4. (ecidentify)
+.LS
+Approximate full base width (in pixels) of arc lines.
+.LE
+cradius = 10. (reidentify)
+.LS
+Radius from previous position to reidentify arc line.
+.LE
+i_function = "legendre", i_xorder = 3, i_yorder = 3 (ecidentify)
+.LS
+The default function, function order for the pixel position dependence, and
+function order for the aperture number dependence to be fit to the arc
+wavelengths.  The functions choices are "chebyshev" or "legendre".
+.LE
+i_niterate = 3, i_low = 3.0, i_high = 3.0 (ecidentify)
+.LS
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.LE
+refit = yes (ecreidentify)
+.LS
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.LE
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+
+select = "interp" (refspectra)
+.LS
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+
+average
+.LS
+Average two reference spectra without regard to any sort parameter.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.
+This option is used to assign two reference spectra, with equal weights,
+independent of any sorting parameter.
+.LE
+following
+.LS
+Select the nearest following spectrum in the reference list based on the
+sorting parameter.  If there is no following spectrum use the nearest preceding
+spectrum.
+.LE
+interp
+.LS
+Interpolate between the preceding and following spectra in the reference
+list based on the sorting parameter.  If there is no preceding and following
+spectrum use the nearest spectrum.  The interpolation is weighted by the
+relative distances of the sorting parameter.
+.LE
+match
+.LS
+Match each input spectrum with the reference spectrum list in order.
+This overrides the reference aperture check.
+.LE
+nearest
+.LS
+Select the nearest spectrum in the reference list based on the sorting
+parameter.
+.LE
+preceding
+.LS
+Select the nearest preceding spectrum in the reference list based on the
+sorting parameter.  If there is no preceding spectrum use the nearest following
+spectrum.
+.LE
+.LE
+sort = "jd" (setjd and refspectra)
+.LS
+Image header keyword to be used as the sorting parameter for selection
+based on order.  The header parameter must be numeric but otherwise may
+be anything.  Common sorting parameters are times or positions.
+.LE
+group = "ljd" (setjd and refspectra)
+.LS
+Image header keyword to be used to group spectra.  For those selection
+methods which use the group parameter the reference and object
+spectra must have identical values for this keyword.  This can
+be anything but it must be constant within a group.  Common grouping
+parameters are the date of observation "date-obs" (provided it does not
+change over a night) or the local Julian day number.
+.LE
+time = no, timewrap = 17. (refspectra)
+.LS
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.LE
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+
+linearize = yes (dispcor)
+.LS
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling using
+the linear dispersion parameters specified by other parameters.  If
+no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data is not interpolated.  Note the interpolation
+function type is set by the package parameter \f(CWinterp\fR.
+.LE
+log = no (ecdispcor)
+.LS
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.LE
+flux = yes (ecdispcor)
+.LS
+Conserve the total flux during interpolation?  If \f(CWno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \f(CWyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.LE
+
+.ce
+-- SENSITIVITY CALIBRATION PARAMETERS --
+
+bandwidth = 10., bandsep = 10. (standard)
+.LS
+Interpolated bandpass grid.  If INDEF then the same bandpasses as in the
+calibration files are used otherwise the calibration data is interpolated
+to the specified set of bandpasses.
+.LE
+s_interact = yes (standard)
+.LS
+Display the bandpasses on the standard star data and allow interactive
+addition and deletion of bandpasses.
+.LE
+s_function = "spline3", s_order = 1 (sensfunc)
+.LS
+Function and order used to fit the sensitivity data.  The function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline3" cubic spline,
+and "spline1" linear spline.
+Order of the sensitivity fitting function.  The value corresponds to the
+number of polynomial terms or the number of spline pieces.  The default
+values may be changed interactively.
+.LE
+fnu = no (calibrate)
+.LS
+The default calibration is into units of F-lambda. If \f(CWfnu\fR = yes then
+the calibrated spectrum will be in units of F-nu.
+.LE
+
+.ce
+PACKAGE PARAMETERS
+
+dispaxis = 2
+.LS
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.  The default value defers to the
+package parameter of the same name.
+.LE
+extinction = "onedstds$kpnoextinct.dat" (standard, sensfunc, calibrate)
+.LS
+Extinction file for a site.  There are two extinction files in the
+NOAO standards library, onedstds$, for KPNO and CTIO.  These extinction
+files are used for extinction and flux calibration.
+.LE
+caldir (standard)
+.LS
+Standard star calibration directory.  A directory containing standard
+star data files.  Note that the directory name must end with '/'.
+There are a number of standard star calibrations directories in the NOAO
+standards library, onedstds$.
+.LE
+observatory = "observatory" (observatory)
+.LS
+The default observatory to use for latitude dependent computations.
+If the OBSERVAT keyword in the image header it takes precedence over
+this parameter.
+.LE
+interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc) (dispcor)
+.LS
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.V1
+        nearest - nearest neighbor
+         linear - linear
+          poly3 - 3rd order polynomial
+          poly5 - 5th order polynomial
+        spline3 - cubic spline
+           sinc - sinc function
+.V2
+.LE
+database = "database"
+.LS
+Database name used by various tasks.  This is a directory which is created
+if necessary.
+.LE
+verbose = no
+.LS
+Verbose output?  If set then almost all the information written to the
+logfile is also written to the terminal except when the task is a
+background or batch process.
+.LE
+logfile = "logfile"
+.LS
+If specified detailed text log information is written to this file.
+.LE
+plotfile = ""
+.LS
+If specified metacode plots are recorded in this file for later review.
+Since plot information can become large this should be used only if
+really desired.
+.LE
+
+.ce
+ENVIRONMENT PARAMETERS
+.LP
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
diff --git a/noao/imred/echelle/doc/dofoe.hlp b/noao/imred/echelle/doc/dofoe.hlp
new file mode 100644
index 00000000..6dfab76a
--- /dev/null
+++ b/noao/imred/echelle/doc/dofoe.hlp
@@ -0,0 +1,1155 @@
+.help dofoe Feb93 noao.imred.echelle
+.ih
+NAME
+dofoe -- Fiber Optic Echelle (FOE) data reduction task
+.ih
+USAGE
+dofoe objects
+.ih
+SUMMARY
+The \fBdofoe\fR reduction task is specialized for scattered light
+subtraction, extraction, flat fielding, and wavelength calibration of Fiber
+Optic Echelle (FOE) spectra.  There may be one fiber or two fibers where
+the second fiber is illuminated by an arc calibration during arc and object
+exposures and a flat field during flat field exposures.  It is a command
+language script which collects and combines the functions and parameters of
+many general purpose tasks to provide a single complete data reduction
+path.  The task provides a degree of guidance, automation, and record
+keeping necessary when dealing with the complexities of reducing this type
+of data.
+.ih
+PARAMETERS
+.ls objects
+List of object spectra to be processed.  Previously processed spectra are
+ignored unless the \fIredo\fR flag is set or the \fIupdate\fR flag is set and
+dependent calibration data has changed.  Extracted spectra are ignored.
+.le
+.ls apref = ""
+Aperture reference spectrum.  This spectrum is used to define the basic
+extraction apertures and is typically a flat field spectrum.
+.le
+.ls flat = "" (optional)
+Flat field spectrum.  If specified the one dimensional flat field spectrum
+is extracted and used to make flat field calibrations.
+.le
+.ls arcs = "" (at least one if dispersion correcting)
+List of arc spectra.  The first arc in the list is used to create a
+dispersion solution interactively.  All other arc spectra will be
+automatically reidentified.
+.le
+.ls arctable = "" (optional) (refspectra)
+Table defining arc spectra to be assigned to object spectra (see
+\fBrefspectra\fR).  If not specified an assignment based on a header
+parameter, \fIparams.sort\fR, such as the observation time is made.
+.le
+
+.ls readnoise = "0." (apsum)
+Read out noise in photons.  This parameter defines the minimum noise
+sigma.  It is defined in terms of photons (or electrons) and scales
+to the data values through the gain parameter.  A image header keyword
+(case insensitive) may be specified to get the value from the image.
+.le
+.ls gain = "1." (apsum)
+Detector gain or conversion factor between photons/electrons and
+data values.  It is specified as the number of photons per data value.
+A image header keyword (case insensitive) may be specified to get the value
+from the image.
+.le
+.ls datamax = INDEF (apsum.saturation)
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the flat field or
+arc spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.le
+.ls norders = 12 (apfind)
+Number of orders to be found.  This number is used during the automatic
+definition of the apertures from the aperture reference spectrum.  Note
+that when there is a second fiber for simultaneous arcs the specified
+number will be automatically doubled for finding both sets of orders.
+So in either case specify only the number of orders from a single fiber.
+The interactive review of the aperture assignments allows verification
+and adjustments to the automatic aperture definitions.
+.le
+.ls width = 4. (apedit)
+Approximate base full width of the fiber profiles.  This parameter is used
+for the profile centering algorithm.
+.le
+.ls arcaps = "2x2"
+When there is only a single fiber set this parameter to "".  When there is
+a second fiber used to create simultaneous arcs during the object exposures
+this parameter specifies a list of aperture numbers for the arc fibers.
+Since the object and arc fiber orders are paired the default setting
+expects the even number apertures to be the are apertures.  This should be
+checked interactively.
+.le
+
+.ls fitflat = yes (flat1d)
+Fit and divide the extracted flat field orders by a smooth function
+in order to normalize the wavelength response?  If not done the flat field
+spectral shape (which includes the blaze function) will be divided
+out of the object spectra, thus altering the object data values.
+If done only the small scale response variations are included in the
+flat field and the object spectra will retain their observed flux
+levels and blaze function.
+.le
+.ls background = "none" (apsum, apscatter)
+Type of background light subtraction.  The choices are "none" for no
+background subtraction, "scattered" for a global scattered light
+subtraction, "average" to average the background within background regions,
+"median" to use the median in background regions, "minimum" to use the
+minimum in background regions, or "fit" to fit across the dispersion using
+the background within background regions.  The scattered light option fits
+and subtracts a smooth global background and modifies the input images.
+This is a slow operation and so is NOT performed in quicklook mode.  The
+other background options are local to each aperture at each point along the
+dispersion.  The "fit" option uses additional fitting parameters from
+\fBparams\fR and the "scattered" option uses parameters from \fBapscat1\fR
+and \fBapscat2\fR.
+.le
+.ls clean = yes (apsum)
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction and requires reasonably good values
+for the readout noise and gain.  In addition the datamax parameters
+can be useful.
+.le
+.ls dispcor = yes
+Dispersion correct spectra?  Depending on the \fIparams.linearize\fR
+parameter this may either resample the spectra or insert a dispersion
+function in the image header.
+.le
+.ls redo = no
+Redo operations previously done?  If no then previously processed spectra
+in the objects list will not be processed (unless they need to be updated).
+.le
+.ls update = no
+Update processing of previously processed spectra if aperture, flat
+field, or dispersion reference definitions are changed?
+.le
+.ls batch = no
+Process spectra as a background or batch job.
+.le
+.ls listonly = no
+List processing steps but don't process?
+.le
+
+.ls params = "" (pset)
+Name of parameter set containing additional processing parameters.  The
+default is parameter set \fBparams\fR.  The parameter set may be examined
+and modified in the usual ways (typically with "epar params" or ":e params"
+from the parameter editor).  Note that using a different parameter file
+is not allowed.  The parameters are described below.
+.le
+
+.ce
+-- PACKAGE PARAMETERS
+
+Package parameters are those which generally apply to all task in the
+package.  This is also true of \fBdofoe\fR.
+.ls observatory = "observatory"
+Observatory at which the spectra were obtained if not specified in the
+image header by the keyword OBSERVAT.  For FOE data the image headers
+identify the observatory as "kpno" so this parameter is not used.
+For data from other observatories this parameter may be used
+as describe in \fBobservatory\fR.
+.le
+.ls interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc)
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.nf
+	nearest - nearest neighbor
+	 linear - linear
+	  poly3 - 3rd order polynomial
+	  poly5 - 5th order polynomial
+	spline3 - cubic spline
+	   sinc - sinc function
+.fi
+.le
+.ls dispaxis = 2
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.
+.le
+.ls database = "database"
+Database (directory) used for storing aperture and dispersion information.
+.le
+.ls verbose = no
+Print verbose information available with various tasks.
+.le
+.ls logfile = "logfile", plotfile = ""
+Text and plot log files.  If a filename is not specified then no log is
+kept.  The plot file contains IRAF graphics metacode which may be examined
+in various ways such as with \fBgkimosaic\fR.
+.le
+.ls records = ""
+Dummy parameter to be ignored.
+.le
+.ls version = "ECHELLE: ..."
+Version of the package.
+.le
+
+.ce
+PARAMS PARAMETERS
+
+The following parameters are part of the \fBparams\fR parameter set and
+define various algorithm parameters for \fBdofoe\fR.
+
+.ce
+--  GENERAL PARAMETERS --
+.ls line = INDEF, nsum = 10
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, recentering, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.le
+.ls extras = no (apsum)
+Include extra information in the output spectra?  When cleaning or using
+variance weighting the cleaned and weighted spectra are recorded in the
+first 2D plane of a 3D image, the raw, simple sum spectra are recorded in
+the second plane, and the estimated sigmas are recorded in the third plane.
+.le
+
+.ce
+-- DEFAULT APERTURE LIMITS --
+.ls lower = -3., upper = 3. (apdefault)
+Default lower and upper aperture limits relative to the aperture center.
+These limits are used when the apertures are first found and may be
+resized automatically or interactively.
+.le
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+.ls ylevel = 0.05 (apresize)
+Data level at which to set aperture limits during automatic resizing.
+It is a fraction of the peak relative to a local background.
+.le
+
+.ce
+-- TRACE PARAMETERS --
+.ls t_step = 10 (aptrace)
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \fInsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.le
+.ls t_function = "spline3", t_order = 2 (aptrace)
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.le
+.ls t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+Default number of rejection iterations and rejection sigma thresholds.
+.le
+
+.ce
+-- DEFAULT BACKGROUND PARAMETERS --
+.ls buffer = 1. (apscatter)
+Buffer distance from the edge of any aperture for data to be included
+in the scattered light determination.  This parameter may be modified
+interactively.
+.le
+.ls apscat1 = "", apscat2 = "" (apscatter)
+Parameter sets for the fitting functions across and along the dispersion.
+These parameters are those used by \fBicfit\fR.  These parameters are
+usually set interactively.
+.le
+.ls b_function = "legendre", b_order = 1 (apsum)
+Default background fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.le
+.ls b_naverage = -100 (apsum)
+Default number of points to average or median.  Positive numbers
+average that number of sequential points to form a fitting point.
+Negative numbers median that number, in absolute value, of sequential
+points.  A value of 1 does no averaging and each data point is used in the
+fit.
+.le
+.ls b_niterate = 0 (apsum)
+Default number of rejection iterations.  If greater than zero the fit is
+used to detect deviant fitting points and reject them before repeating the
+fit.  The number of iterations of this process is given by this parameter.
+.le
+.ls b_low_reject = 3., b_high_reject = 3. (apsum)
+Default background lower and upper rejection sigmas.  If greater than zero
+points deviating from the fit below and above the fit by more than this
+number of times the sigma of the residuals are rejected before refitting.
+.le
+.ls b_smooth = 10 (apsum)
+Box car smoothing length for background when using background
+subtraction.  Since the background noise is often the limiting factor
+for good extraction one may box car smooth the background to improve the
+statistics.
+.le
+
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+.ls weights = "none" (apsum)
+Type of extraction weighting.  Note that if the \fIclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+.ls "none"
+The pixels are summed without weights except for partial pixels at the
+ends.
+.le
+.ls "variance"
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \fIgain\fR and \fIreadnoise\fR
+parameters.
+.le
+.le
+.ls pfit = "fit1d" (apsum) (fit1d|fit2d)
+Profile fitting algorithm for cleaning and variance weighted extractions.
+The default is generally appropriate for FOE data but users
+may try the other algorithm.  See \fBapprofiles\fR for further information.
+.le
+.ls lsigma = 3., usigma = 3. (apsum)
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.le
+
+.ce
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --
+.ls f_interactive = no (fit1d)
+Fit the one dimensional flat field order spectra interactively?
+This is used if \fIfitflat\fR is set and a two dimensional flat field
+spectrum is specified.
+.le
+.ls f_function = "spline3", f_order = 20 (fit1d)
+Function and order used to fit the composite one dimensional flat field
+spectrum.  The functions are "legendre", "chebyshev", "spline1", and
+"spline3".  The spline functions are linear and cubic splines with the
+order specifying the number of pieces.
+.le
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+.ls threshold = 10. (identify/reidentify)
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.le
+.ls coordlist = "linelist$thar.dat" (ecidentify)
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelist$".
+.le
+.ls match = 1. (ecidentify)
+The maximum difference for a match between the dispersion function computed
+value and a wavelength in the coordinate list.
+.le
+.ls fwidth = 4. (ecidentify)
+Approximate full base width (in pixels) of arc lines.
+.le
+.ls cradius = 4. (reidentify)
+Radius from previous position to reidentify arc line.
+.le
+.ls i_function = "chebyshev", i_xorder = 3, i_yorder = 3 (ecidentify)
+The default function, function order for the pixel position dependence, and
+function order for the aperture number dependence to be fit to the arc
+wavelengths.  The functions choices are "chebyshev" or "legendre".
+.le
+.ls i_niterate = 3, i_low = 3.0, i_high = 3.0 (ecidentify)
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.le
+.ls refit = yes (ecreidentify)
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.le
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+.ls select = "interp" (refspectra)
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+.ls average
+Average two reference spectra without regard to any sort parameter.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.
+This option is used to assign two reference spectra, with equal weights,
+independent of any sorting parameter.
+.le
+.ls following
+Select the nearest following spectrum in the reference list based on the
+sorting parameter.  If there is no following spectrum use the nearest preceding
+spectrum.
+.le
+.ls interp
+Interpolate between the preceding and following spectra in the reference
+list based on the sorting parameter.  If there is no preceding and following
+spectrum use the nearest spectrum.  The interpolation is weighted by the
+relative distances of the sorting parameter.
+.le
+.ls match
+Match each input spectrum with the reference spectrum list in order.
+This overrides the reference aperture check.
+.le
+.ls nearest
+Select the nearest spectrum in the reference list based on the sorting
+parameter.
+.le
+.ls preceding
+Select the nearest preceding spectrum in the reference list based on the
+sorting parameter.  If there is no preceding spectrum use the nearest following
+spectrum.
+.le
+.le
+.ls sort = "jd", group = "ljd" (refspectra)
+Image header keywords to be used as the sorting parameter for selection
+based on order and to group spectra.
+A null string, "", or the word "none" may be use to disable the sorting
+or grouping parameters.
+The sorting parameter
+must be numeric but otherwise may be anything.  The grouping parameter
+may be a string or number and must simply be the same for all spectra within
+the same group (say a single night).
+Common sorting parameters are times or positions.
+In \fBdofoe\fR the Julian date (JD) and the local Julian day number (LJD)
+at the middle of the exposure are automatically computed from the universal
+time at the beginning of the exposure and the exposure time.  Also the
+parameter UTMIDDLE is computed.
+.le
+.ls time = no, timewrap = 17. (refspectra)
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.le
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+.ls linearize = yes (dispcor)
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling
+If no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data are not interpolated.
+.le
+.ls log = no (dispcor)
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.le
+.ls flux = yes (dispcor)
+Conserve the total flux during interpolation?  If \fIno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \fIyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.le
+.ih
+ENVIRONMENT PARAMETERS
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
+.ih
+DESCRIPTION
+The \fBdofoe\fR reduction task is specialized for scattered light
+subtraction, extraction, flat fielding, and wavelength calibration of Fiber
+Optic Echelle (FOE) spectra.  There may be one fiber or two fibers where
+the second fiber is illuminated by an arc calibration during arc and object
+exposures and a flat field during flat field exposures.  When there is
+just one fiber the parameter \fIarcaps\fR is set to "" and when there are
+two fibers the parameter is used to select which of the defined
+apertures are the orders from the simultaneous arc fiber.
+
+This task is a command language script which collects and combines the
+functions and parameters of many general purpose tasks to provide a single
+complete data reduction path.  The task provides a degree of guidance,
+automation, and record keeping necessary when dealing with the complexities
+of reducing this type of data.
+
+The general organization of the task is to do the interactive setup steps
+first using representative calibration data and then perform the majority
+of the reductions automatically, possibly as a background process, with
+reference to the setup data.  In addition, the task determines which setup
+and processing operations have been completed in previous executions of the
+task and, contingent on the \fIredo\fR and \fIupdate\fR options, skip or
+repeat some or all the steps.
+
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage.  Since
+\fBdofoe\fR combines many separate, general purpose tasks the description
+given here refers to these tasks and leaves some of the details to their
+help documentation.
+
+\fBUsage Outline\fR
+
+.ls 6 [1]
+The images must first be processed with \fBccdproc\fR for overscan,
+bias, and dark corrections.
+.le
+.ls [2]
+Set the \fBdofoe\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed, the flat field image as the aperture reference and
+the flat field, and one or more arc images.  If there are many
+object or arc spectra per setup you might want to prepare "@ files".
+Verify and set the format parameters, particularly the number of orders to be
+extracted and processed.  The processing parameters are set
+for simple extraction and dispersion correction but dispersion correction
+can be turned off for quicklook or background subtraction and cleaning
+may be added.
+.le
+.ls [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the execution and no further queries of that
+type will be made.
+.le
+.ls [4]
+The apertures are defined using the specified aperture reference image
+which is usually a flat field in which both the object and arc fibers are
+illuminated.  The specified number of orders are found automatically and
+sequential apertures assigned.  The resize option sets the aperture size to
+the widths of the profiles at a fixed fraction of the peak height.
+.le
+.ls [5]
+The automatic order identification and aperture assignment is based on peak
+height and may be incorrect.  The interactive aperture editor is entered
+with a plot of the apertures.  When there is a second simultaneous arc
+fiber it is essential that the object and arc
+fiber orders are properly paired with the arc fibers having even aperture
+numbers and the object fibers having odd aperture numbers.  It is also
+required that no orders be skipped in the region of interest.  Missing
+orders are added with the 'm' key.  Once all orders have been marked the
+aperture numbers are resequenced with 'o'.  If local background subtraction
+is selected the background regions should be checked with the 'b' key.
+Preceding this with the 'a' key allows any changes to the background
+regions to be applied to all orders.  To exit type 'q'.
+.le
+.ls [6]
+The order positions at a series of points along the dispersion are measured
+and a function is fit to these positions.  This may be done interactively to
+adjust the fitting parameters.  Not all orders need be examined and the "NO"
+response will quit the interactive fitting.  To exit the interactive
+fitting type 'q'.
+.le
+.ls [7]
+If flat fielding is to be done the flat field spectra are extracted.  A
+smooth function is fit to each flat field spectrum to remove the large
+scale spectral signature.  The final response spectra are normalized to a
+unit mean over all fibers.
+.le
+.ls [8]
+If scattered light subtraction is selected the scattered light parameters
+are set using the aperture reference image and the task \fBapscatter\fR.
+The purpose of this is to interactively define the aperture buffer distance
+for the scattered light and the cross and parallel dispersion fitting
+parameters.  The fitting parameters are taken from and recorded in the
+parameter sets \fBapscat1\fR and \fBapscat2\fR.  All other scattered light
+subtractions are done noninteractively with these parameters.  Note that
+the scattered light correction modifies the input images.
+.le
+.ls [9]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  One fiber is used to identify the arc lines and define the
+dispersion function using the task \fBecidentify\fR.  Identify a few arc
+lines in a few orders with 'm' and 'k' or 'o', use the 'l' line list
+identification command to automatically add additional lines and fit the
+dispersion function.  Check the quality of the dispersion function fit
+with 'f'.  When satisfied exit with 'q'.
+.le
+.ls [10]
+If there is a second fiber the dispersion function is automatically
+determined using the task \fBecreidentify\fR.
+.le
+.ls [11]
+The arc reference spectrum is dispersion corrected.
+If the spectra are resampled to a linear dispersion system
+(which will be the same for all spectra) the dispersion parameters
+determined from the dispersion solution are printed.
+.le
+.ls [12]
+The object spectra are now automatically background subtracted (an
+alternative to scattered light subtraction), extracted, flat fielded,
+and dispersion corrected.  Any new dispersion function reference arcs
+assigned to the object images are automatically extracted and
+dispersion functions determined.  A zero point wavelength correction
+is computed from the simultaneous arc fiber spectrum and applied to
+the object spectrum if orders from the second fiber have been identified
+with the \fIarcaps\fR parameter.
+.le
+.ls [13]
+The final spectra will have the same name as the original 2D images
+with a ".ec" extension added.
+.le
+
+\fBSpectra and Data Files\fR
+
+The basic input consists of single or dual fiber FOE object and calibration
+spectra stored as IRAF images.  The \fIarcaps\fR parameter is used to
+discriminate between the two cases.  The type of image format is defined by
+the environment parameter \fIimtype\fR.  Only images with that extension
+will be processed and created.  The raw CCD images must be processed to
+remove overscan, bias, and dark count effects.  This is generally done
+using the \fBccdred\fR package.  Flat fielding is generally not done at
+this stage but as part of \fBdofoe\fR.  The calibration spectra are flat
+field observations in all fibers, comparison arc lamp spectra in all
+fibers, and, for dual fiber model, arc spectra in one fiber while the
+second fiber observes the object.  If for some reason the flat field or
+calibration arc spectra have separate exposures for the two fibers the
+separate exposures may simply be added.
+
+The assignment of arc calibration exposures to object exposures is
+generally done by selecting the nearest in time and interpolating.
+However, the optional \fIarc assignment table\fR may be used to explicitly
+assign arc images to specific objects.  The format of this file is
+described in the task \fBrefspectra\fR.
+
+The final reduced spectra are recorded in two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ec" extension.  Each line in the reduced image is a one dimensional
+spectrum (an echelle order) with associated aperture and wavelength
+information.  When the \fIextras\fR parameter is set the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tasks such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.  The special task \fBscopy\fR may be used to extract
+specific apertures or to change format to individual one dimensional
+images.  The task \fBscombine\fR is used to combine or merge orders into
+a single spectrum.
+
+\fBPackage Parameters\fR
+
+The \fBechelle\fR package parameters set parameters affecting all the tasks
+in the package.  Some of the parameters are not applicable to the
+\fBdofoe\fR task.  The observatory parameter is only required for data
+without an OBSERVAT header parameter (currently included in NOAO data).
+The spectrum interpolation type might be changed to "sinc" but with the
+cautions given in \fBonedspec.package\fR.  The dispersion axis parameter is
+only needed if a DISPAXIS image header parameter is not defined.  The other
+parameters define the standard I/O functions.  The verbose parameter
+selects whether to print everything which goes into the log file on the
+terminal.  It is useful for monitoring what the \fBdofoe\fR task does.  The
+log and plot files are useful for keeping a record of the processing.  A
+log file is highly recommended.  A plot file provides a record of
+apertures, traces, and extracted spectra but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+
+\fBProcessing Parameters\fR
+
+The input images are specified by image lists.  The lists may be
+a list of explicit, comma separate image names, @ files, or image
+templates using pattern matching against file names in the directory.
+The aperture reference spectrum is used to find the orders and trace
+them.  Thus, this requires an image with good signal in both fibers
+which usually means a flat field spectrum.  It is recommended that
+flat field correction be done using one dimensional extracted spectra
+rather than as two dimensional images.  This is done if a flat field
+spectrum is specified.  The arc assignment table is used to specifically
+assign arc spectra to particular object spectra and the format
+of the file is described in \fBrefspectra\fR.
+
+The detector read out noise and gain are used for cleaning and variance
+(optimal) extraction.  The dispersion axis defines the wavelength direction
+of spectra in the image if not defined in the image header by the keyword
+DISPAXIS.  The width parameter (in pixels) is used for the profile
+centering algorithm (\fBcenter1d\fR).
+
+The number of orders selects the number of orders for a single
+fiber and "pairs" of object and arc
+fiber profiles for dual fibers.   The number specified will be
+automatically found based on the strongest peaks.
+In the  dual fiber case it is important that both elements of a pair be found,
+so no orders be skipped, and the aperture numbers must be sequential with
+arc profiles having even aperture numbers and object profiles having
+odd numbers in the region of interest, the automatic identification is  
+just a starting point for the interactive review.  The even/odd
+relationship between object and arc profiles is set by the \fIarcaps\fR
+parameter and so may be reversed if desired.
+
+The next set of parameters select the processing steps and options.  The
+flat fitting option allows fitting and removing the overall shape of the
+flat field spectra while preserving the pixel-to-pixel response
+corrections.  This is useful for maintaining the approximate object count
+levels, including the blaze function, and not introducing the reciprocal of
+the flat field spectrum into the object spectra.  If not selected the flat
+field will remove the blaze function from the observations and introduce
+some wavelength dependence from the flat field lamp spectrum.
+
+The \fIbackground\fR option selects the type of correction for background or
+scattered light.  If the type is "scattered" a global scattered light is
+fit to the data between the apertures  and subtracted from the images.
+\fINote that the input images are modified by this operation\fR.  This
+option is slow.  Alternatively, a local background may be subtracted using
+background regions defined for each aperture.  The data in the regions may
+be averaged, medianed, or the minimum value used.  Another choice is to fit
+the data in the background regions by a function and interpolate to the
+object aperture.
+
+The \fIclean\fR option invokes a profile fitting and deviant point rejection
+algorithm as well as a variance weighting of points in the aperture.  These
+options require knowing the effective (i.e. accounting for any image
+combining) read out noise and gain.  For a discussion of cleaning and
+variance weighted extraction see \fBapvariance\fR and \fBapprofiles\fR.
+
+The dispersion correction option selects whether to extract arc spectra,
+determine a dispersion function, assign them to the object spectra, and,
+possibly, resample the spectra to a linear (or log-linear) wavelength
+scale.
+
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\fIupdate\fR flag is set.  The changes which will cause an update are a new
+reference image, new flat field, adding the scattered light option, and a
+new arc reference image.  If all input spectra are to be processed
+regardless of previous processing the \fIredo\fR flag may be used.  Note
+that reprocessing clobbers the previously processed output spectra.
+
+The \fIbatch\fR processing option allows object spectra to be processed as
+a background or batch job.  The \fIlistonly\fR option prints a summary of
+the processing steps which will be performed on the input spectra without
+actually doing anything.  This is useful for verifying which spectra will
+be affected if the input list contains previously processed spectra.  The
+listing does not include any arc spectra which may be extracted to
+dispersion calibrate an object spectrum.
+
+The last parameter (excluding the task mode parameter) points to another
+parameter set for the algorithm parameters.  The way \fBdofoe\fR works
+this may not have any value and the parameter set \fBparams\fR is always
+used.  The algorithm parameters are discussed further in the next section.
+
+\fBAlgorithms and Algorithm Parameters\fR
+
+This section summarizes the various algorithms used by the \fBdofoe\fR
+task and the parameters which control and modify the algorithms.  The
+algorithm parameters available to the user are collected in the parameter
+set \fBparams\fR.  These parameters are taken from the various general
+purpose tasks used by the \fBdofoe\fR processing task.  Additional
+information about these parameters and algorithms may be found in the help
+for the actual task executed.  These tasks are identified in the parameter
+section listing in parenthesis.  The aim of this parameter set organization
+is to collect all the algorithm parameters in one place separate from the
+processing parameters and include only those which are relevant for
+FOE data.  The parameter values can be changed from the
+defaults by using the parameter editor,
+.nf
+
+	cl> epar params
+
+.fi
+or simple typing \fIparams\fR.  The parameter editor can also be
+entered when editing the \fBdofoe\fR parameters by typing \fI:e
+params\fR or simply \fI:e\fR if positioned at the \fIparams\fR
+parameter.
+
+\fBAperture Definitions\fR
+
+The first operation is to define the extraction apertures, which include the
+aperture width, background regions, and position dependence with
+wavelength, for the object and arc orders of interest.  This is done
+on a reference spectrum which is usually a flat field taken through
+all fibers.  Other spectra will inherit the reference apertures and
+apply a correction for any shift of the orders across the dispersion.
+The reference apertures are defined only once unless the \fIredo\fR
+option is set.
+
+The selected number of orders are found automatically by selecting the
+highest peaks in a cut across the dispersion.  Note that the specified
+number of orders is multiplied by two in defining the apertures when
+there is a second fiber.  Apertures
+are assigned with a limits set by the \fIlower\fR and
+\fIupper\fR parameter and numbered sequentially.  A query is then
+given allowing the aperture limits to be "resized" based on the profile
+itself (see \fBapresize\fR).
+
+A cut across the orders is then shown with the apertures marked and
+an interactive aperture editing mode is entered (see \fBapedit\fR).
+For \fBdofoe\fR the aperture identifications and numbering is particularly
+critical.  When there is a single fiber the aperture numbers must
+be sequential with the order numbers.  If an order is skipped then the
+aperture number must also be skipped.
+
+For dual fibers all "pairs" of object and arc orders in the region of
+interest must be defined without skipping any orders.  The orders must
+also be numbered sequentially (though the direction does not matter)
+so that the arc apertures are either all even or all odd as defined
+by the \fIarcaps\fR parameter (the default is even numbers for the
+arc apertures).  The 'o' key will provide the necessary reordering.
+
+If local background subtraction is used the background regions should
+also be checked with the 'b' key.  Typically one adjusts all
+the background regions at the same time by selecting all apertures with
+the 'a' key first.  To exit the background and aperture editing steps type
+'q'.
+
+Next the positions of the orders at various points along the dispersion are
+measured and "trace functions" are fit.  The user is asked whether to fit
+each trace function interactively.  This is selected to adjust the fitting
+parameters such as function type and order.  When interactively fitting a
+query is given for each aperture.  After the first aperture one may skip
+reviewing the other traces by responding with "NO".  Queries made by
+\fBdofoe\fR generally may be answered with either lower case "yes" or "no"
+or with upper case "YES" or "NO".  The upper case responses apply to all
+further queries and so are used to eliminate further queries of that kind.
+
+The above steps are all performed using tasks from the \fBapextract\fR
+package and parameters from the \fBparams\fR parameters.  As a quick
+summary, the dispersion direction of the spectra are determined from the
+package \fBdispaxis\fR parameter if not defined in the image header.  The
+default line or column for finding the orders and the number of image lines
+or columns to sum are set by the \fIline\fR and \fInsum\fR parameters.  A
+line of INDEF (the default) selects the middle of the image.  The automatic
+finding algorithm is described for the task \fBapfind\fR and basically
+finds the strongest peaks.  The resizing is described in the task
+\fBapresize\fR and the parameters used are also described there and
+identified in the PARAMETERS section.  The tracing is done as described in
+\fBaptrace\fR and consists of stepping along the image using the specified
+\fIt_step\fR parameter.  The function fitting uses the \fBicfit\fR commands
+with the other parameters from the tracing section.
+
+\fBBackground or Scattered Light Subtraction\fR
+
+In addition to not subtracting any background scattered light there are two
+approaches to subtracting this light.  The first is to determine a smooth
+global scattered light component.  The second is to subtract a locally
+determined background at each point along the dispersion and for each
+aperture.  Note that background subtraction is only done for object images
+and not for arc images.
+
+The global scattered light fitting and subtraction is done with the task
+\fBapscatter\fR.  The function fitting parameters are set interactively
+using the aperture reference spectrum.  All other subtractions are done
+noninteractively with the same set of parameters.  The scattered light is
+subtracted from the input images, thus modifying them, and one might wish
+to first make backups of the original images.
+
+The scattered light is measured between the apertures using a specified
+buffer distance from the aperture edges.  The scattered light pixels are
+fit by a series of one dimensional functions across the dispersion.  The
+independent fits are then smoothed along the dispersion by again fitting
+low order functions.  These fits then define the smooth scattered light
+surface to be subtracted from the image.  The fitting parameters are
+defined and recorded in the two parameter sets \fIapscat1\fR and
+\fIapscat2\fR.  The scattered light algorithm is described more fully in
+\fBapscatter\fR.  This algorithm is relatively slow.
+
+Local background subtraction is done during extraction based on background
+regions and parameters defined by the default background parameters or
+changed during interactive review of the apertures.  The background
+subtraction options are to subtract the average, median, or minimum of the
+pixels in the background regions, or to fit a function and subtract the
+function from under the extracted object pixels.  The background regions
+are specified in pixels from the aperture center and follow changes in
+center of the spectrum along the dispersion.  The syntax is colon separated
+ranges with multiple ranges separated by a comma or space.  The background
+fitting uses the \fBicfit\fR routines which include medians, iterative
+rejection of deviant points, and a choice of function types and orders.
+Note that it is important to use a method which rejects cosmic rays such as
+using either medians over all the background regions (\fIbackground\fR =
+"median") or median samples during fitting (\fIb_naverage\fR < -1).
+The background smoothing parameter \fIb_smooth\fR is may be used
+to provide some additional local smoothing of the background light.
+The background subtraction algorithm and options are described in greater
+detail in \fBapsum\fR and \fBapbackground\fR.
+
+\fBExtraction\fR
+
+The actual extraction of the spectra is done by summing across the fixed
+width apertures at each point along the dispersion.  The default is to
+simply sum the pixels using partial pixels at the ends.  There is an
+option to weight the sum based on a Poisson noise model using the
+\fIreadnoise\fR and \fIgain\fR detector parameters.  Note that if the
+\fIclean\fR option is selected the variance weighted extraction is used
+regardless of the \fIweights\fR parameter.  The sigma threshold for
+cleaning are also set in the \fBparams\fR parameters.
+
+The cleaning and variance weighting options require knowing the effective
+(i.e. accounting for any image combining) read out noise and gain.  These
+numbers need to be adjusted if the image has been processed such that the
+intensity scale has a different origin (such as a scattered light
+subtraction) or scaling (such as caused by unnormalized flat fielding).
+These options also require using background subtraction if the profile does
+not go to zero.  For optimal extraction and cleaning to work it is
+recommended that any scattered light be accounted for by local background
+subtraction rather than with the scattered light subtraction and the
+\fIfitflat\fR option be used.  The \fIb_smooth\fR parameter is also
+appropriate in this application and improves the optimal extraction results
+by reducing noise in the background signal.  For further discussion of
+cleaning and variance weighted extraction see \fBapvariance\fR and
+\fBapprofiles\fR as well as  \fBapsum\fR.
+
+\fBFlat Field Correction\fR
+
+Flat field corrections may be made during the basic CCD processing; i.e.
+direct division by the two dimensional flat field observation.  In that
+case do not specify a flat field spectrum; use the null string "".  The
+\fBdofoe\fR task provides an alternative flat field response correction
+based on division of the extracted object spectra by the extracted flat field
+spectra.  A discussion of the theory and merits of flat fielding directly
+verses using the extracted spectra will not be made here.  The
+\fBdofoe\fR flat fielding algorithm is the \fIrecommended\fR method for
+flat fielding since it works well and is not subject to the many problems
+involved in two dimensional flat fielding.
+
+The first step is extraction of the flat field spectrum, if one is specified,
+using the reference apertures.  Only one flat field is allowed so if
+multiple flat fields are required the data must be reduced in groups.  When
+the \fIfitflat\fR option is selected (the default) the extracted flat field
+spectra are fit by smooth functions and the ratio of the flat field spectra
+to the smooth functions define the response spectra.  The default fitting
+function and order are given by the parameters \fIf_function\fR and
+\fIf_order\fR.  If the parameter \fIf_interactive\fR is "yes" then the
+fitting is done interactively using the \fBfit1d\fR task which uses the
+\fBicfit\fR interactive fitting commands.
+
+If the \fIfitflat\fR option is not selected the extracted and globally
+normalized flat field spectra are directly divided in the object spectra.
+This removes the blaze function, thus altering the data counts, and
+introduces the reciprocal of the flat field spectrum in the object
+spectra.
+
+The final step is to normalize the flat field spectra by the mean counts over
+all the fibers.  This normalization step is simply to preserve the average
+counts of the extracted object and arc spectra after division by the
+response spectra.
+
+\fBDispersion Correction\fR
+
+If dispersion correction is not selected, \fIdispcor\fR=no, then the object
+spectra are simply extracted.  If it is selected the arc spectra are used
+to dispersion calibrate the object spectra.  There are three steps involved;
+determining the dispersion functions relating pixel position to wavelength,
+assigning the appropriate dispersion function to a particular observation,
+and either storing the nonlinear
+dispersion function in the image headers or resampling the spectra to
+evenly spaced pixels in wavelength.  When there are two fibers there is
+also a step of applying a zero point correction to the object fiber based
+on the arc fiber.
+
+The first arc spectrum in the arc list is used to define the reference
+dispersion solution.  It is extracted using the reference aperture
+definitions.  Note extractions of arc spectra are not background or
+scattered light subtracted.  The interactive task \fBecidentify\fR is used
+to define the dispersion function in one fiber.  The idea is to mark some
+lines in a few orders whose wavelengths are known (with the line list used
+to supply additional lines after the first few identifications define the
+approximate wavelengths) and to fit a function giving the wavelength from
+the aperture number and pixel position.  The dispersion function for the
+second fiber, if one is present, is then determined automatically by
+reference to the first fiber using the task \fBecreidentify\fR.
+
+The arc dispersion function parameters are for \fBecidentify\fR and it's
+related partner \fBecreidentify\fR.  The parameters define a line list for
+use in automatically assigning wavelengths to arc lines, a centering width
+(which should match the line widths at the base of the lines), the
+dispersion function type and orders, parameters to exclude bad lines from
+function fits, and defining whether to refit the dispersion function as
+opposed to simply determining a zero point shift.  The defaults should
+generally be adequate and the dispersion function fitting parameters may be
+altered interactively.  One should consult the help for the two tasks for
+additional details of these parameters and the interactive operation of
+\fBecidentify\fR.
+
+Once the reference dispersion functions are defined other arc spectra are
+extracted as they are assign to the object spectra.  The assignment of
+arcs is done either explicitly with an arc assignment table (parameter
+\fIarctable\fR) or based on a header parameter such as a time.
+The assignments are made by the task \fBrefspectra\fR.  When two arcs are
+assigned to an object spectrum an interpolation is done between the two
+dispersion functions.  This makes an approximate correction for steady
+drifts in the dispersion.
+
+When a second arc fiber monitors any zero point shifts in the dispersion
+functions it is probably only necessary to have one or two arc spectra, one
+at the beginning and/or one at the end of the night.
+
+The tasks \fBsetjd\fR and \fBsetairmass\fR are automatically run on all
+spectra.  This computes and adds the header parameters for the Julian date
+(JD), the local Julian day number (LJD), the universal time (UTMIDDLE), and
+the air mass at the middle of the exposure.  The default arc assignment is
+to use the Julian date grouped by the local Julian day number.  The
+grouping allows multiple nights of data to be correctly assigned at the
+same time.
+
+Defining the dispersion function for a new arc extraction is done with
+the task \fBecreidentify\fR.  This is done noninteractively with log
+information recorded about the line reidentifications and the fit.
+
+When there are two fibers there are two full dispersion function from the
+single or pair of arc spectra, one for the object fiber and one for the arc
+fiber.  When an object spectrum is extracted so is the simultaneous arc
+spectrum.  A zero point shift of the arc spectrum relative to the
+dispersion solution of the dual arc observation is computed using
+\fBecreidentify\fR (\fIrefit\fR=no).  This zero point shift is assumed to
+be the same for the object fiber and it is added to the dispersion function
+of the dual arc observation for the object fiber.  Note that this does not
+assume that the object and arc fiber dispersion functions are the same or
+have the same wavelength origin, but only that the same shift in wavelength
+zero point applies to both fibers.  Once the dispersion function correction
+is determined from the extracted arc fiber spectrum it is deleted leaving
+only the object spectrum.
+
+The last step of dispersion correction is setting the dispersion
+of the object spectrum.  There are two choices here.
+If the \fIlinearize\fR parameter is not set the nonlinear dispersion
+function is stored in the image header.  Other IRAF tasks interpret
+this information when dispersion coordinates are needed for plotting
+or analysis.  This has the advantage of not requiring the spectra
+to be interpolated and the disadvantage that the dispersion
+information is only understood by IRAF tasks and cannot be readily
+exported to other analysis software.
+
+If the \fIlinearize\fR parameter is set then the spectra are resampled to a
+linear dispersion relation either in wavelength or the log of the
+wavelength.  For echelle spectra each order is linearized independently so
+that the wavelength interval per pixel is different in different orders.
+This preserves most of the resolution and avoids over or under sampling of
+the highest or lowest dispersion orders.  The wavelength limits are
+taken from the limits determined from the arc reference spectrum and
+the number of pixels is the same as the original images.  The dispersion
+per pixel is then derived from these constraints.
+
+The linearization algorithm  parameters allow selecting the interpolation
+function type, whether to conserve flux per pixel by integrating across the
+extent of the final pixel, and whether to linearize to equal linear or
+logarithmic intervals.  The latter may be appropriate for radial velocity
+studies.  The default is to use a fifth order polynomial for interpolation,
+to conserve flux, and to not use logarithmic wavelength bins.  These
+parameters are described fully in the help for the task \fBdispcor\fR which
+performs the correction.
+.ih
+EXAMPLES
+1.  The following example uses artificial data and may be executed
+at the terminal (with IRAF V2.10).  This is also the sequence performed
+by the test procedure "demos dofoe".  Because the images are small the
+dispersion solution is somewhat simplistic.
+
+.nf
+ec> demos mkdofoe
+Creating image demoobj ...
+Creating image demoflat ...
+Creating image demoarc ...
+ec> echelle.verbose = yes
+ec> dofoe demoobj apref=demoflat flat=demoflat arcs=demoarc \
+>>> norders=3 width=5.
+Set reference apertures for demoflat
+Searching aperture database ...
+Finding apertures ...
+Mar  4  9:39: FIND - 6 apertures found for demoflat
+Resize apertures for demoflat?  (yes):
+Resizing apertures ...
+Mar  4  9:39: RESIZE - 6 apertures resized for demoflat
+<Review aperture assignments.  Exit with 'q'>
+Fit traced positions for demoflat interactively?  (yes):
+Tracing apertures ...
+Fit curve to aperture 1 of demoflat interactively  (yes):
+<Review trace and fit. Exit with 'q'>
+Fit curve to aperture 2 of demoflat interactively  (yes): N
+Mar  4  9:39: TRACE - 6 apertures traced in demoflat.
+Mar  4  9:39: DATABASE - 6 apertures for demoflat written to database
+Create response function demoflatnorm.ec
+Extract flat field demoflat
+Searching aperture database ...
+Mar  4  9:39: DATABASE  - 6 apertures read for demoflat from database
+Extracting apertures ...
+Mar  4  9:39: EXTRACT - Aperture 1 from demoflat --> demoflat.ec
+Mar  4  9:39: EXTRACT - Aperture 2 from demoflat --> demoflat.ec
+Mar  4  9:39: EXTRACT - Aperture 3 from demoflat --> demoflat.ec
+Mar  4  9:39: EXTRACT - Aperture 4 from demoflat --> demoflat.ec
+Mar  4  9:39: EXTRACT - Aperture 5 from demoflat --> demoflat.ec
+Mar  4  9:40: EXTRACT - Aperture 6 from demoflat --> demoflat.ec
+Fit and ratio flat field demoflat
+Create the normalized response demoflatnorm.ec
+demoflatnorm.ec -> demoflatnorm.ec  using bzero: 0.  and bscale: 1.
+    mean: 1.  median: 0.9990048  mode: 0.9876572
+    upper: INDEF  lower: INDEF
+Extract arc reference image demoarc
+Mar  4  9:40: DATABASE  - 6 apertures read for demoflat from database
+Mar  4  9:40: DATABASE - 6 apertures for demoarc written to database
+Mar  4  9:40: EXTRACT - Aperture 1 from demoarc --> demoarc.ec
+Mar  4  9:40: EXTRACT - Aperture 2 from demoarc --> demoarc.ec
+Mar  4  9:40: EXTRACT - Aperture 3 from demoarc --> demoarc.ec
+Mar  4  9:40: EXTRACT - Aperture 4 from demoarc --> demoarc.ec
+Mar  4  9:40: EXTRACT - Aperture 5 from demoarc --> demoarc.ec
+Mar  4  9:40: EXTRACT - Aperture 6 from demoarc --> demoarc.ec
+Determine dispersion solution for demoarc
+<Mark lines with 'm' and change orders with 'k'
+<'m' line at pixel 78 and assign 4965.
+<'k' to order 2
+<'m' line at pixel 78 and assign 5009
+<'m' line at pixel 78 and assign 5020
+<'k' to order 3
+<'m' line at pixel 78 and assign 5049.8
+<'m' line at pixel 78 and assign 5050.8
+<'m' line at pixel 78 and assign 5055.3
+<'m' line at pixel 78 and assign 5062
+<'m' line at pixel 78 and assign 5064.9
+<'f' to fit
+<'q' to quit fit and 'q' to quit ECIDENTIFY
+
+ECREIDENTIFY: NOAO/IRAF V2.10BETA valdes@puppis Wed 09:54:16 04-Mar-92
+  Reference image = demoarc.ec, Refit = yes
+   Image    Found     Fit Pix Shift  User Shift  Z Shift      RMS
+  d...ec    8/8     8/8        1.48        7.06  2.11E-5  0.00879
+d...ec: ap = 1, w1 = 4959.1, w2 = 4978.5, dw = 0.076, nw = 256
+d...ec: ap = 2, w1 = 5003.4, w2 = 5022.1, dw = 0.073, nw = 256
+d...ec: ap = 3, w1 = 5049.0, w2 = 5067.0, dw = 0.070, nw = 256
+Extract object spectrum demoobj
+Searching aperture database ...
+Mar  4  9:54: DATABASE  - 6 apertures read for demoflat from database
+Recentering apertures ...
+Mar  4  9:54: RECENTER  - 6 apertures shifted by -0.03 for demoobj.
+Mar  4  9:54: DATABASE - 6 apertures for demoobj written to database
+Extracting apertures ...
+Mar  4  9:54: EXTRACT - Aperture 1 from demoobj --> demoobj.ec
+Mar  4  9:54: EXTRACT - Aperture 2 from demoobj --> demoobj.ec
+Mar  4  9:54: EXTRACT - Aperture 3 from demoobj --> demoobj.ec
+Mar  4  9:54: EXTRACT - Aperture 4 from demoobj --> demoobj.ec
+Mar  4  9:54: EXTRACT - Aperture 5 from demoobj --> demoobj.ec
+Mar  4  9:54: EXTRACT - Aperture 6 from demoobj --> demoobj.ec
+Assign arc spectra for demoobj
+[demoobj] refspec1='demoarc'
+Reidentify arc fibers in demoobj with respect to demoarc
+
+ECREIDENTIFY: NOAO/IRAF V2.10BETA valdes@puppis Wed 09:54:28 04-Mar-92
+  Reference image = demoarcarc.ec, Refit = no
+   Image    Found     Fit Pix Shift  User Shift  Z Shift      RMS
+  d...ec    8/8     8/8       0.119       0.566  1.69E-6  0.00834
+Dispersion correct demoobj
+d...ec.imh: ap = 1, w1 = 4959.1, w2 = 4978.5, dw = 0.076, nw = 256
+d...ec.imh: ap = 2, w1 = 5003.4, w2 = 5022.1, dw = 0.073, nw = 256
+d...ec.imh: ap = 3, w1 = 5049.0, w2 = 5067.0, dw = 0.070, nw = 256
+.fi
+.ih
+REVISIONS
+.ls DOFOE V2.10.3
+The image format type to be
+processed is selected with the \fIimtype\fR environment parameter.  The
+dispersion axis parameter is now a package parameter.  Images will only
+be processed if the have the CCDPROC keyword.  A \fIdatamax\fR parameter
+has been added to help improve cosmic ray rejection.  A scattered
+light subtraction processing option has been added.
+.le
+.ih
+SEE ALSO
+apedit, apfind, approfiles, aprecenter, apresize, apsum, aptrace, apvariance,
+ccdred, center1d, dispcor, fit1d, icfit, ecidentify, observatory,
+onedspec.package, refspectra, ecreidentify, setairmass, setjd
+.endhelp
diff --git a/noao/imred/echelle/doc/dofoe.ms b/noao/imred/echelle/doc/dofoe.ms
new file mode 100644
index 00000000..1f283f46
--- /dev/null
+++ b/noao/imred/echelle/doc/dofoe.ms
@@ -0,0 +1,1371 @@
+.nr PS 9
+.nr VS 11
+.de V1
+.ft CW
+.nf
+..
+.de V2
+.fi
+.ft R
+..
+.de LS
+.br
+.in +2
+..
+.de LE
+.br
+.sp .5v
+.in -2
+..
+.ND February 1993
+.TL
+Guide to the Fiber Optic Echelle Reduction Task DOFOE
+.AU
+Francisco Valdes
+.AI
+IRAF Group - Central Computer Services
+.K2
+.DY
+
+.AB
+The \fBdofoe\fR reduction task is specialized for scattered light
+subtraction, extraction, flat fielding, and wavelength calibration of Fiber
+Optic Echelle (FOE) spectra.  It is a command language script which
+collects and combines the functions and parameters of many general purpose
+tasks to provide a single complete data reduction path.  The task provides
+a degree of guidance, automation, and record keeping necessary when dealing
+with the complexities of reducing this type of data.
+.AE
+.NH
+Introductions
+.LP
+The \fBdofoe\fR reduction task is specialized for scattered light
+subtraction, extraction, flat fielding, and wavelength calibration of Fiber
+Optic Echelle (FOE) spectra.  It is a command language script which
+collects and combines the functions and parameters of many general purpose
+tasks to provide a single complete data reduction path.  The task provides
+a degree of guidance, automation, and record keeping necessary when dealing
+with the complexities of reducing this type of data.
+.LP
+The general organization of the task is to do the interactive setup steps
+first using representative calibration data and then perform the majority
+of the reductions automatically, possibly as a background process, with
+reference to the setup data.  In addition, the task determines which setup
+and processing operations have been completed in previous executions of the
+task and, contingent on the \f(CWredo\fR and \f(CWupdate\fR options, skip or
+repeat some or all the steps.
+.LP
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage.  Since
+\fBdofoe\fR combines many separate, general purpose tasks the description
+given here refers to these tasks and leaves some of the details to their
+help documentation.
+.NH
+Usage Outline
+.LP
+.IP [1] 6
+The images must first be processed with \fBccdproc\fR for overscan,
+bias, and dark corrections.
+.IP [2]
+Set the \fBdofoe\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed, the flat field image as the aperture reference and
+the flat field, and one or more arc images.  If there are many
+object or arc spectra per setup you might want to prepare "@ files".
+Verify and set the format parameters, particularly the number of orders to be
+extracted and processed.  The processing parameters are set
+for simple extraction and dispersion correction but dispersion correction
+can be turned off for quicklook or background subtraction and cleaning
+may be added.
+.IP [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the execution and no further queries of that
+type will be made.
+.IP [4]
+The apertures are defined using the specified aperture reference image
+which is usually a flat field in which both the object and arc fibers are
+illuminated.  The specified number of orders are found automatically and
+sequential apertures assigned.  The resize option sets the aperture size to
+the widths of the profiles at a fixed fraction of the peak height.
+.IP [5]
+The automatic order identification and aperture assignment is based on peak
+height and may be incorrect.  The interactive aperture editor is entered
+with a plot of the apertures.  It is essential that the object and arc
+fiber orders are properly paired with the arc fibers having even aperture
+numbers and the object fibers having odd aperture numbers.  It is also
+required that no orders be skipped in the region of interest.  Missing
+orders are added with the 'm' key.  Once all orders have been marked the
+aperture numbers are resequenced with 'o'.  If local background subtraction
+is selected the background regions should be checked with the 'b' key.
+Preceding this with the 'a' key allows any changes to the background
+regions to be applied to all orders.  To exit type 'q'.
+.IP [6]
+The order positions at a series of points along the dispersion are measured
+and a function is fit to these positions.  This may be done interactively to
+adjust the fitting parameters.  Not all orders need be examined and the "NO"
+response will quit the interactive fitting.  To exit the interactive
+fitting type 'q'.
+.IP [7]
+If flat fielding is to be done the flat field spectra are extracted.  A
+smooth function is fit to each flat field spectrum to remove the large
+scale spectral signature.  The final response spectra are normalized to a
+unit mean over all fibers.
+.IP [8]
+If scattered light subtraction is selected the scattered light parameters
+are set using the aperture reference image and the task \fBapscatter\fR.
+The purpose of this is to interactively define the aperture buffer distance
+for the scattered light and the cross and parallel dispersion fitting
+parameters.  The fitting parameters are taken from and recorded in the
+parameter sets \fBapscat1\fR and \fBapscat2\fR.  All other scattered light
+subtractions are done noninteractively with these parameters.  Note that
+the scattered light correction modifies the input images.
+.IP [9]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  One fiber is used to identify the arc lines and define the
+dispersion function using the task \fBecidentify\fR.  Identify a few arc
+lines in a few orders with 'm' and 'k' or 'o', use the 'l' line list
+identification command to automatically add additional lines and fit the
+dispersion function.  Check the quality of the dispersion function fit
+with 'f'.  When satisfied exit with 'q'.
+.IP [10]
+The other fiber dispersion function is automatically determined using
+the task \fBecreidentify\fR.
+.IP [11]
+The arc reference spectrum is dispersion corrected.
+If the spectra are resampled to a linear dispersion system
+(which will be the same for all spectra) the dispersion parameters
+determined from the dispersion solution are printed.
+.IP [12]
+The object spectra are now automatically background subtracted (an
+alternative to scattered light subtraction), extracted, flat fielded,
+and dispersion corrected.  Any new dispersion function reference arcs
+assigned to the object images are automatically extracted and
+dispersion functions determined.  A zero point wavelength correction
+is computed from the simultaneous arc fiber spectrum and applied to
+the object spectrum.
+.IP [13]
+The final spectra will have the same name as the original 2D images
+with a ".ec" extension added.
+.NH
+Spectra and Data Files
+.LP
+The basic input consists of dual fiber FOE object and calibration spectra
+stored as IRAF images.
+The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+The raw CCD images must be processed to remove
+overscan, bias, and dark count effects.  This is generally done using the
+\fBccdred\fR package.  Flat fielding is generally not done at this stage
+but as part of \fBdofoe\fR.  The calibration spectra are
+flat field observations in both fibers, comparison arc lamp spectra
+in both fibers, and arc spectra in one fiber while the second
+fiber observes the object.  If for some reason the flat field or
+calibration arc spectra have separate exposures for the two fibers
+the separate exposures may simply be added.
+.LP
+The assignment of arc calibration exposures to object exposures is
+generally done by selecting the nearest in time and interpolating.
+However, the optional \fIarc assignment table\fR may be used to explicitly
+assign arc images to specific objects.  The format of this file is
+described in the task \fBrefspectra\fR.
+.LP
+The final reduced spectra are recorded in two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ec" extension.  Each line in the reduced image is a one dimensional
+spectrum (an echelle order) with associated aperture and wavelength
+information.  When the \f(CWextras\fR parameter is set the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tasks such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.  The special task \fBscopy\fR may be used to extract
+specific apertures or to change format to individual one dimensional
+images.  The task \fBscombine\fR is used to combine or merge orders into
+a single spectrum.
+.NH
+Package Parameters
+.LP
+The \fBechelle\fR package parameters, shown in Figure 1, set parameters
+affecting all the tasks in the package.  Some of the parameters are not
+applicable to the \fBdofoe\fR task.
+.KS
+.V1
+
+.ce
+Figure 1: Package Parameter Set for the ECHELLE Package
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = imred
+   TASK = echelle
+
+(extinct= onedstds$kpnoextinct.dat) Extinction file
+(caldir = onedstds$spechayescal/) Standard star calibration directory
+(observa=  observatory) Observatory of data
+(interp =        poly5) Interpolation type
+(dispaxi=            2) Image axis for 2D images
+(nsum   =            1) Number of lines/columns to sum for 2D images
+
+(databas=     database) Database
+(verbose=          no) Verbose output?
+(logfile=      logfile) Text log file
+(plotfil=             ) Plot file
+
+(records=                     ) Record number extensions
+(version= ECHELLE V3: July 1991)
+
+.KE
+.V2
+The observatory parameter is only required for data
+without an OBSERVAT header parameter (currently included in NOAO data).
+The spectrum interpolation type might be changed to "sinc" but with the
+cautions given in \fBonedspec.package\fR.  The dispersion axis parameter is
+only needed if a DISPAXIS image header parameter is not defined.  The other
+parameters define the standard I/O functions.  The verbose parameter
+selects whether to print everything which goes into the log file on the
+terminal.  It is useful for monitoring what the \fBdofoe\fR task does.  The
+log and plot files are useful for keeping a record of the processing.  A
+log file is highly recommended.  A plot file provides a record of
+apertures, traces, and extracted spectra but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+.NH
+Processing Parameters
+.LP
+The \fBdofoe\fR parameters are shown in Figure 2.
+.KS
+.V1
+
+.ce
+Figure 2: Parameters Set for DOFOE
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = echelle
+   TASK = dofoe
+
+objects =               List of object spectra
+(apref  =             ) Aperture reference spectrum
+(flat   =             ) Flat field spectrum
+(arcs   =             ) List of arc spectra
+(arctabl=             ) Arc assignment table (optional)
+
+.KE
+.V1
+(readnoi=           0.) Read out noise sigma (photons)
+(gain   =           1.) Photon gain (photons/data number)
+(datamax=        INDEF) Max data value / cosmic ray threshold
+(norders=           12) Number of orders
+(width  =           4.) Width of profiles (pixels)
+(arcaps =          2x2) Arc apertures
+
+(fitflat=          yes) Fit and ratio flat field spectrum?
+(backgro=         none) Background to subtract
+(clean  =           no) Detect and replace bad pixels?
+(dispcor=          yes) Dispersion correct spectra?
+(redo   =           no) Redo operations if previously done?
+(update =           no) Update spectra if cal data changes?
+(batch  =           no) Extract objects in batch?
+(listonl=           no) List steps but don't process?
+
+(params =             ) Algorithm parameters
+
+.V2
+The input images are specified by image lists.  The lists may be
+a list of explicit, comma separate image names, @ files, or image
+templates using pattern matching against file names in the directory.
+The aperture reference spectrum is used to find the orders and trace
+them.  Thus, this requires an image with good signal in both fibers
+which usually means a flat field spectrum.  It is recommended that
+flat field correction be done using one dimensional extracted spectra
+rather than as two dimensional images.  This is done if a flat field
+spectrum is specified.  The arc assignment table is used to specifically
+assign arc spectra to particular object spectra and the format
+of the file is described in \fBrefspectra\fR.
+.LP
+The detector read out noise and gain are used for cleaning and variance
+(optimal) extraction.  The dispersion axis defines the wavelength direction
+of spectra in the image if not defined in the image header by the keyword
+DISPAXIS.  The width parameter (in pixels) is used for the profile
+centering algorithm (\fBcenter1d\fR).
+.LP
+The number of orders selects the number of "pairs" of object and arc
+fiber profiles to be automatically found based on the strongest peaks.
+Because it is important that both elements of a pair be found,
+no orders be skipped, and the aperture numbers be sequential with
+arc profiles having even aperture numbers and object profiles having
+odd numbers in the region of interest, the automatic identification is  
+just a starting point for the interactive review.  The even/odd
+relationship between object and arc profiles is set by the \f(CWarcaps\fR
+parameter and so may be reversed if desired.
+.LP
+The next set of parameters select the processing steps and options.  The
+flat fitting option allows fitting and removing the overall shape of the
+flat field spectra while preserving the pixel-to-pixel response
+corrections.  This is useful for maintaining the approximate object count
+levels, including the blaze function, and not introducing the reciprocal of
+the flat field spectrum into the object spectra.  If not selected the flat
+field will remove the blaze function from the observations and introduce
+some wavelength dependence from the flat field lamp spectrum.
+.LP
+The \f(CWbackground\fR option selects the type of correction for background or
+scattered light.  If the type is "scattered" a global scattered light is
+fit to the data between the apertures  and subtracted from the images.
+\fINote that the input images are modified by this operation\fR.  This
+option is slow.  Alternatively, a local background may be subtracted using
+background regions defined for each aperture.  The data in the regions may
+be averaged, medianed, or the minimum value used.  Another choice is to fit
+the data in the background regions by a function and interpolate to the
+object aperture.
+.LP
+The \f(CWclean\fR option invokes a profile fitting and deviant point rejection
+algorithm as well as a variance weighting of points in the aperture.  These
+options require knowing the effective (i.e. accounting for any image
+combining) read out noise and gain.  For a discussion of cleaning and
+variance weighted extraction see \fBapvariance\fR and \fBapprofiles\fR.
+.LP
+The dispersion correction option selects whether to extract arc spectra,
+determine a dispersion function, assign them to the object spectra, and,
+possibly, resample the spectra to a linear (or log-linear) wavelength
+scale.
+.LP
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\f(CWupdate\fR flag is set.  The changes which will cause an update are a new
+reference image, new flat field, adding the scattered light option, and a
+new arc reference image.  If all input spectra are to be processed
+regardless of previous processing the \f(CWredo\fR flag may be used.  Note
+that reprocessing clobbers the previously processed output spectra.
+.LP
+The \f(CWbatch\fR processing option allows object spectra to be processed as
+a background or batch job.  The \f(CWlistonly\fR option prints a summary of
+the processing steps which will be performed on the input spectra without
+actually doing anything.  This is useful for verifying which spectra will
+be affected if the input list contains previously processed spectra.  The
+listing does not include any arc spectra which may be extracted to
+dispersion calibrate an object spectrum.
+.LP
+The last parameter (excluding the task mode parameter) points to another
+parameter set for the algorithm parameters.  The way \fBdofoe\fR works
+this may not have any value and the parameter set \fBparams\fR is always
+used.  The algorithm parameters are discussed further in the next section.
+.NH
+Algorithms and Algorithm Parameters
+.LP
+This section summarizes the various algorithms used by the \fBdofoe\fR
+task and the parameters which control and modify the algorithms.  The
+algorithm parameters available to the user are collected in the parameter
+set \fBparams\fR.  These parameters are taken from the various general
+purpose tasks used by the \fBdofoe\fR processing task.  Additional
+information about these parameters and algorithms may be found in the help
+for the actual task executed.  These tasks are identified in the parameter
+section listing in parenthesis.  The aim of this parameter set organization
+is to collect all the algorithm parameters in one place separate from the
+processing parameters and include only those which are relevant for
+FOE data.  The parameter values can be changed from the
+defaults by using the parameter editor,
+.V1
+
+	cl> epar params
+
+.V2
+or simple typing \f(CWparams\fR.  The parameter editor can also be
+entered when editing the \fBdofoe\fR parameters by typing \f(CW:e
+params\fR or simply \f(CW:e\fR if positioned at the \f(CWparams\fR
+parameter.  Figure 3 shows the parameter set.
+.KS
+.V1
+
+.ce
+Figure 3: Algorithm Parameter Set
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = echelle
+   TASK = params
+
+(line   =        INDEF) Default dispersion line
+(nsum   =           10) Number of dispersion lines to sum
+(extras =           no) Extract sky, sigma, etc.?
+
+                        -- DEFAULT APERTURE LIMITS --
+(lower  =          -3.) Lower aperture limit relative to center
+(upper  =           3.) Upper aperture limit relative to center
+
+                        -- AUTOMATIC APERTURE RESIZING PARAMETERS --
+(ylevel =         0.05) Fraction of peak or intensity for resizing
+
+.KE
+.KS
+.V1
+                        -- TRACE PARAMETERS --
+(t_step =           10) Tracing step
+(t_funct=      spline3) Trace fitting function
+(t_order=            2) Trace fitting function order
+(t_niter=            1) Trace rejection iterations
+(t_low  =           3.) Trace lower rejection sigma
+(t_high =           3.) Trace upper rejection sigma
+
+.KE
+.KS
+.V1
+                        -- DEFAULT BACKGROUND PARAMETERS --
+(buffer =           1.) Buffer distance from apertures
+(apscat1=             ) Fitting parameters across the dispersion
+(apscat2=             ) Fitting parameters along the dispersion
+(b_funct=     legendre) Background function
+(b_order=            2) Background function order
+(b_sampl=  -10:-6,6:10) Background sample regions
+(b_naver=           -3) Background average or median
+(b_niter=            0) Background rejection iterations
+(b_low  =           3.) Background lower rejection sigma
+(b_high =           3.) Background upper rejection sigma
+(b_grow =           0.) Background rejection growing radius
+(b_smoot=           10) Background smoothing length
+
+.KE
+.KS
+.V1
+                        -- APERTURE EXTRACTION PARAMETERS --
+(weights=         none) Extraction weights (none|variance)
+(pfit   =        fit1d) Profile fitting algorithm (fit1d|fit2d)
+(lsigma =           3.) Lower rejection threshold
+(usigma =           3.) Upper rejection threshold
+
+.KE
+.KS
+.V1
+                        -- FLAT FIELD FUNCTION FITTING PARAMETERS --
+(f_inter=           no) Fit flat field interactively?
+(f_funct=      spline3) Fitting function
+(f_order=           20) Fitting function order
+
+.KE
+.KS
+.V1
+                        -- ARC DISPERSION FUNCTION PARAMETERS --
+(coordli= linelist$thar.dat) Line list
+(match  =           1.) Line list matching limit in Angstroms
+(fwidth =           4.) Arc line widths in pixels
+(cradius=           4.) Centering radius in pixels
+(i_funct=    chebyshev) Echelle coordinate function
+(i_xorde=            3) Order of coordinate function along dispersion
+(i_yorde=            3) Order of coordinate function across dispersion
+(i_niter=            3) Rejection iterations
+(i_low  =           3.) Lower rejection sigma
+(i_high =           3.) Upper rejection sigma
+(refit  =          yes) Refit coordinate function when reidentifying?
+
+.KE
+.KS
+.V1
+                        -- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+(select =       interp) Selection method for reference spectra
+(sort   =           jd) Sort key
+(group  =          ljd) Group key
+(time   =           no) Is sort key a time?
+(timewra=          17.) Time wrap point for time sorting
+
+.KE
+.KS
+.V1
+                        -- DISPERSION CORRECTION PARAMETERS --
+(lineari=          yes) Linearize (interpolate) spectra?
+(log    =           no) Logarithmic wavelength scale?
+(flux   =          yes) Conserve flux?
+
+.KE
+.V2
+.NH 2
+Aperture Definitions
+.LP
+The first operation is to define the extraction apertures, which include the
+aperture width, background regions, and position dependence with
+wavelength, for the object and arc orders of interest.  This is done
+on a reference spectrum which is usually a flat field taken through
+both fibers.  Other spectra will inherit the reference apertures and
+apply a correction for any shift of the orders across the dispersion.
+The reference apertures are defined only once unless the \f(CWredo\fR
+option is set.
+.LP
+The selected number of orders are found automatically by selecting the
+highest peaks in a cut across the dispersion.  Note that the specified
+number of orders is multiplied by two in defining the apertures.  Apertures
+are assigned with a limits set by the \f(CWlower\fR and
+\f(CWupper\fR parameter and numbered sequentially.  A query is then
+given allowing the aperture limits to be "resized" based on the profile
+itself (see \fBapresize\fR).
+.LP
+A cut across the orders is then shown with the apertures marked and
+an interactive aperture editing mode is entered (see \fBapedit\fR).
+For \fBdofoe\fR the aperture identifications and numbering is particularly
+critical.  All "pairs" of object and arc orders in the region of
+interest must be defined without skipping any orders.  The orders must
+also be numbered sequentially (though the direction does not matter)
+so that the arc apertures are either all even or all odd as defined
+by the \f(CWarcaps\fR parameter (the default is even numbers for the
+arc apertures).  The 'o' key will provide the necessary reordering.
+If local background subtraction is used the background regions should
+also be checked with the 'b' key.  Typically one adjusts all
+the background regions at the same time by selecting all apertures with
+the 'a' key first.  To exit the background and aperture editing steps type
+'q'.
+.LP
+Next the positions of the orders at various points along the dispersion are
+measured and "trace functions" are fit.  The user is asked whether to fit
+each trace function interactively.  This is selected to adjust the fitting
+parameters such as function type and order.  When interactively fitting a
+query is given for each aperture.  After the first aperture one may skip
+reviewing the other traces by responding with "NO".  Queries made by
+\fBdofoe\fR generally may be answered with either lower case "yes" or "no"
+or with upper case "YES" or "NO".  The upper case responses apply to all
+further queries and so are used to eliminate further queries of that kind.
+.LP
+The above steps are all performed using tasks from the \fBapextract\fR
+package and parameters from the \fBparams\fR parameters.  As a quick
+summary, the dispersion direction of the spectra are determined from the
+package \fBdispaxis\fR parameter if not defined in the image header.  The default
+line or column for finding the orders and the number of image lines or
+columns to sum are set by the \f(CWline\fR and \f(CWnsum\fR parameters.  A line
+of INDEF (the default) selects the middle of the image.  The automatic
+finding algorithm is described for the task \fBapfind\fR and basically
+finds the strongest peaks.  The resizing is described in the task
+\fBapresize\fR and the parameters used are also described there and
+identified in the PARAMETERS section.  The tracing is done as described in
+\fBaptrace\fR and consists of stepping along the image using the specified
+\f(CWt_step\fR parameter.  The function fitting uses the \fBicfit\fR commands
+with the other parameters from the tracing section.
+.NH 2
+Background or Scattered Light Subtraction
+.LP
+In addition to not subtracting any background scattered light there are two
+approaches to subtracting this light.  The first is to determine a smooth
+global scattered light component.  The second is to subtract a locally
+determined background at each point along the dispersion and for each
+aperture.  Note that background subtraction is only done for object images
+and not for arc images.
+.LP
+The global scattered light fitting and subtraction is done with the task
+\fBapscatter\fR.  The function fitting parameters are set interactively
+using the aperture reference spectrum.  All other subtractions are done
+noninteractively with the same set of parameters.  The scattered light is
+subtracted from the input images, thus modifying them, and one might wish
+to first make backups of the original images.
+.LP
+The scattered light is measured between the apertures using a specified
+buffer distance from the aperture edges.  The scattered light pixels are
+fit by a series of one dimensional functions across the dispersion.  The
+independent fits are then smoothed along the dispersion by again fitting
+low order functions.  These fits then define the smooth scattered light
+surface to be subtracted from the image.  The fitting parameters are
+defined and recorded in the two parameter sets \f(CWapscat1\fR and
+\f(CWapscat2\fR.  The scattered light algorithm is described more fully in
+\fBapscatter\fR.  This algorithm is relatively slow.
+.LP
+Local background subtraction is done during extraction based on background
+regions and parameters defined by the default background parameters or
+changed during interactive review of the apertures.  The background
+subtraction options are to subtract the average, median, or minimum of the
+pixels in the background regions, or to fit a function and subtract the
+function from under the extracted object pixels.  The background regions
+are specified in pixels from the aperture center and follow changes in
+center of the spectrum along the dispersion.  The syntax is colon separated
+ranges with multiple ranges separated by a comma or space.  The background
+fitting uses the \fBicfit\fR routines which include medians, iterative
+rejection of deviant points, and a choice of function types and orders.
+Note that it is important to use a method which rejects cosmic rays such as
+using either medians over all the background regions (\f(CWbackground\fR =
+"median") or median samples during fitting (\f(CWb_naverage\fR < -1).
+The background smoothing parameter \f(CWb_smooth\fR is may be used
+to provide some additional local smoothing of the background light.
+The background subtraction algorithm and options are described in greater
+detail in \fBapsum\fR and \fBapbackground\fR.
+.NH 2
+Extraction
+.LP
+The actual extraction of the spectra is done by summing across the fixed
+width apertures at each point along the dispersion.  The default is to
+simply sum the pixels using partial pixels at the ends.  There is an
+option to weight the sum based on a Poisson noise model using the
+\f(CWreadnoise\fR and \f(CWgain\fR detector parameters.  Note that if the
+\f(CWclean\fR option is selected the variance weighted extraction is used
+regardless of the \f(CWweights\fR parameter.  The sigma threshold for
+cleaning are also set in the \fBparams\fR parameters.
+.LP
+The cleaning and variance weighting options require knowing the effective
+(i.e. accounting for any image combining) read out noise and gain.  These
+numbers need to be adjusted if the image has been processed such that the
+intensity scale has a different origin (such as a scattered light
+subtraction) or scaling (such as caused by unnormalized flat fielding).
+These options also require using background subtraction if the profile does
+not go to zero.  For optimal extraction and cleaning to work it is
+recommended that any scattered light be accounted for by local background
+subtraction rather than with the scattered light subtraction and the
+\f(CWfitflat\fR option be used.  The \f(CWb_smooth\fR parameter is also
+appropriate in this application and improves the optimal extraction results
+by reducing noise in the background signal.  For further discussion of
+cleaning and variance weighted extraction see \fBapvariance\fR and
+\fBapprofiles\fR as well as  \fBapsum\fR.
+.NH 2
+Flat Field Correction
+.LP
+Flat field corrections may be made during the basic CCD processing; i.e.
+direct division by the two dimensional flat field observation.  In that
+case do not specify a flat field spectrum; use the null string "".  The
+\fBdofoe\fR task provides an alternative flat field response correction
+based on division of the extracted object spectra by the extracted flat field
+spectra.  A discussion of the theory and merits of flat fielding directly
+verses using the extracted spectra will not be made here.  The
+\fBdofoe\fR flat fielding algorithm is the \fIrecommended\fR method for
+flat fielding since it works well and is not subject to the many problems
+involved in two dimensional flat fielding.
+.LP
+The first step is extraction of the flat field spectrum, if one is specified,
+using the reference apertures.  Only one flat field is allowed so if
+multiple flat fields are required the data must be reduced in groups.  When
+the \f(CWfitflat\fR option is selected (the default) the extracted flat field
+spectra are fit by smooth functions and the ratio of the flat field spectra
+to the smooth functions define the response spectra.  The default fitting
+function and order are given by the parameters \f(CWf_function\fR and
+\f(CWf_order\fR.  If the parameter \f(CWf_interactive\fR is "yes" then the
+fitting is done interactively using the \fBfit1d\fR task which uses the
+\fBicfit\fR interactive fitting commands.
+.LP
+If the \f(CWfitflat\fR option is not selected the extracted and globally
+normalized flat field spectra are directly divided in the object spectra.
+This removes the blaze function, thus altering the data counts, and
+introduces the reciprocal of the flat field spectrum in the object
+spectra.
+.LP
+The final step is to normalize the flat field spectra by the mean counts over
+all the fibers.  This normalization step is simply to preserve the average
+counts of the extracted object and arc spectra after division by the
+response spectra.
+.NH 2
+Dispersion Correction
+.LP
+If dispersion correction is not selected, \f(CWdispcor\fR=no, then the object
+spectra are simply extracted.  If it is selected the arc spectra are used
+to dispersion calibrate the object spectra.  There are four steps involved;
+determining the dispersion functions relating pixel position to wavelength,
+assigning the appropriate dispersion function to a particular observation,
+determining a zero point wavelength shift from the arc fiber to be applied
+to the object fiber dispersion function, and either storing the nonlinear
+dispersion function in the image headers or resampling the spectra to
+evenly spaced pixels in wavelength.
+.LP
+The first arc spectrum in the arc list is used to define the reference
+dispersion solution.  It is extracted using the reference aperture
+definitions.  Note extractions of arc spectra are not background or
+scattered light subtracted.  The interactive task \fBecidentify\fR is used
+to define the dispersion function in one fiber.  The idea is to mark some
+lines in a few orders whose wavelengths are known (with the line list used
+to supply additional lines after the first few identifications define the
+approximate wavelengths) and to fit a function giving the wavelength from
+the aperture number and pixel position.  The dispersion function for
+the second fiber is then determined automatically by reference to the first
+fiber using the task \fBecreidentify\fR.
+.LP
+The arc dispersion function parameters are for \fBecidentify\fR and it's
+related partner \fBecreidentify\fR.  The parameters define a line list for
+use in automatically assigning wavelengths to arc lines, a centering width
+(which should match the line widths at the base of the lines), the
+dispersion function type and orders, parameters to exclude bad lines from
+function fits, and defining whether to refit the dispersion function as
+opposed to simply determining a zero point shift.  The defaults should
+generally be adequate and the dispersion function fitting parameters may be
+altered interactively.  One should consult the help for the two tasks for
+additional details of these parameters and the interactive operation of
+\fBecidentify\fR.
+.LP
+Once the reference dispersion functions are defined other arc spectra are
+extracted as they are assign to the object spectra.  The assignment of
+arcs is done either explicitly with an arc assignment table (parameter
+\f(CWarctable\fR) or based on a header parameter such as a time.
+The assignments are made by the task \fBrefspectra\fR.  When two arcs are
+assigned to an object spectrum an interpolation is done between the two
+dispersion functions.  This makes an approximate correction for steady
+drifts in the dispersion.  Because the arc fiber monitors any zero point
+shifts in the dispersion functions it is probably only necessary to have
+one or two arc spectra, one at the beginning and/or one at the end of the
+night.
+.LP
+The tasks \fBsetjd\fR and \fBsetairmass\fR are automatically run on all
+spectra.  This computes and adds the header parameters for the Julian date
+(JD), the local Julian day number (LJD), the universal time (UTMIDDLE), and
+the air mass at the middle of the exposure.  The default arc assignment is
+to use the Julian date grouped by the local Julian day number.  The
+grouping allows multiple nights of data to be correctly assigned at the
+same time.
+.LP
+Defining the dispersion function for a new arc extraction is done with
+the task \fBecreidentify\fR.  This is done noninteractively with log
+information recorded about the line reidentifications and the fit.
+.LP
+From the one or two arc spectra come two full dispersion function,
+one for the object fiber and one for the arc fiber.  When an object
+spectrum is extracted so is the simultaneous arc spectrum.  A zero point
+shift of the arc spectrum relative to the dispersion solution of the
+dual arc observation is computed using \fBecreidentify\fR
+(\f(CWrefit\fR=no).  This zero point shift is assumed to be the same for the
+object fiber and it is added to the dispersion function of the dual arc
+observation for the object fiber.  Note that this does not assume that the
+object and arc fiber dispersion functions are the same or have the same
+wavelength origin, but only that the same shift in wavelength zero point
+applies to both fibers.  Once the dispersion function correction is
+determined from the extracted arc fiber spectrum it is deleted leaving only
+the object spectrum.
+.LP
+The last step of dispersion correction is setting the dispersion
+of the object spectrum.  There are two choices here.
+If the \f(CWlinearize\fR parameter is not set the nonlinear dispersion
+function is stored in the image header.  Other IRAF tasks interpret
+this information when dispersion coordinates are needed for plotting
+or analysis.  This has the advantage of not requiring the spectra
+to be interpolated and the disadvantage that the dispersion
+information is only understood by IRAF tasks and cannot be readily
+exported to other analysis software.
+.LP
+If the \f(CWlinearize\fR parameter is set then the spectra are resampled to a
+linear dispersion relation either in wavelength or the log of the
+wavelength.  For echelle spectra each order is linearized independently so
+that the wavelength interval per pixel is different in different orders.
+This preserves most of the resolution and avoids over or under sampling of
+the highest or lowest dispersion orders.  The wavelength limits are
+taken from the limits determined from the arc reference spectrum and
+the number of pixels is the same as the original images.  The dispersion
+per pixel is then derived from these constraints.
+.LP
+The linearization algorithm  parameters allow selecting the interpolation
+function type, whether to conserve flux per pixel by integrating across the
+extent of the final pixel, and whether to linearize to equal linear or
+logarithmic intervals.  The latter may be appropriate for radial velocity
+studies.  The default is to use a fifth order polynomial for interpolation,
+to conserve flux, and to not use logarithmic wavelength bins.  These
+parameters are described fully in the help for the task \fBdispcor\fR which
+performs the correction.
+.NH
+References
+.NH 2
+IRAF Introductory References
+.LP
+Work is underway on a new introductory guide to IRAF.  Currently, the
+work below is the primary introduction.
+.IP
+P. Shames and D. Tody, \fIA User's Introduction to the IRAF Command
+Language\fR, Central Computer Services, NOAO, 1986.
+.NH 2
+CCD Reductions
+.IP
+F. Valdes, \fIThe IRAF CCD Reduction Package -- CCDRED\fR, Central
+Computer Services, NOAO, 1987.
+.IP
+F. Valdes, \fIUser's Guide to the CCDRED Package\fR, Central
+Computer Services, NOAO, 1988.  Also on-line as \f(CWhelp ccdred.guide\fR.
+.IP
+P. Massey, \fIA User's Guide to CCD Reductions with IRAF\fR, Central
+Computer Services, NOAO, 1989.
+.NH 2
+Aperture Extraction Package
+.IP
+F. Valdes, \fIThe IRAF APEXTRACT Package\fR, Central Computer Services,
+NOAO, 1987 (out-of-date).
+.NH 2
+Task Help References
+.LP
+Each task in the \fBspecred\fR packages and tasks used by \fBdofibers\fR have
+help pages describing the parameters and task in some detail.  To get
+on-line help type
+.V1
+
+cl> help \fItaskname\fR
+
+.V2
+The output of this command can be piped to \fBlprint\fR to make a printed
+copy.
+
+.V1
+      apall - Extract 1D spectra (all parameters in one task)
+  apdefault - Set the default aperture parameters and apidtable
+     apedit - Edit apertures interactively
+     apfind - Automatically find spectra and define apertures
+      apfit - Fit 2D spectra and output the fit, difference, or ratio
+  apflatten - Remove overall spectral and profile shapes from flat fields
+     apmask - Create and IRAF pixel list mask of the apertures
+apnormalize - Normalize 2D apertures by 1D functions
+ aprecenter - Recenter apertures
+   apresize - Resize apertures
+  apscatter - Fit and subtract scattered light
+      apsum - Extract 1D spectra
+    aptrace - Trace positions of spectra
+
+      bplot - Batch plots of spectra
+  calibrate - Apply extinction and flux calibrations to spectra
+  continuum - Fit the continuum in spectra
+   deredden - Apply interstellar extinction corrections
+    dispcor - Dispersion correct spectra
+     dopcor - Doppler correct spectra
+ ecidentify - Identify features in spectrum for dispersion solution
+ecreidentify - Automatically identify features in spectra
+ refspectra - Assign wavelength reference spectra to other spectra
+     sarith - Spectrum arithmetic
+   scombine - Combine spectra
+      scopy - Select and copy apertures in different spectral formats
+   sensfunc - Create sensitivity function
+ setairmass - Compute effective airmass and middle UT for an exposure
+      setjd - Compute and set Julian dates in images
+      slist - List spectrum header parameters
+   specplot - Stack and plot multiple spectra
+      splot - Preliminary spectral plot/analysis
+   standard - Identify standard stars to be used in sensitivity calc
+
+      dofoe - Process Fiber Optic Echelle spectra
+      demos - Demonstrations and tests
+
+            Additional help topics
+
+   onedspec.package - Package parameters and general description of package
+  apextract.package - Package parameters and general description of package
+ approfiles - Profile determination algorithms
+ apvariance - Extractions, variance weighting, cleaning, and noise model
+   center1d - One dimensional centering algorithm
+      icfit - Interactive one dimensional curve fitting
+
+.V2
+.SH
+Appendix A: DOFOE Parameters
+.LP
+.nr PS 8
+.nr VS 10
+objects
+.LS
+List of object spectra to be processed.  Previously processed spectra are
+ignored unless the \f(CWredo\fR flag is set or the \f(CWupdate\fR flag is set and
+dependent calibration data has changed.  Extracted spectra are ignored.
+.LE
+apref = ""
+.LS
+Aperture reference spectrum.  This spectrum is used to define the basic
+extraction apertures and is typically a flat field spectrum.
+.LE
+flat = "" (optional)
+.LS
+Flat field spectrum.  If specified the one dimensional flat field spectrum
+is extracted and used to make flat field calibrations.
+.LE
+arcs = "" (at least one if dispersion correcting)
+.LS
+List of arc spectra in which both fibers have arc spectra.  These spectra
+are used to define the dispersion functions for each fiber apart from a
+zero point correction made with the arc fiber during an observation.  One
+fiber from the first spectrum is used to mark lines and set the dispersion
+function interactively and dispersion functions for the other fiber and arc
+spectra are derived from it.
+.LE
+arctable = "" (optional) (refspectra)
+.LS
+Table defining arc spectra to be assigned to object spectra (see
+\fBrefspectra\fR).  If not specified an assignment based on a header
+parameter, \f(CWparams.sort\fR, such as the observation time is made.
+.LE
+
+readnoise = "0." (apsum)
+.LS
+Read out noise in photons.  This parameter defines the minimum noise
+sigma.  It is defined in terms of photons (or electrons) and scales
+to the data values through the gain parameter.  A image header keyword
+(case insensitive) may be specified to get the value from the image.
+.LE
+gain = "1." (apsum)
+.LS
+Detector gain or conversion factor between photons/electrons and
+data values.  It is specified as the number of photons per data value.
+A image header keyword (case insensitive) may be specified to get the value
+from the image.
+.LE
+datamax = INDEF (apsum.saturation)
+.LS
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the flat field or
+arc spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.LE
+norders = 12 (apfind)
+.LS
+Number of orders to be found.  This number is used during the automatic
+definition of the apertures from the aperture reference spectrum.  Note
+that the number of apertures defined is twice this number, one set for
+the object fiber orders and one set for the arc fiber orders.
+The interactive review of the aperture assignments allows verification
+and adjustments to the automatic aperture definitions.
+.LE
+width = 4. (apedit)
+.LS
+Approximate base full width of the fiber profiles.  This parameter is used
+for the profile centering algorithm.
+.LE
+arcaps = "2x2"
+.LS
+List of arc fiber aperture numbers.
+Since the object and arc fiber orders are paired the default setting
+expects the even number apertures to be the are apertures.  This should
+be checked interactively.
+.LE
+
+fitflat = yes (flat1d)
+.LS
+Fit and divide the extracted flat field field orders by a smooth function
+in order to normalize the wavelength response?  If not done the flat field
+spectral shape (which includes the blaze function) will be divided
+out of the object spectra, thus altering the object data values.
+If done only the small scale response variations are included in the
+flat field and the object spectra will retain their observed flux
+levels and blaze function.
+.LE
+background = "none" (apsum, apscatter)
+.LS
+Type of background light subtraction.  The choices are "none" for no
+background subtraction, "scattered" for a global scattered light
+subtraction, "average" to average the background within background regions,
+"median" to use the median in background regions, "minimum" to use the
+minimum in background regions, or "fit" to fit across the dispersion using
+the background within background regions.  The scattered light option fits
+and subtracts a smooth global background and modifies the input images.
+This is a slow operation and so is NOT performed in quicklook mode.  The
+other background options are local to each aperture at each point along the
+dispersion.  The "fit" option uses additional fitting parameters from
+\fBparams\fR and the "scattered" option uses parameters from \fBapscat1\fR
+and \fBapscat2\fR.
+.LE
+clean = yes (apsum)
+.LS
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction and requires reasonably good values
+for the readout noise and gain.  In addition the datamax parameters
+can be useful.
+.LE
+dispcor = yes
+.LS
+Dispersion correct spectra?  Depending on the \f(CWparams.linearize\fR
+parameter this may either resample the spectra or insert a dispersion
+function in the image header.
+.LE
+redo = no
+.LS
+Redo operations previously done?  If no then previously processed spectra
+in the objects list will not be processed (unless they need to be updated).
+.LE
+update = no
+.LS
+Update processing of previously processed spectra if aperture, flat
+field, or dispersion reference definitions are changed?
+.LE
+batch = no
+.LS
+Process spectra as a background or batch job.
+.LE
+listonly = no
+.LS
+List processing steps but don't process?
+.LE
+
+params = "" (pset)
+.LS
+Name of parameter set containing additional processing parameters.  The
+default is parameter set \fBparams\fR.  The parameter set may be examined
+and modified in the usual ways (typically with "epar params" or ":e params"
+from the parameter editor).  Note that using a different parameter file
+is not allowed.  The parameters are described below.
+.LE
+
+.ce
+-- PACKAGE PARAMETERS
+
+Package parameters are those which generally apply to all task in the
+package.  This is also true of \fBdofoe\fR.
+
+observatory = "observatory"
+.LS
+Observatory at which the spectra were obtained if not specified in the
+image header by the keyword OBSERVAT.  For FOE data the image headers
+identify the observatory as "kpno" so this parameter is not used.
+For data from other observatories this parameter may be used
+as describe in \fBobservatory\fR.
+.LE
+interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc)
+.LS
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.V1
+	nearest - nearest neighbor
+	 linear - linear
+	  poly3 - 3rd order polynomial
+	  poly5 - 5th order polynomial
+	spline3 - cubic spline
+	   sinc - sinc function
+.V2
+.LE
+dispaxis = 2
+.LS
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.
+.LE
+database = "database"
+.LS
+Database (directory) used for storing aperture and dispersion information.
+.LE
+verbose = no
+.LS
+Print verbose information available with various tasks.
+.LE
+logfile = "logfile", plotfile = ""
+.LS
+Text and plot log files.  If a filename is not specified then no log is
+kept.  The plot file contains IRAF graphics metacode which may be examined
+in various ways such as with \fBgkimosaic\fR.
+.LE
+records = ""
+.LS
+Dummy parameter to be ignored.
+.LE
+version = "ECHELLE: ..."
+.LS
+Version of the package.
+.LE
+
+.ce
+PARAMS PARAMETERS
+
+The following parameters are part of the \fBparams\fR parameter set and
+define various algorithm parameters for \fBdofoe\fR.
+
+.ce
+--  GENERAL PARAMETERS --
+
+line = INDEF, nsum = 10
+.LS
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, recentering, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.LE
+extras = no (apsum)
+.LS
+Include extra information in the output spectra?  When cleaning or using
+variance weighting the cleaned and weighted spectra are recorded in the
+first 2D plane of a 3D image, the raw, simple sum spectra are recorded in
+the second plane, and the estimated sigmas are recorded in the third plane.
+.LE
+
+.ce
+-- DEFAULT APERTURE LIMITS --
+
+lower = -3., upper = 3. (apdefault)
+.LS
+Default lower and upper aperture limits relative to the aperture center.
+These limits are used when the apertures are first found and may be
+resized automatically or interactively.
+.LE
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+
+ylevel = 0.05 (apresize)
+.LS
+Data level at which to set aperture limits during automatic resizing.
+It is a fraction of the peak relative to a local background.
+.LE
+
+.ce
+-- TRACE PARAMETERS --
+
+t_step = 10 (aptrace)
+.LS
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \f(CWnsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.LE
+t_function = "spline3", t_order = 2 (aptrace)
+.LS
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.LE
+t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+.LS
+Default number of rejection iterations and rejection sigma thresholds.
+.LE
+
+.ce
+-- DEFAULT BACKGROUND PARAMETERS --
+
+buffer = 1. (apscatter)
+.LS
+Buffer distance from the edge of any aperture for data to be included
+in the scattered light determination.  This parameter may be modified
+interactively.
+.LE
+apscat1 = "", apscat2 = "" (apscatter)
+.LS
+Parameter sets for the fitting functions across and along the dispersion.
+These parameters are those used by \fBicfit\fR.  These parameters are
+usually set interactively.
+.LE
+b_function = "legendre", b_order = 1 (apsum)
+.LS
+Default background fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.LE
+b_naverage = -100 (apsum)
+.LS
+Default number of points to average or median.  Positive numbers
+average that number of sequential points to form a fitting point.
+Negative numbers median that number, in absolute value, of sequential
+points.  A value of 1 does no averaging and each data point is used in the
+fit.
+.LE
+b_niterate = 0 (apsum)
+.LS
+Default number of rejection iterations.  If greater than zero the fit is
+used to detect deviant fitting points and reject them before repeating the
+fit.  The number of iterations of this process is given by this parameter.
+.LE
+b_low_reject = 3., b_high_reject = 3. (apsum)
+.LS
+Default background lower and upper rejection sigmas.  If greater than zero
+points deviating from the fit below and above the fit by more than this
+number of times the sigma of the residuals are rejected before refitting.
+.LE
+b_smooth = 10 (apsum)
+.LS
+Box car smoothing length for background when using background
+subtraction.  Since the background noise is often the limiting factor
+for good extraction one may box car smooth the the background to improve the
+statistics.
+.LE
+
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+
+weights = "none" (apsum)
+.LS
+Type of extraction weighting.  Note that if the \f(CWclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+
+"none"
+.LS
+The pixels are summed without weights except for partial pixels at the
+ends.
+.LE
+"variance"
+.LS
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \f(CWgain\fR and \f(CWreadnoise\fR
+parameters.
+.LE
+.LE
+pfit = "fit1d" (apsum) (fit1d|fit2d)
+.LS
+Profile fitting algorithm for cleaning and variance weighted extractions.
+The default is generally appropriate for FOE data but users
+may try the other algorithm.  See \fBapprofiles\fR for further information.
+.LE
+lsigma = 3., usigma = 3. (apsum)
+.LS
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.LE
+
+.ce
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --
+
+f_interactive = no (fit1d)
+.LS
+Fit the one dimensional flat field order spectra interactively?
+This is used if \f(CWfitflat\fR is set and a two dimensional flat field
+spectrum is specified.
+.LE
+f_function = "spline3", f_order = 20 (fit1d)
+.LS
+Function and order used to fit the composite one dimensional flat field
+spectrum.  The functions are "legendre", "chebyshev", "spline1", and
+"spline3".  The spline functions are linear and cubic splines with the
+order specifying the number of pieces.
+.LE
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+
+threshold = 10. (identify/reidentify)
+.LS
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.LE
+coordlist = "linelist$thar.dat" (ecidentify)
+.LS
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelist$".
+.LE
+match = 1. (ecidentify)
+.LS
+The maximum difference for a match between the dispersion function computed
+value and a wavelength in the coordinate list.
+.LE
+fwidth = 4. (ecidentify)
+.LS
+Approximate full base width (in pixels) of arc lines.
+.LE
+cradius = 4. (reidentify)
+.LS
+Radius from previous position to reidentify arc line.
+.LE
+i_function = "chebyshev", i_xorder = 3, i_yorder = 3 (ecidentify)
+.LS
+The default function, function order for the pixel position dependence, and
+function order for the aperture number dependence to be fit to the arc
+wavelengths.  The functions choices are "chebyshev" or "legendre".
+.LE
+i_niterate = 3, i_low = 3.0, i_high = 3.0 (ecidentify)
+.LS
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.LE
+refit = yes (ecreidentify)
+.LS
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.LE
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+
+select = "interp" (refspectra)
+.LS
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+
+average
+.LS
+Average two reference spectra without regard to any sort parameter.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.
+This option is used to assign two reference spectra, with equal weights,
+independent of any sorting parameter.
+.LE
+following
+.LS
+Select the nearest following spectrum in the reference list based on the
+sorting parameter.  If there is no following spectrum use the nearest preceding
+spectrum.
+.LE
+interp
+.LS
+Interpolate between the preceding and following spectra in the reference
+list based on the sorting parameter.  If there is no preceding and following
+spectrum use the nearest spectrum.  The interpolation is weighted by the
+relative distances of the sorting parameter.
+.LE
+match
+.LS
+Match each input spectrum with the reference spectrum list in order.
+This overrides the reference aperture check.
+.LE
+nearest
+.LS
+Select the nearest spectrum in the reference list based on the sorting
+parameter.
+.LE
+preceding
+.LS
+Select the nearest preceding spectrum in the reference list based on the
+sorting parameter.  If there is no preceding spectrum use the nearest following
+spectrum.
+.LE
+.LE
+sort = "jd", group = "ljd" (refspectra)
+.LS
+Image header keywords to be used as the sorting parameter for selection
+based on order and to group spectra.
+A null string, "", or the word "none" may be use to disable the sorting
+or grouping parameters.
+The sorting parameter
+must be numeric but otherwise may be anything.  The grouping parameter
+may be a string or number and must simply be the same for all spectra within
+the same group (say a single night).
+Common sorting parameters are times or positions.
+In \fBdofoe\fR the Julian date (JD) and the local Julian day number (LJD)
+at the middle of the exposure are automatically computed from the universal
+time at the beginning of the exposure and the exposure time.  Also the
+parameter UTMIDDLE is computed.
+.LE
+time = no, timewrap = 17. (refspectra)
+.LS
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.LE
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+
+linearize = yes (dispcor)
+.LS
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling
+If no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data are not interpolated.
+.LE
+log = no (dispcor)
+.LS
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.LE
+flux = yes (dispcor)
+.LS
+Conserve the total flux during interpolation?  If \f(CWno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \f(CWyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.LE
+
+.ce
+ENVIRONMENT PARAMETERS
+.LP
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
diff --git a/noao/imred/echelle/doc/ecidentify.hlp b/noao/imred/echelle/doc/ecidentify.hlp
new file mode 100644
index 00000000..61187a43
--- /dev/null
+++ b/noao/imred/echelle/doc/ecidentify.hlp
@@ -0,0 +1,770 @@
+.help ecidentify May88 noao.imred.echelle
+.ih
+NAME
+ecidentify -- Determine the dispersion relation in echelle spectra
+.ih
+USAGE
+ecidentify images
+.ih
+PARAMETERS
+.ls images
+List of echelle format spectra in which to identify lines and fit
+dispersion functions.
+.le
+.ls database = "database"
+Database in which the feature data and dispersion functions are recorded.
+.le
+.ls coordlist = "linelists$idhenear.dat"
+User coordinate list consisting of an ordered list of line coordinates.  A
+comment line of the form "# units <units>", where <units> is one of the
+understood units names, defines the units of the line list.  If no units
+are specified then Angstroms are assumed.  Some standard line lists are
+available in the directory "linelists$".  The standard line lists are
+described under the topic \fIlinelists\fR.
+.le
+.ls units = ""
+The units to use if no database entry exists.  The units are specified as
+described in
+
+.nf
+    cl> help onedspec.package section=units
+.fi
+
+If no units are specified and a coordinate list is used then the units of
+the coordinate list are selected.  If a database entry exists then the
+units defined there override both this parameter and the coordinate list.
+.le
+.ls match = 1.
+The maximum difference for a match between the feature coordinate function
+value and a coordinate in the coordinate list.  The unit of this parameter
+is that of the user coordinates.
+.le
+.ls maxfeatures = 100
+Maximum number of the strongest features to be selected automatically from
+the coordinate list (function 'l') or from the image data (function 'y').
+.le
+.ls zwidth = 10.
+Width of graphs, in user coordinates, when in zoom mode (function 'z').
+.le
+
+The following parameters are used in determining feature positions.
+.ls ftype = "emission"
+Type of features to be identified.  The possibly abbreviated choices are
+"emission" and "absorption".
+.le
+.ls fwidth = 4.
+Width in pixels of features to be identified.
+.le
+.ls cradius = 5.
+The maximum distance, in pixels, allowed between a feature position
+and the initial estimate when defining a new feature.
+.le
+.ls threshold = 10.
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.le
+.ls minsep = 2.
+The minimum separation, in pixels, allowed between feature positions
+when defining a new feature.
+.le
+
+The following default parameters are used when fitting a function to
+the user coordinates.  If a previous solution is read from the database
+then the parameters from that solution override the defaults below.
+.ls function = "chebyshev"
+The function to be fit to the user coordinates as a function of the pixel
+coordinate and aperture number.  The choices are bi-dimensional
+"chebyshev" and "legendre" polynomials.
+.le
+.ls xorder = 2
+Order of the fitting function along each echelle order.
+The order is the number of polynomial terms; i.e. xorder = 2 is a linear
+function.
+.le
+.ls yorder = 2
+Order of the fitting function with respect to the aperture number.
+The order is the number of polynomial terms; i.e. yorder = 2 is a linear
+function.
+.le
+.ls niterate = 0, lowreject = 3, highreject = 3.
+Default number of rejection iterations and the sigma clipping thresholds.  If
+\fIniterate\fR is zero then no rejection is done.
+.le
+
+The following parameters control the graphics input and output.
+.ls graphics = "stdgraph"
+Graphics device.  The default is the standard graphics device which is
+generally a graphics terminal.
+.le
+.ls curosr = ""
+Cursor input file.  If a cursor file is not given then the standard graphics
+cursor is read.
+.le
+.ih
+CURSOR KEYS
+
+.nf
+           ECIDENTIFY CURSOR KEY AND COLON COMMAND SUMMARY
+
+?  Help                   a  Affect all features     c  Center feature(s)
+d  Delete feature(s)      f  Fit dispersion          g  Fit zero point shift
+i  Initialize             j  Go to previous order    k  Go to next order
+l  Match coordinate list  m  Mark feature            n  Next feature
+o  Go to specified order  p  Pan graph               q  Quit
+r  Redraw graph           s  Shift feature           t  Reset position
+u  Enter user coordinate  w  Window graph            x  Crosscorrelate peaks
+y  Find peaks             z  Zoom graph              .  Nearest feature
++  Next feature           -  Previous feature        I  Interrupt
+
+:show [file]              :features [file]           :coordlist [file]
+:cradius [value]          :threshold [value]         :database [file]
+:ftype [type]             :fwidth [value]            :image [image]
+:labels [type]            :match [value]             :maxfeatures [value]
+:minsep [value]           :read [image]              :write [image]
+:zwidth [value]
+
+
+       ECHELLE DISPERSION FUNCTION FITTING COMMAND SUMMARY
+
+?  Help             c  Print coordinates             d  Delete point
+f  Fit dispersion   o  Fit with fixed order offset   q  Quit
+r  Redraw graph     u  Undelete point                w  Window graph
+x  Set ordinate     y  Set abscissa                  I  Interrupt
+
+:show               :function [value]   :highreject [value]   :lowreject [value]
+:niterate [value]   :xorder [value]     :yorder [value]
+
+.fi
+
+            ECIDENTIFY CURSOR KEYS AND COLON COMMANDS
+.ls ?
+Clear the screen and print a menu of cursor and colon commands.
+.le
+.ls a
+Apply next (c)enter or (d)elete operation to (a)ll features
+.le
+.ls c
+(C)enter the feature nearest the cursor.  Used when changing the position
+finding parameters or when features are defined from a previous feature list.
+May be used in combination with the (a)ll key.
+.le
+.ls d
+(D)elete the feature nearest the cursor.  (D)elete all features when preceded
+by the (a)ll key.  This does not affect the dispersion function.
+.le
+.ls f
+(F)it a function of the pixel coordinates and aperture numbers to the user
+coordinates.  This enters an interactive function fitting package.
+.le
+.ls g
+Fit a zero point shift to the user coordinates by minimizing the difference
+between the user and fitted coordinates.  The coordinate dispersion function
+is not changed.
+.le
+.ls i
+(I)nitialize (delete features and dispersion function fit).
+.le
+.ls j
+Go to the next aperture in decreasing line number in the echelle format image.
+Wrap around to the last line from the first line.
+.le
+.ls k
+Go to the next aperture in increasing line number in the echelle format image.
+Wrap around to the first line from the last line.
+.le
+.ls l
+(L)ocate features in the coordinate list.  A coordinate function must be
+defined or at least four features in more than one aperture must have user
+coordinates from which a coordinate function can be determined by an
+initial automatic function fit.
+.le
+.ls m
+(M)ark a new feature using the cursor position as the initial position
+estimate.
+.le
+.ls n
+Move the cursor or zoom to the (n)ext feature (same as +).
+.le
+.ls o
+Go to a specific aperture (related to an echelle (o)rder).  The user
+is queried for the aperture number.
+.le
+.ls p
+(P)an to the original window after (z)ooming on a feature.
+.le
+.ls q
+(Q)uit and continue with next image.
+.le
+.ls r
+(R)edraw the graph.
+.le
+.ls s
+(S)hift the fit coordinates relative to the pixel coordinates.  The
+user specifies the desired coordinate at the position of the cursor
+and a zero point shift to the fit coordinates is applied.  If features
+are defined then they are recentered and the shift is the average shift.
+The shift in pixels, user coordinates, and z (fractional shift) is printed.
+The user shift is for the fundamental order and the shift for each order
+is then given by this shift divided by the order number.
+.le
+.ls t
+Reset the current feature to the position of the cursor.  The feature
+is \fInot\fR recentered.  This is used to mark an arbitrary position.
+.le
+.ls u
+Enter a new (u)ser coordinate for the current feature.
+When (m)arking a new feature the user coordinate is also requested.
+.le
+.ls w
+(W)indow the graph.  A window prompt is given and a number of windowing
+options may be given.  For more help type '?' to the window prompt or
+see help under \fIgtools\fR.
+.le
+.ls x
+Crosscorrelate features with the data peaks and reregister.  This is
+generally used with a feature list from a different image.
+The mean shift in user coordinates, mean shift in pixels, and the fractional
+shift in user coordinates is printed.  The user shift is scaled to the
+fundamental order.
+.le
+.ls y
+Up to \fImaxfeatures\fR emission peaks are found automatically (in order of
+peak intensity) and, if a dispersion solution is defined, the peaks are
+identified from the coordinate list.
+.le
+.ls z
+(Z)oom on the feature nearest the cursor.  The width of the zoom window
+is determined by the parameter \fIzwidth\fR.
+.le
+.ls .
+Move the cursor or zoom window to the feature nearest the cursor.
+.le
+.ls 4 +
+Move the cursor or zoom window to the (n)ext feature.
+This does not automatically move to the next aperture.
+.le
+.ls 4 -
+Move the cursor or zoom window to the previous feature.
+This does not automatically move to the next aperture.
+.le
+.ls I
+Interrupt the task immediately.  The database is not updated.
+.le
+
+Parameters are shown or set with the following "colon commands", which may be
+abbreviated.  To show the value of a parameter type the parameter name alone
+and to set a new value follow the parameter name by the value.
+.ls :show file
+Show the values of all the parameters.  If a file name is given then the
+output is appended to that file.  If no file is given then the terminal
+is cleared and the output is sent to the terminal.
+.le
+.ls :features file
+Print the feature list and the fit rms.  If a file name is given then the
+output is appended to that file.  If no file is given then the terminal
+is cleared and the output is sent to the terminal.
+.le
+.ls :coordlist file
+Set or show the coordinate list file.
+.le
+.ls :cradius value
+Set or show the centering radius in pixels.
+.le
+.ls :threshold value
+Set or show the detection threshold for centering.
+.le
+.ls :database name
+Set or show the database for recording feature records.
+.le
+.ls :ftype value
+Set or show the feature type (emission or absorption).
+.le
+.ls :fwidth value
+Set or show the feature width in pixels.
+.le
+.ls :image imagename
+Set a new image or show the current image.
+.le
+.ls :labels value
+Set or show the feature label type (none, index, pixel, or user).
+.le
+.ls :match value
+Set or show the coordinate list matching distance.
+.le
+.ls :maxfeatures value
+Set or show the maximum number of features automatically found.
+.le
+.ls :minsep value
+Set or show the minimum separation allowed between features.
+.le
+.ls :read name
+Read a record from the database.  The record name defaults to the image name.
+.le
+.ls :threshold value
+Set or show the centering threshold.
+.le
+.ls :write name
+Write a record to the database.  The record name defaults to the image name.
+.le
+.ls :zwidth value
+Set or show the zoom width in user units.
+.le
+
+
+              DISPERSION FUNCTION FITTING COMMANDS
+.ls ?
+Page help information.
+.le
+.ls c
+Print input and fitted coordinates of point nearest the cursor.
+.le
+.ls d
+Delete the nearest undeleted point to the cursor.
+.le
+.ls f
+Fit a dispersion function including determining the order offset.
+.le
+.ls o
+Fit a dispersion function with the order offset fixed.  The user is queried
+for the order offset.  This is faster than the interactive fit to also
+determine the order.
+.le
+.ls q
+Quit and return to the spectrum display.
+.le
+.ls r
+Redraw the graph.
+.le
+.ls u
+Undelete the nearest deleted point to the cursor (which may be outside the
+graph window).
+.le
+.ls w
+Window the graph (type ? to the window prompt for more help).
+.le
+.ls x
+Set the quantity plotted along the ordinate (x axis).
+.le
+.ls y
+Set the quantity plotted along the abscissa (y axis).
+.le
+.ls I
+Interrupt the task immediately.  No information is saved in the database.
+.le
+
+.ls :function [value]
+Print or set the function type (chebyshev|legendre).
+.le
+.ls :show
+Print current function and orders.
+.le
+.ls :niterate [value], :lowreject [value], :highreject [value]
+Print or set the iterative rejection parameters.
+.le
+.ls :xorder [value]
+Print or set the order for the dispersion dependence.
+.le
+.ls :yorder [value]
+Print or set the order for the echelle order dependence.
+.le
+.ih
+DESCRIPTION
+Emission and absorption features in echelle format spectra (see \fIapsum\fR)
+are identified interactively and from a line list and a dispersion
+function is determined.  The results of the line identifications and
+dispersion function are stored in a database for further reference and
+for use with the tasks \fBecreidentify\fR and \fBecdispcor\fR.  Also
+the reference spectrum keyword REFSPEC is added to the image header.
+This is used by \fBrefspectra\fR and \fBecdispcor\fR.
+
+Each spectrum in the input list is identified in turn.  Initially the
+order in the first image line is graphed.  The user may change the
+displayed order with the 'j', 'k', and 'o' keys.  The initial feature
+list and dispersion function are read from the database if an entry
+exists.  The features are marked on the graph.  The image coordinates
+are in pixels unless a dispersion function is defined, in which case
+they are in user coordinate units (usually wavelength in Angstroms).
+The aperture number, pixel coordinate, coordinate function value, and
+user coordinate for the current feature are displayed on the status
+line.
+
+For consistency the orders are always identified by their aperture
+numbers in this task and all other tasks.  These are the
+identifications assigned when extracting the orders using the task
+\fIapsum\fR.  If the user has assigned true order numbers as the
+aperture numbers then there is no distinction between aperture and
+order number.  However, it is often the case that the aperture numbers
+are simply assigned sequentially and the true order numbers may not
+even be known.  Initially the orders are the same as the apertures
+numbers but after fitting a dispersion function the true order numbers
+will be determined.  This information is also recorded in the database
+and indicated in the graph titles but selecting an order to be graphed
+with 'o' and the status line information is always in terms of the
+aperture number.
+
+The graphics cursor is used to select features and perform various
+functions.  A menu of the keystroke options and functions is printed
+with the key '?'.  The cursor keys and their functions are defined in
+the CURSOR KEYS sections and described further below.  The standard
+cursor mode keys are also available to window and redraw the graph and
+to produce hardcopy "snaps".
+
+There are two types of feature selection functions;  defining new
+features and selecting previously defined features.  The key 'm' marks
+a new feature nearest the cursor position.  The feature position is
+determined by the feature centering algorithm (see help for
+\fBcenter1d\fR).  The type of feature, emission or absorption, is set
+by the \fIftype\fR parameter.  If the new position is within a distance
+given by the parameter \fIminsep\fR of a previous feature it is
+considered to be the same feature and replaces the old feature
+(normally the position of the new feature will be exactly the same as
+the original feature).  The coordinate list is searched for a match
+between the coordinate function value (when defined) and a user
+coordinate in the list.  If a match is found it becomes the default
+user coordinate which the user may override.  The new feature is marked
+on the graph and it becomes the current feature.  The redefinition of a
+feature which is within the minimum separation may be used to set the
+user coordinate from the coordinate list.  The key 't' allows setting
+the position of a feature to other than that found by the centering
+algorithm.
+
+The 'y' key applies a peak finding algorithm and up to the maximum
+number of features (\fImaxfeatures\fR) are found.  If there are more
+peaks only the strongest are kept.  The peaks are then matched against
+the coordinate list to find user coordinate values.
+
+To select a different feature as the current feature the keys '.', 'n',
+'+', and '-' are used.  The '.' selects the feature nearest the cursor,
+the 'n' and '+' select the next feature, and the '-' selects the
+previous feature relative to the current feature in the feature list as
+ordered by pixel coordinate.  These keys are useful when redefining the
+user coordinate with the 'u' key and when examining features in zoom
+mode.  To change apertures (orders) the 'j', 'k', and 'o' keys are
+used.
+
+If four or more features are identified spanning the range of the data
+(in pixel coordinates and in order number) or if a coordinate function
+is defined then the 'l' key may be used to identify additional features
+from a coordinate list.  If a coordinate function is not defined the
+default function is fit to the user coordinates of the currently
+defined features.  Then for each coordinate value in the coordinate
+list the pixel coordinate is determined and a search for a feature at
+that point is made.  If a feature is found (based on the parameters
+\fIftype, fwidth\fR, \fIcradius\fR, and \fBthreshold\fR) its user
+coordinate value based on the coordinate function is determined.  If
+the coordinate function value matches the user coordinate from the
+coordinate list within the error limit set by the parameter \fImatch\fR
+then the new feature is entered in the feature list.  Up to a maximum
+number of features, set by the parameter \fImaxfeatures\fR, may be
+defined in this way.  A new user coordinate function is fit to all the
+located features.  Finally, the graph is redrawn in user coordinates
+with the additional features found from the coordinate list marked.
+
+The 'f' key fits a two dimensional function of the pixel coordinates
+and aperture number to the user coordinates.  The type of function and
+the orders are initially set with the parameters \fIfunction\fR,
+\fIxorder\fR, and \fIyorder\fR.  The value of the function for a
+particular pixel coordinate is called the function coordinate and each
+feature in the feature list has a function coordinate value.  The
+fitted function also is used to convert pixel coordinates to user
+coordinates in the graph.  Depending on the orders of the function
+four or more features are required covering at least two orders.
+A description of the dispersion function fitting is given the section
+ECHELLE DISPERSION FUNCTION FITTING.
+
+If a zero point shift is desired without changing the coordinate function
+the user may specify the coordinate of a point in the spectrum with
+the 's' key from which a shift is determined.  The 'g' key also
+determines a shift by minimizing the difference between the user
+coordinates and the fitted coordinates.  This is used when a previously
+determined coordinate function is applied to a new spectrum having
+fewer or poorer lines and only a zero point shift can reasonably be
+determined.  Note that the zero point shift is in user coordinates
+for the fundamental order.  The shift for any particular order is then
+the zero point shift divided by the order number.
+
+Features may be delete with the key 'd'.  All features are deleted when
+the 'a' key immediately precedes the delete key.  Deleting the features
+does not delete the coordinate function.  To delete both the features
+and the dispersion function the initialize key 'i' is used.  Note
+features deleted during dispersion function fitting also are removed
+from the feature list upon exiting the fitting package.
+
+It is common to transfer the feature identifications and coordinate
+function from one image to another.  When a new image without a
+database entry is examined, such as when going to the next image in the
+input list or selecting a new image with the ":image" command, the
+current feature list and coordinate function are kept.  Alternatively,
+a database record from a different image may be read with the ":read"
+command.  When transferring feature identifications between images the
+feature coordinates will not agree exactly with the new image feature
+positions and several options are available to reregister the feature
+positions.  The key 'c' centers the feature nearest the cursor using
+the current position as the starting point.  When preceded with the 'a'
+key all the features are recentered (the user must refit the coordinate
+function if desired).  As an aside, the recentering function is also
+useful when the parameters governing the feature centering algorithm
+are changed.
+
+The (c)entering function is applicable when the shift between the
+current and true feature positions is small.  Larger shifts may be
+determined automatically with the 'x' function which correlates
+features in the image with the feature list.  The features are then
+recentered.  A zero point shift may also be given interactively with
+the 's' key by using the cursor to indicate the coordinate of a point
+in the spectrum.  If there are no features then the shift is exactly as
+marked by the cursor but if there are features the approximate shift is
+applied and then the features are recentered.  The shift is then the
+mean shift of the features after recentering.  The shift is used as a
+zero point offset added to the dispersion function.  The shift is
+computed in user coordinates for the fundamental order.  Shifts for
+each order are given by scaling of this shift.
+
+In addition to the single keystroke commands there are commands
+initiated by the key ':' (colon commands).  As with the keystroke
+commands there are a number of standard graphics features available
+begining with ":." (type ":.help" for these commands).  The colon
+commands allow the task parameter values to be listed and to be reset
+within the task.  A parameter is listed by typing its name.  The colon
+command ":show" lists all the parameters.  A parameter value is reset
+by typing the parameter name followed by the new value; for example
+":match 10".  Other colon commands display the feature list
+(:features), control reading and writing records to the database (:read
+and :write), and set the graph display format.
+
+The feature identification process for an image is completed by typing
+'q' to quit.  Attempting to quit an image without explicitly recording
+changes in the feature database produces a warning message and an
+opportunity to record the information in the database.  As an immediate
+exit the 'I' interrupt key may be used.  This does not save the feature
+information.
+.ih
+ECHELLE DISPERSION FUNCTION FITTING
+If a minimum of four features over at least two orders, depending on
+the default function orders, have been identified a dispersion function
+relating the user coordinates to the extracted pixel coordinate and
+aperture number may be fit.  However, more features are preferable to
+determine changes in the dispersion as a function of position and
+order.
+
+The form of the function fit explicitly includes the basic order number
+dependence of echelle spectra; namely the wavelength of a particular
+point along the dispersion direction in different orders varies as the
+reciprocal of the order number.  Because of distortions, the differing
+extraction paths through the two dimensional image, and rotations of
+the spectra relative to the axis of constant dispersion (i.e. aligning
+the orders with the image columns or lines instead of aligning the
+emission and absorption features) there will be residual dependancies on
+the extracted pixel positions and orders.  These residual dependancies
+are fit by a two dimensional polynomial of arbitrary order including
+cross terms.  Because the basic order number dependence has been
+removed the orders should be relatively low.  Currently the functions
+are bi-dimensional chebyshev and legendre polynomials though other
+function may be added in the future.
+
+Since the true order number may not be known initially a linear
+relation between the aperture numbers and the order numbers is also
+determined which minimizes the residuals.  This relation allows an
+unknown offset and possible a reversed direction of increasing order.
+The fitted function is then represented as:
+
+.nf
+		y = offset +/- aperture
+
+		wavelength = f (x, y) / y
+.fi
+
+where y is the order number and x is the extracted pixel coordinate along the
+dispersion.
+ 
+If the order offset is known initially or as a result of previous the 'o'
+fit may be used.  The dispersion minimization for the order offset is
+then not done.  This will, therefore, be faster than using the full
+fit, key 'f', to also determine the order offset.
+
+The fitting is done interactively as a submode of \fBecidentify\fR with its
+own set of cursor commands.  It is entered using the 'f' key and exited using
+the 'q' key.  The list of commands is given the CURSOR KEY section and is
+available from the fitting mode with '?'.  The functionality of this fitting
+is fairly simple; the function and orders may be changed, points may be deleted
+and undeleted, and the results of the fit may be displayed in various formats
+by selecting quantities to be plotted along either axis.  Generally one
+changes plotting of the pixel coordinate, order number, and wavelength
+along the x axis and residuals or radial velocity errors along the y axis.
+One switches between increasing the x order and the y order while switching
+between plotting verses x positions and order number until the residuals
+have been reduced to remove all systematic trends.
+.ih
+DATABASE RECORDS
+The database specified by the parameter \fIdatabase\fR is a directory of
+simple text files.  The text files have names beginning with 'ec' followed
+by the entry name, usually the name of the image.  The database text files
+consist of a number of records.  A record begins with a line starting with the
+keyword "begin".  The rest of the line is the record identifier.  Records
+read and written by \fBecidentify\fR have "ecidentify" as the first word of the
+identifier.  Following this is a name which may be specified following the
+":read" or ":write" commands.  If no name is specified then the image name
+is used.  The lines following the record identifier contain
+the feature information and dispersion function coefficients.
+.ih
+ECHELLE DISPERSION FUNCTIONS
+The fitted echelle dispersion functions are evaluated as described in
+this section.  The basic equations are
+
+.nf
+    (1)  w = (f(x,o) + shift) / o
+    (2)  o = ap * slope + offset
+.fi
+
+where w is the wavelength, x is the pixel coordinate along the order, o is
+the order, and ap is the aperture number.  The database parameter "shift"
+provides a wavelength zero point shift and the parameters "slope" and
+"offset" provide the transformation between aperture number and order.
+Note that the function f(x,o) and the shift are in terms of first order
+wavelengths.
+
+The database entries contain "parameter value" pairs.  This includes the
+parameters "shift", "offset", and "slope" defined above.  The default
+values for these if they are absent are 0, 0, and 1 respectively.  The
+"coefficients" parameter specifies the number of coefficients that follow
+and define the first order wavelength dispersion function.  The
+coefficients and functions are described below.
+
+The numerical values following the "coefficients" parameter, shown in
+the order in which they appear, have the following meaning.
+
+.nf
+    type	Function type: 1=chebychev, 2=legendre
+    xpow	Highest power of x
+    opow	Highest power of o
+    xterms	Type of cross terms: Always 1 for echelle functions
+    xmin	Minimum x for normalization
+    xmax	Maximum x for normalization
+    omin	Minimum o for normalization
+    omax	Maximum o for normalization
+    Cmn		Coefficients: m=0-xpow, n=0-opow, m varies first
+.fi
+
+The functions are evaluated by a sum over m and n up to the specified
+highest powers.
+
+.nf
+    (3)  f(x,o) = sum {Cmn * Pm * Pn}	m=0-xpow, n=0-opow
+.fi
+
+The Cmn are the coefficients of the polynomial terms Pm and Pn which
+are defined as follows.
+
+.nf
+    Chebyshev:
+	xnorm = (2 * x - (xmax + xmin)) / (xmax - xmin)
+	P0 = 1.0
+	P1 = xnorm
+	Pm+1 = 2.0 * xnorm * Pm - Pm-1 
+
+	onorm = (2 * o - (omax + omin)) / (omax - omin)
+	P0 = 1.0
+	P1 = onorm
+	Pn+1 = 2.0 * onorm * Pn - Pn-1 
+
+    Legendre:
+	xnorm = (2 * x - (xmax + xmin)) / (xmax - xmin)
+	P0 = 1.0
+	P1 = xnorm
+	Pm+1 = ((2m + 1) * xnorm * Pm - m * Pm-1)/ (m + 1)   
+
+	onorm = (2 * o - (omax + omin)) / (omax - omin)
+	P0 = 1.0
+	P1 = onorm
+	Pn+1 = ((2n + 1) * onorm * Pn - n * Pn-1)/ (n + 1)   
+.fi
+
+Note that the polynomial terms are obtained by first normalizing the x and
+o values to the range -1 to 1 and then iteratively evaluating them.
+.ih
+EXAMPLES
+Because this task is interactive it is difficult to provide an actual
+example.  The following describes a typical usage on arc spectra.
+
+	cl> ecidentify arc1.ec,arc2.ec
+
+.ls (1)
+The database is searched for an entry for arc1.ec.  None is found and
+the first order is plotted as a function of pixel coordinate.
+.le
+.ls (2)
+Using a line identification chart or vast experience one of the
+emission lines is identified and marked with the 'm' key.  Using the
+cursor position a center is found by the centering algorithm.  The
+aperture number, pixel position, wavelength (which is currently the
+same as the pixel position), and a prompt for the true value with the
+default value INDEF is printed.  The true wavelength is typed in and the
+status line is redrawn with the information for the feature.
+.le
+.ls (3)
+The orders are changed with the 'j', 'k', or 'o' key and further lines are
+identified with the 'm' key.
+.le
+.ls (4)
+After a number of lines have been marked spanning the full range of the orders
+and pixel coordinates the key 'l' is typed.  The program now fits a preliminary
+dispersion solution using the current function and function orders.  Using this
+function it examines each line in the line list and checks to see if there is
+an emission line at that point.  With many orders and lots of lines this may
+take some time.  After additional lines have been identified (up to
+\fImaxfeatures\fR lines) the function is refit.  Finally the current order
+is regraphed in user coordinates.
+.le
+.ls (5)
+Again we look at some orders and see if the automatic line identifications
+make sense.
+.le
+.ls (6)
+We next enter the dispersion function fitting mode with 'f'.  A plot of the
+residuals vs. pixel position is drawn.  Some obvious misidentifications may
+be deleted with the 'd' key.  One way to proceed with determining the
+function orders is to start at the lowest orders (xorder = 2 for linear
+and yorder = 1 for no order dependence beyond the basic dependence).  We then
+increase each order one at a time.  The x axis is changed between order
+number and pixel position using the 'x' key to see the dependence on each
+dimension.  The orders are increased until there are no systematic trends
+apparent.  Normally the y order (for the aperture or order number dependence)
+is low such as 2 to 4 while the x order (for the dispersion direction) is
+whatever is needed to account for distortions.  Also one can prune deviant
+points with the 'd' key.  Note that the order offset derived from the
+aperture number is given in the title block along with the RMS.  When done
+we exit with 'q'.
+.le
+.ls (7)
+The new function fit is then evaluated for all orders and the current order
+is redrawn based on the new dispersion.  Note also that the status line
+information for the current feature has both the fitted wavelength and the
+user identified wavelength.  We can add or delete lines and iterate with the
+fitting until we are happy with the feature list and dispersion function.
+.le
+.ls (8)
+Typing 'q' exits the graph and prints a query about saving the information
+in the database.  We answer yes to this query.  Note that information can
+also be saved while still in the graphics loop using ":write".
+.le
+.ls (9)
+The next image in the list is then graphed but the last dispersion solution
+and feature list is maintained.  If the shift is small for the new arc we
+type 'a' 'c' to recenter all the features.  This does not refit the dispersion
+automatically so we then do 'f'.  Alternatively, we could use the 's' or 'x'
+keys to determine a large shift and do the recentering.
+.le
+.ls (10)
+Finally we can exit with 'q' or examine further images with the ":image"
+command.
+.le
+.ih
+REVISIONS
+.ls ECIDENTIFY V2.11
+The dispersion units are now determined from a user parameter,
+the coordinate list, or the database entry.
+.le
+.ih
+SEE ALSO
+apsum, center1d, gtools, ecreidentify, identify
+.endhelp
diff --git a/noao/imred/echelle/doc/ecreidentify.hlp b/noao/imred/echelle/doc/ecreidentify.hlp
new file mode 100644
index 00000000..53ab0f8c
--- /dev/null
+++ b/noao/imred/echelle/doc/ecreidentify.hlp
@@ -0,0 +1,117 @@
+.help ecreidentify Jun88 noao.imred.echelle
+.ih
+NAME
+ecreidentify -- Reidentify features in echelle spectra
+.ih
+USAGE
+ecreidentify images reference
+.ih
+PARAMETERS
+.ls images
+Echelle images in which the features in the reference image are to be
+reidentified and a new dispersion function fit.
+.le
+.ls reference
+Echelle image with previously identified features and dispersion
+function.
+.le
+.ls shift = 0.
+Shift in user coordinates to be added to the reference features before
+centering.  If INDEF then a shift is determined by correlating the
+reference features to features automatically identified in the image to
+be reidentified.
+.le
+.ls cradius = 5.
+Centering radius in pixels.  If a reidentified feature falls further
+than this distance from the reference position (after shifting) it is
+not reidentified.
+.le
+.ls threshold = 10.
+In order for a feature center to be determined the range of pixel
+intensities around the feature must exceed this threshold.
+.le
+.ls refit = yes
+Refit the dispersion function?  If yes and there are more than 4
+features in more than one order and a dispersion function was defined
+in the reference image then a new dispersion function of the same type
+and order offset
+as in the reference image is fit using the new pixel positions.
+Otherwise only a zero point shift is determined from the revised fitted
+coordinates without changing the form of the dispersion function.
+.le
+.ls database = "database"
+Database containing the feature data for the reference image and in
+which the features for the reidentified images are recorded.
+.le
+.ls logfiles = "STDOUT,logfile"
+List of file in which to keep a processing log.  If a null file, "", is
+given then no log is kept.  If the log file is "STDOUT" then the log is
+written to the terminal.
+.le
+.ih
+DESCRIPTION
+Emission or absorption features in a reference echelle spectrum are
+reidentified in other echelle spectra.  The features for the reference
+image and those determined for reidentified images are recorded in the
+specified database.
+
+The first step in transferring identifications from the reference
+spectrum to another spectrum is to add a shift (in wavelength) to each
+feature in the reference image.  The shift is specified by the
+parameter \fIshift\fR.  This shift is for the fundamental order (order
+number 1) which is then applied to each order by dividing by the order
+number.  If the shift is specified as INDEF then a shift is determined
+by finding the peaks in the input spectrum and correlating these peaks
+against the feature in the reference spectrum.  This is the 'x'
+algorithm described in \fBecidentify\fR.
+
+After the shift has been added to move the reference features to near
+the input spectrum features these positions are adjusted by centering
+on the features using the \fBcenter1d\fR algorithm.  The parameters
+\fIcradius\fR and \fIthreshold\fR are used in this operation.  If the
+centering fails to find the feature within the centering radius
+(\fIcradius\fR) that feature is eliminated from the feature list.
+
+If the parameter \fIrefit\fR has the value "no" then the average shift
+in the feature positions is recorded as a zero point wavelength offset
+for the fundamental order without changing the shape of the dispersion
+function.  If the parameter has the value "yes" then the new feature
+positions are used to refit the dispersion function (of the same function
+type and orders).  The order offset is also maintained.
+
+Log information is written to the specified log files.  To log this to
+the terminal, called the standard output, use STDOUT.  The log
+information includes reference spectrum, the spectrum being reidentified,
+the number of initial features and the number actually reidentified,
+the average shift in pixels, the average shift in wavelength (in terms
+of the fundamental order), the average fractional shift in wavelength
+(which can be scaled to a radial velocity), and the RMS of the features
+wavelengths given by the dispersion function to the user specified true
+wavelengths.
+.ih
+EXAMPLES
+The features in the spectrum f033.ec were identified previously
+with the task \fBecidentify\fR.  The features positions in f043.ec are
+are reidentified with and without refitting the dispersion function as
+follows:
+
+.nf
+ec> ecreidentify f043.ec f033.ec
+
+ECREIDENTIFY: NOAO/IRAF V2.7 seaman@puppis Mon 09:03:51 27-Jun-88
+  Reference image = f033.ec, Refit = yes
+               Image    Found  Pix Shift  User Shift  Z Shift      RMS
+             f043.ec  561/561       0.11       -1.07  -1.9E-6   0.0117
+
+
+ec> ecreidentify f043.ec f033.ec refit=no
+
+ECREIDENTIFY: NOAO/IRAF V2.7 seaman@puppis Mon 09:15:21 27-Jun-88
+  Reference image = f033.ec, Refit = no
+               Image    Found  Pix Shift  User Shift  Z Shift      RMS
+             f043.ec  561/561       0.11       -1.07  -1.9E-6   0.0131
+.fi
+.ih
+SEE ALSO
+center1d, ecidentify
+.endhelp
diff --git a/noao/imred/echelle/echelle.cl b/noao/imred/echelle/echelle.cl
new file mode 100644
index 00000000..c911c090
--- /dev/null
+++ b/noao/imred/echelle/echelle.cl
@@ -0,0 +1,82 @@
+#{ ECHELLE -- Echelle Spectral Reduction Package
+
+# Load necessary packages
+proto		# bscale
+
+# Increase header space for echelle format keywords
+s1 = envget ("min_lenuserarea")
+if (s1 == "")
+    reset min_lenuserarea = 100000
+else if (int (s1) < 100000)
+    reset min_lenuserarea = 100000
+
+package echelle
+
+# Ecslitproc and dofoe
+cl < doecslit$slittasks.cl
+cl < dofoe$dofoetasks.cl
+
+# Demos
+set	demos		= "echelle$demos/"
+task	demos		= "demos$demos.cl"
+
+# Onedspec tasks
+task	continuum,
+	deredden,
+	dispcor,
+	dopcor,
+	ecidentify,
+	ecreidentify,
+	refspectra,
+	sapertures,
+	sarith,
+	sflip,
+	slist,
+	specplot,
+	specshift,
+	splot		= "onedspec$x_onedspec.e"
+task	scombine	= "onedspec$scombine/x_scombine.e"
+task	bplot		= "onedspec$bplot.cl"
+task	scopy		= "onedspec$scopy.cl"
+task	dispcor1	= "onedspec$dispcor1.par"
+
+# Different default parameters
+task	calibrate,
+	sensfunc,
+	standard	= "echelle$x_onedspec.e"
+
+# Apextract tasks
+task	apall,
+	apedit,
+	apfind,
+	apfit,
+	apflatten,
+	apmask,
+	apnormalize,
+	aprecenter,
+	apresize,
+	apscatter,
+	apsum,
+	aptrace		= "apextract$x_apextract.e"
+task	apparams	= "apextract$apparams.par"
+task	apall1		= "apextract$apall1.par"
+task	apfit1		= "apextract$apfit1.par"
+task	apflat1		= "apextract$apflat1.par"
+task	apnorm1		= "apextract$apnorm1.par"
+task	apdefault	= "apextract$apdefault.par"
+task	apscat1		= "apextract$apscat1.par"
+task	apscat2		= "apextract$apscat2.par"
+
+# Astutil tasks
+task	setairmass,
+	setjd		= "astutil$x_astutil.e"
+
+# Hide tasks from the user
+hidetask apparams, apall1, apfit1, apflat1, apnorm1
+hidetask apscat1, apscat2, dispcor1
+
+# Set echelle extraction output
+apall.format = "echelle"
+apsum.format = "echelle"
+
+clbye
diff --git a/noao/imred/echelle/echelle.hd b/noao/imred/echelle/echelle.hd
new file mode 100644
index 00000000..b2f73fba
--- /dev/null
+++ b/noao/imred/echelle/echelle.hd
@@ -0,0 +1,11 @@
+# Help directory for the ECHELLE package.
+
+$doc	=	"./doc/"
+
+ecidentify	hlp=doc$ecidentify.hlp
+ecreidentify	hlp=doc$ecreidentify.hlp
+
+doecslit	hlp=doc$doecslit.hlp
+dofoe		hlp=doc$dofoe.hlp
+
+revisions	sys=Revisions
diff --git a/noao/imred/echelle/echelle.men b/noao/imred/echelle/echelle.men
new file mode 100644
index 00000000..c6e94618
--- /dev/null
+++ b/noao/imred/echelle/echelle.men
@@ -0,0 +1,40 @@
+          apall - Extract 1D spectra (all parameters in one task)
+      apdefault - Set the default aperture parameters and apidtable
+         apedit - Edit apertures interactively
+	 apfind - Automatically find spectra and define apertures
+	  apfit - Fit 2D spectra and output the fit, difference, or ratio
+      apflatten - Remove overall spectral and profile shapes from flat fields
+         apmask - Create and IRAF pixel list mask of the apertures
+    apnormalize - Normalize 2D apertures by 1D functions
+     aprecenter - Recenter apertures
+       apresize - Resize apertures
+      apscatter - Fit and subtract scattered light
+          apsum - Extract 1D spectra
+	aptrace - Trace positions of spectra
+
+          bplot - Batch plots of spectra
+      calibrate - Apply extinction and flux calibrations to spectra
+      continuum - Fit the continuum in spectra
+       deredden - Apply interstellar extinction corrections
+        dispcor - Dispersion correct spectra
+	 dopcor - Doppler correct spectra
+     ecidentify - Identify features in spectrum for dispersion solution
+   ecreidentify - Automatically identify features in spectra
+     refspectra - Assign wavelength reference spectra to other spectra
+     sapertures - Set or change aperture header information
+	 sarith - Spectrum arithmetic
+       scombine - Combine spectra
+          scopy - Select and copy apertures in different spectral formats
+       sensfunc - Create sensitivity function
+     setairmass - Compute effective airmass and middle UT for an exposure
+          setjd - Compute and set Julian dates in images
+	  sflip - Flip data and/or dispersion coordinates in spectra
+          slist - List spectrum header parameters
+       specplot - Stack and plot multiple spectra
+      specshift - Shift spectral dispersion coordinate systems
+          splot - Preliminary spectral plot/analysis
+       standard - Identify standard stars to be used in sensitivity calc
+
+       doecslit - Process Echelle slit spectra
+	  dofoe - Process Fiber Optic Echelle (FOE) spectra
+	  demos - Demonstrations and tests
diff --git a/noao/imred/echelle/echelle.par b/noao/imred/echelle/echelle.par
new file mode 100644
index 00000000..679bcb86
--- /dev/null
+++ b/noao/imred/echelle/echelle.par
@@ -0,0 +1,15 @@
+# ECHELLE SPECTRAL REDUCTION PACKAGE
+extinction,s,h,onedstds$kpnoextinct.dat,,,Extinction file
+caldir,s,h,,,,Standard star calibration directory
+observatory,s,h,"observatory",,,Observatory of data
+interp,s,h,"poly5","nearest|linear|poly3|poly5|spline3|sinc",,Interpolation type
+dispaxis,i,h,2,1,3,Image axis for 2D/3D images
+nsum,s,h,"1",,,"Number of lines/columns/bands to sum for 2D/3D images
+"
+database,f,h,"database",,,Database
+verbose,b,h,no,,,Verbose output?
+logfile,s,h,"logfile",,,Text log file
+plotfile,s,h,"",,,"Plot file
+"
+records,s,h,"",,,Record number extensions
+version,s,h,"ECHELLE V3: July 1991"
diff --git a/noao/imred/echelle/sensfunc.par b/noao/imred/echelle/sensfunc.par
new file mode 100644
index 00000000..cd80efbe
--- /dev/null
+++ b/noao/imred/echelle/sensfunc.par
@@ -0,0 +1,17 @@
+standards,s,a,std,,,Input standard star data file (from STANDARD)
+sensitivity,s,a,"sens",,,Output root sensitivity function imagename
+apertures,s,h,"",,,Aperture selection list
+ignoreaps,b,h,no,,,Ignore apertures and make one sensitivity function?
+logfile,f,h,"logfile",,,Output log for statistics information
+extinction,f,h,)_.extinction,,,Extinction file
+newextinction,f,h,"extinct.dat",,,Output revised extinction file
+observatory,s,h,)_.observatory,,,Observatory of data
+function,s,h,"spline3","chebyshev|legendre|spline3|spline1",,Fitting function
+order,i,h,6,1,,Order of fit
+interactive,b,h,yes,,,Determine sensitivity function interactively?
+graphs,s,h,"sr",,,Graphs per frame
+marks,s,h,"plus cross box",,,Data mark types (marks deleted added)
+colors,s,h,"2 1 3 4",,,Colors (lines marks deleted added)
+cursor,*gcur,h,"",,,Graphics cursor input
+device,s,h,"stdgraph",,,Graphics output device
+answer,s,q, yes,"no|yes|NO|YES",,"(no|yes|NO|YES)"
diff --git a/noao/imred/echelle/standard.par b/noao/imred/echelle/standard.par
new file mode 100644
index 00000000..99b98877
--- /dev/null
+++ b/noao/imred/echelle/standard.par
@@ -0,0 +1,21 @@
+input,f,a,,,,Input image file root name
+output,s,a,std,,,Output flux file (used by SENSFUNC)
+samestar,b,h,yes,,,Same star in all apertures?
+beam_switch,b,h,no,,,Beam switch spectra?
+apertures,s,h,"",,,Aperture selection list
+bandwidth,r,h,INDEF,,,Bandpass widths
+bandsep,r,h,INDEF,,,Bandpass separation
+fnuzero,r,h,3.68e-20,,,Absolute flux zero point
+extinction,s,h,)_.extinction,,,Extinction file
+caldir,s,h,)_.caldir,,,Directory containing calibration data
+observatory,s,h,)_.observatory,,,Observatory for data
+interact,b,h,yes,,,Graphic interaction to define new bandpasses
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+star_name,s,q,,,,Star name in calibration list
+airmass,r,q,,1.,,Airmass
+exptime,r,q,,,,Exposure time (seconds)
+mag,r,q,,,,Magnitude of star
+magband,s,q,,"U|B|V|R|I|J|H|K|L|Lprime|M",,"Magnitude type"
+teff,s,q,,,,Effective temperature or spectral type
+answer,s,q,no,,,"(no|yes|NO|YES|NO!|YES!)"
diff --git a/noao/imred/generic/Revisions b/noao/imred/generic/Revisions
new file mode 100644
index 00000000..7ae1bfa5
--- /dev/null
+++ b/noao/imred/generic/Revisions
@@ -0,0 +1,220 @@
+.help revisions Jun88 noao.imred.generic
+.nf
+
+generic$generic.cl
+generic$generic.men
+generic$cosmicrays.par	-
+    Removed the cosmicrays task which is now in crutil.  (6/12/02, Valdes)
+
+=====
+V2.12
+=====
+
+generic$mkpkg
+    Added missing <error.h> dependency for flat1d.x  (12/13/01, MJF)
+
+generic$normalize.cl
+generic$normalize.par	-
+    Rewrote as modern cl procedure script with possiblity to extend to
+    MEF extensions.  (5/13/99, Valdes)
+
+generic$flatten.cl
+generic$normalize.cl
+    Changed use of FILES for image list expansion to SECTIONS.
+    (5/13/99, Valdes)
+
+=======
+V2.11.1
+=======
+
+generic$normalize.cl
+generic$normflat.cl
+    Added CCDMEAN = 1 to final image header.  (4/16/93, Valdes)
+
+generic$flat1d.x
+generic$doc/flat1d.hlp
+    CCDMEAN is set to 1.  (3/15/93, Valdes)
+
+=======
+V2.10.2
+=======
+=======
+V2.10.1
+=======
+=======
+V2.10.0
+=======
+=====
+V2.10
+=====
+generic$flatten.par
+    Changed the default values of the keeplog and logfile parameters from
+    ")_.keeplog" and ")_.logfile" to ")generic.keeplog" and ")generic.logfile" 
+    respectively. This change avoids a parameter redirection in the irred
+    package. (8/26/91 LED)
+
+generic$darksub.cl
+    Included all parameters in IMARITH calls due to complaint about title
+    being changed.  (12/9/91)
+
+====
+V2.9
+====
+
+generic$normalize.cl
+generic$normflat.cl
+generic$normalize.par
+generic$normflat.par
+    Modified use of IMSTATISTICS for additional fields parameter.  If the
+    user redefined the defaults for IMSTAT then NORMALIZE and NORMFLAT
+    will fail.  (11/30/89, Valdes)
+
+generic$flatten.par
+generic$normalize.par
+generic$normflat.par
+    Change parameter reference from )generic. to )_. to allow defining
+    tasks in other packages.
+
+generic$darksub.cl
+    The last change caused the nscan to have the wrong value causing an
+    improper error (exposure time for ... not found).  The value of nscan()
+    is now saved before scanning the output list which must be done before
+    any error breaks to avoid out of sync lists.  (7/1/88 Valdes)
+
+generic$darksub.cl
+    The fscan on the output list must immediately follow the fscan on the
+    input list to prevent the lists getting out of sync.  (2/4/88 Valdes)
+
+generic$cosmicrays.par	+
+generic$generic.cl
+generic$generic.men
+    Added link to COSMICRAY program in CCDRED. (12/11/87 Valdes)
+
+====
+V2.5
+====
+
+====
+V2.3
+====
+
+generic$flat1d.x:  Valdes, July 3, 1986
+    1.  FLAT1D modified to use new ICFIT package.
+
+=========================================
+STScI Pre-release and 1st SUN 2.3 Release
+=========================================
+
+generic$darksub.cl:  Valdes, April 8, 1986
+    1.  DARKSUB rewritten to use exposure times from the image headers and
+	to allow input and output images.
+
+===========
+Release 2.2
+===========
+
+From Valdes Feb 12, 1986:
+
+1.  The GENERIC package script was inadvertently defining CMDSTR which
+was moved to the SYSTEM package.  This caused MKSCRIPT to fail if
+and only if GENERIC was loaded.  This has now been fixed.
+------
+From Valdes Feb 10, 1986:
+
+1.  The scripts DARKSUB, NORMFLAT, and NORMALIZE have been changed so
+that calls to IMCOPY have VERBOSE=NO when dealing with temporary images.
+Previously, output from imcopy was being printed but, of course, the
+temporary image filenames were meaningless to the user.
+------
+From Valdes Nov 7, 1985:
+
+1.  The generally useful task MKSCRIPT has been moved to the system
+package.
+------
+From Valdes Nov 1, 1985:
+
+1.  A general image reduction tool for creating command scripts has
+been added.  The task is called MKSCRIPT.  See the help page for
+this task.  An improved version of this task may eventually replace
+MKSCRIPT as a system task.  (As a technical detail a hidden task CMDSTR
+used by MKSCRIPT has also been added)
+------
+From Valdes Oct 17, 1985:
+
+1.  Flat1d and background now allow averaging of image lines or columns
+when interactively setting the fitting parameters.  The syntax is
+"Fit line = 10 30"; i.e.  blank separated line or column numbers.  A
+single number selects just one line or column.  Be aware however, that
+the actual fitting of the image is still done on each column or line
+individually.
+
+2.  The zero line in the interactive curve fitting graphs has been removed.
+This zero line interfered with fitting data near zero.
+------
+From Valdes Oct 4, 1985:
+
+1.  Flat1d and background modified to allow lower and upper rejection
+limits and rejection iteration.  This means the parameter file has changed.
+------
+From Valdes Oct 1, 1985:
+
+1.  Task revisions renamed to revs.
+-----
+From Valdes on August 26, 1985:
+
+1.  Flat1d was modified to eliminate fitting of lines or columns in which
+all the data is below minflat.  Also if all the data is greater than minflat
+then the ratio is computed without checking each data point which is more
+efficient (particularly with the vector operators).  Thus, flat1d should
+be somewhat faster; particularly for applications like multi-slits where
+many parts of the data are less than minflat.
+
+------
+From Valdes on August 7, 1985:
+
+1.  Flat1d and background have new parameters to select the graphics
+output device and the graphics cursor input.
+
+2.  Flat1d and background (fit1d) have been recompiled to use the "improved"
+icfit and gtools packages.
+
+------
+From Valdes on July 26, 1985:
+
+1.  Help page available for flat1d.
+
+2.  Background has been modified to use new fit1d task.  It now does
+column backgrounds without transposes and allows image sections.
+
+------
+From Valdes on July 25, 1985:
+
+1.  A new task called flat1d replaces lineflat and colflat.  It is
+essentially the same as lineflat except for an extra parameter "axis"
+which selects the axis along which the 1D functions are to be fit.
+Axis 1 is lines and axis 2 is columns.  The advantages of this change are:
+
+	a.  Column fitting is done without transposing the image.
+	b.  The colflat script using image transpositions would not
+	    work the same as lineflat when used with sections.  Now
+	    it is possible to mosaic several flat fields as need with
+	    multiple slits or apertures.
+	c.  Because no transpose is needed and it is not a script
+	    flat1d should work faster than colflat.
+	d.  The prompts for interactive fitting are now correct when
+	    doing column fits.
+
+------
+From Valdes on July 23, 1985:
+
+1.  The task revisions has been added to page revisions to the generic
+package.  The intent is that each package will have a revisions task.
+Note that this means there may be multiple tasks named revisions loaded
+at one time.  Typing revisions alone will give the revisions for the
+current package.  To get the system revisions type system.revisions.
+
+2.  The tasks linebckgrnd and colbckgrnd have been combined into one
+task with the extra hidden parameter "axis".  With axis=1 the task
+is the same as linebckgrnd and with axis=2 the task is the same as
+colbckgrnd.
+.endhelp
diff --git a/noao/imred/generic/background.cl b/noao/imred/generic/background.cl
new file mode 100644
index 00000000..005703ed
--- /dev/null
+++ b/noao/imred/generic/background.cl
@@ -0,0 +1,6 @@
+#{ BACKGROUND -- Subtract a line or column background.
+
+fit1d (input, output, "difference", axis=axis, interactive=interactive,
+    sample=sample, naverage=naverage, function=function, order=order,
+    low_reject=low_reject, high_reject=high_reject, niterate=niterate,
+    grow=grow, graphics=graphics, cursor=cursor.p_filename)
diff --git a/noao/imred/generic/background.par b/noao/imred/generic/background.par
new file mode 100644
index 00000000..aa5c703a
--- /dev/null
+++ b/noao/imred/generic/background.par
@@ -0,0 +1,16 @@
+# BACKGROUND -- Subtract line or column background
+
+input,s,a,,,,Input images to be background subtracted
+output,s,a,,,,Output background subtracted images
+axis,i,h,1,1,2,Axis along which background is fit and subtracted
+interactive,b,h,yes,,,Set fitting parameters interactively?
+sample,s,h,"*",,,Sample of points to use in fit
+naverage,i,h,1,,,Number of points in sample averaging
+function,s,h,"chebyshev","spline3|legendre|chebyshev|spline1",,Fitting function
+order,i,h,1,1,,Order of fitting function
+low_reject,r,h,0.,0.,,Low rejection in sigma of fit
+high_reject,r,h,0.,0.,,High rejection in sigma of fit
+niterate,i,h,1,0,,Number of rejection iterations
+grow,r,h,0.,0.,,Rejection growing radius
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
diff --git a/noao/imred/generic/darksub.cl b/noao/imred/generic/darksub.cl
new file mode 100644
index 00000000..c4197c50
--- /dev/null
+++ b/noao/imred/generic/darksub.cl
@@ -0,0 +1,99 @@
+# DARKSUB -- Scale and subtract a dark count image.
+
+procedure darksub (input, output, darkimage)
+
+string	input		{prompt="Input images to be dark count subtracted"}
+string	output		{prompt="Output dark count subtracted images"}
+file	darkimage	{prompt="Dark count image"}
+
+string	exposure	{prompt="Header parameter for exposure times"}
+string	pixtype="1"	{prompt="Pixel type of final images"}
+bool	verbose=yes	{prompt="Verbose output?"}
+struct	*list1
+struct	*list2
+
+begin
+	file	darkim
+	file	dark
+	file	file1
+	file	file2
+	string	in
+	string	out
+	real	exp
+	real	expd
+	real	expi
+	int	stat
+
+	# Make temporary filenames.
+	dark = mktemp ("tmp")
+	file1 = mktemp ("tmp")
+	file2 = mktemp ("tmp")
+
+	# Determine exposure time of dark image.  Quit if no exposure time.
+	darkim = darkimage
+	hselect (darkim, exposure, yes, > file1)
+	list1 = file1
+	stat = fscan (list1, expd)
+	list1 = ""
+	delete (file1, verify=no)
+
+	if (stat == EOF || nscan() < 1)
+	    error (1, "Exposure time for " // darkim // " not found.")
+	if (expd == 0.)
+	    error (2, "Exposure time for " // darkim // " is zero.")
+	exp = expd
+
+	# Make a temporary image for the scaled dark.
+	imcopy (darkim, dark, verbose=no)
+
+	# Expand the list of input and output images in temporary files.
+	hselect (input, "$I,"//exposure, yes, > file1)
+	sections (output, option="root", > file2)
+
+	# Loop through the input and output images.
+	list1 = file1
+	list2 = file2
+	while (fscan (list1, in, expi) != EOF) {
+
+	    stat = nscan()
+
+	    # Check that the output list has not been exhausted.
+	    if (fscan (list2, out) == EOF) {
+		print ("  Output list exhausted before input list.")
+		break
+	    }
+
+	    # Check that there is an exposure time for the input image.
+	    if (stat < 2) {
+		print ("  Exposure time for ", in, " not found.")
+		next
+	    }
+	    if (expi == 0.) {
+		print ("  Exposure time for ", in, " is zero.")
+		next
+	    }
+
+	    # Print log output.
+	    if (verbose) {
+	        time ()
+		print ("  ", out, " = ", in, " - ", expi/expd, "* ", darkim)
+	    }
+
+	    # Scale the dark image if necessary.
+	    if (expi != exp) {
+		imarith (dark, "*", expi / exp, dark, title="", divzero=0.,
+    		    hparams="", pixtype="", calctype="", verbose=no, noact=no)
+		exp = expi
+	    }
+
+	    # Subtract the dark image from the input image.
+	    imarith (in, "-", dark, out, title="", divzero=0.,
+		hparams="", pixtype=pixtype, calctype=pixtype,
+		verbose=no, noact=no)
+	}
+
+	# Finish up.
+	imdelete (dark, verify=no)
+	delete (file1, verify=no)
+	delete (file2, verify=no)
+end
diff --git a/noao/imred/generic/doc/Spelldict b/noao/imred/generic/doc/Spelldict
new file mode 100644
index 00000000..bb9573fb
--- /dev/null
+++ b/noao/imred/generic/doc/Spelldict
@@ -0,0 +1,51 @@
+Chebyshev
+INDEF
+IRAF
+Oct84
+RMS
+Sep84
+biasimage
+biassub
+ccd
+chebyshev
+chimage.section
+chimages
+chimages.section
+chimages.transpose
+colbckgrnd
+colflat
+darkimage
+darksub
+datatype
+dcbias
+dcbias.bias
+dcbias.trim
+div
+elp
+expdark
+expimage
+flatfield
+fliplines
+frame1
+frame2
+frame3
+images.imcopy
+imarith
+imcopy
+imlinefit
+imred.keeplog
+imred.logfile
+imstatistics
+imtranspose
+legendre
+linebckgrnd
+lineflat
+min
+minflat
+ndhelp
+ngrow
+normflat
+pixtype
+spline3
+trim.section
+
diff --git a/noao/imred/generic/doc/background.hlp b/noao/imred/generic/doc/background.hlp
new file mode 100644
index 00000000..7fa1fdd6
--- /dev/null
+++ b/noao/imred/generic/doc/background.hlp
@@ -0,0 +1,82 @@
+.help background Jul85 noao.imred.generic
+.ih
+NAME
+background -- Fit and subtract a line or column background
+.ih
+USAGE	
+background input output
+.ih
+PARAMETERS
+.ls input
+Images to be background subtracted.  The images may contain image sections.
+.le
+.ls output
+Output images to be created and modified.  The number of output images must
+match the number of input images.
+.le
+.ls axis = 1
+Axis along which to fit the background and subtract.  Axis 1 fits and
+subtracts the background along the lines and axis 2 fits and subtracts
+the background along the columns.
+.le
+.ls interactive = yes
+Set the fitting parameters interactively?
+.le
+.ls sample = "*"
+Lines or columns to be used in the background fits.  The default "*" selects
+all lines or columns.
+.le
+.ls naverage = 1
+Number of sample points to combined to create a fitting point.
+A positive value specifies an average and a negative value specifies
+a median.
+.le
+.ls function = spline3
+Function to be fit to the image lines or columns.  The functions are
+"legendre" (legendre polynomial), "chebyshev" (chebyshev polynomial),
+"spline1" (linear spline), and "spline3" (cubic spline).  The functions
+may be abbreviated.
+.le
+.ls order = 1
+The order of the polynomials or the number of spline pieces.
+.le
+.ls low_reject = 0., high_reject = 0.
+Low and high rejection limits in units of the residual sigma.
+.le
+.ls niterate = 1
+Number of rejection iterations.
+.le
+.ls grow = 1.
+When a pixel is rejected, pixels within this distance of the rejected pixel
+are also rejected.
+.le
+.ls graphics = "stdgraph"
+Graphics device for interactive graphics output.
+.le
+.ls cursor = ""
+Graphics cursor input
+.le
+.ih
+DESCRIPTION
+For each line or column in the input images a function is fit to the columns
+or lines specified by the sample parameter.  This function is then subtracted
+from the entire line or column to create an output line or column.
+The function fitting parameters may be set interactively.
+This task is a script using \fBfit1d\fR.  For more discussion about
+the parameters see the help text for \fBicfit\fR and \fBfit1d\fR.
+.ih
+EXAMPLES
+A spectrum of an object runs down the center of a 500 x 500 image.  To
+subtract a constant background using columns 10 to 100 and 410 to 500:
+
+	cl> background image image sample="10:100,410:500"
+
+To subtract a quadratic background from the columns of an image in which
+the spectrum lies between lines 50 and 70:
+
+	cl> background image image axis=2 sample="1:40,80:120" o=3
+
+.ih
+SEE ALSO
+fit1d, icfit
+.endhelp
diff --git a/noao/imred/generic/doc/darksub.hlp b/noao/imred/generic/doc/darksub.hlp
new file mode 100644
index 00000000..c6349e03
--- /dev/null
+++ b/noao/imred/generic/doc/darksub.hlp
@@ -0,0 +1,60 @@
+.help darksub Apr86 noao.imred.generic
+.ih
+NAME
+darksub -- Scale and subtract a dark count image
+.ih
+USAGE	
+darksub input output darkimage
+.ih
+PARAMETERS
+.ls input
+List of input images from which to subtract the dark count image.
+.le
+.ls output
+List of output dark count subtracted images.  The output images may
+be the same as the input images.  The input and output image lists should
+contain the same number of images.
+.le
+.ls darkimage
+Dark count image to be scaled and subtracted from the input images.
+.le
+.ls exposure = ""
+Header parameter name from which to obtain the exposure times.
+.le
+.ls pixtype = "1"
+The pixel datatype of the dark subtracted images.  The default ("1")
+is the pixel datatype of the original image.  The other choices are
+"short", "integer", "long", "real", and "double".
+.le
+.ls verbose = yes
+Print log of operations performed.
+.le
+.ih
+DESCRIPTION
+The dark count image is scaled by the ratio of the input image exposure to the
+dark count image exposure and subtracted from each of the input images.
+The exposures are obtained from the image headers under the specified
+name.  The output images may have the same names as the input images.
+A temporary image is used for the scaled dark count image and the original
+image is not modified.  The pixel datatype of the output images is
+specified by the parameter \fIpixtype\fR.  The default ("1") uses the
+datatype of the input image.  A log of the operations performed may be
+printed on the standard output when the verbose options is specified.
+
+Note that this task can be used to subtract any type of image from a set
+of images in which the subtracted image must be scaled to a given exposure.
+.ih
+EXAMPLES
+To subtract the dark count image 'dark' from obs1, obs2, and obs3:
+
+.nf
+	cl> darksub obs1,obs2 obs1,obs2 dark exp="exposure"
+	Tue 18:50:56 08-Apr-86
+	  obs1 = obs1 - 5.0049997336067 * dark
+	Tue 18:51:05 08-Apr-86
+	  obs2 = obs2 - 5.009999733075 * dark
+.fi
+.ih
+SEE ALSO
+imarith
+.endhelp
diff --git a/noao/imred/generic/doc/flat1d.hlp b/noao/imred/generic/doc/flat1d.hlp
new file mode 100644
index 00000000..0f855828
--- /dev/null
+++ b/noao/imred/generic/doc/flat1d.hlp
@@ -0,0 +1,157 @@
+.help flat1d Mar93 noao.imred.generic
+.ih
+NAME
+flat1d -- Make flat fields by fitting a 1D function to the image
+.ih
+USAGE	
+flat1d input output
+.ih
+PARAMETERS
+.ls input
+Calibration images to be used to make the flat fields.  The images may
+contain image sections.  Only the region covered by the section will be
+modified in the output image.
+.le
+.ls output
+Flat field images to be created or modified.  The number of output images
+must match the number of input images.  If an output image does not exist
+it is first created and initialized to unit response.
+.le
+.ls axis = 1
+Axis along which the one dimensional fitting is done.  Axis 1 corresponds
+to fitting the image lines and axis 2 corresponds to fitting the columns.
+.le
+.ls interactive = yes
+Set the fitting parameters interactively?
+.le
+.ls sample = "*"
+Lines or columns to be used in the fits.
+.le
+.ls naverage = 1
+Number of sample points to combined to create a fitting point.
+A positive value specifies an average and a negative value specifies
+a median.
+.le
+.ls function = spline3
+Function to be fit to the image lines or columns.  The functions are
+"legendre" (legendre polynomial), "chebyshev" (chebyshev polynomial),
+"spline1" (linear spline), and "spline3" (cubic spline).  The functions
+may be abbreviated.
+.le
+.ls order = 1
+The order of the polynomials or the number of spline pieces.
+.le
+.ls low_reject = 2.5, high_reject = 2.5
+Low and high rejection limits in units of the residual sigma.
+.le
+.ls niterate = 1
+Number of rejection iterations.
+.le
+.ls grow = 1.
+When a pixel is rejected, pixels within this distance of the rejected pixel
+are also rejected.
+.le
+.ls minflat = 0.
+When the fitted value is less than the value of this parameter the flat
+field value is set to unity.
+.le
+.ls graphics = "stdgraph"
+Graphics device for interactive graphics output.
+.le
+.ls cursor = ""
+Graphics cursor input
+.le
+.ih
+DESCRIPTION
+Flat fields are created containing only the small scale variations in the
+calibration images.  The large scale variations in the images are modeled
+by fitting a function to each image line or column with deviant pixel rejection.
+The flat field values are obtained by taking the ratio of the image values
+to the function fit.  However, if the fitted value is less than the
+parameter \fIminflat\fR the flat field value is set to unity.
+
+The function fitting parameters may be set interactively when the interactive
+flag is set using the interactive curve fitting package \fBicfit\fR.
+The cursor mode commands for this package are described in a separate
+help entry under "icfit".  For two dimensional images the user is
+prompted for the sample line or column or a blank-separated range to be
+averaged and graphed.
+Note that the lines or columns are relative the input image section; for
+example line 1 is the first line of the image section and not the first
+line of the image.  Any number of lines or columns may be examined.
+When satisfied with the fit parameters the user
+responds with a carriage return to the line or column prompt.
+The function is then fit to all the lines or columns and the flat field
+ratios are determined.
+
+If the output image does not exist initially it is created with the same
+size as the input image \fIwithout\fR an image section and initialized
+to unit response.  Subsequently the flat field data modifies the pixel
+values in the output image.  Input image sections may be used to restrict
+the region in which the flat field response is determined leaving the
+rest of the output image unmodified.  This ability is particularly useful
+when dealing with multi-aperture data.
+
+This task is very similar to \fBfit1d\fR with the addition of the
+parameter \fIminflat\fR and the deletion of the parameter \fItype\fR
+which is always "ratio".
+.ih
+EXAMPLES
+1.  Create a flat field from the calibration image "quartz" with the
+spectrum running along the lines.  Exclude the first and last columns,
+use a spline fit of 25 pieces (a width of 32 pixels over 800 columns),
+and set grow to 4 pixels.
+
+.nf
+	cl> flat1d quartz flat order=25 sample="2:799" grow=4 \
+	>>> interactive=no
+
+			or
+
+	cl> flat1d quartz[2:799,*] flat order=25 grow=4 inter-
+.fi
+
+The fitting parameters may be set interactively in which case the fitting
+parameters need not be specified.  The command would be
+
+.nf
+	cl> flat1d quartz flat
+	quartz: Fit column = 1 10
+	quartz: Fit column =
+.fi
+
+The user selects sample columns to be fit interactively with the interactive
+curve fitting package.  When satisfied with the fit parameters
+respond with a carriage return to the prompt.  The function is then fit to
+all the columns and the flat field ratios are determined.
+
+2.  As an example for multi-slit spectra the locations of the slits are
+determined and a file containing the image sections is created.
+Since there must be the same number of output images another file
+containing the output images is also created.  For
+example the files might contain
+
+.nf
+	  File quartzs			File flats
+	_______________			__________
+	quartz[23:40,*]			   flat
+	quartz[55:61,*]			   flat
+	quartz[73:84,*]			   flat
+.fi
+
+A flat field for the slits is then obtained with the command
+
+	cl> flat1d @quartzs flats axis=2
+.ih
+REVISIONS
+.ls FLAT1D V2.10.3
+The image header keyword "CCDMEAN = 1." is now added or updated.
+.le
+.ih
+BUGS
+The creation of multi-slit files and the need for an equal number of
+repeated output files is annoying.  It will be worked on in the future.
+.ih
+SEE ALSO
+fit1d, icfit
+.endhelp
diff --git a/noao/imred/generic/doc/flatten.hlp b/noao/imred/generic/doc/flatten.hlp
new file mode 100644
index 00000000..0e35f647
--- /dev/null
+++ b/noao/imred/generic/doc/flatten.hlp
@@ -0,0 +1,42 @@
+.help flatten Sep84 noao.imred.generic
+.ih
+NAME
+flatten -- Flatten images by dividing by a flat field
+.ih
+USAGE	
+flatten images flatfield
+.ih
+PARAMETERS
+.ls images
+Images to be flattened.
+.le
+.ls flatfield
+Flat field image to be divided into the images.
+.le
+.ls minflat = INDEF
+All flat field pixels less than or equal to this value are replaced by
+unit response.  If INDEF all the flat field pixels are used.
+.le
+.ls pixtype = "real"
+The pixel datatype of the flattened image.  The null string ("") defaults
+the pixel datatype to that of the original image before flattening.
+The other choices are "short", "integer", "long", and "real".
+.le
+.ih
+DESCRIPTION
+Each of the \fIimages\fR is flatten by dividing by the \fIflatfield\fR
+flat field image.  The flattened images replace the original images.
+The pixel datatype of the flattened images is specified by the
+\fIpixtype\fR.  The null string ("") leaves the datatype of the images
+unchanged.  Low values in the flat field may be replaced by unit response
+by specifying a \fIminflat\fR value.  All pixels in the flat field less
+than or equal to \fIminflat\fR are given unit response.
+.ih
+EXAMPLES
+To flatten a set of two dimensional images excluding pixels below
+.2 in the flat field:
+
+.nf
+	cl> flatten frame* flat minflat=0.2
+.fi
+.endhelp
diff --git a/noao/imred/generic/doc/normalize.hlp b/noao/imred/generic/doc/normalize.hlp
new file mode 100644
index 00000000..f5fb80f7
--- /dev/null
+++ b/noao/imred/generic/doc/normalize.hlp
@@ -0,0 +1,45 @@
+.help normalize Sep84 noao.imred.generic
+.ih
+NAME
+normalize -- Normalize images
+.ih
+USAGE	
+normalize images
+.ih
+PARAMETERS
+.ls images
+Images to be normalized.
+.le
+.ls norm = INDEF
+Normalization factor to be used if not INDEF.  If INDEF the normalization
+factor is determined by sampling the images.
+.le
+.ls sample_section = "[]"
+Section of the image to be sampled in determining the image mean.
+.le
+.ls lower = INDEF
+Lower limit of pixel values for calculating the normalization.
+INDEF corresponds to the minimum possible pixel value.
+.le
+.ls upper = INDEF
+Upper limit of pixel values for calculating the normalization.
+INDEF corresponds to the maximum possible pixel value.
+.le
+.ih
+DESCRIPTION
+Each of the images is normalized.  The normalization is specified by the
+parameter \fInorm\fR.  If the value of \fInorm\fR is INDEF then a normalization
+is determined by sampling the image.  The normalization is then the mean
+of the pixels in the sample section with values in the range \fIlower\fR
+to \fIupper\fR.  The default sample section selects all pixels in the image.
+The normalized images are of datatype "real" and replace the original images.
+.ih
+EXAMPLES
+To normalize a set of two dimensional images excluding deviant pixels below
+1000 and above 5000 and subsampling every fifth pixel in each dimension:
+
+	cl> normalize frame* sample=[*:5,*:5] low=1000 up=5000
+.ih
+SEE ALSO
+imstatistics, normflat
+.endhelp
diff --git a/noao/imred/generic/doc/normflat.hlp b/noao/imred/generic/doc/normflat.hlp
new file mode 100644
index 00000000..3020d296
--- /dev/null
+++ b/noao/imred/generic/doc/normflat.hlp
@@ -0,0 +1,54 @@
+.help normflat Sep84 noao.imred.generic
+.ih
+NAME
+normflat -- Create a flat field by normalizing a calibration image
+.ih
+USAGE	
+normflat image flatfield
+.ih
+PARAMETERS
+.ls image
+Calibration image to be used.
+.le
+.ls flatfield
+Flat field to be created.
+.le
+.ls norm = INDEF
+Normalization factor to be used if not INDEF.  If INDEF the normalization
+factor is automatically determined.
+.le
+.ls minflat = INDEF
+Minimum data value to be used in determining the normalization and in
+creating the flat field.  Values less than or equal to this value are
+replaced with a flat field value of 1.
+.le
+.ls sample_section = "[]"
+Section of the image to be sampled in determining the normalization if
+norm = INDEF.
+.le
+.ih
+DESCRIPTION
+A flat field is created from a calibration image by normalizing the calibration
+image.  The normalization is specified with the parameter \fInorm\fR.  If the
+value of \fInorm\fR is INDEF then the normalization is determined by sampling
+the pixels in the sample section with values greater than \fIminflat\fR.
+This task differs from the task \fBnormalize\fR in that data values less
+than or equal to \fIminflat\fR are replaced with unity in the normalized
+flat field.
+.ih
+EXAMPLES
+To create a flat field from a calibration image "quartz" using pixels
+above 1000 and selecting the normalization to be 3500:
+
+	cl> normflat quartz flat norm=3500 minflat=1000
+
+To determine a normalization from the pixels above 1000 and sampling
+every fifth pixel in each dimension:
+
+.nf
+	cl> normflat quartz flat minflat=1000 sample=[*:5,*:5]
+.fi
+.ih
+SEE ALSO
+normalize
+.endhelp
diff --git a/noao/imred/generic/flat1d.par b/noao/imred/generic/flat1d.par
new file mode 100644
index 00000000..90e0ad3d
--- /dev/null
+++ b/noao/imred/generic/flat1d.par
@@ -0,0 +1,17 @@
+# FLAT1D -- Make flat fields by fitting a function to the image line or cols.
+
+input,s,a,,,,Calibration images
+output,s,a,,,,Flat field images
+axis,i,h,1,1,2,Axis to fit
+interactive,b,h,yes,,,Set fitting parameters interactively?
+sample,s,h,"*",,,Sample points to use in fit
+naverage,i,h,1,,,Number of points in sample averaging
+function,s,h,"spline3","spline3|legendre|chebyshev|spline1",,Fitting function
+order,i,h,1,1,,Order of fitting function
+low_reject,r,h,2.5,0.,,Low rejection in sigma of fit
+high_reject,r,h,2.5,0.,,High rejection in sigma of fit
+niterate,i,h,1,0,,Number of rejection iterations
+grow,r,h,1.,0.,,Rejection growing radius in pixels
+minflat,r,h,0.,,,Minimum fit value for computing a flat field value
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
diff --git a/noao/imred/generic/flat1d.x b/noao/imred/generic/flat1d.x
new file mode 100644
index 00000000..5a0797fc
--- /dev/null
+++ b/noao/imred/generic/flat1d.x
@@ -0,0 +1,478 @@
+include	<error.h>
+include	<imhdr.h>
+include <pkg/gtools.h>
+
+# FLAT1D -- Fit a function to image lines or columns and output an image
+# consisting of the ratio.  Set a minimum value test to the denominator.
+# The fitting parameters may be set interactively using the icfit package.
+
+procedure flat1d ()
+
+int	listin				# Input image list
+int	listout				# Output image list
+int	axis				# Image axis to fit
+real	minflat				# Minimum fit value for ratio
+bool	interactive			# Interactive?
+
+char	sample[SZ_LINE]			# Sample ranges
+int	naverage			# Sample averaging size
+char	function[SZ_LINE]		# Curve fitting function
+int	order				# Order of curve fitting function
+real	low_reject,  high_reject	# Rejection thresholds
+int	niterate			# Number of rejection iterations
+real	grow				# Rejection growing radius
+
+char	input[SZ_LINE]			# Input image
+char	output[SZ_FNAME]		# Output image
+pointer	in, out				# IMIO pointers
+pointer	ic				# ICFIT pointer
+pointer	gt				# GTOOLS pointer
+
+int	imtopen(), imtgetim(), imtlen(), gt_init()
+int	clgeti()
+real	clgetr()
+bool	clgetb()
+
+begin
+	# Get input and output lists and check that the number of images
+	# are the same.
+
+	call clgstr ("input", input, SZ_LINE)
+	listin = imtopen (input)
+	call clgstr ("output", input, SZ_LINE)
+	listout = imtopen (input)
+	if (imtlen (listin) != imtlen (listout)) {
+	    call imtclose (listin)
+	    call imtclose (listout)
+	    call error (0, "Input and output image lists do not match")
+	}
+
+	# Get task parameters.
+
+	axis = clgeti ("axis")
+	minflat = clgetr ("minflat")
+	interactive = clgetb ("interactive")
+
+	# Initialize the ICFIT package.
+	call clgstr ("sample", sample, SZ_LINE)
+	naverage = clgeti ("naverage")
+	call clgstr ("function", function, SZ_LINE)
+	order = clgeti ("order")
+	low_reject = clgetr ("low_reject")
+	high_reject = clgetr ("high_reject")
+	niterate = clgeti ("niterate")
+	grow = clgetr ("grow")
+
+	call ic_open (ic)
+	call ic_pstr (ic, "sample", sample)
+	call ic_puti (ic, "naverage", naverage)
+	call ic_pstr (ic, "function", function)
+	call ic_puti (ic, "order", order)
+	call ic_putr (ic, "low", low_reject)
+	call ic_putr (ic, "high", high_reject)
+	call ic_puti (ic, "niterate", niterate)
+	call ic_putr (ic, "grow", grow)
+	call ic_pstr (ic, "ylabel", "")
+
+	gt = gt_init()
+	call gt_sets (gt, GTTYPE, "line")
+
+	# Fit each input image.
+
+	while ((imtgetim (listin, input, SZ_LINE) != EOF) &&
+	    (imtgetim (listout, output, SZ_FNAME) != EOF)) {
+
+	    iferr (call f1d_immap (input, output, in, out)) {
+		call erract (EA_WARN)
+		next
+	    }
+	    call f1d_flat1d (in, out, ic, gt, input, axis, minflat, interactive)
+	    call imunmap (in)
+	    call imunmap (out)
+	}
+
+	call ic_closer (ic)
+	call gt_free (gt)
+	call imtclose (listin)
+	call imtclose (listout)
+end
+
+
+# F1D_FLAT1D -- Given the image descriptor determine the fitting function
+# for each line or column and create an output image.  If the interactive flag
+# is set then set the fitting parameters interactively.
+
+define	MAXBUF	512 * 100		# Maximum number of pixels per block
+
+procedure f1d_flat1d (in, out, ic, gt, title, axis, minflat, interactive)
+
+pointer	in				# IMIO pointer for input image
+pointer	out				# IMIO pointer for output image
+pointer	ic				# ICFIT pointer
+pointer	gt				# GTOOLS pointer
+char	title[ARB]			# Title
+int	axis				# Image axis to fit
+real	minflat				# Minimum value for flat division
+bool	interactive			# Interactive?
+
+char	graphics[SZ_FNAME]
+int	i, nx, new
+real	mindata, maxdata
+pointer	cv, gp, sp, x, wts, indata, outdata
+
+int	f1d_getline(), f1d_getdata(), strlen()
+pointer	gopen()
+
+begin
+	# Error check.
+
+	if (IM_NDIM (in) > 2)
+	    call error (0, "Image dimensions > 2 are not implemented")
+	if (axis > IM_NDIM (in))
+	    call error (0, "Axis exceeds image dimension")
+
+	# Allocate memory for curve fitting.
+
+	nx = IM_LEN (in, axis)
+	call smark (sp)
+	call salloc (x, nx, TY_REAL)
+	call salloc (wts, nx, TY_REAL)
+
+	do i = 1, nx
+	    Memr[x+i-1] = i
+	call amovkr (1., Memr[wts], nx)
+
+	call ic_putr (ic, "xmin", Memr[x])
+	call ic_putr (ic, "xmax", Memr[x+nx-1])
+
+	# If the interactive flag is set then use icg_fit to set the
+	# fitting parameters.  Get_fitline returns EOF when the user
+	# is done.  The weights are reset since the user may delete
+	# points.
+
+	if (interactive) {
+	    call clgstr ("graphics", graphics, SZ_FNAME)
+	    gp = gopen (graphics, NEW_FILE, STDGRAPH)
+	    i = strlen (title)
+	    indata = NULL
+	    while (f1d_getline (ic, gt, in, axis, title, indata) != EOF) {
+		title[i + 1] = EOS
+	        call icg_fit (ic, gp, "cursor", gt, cv, Memr[x], Memr[indata],
+		    Memr[wts], nx)
+		call amovkr (1., Memr[wts], nx)
+	    }
+	    call gclose (gp)
+	}
+
+	# Loop through the input image and create an output image.
+
+	new = YES
+
+	while (f1d_getdata (in, out, axis, MAXBUF, indata, outdata) != EOF) {
+
+	    call alimr (Memr[indata], nx, mindata, maxdata)
+	    if (maxdata >= minflat) {
+	        call ic_fit (ic, cv, Memr[x], Memr[indata], Memr[wts],
+		    nx, new, YES, new, new)
+	        new = NO
+
+	        call cvvector (cv, Memr[x], Memr[outdata], nx)
+	    }
+
+	    call f1d_flat (Memr[indata], Memr[outdata], Memr[outdata], nx,
+		minflat, mindata, maxdata)
+	}
+
+	call imaddr (out, "ccdmean", 1.)
+
+	call cvfree (cv)
+	call sfree (sp)
+end
+
+
+# F1D_IMMAP -- Map images for flat1d.
+
+procedure f1d_immap (input, output, in, out)
+
+char	input[ARB]		# Input image
+char	output[ARB]		# Output image
+pointer	in			# Input IMIO pointer
+pointer	out			# Output IMIO pointer
+
+pointer	sp, root, sect, line, data
+
+int	access(), impnlr()
+pointer	immap()
+errchk	immap
+
+begin
+	# Get the root name and section of the input image.
+
+	call smark (sp)
+	call salloc (root, SZ_FNAME, TY_CHAR)
+	call salloc (sect, SZ_FNAME, TY_CHAR)
+
+	call get_root (input, Memc[root], SZ_FNAME)
+	call get_section (input, Memc[sect], SZ_FNAME)
+
+	# If the output image is not accessible then create it as a new copy
+	# of the full input image and initialize to unit response.
+
+	if (access (output, READ_WRITE, BINARY_FILE) == NO) {
+	    in = immap (Memc[root], READ_ONLY, 0)
+	    out = immap (output, NEW_COPY, in)
+	    IM_PIXTYPE(out) = TY_REAL
+
+	    call salloc (line, IM_MAXDIM, TY_LONG)
+	    call amovkl (long (1), Meml[line], IM_MAXDIM)
+	    while (impnlr (out, data, Meml[line]) != EOF)
+	        call amovkr (1., Memr[data], IM_LEN(out, 1))
+
+	    call imunmap (in)
+	    call imunmap (out)
+	}
+
+	# Map the input and output images.
+
+	in = immap (input, READ_ONLY, 0)
+
+	call sprintf (Memc[root], SZ_FNAME, "%s%s")
+	    call pargstr (output)
+	    call pargstr (Memc[sect])
+	out = immap (Memc[root], READ_WRITE, 0)
+
+	call sfree (sp)
+end
+
+
+# F1D_GETDATA -- Get a line of image data.
+
+int procedure f1d_getdata (in, out, axis, maxbuf, indata, outdata)
+
+pointer	in			# Input IMIO pointer
+pointer	out			# Output IMIO pointer
+int	axis			# Image axis
+int	maxbuf			# Maximum buffer size for column axis
+pointer	indata			# Input data pointer
+pointer	outdata			# Output data pointer
+
+int	i, index, last_index, col1, col2, nc, ncols, nlines, ncols_block
+pointer	inbuf, outbuf, ptr
+
+pointer	imgl1r(), impl1r(), imgl2r(), impl2r(), imgs2r(), imps2r()
+
+data	index/0/
+
+begin
+	# Increment to the next image vector.
+
+	index = index + 1
+
+	# Initialize for the first vector.
+
+	if (index == 1) {
+	    ncols = IM_LEN (in, 1)
+	    if (IM_NDIM (in) == 1)
+		nlines = 1
+	    else
+		nlines = IM_LEN (in, 2)
+
+	    switch (axis) {
+	    case 1:
+		last_index = nlines
+	    case 2:
+		last_index = ncols
+	        ncols_block = max (1, min (ncols, maxbuf / nlines))
+		col2 = 0
+
+	        call malloc (indata, nlines, TY_REAL)
+	        call malloc (outdata, nlines, TY_REAL)
+	    }
+	}
+
+	# Finish up if the last vector has been done.
+
+	if (index > last_index) {
+	    if (axis == 2) {
+	        ptr = outbuf + index - 1 - col1
+	        do i = 1, nlines {
+		    Memr[ptr] = Memr[outdata+i-1]
+		    ptr = ptr + nc
+	        }
+
+	        call mfree (indata, TY_REAL)
+	        call mfree (outdata, TY_REAL)
+	    }
+
+	    index = 0
+	    return (EOF)
+	}
+
+	# Get the next image vector.
+
+	switch (axis) {
+	case 1:
+	    if (IM_NDIM (in) == 1) {
+		indata = imgl1r (in)
+		outdata = impl1r (out)
+	    } else {
+		indata = imgl2r (in, index)
+		outdata = impl2r (out, index)
+	    }
+	case 2:
+	    if (index > 1) {
+		ptr = outbuf + index - 1 - col1
+		do i = 1, nlines {
+		    Memr[ptr] = Memr[outdata+i-1]
+		    ptr = ptr + nc
+		}
+	    }
+
+	    if (index > col2) {
+		col1 = col2 + 1
+		col2 = min (ncols, col1 + ncols_block - 1)
+		inbuf = imgs2r (in, col1, col2, 1, nlines)
+		outbuf = imps2r (out, col1, col2, 1, nlines)
+		nc = col2 - col1 + 1
+	    }
+
+	    ptr = inbuf + index - col1
+	    do i = 1, nlines {
+		Memr[indata+i-1] = Memr[ptr]
+		ptr = ptr + nc
+	    }
+	}
+	return (index)
+end
+
+# F1D_FLAT -- For the flat field values by ratioing the image data by the fit.
+# If the fit value is less than minflat then the ratio is set to 1.
+
+procedure f1d_flat (data, fit, flat, npts, minflat, mindata, maxdata)
+
+real	data[npts]		# Image data
+real	fit[npts]		# Fit to image data
+real	flat[npts]		# Ratio of image data to the fit
+int	npts			# Number of points
+real	minflat			# Minimum fit value for ratio
+real	mindata			# Minimum data value
+real	maxdata			# Maximum data value
+
+int	i
+
+begin
+	if (mindata >= minflat)
+	    call adivr (data, fit, flat, npts)
+
+	else if (maxdata < minflat)
+	    call amovkr (1., flat, npts)
+
+	else {
+	    do i = 1, npts {
+	        if (fit[i] < minflat)
+		    flat[i] = 1.
+	        else
+		    flat[i] = data[i] / fit[i]
+	    }
+	}
+end
+
+
+# F1D_GETLINE -- Get image data to be fit interactively.  Return EOF
+# when the user enters EOF or CR.  Default is 1 and the out of bounds
+# requests are silently limited to the nearest in edge.
+
+int procedure f1d_getline (ic, gt, im, axis, title, data)
+
+pointer	ic			# ICFIT pointer
+pointer	gt			# GTOOLS pointer
+pointer	im			# IMIO pointer
+int	axis			# Image axis
+char	title[ARB]		# Title
+pointer	data			# Image data
+
+char	line[SZ_LINE]
+int	i, j, stat, imlen
+pointer	x
+
+int	getline(), nscan()
+pointer	imgl1r()
+
+data	stat/EOF/
+
+begin
+	# If the image is one dimensional do not prompt.
+
+	if (IM_NDIM (im) == 1) {
+	    if (stat == EOF) {
+		call sprintf (title, SZ_LINE, "%s\n%s")
+	    	    call pargstr (title)
+	    	    call pargstr (IM_TITLE(im))
+		call gt_sets (gt, GTTITLE, title)
+		call mfree (data, TY_REAL)
+		call malloc (data, IM_LEN(im, 1), TY_REAL)
+		call amovr (Memr[imgl1r(im)], Memr[data], IM_LEN(im, 1))
+		stat = OK
+	    } else
+		stat = EOF
+
+	    return (stat)
+	}
+
+	# If the image is two dimensional prompt for the line or column.
+
+	switch (axis) {
+	case 1:
+	    imlen = IM_LEN (im, 2)
+	    call sprintf (title, SZ_LINE, "%s: Fit line =")
+	        call pargstr (title)
+	case 2:
+	    imlen = IM_LEN (im, 1)
+	    call sprintf (title, SZ_LINE, "%s: Fit column =")
+	        call pargstr (title)
+	}
+
+	call printf ("%s ")
+	    call pargstr (title)
+	call flush (STDOUT)
+
+	if (getline(STDIN, line) == EOF)
+	    return (EOF)
+
+	call sscan (line)
+	call gargi (i)
+	call gargi (j)
+
+	switch (nscan()) {
+	case 0:
+	    stat = EOF
+	    return (stat)
+	case 1:
+	    i = max (1, min (imlen, i))
+	    j = i
+	case 2:
+	    i = max (1, min (imlen, i))
+	    j = max (1, min (imlen, j))
+	}
+
+	call sprintf (title, SZ_LINE, "%s %d - %d\n%s")
+	    call pargstr (title)
+	    call pargi (i)
+	    call pargi (j)
+	    call pargstr (IM_TITLE(im))
+
+	call gt_sets (gt, GTTITLE, title)
+
+	switch (axis) {
+	case 1:
+	    call ic_pstr (ic, "xlabel", "Column")
+	    call xt_21imavg (im, axis, 1, IM_LEN(im, 1), i, j, x, data, imlen)
+	case 2:
+	    call ic_pstr (ic, "xlabel", "Line")
+	    call xt_21imavg (im, axis, i, j, 1, IM_LEN(im, 2), x, data, imlen)
+	}
+	call mfree (x, TY_REAL)
+
+	stat = OK
+	return (stat)
+end
diff --git a/noao/imred/generic/flatten.cl b/noao/imred/generic/flatten.cl
new file mode 100644
index 00000000..928e09b2
--- /dev/null
+++ b/noao/imred/generic/flatten.cl
@@ -0,0 +1,64 @@
+#{ FLATTEN -- Divide images by a flat field
+
+#images,s,a,,,,Images to be flattened
+#flatfield,f,a,,,,Flat field
+#minflat,r,h,INDEF,,,Minimum flat field value
+#pixtype,s,h,"real",,,Flattened image pixel datatype
+#keeplog,b,h,@generic.keeplog,,,Keep log of processing?
+#logfile,f,h,@generic.logfile,,,Log file
+#imlist,f,h
+#imfd,*s,h
+#input,f,h
+#flat,f,h
+#flt,f,h
+
+{
+	# Startup message.
+	if (keeplog) {
+	    time (>> logfile)
+	    print ("  FLATTEN: Flatten images.", >> logfile)
+	}
+
+	# Set temporary files.
+	imlist = mktemp ("tmp$ims")
+
+	# Replace low flat field values if needed.
+	flat = flatfield
+	if (minflat == INDEF)
+	    flt = flat
+	else {
+	    if (keeplog)
+		print ("  Minimum flat field value = ", minflat, >> logfile)
+	    flt = mktemp ("tmp$ims")
+	    imcopy (flat, flt, verbose=no)
+	    imreplace (flt, 1., upper=minflat)
+	}
+
+	# Generate image list.
+	sections (images, option="fullname", >imlist)
+	imfd = imlist
+
+	while (fscan (imfd, input) != EOF) {
+
+	    # Print output.
+	    if (keeplog) {
+	        time (>> logfile)
+	        print ("  Flatten ", input, " with ", flat, ".", >> logfile)
+	    }
+
+	    # Flatten the image with the flat field.  Replace the input
+	    # image by the flattened image.
+
+	    imarith (input, "/", flt, input, pixtype=pixtype, calctype="real")
+	}
+
+	if (minflat != INDEF)
+	    imdelete (flt, verify=no)
+	delete (imlist, verify=no)
+
+	# Ending message.
+	if (keeplog) {
+	    time (>> logfile)
+	    print ("  FLATTEN: Done.", >> logfile)
+	}
+}
diff --git a/noao/imred/generic/flatten.par b/noao/imred/generic/flatten.par
new file mode 100644
index 00000000..7eedfe58
--- /dev/null
+++ b/noao/imred/generic/flatten.par
@@ -0,0 +1,13 @@
+# FLATTEN -- Divide images by a flat field
+
+images,s,a,,,,Images to be flattened
+flatfield,f,a,,,,Flat field
+minflat,r,h,INDEF,,,Minimum flat field value
+pixtype,s,h,"real",,,Flattened image pixel datatype
+keeplog,b,h,)generic.keeplog,,,Keep log of processing?
+logfile,f,h,)generic.logfile,,,Log file
+imlist,f,h
+imfd,*s,h
+input,f,h
+flat,f,h
+flt,f,h
diff --git a/noao/imred/generic/generic.cl b/noao/imred/generic/generic.cl
new file mode 100644
index 00000000..8a187758
--- /dev/null
+++ b/noao/imred/generic/generic.cl
@@ -0,0 +1,17 @@
+#{ GENERIC -- Generic image reduction tools
+
+# Load dependent packages:
+images
+proto			# Task "imreplace"
+
+package generic
+
+task	flat1d		= generic$x_generic.e
+
+task	background	= generic$background.cl
+task	darksub		= generic$darksub.cl
+task	flatten		= generic$flatten.cl
+task	normalize	= generic$normalize.cl
+task	normflat	= generic$normflat.cl
+
+clbye()
diff --git a/noao/imred/generic/generic.hd b/noao/imred/generic/generic.hd
new file mode 100644
index 00000000..3464ed28
--- /dev/null
+++ b/noao/imred/generic/generic.hd
@@ -0,0 +1,11 @@
+# Help directory for the GENERIC package.
+
+$doc = "./doc/"
+
+background	hlp=doc$background.hlp,	src=background.cl
+darksub		hlp=doc$darksub.hlp,	src=darksub.cl
+flatten		hlp=doc$flatten.hlp,	src=flatten.cl
+flat1d		hlp=doc$flat1d.hlp,	src=flat1d.x
+normalize	hlp=doc$normalize.hlp,	src=normalize.cl
+normflat	hlp=doc$normflat.hlp,	src=normflat.cl
+revisions	sys=Revisions
diff --git a/noao/imred/generic/generic.men b/noao/imred/generic/generic.men
new file mode 100644
index 00000000..9241c0d7
--- /dev/null
+++ b/noao/imred/generic/generic.men
@@ -0,0 +1,6 @@
+     background - Fit and subtract a line or column background
+	darksub - Scale and subtract a dark count image
+         flat1d - Make flat field by fitting a 1D func. to the lines or columns
+        flatten - Flatten images using a flat field
+      normalize - Normalize images
+       normflat - Create a flat field by normalizing and replacing low values
diff --git a/noao/imred/generic/generic.par b/noao/imred/generic/generic.par
new file mode 100644
index 00000000..7c5c6b6c
--- /dev/null
+++ b/noao/imred/generic/generic.par
@@ -0,0 +1,5 @@
+# GENERIC package parameter file.
+
+keeplog,b,h,)imred.keeplog,,,Keep log of processing?
+logfile,f,h,)imred.logfile,,,Log file
+version,s,h,"May 1985"
diff --git a/noao/imred/generic/mkpkg b/noao/imred/generic/mkpkg
new file mode 100644
index 00000000..2c33031b
--- /dev/null
+++ b/noao/imred/generic/mkpkg
@@ -0,0 +1,54 @@
+# Make the GENERIC package.
+# Make the GENERIC package.
+
+$call	relink
+$exit
+
+update:
+	$call	relink
+	$call	install
+	;
+
+relink:
+	$update	libpkg.a
+	$call	generic
+	;
+
+install:
+	$move	x_generic.e noaobin$
+	;
+
+generic:
+	$omake	x_generic.x
+	$link	x_generic.o libpkg.a -lxtools -lcurfit
+	;
+
+libpkg.a:
+	flat1d.x	<imhdr.h> <pkg/gtools.h>
+	;
+
+$call	relink
+$exit
+
+update:
+	$call	relink
+	$call	install
+	;
+
+relink:
+	$update	libpkg.a
+	$call	generic
+	;
+
+install:
+	$move	x_generic.e noaobin$
+	;
+
+generic:
+	$omake	x_generic.x
+	$link	x_generic.o libpkg.a -lxtools -lcurfit
+	;
+
+libpkg.a:
+	flat1d.x	<imhdr.h> <pkg/gtools.h> <error.h>
+	;
diff --git a/noao/imred/generic/normalize.cl b/noao/imred/generic/normalize.cl
new file mode 100644
index 00000000..59290c1c
--- /dev/null
+++ b/noao/imred/generic/normalize.cl
@@ -0,0 +1,79 @@
+# NORMALIZE -- Compute the average of a sample region and normalize.
+
+procedure normalize (images)
+
+string	images			{prompt="Images to be normalized"}
+real	norm = INDEF		{prompt="Normalization value"}
+string	sample_section = "[]"	{prompt="Sample section"}
+real	lower = INDEF	{prompt="Lower limit of data values for sampling"}
+real	upper = INDEF	{prompt="Upper limit of data values for sampling"}
+bool	keeplog = ")_.keeplog"	{prompt="Keep log of processing?"}
+file	logfile = ")_.logfile"	{prompt="Log file"}
+
+struct	*imfd
+
+begin
+	file	imlist, input, tmp
+	real	mean
+	int	stat
+	bool	mef
+
+	mef = no
+
+	# Query parameters.
+	input = images
+
+	# Set temporary files.
+	imlist = mktemp ("tmp$ims")
+	tmp = mktemp ("tmp")
+
+	# Startup message.
+	if (keeplog) {
+	    time (>> logfile)
+	    print ("  NORMALIZE: Normalize images.", >> logfile)
+	}
+
+	# Generate image list.
+	sections (input, option="fullname", >imlist)
+
+	# Process list.
+	imfd = imlist
+	while (fscan (imfd, input) != EOF) {
+
+	    # Determine normalization.
+	    if (norm == INDEF) {
+	        # Determine the mean of the sample region.
+	        imstatistics (input // sample_section, fields="mean",
+		    lower=lower, upper=upper, format=no) | scan (mean)
+	    } else
+		mean = norm
+
+	    # Print output.
+	    if (keeplog) {
+		time (>> logfile)
+	        print ("  Normalization  for ", input, " = ", mean, >> logfile)
+	    }
+
+	    if (mean != 0.) {
+	        # Normalize the image by the mean.
+		if (mef) {
+		    imarith (input, "/", mean, tmp, pixtype="real",
+			calctype="real")
+		    imcopy (tmp, input//"[]", verbose-)
+		    imdelete (tmp, verify-)
+		} else
+		    imarith (input, "/", mean, input, pixtype="real",
+			calctype="real")
+		hedit (input, "ccdmean", 1., add=yes, verify=no, show=no,
+		    update=yes)
+	    } else
+		print ("  WARNING: Cannot normalize ", input, ".")
+	}
+	imfd = ""; delete (imlist, verify=no)
+
+	# Ending message.
+	if (keeplog) {
+	    time (>> logfile)
+	    print ("  NORMALIZE: Done.", >> logfile)
+	}
+end
diff --git a/noao/imred/generic/normflat.cl b/noao/imred/generic/normflat.cl
new file mode 100644
index 00000000..60b7025b
--- /dev/null
+++ b/noao/imred/generic/normflat.cl
@@ -0,0 +1,69 @@
+#{ NORMFLAT -- Make a flat field by normalizing and replacing low values.
+
+# image,f,a,,,,Calibration image
+# flatfield,f,a,,,,Flat field image
+# norm,r,h,INDEF,,,Normalization if not INDEF
+# minflat,r,h,INDEF,,,Minimum data value to use in the flat field
+# sample_section,s,h,"[]",,,Sample section for determining normalization
+# keeplog,b,h,@generic.keeplog,,,Keep log of processing?
+# logfile,f,h,@generic.logfile,,,Log file
+# img,f,h
+# flt,f,h
+# tmp,f,h
+# rlist,*s,h
+# mean,r,h
+# stat,i,h
+
+{
+	# Get query parameters and set temporary parameters.
+	img = image
+	flt = flatfield
+	tmp = mktemp ("tmp$gec")
+
+	# Startup message.
+	if (keeplog) {
+	    time (>> logfile)
+	    print ("  NORMFLAT: Create a flat field.\n", >> logfile)
+	    print ("  Calibration image: ", img, >> logfile)
+	    print ("  Flat field: ", flt, >> logfile)
+	    if (minflat != INDEF)
+		print ("  Minimum data value used in flat field = ", minflat,
+		    >> logfile)
+	}
+
+	# Determine normalization.
+	if (norm == INDEF) {
+	    # Determine the mean of the sample region.
+
+	    imstatistics (img // sample_section, fields="mean",
+		lower=minflat, upper=INDEF, format=no, > tmp)
+	    rlist = tmp
+	    stat = fscan (rlist, mean)
+	    rlist = ""
+	    delete (tmp, verify=no)
+	} else
+	    mean = norm
+
+	if (keeplog)
+	    print ("  Normalization = ", mean, >> logfile)
+
+	# Replace low values by the mean and normalize.
+	if (mean != 0.) {
+	    if (minflat != INDEF) {
+		imcopy (img, flt, verbose=no)
+	        imreplace (flt, mean, upper=minflat)
+	        imarith (flt, "/", mean, flt, pixtype="real")
+	    } else
+	        imarith (img, "/", mean, flt, pixtype="real")
+	} else
+	    print ("  ERROR: Cannot normalize calibration image.")
+
+	# Set CCDMEAN to 1.
+	hedit (flt, "ccdmean", "1.", add=yes, update=yes, show=no, verify=no)
+
+	# Ending message.
+	if (keeplog) {
+	    time (>> logfile)
+	    print ("  NORMFLAT: Done.", >> logfile)
+	}
+}
diff --git a/noao/imred/generic/normflat.par b/noao/imred/generic/normflat.par
new file mode 100644
index 00000000..bec48aa3
--- /dev/null
+++ b/noao/imred/generic/normflat.par
@@ -0,0 +1,15 @@
+# NORMFLAT -- Make a flat field by normalizing and replacing low values.
+
+image,f,a,,,,Calibration image
+flatfield,f,a,,,,Flat field image
+norm,r,h,INDEF,,,Normalization if not INDEF
+minflat,r,h,INDEF,,,Minimum data value to use in the flat field
+sample_section,s,h,"[]",,,Sample section for determining normalization
+keeplog,b,h,)_.keeplog,,,Keep log of processing?
+logfile,f,h,)_.logfile,,,Log file
+img,f,h
+flt,f,h
+tmp,f,h
+rlist,*s,h
+mean,r,h
+stat,i,h
diff --git a/noao/imred/generic/x_generic.x b/noao/imred/generic/x_generic.x
new file mode 100644
index 00000000..f2a61e43
--- /dev/null
+++ b/noao/imred/generic/x_generic.x
@@ -0,0 +1 @@
+task	flat1d
diff --git a/noao/imred/hydra/Revisions b/noao/imred/hydra/Revisions
new file mode 100644
index 00000000..b8318135
--- /dev/null
+++ b/noao/imred/hydra/Revisions
@@ -0,0 +1,61 @@
+.help revisions Jul91 noao.imred.hydra
+.nf
+imred$hydra/doc/dohydra.hlp
+    Fixed minor formating problem.  (4/22/99, Valdes)
+
+=======
+V2.11.1
+=======
+
+imred$hydra/doc/dohdydra.hlp
+imred$hydra/doc/dohdydra.ms
+    Updated for change where if both crval and cdelt are INDEF then the
+    automatic identification is not done.  (5/2/96, Valdes)
+
+imred$hydra/doc/dohydra.hlp
+    Fixed typo.  (4/22/97, Valdes)
+
+imred$hydra/demos/mkbig.cl
+imred$hydra/demos/mkdohydra.cl
+imred$hydra/demos/mkdonessie.cl
+    Made the ARTDATA package parameters explicit (4/15/97, Valdes)
+
+imred$hydra/hydra.cl
+    Increased the minimum min_lenuserarea from 40000 to 100000.
+    (7/31/96, Valdes)
+
+imred$hydra/dohydra.cl
+imred$hydra/dohydra.par
+imred$hydra/params.par
+imred$hydra/doc/dohydra.hlp
+imred$hydra/doc/dohydra.ms
+    Added crval/cdelt parameters used in new version with automatic arc
+    line identification.  (4/5/96, Valdes)
+
+imred$hydra/doc/dohydra.hlp
+imred$hydra/doc/dohydra.ms
+    Describes the new header option for the aperture identification table.
+    (7/25/95, Valdes)
+
+imred$hydra/hydra.cl
+imred$hydra/dohydra.cl
+imred$hydra/dohydra.par
+imred$hydra/doc/dohydra.hlp
+imred$hydra/doc/dohydra.ms
+imred$hydra/demos/xgdohydra.dat
+imred$hydra/demos/xgbig.dat
+imred$hydra/demos/xgdohydra1.dat
+imred$hydra/demos/xgdohydranl.dat
+imred$hydra/demos/xgdonessie.dat
+    Added sky alignment option.  (7/19/95, Valdes)
+
+=======
+V2.10.4
+=======
+
+imred$hydra/hydra.cl
+    Renamed "response" to "fibresponse". (12/31/94, Valdes)
+
+imred/hydra/*
+    Installed (7/24/91, Valdes)
+.endhelp
diff --git a/noao/imred/hydra/demos/big.cl b/noao/imred/hydra/demos/big.cl
new file mode 100644
index 00000000..7596599f
--- /dev/null
+++ b/noao/imred/hydra/demos/big.cl
@@ -0,0 +1,13 @@
+# Create demo data if needed.
+
+cl (< "demos$mkbig.cl")
+
+unlearn dohydra params
+params.order = "increasing"
+delete ("demologfile,demoplotfile", verify=no, >& "dev$null")
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgbig.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/hydra/demos/demos.cl b/noao/imred/hydra/demos/demos.cl
new file mode 100644
index 00000000..5b065c51
--- /dev/null
+++ b/noao/imred/hydra/demos/demos.cl
@@ -0,0 +1,18 @@
+# DEMOS -- Run specified demo provided a demo file exists.
+
+procedure demos (demoname)
+
+file	demoname	{prompt="Demo name"}
+
+begin
+	file	demo, demofile
+
+	if ($nargs == 0 && mode != "h")
+	    type ("demos$demos.men")
+	demo = demoname
+	demofile = "demos$" // demo // ".cl"
+	if (access (demofile))
+	    cl (< demofile)
+	else
+	    error (1, "Unknown demo " // demo)
+end
diff --git a/noao/imred/hydra/demos/demos.men b/noao/imred/hydra/demos/demos.men
new file mode 100644
index 00000000..8c81d0f6
--- /dev/null
+++ b/noao/imred/hydra/demos/demos.men
@@ -0,0 +1,13 @@
+	MENU of HYDRA Demonstrations
+
+    mkdohdyra - Make Hydra test data (12 fibers, 100x256)
+      dohydra - Quick Hydra test with linear resampling
+     dohydra1 - Quick Hydra test with single standard star
+     dohydral - Quick Hydra test with logarithmic resampling
+    dohydranl - Quick Hydra test with nonlinear dispersion
+
+   mkdonessie - Make Nessie test data (12 fibers, 100x256)
+     donessie - Quick Nessie test (small images, no comments, no delays)
+
+        mkbig - Make large number of fiber test data (300 fibers, 1500x256)
+          big - Test with a large number of fibers
diff --git a/noao/imred/hydra/demos/demos.par b/noao/imred/hydra/demos/demos.par
new file mode 100644
index 00000000..4181ed59
--- /dev/null
+++ b/noao/imred/hydra/demos/demos.par
@@ -0,0 +1,2 @@
+demoname,f,a,"",,,"Demo name"
+mode,s,h,"ql",,,
diff --git a/noao/imred/hydra/demos/dohydra.cl b/noao/imred/hydra/demos/dohydra.cl
new file mode 100644
index 00000000..7a81d37e
--- /dev/null
+++ b/noao/imred/hydra/demos/dohydra.cl
@@ -0,0 +1,12 @@
+# Create demo data if needed.
+
+cl (< "demos$mkdohydra.cl")
+
+unlearn dohydra params
+delete ("demologfile,demoplotfile", verify=no, >& "dev$null")
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgdohydra.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/hydra/demos/dohydra1.cl b/noao/imred/hydra/demos/dohydra1.cl
new file mode 100644
index 00000000..d18ac1bb
--- /dev/null
+++ b/noao/imred/hydra/demos/dohydra1.cl
@@ -0,0 +1,12 @@
+# Create demo data if needed.
+
+cl (< "demos$mkdohydra.cl")
+
+unlearn dohydra params
+delete ("demologfile,demoplotfile", verify=no, >& "dev$null")
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgdohydra1.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/hydra/demos/dohydral.cl b/noao/imred/hydra/demos/dohydral.cl
new file mode 100644
index 00000000..b0b99f4f
--- /dev/null
+++ b/noao/imred/hydra/demos/dohydral.cl
@@ -0,0 +1,13 @@
+# Create demo data if needed.
+
+cl (< "demos$mkdohydra.cl")
+
+unlearn dohydra params
+params.log = yes
+delete ("demologfile,demoplotfile", verify=no, >& "dev$null")
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgdohydra.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/hydra/demos/dohydranl.cl b/noao/imred/hydra/demos/dohydranl.cl
new file mode 100644
index 00000000..8b90cd54
--- /dev/null
+++ b/noao/imred/hydra/demos/dohydranl.cl
@@ -0,0 +1,14 @@
+
+# Create demo data if needed.
+
+cl (< "demos$mkdohydra.cl")
+
+unlearn dohydra params
+params.linearize = no
+delete ("demologfile,demoplotfile", verify=no, >& "dev$null")
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgdohydranl.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/hydra/demos/donessie.cl b/noao/imred/hydra/demos/donessie.cl
new file mode 100644
index 00000000..154992f2
--- /dev/null
+++ b/noao/imred/hydra/demos/donessie.cl
@@ -0,0 +1,12 @@
+# Create demo data if needed.
+
+cl (< "demos$mkdonessie.cl")
+
+unlearn dohydra params
+delete ("demologfile,demoplotfile", verify=no, >& "dev$null")
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgdonessie.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/hydra/demos/fibers.dat b/noao/imred/hydra/demos/fibers.dat
new file mode 100644
index 00000000..fcfa74b5
--- /dev/null
+++ b/noao/imred/hydra/demos/fibers.dat
@@ -0,0 +1,44 @@
+ 1 2 0.804985 gauss 2.7 0 355.825 0.002
+ 2 0 0.642824 gauss 2.7 0 349.692 0.002
+ 3 1 0.901402 gauss 2.7 0 343.900 0.002
+ 4 0 0.795503 gauss 2.7 0 337.464 0.002
+ 5 1 0.989898 gauss 2.7 0 331.099 0.002
+ 6 1 0.934496 gauss 2.7 0 324.886 0.002
+ 7 1 0.888073 gauss 2.7 0 318.907 0.002
+ 8 0 0.860567 gauss 2.7 0 312.805 0.002
+ 9 1 0.677534 gauss 2.7 0 306.601 0.002
+11 1 1.086792 gauss 2.7 0 294.340 0.002
+12 1 1.000867 gauss 2.7 0 288.223 0.002
+13 1 1.011535 gauss 2.7 0 282.295 0.002
+14 1 1.059941 gauss 2.7 0 276.397 0.002
+15 1 1.070633 gauss 2.7 0 270.036 0.002
+16 1 1.014929 gauss 2.7 0 263.795 0.002
+17 0 1.056154 gauss 2.7 0 257.857 0.002
+19 1 1.010262 gauss 2.7 0 245.340 0.002
+20 1 1.329210 gauss 2.7 0 239.071 0.002
+21 1 1.012730 gauss 2.7 0 232.936 0.002
+22 2 1.053946 gauss 2.7 0 226.763 0.002
+23 1 1.376721 gauss 2.7 0 220.742 0.002
+24 1 1.396739 gauss 2.7 0 214.579 0.002
+25 1 1.301325 gauss 2.7 0 208.787 0.002
+26 1 0.810463 gauss 2.7 0 202.392 0.002
+27 1 1.219917 gauss 2.7 0 196.406 0.002
+28 1 0.729413 gauss 2.7 0 189.815 0.002
+30 1 1.257244 gauss 2.7 0 177.277 0.002
+31 1 1.077903 gauss 2.7 0 171.462 0.002
+32 1 1.085670 gauss 2.7 0 165.604 0.002
+33 1 0.800563 gauss 2.7 0 159.134 0.002
+34 1 1.147771 gauss 2.7 0 152.901 0.002
+35 0 1.096679 gauss 2.7 0 146.801 0.002
+36 1 1.164292 gauss 2.7 0 141.093 0.002
+37 1 0.457727 gauss 2.7 0 134.824 0.002
+38 1 1.269284 gauss 2.7 0 128.719 0.002
+39 1 1.309297 gauss 2.7 0 122.536 0.002
+41 1 1.283618 gauss 2.7 0 110.218 0.002
+42 1 0.687173 gauss 2.7 0 103.963 0.002
+43 1 1.175850 gauss 2.7 0 98.0091 0.002
+44 1 0.757532 gauss 2.7 0 91.9606 0.002
+45 1 1.015546 gauss 2.7 0 79.5097 0.002
+46 1 0.372036 gauss 2.7 0 73.5889 0.002
+47 0 1.065080 gauss 2.7 0 67.4535 0.002
+48 2 0.939866 gauss 2.7 0 60.9762 0.002
diff --git a/noao/imred/hydra/demos/header.dat b/noao/imred/hydra/demos/header.dat
new file mode 100644
index 00000000..b9891d07
--- /dev/null
+++ b/noao/imred/hydra/demos/header.dat
@@ -0,0 +1,36 @@
+OBJECT  = 'V640Mon 4500      '  /  object name
+OBSERVAT= 'KPNO              '  /  observatory
+OBSERVER= 'Massey            '  /  observers
+COMMENTS= 'Final New Ice     '  /  comments
+EXPTIME =                1200.  /  actual integration time
+DARKTIME=                1200.  /  total elapsed time
+IMAGETYP= 'object            '  /  object, dark, bias, etc.
+DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+UT      = '12:19:55.00       '  /  universal time
+ST      = '09:13:15.00       '  /  sidereal time
+RA      = '06:37:02.00       '  /  right ascension
+DEC     = '06:08:52.00       '  /  declination
+EPOCH   =               1991.9  /  epoch of ra and dec
+ZD      = '44.580            '  /  zenith distance
+TELESCOP= 'kpcdf             '  /  telescope name
+DETECTOR= 'te1k              '  /  detector
+PREFLASH=                    0  /  preflash time, seconds
+GAIN    =                  5.4  /  gain, electrons per adu
+DWELL   =                    5  /  sample integration time
+RDNOISE =                  3.5  /  read noise, electrons per adu
+DELAY0  =                    0  /  time delay after each pixel
+DELAY1  =                    0  /  time delay after each row
+CAMTEMP =                 -111  /  camera temperature
+DEWTEMP =                 -183  /  dewar temperature
+CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+CCDSUM  = '1 1               '  /  on chip summation
+INSTRUME= 'IRAF/ARTDATA      '  /  instrument
+APERTURE= '250micron slit    '  /  aperture
+TVFILT  = '4-96              '  /  tv filter
+DISPAXIS= '2                 '  /  dispersion axis
+GRATPOS =               4624.3  /  grating position
+TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/hydra/demos/mkbig.cl b/noao/imred/hydra/demos/mkbig.cl
new file mode 100644
index 00000000..80b88572
--- /dev/null
+++ b/noao/imred/hydra/demos/mkbig.cl
@@ -0,0 +1,29 @@
+# Create demo data if needed.
+
+artdata
+artdata.nxc = 5
+artdata.nyc = 5
+artdata.nxsub = 10
+artdata.nysub = 10
+artdata.nxgsub = 5
+artdata.nygsub = 5
+artdata.dynrange = 100000.
+artdata.psfrange = 10.
+artdata.ranbuf = 0
+
+mkfibers ("demoobj", type="object", fibers="demos$mkbig.dat",
+    title="Hydra artificial image", header="demos$header.dat",
+    ncols=1500, nlines=256, wstart=5786., wend=7362., seed=1)
+mkfibers ("demoflat", type="flat", fibers="demos$mkbig.dat",
+    title="Hydra artificial image", header="demos$header.dat",
+    ncols=1500, nlines=256, wstart=5786., wend=7362., seed=2)
+mkfibers ("demoarc", type="henear", fibers="demos$mkbig.dat",
+    title="Hydra artificial image", header="demos$header.dat",
+    ncols=1500, nlines=256, wstart=5786., wend=7362., seed=3)
+
+# Create the setup files.
+delete ("demoapid", verify=no, >& "dev$null")
+list = "demos$mkbig.dat"
+while (fscan (list, i, j) != EOF)
+    print (i, j, >> "demoapid")
+list = ""
diff --git a/noao/imred/hydra/demos/mkbig.dat b/noao/imred/hydra/demos/mkbig.dat
new file mode 100644
index 00000000..c2260523
--- /dev/null
+++ b/noao/imred/hydra/demos/mkbig.dat
@@ -0,0 +1,300 @@
+1 1 1.104 gauss  2.0 0    9.8 .002
+2 0 0.963 gauss  2.0 0   14.7 .002
+3 1 1.245 gauss  2.0 0   19.6 .002
+4 0 1.007 gauss  2.0 0   24.5 .002
+5 1 0.961 gauss  2.0 0   29.4 .002
+6 0 1.074 gauss  2.0 0   34.3 .002
+7 1 1.104 gauss  2.0 0   39.2 .002
+8 0 1.167 gauss  2.0 0   44.1 .002
+9 1 1.152 gauss  2.0 0   49.0 .002
+10 0 1.035 gauss  2.0 0   53.9 .002
+11 1 1.089 gauss  2.0 0   58.8 .002
+12 0 0.901 gauss  2.0 0   63.7 .002
+13 1 1.054 gauss  2.0 0   68.6 .002
+14 0 0.999 gauss  2.0 0   73.5 .002
+15 1 1.017 gauss  2.0 0   78.4 .002
+16 0 0.930 gauss  2.0 0   83.3 .002
+17 1 0.821 gauss  2.0 0   88.2 .002
+18 0 0.903 gauss  2.0 0   93.1 .002
+19 1 0.957 gauss  2.0 0   98.0 .002
+20 0 1.004 gauss  2.0 0  102.9 .002
+21 1 0.777 gauss  2.0 0  107.8 .002
+22 0 0.978 gauss  2.0 0  112.7 .002
+23 1 0.820 gauss  2.0 0  117.6 .002
+24 0 0.902 gauss  2.0 0  122.5 .002
+25 1 0.825 gauss  2.0 0  127.4 .002
+26 0 0.975 gauss  2.0 0  132.3 .002
+27 1 1.121 gauss  2.0 0  137.2 .002
+28 0 1.158 gauss  2.0 0  142.1 .002
+29 1 0.782 gauss  2.0 0  147.0 .002
+30 0 0.956 gauss  2.0 0  151.9 .002
+31 1 0.994 gauss  2.0 0  156.8 .002
+32 0 1.020 gauss  2.0 0  161.7 .002
+33 1 0.817 gauss  2.0 0  166.6 .002
+34 0 0.786 gauss  2.0 0  171.5 .002
+35 1 1.227 gauss  2.0 0  176.4 .002
+36 0 0.863 gauss  2.0 0  181.3 .002
+37 1 0.914 gauss  2.0 0  186.2 .002
+38 0 1.154 gauss  2.0 0  191.1 .002
+39 1 0.878 gauss  2.0 0  196.0 .002
+40 0 1.044 gauss  2.0 0  200.9 .002
+41 1 1.034 gauss  2.0 0  205.8 .002
+42 0 0.756 gauss  2.0 0  210.7 .002
+43 1 0.773 gauss  2.0 0  215.6 .002
+44 0 0.933 gauss  2.0 0  220.5 .002
+45 1 0.888 gauss  2.0 0  225.4 .002
+46 0 0.990 gauss  2.0 0  230.3 .002
+47 1 0.920 gauss  2.0 0  235.2 .002
+48 0 1.113 gauss  2.0 0  240.1 .002
+49 1 1.010 gauss  2.0 0  245.0 .002
+50 0 0.767 gauss  2.0 0  249.9 .002
+51 1 1.146 gauss  2.0 0  254.8 .002
+52 0 0.962 gauss  2.0 0  259.7 .002
+53 1 1.030 gauss  2.0 0  264.6 .002
+54 0 0.812 gauss  2.0 0  269.5 .002
+55 1 1.001 gauss  2.0 0  274.4 .002
+56 0 1.126 gauss  2.0 0  279.3 .002
+57 1 0.845 gauss  2.0 0  284.2 .002
+58 0 1.050 gauss  2.0 0  289.1 .002
+59 1 1.221 gauss  2.0 0  294.0 .002
+60 0 1.103 gauss  2.0 0  298.9 .002
+61 1 1.079 gauss  2.0 0  303.8 .002
+62 0 0.944 gauss  2.0 0  308.7 .002
+63 1 0.810 gauss  2.0 0  313.6 .002
+64 0 0.922 gauss  2.0 0  318.5 .002
+65 1 1.039 gauss  2.0 0  323.4 .002
+66 0 0.892 gauss  2.0 0  328.3 .002
+67 1 1.021 gauss  2.0 0  333.2 .002
+68 0 1.160 gauss  2.0 0  338.1 .002
+69 1 1.053 gauss  2.0 0  343.0 .002
+70 0 1.043 gauss  2.0 0  347.9 .002
+71 1 0.794 gauss  2.0 0  352.8 .002
+72 0 0.777 gauss  2.0 0  357.7 .002
+73 1 0.890 gauss  2.0 0  362.6 .002
+74 0 1.143 gauss  2.0 0  367.5 .002
+75 1 0.945 gauss  2.0 0  372.4 .002
+76 0 0.994 gauss  2.0 0  377.3 .002
+77 1 1.174 gauss  2.0 0  382.2 .002
+78 0 0.766 gauss  2.0 0  387.1 .002
+79 1 1.157 gauss  2.0 0  392.0 .002
+80 0 1.219 gauss  2.0 0  396.9 .002
+81 1 0.951 gauss  2.0 0  401.8 .002
+82 0 1.044 gauss  2.0 0  406.7 .002
+83 1 1.054 gauss  2.0 0  411.6 .002
+84 0 1.236 gauss  2.0 0  416.5 .002
+85 1 0.862 gauss  2.0 0  421.4 .002
+86 0 0.755 gauss  2.0 0  426.3 .002
+87 1 0.933 gauss  2.0 0  431.2 .002
+88 0 1.149 gauss  2.0 0  436.1 .002
+89 1 1.053 gauss  2.0 0  441.0 .002
+90 0 0.870 gauss  2.0 0  445.9 .002
+91 1 0.920 gauss  2.0 0  450.8 .002
+92 0 0.820 gauss  2.0 0  455.7 .002
+93 1 0.786 gauss  2.0 0  460.6 .002
+94 0 0.934 gauss  2.0 0  465.5 .002
+95 1 1.117 gauss  2.0 0  470.4 .002
+96 0 0.776 gauss  2.0 0  475.3 .002
+97 1 0.887 gauss  2.0 0  480.2 .002
+98 0 0.876 gauss  2.0 0  485.1 .002
+99 1 1.037 gauss  2.0 0  490.0 .002
+100 0 0.824 gauss  2.0 0  494.9 .002
+101 1 0.979 gauss  2.0 0  499.8 .002
+102 0 1.112 gauss  2.0 0  504.7 .002
+103 1 0.856 gauss  2.0 0  509.6 .002
+104 0 0.864 gauss  2.0 0  514.5 .002
+105 1 1.154 gauss  2.0 0  519.4 .002
+106 0 1.060 gauss  2.0 0  524.3 .002
+107 1 0.800 gauss  2.0 0  529.2 .002
+108 0 1.121 gauss  2.0 0  534.1 .002
+109 1 1.017 gauss  2.0 0  539.0 .002
+110 0 0.905 gauss  2.0 0  543.9 .002
+111 1 1.203 gauss  2.0 0  548.8 .002
+112 0 0.795 gauss  2.0 0  553.7 .002
+113 1 0.770 gauss  2.0 0  558.6 .002
+114 0 1.246 gauss  2.0 0  563.5 .002
+115 1 1.035 gauss  2.0 0  568.4 .002
+116 0 0.852 gauss  2.0 0  573.3 .002
+117 1 0.757 gauss  2.0 0  578.2 .002
+118 0 0.969 gauss  2.0 0  583.1 .002
+119 1 0.943 gauss  2.0 0  588.0 .002
+120 0 0.943 gauss  2.0 0  592.9 .002
+121 1 1.141 gauss  2.0 0  597.8 .002
+122 0 0.965 gauss  2.0 0  602.7 .002
+123 1 1.107 gauss  2.0 0  607.6 .002
+124 0 1.199 gauss  2.0 0  612.5 .002
+125 1 1.141 gauss  2.0 0  617.4 .002
+126 0 1.043 gauss  2.0 0  622.3 .002
+127 1 0.964 gauss  2.0 0  627.2 .002
+128 0 0.856 gauss  2.0 0  632.1 .002
+129 1 0.993 gauss  2.0 0  637.0 .002
+130 0 1.160 gauss  2.0 0  641.9 .002
+131 1 1.076 gauss  2.0 0  646.8 .002
+132 0 0.981 gauss  2.0 0  651.7 .002
+133 1 1.061 gauss  2.0 0  656.6 .002
+134 0 0.811 gauss  2.0 0  661.5 .002
+135 1 1.210 gauss  2.0 0  666.4 .002
+136 0 0.753 gauss  2.0 0  671.3 .002
+137 1 0.773 gauss  2.0 0  676.2 .002
+138 0 1.202 gauss  2.0 0  681.1 .002
+139 1 0.922 gauss  2.0 0  686.0 .002
+140 0 1.055 gauss  2.0 0  690.9 .002
+141 1 0.790 gauss  2.0 0  695.8 .002
+142 0 1.064 gauss  2.0 0  700.7 .002
+143 1 1.179 gauss  2.0 0  705.6 .002
+144 0 0.843 gauss  2.0 0  710.5 .002
+145 1 1.105 gauss  2.0 0  715.4 .002
+146 0 1.208 gauss  2.0 0  720.3 .002
+147 1 0.835 gauss  2.0 0  725.2 .002
+148 0 1.039 gauss  2.0 0  730.1 .002
+149 1 0.966 gauss  2.0 0  735.0 .002
+150 0 1.191 gauss  2.0 0  739.9 .002
+151 1 0.995 gauss  2.0 0  744.8 .002
+152 0 0.936 gauss  2.0 0  749.7 .002
+153 1 0.813 gauss  2.0 0  754.6 .002
+154 0 1.190 gauss  2.0 0  759.5 .002
+155 1 1.064 gauss  2.0 0  764.4 .002
+156 0 0.832 gauss  2.0 0  769.3 .002
+157 1 1.147 gauss  2.0 0  774.2 .002
+158 0 0.967 gauss  2.0 0  779.1 .002
+159 1 1.040 gauss  2.0 0  784.0 .002
+160 0 0.890 gauss  2.0 0  788.9 .002
+161 1 1.002 gauss  2.0 0  793.8 .002
+162 0 0.999 gauss  2.0 0  798.7 .002
+163 1 0.828 gauss  2.0 0  803.6 .002
+164 0 0.962 gauss  2.0 0  808.5 .002
+165 1 0.932 gauss  2.0 0  813.4 .002
+166 0 1.166 gauss  2.0 0  818.3 .002
+167 1 1.144 gauss  2.0 0  823.2 .002
+168 0 0.850 gauss  2.0 0  828.1 .002
+169 1 1.209 gauss  2.0 0  833.0 .002
+170 0 1.089 gauss  2.0 0  837.9 .002
+171 1 0.788 gauss  2.0 0  842.8 .002
+172 0 1.242 gauss  2.0 0  847.7 .002
+173 1 1.130 gauss  2.0 0  852.6 .002
+174 0 0.977 gauss  2.0 0  857.5 .002
+175 1 0.843 gauss  2.0 0  862.4 .002
+176 0 0.815 gauss  2.0 0  867.3 .002
+177 1 1.110 gauss  2.0 0  872.2 .002
+178 0 1.098 gauss  2.0 0  877.1 .002
+179 1 1.090 gauss  2.0 0  882.0 .002
+180 0 1.230 gauss  2.0 0  886.9 .002
+181 1 1.004 gauss  2.0 0  891.8 .002
+182 0 1.237 gauss  2.0 0  896.7 .002
+183 1 1.197 gauss  2.0 0  901.6 .002
+184 0 1.007 gauss  2.0 0  906.5 .002
+185 1 0.790 gauss  2.0 0  911.4 .002
+186 0 1.233 gauss  2.0 0  916.3 .002
+187 1 0.962 gauss  2.0 0  921.2 .002
+188 0 1.014 gauss  2.0 0  926.1 .002
+189 1 1.076 gauss  2.0 0  931.0 .002
+190 0 0.978 gauss  2.0 0  935.9 .002
+191 1 1.173 gauss  2.0 0  940.8 .002
+192 0 1.058 gauss  2.0 0  945.7 .002
+193 1 1.077 gauss  2.0 0  950.6 .002
+194 0 0.970 gauss  2.0 0  955.5 .002
+195 1 0.874 gauss  2.0 0  960.4 .002
+196 0 0.803 gauss  2.0 0  965.3 .002
+197 1 0.990 gauss  2.0 0  970.2 .002
+198 0 0.783 gauss  2.0 0  975.1 .002
+199 1 1.083 gauss  2.0 0  980.0 .002
+200 0 1.009 gauss  2.0 0  984.9 .002
+201 1 0.943 gauss  2.0 0  989.8 .002
+202 0 1.071 gauss  2.0 0  994.7 .002
+203 1 0.764 gauss  2.0 0  999.6 .002
+204 0 0.827 gauss  2.0 0 1004.5 .002
+205 1 0.938 gauss  2.0 0 1009.4 .002
+206 0 0.956 gauss  2.0 0 1014.3 .002
+207 1 1.094 gauss  2.0 0 1019.2 .002
+208 0 1.119 gauss  2.0 0 1024.1 .002
+209 1 0.957 gauss  2.0 0 1029.0 .002
+210 0 0.910 gauss  2.0 0 1033.9 .002
+211 1 0.827 gauss  2.0 0 1038.8 .002
+212 0 1.060 gauss  2.0 0 1043.7 .002
+213 1 1.154 gauss  2.0 0 1048.6 .002
+214 0 1.002 gauss  2.0 0 1053.5 .002
+215 1 0.797 gauss  2.0 0 1058.4 .002
+216 0 0.989 gauss  2.0 0 1063.3 .002
+217 1 0.810 gauss  2.0 0 1068.2 .002
+218 0 1.106 gauss  2.0 0 1073.1 .002
+219 1 0.863 gauss  2.0 0 1078.0 .002
+220 0 1.246 gauss  2.0 0 1082.9 .002
+221 1 0.963 gauss  2.0 0 1087.8 .002
+222 0 0.929 gauss  2.0 0 1092.7 .002
+223 1 0.835 gauss  2.0 0 1097.6 .002
+224 0 0.995 gauss  2.0 0 1102.5 .002
+225 1 0.897 gauss  2.0 0 1107.4 .002
+226 0 0.983 gauss  2.0 0 1112.3 .002
+227 1 1.187 gauss  2.0 0 1117.2 .002
+228 0 1.239 gauss  2.0 0 1122.1 .002
+229 1 0.900 gauss  2.0 0 1127.0 .002
+230 0 0.846 gauss  2.0 0 1131.9 .002
+231 1 1.096 gauss  2.0 0 1136.8 .002
+232 0 1.041 gauss  2.0 0 1141.7 .002
+233 1 0.968 gauss  2.0 0 1146.6 .002
+234 0 0.827 gauss  2.0 0 1151.5 .002
+235 1 1.108 gauss  2.0 0 1156.4 .002
+236 0 1.162 gauss  2.0 0 1161.3 .002
+237 1 0.884 gauss  2.0 0 1166.2 .002
+238 0 0.891 gauss  2.0 0 1171.1 .002
+239 1 0.974 gauss  2.0 0 1176.0 .002
+240 0 1.116 gauss  2.0 0 1180.9 .002
+241 1 0.830 gauss  2.0 0 1185.8 .002
+242 0 0.964 gauss  2.0 0 1190.7 .002
+243 1 0.963 gauss  2.0 0 1195.6 .002
+244 0 0.869 gauss  2.0 0 1200.5 .002
+245 1 0.962 gauss  2.0 0 1205.4 .002
+246 0 0.959 gauss  2.0 0 1210.3 .002
+247 1 1.182 gauss  2.0 0 1215.2 .002
+248 0 1.167 gauss  2.0 0 1220.1 .002
+249 1 1.124 gauss  2.0 0 1225.0 .002
+250 0 1.151 gauss  2.0 0 1229.9 .002
+251 1 1.218 gauss  2.0 0 1234.8 .002
+252 0 1.229 gauss  2.0 0 1239.7 .002
+253 1 1.108 gauss  2.0 0 1244.6 .002
+254 0 1.248 gauss  2.0 0 1249.5 .002
+255 1 1.135 gauss  2.0 0 1254.4 .002
+256 0 0.787 gauss  2.0 0 1259.3 .002
+257 1 1.156 gauss  2.0 0 1264.2 .002
+258 0 0.773 gauss  2.0 0 1269.1 .002
+259 1 1.129 gauss  2.0 0 1274.0 .002
+260 0 1.212 gauss  2.0 0 1278.9 .002
+261 1 1.092 gauss  2.0 0 1283.8 .002
+262 0 1.116 gauss  2.0 0 1288.7 .002
+263 1 0.892 gauss  2.0 0 1293.6 .002
+264 0 1.208 gauss  2.0 0 1298.5 .002
+265 1 0.795 gauss  2.0 0 1303.4 .002
+266 0 0.860 gauss  2.0 0 1308.3 .002
+267 1 0.967 gauss  2.0 0 1313.2 .002
+268 0 0.800 gauss  2.0 0 1318.1 .002
+269 1 0.902 gauss  2.0 0 1323.0 .002
+270 0 0.752 gauss  2.0 0 1327.9 .002
+271 1 1.164 gauss  2.0 0 1332.8 .002
+272 0 1.119 gauss  2.0 0 1337.7 .002
+273 1 0.932 gauss  2.0 0 1342.6 .002
+274 0 0.912 gauss  2.0 0 1347.5 .002
+275 1 0.806 gauss  2.0 0 1352.4 .002
+276 0 1.198 gauss  2.0 0 1357.3 .002
+277 1 1.242 gauss  2.0 0 1362.2 .002
+278 0 1.158 gauss  2.0 0 1367.1 .002
+279 1 0.881 gauss  2.0 0 1372.0 .002
+280 0 0.782 gauss  2.0 0 1376.9 .002
+281 1 1.000 gauss  2.0 0 1381.8 .002
+282 0 1.038 gauss  2.0 0 1386.7 .002
+283 1 0.872 gauss  2.0 0 1391.6 .002
+284 0 0.868 gauss  2.0 0 1396.5 .002
+285 1 1.079 gauss  2.0 0 1401.4 .002
+286 0 0.943 gauss  2.0 0 1406.3 .002
+287 1 0.825 gauss  2.0 0 1411.2 .002
+288 0 0.973 gauss  2.0 0 1416.1 .002
+289 1 1.061 gauss  2.0 0 1421.0 .002
+290 0 0.905 gauss  2.0 0 1425.9 .002
+291 1 0.954 gauss  2.0 0 1430.8 .002
+292 0 0.865 gauss  2.0 0 1435.7 .002
+293 1 0.761 gauss  2.0 0 1440.6 .002
+294 0 0.932 gauss  2.0 0 1445.5 .002
+295 1 0.818 gauss  2.0 0 1450.4 .002
+296 0 1.225 gauss  2.0 0 1455.3 .002
+297 1 0.949 gauss  2.0 0 1460.2 .002
+298 0 1.006 gauss  2.0 0 1465.1 .002
+299 1 0.880 gauss  2.0 0 1470.0 .002
+300 0 0.998 gauss  2.0 0 1474.9 .002
diff --git a/noao/imred/hydra/demos/mkdohydra.cl b/noao/imred/hydra/demos/mkdohydra.cl
new file mode 100644
index 00000000..543dadb5
--- /dev/null
+++ b/noao/imred/hydra/demos/mkdohydra.cl
@@ -0,0 +1,41 @@
+# Create demo data if needed.
+
+artdata
+artdata.nxc = 5
+artdata.nyc = 5
+artdata.nxsub = 10
+artdata.nysub = 10
+artdata.nxgsub = 5
+artdata.nygsub = 5
+artdata.dynrange = 100000.
+artdata.psfrange = 10.
+artdata.ranbuf = 0
+
+mkfibers ("demoobj", type="object", fibers="demos$mkdohydra1.dat",
+    title="Hydra artificial image", header="demos$header.dat",
+    ncols=100, nlines=256, wstart=5786., wend=7362., seed=1)
+mkfibers ("demoflat", type="flat", fibers="demos$mkdohydra1.dat",
+    title="Hydra artificial image", header="demos$header.dat",
+    ncols=100, nlines=256, wstart=5786., wend=7362., seed=2)
+mkfibers ("demoarc", type="henear", fibers="demos$mkdohydra1.dat",
+    title="Hydra artificial image", header="demos$header.dat",
+    ncols=100, nlines=256, wstart=5786., wend=7362., seed=3)
+mkfibers ("demostd", type="object", fibers="demos$mkdohydra2.dat",
+    title="Hydra artificial image", header="demos$header.dat",
+    ncols=100, nlines=256, wstart=5786., wend=7362., seed=1)
+
+# Create the setup files.
+delete ("demoapid1", verify=no, >& "dev$null")
+list = "demos$mkdohydra1.dat"
+while (fscan (list, i, j) != EOF) {
+    print (i, j, "Title", >> "demoapid1")
+    s1 = i // " " // j // " 01:23:45.67 +01:23:45.67 Title"
+    hedit ("demoobj,demoflat,demoarc,demostd", "slfib"//i, s1,
+	add=yes, verify=no, show=no, update=yes)
+}
+list = ""
+delete ("demoapid2", verify=no, >& "dev$null")
+list = "demos$mkdohydra2.dat"
+while (fscan (list, i, j) != EOF)
+    print (i, j, >> "demoapid2")
+list = ""
diff --git a/noao/imred/hydra/demos/mkdohydra1.dat b/noao/imred/hydra/demos/mkdohydra1.dat
new file mode 100644
index 00000000..87640612
--- /dev/null
+++ b/noao/imred/hydra/demos/mkdohydra1.dat
@@ -0,0 +1,12 @@
+36 1 1.164292 gauss 2.7 0 91.093 0.002
+37 0 0.457727 gauss 2.7 0 84.824 0.002
+38 1 1.269284 gauss 2.7 0 78.719 0.002
+39 1 1.309297 gauss 2.7 0 72.536 0.002
+41 0 1.283618 gauss 2.7 0 60.218 0.002
+42 1 0.687173 gauss 2.7 0 53.963 0.002
+43 1 1.175850 gauss 2.7 0 48.0091 0.002
+44 0 0.757532 gauss 2.7 0 41.9606 0.002
+45 1 1.015546 gauss 2.7 0 29.5097 0.002
+46 -1 0.372036 gauss 2.7 0 23.5889 0.002
+47 0 1.065080 gauss 2.7 0 17.4535 0.002
+48 1 0.939866 gauss 2.7 0 10.9762 0.002
diff --git a/noao/imred/hydra/demos/mkdohydra2.dat b/noao/imred/hydra/demos/mkdohydra2.dat
new file mode 100644
index 00000000..4b848596
--- /dev/null
+++ b/noao/imred/hydra/demos/mkdohydra2.dat
@@ -0,0 +1,12 @@
+36 0 1.164292 gauss 2.7 0 91.093 0.002
+37 0 0.457727 gauss 2.7 0 84.824 0.002
+38 0 1.269284 gauss 2.7 0 78.719 0.002
+39 0 1.309297 gauss 2.7 0 72.536 0.002
+41 0 1.283618 gauss 2.7 0 60.218 0.002
+42 0 0.687173 gauss 2.7 0 53.963 0.002
+43 1 1.175850 gauss 2.7 0 48.0091 0.002
+44 0 0.757532 gauss 2.7 0 41.9606 0.002
+45 0 1.015546 gauss 2.7 0 29.5097 0.002
+46 -1 0.372036 gauss 2.7 0 23.5889 0.002
+47 0 1.065080 gauss 2.7 0 17.4535 0.002
+48 0 0.939866 gauss 2.7 0 10.9762 0.002
diff --git a/noao/imred/hydra/demos/mkdonessie.cl b/noao/imred/hydra/demos/mkdonessie.cl
new file mode 100644
index 00000000..e67a90e1
--- /dev/null
+++ b/noao/imred/hydra/demos/mkdonessie.cl
@@ -0,0 +1,36 @@
+# Create demo data if needed.
+
+artdata
+artdata.nxc = 5
+artdata.nyc = 5
+artdata.nxsub = 10
+artdata.nysub = 10
+artdata.nxgsub = 5
+artdata.nygsub = 5
+artdata.dynrange = 100000.
+artdata.psfrange = 10.
+artdata.ranbuf = 0
+
+mkfibers ("demoobj", type="object", fibers="demos$mkdonessie.dat",
+    title="Hydra artificial image", header="demos$header.dat",
+    ncols=100, nlines=256, wstart=5786., wend=7362., seed=1)
+mkfibers ("demoflat", type="flat", fibers="demos$mkdonessie.dat",
+    title="Hydra artificial image", header="demos$header.dat",
+    ncols=100, nlines=256, wstart=5786., wend=7362., seed=2)
+mkfibers ("demoarc1", type="ehenear", fibers="demos$mkdonessie.dat",
+    title="Hydra artificial image", header="demos$header.dat",
+    ncols=100, nlines=256, wstart=5786., wend=7362., seed=3)
+mkfibers ("demoarc2", type="ohenear", fibers="demos$mkdonessie.dat",
+    title="Hydra artificial image", header="demos$header.dat",
+    ncols=100, nlines=256, wstart=5786., wend=7362., seed=4)
+#mkfibers ("demoarc3", type="mercury", fibers="demos$mkdonessie.dat",
+#    title="Hydra artificial image", header="demos$header.dat",
+#    ncols=100, nlines=256, wstart=5786., wend=7362., seed=4)
+
+# Create the setup files.
+delete ("demoapid,demoarcrep", verify=no, >& "dev$null")
+list = "demos$mkdonessie.dat"
+while (fscan (list, i, j) != EOF)
+    print (i, j, >> "demoapid")
+list = ""
+print ("demoarc1 demoarc2 1x2", > "demoarcrep")
diff --git a/noao/imred/hydra/demos/mkdonessie.dat b/noao/imred/hydra/demos/mkdonessie.dat
new file mode 100644
index 00000000..1113aae6
--- /dev/null
+++ b/noao/imred/hydra/demos/mkdonessie.dat
@@ -0,0 +1,12 @@
+36 2 1.164292 gauss 2.7 0 91.093 0.002
+37 0 0.457727 gauss 2.7 0 84.824 0.002
+38 1 1.269284 gauss 2.7 0 78.719 0.002
+39 1 1.309297 gauss 2.7 0 72.536 0.002
+41 0 1.283618 gauss 2.7 0 60.218 0.002
+42 1 0.687173 gauss 2.7 0 53.963 0.002
+43 1 1.175850 gauss 2.7 0 48.0091 0.002
+44 0 0.757532 gauss 2.7 0 41.9606 0.002
+45 1 1.015546 gauss 2.7 0 29.5097 0.002
+46 1 0.372036 gauss 2.7 0 23.5889 0.002
+47 0 1.065080 gauss 2.7 0 17.4535 0.002
+48 2 0.939866 gauss 2.7 0 10.9762 0.002
diff --git a/noao/imred/hydra/demos/mklist.cl b/noao/imred/hydra/demos/mklist.cl
new file mode 100644
index 00000000..b36b3a3e
--- /dev/null
+++ b/noao/imred/hydra/demos/mklist.cl
@@ -0,0 +1,27 @@
+# MKLIST - Make a fiber list.
+
+int	nfibers
+real	width, sep, flux
+file	temp
+
+#nfibers = 300
+#width = 2.0
+#sep = 4.9
+nfibers = j
+width = x
+sep = y
+
+temp = mktemp ("tmp")
+urand (nfibers, 1, ndigits=4, seed=1, scale_factor=0.5, > temp)
+list = temp
+
+for (i=1; i<=nfibers; i+=1) {
+    if (fscan (list, flux) == EOF)
+	break
+    flux = 0.75 + flux
+    printf ("%d %d %5.3f gauss %4.1f 0 %6.1f .002\n", i, mod(i,2),
+	flux, width, sep*(i+1))
+}
+
+list = ""
+delete (temp, verify=no)
diff --git a/noao/imred/hydra/demos/xgbig.dat b/noao/imred/hydra/demos/xgbig.dat
new file mode 100644
index 00000000..074d8db5
--- /dev/null
+++ b/noao/imred/hydra/demos/xgbig.dat
@@ -0,0 +1,81 @@
+\O=NOAO/IRAF IRAFX valdes@puppis Mon 14:58:37 15-Nov-93
+\T=xgterm
+\G=xgterm
+epar\shydra\n
+\r
+\r
+\r
+\r
+\r
+y\r
+demologfile\r
+""\r
+^Z
+epar\sdohydra\n
+demoobj\r
+demoflat\r
+demoflat\r
+\r
+demoarc\r
+\r
+\r
+\r
+rdnoise\r
+gain\r
+\r
+300\r
+3\r
+4\r
+6\r
+demoapid\r
+6600\r
+6.1\r
+\r
+\r
+\r
+\r
+\r
+\r
+n\r
+\r
+n\r
+\r
+\r
+\r
+\r
+\r
+\r
+y\r
+^Z
+dohydra\sredo+\n
+\n
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\r
+j/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+n\n
+y\n
+f/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\n
+n\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\n
+\n
+41\n
+#/<-5\s\s\s\s/=(.\s=\r 37\r
+#/<-5\s\s\s\s/=(.\s=\r 45\r
+q/<-5\s\s\s\s/=(.\s=\r
+imdelete\sdemoobj.ms\n
+dohydra\sdemoobj\sskyedit-\ssplot-\sbatch+\n
diff --git a/noao/imred/hydra/demos/xgdohydra.dat b/noao/imred/hydra/demos/xgdohydra.dat
new file mode 100644
index 00000000..be94c8b0
--- /dev/null
+++ b/noao/imred/hydra/demos/xgdohydra.dat
@@ -0,0 +1,93 @@
+\O=NOAO/IRAF V2.10EXPORT valdes@puppis Tue 14:30:46 09-Feb-93
+\T=xgterm
+\G=xgterm
+epar\shydra\n
+\r
+\r
+\r
+\r
+\r
+y\r
+demologfile\r
+demoplotfile\r
+^Z
+epar\sdohydra\n
+demoobj\r
+demoflat\r
+demoflat\r
+\r
+demoarc\r
+\r
+\r
+\r
+rdnoise\r
+gain\r
+\r
+12\r
+4\r
+5\r
+7\r
+demoflat\r
+6600\r
+6.1\r
+\r
+\r
+\r
+\r
+\r
+\r
+y\r
+\r
+n\r
+\r
+\r
+\r
+\r
+\r
+\r
+y\r
+^Z
+dohydra\sredo+\n
+\n
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\r
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+j/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+n\n
+y\n
+f/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\n
+n\n
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\n
+\n
+41\n
+#/<-5\s\s\s\s/=(.\s=\r 37\r
+#/<-5\s\s\s\s/=(.\s=\r 45\r
+q/<-5\s\s\s\s/=(.\s=\r
+imdelete\sdemoobj.ms\n
+dohydra\sdemoobj\sskyedit-\ssplot-\sbatch+\n
diff --git a/noao/imred/hydra/demos/xgdohydra1.dat b/noao/imred/hydra/demos/xgdohydra1.dat
new file mode 100644
index 00000000..ce9cebb7
--- /dev/null
+++ b/noao/imred/hydra/demos/xgdohydra1.dat
@@ -0,0 +1,89 @@
+\O=NOAO/IRAF IRAFX valdes@puppis Mon 14:58:37 15-Nov-93
+\T=xgterm
+\G=xgterm
+epar\shydra\n
+\r
+\r
+\r
+\r
+\r
+y\r
+demologfile\r
+demoplotfile\r
+^Z
+epar\sdohydra\n
+demostd\r
+demoflat\r
+demoflat\r
+\r
+demoarc\r
+\r
+\r
+\r
+rdnoise\r
+gain\r
+\r
+12\r
+4\r
+5\r
+7\r
+demoapid2\r
+6600\r
+6.1\r
+\r
+\r
+\r
+1\r
+\r
+\r
+y\r
+\r
+n\r
+\r
+\r
+\r
+\r
+\r
+\r
+y\r
+^Z
+type\sdemoapid2\n
+dohydra\sredo+\n
+\n
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\r
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+j/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+n\n
+y\n
+f/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\n
+n\n
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
diff --git a/noao/imred/hydra/demos/xgdohydranl.dat b/noao/imred/hydra/demos/xgdohydranl.dat
new file mode 100644
index 00000000..9efdb764
--- /dev/null
+++ b/noao/imred/hydra/demos/xgdohydranl.dat
@@ -0,0 +1,91 @@
+\O=NOAO/IRAF IRAFX valdes@puppis Mon 14:58:37 15-Nov-93
+\T=xgterm
+\G=xgterm
+epar\shydra\n
+\r
+\r
+\r
+\r
+\r
+y\r
+demologfile\r
+demoplotfile\r
+^Z
+epar\sdohydra\n
+demoobj\r
+demoflat\r
+demoflat\r
+\r
+demoarc\r
+\r
+\r
+\r
+rdnoise\r
+gain\r
+\r
+12\r
+4\r
+5\r
+7\r
+demoapid1\r
+6600\r
+6.1\r
+\r
+\r
+\r
+\r
+\r
+\r
+y\r
+\r
+n\r
+\r
+\r
+\r
+\r
+\r
+\r
+y\r
+^Z
+type\sdemoapid1\n
+dohydra\sredo+\n
+\n
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\r
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+j/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+n\n
+y\n
+f/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\n
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\n
+\n
+41\n
+#/<-5\s\s\s\s/=(.\s=\r 37\r
+#/<-5\s\s\s\s/=(.\s=\r 45\r
+q/<-5\s\s\s\s/=(.\s=\r
diff --git a/noao/imred/hydra/demos/xgdonessie.dat b/noao/imred/hydra/demos/xgdonessie.dat
new file mode 100644
index 00000000..49e57ff0
--- /dev/null
+++ b/noao/imred/hydra/demos/xgdonessie.dat
@@ -0,0 +1,94 @@
+\O=NOAO/IRAF IRAFX valdes@puppis Mon 14:58:37 15-Nov-93
+\T=xgterm
+\G=xgterm
+epar\shydra\n
+\r
+\r
+\r
+\r
+\r
+y\r
+demologfile\r
+demoplotfile\r
+^Z
+epar\sdohydra\n
+demoobj\r
+demoflat\r
+demoflat\r
+\r
+demoarc1\r
+\r
+demoarcrep\r
+\r
+rdnoise\r
+gain\r
+\r
+12\r
+4\r
+5\r
+7\r
+demoapid\r
+6600\r
+6.1\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+n\r
+\r
+\r
+\r
+\r
+\r
+\r
+y\r
+^Z
+type\sdemoapid,demoarcrep\n
+dohydra\sredo+\n
+\n
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\r
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+k/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+n\n
+y\n
+f/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\n
+n\n
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+q/<-5\s\s\s\s/=(.\s=\r
+q\r
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\n
+\n
+41\n
+#/<-5\s\s\s\s/=(.\s=\r 37\r
+#/<-5\s\s\s\s/=(.\s=\r 45\r
+q/<-5\s\s\s\s/=(.\s=\r
+imdelete\sdemoobj.ms\n
+dohydra\sdemoobj\sskyedit-\ssplot-\sbatch+\n
diff --git a/noao/imred/hydra/doc/dohydra.hlp b/noao/imred/hydra/doc/dohydra.hlp
new file mode 100644
index 00000000..7c762d3b
--- /dev/null
+++ b/noao/imred/hydra/doc/dohydra.hlp
@@ -0,0 +1,1588 @@
+.help dohydra Jul95 noao.imred.hydra
+.ih
+NAME
+dohydra -- Hydra and Nessie data reduction task
+.ih
+USAGE
+dohydra objects
+.ih
+SUMMARY
+The \fBdohydra\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, fiber throughput correction, wavelength calibration, and sky
+subtraction of \fIHydra\fR and \fINessie\fR fiber spectra.  It is a
+command language script which collects and combines the functions and
+parameters of many general purpose tasks to provide a single complete data
+reduction path.  The task provides a degree of guidance, automation, and
+record keeping necessary when dealing with the large amount of data
+generated by these multifiber instruments.
+.ih
+PARAMETERS
+.ls objects
+List of object spectra to be processed.  Previously processed spectra are
+ignored unless the \fIredo\fR flag is set or the \fIupdate\fR flag is set and
+dependent calibration data has changed.  Extracted spectra are ignored.
+.le
+.ls apref = ""
+Aperture reference spectrum.  This spectrum is used to define the basic
+extraction apertures and is typically a flat field spectrum.
+.le
+.ls flat = "" (optional)
+Flat field spectrum.  If specified the one dimensional flat field spectra
+are extracted and used to make flat field calibrations.  If a separate
+throughput file or image is not specified the flat field is also used
+for computing a fiber throughput correction.
+.le
+.ls throughput = "" (optional)
+Throughput file or image.  If an image is specified, typically a blank
+sky observation, the total flux through
+each fiber is used to correct for fiber throughput.  If a file consisting
+of lines with the aperture number and relative throughput is specified
+then the fiber throughput will be corrected by those values.  If neither
+is specified but a flat field image is given it is used to compute the
+throughput.  
+.le
+.ls arcs1 = "" (at least one if dispersion correcting)
+List of primary arc spectra.  These spectra are used to define the dispersion
+functions for each fiber apart from a possible zero point correction made
+with secondary shift spectra or arc calibration fibers in the object spectra.
+One fiber from the first spectrum is used to mark lines and set the dispersion
+function interactively and dispersion functions for all other fibers and
+arc spectra are derived from it.
+.le
+.ls arcs2 = "" (optional for Nessie)
+List of optional shift arc spectra.  Features in these secondary observations
+are used to supply a wavelength zero point shift through the observing
+sequence.  One type of observation is dome lamps containing characteristic
+emission lines.
+.le
+.ls arcreplace = "" (optional for Nessie)
+Special aperture replacement file.  A characteristic of Nessie (though not
+Hydra) spectra is that it requires two exposures to illuminate all fibers
+with an arc calibration.  The aperture replacement file assigns fibers from
+the second exposure to replace those in the first exposure.  Only the first
+exposures are specified in the \fIarcs1\fR list.  The file contains lines
+with the first exposure image name, the second exposure image name, and a
+list of apertures from the second exposure to be used instead of those in
+the first exposure.
+.le
+.ls arctable = "" (optional) (refspectra)
+Table defining arc spectra to be assigned to object
+spectra (see \fBrefspectra\fR).  If not specified an assignment based
+on a header parameter, \fIparams.sort\fR, such as the observation time is made.
+.le
+
+.ls readnoise = "RDNOISE" (apsum)
+Read out noise in photons.  This parameter defines the minimum noise
+sigma.  It is defined in terms of photons (or electrons) and scales
+to the data values through the gain parameter.  A image header keyword
+(case insensitive) may be specified to get the value from the image.
+.le
+.ls gain = "GAIN" (apsum)
+Detector gain or conversion factor between photons/electrons and
+data values.  It is specified as the number of photons per data value.
+A image header keyword (case insensitive) may be specified to get the value
+from the image.
+.le
+.ls datamax = INDEF (apsum.saturation)
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the flat field or
+arc spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.le
+.ls fibers = 97 (apfind)
+Number of fibers.  This number is used during the automatic definition of
+the apertures from the aperture reference spectrum.  It is best if this
+reflects the actual number of fibers which may be found in the aperture
+reference image.
+The interactive
+review of the aperture assignments allows verification and adjustments
+to the automatic aperture definitions.
+.le
+.ls width = 12. (apedit)
+Approximate base full width of the fiber profiles.  This parameter is used
+for the profile centering algorithm.
+.le
+.ls minsep = 8. (apfind)
+Minimum separation between fibers.  Weaker spectra or noise within this
+distance of a stronger spectrum are rejected.
+.le
+.ls maxsep = 15. (apfind)
+Maximum separation between adjacent fibers.  This parameter
+is used to identify missing fibers.  If two adjacent spectra exceed this
+separation then it is assumed that a fiber is missing and the aperture
+identification assignments will be adjusted accordingly.
+.le
+.ls apidtable = "" (apfind)
+Aperture identification table.  This may be either a text file or an
+image.  A text file contains the fiber number, beam number defining object
+(1), sky (0), and arc (2) fibers, and a object title.  An image contains
+the keywords SLFIBnnn with string value consisting of the fiber number,
+beam number, optional right ascension and declination, and an object
+title.  For Nessie the user had to prepare the file for each plugboard, for
+Hydra at the 4meter the file was generated for the user, and for Hydra at
+the WIYN the image header contains the information.  Unassigned and broken
+fibers (beam of -1) should be included in the identification information
+since they will automatically be excluded.
+.le
+.ls crval = INDEF, cdelt = INDEF (autoidentify)
+These parameters specify an approximate central wavelength and dispersion.
+They may be specified as numerical values, INDEF, or image header keyword
+names whose values are to be used.
+If both these parameters are INDEF then the automatic identification will
+not be done.
+.le
+.ls objaps = "", skyaps = "", arcaps = ""
+List of object, sky, and arc aperture numbers.  These are used to
+identify arc apertures for wavelength calibration and object and sky
+apertures for sky subtraction.  Note sky apertures may be identified as
+both object and sky if one wants to subtract the mean sky from the
+individual sky spectra.  Typically the different spectrum types are
+identified by their beam numbers and the default, null string,
+lists select all apertures.
+.le
+.ls objbeams = "0,1", skybeams = "0", arcbeams = 2
+List of object, sky, and arc beam numbers.  The convention is that sky
+fibers are given a beam number of 0, object fibers a beam number of 1, and
+arc fibers a beam number of 2.  The beam numbers are typically set in the
+\fIapidtable\fR.  Unassigned or broken fibers may be given a beam number of
+-1 in the aperture identification table since apertures with negative beam
+numbers are not extracted.  Note it is valid to identify sky fibers as both
+object and sky.
+.le
+
+.ls scattered = no (apscatter)
+Smooth and subtracted scattered light from the object and flat field
+images.  This operation consists of fitting independent smooth functions
+across the dispersion using data outside the fiber apertures and then
+smoothing the individual fits along the dispersion.  The initial
+flat field, or if none is given the aperture reference image, are
+done interactively to allow setting the fitting parameters.  All
+subsequent subtractions use the same fitting parameters.
+.le
+.ls fitflat = yes (flat1d)
+Fit the composite flat field spectrum by a smooth function and divide each
+flat field spectrum by this function?  This operation removes the average
+spectral signature of the flat field lamp from the sensitivity correction to
+avoid modifying the object fluxes.
+.le
+.ls clean = yes (apsum)
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction and requires reasonably good values
+for the readout noise and gain.  In addition the datamax parameters
+can be useful.
+.le
+.ls dispcor = yes
+Dispersion correct spectra?  Depending on the \fIparams.linearize\fR
+parameter this may either resample the spectra or insert a dispersion
+function in the image header.
+.le
+.ls savearcs = yes
+Save any simultaneous arc apertures?  If no then the arc apertures will
+be deleted after use.
+.le
+.ls skyalign = no
+Align sky lines?  If yes then for the first object spectrum you are asked
+to mark one or more sky lines to use for alignment.  Then these lines will
+be found in all spectra and an average zeropoint shift computed and applied
+to the dispersion solution to align these lines.  Note that this assumes
+the sky lines are seen in all fibers.
+.le
+.ls skysubtract = yes
+Subtract sky from the object spectra?  If yes the sky spectra are combined
+and subtracted from the object spectra as defined by the object and sky
+aperture/beam parameters.
+.le
+.ls skyedit = yes
+Overplot all the sky spectra and allow contaminated sky spectra to be
+deleted?
+.le
+.ls saveskys = yes
+Save the combined sky spectrum?  If no then the sky spectrum will be
+deleted after sky subtraction is completed.
+.le
+.ls splot = no
+Plot the final spectra with the task \fBsplot\fR?
+.le
+.ls redo = no
+Redo operations previously done?  If no then previously processed spectra
+in the objects list will not be processed (unless they need to be updated).
+.le
+.ls update = yes
+Update processing of previously processed spectra if aperture, flat
+field, or dispersion reference definitions are changed?
+.le
+.ls batch = no
+Process spectra as a background or batch job provided there are no interactive
+options (\fIskyedit\fR and \fIsplot\fR) selected.
+.le
+.ls listonly = no
+List processing steps but don't process?
+.le
+
+.ls params = "" (pset)
+Name of parameter set containing additional processing parameters.  The
+default is parameter set \fBparams\fR.  The parameter set may be examined
+and modified in the usual ways (typically with "epar params" or ":e params"
+from the parameter editor).  Note that using a different parameter file
+is not allowed.  The parameters are described below.
+.le
+
+.ce
+-- PACKAGE PARAMETERS
+
+Package parameters are those which generally apply to all task in the
+package.  This is also true of \fBdohydra\fR.
+.ls dispaxis = 2
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.  The default value defers to the
+package parameter of the same name.
+.le
+.ls observatory = "observatory"
+Observatory at which the spectra were obtained if not specified in the
+image header by the keyword OBSERVAT.  For Hydra data the image headers
+identify the observatory as "kpno" so this parameter is not used.
+For data from other observatories this parameter may be used
+as describe in \fBobservatory\fR.
+.le
+.ls interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc)
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.nf
+	nearest - nearest neighbor
+	 linear - linear
+	  poly3 - 3rd order polynomial
+	  poly5 - 5th order polynomial
+	spline3 - cubic spline
+	   sinc - sinc function
+.fi
+.le
+.ls database = "database"
+Database (directory) used for storing aperture and dispersion information.
+.le
+.ls verbose = no
+Print verbose information available with various tasks.
+.le
+.ls logfile = "logfile", plotfile = ""
+Text and plot log files.  If a filename is not specified then no log is
+kept.  The plot file contains IRAF graphics metacode which may be examined
+in various ways such as with \fBgkimosaic\fR.
+.le
+.ls records = ""
+Dummy parameter to be ignored.
+.le
+.ls version = "HYDRA: ..."
+Version of the package.
+.le
+
+.ce
+PARAMS PARAMETERS
+
+The following parameters are part of the \fBparams\fR parameter set and
+define various algorithm parameters for \fBdohydra\fR.
+
+.ce
+--  GENERAL PARAMETERS --
+.ls line = INDEF, nsum = 10
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, recentering, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.le
+.ls order = "decreasing" (apfind)
+When assigning aperture identifications order the spectra "increasing"
+or "decreasing" with increasing pixel position (left-to-right or
+right-to-left in a cross-section plot of the image).
+.le
+.ls extras = no (apsum)
+Include extra information in the output spectra?  When cleaning or using
+variance weighting the cleaned and weighted spectra are recorded in the
+first 2D plane of a 3D image, the raw, simple sum spectra are recorded in
+the second plane, and the estimated sigmas are recorded in the third plane.
+.le
+
+.ce
+-- DEFAULT APERTURE LIMITS --
+.ls lower = -5., upper = 5. (apdefault)
+Default lower and upper aperture limits relative to the aperture center.
+These limits are used when the apertures are first found and may be
+resized automatically or interactively.
+.le
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+.ls ylevel = 0.05 (apresize)
+Data level at which to set aperture limits during automatic resizing.
+It is a fraction of the peak relative to a local background.
+.le
+
+.ce
+-- TRACE PARAMETERS --
+.ls t_step = 10 (aptrace)
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \fInsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.le
+.ls t_function = "spline3", t_order = 3 (aptrace)
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.le
+.ls t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+Default number of rejection iterations and rejection sigma thresholds.
+.le
+
+.ce
+-- SCATTERED LIGHT PARAMETERS --
+.ls buffer = 1. (apscatter)
+Buffer distance from the aperture edges to be excluded in selecting the
+scattered light pixels to be used.
+.le
+.ls apscat1 = "" (apscatter)
+Fitting parameters across the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat1"
+parameter set.
+.le
+.ls apscat2 = "" (apscatter)
+Fitting parameters along the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat2"
+parameter set.
+.le
+
+.ce
+
+-- APERTURE EXTRACTION PARAMETERS --
+.ls weights = "none" (apsum)
+Type of extraction weighting.  Note that if the \fIclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+.ls "none"
+The pixels are summed without weights except for partial pixels at the
+ends.
+.le
+.ls "variance"
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \fIgain\fR and \fIreadnoise\fR
+parameters.
+.le
+.le
+.ls pfit = "fit1d" (apsum) (fit1d|fit2d)
+Profile fitting algorithm for cleaning and variance weighted extractions.
+The default is generally appropriate for Hydra/Nessie data but users
+may try the other algorithm.  See \fBapprofiles\fR for further information.
+.le
+.ls lsigma = 3., usigma = 3. (apsum)
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.le
+.ls nsubaps = 1 (apsum)
+During extraction it is possible to equally divide the apertures into
+this number of subapertures.
+.le
+
+.ce
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --
+.ls f_interactive = yes (fit1d)
+Fit the composite one dimensional flat field spectrum interactively?
+This is used if \fIfitflat\fR is set and a two dimensional flat field
+spectrum is specified.
+.le
+.ls f_function = "spline3", f_order = 10 (fit1d)
+Function and order used to fit the composite one dimensional flat field
+spectrum.  The functions are "legendre", "chebyshev", "spline1", and
+"spline3".  The spline functions are linear and cubic splines with the
+order specifying the number of pieces.
+.le
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+.ls threshold = 10. (autoidentify/identify/reidentify)
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.le
+.ls coordlist = "linelists$idhenear.dat" (autoidentify/identify)
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelists$".
+.le
+.ls match = -3. (autoidentify/identify)
+The maximum difference for a match between the dispersion function prediction
+value and a wavelength in the coordinate list.
+.le
+.ls fwidth = 4. (autoidentify/identify)
+Approximate full base width (in pixels) of arc lines.
+.le
+.ls cradius = 10. (reidentify)
+Radius from previous position to reidentify arc line.
+.le
+.ls i_function = "spline3", i_order = 3 (autoidentify/identify)
+The default function and order to be fit to the arc wavelengths as a
+function of the pixel coordinate.  The functions choices are "chebyshev",
+"legendre", "spline1", or "spline3".
+.le
+.ls i_niterate = 2, i_low = 3.0, i_high = 3.0 (autoidentify/identify)
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.le
+.ls refit = yes (reidentify)
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.le
+.ls addfeatures = no (reidentify)
+Add new features from a line list during each reidentification?
+This option can be used to compensate for lost features from the
+reference solution.  Care should be exercised that misidentified features
+are not introduced.
+.le
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+.ls select = "interp" (refspectra)
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+.ls average
+Average two reference spectra without regard to any sort parameter.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.
+This option is used to assign two reference spectra, with equal weights,
+independent of any sorting parameter.
+.le
+.ls following
+Select the nearest following spectrum in the reference list based on the
+sorting parameter.  If there is no following spectrum use the nearest preceding
+spectrum.
+.le
+.ls interp
+Interpolate between the preceding and following spectra in the reference
+list based on the sorting parameter.  If there is no preceding and following
+spectrum use the nearest spectrum.  The interpolation is weighted by the
+relative distances of the sorting parameter.
+.le
+.ls match
+Match each input spectrum with the reference spectrum list in order.
+This overrides the reference aperture check.
+.le
+.ls nearest
+Select the nearest spectrum in the reference list based on the sorting
+parameter.
+.le
+.ls preceding
+Select the nearest preceding spectrum in the reference list based on the
+sorting parameter.  If there is no preceding spectrum use the nearest following
+spectrum.
+.le
+.le
+.ls sort = "jd", group = "ljd" (refspectra)
+Image header keywords to be used as the sorting parameter for selection
+based on order and to group spectra.
+A null string, "", or the word "none" may be use to disable the sorting
+or grouping parameters.
+The sorting parameter
+must be numeric but otherwise may be anything.  The grouping parameter
+may be a string or number and must simply be the same for all spectra within
+the same group (say a single night).
+Common sorting parameters are times or positions.
+In \fBdohydra\fR the Julian date (JD) and the local Julian day number (LJD)
+at the middle of the exposure are automatically computed from the universal
+time at the beginning of the exposure and the exposure time.  Also the
+parameter UTMIDDLE is computed.
+.le
+.ls time = no, timewrap = 17. (refspectra)
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.le
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+.ls linearize = yes (dispcor)
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling
+If no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data are not interpolated.
+.le
+.ls log = no (dispcor)
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.le
+.ls flux = yes (dispcor)
+Conserve the total flux during interpolation?  If \fIno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \fIyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.le
+
+.ce
+-- SKY SUBTRACTION PARAMETERS --
+.ls combine = "average" (scombine) (average|median)
+Option for combining sky pixels at the same dispersion coordinate after any
+rejection operation.  The options are to compute the  "average" or "median"
+of the pixels.  The median uses the average of the two central
+values when the number of pixels is even.
+.le
+.ls reject = "none" (scombine) (none|minmax|avsigclip)
+Type of rejection operation performed on the pixels which overlap at each
+dispersion coordinate.  The algorithms are discussed in the
+help for \fBscombine\fR.  The rejection choices are:
+
+.nf
+      none - No rejection
+    minmax - Reject the low and high pixels
+ avsigclip - Reject pixels using an averaged sigma clipping algorithm
+.fi
+
+.le
+.ls scale = "none" (none|mode|median|mean)
+Multiplicative scaling to be applied to each spectrum.  The choices are none
+or scale by the mode, median, or mean.  This should not be necessary if the
+flat field and throughput corrections have been properly made. 
+.le
+.ih
+ENVIRONMENT PARAMETERS
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
+.ih
+DESCRIPTION
+The \fBdohydra\fR reduction task is specialized for the extraction, flat
+fielding, fiber throughput correction, wavelength calibration, and sky
+subtraction of \fIHydra\fR and \fINessie\fR fiber spectra.  It is a
+command language script which collects and combines the functions and
+parameters of many general purpose tasks to provide a single, complete data
+reduction path.  The task provides a degree of guidance, automation, and
+record keeping necessary when dealing with the large amount of data
+generated by these multifiber instruments.
+
+The general organization of the task is to do the interactive setup steps
+first using representative calibration data and then perform the majority
+of the reductions automatically, and possibly as a background process, with
+reference to the setup data.  In addition, the task determines which setup
+and processing operations have been completed in previous executions of the
+task and, contingent on the \fIredo\fR and \fIupdate\fR options, skip or
+repeat some or all the steps.
+
+The following description is oriented specifically to Hydra data but
+applies equally well to Nessie data except for a few minor differences
+which are discussed in a separate section.  Since \fBdohydra\fR combines many
+separate, general purpose tasks the description given here refers to these
+tasks and leaves some of the details to their help documentation.
+
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage for
+Hydra since there are many variations possible.
+
+\fBUsage Outline\fR
+
+.ls 6 [1]
+The images are first processed with \fBccdproc\fR for overscan,
+bias, and dark corrections.
+The \fBdofiber\fR task will abort if the image header keyword CCDRPOC,
+which is added by \fBccdproc\fR, is missing.  If the data is processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+.le
+.ls [2]
+Set the \fBdohydra\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed, the flat field image as the aperture reference and
+the flat field, and one or more arc images.  A throughput file or image,
+such as a blank sky observation, may also be specified.  If there are many
+object or arc spectra per setup you might want to prepare "@ files".
+Specify the aperture identification table (a file for 4meter data or an image
+for WIYN data) which is provided for each Hydra
+configuration.  You might wish to verify the geometry parameters,
+separations, dispersion direction, etc., which may
+change with different detector setups.  The processing parameters are set
+for complete reductions but for quicklook you might not use the clean
+option or dispersion calibration and sky subtraction.
+
+The parameters are set for a particular Hydra configuration and different
+configurations may use different flat fields, arcs, and aperture
+identification tables.
+.le
+.ls [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the execution and no further queries of that
+type will be made.
+.le
+.ls [4]
+The apertures are defined using the specified aperture reference image.
+The spectra are found automatically and apertures assigned based on
+task parameters and the aperture identification table.  Unassigned
+fibers will have a negative beam number and will be ignored in subsequent
+processing.  The resize option sets the aperture size to the widths of
+the profiles at a fixed fraction of the peak height.  The interactive
+review of the apertures is recommended.  If the identifications are off
+by a shift the 'o' key is used.  To exit the aperture review type 'q'.
+.le
+.ls [5]
+The fiber positions at a series of points along the dispersion are measured
+and a function is fit to these positions.  This may be done interactively to
+adjust the fitting parameters.  Not all fibers need be examined and the "NO"
+response will quit the interactive fitting.  To exit the interactive
+fitting type 'q'.
+.le
+.ls [6]
+If scattered light subtraction is to be done the flat field image is
+used to define the scattered light fitting parameters interactively.
+If one is not specified then the aperture reference image is used for
+this purpose.
+
+There are two queries for the interactive fitting.  A graph of the
+data between the defined reference apertures separated by a specified
+buffer distance is first shown.  The function order and type may be
+adjusted.  After quiting with 'q' the user has the option of changing
+the buffer value and returning to the fitting, changing the image line
+or column to check if the fit parameters are satisfactory at other points,
+or to quit and accept the fit parameters.  After fitting all points
+across the dispersion another graph showing the scattered light from
+the individual fits is shown and the smoothing parameters along the
+dispersion may be adjusted.  Upon quiting with 'q' you have the option
+of checking other cuts parallel to the dispersion or quiting and finishing
+the scattered light function smoothing and subtraction.
+
+If there is a throughput image then this is corrected for scattered light
+noninteractively using the previous fitting parameters.
+.le
+.ls [7]
+If flat fielding is to be done the flat field spectra are extracted.  The
+average spectrum over all fibers is determined and a function is fit
+interactively (exit with 'q').  This function is generally of sufficiently
+high order that the overall shape is well fit.  This function is then used
+to normalize the individual flat field spectra.  If a throughput image, a
+sky flat, is specified then the total sky counts through each fiber are
+used to correct the total flat field counts.  Alternatively, a separately
+derived throughput file can be used for specifying throughput corrections.
+If neither type of throughput is used the flat field also provides the
+throughput correction.  The final response spectra are normalized to a unit
+mean over all fibers.  The relative average throughput for each fiber is
+recorded in the log and possibly printed to the terminal.
+.le
+.ls [8]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  The middle fiber is used to identify the arc lines and define
+the dispersion function using the task \fBautoidentify\fR.  The
+\fIcrval\fR and \fIcdelt\fR parameters are used in the automatic
+identification.  Whether or not the automatic identification is
+successful you will be shown the result of the arc line identification.
+If the automatic identification is not successful identify a few arc
+lines with 'm' and use the 'l' line list identification command to
+automatically add additional lines and fit the dispersion function.  Check
+the quality of the dispersion function fit with 'f'.  When satisfied exit
+with 'q'.
+.le
+.ls [9]
+The remaining fibers are automatically reidentified.  You have the option
+to review the line identifications and dispersion function for each fiber
+and interactively add or delete arc lines and change fitting parameters.
+This can be done selectively, such as when the reported RMS increases
+significantly.
+.le
+.ls [10]
+If the spectra are to be resampled to a linear dispersion system
+(which will be the same for all spectra) default dispersion parameters
+are printed and you are allowed to adjust these as desired.
+.le
+.ls [11]
+If the sky line alignment option is selected and the sky lines have not
+been identified for a particular aperture identification table then you are
+asked to mark one or more sky lines.  You may simply accept the wavelengths
+of these lines as defined by the dispersion solution for this spectrum and
+fiber or you may specify knowns wavelengths for the lines. These lines will
+be reidentified in all object spectra extracted and a mean zeropoint shift
+will be added to the dispersion solution.  This has the effect of aligning
+these lines to optimize sky subtraction.
+.le
+.ls [12]
+The object spectra are now automatically scattered light subtracted,
+extracted, flat fielded, and dispersion corrected.
+.le
+.ls [13]
+When sky subtracting, the individual sky spectra may be reviewed and some
+spectra eliminated using the 'd' key.  The last deleted spectrum may be
+recovered with the 'e' key.  After exiting the review with 'q' you are
+asked for the combining option.  The type of combining is dictated by the
+number of sky fibers.
+.le
+.ls [14]
+The option to examine the final spectra with \fBsplot\fR may be given.
+To exit type 'q'.
+.le
+.ls [15]
+If scattered light is subtracted from the input data a copy of the
+original image is made by appending "noscat" to the image name.
+If the data are reprocessed with the \fIredo\fR flag the original
+image will be used again to allow modification of the scattered
+light parameters.
+
+The final spectra will have the same name as the original 2D images
+with a ".ms" extension added.  The flat field and arc spectra will
+also have part of the aperture identification table name added to
+allow different configurations to use the same 2D flat field and arcs
+but with different aperture definitions.  If using the sky alignment
+option an image "align" with the aperture identification table name
+applied will also be created.
+.le
+
+\fBSpectra and Data Files\fR
+
+The basic input consists of Hydra or Nessie object and
+calibration spectra stored as IRAF images.
+The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+The raw CCD images must
+be processed to remove overscan, bias, and dark count effects.
+This is generally done using the \fBccdred\fR package.
+The \fBdohydra\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+Flat fielding is
+generally not done at this stage but as part of \fBdohydra\fR.
+If flat fielding is done as part of the basic CCD processing then
+a flattened flat field, blank sky observation, or throughput file
+should still be created for applying fiber throughput corrections.
+
+The task \fBdohydra\fR uses several types of calibration spectra.  These
+are flat fields, blank sky flat fields, comparison lamp spectra, auxiliary
+mercury line (from the dome lights) or sky line spectra, and simultaneous
+arc spectra taken during the object observation.  The flat field,
+throughput image or file, auxiliary emission line spectra, and simultaneous
+comparison fibers are optional.  If a flat field is used then the sky flat
+or throughput file is optional assuming the flat field has the same fiber
+iillumination.  It is legal to specify only a throughput image or file and
+leave the flat field blank in order to simply apply a throughput
+correction.  Because only the total counts through each fiber are used from
+a throughput image, sky flat exposures need not be of high signal per
+pixel.
+
+There are three types of arc calibration methods.  One is to take arc
+calibration exposures through all fibers periodically and apply the
+dispersion function derived from one or interpolated between pairs to the
+object fibers.  This is the usual method with Hydra.  Another method is to
+use only one or two all-fiber arcs to define the shape of the dispersion
+function and track zero point wavelength shifts with \fIsimultaneous arc\fR
+fibers taken during the object exposure.  The simultaneous arcs may or may
+not be available at the instrument but \fBdohydra\fR can use this type of
+observation.  The arc fibers are identified by their beam or aperture
+numbers.  A related and mutually exclusive method is to use \fIauxiliary
+line spectra\fR such as lines in the dome lights or sky lines to monitor
+shifts relative to a few actual arc exposures.  The main reason to do this
+is if taking arc exposures through all fibers is inconvenient as is the
+case with the manual Nessie plugboards.
+
+The assignment of arc or auxiliary line calibration exposures to object
+exposures is generally done by selecting the nearest in time and
+interpolating.  There are other options possible which are described under
+the task \fBrefspectra\fR.  The most general option is to define a table
+giving the object image name and the one or two arc spectra to be assigned
+to that object.  That file is called an \fIarc assignment table\fR and it
+is one of the optional setup files which can used with \fBdohydra\fR.
+
+The first step in the processing is identifying the spectra in the images.
+The \fIaperture identification table\fR, which may be a text file or
+an image, contains information about the fiber
+assignments.  This table is created for you when using Hydra but must be
+prepared by the user when using Nessie.  A description of a file is
+given in the section concerning Nessie.
+
+The final reduced spectra are recorded in two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ms" extension.  Each line in the reduced image is a one dimensional
+spectrum with associated aperture, wavelength, and identification
+information.  When the \fIextras\fR parameter is set the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tools such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.  The special task \fBscopy\fR may be used to extract
+specific apertures or to change format to individual one dimensional
+images.
+
+\fBPackage Parameters\fR
+
+The \fBhydra\fR package parameters set parameters affecting all the
+tasks in the package.
+The dispersion axis parameter defines the image axis along which the
+dispersion runs.  This is used if the image header doesn't define the
+dispersion axis with the DISPAXIS keyword.
+The observatory parameter is only required
+for data taken with fiber instruments other than Hydra or Nessie.
+The spectrum interpolation type might be changed to "sinc" but
+with the cautions given in \fBonedspec.package\fR.
+The other parameters define the standard I/O functions.
+The verbose parameter selects whether to print everything which goes
+into the log file on the terminal.  It is useful for monitoring
+what the \fBdohydra\fR task does.  The log and plot files are useful for
+keeping a record of the processing.  A log file is highly recommended.
+A plot file provides a record of apertures, traces, and extracted spectra
+but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+
+\fBProcessing Parameters\fR
+
+The list of objects and arcs can be @ files if desired.  The aperture
+reference spectrum is usually the same as the flat field spectrum though it
+could be any exposure with enough signal to accurately define the positions
+and trace the spectra.  The first list of arcs are the standard Th-Ar or
+HeNeAr comparison arc spectra (they must all be of the same type).  The
+second list of arcs are the auxiliary emission line exposures mentioned
+previously and in the Nessie section.
+
+The arc replacement file is described in the Nessie section and the arc
+assignment table was described in the data file section.  Note that even if
+an arc assignment table is specified, \fIall arcs to be used must also
+appear in the arc lists\fR in order for the task to know the type of arc
+spectrum.
+
+The detector read out noise and gain are used for cleaning and variance
+(optimal) extraction.  The default will determine the values from the image
+itself.  The dispersion axis defines the wavelength direction of spectra in
+the image if not defined in the image header by the keyword DISPAXIS.  The
+width and separation parameters define the dimensions (in pixels) of the
+spectra (fiber profile) across the dispersion.  The width parameter
+primarily affects the centering.  The maximum separation parameter is
+important if missing spectra from the aperture identification table are to
+be correctly skipped.  The number of fibers can be left at the default
+(for Hydra) and the task will try to account for unassigned or missing fibers.
+
+The approximate central wavelength and dispersion are used for the
+automatic identification of the arc reference.  They may be specified
+as image header keywords or values.  The INDEF values search the
+entire range of the coordinate reference file but the automatic
+line identification algorithm works much better and faster if
+approximate values are given.
+
+The task needs to know which fibers are object, sky if sky subtraction is
+to be done, and simultaneous arcs if used.  One could explicitly give the
+aperture numbers but the recommended way, provided an aperture
+identification file or image is used, is to select the apertures based on
+the beam numbers.  The default values are those appropriate for the
+identification files generated for Hydra configurations.  Sky subtracted
+sky spectra are useful for evaluating the sky subtraction.  Since only the
+spectra identified as objects are sky subtracted one can exclude fibers
+from the sky subtraction.  For example, if the \fIobjbeams\fR parameter is
+set to 1 then only those fibers with a beam of 1 will be sky subtracted.
+All other fibers will remain in the extracted spectra but will not be sky
+subtracted.
+
+The next set of parameters select the processing steps and options.  The
+scattered light option allows fitting and subtracting a scattered light
+surface from the input object and flat field.  If there is significant
+scattered light which is not subtracted the fiber throughput correction
+will not be accurate.  The
+flat fitting option allows fitting and removing the overall shape of the
+flat field spectra while preserving the pixel-to-pixel response
+corrections.  This is useful for maintaining the approximate object count
+levels and not introducing the reciprocal of the flat field spectrum into
+the object spectra.  The \fIclean\fR option invokes a profile fitting and
+deviant point rejection algorithm as well as a variance weighting of points
+in the aperture.  These options require knowing the effective (i.e.
+accounting for any image combining) read out noise and gain.  For a
+discussion of cleaning and variance weighted extraction see
+\fBapvariance\fR and \fBapprofiles\fR.
+
+The dispersion correction option selects whether to extract arc spectra,
+determine a dispersion function, assign them to the object spectra, and,
+possibly, resample the spectra to a linear (or log-linear) wavelength
+scale.  If simultaneous arc fibers are defined there is an option to delete
+them from the final spectra when they are no longer needed.
+
+The sky alignment option allows applying a zeropoint dispersion shift
+to all fibers based on one or more sky lines.  This requires all fibers
+to have the sky lines visible.  When there are sky lines this will
+improve the sky subtraction if there is a systematic error in the
+fiber iillumination between the sky and the arc calibration.
+
+The sky subtraction option selects whether to combine the sky fiber spectra
+and subtract this sky from the object fiber spectra.  \fIDispersion
+correction and sky subtraction are independent operations.\fR  This means
+that if dispersion correction is not done then the sky subtraction will be
+done with respect to pixel coordinates.  This might be desirable in some
+quick look cases though it is incorrect for final reductions.
+
+The sky subtraction option has two additional options.  The individual sky
+spectra may be examined and contaminated spectra deleted interactively
+before combining.  This can be a useful feature in crowded regions.  The
+final combined sky spectrum may be saved for later inspection in an image
+with the spectrum name prefixed by \fBsky\fR.
+
+After a spectrum has been processed it is possible to examine the results
+interactively using the \fBsplot\fR tasks.  This option has a query which
+may be turned off with "YES" or "NO" if there are multiple spectra to be
+processed.
+
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\fIupdate\fR flag is set.  The changes which will cause an update are new
+aperture identification table, new reference image, new flat fields, and a
+new arc reference.  If all input spectra are to be processed regardless of
+previous processing the \fIredo\fR flag may be used.  Note that
+reprocessing clobbers the previously processed output spectra.
+
+The \fIbatch\fR processing option allows object spectra to be processed as
+a background or batch job.  This will only occur if sky spectra editing and
+\fBsplot\fR review (interactive operations) are turned off, either when the
+task is run or by responding with "NO" to the queries during processing.
+
+The \fIlistonly\fR option prints a summary of the processing steps which
+will be performed on the input spectra without actually doing anything.
+This is useful for verifying which spectra will be affected if the input
+list contains previously processed spectra.  The listing does not include
+any arc spectra which may be extracted to dispersion calibrate an object
+spectrum.
+
+The last parameter (excluding the task mode parameter) points to another
+parameter set for the algorithm parameters.  The way \fBdohydra\fR works
+this may not have any value and the parameter set \fBparams\fR is always
+used.  The algorithm parameters are discussed further in the next section.
+
+\fBAlgorithms and Algorithm Parameters\fR
+
+This section summarizes the various algorithms used by the \fBdohydra\fR
+task and the parameters which control and modify the algorithms.  The
+algorithm parameters available to the user are collected in the parameter
+set \fBparams\fR.  These parameters are taken from the various general
+purpose tasks used by the \fBdohydra\fR processing task.  Additional
+information about these parameters and algorithms may be found in the help
+for the actual task executed.  These tasks are identified in the parameter
+section listing in parenthesis.  The aim of this parameter set organization
+is to collect all the algorithm parameters in one place separate from the
+processing parameters and include only those which are relevant for
+Hydra or Nessie data.  The parameter values can be changed from the
+defaults by using the parameter editor,
+.nf
+
+	cl> epar params
+
+.fi
+or simple typing \fIparams\fR.  The parameter editor can also be
+entered when editing the \fBdohydra\fR parameters by typing \fI:e
+params\fR or simply \fI:e\fR if positioned at the \fIparams\fR
+parameter.
+
+\fBExtraction\fR
+
+The identification of the spectra in the two dimensional images and their
+scattered light subtraction and extraction to one dimensional spectra
+in multispec format is accomplished
+using the tasks from the \fBapextract\fR package.  The first parameters
+through \fInsubaps\fR control the extractions.
+
+The dispersion line is that used for finding the spectra, for plotting in
+the aperture editor, and as the starting point for tracing.  The default
+value of \fBINDEF\fR selects the middle of the image.  The aperture
+finding, adjusting, editing, and tracing operations also allow summing a
+number of dispersion lines to improve the signal.  The number of lines is
+set by the \fInsum\fR parameter.
+
+The \fIorder\fR parameter defines whether the order of the aperture
+identifications in the aperture identification table (or the default
+sequential numbers if no file is used) is in the same sense as the image
+coordinates (increasing) or the opposite sense (decreasing).  If the
+aperture identifications turn out to be opposite to what is desired when
+viewed in the aperture editing graph then simply change this parameter.
+
+The basic data output by the spectral extraction routines are the one
+dimensional spectra.  Additional information may be output when the
+\fIextras\fR option is selected and the cleaning or variance weighting
+options are also selected.  In this case a three dimensional image is
+produced with the first element of the third dimension being the cleaned
+and/or weighted spectra, the second element being the uncleaned and
+unweighted spectra, and the third element being an estimate of the sigma
+of each pixel in the extracted spectrum.  Currently the sigma data is not
+used by any other tasks and is only for reference.
+
+The initial step of finding the fiber spectra in the aperture reference
+image consists of identifying the peaks in a cut across the dispersion,
+eliminating those which are closer to each other than the \fIminsep\fR
+distance, and then keeping the specified \fInfibers\fR highest peaks.  The
+centers of the profiles are determined using the \fBcenter1d\fR algorithm
+which uses the \fIwidth\fR parameter.
+
+Apertures are then assigned to each spectrum.  The initial edges of the
+aperture relative to the center are defined by the \fIlower\fR and
+\fIupper\fR parameters.  The trickiest part of assigning the apertures is
+relating the aperture identification from the aperture identification table
+to automatically selected fiber profiles.  The first aperture id in the
+file is assigned to the first spectrum found using the \fIorder\fR parameter to
+select the assignment direction.  The numbering proceeds in this way except
+that if a gap greater than a multiple of the \fImaxsep\fR parameter is
+encountered then assignments in the file are skipped under the assumption
+that a fiber is missing (broken).  In Hydra data it is expected that all
+fibers will be found in flat fields including the unassigned fibers and the
+assignment file will then identify the unassigned fibers.  The unassigned
+fibers will later be excluded from extraction.  For more on the finding and
+assignment algorithms see \fBapfind\fR.
+
+The initial apertures are the same for all spectra but they can each be
+automatically resized.  The automatic resizing sets the aperture limits
+at a fraction of the peak relative to the interfiber minimum.
+The default \fIylevel\fR is to resize the apertures to 5% of the peak.
+See the description for the task \fBapresize\fR for further details.
+
+The user is given the opportunity to graphically review and adjust the
+aperture definitions.  This is recommended.  As mentioned previously, the
+correct identification of the fibers is tricky and it is fundamentally
+important that this be done correctly; otherwise the spectrum
+identifications will not be for the objects they say.  An important command in
+this regard is the 'o' key which allows reordering the identifications
+based on the aperture identification table.  This is required if the first
+fiber is actually missing since the initial assignment begins assigning the
+first spectrum found with the first entry in the aperture file.  The
+aperture editor is a very powerful tool and is described in detail as
+\fBapedit\fR.
+
+The next set of parameters control the tracing and function fitting of the
+aperture reference positions along the dispersion direction.  The position
+of a spectrum across the dispersion is determined by the centering
+algorithm (see \fBcenter1d\fR) at a series of evenly spaced steps, given by
+the parameter \fIt_step\fR, along the dispersion.  The step size should be
+fine enough to follow position changes but it is not necessary to measure
+every point.  The fitted points may jump around a little bit due to noise
+and cosmic rays even when summing a number of lines.  Thus, a smooth
+function is fit.  The function type, order, and iterative rejection of
+deviant points is controlled by the other trace parameters.  For more
+discussion consult the help pages for \fBaptrace\fR and \fBicfit\fR.  The
+default is to fit a cubic spline of three pieces with a single iteration of
+3 sigma rejection.
+
+The actual extraction of the spectra by summing across the aperture at each
+point along the dispersion is controlled by the next set of parameters.
+The default extraction simply sums the pixels using partial pixels at the
+ends.  The options allow selection of a weighted sum based on a Poisson
+variance model using the \fIreadnoise\fR and \fIgain\fR detector
+parameters.  Note that if the \fIclean\fR option is selected the variance
+weighted extraction is used regardless of the \fIweights\fR parameter.  The
+sigma thresholds for cleaning are also set in the \fBparams\fR parameters.
+For more on the variance weighted extraction and cleaning see
+\fBapvariance\fR and \fBapprofiles\fR as well as \fBapsum\fR.
+
+The last parameter, \fInsubaps\fR, is used only in special cases when it is
+desired to subdivide the fiber profiles into subapertures prior to
+dispersion correction.  After dispersion correction the subapertures are
+then added together.  The purpose of this is to correct for wavelength
+shifts across a fiber.
+
+\fBScattered Light Subtraction\fR
+
+Scattered light may be subtracted from the input two dimensional image as
+the first step.  This is done using the algorithm described in
+\fBapscatter\fR.  This can be important if there is significant scattered
+light since the flat field/throughput correction will otherwise be
+incorrect.  The algorithm consists of fitting a function to the data
+outside the defined apertures by a specified \fIbuffer\fR at each line or
+column across the dispersion.  The function fitting parameters are the same
+at each line.  Because the fitted functions are independent at each line or
+column a second set of one dimensional functions are fit parallel to the
+dispersion using the evaluated fit values from the cross-dispersion step.
+This produces a smooth scattered light surface which is finally subtracted
+from the input image.  Again the function fitting parameters are the
+same at each line or column though they may be different than the parameters
+used to fit across the dispersion.
+
+The first time the task is run with a particular flat field (or aperture
+reference image if no flat field is used) the scattered light fitting
+parameters are set interactively using that image.  The interactive step
+selects a particular line or column upon which the fitting is done
+interactively with the \fBicfit\fR commands.  A query is first issued
+which allows skipping this interactive stage.  Note that the interactive
+fitting is only for defining the fitting functions and orders.  When
+the graphical \fBicfit\fR fitting is exited (with 'q') there is a second prompt
+allowing you to change the buffer distance (in the first cross-dispersion
+stage) from the apertures, change the line/column, or finally quit.
+
+The initial fitting parameters and the final set parameters are recorded
+in the \fBapscat1\fR and \fBapscat2\fR hidden parameter sets.  These
+parameters are then used automatically for every subsequent image
+which is scattered light corrected.
+
+The scattered light subtraction modifies the input 2D images.  To preserve
+the original data a copy of the original image is made with the same
+root name and the word "noscat" appended.  The scattered light subtracted
+images will have the header keyword "APSCATTE" which is how the task
+avoids repeating the scattered light subtraction during any reprocessing.
+However if the \fIredo\fR option is selected the scattered light subtraction
+will also be redone by first restoring the "noscat" images to the original
+input names.
+
+\fBFlat Field and Fiber Throughput Corrections\fR
+
+Flat field corrections may be made during the basic CCD processing; i.e.
+direct division by the two dimensional flat field observation.  In that
+case do not specify a flat field spectrum; use the null string "".  The
+\fBdohydra\fR task provides an alternative flat field response correction
+based on division of the extracted object spectra by the extracted flat field
+spectra.  A discussion of the theory and merits of flat fielding directly
+verses using the extracted spectra will not be made here.  The
+\fBdohydra\fR flat fielding algorithm is the \fIrecommended\fR method for
+flat fielding since it works well and is not subject to the many problems
+involved in two dimensional flat fielding.
+
+In addition to correcting for pixel-to-pixel response the flat field step
+also corrects for differences in the fiber throughput.  Thus, even if the
+pixel-to-pixel flat field corrections have been made in some other way it
+is desirable to use a sky or dome flat observation for determining a fiber
+throughput correction.  Alternatively, a separately derived throughput
+file may be specified.  This file consists of the aperture numbers
+(the same as used for the aperture reference) and relative throughput
+numbers.
+
+The first step is extraction of the flat field spectrum, if specified,
+using the reference apertures.  Only one flat field is allowed so if
+multiple flat fields are required the data must be reduced in groups.
+After extraction one or more corrections are applied.  If the \fIfitflat\fR
+option is selected (the default) the extracted flat field spectra are
+averaged together and a smooth function is fit.  The default fitting
+function and order are given by the parameters \fIf_function\fR and
+\fIf_order\fR.  If the parameter \fIf_interactive\fR is "yes" then the
+fitting is done interactively using the \fBfit1d\fR task which uses the
+\fBicfit\fR interactive fitting commands.
+
+The fitted function is divided into the individual flat field spectra to
+remove the basic shape of the spectrum while maintaining the relative
+individual pixel responses and any fiber to fiber differences.  This step
+avoids introducing the flat field spectrum shape into the object spectra
+and closely preserves the object counts.
+
+If a throughput image is available (an observation of blank sky
+usually at twilight) it is extracted.  If no flat field is used the average
+signal through each fiber is computed and this becomes the response
+normalization function.  Note that a dome flat may be used in place of a
+sky in the sky flat field parameter for producing throughput only
+corrections.  If a flat field is specified then each sky spectrum is
+divided by the appropriate flat field spectrum.  The total counts through
+each fiber are multiplied into the flat field spectrum thus making the sky
+throughput of each fiber the same.  This correction is important if the
+iillumination of the fibers differs between the flat field source and the
+sky.  Since only the total counts are required the sky or dome flat field
+spectra need not be particularly strong though care must be taken to avoid
+objects.
+
+Instead of a sky flat or other throughput image a separately derived
+throughput file may be used.  It may be used with or without a
+flat field.
+
+The final step is to normalize the flat field spectra by the mean counts of
+all the fibers.  This normalization step is simply to preserve the average
+counts of the extracted object and arc spectra after division by the
+response spectra.  The final relative throughput values are recorded in the
+log and possibly printed on the terminal.
+
+These flat field response steps and algorithm are available as a separate
+task called \fBmsresp1d\fR.
+
+\fBDispersion Correction\fR
+
+Dispersion corrections are applied to the extracted spectra if the
+\fBdispcor\fR parameter is set.  This can be a complicated process which
+the \fBdohydra\fR task tries to simplify for you.  There are three basic
+steps involved; determining the dispersion functions relating pixel
+position to wavelength, assigning the appropriate dispersion function to a
+particular observation, and resampling the spectra to evenly spaced pixels
+in wavelength.
+
+The comparison arc spectra are used to define dispersion functions for the
+fibers using the tasks \fBautoidentify\fR and \fBreidentify\fR.  The
+interactive \fBautoidentify\fR task is only used on the central fiber of the
+first arc spectrum to define the basic reference dispersion solution from
+which all other fibers and arc spectra are automatically derived using
+\fBreidentify\fR. \fBAutoidentify\fR attempts to automatically identify
+the arc lines using the \fIcrval\fR and \fIcdelt\fR parameters.  Whether
+or not it is successful the user is presented with the interactive
+identification graph.  The automatic identifications can be reviewed and a
+new solution or corrections to the automatic solution may be performed.
+
+The set of arc dispersion function parameters are from \fBautoidentify\fR and
+\fBreidentify\fR.  The parameters define a line list for use in
+automatically assigning wavelengths to arc lines, a parameter controlling
+the width of the centering window (which should match the base line
+widths), the dispersion function type and order, parameters to exclude bad
+lines from function fits, and parameters defining whether to refit the
+dispersion function, as opposed to simply determining a zero point shift,
+and the addition of new lines from the line list when reidentifying
+additional arc spectra.  The defaults should generally be adequate and the
+dispersion function fitting parameters may be altered interactively.  One
+should consult the help for the two tasks for additional details of these
+parameters and the operation of \fBautoidentify\fR.
+
+Generally, taking a number of comparison arc lamp exposures interspersed
+with the program spectra is sufficient to accurately dispersion calibrate
+Hydra spectra.  However, there are some other calibration options
+which may be of interest.  These options apply additional calibration data
+consisting either of auxiliary line spectra, such as from dome lights or
+night sky lines, or simultaneous arc lamp spectra taken through a few
+fibers during the object exposure.  These options add complexity to the
+dispersion calibration process and were provided primarily for Nessie
+data.  Therefore they are described later in the Nessie section.
+
+When only arc comparison lamp spectra are used,  dispersion functions are
+determined independently for each fiber of each arc image and then assigned
+to the matching fibers in the program object observations.  The assignment
+consists of selecting one or two arc images to calibrate each object
+image.  When two bracketing arc spectra are used the dispersion functions
+are linearly interpolated (usually based on the time of the observations).
+
+The arc assignments may be done either explicitly with an arc assignment
+table (parameter \fIarctable\fR) or based on a header parameter.  The task
+used is \fBrefspectra\fR and the user should consult this task if the
+default behavior is not what is desired.  The default is to interpolate
+linearly between the nearest arcs based on the Julian date (corrected to
+the middle of the exposure).  The Julian date and a local Julian day number
+(the day number at local noon) are computed automatically by the task
+\fBsetjd\fR and recorded in the image headers under the keywords JD and
+LJD.  In addition the universal time at the middle of the exposure, keyword
+UTMIDDLE, is computed by the task \fBsetairmass\fR and this may also be used
+for ordering the arc and object observations.
+
+An optional step is to use sky lines in the spectra to compute a zeropoint
+dispersion shift that will align the sky lines.  This may improve sky
+subtraction if the iillumination is not the same between the arc calibration
+and the sky.  When selected the object spectrum is dispersion corrected
+using a non-linear dispersion function to avoid resampling the spectrum.
+The sky lines are then reidentified in wavelength space from a template
+list of sky lines.  The mean shift in the lines for each fiber relative to
+the template in that fiber is computed to give the zeropoint shift.  The
+database file is created when the first object is extracted.  You are asked
+to mark the sky lines in one fiber and then the lines are automatically
+reidentified in all other fibers.  Note that this technique requires the
+sky lines be found in all fibers.
+
+The last step of dispersion correction (resampling the spectrum to evenly
+spaced pixels in wavelength) is optional and relatively straightforward.
+If the \fIlinearize\fR parameter is no then the spectra are not resampled
+and the nonlinear dispersion information is recorded in the image header.
+Other IRAF tasks (the coordinate description is specific to IRAF) will use
+this information whenever wavelengths are needed.  If linearizing is
+selected a linear dispersion relation, either linear in the wavelength or
+the log of the wavelength, is defined once and applied to every extracted
+spectrum.  The resampling algorithm  parameters allow selecting the
+interpolation function type, whether to conserve flux per pixel by
+integrating across the extent of the final pixel, and whether to linearize
+to equal linear or logarithmic intervals.  The latter may be appropriate
+for radial velocity studies.  The default is to use a fifth order
+polynomial for interpolation, to conserve flux, and to not use logarithmic
+wavelength bins.  These parameters are described fully in the help for the
+task \fBdispcor\fR which performs the correction.  The interpolation
+function options and the nonlinear dispersion coordinate system is
+described in the help topic \fBonedspec.package\fR.
+
+\fBSky Subtraction\fR
+
+Sky subtraction is selected with the \fIskysubtract\fR processing option.
+The sky spectra are selected by their aperture and beam numbers and
+combined into a single master sky spectrum
+which is then subtracted from each object spectrum.  If the \fIskyedit\fR
+option is selected the sky spectra are plotted using the task
+\fBspecplot\fR.  By default they are superposed to allow identifying
+spectra with unusually high signal due to object contamination.  To
+eliminate a sky spectrum from consideration point at it with the cursor and
+type 'd'.  The last deleted spectrum may be undeleted with 'e'.  This
+allows recovery of incorrect or accidental deletions.
+
+The sky combining algorithm parameters define how the individual sky fiber
+spectra, after interactive editing, are combined before subtraction from
+the object fibers.  The goals of combining are to reduce noise, eliminate
+cosmic-rays, and eliminate fibers with inadvertent objects.  The common
+methods for doing this to use a median and/or a special sigma clipping
+algorithm (see \fBscombine\fR for details).  The scale
+parameter determines whether the individual skys are first scaled to a
+common mode.  The scaling should be used if the throughput is uncertain,
+but in that case you probably did the wrong thing in the throughput
+correction.  If the sky subtraction is done interactively, i.e. with the
+\fIskyedit\fR option selected, then after selecting the spectra to be
+combined a query is made for the combining algorithm.  This allows
+modifying the default algorithm based on the number of sky spectra
+selected since the "avsigclip" rejection algorithm requires at least
+three spectra.
+
+The combined sky spectrum is subtracted from only those spectra specified
+by the object aperture and beam numbers.  Other spectra, such as comparison
+arc spectra, are retained unchanged.  One may include the sky spectra as
+object spectra to produce residual sky spectra for analysis.  The combined
+master sky spectra may be saved if the \fIsaveskys\fR parameter is set.
+The saved sky is given the name of the object spectrum with the prefix
+"sky".
+
+\fBNessie Data\fR
+
+Reducing Nessie data with \fBdohydra\fR is very similar.  The differences
+are that additional setup and calibration are required since this
+instrument was a precursor to the more developed Hydra instrument.
+The discussion in this section also describes some features which may
+be applicable to other fiber instruments outside of the NOAO instruments.
+
+The Nessie comparison lamp exposures suffer from vignetting resulting in
+some fibers being poorly illuminated.  By rearranging the fibers in the
+calibration plugboard and taking additional exposures one can obtain good
+arc spectra through all fibers.  The task will merge the well exposed
+fibers from the multiple exposures into a single final extracted
+arc calibration image.  One of the exposures of a set is selected as
+the primary exposure.  This is the one specified in list of arcs,
+\fIarc1\fR.  The other exposures of the set are referenced only in
+a a setup file, called an \fIarc replacement file\fR.
+
+The format of the arc replacement file is lines containing the primary
+arc image, a secondary arc image,
+and the apertures from the secondary arc to be merged into the
+final arc spectra.  There can be more than one secondary
+exposure though it is unlikely.  Figure 1 gives an example of this
+setup file.
+.nf
+
+    Figure 1: Example Arc Aperture Replacement File
+
+    cl> type arcreplace
+    nesjun042c nesjun049c 1,7,9,13,17,19,28,34
+
+.fi
+The primary arc exposure is "nesjun042c", the secondary arc is
+"nesjun049c", and the secondary apertures are 1, 7, etc.  The syntax for
+the list of apertures also includes hyphen delimited ranges such as
+"8-10".
+
+With Hydra the aperture identification file (4meter) or image header
+keywords (WIYN) are produced for the user.  With
+Nessie this is not the case, hence, the user must prepare a file
+manually.  The aperture identification file is not mandatory, sequential
+numbering will be used, but it is highly recommended for keeping track of
+the objects assigned to the fibers.  The aperture identification table
+contains lines consisting of an aperture number, a beam number, and an
+object identification.  These must be in the same order as the fibers in
+the image.  The aperture number may be any unique number but it is
+recommended that the fiber number be used.  The beam number is used to flag
+object, sky, arc, or other types of spectra.  The default beam numbers used
+by the task are 0 for sky, 1 for object, and 2 for arc.  The object
+identifications are optional but it is good practice to include them so
+that the data will contain the object information independent of other
+records.  Figure 2 shows an example for the \fIblue\fR fibers from a board
+called M33Sch2.
+.nf
+
+    Figure 2: Example Aperture Identification File
+
+    cl> type m33sch2
+    1 1 143
+    2 1 254
+    3 0 sky
+    4 1 121
+    5 2 arc
+       .
+       .
+       .
+    44 1 s92
+    49 -1 Broken
+    45 1 156
+    46 2 arc
+    47 0 sky
+    48 1 phil2
+
+.fi
+Note the identification of the sky fibers with beam number 0, the object
+fibers with 1, and the arc fibers with 2.  Also note that broken fiber 49
+is actually between fibers 44 and 45.  The broken fiber entries, given beam
+number -1, are optional but recommended to give the automatic spectrum
+finding operation the best chance to make the correct identifications.  The
+identification file will vary for each plugboard setup.  Additional
+information about the aperture identification table may be found in the
+description of the task \fBapfind\fR.
+
+An alternative to using an aperture identification table is to give no
+name, the "" empty string, and to explicitly give a range of
+aperture numbers for the skys and possibly for the sky subtraction
+object list in the parameters \fIobjaps, skyaps, arcaps, objbeams,
+skybeams,\fR and \fIarcbeams\fR.
+
+Because taking comparison exposures with Nessie requires replugging the
+fibers, possibly in more than one configuration, and the good stability of
+the instrument, there are two mutually exclusive methods for monitoring
+shifts in the dispersion zero point from the basic arc lamp spectra other
+than taking many arc lamp exposures.  One is to use some fibers to take a
+simultaneous arc spectrum while observing the program objects.  The fibers
+are identified by aperture or beam numbers.  The second method is to use
+\fIauxiliary line spectra\fR, such as mercury lines from the dome lights.
+These spectra are specified with an auxiliary shift arc list, \fIarc2\fR.
+
+When using auxiliary line spectra for monitoring zero point shifts one of
+these spectra is plotted interactively by \fBidentify\fR with the
+reference dispersion function from the reference arc spectrum.  The user
+marks one or more lines which will be used to compute zero point wavelength
+shifts in the dispersion functions automatically.  The actual wavelengths
+of the lines need not be known.  In this case accept the wavelength based
+on the reference dispersion function.  As other observations of the same
+features are made the changes in the positions of the features will be
+tracked as zero point wavelength changes such that wavelengths of the
+features remain constant.
+
+When using auxiliary line spectra the only arc lamp spectrum used is the
+initial arc reference spectrum (the first image in the \fIarcs1\fR list).
+The master dispersion functions are then shifted based on the spectra in
+the \fIarcs2\fR list (which must all be of the same type).  The dispersion
+function assignments made by \fBrefspectra\fR using either the arc
+assignment file or based on header keywords is done in the same way as
+described for the arc lamp images except using the auxiliary spectra.
+
+If simultaneous arcs are used the arc lines are reidentified to determine a
+zero point shift relative to the comparison lamp spectra selected, by
+\fBrefspectra\fR, of the same fiber.  A linear function of aperture
+position on the image across the dispersion verses the zero point shifts
+from the arc fibers is determined and applied to the dispersion functions
+from the assigned calibration arcs for the non-arc fibers.  Note that if
+there are two comparison lamp spectra (before and after the object
+exposure) then there will be two shifts applied to two dispersion functions
+which are then combined using the weights based on the header parameters
+(usually the observation time).
+.ih
+EXAMPLES
+1.  The following example uses artificial data and may be executed
+at the terminal (with IRAF V2.10).  This is also the sequence performed
+by the test procedure "demos dohydra".
+
+.nf
+hy> demos mkhydra
+Creating image demoobj ...
+Creating image demoflat ...
+Creating image demoarc ...
+hy> type demoapid
+===> demoapid <===
+36 1
+37 0
+38 1
+39 1
+41 0
+42 1
+43 1
+44 0
+45 1
+46 -1
+47 0
+48 1
+hy> hydra.verbose = yes
+hy> dohydra demoobj apref=demoflat flat=demoflat arcs1=demoarc \
+>>> fib=12 apid=demoapid width=4. minsep=5. maxsep=7. clean- splot+
+Set reference apertures for demoflat
+Resize apertures for demoflat?  (yes):
+Edit apertures for demoflat?  (yes):
+<Exit with 'q'>
+Fit curve to aperture 36 of demoflat interactively  (yes):
+<Exit with 'q'>
+Fit curve to aperture 37 of demoflat interactively  (yes): N
+Create response function demoflatdemoad.ms
+Extract flat field demoflat
+Fit and ratio flat field demoflat
+<Exit with 'q'>
+Create the normalized response demoflatdemoad.ms
+demoflatdemoad.ms -> demoflatdemoad.ms  using bzero: 0.
+    and bscale: 1.000001
+    mean: 1.000001  median: 1.052665  mode: 1.273547
+    upper: INDEF  lower: INDEF
+Average fiber response:
+1.  1.151023
+2.  0.4519709
+3.  1.250614
+4.  1.287281
+5.  1.271358
+6.  0.6815334
+7.  1.164336
+8.  0.7499605
+9.  1.008654
+10.  1.053296
+11.  0.929967
+Extract arc reference image demoarc
+Determine dispersion solution for demoarc
+<A dispersion solution is found automatically.>
+<Type 'f' to look at fit.  Type 'q' to exit fit.>
+<Exit with 'q'>
+
+REIDENTIFY: NOAO/IRAF V2.10BETA valdes@puppis Tue 16:01:07 11-Feb-92
+  Reference image = d....ms.imh, New image = d....ms, Refit = yes
+     Image Data Found    Fit Pix Shift User Shift  Z Shift     RMS
+d....ms - Ap 41 16/20  16/16   0.00796     0.0682  8.09E-6    3.86
+Fit dispersion function interactively? (no|yes|NO|YES) (NO): y
+<Exit with 'q'>
+d....ms - Ap 41 16/20  16/16   0.00796     0.0682  8.09E-6    3.86
+d....ms - Ap 39 19/20  19/19     0.152        1.3  1.95E-4    3.89
+Fit dispersion function interactively? (no|yes|NO|YES) (yes): N
+d....ms - Ap 39 19/20  19/19     0.152        1.3  1.95E-4    3.89
+d....ms - Ap 38 18/20  18/18     0.082      0.697  9.66E-5    3.64
+d....ms - Ap 37 19/20  19/19    0.0632      0.553  1.09E-4    6.05
+d....ms - Ap 36 18/20  18/18    0.0112     0.0954  1.35E-5    4.12
+d....ms - Ap 43 17/20  17/17    0.0259      0.221  3.00E-5    3.69
+d....ms - Ap 44 19/20  19/19     0.168       1.44  2.22E-4    4.04
+d....ms - Ap 45 20/20  20/20      0.18       1.54  2.35E-4    3.95
+d....ms - Ap 47 18/20  18/18  -2.02E-4    0.00544  9.86E-6     4.4
+d....ms - Ap 48 16/20  16/16   0.00192     0.0183  1.44E-6    3.82
+
+Dispersion correct demoarc
+d....ms.imh: w1 = 5748.07..., w2 = 7924.62..., dw = 8.50..., nw = 257
+  Change wavelength coordinate assignments? (yes|no|NO): n
+Extract object spectrum demoobj
+Assign arc spectra for demoobj
+[demoobj] refspec1='demoarc'
+Dispersion correct demoobj
+demoobj.ms.imh: w1 = 5748.078, w2 = 7924.622, dw = 8.502127, nw = 257
+Sky subtract demoobj:  skybeams=0
+Edit the sky spectra? (yes):
+<Exit with 'q'>
+Sky rejection option (none|minmax|avsigclip) (avsigclip):
+demoobj.ms.imh:
+Splot spectrum? (no|yes|NO|YES) (yes):
+Image line/aperture to plot (1:) (1):
+<Look at spectra and change apertures with # key>
+<Exit with 'q'>
+.fi
+.ih
+REVISIONS
+.ls DOHYDRA V2.11
+A sky alignment option was added.
+
+The aperture identification can now be taken from image header keywords.
+
+The initial arc line identifications is done with the automatic line
+identification algorithm.
+.le
+.ls DOHYDRA V2.10.3
+The usual output WCS format is "equispec".  The image format type to be
+processed is selected with the \fIimtype\fR environment parameter.  The
+dispersion axis parameter is now a package parameter.  Images will only
+be processed if the have the CCDPROC keyword.  A \fIdatamax\fR parameter
+has been added to help improve cosmic ray rejection.  A scattered
+light subtraction processing option has been added.
+.le
+.ih
+SEE ALSO
+apedit, apfind, approfiles, aprecenter, apresize, apsum, aptrace, apvariance,
+ccdred, center1d, dispcor, fit1d, icfit, identify, msresp1d, observatory,
+onedspec.package, refspectra, reidentify, scombine, setairmass, setjd,
+specplot, splot
+.endhelp
diff --git a/noao/imred/hydra/doc/dohydra.ms b/noao/imred/hydra/doc/dohydra.ms
new file mode 100644
index 00000000..4b505ee3
--- /dev/null
+++ b/noao/imred/hydra/doc/dohydra.ms
@@ -0,0 +1,1853 @@
+.nr PS 9
+.nr VS 11
+.de V1
+.ft CW
+.nf
+..
+.de V2
+.fi
+.ft R
+..
+.de LS
+.br
+.in +2
+..
+.de LE
+.br
+.sp .5v
+.in -2
+..
+.ND July 1995
+.TL
+Guide to the HYDRA Reduction Task DOHYDRA
+.AU
+Francisco Valdes
+.AI
+IRAF Group - Central Computer Services
+.K2
+.DY
+
+.AB
+The \fBdohydra\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, fiber throughput correction, wavelength calibration, and sky
+subtraction of \fIHydra\fR and \fINessie\fR fiber spectra.  It is a
+command language script which collects and combines the functions and
+parameters of many general purpose tasks to provide a single complete data
+reduction path.  The task provides a degree of guidance, automation, and
+record keeping necessary when dealing with the large amount of data
+generated by these multifiber instruments.  This guide describes what
+this task does, it's usage, and parameters.
+.AE
+.NH
+Introduction
+.LP
+The \fBdohydra\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, fiber throughput correction, wavelength calibration, and sky
+subtraction of \fIHydra\fR and \fINessie\fR fiber spectra.  It is a
+command language script which collects and combines the functions and
+parameters of many general purpose tasks to provide a single, complete data
+reduction path.  The task provides a degree of guidance, automation, and
+record keeping necessary when dealing with the large amount of data
+generated by these multifiber instruments.
+.LP
+The general organization of the task is to do the interactive setup steps
+first using representative calibration data and then perform the majority
+of the reductions automatically, and possibly as a background process, with
+reference to the setup data.  In addition, the task determines which setup
+and processing operations have been completed in previous executions of the
+task and, contingent on the \f(CWredo\fR and \f(CWupdate\fR options, skip or
+repeat some or all the steps.
+.LP
+The following description is oriented specifically to Hydra data but
+applies equally well to Nessie data except for a few minor differences
+which are discussed in a separate section.  Since \fBdohydra\fR combines many
+separate, general purpose tasks the description given here refers to these
+tasks and leaves some of the details to their help documentation.
+.LP
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage for
+Hydra since there are many variations possible.
+.NH
+Usage Outline
+.LP
+.IP [1] 6
+The images are first processed with \fBccdproc\fR for overscan,
+bias, and dark corrections.
+The \fBdohydra\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+.IP [2]
+Set the \fBdohydra\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed, the flat field image as the aperture reference and
+the flat field, and one or more arc images.  A throughput file or image,
+such as a blank sky observation, may also be specified.  If there are many
+object or arc spectra per setup you might want to prepare "@ files".
+Specify the aperture identification table (a file for 4meter data or an
+image for WIYN data) which is provided for each Hydra
+configuration.  You might wish to verify the geometry parameters,
+separations, dispersion direction, etc., which may
+change with different detector setups.  The processing parameters are set
+for complete reductions but for quicklook you might not use the clean
+option or dispersion calibration and sky subtraction.
+.IP
+The parameters are set for a particular Hydra configuration and different
+configurations may use different flat fields, arcs, and aperture
+identification tables.
+.IP [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the execution and no further queries of that
+type will be made.
+.IP [4]
+The apertures are defined using the specified aperture reference image.
+The spectra are found automatically and apertures assigned based on
+task parameters and the aperture identification table.  Unassigned
+fibers will have a negative beam number and will be ignored in subsequent
+processing.  The resize option sets the aperture size to the widths of
+the profiles at a fixed fraction of the peak height.  The interactive
+review of the apertures is recommended.  If the identifications are off
+by a shift the 'o' key is used.  To exit the aperture review type 'q'.
+.IP [5]
+The fiber positions at a series of points along the dispersion are measured
+and a function is fit to these positions.  This may be done interactively to
+adjust the fitting parameters.  Not all fibers need be examined and the "NO"
+response will quit the interactive fitting.  To exit the interactive
+fitting type 'q'.
+.IP [6]
+If scattered light subtraction is to be done the flat field image is
+used to define the scattered light fitting parameters interactively.
+If one is not specified then the aperture reference image is used for
+this purpose.
+
+There are two queries for the interactive fitting.  A graph of the
+data between the defined reference apertures separated by a specified
+buffer distance is first shown.  The function order and type may be
+adjusted.  After quiting with 'q' the user has the option of changing
+the buffer value and returning to the fitting, changing the image line
+or column to check if the fit parameters are satisfactory at other points,
+or to quit and accept the fit parameters.  After fitting all points
+across the dispersion another graph showing the scattered light from
+the individual fits is shown and the smoothing parameters along the
+dispersion may be adjusted.  Upon quiting with 'q' you have the option
+of checking other cuts parallel to the dispersion or quiting and finishing
+the scattered light function smoothing and subtraction.
+
+If there is a throughput image then this is corrected for scattered light
+noninteractively using the previous fitting parameters.
+.IP [7]
+If flat fielding is to be done the flat field spectra are extracted.  The
+average spectrum over all fibers is determined and a function is fit
+interactively (exit with 'q').  This function is generally of sufficiently
+high order that the overall shape is well fit.  This function is then used
+to normalize the individual flat field spectra.  If a throughput image, a
+sky flat, is specified then the total sky counts through each fiber are
+used to correct the total flat field counts.  Alternatively, a separately
+derived throughput file can be used for specifying throughput corrections.
+If neither type of throughput is used the flat field also provides the
+throughput correction.  The final response spectra are normalized to a unit
+mean over all fibers.  The relative average throughput for each fiber is
+recorded in the log and possibly printed to the terminal.
+.IP [8]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  The middle fiber is used to identify the arc lines and define
+the dispersion function using the task \fBautoidentify\fR.  The
+\fIcrval\fR and \fIcdelt\fR parameters are used in the automatic
+identification.  Whether or not the automatic identification is
+successful you will be shown the result of the arc line identification.
+If the automatic identification is not successful identify a few arc
+lines with 'm' and use the 'l' line list identification command to
+automatically add additional lines and fit the dispersion function.  Check
+the quality of the dispersion function fit with 'f'.  When satisfied exit
+with 'q'.
+.IP [9]
+The remaining fibers are automatically reidentified.  You have the option
+to review the line identifications and dispersion function for each fiber
+and interactively add or delete arc lines and change fitting parameters.
+This can be done selectively, such as when the reported RMS increases
+significantly.
+.IP [10]
+If the spectra are to be resampled to a linear dispersion system
+(which will be the same for all spectra) default dispersion parameters
+are printed and you are allowed to adjust these as desired.
+.IP [11]
+If the sky line alignment option is selected and the sky lines have not
+been identified for a particular aperture identification table then you are
+asked to mark one or more sky lines.  You may simply accept the wavelengths
+of these lines as defined by the dispersion solution for this spectrum and
+fiber or you may specify knowns wavelengths for the lines. These lines will
+be reidentified in all object spectra extracted and a mean zeropoint shift
+will be added to the dispersion solution.  This has the effect of aligning
+these lines to optimize sky subtraction.
+.IP [12]
+The object spectra are now automatically scatteredl ight subtracted,
+ extracted, flat fielded, and dispersion corrected.
+.IP [13]
+When sky subtracting, the individual sky spectra may be reviewed and some
+spectra eliminated using the 'd' key.  The last deleted spectrum may be
+recovered with the 'e' key.  After exiting the review with 'q' you are
+asked for the combining option.  The type of combining is dictated by the
+number of sky fibers.
+.IP [14]
+The option to examine the final spectra with \fBsplot\fR may be given.
+To exit type 'q'.
+.IP [15]
+If scattered light is subtracted from the input data a copy of the
+original image is made by appending "noscat" to the image name.
+If the data are reprocessed with the \fIredo\fR flag the original
+image will be used again to allow modification of the scattered
+light parameters.
+
+The final spectra will have the same name as the original 2D images
+with a ".ms" extension added.  The flat field and arc spectra will
+also have part of the aperture identification table name added to
+allow different configurations to use the same 2D flat field and arcs
+but with different aperture definitions.  If using the sky alignment
+option an image "align" with the aperture identification table name
+applied will also be created.
+
+.NH
+Spectra and Data Files
+.LP
+The basic input consists of Hydra or Nessie object and
+calibration spectra stored as IRAF images.
+The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+The raw CCD images must
+be processed to remove overscan, bias, and dark count effects.  This
+is generally done using the \fBccdred\fR package.
+The \fBdoargus\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+Flat fielding is
+generally not done at this stage but as part of \fBdohydra\fR.
+If flat fielding is done as part of the basic CCD processing then
+a flattened flat field, blank sky observation, or throughput file
+should still be created for applying fiber throughput corrections.
+.LP
+The task \fBdohydra\fR uses several types of calibration spectra.  These
+are flat fields, blank sky flat fields, comparison lamp spectra, auxiliary
+mercury line (from the dome lights) or sky line spectra, and simultaneous
+arc spectra taken during the object observation.  The flat field,
+throughput image or file, auxiliary emission line spectra, and simultaneous
+comparison fibers are optional.  If a flat field is used then the sky flat
+or throughput file is optional assuming the flat field has the same fiber
+illumination.  It is legal to specify only a throughput image or file and
+leave the flat field blank in order to simply apply a throughput
+correction.  Because only the total counts through each fiber are used from
+a throughput image, sky flat exposures need not be of high signal per
+pixel.
+.LP
+There are three types of arc calibration methods.  One is to take arc
+calibration exposures through all fibers periodically and apply the
+dispersion function derived from one or interpolated between pairs to the
+object fibers.  This is the usual method with Hydra.  Another method is to
+use only one or two all-fiber arcs to define the shape of the dispersion
+function and track zero point wavelength shifts with \fIsimultaneous arc\fR
+fibers taken during the object exposure.  The simultaneous arcs may or may
+not be available at the instrument but \fBdohydra\fR can use this type of
+observation.  The arc fibers are identified by their beam or aperture
+numbers.  A related and mutually exclusive method is to use \fIauxiliary
+line spectra\fR such as lines in the dome lights or sky lines to monitor
+shifts relative to a few actual arc exposures.  The main reason to do this
+is if taking arc exposures through all fibers is inconvenient as is the
+case with the manual Nessie plugboards.
+.LP
+The assignment of arc or auxiliary line calibration exposures to object
+exposures is generally done by selecting the nearest in time and
+interpolating.  There are other options possible which are described under
+the task \fBrefspectra\fR.  The most general option is to define a table
+giving the object image name and the one or two arc spectra to be assigned
+to that object.  That file is called an \fIarc assignment table\fR and it
+is one of the optional setup files which can used with \fBdohydra\fR.
+.LP
+The first step in the processing is identifying the spectra in the images.
+The \fIaperture identification table\fR (which may be a file or an image)
+contains information about the fiber assignments.  This table is created
+for you when using Hydra but must be prepared by the user when using
+Nessie.  A description of this table as a text file is given in the section
+concerning Nessie.
+.LP
+The final reduced spectra are recorded in two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ms" extension.  Each line in the reduced image is a one dimensional
+spectrum with associated aperture, wavelength, and identification
+information.  When the \f(CWextras\fR parameter is set the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tools such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.  The special task \fBscopy\fR may be used to extract
+specific apertures or to change format to individual one dimensional
+images.
+.NH
+Package Parameters
+.LP
+The \fBhydra\fR package parameters, shown in Figure 1, set parameters
+affecting all the tasks in the package.
+.KS
+.V1
+
+.ce
+Figure 1: Package Parameter Set for HYDRA
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = imred
+   TASK = hydra
+
+(dispaxi=            2) Image axis for 2D images
+(observa=  observatory) Observatory of data
+(interp =        poly5) Interpolation type
+
+(databas=     database) Database
+(verbose=           no) Verbose output?
+(logfile=      logfile) Log file
+(plotfil=             ) Plot file
+
+(records=             )
+(version= HYDRA V1: January 1992)
+
+.KE
+.V2
+The dispersion axis parameter defines the image axis along which the
+dispersion runs.  This is used if the image header doesn't define the
+dispersion axis with the DISPAXIS keyword.
+The observatory parameter is only required
+for data taken with fiber instruments other than Hydra or Nessie.
+The spectrum interpolation type might be changed to "sinc" but
+with the cautions given in \fBonedspec.package\fR.
+The other parameters define the standard I/O functions.
+The verbose parameter selects whether to print everything which goes
+into the log file on the terminal.  It is useful for monitoring
+what the \fBdohydra\fR task does.  The log and plot files are useful for
+keeping a record of the processing.  A log file is highly recommended.
+A plot file provides a record of apertures, traces, and extracted spectra
+but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+.NH
+Processing Parameters
+.LP
+The \fBdohydra\fR parameters are shown in Figure 2.
+.KS
+.V1
+
+.ce
+Figure 2: Parameter Set for DOHYDRA
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = hydra
+   TASK = dohydra
+
+objects =               List of object spectra
+(apref  =             ) Aperture reference spectrum
+(flat   =             ) Flat field spectrum
+(through=             ) Throughput file or image (optional)
+(arcs1  =             ) List of arc spectra
+(arcs2  =             ) List of shift arc spectra
+(arcrepl=             ) Special aperture replacements
+(arctabl=             ) Arc assignment table (optional)
+
+.KE
+.V1
+(readnoi=      RDNOISE) Read out noise sigma (photons)
+(gain   =         GAIN) Photon gain (photons/data number)
+(datamax=        INDEF) Max data value / cosmic ray threshold
+(fibers =           97) Number of fibers
+(width  =          12.) Width of profiles (pixels)
+(minsep =           8.) Minimum separation between fibers (pixels)
+(maxsep =          15.) Maximum separation between fibers (pixels)
+(apidtab=             ) Aperture identifications
+(crval  =        INDEF) Approximate wavelength
+(cdelt  =        INDEF) Approximate dispersion
+(objaps =             ) Object apertures
+(skyaps =             ) Sky apertures
+(arcaps =             ) Arc apertures
+(objbeam=          0,1) Object beam numbers
+(skybeam=            0) Sky beam numbers
+(arcbeam=             ) Arc beam numbers
+
+(scatter=           no) Subtract scattered light?
+(fitflat=          yes) Fit and ratio flat field spectrum?
+(clean  =          yes) Detect and replace bad pixels?
+(dispcor=          yes) Dispersion correct spectra?
+(savearc=          yes) Save simultaneous arc apertures?
+(skysubt=          yes) Subtract sky?
+(skyedit=          yes) Edit the sky spectra?
+(savesky=          yes) Save sky spectra?
+(splot  =           no) Plot the final spectrum?
+(redo   =           no) Redo operations if previously done?
+(update =          yes) Update spectra if cal data changes?
+(batch  =           no) Extract objects in batch?
+(listonl=           no) List steps but don't process?
+
+(params =             ) Algorithm parameters
+
+.V2
+The list of objects and arcs can be @ files if desired.  The aperture
+reference spectrum is usually the same as the flat field spectrum though it
+could be any exposure with enough signal to accurately define the positions
+and trace the spectra.  The first list of arcs are the standard Th-Ar or
+HeNeAr comparison arc spectra (they must all be of the same type).  The
+second list of arcs are the auxiliary emission line exposures mentioned
+previously and in the Nessie section.
+.LP
+The arc replacement file is described in the Nessie section and the arc
+assignment table was described in the data file section.  Note that even if
+an arc assignment table is specified, \fIall arcs to be used must also
+appear in the arc lists\fR in order for the task to know the type of arc
+spectrum.
+.LP
+The detector read out noise and gain are used for cleaning and variance
+(optimal) extraction.  The default will determine the values from the image
+itself.
+The variance
+weighting and cosmic-ray cleanning are sensitive to extremely strong
+cosmic-rays; ones which are hundreds of times brighter than the
+spectrum.  The \fIdatamax\fR is used to set an upper limit for any
+real data.  Any pixels above this value will be flagged as cosmic-rays
+and will not affect the extractions.
+The dispersion axis defines the wavelength direction of spectra in
+the image if not defined in the image header by the keyword DISPAXIS.  The
+width and separation parameters define the dimensions (in pixels) of the
+spectra (fiber profile) across the dispersion.  The width parameter
+primarily affects the centering.  The maximum separation parameter is
+important if missing spectra from the aperture identification table are to
+be correctly skipped.  The number of fibers can be left at the default
+(for Hydra) and the task will try to account for unassigned or missing fibers.
+.LP
+The approximate central wavelength and dispersion are used for the
+automatic identification of the arc reference.  They may be specified
+as image header keywords or values.  The INDEF values search the
+entire range of the coordinate reference file but the automatic
+line identification algorithm works much better and faster if
+approximate values are given.
+.LP
+The task needs to know which fibers are object, sky if sky subtraction is
+to be done, and simultaneous arcs if used.  One could explicitly give the
+aperture numbers but the recommended way, provided an aperture
+identification table is used, is to select the apertures based on
+the beam numbers.  The default values are those appropriate for the
+identification files generated for Hydra configurations.  Sky subtracted
+sky spectra are useful for evaluating the sky subtraction.  Since only the
+spectra identified as objects are sky subtracted one can exclude fibers
+from the sky subtraction.  For example, if the \fIobjbeams\fR parameter is
+set to 1 then only those fibers with a beam of 1 will be sky subtracted.
+All other fibers will remain in the extracted spectra but will not be sky
+subtracted.
+.LP
+The next set of parameters select the processing steps and options.  The
+scattered light option allows fitting and subtracting a scattered light
+surface from the input object and flat field.  If there is significant
+scattered light which is not subtracted the fiber throughput correction
+will not be accurate.  The
+flat fitting option allows fitting and removing the overall shape of the
+flat field spectra while preserving the pixel-to-pixel response
+corrections.  This is useful for maintaining the approximate object count
+levels and not introducing the reciprocal of the flat field spectrum into
+the object spectra.  The \f(CWclean\fR option invokes a profile fitting and
+deviant point rejection algorithm as well as a variance weighting of points
+in the aperture.  These options require knowing the effective (i.e.
+accounting for any image combining) read out noise and gain.  For a
+discussion of cleaning and variance weighted extraction see
+\fBapvariance\fR and \fBapprofiles\fR.
+.LP
+The dispersion correction option selects whether to extract arc spectra,
+determine a dispersion function, assign them to the object spectra, and,
+possibly, resample the spectra to a linear (or log-linear) wavelength
+scale.  If simultaneous arc fibers are defined there is an option to delete
+them from the final spectra when they are no longer needed.
+.LP
+The sky alignment option allows applying a zeropoint dispersion shift
+to all fibers based on one or more sky lines.  This requires all fibers
+to have the sky lines visible.  When there are sky lines this will
+improve the sky subtraction if there is a systematic error in the
+fiber illumination between the sky and the arc calibration.
+.LP
+The sky subtraction option selects whether to combine the sky fiber spectra
+and subtract this sky from the object fiber spectra.  \fIDispersion
+correction and sky subtraction are independent operations.\fR  This means
+that if dispersion correction is not done then the sky subtraction will be
+done with respect to pixel coordinates.  This might be desirable in some
+quick look cases though it is incorrect for final reductions.
+.LP
+The sky subtraction option has two additional options.  The individual sky
+spectra may be examined and contaminated spectra deleted interactively
+before combining.  This can be a useful feature in crowded regions.  The
+final combined sky spectrum may be saved for later inspection in an image
+with the spectrum name prefixed by \fBsky\fR.
+.LP
+After a spectrum has been processed it is possible to examine the results
+interactively using the \fBsplot\fR tasks.  This option has a query which
+may be turned off with "YES" or "NO" if there are multiple spectra to be
+processed.
+.LP
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\f(CWupdate\fR flag is set.  The changes which will cause an update are a new
+aperture identification table, a new reference image, new flat fields, and a
+new arc reference.  If all input spectra are to be processed regardless of
+previous processing the \f(CWredo\fR flag may be used.  Note that
+reprocessing clobbers the previously processed output spectra.
+.LP
+The \f(CWbatch\fR processing option allows object spectra to be processed as
+a background or batch job.  This will only occur if sky spectra editing and
+\fBsplot\fR review (interactive operations) are turned off, either when the
+task is run or by responding with "NO" to the queries during processing.
+.LP
+The \f(CWlistonly\fR option prints a summary of the processing steps which
+will be performed on the input spectra without actually doing anything.
+This is useful for verifying which spectra will be affected if the input
+list contains previously processed spectra.  The listing does not include
+any arc spectra which may be extracted to dispersion calibrate an object
+spectrum.
+.LP
+The last parameter (excluding the task mode parameter) points to another
+parameter set for the algorithm parameters.  The way \fBdohydra\fR works
+this may not have any value and the parameter set \fBparams\fR is always
+used.  The algorithm parameters are discussed further in the next section.
+.NH
+Algorithms and Algorithm Parameters
+.LP
+This section summarizes the various algorithms used by the \fBdohydra\fR
+task and the parameters which control and modify the algorithms.  The
+algorithm parameters available to the user are collected in the parameter
+set \fBparams\fR.  These parameters are taken from the various general
+purpose tasks used by the \fBdohydra\fR processing task.  Additional
+information about these parameters and algorithms may be found in the help
+for the actual task executed.  These tasks are identified in the parameter
+section listing in parenthesis.  The aim of this parameter set organization
+is to collect all the algorithm parameters in one place separate from the
+processing parameters and include only those which are relevant for
+Hydra or Nessie data.  The parameter values can be changed from the
+defaults by using the parameter editor,
+.V1
+
+	cl> epar params
+
+.V2
+or simple typing \f(CWparams\fR.  The parameter editor can also be
+entered when editing the \fBdohydra\fR parameters by typing \f(CW:e
+params\fR or simply \f(CW:e\fR if positioned at the \f(CWparams\fR
+parameter.  Figure 3 shows the parameter set.
+.KS
+.V1
+
+.ce
+Figure 3: Algorithm Parameter Set
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = hydra
+   TASK = params
+
+(line   =        INDEF) Default dispersion line
+(nsum   =           10) Number of dispersion lines to sum
+(order  =   decreasing) Order of apertures
+(extras =           no) Extract sky, sigma, etc.?
+
+                        -- DEFAULT APERTURE LIMITS --
+(lower  =          -5.) Lower aperture limit relative to center
+(upper  =           5.) Upper aperture limit relative to center
+
+                        -- AUTOMATIC APERTURE RESIZING PARAMETERS --
+(ylevel =         0.05) Fraction of peak or intensity for resizing
+
+.KE
+.KS
+.V1
+                        -- TRACE PARAMETERS --
+(t_step =           10) Tracing step
+(t_funct=      spline3) Trace fitting function
+(t_order=            3) Trace fitting function order
+(t_niter=            1) Trace rejection iterations
+(t_low  =           3.) Trace lower rejection sigma
+(t_high =           3.) Trace upper rejection sigma
+
+.KE
+.KS
+.V1
+                        -- SCATTERED LIGHT PARAMETERS --
+(buffer =           1.) Buffer distance from apertures
+(apscat1=             ) Fitting parameters across the dispersion
+(apscat2=             ) Fitting parameters along the dispersion
+
+.KE
+.KS
+.V1
+                        -- APERTURE EXTRACTION PARAMETERS --
+(weights=         none) Extraction weights (none|variance)
+(pfit   =        fit1d) Profile fitting algorithm (fit1d|fit2d)
+(lsigma =           3.) Lower rejection threshold
+(usigma =           3.) Upper rejection threshold
+(nsubaps=            1) Number of subapertures
+
+.KE
+.KS
+.V1
+                        -- FLAT FIELD FUNCTION FITTING PARAMETERS --
+(f_inter=          yes) Fit flat field interactively?
+(f_funct=      spline3) Fitting function
+(f_order=           10) Fitting function order
+
+.KE
+.KS
+.V1
+                        -- ARC DISPERSION FUNCTION PARAMETERS --
+(coordli=linelists$idhenear.dat) Line list
+(match  =          10.) Line list matching limit in Angstroms
+(fwidth =           4.) Arc line widths in pixels
+(cradius=          10.) Centering radius in pixels
+(i_funct=      spline3) Coordinate function
+(i_order=            3) Order of dispersion function
+(i_niter=            2) Rejection iterations
+(i_low  =           3.) Lower rejection sigma
+(i_high =           3.) Upper rejection sigma
+(refit  =          yes) Refit coordinate function when reidentifying?
+(addfeat=           no) Add features when reidentifying?
+
+.KE
+.KS
+.V1
+                        -- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+(select =       interp) Selection method for reference spectra
+(sort   =           jd) Sort key
+(group  =          ljd) Group key
+(time   =           no) Is sort key a time?
+(timewra=          17.) Time wrap point for time sorting
+
+.KE
+.KS
+.V1
+                        -- DISPERSION CORRECTION PARAMETERS --
+(lineari=          yes) Linearize (interpolate) spectra?
+(log    =           no) Logarithmic wavelength scale?
+(flux   =          yes) Conserve flux?
+
+.KE
+.KS
+.V1
+                        -- SKY SUBTRACTION PARAMETERS --
+(combine=      average) Type of combine operation
+(reject =    avsigclip) Sky rejection option
+(scale  =         none) Sky scaling option
+
+.KE
+.V2
+.NH 2
+Extraction
+.LP
+The identification of the spectra in the two dimensional images and their
+scattered light subtraction and extraction to one dimensional spectra
+in multispec format is accomplished
+using the tasks from the \fBapextract\fR package.  The first parameters
+through \f(CWnsubaps\fR control the extractions.
+.LP
+The dispersion line is that used for finding the spectra, for plotting in
+the aperture editor, and as the starting point for tracing.  The default
+value of \fBINDEF\fR selects the middle of the image.  The aperture
+finding, adjusting, editing, and tracing operations also allow summing a
+number of dispersion lines to improve the signal.  The number of lines is
+set by the \f(CWnsum\fR parameter.
+.LP
+The \f(CWorder\fR parameter defines whether the order of the aperture
+identifications in the aperture identification table (or the default
+sequential numbers if no file is used) is in the same sense as the image
+coordinates (increasing) or the opposite sense (decreasing).  If the
+aperture identifications turn out to be opposite to what is desired when
+viewed in the aperture editing graph then simply change this parameter.
+.LP
+The basic data output by the spectral extraction routines are the one
+dimensional spectra.  Additional information may be output when the
+\f(CWextras\fR option is selected and the cleaning or variance weighting
+options are also selected.  In this case a three dimensional image is
+produced with the first element of the third dimension being the cleaned
+and/or weighted spectra, the second element being the uncleaned and
+unweighted spectra, and the third element being an estimate of the sigma
+of each pixel in the extracted spectrum.  Currently the sigma data is not
+used by any other tasks and is only for reference.
+.LP
+The initial step of finding the fiber spectra in the aperture reference
+image consists of identifying the peaks in a cut across the dispersion,
+eliminating those which are closer to each other than the \f(CWminsep\fR
+distance, and then keeping the specified \f(CWnfibers\fR highest peaks.  The
+centers of the profiles are determined using the \fBcenter1d\fR algorithm
+which uses the \f(CWwidth\fR parameter.
+.LP
+Apertures are then assigned to each spectrum.  The initial edges of the
+aperture relative to the center are defined by the \f(CWlower\fR and
+\f(CWupper\fR parameters.  The trickiest part of assigning the apertures is
+relating the aperture identification from the aperture identification table
+to automatically selected fiber profiles.  The first aperture id in the
+file is assigned to the first spectrum found using the \f(CWorder\fR
+parameter to select the assignment direction.  The numbering proceeds in
+this way except that if a gap greater than a multiple of the \f(CWmaxsep\fR
+parameter is encountered then assignments in the file are skipped under the
+assumption that a fiber is missing (broken).  In Hydra data it is expected
+that all fibers will be found in flat fields including the unassigned
+fibers and the assignment file will then identify the unassigned fibers.
+The unassigned fibers will later be excluded from extraction.  For more on
+the finding and assignment algorithms see \fBapfind\fR.
+.LP
+The initial apertures are the same for all spectra but they can each be
+automatically resized.  The automatic resizing sets the aperture limits
+at a fraction of the peak relative to the interfiber minimum.
+The default \fIylevel\fR is to resize the apertures to 5% of the peak.
+See the description for the task \fBapresize\fR for further details.
+.LP
+The user is given the opportunity to graphically review and adjust the
+aperture definitions.  This is recommended.  As mentioned previously, the
+correct identification of the fibers is tricky and it is fundamentally
+important that this be done correctly; otherwise the spectrum
+identifications will not be for the objects they say.  An important command in
+this regard is the 'o' key which allows reordering the identifications
+based on the aperture identification table.  This is required if the first
+fiber is actually missing since the initial assignment begins assigning the
+first spectrum found with the first entry in the aperture file.  The
+aperture editor is a very powerful tool and is described in detail as
+\fBapedit\fR.
+.LP
+The next set of parameters control the tracing and function fitting of the
+aperture reference positions along the dispersion direction.  The position
+of a spectrum across the dispersion is determined by the centering
+algorithm (see \fBcenter1d\fR) at a series of evenly spaced steps, given by
+the parameter \f(CWt_step\fR, along the dispersion.  The step size should be
+fine enough to follow position changes but it is not necessary to measure
+every point.  The fitted points may jump around a little bit due to noise
+and cosmic rays even when summing a number of lines.  Thus, a smooth
+function is fit.  The function type, order, and iterative rejection of
+deviant points is controlled by the other trace parameters.  For more
+discussion consult the help pages for \fBaptrace\fR and \fBicfit\fR.  The
+default is to fit a cubic spline of three pieces with a single iteration of
+3 sigma rejection.
+.LP
+The actual extraction of the spectra by summing across the aperture at each
+point along the dispersion is controlled by the next set of parameters.
+The default extraction simply sums the pixels using partial pixels at the
+ends.  The options allow selection of a weighted sum based on a Poisson
+variance model using the \f(CWreadnoise\fR and \f(CWgain\fR detector
+parameters.  Note that if the \f(CWclean\fR option is selected the variance
+weighted extraction is used regardless of the \f(CWweights\fR parameter.  The
+sigma thresholds for cleaning are also set in the \fBparams\fR parameters.
+For more on the variance weighted extraction and cleaning see
+\fBapvariance\fR and \fBapprofiles\fR as well as \fBapsum\fR.
+.LP
+The last parameter, \f(CWnsubaps\fR, is used only in special cases when it is
+desired to subdivide the fiber profiles into subapertures prior to
+dispersion correction.  After dispersion correction the subapertures are
+then added together.  The purpose of this is to correct for wavelength
+shifts across a fiber.
+.NH 2
+Scattered Light Subtraction
+.LP
+Scattered light may be subtracted from the input two dimensional image as
+the first step.  This is done using the algorithm described in
+\fBapscatter\fR.  This can be important if there is significant scattered
+light since the flat field/throughput correction will otherwise be
+incorrect.  The algorithm consists of fitting a function to the data
+outside the defined apertures by a specified \fIbuffer\fR at each line or
+column across the dispersion.  The function fitting parameters are the same
+at each line.  Because the fitted functions are independent at each line or
+column a second set of one dimensional functions are fit parallel to the
+dispersion using the evaluated fit values from the cross-dispersion step.
+This produces a smooth scattered light surface which is finally subtracted
+from the input image.  Again the function fitting parameters are the
+same at each line or column though they may be different than the parameters
+used to fit across the dispersion.
+.LP
+The first time the task is run with a particular flat field (or aperture
+reference image if no flat field is used) the scattered light fitting
+parameters are set interactively using that image.  The interactive step
+selects a particular line or column upon which the fitting is done
+interactively with the \fBicfit\fR commands.  A query is first issued
+which allows skipping this interactive stage.  Note that the interactive
+fitting is only for defining the fitting functions and orders.  When
+the graphical \fBicfit\fR fitting is exited (with 'q') there is a second prompt
+allowing you to change the buffer distance (in the first cross-dispersion
+stage) from the apertures, change the line/column, or finally quit.
+.LP
+The initial fitting parameters and the final set parameters are recorded
+in the \fBapscat1\fR and \fBapscat2\fR hidden parameter sets.  These
+parameters are then used automatically for every subsequent image
+which is scattered light corrected.
+.LP
+The scattered light subtraction modifies the input 2D images.  To preserve
+the original data a copy of the original image is made with the same
+root name and the word "noscat" appended.  The scattered light subtracted
+images will have the header keyword "APSCATTE" which is how the task
+avoids repeating the scattered light subtraction during any reprocessing.
+However if the \fIredo\fR option is selected the scattered light subtraction
+will also be redone by first restoring the "noscat" images to the original
+input names.
+.NH 2
+Flat Field and Fiber Throughput Corrections
+.LP
+Flat field corrections may be made during the basic CCD processing; i.e.
+direct division by the two dimensional flat field observation.  In that
+case do not specify a flat field spectrum; use the null string "".  The
+\fBdohydra\fR task provides an alternative flat field response correction
+based on division of the extracted object spectra by the extracted flat field
+spectra.  A discussion of the theory and merits of flat fielding directly
+verses using the extracted spectra will not be made here.  The
+\fBdohydra\fR flat fielding algorithm is the \fIrecommended\fR method for
+flat fielding since it works well and is not subject to the many problems
+involved in two dimensional flat fielding.
+.LP
+In addition to correcting for pixel-to-pixel response the flat field step
+also corrects for differences in the fiber throughput.  Thus, even if the
+pixel-to-pixel flat field corrections have been made in some other way it
+is desirable to use a sky or dome flat observation for determining a fiber
+throughput correction.  Alternatively, a separately derived throughput
+file may be specified.  This file consists of the aperture numbers
+(the same as used for the aperture reference) and relative throughput
+numbers.
+.LP
+The first step is extraction of the flat field spectrum, if specified,
+using the reference apertures.  Only one flat field is allowed so if
+multiple flat fields are required the data must be reduced in groups.
+After extraction one or more corrections are applied.  If the \f(CWfitflat\fR
+option is selected (the default) the extracted flat field spectra are
+averaged together and a smooth function is fit.  The default fitting
+function and order are given by the parameters \f(CWf_function\fR and
+\f(CWf_order\fR.  If the parameter \f(CWf_interactive\fR is "yes" then the
+fitting is done interactively using the \fBfit1d\fR task which uses the
+\fBicfit\fR interactive fitting commands.
+.LP
+The fitted function is divided into the individual flat field spectra to
+remove the basic shape of the spectrum while maintaining the relative
+individual pixel responses and any fiber to fiber differences.  This step
+avoids introducing the flat field spectrum shape into the object spectra
+and closely preserves the object counts.
+.LP
+If a throughput image is available (an observation of blank sky
+usually at twilight) it is extracted.  If no flat field is used the average
+signal through each fiber is computed and this becomes the response
+normalization function.  Note that a dome flat may be used in place of a
+sky in the sky flat field parameter for producing throughput only
+corrections.  If a flat field is specified then each sky spectrum is
+divided by the appropriate flat field spectrum.  The total counts through
+each fiber are multiplied into the flat field spectrum thus making the sky
+throughput of each fiber the same.  This correction is important if the
+illumination of the fibers differs between the flat field source and the
+sky.  Since only the total counts are required the sky or dome flat field
+spectra need not be particularly strong though care must be taken to avoid
+objects.
+.LP
+Instead of a sky flat or other throughput image a separately derived
+throughput file may be used.  It may be used with or without a
+flat field.
+.LP
+The final step is to normalize the flat field spectra by the mean counts of
+all the fibers.  This normalization step is simply to preserve the average
+counts of the extracted object and arc spectra after division by the
+response spectra.  The final relative throughput values are recorded in the
+log and possibly printed on the terminal.
+.LP
+These flat field response steps and algorithm are available as a separate
+task called \fBmsresp1d\fR.
+.NH 2
+Dispersion Correction
+.LP
+Dispersion corrections are applied to the extracted spectra if the
+\fBdispcor\fR parameter is set.  This can be a complicated process which
+the \fBdohydra\fR task tries to simplify for you.  There are three basic
+steps involved; determining the dispersion functions relating pixel
+position to wavelength, assigning the appropriate dispersion function to a
+particular observation, and resampling the spectra to evenly spaced pixels
+in wavelength.
+.LP
+The comparison arc spectra are used to define dispersion functions for the
+fibers using the tasks \fBautoidentify\fR and \fBreidentify\fR.  The
+interactive \fBautoidentify\fR task is only used on the central fiber of the
+first arc spectrum to define the basic reference dispersion solution from
+which all other fibers and arc spectra are automatically derived using
+\fBreidentify\fR. \fBAutoidentify\fR attempts to automatically identify
+the arc lines using the \fIcrval\fR and \fIcdelt\fR parameters.  Whether
+or not it is successful the user is presented with the interactive
+identification graph.  The automatic identifications can be reviewed and a
+new solution or corrections to the automatic solution may be performed.
+.LP
+The set of arc dispersion function parameters are from \fBautoidentify\fR and
+\fBreidentify\fR.  The parameters define a line list for use in
+automatically assigning wavelengths to arc lines, a parameter controlling
+the width of the centering window (which should match the base line
+widths), the dispersion function type and order, parameters to exclude bad
+lines from function fits, and parameters defining whether to refit the
+dispersion function, as opposed to simply determining a zero point shift,
+and the addition of new lines from the line list when reidentifying
+additional arc spectra.  The defaults should generally be adequate and the
+dispersion function fitting parameters may be altered interactively.  One
+should consult the help for the two tasks for additional details of these
+parameters and the operation of \fBautoidentify\fR.
+.LP
+Generally, taking a number of comparison arc lamp exposures interspersed
+with the program spectra is sufficient to accurately dispersion calibrate
+Hydra spectra.  However, there are some other calibration options
+which may be of interest.  These options apply additional calibration data
+consisting either of auxiliary line spectra, such as from dome lights or
+night sky lines, or simultaneous arc lamp spectra taken through a few
+fibers during the object exposure.  These options add complexity to the
+dispersion calibration process and were provided primarily for Nessie
+data.  Therefore they are described later in the Nessie section.
+.LP
+When only arc comparison lamp spectra are used,  dispersion functions are
+determined independently for each fiber of each arc image and then assigned
+to the matching fibers in the program object observations.  The assignment
+consists of selecting one or two arc images to calibrate each object
+image.  When two bracketing arc spectra are used the dispersion functions
+are linearly interpolated (usually based on the time of the observations).
+.LP
+The arc assignments may be done either explicitly with an arc assignment
+table (parameter \f(CWarctable\fR) or based on a header parameter.  The task
+used is \fBrefspectra\fR and the user should consult this task if the
+default behavior is not what is desired.  The default is to interpolate
+linearly between the nearest arcs based on the Julian date (corrected to
+the middle of the exposure).  The Julian date and a local Julian day number
+(the day number at local noon) are computed automatically by the task
+\fBsetjd\fR and recorded in the image headers under the keywords JD and
+LJD.  In addition the universal time at the middle of the exposure, keyword
+UTMIDDLE, is computed by the task \fBsetairmass\fR and this may also be used
+for ordering the arc and object observations.
+.LP
+An optional step is to use sky lines in the spectra to compute a zeropoint
+dispersion shift that will align the sky lines.  This may improve sky
+subtraction if the illumination is not the same between the arc calibration
+and the sky.  When selected the object spectrum is dispersion corrected
+using a non-linear dispersion function to avoid resampling the spectrum.
+The sky lines are then reidentified in wavelength space from a template
+list of sky lines.  The mean shift in the lines for each fiber relative to
+the template in that fiber is computed to give the zeropoint shift.  The
+database file is created when the first object is extracted.  You are asked
+to mark the sky lines in one fiber and then the lines are automatically
+reidentified in all other fibers.  Note that this technique requires the
+sky lines be found in all fibers.
+.LP
+The last step of dispersion correction (resampling the spectrum to evenly
+spaced pixels in wavelength) is optional and relatively straightforward.
+If the \f(CWlinearize\fR parameter is no then the spectra are not resampled
+and the nonlinear dispersion information is recorded in the image header.
+Other IRAF tasks (the coordinate description is specific to IRAF) will use
+this information whenever wavelengths are needed.  If linearizing is
+selected a linear dispersion relation, either linear in the wavelength or
+the log of the wavelength, is defined once and applied to every extracted
+spectrum.  The resampling algorithm  parameters allow selecting the
+interpolation function type, whether to conserve flux per pixel by
+integrating across the extent of the final pixel, and whether to linearize
+to equal linear or logarithmic intervals.  The latter may be appropriate
+for radial velocity studies.  The default is to use a fifth order
+polynomial for interpolation, to conserve flux, and to not use logarithmic
+wavelength bins.  These parameters are described fully in the help for the
+task \fBdispcor\fR which performs the correction.  The interpolation
+function options and the nonlinear dispersion coordinate system is
+described in the help topic \fBonedspec.package\fR.
+.NH 2
+Sky Subtraction
+.LP
+Sky subtraction is selected with the \f(CWskysubtract\fR processing option.
+The sky spectra are selected by their aperture and beam numbers and
+combined into a single master sky spectrum
+which is then subtracted from each object spectrum.  If the \f(CWskyedit\fR
+option is selected the sky spectra are plotted using the task
+\fBspecplot\fR.  By default they are superposed to allow identifying
+spectra with unusually high signal due to object contamination.  To
+eliminate a sky spectrum from consideration point at it with the cursor and
+type 'd'.  The last deleted spectrum may be undeleted with 'e'.  This
+allows recovery of incorrect or accidental deletions.
+.LP
+The sky combining algorithm parameters define how the individual sky fiber
+spectra, after interactive editing, are combined before subtraction from
+the object fibers.  The goals of combining are to reduce noise, eliminate
+cosmic-rays, and eliminate fibers with inadvertent objects.  The common
+methods for doing this to use a median and/or a special sigma clipping
+algorithm (see \fBscombine\fR for details).  The scale
+parameter determines whether the individual skys are first scaled to a
+common mode.  The scaling should be used if the throughput is uncertain,
+but in that case you probably did the wrong thing in the throughput
+correction.  If the sky subtraction is done interactively, i.e. with the
+\f(CWskyedit\fR option selected, then after selecting the spectra to be
+combined a query is made for the combining algorithm.  This allows
+modifying the default algorithm based on the number of sky spectra
+selected since the "avsigclip" rejection algorithm requires at least
+three spectra.
+.LP
+The combined sky spectrum is subtracted from only those spectra specified
+by the object aperture and beam numbers.  Other spectra, such as comparison
+arc spectra, are retained unchanged.  One may include the sky spectra as
+object spectra to produce residual sky spectra for analysis.  The combined
+master sky spectra may be saved if the \f(CWsaveskys\fR parameter is set.
+The saved sky is given the name of the object spectrum with the prefix
+"sky".
+.NH
+Nessie Data
+.LP
+Reducing Nessie data with \fBdohydra\fR is very similar.  The differences
+are that additional setup and calibration are required since this
+instrument was a precursor to the more developed Hydra instrument.
+The discussion in this section also describes some features which may
+be applicable to other fiber instruments outside of the NOAO instruments.
+.LP
+The Nessie comparison lamp exposures suffer from vignetting resulting in
+some fibers being poorly illuminated.  By rearranging the fibers in the
+calibration plugboard and taking additional exposures one can obtain good
+arc spectra through all fibers.  The task will merge the well exposed
+fibers from the multiple exposures into a single final extracted
+arc calibration image.  One of the exposures of a set is selected as
+the primary exposure.  This is the one specified in list of arcs,
+\f(CWarc1\fR.  The other exposures of the set are referenced only in
+a a setup file, called an \fIarc replacement file\fR.
+.LP
+The format of the arc replacement file is lines containing the primary
+arc image, a secondary arc image,
+and the apertures from the secondary arc to be merged into the
+final arc spectra.  There can be more than one secondary
+exposure though it is unlikely.  Figure 4 gives an example of this
+setup file.
+
+.ce
+Figure 4: Example Arc Aperture Replacement File
+
+.V1
+    cl> type arcreplace
+    nesjun042c nesjun049c 1,7,9,13,17,19,28,34
+.V2
+
+.fi
+The primary arc exposure is \f(CWnesjun042c\fR, the secondary arc is
+\f(CWnesjun049c\fR, and the secondary apertures are 1, 7, etc.  The syntax for
+the list of apertures also includes hyphen delimited ranges such as
+"8-10".
+.LP
+With Hydra the aperture identification table is produced for the user.  With
+Nessie this is not the case, hence, the user must prepare a file
+manually.  The aperture identification file is not mandatory, sequential
+numbering will be used, but it is highly recommended for keeping track of
+the objects assigned to the fibers.  The aperture identification file
+contains lines consisting of an aperture number, a beam number, and an
+object identification.  These must be in the same order as the fibers in
+the image.  The aperture number may be any unique number but it is
+recommended that the fiber number be used.  The beam number is used to flag
+object, sky, arc, or other types of spectra.  The default beam numbers used
+by the task are 0 for sky, 1 for object, and 2 for arc.  The object
+identifications are optional but it is good practice to include them so
+that the data will contain the object information independent of other
+records.  Figure 5 shows an example for the \fIblue\fR fibers from a board
+called M33Sch2.
+
+.ce
+Figure 5: Example Aperture Identification File
+
+.V1
+    cl> type m33sch2
+    1 1 143
+    2 1 254
+    3 0 sky
+    4 1 121
+    5 2 arc
+       .
+       .
+       .
+    44 1 s92
+    49 -1 Broken
+    45 1 156
+    46 2 arc
+    47 0 sky
+    48 1 phil2
+.V2
+
+Note the identification of the sky fibers with beam number 0, the object
+fibers with 1, and the arc fibers with 2.  Also note that broken fiber 49
+is actually between fibers 44 and 45.  The broken fiber entries, given beam
+number -1, are optional but recommended to give the automatic spectrum
+finding operation the best chance to make the correct identifications.  The
+identification file will vary for each plugboard setup.  Additional
+information about the aperture identification table may be found in the
+description of the task \fBapfind\fR.
+.LP
+An alternative to using an aperture identification table is to give no
+name, the "" empty string, and to explicitly give a range of
+aperture numbers for the skys and possibly for the sky subtraction
+object list in the parameters \f(CWobjaps, skyaps, arcaps, objbeams,
+skybeams,\fR and \f(CWarcbeams\fR.
+.LP
+Because taking comparison exposures with Nessie requires replugging the
+fibers, possibly in more than one configuration, and the good stability of
+the instrument, there are two mutually exclusive methods for monitoring
+shifts in the dispersion zero point from the basic arc lamp spectra other
+than taking many arc lamp exposures.  One is to use some fibers to take a
+simultaneous arc spectrum while observing the program objects.  The fibers
+are identified by aperture or beam numbers.  The second method is to use
+\fIauxiliary line spectra\fR, such as mercury lines from the dome lights.
+These spectra are specified with an auxiliary shift arc list, \f(CWarc2\fR.
+.LP
+When using auxiliary line spectra for monitoring zero point shifts one of
+these spectra is plotted interactively by \fBidentify\fR with the
+reference dispersion function from the reference arc spectrum.  The user
+marks one or more lines which will be used to compute zero point wavelength
+shifts in the dispersion functions automatically.  The actual wavelengths
+of the lines need not be known.  In this case accept the wavelength based
+on the reference dispersion function.  As other observations of the same
+features are made the changes in the positions of the features will be
+tracked as zero point wavelength changes such that wavelengths of the
+features remain constant.
+.LP
+When using auxiliary line spectra the only arc lamp spectrum used is the
+initial arc reference spectrum (the first image in the \f(CWarcs1\fR list).
+The master dispersion functions are then shifted based on the spectra in
+the \f(CWarcs2\fR list (which must all be of the same type).  The dispersion
+function assignments made by \fBrefspectra\fR using either the arc
+assignment file or based on header keywords is done in the same way as
+described for the arc lamp images except using the auxiliary spectra.
+.LP
+If simultaneous arcs are used the arc lines are reidentified to determine a
+zero point shift relative to the comparison lamp spectra selected, by
+\fBrefspectra\fR, of the same fiber.  A linear function of aperture
+position on the image across the dispersion verses the zero point shifts
+from the arc fibers is determined and applied to the dispersion functions
+from the assigned calibration arcs for the non-arc fibers.  Note that if
+there are two comparison lamp spectra (before and after the object
+exposure) then there will be two shifts applied to two dispersion functions
+which are then combined using the weights based on the header parameters
+(usually the observation time).
+.NH
+References
+.NH 2
+IRAF Introductory References
+.LP
+Work is underway on a new introductory guide to IRAF.  Currently, the
+work below is the primary introduction.
+.IP
+P. Shames and D. Tody, \fIA User's Introduction to the IRAF Command
+Language\fR, Central Computer Services, NOAO, 1986.
+.NH 2
+CCD Reductions
+.IP
+F. Valdes, \fIThe IRAF CCD Reduction Package -- CCDRED\fR, Central
+Computer Services, NOAO, 1987.
+.IP
+F. Valdes, \fIUser's Guide to the CCDRED Package\fR, Central
+Computer Services, NOAO, 1988.  Also on-line as \f(CWhelp ccdred.guide\fR.
+.IP
+P. Massey, \fIA User's Guide to CCD Reductions with IRAF\fR, Central
+Computer Services, NOAO, 1989.
+.NH 2
+Aperture Extraction Package
+.IP
+F. Valdes, \fIThe IRAF APEXTRACT Package\fR, Central Computer Services,
+NOAO, 1987 (out-of-date).
+.NH 2
+Task Help References
+.LP
+Each task in the \fBhydra\fR package and tasks used by \fBdohydra\fR have
+help pages describing the parameters and task in some detail.  To get
+on-line help type
+.V1
+
+cl> help \fItaskname\fR
+
+.V2
+The output of this command can be piped to \fBlprint\fR to make a printed
+copy.
+
+.V1
+      apall - Extract 1D spectra (all parameters in one task)
+  apdefault - Set the default aperture parameters
+     apedit - Edit apertures interactively
+     apfind - Automatically find spectra and define apertures
+ aprecenter - Recenter apertures
+   apresize - Resize apertures
+  apscatter - Fit and subtract scattered light
+      apsum - Extract 1D spectra
+    aptrace - Trace positions of spectra
+
+      bplot - Batch plots of spectra
+  continuum - Fit the continuum in spectra
+    dispcor - Dispersion correct spectra
+     dopcor - Doppler correct spectra
+   identify - Identify features in spectrum for dispersion solution
+   msresp1d - Create 1D response spectra from flat field and sky spectra
+ refspectra - Assign wavelength reference spectra to other spectra
+ reidentify - Automatically identify features in spectra
+ sapertures - Set or change aperture header information
+     sarith - Spectrum arithmetic
+   scombine - Combine spectra having different wavelength ranges
+      scopy - Select and copy apertures in different spectral formats
+ setairmass - Compute effective airmass and middle UT for an exposure
+      setjd - Compute and set Julian dates in images
+      slist - List spectrum header parameters
+   specplot - Stack and plot multiple spectra
+      splot - Preliminary spectral plot/analysis
+
+    dohydra - Process HYDRA spectra
+      demos - Demonstrations and tests
+
+	    Additional help topics
+
+   onedspec.package - Package parameters and general description of package
+  apextract.package - Package parameters and general description of package
+ approfiles - Profile determination algorithms
+ apvariance - Extractions, variance weighting, cleaning, and noise model
+   center1d - One dimensional centering algorithm
+      icfit - Interactive one dimensional curve fitting
+.V2
+.SH
+Appendix A:  DOHYDRA Parameters
+.LP
+.nr PS 8
+.nr VS 10
+objects
+.LS
+List of object spectra to be processed.  Previously processed spectra are
+ignored unless the \f(CWredo\fR flag is set or the \f(CWupdate\fR flag is set and
+dependent calibration data has changed.  Extracted spectra are ignored.
+.LE
+apref = ""
+.LS
+Aperture reference spectrum.  This spectrum is used to define the basic
+extraction apertures and is typically a flat field spectrum.
+.LE
+flat = "" (optional)
+.LS
+Flat field spectrum.  If specified the one dimensional flat field spectra
+are extracted and used to make flat field calibrations.  If a separate
+throughput file or image is not specified the flat field is also used
+for computing a fiber throughput correction.
+.LE
+throughput = "" (optional)
+.LS
+Throughput file or image.  If an image is specified, typically a blank
+sky observation, the total flux through
+each fiber is used to correct for fiber throughput.  If a file consisting
+of lines with the aperture number and relative throughput is specified
+then the fiber throughput will be corrected by those values.  If neither
+is specified but a flat field image is given it is used to compute the
+throughput.  
+.LE
+arcs1 = "" (at least one if dispersion correcting)
+.LS
+List of primary arc spectra.  These spectra are used to define the dispersion
+functions for each fiber apart from a possible zero point correction made
+with secondary shift spectra or arc calibration fibers in the object spectra.
+One fiber from the first spectrum is used to mark lines and set the dispersion
+function interactively and dispersion functions for all other fibers and
+arc spectra are derived from it.
+.LE
+arcs2 = "" (optional for Nessie)
+.LS
+List of optional shift arc spectra.  Features in these secondary observations
+are used to supply a wavelength zero point shift through the observing
+sequence.  One type of observation is dome lamps containing characteristic
+emission lines.
+.LE
+arcreplace = "" (optional for Nessie)
+.LS
+Special aperture replacement file.  A characteristic of Nessie (though not
+Hydra) spectra is that it requires two exposures to illuminate all fibers
+with an arc calibration.  The aperture replacement file assigns fibers from
+the second exposure to replace those in the first exposure.  Only the first
+exposures are specified in the \f(CWarcs1\fR list.  The file contains lines
+with the first exposure image name, the second exposure image name, and a
+list of apertures from the second exposure to be used instead of those in
+the first exposure.
+.LE
+arctable = "" (optional) (refspectra)
+.LS
+Table defining arc spectra to be assigned to object
+spectra (see \fBrefspectra\fR).  If not specified an assignment based
+on a header parameter, \f(CWparams.sort\fR, such as the observation time is made.
+.LE
+
+readnoise = "RDNOISE" (apsum)
+.LS
+Read out noise in photons.  This parameter defines the minimum noise
+sigma.  It is defined in terms of photons (or electrons) and scales
+to the data values through the gain parameter.  A image header keyword
+(case insensitive) may be specified to get the value from the image.
+.LE
+gain = "GAIN" (apsum)
+.LS
+Detector gain or conversion factor between photons/electrons and
+data values.  It is specified as the number of photons per data value.
+A image header keyword (case insensitive) may be specified to get the value
+from the image.
+.LE
+datamax = INDEF (apsum.saturation)
+.LS
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the flat field or
+arc spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.LE
+fibers = 97 (apfind)
+.LS
+Number of fibers.  This number is used during the automatic definition of
+the apertures from the aperture reference spectrum.  It is best if this
+reflects the actual number of fibers which may be found in the aperture
+reference image.  The interactive
+review of the aperture assignments allows verification and adjustments
+to the automatic aperture definitions.
+.LE
+width = 12. (apedit)
+.LS
+Approximate base full width of the fiber profiles.  This parameter is used
+for the profile centering algorithm.
+.LE
+minsep = 8. (apfind)
+.LS
+Minimum separation between fibers.  Weaker spectra or noise within this
+distance of a stronger spectrum are rejected.
+.LE
+maxsep = 15. (apfind)
+.LS
+Maximum separation between adjacent fibers.  This parameter
+is used to identify missing fibers.  If two adjacent spectra exceed this
+separation then it is assumed that a fiber is missing and the aperture
+identification assignments will be adjusted accordingly.
+.LE
+apidtable = "" (apfind)
+.LS
+Aperture identification table.  This may be either a text file or an
+image.  A text file contains the fiber number, beam number defining object
+(1), sky (0), and arc (2) fibers, and a object title.  An image contains
+the keywords SLFIBnnn with string value consisting of the fiber number,
+beam number, optional right ascension and declination, and an object
+title.  For Nessie the user had to prepare the file for each plugboard, for
+Hydra at the 4meter the file was generated for the user, and for Hydra at
+the WIYN the image header contains the information.  Unassigned and broken
+fibers (beam of -1) should be included in the identification information
+since they will automatically be excluded.
+.LE
+crval = INDEF, cdelt = INDEF (autoidentify)
+.LS
+These parameters specify an approximate central wavelength and dispersion.
+They may be specified as numerical values, INDEF, or image header keyword
+names whose values are to be used.
+If both these parameters are INDEF then the automatic identification will
+not be done.
+.LE
+objaps = "", skyaps = "", arcaps = ""
+.LS
+List of object, sky, and arc aperture numbers.  These are used to
+identify arc apertures for wavelength calibration and object and sky
+apertures for sky subtraction.  Note sky apertures may be identified as
+both object and sky if one wants to subtract the mean sky from the
+individual sky spectra.  Typically the different spectrum types are
+identified by their beam numbers and the default, null string,
+lists select all apertures.
+.LE
+objbeams = "0,1", skybeams = "0", arcbeams = 2
+.LS
+List of object, sky, and arc beam numbers.  The convention is that sky
+fibers are given a beam number of 0, object fibers a beam number of 1, and
+arc fibers a beam number of 2.  The beam numbers are typically set in the
+\f(CWapidtable\fR.  Unassigned or broken fibers may be given a beam number of
+-1 in the aperture identification table since apertures with negative beam
+numbers are not extracted.  Note it is valid to identify sky fibers as both
+object and sky.
+.LE
+
+scattered = no (apscatter)
+.LS
+Smooth and subtracted scattered light from the object and flat field
+images.  This operation consists of fitting independent smooth functions
+across the dispersion using data outside the fiber apertures and then
+smoothing the individual fits along the dispersion.  The initial
+flat field, or if none is given the aperture reference image, are
+done interactively to allow setting the fitting parameters.  All
+subsequent subtractions use the same fitting parameters.
+.LE
+fitflat = yes (flat1d)
+.LS
+Fit the composite flat field spectrum by a smooth function and divide each
+flat field spectrum by this function?  This operation removes the average
+spectral signature of the flat field lamp from the sensitivity correction to
+avoid modifying the object fluxes.
+.LE
+clean = yes (apsum)
+.LS
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction and requires reasonably good values
+for the readout noise and gain.  In addition the datamax parameters
+can be useful.
+.LE
+dispcor = yes
+.LS
+Dispersion correct spectra?  Depending on the \f(CWparams.linearize\fR
+parameter this may either resample the spectra or insert a dispersion
+function in the image header.
+.LE
+savearcs = yes
+.LS
+Save any simultaneous arc apertures?  If no then the arc apertures will
+be deleted after use.
+.LE
+skyalign = no
+.LS
+Align sky lines?  If yes then for the first object spectrum you are asked
+to mark one or more sky lines to use for alignment.  Then these lines will
+be found in all spectra and an average zeropoint shift computed and applied
+to the dispersion solution to align these lines.  Note that this assumes
+the sky lines are seen in all fibers.
+.LE
+skysubtract = yes
+.LS
+Subtract sky from the object spectra?  If yes the sky spectra are combined
+and subtracted from the object spectra as defined by the object and sky
+aperture/beam parameters.
+.LE
+skyedit = yes
+.LS
+Overplot all the sky spectra and allow contaminated sky spectra to be
+deleted?
+.LE
+saveskys = yes
+.LS
+Save the combined sky spectrum?  If no then the sky spectrum will be
+deleted after sky subtraction is completed.
+.LE
+splot = no
+.LS
+Plot the final spectra with the task \fBsplot\fR?
+.LE
+redo = no
+.LS
+Redo operations previously done?  If no then previously processed spectra
+in the objects list will not be processed (unless they need to be updated).
+.LE
+update = yes
+.LS
+Update processing of previously processed spectra if aperture, flat
+field, or dispersion reference definitions are changed?
+.LE
+batch = no
+.LS
+Process spectra as a background or batch job provided there are no interactive
+options (\f(CWskyedit\fR and \f(CWsplot\fR) selected.
+.LE
+listonly = no
+.LS
+List processing steps but don't process?
+.LE
+
+params = "" (pset)
+.LS
+Name of parameter set containing additional processing parameters.  The
+default is parameter set \fBparams\fR.  The parameter set may be examined
+and modified in the usual ways (typically with "epar params" or ":e params"
+from the parameter editor).  Note that using a different parameter file
+is not allowed.  The parameters are described below.
+.LE
+
+.ce
+-- PACKAGE PARAMETERS
+
+Package parameters are those which generally apply to all task in the
+package.  This is also true of \fBdohydra\fR.
+
+dispaxis = 2
+.LS
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.  The default value defers to the
+package parameter of the same name.
+.LE
+observatory = "observatory"
+.LS
+Observatory at which the spectra were obtained if not specified in the
+image header by the keyword OBSERVAT.  For Hydra data the image headers
+identify the observatory as "kpno" so this parameter is not used.
+For data from other observatories this parameter may be used
+as describe in \fBobservatory\fR.
+.LE
+interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc)
+.LS
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.V1
+	nearest - nearest neighbor
+	 linear - linear
+	  poly3 - 3rd order polynomial
+	  poly5 - 5th order polynomial
+	spline3 - cubic spline
+	   sinc - sinc function
+.V2
+.LE
+database = "database"
+.LS
+Database (directory) used for storing aperture and dispersion information.
+.LE
+verbose = no
+.LS
+Print verbose information available with various tasks.
+.LE
+logfile = "logfile", plotfile = ""
+.LS
+Text and plot log files.  If a filename is not specified then no log is
+kept.  The plot file contains IRAF graphics metacode which may be examined
+in various ways such as with \fBgkimosaic\fR.
+.LE
+records = ""
+.LS
+Dummy parameter to be ignored.
+.LE
+version = "HYDRA: ..."
+.LS
+Version of the package.
+.LE
+
+.ce
+PARAMS PARAMETERS
+
+The following parameters are part of the \fBparams\fR parameter set and
+define various algorithm parameters for \fBdohydra\fR.
+
+.ce
+--  GENERAL PARAMETERS --
+
+line = INDEF, nsum = 10
+.LS
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, recentering, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.LE
+order = "decreasing" (apfind)
+.LS
+When assigning aperture identifications order the spectra "increasing"
+or "decreasing" with increasing pixel position (left-to-right or
+right-to-left in a cross-section plot of the image).
+.LE
+extras = no (apsum)
+.LS
+Include extra information in the output spectra?  When cleaning or using
+variance weighting the cleaned and weighted spectra are recorded in the
+first 2D plane of a 3D image, the raw, simple sum spectra are recorded in
+the second plane, and the estimated sigmas are recorded in the third plane.
+.LE
+
+.ce
+-- DEFAULT APERTURE LIMITS --
+
+lower = -5., upper = 5. (apdefault)
+.LS
+Default lower and upper aperture limits relative to the aperture center.
+These limits are used when the apertures are first found and may be
+resized automatically or interactively.
+.LE
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+
+ylevel = 0.05 (apresize)
+.LS
+Data level at which to set aperture limits during automatic resizing.
+It is a fraction of the peak relative to a local background.
+.LE
+
+.ce
+-- TRACE PARAMETERS --
+
+t_step = 10 (aptrace)
+.LS
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \f(CWnsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.LE
+t_function = "spline3", t_order = 3 (aptrace)
+.LS
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.LE
+t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+.LS
+Default number of rejection iterations and rejection sigma thresholds.
+.LE
+
+.ce
+-- SCATTERED LIGHT PARAMETERS --
+
+buffer = 1. (apscatter)
+.LS
+Buffer distance from the aperture edges to be excluded in selecting the
+scattered light pixels to be used.
+.LE
+apscat1 = "" (apscatter)
+.LS
+Fitting parameters across the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat1"
+parameter set.
+.LE
+apscat2 = "" (apscatter)
+.LS
+Fitting parameters along the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat2"
+parameter set.
+.LE
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+
+weights = "none" (apsum)
+.LS
+Type of extraction weighting.  Note that if the \f(CWclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+
+"none"
+.LS
+The pixels are summed without weights except for partial pixels at the
+ends.
+.LE
+"variance"
+.LS
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \f(CWgain\fR and \f(CWreadnoise\fR
+parameters.
+.LE
+.LE
+pfit = "fit1d" (apsum) (fit1d|fit2d)
+.LS
+Profile fitting algorithm for cleaning and variance weighted extractions.
+The default is generally appropriate for Hydra/Nessie data but users
+may try the other algorithm.  See \fBapprofiles\fR for further information.
+.LE
+lsigma = 3., usigma = 3. (apsum)
+.LS
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.LE
+nsubaps = 1 (apsum)
+.LS
+During extraction it is possible to equally divide the apertures into
+this number of subapertures.
+.LE
+
+.ce
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --
+
+f_interactive = yes (fit1d)
+.LS
+Fit the composite one dimensional flat field spectrum interactively?
+This is used if \f(CWfitflat\fR is set and a two dimensional flat field
+spectrum is specified.
+.LE
+f_function = "spline3", f_order = 10 (fit1d)
+.LS
+Function and order used to fit the composite one dimensional flat field
+spectrum.  The functions are "legendre", "chebyshev", "spline1", and
+"spline3".  The spline functions are linear and cubic splines with the
+order specifying the number of pieces.
+.LE
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+
+threshold = 10. (autoidentify/identify/reidentify)
+.LS
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.LE
+coordlist = "linelists$idhenear.dat" (autoidentify/identify)
+.LS
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelists$".
+.LE
+match = -3. (autoidentify/identify)
+.LS
+The maximum difference for a match between the dispersion function prediction
+value and a wavelength in the coordinate list.
+.LE
+fwidth = 4. (autoidentify/identify)
+.LS
+Approximate full base width (in pixels) of arc lines.
+.LE
+cradius = 10. (reidentify)
+.LS
+Radius from previous position to reidentify arc line.
+.LE
+i_function = "spline3", i_order = 3 (autoidentify/identify)
+.LS
+The default function and order to be fit to the arc wavelengths as a
+function of the pixel coordinate.  The functions choices are "chebyshev",
+"legendre", "spline1", or "spline3".
+.LE
+i_niterate = 2, i_low = 3.0, i_high = 3.0 (autoidentify/identify)
+.LS
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.LE
+refit = yes (reidentify)
+.LS
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.LE
+addfeatures = no (reidentify)
+.LS
+Add new features from a line list during each reidentification?
+This option can be used to compensate for lost features from the
+reference solution.  Care should be exercised that misidentified features
+are not introduced.
+.LE
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+
+select = "interp" (refspectra)
+.LS
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+
+average
+.LS
+Average two reference spectra without regard to any sort parameter.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.
+This option is used to assign two reference spectra, with equal weights,
+independent of any sorting parameter.
+.LE
+following
+.LS
+Select the nearest following spectrum in the reference list based on the
+sorting parameter.  If there is no following spectrum use the nearest preceding
+spectrum.
+.LE
+interp
+.LS
+Interpolate between the preceding and following spectra in the reference
+list based on the sorting parameter.  If there is no preceding and following
+spectrum use the nearest spectrum.  The interpolation is weighted by the
+relative distances of the sorting parameter.
+.LE
+match
+.LS
+Match each input spectrum with the reference spectrum list in order.
+This overrides the reference aperture check.
+.LE
+nearest
+.LS
+Select the nearest spectrum in the reference list based on the sorting
+parameter.
+.LE
+preceding
+.LS
+Select the nearest preceding spectrum in the reference list based on the
+sorting parameter.  If there is no preceding spectrum use the nearest following
+spectrum.
+.LE
+.LE
+sort = "jd", group = "ljd" (refspectra)
+.LS
+Image header keywords to be used as the sorting parameter for selection
+based on order and to group spectra.
+A null string, "", or the word "none" may be use to disable the sorting
+or grouping parameters.
+The sorting parameter
+must be numeric but otherwise may be anything.  The grouping parameter
+may be a string or number and must simply be the same for all spectra within
+the same group (say a single night).
+Common sorting parameters are times or positions.
+In \fBdohydra\fR the Julian date (JD) and the local Julian day number (LJD)
+at the middle of the exposure are automatically computed from the universal
+time at the beginning of the exposure and the exposure time.  Also the
+parameter UTMIDDLE is computed.
+.LE
+time = no, timewrap = 17. (refspectra)
+.LS
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.LE
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+
+linearize = yes (dispcor)
+.LS
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling
+If no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data are not interpolated.
+.LE
+log = no (dispcor)
+.LS
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.LE
+flux = yes (dispcor)
+.LS
+Conserve the total flux during interpolation?  If \f(CWno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \f(CWyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.LE
+
+.ce
+-- SKY SUBTRACTION PARAMETERS --
+
+combine = "average" (scombine) (average|median)
+.LS
+Option for combining sky pixels at the same dispersion coordinate after any
+rejection operation.  The options are to compute the  "average" or "median"
+of the pixels.  The median uses the average of the two central
+values when the number of pixels is even.
+.LE
+reject = "none" (scombine) (none|minmax|avsigclip)
+.LS
+Type of rejection operation performed on the pixels which overlap at each
+dispersion coordinate.  The algorithms are discussed in the
+help for \fBscombine\fR.  The rejection choices are:
+
+.V1
+      none - No rejection
+    minmax - Reject the low and high pixels
+ avsigclip - Reject pixels using an averaged sigma clipping algorithm
+.V2
+
+.LE
+scale = "none" (none|mode|median|mean)
+.LS
+Multiplicative scaling to be applied to each spectrum.  The choices are none
+or scale by the mode, median, or mean.  This should not be necessary if the
+flat field and throughput corrections have been properly made. 
+.LE
+
+.ce
+ENVIRONMENT PARAMETERS
+.LP
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
diff --git a/noao/imred/hydra/dohydra.cl b/noao/imred/hydra/dohydra.cl
new file mode 100644
index 00000000..74264633
--- /dev/null
+++ b/noao/imred/hydra/dohydra.cl
@@ -0,0 +1,75 @@
+# DOHYDRA -- Process HYDRA spectra from 2D to wavelength calibrated 1D.
+#
+# The task PROC does all of the interactive work and BATCH does the
+# background work.  This procedure is organized this way to minimize the
+# dictionary space when the background task is submitted.
+
+procedure dohydra (objects)
+
+string	objects = ""		{prompt="List of object spectra"}
+
+file	apref = ""		{prompt="Aperture reference spectrum"}
+file	flat = ""		{prompt="Flat field spectrum"}
+file	throughput = ""		{prompt="Throughput file or image (optional)"}
+string	arcs1 = ""		{prompt="List of arc spectra"}
+string	arcs2 = ""		{prompt="List of shift arc spectra"}
+file	arcreplace = ""		{prompt="Special aperture replacements"}
+file	arctable = ""		{prompt="Arc assignment table (optional)\n"}
+
+string	readnoise = "RDNOISE"	{prompt="Read out noise sigma (photons)"}
+string	gain = "GAIN"		{prompt="Photon gain (photons/data number)"}
+real	datamax = INDEF		{prompt="Max data value / cosmic ray threshold"}
+int	fibers = 97		{prompt="Number of fibers"}
+real	width = 12.		{prompt="Width of profiles (pixels)"}
+real	minsep = 8.	{prompt="Minimum separation between fibers (pixels)"}
+real	maxsep = 15.	{prompt="Maximum separation between fibers (pixels)"}
+file	apidtable = ""		{prompt="Aperture identifications"}
+string	crval = "INDEF"		{prompt="Approximate central wavelength"}
+string	cdelt = "INDEF"		{prompt="Approximate dispersion"}
+string	objaps = ""		{prompt="Object apertures"}
+string	skyaps = ""		{prompt="Sky apertures"}
+string	arcaps = ""		{prompt="Arc apertures"}
+string	objbeams = "0,1"	{prompt="Object beam numbers"}
+string	skybeams = "0"		{prompt="Sky beam numbers"}
+string	arcbeams = ""		{prompt="Arc beam numbers\n"}
+
+bool	scattered = no		{prompt="Subtract scattered light?"}
+bool	fitflat = yes		{prompt="Fit and ratio flat field spectrum?"}
+bool	clean = yes		{prompt="Detect and replace bad pixels?"}
+bool	dispcor = yes		{prompt="Dispersion correct spectra?"}
+bool	savearcs = yes		{prompt="Save simultaneous arc apertures?"}
+bool	skyalign = no		{prompt="Align sky lines?"}
+bool	skysubtract = yes	{prompt="Subtract sky?"}
+bool	skyedit = yes		{prompt="Edit the sky spectra?"}
+bool	saveskys = yes		{prompt="Save sky spectra?"}
+bool	splot = no		{prompt="Plot the final spectrum?"}
+bool	redo = no		{prompt="Redo operations if previously done?"}
+bool	update = yes		{prompt="Update spectra if cal data changes?"}
+bool	batch = no		{prompt="Extract objects in batch?"}
+bool	listonly = no		{prompt="List steps but don't process?\n"}
+
+pset	params = ""		{prompt="Algorithm parameters"}
+
+begin
+	apscript.readnoise = readnoise
+	apscript.gain = gain
+	apscript.nfind = fibers
+	apscript.width = width
+	apscript.t_width = width
+	apscript.minsep = minsep
+	apscript.maxsep = maxsep
+	apscript.radius = minsep
+	apscript.clean = clean
+	proc.datamax = datamax
+
+	proc (objects, apref, flat, throughput, arcs1, arcs2, arcreplace,
+	    arctable, fibers, apidtable, crval, cdelt, objaps, skyaps,
+	    arcaps, objbeams, skybeams, arcbeams, scattered, fitflat, no,
+	    no, no, no, clean, dispcor, savearcs, skyalign, skysubtract,
+	    skyedit, saveskys, splot, redo, update, batch, listonly)
+
+	if (proc.dobatch) {
+	    print ("-- Do remaining spectra as a batch job --")
+	    print ("batch&batch") | cl
+	}
+end
diff --git a/noao/imred/hydra/dohydra.par b/noao/imred/hydra/dohydra.par
new file mode 100644
index 00000000..7bca4821
--- /dev/null
+++ b/noao/imred/hydra/dohydra.par
@@ -0,0 +1,43 @@
+objects,s,a,"",,,"List of object spectra"
+apref,f,h,"",,,"Aperture reference spectrum"
+flat,f,h,"",,,"Flat field spectrum"
+throughput,f,h,"",,,"Throughput file or image (optional)"
+arcs1,s,h,"",,,"List of arc spectra"
+arcs2,s,h,"",,,"List of shift arc spectra"
+arcreplace,f,h,"",,,"Special aperture replacements"
+arctable,f,h,"",,,"Arc assignment table (optional)
+"
+readnoise,s,h,"RDNOISE",,,"Read out noise sigma (photons)"
+gain,s,h,"GAIN",,,"Photon gain (photons/data number)"
+datamax,r,h,INDEF,,,"Max data value / cosmic ray threshold"
+fibers,i,h,97,,,"Number of fibers"
+width,r,h,12.,,,"Width of profiles (pixels)"
+minsep,r,h,8.,,,"Minimum separation between fibers (pixels)"
+maxsep,r,h,15.,,,"Maximum separation between fibers (pixels)"
+apidtable,f,h,"",,,"Aperture identifications"
+crval,s,h,INDEF,,,"Approximate central wavelength"
+cdelt,s,h,INDEF,,,"Approximate dispersion"
+objaps,s,h,"",,,"Object apertures"
+skyaps,s,h,"",,,"Sky apertures"
+arcaps,s,h,"",,,"Arc apertures"
+objbeams,s,h,"0,1",,,"Object beam numbers"
+skybeams,s,h,"0",,,"Sky beam numbers"
+arcbeams,s,h,"",,,"Arc beam numbers
+"
+scattered,b,h,no,,,"Subtract scattered light?"
+fitflat,b,h,yes,,,"Fit and ratio flat field spectrum?"
+clean,b,h,yes,,,"Detect and replace bad pixels?"
+dispcor,b,h,yes,,,"Dispersion correct spectra?"
+savearcs,b,h,yes,,,"Save simultaneous arc apertures?"
+skyalign,b,h,no,,,"Align sky lines?"
+skysubtract,b,h,yes,,,"Subtract sky?"
+skyedit,b,h,yes,,,"Edit the sky spectra?"
+saveskys,b,h,yes,,,"Save sky spectra?"
+splot,b,h,no,,,"Plot the final spectrum?"
+redo,b,h,no,,,"Redo operations if previously done?"
+update,b,h,yes,,,"Update spectra if cal data changes?"
+batch,b,h,no,,,"Extract objects in batch?"
+listonly,b,h,no,,,"List steps but don\'t process?
+"
+params,pset,h,"",,,"Algorithm parameters"
+mode,s,h,"ql",,,
diff --git a/noao/imred/hydra/hydra.cl b/noao/imred/hydra/hydra.cl
new file mode 100644
index 00000000..4312a490
--- /dev/null
+++ b/noao/imred/hydra/hydra.cl
@@ -0,0 +1,82 @@
+#{ HYDRA package definition
+
+proto		# bscale
+
+s1 = envget ("min_lenuserarea")
+if (s1 == "")
+    reset min_lenuserarea = 100000
+else if (int (s1) < 100000)
+    reset min_lenuserarea = 100000
+
+# Define HYDRA package
+package hydra
+
+# Package script tasks
+task	dohydra		= "hydra$dohydra.cl"
+task	params		= "hydra$params.par"
+
+# Fiber reduction script tasks
+task	proc		= "srcfibers$proc.cl"
+task	fibresponse	= "srcfibers$fibresponse.cl"
+task	arcrefs		= "srcfibers$arcrefs.cl"
+task	doarcs		= "srcfibers$doarcs.cl"
+task	doalign		= "srcfibers$doalign.cl"
+task	skysub		= "srcfibers$skysub.cl"
+task	batch		= "srcfibers$batch.cl"
+task	listonly	= "srcfibers$listonly.cl"
+task	getspec		= "srcfibers$getspec.cl"
+
+task	msresp1d	= "specred$msresp1d.cl"
+
+# Demos
+set	demos		= "hydra$demos/"
+task	demos		= "demos$demos.cl"
+task	mkfibers	= "srcfibers$mkfibers.cl"
+
+# Onedspec tasks
+task	autoidentify,
+	continuum,
+	dispcor,
+	dopcor,
+	identify,
+	refspectra,
+	reidentify,
+	sapertures,
+	sarith,
+	sflip,
+	slist,
+	specplot,
+	specshift,
+	splot		= "onedspec$x_onedspec.e"
+task	scombine	= "onedspec$scombine/x_scombine.e"
+task	aidpars		= "onedspec$aidpars.par"
+task	bplot		= "onedspec$bplot.cl"
+task	scopy		= "onedspec$scopy.cl"
+task	dispcor1	= "onedspec$dispcor1.par"
+
+# Apextract tasks
+task	apall,
+	apedit,
+	apfind,
+	aprecenter,
+	apresize,
+	apscatter,
+	apsum,
+	aptrace		= "apextract$x_apextract.e"
+task	apdefault	= "apextract$apdefault.par"
+task	apparams	= "apextract$apparams.par"
+task	apall1		= "apextract$apall1.par"
+task	apscat1		= "apextract$apscat1.par"
+task	apscat2		= "apextract$apscat2.par"
+task	apscript	= "srcfibers$x_apextract.e"
+
+# Astutil tasks
+task	setairmass,
+	setjd		= "astutil$x_astutil.e"
+
+# Hide tasks from the user
+hidetask apparams, apall1, apscript, apscat1, apscat2, dispcor1, mkfibers
+hidetask params, proc, batch, arcrefs, doarcs, doalign
+hidetask listonly, fibresponse, getspec
+
+clbye()
diff --git a/noao/imred/hydra/hydra.hd b/noao/imred/hydra/hydra.hd
new file mode 100644
index 00000000..c9e04d8a
--- /dev/null
+++ b/noao/imred/hydra/hydra.hd
@@ -0,0 +1,7 @@
+# Help directory for the HYDRA package.
+
+$doc		 = "./doc/"
+
+dohydra		hlp=doc$dohydra.hlp
+
+revisions	sys=Revisions
diff --git a/noao/imred/hydra/hydra.men b/noao/imred/hydra/hydra.men
new file mode 100644
index 00000000..a01bc9b5
--- /dev/null
+++ b/noao/imred/hydra/hydra.men
@@ -0,0 +1,32 @@
+          apall - Extract 1D spectra (all parameters in one task)
+      apdefault - Set the default aperture parameters
+         apedit - Edit apertures interactively
+	 apfind - Automatically find spectra and define apertures
+     aprecenter - Recenter apertures
+       apresize - Resize apertures
+      apscatter - Fit and remove scattered light
+          apsum - Extract 1D spectra
+	aptrace - Trace positions of spectra
+
+          bplot - Batch plots of spectra
+      continuum - Fit the continuum in spectra
+        dispcor - Dispersion correct spectra
+	 dopcor - Doppler correct spectra
+       identify - Identify features in spectrum for dispersion solution
+       msresp1d - Create 1D response spectra from flat field and sky spectra
+     refspectra - Assign wavelength reference spectra to other spectra
+     reidentify - Automatically identify features in spectra
+     sapertures - Set or change aperture header information
+	 sarith - Spectrum arithmetic
+       scombine - Combine spectra having different wavelength ranges
+          scopy - Select and copy apertures in different spectral formats
+     setairmass - Compute effective airmass and middle UT for an exposure
+          setjd - Compute and set Julian dates in images
+	  sflip - Flip data and/or dispersion coordinates in spectra
+          slist - List spectrum header parameters
+       specplot - Stack and plot multiple spectra
+      specshift - Shift spectral dispersion coordinate systems
+          splot - Preliminary spectral plot/analysis
+
+        dohydra - Process HYDRA spectra
+	  demos - Demonstrations and tests
diff --git a/noao/imred/hydra/hydra.par b/noao/imred/hydra/hydra.par
new file mode 100644
index 00000000..b560f84d
--- /dev/null
+++ b/noao/imred/hydra/hydra.par
@@ -0,0 +1,13 @@
+# HYDRA parameter file
+observatory,s,h,"observatory",,,Observatory of data
+interp,s,h,"poly5","nearest|linear|poly3|poly5|spline3|sinc",,Interpolation type
+dispaxis,i,h,2,1,3,Image axis for 2D/3D images
+nsum,s,h,"1",,,"Number of lines/columns/bands to sum for 2D/3D images
+"
+database,f,h,"database",,,Database
+verbose,b,h,no,,,Verbose output?
+logfile,s,h,"logfile",,,Log file
+plotfile,s,h,"",,,"Plot file
+"
+records,s,h,""
+version,s,h,"HYDRA V1: January 1992"
diff --git a/noao/imred/hydra/params.par b/noao/imred/hydra/params.par
new file mode 100644
index 00000000..af56a1b8
--- /dev/null
+++ b/noao/imred/hydra/params.par
@@ -0,0 +1,67 @@
+line,i,h,INDEF,,,"Default dispersion line"
+nsum,i,h,10,,,"Number of dispersion lines to sum or median"
+order,s,h,"decreasing","increasing|decreasing",,"Order of apertures"
+extras,b,h,no,,,"Extract sky, sigma, etc.?
+
+-- DEFAULT APERTURE LIMITS --"
+lower,r,h,-5.,,,"Lower aperture limit relative to center"
+upper,r,h,5.,,,"Upper aperture limit relative to center
+
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --"
+ylevel,r,h,0.05,,,"Fraction of peak or intensity for resizing
+
+-- TRACE PARAMETERS --"
+t_step,i,h,10,,,"Tracing step"
+t_function,s,h,"spline3","chebyshev|legendre|spline1|spline3",,"Trace fitting function"
+t_order,i,h,3,,,"Trace fitting function order"
+t_niterate,i,h,1,0,,"Trace rejection iterations"
+t_low,r,h,3.,0.,,"Trace lower rejection sigma"
+t_high,r,h,3.,0.,,"Trace upper rejection sigma
+
+-- SCATTERED LIGHT PARAMETERS --"
+buffer,r,h,1.,0.,,Buffer distance from apertures
+apscat1,pset,h,"",,,Fitting parameters across the dispersion
+apscat2,pset,h,"",,,"Fitting parameters along the dispersion
+
+-- APERTURE EXTRACTION PARAMETERS --"
+weights,s,h,"none","none|variance",,Extraction weights (none|variance)
+pfit,s,h,"fit1d","fit1d|fit2d",,Profile fitting algorithm (fit1d|fit2d)
+lsigma,r,h,3.,,,Lower rejection threshold
+usigma,r,h,3.,,,Upper rejection threshold
+nsubaps,i,h,1,1,,"Number of subapertures
+
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --"
+f_interactive,b,h,yes,,,"Fit flat field interactively?"
+f_function,s,h,"spline3",spline3|legendre|chebyshev|spline1,,"Fitting function"
+f_order,i,h,10,1,,"Fitting function order
+
+-- ARC DISPERSION FUNCTION PARAMETERS --"
+threshold,r,h,10.,0.,,"Minimum line contrast threshold"
+coordlist,f,h,linelists$ctiohenear.dat,,,"Line list"
+match,r,h,-3.,,,"Line list matching limit in Angstroms"
+fwidth,r,h,4.,,,"Arc line widths in pixels"
+cradius,r,h,10.,,,Centering radius in pixels
+i_function,s,h,"spline3","legendre|chebyshev|spline1|spline3",,"Coordinate function"
+i_order,i,h,3,1,,"Order of dispersion function"
+i_niterate,i,h,2,0,,"Rejection iterations"
+i_low,r,h,3.,0.,,"Lower rejection sigma"
+i_high,r,h,3.,0.,,"Upper rejection sigma"
+refit,b,h,yes,,,"Refit coordinate function when reidentifying?"
+addfeatures,b,h,no,,,"Add features when reidentifying?
+
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --"
+select,s,h,"interp",,,"Selection method for reference spectra"
+sort,s,h,"jd",,,"Sort key"
+group,s,h,"ljd",,,"Group key"
+time,b,h,no,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting
+
+-- DISPERSION CORRECTION PARAMETERS --"
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+log,b,h,no,,,"Logarithmic wavelength scale?"
+flux,b,h,yes,,,"Conserve flux?
+
+-- SKY SUBTRACTION PARAMETERS --"
+combine,s,h,"average","average|median",,Type of combine operation
+reject,s,h,"avsigclip","none|minmax|avsigclip",,"Sky rejection option"
+scale,s,h,"none","none|mode|median|mean",,"Sky scaling option"
diff --git a/noao/imred/iids/Revisions b/noao/imred/iids/Revisions
new file mode 100644
index 00000000..7472a80c
--- /dev/null
+++ b/noao/imred/iids/Revisions
@@ -0,0 +1,131 @@
+.help revisions Jun88 noao.imred.iids
+.nf
+
+=====
+V2.12
+=====
+
+imred$iids/standard.par
+    Added blackbody query parameters.  (5/2/02, Valdes)
+
+========
+V2.11.3b
+========
+
+imred$iids/identify.par
+    Added new units parameters.  (3/11/97, Valdes)
+
+=========
+V2.10.4p2
+=========
+
+imred$iids/standard.par
+    Removed ennumerated list.  (4/10/89, Valdes)
+
+imred$iids/iids.cl
+imred$iids/iids.men
+specplot.par+
+	Task SPECPLOT added.  (4/3/89 ShJ)
+
+imred$iids/batchred.cl
+imred$iids/batchred.par
+imred$iids/iids.cl
+imred$iids/iids.men
+   1. New BATCHRED script. (4/27/88 Valdes)
+   2. Eliminated EXTINCT.
+
+imred$iids/sensfunc.par
+    Added aperture selection and query parameters.  (4/15/88 Valdes)
+
+imred$iids/iids.cl
+imred$iids/refspectra.par +
+    Refer to new ONEDSPEC executable and tasks.  (4/7/88 Valdes)
+
+noao$imred/iids/reidentify.par
+    Valdes, Jan 4, 1988
+    Updated parameter file for new REIDENTIFY parameter.
+
+noao$imred/iids/iids.hd -
+noao$imred/iids/doc/ -
+    Valdes, June 1, 1987
+    1.  The documentation for POWERCOR has been moved to ONEDSPEC.  A
+	copy of POWERCOR has been installed as part of the ONEDSPEC
+	package.
+
+noao$imred/iids/dispcor.par
+    Valdes, March 5, 1987
+    1.  The DISPCOR default parameter file has been updated because of
+	changes to the task; most notable being that wstart and wpc are
+	list structured.
+
+noao$imred/iids/flatdiv.par
+noao$imred/iids/flatfit.par
+    Valdes, December, 2, 1986
+    1.  New parameter "power" added to these tasks.
+
+noao$imred/iids/coincor.par
+noao$imred/iids/powercor.cl
+    Valdes, October 20, 1986
+    1.  New parameter "checkdone" added to COINCOR to allow overriding
+	coincidence correction checking.
+    2.  POWERCOR script modified so that it will apply correction on
+	previously coincidence corrected spectra.
+
+noao$imred/iids/iids.cl
+noao$imred/iids/iids.men
+noao$imred/iids/iids.hd +
+noao$imred/iids/powercor.cl +
+noao$imred/iids/powercor.par +
+noao$imred/iids/doc/powercor.hlp +
+    Valdes, October 13, 1986
+    1.  Added a new script task POWERCOR to apply the power law correction
+	to mountain reduced IIDS spectra.
+    2.  A help page was also added.
+
+noao$imred/iids/iids.par
+noao$imred/iids/coincor.par
+noao$imred/iids/iids.men
+    Valdes, October 13, 1986
+    1.  Added new COINCOR parameter "power".
+
+noao$imred/iids/iids.cl
+noao$imred/iids/iids.men
+noao$imred/irs/shedit.par +
+    Valdes, October 6, 1986
+    1.  Added new task SHEDIT.
+
+noao$imred/iids/identify.par
+    Valdes, October 3, 1986
+    1.  Added new IDENTIFY parameter "threshold".
+
+====================================
+Version 2.3 Release, August 18, 1986
+====================================
+
+iids:  Valdes, July 3, 1986:
+    1.  New coordlist name in IDENTIFY parameter file.
+    2.  New calibration file name in package parameter file.
+
+=====================================
+STScI Pre-release and SUN 2.3 Release
+=====================================
+
+iids$bswitch.par:  Valdes, May 19, 1986
+    1.  The parameter "add_const" in BSWITCH is directed to the parameter
+	in SENSFUNC of the same name.
+
+iids:  Valdes, May 12, 1986:
+    1.  SPLOT updated.  New parameters XMIN, XMAX, YMIN, YMAX.
+
+iids:  Valdes, April 7, 1986
+    1.  Package parameter file changed to delete latitude.
+    2.  DISPCOR, BSWITCH, and STANDARD latitude parameter now obtained from
+	OBSERVATORY.
+
+iids:  Valdes, March 27, 1986
+    1.  New task SETDISP added.
+
+===========
+Release 2.2
+===========
+.endhelp
diff --git a/noao/imred/iids/calibrate.par b/noao/imred/iids/calibrate.par
new file mode 100644
index 00000000..795965b7
--- /dev/null
+++ b/noao/imred/iids/calibrate.par
@@ -0,0 +1,14 @@
+# CALIBRATE parameter file
+
+input,s,a,,,,Input spectra to calibrate
+output,s,a,,,,Output calibrated spectra
+records,s,a,,,,Record number extensions
+extinct,b,h,yes,,,Apply extinction correction?
+flux,b,h,yes,,,Apply flux calibration?
+extinction,s,h,)_.extinction,,,Extinction file
+observatory,s,h,)_.observatory,,,Observatory of observation
+ignoreaps,b,h,no,,,Ignore aperture numbers in flux calibration?
+sensitivity,s,h,"sens",,,Image root name for sensitivity spectra
+fnu,b,h,no,,,Create spectra having units of FNU?
+airmass,r,q,,1.,,Airmass
+exptime,r,q,,,,Exposure time (seconds)
diff --git a/noao/imred/iids/dispcor.par b/noao/imred/iids/dispcor.par
new file mode 100644
index 00000000..186c0ca1
--- /dev/null
+++ b/noao/imred/iids/dispcor.par
@@ -0,0 +1,19 @@
+input,s,a,,,,List of input spectra
+output,s,a,,,,List of output spectra
+records,s,a,,,,Record number extensions
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+database,s,h,"database",,,Dispersion solution database
+table,s,h,"",,,Wavelength table for apertures
+w1,r,h,INDEF,,,Starting wavelength
+w2,r,h,INDEF,,,Ending wavelength
+dw,r,h,INDEF,,,Wavelength interval per pixel
+nw,i,h,1024,,,Number of output pixels
+log,b,h,no,,,Logarithmic wavelength scale?
+flux,b,h,yes,,,Conserve total flux?
+samedisp,b,h,yes,,,Same dispersion in all apertures?
+global,b,h,yes,,,Apply global defaults?
+confirm,b,h,yes,,,Confirm dispersion coordinates?
+ignoreaps,b,h,no,,,Ignore apertures?
+listonly,b,h,no,,,List the dispersion coordinates only?
+verbose,b,h,yes,,,Print linear dispersion assignments?
+logfile,s,h,"logfile",,,Log file
diff --git a/noao/imred/iids/identify.par b/noao/imred/iids/identify.par
new file mode 100644
index 00000000..92049af8
--- /dev/null
+++ b/noao/imred/iids/identify.par
@@ -0,0 +1,33 @@
+# Parameters for identify task.
+
+images,s,a,,,,Images containing features to be identified
+section,s,h,"middle line",,,Section to apply to two dimensional images
+database,f,h,database,,,Database in which to record feature data
+coordlist,f,h,linelists$henear.dat,,,User coordinate list
+units,s,h,"",,,Coordinate units
+nsum,s,h,"10",,,Number of lines/columns/bands to sum in 2D images
+match,r,h,50.,,,Coordinate list matching limit
+maxfeatures,i,h,50,,,Maximum number of features for automatic identification
+zwidth,r,h,100.,,,Zoom graph width in user units
+
+ftype,s,h,"emission","emission|absorption",,Feature type
+fwidth,r,h,4.,,,Feature width in pixels
+cradius,r,h,5.,,,Centering radius in pixels
+threshold,r,h,10.,0.,,Feature threshold for centering
+minsep,r,h,2.,0.,,Minimum pixel separation
+
+function,s,h,"chebyshev","legendre|chebyshev|spline1|spline3",,Coordinate function
+order,i,h,6,1,,Order of coordinate function
+sample,s,h,"*",,,Coordinate sample regions
+niterate,i,h,0,0,,Rejection iterations
+low_reject,r,h,3.,0.,,Lower rejection sigma
+high_reject,r,h,3.,0.,,Upper rejection sigma
+grow,r,h,0.,0.,,Rejection growing radius
+
+autowrite,b,h,no,,,"Automatically write to database"
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+
+crval,s,q,,,,"Approximate coordinate (at reference pixel)"
+cdelt,s,q,,,,"Approximate dispersion"
+aidpars,pset,h,,,,"Automatic identification algorithm parameters"
diff --git a/noao/imred/iids/iids.cl b/noao/imred/iids/iids.cl
new file mode 100644
index 00000000..19b8ac79
--- /dev/null
+++ b/noao/imred/iids/iids.cl
@@ -0,0 +1,66 @@
+#{ IIDS -- KPNO IIDS Spectral Reduction Package
+
+# Load necessary packages
+
+lists		# List package for table
+
+# Define necessary paths
+
+set	iidscal		= "onedstds$iidscal/"
+set	irsiids		= "onedspec$irsiids/"
+
+package iids
+
+# Standard ONEDSPEC tasks
+task	autoidentify,
+	continuum,
+	deredden,
+	dopcor,
+	mkspec,
+	names,
+	sarith,
+	sflip,
+	sinterp,
+	splot,
+	specplot,
+	specshift	= onedspec$x_onedspec.e
+task	scombine	= "onedspec$scombine/x_scombine.e"
+task	aidpars		= "onedspec$aidpars.par"
+task	dispcor1	= onedspec$dispcor1.par
+task	scopy		= onedspec$scopy.cl
+hidetask dispcor1
+
+# Special  IRS/IIDS tasks
+task	addsets,
+	bswitch,
+	coefs,
+	coincor,
+	flatdiv,
+	flatfit,
+	slist1d,
+	subsets,
+	sums		= irsiids$x_onedspec.e
+task	batchred	= irsiids$batchred.cl
+task	bplot		= irsiids$bplot.cl
+task	extinct		= irsiids$extinct.cl
+task	powercor	= irsiids$powercor.cl
+
+# Different default parameters
+task	calibrate,
+	dispcor,
+	identify,
+	lcalib,
+	refspectra,
+	reidentify,
+	sensfunc,
+	standard	= iids$x_onedspec.e
+
+# Astutil tasks
+task	setairmass,
+	setjd		= "astutil$x_astutil.e"
+
+# Define a task living in the users directory - it is created by BATCHRED
+
+task	$process	= process.cl
+
+clbye()
diff --git a/noao/imred/iids/iids.hd b/noao/imred/iids/iids.hd
new file mode 100644
index 00000000..5398f372
--- /dev/null
+++ b/noao/imred/iids/iids.hd
@@ -0,0 +1 @@
+# Help directory for the IIDS package.
diff --git a/noao/imred/iids/iids.men b/noao/imred/iids/iids.men
new file mode 100644
index 00000000..faa77978
--- /dev/null
+++ b/noao/imred/iids/iids.men
@@ -0,0 +1,37 @@
+	addsets - Add subsets of strings of spectra
+       batchred - Batch processing of IIDS/IRS spectra
+          bplot - Batch plots of spectra
+	bswitch - Beam-switch strings of spectra to make obj-sky pairs
+      calibrate - Apply sensitivity correction to spectra
+          coefs - Extract mtn reduced coefficients from henear scans
+	coincor - Correct spectra for detector count rates
+      continuum - Fit the continuum in spectra
+       deredden - Apply interstellar extinction corrections
+	dispcor - Dispersion correct spectra
+	 dopcor - Doppler correct spectra
+	extinct - Use BSWITCH for extinction correction
+	flatdiv - Divide spectra by flat field
+	flatfit - Sum and normalize flat field spectra
+       identify - Identify features in spectrum for dispersion solution
+         lcalib - List calibration file data
+         mkspec - Generate an artificial spectrum
+          names - Generate a list of image names from a string
+       powercor - Apply power law correction to mountain reduced spectra
+	process - A task generated by BATCHRED
+     refspectra - Assign reference spectra to object spectra
+     reidentify - Automatically identify features in spectra
+         sarith - Spectrum arithmetic
+       scombine - Combine spectra having different wavelength ranges
+          scopy - Select and copy apertures in different spectral formats
+       sensfunc - Create sensitivity function
+     setairmass - Compute effective airmass and middle UT for an exposure
+          setjd - Compute and set Julian dates in images
+	  sflip - Flip data and/or dispersion coordinates in spectra
+        sinterp - Interpolate a table of x,y pairs to create a spectrum
+	slist1d - List spectral header elements
+       specplot - Stack and plot multiple spectra
+      specshift - Shift spectral dispersion coordinate systems
+	  splot - Preliminary spectral plot/analysis
+       standard - Identify standard stars to be used in sensitivity calc
+	subsets - Subtract pairs in strings of spectra
+           sums - Generate sums of object and sky spectra by aperture
diff --git a/noao/imred/iids/iids.par b/noao/imred/iids/iids.par
new file mode 100644
index 00000000..9035bc1b
--- /dev/null
+++ b/noao/imred/iids/iids.par
@@ -0,0 +1,17 @@
+# PARAMETERS FOR KPNO IIDS SPECTRAL REDUCTION PACKAGE
+
+observatory,s,h,"kpno",,,Observatory for data
+interp,s,h,"poly5","nearest|linear|poly3|poly5|spline3|sinc",,Interpolation type
+extinction,s,h,"onedstds$kpnoextinct.dat",,,Extinction file
+caldir,s,h,"iidscal$",,,Directory containing calibration data
+coincor,b,h,yes,,,Apply coincidence correction to flats
+ccmode,s,h,"iids",,,Correction mode (photo|iids|power)
+deadtime,r,h,1.424e-3,0,,Deadtime in seconds
+power,r,h,0.975,,,IIDS power law coefficient
+
+dispaxis,i,h,1,1,3,Image axis for 2D/3D images
+nsum,s,h,"1",,,Number of lines/columns/bands to sum for 2D/3D images
+
+next_rec,i,h,1,,,"Next output record"
+
+version,s,h,"IRS V3: July 1991"
diff --git a/noao/imred/iids/irs.men b/noao/imred/iids/irs.men
new file mode 100644
index 00000000..6ebc9281
--- /dev/null
+++ b/noao/imred/iids/irs.men
@@ -0,0 +1,5 @@
+      addsets     coefs       flatfit     powercor    scombine    splot
+      batchred    coincor     identify    process     sensfunc    standard
+      bplot       continuum   lcalib      rebin       sinterp     subsets
+      bswitch     dispcor     mkspec      refspectra  slist1d     sums
+      calibrate   flatdiv     names       reidentify  specplot    
diff --git a/noao/imred/iids/lcalib.par b/noao/imred/iids/lcalib.par
new file mode 100644
index 00000000..30436625
--- /dev/null
+++ b/noao/imred/iids/lcalib.par
@@ -0,0 +1,7 @@
+# CALIBLIST parameter file
+
+option,s,a,,,,"List option (bands, ext, mags, fnu, flam, stars)"
+star_name,s,a,,,,Star name in calibration list
+extinction,s,h,,,,Extinction file
+caldir,s,h,)_.caldir,,,Directory containing calibration data
+fnuzero,r,h,3.68e-20,,,Absolute flux zero point
diff --git a/noao/imred/iids/refspectra.par b/noao/imred/iids/refspectra.par
new file mode 100644
index 00000000..47cd54f9
--- /dev/null
+++ b/noao/imred/iids/refspectra.par
@@ -0,0 +1,17 @@
+input,s,a,,,,"List of input spectra"
+records,s,a,,,,Record number extensions
+references,s,h,"*.imh",,,"List of reference spectra"
+apertures,s,h,"",,,"Input aperture selection list"
+refaps,s,h,"",,,"Reference aperture selection list"
+ignoreaps,b,h,no,,,Ignore input and reference apertures?
+select,s,h,"interp","match|nearest|preceding|following|interp|average",,"Selection method for reference spectra"
+sort,s,h,"ut",,,"Sort key"
+group,s,h,"none",,,"Group key"
+time,b,h,yes,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting"
+override,b,h,no,,,"Override previous assignments?"
+confirm,b,h,yes,,,"Confirm reference spectrum assignments?"
+assign,b,h,yes,,,"Assign the reference spectra to the input spectrum?"
+logfiles,s,h,"STDOUT,logfile",,,"List of logfiles"
+verbose,b,h,no,,,"Verbose log output?"
+answer,s,q,,"no|yes|YES",,"Accept assignment?"
diff --git a/noao/imred/iids/reidentify.par b/noao/imred/iids/reidentify.par
new file mode 100644
index 00000000..13b21740
--- /dev/null
+++ b/noao/imred/iids/reidentify.par
@@ -0,0 +1,36 @@
+# Parameters for reidentify task.
+
+reference,s,a,,,,Reference image
+images,s,a,,,,Images to be reidentified
+interactive,s,h,"no","no|yes|NO|YES",,Interactive fitting?
+section,s,h,"middle line",,,Section to apply to two dimensional images
+newaps,b,h,yes,,,Reidentify apertures in images not in reference?
+override,b,h,no,,,Override previous solutions?
+refit,b,h,yes,,,"Refit coordinate function?
+"
+trace,b,h,no,,,Trace reference image?
+step,s,h,"10",,,Step in lines/columns/bands for tracing an image
+nsum,s,h,"10",,,Number of lines/columns/bands to sum
+shift,s,h,"0.",,,Shift to add to reference features (INDEF to search)
+search,r,h,0.,,,Search radius
+nlost,i,h,0,0,,"Maximum number of features which may be lost
+"
+cradius,r,h,5.,,,Centering radius
+threshold,r,h,10.,0.,,Feature threshold for centering
+addfeatures,b,h,no,,,Add features from a line list?
+coordlist,f,h,linelists$henear.dat,,,User coordinate list
+match,r,h,10.,,,Coordinate list matching limit
+maxfeatures,i,h,50,,,Maximum number of features for automatic identification
+minsep,r,h,2.,0.,,"Minimum pixel separation
+"
+database,f,h,database,,,Database
+logfiles,s,h,"logfile",,,List of log files
+plotfile,s,h,"",,,Plot file for residuals
+verbose,b,h,no,,,Verbose output?
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,"Graphics cursor input
+"
+answer,s,q,"yes","no|yes|NO|YES",,Fit dispersion function interactively?
+crval,s,q,,,,"Approximate coordinate (at reference pixel)"
+cdelt,s,q,,,,"Approximate dispersion"
+aidpars,pset,h,,,,"Automatic identification algorithm parameters"
diff --git a/noao/imred/iids/sensfunc.par b/noao/imred/iids/sensfunc.par
new file mode 100644
index 00000000..022190a4
--- /dev/null
+++ b/noao/imred/iids/sensfunc.par
@@ -0,0 +1,17 @@
+standards,s,a,std,,,Input standard star data file (from STANDARD)
+sensitivity,s,a,"sens",,,Output root sensitivity function imagename
+apertures,s,h,"",,,Aperture selection list
+ignoreaps,b,h,no,,,Ignore apertures and make one sensitivity function?
+logfile,f,h,"logfile",,,Output log for statistics information
+extinction,f,h,")_.extinction",,,Extinction file
+newextinction,f,h,"extinct.dat",,,Output revised extinction file
+observatory,s,h,)_.observatory,,,Observatory of data
+function,s,h,"spline3","chebyshev|legendre|spline3|spline1",,Fitting function
+order,i,h,6,1,,Order of fit
+interactive,b,h,yes,,,Determine sensitivity function interactively?
+graphs,s,h,"sr",,,Graphs per frame
+marks,s,h,"plus cross box",,,Data mark types (marks deleted added)
+colors,s,h,"2 1 3 4",,,Colors (lines marks deleted added)
+cursor,*gcur,h,"",,,Graphics cursor input
+device,s,h,"stdgraph",,,Graphics output device
+answer,s,q, yes,"no|yes|NO|YES",,"(no|yes|NO|YES)"
diff --git a/noao/imred/iids/standard.par b/noao/imred/iids/standard.par
new file mode 100644
index 00000000..3abf645a
--- /dev/null
+++ b/noao/imred/iids/standard.par
@@ -0,0 +1,22 @@
+input,f,a,,,,Input image file root name
+records,s,a,,,,Spectral records
+output,s,a,std,,,Output flux file (used by SENSFUNC)
+samestar,b,h,yes,,,Same star in all apertures?
+beam_switch,b,h,yes,,,Beam switch spectra?
+apertures,s,h,"",,,Aperture selection list
+bandwidth,r,h,INDEF,,,Bandpass widths
+bandsep,r,h,INDEF,,,Bandpass separation
+fnuzero,r,h,3.68e-20,,,Absolute flux zero point
+extinction,s,h,)_.extinction,,,Extinction file
+caldir,s,h,)_.caldir,,,Directory containing calibration data
+observatory,s,h,)_.observatory,,,Observatory for data
+interact,b,h,yes,,,Graphic interaction to define new bandpasses
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+star_name,s,q,,,,Star name in calibration list
+airmass,r,q,,1.,,Airmass
+exptime,r,q,,,,Exposure time (seconds)
+mag,r,q,,,,Magnitude of star
+magband,s,q,,"U|B|V|R|I|J|H|K|L|Lprime|M",,"Magnitude type"
+teff,s,q,,,,Effective temperature or spectral type
+answer,s,q,no,,,"(no|yes|NO|YES|NO!|YES!)"
diff --git a/noao/imred/imred.cl b/noao/imred/imred.cl
new file mode 100644
index 00000000..634b7b27
--- /dev/null
+++ b/noao/imred/imred.cl
@@ -0,0 +1,55 @@
+#{ IMRED -- Image reduction package.
+
+# Define directories.
+
+set	argus		= "imred$argus/"
+set	biasdir		= "imred$bias/"
+set	ccdred		= "imred$ccdred/"
+set	crutil		= "imred$crutil/"
+set	ctioslit	= "imred$ctioslit/"
+set	dtoi		= "imred$dtoi/"
+set	echelle		= "imred$echelle/"
+set	generic		= "imred$generic/"
+set	hydra		= "imred$hydra/"
+set	iids		= "imred$iids/"
+set	irred		= "imred$irred/"
+set	irs		= "imred$irs/"
+set	kpnocoude	= "imred$kpnocoude/"
+set	kpnoslit	= "imred$kpnoslit/"
+set	quadred		= "imred$quadred/"
+set	specred		= "imred$specred/"
+set	vtel		= "imred$vtel/"
+
+set	apextract	= "twodspec$apextract/"
+set	doecslit	= "imred$src/doecslit/"
+set	dofoe		= "imred$src/dofoe/"
+set	doslit		= "imred$src/doslit/"
+set	srcfibers	= "imred$src/fibers/"
+
+# Define the package.
+
+package imred
+
+# Tasks
+#task	tutor		= "imred$tutor.cl"
+
+# Packages
+task	argus.pkg	= "argus$argus.cl"
+task	bias.pkg	= "biasdir$bias.cl"
+task	ccdred.pkg	= "ccdred$ccdred.cl"
+task	crutil.pkg	= "crutil$crutil.cl"
+task	ctioslit.pkg	= "ctioslit$ctioslit.cl"
+task	dtoi.pkg	= "dtoi$dtoi.cl"
+task	echelle.pkg	= "echelle$echelle.cl"
+task	generic.pkg	= "generic$generic.cl"
+task	hydra.pkg	= "hydra$hydra.cl"
+task	iids.pkg	= "iids$iids.cl"
+task	irred.pkg	= "irred$irred.cl"
+task	irs.pkg		= "irs$irs.cl"
+task	kpnocoude.pkg	= "kpnocoude$kpnocoude.cl"
+task	kpnoslit.pkg	= "kpnoslit$kpnoslit.cl"
+task	quadred.pkg	= "quadred$quadred.cl"
+task	specred.pkg	= "specred$specred.cl"
+task	vtel.pkg	= "vtel$vtel.cl"
+
+clbye
diff --git a/noao/imred/imred.hd b/noao/imred/imred.hd
new file mode 100644
index 00000000..7e349d7e
--- /dev/null
+++ b/noao/imred/imred.hd
@@ -0,0 +1,119 @@
+# Help directory for the IMRED package.
+
+$doc		= "./doc/"
+
+$argus		= "noao$imred/argus/"
+$bias		= "noao$imred/bias/"
+$ccdred		= "noao$imred/ccdred/"
+$crutil		= "noao$imred/crutil/"
+$ctioslit	= "noao$imred/ctioslit/"
+$dtoi		= "noao$imred/dtoi/"
+$echelle	= "noao$imred/echelle/"
+$generic	= "noao$imred/generic/"
+$hydra		= "noao$imred/hydra/"
+$iids		= "noao$imred/iids/"
+$irred		= "noao$imred/irred/"
+$irs		= "noao$imred/irs/"
+$kpnocoude	= "noao$imred/kpnocoude/"
+$kpnoslit	= "noao$imred/kpnoslit/"
+$quadred	= "noao$imred/quadred/"
+$specred	= "noao$imred/specred/"
+$vtel		= "noao$imred/vtel/"
+
+demos		hlp=doc$demos.hlp
+#tutor		hlp=doc$tutor.hlp,		src=tutor.cl
+
+argus		men=argus$argus.men,
+		hlp=..,
+		pkg=argus$argus.hd,
+		src=argus$argus.cl
+
+bias		men=bias$bias.men,
+		hlp=..,
+		pkg=bias$bias.hd,
+		src=bias$bias.cl
+
+ccdred		men=ccdred$ccdred.men,
+		hlp=..,
+		sys=ccdred$ccdred.hlp,
+		pkg=ccdred$ccdred.hd,
+		src=ccdred$ccdred.cl
+
+crutil		men=crutil$crutil.men,
+		hlp=..,
+		sys=crutil$crutil.hlp,
+		pkg=crutil$crutil.hd,
+		src=crutil$crutil.cl
+
+ctioslit	men=ctioslit$ctioslit.men,
+		hlp=..,
+		pkg=ctioslit$ctioslit.hd,
+		src=ctioslit$ctioslit.cl
+
+dtoi		men=dtoi$dtoi.men,
+		hlp=..,
+		pkg=dtoi$dtoi.hd,
+		src=dtoi$dtoi.cl
+
+echelle		men=echelle$echelle.men,
+		hlp=..,
+		sys=echelle$echelle.hlp,
+		pkg=echelle$echelle.hd,
+		src=echelle$echelle.cl
+
+generic		men=generic$generic.men,
+		hlp=..,
+		sys=generic$generic.hlp,
+		pkg=generic$generic.hd,
+		src=generic$generic.cl
+
+hydra		men=hydra$hydra.men,
+		hlp=..,
+		pkg=hydra$hydra.hd,
+		src=hydra$hydra.cl
+
+iids		men=iids$iids.men,
+		hlp=..,
+		sys=iids$iids.hlp,
+		pkg=iids$iids.hd,
+		src=iids$iids.cl
+
+irred		men=irred$irred.men,
+		hlp=..,
+		sys=irred$irred.hlp,
+		pkg=irred$irred.hd,
+		src=irred$irred.cl
+
+irs		men=irs$irs.men,
+		hlp=..,
+		sys=irs$irs.hlp,
+		pkg=irs$irs.hd,
+		src=irs$irs.cl
+
+kpnocoude	men=kpnocoude$kpnocoude.men,
+		hlp=..,
+		pkg=kpnocoude$kpnocoude.hd,
+		src=kpnocoude$kpnocoude.cl
+
+kpnoslit	men=kpnoslit$kpnoslit.men,
+		hlp=..,
+		pkg=kpnoslit$kpnoslit.hd,
+		src=kpnoslit$kpnoslit.cl
+
+quadred		men=quadred$quadred.men,
+		hlp=..,
+		sys=quadred$quadred.hlp,
+		pkg=quadred$quadred.hd,
+		src=quadred$quadred.cl
+
+specred		men=specred$specred.men,
+		hlp=..,
+		sys=specred$specred.hlp,
+		pkg=specred$specred.hd,
+		src=specred$specred.cl
+
+vtel		men=vtel$vtel.men,
+		hlp=..,
+		sys=vtel$vtel.hlp,
+		pkg=vtel$vtel.hd,
+		src=vtel$vtel.cl
diff --git a/noao/imred/imred.men b/noao/imred/imred.men
new file mode 100644
index 00000000..b9ddc234
--- /dev/null
+++ b/noao/imred/imred.men
@@ -0,0 +1,17 @@
+ 	  argus - CTIO ARGUS reduction package
+	   bias - General bias subtraction tools
+	 crutil - Tasks for detecting and removing cosmic rays
+	 ccdred - Generic CCD reductions
+       ctioslit - CTIO spectrophotometric reduction package
+	   dtoi - Density to Intensity reductions for photographic plates
+	echelle - Echelle spectral reductions (slit and FOE)
+        generic - Generic image reductions tools
+ 	  hydra - KPNO HYDRA (and NESSIE) reduction package
+	   iids - KPNO IIDS spectral reductions
+	  irred - KPNO IR camera reductions
+	    irs - KPNO IRS spectral reductions
+      kpnocoude - KPNO coude reduction package (slit and 3 fiber)
+       kpnoslit - KPNO low/moderate dispersion slits (Goldcam, RCspec, Whitecam)
+	quadred - CCD reductions for QUAD amplifier data
+        specred - Generic slit and fiber spectral reduction package
+	   vtel - NSO Solar vacuum telescope image reductions
diff --git a/noao/imred/imred.par b/noao/imred/imred.par
new file mode 100644
index 00000000..c0e775bf
--- /dev/null
+++ b/noao/imred/imred.par
@@ -0,0 +1,5 @@
+# IMRED package parameter file
+
+keeplog,b,h,no,,,Keep log of processing?
+logfile,f,h,"imred.log",,,Log file
+version,s,h,"IMRED V3: August 2001"
diff --git a/noao/imred/irred/Revisions b/noao/imred/irred/Revisions
new file mode 100644
index 00000000..22a23670
--- /dev/null
+++ b/noao/imred/irred/Revisions
@@ -0,0 +1,61 @@
+.help revisions Jun88 noao.imred.irred
+.nf
+irred$irred.cl
+    The IRLINCOR task was mistakenly declared using 'x_irred.x' instead
+    of 'x_irred.e'.  Works fine under the CL but broke Pyraf  (1/18/07, MJF)
+
+irred$center.par
+irred$doc/center.hlp
+    Updated the center task parameter file to support the new cache, wcsin,
+    and wcsout parameters.
+
+    Added a copy of the center task help page so it is accessible even
+    if apphot is not loaded. Center1d gets picked up instead in that case.
+
+    Davis, April 8, 2001
+
+irred$mosproc.cl
+    Changed the outtype parameter setting in the imcombine task call from
+    "" to "real". Added default values for the rejmask, nkeep, and snoise
+    parameters.
+
+    Davis, January 18, 1999
+
+irred$irred.cl
+irred$irred.hd
+irred$irred.men
+irred$mkpkg
+irred$irlincor.par
+irred$x_irred.x
+irred$t_irlincor.x
+irred$doc/irlincor.hlp
+    Added the ctio.irlincor package task to the irred package.
+
+irred$irred.cl
+irred$mosproc.cl
+    1. The irred cl script was modified to reference nproto instead of proto.
+    2. The irred script was modified to load the core proto package in order to
+       pick up the bscale task.
+    3. The references to the apselect task were replace by references to the
+       txdump task.
+    4. The bscale.par file was removed since one cannot have private copies
+       of .par files across package boundaries.
+    5. Replaced the obsolete version of datapars.par with the new version.
+    6. Replaced the obsolate versions of irmosaic.par, iralign.par,
+       irmatch1d.par, and irmatch2d.par with new ones.
+
+    Davis, January 25, 1992
+
+irred$mosproc.cl
+    1. Replaced the call to imcombine with a call to the new imcombine.
+
+    Davis, January 25, 1992
+
+    
+irred$
+    The IRRED package was added to the imred package menu. The current
+    tasks are bscale, center, irmosaic, iralign, irmatch1d, and irmatch2d,
+    mosproc, and txdump.
+    Davis, April 1, 1989
+
+.endhelp
diff --git a/noao/imred/irred/center.par b/noao/imred/irred/center.par
new file mode 100644
index 00000000..4cc613cd
--- /dev/null
+++ b/noao/imred/irred/center.par
@@ -0,0 +1,21 @@
+# CENTER
+
+image,f,a,,,,"Input image(s)"
+coords,f,h,"",,,"Input coordinate list(s) (default: image.coo.?)"
+output,f,h,"default",,,"Output center file(s) (default: image.ctr.?)"
+plotfile,s,h,"",,,"Output plot metacode file"
+datapars,pset,h,"",,,"Data dependent parameters"
+centerpars,pset,h,"",,,"Centering parameters"
+interactive,b,h,yes,,,"Interactive mode ?"
+radplots,b,h,no,,,"Plot the radial profiles in interactive mode ?"
+icommands,*imcur,h,"",,,"Image cursor: [x y wcs] key [cmd]"
+gcommands,*gcur,h,"",,,"Graphics cursor: [x y wcs] key [cmd]"
+wcsin,s,h,logical,,,"The input coordinate system (logical,tv,physical,world)"
+wcsout,s,h,logical,,,"The output coordinate system (logical,tv,physical)"
+cache,b,h,no,,,"Cache the input image pixels in memory ?"
+verify,b,h,yes,,,"Verify critical parameters in non-interactive mode ?"
+update,b,h,no,,,"Update critical parameters in non-interactive mode ?"
+verbose,b,h,yes,,,"Print messages in non-interactive mode ?"
+graphics,s,h,"stdgraph",,,"Graphics device"
+display,s,h,"stdimage",,,"Display device"
+mode,s,h,'ql'
diff --git a/noao/imred/irred/centerpars.par b/noao/imred/irred/centerpars.par
new file mode 100644
index 00000000..1692b29e
--- /dev/null
+++ b/noao/imred/irred/centerpars.par
@@ -0,0 +1,14 @@
+# CENTERPARS
+
+calgorithm,s,h,"centroid","|centroid|gauss|none|ofilter|",,Centering algorithm
+cbox,r,h,5.0,,,Centering box width in scale units
+cthreshold,r,h,0.0,,,Centering threshold in sigma above background
+minsnratio,r,h,1.0,0.0,,Minimum signal-to-noise ratio for centering algorithm
+cmaxiter,i,h,10,,,Maximum number of iterations for centering algorithm
+maxshift,r,h,1.0,,,Maximum center shift in scale units
+clean,b,h,no,,,Symmetry clean before centering ?
+rclean,r,h,1.0,,,Cleaning radius in scale units
+rclip,r,h,2.0,,,Clipping radius in scale units
+kclean,r,h,3.0,,,Rejection limit in sigma
+mkcenter,b,h,no,,,Mark the computed center on display ?
+mode,s,h,'ql'
diff --git a/noao/imred/irred/datapars.par b/noao/imred/irred/datapars.par
new file mode 100644
index 00000000..15778b9f
--- /dev/null
+++ b/noao/imred/irred/datapars.par
@@ -0,0 +1,25 @@
+# DATAPARS
+
+scale,r,h,1.0,0.0,,Image scale in units per pixel
+fwhmpsf,r,h,2.5,0.0,,FWHM of the PSF in scale units
+emission,b,h,y,,,Features are positive ?
+sigma,r,h,INDEF,,,Standard deviation of background in counts
+datamin,r,h,INDEF,,,Minimum good data value
+datamax,r,h,INDEF,,,Maximum good data value
+
+noise,s,h,"poisson","|constant|poisson|",,Noise model
+ccdread,s,h,"",,,CCD readout noise image header keyword
+gain,s,h,"",,,CCD gain image header keyword
+readnoise,r,h,0.0,,,CCD readout noise in electrons
+epadu,r,h,1.0,,,Gain in electrons per count
+
+exposure,s,h,"",,,Exposure time image header keyword
+airmass,s,h,"",,,Airmass image header keyword
+filter,s,h,"",,,Filter image header keyword
+obstime,s,h,"",,,Time of observation image header keyword
+itime,r,h,1.0,,,Exposure time
+xairmass,r,h,INDEF,,,Airmass
+ifilter,s,h,"INDEF",,,Filter
+otime,s,h,"INDEF",,,Time of observation
+
+mode,s,h,'ql'
diff --git a/noao/imred/irred/doc/center.hlp b/noao/imred/irred/doc/center.hlp
new file mode 100644
index 00000000..1171deb4
--- /dev/null
+++ b/noao/imred/irred/doc/center.hlp
@@ -0,0 +1,637 @@
+.help center May00 irred
+.ih
+NAME
+center -- compute accurate centers for a list of objects
+.ih
+USAGE
+center image
+.ih
+PARAMETERS
+.ls image
+The list of images containing the objects to be centered.
+.le
+.ls coords = ""
+The list of text files containing initial coordinates for the objects to
+be centered. Objects are listed in coords one object per line with the
+initial coordinate values in columns one and two. The number of coordinate
+files must be zero, one, or equal to the number of images.
+If coords is "default", "dir$default", or a directory specification then an
+coords file name of the form dir$root.extension.version is constructed and
+searched for, where dir is the directory, root is the root image name,
+extension is "coo" and version is the next available version number for the
+file.
+.le
+.ls output = "default"
+The name of the results file or results directory. If output is
+"default", "dir$default", or a directory specification then an output file name
+of the form dir$root.extension.version is constructed, where dir is the
+directory, root is the root image name, extension is "ctr" and version is
+the next available version number for the file. The number of output files
+must be zero, one, or equal to the number of image files.  In both interactive
+and batch mode full output is written to output. In interactive mode
+an output summary is also written to the standard output.
+.le
+.ls plotfile = ""
+The name of the file containing radial profile plots of the stars written
+to the output file. If plotfile is defined then a radial profile plot
+is written to plotfile every time a record is written to \fIoutput\fR.
+The user should be aware that this can be a time consuming operation.
+.le
+.ls datapars = ""
+The name of the file containing the data dependent parameters.
+The critical parameters \fIfwhmpsf\fR and \fIsigma\fR are located in
+datapars.  If datapars is undefined then the default parameter set in 
+uparm directory is used.
+.le
+.ls centerpars = ""
+The name of the file containing the centering algorithm parameters.
+The critical parameters \fIcalgorithm\fR and \fIcbox\fR are located in
+centerpars. If centerpars is undefined then the default parameter
+set in uparm is used.
+.le
+.ls interactive = yes
+Interactive or non-interactive mode?
+.le
+.ls radplots = no
+If \fIradplots\fR is "yes" and CENTER is run in interactive mode, a radial
+profile of each star is plotted on the screen after the center is fit.
+.le
+.ls icommands = ""
+The image display cursor or image cursor command file. 
+.le
+.ls gcommands = ""
+The graphics cursor or graphics cursor command file.
+.le
+.ls wcsin = "logical", wcsout = "logical"
+The coordinate system of the input coordinates read from \fIcoords\fR and
+of the output coordinates written to \fIoutput\fR respectively. The image
+header coordinate system is used to transform from the input coordinate
+system to the "logical" pixel coordinate system used internally,
+and from the internal "logical" pixel coordinate system to the output
+coordinate system. The input coordinate system options are "logical", tv",
+"physical", and "world". The output coordinate system options are "logical",
+"tv", and "physical". The image cursor coordinate system is assumed to
+be the "tv" system.
+.ls logical
+Logical coordinates are pixel coordinates relative to the current image.
+The  logical coordinate system is the coordinate system used by the image
+input/output routines to access the image data on disk. In the logical
+coordinate system the coordinates of the first pixel of a  2D image, e.g.
+dev$ypix  and a 2D image section, e.g. dev$ypix[200:300,200:300] are
+always (1,1).
+.le
+.ls tv  
+Tv coordinates are the pixel coordinates used by the display servers. Tv
+coordinates  include  the effects of any input image section, but do not
+include the effects of previous linear transformations. If the input
+image name does not include an image section, then tv coordinates are
+identical to logical coordinates.  If the input image name does include a
+section, and the input image has not been linearly transformed or copied from
+a parent image, tv coordinates are identical to physical coordinates.
+In the tv coordinate system the coordinates of the first pixel of a 
+2D image, e.g. dev$ypix and a 2D image section, e.g. dev$ypix[200:300,200:300]
+are (1,1) and (200,200) respectively.
+.le
+.ls physical
+Physical coordinates are pixel coordinates invariant  with respect to linear
+transformations of the physical image data.  For example, if the current image
+was created by extracting a section of another image,  the  physical
+coordinates of an object in the current image will be equal to the physical
+coordinates of the same object in the parent image,  although the logical
+coordinates will be different.  In the physical coordinate system the
+coordinates of the first pixel of a 2D image, e.g. dev$ypix and a 2D
+image section, e.g. dev$ypix[200:300,200:300] are (1,1) and (200,200)
+respectively.
+.le
+.ls world
+World coordinates are image coordinates in any units which are invariant
+with respect to linear transformations of the physical image data. For
+example, the ra and dec of an object will always be the same no matter
+how the image is linearly transformed. The units of input world coordinates
+must be the same as those expected by the image header wcs, e. g. 
+degrees and degrees for celestial coordinate systems.
+.le
+The wcsin and wcsout parameters default to the values of the package
+parameters of the same name. The default values of the package parameters
+wcsin and wcsout are "logical" and "logical" respectively. 
+.le
+.ls cache = no
+Cache the image pixels in memory. Cache may be set to "yes", or "no".
+By default cacheing is 
+disabled.
+.le
+.ls verify = yes
+Verify the critical parameters in non-interactive mode ? Verify may be set to
+or "no.
+.le
+.ls update = no
+Update the critical parameters in non-interactive mode if \fIverify\fR is
+set to yes? Update may be set to "yes" or "no.
+.le
+.ls verbose = yes
+Print messages on the terminal in non-interactive mode ? Verbose may be set
+to "yes" or "no.
+.le
+.ls graphics = ")_.graphics"
+The default graphics device.
+Graphics may be set to the apphot package parameter value (the default), "yes",
+or "no.
+.le
+.ls display = ")_.display"
+The default display device.  Display may be set to the apphot package
+parameter value (the default), "yes", or "no. By default graphics overlay
+is disabled.  Setting display to one of "imdr", "imdg", "imdb", or "imdy"
+enables graphics overlay with the IMD graphics kernel.  Setting display to
+"stdgraph" enables CENTER to work interactively from a contour plot.
+.le
+
+.ih
+DESCRIPTION
+CENTER computes accurate centers for a set of objects in the IRAF image
+\fIimage\fR, whose initial coordinates are read from the image display cursor, 
+from the text file \fIcoords\fR, or from a cursor command file.
+The computed x and y coordinates, the errors,  and the fitting parameters
+are written to the text file \fIoutput\fR.
+
+The coordinates read from \fIcoords\fR are assumed to be in coordinate
+system defined by \fIwcsin\fR. The options are "logical", "tv", "physical",
+and "world" and the transformation from the input coordinate system to
+the internal "logical" system is defined by the image coordinate system.
+The simplest default is the "logical" pixel system. Users working on with
+image sections but importing pixel coordinate lists generated from the parent
+image must use the "tv" or "physical" input coordinate systems.
+Users importing coordinate lists in world coordinates, e.g. ra and dec,
+must use the "world" coordinate system and may need to convert their
+equatorial coordinate units from hours and degrees to degrees and degrees first.
+
+The coordinates written to \fIoutput\fR are in the coordinate
+system defined by \fIwcsout\fR. The options are "logical", "tv",
+and "physical". The simplest default is the "logical" system. Users
+wishing to correlate the output coordinates of objects measured in
+image sections or mosaic pieces with coordinates in the parent
+image must use the "tv" or "physical" coordinate systems.
+
+If \fIcache\fR is yes and the host machine physical memory and working set size
+are large enough, the input image pixels are cached in memory. If cacheing
+is enabled and CENTER is run interactively the first measurement will appear
+to take a long time as the entire image must be read in before the measurement
+is actually made. All subsequent measurements will be very fast because CENTER
+is accessing memory not disk. The point of cacheing is to speed up random
+image access by making the internal image i/o buffers the same size as the
+image itself. However if the input object lists are sorted in row order and
+sparse cacheing may actually worsen not improve the execution time. Also at
+present there is no point in enabling cacheing for images that are less than
+or equal to 524288 bytes, i.e. the size of the test image dev$ypix, as the
+default image i/o buffer is exactly that size. However if the size of dev$ypix
+is doubled by converting it to a real image with the chpixtype task then the
+effect of cacheing in interactive is can be quite noticeable if measurements
+of objects in the top and bottom halves of the image are alternated.
+
+CENTER can be run either interactively or in batch mode by setting the
+parameter \fIinteractive\fR. In interactive mode starting x and y positions
+can either be read directly from the image cursor or read from the text
+file \fIcoords\fR. In interactive mode the user can examine, adjust, and
+save the algorithm parameters, change ojects interactively, query for
+the next or nth object in the list, or fit the entire coordinate list with
+the chosen parameter set.  In batch mode the positions can be read from the
+text file \fIcoords\fR or the image cursor can be redirected to a text file
+containing a list of cursor commands as specified by the parameter
+\fIicommands\fR. 
+
+.ih
+CURSOR COMMANDS
+
+The following cursor commands are currently available.
+
+.nf
+	Interactive Keystroke Commands
+
+?	Print help
+:	Colon commands
+v	Verify the critical parameters
+w	Save the current parameters
+d	Plot radial profile of current star
+i	Interactively set parameters using current star
+f	Fit center of current star
+spbar	Fit center of current star, output results
+m	Move to next star in coordinate list
+n	Center next star in coordinate list, output results
+l	Center remaining stars in coordinate list, output results
+e	Print error messages
+r	Rewind the coordinate list
+q	Exit task
+
+
+	Colon Commands
+
+:show	[data/center]	List the parameters
+:m      [n]	        Move to next [nth] star in coordinate list
+:n      [n]	        Center next [nth] star in coordinate list,
+			output results
+
+
+	Colon Parameter Editing Commands
+
+# Image and file name parameters
+
+:image		[string]	Image name
+:coords		[string]	Coordinate file name
+:output 	[string]	Output file name
+
+# Data dependent parameters
+
+:scale		[value]		Image scale (units per pixel)
+:fwhmpsf	[value]		Full-width half-maximum of PSF (scale units)
+:emission	[y/n]		Emission feature (y), absorption (n)
+:sigma		[value]		Standard deviation of sky (counts)
+:datamin	[value]		Minimum good data value (counts)
+:datamax	[value]		Maximum good data value (counts)
+
+# Noise parameters
+
+:noise 		[string]	Noise model (constant|poisson)
+:gain		[string]	Gain image header keyword
+:ccdread	[string]	Readout noise image header keyword
+:epadu		[value]		Gain (electrons per adu)
+:readnoise	[value]		Readout noise (electrons)
+
+# Observations parameters
+
+:exposure	[string]	Exposure time image header keyword
+:airmass	[string]	Airmass image header keyword
+:filter		[string]	Filter image header keyword
+:obstime	[string]	Time of observation image header keyword
+:itime		[value]		Exposure time (time units)
+:xairmass	[value]		Airmass value (number)
+:ifilter	[string]	Filter id string
+:otime		[string]	Time of observation (time units)
+
+# Centering parameters 
+
+:calgorithm	[string]	Centering algorithm
+:cbox		[value]		Width of centering box (scale units)
+:cthreshold	[value]		Centering intensity threshold (sigma)
+:cmaxiter	[value]		Maximum number of iterations
+:maxshift	[value]		Maximum center shift (scale units)
+:minsnratio	[value]		Minimum signal to noise for centering
+:clean		[y/n]		Clean subraster before centering
+:rclean		[value]		Cleaning radius (scale units)
+:rclip		[value]		Clipping radius (scale units)
+:kclean		[value]		Clean K-sigma rejection limit (sigma)
+
+# Plotting and marking parameters
+
+:mkcenter	[y/n]		Mark computed centers on the display
+:radplot	[y/n]		Plot radial profile of object
+
+
+The following keystroke commands are available from the interactive setup
+menu.
+
+                    Interactive Center Setup Menu
+
+	v	Mark and verify the critical center parameters (f,s,c)
+
+	f	Mark and verify the full-width half-maximum of the psf
+	s	Mark and verify the standard deviation of the background
+	l	Mark and verify the minimum good data value
+	u	Mark and verify the maximum good data value
+
+	c	Mark and verify the centering box half-width
+	n	Mark and verify the cleaning radius
+	p	Mark and verify the clipping radius
+.fi
+
+.ih
+ALGORITHMS
+
+Descriptions of the data dependent parameters and the centering
+algorithm parameters can be found in the online manual pages for
+\fIdatapars\fR and \fIcenterpars\fR.
+
+.ih
+OUTPUT
+
+In interactive mode the following quantities are written to the terminal
+as each object is measured. Error is a simple string which indicates
+whether an error condition has been flagged.  The centers and their errors are
+in pixel units.
+
+.nf
+	image  xinit  yinit  xcenter  ycenter  xerr  yerr  error
+.fi
+
+In both interactive and batch mode the full output is written to the
+text file \fIoutput\fR. At the beginning of each file is a header
+listing the current values of the parameters when the first stellar
+record was written. These parameters can be subsequently altered.
+For each star measured the following record is written
+
+.nf
+	image  xinit  yinit  id  coords  lid
+	   xcenter  ycenter  xshift  yshift  xerr  yerr  cier error
+.fi
+
+Image and coords are the name of the image and coordinate file respectively.
+Id and lid are the sequence numbers of stars in the output and coordinate
+files respectively. Cier and error are the centering error code and accompanying
+error message respectively.  Xinit, yinit, xcenter, ycenter, xshift, yshift,
+and xerr, yerr are self explanatory and output in pixel units. The sense of
+the xshift and yshift definitions is the following.
+
+.nf
+	xshift = xcenter - xinit
+	yshift = ycenter - yinit
+.fi
+
+In interactive mode a radial profile of each measured object is plotted
+in the graphics window if \fIradplots\fR is "yes".
+
+In interactive and batchmode a radial profile plot is written to
+\fIplotfile\fR  if it is defined each time the result of an object
+measurement is written to \fIoutput\fR .
+
+.ih
+ERRORS
+
+If the object centering was error free then the field cier will be zero.
+Non-zero values in the cier column flag the following error conditions.
+
+.nf
+	0        # No error
+	101      # The centering box is off the image
+	102      # The centering box is partially off the image
+	103      # The S/N ratio is low in the centering box
+	104      # There are two few points for a good fit
+	105      # The x or y center fit is singular
+	106      # The x or y center fit did not converge
+	107      # The x or y center shift is greater than maxshift
+	108      # There is bad data in the centering box
+.fi
+
+.ih
+EXAMPLES
+
+1. Compute the centers for a few  stars in dev$ypix using the image display
+and the image cursor. Setup the task parameters using the interactive
+setup menu defined by the i keystroke command and a radial profile plot.
+
+.nf
+	ap> display dev$ypix 1 fi+
+
+	... display the image
+
+	ap> center dev$ypix
+
+	... type ? to see help screen
+
+	... move image cursor to a star
+	... type i to enter the interactive setup menu
+	... enter the maximum radius in pixels for the radial profile or
+	    accept the default with a CR
+	... type  v to get the default menu
+	... set the fwhmpsf, sigma, and centering box half-width using the
+	    graphics cursor and the stellar radial profile plot
+	... typing <CR> after a prompt leaves the parameter at its default
+	    value
+	... type q to exit setup menu
+
+	... type the v key to verify the critical parameters
+
+	... type the w key to save the parameters in the parameter files
+
+	... move the image cursor to the stars of interest and tap
+	    the space bar
+
+	... type q to quit followed by q to confirm the quit
+
+	... the output will appear in ypix.ctr.1
+
+.fi
+
+2. Compute the centers for a few stars in dev$ypix using the contour plot
+and the graphics cursor. This option is only useful for those (now very few)
+users who have access to a graphics terminal but not to an image display
+server. Setup the task parameters using the interactive setup menu defined by
+the i key command as in example 1.
+
+.nf
+	ap> show stdimcur
+
+	... record the default value of stdimcur
+
+	ap> set stdimcur = stdgraph
+
+	... define the image cursor to be the graphics cursor
+
+	ap> contour dev$ypix
+
+	... make a contour plot of dev$ypix
+
+	ap> contour dev$ypix >G ypix.plot1
+
+	... store the contour plot of ypix in the file ypix.plot
+
+	ap> center dev$ypix display=stdgraph
+
+	... type ? to see the help screen
+
+	... move graphics cursor to a star
+	... type i to enter the interactive setup menu
+	... enter the maximum radius in pixels for the radial profile or
+	    accept the default with a CR
+	... type v key to get the default setup menu
+	... enter maximum radius in pixels of the radial profile
+	... set the fwhmpsf, sigma, and centering box half-width
+	    using the graphics cursor and the stellar radial profile plot
+	... typing <CR> after the prompt leaves the parameter at its
+	    default value
+	... type q to quit the setup menu
+
+	... type the v key to verify critical parameters
+
+	... type the w key to save the parameters in the parameter files
+
+	... retype :.read ypix.plot1 to reload the contour plot
+
+	... move the graphics cursor to the stars of interest and tap
+	    the space bar
+
+	... a one line summary of the answers will appear on the standard
+	    output for each star measured
+
+	... type q to quit followed by q to confirm the quit
+
+	... full output will appear in the text file ypix.ctr.2 
+
+	ap> set stdimcur = <default>
+
+	... reset stdimcur to its previous value
+.fi
+
+
+3. Setup and run CENTER interactively on a list of objects temporarily
+overriding the fwhmpsf, sigma, and cbox parameters determined in examples
+1 or 2.
+
+.nf
+	ap> daofind dev$ypix fwhmpsf=2.6 sigma=25.0 verify-
+
+	... make a coordinate list 
+
+	... the output will appear in the text file ypix.coo.1
+
+	ap> center dev$ypix cbox=7.0 coords=ypix.coo.1 
+
+	... type ? for optional help
+
+
+	... move the graphics cursor to the stars and tap space bar
+
+				or
+
+	... select stars from the input coordinate list with m / :m #
+	    and measure with spbar
+
+	... measure stars selected from the input coordinate list
+	    with n / n #
+
+	... a one line summary of results will appear on the standard output
+	    for each star measured
+
+	... the output will appear in ypix.ctr.3 ...
+.fi
+
+
+4. Display and measure some stars in an image section and write the output
+coordinates in the coordinate system of the parent image.
+
+.nf
+	ap> display dev$ypix[150:450,150:450] 1
+
+	... display the image section
+
+	ap> center dev$ypix[150:450,150:450] wcsout=tv
+
+	... move cursor to stars and type spbar
+
+	... type q to quit and q again to confirm quit
+
+	... output will appear in ypix.ctr.4
+
+	ap> pdump ypix.ctr.4 xc,yc yes | tvmark 1 STDIN col=204 
+.fi
+
+
+5. Run CENTER in batch mode using the coordinate file and the previously
+saved parameters. Verify the critical parameters.
+
+.nf
+	ap> center dev$ypix coords=ypix.coo.1 verify+ inter-
+
+	... output will appear in ypix.ctr.5 ...
+.fi
+
+
+6. Repeat example 5 but assume that the input coordinate are ra and dec
+in degrees and degrees, turn off verification, and submit the task to to
+the background.
+
+.nf
+	ap> display dev$ypix
+
+	ap> rimcursor wcs=world > radec.coo
+
+	... move to selected stars and type any key
+
+	... type ^Z to quit
+
+	ap> center dev$ypix coords=radec.coo wcsin=world verify- inter- &
+
+	... output will appear in ypix.ctr.6
+
+	ap> pdump ypix.ctr.6 xc,yc yes | tvmark 1 STDIN col=204
+
+	... mark the stars on the display
+
+
+7. Run CENTER interactively without using the image display.
+
+.nf
+	ap> show stdimcur
+
+	... record the default value of stdimcur
+
+	ap> set stdimcur = text
+
+	... set the image cursor to the standard input
+
+	ap> center dev$ypix coords=ypix.coo.1
+
+	... type ? for optional help
+
+	... type :m 3 to set the initial coordinates to those of the
+	    third star in the list
+
+	... type i to enter the interactive setup menu
+	... enter the maximum radius in pixels for the radial profile or
+	    accept the default with a CR
+	... type v to enter the default menu
+	... set the fwhmpsf, sigma, and centering box half-width
+	    using the graphics cursor and the stellar radial profile plot
+	... typing <CR> after the prompt leaves the parameter at its default
+	    value
+
+	... type r to rewind the coordinate list
+
+	... type l to measure all the stars in the coordinate list
+
+	... a one line summary of the answers will appear on the standard
+	    output for each star measured
+
+	... type q to quit followed by q to confirm the quit
+
+	... full output will appear in the text file ypix.ctr.7 
+
+	ap> set stdimcur = <default>
+
+	... reset the value of stdimcur
+.fi
+
+8. Use a image cursor command file to drive the CENTER task. The cursor command
+file shown below sets the fwhmpsf, calgorithm, and cbox parameters, computes
+the centers for 3 stars, updates the parameter files, and quits the task.
+
+.nf
+	ap> type cmdfile
+	: calgorithm gauss
+	: fwhmpsf 2.5
+	: cbox 9.0
+	442 410 101 \040 
+	349 188 101 \040 
+	225 131 101 \040 
+	w
+	q
+
+	ap> center dev$ypix icommands=cmdfile  verify-
+
+	... full output will appear in ypix.ctr.8
+.fi
+
+.ih
+BUGS
+
+It is the responsibility of the user to make sure that the image displayed
+in the image display is the same as the image specified by the image parameter.
+
+Commands which draw to the image display are disabled by default.
+To enable graphics overlay on the image display, set the display
+parameter to "imdr", "imdg", "imdb", or "imdy" to get red, green,
+blue or yellow overlays and set the centerpars mkcenter switch to
+"yes". It may be necessary to run gflush and to redisplay the image
+to get the overlays position correctly. 
+
+.ih
+SEE ALSO
+datapars, centerpars
+.endhelp
diff --git a/noao/imred/irred/doc/irlincor.hlp b/noao/imred/irred/doc/irlincor.hlp
new file mode 100644
index 00000000..630370a1
--- /dev/null
+++ b/noao/imred/irred/doc/irlincor.hlp
@@ -0,0 +1,81 @@
+.help irlincor Nov94 irred
+.ih
+NAME
+irlincor -- Correct IR imager frames for non-linearity.
+.ih
+USAGE
+irlincor input output
+.ih
+PARAMETERS
+.ls input
+The list of images to be corrected for non-linearity
+.le
+.ls output
+The list of corrected output images
+.le
+
+.ls coeff1 = 1.0
+The first coefficient of the correction function
+.le
+
+.ls coeff2 = 0.0
+The second coefficient of the correction function
+.le
+
+.ls coeff3 = 0.0
+The third coefficient of the correction function
+.le
+
+.ih
+DESCRIPTION
+The IR imager frames specified by \fIinput\fR, which may be a general image
+template including wild cards or an @list, are corrected for non-linearity
+on a pixel by pixel basis and written to \fIoutput\fR. The number of output
+images must match the number input. The pixel type of the output image(s) will
+match that of the input image(s), however, internally all calculations are 
+performed as type real. The correction is performed assuming 
+that the non-linearity can be represented by the following simple relationship:
+.nf
+
+ADU' = ADU * [ coeff1 + coeff2 * (ADU / 32767) + coeff3 * (ADU / 32767)**2 ]
+
+.fi
+The coefficients which occur in this expression are specified by the
+parameters \fIcoeff1\fR, \fIcoeff2\fR and \fIcoeff3\fR. Their values are 
+derived from periodic instrumental calibrations and are believed to be
+fairly constant. The  default values specify a \fBnull\fR correction.
+You should consult \fBJay Elias\fR for the latest values.
+Note that the coefficients are expressed in terms of ADU normalised to the
+maximum possible value 32767, in order that their values can be input
+more easily.
+.ih
+EXAMPLES
+1. Correct input to output using the default values for the coefficients (not a very rewarding operation!)
+
+.nf
+	cl> irlincor input output
+
+.fi
+
+2. Correct a list of images in place using specified values for the coefficients
+
+.nf
+	cl> irlincor @list @list coeff1=1.0 coeff2=0.1 coeff3=0.01
+
+.fi
+.ih
+TIME REQUIREMENTS
+.ih
+AUTHORS
+The IRLINCOR task was originally written by Steve Heathcote as part of the
+CTIO package. 
+.ih
+BUGS
+The form of the correction equation is currently experimental;
+a higher order polynomial or a different functional form could be accommodated
+very easily if required.
+It may be advisable to carry out the calculations in double precision.
+.ih
+SEE ALSO
+onedspec.coincor, proto.imfunction
+.endhelp
diff --git a/noao/imred/irred/doc/mosproc.hlp b/noao/imred/irred/doc/mosproc.hlp
new file mode 100644
index 00000000..d0f5c931
--- /dev/null
+++ b/noao/imred/irred/doc/mosproc.hlp
@@ -0,0 +1,170 @@
+.help mosproc May89 irred
+.ih
+NAME
+mosproc -- Prepare images for quick look mosaicing
+.ih
+USAGE
+mosproc input output nxsub nysub
+.ih
+PARAMETERS
+.ls input
+The list of input images to be mosaiced. The images are assumed
+to be ordered either by row, column, or in a raster pattern. If
+the image list is not in order then the iraf \fBfiles\fR task plus
+the \fBeditor\fR must be used to construct an image list. The images
+in the input list are assumed to all be the same size.
+.le
+.ls output
+The name of the output mosaiced image.
+.le
+.ls nxsub
+The number of subrasters along a row of the output image.
+.le
+.ls nysub
+The number of subrasters along a column of the output image.
+.le
+.ls skysubtract = yes
+Subtract a sky image from all the input images. The sky image
+to be subtracted is either \fIsky\fR or a sky image computed
+by median filtering selected input images after weighting the images
+by the exposure time..
+.le
+.ls sky = ""
+The name of the sky image.
+.le
+.ls exclude = ""
+The input images to be excluded from the computation of the sky image.
+For example if \fIexclude\fR="1,3-5" then input images 1, 3, 4, 5 are
+not used for computing the sky frame.
+.le
+.ls expname = "exptime"
+The image header exposure time keyword. If the sky frame is computed
+internally by median filtering the input images, the individual images
+are weighted by the exposure time defined by the exposure time
+keyword \fIexpname\fR. Weights of 1 are assigned when no exposure time
+is given.
+.le
+.ls flatten = yes
+Divide all the images by a flat field image. Flat fielding is done
+after sky subtraction. If the name of a flat field image \fIflat\fR
+is supplied that image is divided directly into all the input images.
+Otherwise the skyframe computed above is normalized by the mode of the
+pixels and divided into all the input images.
+.le
+.ls flat = ""
+The name of the flat field image.
+.le
+.ls transpose = no
+Transpose the input images before inserting them into the mosaic.
+.le
+.ls trim_section = "[*,*]"
+The section of the input images to be mosaiced into the output
+image. Section can be used to flip and/or trim the individual
+subrasters before adding them to the mosaic. For example if we
+want to flip each subraster around the y axis before adding it
+to the mosaic, then \fItrim_section\fR = "[*,-*]".
+.le
+.ls corner = "lr"
+The starting position in the output image. The four options are "ll" for
+lower left corner, "lr" for lower right corner, "ul" for upper left
+corner and "ur" for upper right corner.
+.le
+.ls direction = "row"
+Add input images to the output image in row or column order. The options
+are "row" for row order and "column" for column order. The direction
+specified must agree with the order of the input list.
+.le
+.ls raster = no
+Add the columns or rows to the output image in a raster pattern or return
+to the start of a column or a row.
+.le
+.ls median_section = ""
+Compute the median of each input image inserted into the mosaic using the
+specified section.
+.le
+.ls subtract = no
+Subtract the computed median from each input image before inserting it
+into the mosaic.
+.le
+.ls oval = -1.0
+The value of border pixels.
+.le
+.ls delete = yes
+Delete sky subtracted, flat fielded and transposed images upon exit from
+the script.
+.le
+.ls logfile = STDOUT
+The name of the log file.
+.le
+
+.ih
+DESCRIPTION
+
+MOSPROC takes the list of input images \fIinput\fR of identical dimensions and
+inserts them into a single output image \fIoutput\fR. Before mosaicing the user
+can optionally sky subtract, flat field or transpose the input images.
+If \fIskysubtract\fR = yes, a single sky
+image is subtracted from all the input images. The sky image
+may be the externally derived image \fIsky\fR or calculated internally 
+by computing the exposure time weighted median of the input images, minus
+those input images specifically excluded by the \fIexclude\fR parameter.
+If \fIflatten\fR = yes, the input images are flat fielded using either
+the externally defined flat field image \fIflat\fR or the internally
+derived sky image normalized by its mode.
+If \fItranspose\fR is enabled all the input images are optionally transposed
+before mosaicing.
+
+MOSPROC takes the list of processed images and inserts them into the 
+output image in positions determined by their order in the input list,
+\fInxsub\fR, \fInysub\fR and the parameters  \fIcorner\fR, \fIdirection\fR
+and \fIraster\fR. 
+The orientation and size of each individual subraster in the output image
+may be altered by setting the parameter \fItrim_section\fR. The size
+of the output image is determined by nxsub and nysub and the size of
+the individual input images. A one column wide border is drawn between
+each of the output image subrasters with a pixel value of \fIoval\fR.
+The user may optionally  compute and subtract the median from each input
+image before inserting it into the mosaic.
+
+MOSPROC produces an output mosaiced image \fIoutput\fR and an accompanying
+database file \fIdboutput\fR. These two files plus an interactively
+generated coordinate list comprise the necessary input for the IRALIGN,
+IRMATCH1D and IRMATCH2D tasks.
+The temporary images generated (sky substracted, flat fielded, and
+transposed)
+can be deleted automatically if \fBdelete=yes\fR, before the task completes.
+Otherwise they will be left in the same directory of the input images.
+The temporary sky and flat field images if created are not deleted.
+
+The computation of the sky frame is done with IMAGES.IMCOMBINE and the
+subsequent sky subraction with IMAGES.IMARITH. The computation of
+the flat field is done with PROTO.BSCALE and the flat field division
+with FLATTEN. The task IMAGES.TRANSPOSE transpose the input.
+The mosaicing itself is done with PROTO.IRMOSAIC.
+
+.ih
+EXAMPLES
+
+1. Mosaic a list of 64 infrared images onto an 8 by 8 grid after sky 
+   subtraction and flat fielding. Use an externally derived sky and
+   flat field image
+ 
+    ir> mosproc @imlist mosaic 8 8 skysub+ sky=skyimage flatten+ \
+    >>>  flat=flatfield
+
+2. Mosaic a list of 64 infrared images onto an 8 by 8 grid after sky 
+   subtraction and flat fielding. Derive the sky and flat field frames
+   from the data excluding image number 5
+ 
+    ir> mosproc @imlist mosaic 8 8 skysub+ exclude="5" flatten+ 
+
+.ih
+TIME REQUIREMENTS
+
+.ih
+BUGS
+
+.ih
+SEE ALSO
+images.imcombine, images.imarith, proto.bscale, images.imtrans, proto.irmosaic
+.endhelp
diff --git a/noao/imred/irred/imcombine b/noao/imred/irred/imcombine
new file mode 100644
index 00000000..c95d8302
--- /dev/null
+++ b/noao/imred/irred/imcombine
@@ -0,0 +1,11 @@
+imcombine ("@"//tmptmp, skyframe, sigma="", logfile=logfile,
+    outtype="", option="median", expname=expname, exposure+,
+    sca-, off-, wei+, modesec="", low=3., high=3., blank=-1)
+
+imcombine ("@"//tmptmp, skyframe, plfile="", sigma="", logfile=logfile,
+    combine="median", reject="none", project=no, outtype="", offsets="none",
+    masktype="none", maskvalue=0.0, blank=-1.0, scale="exposure",
+    zero="none", weight="exposure", statsec="", expname=expname,
+    lthreshold=INDEF, hthreshold=INDEF, nlow=1, nhigh=1, mclip=yes,
+    lsigma=3.0, hsigma=3.0, rdnoise="0.0", gain="1.0", sigscale=0.1,
+    pclip=-0.5, grow=0)
diff --git a/noao/imred/irred/iralign.par b/noao/imred/irred/iralign.par
new file mode 100644
index 00000000..0865c07d
--- /dev/null
+++ b/noao/imred/irred/iralign.par
@@ -0,0 +1,20 @@
+# IRALIGN
+
+input,f,a,,,,Input image
+output,f,a,,,,Output image
+database,f,a,,,,Database file
+coords,f,a,,,,Coordinate file
+xshift,r,a,0.0,,,Xshift for align by shifts
+yshift,r,a,0.0,,,Yshift for align by shifts
+alignment,s,h,"coords",,,'Alignment technique (coords|shifts|file)'
+nxrsub,i,h,INDEF,,,Row index of reference subraster
+nyrsub,i,h,INDEF,,,Column index of reference subraster
+xref,i,h,0,,,X offset of reference subraster in pixels
+yref,i,h,0,,,Y offset of reference subraster in pixels
+trimlimits,s,h,"[1:1,1:1]",,,Trim limits for each subraster
+nimcols,i,h,INDEF,,,Number of column in the output image
+nimlines,i,h,INDEF,,,Number of lines in the output image
+oval,r,h,INDEF,,,The value of undefined regions the image
+interpolant,s,h,'linear',,,'Interpolant (nearest|linear|poly3|poly5,spline3)'
+verbose,b,h,yes,,,Print messages
+mode,s,h,'ql'
diff --git a/noao/imred/irred/irlincor.par b/noao/imred/irred/irlincor.par
new file mode 100644
index 00000000..701a0483
--- /dev/null
+++ b/noao/imred/irred/irlincor.par
@@ -0,0 +1,7 @@
+# irlincor parameter file
+input,s,a,"",,,Input  images
+output,s,a,"",,,Output images
+section,s,h,"",,,Image section to correct
+coeff1,r,h,1.0,,,First  coefficient of correction equation
+coeff2,r,h,0.0,,,Second coefficient of correction equation
+coeff3,r,h,0.0,,,Third  coefficient of correction equation
diff --git a/noao/imred/irred/irmatch1d.par b/noao/imred/irred/irmatch1d.par
new file mode 100644
index 00000000..a9c40ff6
--- /dev/null
+++ b/noao/imred/irred/irmatch1d.par
@@ -0,0 +1,21 @@
+# IRMATCH1D
+
+input,f,a,,,,Input image
+output,f,a,,,,Output image
+database,f,a,,,,Database file
+coords,f,a,,,,Coordinate file
+xshift,r,a,0.0,,,Xshift for align by shifts
+yshift,r,a,0.0,,,Yshift for align by shifts
+alignment,s,h,"coords",,,'Alignment technique (coords|shifts|file)'
+match,s,h,"*",,,Intensity match the following subrastrers
+nxrsub,i,h,INDEF,,,Row index of reference subraster
+nyrsub,i,h,INDEF,,,Column index of reference subraster
+xref,i,h,0,,,Column offset of reference subraster
+yref,i,h,0,,,Line offset of reference subraster
+trimlimits,s,h,"[1:1,1:1]",,,Trim limits for the input subraster
+nimcols,i,h,INDEF,,,Number of column in the output image
+nimlines,i,h,INDEF,,,Number of lines in the output image
+oval,r,h,INDEF,,,The value of undefined regions the image
+interpolant,s,h,'linear',,,'Interpolant (nearest|linear|poly3|poly5,spline3)'
+verbose,b,h,yes,,,Print messages
+mode,s,h,'ql'
diff --git a/noao/imred/irred/irmatch2d.par b/noao/imred/irred/irmatch2d.par
new file mode 100644
index 00000000..7a159eba
--- /dev/null
+++ b/noao/imred/irred/irmatch2d.par
@@ -0,0 +1,21 @@
+# IRMATCH2D
+
+input,f,a,,,,Input image
+output,f,a,,,,Output image
+database,f,a,,,,Database file
+coords,f,a,,,,Coordinate file
+xshift,r,a,0.0,,,Xshift for align by shifts
+yshift,r,a,0.0,,,Yshift for align by shifts
+alignment,s,h,"coords",,,'Alignment technique (coords|shifts|file)'
+match,s,h,"*",,,Intensity match the following subrastrers
+nxrsub,i,h,INDEF,,,Row index of reference subraster
+nyrsub,i,h,INDEF,,,Column index of reference subraster
+xref,i,h,0,,,Column offset of the reference subraster
+yref,i,h,0,,,Line offset of the reference subraster
+trimlimits,s,h,"[1:1,1:1]",,,Trim limits for the input subraster
+nimcols,i,h,INDEF,,,Number of column in the output image
+nimlines,i,h,INDEF,,,Number of lines in the output image
+oval,r,h,INDEF,,,The value of undefined regions the image
+interpolant,s,h,'linear',,,'Interpolant (nearest|linear|poly3|poly5,spline3)'
+verbose,b,h,yes,,,Print messages
+mode,s,h,'ql'
diff --git a/noao/imred/irred/irmosaic.par b/noao/imred/irred/irmosaic.par
new file mode 100644
index 00000000..7fc573ff
--- /dev/null
+++ b/noao/imred/irred/irmosaic.par
@@ -0,0 +1,22 @@
+# IRMOSAIC
+
+input,f,a,,,,List of input images
+output,f,a,,,,Output image
+database,f,a,,,,Output database file
+nxsub,i,a,,,,Number of input images along the x direction
+nysub,i,a,,,,Number of input images along the y direction
+trim_section,s,h,"[*,*]",,,Input image section written to the output image
+null_input,s,h,"",,,List of missing input images
+corner,s,h,"ll",,,Position of first subraster
+direction,s,h,"row",,,Row or column order placement
+raster,b,h,no,,,Raster scan mode
+median_section,s,h,"",,,Input image section used to compute the median
+subtract,b,h,no,,,Subtract median from each input image
+nimcols,i,h,INDEF,,,The number of columns in the output image
+nimrows,i,h,INDEF,,,The number of rows in the output image
+nxoverlap,i,h,-1,,,Number of columns of overlap between input images
+nyoverlap,i,h,-1,,,Number of rows of overlap between input images
+opixtype,s,h,"r",,,Output image pixel type
+oval,r,h,0.0,,,Value of undefined output image pixels
+verbose,b,h,yes,,,Print out messages
+mode,s,h,'ql'
diff --git a/noao/imred/irred/irred.cl b/noao/imred/irred/irred.cl
new file mode 100644
index 00000000..a3b33765
--- /dev/null
+++ b/noao/imred/irred/irred.cl
@@ -0,0 +1,36 @@
+#{ IRRED -- KPNO IR Camera Reduction Package
+
+# Load necessary core packages
+
+images			# tasks sections,imcopy,imarith,imcombine,imdelete 
+lists			# tokens task
+utilities		# task translit
+proto			# task bscale
+
+# Define necessary paths
+
+set	generic		= "noao$imred/generic/"
+set	nproto		= "noao$nproto/"
+
+package irred
+
+task	irlincor	= "irred$x_irred.e"
+
+task	iralign,
+	irmatch1d,
+	irmatch2d,
+	irmosaic	= "nproto$x_nproto.e"
+
+# Define the apphot centering and related tasks
+
+task	center		= "irred$x_apphot.e"
+task	centerpars	= "irred$centerpars.par"
+task	datapars	= "irred$datapars.par"
+task	txdump		= "irred$x_ptools.e"
+
+# Scripts
+
+task	flatten		= "generic$flatten.cl"
+task	mosproc		= "irred$mosproc.cl"
+
+clbye()
diff --git a/noao/imred/irred/irred.hd b/noao/imred/irred/irred.hd
new file mode 100644
index 00000000..8a2e6437
--- /dev/null
+++ b/noao/imred/irred/irred.hd
@@ -0,0 +1,8 @@
+# Help directory for the IRRED package.
+
+$doc = "./doc/"
+
+center		hlp=doc$center.hlp
+irlincor	hlp=doc$irlincor.hlp,	src=t_irlincor.x
+mosproc		hlp=doc$mosproc.hlp,	src=mosproc.cl
+revisions	sys=Revisions
diff --git a/noao/imred/irred/irred.men b/noao/imred/irred/irred.men
new file mode 100644
index 00000000..e3500032
--- /dev/null
+++ b/noao/imred/irred/irred.men
@@ -0,0 +1,11 @@
+         txdump - Select fields from the center task output text file
+	 center - Compute accurate centers for a list of objects
+     centerpars - Edit the centering parameters
+       datapars - Edit the data dependent parameters
+        flatten - Flatten images using a flat field
+        iralign - Align the image produced by irmosaic
+       irlincor - Correct IR imager frames for non-linearity
+      irmatch1d - Align and intensity match the image produced by irmosaic (1D)
+      irmatch2d - Align and intensity match the image produced by irmosaic (2D)
+       irmosaic - Mosaic an ordered list of images onto a grid
+        mosproc - Prepare images for quick look mosaicing
diff --git a/noao/imred/irred/irred.par b/noao/imred/irred/irred.par
new file mode 100644
index 00000000..18e57b78
--- /dev/null
+++ b/noao/imred/irred/irred.par
@@ -0,0 +1,3 @@
+# PARAMETERS FOR KPNO IR CAMERA REDUCTION PACKAGE
+
+version,s,h,"Mar 1989"
diff --git a/noao/imred/irred/mkpkg b/noao/imred/irred/mkpkg
new file mode 100644
index 00000000..b62021e8
--- /dev/null
+++ b/noao/imred/irred/mkpkg
@@ -0,0 +1,24 @@
+# Make the IRRED package.
+
+$call	relink
+$exit
+
+update:
+	$call	relink
+	$call	install
+	;
+
+relink:
+	$set LIBS="-lxtools"
+	$update	libpkg.a
+	$omake	x_irred.x
+	$link	x_irred.o libpkg.a $(LIBS) -o xx_irred.e
+	;
+
+install:
+	$move	xx_irred.e noaobin$x_irred.e
+	;
+
+libpkg.a:
+	t_irlincor.x	<error.h> <imhdr.h>
+	;
diff --git a/noao/imred/irred/mosproc.cl b/noao/imred/irred/mosproc.cl
new file mode 100644
index 00000000..3fa89405
--- /dev/null
+++ b/noao/imred/irred/mosproc.cl
@@ -0,0 +1,172 @@
+# MOSPROC - Sky subtract, flat field and transpose images before mosaicing.
+
+procedure mosproc (input, output, nxsub, nysub)
+
+string  input           {prompt="Input images"}
+string  output		{prompt="Output image"}
+int     nxsub           {8, prompt="Number of subrasters in x"}
+int     nysub           {8, prompt="Number of subrasters in y"}
+
+bool	skysubtract	{yes, prompt="Sky subtract images before mosaicing"}
+string	sky		{"", prompt="Sky image to subtract"}
+string  exclude         {"", prompt="Input images excluded from sky frame"}
+string	expname		{"EXPTIME", prompt="Image exposure time keywords"} 
+
+bool	flatten		{yes, prompt="Flatten images before mosaicing"}
+string	flat		{"", prompt="Flat field image"}
+bool	transpose	{no,  prompt="Transpose images before mosaicing?"}
+
+string  trim_section    {"[*,*]", prompt="Input image section to be extracted"}
+string	corner          {"lr", prompt="Starting corner for the mosaic"}
+string  direction       {"row", prompt="Starting direction for the mosaic"}
+bool	raster          {no, prompt="Raster scan?"}
+string  median_section  {"", prompt="Input subraster section for median ?"}
+bool    subtract        {no, prompt="Substract median from each subraster?"}
+real	oval		{-1.0, prompt="Mosaic border pixel values"}
+
+bool    delete		{yes, prompt="Delete temporary images?"}
+file    logfile		{"STDOUT", prompt="Log file name"}
+
+struct	*list1, *list2
+ 
+begin
+	file	tmpimg, tmptmp, tmpred, tmpexc
+	int	nx, ny, i, nin, lo, hi
+	string	skyframe, normframe, in, out, img, delim, junk
+
+	tmpimg = mktemp ("MOS")
+	tmptmp = mktemp ("MOS")
+	tmpred = mktemp ("MOS")
+	tmpexc = mktemp ("tmp$MOS")
+
+	# Get positional parameters
+	in  = input
+	out = output
+	nx  = nxsub
+	ny  = nysub
+
+	# Expand input file name list removing the ".imh" extensions.
+	sections (in, option="fullname", > tmptmp)
+	list1 = tmptmp
+	for (nin = 0; fscan (list1, img) != EOF; nin += 1) {
+	    i = strlen (img)
+	    if (substr (img, i-3, i) == ".imh")
+		img = substr (img, 1, i-4)
+	    print (img, >> tmpimg)
+	    print (img // ".red", >> tmpred)
+	}
+	list1 = ""; delete (tmptmp, ver-, >& "dev$null")
+ 
+	# Expand the range of images to skip.
+	if (skysubtract && sky != "") {
+
+	    skyframe = sky
+	    imarith ("@"//tmpimg, "-", skyframe, "@"//tmpred, title="",
+	        divzero=0., hparams="", pixtype="", calctype="", verbose+,
+		noact-, >> logfile)
+
+	} else if (skysubtract) {
+
+	    print (exclude, ",") | translit ("", "^-,0-9", del+) |
+	        translit ("", "-", "!", del-) | tokens (new-) |
+	        translit ("", "\n,", " \n", del-, > tmpexc)
+
+	    type (tmpexc, >> logfile)
+
+	    list1 = tmpexc
+	    while (fscan (list1, lo, delim, hi, junk) != EOF) {
+		if (nscan() == 0)
+		    next
+	        else if (nscan() == 1 && lo >= 1)
+		    print (lo, >> tmptmp)
+	        else if (nscan() == 3) {
+		    lo = min (max (lo, 1), nin); hi = min (max (hi, 1), nin)
+		    for (i = lo; i <= hi; i += 1)
+		        print (i, >> tmptmp)
+	        }
+	    }
+	    list1 = ""; delete (tmpexc, ver-, >& "dev$null")
+
+	    if (access (tmptmp)) {
+	        sort (tmptmp, col=0, ign+, num+, rev-) | unique (> tmpexc)
+	        delete (tmptmp, ver-, >& "dev$null")
+
+	        list1 = tmpimg; list2 = tmpexc; junk = fscan (list2, nin)
+	        for (i = 1; fscan (list1, img) != EOF; i += 1) {
+		    if (i == nin) {
+		        junk = fscan (list2, nin)
+		        next
+		    }
+		    print (img, >> tmptmp)
+	        }
+	        list1 = ""; list2 = ""; delete (tmpexc, ver-, >& "dev$null")
+	    } else
+	        tmptmp = tmpimg
+ 
+	    skyframe = out // ".sky"
+
+	    imcombine ("@"//tmptmp, skyframe, rejmask="", plfile="", sigma="",
+	        logfile=logfile, combine="median", reject="none", project=no,
+		outtype="real", offsets="none", masktype="none", maskvalue=0.0,
+		blank=-1.0, scale="exposure", zero="none", weight="exposure",
+		statsec="", expname=expname, lthreshold=INDEF,
+		hthreshold=INDEF, nlow=1, nhigh=1, nkeep=1, mclip=yes,
+		lsigma=3.0, hsigma=3.0, rdnoise="0.0", gain="1.0", snoise="0.0",
+		sigscale=0.1, pclip=-0.5, grow=0)
+	    print ("\n", >> logfile)
+	    imarith ("@"//tmpimg, "-", skyframe, "@"//tmpred, title="",
+	        divzero=0., hparams="", pixtype="", calctype="", verbose+,
+		noact-, >> logfile)
+
+	} else {
+
+	    skyframe = ""
+	    imcopy ("@"//tmpimg, "@"//tmpred, verbose-)
+	}
+
+	if (flatten) {
+	    if (flat != "") {
+	        print ("\n", >> logfile)
+	        flatten ("@"//tmpred, flat, minflat=INDEF, pixtype="",
+		    keeplog=yes, logfile=logfile)
+	    } else if (skyframe != "")  {
+	        print ("\n", >> logfile)
+		normframe = out // ".norm"
+		imcopy (skyframe, normframe, verbose-)
+		bscale (normframe, normframe, bzero="0.0", bscale="mode",
+		    section="", step=10, lower=INDEF, upper=INDEF,
+		    verbose+, >>logfile)
+	        print ("\n", >> logfile)
+	        flatten ("@"//tmpred, normframe, minflat=INDEF, pixtype="",
+		    keeplog=yes, logfile=logfile)
+	    }
+	}
+
+	if (transpose) {
+	    print ("\nTRANSPOSE: Transpose images", >> logfile)
+	    time (, >> logfile)
+	    imtrans ("@"//tmpred, "@"//tmpred)
+	    time (, >> logfile)
+	    print ("TRANSPOSE: done", >> logfile)
+	}
+
+	print ("\nIRMOSAIC: Mosaic images", >> logfile)
+	time (, >> logfile)
+	irmosaic ("@"//tmpred, out, "db"//out, nx, ny,
+	    trim_section=trim_section, null_input="", corner=corner,
+	    direction=direction, raster=raster, nxover=-1, nyover=-1,
+	    nimcols=INDEF, nimrows=INDEF, oval=oval,
+	    median_section=median_section, sub=subtract, opixtype="r",
+	    verbose+, >> logfile)
+	time (, >> logfile)
+	print ("IRMOSAIC: done", >> logfile)
+ 
+	if (delete) {
+	    if (access (tmpred))
+		imdelete ("@"//tmpred, ver-, >& "dev$null")
+	}
+
+	delete (tmpimg, ver-, >& "dev$null")
+	delete (tmptmp, ver-, >& "dev$null")
+	delete (tmpred, ver-, >& "dev$null")
+end
diff --git a/noao/imred/irred/t_irlincor.x b/noao/imred/irred/t_irlincor.x
new file mode 100644
index 00000000..053c383d
--- /dev/null
+++ b/noao/imred/irred/t_irlincor.x
@@ -0,0 +1,254 @@
+include <imhdr.h>
+include	<error.h>
+
+# Maximum number of correction function coefficients.
+define	MAXCOEF	3
+
+# Maximum number of ADU....
+define	MAXADU	32767.0
+
+
+# T_ARLINCOR -- Corrects IR imager frames for non linearity. This task
+# only corrects a section of the total image and copies the rest of
+# the image intact to the output image.
+
+procedure t_irlincor ()
+
+pointer	inlist, outlist		# input and output image lists
+char	section[SZ_LINE]	# image section
+pointer	coeff			# coeficients of correction function
+
+bool	sflag
+pointer	imin, imout
+pointer	input, output, orig, temp
+pointer	sp
+
+int	strlen()
+int	imtgetim(), imtlen()
+real	clgetr()
+pointer	immap(), imtopenp()
+
+begin
+	# Get parameters
+	inlist  = imtopenp ("input")
+	outlist = imtopenp ("output")
+	call clgstr ("section", section, SZ_LINE)
+
+	# Check that the input and output image lists have the
+	# same number of images. Abort if that's not the case.
+	if (imtlen (inlist) != imtlen (outlist)) {
+	    call imtclose (inlist)
+	    call imtclose (outlist)
+	    call error (1, "Input and output image lists don't match")
+	}
+
+	# Set section flag
+	sflag = (strlen (section) > 0)
+
+	# Allocate string space
+	call smark  (sp)
+	call salloc (input,  SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (orig,   SZ_FNAME, TY_CHAR)
+	call salloc (temp,   SZ_FNAME, TY_CHAR)
+
+	# Allocate memory for the correction coefficients and
+	# read them from the parameter file.
+	call malloc (coeff, MAXCOEF, TY_REAL)
+	Memr[coeff]   = clgetr ("coeff1")
+	Memr[coeff+1] = clgetr ("coeff2")
+	Memr[coeff+2] = clgetr ("coeff3")
+
+	# Loop over all images in the input and output lists
+	while ((imtgetim (inlist, Memc[input], SZ_FNAME) != EOF) &&
+	       (imtgetim (outlist, Memc[output], SZ_FNAME) != EOF)) {
+
+	    # Generate temporary output image name to allow for
+	    # input and output images having the same name
+	    call xt_mkimtemp (Memc[input], Memc[output], Memc[orig], SZ_FNAME)
+
+	    # Take different actions depending on whether the image section
+	    # is specified or not, in order to optimize speed. When the image
+	    # section is specified the input image is copied to the output
+	    # image and then the output image opened to work on the section.
+	    # Otherwise the output image is created only once.
+	    if (sflag) {
+
+	        # Copy input image into output image using fast copy
+		iferr (call irl_imcopy (Memc[input], Memc[output])) {
+		    call erract (EA_WARN)
+		    next
+		}
+
+		# Append section to image names. The output name should
+		# be preserved without the section for later use.
+		call strcat (section, Memc[input], SZ_FNAME)
+		call sprintf (Memc[temp], SZ_FNAME, "%s%s")
+		    call pargstr (Memc[output])
+		    call pargstr (section)
+
+		# Open input and output images. The output image already
+		# exists, since it was created by the copy operation, so
+		# it is opened as read/write.
+		iferr (imin = immap (Memc[input], READ_ONLY, 0)) {
+		    call erract (EA_WARN)
+		    next
+		}
+		iferr (imout = immap (Memc[temp], READ_WRITE, 0)) {
+		    call imunmap (imin)
+		    call erract (EA_WARN)
+		    next
+		}
+
+	    } else {
+
+		# Open input and output images. The output image does not
+		# exist already so it is opened as a new copy of the input
+		# image.
+		iferr (imin = immap (Memc[input], READ_ONLY, 0)) {
+		    call erract (EA_WARN)
+		    next
+		}
+		iferr (imout = immap (Memc[output], NEW_COPY, imin)) {
+		    call imunmap (imin)
+		    call erract (EA_WARN)
+		    next
+		}
+
+	    }
+
+	    # Perform the linear correction.
+	    call irl_correct (imin, imout, Memr[coeff], MAXCOEF)
+
+	    # Close images
+	    call imunmap (imin)
+	    call imunmap (imout)
+
+	    # Replace output image with the temporary image. This is a
+	    # noop if the input and output images have different names
+	    call xt_delimtemp (Memc[output], Memc[orig])
+	}
+
+	# Free memory and close image lists
+	call mfree (coeff, TY_REAL)
+	call imtclose (inlist)
+	call imtclose (outlist)
+end
+
+
+# IRL_CORRECT -- Corrects an IR imager frame for non-linearity using a
+# simple power series polynomial correction function:
+#
+# ADU' = ADU * [ a + b * (ADU / MAXADU) + c * (ADU / MAXADU) **2 ]
+#
+
+procedure irl_correct (imin, imout, coeff, ncoef)
+
+pointer	imin				# input image pointer
+pointer	imout				# output image pointer
+real	coeff[ncoef]			# coefficients of polynomial function
+int	ncoef				# number of polynomial coeficients
+
+int	col, ncols
+long	v1[IM_MAXDIM], v2[IM_MAXDIM]
+pointer	inbuf, outbuf
+
+int	imgeti()
+int	imgnlr(), impnlr()
+real	apolr()
+
+begin
+	# Initiliaze counters for line i/o
+	call amovkl (long(1), v1, IM_MAXDIM)
+	call amovkl (long(1), v2, IM_MAXDIM)
+
+	# Number of pixels per line
+	ncols = imgeti (imin, "i_naxis1")
+
+	# Loop over image lines
+	while ((imgnlr (imin, inbuf, v1) != EOF) &&
+	       (impnlr (imout, outbuf, v2) != EOF)) {
+	    call adivkr (Memr[inbuf], MAXADU, Memr[outbuf], ncols)
+	    do col = 1, ncols {
+		Memr[outbuf+col-1] = apolr (Memr[outbuf+col-1], coeff, ncoef)
+	    }
+	    call amulr (Memr[inbuf], Memr[outbuf], Memr[outbuf], ncols)
+	}
+end
+
+
+# IRL_IMCOPY -- Copy input image into the output image. Avoid data type
+# conversion in order to opetimize speed.
+
+procedure irl_imcopy (input, output)
+
+char	input[ARB]		# input image name
+char	output[ARB]		# output image name
+
+int	npix
+long	vin[IM_MAXDIM], vout[IM_MAXDIM]
+pointer	imin, imout
+pointer	inline, outline
+
+int	imgeti()
+int	imgnls(), impnls()
+int	imgnli(), impnli()
+int	imgnll(), impnll()
+int	imgnlr(), impnlr()
+int	imgnld(), impnld()
+int	imgnlx(), impnlx()
+pointer	immap()
+
+begin
+	# Open input and output images
+	iferr (imin = immap (input, READ_ONLY, 0))
+	    call erract (EA_ERROR)
+	iferr (imout = immap (output, NEW_COPY, imin)) {
+	    call imunmap (imin)
+	    call erract (EA_ERROR)
+	}
+
+	# Initiliaze counters
+	call amovkl (long(1), vin,  IM_MAXDIM)
+	call amovkl (long(1), vout, IM_MAXDIM)
+
+	# Copy image lines
+	switch (imgeti (imin, "i_pixtype")) {
+	case TY_SHORT, TY_USHORT:
+	    while (imgnls (imin, inline, vin) != EOF) {
+		npix = impnls (imout, outline, vout)
+		call amovs (Mems[inline], Mems[outline], npix)
+	    }
+	case TY_INT:
+	    while (imgnli (imin, inline, vin) != EOF) {
+		npix = impnli (imout, outline, vout)
+		call amovi (Memi[inline], Memi[outline], npix)
+	    }
+	case TY_LONG:
+	    while (imgnll (imin, inline, vin) != EOF) {
+		npix = impnll (imout, outline, vout)
+		call amovl (Meml[inline], Meml[outline], npix)
+	    }
+	case TY_REAL:
+	    while (imgnlr (imin, inline, vin) != EOF) {
+		npix = impnlr (imout, outline, vout)
+		call amovr (Memr[inline], Memr[outline], npix)
+	    }
+	case TY_DOUBLE:
+	    while (imgnld (imin, inline, vin) != EOF) {
+		npix = impnld (imout, outline, vout)
+		call amovd (Memd[inline], Memd[outline], npix)
+	    }
+	case TY_COMPLEX:
+	    while (imgnlx (imin, inline, vin) != EOF) {
+		npix = impnlx (imout, outline, vout)
+		call amovx (Memx[inline], Memx[outline], npix)
+	    }
+	default:
+	    call error (0, "Unsupported pixel type")
+	}
+
+	# Close images
+	call imunmap (imin)
+	call imunmap (imout)
+end
diff --git a/noao/imred/irred/txdump.par b/noao/imred/irred/txdump.par
new file mode 100644
index 00000000..ce400817
--- /dev/null
+++ b/noao/imred/irred/txdump.par
@@ -0,0 +1,8 @@
+# TXDUMP Parameters
+
+textfiles,s,a,,,,Input apphot/daophot text database(s)
+fields,s,a,,,,Fields to be extracted
+expr,s,a,yes,,,Boolean expression for record selection
+headers,b,h,no,,,Print the field headers ?
+parameters,b,h,yes,,,Print the parameters if headers is yes ?
+mode,s,h,"ql",,,Mode of task
diff --git a/noao/imred/irred/x_irred.x b/noao/imred/irred/x_irred.x
new file mode 100644
index 00000000..25e406aa
--- /dev/null
+++ b/noao/imred/irred/x_irred.x
@@ -0,0 +1 @@
+task	irlincor	= t_irlincor
diff --git a/noao/imred/irs/Revisions b/noao/imred/irs/Revisions
new file mode 100644
index 00000000..ac156735
--- /dev/null
+++ b/noao/imred/irs/Revisions
@@ -0,0 +1,111 @@
+.help revisions Jun88 noao.imred.irs
+.nf
+
+=====
+V2.12
+=====
+
+imred$irs/standard.par
+    Added blackbody query parameters.  (5/2/02, Valdes)
+
+========
+V2.11.3b
+========
+
+imred$irs/identify.par
+    Added new units parameters.  (3/11/97, Valdes)
+
+=========
+V2.10.4p2
+=========
+
+imred$irs/
+   Updated to new version of ONEDSPEC (7/11/91, Valdes)
+
+================
+
+imred$irs/standard.par
+   Removed ennumerated list.  (4/10/89, Valdes)
+
+imred$irs/irs.cl
+imred$irs/irs.men
+specplot.par+
+	Task SPECPLOT added.  (4/3/89 ShJ)
+
+imred$irs/batchred.cl
+imred$irs/batchred.par
+imred$irs/irs.cl
+imred$irs/irs.men
+   1. New BATCHRED script. (4/27/88 Valdes)
+   2. Eliminated EXTINCT. (4/27/88 Valdes)
+
+imred$irs/sensfunc.par
+    Added aperture selection and query parameters.  (4/15/88 Valdes)
+
+imred$irs/irs.cl
+imred$irs/refspectra.par +
+    Refer to new ONEDSPEC executable and tasks.  (4/7/88 Valdes)
+
+noao$imred/irs/reidentify.par
+    Valdes, Jan 4, 1988
+    Updated parameter file for new REIDENTIFY parameter.
+
+noao$imred/irs/dispcor.par
+    Valdes, March 5, 1987
+    1.  The DISPCOR default parameter file has been updated because of
+	changes to the task; most notable being that wstart and wpc are
+	list structured.
+
+noao$imred/irs/flatdiv.par
+noao$imred/irs/flatfit.par
+    Valdes, December, 2, 1986
+    1.  New parameter "power" added to these tasks.
+
+noao$imred/irs/coincor.par
+    Valdes, October 20, 1986
+    1.  New parameter "checkdone" added to COINCOR to allow overriding
+	coincidence correction checking.
+
+noao$imred/irs/irs.par
+noao$imred/irs/coincor.par
+noao$imred/irs/irs.men
+    Valdes, October 13, 1986
+    1.  Added new COINCOR parameter "power".
+
+noao$imred/irs/irs.cl
+noao$imred/irs/irs.men
+noao$imred/irs/shedit.par +
+    Valdes, October 6, 1986
+    1.  Added new task SHEDIT.
+
+noao$imred/irs/identify.par
+    Valdes, October 3, 1986
+    1.  Added new IDENTIFY parameter "threshold".
+
+irs:  Valdes, July 3, 1986:
+    1.  New coordlist name in IDENTIFY parameter file.
+    2.  New calibration file name in package parameter file.
+
+=====================================
+STScI Pre-release and SUN 2.3 Release
+=====================================
+
+irs$bswitch.par:  Valdes, May 19, 1986
+    1.  The parameter "add_const" in BSWITCH is directed to the parameter
+	in SENSFUNC of the same name.
+
+irs:  Valdes, May 12, 1986:
+    1.  SPLOT updated.  New parameters XMIN, XMAX, YMIN, YMAX.
+
+irs:  Valdes, April 7, 1986:
+    1.  Package parameter file changed to delete latitude.
+    2.  DISPCOR, BSWITCH, and STANDARD latitude parameter now obtained from
+	OBSERVATORY.
+
+irs:  Valdes, March 27, 1986:
+    1.  New task SETDISP added.
+
+===========
+Release 2.2
+===========
+.endhelp
diff --git a/noao/imred/irs/calibrate.par b/noao/imred/irs/calibrate.par
new file mode 100644
index 00000000..795965b7
--- /dev/null
+++ b/noao/imred/irs/calibrate.par
@@ -0,0 +1,14 @@
+# CALIBRATE parameter file
+
+input,s,a,,,,Input spectra to calibrate
+output,s,a,,,,Output calibrated spectra
+records,s,a,,,,Record number extensions
+extinct,b,h,yes,,,Apply extinction correction?
+flux,b,h,yes,,,Apply flux calibration?
+extinction,s,h,)_.extinction,,,Extinction file
+observatory,s,h,)_.observatory,,,Observatory of observation
+ignoreaps,b,h,no,,,Ignore aperture numbers in flux calibration?
+sensitivity,s,h,"sens",,,Image root name for sensitivity spectra
+fnu,b,h,no,,,Create spectra having units of FNU?
+airmass,r,q,,1.,,Airmass
+exptime,r,q,,,,Exposure time (seconds)
diff --git a/noao/imred/irs/dispcor.par b/noao/imred/irs/dispcor.par
new file mode 100644
index 00000000..90257214
--- /dev/null
+++ b/noao/imred/irs/dispcor.par
@@ -0,0 +1,19 @@
+input,s,a,,,,List of input spectra
+output,s,a,,,,List of output spectra
+records,s,a,,,,Record number extensions
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+database,s,h,"database",,,Dispersion solution database
+table,s,h,"",,,Wavelength table for apertures
+w1,r,h,INDEF,,,Starting wavelength
+w2,r,h,INDEF,,,Ending wavelength
+dw,r,h,INDEF,,,Wavelength interval per pixel
+nw,i,h,1024,,,Number of output pixels
+log,b,h,no,,,Logarithmic wavelength scale?
+flux,b,h,yes,,,Conserve total flux?
+samedisp,b,h,yes,,,Same dispersion in all apertures?
+global,b,h,yes,,,Apply global defaults?
+ignoreaps,b,h,no,,,Ignore apertures?
+confirm,b,h,yes,,,Confirm dispersion coordinates?
+listonly,b,h,no,,,List the dispersion coordinates only?
+verbose,b,h,yes,,,Print linear dispersion assignments?
+logfile,s,h,"logfile",,,Log file
diff --git a/noao/imred/irs/flatfit.par b/noao/imred/irs/flatfit.par
new file mode 100644
index 00000000..bd693aed
--- /dev/null
+++ b/noao/imred/irs/flatfit.par
@@ -0,0 +1,24 @@
+# FLATFIT parameter file
+
+input,s,a,,,,Input image root file name
+records,s,a,,,,Range of spectral records
+output,s,a,,,,Output file root name for new spectra
+function,s,h,"chebyshev",,,Function to fit (chebyshev|legendre|spline3|spline1)
+order,i,h,1,1,,Fitting order (number of terms)
+niter,i,h,1,1,,Number of rejection iterations
+lower,r,h,100.,0,,Lower rejection criterion in sigmas
+upper,r,h,100.,0,,Upper rejection criterion in sigmas
+ngrow,i,h,0,,,Growing region
+div_min,r,h,1.0,,,Value to use if division by zero occurs
+interact,b,h,yes,,,Interact with the first accumulation?
+all_interact,b,h,no,,,Interact with all accumulations?
+coincor,b,h,)_.coincor,,,Apply coincidence correction to flats
+ccmode,s,h,)_.ccmode,,,Correction mode (photo|iids)
+deadtime,r,h,)_.deadtime,,,Deadtime in seconds
+power,r,h,)_.power,,,IIDS power law coefficient
+new_order,i,a,4,1,,enter order
+new_lower,r,a,,,,enter nr sigma
+new_upper,r,a,,,,enter nr sigma
+new_niter,i,a,,,,enter nr of iterations
+confirm,b,a,,,,Exit and save solution?
+cursor,*gcur,h,"",,,Graphics cursor input
diff --git a/noao/imred/irs/identify.par b/noao/imred/irs/identify.par
new file mode 100644
index 00000000..d42065e1
--- /dev/null
+++ b/noao/imred/irs/identify.par
@@ -0,0 +1,33 @@
+# Parameters for identify task.
+
+images,s,a,,,,Images containing features to be identified
+section,s,h,"middle line",,,Section to apply to two dimensional images
+database,f,h,database,,,Database in which to record feature data
+coordlist,f,h,linelists$henear.dat,,,User coordinate list
+units,s,h,"",,,Coordinate units
+nsum,s,h,"10",,,Number of lines/columns/bands to sum in 2D images
+match,r,h,50.,,,Coordinate list matching limit
+maxfeatures,i,h,50,,,Maximum number of features for automatic identification
+zwidth,r,h,100.,,,Zoom graph width in user units
+
+ftype,s,h,"emission","emission|absorption",,Feature type
+fwidth,r,h,4.,,,Feature width in pixels
+cradius,r,h,5.,,,Centering radius in pixels
+threshold,r,h,10.,0.,,Feature threshold for centering
+minsep,r,h,2.,0.,,Minimum pixel separation
+
+function,s,h,"chebyshev","legendre|chebyshev|spline1|spline3",,Coordinate function
+order,i,h,8,1,,Order of coordinate function
+sample,s,h,"*",,,Coordinate sample regions
+niterate,i,h,0,0,,Rejection iterations
+low_reject,r,h,3.,0.,,Lower rejection sigma
+high_reject,r,h,3.,0.,,Upper rejection sigma
+grow,r,h,0.,0.,,Rejection growing radius
+
+autowrite,b,h,no,,,"Automatically write to database"
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+
+crval,s,q,,,,"Approximate coordinate (at reference pixel)"
+cdelt,s,q,,,,"Approximate dispersion"
+aidpars,pset,h,,,,"Automatic identification algorithm parameters"
diff --git a/noao/imred/irs/irs.cl b/noao/imred/irs/irs.cl
new file mode 100644
index 00000000..6814185f
--- /dev/null
+++ b/noao/imred/irs/irs.cl
@@ -0,0 +1,64 @@
+#{ IRS -- KPNO IRS Spectral Reduction Package
+
+# Load necessary packages
+
+lists		# List package for table
+
+# Define necessary paths
+
+set	irscal		= "onedstds$irscal/"
+set	irsiids		= "onedspec$irsiids/"
+
+package irs
+
+# Standard ONEDSPEC tasks
+task	autoidentify,
+	continuum,
+	deredden,
+	dopcor,
+	mkspec,
+	names,
+	sarith,
+	sflip,
+	sinterp,
+	splot,
+	specplot,
+	specshift	= onedspec$x_onedspec.e
+task	scombine	= "onedspec$scombine/x_scombine.e"
+task	aidpars		= "onedspec$aidpars.par"
+task	dispcor1	= onedspec$dispcor1.par
+task	scopy		= onedspec$scopy.cl
+hidetask dispcor1
+
+# Special  IRS/IIDS tasks
+task	addsets,
+	bswitch,
+	coefs,
+	flatdiv,
+	slist1d,
+	subsets,
+	sums		= irsiids$x_onedspec.e
+task	batchred	= irsiids$batchred.cl
+task	bplot		= irsiids$bplot.cl
+task	extinct		= irsiids$extinct.cl
+
+# Different default parameters
+task	calibrate,
+	dispcor,
+	flatfit,
+	identify,
+	lcalib,
+	reidentify,
+	refspectra,
+	sensfunc,
+	standard	= irs$x_onedspec.e
+
+# Astutil tasks
+task	setairmass,
+	setjd		= "astutil$x_astutil.e"
+
+# Define a task living in the users directory - it is created by BATCHRED
+
+task	$process	= process.cl
+
+clbye()
diff --git a/noao/imred/irs/irs.hd b/noao/imred/irs/irs.hd
new file mode 100644
index 00000000..e5125e4f
--- /dev/null
+++ b/noao/imred/irs/irs.hd
@@ -0,0 +1 @@
+# Help directory for the KPNOSLIT package.
diff --git a/noao/imred/irs/irs.men b/noao/imred/irs/irs.men
new file mode 100644
index 00000000..60e4a37d
--- /dev/null
+++ b/noao/imred/irs/irs.men
@@ -0,0 +1,35 @@
+	addsets - Add subsets of strings of spectra
+       batchred - Batch processing of IIDS/IRS spectra
+          bplot - Batch plots of spectra
+	bswitch - Beam-switch strings of spectra to make obj-sky pairs
+      calibrate - Apply sensitivity correction to spectra
+          coefs - Extract mtn reduced coefficients from henear scans
+      continuum - Fit the continuum in spectra
+       deredden - Apply interstellar extinction corrections
+	dispcor - Dispersion correct spectra
+	 dopcor - Doppler correct spectra
+	extinct - Use BSWITCH for extinction correction
+	flatdiv - Divide spectra by flat field
+	flatfit - Sum and normalize flat field spectra
+       identify - Identify features in spectrum for dispersion solution
+         lcalib - List calibration file data
+         mkspec - Generate an artificial spectrum
+          names - Generate a list of image names from a string
+	process - A task generated by BATCHRED
+     refspectra - Assign reference spectra to object spectra
+     reidentify - Automatically identify features in spectra
+         sarith - Spectrum arithmetic
+       scombine - Combine spectra having different wavelength ranges
+          scopy - Select and copy apertures in different spectral formats
+       sensfunc - Create sensitivity function
+     setairmass - Compute effective airmass and middle UT for an exposure
+          setjd - Compute and set Julian dates in images
+	  sflip - Flip data and/or dispersion coordinates in spectra
+        sinterp - Interpolate a table of x,y pairs to create a spectrum
+	slist1d - List spectral header elements
+       specplot - Stack and plot multiple spectra
+      specshift - Shift spectral dispersion coordinate systems
+	  splot - Preliminary spectral plot/analysis
+       standard - Identify standard stars to be used in sensitivity calc
+	subsets - Subtract pairs in strings of spectra
+           sums - Generate sums of object and sky spectra by aperture
diff --git a/noao/imred/irs/irs.par b/noao/imred/irs/irs.par
new file mode 100644
index 00000000..1a59fd5e
--- /dev/null
+++ b/noao/imred/irs/irs.par
@@ -0,0 +1,17 @@
+# PARAMETERS FOR KPNO IRS SPECTRAL REDUCTION PACKAGE
+
+observatory,s,h,"kpno",,,Observatory for data
+interp,s,h,"poly5","nearest|linear|poly3|poly5|spline3|sinc",,Interpolation type
+extinction,s,h,"onedstds$kpnoextinct.dat",,,Extinction file
+caldir,s,h,"irscal$",,,Directory containing calibration data
+coincor,b,h,no,,,Apply coincidence correction to flats
+ccmode,s,h,"",,,Correction mode (photo|iids|power)
+deadtime,r,h,,0,,Deadtime in seconds
+power,r,h,,,,IIDS power law coefficient
+
+dispaxis,i,h,1,1,3,Image axis for 2D/3D images
+nsum,s,h,"1",,,Number of lines/columns/bands to sum for 2D/3D images
+
+next_rec,i,h,1,,,"Next output record"
+
+version,s,h,"IRS V3: July 1991"
diff --git a/noao/imred/irs/lcalib.par b/noao/imred/irs/lcalib.par
new file mode 100644
index 00000000..30436625
--- /dev/null
+++ b/noao/imred/irs/lcalib.par
@@ -0,0 +1,7 @@
+# CALIBLIST parameter file
+
+option,s,a,,,,"List option (bands, ext, mags, fnu, flam, stars)"
+star_name,s,a,,,,Star name in calibration list
+extinction,s,h,,,,Extinction file
+caldir,s,h,)_.caldir,,,Directory containing calibration data
+fnuzero,r,h,3.68e-20,,,Absolute flux zero point
diff --git a/noao/imred/irs/refspectra.par b/noao/imred/irs/refspectra.par
new file mode 100644
index 00000000..47cd54f9
--- /dev/null
+++ b/noao/imred/irs/refspectra.par
@@ -0,0 +1,17 @@
+input,s,a,,,,"List of input spectra"
+records,s,a,,,,Record number extensions
+references,s,h,"*.imh",,,"List of reference spectra"
+apertures,s,h,"",,,"Input aperture selection list"
+refaps,s,h,"",,,"Reference aperture selection list"
+ignoreaps,b,h,no,,,Ignore input and reference apertures?
+select,s,h,"interp","match|nearest|preceding|following|interp|average",,"Selection method for reference spectra"
+sort,s,h,"ut",,,"Sort key"
+group,s,h,"none",,,"Group key"
+time,b,h,yes,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting"
+override,b,h,no,,,"Override previous assignments?"
+confirm,b,h,yes,,,"Confirm reference spectrum assignments?"
+assign,b,h,yes,,,"Assign the reference spectra to the input spectrum?"
+logfiles,s,h,"STDOUT,logfile",,,"List of logfiles"
+verbose,b,h,no,,,"Verbose log output?"
+answer,s,q,,"no|yes|YES",,"Accept assignment?"
diff --git a/noao/imred/irs/reidentify.par b/noao/imred/irs/reidentify.par
new file mode 100644
index 00000000..13b21740
--- /dev/null
+++ b/noao/imred/irs/reidentify.par
@@ -0,0 +1,36 @@
+# Parameters for reidentify task.
+
+reference,s,a,,,,Reference image
+images,s,a,,,,Images to be reidentified
+interactive,s,h,"no","no|yes|NO|YES",,Interactive fitting?
+section,s,h,"middle line",,,Section to apply to two dimensional images
+newaps,b,h,yes,,,Reidentify apertures in images not in reference?
+override,b,h,no,,,Override previous solutions?
+refit,b,h,yes,,,"Refit coordinate function?
+"
+trace,b,h,no,,,Trace reference image?
+step,s,h,"10",,,Step in lines/columns/bands for tracing an image
+nsum,s,h,"10",,,Number of lines/columns/bands to sum
+shift,s,h,"0.",,,Shift to add to reference features (INDEF to search)
+search,r,h,0.,,,Search radius
+nlost,i,h,0,0,,"Maximum number of features which may be lost
+"
+cradius,r,h,5.,,,Centering radius
+threshold,r,h,10.,0.,,Feature threshold for centering
+addfeatures,b,h,no,,,Add features from a line list?
+coordlist,f,h,linelists$henear.dat,,,User coordinate list
+match,r,h,10.,,,Coordinate list matching limit
+maxfeatures,i,h,50,,,Maximum number of features for automatic identification
+minsep,r,h,2.,0.,,"Minimum pixel separation
+"
+database,f,h,database,,,Database
+logfiles,s,h,"logfile",,,List of log files
+plotfile,s,h,"",,,Plot file for residuals
+verbose,b,h,no,,,Verbose output?
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,"Graphics cursor input
+"
+answer,s,q,"yes","no|yes|NO|YES",,Fit dispersion function interactively?
+crval,s,q,,,,"Approximate coordinate (at reference pixel)"
+cdelt,s,q,,,,"Approximate dispersion"
+aidpars,pset,h,,,,"Automatic identification algorithm parameters"
diff --git a/noao/imred/irs/sensfunc.par b/noao/imred/irs/sensfunc.par
new file mode 100644
index 00000000..022190a4
--- /dev/null
+++ b/noao/imred/irs/sensfunc.par
@@ -0,0 +1,17 @@
+standards,s,a,std,,,Input standard star data file (from STANDARD)
+sensitivity,s,a,"sens",,,Output root sensitivity function imagename
+apertures,s,h,"",,,Aperture selection list
+ignoreaps,b,h,no,,,Ignore apertures and make one sensitivity function?
+logfile,f,h,"logfile",,,Output log for statistics information
+extinction,f,h,")_.extinction",,,Extinction file
+newextinction,f,h,"extinct.dat",,,Output revised extinction file
+observatory,s,h,)_.observatory,,,Observatory of data
+function,s,h,"spline3","chebyshev|legendre|spline3|spline1",,Fitting function
+order,i,h,6,1,,Order of fit
+interactive,b,h,yes,,,Determine sensitivity function interactively?
+graphs,s,h,"sr",,,Graphs per frame
+marks,s,h,"plus cross box",,,Data mark types (marks deleted added)
+colors,s,h,"2 1 3 4",,,Colors (lines marks deleted added)
+cursor,*gcur,h,"",,,Graphics cursor input
+device,s,h,"stdgraph",,,Graphics output device
+answer,s,q, yes,"no|yes|NO|YES",,"(no|yes|NO|YES)"
diff --git a/noao/imred/irs/standard.par b/noao/imred/irs/standard.par
new file mode 100644
index 00000000..3abf645a
--- /dev/null
+++ b/noao/imred/irs/standard.par
@@ -0,0 +1,22 @@
+input,f,a,,,,Input image file root name
+records,s,a,,,,Spectral records
+output,s,a,std,,,Output flux file (used by SENSFUNC)
+samestar,b,h,yes,,,Same star in all apertures?
+beam_switch,b,h,yes,,,Beam switch spectra?
+apertures,s,h,"",,,Aperture selection list
+bandwidth,r,h,INDEF,,,Bandpass widths
+bandsep,r,h,INDEF,,,Bandpass separation
+fnuzero,r,h,3.68e-20,,,Absolute flux zero point
+extinction,s,h,)_.extinction,,,Extinction file
+caldir,s,h,)_.caldir,,,Directory containing calibration data
+observatory,s,h,)_.observatory,,,Observatory for data
+interact,b,h,yes,,,Graphic interaction to define new bandpasses
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+star_name,s,q,,,,Star name in calibration list
+airmass,r,q,,1.,,Airmass
+exptime,r,q,,,,Exposure time (seconds)
+mag,r,q,,,,Magnitude of star
+magband,s,q,,"U|B|V|R|I|J|H|K|L|Lprime|M",,"Magnitude type"
+teff,s,q,,,,Effective temperature or spectral type
+answer,s,q,no,,,"(no|yes|NO|YES|NO!|YES!)"
diff --git a/noao/imred/kpnocoude/Revisions b/noao/imred/kpnocoude/Revisions
new file mode 100644
index 00000000..da682fb8
--- /dev/null
+++ b/noao/imred/kpnocoude/Revisions
@@ -0,0 +1,59 @@
+.help revisions Dec94 noao.imred.kpnocoude
+.nf
+
+=====
+V2.12
+=====
+
+imred$kpnocoude/standard.par
+    Added blackbody query parameters.  (5/2/02, Valdes)
+
+========
+V2.11.3b
+========
+
+iimred$kpnocoude/doc/do3fiber.hlp
+    Fixed minor formating problem.  (4/22/99, Valdes)
+
+=======
+V2.11.1
+=======
+
+imred$kpnocoude/demos/mkdo3fiber.cl
+imred$kpnocoude/demos/mkdoslit.cl
+    Made the ARTDATA package parameters explicit (4/15/97, Valdes)
+
+imred$kpnocoude/identify.par
+    Added the new units parameter. (3/11/97, Valdes)
+
+imred$kpnocoude/kpnocoude.cl
+    Increased the minimum min_lenuserarea from 40000 to 100000.
+    (7/31/96, Valdes)
+
+imred$kpnocoude/sparams.par
+    Changed match from 0.2 to -3.  (4/5/96, Valdes)
+
+imred$kpnocoude/do3fiber.cl
+imred$kpnocoude/do3fiber.par
+imred$kpnocoude/params.par
+imred$kpnocoude/doc/do3fiber.hlp
+imred$kpnocoude/doc/do3fiber.ms
+    Added crval/cdelt parameters used in new version with automatic arc
+    line identification.  (4/5/96, Valdes)
+
+imred$kpnocoude/do3fiber.cl
+    The script needed to be modifed for the extra argument to proc for
+    sky alignment.  The sky alignment option is not used in DO3FIBER.
+    (7/19/95, Valdes)
+
+=======
+V2.10.4
+=======
+
+kpnocoude$kpnocoude.cl
+kpnocoude$kpnocoude.men
+    1. Added background, illumination, response, apflatten, apnormalize.
+    2. Renamed fiber response task to "fibresponse".
+    (12/29/94, Valdes)
+
+.endhelp
diff --git a/noao/imred/kpnocoude/calibrate.par b/noao/imred/kpnocoude/calibrate.par
new file mode 100644
index 00000000..e09457a2
--- /dev/null
+++ b/noao/imred/kpnocoude/calibrate.par
@@ -0,0 +1,13 @@
+# CALIBRATE parameter file
+
+input,s,a,,,,Input spectra to calibrate
+output,s,a,,,,Output calibrated spectra
+extinct,b,h,yes,,,Apply extinction correction?
+flux,b,h,yes,,,Apply flux calibration?
+extinction,s,h,)_.extinction,,,Extinction file
+observatory,s,h,)_.observatory,,,Observatory of observation
+ignoreaps,b,h,yes,,,Ignore aperture numbers in flux calibration?
+sensitivity,s,h,"sens",,,Image root name for sensitivity spectra
+fnu,b,h,no,,,Create spectra having units of FNU?
+airmass,r,q,,1.,,Airmass
+exptime,r,q,,,,Exposure time (seconds)
diff --git a/noao/imred/kpnocoude/demos/demoarc1.dat b/noao/imred/kpnocoude/demos/demoarc1.dat
new file mode 100644
index 00000000..fa0a179d
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/demoarc1.dat
@@ -0,0 +1,38 @@
+    OBJECT  = 'First comp        '  /  object name
+    OBSERVAT= 'KPNO              '  /  observatory
+    OBSERVER= 'Massey            '  /  observers
+    COMMENTS= 'Final New Ice     '  /  comments
+    EXPTIME =                  60.  /  actual integration time
+    DARKTIME=                  60.  /  total elapsed time
+    IMAGETYP= 'comp              '  /  object, dark, bias, etc.
+    DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+    UT      = '12:11:30.00       '  /  universal time
+    ST      = '09:04:54.00       '  /  sidereal time
+    RA      = '06:37:02.00       '  /  right ascension
+    DEC     = '06:09:03.00       '  /  declination
+    EPOCH   =               1991.9  /  epoch of ra and dec
+    ZD      = '48.760            '  /  zenith distance
+    AIRMASS =                   0.  /  airmass
+    TELESCOP= 'kpcdf             '  /  telescope name
+    DETECTOR= 'te1k              '  /  detector
+    PREFLASH=                    0  /  preflash time, seconds
+    GAIN    =                  5.4  /  gain, electrons per adu
+    DWELL   =                    5  /  sample integration time
+    RDNOISE =                  3.5  /  read noise, electrons per adu
+    DELAY0  =                    0  /  time delay after each pixel
+    DELAY1  =                    0  /  time delay after each row
+    CAMTEMP =                 -111  /  camera temperature
+    DEWTEMP =                 -183  /  dewar temperature
+    CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+    ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+    CCDSUM  = '1 1               '  /  on chip summation
+    INSTRUME= 'test              '  /  instrument
+    APERTURE= '250micron slit    '  /  aperture
+    TVFILT  = '4-96              '  /  tv filter
+    DISPAXIS= '2                 '  /  dispersion axis
+    GRATPOS =               4624.3  /  grating position
+    TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+    OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+    ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+    CCDMEAN =              179.398
+    CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/kpnocoude/demos/demoarc2.dat b/noao/imred/kpnocoude/demos/demoarc2.dat
new file mode 100644
index 00000000..4cd9975d
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/demoarc2.dat
@@ -0,0 +1,38 @@
+    OBJECT  = 'Last comp         '  /  object name
+    OBSERVAT= 'KPNO              '  /  observatory
+    OBSERVER= 'Massey            '  /  observers
+    COMMENTS= 'Final New Ice     '  /  comments
+    EXPTIME =                  60.  /  actual integration time
+    DARKTIME=                  60.  /  total elapsed time
+    IMAGETYP= 'comp              '  /  object, dark, bias, etc.
+    DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+    UT      = '12:41:30.00       '  /  universal time
+    ST      = '09:34:54.00       '  /  sidereal time
+    RA      = '06:37:02.00       '  /  right ascension
+    DEC     = '06:09:03.00       '  /  declination
+    EPOCH   =               1991.9  /  epoch of ra and dec
+    ZD      = '48.760            '  /  zenith distance
+    AIRMASS =                   0.  /  airmass
+    TELESCOP= 'kpcdf             '  /  telescope name
+    DETECTOR= 'te1k              '  /  detector
+    PREFLASH=                    0  /  preflash time, seconds
+    GAIN    =                  5.4  /  gain, electrons per adu
+    DWELL   =                    5  /  sample integration time
+    RDNOISE =                  3.5  /  read noise, electrons per adu
+    DELAY0  =                    0  /  time delay after each pixel
+    DELAY1  =                    0  /  time delay after each row
+    CAMTEMP =                 -111  /  camera temperature
+    DEWTEMP =                 -183  /  dewar temperature
+    CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+    ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+    CCDSUM  = '1 1               '  /  on chip summation
+    INSTRUME= 'test              '  /  instrument
+    APERTURE= '250micron slit    '  /  aperture
+    TVFILT  = '4-96              '  /  tv filter
+    DISPAXIS= '2                 '  /  dispersion axis
+    GRATPOS =               4624.3  /  grating position
+    TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+    OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+    ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+    CCDMEAN =              179.398
+    CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/kpnocoude/demos/demoobj1.dat b/noao/imred/kpnocoude/demos/demoobj1.dat
new file mode 100644
index 00000000..78f3b9ad
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/demoobj1.dat
@@ -0,0 +1,37 @@
+    OBJECT  = 'V640Mon 4500      '  /  object name
+    OBSERVAT= 'KPNO              '  /  observatory
+    OBSERVER= 'Massey            '  /  observers
+    COMMENTS= 'Final New Ice     '  /  comments
+    EXPTIME =                1200.  /  actual integration time
+    DARKTIME=                1200.  /  total elapsed time
+    IMAGETYP= 'object            '  /  object, dark, bias, etc.
+    DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+    UT      = '12:19:55.00       '  /  universal time
+    ST      = '09:13:15.00       '  /  sidereal time
+    RA      = '06:37:02.00       '  /  right ascension
+    DEC     = '06:08:52.00       '  /  declination
+    EPOCH   =               1991.9  /  epoch of ra and dec
+    ZD      = '44.580            '  /  zenith distance
+    AIRMASS =                   0.  /  airmass
+    TELESCOP= 'kpcdf             '  /  telescope name
+    DETECTOR= 'te1k              '  /  detector
+    PREFLASH=                    0  /  preflash time, seconds
+    GAIN    =                  5.4  /  gain, electrons per adu
+    DWELL   =                    5  /  sample integration time
+    RDNOISE =                  3.5  /  read noise, electrons per adu
+    DELAY0  =                    0  /  time delay after each pixel
+    DELAY1  =                    0  /  time delay after each row
+    CAMTEMP =                 -111  /  camera temperature
+    DEWTEMP =                 -183  /  dewar temperature
+    CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+    ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+    CCDSUM  = '1 1               '  /  on chip summation
+    INSTRUME= 'test              '  /  instrument
+    APERTURE= '250micron slit    '  /  aperture
+    TVFILT  = '4-96              '  /  tv filter
+    DISPAXIS= '2                 '  /  dispersion axis
+    GRATPOS =               4624.3  /  grating position
+    TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+    OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+    ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+    CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/kpnocoude/demos/demos.cl b/noao/imred/kpnocoude/demos/demos.cl
new file mode 100644
index 00000000..5b065c51
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/demos.cl
@@ -0,0 +1,18 @@
+# DEMOS -- Run specified demo provided a demo file exists.
+
+procedure demos (demoname)
+
+file	demoname	{prompt="Demo name"}
+
+begin
+	file	demo, demofile
+
+	if ($nargs == 0 && mode != "h")
+	    type ("demos$demos.men")
+	demo = demoname
+	demofile = "demos$" // demo // ".cl"
+	if (access (demofile))
+	    cl (< demofile)
+	else
+	    error (1, "Unknown demo " // demo)
+end
diff --git a/noao/imred/kpnocoude/demos/demos.men b/noao/imred/kpnocoude/demos/demos.men
new file mode 100644
index 00000000..cdd3d484
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/demos.men
@@ -0,0 +1,6 @@
+	MENU of KPNOCOUDE Demonstrations
+
+       doslit - Quick test of DOSLIT (no comments, no delays)
+     do3fiber - Quick test of DO3FIBER (small images, no comments, no delays)
+     mkdoslit - Make DOSLIT test data
+   mkdo3fiber - Make DO3FIBER test data (50x256)
diff --git a/noao/imred/kpnocoude/demos/demos.par b/noao/imred/kpnocoude/demos/demos.par
new file mode 100644
index 00000000..4181ed59
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/demos.par
@@ -0,0 +1,2 @@
+demoname,f,a,"",,,"Demo name"
+mode,s,h,"ql",,,
diff --git a/noao/imred/kpnocoude/demos/demostd1.dat b/noao/imred/kpnocoude/demos/demostd1.dat
new file mode 100644
index 00000000..78f3b9ad
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/demostd1.dat
@@ -0,0 +1,37 @@
+    OBJECT  = 'V640Mon 4500      '  /  object name
+    OBSERVAT= 'KPNO              '  /  observatory
+    OBSERVER= 'Massey            '  /  observers
+    COMMENTS= 'Final New Ice     '  /  comments
+    EXPTIME =                1200.  /  actual integration time
+    DARKTIME=                1200.  /  total elapsed time
+    IMAGETYP= 'object            '  /  object, dark, bias, etc.
+    DATE-OBS= '26/11/91          '  /  date (dd/mm/yy) of obs.
+    UT      = '12:19:55.00       '  /  universal time
+    ST      = '09:13:15.00       '  /  sidereal time
+    RA      = '06:37:02.00       '  /  right ascension
+    DEC     = '06:08:52.00       '  /  declination
+    EPOCH   =               1991.9  /  epoch of ra and dec
+    ZD      = '44.580            '  /  zenith distance
+    AIRMASS =                   0.  /  airmass
+    TELESCOP= 'kpcdf             '  /  telescope name
+    DETECTOR= 'te1k              '  /  detector
+    PREFLASH=                    0  /  preflash time, seconds
+    GAIN    =                  5.4  /  gain, electrons per adu
+    DWELL   =                    5  /  sample integration time
+    RDNOISE =                  3.5  /  read noise, electrons per adu
+    DELAY0  =                    0  /  time delay after each pixel
+    DELAY1  =                    0  /  time delay after each row
+    CAMTEMP =                 -111  /  camera temperature
+    DEWTEMP =                 -183  /  dewar temperature
+    CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+    ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+    CCDSUM  = '1 1               '  /  on chip summation
+    INSTRUME= 'test              '  /  instrument
+    APERTURE= '250micron slit    '  /  aperture
+    TVFILT  = '4-96              '  /  tv filter
+    DISPAXIS= '2                 '  /  dispersion axis
+    GRATPOS =               4624.3  /  grating position
+    TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+    OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+    ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+    CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/kpnocoude/demos/do3fiber.cl b/noao/imred/kpnocoude/demos/do3fiber.cl
new file mode 100644
index 00000000..c4ab15a5
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/do3fiber.cl
@@ -0,0 +1,14 @@
+# Create demo data if needed.
+
+cl (< "demos$mkdo3fiber.cl")
+
+unlearn do3fiber
+params.coordlist = "linelists$idhenear.dat"
+params.match = 10.
+delete demologfile,demoplotfile verify=no >& dev$null
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgdo3fiber.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/kpnocoude/demos/doslit.cl b/noao/imred/kpnocoude/demos/doslit.cl
new file mode 100644
index 00000000..dd7a0955
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/doslit.cl
@@ -0,0 +1,15 @@
+# Create demo data if needed.
+
+cl (< "demos$mkdoslit.cl")
+
+unlearn doslit
+sparams.extras = no
+sparams.coordlist = "linelists$idhenear.dat"
+sparams.match = 10.
+delete demologfile,demoplotfile verify=no >& dev$null
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgdoslit.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/kpnocoude/demos/mkdo3fiber.cl b/noao/imred/kpnocoude/demos/mkdo3fiber.cl
new file mode 100644
index 00000000..00a775f4
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/mkdo3fiber.cl
@@ -0,0 +1,22 @@
+# Create demo data if needed.
+
+artdata
+artdata.nxc = 5
+artdata.nyc = 5
+artdata.nxsub = 10
+artdata.nysub = 10
+artdata.nxgsub = 5
+artdata.nygsub = 5
+artdata.dynrange = 100000.
+artdata.psfrange = 10.
+artdata.ranbuf = 0
+
+mkfibers ("demoobj", type="objnosky", fibers="demos$mkdo3fiber.dat",
+    title="Coude artificial image", header="demos$demoobj1.dat",
+    ncols=50, nlines=256, wstart=5786., wend=7362., seed=1)
+mkfibers ("demoflat", type="flat", fibers="demos$mkdo3fiber.dat",
+    title="Coude artificial image", header="demos$demostd1.dat",
+    ncols=50, nlines=256, wstart=5786., wend=7362., seed=2)
+mkfibers ("demoarc", type="henear", fibers="demos$mkdo3fiber.dat",
+    title="Coude artificial image", header="demos$demoarc1.dat",
+    ncols=50, nlines=256, wstart=5786., wend=7362., seed=3)
diff --git a/noao/imred/kpnocoude/demos/mkdo3fiber.dat b/noao/imred/kpnocoude/demos/mkdo3fiber.dat
new file mode 100644
index 00000000..e0d2d241
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/mkdo3fiber.dat
@@ -0,0 +1,3 @@
+1 2 0.757532 gauss 2.7 0 14.6 0.002
+2 1 0.939866 gauss 2.7 0 25.1 0.002
+3 2 1.015546 gauss 2.7 0 35.5 0.002
diff --git a/noao/imred/kpnocoude/demos/mkdoslit.cl b/noao/imred/kpnocoude/demos/mkdoslit.cl
new file mode 100644
index 00000000..b76f467d
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/mkdoslit.cl
@@ -0,0 +1,25 @@
+# Create demo data if needed.
+
+artdata
+artdata.nxc = 5
+artdata.nyc = 5
+artdata.nxsub = 10
+artdata.nysub = 10
+artdata.nxgsub = 5
+artdata.nygsub = 5
+artdata.dynrange = 100000.
+artdata.psfrange = 10.
+artdata.ranbuf = 0
+
+mkexample ("longslit", "demoarc1", oseed=5,  nseed=1,
+    errors=no, verbose=yes, list=no)
+mkheader ("demoarc1", "demos$demoarc1.dat", append=no, verbose=no)
+mkexample ("longslit", "demoobj1", oseed=1,  nseed=1,
+    errors=no, verbose=yes, list=no)
+mkheader ("demoobj1", "demos$demoobj1.dat", append=no, verbose=no)
+mkexample ("longslit", "demostd1", oseed=2, nseed=2,
+    errors=no, verbose=yes, list=no)
+mkheader ("demostd1", "demos$demostd1.dat", append=no, verbose=no)
+mkexample ("longslit", "demoarc2", oseed=5,  nseed=2,
+    errors=no, verbose=yes, list=no)
+mkheader ("demoarc2", "demos$demoarc2.dat", append=no, verbose=no)
diff --git a/noao/imred/kpnocoude/demos/xgdo3fiber.dat b/noao/imred/kpnocoude/demos/xgdo3fiber.dat
new file mode 100644
index 00000000..498209b4
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/xgdo3fiber.dat
@@ -0,0 +1,60 @@
+\O=NOAO/IRAF IRAFX valdes@puppis Mon 14:58:37 15-Nov-93
+\T=xgterm
+\G=xgterm
+epar\skpnocoude\n
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+y\r
+demologfile\r
+demoplotfile
+^Z
+epar\sdo3fiber\n
+demoobj\r
+demoflat\r
+demoflat\r
+demoarc\r
+\r
+rdnoise\r
+gain\r
+\r
+\r
+4\r
+6600\r
+6.1\r
+\r
+\r
+\r
+\r
+y\r
+y\r
+\r
+\r
+y\r
+^Z
+do3fiber\sredo+\n
+\n
+\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\r
+q/<-5\s\s\s\s/=(.\s=\r
+:/<-5\s\s\s\s/=(.\s=\r coord\slinelists$idhenear.dat\r
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+n\n
+y\n
+q/<-5\s\s\s\s/=(.\s=\r
+N\n
+n\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
diff --git a/noao/imred/kpnocoude/demos/xgdoslit.dat b/noao/imred/kpnocoude/demos/xgdoslit.dat
new file mode 100644
index 00000000..4ba38e19
--- /dev/null
+++ b/noao/imred/kpnocoude/demos/xgdoslit.dat
@@ -0,0 +1,71 @@
+\O=NOAO/IRAF IRAFX valdes@puppis Mon 14:58:37 15-Nov-93
+\T=xgterm
+\G=xgterm
+epar\skpnocoude\n
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+y\r
+demologfile\r
+demoplotfile\r
+^Z
+epar\sdoslit\n
+demoobj1\r
+demoarc1,demoarc2\r
+\r
+demostd1\r
+rdnoise\r
+gain\r
+\r
+\r
+5700\r
+6.2\r
+\r
+y\r
+y\r
+y\r
+y\r
+y\r
+^Z
+doslit\sredo+\n
+\n
+\n
+b/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+y\n
+4210\n
+7350\n
+6.2\n
+\n
+n\n
+\n
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\n
+hz14\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+Y\n
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+gkimos\sdemoplotfile\snx=3\sny=3\sdev=stdgraph\n
+q/<-5\s\s\s\s/=(.\s=\r
diff --git a/noao/imred/kpnocoude/do3fiber.cl b/noao/imred/kpnocoude/do3fiber.cl
new file mode 100644
index 00000000..649684cb
--- /dev/null
+++ b/noao/imred/kpnocoude/do3fiber.cl
@@ -0,0 +1,60 @@
+# DO3FIBERS -- Process Coude fiber spectra from 2D to wavelength calibrated 1D.
+#
+# The task PROC does all of the interactive work and BATCH does the
+# background work.  This procedure is organized this way to minimize the
+# dictionary space when the background task is submitted.
+
+procedure do3fiber (objects)
+
+string	objects = ""		{prompt="List of object spectra"}
+
+file	apref = ""		{prompt="Aperture reference spectrum"}
+file	flat = ""		{prompt="Flat field spectrum"}
+string	arcs = ""		{prompt="List of arc spectra"}
+file	arctable = ""		{prompt="Arc assignment table (optional)\n"}
+
+string	readnoise = "RDNOISE"	{prompt="Read out noise sigma (photons)"}
+string	gain = "GAIN"		{prompt="Photon gain (photons/data number)"}
+real	datamax = INDEF		{prompt="Max data value / cosmic ray threshold"}
+int	fibers = 3		{prompt="Number of fibers"}
+real	width = 6.		{prompt="Width of profiles (pixels)"}
+string	crval = "INDEF"		{prompt="Approximate central wavelength"}
+string	cdelt = "INDEF"		{prompt="Approximate dispersion"}
+string	objaps = "2"		{prompt="Object apertures"}
+string	arcaps = "1,3"		{prompt="Arc apertures\n"}
+
+bool	scattered = no		{prompt="Subtract scattered light?"}
+bool	fitflat = yes		{prompt="Fit and ratio flat field spectrum?"}
+bool	recenter = yes		{prompt="Recenter object apertures?"}
+bool	edit = no		{prompt="Edit/review object apertures?"}
+bool	clean = no		{prompt="Detect and replace bad pixels?"}
+bool	dispcor = yes		{prompt="Dispersion correct spectra?"}
+bool	splot = yes		{prompt="Plot the final spectrum?"}
+bool	redo = no		{prompt="Redo operations if previously done?"}
+bool	update = yes		{prompt="Update spectra if cal data changes?"}
+bool	batch = no		{prompt="Extract objects in batch?"}
+bool	listonly = no		{prompt="List steps but don't process?\n"}
+
+pset	params = ""		{prompt="Algorithm parameters"}
+
+begin
+	apscript.readnoise = readnoise
+	apscript.gain = gain
+	apscript.nfind = fibers
+	apscript.width = width
+	apscript.t_width = width
+	apscript.radius = width
+	apscript.clean = clean
+	apscript.order = "increasing"
+	proc.datamax = datamax
+
+	proc (objects, apref, flat, "", arcs, "", "",
+	    arctable, fibers, "", crval, cdelt, objaps, "", arcaps, "",
+	    "", "", scattered, fitflat, recenter, edit, no, no, clean,
+	    dispcor, no, no, no, no, no, splot, redo, update, batch, listonly)
+
+	if (proc.dobatch) {
+	    print ("-- Do remaining spectra as a batch job --")
+	    print ("batch&batch") | cl
+	}
+end
diff --git a/noao/imred/kpnocoude/do3fiber.par b/noao/imred/kpnocoude/do3fiber.par
new file mode 100644
index 00000000..8a30a4e0
--- /dev/null
+++ b/noao/imred/kpnocoude/do3fiber.par
@@ -0,0 +1,30 @@
+objects,s,a,"",,,"List of object spectra"
+apref,f,h,"",,,"Aperture reference spectrum"
+flat,f,h,"",,,"Flat field spectrum"
+arcs,s,h,"",,,"List of arc spectra"
+arctable,f,h,"",,,"Arc assignment table (optional)
+"
+readnoise,s,h,"RDNOISE",,,"Read out noise sigma (photons)"
+gain,s,h,"GAIN",,,"Photon gain (photons/data number)"
+datamax,r,h,INDEF,,,"Max data value / cosmic ray threshold"
+fibers,i,h,3,,,"Number of fibers"
+width,r,h,6.,,,"Width of profiles (pixels)"
+crval,s,h,INDEF,,,"Approximate central wavelength"
+cdelt,s,h,INDEF,,,"Approximate dispersion"
+objaps,s,h,"2",,,"Object apertures"
+arcaps,s,h,"1,3",,,"Arc apertures
+"
+scattered,b,h,no,,,"Subtract scattered light?"
+fitflat,b,h,yes,,,"Fit and ratio flat field spectrum?"
+recenter,b,h,yes,,,"Recenter object apertures?"
+edit,b,h,no,,,"Edit/review object apertures?"
+clean,b,h,no,,,"Detect and replace bad pixels?"
+dispcor,b,h,yes,,,"Dispersion correct spectra?"
+splot,b,h,yes,,,"Plot the final spectrum?"
+redo,b,h,no,,,"Redo operations if previously done?"
+update,b,h,yes,,,"Update spectra if cal data changes?"
+batch,b,h,no,,,"Extract objects in batch?"
+listonly,b,h,no,,,"List steps but don\'t process?
+"
+params,pset,h,"",,,"Algorithm parameters"
+mode,s,h,"ql",,,
diff --git a/noao/imred/kpnocoude/doc/do3fiber.hlp b/noao/imred/kpnocoude/doc/do3fiber.hlp
new file mode 100644
index 00000000..af99e15b
--- /dev/null
+++ b/noao/imred/kpnocoude/doc/do3fiber.hlp
@@ -0,0 +1,1146 @@
+.help do3fiber Feb93 noao.imred.kpnocoude
+.ih
+NAME
+do3fiber -- Three fiber data reduction task
+.ih
+USAGE
+do3fiber objects
+.ih
+SUMMARY
+The \fBdo3fiber\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, and wavelength calibration of multifiber data in which some
+fibers are used to take object spectra and other fibers are used to
+take simultaneous arc spectra.  A three fiber instrument of this
+type (one object and two arc fibers) is available at the KPNO coude feed.
+The default parameters are set for this configuration.
+If there are a large number of fibers and fiber throughput and sky
+fiber subtraction is needed the \fBdofiber\fR task should be used.
+
+The \fBdo3fiber\fR task is a command language script which collects
+and combines the functions and parameters of many general purpose tasks to
+provide a single complete data reduction path.  The task provides a degree
+of guidance, automation, and record keeping necessary when dealing with
+this type of multifiber data.
+.ih
+PARAMETERS
+.ls objects
+List of object spectra to be processed.  Previously processed spectra are
+ignored unless the \fIredo\fR flag is set or the \fIupdate\fR flag is set and
+dependent calibration data has changed.  Extracted spectra are ignored.
+.le
+.ls apref = ""
+Aperture reference spectrum.  This spectrum is used to define the basic
+extraction apertures and is typically a flat field spectrum.
+.le
+.ls flat = "" (optional)
+Flat field spectrum.  If specified the one dimensional flat field spectra
+are extracted and used to make flat field corrections.
+.le
+.ls arcs = "" (at least one if dispersion correcting)
+List of primary, all fiber arc spectra.  These spectra are used to define
+the dispersion functions for each fiber apart from a possible zero point
+correction made with simultaneous arc calibration fibers in the object
+spectra.  One fiber from the first spectrum is used to mark lines and set
+the dispersion function interactively and dispersion functions for all
+other fibers and arc spectra are derived from it.
+.le
+.ls arctable = "" (optional) (refspectra)
+Table defining arc spectra to be assigned to object
+spectra (see \fBrefspectra\fR).  If not specified an assignment based
+on a header parameter, \fIparams.sort\fR, such as the observation time is made.
+.le
+
+.ls readnoise = "RDNOISE" (apsum)
+Read out noise in photons.  This parameter defines the minimum noise
+sigma.  It is defined in terms of photons (or electrons) and scales
+to the data values through the gain parameter.  A image header keyword
+(case insensitive) may be specified to get the value from the image.
+.le
+.ls gain = "GAIN" (apsum)
+Detector gain or conversion factor between photons/electrons and
+data values.  It is specified as the number of photons per data value.
+A image header keyword (case insensitive) may be specified to get the value
+from the image.
+.le
+.ls datamax = INDEF (apsum.saturation)
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the flat field or arc
+spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.le
+.ls fibers = 3 (apfind)
+Number of fibers.  This number is used during the automatic definition of
+the apertures from the aperture reference spectrum.
+.le
+.ls width = 6. (apedit)
+Approximate base full width of the fiber profiles.  This parameter is used
+for the profile centering algorithm.
+.le
+.ls crval = INDEF, cdelt = INDEF (autoidentify)
+These parameters specify an approximate central wavelength and dispersion.
+They may be specified as numerical values, INDEF, or image header keyword
+names whose values are to be used.  If one or both of these parameters are
+specified as INDEF the search for a solution will be slower and more likely
+to fail.
+.le
+.ls objaps = "2", arcaps = "1,3"
+List of object and arc aperture numbers.  These are used to
+identify arc apertures for wavelength calibration and object apertures
+for the final results.
+.le
+
+.ls scattered = no (apscatter)
+Smooth and subtracted scattered light from the object and flat field
+images.  This operation consists of fitting independent smooth functions
+across the dispersion using data outside the fiber apertures and then
+smoothing the individual fits along the dispersion.  The initial
+flat field, or if none is given the aperture reference image, are
+done interactively to allow setting the fitting parameters.  All
+subsequent subtractions use the same fitting parameters.
+.le
+.ls fitflat = yes (flat1d)
+Fit the composite flat field spectrum by a smooth function and divide each
+flat field spectrum by this function?  This operation removes the average
+spectral signature of the flat field lamp from the sensitivity correction to
+avoid modifying the object fluxes.
+.le
+.ls recenter = yes (aprecenter)
+Recenter reference apertures for each object spectrum?
+.le
+.ls edit = no (apedit)
+Review aperture definitions for each object spectrum?  Note that this does
+not apply to the initial reference aperture which always allows
+interactive review of the aperture definitions.
+.le
+.ls clean = no (apsum)
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction and requires reasonably good values
+for the readout noise and gain.  In addition the datamax parameters
+can be useful.
+.le
+.ls dispcor = yes
+Dispersion correct spectra?  Depending on the \fIparams.linearize\fR
+parameter this may either resample the spectra or insert a dispersion
+function in the image header.
+.le
+.ls splot = yes
+Plot the final spectra with the task \fBsplot\fR?
+.le
+.ls redo = no
+Redo operations previously done?  If no then previously processed spectra
+in the objects list will not be processed (unless they need to be updated).
+.le
+.ls update = yes
+Update processing of previously processed spectra if aperture, flat
+field, or dispersion reference definitions are changed?
+.le
+.ls batch = no
+Process spectra as a background or batch job provided there are no interactive
+options (\fIedit\fR and \fIsplot\fR) selected.
+.le
+.ls listonly = no
+List processing steps but don't process?
+.le
+
+.ls params = "" (pset)
+Name of parameter set containing additional processing parameters.  The
+default is parameter set \fBparams\fR.  The parameter set may be examined
+and modified in the usual ways (typically with "epar params" or ":e params"
+from the parameter editor).  Note that using a different parameter file
+is not allowed.  The parameters are described below.
+.le
+
+.ce
+-- PACKAGE PARAMETERS
+
+Package parameters are those which generally apply to all task in the
+package.  This is also true of \fBdo3fiber\fR.
+.ls observatory = "observatory"
+Observatory at which the spectra were obtained if not specified in the
+image header by the keyword OBSERVAT.  For NOAO data the image headers
+identify the observatory as "kpno" or "ctio" so this parameter is not used.
+For data from other observatories this parameter may be used
+as describe in \fBobservatory\fR.
+.le
+.ls interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc)
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.nf
+	nearest - nearest neighbor
+	 linear - linear
+	  poly3 - 3rd order polynomial
+	  poly5 - 5th order polynomial
+	spline3 - cubic spline
+	   sinc - sinc function
+.fi
+.le
+.ls dispaxis = 2
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.
+.le
+.ls database = "database"
+Database (directory) used for storing aperture and dispersion information.
+.le
+.ls verbose = no
+Print verbose information available with various tasks.
+.le
+.ls logfile = "logfile", plotfile = ""
+Text and plot log files.  If a filename is not specified then no log is
+kept.  The plot file contains IRAF graphics metacode which may be examined
+in various ways such as with \fBgkimosaic\fR.
+.le
+.ls records = ""
+Dummy parameter to be ignored.
+.le
+.ls version = "KPNOCOUDE: ..."
+Version of the package.
+.le
+
+.ce
+PARAMS PARAMETERS
+
+The following parameters are part of the \fBparams\fR parameter set and
+define various algorithm parameters for \fBdo3fiber\fR.
+
+.ce
+--  GENERAL PARAMETERS --
+.ls line = INDEF, nsum = 10
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, recentering, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.le
+.ls extras = no (apsum)
+Include extra information in the output spectra?  When cleaning or using
+variance weighting the cleaned and weighted spectra are recorded in the
+first 2D plane of a 3D image, the raw, simple sum spectra are recorded in
+the second plane, and the estimated sigmas are recorded in the third plane.
+.le
+
+.ce
+-- DEFAULT APERTURE LIMITS --
+.ls lower = -3., upper = 3. (apdefault)
+Default lower and upper aperture limits relative to the aperture center.
+These limits are used when the apertures are first found and may be
+resized automatically or interactively.
+.le
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+.ls ylevel = 0.05 (apresize)
+Data level at which to set aperture limits during automatic resizing.
+It is a fraction of the peak relative to a local background.
+.le
+
+.ce
+-- TRACE PARAMETERS --
+.ls t_step = 10 (aptrace)
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \fInsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.le
+.ls t_function = "spline3", t_order = 2 (aptrace)
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.le
+.ls t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+Default number of rejection iterations and rejection sigma thresholds.
+.le
+
+.ce
+-- SCATTERED LIGHT PARAMETERS --
+.ls buffer = 1. (apscatter)
+Buffer distance from the aperture edges to be excluded in selecting the
+scattered light pixels to be used.
+.le
+.ls apscat1 = "" (apscatter)
+Fitting parameters across the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat1"
+parameter set.
+.le
+.ls apscat2 = "" (apscatter)
+Fitting parameters along the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat2"
+parameter set.
+.le
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+.ls weights = "none" (apsum)
+Type of extraction weighting.  Note that if the \fIclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+.ls "none"
+The pixels are summed without weights except for partial pixels at the
+ends.
+.le
+.ls "variance"
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \fIgain\fR and \fIreadnoise\fR
+parameters.
+.le
+.le
+.ls pfit = "fit1d" (apsum) (fit1d|fit2d)
+Profile fitting algorithm for cleaning and variance weighted extractions.
+The default is generally appropriate for most data but users
+may try the other algorithm.  See \fBapprofiles\fR for further information.
+.le
+.ls lsigma = 3., usigma = 3. (apsum)
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.le
+.ls nsubaps = 1 (apsum)
+During extraction it is possible to equally divide the apertures into
+this number of subapertures.
+.le
+
+.ce
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --
+.ls f_interactive = yes (fit1d)
+Fit the composite one dimensional flat field spectrum interactively?
+This is used if \fIfitflat\fR is set and a two dimensional flat field
+spectrum is specified.
+.le
+.ls f_function = "spline3", f_order = 20 (fit1d)
+Function and order used to fit the composite one dimensional flat field
+spectrum.  The functions are "legendre", "chebyshev", "spline1", and
+"spline3".  The spline functions are linear and cubic splines with the
+order specifying the number of pieces.
+.le
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+.ls threshold = 10. (autoidentify/identify/reidentify)
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.le
+.ls coordlist = "linelists$idhenear.dat" (autoidentify/identify)
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelists$".
+.le
+.ls match = -3. (autoidentify/identify)
+The maximum difference for a match between the dispersion function prediction
+value and a wavelength in the coordinate list.
+.le
+.ls fwidth = 3.5 (autoidentify/identify)
+Approximate full base width (in pixels) of arc lines.
+.le
+.ls cradius = 4. (reidentify)
+Radius from previous position to reidentify arc line.
+.le
+.ls i_function = "legendre", i_order = 3 (autoidentify/identify)
+The default function and order to be fit to the arc wavelengths as a
+function of the pixel coordinate.  The functions choices are "chebyshev",
+"legendre", "spline1", or "spline3".
+.le
+.ls i_niterate = 3, i_low = 3.0, i_high = 3.0 (autoidentify/identify)
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.le
+.ls refit = yes (reidentify)
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.le
+.ls addfeatures = no (reidentify)
+Add new features from a line list during each reidentification?
+This option can be used to compensate for lost features from the
+reference solution.  Care should be exercised that misidentified features
+are not introduced.
+.le
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+.ls select = "interp" (refspectra)
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+.ls average
+Average two reference spectra without regard to any sort parameter.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.
+This option is used to assign two reference spectra, with equal weights,
+independent of any sorting parameter.
+.le
+.ls following
+Select the nearest following spectrum in the reference list based on the
+sorting parameter.  If there is no following spectrum use the nearest preceding
+spectrum.
+.le
+.ls interp
+Interpolate between the preceding and following spectra in the reference
+list based on the sorting parameter.  If there is no preceding and following
+spectrum use the nearest spectrum.  The interpolation is weighted by the
+relative distances of the sorting parameter.
+.le
+.ls match
+Match each input spectrum with the reference spectrum list in order.
+This overrides the reference aperture check.
+.le
+.ls nearest
+Select the nearest spectrum in the reference list based on the sorting
+parameter.
+.le
+.ls preceding
+Select the nearest preceding spectrum in the reference list based on the
+sorting parameter.  If there is no preceding spectrum use the nearest following
+spectrum.
+.le
+.le
+.ls sort = "jd", group = "ljd" (refspectra)
+Image header keywords to be used as the sorting parameter for selection
+based on order and to group spectra.
+A null string, "", or the word "none" may be use to disable the sorting
+or grouping parameters.
+The sorting parameter
+must be numeric but otherwise may be anything.  The grouping parameter
+may be a string or number and must simply be the same for all spectra within
+the same group (say a single night).
+Common sorting parameters are times or positions.
+In \fBdo3fiber\fR the Julian date (JD) and the local Julian day number (LJD)
+at the middle of the exposure are automatically computed from the universal
+time at the beginning of the exposure and the exposure time.  Also the
+parameter UTMIDDLE is computed.
+.le
+.ls time = no, timewrap = 17. (refspectra)
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.le
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+.ls linearize = yes (dispcor)
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling
+If no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data are not interpolated.
+.le
+.ls log = no (dispcor)
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.le
+.ls flux = yes (dispcor)
+Conserve the total flux during interpolation?  If \fIno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \fIyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.le
+.ih
+ENVIRONMENT PARAMETERS
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
+.ih
+DESCRIPTION
+The \fBdo3fiber\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, and wavelength calibration of multifiber data in which some
+fibers are used to take object spectra and other fibers are used to
+take simultaneous arc spectra.  A three fiber instrument of this
+type (one object and two arc fibers) is available at the KPNO coude feed.
+The default parameters are set for this configuration.
+If there are a large number of fibers and fiber throughput and sky
+fiber subtraction is needed the \fBdofiber\fR task should be used.
+
+The \fBdo3fiber\fR task is a command language script which collects
+and combines the functions and parameters of many general purpose tasks to
+provide a single complete data reduction path.  The task provides a degree
+of guidance, automation, and record keeping necessary when dealing with
+this type of multifiber data.
+
+The general organization of the task is to do the interactive setup steps
+first using representative calibration data and then perform the majority
+of the reductions automatically, and possibly as a background process, with
+reference to the setup data.  In addition, the task determines which setup
+and processing operations have been completed in previous executions of the
+task and, contingent on the \fIredo\fR and \fIupdate\fR options, skip or
+repeat some or all the steps.
+
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage.  Since
+\fBdo3fiber\fR combines many separate, general purpose tasks the
+description given here refers to these tasks and leaves some of the details
+to their help documentation.
+
+\fBUsage Outline\fR
+
+.ls 6 [1]
+The images are first processed with \fBccdproc\fR for overscan,
+bias, and dark corrections.
+The \fBdo3fibers\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+.le
+.ls [2]
+Set the \fBdo3fiber\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed, the flat field image as the aperture reference and
+the flat field, and one or more arc images.  If there are many
+object or arc spectra per setup you might want to prepare "@ files".
+.le
+.ls [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the execution and no further queries of that
+type will be made.
+.le
+.ls [4]
+The apertures are defined using the specified aperture reference image
+which is usually a flat field in which both the object and arc fibers are
+illuminated.  The specified number of fibers are found automatically and
+sequential apertures assigned.
+.le
+.ls [5]
+A query is given allowing the apertures to be interactively reviewed.
+In this mode one may adjust the aperture widths as desired either
+explicitly (:lower and :upper), with the cursor ('l' and 'u'), at a
+particular flux level ('y'), or with an automatic algorithm ('z')
+as described by \fBapresize\fR.  To exit type 'q'.
+.le
+.ls [6]
+The fiber positions at a series of points along the dispersion are measured
+and a function is fit to these positions.  This may be done interactively to
+adjust the fitting parameters.  Not all fibers need be examined and the "NO"
+response will quit the interactive fitting.  To exit the interactive
+fitting type 'q'.
+.le
+.ls [7]
+If scattered light subtraction is to be done the flat field image is
+used to define the scattered light fitting parameters interactively.
+If one is not specified then the aperture reference image is used for
+this purpose.
+
+There are two queries for the interactive fitting.  A graph of the
+data between the defined reference apertures separated by a specified
+buffer distance is first shown.  The function order and type may be
+adjusted.  After quiting with 'q' the user has the option of changing
+the buffer value and returning to the fitting, changing the image line
+or column to check if the fit parameters are satisfactory at other points,
+or to quit and accept the fit parameters.  After fitting all points
+across the dispersion another graph showing the scattered light from
+the individual fits is shown and the smoothing parameters along the
+dispersion may be adjusted.  Upon quiting with 'q' you have the option
+of checking other cuts parallel to the dispersion or quiting and finishing
+the scattered light function smoothing and subtraction.
+
+If there is a throughput image then this is corrected for scattered light
+noninteractively using the previous fitting parameters.
+.le
+.ls [8]
+If flat fielding is to be done the flat field spectra are extracted.  The
+average spectrum over all fibers is determined and a function is fit
+interactively (exit with 'q').  This function is generally of sufficiently
+high order that the overall shape is well fit.  This function is then used
+to normalize the individual flat field spectra.
+The final response spectra are normalized to a unit
+mean over all fibers.
+.le
+.ls [9]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  The middle fiber is used to identify the arc lines and define
+the dispersion function using the task \fBautoidentify\fR.  The
+\fIcrval\fR and \fIcdelt\fR parameters are used in the automatic
+identification.  Whether or not the automatic identification is
+successful you will be shown the result of the arc line identification.
+If the automatic identification is not successful identify a few arc
+lines with 'm' and use the 'l' line list identification command to
+automatically add additional lines and fit the dispersion function.  Check
+the quality of the dispersion function fit with 'f'.  When satisfied exit
+with 'q'.
+.le
+.ls [10]
+The remaining fibers are automatically reidentified.  You have the option
+to review the line identifications and dispersion function for each fiber
+and interactively add or delete arc lines and change fitting parameters.
+This can be done selectively, such as when the reported RMS increases
+significantly.
+.le
+.ls [11]
+If the spectra are to be resampled to a linear dispersion system
+(which will be the same for all spectra) default dispersion parameters
+are printed and you are allowed to adjust these as desired.
+.le
+.ls [12]
+The object spectra are now automatically scattered light subtracted,
+ extracted, flat fielded, and dispersion corrected.
+The reference apertures are first assigned
+to the object spectra.  If the \fIrecenter\fR option is set the apertures
+will have a shift applied based on recentering the fiber profiles.
+If the \fIedit\fR option is set you may review and modify
+the aperture definitions interactively.  Any new
+arcs assigned to the object images are automatically extracted and
+dispersion functions determined.  A zero point wavelength correction
+is computed from the arc fiber spectra and applied to the object spectrum.
+.le
+.ls [13]
+The option to examine the final spectra with \fBsplot\fR may be given.
+To exit type 'q'.
+.le
+.ls [14]
+If scattered light is subtracted from the input data a copy of the
+original image is made by appending "noscat" to the image name.
+If the data are reprocessed with the \fIredo\fR flag the original
+image will be used again to allow modification of the scattered
+light parameters.
+
+The final spectra will have the same name as the original 2D images
+with a ".ms" extension added.
+.le
+
+\fBSpectra and Data Files\fR
+
+The basic input consists of multifiber object and calibration spectra
+stored as IRAF images.  The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+There are two types of calibration images.  These
+are flat fields and comparison lamp arc spectra.  The raw CCD images must
+be processed to remove overscan, bias, and dark count effects.  This is
+generally done using the \fBccdred\fR package.
+The \fBdo3fiber\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+Flat fielding is generally
+not done at this stage but as part of \fBdo3fiber\fR.  If for some reason
+the flat field or calibration arc spectra have separate exposures through
+different fibers they may be simply added.
+
+The assignment of arc calibration exposures to object exposures is
+generally done by selecting the nearest in time and interpolating.
+However, the optional \fIarc assignment table\fR may be used to explicitly
+assign arc images to specific objects.  The format of this file is
+described in the task \fBrefspectra\fR.
+
+The final reduced spectra are recorded in one, two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ms" extension.  Each line in the reduced image is a one dimensional
+spectrum with associated aperture, wavelength, and identification
+information.  With a single object spectrum the image will be one dimensional
+and with multiple object spectra the image will be two dimensional.
+When the \fIextras\fR parameter is set the images will be three
+dimensional (regardless of the number of apertures) and the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tasks such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.
+
+\fBPackage Parameters\fR
+
+The \fBkpnocoude\fR package parameters set parameters affecting all the tasks
+in the package.  Some of the parameters are not applicable to the
+\fBdo3fiber\fR task.  The observatory parameter is only required for data
+without an OBSERVAT header parameter (currently included in NOAO data).
+The spectrum interpolation type might be changed to "sinc" but with the
+cautions given in \fBonedspec.package\fR.  The dispersion axis parameter is
+only needed if a DISPAXIS image header parameter is not defined.  The other
+parameters define the standard I/O functions.  The verbose parameter
+selects whether to print everything which goes into the log file on the
+terminal.  It is useful for monitoring what the \fBdo3fiber\fR task does.  The
+log and plot files are useful for keeping a record of the processing.  A
+log file is highly recommended.  A plot file provides a record of
+apertures, traces, and extracted spectra but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+
+\fBProcessing Parameters\fR
+
+The input images are specified by image lists.  The lists may be
+a list of explicit, comma separate image names, @ files, or image
+templates using pattern matching against file names in the directory.
+The aperture reference spectrum is used to find the spectrum profiles and trace
+them.  Thus, this requires an image with good signal in all fibers
+which usually means a flat field spectrum.  It is recommended that
+flat field correction be done using one dimensional extracted spectra
+rather than as two dimensional images.  This is done if a flat field
+spectrum is specified.  The arc assignment table is used to specifically
+assign arc spectra to particular object spectra and the format
+of the file is described in \fBrefspectra\fR.
+
+The detector read out noise and gain are used for cleaning and variance
+(optimal) extraction.  The dispersion axis defines the wavelength direction
+of spectra in the image if not defined in the image header by the keyword
+DISPAXIS.  The width parameter (in pixels) is used for the profile finding and
+centering algorithm (\fBcenter1d\fR).
+
+The number of fibers is fairly obvious.  It is the number of
+fibers, including the arc fibers, to be automatically found and
+assigned apertures.  The apertures are assigned aperture
+numbers sequentially.  The object and arc fibers are identified
+by these aperture numbers as specified by the \fIobjaps\fR and
+\fIarcaps\fR parameters.  The defaults are for the case of three
+fibers in the sequence arc fiber, object fiber, and arc fiber.
+
+The approximate central wavelength and dispersion are used for the
+automatic identification of the arc reference.  They may be specified
+as image header keywords or values.  The INDEF values search the
+entire range of the coordinate reference file but the automatic
+line identification algorithm works much better and faster if
+approximate values are given.
+
+The next set of parameters select the processing steps and options.  The
+scattered light option allows fitting and subtracting a scattered light
+surface from the input object and flat field.  If there is significant
+scattered light which is not subtracted the fiber throughput correction
+will not be accurate.  The
+flat fitting option allows fitting and removing the overall shape of the
+flat field spectra while preserving the pixel-to-pixel response
+corrections.  This is useful for maintaining the approximate object count
+levels and not introducing the reciprocal of the flat field spectrum into
+the object spectra.
+
+The apertures defined for the aperture reference image are assigned to
+each image.  For the object images the apertures may be shifted across
+the dispersion by recentering the strongest profiles and averaging
+the individual shifts to form a single shift for all apertures.  This
+corrects for shifts in the detector during the observations.  The
+\fIrecenter\fR parameter selects whether to apply this shift or not.
+
+The \fIedit\fR option allows you to be queried to review the apertures
+assigned to each object image.  If selected and the query answered
+affirmatively the apertures may be interactively shifted and resized.  The
+query may also be answered with "NO" to turn off this option during
+processing.  Note that the initial aperture definitions for the aperture
+reference image always allows editing.
+
+The \fIclean\fR option invokes a profile fitting and deviant
+point rejection algorithm as well as a variance weighting of points in the
+aperture.  These options require knowing the effective (i.e. accounting for
+any image combining) read out noise and gain.  For a discussion of cleaning
+and variance weighted extraction see \fBapvariance\fR and
+\fBapprofiles\fR.
+
+The dispersion correction option selects whether to extract arc spectra,
+determine dispersion functions, assign them to the object spectra, and,
+possibly, resample the spectra to a linear (or log-linear) wavelength
+scale.
+
+The \fIsplot\fR option allows a query (which may be answered with "YES"
+or "NO" to eliminate the query) and then plotting of the final object
+spectra if answered affirmatively.  The plotting is done with the
+task \fBsplot\fR.
+
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\fIupdate\fR flag is set.  The changes which will cause an update are a new
+reference image, new flat field, and a new arc reference image.  If all
+input spectra are to be processed regardless of previous processing the
+\fIredo\fR flag may be used.  Note that reprocessing clobbers the
+previously processed output spectra.
+
+The \fIbatch\fR processing option allows object spectra to be processed as
+a background or batch job.  This will only occur if the aperture editing
+and final spectrum plotting have been turned off, either with the task
+option parameter or by answering "NO" to the queries.  The \fIlistonly\fR
+option prints a summary of the processing steps which will be performed on
+the input spectra without actually doing anything.  This is useful for
+verifying which spectra will be affected if the input list contains
+previously processed spectra.  The listing does not include any arc spectra
+which may be extracted to dispersion calibrate an object spectrum.
+
+The last parameter (excluding the task mode parameter) points to another
+parameter set for the algorithm parameters.  The way \fBdo3fiber\fR works
+this may not have any value and the parameter set \fBparams\fR is always
+used.  The algorithm parameters are discussed further in the next section.
+
+\fBAlgorithms and Algorithm Parameters\fR
+
+This section summarizes the various algorithms used by the \fBdo3fiber\fR
+task and the parameters which control and modify the algorithms.  The
+algorithm parameters available to the user are collected in the parameter
+set \fBparams\fR.  These parameters are taken from the various general
+purpose tasks used by the \fBdo3fiber\fR processing task.  Additional
+information about these parameters and algorithms may be found in the help
+for the actual task executed.  These tasks are identified in the parameter
+section listing in parenthesis.  The aim of this parameter set organization
+is to collect all the algorithm parameters in one place separate from the
+processing parameters and include only those which are relevant for
+this type of data.  The parameter values can be changed from the
+defaults by using the parameter editor,
+.nf
+
+	cl> epar params
+
+.fi
+or simple typing \fIparams\fR.  The parameter editor can also be
+entered when editing the \fBdo3fiber\fR parameters by typing \fI:e
+params\fR or simply \fI:e\fR if positioned at the \fIparams\fR
+parameter.
+
+\fBAperture Definitions\fR
+
+The first operation is to define the extraction apertures, which include
+the aperture width and position dependence with wavelength, for the object
+and arc fibers.  This is done on a reference spectrum which is usually a
+flat field taken through both fibers.  Other spectra will inherit the
+reference apertures and may apply a correction for any shift of the orders
+across the dispersion.  The reference apertures are defined only once
+unless the \fIredo\fR option is set.
+
+The selected number of fibers are found automatically by selecting the
+highest peaks in a cut across the dispersion.  Apertures are assigned with
+a limits set by the \fIlower\fR and \fIupper\fR parameter and numbered
+sequentially.  A query is then given allowing the apertures to be reviewed
+interactively.  If answered affirmatively a cut across the orders is shown
+with the apertures marked and an interactive aperture editing mode is
+entered (see \fBapedit\fR).  The main thing to be concerned about is that
+the aperture numbers agree with the \fIobjaps\fR and \fIarcaps\fR
+definitions.  The aperture numbers may be changed with the 'i' or 'o'
+keys.  The apertures may also be resized from the default limits.
+To exit the background and aperture editing steps type 'q'.
+
+Next the positions of the fiber profiles at various points along the
+dispersion are measured and a "trace function" is fit.  The user is asked
+whether to fit the trace function interactively.  This is selected to
+adjust the fitting parameters such as function type and order.  When
+interactively fitting a query is given for each aperture.  After the first
+aperture one may skip reviewing the other traces by responding with "NO".
+Queries made by \fBdo3fiber\fR generally may be answered with either lower
+case "yes" or "no" or with upper case "YES" or "NO".  The upper case
+responses apply to all further queries and so are used to eliminate further
+queries of that kind.
+
+The above steps are all performed using tasks from the \fBapextract\fR
+package and parameters from the \fBparams\fR parameters.  As a quick
+summary, the dispersion direction of the spectra are determined from the
+package \fBdispaxis\fR parameter if not defined in the image header.  The default
+line or column for finding the orders and the number of image lines or
+columns to sum are set by the \fIline\fR and \fInsum\fR parameters.  A line
+of INDEF (the default) selects the middle of the image.  The automatic
+finding algorithm is described for the task \fBapfind\fR and basically
+finds the strongest peaks.  The tracing is done as described in
+\fBaptrace\fR and consists of stepping along the image using the specified
+\fIt_step\fR parameter.  The function fitting uses the \fBicfit\fR commands
+with the other parameters from the tracing section.
+
+\fBExtraction\fR
+
+The actual extraction of the spectra is done by summing across the fixed
+width apertures at each point along the dispersion.  The default is to
+simply sum the pixels using partial pixels at the ends.  There is an
+option to weight the sum based on a Poisson noise model using the
+\fIreadnoise\fR and \fIgain\fR detector parameters.  Note that if the
+\fIclean\fR option is selected the variance weighted extraction is used
+regardless of the \fIweights\fR parameter.  The sigma thresholds for
+cleaning are also set in the \fBparams\fR parameters.
+
+The cleaning and variance weighting options require knowing the effective
+(i.e. accounting for any image combining) read out noise and gain.  These
+numbers need to be adjusted if the image has been processed such that the
+intensity scale has a different origin (such as a background light
+subtraction) or scaling (such as caused by unnormalized flat fielding).
+For optimal extraction and cleaning to work it is recommended that
+a \fIdatamax\fR value be determined for the data and the
+\fIfitflat\fR option be used.  For further discussion of cleaning and
+variance weighted extraction see \fBapvariance\fR and \fBapprofiles\fR as
+well as  \fBapsum\fR.
+
+\fBScattered Light Subtraction\fR
+
+Scattered light may be subtracted from the input two dimensional image as
+the first step.  This is done using the algorithm described in
+\fBapscatter\fR.  This can be important if there is significant scattered
+light since the flat field/throughput correction will otherwise be
+incorrect.  The algorithm consists of fitting a function to the data
+outside the defined apertures by a specified \fIbuffer\fR at each line or
+column across the dispersion.  The function fitting parameters are the same
+at each line.  Because the fitted functions are independent at each line or
+column a second set of one dimensional functions are fit parallel to the
+dispersion using the evaluated fit values from the cross-dispersion step.
+This produces a smooth scattered light surface which is finally subtracted
+from the input image.  Again the function fitting parameters are the
+same at each line or column though they may be different than the parameters
+used to fit across the dispersion.
+
+The first time the task is run with a particular flat field (or aperture
+reference image if no flat field is used) the scattered light fitting
+parameters are set interactively using that image.  The interactive step
+selects a particular line or column upon which the fitting is done
+interactively with the \fBicfit\fR commands.  A query is first issued
+which allows skipping this interactive stage.  Note that the interactive
+fitting is only for defining the fitting functions and orders.  When
+the graphical \fBicfit\fR fitting is exited (with 'q') there is a second prompt
+allowing you to change the buffer distance (in the first cross-dispersion
+stage) from the apertures, change the line/column, or finally quit.
+
+The initial fitting parameters and the final set parameters are recorded
+in the \fBapscat1\fR and \fBapscat2\fR hidden parameter sets.  These
+parameters are then used automatically for every subsequent image
+which is scattered light corrected.
+
+The scattered light subtraction modifies the input 2D images.  To preserve
+the original data a copy of the original image is made with the same
+root name and the word "noscat" appended.  The scattered light subtracted
+images will have the header keyword "APSCATTE" which is how the task
+avoids repeating the scattered light subtraction during any reprocessing.
+However if the \fIredo\fR option is selected the scattered light subtraction
+will also be redone by first restoring the "noscat" images to the original
+input names.
+
+\fBFlat Field Correction\fR
+
+Flat field corrections may be made during the basic CCD processing; i.e.
+direct division by the two dimensional flat field observation.  In that
+case do not specify a flat field spectrum; use the null string "".  The
+\fBdo3fiber\fR task provides an alternative flat field response correction
+based on division of the extracted object spectra by the extracted flat field
+spectra.  A discussion of the theory and merits of flat fielding directly
+verses using the extracted spectra will not be made here.  The
+\fBdo3fiber\fR flat fielding algorithm is the \fIrecommended\fR method for
+flat fielding since it works well and is not subject to the many problems
+involved in two dimensional flat fielding.
+
+The first step is extraction of the flat field spectrum, if specified,
+using the reference apertures.  Only one flat field is allowed so if
+multiple flat fields are required the data must be reduced in groups.
+If the \fIfitflat\fR
+option is selected (the default) the extracted flat field spectra are
+averaged together and a smooth function is fit.  The default fitting
+function and order are given by the parameters \fIf_function\fR and
+\fIf_order\fR.  If the parameter \fIf_interactive\fR is "yes" then the
+fitting is done interactively using the \fBfit1d\fR task which uses the
+\fBicfit\fR interactive fitting commands.
+
+The fitted function is divided into the individual flat field spectra to
+remove the basic shape of the spectrum while maintaining the relative
+individual pixel responses and any fiber to fiber differences.  This step
+avoids introducing the flat field spectrum shape into the object spectra
+and closely preserves the object counts.
+
+The final step is to normalize the flat field spectra by the mean counts over
+all the fibers.  This normalization step is simply to preserve the average
+counts of the extracted object and arc spectra after division by the
+response spectra.
+
+\fBDispersion Correction\fR
+
+If dispersion correction is not selected, \fIdispcor\fR=no, then the object
+spectra are simply extracted.  If it is selected the arc spectra are used
+to dispersion calibrate the object spectra.  There are four steps involved;
+determining the dispersion functions relating pixel position to wavelength,
+assigning the appropriate dispersion functions to a particular observation,
+determining a zero point wavelength shift from the arc fibers to be applied
+to the object fiber dispersion functions, and either storing the nonlinear
+dispersion function in the image headers or resampling the spectra to
+evenly spaced pixels in wavelength.
+
+The first arc spectrum in the arc list is used to define the reference
+dispersion solution.  It is extracted using the reference aperture
+definitions.  The interactive task \fBautoidentify\fR is used to
+automatically define the dispersion function in one fiber.  Whether or not
+it is successful the user is presented with the interactive identification
+graph.  The automatic identifications can be reviewed and a new solution or
+corrections to the automatic solution may be performed.  The dispersion
+functions for the other fibers are then determined automatically by
+reference to the first fiber using the task \fBreidentify\fR.  Except in
+batch mode a query is given allowing the reidentified arc spectra to be
+examined interactively with \fBidentify\fR.  This would normally be done
+only if the information about the reidentification printed on the terminal
+indicates a problem such as a large increase in the RMS.  This query may be
+eliminated in the usual way.
+
+The set of arc dispersion function parameters are from \fBautoidentify\fR and
+\fBreidentify\fR.  The parameters define a line list for use in
+automatically assigning wavelengths to arc lines, a parameter controlling
+the width of the centering window (which should match the base line
+widths), the dispersion function type and order, parameters to exclude bad
+lines from function fits, and parameters defining whether to refit the
+dispersion function, as opposed to simply determining a zero point shift,
+and the addition of new lines from the line list when reidentifying
+additional arc spectra.  The defaults should generally be adequate and the
+dispersion function fitting parameters may be altered interactively.  One
+should consult the help for the two tasks for additional details of these
+parameters and the operation of \fBautoidentify\fR.
+
+If resampling of the spectra is selected by the parameter \fIlinearize\fR
+all the arc dispersion functions are combined to provide a default
+starting and ending wavelength and dispersion with the same number of
+pixels is determined and the user is queried for any changes.  This
+linear dispersion system will be applied to all spectra so that all
+the final processed object spectra will have the same dispersion
+sampling.
+
+Once the reference dispersion functions are defined other arc spectra are
+extracted as they are assign to the object spectra.  The assignment of
+arcs is done either explicitly with an arc assignment table (parameter
+\fIarctable\fR) or based on a header parameter such as a time.
+The assignments are made by the task \fBrefspectra\fR.  When two arcs are
+assigned to an object spectrum an interpolation is done between the two
+dispersion functions.  This makes an approximate correction for steady
+drifts in the dispersion.  Because the arc fibers monitor any zero point
+shifts in the dispersion functions, due to translation and rotation of the
+detector, it is probably only necessary to have one or two arc spectra, one
+at the beginning and/or one at the end of the night.
+
+The tasks \fBsetjd\fR and \fBsetairmass\fR are automatically run on all
+spectra.  This computes and adds the header parameters for the Julian date
+(JD), the local Julian day number (LJD), the universal time (UTMIDDLE), and
+the air mass at the middle of the exposure.  The default arc assignment is
+to use the Julian date grouped by the local Julian day number.  The
+grouping allows multiple nights of data to be correctly assigned at the
+same time.
+
+When the object spectra are extracted so are the simultaneous arc spectra.
+A zero point shift of the arc spectra relative to the dispersion solutions
+of an assigned full arc observation is computed using \fBreidentify\fR.
+The zero point shifts from the arc fibers are then
+interpolated across the detector based on the positions of the arc
+apertures to the positions of the object apertures.  A linear interpolation
+is used which accounts for a rotation of the detector as well as a
+translation along the dispersion.  The interpolated zero point wavelength
+shifts are then added to the dispersion functions from the full arc
+observation for the object fibers.  Note that this does not assume that the
+object and arc fiber dispersion functions are the same or have the same
+wavelength origin, but only that the interpolated shifts in wavelength zero
+point apply to all fibers.  When there are two assigned full arc spectra
+the above steps are done independently and the final pair of zero point
+corrected dispersion functions for each object fiber are combined using the
+assigned weights.  Once the dispersion function correction is determined
+from the extracted arc fiber spectra they are deleted leaving only the
+object spectra.
+
+The last step of dispersion correction is setting the dispersion
+of the object spectra.  There are two choices here.
+If the \fIlinearize\fR parameter is not set the nonlinear dispersion
+functions are stored in the image header.  Other IRAF tasks interpret
+this information when dispersion coordinates are needed for plotting
+or analysis.  This has the advantage of not requiring the spectra
+to be interpolated and the disadvantage that the dispersion
+information is only understood by IRAF tasks and cannot be readily
+exported to other analysis software.
+
+If the \fIlinearize\fR parameter is set then the spectra are resampled to a
+linear dispersion relation either in wavelength or the log of the
+wavelength.  The linear dispersion parameters are those defined
+previously for the arc reference image.
+
+The linearization algorithm  parameters allow selecting the interpolation
+function type, whether to conserve flux per pixel by integrating across the
+extent of the final pixel, and whether to linearize to equal linear or
+logarithmic intervals.  The latter may be appropriate for radial velocity
+studies.  The default is to use a fifth order polynomial for interpolation,
+to conserve flux, and to not use logarithmic wavelength bins.  These
+parameters are described fully in the help for the task \fBdispcor\fR which
+performs the correction.
+.ih
+EXAMPLES
+1.  The following example uses artificial data and may be executed
+at the terminal (with IRAF V2.10).  This is also the sequence performed
+by the test procedure "demos do3fiber".
+
+.nf
+kp> demos mkdo3fiber
+Creating image demoobj ...
+Creating image demoflat ...
+Creating image demoarc ...
+kp> do3fiber demoobj apref=demoflat flat=demoflat arcs=demoarc \
+>>> width=4 edit=yes
+Set reference apertures for demoflat
+Resize apertures for demoflat?  (yes):
+Edit apertures for demoflat?  (yes):
+<Exit with 'q'>
+Fit traced positions for demoflat interactively?  (yes):
+Fit curve to aperture 1 of demoflat interactively  (yes):
+<Exit with 'q'>
+Fit curve to aperture 2 of demoflat interactively  (yes): N
+Create response function demoflatnorm.ms
+Extract flat field demoflat
+Fit and ratio flat field demoflat
+Create the normalized response demoflatnorm.ms
+demoflatnorm.ms -> demoflatnorm.ms  using bzero: 0.  and bscale: 1.
+    mean: 1.  median: 1.034214  mode: 0.8378798
+    upper: INDEF  lower: INDEF
+Average aperture response:
+1.  0.8394014
+2.  1.034403
+3.  1.126194
+Extract arc reference image demoarc
+Determine dispersion solution for demoarc
+<Reset default line list with ":coord linelists$idhenear.dat">
+<A dispersion solution is found automatically.>
+<Examine the fit with 'f'>
+<Exit fit with 'q' and exit task with 'q'>
+
+REIDENTIFY: NOAO/IRAF V2.10BETA valdes@puppis Fri 11:04:32 06-Mar-92
+  Reference image = demoarc.ms, New image = demoarc.ms, Refit = yes
+     Image Data Found    Fit Pix Shift  User Shift  Z Shift     RMS
+d...ms - Ap 1   30/30  29/30  -0.00675       -0.04  -6.9E-6   0.252
+Fit dispersion function interactively? (no|yes|NO|YES) (yes): n
+d...ms - Ap 3   30/30  29/30   -0.0154     -0.0928  -1.4E-5   0.303
+Fit dispersion function interactively? (no|yes|NO|YES) (no): y
+<Exit with 'q'>
+d...ms - Ap 3   30/30  29/30   -0.0154     -0.0928  -1.4E-5   0.303
+
+Dispersion correct demoarc
+d...ms: w1 = 5785.86, w2 = 7351.59, dw = 6.14, nw = 256
+  Change wavelength coordinate assignments? (yes|no|NO): N
+Extract object spectrum demoobj
+Edit apertures for demoobj?  (yes): n
+Assign arc spectra for demoobj
+[demoobj] refspec1='demoarc'
+Reidentify arc fibers in demoobj with respect to demoarc
+
+REIDENTIFY: NOAO/IRAF V2.10BETA valdes@puppis Fri 11:04:52 06-Mar-92
+  Reference image = demoarc.ms, New image = demoobjarc.ms, Refit = no
+  Image Data   Found    Fit Pix Shift  User Shift  Z Shift     RMS
+d...ms - Ap 1  27/30  27/27   0.00502      0.0263  3.99E-6   0.175
+d...ms - Ap 3  27/30  27/27   8.62E-4       0.006  5.07E-7   0.248
+Dispersion correct demoobj
+demoobj.ms.imh: REFSHFT1 = 'demoobjarc.ms interp', shift = -0.0050,
+rms = 0.00282813 intercept = -0.0118401, slope = 2.70764E-4
+d...ms: ap = 2, w1 = 5785.86, w2 = 7351.59, dw = 6.14, nw = 256
+demoobj.ms.imh:
+Splot spectrum? (no|yes|NO|YES) (yes):
+<Exit with 'q'>
+.fi
+.ih
+REVISIONS
+.ls DO3FIBER V2.11
+The initial arc line identifications is done with the automatic line
+identification algorithm.
+.le
+.ls DO3FIBER V2.10.3
+The usual output WCS format is "equispec".  The image format type to be
+processed is selected with the \fIimtype\fR environment parameter.  The
+dispersion axis parameter is now a package parameter.  Images will only
+be processed if the have the CCDPROC keyword.  A \fIdatamax\fR parameter
+has been added to help improve cosmic ray rejection.  A scattered
+light subtraction processing option has been added.
+.le
+.ih
+SEE ALSO
+apedit, apfind, approfiles, aprecenter, apresize, apsum, aptrace, apvariance,
+ccdred, center1d, dispcor, fit1d, icfit, identify, observatory,
+onedspec.package, refspectra, reidentify, setairmass, setjd
+.endhelp
diff --git a/noao/imred/kpnocoude/doc/do3fiber.ms b/noao/imred/kpnocoude/doc/do3fiber.ms
new file mode 100644
index 00000000..d572d035
--- /dev/null
+++ b/noao/imred/kpnocoude/doc/do3fiber.ms
@@ -0,0 +1,1413 @@
+.nr PS 9
+.nr VS 11
+.de V1
+.ft CW
+.nf
+..
+.de V2
+.fi
+.ft R
+..
+.de LS
+.br
+.in +2
+..
+.de LE
+.br
+.sp .5v
+.in -2
+..
+.ND February 1993
+.TL
+Guide to the Coude Three Fiber Reduction Task DO3FIBER
+.AU
+Francisco Valdes
+.AI
+IRAF Group - Central Computer Services
+.K2
+.DY
+
+.AB
+The \fBdo3fiber\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, and wavelength calibration of multifiber data in which some
+fibers are used to take object spectra and other fibers are used to
+take simultaneous arc spectra.  A three fiber instrument of this
+type (one object and two arc fibers) is available at the KPNO coude feed.
+The default parameters are set for this configuration.
+If there are a large number of fibers and fiber throughput and sky
+fiber subtraction is needed the \fBdofiber\fR task should be used.
+.LP
+The \fBdo3fiber\fR task is a command language script which collects
+and combines the functions and parameters of many general purpose tasks to
+provide a single complete data reduction path.  The task provides a degree
+of guidance, automation, and record keeping necessary when dealing with
+this type of multifiber data.
+.AE
+.NH
+Introduction
+.LP
+The \fBdo3fiber\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, and wavelength calibration of multifiber data in which some
+fibers are used to take object spectra and other fibers are used to
+take simultaneous arc spectra.  A three fiber instrument of this
+type (one object and two arc fibers) is available at the KPNO coude feed.
+The default parameters are set for this configuration.
+If there are a large number of fibers and fiber throughput and sky
+fiber subtraction is needed the \fBdofiber\fR task should be used.
+.LP
+The \fBdo3fiber\fR task is a command language script which collects
+and combines the functions and parameters of many general purpose tasks to
+provide a single complete data reduction path.  The task provides a degree
+of guidance, automation, and record keeping necessary when dealing with
+this type of multifiber data.
+.LP
+The general organization of the task is to do the interactive setup steps
+first using representative calibration data and then perform the majority
+of the reductions automatically, and possibly as a background process, with
+reference to the setup data.  In addition, the task determines which setup
+and processing operations have been completed in previous executions of the
+task and, contingent on the \f(CWredo\fR and \f(CWupdate\fR options, skip or
+repeat some or all the steps.
+.LP
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage.  Since
+\fBdo3fiber\fR combines many separate, general purpose tasks the
+description given here refers to these tasks and leaves some of the details
+to their help documentation.
+.NH
+Usage Outline
+.LP
+.IP [1] 6
+The images are first processed with \fBccdproc\fR for overscan,
+bias, and dark corrections.
+The \fBdo3fibers\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+.IP [2]
+Set the \fBdo3fiber\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed, the flat field image as the aperture reference and
+the flat field, and one or more arc images.  If there are many
+object or arc spectra per setup you might want to prepare "@ files".
+.IP [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the execution and no further queries of that
+type will be made.
+.IP [4]
+The apertures are defined using the specified aperture reference image
+which is usually a flat field in which both the object and arc fibers are
+illuminated.  The specified number of fibers are found automatically and
+sequential apertures assigned.
+.IP [5]
+A query is given allowing the apertures to be interactively reviewed.
+In this mode one may adjust the aperture widths as desired either
+explicitly (:lower and :upper), with the cursor ('l' and 'u'), at a
+particular flux level ('y'), or with an automatic algorithm ('z')
+as described by \fBapresize\fR.  To exit type 'q'.
+.IP [6]
+The fiber positions at a series of points along the dispersion are measured
+and a function is fit to these positions.  This may be done interactively to
+adjust the fitting parameters.  Not all fibers need be examined and the "NO"
+response will quit the interactive fitting.  To exit the interactive
+fitting type 'q'.
+.IP [7]
+If scattered light subtraction is to be done the flat field image is
+used to define the scattered light fitting parameters interactively.
+If one is not specified then the aperture reference image is used for
+this purpose.
+
+There are two queries for the interactive fitting.  A graph of the
+data between the defined reference apertures separated by a specified
+buffer distance is first shown.  The function order and type may be
+adjusted.  After quiting with 'q' the user has the option of changing
+the buffer value and returning to the fitting, changing the image line
+or column to check if the fit parameters are satisfactory at other points,
+or to quit and accept the fit parameters.  After fitting all points
+across the dispersion another graph showing the scattered light from
+the individual fits is shown and the smoothing parameters along the
+dispersion may be adjusted.  Upon quiting with 'q' you have the option
+of checking other cuts parallel to the dispersion or quiting and finishing
+the scattered light function smoothing and subtraction.
+
+If there is a throughput image then this is corrected for scattered light
+noninteractively using the previous fitting parameters.
+.IP [8]
+If flat fielding is to be done the flat field spectra are extracted.  The
+average spectrum over all fibers is determined and a function is fit
+interactively (exit with 'q').  This function is generally of sufficiently
+high order that the overall shape is well fit.  This function is then used
+to normalize the individual flat field spectra.
+The final response spectra are normalized to a unit
+mean over all fibers.
+.IP [9]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  The middle fiber is used to identify the arc lines and define
+the dispersion function using the task \fBautoidentify\fR.  The
+\fIcrval\fR and \fIcdelt\fR parameters are used in the automatic
+identification.  Whether or not the automatic identification is
+successful you will be shown the result of the arc line identification.
+If the automatic identification is not successful identify a few arc
+lines with 'm' and use the 'l' line list identification command to
+automatically add additional lines and fit the dispersion function.  Check
+the quality of the dispersion function fit with 'f'.  When satisfied exit
+with 'q'.
+.IP [10]
+The remaining fibers are automatically reidentified.  You have the option
+to review the line identifications and dispersion function for each fiber
+and interactively add or delete arc lines and change fitting parameters.
+This can be done selectively, such as when the reported RMS increases
+significantly.
+.IP [11]
+If the spectra are to be resampled to a linear dispersion system
+(which will be the same for all spectra) default dispersion parameters
+are printed and you are allowed to adjust these as desired.
+.IP [12]
+The object spectra are now automatically scattered light subtracted,
+ extracted, flat fielded, and dispersion corrected.
+The reference apertures are first assigned
+to the object spectra.  If the \f(CWrecenter\fR option is set the apertures
+will have a shift applied based on recentering the fiber profiles.
+If the \f(CWedit\fR option is set you may review and modify
+the aperture definitions interactively.  Any new
+arcs assigned to the object images are automatically extracted and
+dispersion functions determined.  A zero point wavelength correction
+is computed from the arc fiber spectra and applied to the object spectrum.
+.IP [13]
+The option to examine the final spectra with \fBsplot\fR may be given.
+To exit type 'q'.
+.IP [14]
+If scattered light is subtracted from the input data a copy of the
+original image is made by appending "noscat" to the image name.
+If the data are reprocessed with the \fIredo\fR flag the original
+image will be used again to allow modification of the scattered
+light parameters.
+
+The final spectra will have the same name as the original 2D images
+with a ".ms" extension added.
+.NH
+Spectra and Data Files
+.LP
+The basic input consists of multifiber object and calibration spectra
+stored as IRAF images.
+The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+There are two types of calibration images.  These
+are flat fields and comparison lamp arc spectra.  The raw CCD images must
+be processed to remove overscan, bias, and dark count effects.  This is
+generally done using the \fBccdred\fR package.
+The \fBdo3fiber\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+Flat fielding is generally
+not done at this stage but as part of \fBdo3fiber\fR.  If for some reason
+the flat field or calibration arc spectra have separate exposures through
+different fibers they may be simply added.
+.LP
+The assignment of arc calibration exposures to object exposures is
+generally done by selecting the nearest in time and interpolating.
+However, the optional \fIarc assignment table\fR may be used to explicitly
+assign arc images to specific objects.  The format of this file is
+described in the task \fBrefspectra\fR.
+.LP
+The final reduced spectra are recorded in one, two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ms" extension.  Each line in the reduced image is a one dimensional
+spectrum with associated aperture, wavelength, and identification
+information.  With a single object spectrum the image will be one dimensional
+and with multiple object spectra the image will be two dimensional.
+When the \f(CWextras\fR parameter is set the images will be three
+dimensional (regardless of the number of apertures) and the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tasks such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.
+.NH
+Package Parameters
+.LP
+The \fBkpnocoude\fR package parameters, shown in Figure 1, set parameters
+affecting all the tasks in the package.  Some of the parameters are not
+applicable to the \fBdo3fiber\fR task.
+.KS
+.V1
+
+.ce
+Figure 1: Package Parameters for KPNOCOUDE
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = imred
+   TASK = kpnocoude
+
+(extinct= onedstds$kpnoextinct.dat) Extinction file
+(caldir = onedstds$spec50cal/) Standard star calibration directory
+(observa=  observatory) Observatory of data
+(interp =        poly5) Interpolation type
+(dispaxi=            2) Image axis for 2D images
+(nsum   =            1) Number of lines/columns to sum for 2D images
+
+(databas=     database) Database
+(verbose=           no) Verbose output?
+(logfile=      logfile) Log file
+(plotfil=             ) Plot file
+
+(records=                     ) Record number extensions
+(version= KPNOCOUDE V3: January 1992)
+
+.KE
+.V2
+The observatory parameter is only required for data
+without an OBSERVAT header parameter (currently included in NOAO data).
+The spectrum interpolation type might be changed to "sinc" but with the
+cautions given in \fBonedspec.package\fR.  The dispersion axis parameter is
+only needed if a DISPAXIS image header parameter is not defined.  The other
+parameters define the standard I/O functions.  The verbose parameter
+selects whether to print everything which goes into the log file on the
+terminal.  It is useful for monitoring what the \fBdo3fiber\fR task does.  The
+log and plot files are useful for keeping a record of the processing.  A
+log file is highly recommended.  A plot file provides a record of
+apertures, traces, and extracted spectra but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+.NH
+Processing Parameters
+.LP
+The \fBdo3fiber\fR parameters are shown in Figure 2.
+.KS
+.V1
+
+.ce
+Figure 2: Parameter Set for DO3FIBER
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = kpnocoude
+   TASK = do3fiber
+
+objects =               List of object spectra
+(apref  =             ) Aperture reference spectrum
+(flat   =             ) Flat field spectrum
+(arcs   =             ) List of arc spectra
+(arctabl=             ) Arc assignment table (optional)
+
+.KE
+.V1
+(readnoi=      RDNOISE) Read out noise sigma (photons)
+(gain   =         GAIN) Photon gain (photons/data number)
+(datamax=        INDEF) Max data value / cosmic ray threshold
+(fibers =            3) Number of fibers
+(width  =           6.) Width of profiles (pixels)
+(crval  =        INDEF) Approximate wavelength
+(cdelt  =        INDEF) Approximate dispersion
+(objaps =            2) Object apertures
+(arcaps =          1,3) Arc apertures
+
+(scatter=           no) Subtract scattered light?
+(fitflat=          yes) Fit and ratio flat field spectrum?
+(recente=          yes) Recenter object apertures?
+(edit   =           no) Edit/review object apertures?
+(clean  =           no) Detect and replace bad pixels?
+(dispcor=          yes) Dispersion correct spectra?
+(splot  =          yes) Plot the final spectrum?
+(redo   =           no) Redo operations if previously done?
+(update =          yes) Update spectra if cal data changes?
+(batch  =           no) Extract objects in batch?
+(listonl=           no) List steps but don't process?
+
+(params =             ) Algorithm parameters
+
+.V2
+The input images are specified by image lists.  The lists may be
+a list of explicit, comma separate image names, @ files, or image
+templates using pattern matching against file names in the directory.
+The aperture reference spectrum is used to find the spectrum profiles and trace
+them.  Thus, this requires an image with good signal in all fibers
+which usually means a flat field spectrum.  It is recommended that
+flat field correction be done using one dimensional extracted spectra
+rather than as two dimensional images.  This is done if a flat field
+spectrum is specified.  The arc assignment table is used to specifically
+assign arc spectra to particular object spectra and the format
+of the file is described in \fBrefspectra\fR.
+.LP
+The detector read out noise and gain are used for cleaning and variance
+(optimal) extraction.
+The variance
+weighting and cosmic-ray cleanning are sensitive to extremely strong
+cosmic-rays; ones which are hundreds of times brighter than the
+spectrum.  The \fIdatamax\fR is used to set an upper limit for any
+real data.  Any pixels above this value will be flagged as cosmic-rays
+and will not affect the extractions.
+The dispersion axis defines the wavelength direction
+of spectra in the image if not defined in the image header by the keyword
+DISPAXIS.  The width parameter (in pixels) is used for the profile finding and
+centering algorithm (\fBcenter1d\fR).
+.LP
+The number of fibers is fairly obvious.  It is the number of
+fibers, including the arc fibers, to be automatically found and
+assigned apertures.  The apertures are assigned aperture
+numbers sequentially.  The object and arc fibers are identified
+by these aperture numbers as specified by the \f(CWobjaps\fR and
+\f(CWarcaps\fR parameters.  The defaults are for the case of three
+fibers in the sequence arc fiber, object fiber, and arc fiber.
+.LP
+The approximate central wavelength and dispersion are used for the
+automatic identification of the arc reference.  They may be specified
+as image header keywords or values.  The INDEF values search the
+entire range of the coordinate reference file but the automatic
+line identification algorithm works much better and faster if
+approximate values are given.
+.LP
+The next set of parameters select the processing steps and options.  The
+scattered light option allows fitting and subtracting a scattered light
+surface from the input object and flat field.  If there is significant
+scattered light which is not subtracted the fiber throughput correction
+will not be accurate.  The
+flat fitting option allows fitting and removing the overall shape of the
+flat field spectra while preserving the pixel-to-pixel response
+corrections.  This is useful for maintaining the approximate object count
+levels and not introducing the reciprocal of the flat field spectrum into
+the object spectra.
+.LP
+The apertures defined for the aperture reference image are assigned to
+each image.  For the object images the apertures may be shifted across
+the dispersion by recentering the strongest profiles and averaging
+the individual shifts to form a single shift for all apertures.  This
+corrects for shifts in the detector during the observations.  The
+\f(CWrecenter\fR parameter selects whether to apply this shift or not.
+.LP
+The \f(CWedit\fR option allows you to be queried to review the apertures
+assigned to each object image.  If selected and the query answered
+affirmatively the apertures may be interactively shifted and resized.  The
+query may also be answered with "NO" to turn off this option during
+processing.  Note that the initial aperture definitions for the aperture
+reference image always allows editing.
+.LP
+The \f(CWclean\fR option invokes a profile fitting and deviant
+point rejection algorithm as well as a variance weighting of points in the
+aperture.  These options require knowing the effective (i.e. accounting for
+any image combining) read out noise and gain.  For a discussion of cleaning
+and variance weighted extraction see \fBapvariance\fR and
+\fBapprofiles\fR.
+.LP
+The dispersion correction option selects whether to extract arc spectra,
+determine dispersion functions, assign them to the object spectra, and,
+possibly, resample the spectra to a linear (or log-linear) wavelength
+scale.
+.LP
+The \f(CWsplot\fR option allows a query (which may be answered with "YES"
+or "NO" to eliminate the query) and then plotting of the final object
+spectra if answered affirmatively.  The plotting is done with the
+task \fBsplot\fR.
+.LP
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\f(CWupdate\fR flag is set.  The changes which will cause an update are a new
+reference image, new flat field, and a new arc reference image.  If all
+input spectra are to be processed regardless of previous processing the
+\f(CWredo\fR flag may be used.  Note that reprocessing clobbers the
+previously processed output spectra.
+.LP
+The \f(CWbatch\fR processing option allows object spectra to be processed as
+a background or batch job.  This will only occur if the aperture editing
+and final spectrum plotting have been turned off, either with the task
+option parameter or by answering "NO" to the queries.  The \f(CWlistonly\fR
+option prints a summary of the processing steps which will be performed on
+the input spectra without actually doing anything.  This is useful for
+verifying which spectra will be affected if the input list contains
+previously processed spectra.  The listing does not include any arc spectra
+which may be extracted to dispersion calibrate an object spectrum.
+.LP
+The last parameter (excluding the task mode parameter) points to another
+parameter set for the algorithm parameters.  The way \fBdo3fiber\fR works
+this may not have any value and the parameter set \fBparams\fR is always
+used.  The algorithm parameters are discussed further in the next section.
+.NH
+Algorithms and Algorithm Parameters
+.LP
+This section summarizes the various algorithms used by the \fBdo3fiber\fR
+task and the parameters which control and modify the algorithms.  The
+algorithm parameters available to the user are collected in the parameter
+set \fBparams\fR.  These parameters are taken from the various general
+purpose tasks used by the \fBdo3fiber\fR processing task.  Additional
+information about these parameters and algorithms may be found in the help
+for the actual task executed.  These tasks are identified in the parameter
+section listing in parenthesis.  The aim of this parameter set organization
+is to collect all the algorithm parameters in one place separate from the
+processing parameters and include only those which are relevant for
+this type of data.  The parameter values can be changed from the
+defaults by using the parameter editor,
+.V1
+
+	cl> epar params
+
+.V2
+or simple typing \f(CWparams\fR.  The parameter editor can also be
+entered when editing the \fBdo3fiber\fR parameters by typing \f(CW:e
+params\fR or simply \f(CW:e\fR if positioned at the \f(CWparams\fR
+parameter.  Figure 3 shows the parameter set.
+.KS
+.V1
+
+.ce
+Figure 3: Algorithm Parameter Set
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = kpnocoude
+   TASK = params
+
+(line   =        INDEF) Default dispersion line
+(nsum   =           10) Number of dispersion lines to sum
+(extras =           no) Extract sky, sigma, etc.?
+
+                        -- DEFAULT APERTURE LIMITS --
+(lower  =          -3.) Lower aperture limit relative to center
+(upper  =           3.) Upper aperture limit relative to center
+
+                        -- AUTOMATIC APERTURE RESIZING PARAMETERS --
+(ylevel =         0.05) Fraction of peak or intensity for resizing
+
+.KE
+.KS
+.V1
+                        -- TRACE PARAMETERS --
+(t_step =           10) Tracing step
+(t_funct=      spline3) Trace fitting function
+(t_order=            2) Trace fitting function order
+(t_niter=            1) Trace rejection iterations
+(t_low  =           3.) Trace lower rejection sigma
+(t_high =           3.) Trace upper rejection sigma
+
+.KE
+.KS
+.V1
+                        -- SCATTERED LIGHT PARAMETERS --
+(buffer =           1.) Buffer distance from apertures
+(apscat1=             ) Fitting parameters across the dispersion
+(apscat2=             ) Fitting parameters along the dispersion
+
+.KE
+.KS
+.V1
+                        -- APERTURE EXTRACTION PARAMETERS --
+(weights=         none) Extraction weights (none|variance)
+(pfit   =        fit1d) Profile fitting algorithm (fit1d|fit2d)
+(lsigma =           3.) Lower rejection threshold
+(usigma =           3.) Upper rejection threshold
+(nsubaps=            1) Number of subapertures
+
+.KE
+.KS
+.V1
+                        -- FLAT FIELD FUNCTION FITTING PARAMETERS --
+(f_inter=          yes) Fit flat field interactively?
+(f_funct=      spline3) Fitting function
+(f_order=           20) Fitting function order
+
+.KE
+.KS
+.V1
+                        -- ARC DISPERSION FUNCTION PARAMETERS --
+(coordli= linelists$idhenear.dat) Line list
+(match  =          10.) Line list matching limit in Angstroms
+(fwidth =          3.5) Arc line widths in pixels
+(cradius=           4.) Centering radius in pixels
+(i_funct=     legendre) Coordinate function
+(i_order=            3) Order of dispersion function
+(i_niter=            3) Rejection iterations
+(i_low  =           3.) Lower rejection sigma
+(i_high =           3.) Upper rejection sigma
+(refit  =          yes) Refit coordinate function when reidentifying?
+(addfeat=           no) Add features when reidentifying?
+
+.KE
+.KS
+.V1
+                        -- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+(select =       interp) Selection method for reference spectra
+(sort   =           jd) Sort key
+(group  =          ljd) Group key
+(time   =           no) Is sort key a time?
+(timewra=          17.) Time wrap point for time sorting
+
+.KE
+.KS
+.V1
+                        -- DISPERSION CORRECTION PARAMETERS --
+(lineari=          yes) Linearize (interpolate) spectra?
+(log    =           no) Logarithmic wavelength scale?
+(flux   =          yes) Conserve flux?
+
+.KE
+.V2
+.NH 2
+Aperture Definitions
+.LP
+The first operation is to define the extraction apertures, which include
+the aperture width and position dependence with wavelength, for the object
+and arc fibers.  This is done on a reference spectrum which is usually a
+flat field taken through both fibers.  Other spectra will inherit the
+reference apertures and may apply a correction for any shift of the orders
+across the dispersion.  The reference apertures are defined only once
+unless the \f(CWredo\fR option is set.
+.LP
+The selected number of fibers are found automatically by selecting the
+highest peaks in a cut across the dispersion.  Apertures are assigned with
+a limits set by the \f(CWlower\fR and \f(CWupper\fR parameter and numbered
+sequentially.  A query is then given allowing the apertures to be reviewed
+interactively.  If answered affirmatively a cut across the orders is shown
+with the apertures marked and an interactive aperture editing mode is
+entered (see \fBapedit\fR).  The main thing to be concerned about is that
+the aperture numbers agree with the \f(CWobjaps\fR and \f(CWarcaps\fR
+definitions.  The aperture numbers may be changed with the 'i' or 'o'
+keys.  The apertures may also be resized from the default limits.
+To exit the background and aperture editing steps type 'q'.
+.LP
+Next the positions of the fiber profiles at various points along the
+dispersion are measured and a "trace function" is fit.  The user is asked
+whether to fit the trace function interactively.  This is selected to
+adjust the fitting parameters such as function type and order.  When
+interactively fitting a query is given for each aperture.  After the first
+aperture one may skip reviewing the other traces by responding with "NO".
+Queries made by \fBdo3fiber\fR generally may be answered with either lower
+case "yes" or "no" or with upper case "YES" or "NO".  The upper case
+responses apply to all further queries and so are used to eliminate further
+queries of that kind.
+.LP
+The above steps are all performed using tasks from the \fBapextract\fR
+package and parameters from the \fBparams\fR parameters.  As a quick
+summary, the dispersion direction of the spectra are determined from the
+package \fBdispaxis\fR parameter if not defined in the image header.  The default
+line or column for finding the orders and the number of image lines or
+columns to sum are set by the \f(CWline\fR and \f(CWnsum\fR parameters.  A line
+of INDEF (the default) selects the middle of the image.  The automatic
+finding algorithm is described for the task \fBapfind\fR and basically
+finds the strongest peaks.  The tracing is done as described in
+\fBaptrace\fR and consists of stepping along the image using the specified
+\f(CWt_step\fR parameter.  The function fitting uses the \fBicfit\fR commands
+with the other parameters from the tracing section.
+.NH 2
+Extraction
+.LP
+The actual extraction of the spectra is done by summing across the fixed
+width apertures at each point along the dispersion.  The default is to
+simply sum the pixels using partial pixels at the ends.  There is an
+option to weight the sum based on a Poisson noise model using the
+\f(CWreadnoise\fR and \f(CWgain\fR detector parameters.  Note that if the
+\f(CWclean\fR option is selected the variance weighted extraction is used
+regardless of the \f(CWweights\fR parameter.  The sigma thresholds for
+cleaning are also set in the \fBparams\fR parameters.
+.LP
+The cleaning and variance weighting options require knowing the effective
+(i.e. accounting for any image combining) read out noise and gain.  These
+numbers need to be adjusted if the image has been processed such that the
+intensity scale has a different origin (such as a background light
+subtraction) or scaling (such as caused by unnormalized flat fielding).
+For optimal extraction and cleaning to work it is recommended that the
+\f(CWfitflat\fR option be used.  For further discussion of cleaning and
+variance weighted extraction see \fBapvariance\fR and \fBapprofiles\fR as
+well as  \fBapsum\fR.
+.NH 2
+Scattered Light Subtraction
+.LP
+Scattered light may be subtracted from the input two dimensional image as
+the first step.  This is done using the algorithm described in
+\fBapscatter\fR.  This can be important if there is significant scattered
+light since the flat field/throughput correction will otherwise be
+incorrect.  The algorithm consists of fitting a function to the data
+outside the defined apertures by a specified \fIbuffer\fR at each line or
+column across the dispersion.  The function fitting parameters are the same
+at each line.  Because the fitted functions are independent at each line or
+column a second set of one dimensional functions are fit parallel to the
+dispersion using the evaluated fit values from the cross-dispersion step.
+This produces a smooth scattered light surface which is finally subtracted
+from the input image.  Again the function fitting parameters are the
+same at each line or column though they may be different than the parameters
+used to fit across the dispersion.
+.LP
+The first time the task is run with a particular flat field (or aperture
+reference image if no flat field is used) the scattered light fitting
+parameters are set interactively using that image.  The interactive step
+selects a particular line or column upon which the fitting is done
+interactively with the \fBicfit\fR commands.  A query is first issued
+which allows skipping this interactive stage.  Note that the interactive
+fitting is only for defining the fitting functions and orders.  When
+the graphical \fBicfit\fR fitting is exited (with 'q') there is a second prompt
+allowing you to change the buffer distance (in the first cross-dispersion
+stage) from the apertures, change the line/column, or finally quit.
+.LP
+The initial fitting parameters and the final set parameters are recorded
+in the \fBapscat1\fR and \fBapscat2\fR hidden parameter sets.  These
+parameters are then used automatically for every subsequent image
+which is scattered light corrected.
+.LP
+The scattered light subtraction modifies the input 2D images.  To preserve
+the original data a copy of the original image is made with the same
+root name and the word "noscat" appended.  The scattered light subtracted
+images will have the header keyword "APSCATTE" which is how the task
+avoids repeating the scattered light subtraction during any reprocessing.
+However if the \fIredo\fR option is selected the scattered light subtraction
+will also be redone by first restoring the "noscat" images to the original
+input names.
+.NH 2
+Flat Field Correction
+.LP
+Flat field corrections may be made during the basic CCD processing; i.e.
+direct division by the two dimensional flat field observation.  In that
+case do not specify a flat field spectrum; use the null string "".  The
+\fBdo3fiber\fR task provides an alternative flat field response correction
+based on division of the extracted object spectra by the extracted flat field
+spectra.  A discussion of the theory and merits of flat fielding directly
+verses using the extracted spectra will not be made here.  The
+\fBdo3fiber\fR flat fielding algorithm is the \fIrecommended\fR method for
+flat fielding since it works well and is not subject to the many problems
+involved in two dimensional flat fielding.
+.LP
+The first step is extraction of the flat field spectrum, if specified,
+using the reference apertures.  Only one flat field is allowed so if
+multiple flat fields are required the data must be reduced in groups.
+If the \f(CWfitflat\fR
+option is selected (the default) the extracted flat field spectra are
+averaged together and a smooth function is fit.  The default fitting
+function and order are given by the parameters \f(CWf_function\fR and
+\f(CWf_order\fR.  If the parameter \f(CWf_interactive\fR is "yes" then the
+fitting is done interactively using the \fBfit1d\fR task which uses the
+\fBicfit\fR interactive fitting commands.
+.LP
+The fitted function is divided into the individual flat field spectra to
+remove the basic shape of the spectrum while maintaining the relative
+individual pixel responses and any fiber to fiber differences.  This step
+avoids introducing the flat field spectrum shape into the object spectra
+and closely preserves the object counts.
+.LP
+The final step is to normalize the flat field spectra by the mean counts over
+all the fibers.  This normalization step is simply to preserve the average
+counts of the extracted object and arc spectra after division by the
+response spectra.
+.NH 2
+Dispersion Correction
+.LP
+If dispersion correction is not selected, \f(CWdispcor\fR=no, then the object
+spectra are simply extracted.  If it is selected the arc spectra are used
+to dispersion calibrate the object spectra.  There are four steps involved;
+determining the dispersion functions relating pixel position to wavelength,
+assigning the appropriate dispersion function to a particular observation,
+determining a zero point wavelength shift from the arc fibers to be applied
+to the object fiber dispersion functions, and either storing the nonlinear
+dispersion functions in the image headers or resampling the spectra to
+evenly spaced pixels in wavelength.
+.LP
+The first arc spectrum in the arc list is used to define the reference
+dispersion solution.  It is extracted using the reference aperture
+definitions.  The interactive task \fBautoidentify\fR is used to
+automatically define the dispersion function in one fiber.  Whether or not
+it is successful the user is presented with the interactive identification
+graph.  The automatic identifications can be reviewed and a new solution or
+corrections to the automatic solution may be performed.  The dispersion
+functions for the other fibers are then determined automatically by
+reference to the first fiber using the task \fBreidentify\fR.  Except in
+batch mode a query is given allowing the reidentified arc spectra to be
+examined interactively with \fBidentify\fR.  This would normally be done
+only if the information about the reidentification printed on the terminal
+indicates a problem such as a large increase in the RMS.  This query may be
+eliminated in the usual way.
+.LP
+The set of arc dispersion function parameters are from \fBidentify\fR and
+\fBreidentify\fR.  The parameters define a line list for use in
+automatically assigning wavelengths to arc lines, a parameter controlling
+the width of the centering window (which should match the base line
+widths), the dispersion function type and order, parameters to exclude bad
+lines from function fits, and parameters defining whether to refit the
+dispersion function, as opposed to simply determining a zero point shift,
+and the addition of new lines from the line list when reidentifying
+additional arc spectra.  The defaults should generally be adequate and the
+dispersion function fitting parameters may be altered interactively.  One
+should consult the help for the two tasks for additional details of these
+parameters and the operation of \fBidentify\fR.
+.LP
+If resampling of the spectra is selected by the parameter \f(CWlinearize\fR
+all the arc dispersion functions are combined to provide a default
+starting and ending wavelength and dispersion with the same number of
+pixels is determined and the user is queried for any changes.  This
+linear dispersion system will be applied to all spectra so that all
+the final processed object spectra will have the same dispersion
+sampling.
+.LP
+Once the reference dispersion functions are defined other arc spectra are
+extracted as they are assign to the object spectra.  The assignment of
+arcs is done either explicitly with an arc assignment table (parameter
+\f(CWarctable\fR) or based on a header parameter such as a time.
+The assignments are made by the task \fBrefspectra\fR.  When two arcs are
+assigned to an object spectrum an interpolation is done between the two
+dispersion functions.  This makes an approximate correction for steady
+drifts in the dispersion.  Because the arc fibers monitor any zero point
+shifts in the dispersion functions, due to translation and rotation of the
+detector, it is probably only necessary to have one or two arc spectra, one
+at the beginning and/or one at the end of the night.
+.LP
+The tasks \fBsetjd\fR and \fBsetairmass\fR are automatically run on all
+spectra.  This computes and adds the header parameters for the Julian date
+(JD), the local Julian day number (LJD), the universal time (UTMIDDLE), and
+the air mass at the middle of the exposure.  The default arc assignment is
+to use the Julian date grouped by the local Julian day number.  The
+grouping allows multiple nights of data to be correctly assigned at the
+same time.
+.LP
+When the object spectra are extracted so are the simultaneous arc spectra.
+A zero point shift of the arc spectra relative to the dispersion solutions
+of an assigned full arc observation is computed using \fBreidentify\fR.
+The zero point shifts from the arc fibers are then
+interpolated across the detector based on the positions of the arc
+apertures to the positions of the object apertures.  A linear interpolation
+is used which accounts for a rotation of the detector as well as a
+translation along the dispersion.  The interpolated zero point wavelength
+shifts are then added to the dispersion functions from the full arc
+observation for the object fibers.  Note that this does not assume that the
+object and arc fiber dispersion functions are the same or have the same
+wavelength origin, but only that the interpolated shifts in wavelength zero
+point apply to all fibers.  When there are two assigned full arc spectra
+the above steps are done independently and the final pair of zero point
+corrected dispersion functions for each object fiber are combined using the
+assigned weights.  Once the dispersion function correction is determined
+from the extracted arc fiber spectra they are deleted leaving only the
+object spectra.
+.LP
+The last step of dispersion correction is setting the dispersion
+of the object spectra.  There are two choices here.
+If the \f(CWlinearize\fR parameter is not set the nonlinear dispersion
+functions are stored in the image header.  Other IRAF tasks interpret
+this information when dispersion coordinates are needed for plotting
+or analysis.  This has the advantage of not requiring the spectra
+to be interpolated and the disadvantage that the dispersion
+information is only understood by IRAF tasks and cannot be readily
+exported to other analysis software.
+.LP
+If the \f(CWlinearize\fR parameter is set then the spectra are resampled to a
+linear dispersion relation either in wavelength or the log of the
+wavelength.  The linear dispersion parameters are those defined
+previously for the arc reference image.
+.LP
+The linearization algorithm  parameters allow selecting the interpolation
+function type, whether to conserve flux per pixel by integrating across the
+extent of the final pixel, and whether to linearize to equal linear or
+logarithmic intervals.  The latter may be appropriate for radial velocity
+studies.  The default is to use a fifth order polynomial for interpolation,
+to conserve flux, and to not use logarithmic wavelength bins.  These
+parameters are described fully in the help for the task \fBdispcor\fR which
+performs the correction.
+.NH
+References
+.NH 2
+IRAF Introductory References
+.LP
+Work is underway on a new introductory guide to IRAF.  Currently, the
+work below is the primary introduction.
+.IP
+P. Shames and D. Tody, \fIA User's Introduction to the IRAF Command
+Language\fR, Central Computer Services, NOAO, 1986.
+.NH 2
+CCD Reductions
+.IP
+F. Valdes, \fIThe IRAF CCD Reduction Package -- CCDRED\fR, Central
+Computer Services, NOAO, 1987.
+.IP
+F. Valdes, \fIUser's Guide to the CCDRED Package\fR, Central
+Computer Services, NOAO, 1988.  Also on-line as \f(CWhelp ccdred.guide\fR.
+.IP
+P. Massey, \fIA User's Guide to CCD Reductions with IRAF\fR, Central
+Computer Services, NOAO, 1989.
+.NH 2
+Aperture Extraction Package
+.IP
+F. Valdes, \fIThe IRAF APEXTRACT Package\fR, Central Computer Services,
+NOAO, 1987 (out-of-date).
+.NH 2
+Task Help References
+.LP
+Each task in the \fBspecred\fR packages and tasks used by \fBdofibers\fR have
+help pages describing the parameters and task in some detail.  To get
+on-line help type
+.V1
+
+cl> help \fItaskname\fR
+
+.V2
+The output of this command can be piped to \fBlprint\fR to make a printed
+copy.
+
+.V1
+      apall - Extract 1D spectra (all parameters in one task)
+  apdefault - Set the default aperture parameters
+     apedit - Edit apertures interactively
+     apfind - Automatically find spectra and define apertures
+ aprecenter - Recenter apertures
+   apresize - Resize apertures
+      apsum - Extract 1D spectra
+    aptrace - Trace positions of spectra
+
+      bplot - Batch plot of spectra with SPLOT
+  calibrate - Apply extinction and flux calibrations to spectra
+  continuum - Fit and normalize the continuum of multispec spectra
+   deredden - Apply interstellar extinction corrections
+    dispcor - Dispersion correct spectra
+     dopcor - Doppler correct spectra
+   identify - Identify arc lines and determine a dispersion function
+   msresp1d - Create fiber response spectra from flat field and sky spectra
+ refspectra - Assign reference spectra to observations
+ reidentify - Reidentify arc lines and determine new dispersion functions
+ sapertures - Set or change aperture header information
+     sarith - Spectrum arithmetic
+   scombine - Combine spectra
+      scopy - Copy spectra including aperture selection and format changes
+   sensfunc - Create sensitivity function
+ setairmass - Compute effective airmass and middle UT for an exposure
+      setjd - Compute and set Julian dates in images
+      slist - List spectrum headers
+   specplot - Stack and plot multiple spectra
+      splot - Plot and analyze spectra
+   standard - Identify standard stars to be used in sensitivity calc
+
+   do3fiber - Process KPNO coude three fiber spectra
+      demos - Demonstrations and tests
+
+            Additional help topics
+
+   onedspec.package - Package parameters and general description of package
+  apextract.package - Package parameters and general description of package
+ approfiles - Profile determination algorithms
+ apvariance - Extractions, variance weighting, cleaning, and noise model
+   center1d - One dimensional centering algorithm
+      icfit - Interactive one dimensional curve fitting
+.V2
+.SH
+Appendix A: DO3FIBER Parameters
+.LP
+.nr PS 8
+.nr VS 10
+objects
+.LS
+List of object spectra to be processed.  Previously processed spectra are
+ignored unless the \f(CWredo\fR flag is set or the \f(CWupdate\fR flag is set and
+dependent calibration data has changed.  Extracted spectra are ignored.
+.LE
+apref = ""
+.LS
+Aperture reference spectrum.  This spectrum is used to define the basic
+extraction apertures and is typically a flat field spectrum.
+.LE
+flat = "" (optional)
+.LS
+Flat field spectrum.  If specified the one dimensional flat field spectra
+are extracted and used to make flat field corrections.
+.LE
+arcs = "" (at least one if dispersion correcting)
+.LS
+List of primary, all fiber arc spectra.  These spectra are used to define
+the dispersion functions for each fiber apart from a possible zero point
+correction made with simultaneous arc calibration fibers in the object
+spectra.  One fiber from the first spectrum is used to mark lines and set
+the dispersion function interactively and dispersion functions for all
+other fibers and arc spectra are derived from it.
+.LE
+arctable = "" (optional) (refspectra)
+.LS
+Table defining arc spectra to be assigned to object
+spectra (see \fBrefspectra\fR).  If not specified an assignment based
+on a header parameter, \f(CWparams.sort\fR, such as the observation time is made.
+.LE
+
+readnoise = "RDNOISE" (apsum)
+.LS
+Read out noise in photons.  This parameter defines the minimum noise
+sigma.  It is defined in terms of photons (or electrons) and scales
+to the data values through the gain parameter.  A image header keyword
+(case insensitive) may be specified to get the value from the image.
+.LE
+gain = "GAIN" (apsum)
+.LS
+Detector gain or conversion factor between photons/electrons and
+data values.  It is specified as the number of photons per data value.
+A image header keyword (case insensitive) may be specified to get the value
+from the image.
+.LE
+datamax = INDEF (apsum.saturation)
+.LS
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the flat field or
+arc spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.LE
+fibers = 3 (apfind)
+.LS
+Number of fibers.  This number is used during the automatic definition of
+the apertures from the aperture reference spectrum.
+.LE
+width = 6. (apedit)
+.LS
+Approximate base full width of the fiber profiles.  This parameter is used
+for the profile centering algorithm.
+.LE
+crval = INDEF, cdelt = INDEF (autoidentify)
+.LS
+These parameters specify an approximate central wavelength and dispersion.
+They may be specified as numerical values, INDEF, or image header keyword
+names whose values are to be used.  If one or both of these parameters are
+specified as INDEF the search for a solution will be slower and more likely
+to fail.
+.LE
+objaps = "2", arcaps = "1,3"
+.LS
+List of object and arc aperture numbers.  These are used to
+identify arc apertures for wavelength calibration and object apertures
+for the final results.
+.LE
+
+scattered = no (apscatter)
+.LS
+Smooth and subtracted scattered light from the object and flat field
+images.  This operation consists of fitting independent smooth functions
+across the dispersion using data outside the fiber apertures and then
+smoothing the individual fits along the dispersion.  The initial
+flat field, or if none is given the aperture reference image, are
+done interactively to allow setting the fitting parameters.  All
+subsequent subtractions use the same fitting parameters.
+.LE
+fitflat = yes (flat1d)
+.LS
+Fit the composite flat field spectrum by a smooth function and divide each
+flat field spectrum by this function?  This operation removes the average
+spectral signature of the flat field lamp from the sensitivity correction to
+avoid modifying the object fluxes.
+.LE
+recenter = yes (aprecenter)
+.LS
+Recenter reference apertures for each object spectrum?
+.LE
+edit = no (apedit)
+.LS
+Review aperture definitions for each object spectrum?  Note that this does
+not apply to the initial reference aperture which always allows
+interactive review of the aperture definitions.
+.LE
+clean = no (apsum)
+.LS
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction and requires reasonably good values
+for the readout noise and gain.  In addition the datamax parameters
+can be useful.
+.LE
+dispcor = yes
+.LS
+Dispersion correct spectra?  Depending on the \f(CWparams.linearize\fR
+parameter this may either resample the spectra or insert a dispersion
+function in the image header.
+.LE
+splot = yes
+.LS
+Plot the final spectra with the task \fBsplot\fR?
+.LE
+redo = no
+.LS
+Redo operations previously done?  If no then previously processed spectra
+in the objects list will not be processed (unless they need to be updated).
+.LE
+update = yes
+.LS
+Update processing of previously processed spectra if aperture, flat
+field, or dispersion reference definitions are changed?
+.LE
+batch = no
+.LS
+Process spectra as a background or batch job provided there are no interactive
+options (\f(CWedit\fR and \f(CWsplot\fR) selected.
+.LE
+listonly = no
+.LS
+List processing steps but don't process?
+.LE
+
+params = "" (pset)
+.LS
+Name of parameter set containing additional processing parameters.  The
+default is parameter set \fBparams\fR.  The parameter set may be examined
+and modified in the usual ways (typically with "epar params" or ":e params"
+from the parameter editor).  Note that using a different parameter file
+is not allowed.  The parameters are described below.
+.LE
+
+.ce
+-- PACKAGE PARAMETERS
+
+Package parameters are those which generally apply to all task in the
+package.  This is also true of \fBdo3fiber\fR.
+
+observatory = "observatory"
+.LS
+Observatory at which the spectra were obtained if not specified in the
+image header by the keyword OBSERVAT.  For NOAO data the image headers
+identify the observatory as "kpno" or "ctio" so this parameter is not used.
+For data from other observatories this parameter may be used
+as describe in \fBobservatory\fR.
+.LE
+interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc)
+.LS
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.V1
+	nearest - nearest neighbor
+	 linear - linear
+	  poly3 - 3rd order polynomial
+	  poly5 - 5th order polynomial
+	spline3 - cubic spline
+	   sinc - sinc function
+.V2
+.LE
+dispaxis = 2
+.LS
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.
+.LE
+database = "database"
+.LS
+Database (directory) used for storing aperture and dispersion information.
+.LE
+verbose = no
+.LS
+Print verbose information available with various tasks.
+.LE
+logfile = "logfile", plotfile = ""
+.LS
+Text and plot log files.  If a filename is not specified then no log is
+kept.  The plot file contains IRAF graphics metacode which may be examined
+in various ways such as with \fBgkimosaic\fR.
+.LE
+records = ""
+.LS
+Dummy parameter to be ignored.
+.LE
+version = "KPNOCOUDE: ..."
+.LS
+Version of the package.
+.LE
+
+.ce
+PARAMS PARAMETERS
+
+The following parameters are part of the \fBparams\fR parameter set and
+define various algorithm parameters for \fBdo3fiber\fR.
+
+.ce
+--  GENERAL PARAMETERS --
+
+line = INDEF, nsum = 10
+.LS
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, recentering, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.LE
+extras = no (apsum)
+.LS
+Include extra information in the output spectra?  When cleaning or using
+variance weighting the cleaned and weighted spectra are recorded in the
+first 2D plane of a 3D image, the raw, simple sum spectra are recorded in
+the second plane, and the estimated sigmas are recorded in the third plane.
+.LE
+
+.ce
+-- DEFAULT APERTURE LIMITS --
+
+lower = -3., upper = 3. (apdefault)
+.LS
+Default lower and upper aperture limits relative to the aperture center.
+These limits are used when the apertures are first found and may be
+resized automatically or interactively.
+.LE
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+
+ylevel = 0.05 (apresize)
+.LS
+Data level at which to set aperture limits during automatic resizing.
+It is a fraction of the peak relative to a local background.
+.LE
+
+.ce
+-- TRACE PARAMETERS --
+
+t_step = 10 (aptrace)
+.LS
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \f(CWnsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.LE
+t_function = "spline3", t_order = 2 (aptrace)
+.LS
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.LE
+t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+.LS
+Default number of rejection iterations and rejection sigma thresholds.
+.LE
+
+.ce
+-- SCATTERED LIGHT PARAMETERS --
+
+buffer = 1. (apscatter)
+.LS
+Buffer distance from the aperture edges to be excluded in selecting the
+scattered light pixels to be used.
+.LE
+apscat1 = "" (apscatter)
+.LS
+Fitting parameters across the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat1"
+parameter set.
+.LE
+apscat2 = "" (apscatter)
+.LS
+Fitting parameters along the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat2"
+parameter set.
+.LE
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+
+weights = "none" (apsum)
+.LS
+Type of extraction weighting.  Note that if the \f(CWclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+
+"none"
+.LS
+The pixels are summed without weights except for partial pixels at the
+ends.
+.LE
+"variance"
+.LS
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \f(CWgain\fR and \f(CWreadnoise\fR
+parameters.
+.LE
+.LE
+pfit = "fit1d" (apsum) (fit1d|fit2d)
+.LS
+Profile fitting algorithm for cleaning and variance weighted extractions.
+The default is generally appropriate for most data but users
+may try the other algorithm.  See \fBapprofiles\fR for further information.
+.LE
+lsigma = 3., usigma = 3. (apsum)
+.LS
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.LE
+nsubaps = 1 (apsum)
+.LS
+During extraction it is possible to equally divide the apertures into
+this number of subapertures.
+.LE
+
+.ce
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --
+
+f_interactive = yes (fit1d)
+.LS
+Fit the composite one dimensional flat field spectrum interactively?
+This is used if \f(CWfitflat\fR is set and a two dimensional flat field
+spectrum is specified.
+.LE
+f_function = "spline3", f_order = 20 (fit1d)
+.LS
+Function and order used to fit the composite one dimensional flat field
+spectrum.  The functions are "legendre", "chebyshev", "spline1", and
+"spline3".  The spline functions are linear and cubic splines with the
+order specifying the number of pieces.
+.LE
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+
+threshold = 10. (autoidentify/identify/reidentify)
+.LS
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.LE
+coordlist = "linelists$idhenear.dat" (autoidentify/identify)
+.LS
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelists$".
+.LE
+match = -3. (autoidentify/identify)
+.LS
+The maximum difference for a match between the dispersion function prediction
+value and a wavelength in the coordinate list.
+.LE
+fwidth = 3.5 (autoidentify/identify)
+.LS
+Approximate full base width (in pixels) of arc lines.
+.LE
+cradius = 4. (reidentify)
+.LS
+Radius from previous position to reidentify arc line.
+.LE
+i_function = "legendre", i_order = 3 (autoidentify/identify)
+.LS
+The default function and order to be fit to the arc wavelengths as a
+function of the pixel coordinate.  The functions choices are "chebyshev",
+"legendre", "spline1", or "spline3".
+.LE
+i_niterate = 3, i_low = 3.0, i_high = 3.0 (autoidentify/identify)
+.LS
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.LE
+refit = yes (reidentify)
+.LS
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.LE
+addfeatures = no (reidentify)
+.LS
+Add new features from a line list during each reidentification?
+This option can be used to compensate for lost features from the
+reference solution.  Care should be exercised that misidentified features
+are not introduced.
+.LE
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+
+select = "interp" (refspectra)
+.LS
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+
+average
+.LS
+Average two reference spectra without regard to any sort parameter.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.
+This option is used to assign two reference spectra, with equal weights,
+independent of any sorting parameter.
+.LE
+following
+.LS
+Select the nearest following spectrum in the reference list based on the
+sorting parameter.  If there is no following spectrum use the nearest preceding
+spectrum.
+.LE
+interp
+.LS
+Interpolate between the preceding and following spectra in the reference
+list based on the sorting parameter.  If there is no preceding and following
+spectrum use the nearest spectrum.  The interpolation is weighted by the
+relative distances of the sorting parameter.
+.LE
+match
+.LS
+Match each input spectrum with the reference spectrum list in order.
+This overrides the reference aperture check.
+.LE
+nearest
+.LS
+Select the nearest spectrum in the reference list based on the sorting
+parameter.
+.LE
+preceding
+.LS
+Select the nearest preceding spectrum in the reference list based on the
+sorting parameter.  If there is no preceding spectrum use the nearest following
+spectrum.
+.LE
+.LE
+sort = "jd", group = "ljd" (refspectra)
+.LS
+Image header keywords to be used as the sorting parameter for selection
+based on order and to group spectra.
+A null string, "", or the word "none" may be use to disable the sorting
+or grouping parameters.
+The sorting parameter
+must be numeric but otherwise may be anything.  The grouping parameter
+may be a string or number and must simply be the same for all spectra within
+the same group (say a single night).
+Common sorting parameters are times or positions.
+In \fBdo3fiber\fR the Julian date (JD) and the local Julian day number (LJD)
+at the middle of the exposure are automatically computed from the universal
+time at the beginning of the exposure and the exposure time.  Also the
+parameter UTMIDDLE is computed.
+.LE
+time = no, timewrap = 17. (refspectra)
+.LS
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.LE
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+
+linearize = yes (dispcor)
+.LS
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling
+If no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data are not interpolated.
+.LE
+log = no (dispcor)
+.LS
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.LE
+flux = yes (dispcor)
+.LS
+Conserve the total flux during interpolation?  If \f(CWno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \f(CWyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.LE
+
+.ce
+ENVIRONMENT PARAMETERS
+.LP
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
diff --git a/noao/imred/kpnocoude/identify.par b/noao/imred/kpnocoude/identify.par
new file mode 100644
index 00000000..4aec4ad2
--- /dev/null
+++ b/noao/imred/kpnocoude/identify.par
@@ -0,0 +1,33 @@
+# Parameters for identify task.
+
+images,s,a,,,,Images containing features to be identified
+section,s,h,"middle line",,,Section to apply to two dimensional images
+database,f,h,database,,,Database in which to record feature data
+coordlist,f,h,linelists$thar.dat,,,User coordinate list
+units,s,h,"",,,Coordinate units
+nsum,s,h,"1",,,Number of lines/columns/bands to sum in 2D images
+match,r,h,0.2.,,,Coordinate list matching limit
+maxfeatures,i,h,100,,,Maximum number of features for automatic identification
+zwidth,r,h,100.,,,Zoom graph width in user units
+
+ftype,s,h,"emission","emission|absorption",,Feature type
+fwidth,r,h,3.5,,,Feature width in pixels
+cradius,r,h,4.,,,Centering radius in pixels
+threshold,r,h,10.,0.,,Feature threshold for centering
+minsep,r,h,4.,0.,,Minimum pixel separation
+
+function,s,h,"legendre","legendre|chebyshev|spline1|spline3",,Coordinate function
+order,i,h,3,1,,Order of coordinate function
+sample,s,h,"*",,,Coordinate sample regions
+niterate,i,h,3,0,,Rejection iterations
+low_reject,r,h,3.,0.,,Lower rejection sigma
+high_reject,r,h,3.,0.,,Upper rejection sigma
+grow,r,h,0.,0.,,Rejection growing radius
+
+autowrite,b,h,no,,,"Automatically write to database"
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+
+crval,s,q,,,,"Approximate coordinate (at reference pixel)"
+cdelt,s,q,,,,"Approximate dispersion"
+aidpars,pset,h,,,,"Automatic identification algorithm parameters"
diff --git a/noao/imred/kpnocoude/kpnocoude.cl b/noao/imred/kpnocoude/kpnocoude.cl
new file mode 100644
index 00000000..60b45595
--- /dev/null
+++ b/noao/imred/kpnocoude/kpnocoude.cl
@@ -0,0 +1,98 @@
+#{ KPNOCOUDE package definition
+
+proto		# bscale
+
+s1 = envget ("min_lenuserarea")
+if (s1 == "")
+    reset min_lenuserarea = 100000
+else if (int (s1) < 100000)
+    reset min_lenuserarea = 100000
+
+# Define KPNOCOUDE package
+package kpnocoude
+
+set	demos		= "kpnocoude$demos/"
+
+# Slitproc
+cl < doslit$doslittasks.cl
+task	sparams		= "kpnocoude$sparams.par"
+
+# Dofibers
+task	do3fiber	= "kpnocoude$do3fiber.cl"
+task	params		= "kpnocoude$params.par"
+
+task	proc		= "srcfibers$proc.cl"
+task	fibresponse	= "srcfibers$fibresponse.cl"
+task	arcrefs		= "srcfibers$arcrefs.cl"
+task	doarcs		= "srcfibers$doarcs.cl"
+task	doalign		= "srcfibers$doalign.cl"
+task	skysub		= "srcfibers$skysub.cl"
+task	batch		= "srcfibers$batch.cl"
+task	getspec		= "srcfibers$getspec.cl"
+task	listonly	= "srcfibers$listonly.cl"
+task	mkfibers	= "srcfibers$mkfibers.cl"
+task	apscript	= "srcfibers$x_apextract.e"
+
+task	msresp1d	= "specred$msresp1d.cl"
+
+# Onedspec tasks
+task	autoidentify,
+	continuum,
+	deredden,
+	dispcor,
+	dopcor,
+	refspectra,
+	sapertures,
+	sarith,
+	sflip,
+	slist,
+	specplot,
+	specshift,
+	splot		= "onedspec$x_onedspec.e"
+task	scombine	= "onedspec$scombine/x_scombine.e"
+task	aidpars		= "onedspec$aidpars.par"
+task	bplot		= "onedspec$bplot.cl"
+task	scopy		= "onedspec$scopy.cl"
+task	dispcor1	= "onedspec$dispcor1.par"
+
+# Different default parameters
+task	calibrate,
+	identify,
+	reidentify,
+	sensfunc,
+	standard	= "kpnocoude$x_onedspec.e"
+
+# Apextract tasks
+task	apall,
+	apedit,
+	apfind,
+	apflatten,
+	apnormalize,
+	aprecenter,
+	apresize,
+	apsum,
+	aptrace		= "apextract$x_apextract.e"
+task	apdefault	= "apextract$apdefault.par"
+task	apparams	= "apextract$apparams.par"
+task	apall1		= "apextract$apall1.par"
+task	apflat1		= "apextract$apflat1.par"
+task	apnorm1		= "apextract$apnorm1.par"
+
+# Longslit tasks
+task	illumination,
+	response	= "twodspec$longslit/x_longslit.e"
+task	background	= "generic$background.cl"
+
+# Astutil tasks
+task	setairmass,
+	setjd		= "astutil$x_astutil.e"
+
+# Demos
+task	demos		= "demos$demos.cl"
+
+# Hide tasks from the user
+hidetask apparams, apall1, apflat1, apnorm1, dispcor1, sparams
+hidetask mkfibers, params, doalign
+hidetask apscript, proc, batch, arcrefs, doarcs, getspec, listonly, fibresponse
+
+clbye
diff --git a/noao/imred/kpnocoude/kpnocoude.hd b/noao/imred/kpnocoude/kpnocoude.hd
new file mode 100644
index 00000000..71d12a4d
--- /dev/null
+++ b/noao/imred/kpnocoude/kpnocoude.hd
@@ -0,0 +1,5 @@
+# Help directory for the KPNOCOUDE package.
+
+$doc		 = "./doc/"
+
+do3fiber	hlp=doc$do3fiber.hlp
diff --git a/noao/imred/kpnocoude/kpnocoude.men b/noao/imred/kpnocoude/kpnocoude.men
new file mode 100644
index 00000000..a5f29a3a
--- /dev/null
+++ b/noao/imred/kpnocoude/kpnocoude.men
@@ -0,0 +1,41 @@
+          apall - Extract 1D spectra (all parameters in one task)
+      apdefault - Set the default aperture parameters
+         apedit - Edit apertures interactively
+	 apfind - Automatically find spectra and define apertures
+      apflatten - Remove overall spectral and profile shapes from flat fields
+    apnormalize - Normalize 2D apertures by 1D functions
+     aprecenter - Recenter apertures
+       apresize - Resize apertures
+          apsum - Extract 1D spectra
+	aptrace - Trace positions of spectra
+
+     background - Fit and subtract a line or column background
+	  bplot - Batch plot of spectra with SPLOT
+      calibrate - Apply extinction and flux calibrations to spectra
+      continuum - Fit and normalize the continuum of multispec spectra
+       deredden - Apply interstellar extinction corrections
+        dispcor - Dispersion correct spectra
+	 dopcor - Doppler correct spectra
+       identify - Identify arc lines and determine a dispersion function
+   illumination - Determine illumination calibration
+       msresp1d - Create fiber response spectra from flat field and sky spectra
+     refspectra - Assign reference spectra to observations
+     reidentify - Reidentify arc lines and determine new dispersion functions
+       response - Determine response calibration
+     sapertures - Set or change aperture header information
+	 sarith - Spectrum arithmetic
+       scombine - Combine spectra
+          scopy - Copy spectra including aperture selection and format changes
+       sensfunc - Create sensitivity function
+     setairmass - Compute effective airmass and middle UT for an exposure
+          setjd - Compute and set Julian dates in images
+	  sflip - Flip data and/or dispersion coordinates in spectra
+          slist - List spectrum headers
+       specplot - Stack and plot multiple spectra
+      specshift - Shift spectral dispersion coordinate systems
+	  splot - Plot and analyze spectra
+       standard - Identify standard stars to be used in sensitivity calc
+
+       do3fiber - Process KPNO coude three fiber spectra
+         doslit - Process KPNO coude slit spectra
+	  demos - Demonstrations and tests
diff --git a/noao/imred/kpnocoude/kpnocoude.par b/noao/imred/kpnocoude/kpnocoude.par
new file mode 100644
index 00000000..b653f211
--- /dev/null
+++ b/noao/imred/kpnocoude/kpnocoude.par
@@ -0,0 +1,15 @@
+# KPNOCOUDE parameter file
+extinction,s,h,onedstds$kpnoextinct.dat,,,Extinction file
+caldir,s,h,onedstds$spec50cal/,,,Standard star calibration directory
+observatory,s,h,"observatory",,,Observatory of data
+interp,s,h,"poly5","nearest|linear|poly3|poly5|spline3|sinc",,Interpolation type
+dispaxis,i,h,2,1,3,Image axis for 2D/3D images
+nsum,s,h,"1",,,"Number of lines/columns/bands to sum for 2D/3D images
+"
+database,f,h,"database",,,Database
+verbose,b,h,no,,,Verbose output?
+logfile,s,h,"logfile",,,Log file
+plotfile,s,h,"",,,"Plot file
+"
+records,s,h,"",,,Record number extensions
+version,s,h,"KPNOCOUDE V3: January 1992"
diff --git a/noao/imred/kpnocoude/params.par b/noao/imred/kpnocoude/params.par
new file mode 100644
index 00000000..239a0efd
--- /dev/null
+++ b/noao/imred/kpnocoude/params.par
@@ -0,0 +1,61 @@
+line,i,h,INDEF,,,Default dispersion line
+nsum,i,h,10,,,"Number of dispersion lines to sum or median"
+extras,b,h,no,,,"Extract sky, sigma, etc.?
+
+-- DEFAULT APERTURE LIMITS --"
+lower,r,h,-3.,,,"Lower aperture limit relative to center"
+upper,r,h,3.,,,"Upper aperture limit relative to center
+
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --"
+ylevel,r,h,0.05,,,"Fraction of peak or intensity for resizing
+
+-- TRACE PARAMETERS --"
+t_step,i,h,10,,,"Tracing step"
+t_function,s,h,"spline3","chebyshev|legendre|spline1|spline3",,"Trace fitting function"
+t_order,i,h,2,,,"Trace fitting function order"
+t_niterate,i,h,1,0,,"Trace rejection iterations"
+t_low,r,h,3.,0.,,"Trace lower rejection sigma"
+t_high,r,h,3.,0.,,"Trace upper rejection sigma
+
+-- SCATTERED LIGHT PARAMETERS --"
+buffer,r,h,1.,0.,,Buffer distance from apertures
+apscat1,pset,h,"",,,Fitting parameters across the dispersion
+apscat2,pset,h,"",,,"Fitting parameters along the dispersion
+
+-- APERTURE EXTRACTION PARAMETERS --"
+weights,s,h,"none","none|variance",,Extraction weights (none|variance)
+pfit,s,h,"fit1d","fit1d|fit2d",,Profile fitting algorithm (fit1d|fit2d)
+lsigma,r,h,3.,,,Lower rejection threshold
+usigma,r,h,3.,,,Upper rejection threshold
+nsubaps,i,h,1,1,,"Number of subapertures
+
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --"
+f_interactive,b,h,yes,,,"Fit flat field interactively?"
+f_function,s,h,"spline3",spline3|legendre|chebyshev|spline1,,"Fitting function"
+f_order,i,h,20,1,,"Fitting function order
+
+-- ARC DISPERSION FUNCTION PARAMETERS --"
+threshold,r,h,10.,0.,,"Minimum line contrast threshold"
+coordlist,f,h,linelists$thar.dat,,,"Line list"
+match,r,h,-3.,,,"Line list matching limit in Angstroms"
+fwidth,r,h,3.5,,,"Arc line widths in pixels"
+cradius,r,h,4.,,,Centering radius in pixels
+i_function,s,h,"legendre","legendre|chebyshev|spline1|spline3",,"Coordinate function"
+i_order,i,h,3,1,,"Order of dispersion function"
+i_niterate,i,h,3,0,,"Rejection iterations"
+i_low,r,h,3.,0.,,"Lower rejection sigma"
+i_high,r,h,3.,0.,,"Upper rejection sigma"
+refit,b,h,yes,,,"Refit coordinate function when reidentifying?"
+addfeatures,b,h,no,,,"Add features when reidentifying?
+
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --"
+select,s,h,"interp",,,"Selection method for reference spectra"
+sort,s,h,"jd",,,"Sort key"
+group,s,h,"ljd",,,"Group key"
+time,b,h,no,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting
+
+-- DISPERSION CORRECTION PARAMETERS --"
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+log,b,h,no,,,"Logarithmic wavelength scale?"
+flux,b,h,yes,,,"Conserve flux?"
diff --git a/noao/imred/kpnocoude/reidentify.par b/noao/imred/kpnocoude/reidentify.par
new file mode 100644
index 00000000..74d57b7f
--- /dev/null
+++ b/noao/imred/kpnocoude/reidentify.par
@@ -0,0 +1,36 @@
+# Parameters for reidentify task.
+
+reference,s,a,,,,Reference image
+images,s,a,,,,Images to be reidentified
+interactive,s,h,"no","no|yes|NO|YES",,Interactive fitting?
+section,s,h,"middle line",,,Section to apply to two dimensional images
+newaps,b,h,yes,,,Reidentify apertures in images not in reference?
+override,b,h,no,,,Override previous solutions?
+refit,b,h,yes,,,"Refit coordinate function?
+"
+trace,b,h,no,,,Trace reference image?
+step,s,h,"10",,,Step in lines/columns/bands for tracing an image
+nsum,s,h,"10",,,Number of lines/columns/bands to sum
+shift,s,h,"0.",,,Shift to add to reference features (INDEF to search)
+search,r,h,0.,,,Search radius
+nlost,i,h,3,0,,"Maximum number of features which may be lost
+"
+cradius,r,h,5.,,,Centering radius
+threshold,r,h,10.,0.,,Feature threshold for centering
+addfeatures,b,h,no,,,Add features from a line list?
+coordlist,f,h,linelists$thar.dat,,,User coordinate list
+match,r,h,0.2,,,Coordinate list matching limit
+maxfeatures,i,h,100,,,Maximum number of features for automatic identification
+minsep,r,h,4.,0.,,"Minimum pixel separation
+"
+database,f,h,database,,,Database
+logfiles,s,h,"logfile",,,List of log files
+plotfile,s,h,"",,,Plot file for residuals
+verbose,b,h,no,,,Verbose output?
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,"Graphics cursor input
+"
+answer,s,q,"yes","no|yes|NO|YES",,Fit dispersion function interactively?
+crval,s,q,,,,"Approximate coordinate (at reference pixel)"
+cdelt,s,q,,,,"Approximate dispersion"
+aidpars,pset,h,,,,"Automatic identification algorithm parameters"
diff --git a/noao/imred/kpnocoude/sensfunc.par b/noao/imred/kpnocoude/sensfunc.par
new file mode 100644
index 00000000..94f84f4a
--- /dev/null
+++ b/noao/imred/kpnocoude/sensfunc.par
@@ -0,0 +1,17 @@
+standards,s,a,std,,,Input standard star data file (from STANDARD)
+sensitivity,s,a,"sens",,,Output root sensitivity function imagename
+apertures,s,h,"",,,Aperture selection list
+ignoreaps,b,h,yes,,,Ignore apertures and make one sensitivity function?
+logfile,f,h,"logfile",,,Output log for statistics information
+extinction,f,h,)_.extinction,,,Extinction file
+newextinction,f,h,"extinct.dat",,,Output revised extinction file
+observatory,s,h,)_.observatory,,,Observatory of data
+function,s,h,"spline3","chebyshev|legendre|spline3|spline1",,Fitting function
+order,i,h,6,1,,Order of fit
+interactive,b,h,yes,,,Determine sensitivity function interactively?
+graphs,s,h,"sr",,,Graphs per frame
+marks,s,h,"plus cross box",,,Data mark types (marks deleted added)
+colors,s,h,"2 1 3 4",,,Colors (lines marks deleted added)
+cursor,*gcur,h,"",,,Graphics cursor input
+device,s,h,"stdgraph",,,Graphics output device
+answer,s,q, yes,"no|yes|NO|YES",,"(no|yes|NO|YES)"
diff --git a/noao/imred/kpnocoude/sparams.par b/noao/imred/kpnocoude/sparams.par
new file mode 100644
index 00000000..06ccbb94
--- /dev/null
+++ b/noao/imred/kpnocoude/sparams.par
@@ -0,0 +1,65 @@
+line,i,h,INDEF,,,"Default dispersion line"
+nsum,i,h,10,,,"Number of dispersion lines to sum or median"
+extras,b,h,no,,,"Extract sky, sigma, etc.?
+
+-- DEFAULT APERTURE PARAMETERS -- "
+lower,r,h,-3.,,,Lower aperture limit relative to center
+upper,r,h,3.,,,"Upper aperture limit relative to center
+
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --"
+ylevel,r,h,0.05,,,"Fraction of peak or intensity for resizing
+
+-- TRACE PARAMETERS --"
+t_step,i,h,10,,,"Tracing step"
+t_function,s,h,"spline3","chebyshev|legendre|spline1|spline3",,"Trace fitting function"
+t_order,i,h,1,,,"Trace fitting function order"
+t_niterate,i,h,1,0,,"Trace rejection iterations"
+t_low,r,h,3.,0.,,"Trace lower rejection sigma"
+t_high,r,h,3.,0.,,"Trace upper rejection sigma
+
+-- APERTURE EXTRACTION PARAMETERS --"
+weights,s,h,"none",,,Extraction weights (none|variance)
+pfit,s,h,"fit1d","fit1d|fit2d",,Profile fitting algorithm (fit1d|fit2d)
+lsigma,r,h,3.,,,Lower rejection threshold
+usigma,r,h,3.,,,"Upper rejection threshold
+
+-- BACKGROUND SUBTRACTION PARAMETERS --"
+background,s,h,"fit","none|average|median|minimum|fit",,Background to subtract
+b_function,s,h,"legendre","chebyshev|legendre|spline1|spline3",,"Background function"
+b_order,i,h,1,,,"Background function order"
+b_sample,s,h,"-10:-6,6:10",,,"Background sample regions"
+b_naverage,i,h,-100,,,"Background average or median"
+b_niterate,i,h,1,0,,"Background rejection iterations"
+b_low,r,h,3.,0.,,"Background lower rejection sigma"
+b_high,r,h,3.,0.,,"Background upper rejection sigma
+
+-- ARC DISPERSION FUNCTION PARAMETERS --"
+threshold,r,h,10.,0.,,"Minimum line contrast threshold"
+coordlist,f,h,linelists$thar.dat,,,"Line list"
+match,r,h,-3.,,,"Line list matching limit in Angstroms"
+fwidth,r,h,3.5.,,,"Arc line widths in pixels"
+cradius,r,h,4.,,,Centering radius in pixels
+i_function,s,h,"legendre","legendre|chebyshev|spline1|spline3",,"Coordinate function"
+i_order,i,h,3,1,,"Order of dispersion function"
+i_niterate,i,h,3,0,,"Rejection iterations"
+i_low,r,h,3.,0.,,"Lower rejection sigma"
+i_high,r,h,3.,0.,,"Upper rejection sigma"
+refit,b,h,yes,,,"Refit coordinate function when reidentifying?"
+addfeatures,b,h,no,,,"Add features when reidentifying?
+
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --"
+select,s,h,"interp",,,"Selection method for reference spectra"
+sort,s,h,"jd",,,"Sort key"
+group,s,h,"ljd",,,"Group key"
+time,b,h,no,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting
+
+-- DISPERSION CORRECTION PARAMETERS --"
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+log,b,h,no,,,"Logarithmic wavelength scale?"
+flux,b,h,yes,,,"Conserve flux?
+
+-- SENSITIVITY CALIBRATION PARAMETERS --"
+s_function,s,h,"spline3","chebyshev|legendre|spline3|spline1",,"Fitting function"
+s_order,i,h,1,1,,"Order of sensitivity function"
+fnu,b,h,no,,,"Create spectra having units of FNU?"
diff --git a/noao/imred/kpnocoude/standard.par b/noao/imred/kpnocoude/standard.par
new file mode 100644
index 00000000..99b98877
--- /dev/null
+++ b/noao/imred/kpnocoude/standard.par
@@ -0,0 +1,21 @@
+input,f,a,,,,Input image file root name
+output,s,a,std,,,Output flux file (used by SENSFUNC)
+samestar,b,h,yes,,,Same star in all apertures?
+beam_switch,b,h,no,,,Beam switch spectra?
+apertures,s,h,"",,,Aperture selection list
+bandwidth,r,h,INDEF,,,Bandpass widths
+bandsep,r,h,INDEF,,,Bandpass separation
+fnuzero,r,h,3.68e-20,,,Absolute flux zero point
+extinction,s,h,)_.extinction,,,Extinction file
+caldir,s,h,)_.caldir,,,Directory containing calibration data
+observatory,s,h,)_.observatory,,,Observatory for data
+interact,b,h,yes,,,Graphic interaction to define new bandpasses
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+star_name,s,q,,,,Star name in calibration list
+airmass,r,q,,1.,,Airmass
+exptime,r,q,,,,Exposure time (seconds)
+mag,r,q,,,,Magnitude of star
+magband,s,q,,"U|B|V|R|I|J|H|K|L|Lprime|M",,"Magnitude type"
+teff,s,q,,,,Effective temperature or spectral type
+answer,s,q,no,,,"(no|yes|NO|YES|NO!|YES!)"
diff --git a/noao/imred/kpnoslit/Revisions b/noao/imred/kpnoslit/Revisions
new file mode 100644
index 00000000..2d50d554
--- /dev/null
+++ b/noao/imred/kpnoslit/Revisions
@@ -0,0 +1,32 @@
+.help revisions Jun88 noao.imred.kpnoslit
+.nf
+
+=====
+V2.12
+=====
+
+imred$kpnoslit/standard.par
+    Added blackbody query parameters.  (5/2/02, Valdes)
+
+========
+V2.11.3b
+========
+
+imred$kpnoslit/demos/mkdoslit.cl
+    Made the ARTDATA package parameters explicit (4/15/97, Valdes)
+
+imred$kpnoslit/sparams.par
+    Changed match from 10 to -3.  (4/5/96, Valdes)
+
+imred$kpnoslit/kpnoslit.cl
+imred$kpnoslit/kpnoslit.men
+    Added background, illumination, response, apflatten, apnormalize.
+    (12/29/94, Valdes)
+
+imred$kpnoslit/demos/xdoslit.dat
+    Incorrectly used hz2 as a standard star instead of hz44.  (8/10/92, Valdes)
+
+=======
+V2.10.1
+=======
+.endhelp
diff --git a/noao/imred/kpnoslit/calibrate.par b/noao/imred/kpnoslit/calibrate.par
new file mode 100644
index 00000000..e09457a2
--- /dev/null
+++ b/noao/imred/kpnoslit/calibrate.par
@@ -0,0 +1,13 @@
+# CALIBRATE parameter file
+
+input,s,a,,,,Input spectra to calibrate
+output,s,a,,,,Output calibrated spectra
+extinct,b,h,yes,,,Apply extinction correction?
+flux,b,h,yes,,,Apply flux calibration?
+extinction,s,h,)_.extinction,,,Extinction file
+observatory,s,h,)_.observatory,,,Observatory of observation
+ignoreaps,b,h,yes,,,Ignore aperture numbers in flux calibration?
+sensitivity,s,h,"sens",,,Image root name for sensitivity spectra
+fnu,b,h,no,,,Create spectra having units of FNU?
+airmass,r,q,,1.,,Airmass
+exptime,r,q,,,,Exposure time (seconds)
diff --git a/noao/imred/kpnoslit/demos/demoarc1.dat b/noao/imred/kpnoslit/demos/demoarc1.dat
new file mode 100644
index 00000000..dd6b0161
--- /dev/null
+++ b/noao/imred/kpnoslit/demos/demoarc1.dat
@@ -0,0 +1,38 @@
+OBJECT  = 'First comp        '  /  object name
+OBSERVAT= 'KPNO              '  /  observatory
+OBSERVER= 'Massey            '  /  observers
+COMMENTS= 'Final New Ice     '  /  comments
+EXPTIME =                  60.  /  actual integration time
+DARKTIME=                  60.  /  total elapsed time
+IMAGETYP= 'comp              '  /  object, dark, bias, etc.
+DATE-OBS= '1991-11-26T12:11:30.00' /  date (dd/mm/yy) of obs.
+UT      = '12:11:30.00       '  /  universal time
+ST      = '09:04:54.00       '  /  sidereal time
+RA      = '06:37:02.00       '  /  right ascension
+DEC     = '06:09:03.00       '  /  declination
+EPOCH   =               1991.9  /  epoch of ra and dec
+ZD      = '48.760            '  /  zenith distance
+AIRMASS =                   0.  /  airmass
+TELESCOP= 'kpcdf             '  /  telescope name
+DETECTOR= 'te1k              '  /  detector
+PREFLASH=                    0  /  preflash time, seconds
+GAIN    =                  5.4  /  gain, electrons per adu
+DWELL   =                    5  /  sample integration time
+RDNOISE =                  3.5  /  read noise, electrons per adu
+DELAY0  =                    0  /  time delay after each pixel
+DELAY1  =                    0  /  time delay after each row
+CAMTEMP =                 -111  /  camera temperature
+DEWTEMP =                 -183  /  dewar temperature
+CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+CCDSUM  = '1 1               '  /  on chip summation
+INSTRUME= 'test              '  /  instrument
+APERTURE= '250micron slit    '  /  aperture
+TVFILT  = '4-96              '  /  tv filter
+DISPAXIS= '2                 '  /  dispersion axis
+GRATPOS =               4624.3  /  grating position
+TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+CCDMEAN =              179.398
+CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/kpnoslit/demos/demoarc2.dat b/noao/imred/kpnoslit/demos/demoarc2.dat
new file mode 100644
index 00000000..5c2d8050
--- /dev/null
+++ b/noao/imred/kpnoslit/demos/demoarc2.dat
@@ -0,0 +1,38 @@
+OBJECT  = 'Last comp         '  /  object name
+OBSERVAT= 'KPNO              '  /  observatory
+OBSERVER= 'Massey            '  /  observers
+COMMENTS= 'Final New Ice     '  /  comments
+EXPTIME =                  60.  /  actual integration time
+DARKTIME=                  60.  /  total elapsed time
+IMAGETYP= 'comp              '  /  object, dark, bias, etc.
+DATE-OBS= '1991-11-26T12:41:30.00' /  date (dd/mm/yy) of obs.
+UT      = '12:41:30.00       '  /  universal time
+ST      = '09:34:54.00       '  /  sidereal time
+RA      = '06:37:02.00       '  /  right ascension
+DEC     = '06:09:03.00       '  /  declination
+EPOCH   =               1991.9  /  epoch of ra and dec
+ZD      = '48.760            '  /  zenith distance
+AIRMASS =                   0.  /  airmass
+TELESCOP= 'kpcdf             '  /  telescope name
+DETECTOR= 'te1k              '  /  detector
+PREFLASH=                    0  /  preflash time, seconds
+GAIN    =                  5.4  /  gain, electrons per adu
+DWELL   =                    5  /  sample integration time
+RDNOISE =                  3.5  /  read noise, electrons per adu
+DELAY0  =                    0  /  time delay after each pixel
+DELAY1  =                    0  /  time delay after each row
+CAMTEMP =                 -111  /  camera temperature
+DEWTEMP =                 -183  /  dewar temperature
+CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+CCDSUM  = '1 1               '  /  on chip summation
+INSTRUME= 'test              '  /  instrument
+APERTURE= '250micron slit    '  /  aperture
+TVFILT  = '4-96              '  /  tv filter
+DISPAXIS= '2                 '  /  dispersion axis
+GRATPOS =               4624.3  /  grating position
+TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+CCDMEAN =              179.398
+CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/kpnoslit/demos/demoflat.dat b/noao/imred/kpnoslit/demos/demoflat.dat
new file mode 100644
index 00000000..0d5ed308
--- /dev/null
+++ b/noao/imred/kpnoslit/demos/demoflat.dat
@@ -0,0 +1,38 @@
+OBJECT  = 'Flat field        '  /  object name
+OBSERVAT= 'KPNO              '  /  observatory
+OBSERVER= 'Massey            '  /  observers
+COMMENTS= 'Final New Ice     '  /  comments
+EXPTIME =                   3.  /  actual integration time
+DARKTIME=                   3.  /  total elapsed time
+IMAGETYP= 'flat              '  /  object, dark, bias, etc.
+DATE-OBS= '1991-11-26T11:11:30.00' /  date (dd/mm/yy) of obs.
+UT      = '11:11:30.00       '  /  universal time
+ST      = '09:04:54.00       '  /  sidereal time
+RA      = '06:37:02.00       '  /  right ascension
+DEC     = '06:09:03.00       '  /  declination
+EPOCH   =               1991.9  /  epoch of ra and dec
+ZD      = '48.760            '  /  zenith distance
+AIRMASS =                   0.  /  airmass
+TELESCOP= 'kpcdf             '  /  telescope name
+DETECTOR= 'te1k              '  /  detector
+PREFLASH=                    0  /  preflash time, seconds
+GAIN    =                  5.4  /  gain, electrons per adu
+DWELL   =                    5  /  sample integration time
+RDNOISE =                  3.5  /  read noise, electrons per adu
+DELAY0  =                    0  /  time delay after each pixel
+DELAY1  =                    0  /  time delay after each row
+CAMTEMP =                 -111  /  camera temperature
+DEWTEMP =                 -183  /  dewar temperature
+CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+CCDSUM  = '1 1               '  /  on chip summation
+INSTRUME= 'test              '  /  instrument
+APERTURE= '250micron slit    '  /  aperture
+TVFILT  = '4-96              '  /  tv filter
+DISPAXIS= '2                 '  /  dispersion axis
+GRATPOS =               4624.3  /  grating position
+TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+CCDMEAN =              179.398
+CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/kpnoslit/demos/demoobj1.dat b/noao/imred/kpnoslit/demos/demoobj1.dat
new file mode 100644
index 00000000..bf571862
--- /dev/null
+++ b/noao/imred/kpnoslit/demos/demoobj1.dat
@@ -0,0 +1,37 @@
+OBJECT  = 'V640Mon 4500      '  /  object name
+OBSERVAT= 'KPNO              '  /  observatory
+OBSERVER= 'Massey            '  /  observers
+COMMENTS= 'Final New Ice     '  /  comments
+EXPTIME =                1200.  /  actual integration time
+DARKTIME=                1200.  /  total elapsed time
+IMAGETYP= 'object            '  /  object, dark, bias, etc.
+DATE-OBS= '1991-11-26T12:19:55.00' /  date (dd/mm/yy) of obs.
+UT      = '12:19:55.00       '  /  universal time
+ST      = '09:13:15.00       '  /  sidereal time
+RA      = '06:37:02.00       '  /  right ascension
+DEC     = '06:08:52.00       '  /  declination
+EPOCH   =               1991.9  /  epoch of ra and dec
+ZD      = '44.580            '  /  zenith distance
+AIRMASS =                   0.  /  airmass
+TELESCOP= 'kpcdf             '  /  telescope name
+DETECTOR= 'te1k              '  /  detector
+PREFLASH=                    0  /  preflash time, seconds
+GAIN    =                  5.4  /  gain, electrons per adu
+DWELL   =                    5  /  sample integration time
+RDNOISE =                  3.5  /  read noise, electrons per adu
+DELAY0  =                    0  /  time delay after each pixel
+DELAY1  =                    0  /  time delay after each row
+CAMTEMP =                 -111  /  camera temperature
+DEWTEMP =                 -183  /  dewar temperature
+CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+CCDSUM  = '1 1               '  /  on chip summation
+INSTRUME= 'test              '  /  instrument
+APERTURE= '250micron slit    '  /  aperture
+TVFILT  = '4-96              '  /  tv filter
+DISPAXIS= '2                 '  /  dispersion axis
+GRATPOS =               4624.3  /  grating position
+TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/kpnoslit/demos/demos.cl b/noao/imred/kpnoslit/demos/demos.cl
new file mode 100644
index 00000000..5b065c51
--- /dev/null
+++ b/noao/imred/kpnoslit/demos/demos.cl
@@ -0,0 +1,18 @@
+# DEMOS -- Run specified demo provided a demo file exists.
+
+procedure demos (demoname)
+
+file	demoname	{prompt="Demo name"}
+
+begin
+	file	demo, demofile
+
+	if ($nargs == 0 && mode != "h")
+	    type ("demos$demos.men")
+	demo = demoname
+	demofile = "demos$" // demo // ".cl"
+	if (access (demofile))
+	    cl (< demofile)
+	else
+	    error (1, "Unknown demo " // demo)
+end
diff --git a/noao/imred/kpnoslit/demos/demos.men b/noao/imred/kpnoslit/demos/demos.men
new file mode 100644
index 00000000..b35ba7be
--- /dev/null
+++ b/noao/imred/kpnoslit/demos/demos.men
@@ -0,0 +1,4 @@
+	MENU of KPNOSLIT Demonstrations
+
+       doslit - Quick test of DOSLIT (no comments, no delays)
+     mkdoslit - Make DOSLIT test data
diff --git a/noao/imred/kpnoslit/demos/demos.par b/noao/imred/kpnoslit/demos/demos.par
new file mode 100644
index 00000000..4181ed59
--- /dev/null
+++ b/noao/imred/kpnoslit/demos/demos.par
@@ -0,0 +1,2 @@
+demoname,f,a,"",,,"Demo name"
+mode,s,h,"ql",,,
diff --git a/noao/imred/kpnoslit/demos/demostd1.dat b/noao/imred/kpnoslit/demos/demostd1.dat
new file mode 100644
index 00000000..bf571862
--- /dev/null
+++ b/noao/imred/kpnoslit/demos/demostd1.dat
@@ -0,0 +1,37 @@
+OBJECT  = 'V640Mon 4500      '  /  object name
+OBSERVAT= 'KPNO              '  /  observatory
+OBSERVER= 'Massey            '  /  observers
+COMMENTS= 'Final New Ice     '  /  comments
+EXPTIME =                1200.  /  actual integration time
+DARKTIME=                1200.  /  total elapsed time
+IMAGETYP= 'object            '  /  object, dark, bias, etc.
+DATE-OBS= '1991-11-26T12:19:55.00' /  date (dd/mm/yy) of obs.
+UT      = '12:19:55.00       '  /  universal time
+ST      = '09:13:15.00       '  /  sidereal time
+RA      = '06:37:02.00       '  /  right ascension
+DEC     = '06:08:52.00       '  /  declination
+EPOCH   =               1991.9  /  epoch of ra and dec
+ZD      = '44.580            '  /  zenith distance
+AIRMASS =                   0.  /  airmass
+TELESCOP= 'kpcdf             '  /  telescope name
+DETECTOR= 'te1k              '  /  detector
+PREFLASH=                    0  /  preflash time, seconds
+GAIN    =                  5.4  /  gain, electrons per adu
+DWELL   =                    5  /  sample integration time
+RDNOISE =                  3.5  /  read noise, electrons per adu
+DELAY0  =                    0  /  time delay after each pixel
+DELAY1  =                    0  /  time delay after each row
+CAMTEMP =                 -111  /  camera temperature
+DEWTEMP =                 -183  /  dewar temperature
+CCDSEC  = '[97:134,2:1023]'     /  orientation to full frame
+ORIGSEC = '[1:1024,1:1024]   '  /  original size  full frame
+CCDSUM  = '1 1               '  /  on chip summation
+INSTRUME= 'test              '  /  instrument
+APERTURE= '250micron slit    '  /  aperture
+TVFILT  = '4-96              '  /  tv filter
+DISPAXIS= '2                 '  /  dispersion axis
+GRATPOS =               4624.3  /  grating position
+TRIM    = 'Nov 26  5:44 Trim data section is [23:60,2:1023]'
+OVERSCAN= 'Nov 26  5:44 Overscan section is [103:133,2:1023] with mean=611.1
+ZEROCOR = 'Nov 26  5:44 Zero level correction image is Zerof'
+CCDPROC = 'Nov 26  5:44 CCD processing done'
diff --git a/noao/imred/kpnoslit/demos/doslit.cl b/noao/imred/kpnoslit/demos/doslit.cl
new file mode 100644
index 00000000..b2ecbde2
--- /dev/null
+++ b/noao/imred/kpnoslit/demos/doslit.cl
@@ -0,0 +1,14 @@
+# Create demo data if needed.
+
+cl (< "demos$mkdoslit.cl")
+
+unlearn doslit
+sparams.extras = no
+sparams.coordlist = "linelists$idhenear.dat"
+delete demologfile,demoplotfile verify=no >& dev$null
+
+# Execute playback.
+if (substr (envget("stdgraph"), 1, 6) == "xgterm")
+    stty (playback="demos$xgdoslit.dat", nlines=24, verify=no, delay=0)
+else
+    error (1, "Playback for current terminal type not available")
diff --git a/noao/imred/kpnoslit/demos/mkdoslit.cl b/noao/imred/kpnoslit/demos/mkdoslit.cl
new file mode 100644
index 00000000..63acb123
--- /dev/null
+++ b/noao/imred/kpnoslit/demos/mkdoslit.cl
@@ -0,0 +1,28 @@
+# Create demo data if needed.
+
+artdata
+artdata.nxc = 5
+artdata.nyc = 5
+artdata.nxsub = 10
+artdata.nysub = 10
+artdata.nxgsub = 5
+artdata.nygsub = 5
+artdata.dynrange = 100000.
+artdata.psfrange = 10.
+artdata.ranbuf = 0
+
+mkexample ("longslit", "demoflat", oseed=4,  nseed=1,
+    errors=no, verbose=yes, list=no)
+mkheader ("demoflat", "demos$demoflat.dat", append=no, verbose=no)
+mkexample ("longslit", "demoarc1", oseed=5,  nseed=1,
+    errors=no, verbose=yes, list=no)
+mkheader ("demoarc1", "demos$demoarc1.dat", append=no, verbose=no)
+mkexample ("longslit", "demoobj1", oseed=1,  nseed=1,
+    errors=no, verbose=yes, list=no)
+mkheader ("demoobj1", "demos$demoobj1.dat", append=no, verbose=no)
+mkexample ("longslit", "demostd1", oseed=2, nseed=2,
+    errors=no, verbose=yes, list=no)
+mkheader ("demostd1", "demos$demostd1.dat", append=no, verbose=no)
+mkexample ("longslit", "demoarc2", oseed=5,  nseed=2,
+    errors=no, verbose=yes, list=no)
+mkheader ("demoarc2", "demos$demoarc2.dat", append=no, verbose=no)
diff --git a/noao/imred/kpnoslit/demos/xgdoslit.dat b/noao/imred/kpnoslit/demos/xgdoslit.dat
new file mode 100644
index 00000000..0cd3a8d9
--- /dev/null
+++ b/noao/imred/kpnoslit/demos/xgdoslit.dat
@@ -0,0 +1,71 @@
+\O=NOAO/IRAF IRAFX valdes@puppis Mon 14:58:37 15-Nov-93
+\T=xgterm
+\G=xgterm
+epar\skpnoslit\n
+\r
+\r
+\r
+\r
+\r
+\r
+\r
+y\r
+demologfile\r
+demoplotfile\r
+^Z
+epar\sdoslit\n
+demoobj1\r
+demoarc1,demoarc2\r
+\r
+demostd1\r
+rdnoise\r
+gain\r
+\r
+\r
+5700\r
+6.2\r
+\r
+y\r
+y\r
+y\r
+y\r
+y\r
+^Z
+doslit\sredo+\n
+\n
+\n
+b/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+\r
+\r
+q/<-5\s\s\s\s/=(.\s=\r
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+y\n
+4210\n
+7350\n
+6.2\n
+\n
+n\n
+\n
+f/<-5\s\s\s\s/=(.\s=\r
+l/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+N\n
+hz44\n
+\n
+q/<-5\s\s\s\s/=(.\s=\r
+Y\n
+q/<-5\s\s\s\s/=(.\s=\r
+q/<-5\s\s\s\s/=(.\s=\r
+gkimos\sdemoplotfile\snx=3\sny=3\sdev=stdgraph\n
+q/<-5\s\s\s\s/=(.\s=\r
diff --git a/noao/imred/kpnoslit/kpnoslit.cl b/noao/imred/kpnoslit/kpnoslit.cl
new file mode 100644
index 00000000..f9d79756
--- /dev/null
+++ b/noao/imred/kpnoslit/kpnoslit.cl
@@ -0,0 +1,69 @@
+#{ KPNOSLIT package definition
+
+# Define KPNOSLIT package
+package kpnoslit
+
+set	demos		= "kpnoslit$demos/"
+
+# Slitproc
+cl < doslit$doslittasks.cl
+task	sparams		= "kpnoslit$sparams.par"
+
+# Onedspec tasks
+task	autoidentify,
+	continuum,
+	deredden,
+	dispcor,
+	dopcor,
+	identify,
+	refspectra,
+	reidentify,
+	sarith,
+	sflip,
+	slist,
+	splot,
+	specplot,
+	specshift	= "onedspec$x_onedspec.e"
+task	scombine	= "onedspec$scombine/x_scombine.e"
+task	aidpars		= "onedspec$aidpars.par"
+task	bplot		= "onedspec$bplot.cl"
+task	scopy		= "onedspec$scopy.cl"
+task	dispcor1	= "onedspec$dispcor1.par"
+
+# Different default parameters
+task	calibrate,
+	sensfunc,
+	standard	= "kpnoslit$x_onedspec.e"
+
+# Apextract tasks
+task	apall,
+	apedit,
+	apfind,
+	apflatten,
+	apnormalize,
+	aprecenter,
+	apresize,
+	apsum,
+	aptrace		= "apextract$x_apextract.e"
+task	apdefault	= "apextract$apdefault.par"
+task	apparams	= "apextract$apparams.par"
+task	apall1		= "apextract$apall1.par"
+task	apflat1		= "apextract$apflat1.par"
+task	apnorm1		= "apextract$apflat1.par"
+
+# Longslit tasks
+task	illumination,
+	response	= "twodspec$longslit/x_longslit.e"
+task	background	= "generic$background.cl"
+
+# Demos
+task	demos		= "demos$demos.cl"
+
+# Astutil tasks
+task	setairmass,
+	setjd		= "astutil$x_astutil.e"
+
+# Hide tasks from the user
+hidetask apparams, apall1, apflat1, apnorm1, dispcor1, sparams
+
+clbye()
diff --git a/noao/imred/kpnoslit/kpnoslit.hd b/noao/imred/kpnoslit/kpnoslit.hd
new file mode 100644
index 00000000..e5125e4f
--- /dev/null
+++ b/noao/imred/kpnoslit/kpnoslit.hd
@@ -0,0 +1 @@
+# Help directory for the KPNOSLIT package.
diff --git a/noao/imred/kpnoslit/kpnoslit.men b/noao/imred/kpnoslit/kpnoslit.men
new file mode 100644
index 00000000..891ff0b7
--- /dev/null
+++ b/noao/imred/kpnoslit/kpnoslit.men
@@ -0,0 +1,38 @@
+          apall - Extract 1D spectra (all parameters in one task)
+      apdefault - Set the default aperture parameters
+         apedit - Edit apertures interactively
+	 apfind - Automatically find spectra and define apertures
+      apflatten - Remove overall spectral and profile shapes from flat fields
+    apnormalize - Normalize 2D apertures by 1D functions
+     aprecenter - Recenter apertures
+       apresize - Resize apertures
+          apsum - Extract 1D spectra
+	aptrace - Trace positions of spectra
+
+     background - Fit and subtract a line or column background
+	  bplot - Batch plot of spectra with SPLOT
+      calibrate - Apply extinction and flux calibrations to spectra
+      continuum - Fit and normalize the continuum of multispec spectra
+       deredden - Apply interstellar extinction corrections
+        dispcor - Dispersion correct spectra
+	 dopcor - Doppler correct spectra
+       identify - Identify arc lines and determine a dispersion function
+   illumination - Determine illumination calibration
+     refspectra - Assign reference spectra to observations
+     reidentify - Reidentify arc lines and determine new dispersion functions
+       response - Determine response calibration
+	 sarith - Spectrum arithmetic
+       scombine - Combine spectra
+          scopy - Copy spectra including aperture selection and format changes
+       sensfunc - Create sensitivity function
+     setairmass - Compute effective airmass and middle UT for an exposure
+          setjd - Compute and set Julian dates in images
+	  sflip - Flip data and/or dispersion coordinates in spectra
+          slist - List spectrum headers
+       specplot - Stack and plot multiple spectra
+      specshift - Shift spectral dispersion coordinate systems
+	  splot - Plot and analyze spectra
+       standard - Identify standard stars to be used in sensitivity calc
+
+         doslit - Process slit spectra
+	  demos - Demonstrations and tests
diff --git a/noao/imred/kpnoslit/kpnoslit.par b/noao/imred/kpnoslit/kpnoslit.par
new file mode 100644
index 00000000..bd61b8de
--- /dev/null
+++ b/noao/imred/kpnoslit/kpnoslit.par
@@ -0,0 +1,15 @@
+# KPNOSLIT parameter file
+extinction,s,h,onedstds$kpnoextinct.dat,,,Extinction file
+caldir,s,h,onedstds$spec50cal/,,,Standard star calibration directory
+observatory,s,h,"observatory",,,Observatory of data
+interp,s,h,"poly5","nearest|linear|poly3|poly5|spline3|sinc",,Interpolation type
+dispaxis,i,h,2,1,3,Image axis for 2D/3D images
+nsum,s,h,"1",,,"Number of lines/columns/bands to sum for 2D/3D images
+"
+database,f,h,"database",,,Database
+verbose,b,h,no,,,Verbose output?
+logfile,s,h,"logfile",,,Log file
+plotfile,s,h,"",,,"Plot file
+"
+records,s,h,"",,,Record number extensions
+version,s,h,"KPNOSLIT V3: January 1992"
diff --git a/noao/imred/kpnoslit/sensfunc.par b/noao/imred/kpnoslit/sensfunc.par
new file mode 100644
index 00000000..94f84f4a
--- /dev/null
+++ b/noao/imred/kpnoslit/sensfunc.par
@@ -0,0 +1,17 @@
+standards,s,a,std,,,Input standard star data file (from STANDARD)
+sensitivity,s,a,"sens",,,Output root sensitivity function imagename
+apertures,s,h,"",,,Aperture selection list
+ignoreaps,b,h,yes,,,Ignore apertures and make one sensitivity function?
+logfile,f,h,"logfile",,,Output log for statistics information
+extinction,f,h,)_.extinction,,,Extinction file
+newextinction,f,h,"extinct.dat",,,Output revised extinction file
+observatory,s,h,)_.observatory,,,Observatory of data
+function,s,h,"spline3","chebyshev|legendre|spline3|spline1",,Fitting function
+order,i,h,6,1,,Order of fit
+interactive,b,h,yes,,,Determine sensitivity function interactively?
+graphs,s,h,"sr",,,Graphs per frame
+marks,s,h,"plus cross box",,,Data mark types (marks deleted added)
+colors,s,h,"2 1 3 4",,,Colors (lines marks deleted added)
+cursor,*gcur,h,"",,,Graphics cursor input
+device,s,h,"stdgraph",,,Graphics output device
+answer,s,q, yes,"no|yes|NO|YES",,"(no|yes|NO|YES)"
diff --git a/noao/imred/kpnoslit/sparams.par b/noao/imred/kpnoslit/sparams.par
new file mode 100644
index 00000000..cfdf1f4f
--- /dev/null
+++ b/noao/imred/kpnoslit/sparams.par
@@ -0,0 +1,65 @@
+line,i,h,INDEF,,,"Default dispersion line"
+nsum,i,h,10,,,"Number of dispersion lines to sum or median"
+extras,b,h,no,,,"Extract sky, sigma, etc.?
+
+-- DEFAULT APERTURE PARAMETERS -- "
+lower,r,h,-3.,,,Lower aperture limit relative to center
+upper,r,h,3.,,,"Upper aperture limit relative to center
+
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --"
+ylevel,r,h,0.05,,,"Fraction of peak or intensity for resizing
+
+-- TRACE PARAMETERS --"
+t_step,i,h,10,,,"Tracing step"
+t_function,s,h,"spline3","chebyshev|legendre|spline1|spline3",,"Trace fitting function"
+t_order,i,h,1,,,"Trace fitting function order"
+t_niterate,i,h,1,0,,"Trace rejection iterations"
+t_low,r,h,3.,0.,,"Trace lower rejection sigma"
+t_high,r,h,3.,0.,,"Trace upper rejection sigma
+
+-- APERTURE EXTRACTION PARAMETERS --"
+weights,s,h,"none",,,Extraction weights (none|variance)
+pfit,s,h,"fit1d","fit1d|fit2d",,Profile fitting algorithm (fit1d|fit2d)
+lsigma,r,h,3.,,,Lower rejection threshold
+usigma,r,h,3.,,,"Upper rejection threshold
+
+-- BACKGROUND SUBTRACTION PARAMETERS --"
+background,s,h,"fit","none|average|median|minimum|fit",,Background to subtract
+b_function,s,h,"legendre","chebyshev|legendre|spline1|spline3",,"Background function"
+b_order,i,h,1,,,"Background function order"
+b_sample,s,h,"-10:-6,6:10",,,"Background sample regions"
+b_naverage,i,h,-100,,,"Background average or median"
+b_niterate,i,h,1,0,,"Background rejection iterations"
+b_low,r,h,3.,0.,,"Background lower rejection sigma"
+b_high,r,h,3.,0.,,"Background upper rejection sigma
+
+-- ARC DISPERSION FUNCTION PARAMETERS --"
+threshold,r,h,10.,0.,,"Minimum line contrast threshold"
+coordlist,f,h,linelists$idhenear.dat,,,"Line list"
+match,r,h,10.,,,"Line list matching limit in Angstroms"
+fwidth,r,h,4.,,,"Arc line widths in pixels"
+cradius,r,h,10.,,,Centering radius in pixels
+i_function,s,h,"spline3","legendre|chebyshev|spline1|spline3",,"Coordinate function"
+i_order,i,h,1,1,,"Order of dispersion function"
+i_niterate,i,h,1,0,,"Rejection iterations"
+i_low,r,h,3.,0.,,"Lower rejection sigma"
+i_high,r,h,3.,0.,,"Upper rejection sigma"
+refit,b,h,yes,,,"Refit coordinate function when reidentifying?"
+addfeatures,b,h,no,,,"Add features when reidentifying?
+
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --"
+select,s,h,"interp",,,"Selection method for reference spectra"
+sort,s,h,"jd",,,"Sort key"
+group,s,h,"ljd",,,"Group key"
+time,b,h,no,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting
+
+-- DISPERSION CORRECTION PARAMETERS --"
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+log,b,h,no,,,"Logarithmic wavelength scale?"
+flux,b,h,yes,,,"Conserve flux?
+
+-- SENSITIVITY CALIBRATION PARAMETERS --"
+s_function,s,h,"spline3","chebyshev|legendre|spline3|spline1",,"Fitting function"
+s_order,i,h,1,1,,"Order of sensitivity function"
+fnu,b,h,no,,,"Create spectra having units of FNU?"
diff --git a/noao/imred/kpnoslit/standard.par b/noao/imred/kpnoslit/standard.par
new file mode 100644
index 00000000..99b98877
--- /dev/null
+++ b/noao/imred/kpnoslit/standard.par
@@ -0,0 +1,21 @@
+input,f,a,,,,Input image file root name
+output,s,a,std,,,Output flux file (used by SENSFUNC)
+samestar,b,h,yes,,,Same star in all apertures?
+beam_switch,b,h,no,,,Beam switch spectra?
+apertures,s,h,"",,,Aperture selection list
+bandwidth,r,h,INDEF,,,Bandpass widths
+bandsep,r,h,INDEF,,,Bandpass separation
+fnuzero,r,h,3.68e-20,,,Absolute flux zero point
+extinction,s,h,)_.extinction,,,Extinction file
+caldir,s,h,)_.caldir,,,Directory containing calibration data
+observatory,s,h,)_.observatory,,,Observatory for data
+interact,b,h,yes,,,Graphic interaction to define new bandpasses
+graphics,s,h,"stdgraph",,,Graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+star_name,s,q,,,,Star name in calibration list
+airmass,r,q,,1.,,Airmass
+exptime,r,q,,,,Exposure time (seconds)
+mag,r,q,,,,Magnitude of star
+magband,s,q,,"U|B|V|R|I|J|H|K|L|Lprime|M",,"Magnitude type"
+teff,s,q,,,,Effective temperature or spectral type
+answer,s,q,no,,,"(no|yes|NO|YES|NO!|YES!)"
diff --git a/noao/imred/mkpkg b/noao/imred/mkpkg
new file mode 100644
index 00000000..30057f0d
--- /dev/null
+++ b/noao/imred/mkpkg
@@ -0,0 +1,20 @@
+# Make the IMRED package.
+
+update:
+	$echo "------------------ IMRED.BIAS ----------------------"
+	$call update@bias
+	$echo "------------------ IMRED.CCDRED --------------------"
+	$call update@ccdred
+	$echo "------------------ IMRED.CRUTIL --------------------"
+	$call update@crutil
+	$echo "------------------ IMRED.DTOI ----------------------"
+	$call update@dtoi
+	$echo "------------------ IMRED.GENERIC -------------------"
+	$call update@generic
+	$echo "------------------ IMRED.IRRED ---------------------"
+	$call update@irred
+	$echo "------------------ IMRED.QUADRED -------------------"
+	$call update@quadred
+	$echo "------------------ IMRED.VTEL ----------------------"
+	$call update@vtel
+	;
diff --git a/noao/imred/quadred/doc/package.hlp b/noao/imred/quadred/doc/package.hlp
new file mode 100644
index 00000000..ffea9446
--- /dev/null
+++ b/noao/imred/quadred/doc/package.hlp
@@ -0,0 +1,142 @@
+.help package Sep93 quadred
+.ih
+NAME
+quadred -- CCD reductions of images in multi-amp readout format
+.ih
+SYNOPSIS
+This package is a varient of \fBccdred\fR that operates on a
+multi-amplifier data format in which the various amplifier readouts are
+recorded in sections of a regular two-dimensional image.  The CTIO Arcon
+dual or quad readout data is an example of this format.  See help on
+\fBquadformat\fR for details.  Most tasks are the same as in the
+\fBccdred\fR package.  The difference is the version of \fBccdproc\fR in
+this package also works on the multi-amp format.  An alternative to using
+this version of \fBccdproc\fR is \fBquadproc\fR and the alternate
+calibration combining task based on this task.
+.ih
+USAGE
+quadred
+.ih
+PARAMETERS
+The following are "package" parameters.  This means that they apply to
+many of the tasks in this package.
+
+.ls pixeltype = "real real"
+Output pixel datatype and calculation datatype.  When images are processed
+or created the output pixel datatype is determined by this parameter.
+The allowed types are "short" for short integer, and "real" for real
+floating point.  The calculation datatypes are also short and real with a
+default of real if none is specified.
+.le
+.ls verbose = no
+Print log information to the standard output?
+.le
+.ls logfile = "logfile"
+Text log file.  If no filename is specified then no log file is kept.
+.le
+.ls plotfile = ""
+Log metacode plot file for the overscan bias vector fits.  If
+no filename is specified then no metacode plot file is kept.
+.le
+.ls backup = ""
+Backup prefix for backup images.  If no prefix is specified then no backup
+images are kept when processing.  If specified then the backup image
+has the specified prefix.
+.le
+.ls instrument = ""
+CCD instrument translation file.  This is usually set with \fBsetinstrument\fR.
+.le
+.ls ssfile = "subsets"
+Subset translation file used to define the subset identifier.  See
+\fBsubsets\fR for more.
+.le
+.ls graphics = "stdgraph"
+Interactive graphics output device when fitting the overscan bias vector.
+.le
+.ls cursor = ""
+Graphics cursor input.  The default is the standard graphics cursor.
+.le
+.ls version = "Version 1.0 - August 22, 2001"
+Package version.
+.le
+.ih
+DESCRIPTION
+The \fBquadred\fR package contains all basic tasks necessary for the
+reduction of CCD data in single image format.  This includes both single
+amplifier readout data and multi-amplifier data stored as sections in a
+single two-dimensional image.  One example of this type of multi-amplifier
+data is the CTIO Arcon "dual" or "quad" readout format.  The format is
+described in the help topic \fBquadformat\fR.  This package is a
+combination of two earlier packages called \fBxccdred\fR and
+\fBared.quad\fR, each of which are variants of the original \fBccdred\fR
+package.
+
+The raw data contains overscan/prescan regions in the image.  For multi-amp
+data there are multiple overscan/prescan regions.  The first steps in
+processing the data is to use the overscan/prescan regions to determine
+the amplifier bias, subtract this bias, and trim the regions out of
+the data.  Once this is done the data are just simple images.  It is
+the special step of dealing with the overscan/prescan regions with
+the multi-amp format that is different from the standard \fBccdred\fR
+package.
+
+Two methods are provided for dealing with the special format.  One is a
+special version of \fBccdproc\fR which processes the sections directly.  If
+one uses this task then the reduction steps appear identical to using the
+\fBccdred\fR package.  The other method is to use the tasks \fBquadproc\fR,
+\fBqzerocombine\fR, \fBqdarkcombine\fR, and \fBqflatcombine\fR.  The latter
+calibration combining tasks are the same as the standard versions except
+they use \fBquadproc\fR instead of \fBccdproc\fR.  The task \fBquadproc\fR
+operates internally by splitting the multiple regions into temporary single
+amplifier images, processing them with \fBccdproc\fR, and then joining the
+pieces back together.
+
+The recommended method is to use \fBccdproc\fR.  However, the \fBquadproc\fR
+related tasks have a history of usage for CTIO data and so may also be
+used.
+
+The \fBquadred\fR package itself has several parameters which are
+common to many of the tasks in the package.  When images are processed or
+new image are created the output pixel datatype is that specified by the
+parameter \fBpixeltype\fR. Note that CCD processing replaces the original
+image by the processed image so the pixel type of the CCD images may change
+during processing.  It is unlikely that real images will be processed to
+short images but the reverse is quite likely.  Processing images from short
+to real pixel datatypes will generally increase the amount of disk space
+required (a factor of 2 on most computers).
+
+The tasks produce log output which may be printed on the standard
+output (the terminal unless redirected) and appended to a file.  The
+parameter \fIverbose\fR determines whether processing information
+is printed.  This may be desirable initially, but when using background
+jobs the verbose output should be turned off.  The user may look at
+the end of the log file (for example with \fBtail\fR) to determine
+the status of the processing.
+
+The package was designed to work with data from many different observatories
+and instruments.  In order to accomplish this an instrument translation
+file is used to define a mapping between the package parameters and
+the particular image header format.  The instrument translation file
+is specified to the package by the parameter \fIinstrument\fR.  This
+parameter is generally set by the task \fBsetinstrument\fR.  The other
+file used is a subset file.  This is generally created and maintained
+by the package and the user need not do anything.  For more sophisticated
+users see \fBinstruments\fR and \fBsubsets\fR.
+
+The package has very little graphics output.  The exception is the overscan
+bias subtraction.  The bias vector is logged in the metacode plot file if
+given.  The plot file may be examined with the tasks in the \fBplot\fR
+package such as \fBgkimosaic\fR.  When interactively fitting the overscan
+vector the graphics input and output devices must be specified.  The
+defaults should apply in most cases.
+
+Because processing replaces the input image by the processed image it may
+be desired to save the original image.  This may be done by specifying a
+backup prefix with the parameter \fIbackup\fR.  For example, if the prefix
+is "orig" and the image is "ccd001", the backup image will be
+"origccd001".  The prefix may be a directory but if so it must end with '/'
+or '$' (for logical directories) and the directory must already exist.
+.ih
+SEE ALSO
+quadformat, mscred
+.endhelp
diff --git a/noao/imred/quadred/doc/qhistogram.hlp b/noao/imred/quadred/doc/qhistogram.hlp
new file mode 100644
index 00000000..a34e412c
--- /dev/null
+++ b/noao/imred/quadred/doc/qhistogram.hlp
@@ -0,0 +1,37 @@
+.help qhistogram Aug01 noao.imred.quadred
+.ih
+NAME
+qhistogram -- Compute and print histogram for multi-amp data
+.ih
+USAGE
+qhistogram images
+.ih
+PARAMETERS
+.ls images
+List of image names in \fBquadformat\fR.
+.le
+.ls window = "datasec" (datasec|trimsec|biassec)
+Type of section to use for histogram.  The choices are "datasec" for the
+amplifier section which includes the bias if any is present, "trimsec" for
+the trim section, and "biassec" for the bias section.
+.le
+
+The remaining parameters come from the \fBimhistogram\fR task.
+.ih
+DESCRIPTION
+This script tasks uses the \fBquadsections\fR task to break the
+\fBquadformat\fR data into separate sections and runs the \fBimhistogram\fR
+task on the sections.  The graphics is collected onto a single page.
+.ih
+EXAMPLES
+
+1. To graph the histograms (default behavior).
+
+.nf
+    qu> qhist quad0072
+    [graph appears]
+.fi
+.ih
+SEE ALSO
+quadformat, quadsections, imhistogram
+.endhelp
diff --git a/noao/imred/quadred/doc/qstatistics.hlp b/noao/imred/quadred/doc/qstatistics.hlp
new file mode 100644
index 00000000..222ae778
--- /dev/null
+++ b/noao/imred/quadred/doc/qstatistics.hlp
@@ -0,0 +1,52 @@
+.help qstatistics Aug01 noao.imred.quadred
+.ih
+NAME
+qstatistics -- Compute and print statistics for multi-amp data
+.ih
+USAGE
+qstatistics images
+.ih
+PARAMETERS
+.ls images
+List of image names in \fBquadformat\fR.
+.le
+.ls window = "datasec" (datasec|trimsec|biassec)
+Type of section to output.  The choices are "datasec" for the amplifier
+section which includes the bias if any is present, "trimsec" for the trim
+section, and "biassec" for the bias section.
+.le
+
+The remaining parameters come from the \fBimstatistics\fR task.
+.ih
+DESCRIPTION
+This script tasks uses the \fBquadsections\fR task to break the
+\fBquadformat\fR data into separate sections and runs the \fBimstatistics\fR
+task on the sections.
+.ih
+EXAMPLES
+
+1. To compute the mean and stddev of the data section.
+
+.nf
+    qu> qstat quad0072 fields=image,mean,stddev
+    #               IMAGE      MEAN    STDDEV
+     quad0072[1:1034,1:1024]     5537.     2647.
+     quad0072[1163:2196,1:1024]     6210.     5439.
+     quad0072[1:1034,1025:2048]     5364.     2535.
+     quad0072[1163:2196,1025:2048]     5862.     1327.
+.fi
+
+2. To compute the mean and stdev of the bias section.
+
+.nf
+    qu> qstat quad0072 fields=image,mean,stddev window=biassec
+    #               IMAGE      MEAN    STDDEV
+     quad0072[1045:1098,1:1024]      713.     1.272
+     quad0072[1099:1152,1:1024]     516.2     1.425
+     quad0072[1045:1098,1025:2048]     554.3     1.347
+     quad0072[1099:1152,1025:2048]     530.3     1.377
+.fi
+.ih
+SEE ALSO
+quadformat, quadsections, imstatistics
+.endhelp
diff --git a/noao/imred/quadred/doc/quadformat.hlp b/noao/imred/quadred/doc/quadformat.hlp
new file mode 100644
index 00000000..eb5fbfbd
--- /dev/null
+++ b/noao/imred/quadred/doc/quadformat.hlp
@@ -0,0 +1,392 @@
+.help quadformat Aug01 imred.quadred
+.ih
+NAME
+quadformat - Description of the special multi-amplifier CCD format
+.ih
+DESCRIPTION
+CCDs may be readout from multiple amplifiers at the same time to increase
+the readout speed.  This produces multiple images of rectangular regions in
+the full CCD exposure.  The amplifier readout images may be recorded in
+various ways.  One way is as extensions in a multiextension FITS file.
+This type of format can be reduced using the MSCRED package.
+
+Another way is to paste the regions into a single two-dimensional image.
+This, along with specific keywords to describe the locations of the
+regions, constitutes the \fIquadformat\fR format described here and used by the
+QUADRED package.  The term "quad" originates from the possibility of using
+four amplifiers in quadrants but the format also includes any other
+number of amplifiers.
+
+It is important to realize that this is a special format only as long as
+the overscan or prescan data is included in the image data.  Once this
+information is used and removed as part of the processing the resulting
+image can be treated in the same way as a single amplifier CCD image.
+However, the image can still contain the format keywords allowing the
+regions from the different amplifiers to be identified and extracted as
+needed.
+
+The \fIquadformat\fR consists of a single 2D image for a single CCD
+exposure.  The image storage format may be any standard image type such
+as imh or fits.  Within the image are regions containing the CCD
+pixel data and regions containing overscan or prescan, which we will
+call bias regions, for each amplifier.  The \fIquadformat\fR requires
+the bias regions to be attached to the CCD regions such that a single
+rectangular region contains both.
+
+Generally the rectangular regions are of equal size in order to sequence
+the amplifiers simultaneously.  However, it is possible for the regions
+to be unequal in cases of subregion readouts with certain CCD controllers.
+The figure below illustrates a "dual" and "quad" readout with equal
+size regions.
+
+.nf
+        +-----+-+-+-----+   +-----+-+-+-----+   +----------+-+
+        |  D  !B|B!  D  |   |  D  !B|B!  D  |   |     D    !B|
+        |  3  !3|4!  4  |   |  1  !1|2!  2  |   |     2    !2|
+        |     ! | !     |   |     ! | !     |   |          ! |
+        +-----+-+-+-----+   |     ! | !     |   +----------+-+
+        |  D  !B|B!  D  |   |     ! | !     |   |     D    !B|
+        |  1  !1|2!  2  |   |     ! | !     |   |     1    !1|
+        |     ! | !     |   |     ! | !     |   |          ! |
+        +-----+-+-+-----+   +-----+-+-+-----+   +----------+-+
+.fi
+
+The areas labeled D are the data sections and those labeled B are the
+bias sections.  The data and biases are match by the amplifier labels
+which are 1-4 in these examples.  The combination of the data and
+bias sections are called the amplifier sections.
+
+The regions are identified in the header by various keywords.  There is
+a header translation facility which allows for alternative keyword names.
+Below we describe the default keyword names in the absence of a translation.
+The number of regions and the amplifier labels are described by the
+string keyword AMPLIST.  The value is a string of space separated
+amplifier labels.  For the above four amplifier example it would be
+
+.nf
+    AMPLIST = '1 2 3 4'
+.fi
+
+For CTIO data the labels are '11  12 21 22'.   Note that the labels
+are appended to rootnames so they should be relatively short. 
+
+The amplifier labels are appended to various root names.  The important
+ones define "section" keywords.  The values are image sections that
+describe regions in an raster such as the image or the CCD.  The format
+of a section follows the standard IRAF notation "[c1:c2,l1:l2]" where
+c1 and c2 are inclusive column endpoints and l1 and l2 are inclusive
+line endpoints.
+
+The various sections are defined below.  The labels again show the default
+untranslated keyword roots.
+
+.ls ASEC
+The section of the image containing the amplifier readout.  This is the
+combination of the data and bias regions as shown in the figures.
+.le
+.ls DSEC
+The section of the image containing the actual CCD data exclusive of
+bias data.  In the figures these are the D regions.
+.le
+.ls BSEC
+The section of the image containing the bias data.  In the figures these
+are the B regions.
+.le
+.ls TSEC
+The second of the image containing the useful CCD data.  This defines
+a "trimming" area and lies within the data section.  It may also be
+the same as the data region.  During trimming the final image will only
+include the regions in the trim sections.  Note that it generally does
+not make sense to trim between amplifier regions but does make sense to
+trim regions at the edges of the CCD.
+.le
+.ls CSEC
+The section of the CCD corresponding to the data section in the image.
+The CCD is considered an ideal raster (without bias regions) and a
+section corresponds to the pixels in the CCD.  The CCD section must be
+the same size as the data section.  It is the CCD sections that define
+how the amplifiers will be pieced together to form a single image
+after trimming the bias region.
+.le
+
+There may be other keyword root names for things such as gains which
+have the amplifier labels appended.  However, none of these are used
+by the current software.  Example image headers are given
+in the EXAMPLES section.
+
+There is a limitation in the current software that the regions be recorded
+without horizontal or vertical flips.  In other words, where amplifiers
+from opposite corners are used some of them must be flipped by the
+data acquisition system before recording then in this \fBquadformat\fR.
+
+.ih
+EXAMPLES
+
+1.  The following is an example of a full 2048x2048 CCD readout with
+four amplifiers at CTIO.
+
+.nf
+qu> imhad quad0020
+quad0020[2196,2048][ushort]: IC 1257 5290 180s
+No bad pixels, min=435., max=61973.
+Line storage mode, physdim [2304,2048], length of user area 3079 s.u.
+Created Thu 08:35:57 23-Aug-2001, Last modified Thu 08:35:57 23-Aug-2001
+Pixel file "HDR$pixels/quad0020.pix" [ok]
+'KPNO-IRAF'           /
+'06-07-99'            /
+IRAF-MAX=           6.197300E4  /  DATA MAX
+IRAF-MIN=           4.350000E2  /  DATA MIN
+IRAF-BPX=                   16  /  DATA BITS/PIXEL
+IRAFTYPE= 'USHORT  '            /  PIXEL TYPE
+OPICNUM =                  123 / Original picture number
+HDR_REV = '2.000  13Feb96     (add mode and group to hdrs)' /
+IMAGETYP= 'OBJECT  '           / Type of picture (object, dark, etc.)
+DETECTOR= 'Site2K_6'           / Detector (CCD type, photon counter, etc.)
+PREFLASH=             0.000000 / Preflash time in secs
+CCDSUM  = '1 1     '           / On chip summation (X,Y)
+DATE-OBS= '07/07/99'           / Date (dd/mm/yy) of observation
+UTSHUT  = '01:14:40.0'         / UT of shutter open
+UT      = ' 1:14:41.50'         /  UT of TCS coords
+OBSERVAT= 'CTIO    '           / Origin of data
+TELESCOP= 'CTIO 1.5 meter telescope' / Specific system
+NAMPSYX = '2 2     '           / Num amps in y & x (eg. '2 2'=quad)
+AMPLIST = '11 21 12 22'        / Readout order in y,x
+ASEC11  = '[1:1098,1:1024]'    / Section read with Amp11
+CSEC11  = '[1:1034,1:1024]'    / Section in full CCD for DSEC11
+DSEC11  = '[1:1034,1:1024]'    / Image area in raw frame for Amp11
+TSEC11  = '[11:1034,1:1024]'   / Trim section definition for Amp11
+BSEC11  = '[1045:1098,1:1024]' / Bias section definition for Amp11
+BSEC12  = '[1099:1152,1:1024]' / Bias section definition for Amp12
+ASEC12  = '[1099:2196,1:1024]' / Section read with Amp12
+CSEC12  = '[1035:2068,1:1024]' / Section in full CCD for DSEC12
+DSEC12  = '[1163:2196,1:1024]' / Image area in raw frame for Amp12
+TSEC12  = '[1163:2186,1:1024]' / Trim section definition for Amp12
+ASEC21  = '[1:1098,1025:2048]' / Section read with Amp21
+CSEC21  = '[1:1034,1025:2048]' / Section in full CCD for DSEC21
+DSEC21  = '[1:1034,1025:2048]' / Image area in raw frame for Amp21
+TSEC21  = '[11:1034,1025:2048]' / Trim section definition for Amp21
+BSEC21  = '[1045:1098,1025:2048]' / Bias section definition for Amp21
+BSEC22  = '[1099:1152,1025:2048]' / Bias section definition for Amp22
+ASEC22  = '[1099:2196,1025:2048]' / Section read with Amp22
+CSEC22  = '[1035:2068,1025:2048]' / Section in full CCD for DSEC22
+DSEC22  = '[1163:2196,1025:2048]' / Image area in raw frame for Amp22
+TSEC22  = '[1163:2186,1025:2048]' / Trim section definition for Amp22
+WAVEFILE= 'Obs Tue Jul  6 20:11:59 1999' /
+NOTE    = 'WARNING: Lower amps reaching full well before ADCs saturate' /
+WAVEMODE= 'MPP OverlapXmit EarlyReset' / Waveform mode switches on
+GTRON22 =                4.100 / (e-) predicted read noise, upper right
+GTRON21 =                3.900 / (e-) predicted read noise, upper left
+GTRON12 =                4.200 / (e-) predicted read noise, lower right
+GTRON11 =                4.200 / (e-) predicted read noise, lower left
+GTGAIN22=                2.800 / (e-/ADU), predicted gain, upper right
+GTGAIN21=                3.100 / (e-/ADU) predicted gain, upper left
+GTGAIN12=                2.900 / (e-/ADU) predicted gain, lower right
+GTGAIN11=                3.200 / (e-/ADU) predicted gain, lower left
+GTINDEX =                    2 / Gain selection (index into Gain Table)
+PIXELT  =                29520 / (ns) unbinned pixel read time
+DCS_TIME=                 7000 / (ns) Double Correlated Sample time
+RA      = '17:27:10.82'         /  right ascension (telescope)
+DEC     = '-7:06:35.40'         /  declination (telescope)
+EPOCH   =               2000.0 / epoch of RA & DEC
+ZD      =                 35.9 / zenith distance (degrees)
+HA      = '-01:57:23.7'        / hour angle (H:M:S)
+ST      = '15:29:46.00'         /  sidereal time
+AIRMASS =                1.234 / airmass
+EXPTIME =              180.000 / Exposure time in secs
+DARKTIME=              181.309 / Total elapsed time in secs
+OBSERVER= 'Jacoby'             / Observers
+PROPID  = '92'                 / Proposal Id
+COMMENT Globular PNe
+TELID   = 'ct60'               / CTIO 1.5-m Telescope
+ARCONVER= '17Oct97ver7_22'     / Arcon software version
+COMMENT INSTRUMENT PARAMETERS
+INSTRUME= 'cfccd'              / cassegrain direct imager
+FILTER1 = 'dia'                / Filter in wheel one
+FNAME1  = 'diaphragm'          / Full name of filter in  wheel1
+FILTER2 = 'ocon'               / Filter in wheel two
+FNAME2  = 'O cont'             / Full name of filter in  wheel2
+FILTERS = 'dia ocon'           / Filter positions
+TELFOCUS=                57550 / Telescope focus
+XPIXSIZE=                0.432 / Pixel size in X (arcsec/pix)
+YPIXSIZE=                0.432 / Pixel size in Y (arcsec/pix)
+RECID   = 'ct60.990707.011817' / NOAO Archive record ID
+.fi
+
+2.  The following is a more complex readout of a region where the
+full 2Kx2K CCD is not readout and where even the regions are not the
+same size.
+
+.nf
+qu> imhead quad0013
+quad0013[1686,1538][ushort]: R sky flat 7s
+No bad pixels, min=393., max=65535.
+Line storage mode, physdim [1792,1538], length of user area 3079 s.u.
+Created Thu 08:34:00 23-Aug-2001, Last modified Thu 08:34:00 23-Aug-2001
+Pixel file "HDR$pixels/quad0013.pix" [ok]
+'KPNO-IRAF'           /
+'06-07-99'            /
+IRAF-MAX=           6.553500E4  /  DATA MAX
+IRAF-MIN=           3.930000E2  /  DATA MIN
+IRAF-BPX=                   16  /  DATA BITS/PIXEL
+IRAFTYPE= 'USHORT  '            /  PIXEL TYPE
+OPICNUM =                   15 / Original picture number
+HDR_REV = '2.000  13Feb96     (add mode and group to hdrs)' /
+IMAGETYP= 'SKY FLAT'           / Type of picture (object, dark, etc.)
+DETECTOR= 'Site2K_6'           / Detector (CCD type, photon counter, etc.)
+PREFLASH=             0.000000 / Preflash time in secs
+CCDSUM  = '1 1     '           / On chip summation (X,Y)
+DATE-OBS= '06/07/99'           / Date (dd/mm/yy) of observation
+UTSHUT  = '22:25:22.0'         / UT of shutter open
+UT      = '22:25:34.00'         /  UT of TCS coords
+OBSERVAT= 'CTIO    '           / Origin of data
+TELESCOP= 'CTIO 1.5 meter telescope' / Specific system
+NAMPSYX = '2 2     '           / Num amps in y & x (eg. '2 2'=quad)
+AMPLIST = '11 21 12 22'        / Readout order in y,x
+ASEC11  = '[1:843,1:769]'      / Section read with Amp11
+CSEC11  = '[256:1034,256:1024]' / Section in full CCD for DSEC11
+DSEC11  = '[1:779,1:769]'      / Image area in raw frame for Amp11
+TSEC11  = '[11:779,1:769]'     / Trim section definition for Amp11
+BSEC11  = '[790:843,1:769]'    / Bias section definition for Amp11
+BSEC12  = '[844:897,1:769]'    / Bias section definition for Amp12
+ASEC12  = '[844:1686,1:769]'   / Section read with Amp12
+CSEC12  = '[1035:1813,256:1024]' / Section in full CCD for DSEC12
+DSEC12  = '[908:1686,1:769]'   / Image area in raw frame for Amp12
+TSEC12  = '[908:1418,1:769]'   / Trim section definition for Amp12
+ASEC21  = '[1:843,770:1538]'   / Section read with Amp21
+CSEC21  = '[256:1034,1025:1793]' / Section in full CCD for DSEC21
+DSEC21  = '[1:779,770:1538]'   / Image area in raw frame for Amp21
+TSEC21  = '[11:779,770:1280]'  / Trim section definition for Amp21
+BSEC21  = '[790:843,770:1538]' / Bias section definition for Amp21
+BSEC22  = '[844:897,770:1538]' / Bias section definition for Amp22
+ASEC22  = '[844:1686,770:1538]' / Section read with Amp22
+CSEC22  = '[1035:1813,1025:1793]' / Section in full CCD for DSEC22
+DSEC22  = '[908:1686,770:1538]' / Image area in raw frame for Amp22
+TSEC22  = '[908:1418,770:1280]' / Trim section definition for Amp22
+WAVEFILE= 'Obs Tue Jul  6 18:07:56 1999' /
+NOTE    = 'WARNING: Lower amps reaching full well before ADCs saturate' /
+WAVEMODE= 'MPP OverlapXmit EarlyReset' / Waveform mode switches on
+GTRON22 =                4.100 / (e-) predicted read noise, upper right
+GTRON21 =                3.900 / (e-) predicted read noise, upper left
+GTRON12 =                4.200 / (e-) predicted read noise, lower right
+GTRON11 =                4.200 / (e-) predicted read noise, lower left
+GTGAIN22=                2.800 / (e-/ADU), predicted gain, upper right
+GTGAIN21=                3.100 / (e-/ADU) predicted gain, upper left
+GTGAIN12=                2.900 / (e-/ADU) predicted gain, lower right
+GTGAIN11=                3.200 / (e-/ADU) predicted gain, lower left
+GTINDEX =                    2 / Gain selection (index into Gain Table)
+PIXELT  =                29520 / (ns) unbinned pixel read time
+DCS_TIME=                 7000 / (ns) Double Correlated Sample time
+RA      = '14:53:52.67'         /  right ascension (telescope)
+DEC     = '-19:20:10.70'        /  declination (telescope)
+EPOCH   =               2000.0 / epoch of RA & DEC
+ZD      =                 32.1 / zenith distance (degrees)
+HA      = '-02:13:40.3'        / hour angle (H:M:S)
+ST      = '12:40:10.80'         /  sidereal time
+AIRMASS =                1.180 / airmass
+EXPTIME =                7.000 / Exposure time in secs
+DARKTIME=                8.239 / Total elapsed time in secs
+OBSERVER= 'Jacoby'             / Observers
+PROPID  = '92'                 / Proposal Id
+COMMENT
+TELID   = 'ct60'               / CTIO 1.5-m Telescope
+ARCONVER= '17Oct97ver7_22'     / Arcon software version
+COMMENT INSTRUMENT PARAMETERS
+INSTRUME= 'cfccd'              / cassegrain direct imager
+FILTER1 = 'dia'                / Filter in wheel one
+FNAME1  = 'diaphragm'          / Full name of filter in  wheel1
+FILTER2 = 'r'                  / Filter in wheel two
+FNAME2  = 'R'                  / Full name of filter in  wheel2
+FILTERS = 'dia r'              / Filter positions
+TELFOCUS=                    0 / Telescope focus
+XPIXSIZE=                0.432 / Pixel size in X (arcsec/pix)
+YPIXSIZE=                0.432 / Pixel size in Y (arcsec/pix)
+RECID   = 'ct60.990706.222551' / NOAO Archive record ID
+.fi
+
+3.  The following is for the raw image of example 2 after it has been
+processed by CCDPROC.  Note that the various bias, trim, and CCD sections are
+removed.  The AMPLIST and ASEC keywords remain and may be used to split
+or evaluate the individual amplifier regions with tasks such as QUADSECTIONS,
+QUADSPLIT, and QSTATISTICS.
+
+.nf
+qu> imhead quad0013
+quad0013[1280,1280][real]: R sky flat 7s
+No bad pixels, min=unknown, max=unknown
+Line storage mode, physdim [1280,1280], length of user area 2795 s.u.
+Created Fri 13:29:40 24-Aug-2001, Last modified Fri 13:29:40 24-Aug-2001
+Pixel file "HDR$pixels/quad0013.pix" [ok]
+'KPNO-IRAF'           /
+'06-07-99'            /
+New copy of quad0013
+IRAF-MAX=           6.553500E4  /  DATA MAX
+IRAF-MIN=           3.930000E2  /  DATA MIN
+IRAF-BPX=                   16  /  DATA BITS/PIXEL
+IRAFTYPE= 'USHORT  '            /  PIXEL TYPE
+OPICNUM =                   15 / Original picture number
+HDR_REV = '2.000  13Feb96     (add mode and group to hdrs)' /
+IMAGETYP= 'SKY FLAT'           / Type of picture (object, dark, etc.)
+DETECTOR= 'Site2K_6'           / Detector (CCD type, photon counter, etc.)
+PREFLASH=             0.000000 / Preflash time in secs
+CCDSUM  = '1 1     '           / On chip summation (X,Y)
+DATE-OBS= '06/07/99'           / Date (dd/mm/yy) of observation
+UTSHUT  = '22:25:22.0'         / UT of shutter open
+UT      = '22:25:34.00'         /  UT of TCS coords
+OBSERVAT= 'CTIO    '           / Origin of data
+TELESCOP= 'CTIO 1.5 meter telescope' / Specific system
+NAMPSYX = '2 2     '           / Num amps in y & x (eg. '2 2'=quad)
+AMPLIST = '11 21 12 22'        / Readout order in y,x
+ASEC11  = '[1:769,1:769]'      / Section read with Amp11
+ASEC12  = '[770:1280,1:769]'   / Section read with Amp12
+ASEC21  = '[1:769,770:1280]'   / Section read with Amp21
+ASEC22  = '[770:1280,770:1280]' / Section read with Amp22
+WAVEFILE= 'Obs Tue Jul  6 18:07:56 1999' /
+NOTE    = 'WARNING: Lower amps reaching full well before ADCs saturate' /
+WAVEMODE= 'MPP OverlapXmit EarlyReset' / Waveform mode switches on
+GTRON22 =                4.100 / (e-) predicted read noise, upper right
+GTRON21 =                3.900 / (e-) predicted read noise, upper left
+GTRON12 =                4.200 / (e-) predicted read noise, lower right
+GTRON11 =                4.200 / (e-) predicted read noise, lower left
+GTGAIN22=                2.800 / (e-/ADU), predicted gain, upper right
+GTGAIN21=                3.100 / (e-/ADU) predicted gain, upper left
+GTGAIN12=                2.900 / (e-/ADU) predicted gain, lower right
+GTGAIN11=                3.200 / (e-/ADU) predicted gain, lower left
+GTINDEX =                    2 / Gain selection (index into Gain Table)
+PIXELT  =                29520 / (ns) unbinned pixel read time
+DCS_TIME=                 7000 / (ns) Double Correlated Sample time
+RA      = '14:53:52.67'         /  right ascension (telescope)
+DEC     = '-19:20:10.70'        /  declination (telescope)
+EPOCH   =               2000.0 / epoch of RA & DEC
+ZD      =                 32.1 / zenith distance (degrees)
+HA      = '-02:13:40.3'        / hour angle (H:M:S)
+ST      = '12:40:10.80'         /  sidereal time
+AIRMASS =                1.180 / airmass
+EXPTIME =                7.000 / Exposure time in secs
+DARKTIME=                8.239 / Total elapsed time in secs
+OBSERVER= 'Jacoby'             / Observers
+PROPID  = '92'                 / Proposal Id
+COMMENT
+TELID   = 'ct60'               / CTIO 1.5-m Telescope
+ARCONVER= '17Oct97ver7_22'     / Arcon software version
+COMMENT INSTRUMENT PARAMETERS
+INSTRUME= 'cfccd'              / cassegrain direct imager
+FILTER1 = 'dia'                / Filter in wheel one
+FNAME1  = 'diaphragm'          / Full name of filter in  wheel1
+FILTER2 = 'r'                  / Filter in wheel two
+FNAME2  = 'R'                  / Full name of filter in  wheel2
+FILTERS = 'dia r'              / Filter positions
+TELFOCUS=                    0 / Telescope focus
+XPIXSIZE=                0.432 / Pixel size in X (arcsec/pix)
+YPIXSIZE=                0.432 / Pixel size in Y (arcsec/pix)
+RECID   = 'ct60.990706.222551' / NOAO Archive record ID
+TRIM    = 'Aug 24 13:29 Trim multiple overscan sections'
+OVERSCAN= 'Aug 24 13:29 Overscan is [790:843,1:769] with mean=714.3438'
+OVRSCN2 = 'Aug 24 13:29 Overscan is [790:843,770:1538] with mean=554.01'
+OVRSCN3 = 'Aug 24 13:29 Overscan is [844:897,1:769] with mean=519.7755'
+OVRSCN4 = 'Aug 24 13:29 Overscan is [844:897,770:1538] with mean=531.69'
+CCDSEC  = '[266:1545,256:1535]'
+CCDMEAN =             9727.605
+CCDMEANT=            683126983
+CCDPROC = 'Aug 24 13:29 CCD processing done'
+.fi
+.endhelp
diff --git a/noao/imred/quadred/doc/quadjoin.hlp b/noao/imred/quadred/doc/quadjoin.hlp
new file mode 100644
index 00000000..2a3a075e
--- /dev/null
+++ b/noao/imred/quadred/doc/quadjoin.hlp
@@ -0,0 +1,43 @@
+.help quadjoin Aug01 noao.imred.quadred
+.ih
+NAME
+quadjoin -- Split quadformat data into single amplifier images
+.ih
+USAGE
+quadjoin input
+.ih
+PARAMETERS
+.ls input
+Root name of images to be joined.  Extensions based on the AMPLIST
+keyword are applied to the root name.  This task does not
+allow a list of input root names.
+.le
+.ls output = ""
+Output image name.  If one is not given then the input root name is used.
+.le
+.ls delete = no
+Delete subimages on completion?
+.le
+.ih
+DESCRIPTION
+Images in split "quadformat" (see help topic \fBquadformat\fR and
+\fBquadsplit\fR) are rejoined into "quadformat".  The input images
+have a common root name and then an extension given by the amplifier
+labels in the AMPLIST keyword are added.  The output name may be specified
+or the input root name may be used.
+.ih
+EXAMPLES
+1. To join a split set of images:
+
+.nf
+    qu> dir quad0072*
+    quad0072.11.imh     quad0072.21.imh
+    quad0072.12.imh     quad0072.22.imh     
+    qu> quadjoin quad0072 delete+
+    qu> dir quad0072*
+    quad0072.imh
+.fi
+.ih
+SEE ALSO
+quadformat, quadsplit
+.endhelp
diff --git a/noao/imred/quadred/doc/quadscale.hlp b/noao/imred/quadred/doc/quadscale.hlp
new file mode 100644
index 00000000..7493bcf6
--- /dev/null
+++ b/noao/imred/quadred/doc/quadscale.hlp
@@ -0,0 +1,37 @@
+.help quadscale Aug01 noao.imred.quadred
+.ih
+NAME
+quadscale -- Scale amplifier sections by separate gains
+.ih
+USAGE
+quadscale input output
+.ih
+PARAMETERS
+.ls input
+Input image in \fBquadformat\fR to be scaled.
+.le
+.ls output
+Output scaled image in \fBquadformat\fR.
+.le
+.ls gain11 = 1., gain12 = 1., gain21 = 1., gain22 = 1.
+Gain factors for each quadrant.
+.le
+.ls operation = "multiply" (multiply|divide)
+The operation to apply with the gains.
+.le
+.ih
+DESCRIPTION
+This task multiplies or divides by gain factors for each amplifier in
+\fBquadformat\fR.
+.ih
+EXAMPLES
+
+1. To multiply by different gain factors.
+
+.nf
+    qu> quadscale quad0072 test gain11=1.2 gain12=1.3 gain21=1.4
+.fi
+.ih
+SEE ALSO
+quadformat
+.endhelp
diff --git a/noao/imred/quadred/doc/quadsections.hlp b/noao/imred/quadred/doc/quadsections.hlp
new file mode 100644
index 00000000..2735e3d5
--- /dev/null
+++ b/noao/imred/quadred/doc/quadsections.hlp
@@ -0,0 +1,81 @@
+.help quadsections Aug01 noao.imred.quadred
+.ih
+NAME
+quadsections -- Create image sections
+.ih
+USAGE
+quadsplit images
+.ih
+PARAMETERS
+.ls images
+List of image names for images in \fBquadformat\fR.
+.le
+.ls window = "datasec" (datasec|trimsec|biassec)
+Type of section to output.  The choices are "datasec" for the amplifier
+section which includes the bias if any is present, "trimsec" for the trim
+section, and "biassec" for the bias section.
+.le
+.ls section = ""
+Section to be overlapped.  The output sections will be the parts of the
+amplifier windows which are included within this section.
+.le
+.ls template = ""
+Template for producing the output.  The template replaces occurs of
+$I with the image name, $S with the section, and $A with the amplifier
+label.  If none is specified then the default template "$I$S\\n" is
+used which produces the image name with section separated by new-lines.
+The special characters "\n" is the new-line and the extra "\" is
+required to pass the new-line through to the formatting routine.
+.le
+.ih
+DESCRIPTION
+Images in "quadformat" (see help topic \fBquadformat\fR) are broken down
+in sections and written to the standard output in a specified format.
+.ih
+EXAMPLES
+1. To print the default data sections.
+
+.nf
+    qu> quadsec quad0072
+    quad0072[1:1034,1:1024]
+    quad0072[1163:2196,1:1024]
+    quad0072[1:1034,1025:2048]
+    quad0072[1163:2196,1025:2048]
+.fi
+
+3. To apply an overlap section.
+
+.nf
+    qu> quadsec quad0072 section=[1000:2000,1000:2000]
+    quad0072[1000:1034,1000:1024]
+    quad0072[1163:2000,1000:1024]
+    quad0072[1000:1034,1025:2000]
+    quad0072[1163:2000,1025:2000]
+.fi
+
+2. To print the trim sections.
+
+.nf
+    qu> quadsec quad0072 window=trimsec
+    quad0072[11:1034,1:1024]
+    quad0072[1163:2186,1:1024]
+    quad0072[11:1034,1025:2048]
+    quad0072[1163:2186,1025:2048]
+.fi
+
+
+4.  To make a custom output.
+
+.nf
+    qu> quadsec quad0072 template="image=$I, section=$S, amplifier=$A\\n"
+    image=quad0072, section=[1:1034,1:1024], amplifier=11
+    image=quad0072, section=[1163:2196,1:1024], amplifier=12
+    image=quad0072, section=[1:1034,1025:2048], amplifier=21
+    image=quad0072, section=[1163:2196,1025:2048], amplifier=22
+    qu> quadsec quad0072 template="$I.$A,"
+    quad0072.11,quad0072.12,quad0072.21,quad0072.22,
+.fi
+.ih
+SEE ALSO
+quadformat
+.endhelp
diff --git a/noao/imred/quadred/doc/quadsplit.hlp b/noao/imred/quadred/doc/quadsplit.hlp
new file mode 100644
index 00000000..4a0adf66
--- /dev/null
+++ b/noao/imred/quadred/doc/quadsplit.hlp
@@ -0,0 +1,49 @@
+.help quadsplit Aug01 noao.imred.quadred
+.ih
+NAME
+quadsplit -- Split quadformat data into single amplifier images
+.ih
+USAGE
+quadsplit input
+.ih
+PARAMETERS
+.ls input
+Image name of \fIquadformat\fR image to be split.  This task does not
+allow a list of input names.
+.le
+.ls output = ""
+Output root name to which the AMPLIST amplifier identifiers will be
+appended to form the split images.  If no output name is given then
+the input name is used as the root name.
+.le
+.ls clobber = yes
+Clobber any existing images?
+.le
+.ih
+DESCRIPTION
+Images in "quadformat" (see help topic \fBquadformat\fR) are separated
+into images containing data from only one amplifier.  The output images
+have a common root name and then an extension given by the amplifier
+labels in the AMPLIST keyword.  The output root name may be specified
+or default to the input name.
+
+In addition to producing the individual images keywords, are added that
+are understood by the standard \fBccdproc\fR task for single amplifier
+CCD reductions.
+
+The task \fBquadjoin\fR may be used to rejoin images that were split
+by this task.
+.ih
+EXAMPLES
+1. To spit an image:
+
+.nf
+    qu> quadsplit quad0072
+    qu> dir quad0072*
+    quad0072.11.imh     quad0072.21.imh     quad0072.imh        
+    quad0072.12.imh     quad0072.22.imh     
+.fi
+.ih
+SEE ALSO
+quadformat, quadjoin
+.endhelp
diff --git a/noao/imred/quadred/mkpkg b/noao/imred/quadred/mkpkg
new file mode 100644
index 00000000..3a55a03a
--- /dev/null
+++ b/noao/imred/quadred/mkpkg
@@ -0,0 +1,8 @@
+# Make the package.
+
+$call	update@src
+$exit
+
+update:
+	$call update@src
+	;
diff --git a/noao/imred/quadred/quadred.cl b/noao/imred/quadred/quadred.cl
new file mode 100644
index 00000000..74592010
--- /dev/null
+++ b/noao/imred/quadred/quadred.cl
@@ -0,0 +1,68 @@
+#{ QUADRED -- QUAD CCD Reduction Package
+
+set	ccddb	= "ccdred$ccddb/"
+
+package quadred
+
+# Special version of CCDPROC.
+
+set	quadsrc		= "quadred$src/ccdproc/"
+
+task	ccdproc		= quadsrc$x_quadred.e
+task	qccdproc	= quad$x_ccdred.e
+
+# Task from the CTIO QUAD package.
+
+set	quad		= "quadred$src/quad/"
+
+task	quadsplit,
+	quadjoin,
+	quadscale,
+	quadsections,
+	ccddelete,
+	ccdprcselect,
+	ccdssselect,
+	ccdsection,
+	qpcalimage,
+	qpselect,
+	gainmeasure,
+	ccdgetparam		= "quad$x_quad.e"
+
+task	quadproc		= "quad$quadproc.cl"
+task	qproc			= "quad$qproc.cl"
+task	qnoproc			= "quad$qnoproc.cl"
+task	qstatistics		= "quad$qstatistics.cl"
+task	qhistogram		= "quad$qhistogram.cl"
+
+task	setinstrument		= "quad$setinstrument.cl"
+
+hidetask ccdgetparam, ccddelete, ccdprcselect, ccdssselect, ccdsection
+hidetask qpcalimage, qpselect, qproc, qnoproc, qccdproc
+
+# Special versions which run quadproc rather than ccdproc
+task	qdarkcombine	= quad$qdarkcombine.cl
+task	qflatcombine	= quad$qflatcombine.cl
+task	qzerocombine	= quad$qzerocombine.cl
+
+
+# Tasks from the standard CCDRED package.
+
+task	badpiximage,
+	ccdgroups,
+	ccdhedit,
+	ccdinstrument,
+	ccdlist,
+	ccdmask,
+	combine,
+	mkfringecor,
+	mkillumcor,
+	mkillumflat,
+	mkskycor,
+	mkskyflat	= ccdred$x_ccdred.e
+
+task	darkcombine	= ccdred$darkcombine.cl
+task	flatcombine	= ccdred$flatcombine.cl
+#task	setinstrument	= ccdred$setinstrument.cl
+task	zerocombine	= ccdred$zerocombine.cl
+
+clbye()
diff --git a/noao/imred/quadred/quadred.hd b/noao/imred/quadred/quadred.hd
new file mode 100644
index 00000000..b542fec9
--- /dev/null
+++ b/noao/imred/quadred/quadred.hd
@@ -0,0 +1,22 @@
+# Help directory for the QUADRED package.
+
+$doc		= "./doc/"
+$cdoc		= "./src/ccdproc/doc/"
+$qdoc		= "./src/quad/doc/"
+
+package		hlp=doc$quad.hlp
+quadformat	hlp=doc$quadformat.hlp
+quadsplit	hlp=doc$quadsplit.hlp
+quadjoin	hlp=doc$quadjoin.hlp
+quadsections	hlp=doc$quadsections.hlp
+qstatistics	hlp=doc$qstatistics.hlp
+qhistogram	hlp=doc$qhistogram.hlp
+quadscale	hlp=doc$quadscale.hlp
+
+ccdproc		hlp=cdoc$ccdproc.hlp
+
+quadproc	hlp=qdoc$quadproc.hlp
+#quadreadout	hlp=qdoc$quadreadout.hlp
+#quadman	hlp=qdoc$quadman.hlp
+
+revisions	sys=Revisions
diff --git a/noao/imred/quadred/quadred.men b/noao/imred/quadred/quadred.men
new file mode 100644
index 00000000..6a0225a5
--- /dev/null
+++ b/noao/imred/quadred/quadred.men
@@ -0,0 +1,61 @@
+     SPECIAL VERSION OF CCDRED PACKAGE FOR MULTI-AMPLIFIER CCD IMAGES
+
+The package has a special quad version of CCDPROC that processes
+multi-amplifier CCD images in a particular format.  See help topic
+"quadformat" for a description of the format.  The task QUADPROC is
+largely obsoleted by the quad version of CCDPROC but may be used by
+those familiar with the ARED.QUAD package or to use features in the
+standard CCDPROC that are not in the quad version.  Those features
+include line-by-line overscan functions.
+
+
+	     		STANDARD CCDRED TASKS
+
+    badpiximage - Create a bad pixel mask image from a bad pixel file
+      ccdgroups - Group CCD images into image lists
+       ccdhedit - CCD image header editor
+  ccdinstrument - Review and edit instrument translation files
+        ccdlist - List CCD processing information
+	ccdmask - Make a bad pixel mask from CCD data
+        ccdproc - Process CCD images (including quadformat data)
+        combine - Combine CCD images
+    darkcombine - Combine and process dark count images
+    flatcombine - Combine and process flat field images
+    mkfringecor - Make fringe correction images from sky images
+     mkillumcor - Make flat field illumination correction images
+    mkillumflat - Make illumination corrected flat fields
+       mkskycor - Make sky illumination correction images
+      mkskyflat - Make sky corrected flat field images
+  setinstrument - Set instrument parameters
+    zerocombine - Combine and process zero level images
+
+	     SPECIAL TASKS FOR MULTI-AMPLIFIER CCD IMAGES IN QUADFORMAT
+
+    gainmeasure - Measure gains in quadformat images
+      quadscale - Scale sections by gain factors
+    qstatistics - Calculate image statistics for multi-amplifier CCD images
+   quadsections - Produce image section list for sections of quadformat images
+     qhistogram - Make histogram of multi-amplifier CCD image
+      quadsplit - Split quadformat data into individual single amplifier images
+       quadjoin - Rejoin single amplifier images produced by quadsplit
+
+		ALTERNATIVE TASKS
+
+       quadproc - Process multi-amplifier CCD images (see also ccdproc)
+   qdarkcombine - Combine and process dark count images using quadproc
+   qflatcombine - Combine and process flat field images using quadproc
+   qzerocombine - Combine and process zero level images using quadproc
+
+   There is no separate help for the quadproc versions of the combining
+   tasks.  See the help for the standard versions.
+
+    	      ADDITIONAL HELP TOPICS
+
+        package - Package parameters and overview
+     quadformat - Format for multi-amplifier CCD images
+    ccdgeometry - Discussion of CCD coordinate/geometry keywords
+       ccdtypes - Description of the CCD image types
+     flatfields - Discussion of CCD flat field calibrations
+          guide - Introductory guide to using the CCDRED package
+    instruments - Instrument specific data files
+        subsets - Description of CCD subsets
diff --git a/noao/imred/quadred/quadred.par b/noao/imred/quadred/quadred.par
new file mode 100644
index 00000000..05c8d112
--- /dev/null
+++ b/noao/imred/quadred/quadred.par
@@ -0,0 +1,13 @@
+# QUADRED package parameter file
+
+proctask,s,h,"ccdproc","ccdproc|quadproc",,Processing task
+pixeltype,s,h,"real real",,,Output and calculation pixel datatypes
+verbose,b,h,no,,,Print log information to the standard output?
+logfile,f,h,"logfile",,,Text log file
+plotfile,f,h,"",,,Log metacode plot file
+backup,s,h,"",,,Backup directory or prefix
+instrument,s,h,"",,,CCD instrument file
+ssfile,s,h,"subsets",,,Subset translation file
+graphics,s,h,"stdgraph",,,Interactive graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+version,s,h,"V1.0: August 22, 2001"
diff --git a/noao/imred/quadred/src/Revisions b/noao/imred/quadred/src/Revisions
new file mode 100644
index 00000000..bbdfcc7d
--- /dev/null
+++ b/noao/imred/quadred/src/Revisions
@@ -0,0 +1,42 @@
+.help revisions Jun88 noao.imred.quadred
+.nf
+
+ccdproc/ccdcache.x
+    The 'bufs' pointer was declared as TY_REAL instead of TY_SHORT (5/4/13)
+
+quad/qproc.cl
+quad/quad.cl
+quad/quadjoin.x
+quad/quadproc.cl
+quad/setinstrument.cl
+quad/qccdproc.par	+
+../quadred.cl
+../quadred.men
+    When using quadproc the latest CCDPROC is used with the alias QCCDPROC.
+    This is to allow using the line-by-line overscan function.  Other features
+    in CCDPROC would also be available.  It was too hard to update the
+    quad version of CCDPROC.  (3/12/08, Valdes)
+
+=====
+V2.14
+=====
+
+=======
+V2.12.1
+=======
+
+quad/qproc.cl
+    For some reason the quadsplit call was commented out.  So when quadproc
+    is run the pieces are not split and then the quadjoin call results in
+    a divide by zero error.  The call was uncommented.  Due to my lack
+    of understanding with QUAD and that multipiece CCDPROC is used which
+    does not support trims, the quadsplit with trimming is not used.
+    (7/5/02, Valdes)
+
+=====
+V2.12
+=====
+
+New package consisting of XCCDRED and ARED.QUAD was added.
+
+.endhelp
diff --git a/noao/imred/quadred/src/ccdproc/calimage.x b/noao/imred/quadred/src/ccdproc/calimage.x
new file mode 100644
index 00000000..8a6007c1
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/calimage.x
@@ -0,0 +1,367 @@
+include	<error.h>
+include	<imset.h>
+include	"ccdtypes.h"
+
+define	SZ_SUBSET	16			# Maximum size of subset string
+define	IMAGE	Memc[$1+($2-1)*SZ_FNAME]	# Image string
+define	SUBSET	Memc[$1+($2-1)*SZ_SUBSET]	# Subset string
+
+# CAL_IMAGE -- Return a calibration image for a specified input image.
+# CAL_OPEN  -- Open the calibration image list.
+# CAL_CLOSE -- Close the calibration image list.
+# CAL_LIST  -- Add images to the calibration image list.
+#
+# The open procedure is called first to get the calibration image
+# lists and add them to an internal list.  Calibration images from the
+# input list are also added so that calibration images may be specified
+# either from the calibration image list parameters or in the input image list.
+# Existence errors and duplicate calibration images are ignored.
+# Validity checks are made when the calibration images are requested.
+#
+# During processing the calibration image names are requested for each input
+# image.  The calibration image list is searched for a calibration image of
+# the right type and subset.  If more than one is found the first one is
+# returned and a warning given for the others.  The warning is only issued
+# once.  If no calibration image is found then an error is returned.
+#
+# The calibration image list must be closed at the end of processing the
+# input images.
+
+
+# CAL_IMAGE -- Return a calibration image of a particular type.
+# Search the calibration list for the first calibration image of the desired
+# type and subset.  Print a warning if there  is more than one possible
+# calibration image and return an error if there is no calibration image. 
+
+procedure cal_image (im, ccdtype, nscan, image, maxchars)
+
+pointer	im		# Image to be processed
+int	ccdtype		# Callibration CCD image type desired
+int	nscan		# Number of scan rows desired
+char	image[maxchars]	# Calibration image (returned)
+int	maxchars	# Maximum number chars in image name
+
+int	i, m, n
+pointer	sp, subset, str
+bool	strne(), ccd_cmp()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subsets
+pointer	nscans		# Pointer to array of calibration nscan values
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, nscans, images, nimages
+
+begin
+	call smark (sp)
+	call salloc (subset, SZ_SUBSET, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	m = 0
+	n = 0
+	switch (ccdtype) {
+	case ZERO, DARK:
+	    do i = 1, nimages {
+		if (Memi[ccdtypes+i-1] != ccdtype)
+		    next
+		n = n + 1
+		if (n == 1) {
+		    m = i
+		} else {
+		    if (Memi[nscans+i-1] == Memi[nscans+m-1]) {
+#			call eprintf (
+#			    "Warning: Extra calibration image %s ignored\n")
+#			    call pargstr (IMAGE(images,i))
+
+			# Reset the image type to eliminate further warnings.
+			Memi[ccdtypes+i-1] = UNKNOWN
+		    } else if (Memi[nscans+m-1] != nscan &&
+			       (Memi[nscans+i-1] == nscan ||
+			       Memi[nscans+i-1] == 1)) {
+			m = i
+		    }
+		}
+	    }
+	case FLAT, ILLUM, FRINGE:
+	    call ccdsubset (im, Memc[subset], SZ_SUBSET)
+
+	    do i = 1, nimages {
+		if (Memi[ccdtypes+i-1] != ccdtype)
+		    next
+		if (strne (SUBSET(subsets,i), Memc[subset]))
+		    next
+		n = n + 1
+		if (n == 1) {
+		    m = i
+		} else {
+		    if (Memi[nscans+i-1] == Memi[nscans+m-1]) {
+#			call eprintf (
+#			    "Warning: Extra calibration image %s ignored\n")
+#			    call pargstr (IMAGE(images,i))
+
+			# Reset the image type to eliminate further warnings.
+			Memi[ccdtypes+i-1] = UNKNOWN
+		    } else if (Memi[nscans+m-1] != nscan &&
+			       (Memi[nscans+i-1] == nscan ||
+			       Memi[nscans+i-1] == 1)) {
+			m = i
+		    }
+		}
+	    }
+	}
+
+	# If no calibration image is found then it is an error.
+	if (m == 0) {
+	    switch (ccdtype) {
+	    case ZERO:
+	        call error (0, "No zero level calibration image found")
+	    case DARK:
+	        call error (0, "No dark count calibration image found")
+	    case FLAT:
+		call sprintf (Memc[str], SZ_LINE,
+	             "No flat field calibration image of subset %s found")
+		     call pargstr (Memc[subset])
+	        call error (0, Memc[str])
+	    case ILLUM:
+		call sprintf (Memc[str], SZ_LINE,
+	             "No illumination calibration image of subset %s found")
+		     call pargstr (Memc[subset])
+	        call error (0, Memc[str])
+	    case FRINGE:
+		call sprintf (Memc[str], SZ_LINE,
+	             "No fringe calibration image of subset %s found")
+		     call pargstr (Memc[subset])
+	        call error (0, Memc[str])
+	    }
+	}
+
+	call strcpy (IMAGE(images,m), image, maxchars)
+	if (nscan != Memi[nscans+m-1]) {
+	    if (nscan != 1 && Memi[nscans+m-1] == 1)
+		call cal_scan (nscan, image, maxchars)
+	    else {
+		call sprintf (Memc[str], SZ_LINE,
+	             "Cannot find or create calibration with nscan of %d")
+		     call pargi (nscan)
+	        call error (0, Memc[str])
+	    }
+	}
+
+	# Check that the input image is not the same as the calibration image.
+	call imstats (im, IM_IMAGENAME, Memc[str], SZ_LINE)
+	if (ccd_cmp (Memc[str], IMAGE(images,m))) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Calibration image %s is the same as the input image")
+		call pargstr (image)
+	    call error (0, Memc[str])
+	}
+
+	call sfree (sp)
+end
+
+
+# CAL_OPEN -- Create a list of calibration images from the input image list
+# and the calibration image lists.
+
+procedure cal_open (list)
+
+int	list		# List of input images
+int	list1		# List of calibration images
+
+pointer	sp, str
+int	ccdtype, strdic(), imtopenp()
+bool	clgetb()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subset numbers
+pointer	nscans		# Pointer to array of calibration nscan values
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, nscans, images, nimages
+
+errchk	cal_list
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	call clgstr ("ccdtype", Memc[str], SZ_LINE)
+	call xt_stripwhite (Memc[str])
+	if (Memc[str] == EOS)
+	    ccdtype = NONE
+	else
+	    ccdtype = strdic (Memc[str], Memc[str], SZ_LINE, CCDTYPES)
+
+	# Add calibration images to list.
+	nimages = 0
+	if (ccdtype != ZERO && clgetb ("zerocor")) {
+	    list1 = imtopenp ("zero")
+	    call cal_list (list1, ZERO)
+	    call imtclose (list1)
+	}
+	if (ccdtype != ZERO && ccdtype != DARK && clgetb ("darkcor")) {
+	    list1 = imtopenp ("dark")
+	    call cal_list (list1, DARK)
+	    call imtclose (list1)
+	}
+	if (ccdtype != ZERO && ccdtype != DARK && ccdtype != FLAT &&
+	    clgetb ("flatcor")) {
+	    list1 = imtopenp ("flat")
+	    call cal_list (list1, FLAT)
+	    call imtclose (list1)
+	}
+	if (ccdtype != ZERO && ccdtype != DARK && ccdtype != FLAT &&
+	    ccdtype != ILLUM && clgetb ("illumcor")) {
+	    list1 = imtopenp ("illum")
+	    call cal_list (list1, ILLUM)
+	    call imtclose (list1)
+	}
+	if (ccdtype != ZERO && ccdtype != DARK && ccdtype != FLAT &&
+	    ccdtype != FRINGE && clgetb ("fringecor")) {
+	    list1 = imtopenp ("fringe")
+	    call cal_list (list1, FRINGE)
+	    call imtclose (list1)
+	}
+	if (list != NULL) {
+	    call cal_list (list, UNKNOWN)
+	    call imtrew (list)
+	}
+
+	call sfree (sp)
+end
+
+
+# CAL_CLOSE -- Free memory from the internal calibration image list.
+
+procedure cal_close ()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subset
+pointer	nscans		# Pointer to array of calibration nscan values
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, nscans, images, nimages
+
+begin
+	if (nimages > 0) {
+	    call mfree (ccdtypes, TY_INT)
+	    call mfree (subsets, TY_CHAR)
+	    call mfree (nscans, TY_INT)
+	    call mfree (images, TY_CHAR)
+	}
+end
+
+
+# CAL_LIST -- Add calibration images to an internal list.
+# Map each image and get the CCD image type and subset.
+# If the ccdtype is given as a procedure argument this overrides the
+# image header type.  For the calibration images add the type, subset,
+# and image name to dynamic arrays.  Ignore duplicate names.
+
+procedure cal_list (list, listtype)
+
+pointer	list		# Image list
+int	listtype	# CCD type of image in list.
+			# Overrides header type if not UNKNOWN.
+
+int	i, ccdtype, ccdtypei(), ccdnscan(), imtgetim()
+pointer	sp, image, im, immap()
+bool	streq()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subsets
+pointer	nscans		# Pointer to array of calibration nscan values
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, nscans, images, nimages
+
+begin
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+
+	while (imtgetim (list, Memc[image], SZ_FNAME) != EOF) {
+	    # Open the image.  If an explicit type is given it is an
+	    # error if the image can't be opened.
+	    iferr (im = immap (Memc[image], READ_ONLY, 0)) {
+		if (listtype == UNKNOWN)
+		    next
+		else
+		    call erract (EA_ERROR)
+	    }
+
+	    # Override image header CCD type if a list type is given.
+	    if (listtype == UNKNOWN)
+	        ccdtype = ccdtypei (im)
+	    else
+		ccdtype = listtype
+		
+	    switch (ccdtype) {
+	    case ZERO, DARK, FLAT, ILLUM, FRINGE:
+		# Check for duplication.
+		for (i=1; i<=nimages; i=i+1)
+		    if (streq (Memc[image], IMAGE(images,i)))
+			break
+		if (i <= nimages)
+		    break
+
+		# Allocate memory for a new image.
+		if (i == 1) {
+		    call malloc (ccdtypes, i, TY_INT)
+		    call malloc (subsets, i * SZ_SUBSET, TY_CHAR)
+		    call malloc (nscans, i, TY_INT)
+		    call malloc (images, i * SZ_FNAME, TY_CHAR)
+		} else {
+		    call realloc (ccdtypes, i, TY_INT)
+		    call realloc (subsets, i * SZ_FNAME, TY_CHAR)
+		    call realloc (nscans, i, TY_INT)
+		    call realloc (images, i * SZ_FNAME, TY_CHAR)
+		}
+
+		# Enter the ccdtype, subset, and image name.
+		Memi[ccdtypes+i-1] = ccdtype
+		Memi[nscans+i-1] = ccdnscan (im, ccdtype)
+		call ccdsubset (im, SUBSET(subsets,i), SZ_SUBSET-1)
+		call strcpy (Memc[image], IMAGE(images,i), SZ_FNAME-1)
+		nimages = i
+	    }
+	    call imunmap (im)
+	}
+	call sfree (sp)
+end
+
+
+# CAL_SCAN -- Generate name for scan corrected calibration image.
+
+procedure cal_scan (nscan, image, maxchar)
+
+int	nscan			#I Number of scan lines
+char	image[maxchar]		#U Input root name, output scan name
+int	maxchar			#I Maximum number of chars in image name
+
+bool	clgetb()
+pointer	sp, root, ext
+
+begin
+	# Check if this operation is desired.
+	if (!clgetb ("scancor") || nscan == 1)
+	    return
+
+	call smark (sp)
+	call salloc (root, SZ_FNAME, TY_CHAR)
+	call salloc (ext, SZ_FNAME, TY_CHAR)
+
+	call xt_imroot (image, Memc[root], SZ_FNAME)
+	call xt_imext (image, Memc[ext], SZ_FNAME)
+	if (IS_INDEFI (nscan)) {
+	    call sprintf (image, maxchar, "%s.1d%s")
+		call pargstr (Memc[root])
+		call pargstr (Memc[ext])
+	} else {
+	    call sprintf (image, maxchar, "%s.%d%s")
+		call pargstr (Memc[root])
+		call pargi (nscan)
+		call pargstr (Memc[ext])
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/ccdcache.com b/noao/imred/quadred/src/ccdproc/ccdcache.com
new file mode 100644
index 00000000..91ffae12
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdcache.com
@@ -0,0 +1,10 @@
+# Common data defining the cached images and data.
+
+int	ccd_ncache		# Number of images cached
+int	ccd_maxcache		# Maximum size of cache
+int	ccd_szcache		# Current size of cache
+int	ccd_oldsize		# Original memory size
+int	ccd_pcache		# Pointer to image cache structures
+
+common	/ccdcache_com/ ccd_ncache, ccd_maxcache, ccd_szcache, ccd_oldsize,
+	ccd_pcache
diff --git a/noao/imred/quadred/src/ccdproc/ccdcache.h b/noao/imred/quadred/src/ccdproc/ccdcache.h
new file mode 100644
index 00000000..f7de3a2c
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdcache.h
@@ -0,0 +1,10 @@
+# Definition for image cache structure.
+
+define	CCD_LENCACHE		6
+
+define	CCD_IM		Memi[$1]	# IMIO pointer
+define	CCD_NACCESS	Memi[$1+1]	# Number of accesses requested
+define	CCD_SZDATA	Memi[$1+2]	# Size of data in cache in chars
+define	CCD_DATA	Memi[$1+3]	# Pointer to data cache
+define	CCD_BUFR	Memi[$1+4]	# Pointer to real image line
+define	CCD_BUFS	Memi[$1+5]	# Pointer to short image line
diff --git a/noao/imred/quadred/src/ccdproc/ccdcache.x b/noao/imred/quadred/src/ccdproc/ccdcache.x
new file mode 100644
index 00000000..78f84ace
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdcache.x
@@ -0,0 +1,381 @@
+include	<imhdr.h>
+include	<imset.h>
+include	<mach.h>
+include	"ccdcache.h"
+
+.help ccdcache Jun87
+.nf ---------------------------------------------------------------------
+The purpose of the CCD image caching package is to minimize image mapping
+time, to prevent multiple mapping of the same image, and to keep entire
+calibration images in memory for extended periods to minimize disk
+I/O.  It is selected by specifying a maximum caching size based on the
+available memory.  When there is not enough memory for caching (or by
+setting the size to 0) then standard IMIO is used.  When there is
+enough memory then as many images as will fit into the specified cache
+size are kept in memory.  Images are also kept mapped until explicitly
+flushed or the entire package is closed.
+
+This is a special purpose interface intended only for the CCDRED package.
+It has the following restrictions.
+
+    1.  Images must be processed to be cached.
+    2.  Images must be 2 dimensional to be cached
+    3.  Images must be real or short to be cached.
+    4.  Images must be read_only to be cached.
+    5.  Cached images remain in memory until they are displaced,
+	flushed, or the package is closed.
+
+The package consists of the following procedures.
+
+	      ccd_open ()
+	 im = ccd_cache (image)
+	ptr = ccd_glr (im, col1, col2, line)
+	ptr = ccd_gls (im, col1, col2, line)
+	      ccd_unmap (im)
+	      ccd_flush (im)
+	      ccd_close ()
+
+
+CCD_OPEN:   Initialize the image cache.  Called at the beginning.
+CCD_CLOSE:  Flush the image cache and restore memory.  Called at the end.
+
+CCD_CACHE:  Open an image and save the IMIO pointer.  If the image has been
+opened previously it need not be opened again.  If image data caching
+is specified the image data may be read it into memory.  In order for
+image data caching to occur the the image has to have been processed,
+be two dimensional, be real or short, and the total cache memory not
+be exceeded.  If an error occurs in reading the image into memory
+the data is not cached.
+
+CCD_UNMAP:  The image access number is decremented but the image
+is not closed against the event it will be used again.
+
+CCD_FLUSH:  The image is closed and flushed from the cache.
+
+CCD_GLR, CCD_GLS: Get a real or short image line.  If the image data is cached
+then a pointer to the line is quickly returned.  If the data is not cached then
+IMIO is used to get the pointer.
+.endhelp ---------------------------------------------------------------------
+
+
+
+# CCD_CACHE -- Open an image and possibly cache it in memory.
+
+pointer procedure ccd_cache (image, ccdtype)
+
+char	image[ARB]		# Image to be opened
+int	ccdtype			# Image type
+
+int	i, nc, nl, nbytes
+pointer	sp, str, pcache, pcache1, im
+
+int	sizeof()
+pointer	immap(), imgs2r(), imgs2s()
+bool	streq(), ccdcheck()
+errchk	immap, imgs2r, imgs2s
+
+include	"ccdcache.com"
+
+define	done_		99
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Check if the image is cached.
+	for (i=1; i<=ccd_ncache; i=i+1) {
+	    pcache = Memi[ccd_pcache+i-1]
+	    im = CCD_IM(pcache)
+	    call imstats (im, IM_IMAGENAME, Memc[str], SZ_LINE)
+	    if (streq (image, Memc[str]))
+		break
+	}
+
+	# If the image is not cached open it and allocate memory.
+	if (i > ccd_ncache) {
+	    im = immap (image, READ_ONLY, 0)
+	    ccd_ncache = i
+	    call realloc (ccd_pcache, ccd_ncache, TY_INT)
+	    call malloc (pcache, CCD_LENCACHE, TY_STRUCT)
+	    Memi[ccd_pcache+i-1] = pcache
+	    CCD_IM(pcache) = im
+	    CCD_NACCESS(pcache) = 0
+	    CCD_SZDATA(pcache) = 0
+	    CCD_DATA(pcache) = NULL
+	    CCD_BUFR(pcache) = NULL
+	    CCD_BUFS(pcache) = NULL
+	}
+
+	# If not caching the image data or if the image data has already
+	# been cached we are done.
+	if ((ccd_maxcache == 0) || (CCD_SZDATA(pcache) > 0))
+	    goto done_
+
+	# Don't cache unprocessed calibration image data.
+	# This is the only really CCDRED specific code.
+	if (ccdcheck (im, ccdtype))
+	    goto done_
+
+	# Check image is 2D and a supported pixel type.
+	if (IM_NDIM(im) != 2)
+	    goto done_
+	if ((IM_PIXTYPE(im) != TY_REAL) && (IM_PIXTYPE(im) !=TY_SHORT))
+	    goto done_
+
+	# Compute the size of the image data.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	nbytes = nc * nl * sizeof (IM_PIXTYPE(im)) * SZB_CHAR
+
+	# Free memory not in use.
+	if (ccd_szcache + nbytes > ccd_maxcache) {
+	    for (i=1; i<=ccd_ncache; i=i+1) {
+	        pcache1 = Memi[ccd_pcache+i-1]
+	        if (CCD_NACCESS(pcache1) == 0) {
+		    if (CCD_SZDATA(pcache1) > 0) {
+		        ccd_szcache = ccd_szcache - CCD_SZDATA(pcache1)
+		        CCD_SZDATA(pcache1) = 0
+		        CCD_DATA(pcache1) = NULL
+			call mfree (CCD_BUFR(pcache1), TY_REAL)
+			call mfree (CCD_BUFS(pcache1), TY_SHORT)
+		        call imseti (CCD_IM(pcache1), IM_CANCEL, YES)
+		        if (ccd_szcache + nbytes > ccd_maxcache)
+		            break
+		    }
+	        }
+	    }
+	}
+	if (ccd_szcache + nbytes > ccd_maxcache)
+	    goto done_
+
+	# Cache the image data
+	iferr {
+	    switch (IM_PIXTYPE (im)) {
+	    case TY_SHORT:
+	        CCD_DATA(pcache) = imgs2s (im, 1, nc, 1, nl)
+	    case TY_REAL:
+	        CCD_DATA(pcache) = imgs2r (im, 1, nc, 1, nl)
+	    }
+	    ccd_szcache = ccd_szcache + nbytes
+	    CCD_SZDATA(pcache) = nbytes
+	} then {
+	    call imunmap (im)
+	    im = immap (image, READ_ONLY, 0)
+	    CCD_IM(pcache) = im
+	    CCD_SZDATA(pcache) = 0
+	}
+
+done_
+	CCD_NACCESS(pcache) = CCD_NACCESS(pcache) + 1
+	call sfree (sp)
+	return (im)
+end
+
+
+# CCD_OPEN -- Initialize the CCD image cache.
+
+procedure ccd_open (max_cache)
+
+int	max_cache	# Maximum cache size in bytes
+
+int	max_size, begmem()
+include	"ccdcache.com"
+
+begin
+	ccd_ncache = 0
+	ccd_maxcache = max_cache
+	ccd_szcache = 0
+	call malloc (ccd_pcache, 1, TY_INT)
+
+	# Ask for the maximum physical memory.
+	if (ccd_maxcache > 0) {
+	    ccd_oldsize = begmem (0, ccd_oldsize, max_size)
+	    call fixmem (max_size)
+	}
+end
+
+
+# CCD_UNMAP -- Unmap an image.
+# Don't actually unmap the image since it may be opened again.
+
+procedure ccd_unmap (im)
+
+pointer	im			# IMIO pointer
+
+int	i
+pointer	pcache
+include	"ccdcache.com"
+
+begin
+	for (i=1; i<=ccd_ncache; i=i+1) {
+	    pcache = Memi[ccd_pcache+i-1]
+	    if (CCD_IM(pcache) == im) {
+		CCD_NACCESS(pcache) = CCD_NACCESS(pcache) - 1
+		return
+	    }
+	}
+
+	call imunmap (im)
+end
+
+
+# CCD_FLUSH -- Close image and flush from cache.
+
+procedure ccd_flush (im)
+
+pointer	im			# IMIO pointer
+
+int	i
+pointer	pcache
+include "ccdcache.com"
+
+begin
+	for (i=1; i<=ccd_ncache; i=i+1) {
+	    pcache = Memi[ccd_pcache+i-1]
+	    if (CCD_IM(pcache) == im) {
+		ccd_ncache = ccd_ncache - 1
+	        ccd_szcache = ccd_szcache - CCD_SZDATA(pcache)
+	        call mfree (CCD_BUFR(pcache), TY_REAL)
+	        call mfree (CCD_BUFS(pcache), TY_SHORT)
+		call mfree (pcache, TY_STRUCT)
+		for (; i<=ccd_ncache; i=i+1)
+		    Memi[ccd_pcache+i-1] = Memi[ccd_pcache+i]
+		break
+	    }
+	}
+
+	call imunmap (im)
+end
+
+
+# CCD_CLOSE -- Close the image cache.
+
+procedure ccd_close ()
+
+int	i
+pointer	pcache
+include "ccdcache.com"
+
+begin
+	for (i=1; i<=ccd_ncache; i=i+1) {
+	    pcache = Memi[ccd_pcache+i-1]
+	    call imunmap (CCD_IM(pcache))
+	    call mfree (CCD_BUFR(pcache), TY_REAL)
+	    call mfree (CCD_BUFS(pcache), TY_SHORT)
+	    call mfree (pcache, TY_STRUCT)
+	}
+	call mfree (ccd_pcache, TY_INT)
+
+	# Restore memory.
+	call fixmem (ccd_oldsize)
+end
+
+
+# CCD_GLR -- Get a line of real data from the image.
+# If the image data is cached this is fast (particularly if the datatype
+# matches).  If the image data is not cached then use IMIO.
+
+pointer procedure ccd_glr (im, col1, col2, line)
+
+pointer	im			# IMIO pointer
+int	col1, col2		# Columns
+int	line			# Line
+
+int	i
+pointer	pcache, data, bufr, imgs2r()
+errchk	malloc
+include "ccdcache.com"
+
+begin
+	# Quick test for cached data.
+	if (ccd_maxcache == 0)
+	    return (imgs2r (im, col1, col2, line, line))
+
+	# Return cached data.
+	if (IM_PIXTYPE(im) == TY_REAL) {
+	    for (i=1; i<=ccd_ncache; i=i+1) {
+		pcache = Memi[ccd_pcache+i-1]
+		if (CCD_IM(pcache) == im) {
+		    if (CCD_SZDATA(pcache) > 0)
+		        return (CCD_DATA(pcache)+(line-1)*IM_LEN(im,1)+col1-1)
+		    else
+			break
+		}
+	    }
+	} else {
+	    for (i=1; i<=ccd_ncache; i=i+1) {
+		pcache = Memi[ccd_pcache+i-1]
+		if (CCD_IM(pcache) == im) {
+		    if (CCD_SZDATA(pcache) > 0) {
+		        data = CCD_DATA(pcache)+(line-1)*IM_LEN(im,1)+col1-1
+		        bufr = CCD_BUFR(pcache)
+		        if (bufr == NULL) {
+			    call malloc (bufr, IM_LEN(im,1), TY_REAL)
+			    CCD_BUFR(pcache) = bufr
+			}
+		        call achtsr (Mems[data], Memr[bufr], IM_LEN(im,1))
+		        return (bufr)
+		    } else
+			break
+		}
+	    }
+	}
+
+	# Return uncached data.
+	return (imgs2r (im, col1, col2, line, line))
+end
+
+
+# CCD_GLS -- Get a line of short data from the image.
+# If the image data is cached this is fast (particularly if the datatype
+# matches).  If the image data is not cached then use IMIO.
+
+pointer procedure ccd_gls (im, col1, col2, line)
+
+pointer	im			# IMIO pointer
+int	col1, col2		# Columns
+int	line			# Line
+
+int	i
+pointer	pcache, data, bufs, imgs2s()
+errchk	malloc
+include "ccdcache.com"
+
+begin
+	# Quick test for cached data.
+	if (ccd_maxcache == 0)
+	    return (imgs2s (im, col1, col2, line, line))
+
+	# Return cached data.
+	if (IM_PIXTYPE(im) == TY_SHORT) {
+	    for (i=1; i<=ccd_ncache; i=i+1) {
+		pcache = Memi[ccd_pcache+i-1]
+		if (CCD_IM(pcache) == im) {
+		    if (CCD_SZDATA(pcache) > 0)
+		        return (CCD_DATA(pcache)+(line-1)*IM_LEN(im,1)+col1-1)
+		    else
+			break
+		}
+	    }
+	} else {
+	    for (i=1; i<=ccd_ncache; i=i+1) {
+		pcache = Memi[ccd_pcache+i-1]
+		if (CCD_IM(pcache) == im) {
+		    if (CCD_SZDATA(pcache) > 0) {
+		        data = CCD_DATA(pcache)+(line-1)*IM_LEN(im,1)+col1-1
+		        bufs = CCD_BUFS(pcache)
+		        if (bufs == NULL) {
+			    call malloc (bufs, IM_LEN(im,1), TY_SHORT)
+			    CCD_BUFS(pcache) = bufs
+		        }
+		        call achtrs (Memr[data], Mems[bufs], IM_LEN(im,1))
+		        return (bufs)
+		    } else
+			break
+		}
+	    }
+	}
+
+	# Return uncached data.
+	return (imgs2s (im, col1, col2, line, line))
+end
diff --git a/noao/imred/quadred/src/ccdproc/ccdcheck.x b/noao/imred/quadred/src/ccdproc/ccdcheck.x
new file mode 100644
index 00000000..0dde14f9
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdcheck.x
@@ -0,0 +1,67 @@
+include	<imhdr.h>
+include	"ccdtypes.h"
+
+# CCDCHECK -- Check processing status.
+
+bool procedure ccdcheck (im, ccdtype)
+
+pointer	im			# IMIO pointer
+int	ccdtype			# CCD type
+
+real	ccdmean, hdmgetr()
+bool	clgetb(), ccdflag()
+long	time
+int	hdmgeti()
+
+begin
+	if (clgetb ("trim") && !ccdflag (im, "trim"))
+	    return (true)
+	if (clgetb ("fixpix") && !ccdflag (im, "fixpix"))
+	    return (true)
+	if (clgetb ("overscan") && !ccdflag (im, "overscan"))
+	    return (true)
+
+	switch (ccdtype) {
+	case ZERO:
+	    if (clgetb ("readcor") && !ccdflag (im, "readcor"))
+	        return (true)
+	case DARK:
+	    if (clgetb ("zerocor") && !ccdflag (im, "zerocor"))
+	        return (true)
+	case FLAT:
+	    if (clgetb ("zerocor") && !ccdflag (im, "zerocor"))
+	        return (true)
+	    if (clgetb ("darkcor") && !ccdflag (im, "darkcor"))
+	        return (true)
+	    if (clgetb ("scancor") && !ccdflag (im, "scancor"))
+	        return (true)
+	    iferr (ccdmean = hdmgetr (im, "ccdmean"))
+		    return (true)
+	    iferr (time = hdmgeti (im, "ccdmeant"))
+		time = IM_MTIME(im)
+	    if (time < IM_MTIME(im))
+		return (true)
+	case ILLUM:
+	    if (clgetb ("zerocor") && !ccdflag (im, "zerocor"))
+	        return (true)
+	    if (clgetb ("darkcor") && !ccdflag (im, "darkcor"))
+	        return (true)
+	    if (clgetb ("flatcor") && !ccdflag (im, "flatcor"))
+	        return (true)
+	    iferr (ccdmean = hdmgetr (im, "ccdmean"))
+		return (true)
+	default:
+	    if (clgetb ("zerocor") && !ccdflag (im, "zerocor"))
+	        return (true)
+	    if (clgetb ("darkcor") && !ccdflag (im, "darkcor"))
+	        return (true)
+	    if (clgetb ("flatcor") && !ccdflag (im, "flatcor"))
+	        return (true)
+	    if (clgetb ("illumcor") && !ccdflag (im, "illumcor"))
+	        return (true)
+	    if (clgetb ("fringecor") && !ccdflag (im, "fringcor"))
+	        return (true)
+	}
+
+	return (false)
+end
diff --git a/noao/imred/quadred/src/ccdproc/ccdcmp.x b/noao/imred/quadred/src/ccdproc/ccdcmp.x
new file mode 100644
index 00000000..a2687934
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdcmp.x
@@ -0,0 +1,23 @@
+# CCD_CMP -- Compare two image names with extensions ignored.
+
+bool procedure ccd_cmp (image1, image2)
+
+char	image1[ARB]		# First image
+char	image2[ARB]		# Second image
+
+int	i, j, strmatch(), strlen(), strncmp()
+bool	streq()
+
+begin
+	if (streq (image1, image2))
+	    return (true)
+
+	i = max (strmatch (image1, ".imh"), strmatch (image1, ".hhh"))
+	if (i == 0)
+	    i = strlen (image1)
+	j = max (strmatch (image2, ".imh"), strmatch (image2, ".hhh"))
+	if (j == 0)
+	    j = strlen (image2)
+
+	return (strncmp (image1, image2, max (i, j)) == 0)
+end
diff --git a/noao/imred/quadred/src/ccdproc/ccddelete.x b/noao/imred/quadred/src/ccdproc/ccddelete.x
new file mode 100644
index 00000000..90931135
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccddelete.x
@@ -0,0 +1,55 @@
+# CCDDELETE -- Delete an image by renaming it to a backup image.
+#
+#   1.	Get the backup prefix which may be a path name.
+#   2.  If no prefix is specified then delete the image without a backup.
+#   3.  If there is a prefix then make a backup image name.
+#       Rename the image to the backup image name.
+#
+#   The backup image name is formed by prepending the backup prefix to the
+#   image name.  If a previous backup exist append integers to the backup
+#   prefix until a nonexistant image name is created.
+
+procedure ccddelete (image)
+
+char	image[ARB]		# Image to delete (backup)
+
+int	i, imaccess()
+pointer	sp, prefix, backup
+errchk	imdelete, imrename
+
+begin
+	call smark (sp)
+	call salloc (prefix, SZ_FNAME, TY_CHAR)
+	call salloc (backup, SZ_FNAME, TY_CHAR)
+
+	# Get the backup prefix.
+	call clgstr ("backup", Memc[prefix], SZ_FNAME)
+	call xt_stripwhite (Memc[prefix])
+
+	# If there is no prefix then simply delete the image.
+	if (Memc[prefix] == EOS)
+	    call imdelete (image)
+
+	# Otherwise create a backup image name which does not exist and
+	# rename the image to the backup image.
+
+	else {
+	    i = 0
+	    repeat {
+		if (i == 0) {
+	    	    call sprintf (Memc[backup], SZ_FNAME, "%s%s")
+		        call pargstr (Memc[prefix])
+		        call pargstr (image)
+		} else {
+	            call sprintf (Memc[backup], SZ_FNAME, "%s%d%s")
+			call pargstr (Memc[prefix])
+			call pargi (i)
+			call pargstr (image)
+		}
+	        i = i + 1
+	    } until (imaccess (Memc[backup], READ_ONLY) == NO)
+	    call imrename (image, Memc[backup])
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/ccdflag.x b/noao/imred/quadred/src/ccdproc/ccdflag.x
new file mode 100644
index 00000000..427365d2
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdflag.x
@@ -0,0 +1,27 @@
+# CCDFLAG -- Determine if a CCD processing flag is set.  This is less than
+# obvious because of the need to use the default value to indicate a
+# false flag.
+
+bool procedure ccdflag (im, name)
+
+pointer	im		# IMIO pointer
+char	name[ARB]	# CCD flag name
+
+bool	flag, strne()
+pointer	sp, str1, str2
+
+begin
+	call smark (sp)
+	call salloc (str1, SZ_LINE, TY_CHAR)
+	call salloc (str2, SZ_LINE, TY_CHAR)
+
+	# Get the flag string value and the default value.
+	# The flag is true if the value and the default do not match.
+
+	call hdmgstr (im, name, Memc[str1], SZ_LINE)
+	call hdmgdef (name, Memc[str2], SZ_LINE)
+	flag = strne (Memc[str1], Memc[str2])
+
+	call sfree (sp)
+	return (flag)
+end
diff --git a/noao/imred/quadred/src/ccdproc/ccdlog.x b/noao/imred/quadred/src/ccdproc/ccdlog.x
new file mode 100644
index 00000000..48453704
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdlog.x
@@ -0,0 +1,46 @@
+include	<imhdr.h>
+include	<imset.h>
+
+# CCDLOG -- Log information about the processing with the image name.
+#
+#   1.  If the package "verbose" parameter is set print the string preceded
+#	by the image name.
+#   2.  If the package "logfile" parameter is not null append the string,
+#	preceded by the image name, to the file.
+
+procedure ccdlog (im, str)
+
+pointer	im			# IMIO pointer
+char	str[ARB]		# Log string
+
+int	fd, open()
+bool	clgetb()
+pointer	sp, fname
+errchk	open
+
+begin
+	call smark (sp)
+	call salloc (fname, SZ_FNAME, TY_CHAR)
+
+	# Write to the standard error output if "verbose".
+	if (clgetb ("verbose")) {
+	    call imstats (im, IM_IMAGENAME, Memc[fname], SZ_FNAME)
+	    call eprintf ("%s: %s\n")
+		call pargstr (Memc[fname])
+		call pargstr (str)
+	}
+
+	# Append to the "logfile" if not null.
+	call clgstr ("logfile", Memc[fname], SZ_FNAME)
+	call xt_stripwhite (Memc[fname])
+	if (Memc[fname] != EOS) {
+	    fd = open (Memc[fname], APPEND, TEXT_FILE)
+	    call imstats (im, IM_IMAGENAME, Memc[fname], SZ_FNAME)
+	    call fprintf (fd, "%s: %s\n")
+		call pargstr (Memc[fname])
+		call pargstr (str)
+	    call close (fd)
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/ccdmean.x b/noao/imred/quadred/src/ccdproc/ccdmean.x
new file mode 100644
index 00000000..d38ea97b
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdmean.x
@@ -0,0 +1,50 @@
+include	<imhdr.h>
+
+
+# CCDMEAN -- Compute mean and add to header if needed.
+
+procedure ccdmean (input)
+
+char	input[ARB]		# Input image
+
+int	i, nc, nl, hdmgeti()
+long	time, clktime()
+bool	clgetb()
+real	mean, hdmgetr(), asumr()
+pointer	in, immap(), imgl2r()
+errchk	immap
+
+begin
+	# Check if this operation has been done.
+
+	in = immap (input, READ_WRITE, 0)
+	ifnoerr (mean = hdmgetr (in, "ccdmean")) {
+	    iferr (time = hdmgeti (in, "ccdmeant"))
+		time = IM_MTIME(in)
+	    if (time >= IM_MTIME(in)) {
+		call imunmap (in)
+		return
+	    }
+	}
+
+	if (clgetb ("noproc")) {
+	    call eprintf (
+		"  [TO BE DONE] Compute mean of image\n")
+		call pargstr (input)
+	    call imunmap (in)
+	    return
+	}
+
+	# Compute and record the mean.
+	nc = IM_LEN(in,1)
+	nl = IM_LEN(in,2)
+	mean = 0.
+	do i = 1, nl
+	    mean = mean + asumr (Memr[imgl2r(in,i)], nc)
+	mean = mean / (nc * nl)
+	time = clktime (long(0))
+	call hdmputr (in, "ccdmean", mean)
+	call hdmputi (in, "ccdmeant", int (time))
+
+	call imunmap (in)
+end
diff --git a/noao/imred/quadred/src/ccdproc/ccdnscan.x b/noao/imred/quadred/src/ccdproc/ccdnscan.x
new file mode 100644
index 00000000..3a9fbeba
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdnscan.x
@@ -0,0 +1,38 @@
+include	"ccdtypes.h"
+
+
+# CCDNSCAN -- Return the number CCD scan rows.
+#
+# If not found in the header return the "nscan" parameter for objects and
+# 1 for calibration images.
+
+int procedure ccdnscan (im, ccdtype)
+
+pointer	im			#I Image
+int	ccdtype			#I CCD type
+int	nscan			#O Number of scan lines
+
+bool	clgetb()
+char	type, clgetc()
+int	hdmgeti(), clgeti()
+
+begin
+	iferr (nscan = hdmgeti (im, "nscanrow")) {
+	    switch (ccdtype) {
+	    case ZERO, DARK, FLAT, ILLUM, FRINGE:
+		nscan = 1
+	    default:
+		type = clgetc ("scantype")
+		if (type == 's')
+		    nscan = clgeti ("nscan")
+		else {
+		    if (clgetb ("scancor"))
+			nscan = INDEFI
+		    else
+			nscan = 1
+		}
+	    }
+	}
+
+	return (nscan)
+end
diff --git a/noao/imred/quadred/src/ccdproc/ccdproc.par b/noao/imred/quadred/src/ccdproc/ccdproc.par
new file mode 100644
index 00000000..f20207a7
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdproc.par
@@ -0,0 +1,43 @@
+images,s,a,"",,,List of CCD images to correct
+ccdtype,s,h,"",,,CCD image type to correct
+max_cache,i,h,0,0,,Maximum image caching memory (in Mbytes)
+noproc,b,h,no,,,"List processing steps only?
+"
+fixpix,b,h,yes,,,Fix bad CCD lines and columns?
+overscan,b,h,yes,,,Apply overscan strip correction?
+trim,b,h,yes,,,Trim the image?
+zerocor,b,h,yes,,,Apply zero level correction?
+darkcor,b,h,no,,,Apply dark count correction?
+flatcor,b,h,yes,,,Apply flat field correction?
+illumcor,b,h,no,,,Apply illumination correction?
+fringecor,b,h,no,,,Apply fringe correction?
+readcor,b,h,no,,,Convert zero level image to readout correction?
+scancor,b,h,no,,,"Convert flat field image to scan correction?
+"
+readaxis,s,h,"line","column|line",, Read out axis (column|line)
+fixfile,s,h,"",,,File describing the bad lines and columns
+biassec,s,h,"",,,Overscan strip image section
+trimsec,s,h,"",,,Trim data section
+zero,s,h,"",,,Zero level calibration image
+dark,s,h,"",,,Dark count calibration image
+flat,s,h,"",,,Flat field images
+illum,s,h,"",,,Illumination correction images
+fringe,s,h,"",,,Fringe correction images
+minreplace,r,h,1.,,,Minimum flat field value
+scantype,s,h,"shortscan","shortscan|longscan",,Scan type (shortscan|longscan)
+nscan,i,h,1,1,,"Number of short scan lines
+"
+interactive,b,h,no,,,Fit overscan interactively?
+function,s,h,"legendre",,,Fitting function
+order,i,h,1,1,,Number of polynomial terms or spline pieces
+sample,s,h,"*",,,Sample points to fit
+naverage,i,h,1,,,Number of sample points to combine
+niterate,i,h,1,0,,Number of rejection iterations
+low_reject,r,h,3.,0.,,Low sigma rejection factor
+high_reject,r,h,3.,0.,,High sigma rejection factor
+grow,r,h,0.,0.,,"Rejection growing radius
+"
+verbose,b,h,)_.verbose,,,Print log information to the standard output?
+logfile,f,h,)_.logfile,,,Text log file
+backup,s,h,)_.backup,,,Backup directory or prefix
+output,s,h,"",,,Not used
diff --git a/noao/imred/quadred/src/ccdproc/ccdproc.x b/noao/imred/quadred/src/ccdproc/ccdproc.x
new file mode 100644
index 00000000..1b2a133c
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdproc.x
@@ -0,0 +1,106 @@
+include	<error.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+# CCDPROC -- Process a CCD image of a specified CCD image type.
+#
+# The input image is corrected for bad pixels, overscan levels, zero
+# levels, dark counts, flat field, illumination, and fringing.  It may also
+# be trimmed.  The checking of whether to apply each correction, getting the
+# required parameters, and logging the operations is left to separate
+# procedures, one for each correction.  The actual processing is done by
+# a specialized procedure designed to be very efficient.  These
+# procedures may also process calibration images if necessary.
+# The specified image type overrides the image type in the image header.
+# There are two data type paths; one for short data types and one for
+# all other data types (usually real).
+
+procedure ccdproc (input, ccdtype)
+
+char	input[ARB]		# CCD image to process
+int	ccdtype			# CCD type of image (independent of header).
+
+pointer	sp, output, str, in, out, ccd, immap()
+errchk	immap, set_output, ccddelete
+errchk	set_fixpix, set_zero, set_dark, set_flat, set_illum, set_fringe
+
+begin
+	call smark (sp)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Map the image, make a working output image and set the processing
+	# parameters.
+
+	in = immap (input, READ_ONLY, 0)
+	call mktemp ("tmp", Memc[output], SZ_FNAME)
+	call set_output (in, out, Memc[output])
+	call set_proc (in, out, ccd)
+	call set_sections (ccd)
+	call set_trim (ccd)
+	call set_fixpix (ccd)
+	call set_overscan (ccd)
+
+	# Set processing appropriate for the various image types.
+	switch (ccdtype) {
+	case ZERO:
+	case DARK:
+	    call set_zero (ccd)
+	case FLAT:
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+	    CORS(ccd, FINDMEAN) = YES
+	    CORS(ccd, MINREP) = YES
+	case ILLUM:
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+	    call set_flat (ccd)
+	case OBJECT, COMP:
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+	    call set_flat (ccd)
+	    call set_illum (ccd)
+	    call set_fringe (ccd)
+	default:
+	    call set_zero (ccd)
+	    call set_dark (ccd)
+	    call set_flat (ccd)
+	    call set_illum (ccd)
+	    call set_fringe (ccd)
+	    CORS(ccd, FINDMEAN) = YES
+	}
+
+	# Do the processing if the COR flag is set.
+	if (COR(ccd) == YES) {
+	    call doproc (ccd)
+	    call set_header (ccd)
+
+	    # Replace the input by the output image.
+	    call imunmap (in)
+	    call imunmap (out)
+	    iferr (call ccddelete (input)) {
+		call imdelete (Memc[output])
+		call error (1,
+		    "Can't delete or make backup of original image")
+	    }
+	    call imrename (Memc[output], input)
+	} else {
+	    # Delete the temporary output image leaving the input unchanged.
+	    call imunmap (in)
+	    iferr (call imunmap (out))
+		;
+	    iferr (call imdelete (Memc[output]))
+		;
+	}
+	call free_proc (ccd)
+
+	# Do special processing for calibration images.
+	switch (ccdtype) {
+	case ZERO:
+	    call readcor (input)
+	case FLAT:
+	    call ccdmean (input)
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/ccdred.h b/noao/imred/quadred/src/ccdproc/ccdred.h
new file mode 100644
index 00000000..ef41f592
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdred.h
@@ -0,0 +1,155 @@
+# CCDRED Data Structures and Definitions
+
+# The CCD structure:  This structure is used to communicate processing
+# parameters between the package procedures.  It contains pointers to
+# data, calibration image IMIO pointers, scaling parameters, and the
+# correction flags.  The corrections flags indicate which processing
+# operations are to be performed.  The subsection parameters do not
+# include a step size.  A step size is assumed.  If arbitrary subsampling
+# is desired this would be the next generalization.
+
+define	LEN_CCD		75		# Length of CCD structure
+
+# CCD data coordinates
+define	CCD_C1		Memi[$1]	# CCD starting column
+define	CCD_C2		Memi[$1+1]	# CCD ending column
+define	CCD_L1		Memi[$1+2]	# CCD starting line
+define	CCD_L2		Memi[$1+3]	# CCD ending line
+
+# Input data
+define	IN_IM		Memi[$1+4]	# Input image pointer
+define	IN_C1		Memi[$1+5]	# Input data starting column
+define	IN_C2		Memi[$1+6]	# Input data ending column
+define	IN_L1		Memi[$1+7]	# Input data starting line
+define	IN_L2		Memi[$1+8]	# Input data ending line
+define	IN_NSEC		Memi[$1+71]	# Number of input pieces
+define	IN_SEC		Memi[$1+72]	# Pointer to sections (c1,c2,l1,l2)xn
+
+# Output data
+define	OUT_IM		Memi[$1+9]	# Output image pointer
+define	OUT_C1		Memi[$1+10]	# Output data starting column
+define	OUT_C2		Memi[$1+11]	# Output data ending column
+define	OUT_L1		Memi[$1+12]	# Output data starting line
+define	OUT_L2		Memi[$1+13]	# Output data ending line
+define	OUT_SEC		Memi[$1+73]	# Pointer to sections (c1,c2,l1,l2)xn
+
+# Zero level data
+define	ZERO_IM		Memi[$1+14]	# Zero level image pointer
+define	ZERO_C1		Memi[$1+15]	# Zero level data starting column
+define	ZERO_C2		Memi[$1+16]	# Zero level data ending column
+define	ZERO_L1		Memi[$1+17]	# Zero level data starting line
+define	ZERO_L2		Memi[$1+18]	# Zero level data ending line
+
+# Dark count data
+define	DARK_IM		Memi[$1+19]	# Dark count image pointer
+define	DARK_C1		Memi[$1+20]	# Dark count data starting column
+define	DARK_C2		Memi[$1+21]	# Dark count data ending column
+define	DARK_L1		Memi[$1+22]	# Dark count data starting line
+define	DARK_L2		Memi[$1+23]	# Dark count data ending line
+
+# Flat field data
+define	FLAT_IM		Memi[$1+24]	# Flat field image pointer
+define	FLAT_C1		Memi[$1+25]	# Flat field data starting column
+define	FLAT_C2		Memi[$1+26]	# Flat field data ending column
+define	FLAT_L1		Memi[$1+27]	# Flat field data starting line
+define	FLAT_L2		Memi[$1+28]	# Flat field data ending line
+
+# Illumination data
+define	ILLUM_IM	Memi[$1+29]	# Illumination image pointer
+define	ILLUM_C1	Memi[$1+30]	# Illumination data starting column
+define	ILLUM_C2	Memi[$1+31]	# Illumination data ending column
+define	ILLUM_L1	Memi[$1+32]	# Illumination data starting line
+define	ILLUM_L2	Memi[$1+33]	# Illumination data ending line
+
+# Fringe data
+define	FRINGE_IM	Memi[$1+34]	# Fringe image pointer
+define	FRINGE_C1	Memi[$1+35]	# Fringe data starting column
+define	FRINGE_C2	Memi[$1+36]	# Fringe data ending column
+define	FRINGE_L1	Memi[$1+37]	# Fringe data starting line
+define	FRINGE_L2	Memi[$1+38]	# Fringe data ending line
+
+# Trim section
+define	TRIM_C1		Memi[$1+39]	# Trim starting column
+define	TRIM_C2		Memi[$1+40]	# Trim ending column
+define	TRIM_L1		Memi[$1+41]	# Trim starting line
+define	TRIM_L2		Memi[$1+42]	# Trim ending line
+
+# Bias section
+define	BIAS_C1		Memi[$1+43]	# Bias starting column
+define	BIAS_C2		Memi[$1+44]	# Bias ending column
+define	BIAS_L1		Memi[$1+45]	# Bias starting line
+define	BIAS_L2		Memi[$1+46]	# Bias ending line
+define	BIAS_SEC	Memi[$1+74]	# Multiple bias sections
+
+define	READAXIS	Memi[$1+47]	# Read out axis (1=cols, 2=lines)
+define	CALCTYPE	Memi[$1+48]	# Calculation data type
+define	NBADCOLS	Memi[$1+49]	# Number of column interpolation regions
+define	BADCOLS		Memi[$1+50]	# Pointer to col interpolation regions
+define	NBADLINES	Memi[$1+51]	# Number of line interpolation regions
+define	BADLINES	Memi[$1+52]	# Pointer to line interpolation regions
+define	OVERSCAN_VEC	Memi[$1+53]	# Pointer to overscan vector
+define	DARKSCALE	Memr[P2R($1+54)]	# Dark count scale factor
+define	FRINGESCALE	Memr[P2R($1+55)]	# Fringe scale factor
+define	FLATSCALE	Memr[P2R($1+56)]	# Flat field scale factor
+define	ILLUMSCALE	Memr[P2R($1+57)]	# Illumination scale factor
+define	MINREPLACE	Memr[P2R($1+58)]	# Minimum replacement value
+define	MEAN		Memr[P2R($1+59)]	# Mean of output image
+define	COR		Memi[$1+60]	# Overall correction flag
+define	CORS		Memi[$1+61+($2-1)]  # Individual correction flags
+
+# Individual components of input, output, and bias section pieces.
+define	IN_SC1		Memi[IN_SEC($1)+4*$2-4]
+define	IN_SC2		Memi[IN_SEC($1)+4*$2-3]
+define	IN_SL1		Memi[IN_SEC($1)+4*$2-2]
+define	IN_SL2		Memi[IN_SEC($1)+4*$2-1]
+define	OUT_SC1		Memi[OUT_SEC($1)+4*$2-4]
+define	OUT_SC2		Memi[OUT_SEC($1)+4*$2-3]
+define	OUT_SL1		Memi[OUT_SEC($1)+4*$2-2]
+define	OUT_SL2		Memi[OUT_SEC($1)+4*$2-1]
+define	BIAS_SC1	Memi[BIAS_SEC($1)+4*$2-4]
+define	BIAS_SC2	Memi[BIAS_SEC($1)+4*$2-3]
+define	BIAS_SL1	Memi[BIAS_SEC($1)+4*$2-2]
+define	BIAS_SL2	Memi[BIAS_SEC($1)+4*$2-1]
+
+# The correction array contains the following elements with array indices
+# given by the macro definitions.
+
+define	NCORS		10		# Number of corrections
+
+define	FIXPIX		1		# Fix bad pixels
+define	TRIM		2		# Trim image
+define	OVERSCAN	3		# Apply overscan correction
+define	ZEROCOR		4		# Apply zero level correction
+define	DARKCOR		5		# Apply dark count correction
+define	FLATCOR		6		# Apply flat field correction
+define	ILLUMCOR	7		# Apply illumination correction
+define	FRINGECOR	8		# Apply fringe correction
+define	FINDMEAN	9		# Find the mean of the output image
+define	MINREP		10		# Check and replace minimum value
+
+# The following definitions identify the correction values in the correction
+# array.  They are defined in terms of bit fields so that it is possible to
+# add corrections to form unique combination corrections.  Some of
+# these combinations are implemented as compound operations for efficiency.
+
+define	O	001B	# overscan
+define	Z	002B	# zero level
+define	D	004B	# dark count
+define	F	010B	# flat field
+define	I	020B	# Illumination
+define	Q	040B	# Fringe
+
+# The following correction combinations are recognized.
+
+define	ZO	003B	# zero level + overscan
+define	DO	005B	# dark count + overscan
+define	DZ	006B	# dark count + zero level
+define	DZO	007B	# dark count + zero level + overscan
+define	FO	011B	# flat field + overscan
+define	FZ	012B	# flat field + zero level
+define	FZO	013B	# flat field + zero level + overscan
+define	FD	014B	# flat field + dark count
+define	FDO	015B	# flat field + dark count + overscan
+define	FDZ	016B	# flat field + dark count + zero level
+define	FDZO	017B	# flat field + dark count + zero level + overscan
+define	QI	060B	# fringe + illumination
diff --git a/noao/imred/quadred/src/ccdproc/ccdsection.x b/noao/imred/quadred/src/ccdproc/ccdsection.x
new file mode 100644
index 00000000..aced216a
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdsection.x
@@ -0,0 +1,100 @@
+include	<ctype.h>
+
+# CCD_SECTION -- Parse a 2D image section into its elements.
+# 1. The default values must be set by the caller.
+# 2. A null image section is OK.
+# 3. The first nonwhitespace character must be '['.
+# 4. The last interpreted character must be ']'.
+#
+# This procedure should be replaced with an IMIO procedure at some
+# point.
+
+procedure ccd_section (section, x1, x2, xstep, y1, y2, ystep)
+
+char	section[ARB]		# Image section
+int	x1, x2, xstep		# X image section parameters
+int	y1, y2, ystep		# X image section parameters
+
+int	i, ip, a, b, c, temp, ctoi()
+define	error_	99
+
+begin
+	# Decode the section string.
+	ip = 1
+	while (IS_WHITE(section[ip]))
+	    ip = ip + 1
+	if (section[ip] == '[')
+	    ip = ip + 1
+	else if (section[ip] == EOS)
+	    return
+	else
+	    goto error_
+
+	do i = 1, 2 {
+	    while (IS_WHITE(section[ip]))
+	        ip = ip + 1
+
+	    # Default values
+	    if (i == 1) {
+	        a = x1
+	        b = x2
+	        c = xstep
+	    } else {
+	        a = y1
+	        b = y2
+	        c = ystep
+	    }
+
+	    # Get a:b:c.  Allow notation such as "-*:c"
+	    # (or even "-:c") where the step is obviously negative.
+
+	    if (ctoi (section, ip, temp) > 0) {			# a
+		a = temp
+	        if (section[ip] == ':') {	
+		    ip = ip + 1
+		    if (ctoi (section, ip, b) == 0)		# a:b
+		        goto error_
+	        } else
+		    b = a
+	    } else if (section[ip] == '-') {			# -*
+		temp = a
+		a = b
+		b = temp
+	        ip = ip + 1
+	        if (section[ip] == '*')
+		    ip = ip + 1
+	    } else if (section[ip] == '*')			# *
+	        ip = ip + 1
+	    if (section[ip] == ':') {				# ..:step
+	        ip = ip + 1
+	        if (ctoi (section, ip, c) == 0)
+		    goto error_
+	        else if (c == 0)
+		    goto error_
+	    }
+	    if (a > b && c > 0)
+	        c = -c
+
+	    if (i == 1) {
+		x1 = a
+		x2 = b
+		xstep = c
+	    } else {
+		y1 = a
+		y2 = b
+		ystep = c
+	    }
+
+	    while (IS_WHITE(section[ip]))
+	        ip = ip + 1
+	    if (section[ip] == ',')
+		ip = ip + 1
+	}
+
+	if (section[ip] != ']')
+	    goto error_
+
+	return
+error_
+	call error (0, "Error in image section specification")
+end
diff --git a/noao/imred/quadred/src/ccdproc/ccdsubsets.x b/noao/imred/quadred/src/ccdproc/ccdsubsets.x
new file mode 100644
index 00000000..6152897f
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdsubsets.x
@@ -0,0 +1,92 @@
+# CCDSUBSET -- Return the CCD subset identifier.
+#
+# 1. Get the subset string and search the subset record file for the ID string.
+# 2. If the subset string is not in the record file define a default ID string
+#    based on the first word of the subset string.  If the first word is not
+#    unique append a integer to the first word until it is unique.
+# 3. Add the new subset string and identifier to the record file.
+# 4. Since the ID string is used to generate image names replace all
+#    nonimage name characters with '_'.
+#
+# It is an error if the record file cannot be created or written when needed.
+
+procedure ccdsubset (im, subset, sz_name)
+
+pointer	im			# Image
+char	subset[sz_name]		# CCD subset identifier
+int	sz_name			# Size of subset string
+
+bool	streq()
+int	i, fd, ctowrd(), open(), fscan()
+pointer	sp, fname, str1, str2, subset1, subset2, subset3
+errchk	open
+
+begin
+	call smark (sp)
+	call salloc (fname, SZ_FNAME, TY_CHAR)
+	call salloc (str1, SZ_LINE, TY_CHAR)
+	call salloc (str2, SZ_LINE, TY_CHAR)
+	call salloc (subset1, SZ_LINE, TY_CHAR)
+	call salloc (subset2, SZ_LINE, TY_CHAR)
+	call salloc (subset3, SZ_LINE, TY_CHAR)
+
+	# Get the subset record file and the subset string.
+	call clgstr ("ssfile", Memc[fname], SZ_LINE)
+	call hdmgstr (im, "subset", Memc[str1], SZ_LINE)
+
+	# The default subset identifier is the first word of the subset string.
+	i = 1
+	i = ctowrd (Memc[str1], i, Memc[subset1], SZ_LINE)
+
+	# A null subset string is ok.  If not null check for conflict
+	# with previous subset IDs.
+	if (Memc[str1] != EOS) {
+	    call strcpy (Memc[subset1], Memc[subset3], SZ_LINE)
+
+	    # Search the subset record file for the same subset string.
+	    # If found use the ID string.  If the subset ID has been
+	    # used for another subset string then increment an integer
+	    # suffix to the default ID and check the list again.
+
+	    i = 1
+	    ifnoerr (fd = open (Memc[fname], READ_ONLY, TEXT_FILE)) {
+		while (fscan (fd) != EOF) {
+		    call gargwrd (Memc[str2], SZ_LINE)
+		    call gargwrd (Memc[subset2], SZ_LINE)
+		    if (streq (Memc[str1], Memc[str2])) {
+			i = 0
+			call strcpy (Memc[subset2], Memc[subset1], SZ_LINE)
+			break
+		    } if (streq (Memc[subset1], Memc[subset2])) {
+			call sprintf (Memc[subset1], SZ_LINE, "%s%d")
+			    call pargstr (Memc[subset3])
+			    call pargi (i)
+			i = i + 1
+			call seek (fd, BOF)
+		    }
+		}
+		call close (fd)
+	    }
+
+	    # If the subset is not in the record file add it.
+	    if (i > 0) {
+		fd = open (Memc[fname], APPEND, TEXT_FILE)
+		call fprintf (fd, "'%s'\t%s\n")
+		    call pargstr (Memc[str1])
+		    call pargstr (Memc[subset1])
+		call close (fd)
+	    }
+	}
+
+	# Set the subset ID string and replace magic characters by '_'
+	# since the subset ID is used in forming image names.
+
+	call strcpy (Memc[subset1], subset, sz_name)
+	for (i=1; subset[i]!=EOS; i=i+1)
+	    switch (subset[i]) {
+	    case '-','+','?','*','[',']',' ','\t':
+		subset[i] = '_'
+	    }
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/ccdtypes.h b/noao/imred/quadred/src/ccdproc/ccdtypes.h
new file mode 100644
index 00000000..0d5d4caf
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdtypes.h
@@ -0,0 +1,14 @@
+# Standard CCD image types.
+
+define	CCDTYPES "|object|zero|dark|flat|illum|fringe|other|comp|"
+
+define	NONE		-1
+define	UNKNOWN		0
+define	OBJECT		1
+define	ZERO		2
+define	DARK		3
+define	FLAT		4
+define	ILLUM		5
+define	FRINGE		6
+define	OTHER		7
+define	COMP		8
diff --git a/noao/imred/quadred/src/ccdproc/ccdtypes.x b/noao/imred/quadred/src/ccdproc/ccdtypes.x
new file mode 100644
index 00000000..bf6d29e2
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/ccdtypes.x
@@ -0,0 +1,72 @@
+include	"ccdtypes.h"
+
+# CCDTYPES -- Return the CCD type name string.
+# CCDTYPEI -- Return the CCD type code.
+
+
+# CCDTYPES -- Return the CCD type name string.
+
+procedure ccdtypes (im, name, sz_name)
+
+pointer	im			# Image
+char	name[sz_name]		# CCD type name
+int	sz_name			# Size of name string
+
+int	strdic()
+pointer	sp, str
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the image type string.  If none then return "none".
+	# Otherwise get the corresponding package image type string.
+	# If the image type is unknown return "unknown" otherwise return
+	# the package name.
+
+	call hdmgstr (im, "imagetyp", Memc[str], SZ_LINE)
+	if (Memc[str] == EOS) {
+	    call strcpy ("none", name, sz_name)
+	} else {
+	    call hdmname (Memc[str], name, sz_name)
+	    if (name[1] == EOS)
+		call strcpy (Memc[str], name, sz_name)
+	    if (strdic (name, name, sz_name, CCDTYPES) == UNKNOWN)
+	    	call strcpy ("unknown", name, sz_name)
+	}
+
+	call sfree (sp)
+end
+
+
+# CCDTYPEI -- Return the CCD type code.
+
+int procedure ccdtypei (im)
+
+pointer	im			# Image
+int	ccdtype			# CCD type (returned)
+
+pointer	sp, str1, str2
+int	strdic()
+
+begin
+	call smark (sp)
+	call salloc (str1, SZ_LINE, TY_CHAR)
+	call salloc (str2, SZ_LINE, TY_CHAR)
+
+	# Get the image type and if there is none then return the NONE code.
+	call hdmgstr (im, "imagetyp", Memc[str1], SZ_LINE)
+	if (Memc[str1] == EOS) {
+	    ccdtype = NONE
+
+	# Otherwise get the package type and convert to an image type code.
+	} else {
+	    call hdmname (Memc[str1], Memc[str2], SZ_LINE)
+	    if (Memc[str2] == EOS)
+		call strcpy (Memc[str1], Memc[str2], SZ_LINE)
+	    ccdtype = strdic (Memc[str2], Memc[str2], SZ_LINE, CCDTYPES)
+	}
+
+	call sfree (sp)
+	return (ccdtype)
+end
diff --git a/noao/imred/quadred/src/ccdproc/cor.gx b/noao/imred/quadred/src/ccdproc/cor.gx
new file mode 100644
index 00000000..189f9437
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/cor.gx
@@ -0,0 +1,362 @@
+include	"ccdred.h"
+
+
+.help cor Feb87 noao.imred.ccdred
+.nf ----------------------------------------------------------------------------
+cor -- Process CCD image lines
+
+These procedures are the heart of the CCD processing.  They do the desired
+set of processing operations on the image line data as efficiently as
+possible.  They are called by the PROC procedures.  There are four procedures
+one for each readout axis and one for short and real image data.
+Some sets of operations are coded as single compound operations for efficiency.
+To keep the number of combinations managable only the most common
+combinations are coded as compound operations.  The combinations
+consist of any set of line overscan, column overscan, zero level, dark
+count, and flat field and any set of illumination and fringe
+correction.  The corrections are applied in place to the output vector.
+
+The column readout procedure is more complicated in order to handle
+zero level and flat field corrections specified as one dimensional
+readout corrections instead of two dimensional calibration images.
+Column readout format is probably extremely rare and the 1D readout
+corrections are used only for special types of data.
+.ih
+SEE ALSO
+proc, ccdred.h
+.endhelp -----------------------------------------------------------------------
+
+$for (sr)
+# COR1 -- Correct image lines with readout axis 1 (lines).
+
+procedure cor1$t (cors, out, overscan, zero, dark, flat, illum,
+	fringe, n, darkscale, flatscale, illumscale, frgscale)
+
+int	cors[ARB]	# Correction flags
+PIXEL	out[n]		# Output data
+real	overscan	# Overscan value
+PIXEL	zero[n]		# Zero level correction
+PIXEL	dark[n]		# Dark count correction
+PIXEL	flat[n]		# Flat field correction
+PIXEL	illum[n]	# Illumination correction
+PIXEL	fringe[n]	# Fringe correction
+int	n		# Number of pixels
+real	darkscale	# Dark count scale factor
+real	flatscale	# Flat field scale factor
+real	illumscale	# Illumination scale factor
+real	frgscale	# Fringe scale factor
+
+int	i, op
+
+begin
+	op = cors[OVERSCAN] + cors[ZEROCOR] + cors[DARKCOR] + cors[FLATCOR]
+	switch (op) {
+	case O: # overscan
+	    do i = 1, n
+	        out[i] = out[i] - overscan
+	case Z: # zero level
+	    do i = 1, n
+		out[i] = out[i] - zero[i]
+
+	case ZO: # zero level + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - zero[i]
+
+	case D: # dark count
+	    do i = 1, n
+		out[i] = out[i] - darkscale * dark[i]
+	case DO: # dark count + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - darkscale * dark[i]
+	case DZ: # dark count + zero level
+	    do i = 1, n
+		out[i] = out[i] - zero[i] - darkscale * dark[i]
+	case DZO: # dark count + zero level + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - zero[i] - darkscale * dark[i]
+
+	case F: # flat field
+	    do i = 1, n
+		out[i] = out[i] * flatscale / flat[i]
+	case FO: # flat field + overscan
+	    do i = 1, n
+	        out[i] = (out[i] - overscan) * flatscale / flat[i]
+	case FZ: # flat field + zero level
+	    do i = 1, n
+		out[i] = (out[i] - zero[i]) * flatscale / flat[i]
+	case FZO: # flat field + zero level + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - zero[i]) * flatscale /
+		    flat[i]
+	case FD: # flat field + dark count
+	    do i = 1, n
+		out[i] = (out[i] - darkscale * dark[i]) * flatscale / flat[i]
+	case FDO: # flat field + dark count + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - darkscale * dark[i]) *
+		    flatscale / flat[i]
+	case FDZ: # flat field + dark count + zero level
+	    do i = 1, n
+		out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+		    flatscale / flat[i]
+	case FDZO: # flat field + dark count + zero level + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - zero[i] -
+		    darkscale * dark[i]) * flatscale / flat[i]
+	}
+
+	# Often these operations will not be performed so test for no
+	# correction rather than go through the switch.
+
+	op = cors[ILLUMCOR] + cors[FRINGECOR]
+	if (op != 0) {
+	    switch (op) {
+	    case I: # illumination
+	        do i = 1, n
+		    out[i] = out[i] * illumscale / illum[i]
+	    case Q: # fringe
+	        do i = 1, n
+		    out[i] = out[i] - frgscale * fringe[i]
+	    case QI: # fringe + illumination
+	        do i = 1, n
+		    out[i] = out[i]*illumscale/illum[i] - frgscale*fringe[i]
+	    }
+	}
+end
+
+
+# COR2 -- Correct lines for readout axis 2 (columns).  This procedure is
+# more complex than when the readout is along the image lines because the
+# zero level and/or flat field corrections may be single readout column
+# vectors.
+
+procedure cor2$t (line, cors, out, overscan, zero, dark, flat, illum,
+	fringe, n, zeroim, flatim, darkscale, flatscale, illumscale, frgscale)
+
+int	line		# Line to be corrected
+int	cors[ARB]	# Correction flags
+PIXEL	out[n]		# Output data
+real	overscan[n]	# Overscan value
+PIXEL	zero[n]		# Zero level correction
+PIXEL	dark[n]		# Dark count correction
+PIXEL	flat[n]		# Flat field correction
+PIXEL	illum[n]	# Illumination correction
+PIXEL	fringe[n]	# Fringe correction
+int	n		# Number of pixels
+pointer	zeroim		# Zero level IMIO pointer (NULL if 1D vector)
+pointer	flatim		# Flat field IMIO pointer (NULL if 1D vector)
+real	darkscale	# Dark count scale factor
+real	flatscale	# Flat field scale factor
+real	illumscale	# Illumination scale factor
+real	frgscale	# Fringe scale factor
+
+PIXEL	zeroval
+real	flatval
+int	i, op
+
+begin
+	op = cors[OVERSCAN] + cors[ZEROCOR] + cors[DARKCOR] + cors[FLATCOR]
+	switch (op) {
+	case O: # overscan
+	    do i = 1, n
+	        out[i] = out[i] - overscan[i]
+	case Z: # zero level
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - zero[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - zeroval
+	    }
+
+	case ZO: # zero level + overscan
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zero[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zeroval
+	    }
+
+	case D: # dark count
+	    do i = 1, n
+		out[i] = out[i] - darkscale * dark[i]
+	case DO: # dark count + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan[i] - darkscale * dark[i]
+	case DZ: # dark count + zero level
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - zero[i] - darkscale * dark[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - zeroval - darkscale * dark[i]
+	    }
+	case DZO: # dark count + zero level + overscan
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zero[i] -
+			darkscale * dark[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zeroval -
+			darkscale * dark[i]
+	    }
+
+	case F: # flat field
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = out[i] * flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = out[i] * flatval
+	    }
+	case FO: # flat field + overscan
+	    if (flatim != NULL) {
+	        do i = 1, n
+	            out[i] = (out[i] - overscan[i]) * flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+	            out[i] = (out[i] - overscan[i]) * flatval
+	    }
+	case FZ: # flat field + zero level
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i]) * flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval) * flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval) * flatval
+		}
+	    }
+	case FZO: # flat field + zero level + overscan
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i]) *
+			    flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval) *
+			    flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval) * flatval
+		}
+	    }
+	case FD: # flat field + dark count
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = (out[i] - darkscale * dark[i]) * flatscale/flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = (out[i] - darkscale * dark[i]) * flatval
+	    }
+	case FDO: # flat field + dark count + overscan
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = (out[i] - overscan[i] - darkscale * dark[i]) *
+		        flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = (out[i] - overscan[i] - darkscale * dark[i]) *
+		        flatval
+	    }
+	case FDZ: # flat field + dark count + zero level
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+			    flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval - darkscale * dark[i]) *
+			    flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+			    flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval - darkscale * dark[i]) *
+			    flatval
+		}
+	    }
+	case FDZO: # flat field + dark count + zero level + overscan
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i] -
+			    darkscale * dark[i]) * flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval -
+			    darkscale * dark[i]) * flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i] -
+			    darkscale * dark[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval -
+			    darkscale * dark[i]) * flatval
+		}
+	    }
+	}
+
+	# Often these operations will not be performed so test for no
+	# correction rather than go through the switch.
+
+	op = cors[ILLUMCOR] + cors[FRINGECOR]
+	if (op != 0) {
+	    switch (op) {
+	    case I: # illumination
+	        do i = 1, n
+		    out[i] = out[i] * illumscale / illum[i]
+	    case Q: # fringe
+	        do i = 1, n
+		    out[i] = out[i] - frgscale * fringe[i]
+	    case QI: # fringe + illumination
+	        do i = 1, n
+		    out[i] = out[i]*illumscale/illum[i] - frgscale*fringe[i]
+	    }
+	}
+end
+$endfor
diff --git a/noao/imred/quadred/src/ccdproc/corinput.gx b/noao/imred/quadred/src/ccdproc/corinput.gx
new file mode 100644
index 00000000..241cc34d
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/corinput.gx
@@ -0,0 +1,220 @@
+include	<imhdr.h>
+include	"ccdred.h"
+
+$for (sr)
+# CORINPUT -- Get an input image line, fix the bad pixels, and trim.
+# Return the corrected input line in the output array.
+
+procedure corinput$t (in, line, ccd, output, ncols)
+
+pointer	in		# Input IMIO pointer
+int	line		# Corrected output line
+pointer	ccd		# CCD pointer
+PIXEL	output[ncols]	# Output data (returned)
+int	ncols		# Number of output columns
+
+int	i, inline
+pointer	inbuf, imgl2$t()
+
+begin
+	# Determine the input line in terms of the trimmed output line.
+	if (IN_SEC(ccd) == NULL)
+	    inline = IN_L1(ccd) + line - 1
+	else {
+	    do i = 1, IN_NSEC(ccd) {
+		if (line < OUT_SL1(ccd,i) || line > OUT_SL2(ccd,i))
+		    next
+		inline = IN_SL1(ccd,i) + line - OUT_SL1(ccd,i)
+		break
+	    }
+	}
+
+	# If there are bad lines call a procedure to fix them.  Otherwise
+	# read the image line directly.
+
+	if (NBADLINES(ccd) != 0)
+	    call lfix$t (in, inline, Mems[BADLINES(ccd)], IM_LEN(in,1),
+		IM_LEN(in,2), NBADLINES(ccd), inbuf)
+	else
+	    inbuf = imgl2$t (in, inline)
+
+	# IF there are bad columns call a procedure to fix them.
+	if (NBADCOLS(ccd) != 0)
+	    call cfix$t (inline, Mems[BADCOLS(ccd)], IM_LEN(in,1),
+		IM_LEN(in,2), NBADCOLS(ccd), Mem$t[inbuf])
+
+	# Move the pixels to the output line.
+	if (IN_SEC(ccd) == NULL)
+	    call amov$t (Mem$t[inbuf+IN_C1(ccd)-OUT_C1(ccd)], output, ncols)
+	else {
+	    do i = 1, IN_NSEC(ccd) {
+		if (inline < IN_SL1(ccd,i) || inline > IN_SL2(ccd,i))
+		    next
+		call amov$t (Mem$t[inbuf+IN_SC1(ccd,i)-OUT_C1(ccd)],
+		    output[OUT_SC1(ccd,i)], OUT_SC2(ccd,i)-OUT_SC1(ccd,i)+1)
+	    }
+	}
+end
+
+
+# CFIX -- Interpolate across bad columns defined in the bad column array.
+
+procedure cfix$t (line, badcols, ncols, nlines, nbadcols, data)
+
+int	line				# Line to be fixed
+short	badcols[2, nlines, nbadcols]	# Bad column array
+int	ncols				# Number of columns
+int	nlines				# Number of lines
+int	nbadcols			# Number of bad column regions
+PIXEL	data[ncols]			# Data to be fixed
+
+PIXEL	val
+real	del
+int	i, j, col1, col2
+
+begin
+	do i = 1, nbadcols {
+	    col1 = badcols[1, line, i]
+	    if (col1 == 0)			# No bad columns
+		return
+	    col2 = badcols[2, line, i]
+	    if (col1 == 1) {			# Bad first column
+		val = data[col2+1]
+		do j = col1, col2
+		    data[j] = val
+	    } else if (col2 == ncols) {		# Bad last column
+		val = data[col1-1]
+		do j = col1, col2
+		    data[j] = val
+	    } else {				# Interpolate
+		del = (data[col2+1] - data[col1-1]) / (col2 - col1 + 2)
+		val = data[col1-1] + del
+		do j = col1, col2
+		    data[j] = val + (j - col1) * del
+	    }
+	}
+end
+
+
+# LFIX -- Get image line and replace bad pixels by interpolation from
+# neighboring lines.  Internal buffers are used to keep the last fixed
+# line and the next good line.  They are allocated with LFIXINIT and
+# freed with LFIXFREE.
+
+procedure lfix$t (im, line, badlines, ncols, nlines, nbadlines, data)
+
+pointer	im				# IMIO pointer
+int	line				# Line to be obtained and fixed
+short	badlines[2,nlines,nbadlines]	# Bad line region array
+int	ncols				# Number of columns in image
+int	nlines				# Number of lines in images
+int	nbadlines			# Number of bad line regions
+pointer	data				# Data line pointer (returned)
+
+real	wt1, wt2
+int	i, nextgood, lastgood, col1, col2
+pointer	imgl2$t()
+
+pointer	lastbuf, nextbuf
+common	/lfixcom/ lastbuf, nextbuf, lastgood
+
+begin
+	# If this line has bad pixels replace them.  Otherwise just
+	# read the line.
+
+	if (badlines[1, line, 1] != 0) {
+	    # Save the last line which has already been fixed.
+	    if (line != 1)
+		call amov$t (Mem$t[data], Mem$t[lastbuf], ncols)
+
+	    # Determine the next line with no bad line pixels.  Note that
+	    # this requirement is overly strict since the bad columns
+	    # may not be the same in neighboring lines.
+
+	    nextgood = 0
+	    do i = line+1, nlines {
+		if (badlines[1, i, 1] == 0) {
+		    nextgood = i
+		    break
+		}
+	    }
+
+	    # If the next good line is not the same as previously
+	    # read the data line and store it in a buffer.
+
+	    if ((nextgood != lastgood) && (nextgood != 0)) {
+		data = imgl2$t (im, nextgood)
+		call amov$t (Mem$t[data], Mem$t[nextbuf], ncols)
+		lastgood = nextgood
+	    }
+
+	    # Get the data line.
+	    data = imgl2$t (im, line)
+
+	    # Interpolate the bad columns.  At the ends of the image use
+	    # extension otherwise use linear interpolation.
+
+	    if (line == 1) {				# First line is bad
+		do i = 1, nbadlines {
+		    col1 = badlines[1,line,i] - 1
+		    if (col1 == -1)
+			break
+		    col2 = badlines[2,line,i]
+		    call amov$t (Mem$t[nextbuf+col1], Mem$t[data+col1],
+			col2-col1)
+		}
+	    } else if (nextgood == 0) {			# Last line is bad
+		do i = 1, nbadlines {
+		    col1 = badlines[1,line,i] - 1
+		    if (col1 == -1)
+			break
+		    col2 = badlines[2,line,i]
+		    call amov$t (Mem$t[lastbuf+col1], Mem$t[data+col1],
+			col2-col1)
+		}
+	    } else {					# Interpolate
+		wt1 = 1. / (nextgood - line + 1)
+		wt2 = 1. - wt1
+		do i = 1, nbadlines {
+		    col1 = badlines[1,line,i] - 1
+		    if (col1 == -1)
+			break
+		    col2 = badlines[2,line,i] - 1
+		    call awsu$t (Mem$t[nextbuf+col1], Mem$t[lastbuf+col1],
+			Mem$t[data+col1], col2-col1+1, wt1, wt2)
+		}
+	    }
+	} else
+	    data = imgl2$t (im, line)
+end
+
+
+# LFIXINIT -- Allocate internal buffers.
+
+procedure lfixinit$t (im)
+
+pointer	im		# IMIO pointer
+
+int	lastgood
+pointer	lastbuf, nextbuf
+common	/lfixcom/ lastbuf, nextbuf, lastgood
+
+begin
+	call malloc (lastbuf, IM_LEN(im,1), TY_PIXEL)
+	call malloc (nextbuf, IM_LEN(im,1), TY_PIXEL)
+	lastgood=0
+end
+
+# LFIXFREE -- Free memory when the last line has been obtained.
+
+procedure lfixfree$t ()
+
+int	lastgood
+pointer	lastbuf, nextbuf
+common	/lfixcom/ lastbuf, nextbuf, lastgood
+
+begin
+	call mfree (lastbuf, TY_PIXEL)
+	call mfree (nextbuf, TY_PIXEL)
+end
+$endfor
diff --git a/noao/imred/quadred/src/ccdproc/doc/ccdproc.hlp b/noao/imred/quadred/src/ccdproc/doc/ccdproc.hlp
new file mode 100644
index 00000000..e942a299
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/doc/ccdproc.hlp
@@ -0,0 +1,778 @@
+.help ccdproc Aug01 noao.imred.quadred
+.ih
+NAME
+ccdproc -- Process CCD images
+.ih
+SYNOPSIS
+This is the main processing task for CCD data in single image or
+\fBquadformat\fR image formats.
+.ih
+USAGE	
+ccdproc images
+.ih
+PARAMETERS
+.ls images
+List of input CCD images to process.  The list may include processed
+images and calibration images.
+.le
+.ls output = ""
+List of output images.  If no list is given then the processing will replace
+the input images with the processed images.  If a list is given it must
+match the input image list.  \fINote that any dependent calibration images
+still be processed in-place with optional backup.\fR
+.le
+.ls ccdtype = ""
+CCD image type to select from the input image list.  If no type is given
+then all input images will be selected.  The recognized types are described
+in \fBccdtypes\fR.
+.le
+.ls max_cache = 0
+Maximum image caching memory (in Mbytes).  If there is sufficient memory
+the calibration images, such as zero level, dark count, and flat fields,
+will be cached in memory when processing many input images.  This
+reduces the disk I/O and makes the task run a little faster.  If the
+value is zero image caching is not used.
+.le
+.ls noproc = no
+List processing steps only?
+.le
+
+.ce
+PROCESSING SWITCHES
+.ls fixpix = yes
+Fix bad CCD lines and columns by linear interpolation from neighboring
+lines and columns?  If yes then a bad pixel mask, image, or file must be
+specified.
+.le
+.ls overscan = yes
+Apply overscan or prescan bias correction?  If yes then the overscan
+image section and the readout axis must be specified.
+.le
+.ls trim = yes
+Trim the image of the overscan region and bad edge lines and columns?
+If yes then the trim section must be specified.
+.le
+.ls zerocor = yes
+Apply zero level correction?  If yes a zero level image must be specified.
+.le
+.ls darkcor = yes
+Apply dark count correction?  If yes a dark count image must be specified.
+.le
+.ls flatcor = yes
+Apply flat field correction?  If yes flat field images must be specified.
+.le
+.ls illumcor = no
+Apply iillumination correction?  If yes iillumination images must be specified.
+.le
+.ls fringecor = no
+Apply fringe correction?  If yes fringe images must be specified.
+.le
+.ls readcor = no
+Convert zero level images to readout correction images?  If yes then
+zero level images are averaged across the readout axis to form one
+dimensional zero level readout correction images.
+.le
+.ls scancor = no
+Convert zero level, dark count and flat field images to scan mode flat
+field images?  If yes then the form of scan mode correction is specified by
+the parameter \fIscantype\fR.
+.le
+
+.ce
+PROCESSING PARAMETERS
+.ls readaxis = "line"
+Read out axis specified as "line" or "column".
+.le
+.ls fixfile
+Bad pixel mask, image, or file.  If "image" is specified then the name is
+specified in the image header or instrument translation file.  If "BPM" is
+specified then the standard BPM image header keyword defines a bad pixel
+mask.  A bad pixel mask is a compact format (".pl" extension) with zero
+values indicating good pixels and non-zero values indicating bad pixels.  A
+bad pixel image is a regular image in which zero values are good pixels and
+non-zero values are bad pixels.  A bad pixel file specifies bad pixels or
+rectangular bad pixel regions as described later.  The direction of
+interpolation is determined by the mask value with a value of two
+interpolating across columns, a value of three interpolating across lines,
+and any other non-zero value interpolating along the narrowest dimension.
+.le
+.ls biassec
+Overscan bias strip image section.  If "image" is specified then the overscan
+bias section is specified in the image header or instrument translation file.
+Only the part of the bias section along the readout axis is used.  The
+length of the bias region fit is defined by the trim section.  If one
+wants to limit the region of the overscan used in the fit to be less
+than that of the trim section then the sample region parameter,
+\fIsample\fR, should be used.  It is an error if no section or the
+whole image is specified.
+.le
+.ls trimsec
+Image section for trimming.  If "image" is specified then the trim image
+section is specified in the image header or instrument translation file.
+However, for \fIquadformat\fR data this parameter is not used and the trim
+sections are assumed to be in the image header.
+.le
+.ls zero = ""
+Zero level calibration image.  The zero level image may be one or two
+dimensional.  The CCD image type and subset are not checked for these
+images and they take precedence over any zero level calibration images
+given in the input list.
+.le
+.ls dark = ""
+Dark count calibration image.  The CCD image type and subset are not checked
+for these images and they take precedence over any dark count calibration
+images given in the input list.
+.le
+.ls flat = ""
+Flat field calibration images.  The flat field images may be one or
+two dimensional.  The CCD image type is not checked for these
+images and they take precedence over any flat field calibration images given
+in the input list.  The flat field image with the same subset as the
+input image being processed is selected.
+.le
+.ls illum = ""
+Iillumination correction images.  The CCD image type is not checked for these
+images and they take precedence over any iillumination correction images given
+in the input list.  The iillumination image with the same subset as the
+input image being processed is selected.
+.le
+.ls fringe = ""
+Fringe correction images.  The CCD image type is not checked for these
+images and they take precedence over any fringe correction images given
+in the input list.  The fringe image with the same subset as the
+input image being processed is selected.
+.le
+.ls minreplace = 1.
+When processing flat fields, pixel values below this value (after
+all other processing such as overscan, zero, and dark corrections) are
+replaced by this value.  This allows flat fields processed by \fBccdproc\fR
+to be certain to avoid divide by zero problems when applied to object
+images.
+.le
+.ls scantype = "shortscan"
+Type of scan format used in creating the CCD images.  The modes are:
+.ls "shortscan"
+The CCD is scanned over a number of lines and then read out as a regular
+two dimensional image.  In this mode unscanned zero level, dark count and
+flat fields are numerically scanned to form scanned flat fields comparable
+to the observations.
+.le
+.ls "longscan"
+In this mode the CCD is clocked and read out continuously to form a long
+strip.  Flat fields are averaged across the readout axis to
+form a one dimensional flat field readout correction image.  This assumes
+that all recorded image lines are clocked over the entire active area of the
+CCD.
+.le
+.le
+.ls nscan
+Number of object scan readout lines used in short scan mode.  This parameter
+is used when the scan type is "shortscan" and the number of scan lines
+cannot be determined from the object image header (using the keyword
+nscanrows or it's translation).
+.le
+
+
+.ce
+OVERSCAN FITTING PARAMETERS
+
+There are two types of overscan (or prescan) determinations.  One determines
+a independent overscan value for each line  and is only available for a
+\fIreadaxis\fR of 1.  The other averages the overscan along the readout
+direction to make an overscan vector, fits a smoothing function to the vector,
+and then evaluate and then evaluates the smooth function at each readout
+line or column.  The line-by-line determination only uses the
+\fIfunction\fR parameter and the smoothing determinations uses all
+the following parameters.
+
+.ls function = "legendre"
+Line-by-line determination of the overscan is specified by:
+
+.nf
+         mean - the mean of the biassec columns at each line
+       median - the median of the biassec columns at each line
+       minmax - the mean at each line with the min and max excluded
+.fi
+
+The smoothed overscan vector may be fit by one of the functions:
+
+.nf
+     legendre - legendre polynomial
+    chebyshev - chebyshev polynomial
+      spline1 - linear spline
+      spline3 - cubic spline
+.fi
+.le
+.ls order = 1
+Number of polynomial terms or spline pieces in the overscan fit.
+.le
+.ls sample = "*"
+Sample points to use in the overscan fit.  The string "*" specified all
+points otherwise an \fBicfit\fR range string is used.
+.le
+.ls naverage = 1
+Number of points to average or median to form fitting points.  Positive
+numbers specify averages and negative numbers specify medians.
+.le
+.ls niterate = 1
+Number of rejection iterations to remove deviant points from the overscan fit.
+If 0 then no points are rejected.
+.le
+.ls low_reject = 3., high_reject = 3.
+Low and high sigma rejection factors for rejecting deviant points from the
+overscan fit.
+.le
+.ls grow = 0.
+One dimensional growing radius for rejection of neighbors to deviant points.
+.le
+.ls interactive = no
+Fit the overscan vector interactively?  If yes and the overscan function type
+is one of the \fBicfit\fR types then the average overscan vector is fit
+interactively using the \fBicfit\fR package.  If no then the fitting parameters
+given below are used.
+.le
+
+The parameters \fIverbose\fR, \fIlogfile\fR, and \fIbackup\fR default to
+the package parameters but may be specified to override the package
+values.  This is used by the \fBquadproc\fR script task.  These parameters
+are described in the help topic "quadred.package".
+.ih
+DESCRIPTION
+\fBCcdproc\fR processes CCD images to correct and calibrate for
+detector defects, readout bias, zero level bias, dark counts,
+response, iillumination, and fringing.  It also trims unwanted
+lines and columns and changes the pixel datatype.  It is efficient
+and easy to use; all one has to do is set the parameters and then
+begin processing the images.  The task takes care of most of the
+record keeping and automatically does the prerequisite processing
+of calibration images.  Beneath this simplicity there is much that
+is going on.  In this section a simple description of the usage is
+given.  The following sections present more detailed discussions
+on the different operations performed and the order and logic
+of the processing steps.  For a user's guide to the \fBccdred\fR
+package see \fBguide\fR.  Much of the ease of use derives from using
+information in the image header.  If this information is missing
+see section 13.
+
+One begins by setting the task parameters.  There are many parameters
+but they may be easily reviewed and modified using the task \fBeparam\fR.
+The input CCD images to be processed are given as an image list.
+Previously processed images are ignored and calibration images are
+recognized, provided the CCD image types are in the image header (see
+\fBinstruments\fR and \fBccdtypes\fR).  Therefore it is permissible to
+use simple image templates such as "*.imh".  The \fIccdtype\fR parameter
+may be used to select only certain types of CCD images to process
+(see \fBccdtypes\fR).
+
+The processing operations are selected by boolean (yes/no) parameters.
+Because calibration images are recognized and processed appropriately,
+the processing operations for object images should be set.
+Any combination of operations may be specified and the operations are
+performed simultaneously.  While it is possible to do operations in
+separate steps this is much less efficient.  Two of the operation
+parameters apply only to zero level and flat field images.  These
+are used for certain types of CCDs and modes of operation.
+
+The processing steps selected have related parameters which must be
+set.  These are things like image sections defining the overscan and
+trim regions and calibration images.  There are a number of parameters
+used for fitting the overscan or prescan bias section.  These are
+parameters used by the standard IRAF curve fitting package \fBicfit\fR.
+The parameters are described in more detail in the following sections.
+
+In addition to the task parameters there are package parameters
+which affect \fBccdproc\fR.  These include the instrument and subset
+files, the text and plot log files, the output pixel datatype,
+the amount of memory available for calibration image caching,
+the verbose parameter for logging to the terminal, and the backup
+prefix.  These are described in \fBccdred\fR.
+
+Calibration images are specified by task parameters and/or in the
+input image list.  If more than one calibration image is specified
+then the first one encountered is used and a warning is issued for the
+extra images.  Calibration images specified by
+task parameters take precedence over calibration images in the input list.
+These images also need not have a CCD image type parameter since the task
+parameter identifies the type of calibration image.  This method is
+best if there is only one calibration image for all images
+to be processed.  This is almost always true for zero level and dark
+count images.  If no calibration image is specified by task parameter
+then calibration images in the input image list are identified and
+used.  This requires that the images have CCD image types recognized
+by the package.  This method is useful if one may simply say "*.imh"
+as the image list to process all images or if the images are broken
+up into groups, in "@" files for example, each with their own calibration
+frames.
+
+When an input image is processed the task first determines the processing
+parameters and calibration images.  If a requested operation has been
+done it is skipped and if all requested operations have been completed then
+no processing takes place.  When it determines that a calibration image
+is required it checks for the image from the task parameter and then
+for a calibration image of the proper type in the input list.
+
+Having
+selected a calibration image it checks if it has been processed by
+looking for the image header flag CCDPROC.  If it is not present then
+the calibration image is processed.  When any image has been processed
+the CCDPROC flag is added.  For images processed directly by \fBccdproc\fR
+the individual processing flags are checked even if the CCDPROC flag is
+present.  However, the automatic processing of the calibration images is
+only done if the CCDPROC flag is absent!  This is to make the task more
+efficient by not having to check every flag for every calibration image
+for every input image.  Thus, if additional processing
+steps are added after images have been partially reduced then input images
+will be processed for the new steps but calibration images will not be
+processed automatically.
+
+After the calibration images have been identified, and processed if
+necessary, the images may be cached in memory.  This is done when there
+are more than two input images (it is actually less efficient to
+cache the calibration images for one or two input images) and the parameter
+\fImax_cache\fR is greater than zero.  When caching, as many calibration
+images as allowed by the specified memory are read into memory and
+kept there for all the input images.  Cached images are, therefore,
+only read once from disk which reduces the amount of disk I/O.  This
+makes a modest decrease in the execution time.  It is not dramatic
+because the actual processing is fairly CPU intensive.
+
+Once the processing parameters and calibration images have been determined
+the input image is processed for all the desired operations in one step;
+i.e. there are no intermediate results or images.  This makes the task
+efficient.  If a matching list of output images is given then the processed
+image is written to the specified output image name.  If no output image
+list is given then the corrected image is output as a temporary image until
+the entire image has been processed.  When the image has been completely
+processed then the original image is deleted (or renamed using the
+specified backup prefix) and the corrected image replaces the original
+image.  Using a temporary image protects the data in the event of an abort
+or computer failure.  Keeping the original image name eliminates much of
+the record keeping and the need to generate new image names.
+.sh
+1. Fixpix
+Regions of bad lines and columns may be replaced by linear
+interpolation from neighboring lines and columns when the parameter
+\fIfixpix\fR is set.  This algorithm is the same as used in the
+task \fBfixpix\fR.  The bad pixels may be specified by a pixel mask,
+an image, or a text file.  For the mask or image, values of zero indicate
+good pixels and other values indicate bad pixels to be replaced.
+
+The text file consists of lines with four fields, the starting and
+ending columns and the starting and ending lines.  Any number of
+regions may be specified.  Comment lines beginning with the character
+'#' may be included.  The description applies directly to the input
+image (before trimming) so different files are needed for previously
+trimmed or subsection readouts.  The data in this file is internally
+turned into the same description as a bad pixel mask with values of
+two for regions which are narrower or equal across the columns and
+a value of three for regions narrower across lines.
+
+The direction of interpolation is determined from the values in the
+mask, image, or the converted text file.  A value of two interpolates
+across columns, a value of three interpolates across lines, and any
+other value interpolates across the narrowest dimension of bad pixels
+and using column interpolation if the two dimensions are equal.
+
+The bad pixel description may be specified explicitly with the parameter
+\fIfixfile\fR or indirectly if the parameter has the value "image".  In the
+latter case the instrument file must contain the name of the file.
+.sh
+2. Overscan
+If an overscan or prescan correction is specified (\fIoverscan\fR
+parameter) then the image section (\fIbiassec\fR parameter) defines
+the overscan region.
+
+There are two types of overscan (or prescan) determinations.  One determines
+a independent overscan value for each line  and is only available for a
+\fIreadaxis\fR of 1.  The other averages the overscan along the readout
+direction to make an overscan vector, fits a smoothing function to the vector,
+and then evaluate and then evaluates the smooth function at each readout
+line or column.
+
+The line-by-line determination provides an mean, median, or
+mean with the minimum and maximum values excluded.  The median
+is lowest value of the middle two when the number of overscan columns
+is even rather than the mean.
+
+The smoothed overscan vector determination uses the \fBicfit\fR options
+including interactive fitting.  The fitting function is generally either a
+constant (polynomial of 1 term) or a high order function which fits the
+large scale shape of the overscan vector.  Bad pixel rejection is also
+available to eliminate cosmic ray events.  The function fitting may be done
+interactively using the standard \fBicfit\fR iteractive graphical curve
+fitting tool.  Regardless of whether the fit is done interactively, the
+overscan vector and the fit may be recorded for later review in a metacode
+plot file named by the parameter \fIccdred.plotfile\fR.  The mean value of
+the bias function is also recorded in the image header and log file.
+.sh
+3. Trim
+When the parameter \fItrim\fR is set the input image will be trimmed to
+the image section given by the parameter \fItrimsec\fR.  This trim
+should, of course, be the same as that used for the calibration images.
+.sh
+4. Zerocor
+After the readout bias is subtracted, as defined by the overscan or prescan
+region, there may still be a zero level bias.  This level may be two
+dimensional or one dimensional (the same for every readout line).  A
+zero level calibration is obtained by taking zero length exposures;
+generally many are taken and combined.  To apply this zero
+level calibration the parameter \fIzerocor\fR is set.  In addition if
+the zero level bias is only readout dependent then the parameter \fIreadcor\fR
+is set to reduce two dimensional zero level images to one dimensional
+images.  The zero level images may be specified by the parameter \fIzero\fR
+or given in the input image list (provided the CCD image type is defined).
+
+When the zero level image is needed to correct an input image it is checked
+to see if it has been processed and, if not, it is processed automatically.
+Processing of zero level images consists of bad pixel replacement,
+overscan correction, trimming, and averaging to one dimension if the
+readout correction is specified.
+.sh
+5. Darkcor
+Dark counts are subtracted by scaling a dark count calibration image to
+the same exposure time as the input image and subtracting.  The
+exposure time used is the dark time which may be different than the
+actual integration or exposure time.  A dark count calibration image is
+obtained by taking a very long exposure with the shutter closed; i.e.
+an exposure with no light reaching the detector.  The dark count
+correction is selected with the parameter \fIdarkcor\fR and the dark
+count calibration image is specified either with the parameter
+\fIdark\fR or as one of the input images.  The dark count image is
+automatically processed as needed.  Processing of dark count images
+consists of bad pixel replacement, overscan and zero level correction,
+and trimming.
+.sh
+6. Flatcor
+The relative detector pixel response is calibrated by dividing by a
+scaled flat field calibration image.  A flat field image is obtained by
+exposure to a spatially uniform source of light such as an lamp or
+twilight sky.  Flat field images may be corrected for the spectral
+signature in spectroscopic images (see \fBresponse\fR and
+\fBapnormalize\fR), or for iillumination effects (see \fBmkillumflat\fR
+or \fBmkskyflat\fR).  For more on flat fields and iillumination corrections
+see \fBflatfields\fR.  The flat field response is dependent on the
+wavelength of light so if different filters or spectroscopic wavelength
+coverage are used a flat field calibration for each one is required.
+The different flat fields are  automatically selected by a subset
+parameter (see \fBsubsets\fR).
+
+Flat field calibration is selected with the parameter \fBflatcor\fR
+and the flat field images are specified with the parameter \fBflat\fR
+or as part of the input image list.  The appropriate subset is automatically
+selected for each input image processed.  The flat field image is
+automatically processed as needed.  Processing consists of bad pixel
+replacement, overscan subtraction, zero level subtraction, dark count
+subtraction, and trimming.  Also if a scan mode is used and the
+parameter \fIscancor\fR is specified then a scan mode correction is
+applied (see below).  The processing also computes the mean of the
+flat field image which is used later to scale the flat field before
+division into the input image.  For scan mode flat fields the ramp
+part is included in computing the mean which will affect the level
+of images processed with this flat field.  Note that there is no check for
+division by zero in the interest of efficiency.  If division by zero
+does occur a fatal error will occur.  The flat field can be fixed by
+replacing small values using a task such as \fBimreplace\fR or
+during processing using the \fIminreplace\fR parameter.  Note that the
+\fIminreplace\fR parameter only applies to flat fields processed by
+\fBccdproc\fR.
+.sh
+7. Illumcor
+CCD images processed through the flat field calibration may not be
+completely flat (in the absence of objects).  In particular, a blank
+sky image may still show gradients.  This residual nonflatness is called
+the iillumination pattern.  It may be introduced even if the detector is
+uniformly illuminated by the sky because the flat field lamp
+iillumination may be nonuniform.  The iillumination pattern is found from a
+blank sky, or even object image, by heavily smoothing and rejecting
+objects using sigma clipping.  The iillumination calibration image is
+divided into the data being processed to remove the iillumination
+pattern.  The iillumination pattern is a function of the subset so there
+must be an iillumination correction image for each subset to be
+processed.  The tasks \fBmkillumcor\fR and \fBmkskycor\fR are used to
+create the iillumination correction images.  For more on iillumination
+corrections see \fBflatfields\fR.
+
+An alternative to treating the iillumination correction as a separate
+operation is to combine the flat field and iillumination correction
+into a corrected flat field image before processing the object
+images.  This will save some processing time but does require creating
+the flat field first rather than correcting the images at the same
+time or later.  There are two methods, removing the large scale
+shape of the flat field and combining a blank sky image iillumination
+with the flat field.  These methods are discussed further in the
+tasks which create them; \fBmkillumcor\fR and \fBmkskycor\fR.
+.sh
+8. Fringecor
+There may be a fringe pattern in the images due to the night sky lines.
+To remove this fringe pattern a blank sky image is heavily smoothed
+to produce an iillumination image which is then subtracted from the
+original sky image.  The residual fringe pattern is scaled to the
+exposure time of the image to be fringe corrected and then subtracted.
+Because the intensity of the night sky lines varies with time an
+additional scaling factor may be given in the image header.
+The fringe pattern is a function of the subset so there must be
+a fringe correction image for each subset to be processed.
+The task \fBmkfringecor\fR is used to create the fringe correction images.
+.sh
+9. Readcor
+If a zero level correction is desired (\fIzerocor\fR parameter)
+and the parameter \fIreadcor\fR is yes then a single zero level
+correction vector is applied to each readout line or column.  Use of a
+readout correction rather than a two dimensional zero level image
+depends on the nature of the detector or if the CCD is operated in
+longscan mode (see below).  The readout correction is specified by a
+one dimensional image (\fIzero\fR parameter) and the readout axis
+(\fIreadaxis\fR parameter).  If the zero level image is two dimensional
+then it is automatically processed to a one dimensional image by
+averaging across the readout axis.  Note that this modifies the zero
+level calibration image.
+.sh
+10. Scancor
+CCD detectors may be operated in several modes in astronomical
+applications.  The most common is as a direct imager where each pixel
+integrates one point in the sky or spectrum.  However, the design of most CCD's
+allows the sky to be scanned across the CCD while shifting the
+accumulating signal at the same rate.  \fBCcdproc\fR provides for two
+scanning modes called "shortscan" and "longscan".  The type of scan
+mode is set with the parameter \fIscanmode\fR.
+
+In "shortscan" mode the detector is scanned over a specified number of
+lines (not necessarily at sideral rates).  The lines that scroll off the
+detector during the integration are thrown away.  At the end of the
+integration the detector is read out in the same way as an unscanned
+observation.  The advantage of this mode is that the small scale, zero
+level, dark count and flat field responses are averaged in one dimension
+over the number of lines scanned.  A zero level, dark count or flat field may be
+observed in the same way in which case there is no difference in the
+processing from unscanned imaging and the parameter \fIscancor\fR may be
+no.  If it is yes, though, checking is done to insure that the calibration
+image used has the same number of scan lines as the object being
+processed.  However, one obtains an increase in the statistical accuracy of
+if they are not scanned during the observation but
+digitally scanned during the processing.  In shortscan mode with
+\fIscancor\fR set to yes, zero level, dark count and flat field images are
+digitally scanned, if needed, by the same number of scan lines as the
+object.  The number of scan lines is determined from the object image
+header using the keyword nscanrow (or it's translation).  If not found the
+object is assumed to have been scanned with the value given by the
+\fInscan\fR parameter.  Zero, dark and flat calibration images are assumed
+to be unscanned if the header keyword is not found.
+
+If a scanned zero level, dark count or flat field image is not found
+matching the object then one may be created from the unscanned calibration
+image.  The image will have the root name of the unscanned image with an
+extension of the number of scan rows; i.e. Flat1.32 is created from Flat1
+with a digital scanning of 32 lines.
+
+In "longscan" mode the detector is continuously read out to produce an
+arbitrarily long strip.  Provided data which has not passed over the entire
+detector is thrown away, the zero level, dark count, and flat field
+corrections will be one dimensional.  If \fIscancor\fR is specified and the
+scan mode is "longscan" then a one dimensional zero level, dark count, and
+flat field correction will be applied.
+.sh
+11. Processing Steps
+The following describes the steps taken by the task.  This detailed
+outline provides the most detailed specification of the task.
+
+.ls 5 (1)
+An image to be processed is first checked that it is of the specified
+CCD image type.  If it is not the desired type then go on to the next image.
+.le
+.ls (2)
+A temporary output image is created of the specified pixel data type
+(\fBccdred.pixeltype\fR).  The header parameters are copied from the
+input image.
+.le
+.ls (3)
+If trimming is specified and the image has not been trimmed previously,
+the trim section is determined.
+.le
+.ls (4)
+If bad pixel replacement is specified and this has not been done
+previously, the bad pixel file is determined either from the task
+parameter or the instrument translation file.  The bad pixel regions
+are read.  If the image has been trimmed previously and the bad pixel
+file contains the word "untrimmed" then the bad pixel coordinates are
+translated to those of the trimmed image.
+.le
+.ls (5)
+If an overscan correction is specified and this correction has not been
+applied, the overscan section is averaged along the readout axis.  If
+trimming is to be done the overscan section is trimmed to the same
+limits.  A function is fit either interactively or noninteractively to
+the overscan vector.  The function is used to produce the overscan
+vector to be subtracted from the image.  This is done in real
+arithmetic.
+.le
+.ls (6)
+If the image is a zero level image go to processing step 12.
+If a zero level correction is desired and this correction has not been
+performed, find the zero level calibration image.  If the zero level
+calibration image has not been processed it is processed at this point.
+This is done by going to processing step 1 for this image.  After the
+calibration image has been processed, processing of the input image
+continues from this point.
+The processed calibration image may be
+cached in memory if it has not been previously and if there is enough memory.
+.le
+.ls (7)
+If the image is a dark count image go to processing step 12.
+If a dark count correction is desired and this correction has not been
+performed, find the dark count calibration image.  If the dark count
+calibration image has not been processed it is processed at this point.
+This is done by going to processing step 1 for this image.  After the
+calibration image has been processed, processing of the input image
+continues from this point.  The ratio of the input image dark time
+to the dark count image dark time is determined to be multiplied with
+each pixel of the dark count image before subtracting from the input
+image.
+The processed calibration image may be
+cached in memory if it has not been previously and if there is enough memory.
+.le
+.ls (8)
+If the image is a flat field image go to processing step 12.  If a flat
+field correction is desired and this correction has not been performed,
+find the flat field calibration image of the appropriate subset.  If
+the flat field calibration image has not been processed it is processed
+at this point.  This is done by going to processing step 1 for this
+image.  After the calibration image has been processed, processing of
+the input image continues from this point.  The mean of the image
+is determined from the image header to be used for scaling.  If no
+mean is found then a unit scaling is used.
+The processed calibration image may be
+cached in memory if it has not been previously and if there is enough memory.
+.le
+.ls (9)
+If the image is an iillumination image go to processing step 12.  If an
+iillumination correction is desired and this correction has not been performed,
+find the iillumination calibration image of the appropriate subset.
+The iillumination image must have the "mkillum" processing flag or the
+\fBccdproc\fR will abort with an error.  The mean of the image
+is determined from the image header to be used for scaling.  If no
+mean is found then a unit scaling is used.  The processed calibration
+image may be
+cached in memory if it has not been previously and there is enough memory.
+.le
+.ls (10)
+If the image is a fringe image go to processing step 12.  If a fringe
+correction is desired and this correction has not been performed,
+find the fringe calibration image of the appropriate subset.
+The iillumination image must have the "mkfringe" processing flag or the
+\fBccdproc\fR will abort with an error.  The ratio of the input
+image exposure time to the fringe image exposure time is determined.
+If there is a fringe scaling in the image header then this factor
+is multiplied by the exposure time ratio.  This factor is used
+for scaling.  The processed calibration image may be
+cached in memory if it has not been previously and there is enough memory.
+.le
+.ls (11)
+If there are no processing operations flagged, delete the temporary output
+image, which has been opened but not used, and go to 14.
+.le
+.ls (12)
+The input image is processed line by line with trimmed lines ignored.
+A line of the input image is read.  Bad pixel replacement and trimming
+is applied to the image.  Image lines from the calibration images
+are read from disk or the image cache.  If the calibration is one
+dimensional (such as a readout zero
+level correction or a longscan flat field correction) then the image
+vector is read only once.  Note that IRAF image I/O is buffered for
+efficiency and accessing a line at a time does not mean that image
+lines are read from disk a line at a time.  Given the input line, the
+calibration images, the overscan vector, and the various scale factors
+a special data path for each combination of corrections is used to
+perform all the processing in the most efficient manner.  If the
+image is a flat field any pixels less than the \fIminreplace\fR
+parameter are replaced by that minimum value.  Also a mean is
+computed for the flat field and stored as the CCDMEAN keyword and
+the time, in a internal format, when this value was calculated is stored
+in the CCDMEANT keyword.  The time is checked against the image modify
+time to determine if the value is valid or needs to be recomputed.
+.le
+.ls (13)
+The input image is deleted or renamed to a backup image.  The temporary
+output image is renamed to the input image name.
+.le
+.ls (14)
+If the image is a zero level image and the readout correction is specified
+then it is averaged to a one dimensional readout correction.
+.le
+.ls (15)
+If the image is a zero level, dark count, or flat field image and the scan
+mode correction is specified then the correction is applied.  For shortscan
+mode a modified two dimensional image is produced while for longscan mode a
+one dimensional average image is produced.
+.le
+.ls (16)
+The processing is completed and either the next input image is processed
+beginning at step 1 or, if it is a calibration image which is being
+processed for an input image, control returns to the step which initiated
+the calibration image processing.
+.le
+.sh
+12. Processing Arithmetic
+The \fBccdproc\fR task has two data paths, one for real image pixel datatypes
+and one for short integer pixel datatype.  In addition internal arithmetic
+is based on the rules of FORTRAN.  For efficiency there is
+no checking for division by zero in the flat field calibration.
+The following rules describe the processing arithmetic and data paths.
+
+.ls (1)
+If the input, output, or any calibration image is of type real the
+real data path is used.  This means all image data is converted to
+real on input.  If all the images are of type short all input data
+is kept as short integers.  Thus, if all the images are of the same type
+there is no datatype conversion on input resulting in greater
+image I/O efficiency.
+.le
+.ls (2)
+In the real data path the processing arithmetic is always real and,
+if the output image is of short pixel datatype, the result
+is truncated.
+.le
+.ls (3)
+The overscan vector and the scale factors for dark count, flat field,
+iillumination, and fringe calibrations are always of type real.  Therefore,
+in the short data path any processing which includes these operations
+will be coerced to real arithmetic and the result truncated at the end
+of the computation.
+.le
+.sh
+13. In the Absence of Image Header Information
+The tasks in the \fBccdred\fR package are most convenient to use when
+the CCD image type, subset, and exposure time are contained in the
+image header.  The ability to redefine which header parameters contain
+this information makes it possible to use the package at many different
+observatories (see \fBinstruments\fR).  However, in the absence of any
+image header information the tasks may still be used effectively.
+There are two ways to proceed.  One way is to use \fBccdhedit\fR
+to place the information in the image header.
+
+The second way is to specify the processing operations more explicitly
+than is needed when the header information is present.  The parameter
+\fIccdtype\fR is set to "" or to "none".  The calibration images are
+specified explicitly by task parameter since they cannot be recognized
+in the input list.  Only one subset at a time may be processed.
+
+If dark count and fringe corrections are to be applied the exposure
+times must be added to all the images.  Alternatively, the dark count
+and fringe images may be scaled explicitly for each input image.  This
+works because the exposure times default to 1 if they are not given in
+the image header.
+.ih
+EXAMPLES
+The user's \fBguide\fR presents a tutorial in the use of this task.
+
+1. In general all that needs to be done is to set the task parameters
+and enter
+
+	cl> ccdproc *.imh &
+
+This will run in the background and process all images which have not
+been processed previously.
+.ih
+SEE ALSO
+package, quadformat, instruments, ccdtypes, flatfields, icfit, ccdred,
+guide, mkillumcor, mkskycor, mkfringecor
+.endhelp
diff --git a/noao/imred/quadred/src/ccdproc/doproc.x b/noao/imred/quadred/src/ccdproc/doproc.x
new file mode 100644
index 00000000..909c6f12
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/doproc.x
@@ -0,0 +1,29 @@
+include	"ccdred.h"
+
+# DOPROC -- Call the appropriate processing procedure.
+#
+# There are four data type paths depending on the readout axis and
+# the calculation data type.
+
+procedure doproc (ccd)
+
+pointer	ccd		# CCD processing structure
+
+begin
+	switch (READAXIS (ccd)) {
+	case 1:
+	    switch (CALCTYPE (ccd)) {
+	    case TY_SHORT:
+	        call proc1s (ccd)
+	    default:
+	        call proc1r (ccd)
+	    }
+	case 2:
+	    switch (CALCTYPE (ccd)) {
+	    case TY_SHORT:
+	        call proc2s (ccd)
+	    default:
+	        call proc2r (ccd)
+	    }
+	}
+end
diff --git a/noao/imred/quadred/src/ccdproc/generic/ccdred.h b/noao/imred/quadred/src/ccdproc/generic/ccdred.h
new file mode 100644
index 00000000..ef41f592
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/generic/ccdred.h
@@ -0,0 +1,155 @@
+# CCDRED Data Structures and Definitions
+
+# The CCD structure:  This structure is used to communicate processing
+# parameters between the package procedures.  It contains pointers to
+# data, calibration image IMIO pointers, scaling parameters, and the
+# correction flags.  The corrections flags indicate which processing
+# operations are to be performed.  The subsection parameters do not
+# include a step size.  A step size is assumed.  If arbitrary subsampling
+# is desired this would be the next generalization.
+
+define	LEN_CCD		75		# Length of CCD structure
+
+# CCD data coordinates
+define	CCD_C1		Memi[$1]	# CCD starting column
+define	CCD_C2		Memi[$1+1]	# CCD ending column
+define	CCD_L1		Memi[$1+2]	# CCD starting line
+define	CCD_L2		Memi[$1+3]	# CCD ending line
+
+# Input data
+define	IN_IM		Memi[$1+4]	# Input image pointer
+define	IN_C1		Memi[$1+5]	# Input data starting column
+define	IN_C2		Memi[$1+6]	# Input data ending column
+define	IN_L1		Memi[$1+7]	# Input data starting line
+define	IN_L2		Memi[$1+8]	# Input data ending line
+define	IN_NSEC		Memi[$1+71]	# Number of input pieces
+define	IN_SEC		Memi[$1+72]	# Pointer to sections (c1,c2,l1,l2)xn
+
+# Output data
+define	OUT_IM		Memi[$1+9]	# Output image pointer
+define	OUT_C1		Memi[$1+10]	# Output data starting column
+define	OUT_C2		Memi[$1+11]	# Output data ending column
+define	OUT_L1		Memi[$1+12]	# Output data starting line
+define	OUT_L2		Memi[$1+13]	# Output data ending line
+define	OUT_SEC		Memi[$1+73]	# Pointer to sections (c1,c2,l1,l2)xn
+
+# Zero level data
+define	ZERO_IM		Memi[$1+14]	# Zero level image pointer
+define	ZERO_C1		Memi[$1+15]	# Zero level data starting column
+define	ZERO_C2		Memi[$1+16]	# Zero level data ending column
+define	ZERO_L1		Memi[$1+17]	# Zero level data starting line
+define	ZERO_L2		Memi[$1+18]	# Zero level data ending line
+
+# Dark count data
+define	DARK_IM		Memi[$1+19]	# Dark count image pointer
+define	DARK_C1		Memi[$1+20]	# Dark count data starting column
+define	DARK_C2		Memi[$1+21]	# Dark count data ending column
+define	DARK_L1		Memi[$1+22]	# Dark count data starting line
+define	DARK_L2		Memi[$1+23]	# Dark count data ending line
+
+# Flat field data
+define	FLAT_IM		Memi[$1+24]	# Flat field image pointer
+define	FLAT_C1		Memi[$1+25]	# Flat field data starting column
+define	FLAT_C2		Memi[$1+26]	# Flat field data ending column
+define	FLAT_L1		Memi[$1+27]	# Flat field data starting line
+define	FLAT_L2		Memi[$1+28]	# Flat field data ending line
+
+# Illumination data
+define	ILLUM_IM	Memi[$1+29]	# Illumination image pointer
+define	ILLUM_C1	Memi[$1+30]	# Illumination data starting column
+define	ILLUM_C2	Memi[$1+31]	# Illumination data ending column
+define	ILLUM_L1	Memi[$1+32]	# Illumination data starting line
+define	ILLUM_L2	Memi[$1+33]	# Illumination data ending line
+
+# Fringe data
+define	FRINGE_IM	Memi[$1+34]	# Fringe image pointer
+define	FRINGE_C1	Memi[$1+35]	# Fringe data starting column
+define	FRINGE_C2	Memi[$1+36]	# Fringe data ending column
+define	FRINGE_L1	Memi[$1+37]	# Fringe data starting line
+define	FRINGE_L2	Memi[$1+38]	# Fringe data ending line
+
+# Trim section
+define	TRIM_C1		Memi[$1+39]	# Trim starting column
+define	TRIM_C2		Memi[$1+40]	# Trim ending column
+define	TRIM_L1		Memi[$1+41]	# Trim starting line
+define	TRIM_L2		Memi[$1+42]	# Trim ending line
+
+# Bias section
+define	BIAS_C1		Memi[$1+43]	# Bias starting column
+define	BIAS_C2		Memi[$1+44]	# Bias ending column
+define	BIAS_L1		Memi[$1+45]	# Bias starting line
+define	BIAS_L2		Memi[$1+46]	# Bias ending line
+define	BIAS_SEC	Memi[$1+74]	# Multiple bias sections
+
+define	READAXIS	Memi[$1+47]	# Read out axis (1=cols, 2=lines)
+define	CALCTYPE	Memi[$1+48]	# Calculation data type
+define	NBADCOLS	Memi[$1+49]	# Number of column interpolation regions
+define	BADCOLS		Memi[$1+50]	# Pointer to col interpolation regions
+define	NBADLINES	Memi[$1+51]	# Number of line interpolation regions
+define	BADLINES	Memi[$1+52]	# Pointer to line interpolation regions
+define	OVERSCAN_VEC	Memi[$1+53]	# Pointer to overscan vector
+define	DARKSCALE	Memr[P2R($1+54)]	# Dark count scale factor
+define	FRINGESCALE	Memr[P2R($1+55)]	# Fringe scale factor
+define	FLATSCALE	Memr[P2R($1+56)]	# Flat field scale factor
+define	ILLUMSCALE	Memr[P2R($1+57)]	# Illumination scale factor
+define	MINREPLACE	Memr[P2R($1+58)]	# Minimum replacement value
+define	MEAN		Memr[P2R($1+59)]	# Mean of output image
+define	COR		Memi[$1+60]	# Overall correction flag
+define	CORS		Memi[$1+61+($2-1)]  # Individual correction flags
+
+# Individual components of input, output, and bias section pieces.
+define	IN_SC1		Memi[IN_SEC($1)+4*$2-4]
+define	IN_SC2		Memi[IN_SEC($1)+4*$2-3]
+define	IN_SL1		Memi[IN_SEC($1)+4*$2-2]
+define	IN_SL2		Memi[IN_SEC($1)+4*$2-1]
+define	OUT_SC1		Memi[OUT_SEC($1)+4*$2-4]
+define	OUT_SC2		Memi[OUT_SEC($1)+4*$2-3]
+define	OUT_SL1		Memi[OUT_SEC($1)+4*$2-2]
+define	OUT_SL2		Memi[OUT_SEC($1)+4*$2-1]
+define	BIAS_SC1	Memi[BIAS_SEC($1)+4*$2-4]
+define	BIAS_SC2	Memi[BIAS_SEC($1)+4*$2-3]
+define	BIAS_SL1	Memi[BIAS_SEC($1)+4*$2-2]
+define	BIAS_SL2	Memi[BIAS_SEC($1)+4*$2-1]
+
+# The correction array contains the following elements with array indices
+# given by the macro definitions.
+
+define	NCORS		10		# Number of corrections
+
+define	FIXPIX		1		# Fix bad pixels
+define	TRIM		2		# Trim image
+define	OVERSCAN	3		# Apply overscan correction
+define	ZEROCOR		4		# Apply zero level correction
+define	DARKCOR		5		# Apply dark count correction
+define	FLATCOR		6		# Apply flat field correction
+define	ILLUMCOR	7		# Apply illumination correction
+define	FRINGECOR	8		# Apply fringe correction
+define	FINDMEAN	9		# Find the mean of the output image
+define	MINREP		10		# Check and replace minimum value
+
+# The following definitions identify the correction values in the correction
+# array.  They are defined in terms of bit fields so that it is possible to
+# add corrections to form unique combination corrections.  Some of
+# these combinations are implemented as compound operations for efficiency.
+
+define	O	001B	# overscan
+define	Z	002B	# zero level
+define	D	004B	# dark count
+define	F	010B	# flat field
+define	I	020B	# Illumination
+define	Q	040B	# Fringe
+
+# The following correction combinations are recognized.
+
+define	ZO	003B	# zero level + overscan
+define	DO	005B	# dark count + overscan
+define	DZ	006B	# dark count + zero level
+define	DZO	007B	# dark count + zero level + overscan
+define	FO	011B	# flat field + overscan
+define	FZ	012B	# flat field + zero level
+define	FZO	013B	# flat field + zero level + overscan
+define	FD	014B	# flat field + dark count
+define	FDO	015B	# flat field + dark count + overscan
+define	FDZ	016B	# flat field + dark count + zero level
+define	FDZO	017B	# flat field + dark count + zero level + overscan
+define	QI	060B	# fringe + illumination
diff --git a/noao/imred/quadred/src/ccdproc/generic/cor.x b/noao/imred/quadred/src/ccdproc/generic/cor.x
new file mode 100644
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@@ -0,0 +1,695 @@
+include	"ccdred.h"
+
+
+.help cor Feb87 noao.imred.ccdred
+.nf ----------------------------------------------------------------------------
+cor -- Process CCD image lines
+
+These procedures are the heart of the CCD processing.  They do the desired
+set of processing operations on the image line data as efficiently as
+possible.  They are called by the PROC procedures.  There are four procedures
+one for each readout axis and one for short and real image data.
+Some sets of operations are coded as single compound operations for efficiency.
+To keep the number of combinations managable only the most common
+combinations are coded as compound operations.  The combinations
+consist of any set of line overscan, column overscan, zero level, dark
+count, and flat field and any set of illumination and fringe
+correction.  The corrections are applied in place to the output vector.
+
+The column readout procedure is more complicated in order to handle
+zero level and flat field corrections specified as one dimensional
+readout corrections instead of two dimensional calibration images.
+Column readout format is probably extremely rare and the 1D readout
+corrections are used only for special types of data.
+.ih
+SEE ALSO
+proc, ccdred.h
+.endhelp -----------------------------------------------------------------------
+
+
+# COR1 -- Correct image lines with readout axis 1 (lines).
+
+procedure cor1s (cors, out, overscan, zero, dark, flat, illum,
+	fringe, n, darkscale, flatscale, illumscale, frgscale)
+
+int	cors[ARB]	# Correction flags
+short	out[n]		# Output data
+real	overscan	# Overscan value
+short	zero[n]		# Zero level correction
+short	dark[n]		# Dark count correction
+short	flat[n]		# Flat field correction
+short	illum[n]	# Illumination correction
+short	fringe[n]	# Fringe correction
+int	n		# Number of pixels
+real	darkscale	# Dark count scale factor
+real	flatscale	# Flat field scale factor
+real	illumscale	# Illumination scale factor
+real	frgscale	# Fringe scale factor
+
+int	i, op
+
+begin
+	op = cors[OVERSCAN] + cors[ZEROCOR] + cors[DARKCOR] + cors[FLATCOR]
+	switch (op) {
+	case O: # overscan
+	    do i = 1, n
+	        out[i] = out[i] - overscan
+	case Z: # zero level
+	    do i = 1, n
+		out[i] = out[i] - zero[i]
+
+	case ZO: # zero level + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - zero[i]
+
+	case D: # dark count
+	    do i = 1, n
+		out[i] = out[i] - darkscale * dark[i]
+	case DO: # dark count + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - darkscale * dark[i]
+	case DZ: # dark count + zero level
+	    do i = 1, n
+		out[i] = out[i] - zero[i] - darkscale * dark[i]
+	case DZO: # dark count + zero level + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - zero[i] - darkscale * dark[i]
+
+	case F: # flat field
+	    do i = 1, n
+		out[i] = out[i] * flatscale / flat[i]
+	case FO: # flat field + overscan
+	    do i = 1, n
+	        out[i] = (out[i] - overscan) * flatscale / flat[i]
+	case FZ: # flat field + zero level
+	    do i = 1, n
+		out[i] = (out[i] - zero[i]) * flatscale / flat[i]
+	case FZO: # flat field + zero level + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - zero[i]) * flatscale /
+		    flat[i]
+	case FD: # flat field + dark count
+	    do i = 1, n
+		out[i] = (out[i] - darkscale * dark[i]) * flatscale / flat[i]
+	case FDO: # flat field + dark count + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - darkscale * dark[i]) *
+		    flatscale / flat[i]
+	case FDZ: # flat field + dark count + zero level
+	    do i = 1, n
+		out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+		    flatscale / flat[i]
+	case FDZO: # flat field + dark count + zero level + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - zero[i] -
+		    darkscale * dark[i]) * flatscale / flat[i]
+	}
+
+	# Often these operations will not be performed so test for no
+	# correction rather than go through the switch.
+
+	op = cors[ILLUMCOR] + cors[FRINGECOR]
+	if (op != 0) {
+	    switch (op) {
+	    case I: # illumination
+	        do i = 1, n
+		    out[i] = out[i] * illumscale / illum[i]
+	    case Q: # fringe
+	        do i = 1, n
+		    out[i] = out[i] - frgscale * fringe[i]
+	    case QI: # fringe + illumination
+	        do i = 1, n
+		    out[i] = out[i]*illumscale/illum[i] - frgscale*fringe[i]
+	    }
+	}
+end
+
+
+# COR2 -- Correct lines for readout axis 2 (columns).  This procedure is
+# more complex than when the readout is along the image lines because the
+# zero level and/or flat field corrections may be single readout column
+# vectors.
+
+procedure cor2s (line, cors, out, overscan, zero, dark, flat, illum,
+	fringe, n, zeroim, flatim, darkscale, flatscale, illumscale, frgscale)
+
+int	line		# Line to be corrected
+int	cors[ARB]	# Correction flags
+short	out[n]		# Output data
+real	overscan[n]	# Overscan value
+short	zero[n]		# Zero level correction
+short	dark[n]		# Dark count correction
+short	flat[n]		# Flat field correction
+short	illum[n]	# Illumination correction
+short	fringe[n]	# Fringe correction
+int	n		# Number of pixels
+pointer	zeroim		# Zero level IMIO pointer (NULL if 1D vector)
+pointer	flatim		# Flat field IMIO pointer (NULL if 1D vector)
+real	darkscale	# Dark count scale factor
+real	flatscale	# Flat field scale factor
+real	illumscale	# Illumination scale factor
+real	frgscale	# Fringe scale factor
+
+short	zeroval
+real	flatval
+int	i, op
+
+begin
+	op = cors[OVERSCAN] + cors[ZEROCOR] + cors[DARKCOR] + cors[FLATCOR]
+	switch (op) {
+	case O: # overscan
+	    do i = 1, n
+	        out[i] = out[i] - overscan[i]
+	case Z: # zero level
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - zero[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - zeroval
+	    }
+
+	case ZO: # zero level + overscan
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zero[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zeroval
+	    }
+
+	case D: # dark count
+	    do i = 1, n
+		out[i] = out[i] - darkscale * dark[i]
+	case DO: # dark count + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan[i] - darkscale * dark[i]
+	case DZ: # dark count + zero level
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - zero[i] - darkscale * dark[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - zeroval - darkscale * dark[i]
+	    }
+	case DZO: # dark count + zero level + overscan
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zero[i] -
+			darkscale * dark[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zeroval -
+			darkscale * dark[i]
+	    }
+
+	case F: # flat field
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = out[i] * flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = out[i] * flatval
+	    }
+	case FO: # flat field + overscan
+	    if (flatim != NULL) {
+	        do i = 1, n
+	            out[i] = (out[i] - overscan[i]) * flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+	            out[i] = (out[i] - overscan[i]) * flatval
+	    }
+	case FZ: # flat field + zero level
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i]) * flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval) * flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval) * flatval
+		}
+	    }
+	case FZO: # flat field + zero level + overscan
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i]) *
+			    flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval) *
+			    flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval) * flatval
+		}
+	    }
+	case FD: # flat field + dark count
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = (out[i] - darkscale * dark[i]) * flatscale/flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = (out[i] - darkscale * dark[i]) * flatval
+	    }
+	case FDO: # flat field + dark count + overscan
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = (out[i] - overscan[i] - darkscale * dark[i]) *
+		        flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = (out[i] - overscan[i] - darkscale * dark[i]) *
+		        flatval
+	    }
+	case FDZ: # flat field + dark count + zero level
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+			    flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval - darkscale * dark[i]) *
+			    flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+			    flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval - darkscale * dark[i]) *
+			    flatval
+		}
+	    }
+	case FDZO: # flat field + dark count + zero level + overscan
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i] -
+			    darkscale * dark[i]) * flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval -
+			    darkscale * dark[i]) * flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i] -
+			    darkscale * dark[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval -
+			    darkscale * dark[i]) * flatval
+		}
+	    }
+	}
+
+	# Often these operations will not be performed so test for no
+	# correction rather than go through the switch.
+
+	op = cors[ILLUMCOR] + cors[FRINGECOR]
+	if (op != 0) {
+	    switch (op) {
+	    case I: # illumination
+	        do i = 1, n
+		    out[i] = out[i] * illumscale / illum[i]
+	    case Q: # fringe
+	        do i = 1, n
+		    out[i] = out[i] - frgscale * fringe[i]
+	    case QI: # fringe + illumination
+	        do i = 1, n
+		    out[i] = out[i]*illumscale/illum[i] - frgscale*fringe[i]
+	    }
+	}
+end
+
+# COR1 -- Correct image lines with readout axis 1 (lines).
+
+procedure cor1r (cors, out, overscan, zero, dark, flat, illum,
+	fringe, n, darkscale, flatscale, illumscale, frgscale)
+
+int	cors[ARB]	# Correction flags
+real	out[n]		# Output data
+real	overscan	# Overscan value
+real	zero[n]		# Zero level correction
+real	dark[n]		# Dark count correction
+real	flat[n]		# Flat field correction
+real	illum[n]	# Illumination correction
+real	fringe[n]	# Fringe correction
+int	n		# Number of pixels
+real	darkscale	# Dark count scale factor
+real	flatscale	# Flat field scale factor
+real	illumscale	# Illumination scale factor
+real	frgscale	# Fringe scale factor
+
+int	i, op
+
+begin
+	op = cors[OVERSCAN] + cors[ZEROCOR] + cors[DARKCOR] + cors[FLATCOR]
+	switch (op) {
+	case O: # overscan
+	    do i = 1, n
+	        out[i] = out[i] - overscan
+	case Z: # zero level
+	    do i = 1, n
+		out[i] = out[i] - zero[i]
+
+	case ZO: # zero level + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - zero[i]
+
+	case D: # dark count
+	    do i = 1, n
+		out[i] = out[i] - darkscale * dark[i]
+	case DO: # dark count + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - darkscale * dark[i]
+	case DZ: # dark count + zero level
+	    do i = 1, n
+		out[i] = out[i] - zero[i] - darkscale * dark[i]
+	case DZO: # dark count + zero level + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan - zero[i] - darkscale * dark[i]
+
+	case F: # flat field
+	    do i = 1, n
+		out[i] = out[i] * flatscale / flat[i]
+	case FO: # flat field + overscan
+	    do i = 1, n
+	        out[i] = (out[i] - overscan) * flatscale / flat[i]
+	case FZ: # flat field + zero level
+	    do i = 1, n
+		out[i] = (out[i] - zero[i]) * flatscale / flat[i]
+	case FZO: # flat field + zero level + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - zero[i]) * flatscale /
+		    flat[i]
+	case FD: # flat field + dark count
+	    do i = 1, n
+		out[i] = (out[i] - darkscale * dark[i]) * flatscale / flat[i]
+	case FDO: # flat field + dark count + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - darkscale * dark[i]) *
+		    flatscale / flat[i]
+	case FDZ: # flat field + dark count + zero level
+	    do i = 1, n
+		out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+		    flatscale / flat[i]
+	case FDZO: # flat field + dark count + zero level + overscan
+	    do i = 1, n
+		out[i] = (out[i] - overscan - zero[i] -
+		    darkscale * dark[i]) * flatscale / flat[i]
+	}
+
+	# Often these operations will not be performed so test for no
+	# correction rather than go through the switch.
+
+	op = cors[ILLUMCOR] + cors[FRINGECOR]
+	if (op != 0) {
+	    switch (op) {
+	    case I: # illumination
+	        do i = 1, n
+		    out[i] = out[i] * illumscale / illum[i]
+	    case Q: # fringe
+	        do i = 1, n
+		    out[i] = out[i] - frgscale * fringe[i]
+	    case QI: # fringe + illumination
+	        do i = 1, n
+		    out[i] = out[i]*illumscale/illum[i] - frgscale*fringe[i]
+	    }
+	}
+end
+
+
+# COR2 -- Correct lines for readout axis 2 (columns).  This procedure is
+# more complex than when the readout is along the image lines because the
+# zero level and/or flat field corrections may be single readout column
+# vectors.
+
+procedure cor2r (line, cors, out, overscan, zero, dark, flat, illum,
+	fringe, n, zeroim, flatim, darkscale, flatscale, illumscale, frgscale)
+
+int	line		# Line to be corrected
+int	cors[ARB]	# Correction flags
+real	out[n]		# Output data
+real	overscan[n]	# Overscan value
+real	zero[n]		# Zero level correction
+real	dark[n]		# Dark count correction
+real	flat[n]		# Flat field correction
+real	illum[n]	# Illumination correction
+real	fringe[n]	# Fringe correction
+int	n		# Number of pixels
+pointer	zeroim		# Zero level IMIO pointer (NULL if 1D vector)
+pointer	flatim		# Flat field IMIO pointer (NULL if 1D vector)
+real	darkscale	# Dark count scale factor
+real	flatscale	# Flat field scale factor
+real	illumscale	# Illumination scale factor
+real	frgscale	# Fringe scale factor
+
+real	zeroval
+real	flatval
+int	i, op
+
+begin
+	op = cors[OVERSCAN] + cors[ZEROCOR] + cors[DARKCOR] + cors[FLATCOR]
+	switch (op) {
+	case O: # overscan
+	    do i = 1, n
+	        out[i] = out[i] - overscan[i]
+	case Z: # zero level
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - zero[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - zeroval
+	    }
+
+	case ZO: # zero level + overscan
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zero[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zeroval
+	    }
+
+	case D: # dark count
+	    do i = 1, n
+		out[i] = out[i] - darkscale * dark[i]
+	case DO: # dark count + overscan
+	    do i = 1, n
+		out[i] = out[i] - overscan[i] - darkscale * dark[i]
+	case DZ: # dark count + zero level
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - zero[i] - darkscale * dark[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - zeroval - darkscale * dark[i]
+	    }
+	case DZO: # dark count + zero level + overscan
+	    if (zeroim != NULL)
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zero[i] -
+			darkscale * dark[i]
+	    else {
+		zeroval = zero[line]
+	        do i = 1, n
+		    out[i] = out[i] - overscan[i] - zeroval -
+			darkscale * dark[i]
+	    }
+
+	case F: # flat field
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = out[i] * flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = out[i] * flatval
+	    }
+	case FO: # flat field + overscan
+	    if (flatim != NULL) {
+	        do i = 1, n
+	            out[i] = (out[i] - overscan[i]) * flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+	            out[i] = (out[i] - overscan[i]) * flatval
+	    }
+	case FZ: # flat field + zero level
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i]) * flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval) * flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval) * flatval
+		}
+	    }
+	case FZO: # flat field + zero level + overscan
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i]) *
+			    flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval) *
+			    flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval) * flatval
+		}
+	    }
+	case FD: # flat field + dark count
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = (out[i] - darkscale * dark[i]) * flatscale/flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = (out[i] - darkscale * dark[i]) * flatval
+	    }
+	case FDO: # flat field + dark count + overscan
+	    if (flatim != NULL) {
+	        do i = 1, n
+		    out[i] = (out[i] - overscan[i] - darkscale * dark[i]) *
+		        flatscale / flat[i]
+	    } else {
+		flatval = flatscale / flat[line]
+	        do i = 1, n
+		    out[i] = (out[i] - overscan[i] - darkscale * dark[i]) *
+		        flatval
+	    }
+	case FDZ: # flat field + dark count + zero level
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+			    flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval - darkscale * dark[i]) *
+			    flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - zero[i] - darkscale * dark[i]) *
+			    flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - zeroval - darkscale * dark[i]) *
+			    flatval
+		}
+	    }
+	case FDZO: # flat field + dark count + zero level + overscan
+	    if (flatim != NULL) {
+	        if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i] -
+			    darkscale * dark[i]) * flatscale / flat[i]
+		} else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval -
+			    darkscale * dark[i]) * flatscale / flat[i]
+		}
+	    } else {
+		flatval = flatscale / flat[line]
+		if (zeroim != NULL) {
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zero[i] -
+			    darkscale * dark[i]) * flatval
+	        } else {
+		    zeroval = zero[line]
+	            do i = 1, n
+		        out[i] = (out[i] - overscan[i] - zeroval -
+			    darkscale * dark[i]) * flatval
+		}
+	    }
+	}
+
+	# Often these operations will not be performed so test for no
+	# correction rather than go through the switch.
+
+	op = cors[ILLUMCOR] + cors[FRINGECOR]
+	if (op != 0) {
+	    switch (op) {
+	    case I: # illumination
+	        do i = 1, n
+		    out[i] = out[i] * illumscale / illum[i]
+	    case Q: # fringe
+	        do i = 1, n
+		    out[i] = out[i] - frgscale * fringe[i]
+	    case QI: # fringe + illumination
+	        do i = 1, n
+		    out[i] = out[i]*illumscale/illum[i] - frgscale*fringe[i]
+	    }
+	}
+end
+
diff --git a/noao/imred/quadred/src/ccdproc/generic/corinput.x b/noao/imred/quadred/src/ccdproc/generic/corinput.x
new file mode 100644
index 00000000..07afaa41
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/generic/corinput.x
@@ -0,0 +1,436 @@
+include	<imhdr.h>
+include	"ccdred.h"
+
+
+# CORINPUT -- Get an input image line, fix the bad pixels, and trim.
+# Return the corrected input line in the output array.
+
+procedure corinputs (in, line, ccd, output, ncols)
+
+pointer	in		# Input IMIO pointer
+int	line		# Corrected output line
+pointer	ccd		# CCD pointer
+short	output[ncols]	# Output data (returned)
+int	ncols		# Number of output columns
+
+int	i, inline
+pointer	inbuf, imgl2s()
+
+begin
+	# Determine the input line in terms of the trimmed output line.
+	if (IN_SEC(ccd) == NULL)
+	    inline = IN_L1(ccd) + line - 1
+	else {
+	    do i = 1, IN_NSEC(ccd) {
+		if (line < OUT_SL1(ccd,i) || line > OUT_SL2(ccd,i))
+		    next
+		inline = IN_SL1(ccd,i) + line - OUT_SL1(ccd,i)
+		break
+	    }
+	}
+
+	# If there are bad lines call a procedure to fix them.  Otherwise
+	# read the image line directly.
+
+	if (NBADLINES(ccd) != 0)
+	    call lfixs (in, inline, Mems[BADLINES(ccd)], IM_LEN(in,1),
+		IM_LEN(in,2), NBADLINES(ccd), inbuf)
+	else
+	    inbuf = imgl2s (in, inline)
+
+	# IF there are bad columns call a procedure to fix them.
+	if (NBADCOLS(ccd) != 0)
+	    call cfixs (inline, Mems[BADCOLS(ccd)], IM_LEN(in,1),
+		IM_LEN(in,2), NBADCOLS(ccd), Mems[inbuf])
+
+	# Move the pixels to the output line.
+	if (IN_SEC(ccd) == NULL)
+	    call amovs (Mems[inbuf+IN_C1(ccd)-OUT_C1(ccd)], output, ncols)
+	else {
+	    do i = 1, IN_NSEC(ccd) {
+		if (inline < IN_SL1(ccd,i) || inline > IN_SL2(ccd,i))
+		    next
+		call amovs (Mems[inbuf+IN_SC1(ccd,i)-OUT_C1(ccd)],
+		    output[OUT_SC1(ccd,i)], OUT_SC2(ccd,i)-OUT_SC1(ccd,i)+1)
+	    }
+	}
+end
+
+
+# CFIX -- Interpolate across bad columns defined in the bad column array.
+
+procedure cfixs (line, badcols, ncols, nlines, nbadcols, data)
+
+int	line				# Line to be fixed
+short	badcols[2, nlines, nbadcols]	# Bad column array
+int	ncols				# Number of columns
+int	nlines				# Number of lines
+int	nbadcols			# Number of bad column regions
+short	data[ncols]			# Data to be fixed
+
+short	val
+real	del
+int	i, j, col1, col2
+
+begin
+	do i = 1, nbadcols {
+	    col1 = badcols[1, line, i]
+	    if (col1 == 0)			# No bad columns
+		return
+	    col2 = badcols[2, line, i]
+	    if (col1 == 1) {			# Bad first column
+		val = data[col2+1]
+		do j = col1, col2
+		    data[j] = val
+	    } else if (col2 == ncols) {		# Bad last column
+		val = data[col1-1]
+		do j = col1, col2
+		    data[j] = val
+	    } else {				# Interpolate
+		del = (data[col2+1] - data[col1-1]) / (col2 - col1 + 2)
+		val = data[col1-1] + del
+		do j = col1, col2
+		    data[j] = val + (j - col1) * del
+	    }
+	}
+end
+
+
+# LFIX -- Get image line and replace bad pixels by interpolation from
+# neighboring lines.  Internal buffers are used to keep the last fixed
+# line and the next good line.  They are allocated with LFIXINIT and
+# freed with LFIXFREE.
+
+procedure lfixs (im, line, badlines, ncols, nlines, nbadlines, data)
+
+pointer	im				# IMIO pointer
+int	line				# Line to be obtained and fixed
+short	badlines[2,nlines,nbadlines]	# Bad line region array
+int	ncols				# Number of columns in image
+int	nlines				# Number of lines in images
+int	nbadlines			# Number of bad line regions
+pointer	data				# Data line pointer (returned)
+
+real	wt1, wt2
+int	i, nextgood, lastgood, col1, col2
+pointer	imgl2s()
+
+pointer	lastbuf, nextbuf
+common	/lfixcom/ lastbuf, nextbuf, lastgood
+
+begin
+	# If this line has bad pixels replace them.  Otherwise just
+	# read the line.
+
+	if (badlines[1, line, 1] != 0) {
+	    # Save the last line which has already been fixed.
+	    if (line != 1)
+		call amovs (Mems[data], Mems[lastbuf], ncols)
+
+	    # Determine the next line with no bad line pixels.  Note that
+	    # this requirement is overly strict since the bad columns
+	    # may not be the same in neighboring lines.
+
+	    nextgood = 0
+	    do i = line+1, nlines {
+		if (badlines[1, i, 1] == 0) {
+		    nextgood = i
+		    break
+		}
+	    }
+
+	    # If the next good line is not the same as previously
+	    # read the data line and store it in a buffer.
+
+	    if ((nextgood != lastgood) && (nextgood != 0)) {
+		data = imgl2s (im, nextgood)
+		call amovs (Mems[data], Mems[nextbuf], ncols)
+		lastgood = nextgood
+	    }
+
+	    # Get the data line.
+	    data = imgl2s (im, line)
+
+	    # Interpolate the bad columns.  At the ends of the image use
+	    # extension otherwise use linear interpolation.
+
+	    if (line == 1) {				# First line is bad
+		do i = 1, nbadlines {
+		    col1 = badlines[1,line,i] - 1
+		    if (col1 == -1)
+			break
+		    col2 = badlines[2,line,i]
+		    call amovs (Mems[nextbuf+col1], Mems[data+col1],
+			col2-col1)
+		}
+	    } else if (nextgood == 0) {			# Last line is bad
+		do i = 1, nbadlines {
+		    col1 = badlines[1,line,i] - 1
+		    if (col1 == -1)
+			break
+		    col2 = badlines[2,line,i]
+		    call amovs (Mems[lastbuf+col1], Mems[data+col1],
+			col2-col1)
+		}
+	    } else {					# Interpolate
+		wt1 = 1. / (nextgood - line + 1)
+		wt2 = 1. - wt1
+		do i = 1, nbadlines {
+		    col1 = badlines[1,line,i] - 1
+		    if (col1 == -1)
+			break
+		    col2 = badlines[2,line,i] - 1
+		    call awsus (Mems[nextbuf+col1], Mems[lastbuf+col1],
+			Mems[data+col1], col2-col1+1, wt1, wt2)
+		}
+	    }
+	} else
+	    data = imgl2s (im, line)
+end
+
+
+# LFIXINIT -- Allocate internal buffers.
+
+procedure lfixinits (im)
+
+pointer	im		# IMIO pointer
+
+int	lastgood
+pointer	lastbuf, nextbuf
+common	/lfixcom/ lastbuf, nextbuf, lastgood
+
+begin
+	call malloc (lastbuf, IM_LEN(im,1), TY_SHORT)
+	call malloc (nextbuf, IM_LEN(im,1), TY_SHORT)
+	lastgood=0
+end
+
+# LFIXFREE -- Free memory when the last line has been obtained.
+
+procedure lfixfrees ()
+
+int	lastgood
+pointer	lastbuf, nextbuf
+common	/lfixcom/ lastbuf, nextbuf, lastgood
+
+begin
+	call mfree (lastbuf, TY_SHORT)
+	call mfree (nextbuf, TY_SHORT)
+end
+
+# CORINPUT -- Get an input image line, fix the bad pixels, and trim.
+# Return the corrected input line in the output array.
+
+procedure corinputr (in, line, ccd, output, ncols)
+
+pointer	in		# Input IMIO pointer
+int	line		# Corrected output line
+pointer	ccd		# CCD pointer
+real	output[ncols]	# Output data (returned)
+int	ncols		# Number of output columns
+
+int	i, inline
+pointer	inbuf, imgl2r()
+
+begin
+	# Determine the input line in terms of the trimmed output line.
+	if (IN_SEC(ccd) == NULL)
+	    inline = IN_L1(ccd) + line - 1
+	else {
+	    do i = 1, IN_NSEC(ccd) {
+		if (line < OUT_SL1(ccd,i) || line > OUT_SL2(ccd,i))
+		    next
+		inline = IN_SL1(ccd,i) + line - OUT_SL1(ccd,i)
+		break
+	    }
+	}
+
+	# If there are bad lines call a procedure to fix them.  Otherwise
+	# read the image line directly.
+
+	if (NBADLINES(ccd) != 0)
+	    call lfixr (in, inline, Mems[BADLINES(ccd)], IM_LEN(in,1),
+		IM_LEN(in,2), NBADLINES(ccd), inbuf)
+	else
+	    inbuf = imgl2r (in, inline)
+
+	# IF there are bad columns call a procedure to fix them.
+	if (NBADCOLS(ccd) != 0)
+	    call cfixr (inline, Mems[BADCOLS(ccd)], IM_LEN(in,1),
+		IM_LEN(in,2), NBADCOLS(ccd), Memr[inbuf])
+
+	# Move the pixels to the output line.
+	if (IN_SEC(ccd) == NULL)
+	    call amovr (Memr[inbuf+IN_C1(ccd)-OUT_C1(ccd)], output, ncols)
+	else {
+	    do i = 1, IN_NSEC(ccd) {
+		if (inline < IN_SL1(ccd,i) || inline > IN_SL2(ccd,i))
+		    next
+		call amovr (Memr[inbuf+IN_SC1(ccd,i)-OUT_C1(ccd)],
+		    output[OUT_SC1(ccd,i)], OUT_SC2(ccd,i)-OUT_SC1(ccd,i)+1)
+	    }
+	}
+end
+
+
+# CFIX -- Interpolate across bad columns defined in the bad column array.
+
+procedure cfixr (line, badcols, ncols, nlines, nbadcols, data)
+
+int	line				# Line to be fixed
+short	badcols[2, nlines, nbadcols]	# Bad column array
+int	ncols				# Number of columns
+int	nlines				# Number of lines
+int	nbadcols			# Number of bad column regions
+real	data[ncols]			# Data to be fixed
+
+real	val
+real	del
+int	i, j, col1, col2
+
+begin
+	do i = 1, nbadcols {
+	    col1 = badcols[1, line, i]
+	    if (col1 == 0)			# No bad columns
+		return
+	    col2 = badcols[2, line, i]
+	    if (col1 == 1) {			# Bad first column
+		val = data[col2+1]
+		do j = col1, col2
+		    data[j] = val
+	    } else if (col2 == ncols) {		# Bad last column
+		val = data[col1-1]
+		do j = col1, col2
+		    data[j] = val
+	    } else {				# Interpolate
+		del = (data[col2+1] - data[col1-1]) / (col2 - col1 + 2)
+		val = data[col1-1] + del
+		do j = col1, col2
+		    data[j] = val + (j - col1) * del
+	    }
+	}
+end
+
+
+# LFIX -- Get image line and replace bad pixels by interpolation from
+# neighboring lines.  Internal buffers are used to keep the last fixed
+# line and the next good line.  They are allocated with LFIXINIT and
+# freed with LFIXFREE.
+
+procedure lfixr (im, line, badlines, ncols, nlines, nbadlines, data)
+
+pointer	im				# IMIO pointer
+int	line				# Line to be obtained and fixed
+short	badlines[2,nlines,nbadlines]	# Bad line region array
+int	ncols				# Number of columns in image
+int	nlines				# Number of lines in images
+int	nbadlines			# Number of bad line regions
+pointer	data				# Data line pointer (returned)
+
+real	wt1, wt2
+int	i, nextgood, lastgood, col1, col2
+pointer	imgl2r()
+
+pointer	lastbuf, nextbuf
+common	/lfixcom/ lastbuf, nextbuf, lastgood
+
+begin
+	# If this line has bad pixels replace them.  Otherwise just
+	# read the line.
+
+	if (badlines[1, line, 1] != 0) {
+	    # Save the last line which has already been fixed.
+	    if (line != 1)
+		call amovr (Memr[data], Memr[lastbuf], ncols)
+
+	    # Determine the next line with no bad line pixels.  Note that
+	    # this requirement is overly strict since the bad columns
+	    # may not be the same in neighboring lines.
+
+	    nextgood = 0
+	    do i = line+1, nlines {
+		if (badlines[1, i, 1] == 0) {
+		    nextgood = i
+		    break
+		}
+	    }
+
+	    # If the next good line is not the same as previously
+	    # read the data line and store it in a buffer.
+
+	    if ((nextgood != lastgood) && (nextgood != 0)) {
+		data = imgl2r (im, nextgood)
+		call amovr (Memr[data], Memr[nextbuf], ncols)
+		lastgood = nextgood
+	    }
+
+	    # Get the data line.
+	    data = imgl2r (im, line)
+
+	    # Interpolate the bad columns.  At the ends of the image use
+	    # extension otherwise use linear interpolation.
+
+	    if (line == 1) {				# First line is bad
+		do i = 1, nbadlines {
+		    col1 = badlines[1,line,i] - 1
+		    if (col1 == -1)
+			break
+		    col2 = badlines[2,line,i]
+		    call amovr (Memr[nextbuf+col1], Memr[data+col1],
+			col2-col1)
+		}
+	    } else if (nextgood == 0) {			# Last line is bad
+		do i = 1, nbadlines {
+		    col1 = badlines[1,line,i] - 1
+		    if (col1 == -1)
+			break
+		    col2 = badlines[2,line,i]
+		    call amovr (Memr[lastbuf+col1], Memr[data+col1],
+			col2-col1)
+		}
+	    } else {					# Interpolate
+		wt1 = 1. / (nextgood - line + 1)
+		wt2 = 1. - wt1
+		do i = 1, nbadlines {
+		    col1 = badlines[1,line,i] - 1
+		    if (col1 == -1)
+			break
+		    col2 = badlines[2,line,i] - 1
+		    call awsur (Memr[nextbuf+col1], Memr[lastbuf+col1],
+			Memr[data+col1], col2-col1+1, wt1, wt2)
+		}
+	    }
+	} else
+	    data = imgl2r (im, line)
+end
+
+
+# LFIXINIT -- Allocate internal buffers.
+
+procedure lfixinitr (im)
+
+pointer	im		# IMIO pointer
+
+int	lastgood
+pointer	lastbuf, nextbuf
+common	/lfixcom/ lastbuf, nextbuf, lastgood
+
+begin
+	call malloc (lastbuf, IM_LEN(im,1), TY_REAL)
+	call malloc (nextbuf, IM_LEN(im,1), TY_REAL)
+	lastgood=0
+end
+
+# LFIXFREE -- Free memory when the last line has been obtained.
+
+procedure lfixfreer ()
+
+int	lastgood
+pointer	lastbuf, nextbuf
+common	/lfixcom/ lastbuf, nextbuf, lastgood
+
+begin
+	call mfree (lastbuf, TY_REAL)
+	call mfree (nextbuf, TY_REAL)
+end
+
diff --git a/noao/imred/quadred/src/ccdproc/generic/mkpkg b/noao/imred/quadred/src/ccdproc/generic/mkpkg
new file mode 100644
index 00000000..0f12b368
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/generic/mkpkg
@@ -0,0 +1,12 @@
+# Make CCDRED Package.
+
+$checkout libpkg.a ../
+$update   libpkg.a
+$checkin  libpkg.a ../
+$exit
+
+libpkg.a:
+	cor.x		ccdred.h
+	corinput.x	ccdred.h <imhdr.h>
+	proc.x		ccdred.h <imhdr.h>
+	;
diff --git a/noao/imred/quadred/src/ccdproc/generic/proc.x b/noao/imred/quadred/src/ccdproc/generic/proc.x
new file mode 100644
index 00000000..0251f4f8
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/generic/proc.x
@@ -0,0 +1,678 @@
+include	<imhdr.h>
+include	"ccdred.h"
+
+
+.help proc Feb87 noao.imred.ccdred
+.nf ----------------------------------------------------------------------------
+proc -- Process CCD images
+
+These are the main CCD reduction procedures.  There is one for each
+readout axis (lines or columns) and one for short and real image data.
+They apply corrections for bad pixels, overscan levels, zero levels,
+dark counts, flat field response, illumination response, and fringe
+effects.  The image is also trimmed if it was mapped with an image
+section.  The mean value for the output image is computed when the flat
+field or illumination image is processed to form the scale factor for
+these calibrations in order to avoid reading through these image a
+second time.
+
+The processing information and parameters are specified in the CCD
+structure. The processing operations to be performed are specified by
+the correction array CORS in the ccd structure.  There is one array
+element for each operation with indices defined symbolically by macro
+definitions (see ccdred.h); i.e.  FLATCOR.  The value of the array
+element is an integer bit field in which the bit set is the same as the
+array index; i.e element 3 will have the third bit set for an operation
+with array value 2**(3-1)=4.  If an operation is not to be performed
+the bit is not set and the array element has the numeric value zero.
+Note that the addition of several correction elements gives a unique
+bit field describing a combination of operations.  For efficiency the
+most common combinations are implemented as separate units.
+
+The CCD structure also contains the correction or calibration data
+consisting either pointers to data, IMIO pointers for the calibration
+images, and scale factors.
+
+The processing is performed line-by-line.  The procedure CORINPUT is
+called to get an input line.  This procedure trims and fixes bad pixels by
+interpolation.  The output line and lines from the various calibration
+images are read.  The image vectors as well as the overscan vector and
+the scale factors are passed to the procedure COR (which also
+dereferences the pointer data into simple arrays and variables).  That
+procedure does the actual corrections apart from bad pixel
+corrections.
+
+The final optional step is to add each corrected output line to form a
+mean.  This adds efficiency since the operation is done only if desired
+and the output image data is already in memory so there is no I/O
+penalty.
+
+SEE ALSO
+    ccdred.h, cor, fixpix, setfixpix, setoverscan, settrim,
+    setzero, setdark, setflat, setillum, setfringe
+.endhelp ----------------------------------------------------------------------
+
+
+
+# PROC1 -- Process CCD images with readout axis 1 (lines).
+
+procedure proc1s (ccd)
+
+pointer	ccd		# CCD structure
+
+int	i, line, nlin, ncols, nlines, findmean, rep
+int	c1, c2, l1, l2
+real	overscan, darkscale, flatscale, illumscale, frgscale, mean
+short	minrep
+pointer	in, out, zeroim, darkim, flatim, illumim, fringeim
+pointer	outbuf, overscan_vec, zerobuf, darkbuf, flatbuf, illumbuf, fringebuf
+
+real	asums()
+pointer	imgl2s(), impl2s(), ccd_gls()
+
+begin
+	# Initialize.  If the correction image is 1D then just get the
+	# data once.
+
+	in = IN_IM(ccd)
+	out = OUT_IM(ccd)
+	nlin = IM_LEN(in,2)
+	ncols = OUT_C2(ccd) - OUT_C1(ccd) + 1
+	nlines = OUT_L2(ccd) - OUT_L1(ccd) + 1
+
+	if (CORS(ccd, FIXPIX) == YES)
+	    call lfixinits (in)
+
+	findmean = CORS(ccd, FINDMEAN)
+	if (findmean == YES)
+	    mean = 0.
+	rep = CORS(ccd, MINREP)
+	if (rep == YES)
+	    minrep = MINREPLACE(ccd)
+
+	overscan_vec = OVERSCAN_VEC(ccd)
+
+	if (CORS(ccd, ZEROCOR) == 0) {
+	    zeroim = NULL
+	    zerobuf = 1
+	} else if (IM_LEN(ZERO_IM(ccd),2) == 1) {
+	    zeroim = NULL
+	    zerobuf = ccd_gls (ZERO_IM(ccd), ZERO_C1(ccd), ZERO_C2(ccd), 1)
+	} else
+	    zeroim = ZERO_IM(ccd)
+
+	if (CORS(ccd, DARKCOR) == 0) {
+	    darkim = NULL
+	    darkbuf = 1
+	} else if (IM_LEN(DARK_IM(ccd),2) == 1) {
+	    darkim = NULL
+	    darkbuf = ccd_gls (DARK_IM(ccd), DARK_C1(ccd), DARK_C2(ccd), 1)
+	    darkscale = FLATSCALE(ccd)
+	} else {
+	    darkim = DARK_IM(ccd)
+	    darkscale = DARKSCALE(ccd)
+	}
+
+	if (CORS(ccd, FLATCOR) == 0) {
+	    flatim = NULL
+	    flatbuf = 1
+	} else if (IM_LEN(FLAT_IM(ccd),2) == 1) {
+	    flatim = NULL
+	    flatbuf = ccd_gls (FLAT_IM(ccd), FLAT_C1(ccd), FLAT_C2(ccd), 1)
+	    flatscale = FLATSCALE(ccd)
+	} else {
+	    flatim = FLAT_IM(ccd)
+	    flatscale = FLATSCALE(ccd)
+	}
+
+	if (CORS(ccd, ILLUMCOR) == 0) {
+	    illumim = NULL
+	    illumbuf = 1
+	} else {
+	    illumim = ILLUM_IM(ccd)
+	    illumscale = ILLUMSCALE(ccd)
+	}
+
+	if (CORS(ccd, FRINGECOR) == 0) {
+	    fringeim = NULL
+	    fringebuf = 1
+	} else {
+	    fringeim = FRINGE_IM(ccd)
+	    frgscale = FRINGESCALE(ccd)
+	}
+
+	# For each line read lines from the input.  Procedure CORINPUT
+	# replaces bad pixels by interpolation and applies a trim to the
+	# input.  Get lines from the output image and from the zero level,
+	# dark count, flat field, illumination, and fringe images.
+	# Call COR1 to do the actual pixel corrections.  Finally, add the
+	# output pixels to a sum for computing the mean.
+	# We must copy data outside of the output data section.
+
+	do line = 2 - OUT_L1(ccd), 0
+	    call amovs (
+		Mems[imgl2s(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mems[impl2s(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	do line = 1, nlines {
+	    outbuf = impl2s (out, OUT_L1(ccd)+line-1)
+	    call corinputs (in, line, ccd, Mems[outbuf], IM_LEN(out,1))
+
+	    outbuf = outbuf + OUT_C1(ccd) - 1
+	    if (overscan_vec != NULL)
+		overscan = Memr[overscan_vec+line-1]
+	    if (zeroim != NULL)
+		zerobuf = ccd_gls (zeroim, ZERO_C1(ccd), ZERO_C2(ccd),
+		    ZERO_L1(ccd)+line-1)
+	    if (darkim != NULL)
+		darkbuf = ccd_gls (darkim, DARK_C1(ccd), DARK_C2(ccd),
+		    DARK_L1(ccd)+line-1)
+	    if (flatim != NULL)
+		flatbuf = ccd_gls (flatim, FLAT_C1(ccd), FLAT_C2(ccd),
+		    FLAT_L1(ccd)+line-1)
+	    if (illumim != NULL)
+		illumbuf = ccd_gls (illumim, ILLUM_C1(ccd), ILLUM_C2(ccd),
+		    ILLUM_L1(ccd)+line-1)
+	    if (fringeim != NULL)
+		fringebuf = ccd_gls (fringeim, FRINGE_C1(ccd), FRINGE_C2(ccd),
+		    FRINGE_L1(ccd)+line-1)
+
+	    if (OUT_SEC(ccd) == NULL) {
+		call cor1s (CORS(ccd,1), Mems[outbuf],
+		    overscan, Mems[zerobuf], Mems[darkbuf],
+		    Mems[flatbuf], Mems[illumbuf], Mems[fringebuf], ncols,
+		    darkscale, flatscale, illumscale, frgscale)
+	    } else {
+		do i = 1, IN_NSEC(ccd) {
+		    l1 = OUT_SL1(ccd,i)
+		    l2 = OUT_SL2(ccd,i)
+		    if (line < l1 || line > l2)
+			next
+		    c1 = OUT_SC1(ccd,i) - 1
+		    c2 = OUT_SC2(ccd,i) - 1
+		    ncols = c2 - c1 + 1
+		    if (overscan_vec != NULL)
+			overscan = Memr[overscan_vec+(i-1)*nlin+line-l1]
+		    
+		    call cor1s (CORS(ccd,1), Mems[outbuf+c1],
+			overscan, Mems[zerobuf+c1], Mems[darkbuf+c1],
+			Mems[flatbuf+c1], Mems[illumbuf+c1],
+			Mems[fringebuf+c1], ncols,
+			darkscale, flatscale, illumscale, frgscale)
+		}
+	    }
+
+	    if (rep == YES)
+		call amaxks (Mems[outbuf], minrep, Mems[outbuf], ncols)
+	    if (findmean == YES)
+		mean = mean + asums (Mems[outbuf], ncols)
+	}
+
+	do line = nlines+1, IM_LEN(out,2)-OUT_L1(ccd)+1
+	    call amovs (
+		Mems[imgl2s(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mems[impl2s(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	# Compute the mean from the sum of the output pixels.
+	if (findmean == YES)
+	    MEAN(ccd) = mean / ncols / nlines
+
+	if (CORS(ccd, FIXPIX) == YES)
+	    call lfixfrees ()
+end
+
+
+# PROC2 -- Process CCD images with readout axis 2 (columns).
+
+procedure proc2s (ccd)
+
+pointer	ccd		# CCD structure
+
+int	line, ncols, nlines, findmean, rep
+real	darkscale, flatscale, illumscale, frgscale, mean
+short	minrep
+pointer	in, out, zeroim, darkim, flatim, illumim, fringeim
+pointer	outbuf, overscan_vec, zerobuf, darkbuf, flatbuf, illumbuf, fringebuf
+
+real	asums()
+pointer	imgl2s(), impl2s(), imgs2s(), ccd_gls()
+
+begin
+	# Initialize.  If the correction image is 1D then just get the
+	# data once.
+
+	in = IN_IM(ccd)
+	out = OUT_IM(ccd)
+	ncols = OUT_C2(ccd) - OUT_C1(ccd) + 1
+	nlines = OUT_L2(ccd) - OUT_L1(ccd) + 1
+
+	if (CORS(ccd, FIXPIX) == YES)
+	    call lfixinits (in)
+
+	findmean = CORS(ccd, FINDMEAN)
+	if (findmean == YES)
+	    mean = 0.
+	rep = CORS(ccd, MINREP)
+	if (rep == YES)
+	    minrep = MINREPLACE(ccd)
+
+	overscan_vec = OVERSCAN_VEC(ccd)
+
+	if (CORS(ccd, ZEROCOR) == 0) {
+	    zeroim = NULL
+	    zerobuf = 1
+	} else if (IM_LEN(ZERO_IM(ccd),1) == 1) {
+	    zeroim = NULL
+	    zerobuf = imgs2s (ZERO_IM(ccd), 1, 1, ZERO_L1(ccd), ZERO_L2(ccd))
+	} else
+	    zeroim = ZERO_IM(ccd)
+
+	if (CORS(ccd, DARKCOR) == 0) {
+	    darkim = NULL
+	    darkbuf = 1
+	} else if (IM_LEN(DARK_IM(ccd),1) == 1) {
+	    darkim = NULL
+	    darkbuf = imgs2s (DARK_IM(ccd), 1, 1, DARK_L1(ccd), DARK_L2(ccd))
+	    darkscale = DARKSCALE(ccd)
+	} else {
+	    darkim = DARK_IM(ccd)
+	    darkscale = DARKSCALE(ccd)
+	}
+
+	if (CORS(ccd, FLATCOR) == 0) {
+	    flatim = NULL
+	    flatbuf = 1
+	} else if (IM_LEN(FLAT_IM(ccd),1) == 1) {
+	    flatim = NULL
+	    flatbuf = imgs2s (FLAT_IM(ccd), 1, 1, FLAT_L1(ccd), FLAT_L2(ccd))
+	    flatscale = FLATSCALE(ccd)
+	} else {
+	    flatim = FLAT_IM(ccd)
+	    flatscale = FLATSCALE(ccd)
+	}
+
+	if (CORS(ccd, ILLUMCOR) == 0) {
+	    illumim = NULL
+	    illumbuf = 1
+	} else {
+	    illumim = ILLUM_IM(ccd)
+	    illumscale = ILLUMSCALE(ccd)
+	}
+
+	if (CORS(ccd, FRINGECOR) == 0) {
+	    fringeim = NULL
+	    fringebuf = 1
+	} else {
+	    fringeim = FRINGE_IM(ccd)
+	    frgscale = FRINGESCALE(ccd)
+	}
+
+	# For each line read lines from the input.  Procedure CORINPUT
+	# replaces bad pixels by interpolation and applies a trim to the
+	# input.  Get lines from the output image and from the zero level,
+	# dark count, flat field, illumination, and fringe images.
+	# Call COR2 to do the actual pixel corrections.  Finally, add the
+	# output pixels to a sum for computing the mean.
+	# We must copy data outside of the output data section.
+
+	do line = 2 - OUT_L1(ccd), 0
+	    call amovs (
+		Mems[imgl2s(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mems[impl2s(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	do line = 1, nlines {
+	    outbuf = impl2s (out, OUT_L1(ccd)+line-1)
+	    call corinputs (in, line, ccd, Mems[outbuf], IM_LEN(out,1))
+
+	    outbuf = outbuf + OUT_C1(ccd) - 1
+	    if (zeroim != NULL)
+		zerobuf = ccd_gls (zeroim, ZERO_C1(ccd), ZERO_C2(ccd),
+		    ZERO_L1(ccd)+line-1)
+	    if (darkim != NULL)
+		darkbuf = ccd_gls (darkim, DARK_C1(ccd), DARK_C2(ccd),
+		    DARK_L1(ccd)+line-1)
+	    if (flatim != NULL)
+		flatbuf = ccd_gls (flatim, FLAT_C1(ccd), FLAT_C2(ccd),
+		    FLAT_L1(ccd)+line-1)
+	    if (illumim != NULL)
+		illumbuf = ccd_gls (illumim, ILLUM_C1(ccd), ILLUM_C2(ccd),
+		    ILLUM_L1(ccd)+line-1)
+	    if (fringeim != NULL)
+		fringebuf = ccd_gls (fringeim, FRINGE_C1(ccd), FRINGE_C2(ccd),
+		    FRINGE_L1(ccd)+line-1)
+
+	    call cor2s (line, CORS(ccd,1), Mems[outbuf],
+		Memr[overscan_vec], Mems[zerobuf], Mems[darkbuf],
+		Mems[flatbuf], Mems[illumbuf], Mems[fringebuf], ncols,
+		zeroim, flatim, darkscale, flatscale, illumscale, frgscale)
+
+	    if (rep == YES)
+		call amaxks (Mems[outbuf], minrep, Mems[outbuf], ncols)
+	    if (findmean == YES)
+		mean = mean + asums (Mems[outbuf], ncols)
+	}
+
+	do line = nlines+1, IM_LEN(out,2)-OUT_L1(ccd)+1
+	    call amovs (
+		Mems[imgl2s(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mems[impl2s(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	# Compute the mean from the sum of the output pixels.
+	if (findmean == YES)
+	    MEAN(ccd) = mean / ncols / nlines
+
+	if (CORS(ccd, FIXPIX) == YES)
+	    call lfixfrees ()
+end
+
+# PROC1 -- Process CCD images with readout axis 1 (lines).
+
+procedure proc1r (ccd)
+
+pointer	ccd		# CCD structure
+
+int	i, line, nlin, ncols, nlines, findmean, rep
+int	c1, c2, l1, l2
+real	overscan, darkscale, flatscale, illumscale, frgscale, mean
+real	minrep
+pointer	in, out, zeroim, darkim, flatim, illumim, fringeim
+pointer	outbuf, overscan_vec, zerobuf, darkbuf, flatbuf, illumbuf, fringebuf
+
+real	asumr()
+pointer	imgl2r(), impl2r(), ccd_glr()
+
+begin
+	# Initialize.  If the correction image is 1D then just get the
+	# data once.
+
+	in = IN_IM(ccd)
+	out = OUT_IM(ccd)
+	nlin = IM_LEN(in,2)
+	ncols = OUT_C2(ccd) - OUT_C1(ccd) + 1
+	nlines = OUT_L2(ccd) - OUT_L1(ccd) + 1
+
+	if (CORS(ccd, FIXPIX) == YES)
+	    call lfixinitr (in)
+
+	findmean = CORS(ccd, FINDMEAN)
+	if (findmean == YES)
+	    mean = 0.
+	rep = CORS(ccd, MINREP)
+	if (rep == YES)
+	    minrep = MINREPLACE(ccd)
+
+	overscan_vec = OVERSCAN_VEC(ccd)
+
+	if (CORS(ccd, ZEROCOR) == 0) {
+	    zeroim = NULL
+	    zerobuf = 1
+	} else if (IM_LEN(ZERO_IM(ccd),2) == 1) {
+	    zeroim = NULL
+	    zerobuf = ccd_glr (ZERO_IM(ccd), ZERO_C1(ccd), ZERO_C2(ccd), 1)
+	} else
+	    zeroim = ZERO_IM(ccd)
+
+	if (CORS(ccd, DARKCOR) == 0) {
+	    darkim = NULL
+	    darkbuf = 1
+	} else if (IM_LEN(DARK_IM(ccd),2) == 1) {
+	    darkim = NULL
+	    darkbuf = ccd_glr (DARK_IM(ccd), DARK_C1(ccd), DARK_C2(ccd), 1)
+	    darkscale = FLATSCALE(ccd)
+	} else {
+	    darkim = DARK_IM(ccd)
+	    darkscale = DARKSCALE(ccd)
+	}
+
+	if (CORS(ccd, FLATCOR) == 0) {
+	    flatim = NULL
+	    flatbuf = 1
+	} else if (IM_LEN(FLAT_IM(ccd),2) == 1) {
+	    flatim = NULL
+	    flatbuf = ccd_glr (FLAT_IM(ccd), FLAT_C1(ccd), FLAT_C2(ccd), 1)
+	    flatscale = FLATSCALE(ccd)
+	} else {
+	    flatim = FLAT_IM(ccd)
+	    flatscale = FLATSCALE(ccd)
+	}
+
+	if (CORS(ccd, ILLUMCOR) == 0) {
+	    illumim = NULL
+	    illumbuf = 1
+	} else {
+	    illumim = ILLUM_IM(ccd)
+	    illumscale = ILLUMSCALE(ccd)
+	}
+
+	if (CORS(ccd, FRINGECOR) == 0) {
+	    fringeim = NULL
+	    fringebuf = 1
+	} else {
+	    fringeim = FRINGE_IM(ccd)
+	    frgscale = FRINGESCALE(ccd)
+	}
+
+	# For each line read lines from the input.  Procedure CORINPUT
+	# replaces bad pixels by interpolation and applies a trim to the
+	# input.  Get lines from the output image and from the zero level,
+	# dark count, flat field, illumination, and fringe images.
+	# Call COR1 to do the actual pixel corrections.  Finally, add the
+	# output pixels to a sum for computing the mean.
+	# We must copy data outside of the output data section.
+
+	do line = 2 - OUT_L1(ccd), 0
+	    call amovr (
+		Memr[imgl2r(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Memr[impl2r(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	do line = 1, nlines {
+	    outbuf = impl2r (out, OUT_L1(ccd)+line-1)
+	    call corinputr (in, line, ccd, Memr[outbuf], IM_LEN(out,1))
+
+	    outbuf = outbuf + OUT_C1(ccd) - 1
+	    if (overscan_vec != NULL)
+		overscan = Memr[overscan_vec+line-1]
+	    if (zeroim != NULL)
+		zerobuf = ccd_glr (zeroim, ZERO_C1(ccd), ZERO_C2(ccd),
+		    ZERO_L1(ccd)+line-1)
+	    if (darkim != NULL)
+		darkbuf = ccd_glr (darkim, DARK_C1(ccd), DARK_C2(ccd),
+		    DARK_L1(ccd)+line-1)
+	    if (flatim != NULL)
+		flatbuf = ccd_glr (flatim, FLAT_C1(ccd), FLAT_C2(ccd),
+		    FLAT_L1(ccd)+line-1)
+	    if (illumim != NULL)
+		illumbuf = ccd_glr (illumim, ILLUM_C1(ccd), ILLUM_C2(ccd),
+		    ILLUM_L1(ccd)+line-1)
+	    if (fringeim != NULL)
+		fringebuf = ccd_glr (fringeim, FRINGE_C1(ccd), FRINGE_C2(ccd),
+		    FRINGE_L1(ccd)+line-1)
+
+	    if (OUT_SEC(ccd) == NULL) {
+		call cor1r (CORS(ccd,1), Memr[outbuf],
+		    overscan, Memr[zerobuf], Memr[darkbuf],
+		    Memr[flatbuf], Memr[illumbuf], Memr[fringebuf], ncols,
+		    darkscale, flatscale, illumscale, frgscale)
+	    } else {
+		do i = 1, IN_NSEC(ccd) {
+		    l1 = OUT_SL1(ccd,i)
+		    l2 = OUT_SL2(ccd,i)
+		    if (line < l1 || line > l2)
+			next
+		    c1 = OUT_SC1(ccd,i) - 1
+		    c2 = OUT_SC2(ccd,i) - 1
+		    ncols = c2 - c1 + 1
+		    if (overscan_vec != NULL)
+			overscan = Memr[overscan_vec+(i-1)*nlin+line-l1]
+		    
+		    call cor1r (CORS(ccd,1), Memr[outbuf+c1],
+			overscan, Memr[zerobuf+c1], Memr[darkbuf+c1],
+			Memr[flatbuf+c1], Memr[illumbuf+c1],
+			Memr[fringebuf+c1], ncols,
+			darkscale, flatscale, illumscale, frgscale)
+		}
+	    }
+
+	    if (rep == YES)
+		call amaxkr (Memr[outbuf], minrep, Memr[outbuf], ncols)
+	    if (findmean == YES)
+		mean = mean + asumr (Memr[outbuf], ncols)
+	}
+
+	do line = nlines+1, IM_LEN(out,2)-OUT_L1(ccd)+1
+	    call amovr (
+		Memr[imgl2r(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Memr[impl2r(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	# Compute the mean from the sum of the output pixels.
+	if (findmean == YES)
+	    MEAN(ccd) = mean / ncols / nlines
+
+	if (CORS(ccd, FIXPIX) == YES)
+	    call lfixfreer ()
+end
+
+
+# PROC2 -- Process CCD images with readout axis 2 (columns).
+
+procedure proc2r (ccd)
+
+pointer	ccd		# CCD structure
+
+int	line, ncols, nlines, findmean, rep
+real	darkscale, flatscale, illumscale, frgscale, mean
+real	minrep
+pointer	in, out, zeroim, darkim, flatim, illumim, fringeim
+pointer	outbuf, overscan_vec, zerobuf, darkbuf, flatbuf, illumbuf, fringebuf
+
+real	asumr()
+pointer	imgl2r(), impl2r(), imgs2r(), ccd_glr()
+
+begin
+	# Initialize.  If the correction image is 1D then just get the
+	# data once.
+
+	in = IN_IM(ccd)
+	out = OUT_IM(ccd)
+	ncols = OUT_C2(ccd) - OUT_C1(ccd) + 1
+	nlines = OUT_L2(ccd) - OUT_L1(ccd) + 1
+
+	if (CORS(ccd, FIXPIX) == YES)
+	    call lfixinitr (in)
+
+	findmean = CORS(ccd, FINDMEAN)
+	if (findmean == YES)
+	    mean = 0.
+	rep = CORS(ccd, MINREP)
+	if (rep == YES)
+	    minrep = MINREPLACE(ccd)
+
+	overscan_vec = OVERSCAN_VEC(ccd)
+
+	if (CORS(ccd, ZEROCOR) == 0) {
+	    zeroim = NULL
+	    zerobuf = 1
+	} else if (IM_LEN(ZERO_IM(ccd),1) == 1) {
+	    zeroim = NULL
+	    zerobuf = imgs2r (ZERO_IM(ccd), 1, 1, ZERO_L1(ccd), ZERO_L2(ccd))
+	} else
+	    zeroim = ZERO_IM(ccd)
+
+	if (CORS(ccd, DARKCOR) == 0) {
+	    darkim = NULL
+	    darkbuf = 1
+	} else if (IM_LEN(DARK_IM(ccd),1) == 1) {
+	    darkim = NULL
+	    darkbuf = imgs2r (DARK_IM(ccd), 1, 1, DARK_L1(ccd), DARK_L2(ccd))
+	    darkscale = DARKSCALE(ccd)
+	} else {
+	    darkim = DARK_IM(ccd)
+	    darkscale = DARKSCALE(ccd)
+	}
+
+	if (CORS(ccd, FLATCOR) == 0) {
+	    flatim = NULL
+	    flatbuf = 1
+	} else if (IM_LEN(FLAT_IM(ccd),1) == 1) {
+	    flatim = NULL
+	    flatbuf = imgs2r (FLAT_IM(ccd), 1, 1, FLAT_L1(ccd), FLAT_L2(ccd))
+	    flatscale = FLATSCALE(ccd)
+	} else {
+	    flatim = FLAT_IM(ccd)
+	    flatscale = FLATSCALE(ccd)
+	}
+
+	if (CORS(ccd, ILLUMCOR) == 0) {
+	    illumim = NULL
+	    illumbuf = 1
+	} else {
+	    illumim = ILLUM_IM(ccd)
+	    illumscale = ILLUMSCALE(ccd)
+	}
+
+	if (CORS(ccd, FRINGECOR) == 0) {
+	    fringeim = NULL
+	    fringebuf = 1
+	} else {
+	    fringeim = FRINGE_IM(ccd)
+	    frgscale = FRINGESCALE(ccd)
+	}
+
+	# For each line read lines from the input.  Procedure CORINPUT
+	# replaces bad pixels by interpolation and applies a trim to the
+	# input.  Get lines from the output image and from the zero level,
+	# dark count, flat field, illumination, and fringe images.
+	# Call COR2 to do the actual pixel corrections.  Finally, add the
+	# output pixels to a sum for computing the mean.
+	# We must copy data outside of the output data section.
+
+	do line = 2 - OUT_L1(ccd), 0
+	    call amovr (
+		Memr[imgl2r(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Memr[impl2r(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	do line = 1, nlines {
+	    outbuf = impl2r (out, OUT_L1(ccd)+line-1)
+	    call corinputr (in, line, ccd, Memr[outbuf], IM_LEN(out,1))
+
+	    outbuf = outbuf + OUT_C1(ccd) - 1
+	    if (zeroim != NULL)
+		zerobuf = ccd_glr (zeroim, ZERO_C1(ccd), ZERO_C2(ccd),
+		    ZERO_L1(ccd)+line-1)
+	    if (darkim != NULL)
+		darkbuf = ccd_glr (darkim, DARK_C1(ccd), DARK_C2(ccd),
+		    DARK_L1(ccd)+line-1)
+	    if (flatim != NULL)
+		flatbuf = ccd_glr (flatim, FLAT_C1(ccd), FLAT_C2(ccd),
+		    FLAT_L1(ccd)+line-1)
+	    if (illumim != NULL)
+		illumbuf = ccd_glr (illumim, ILLUM_C1(ccd), ILLUM_C2(ccd),
+		    ILLUM_L1(ccd)+line-1)
+	    if (fringeim != NULL)
+		fringebuf = ccd_glr (fringeim, FRINGE_C1(ccd), FRINGE_C2(ccd),
+		    FRINGE_L1(ccd)+line-1)
+
+	    call cor2r (line, CORS(ccd,1), Memr[outbuf],
+		Memr[overscan_vec], Memr[zerobuf], Memr[darkbuf],
+		Memr[flatbuf], Memr[illumbuf], Memr[fringebuf], ncols,
+		zeroim, flatim, darkscale, flatscale, illumscale, frgscale)
+
+	    if (rep == YES)
+		call amaxkr (Memr[outbuf], minrep, Memr[outbuf], ncols)
+	    if (findmean == YES)
+		mean = mean + asumr (Memr[outbuf], ncols)
+	}
+
+	do line = nlines+1, IM_LEN(out,2)-OUT_L1(ccd)+1
+	    call amovr (
+		Memr[imgl2r(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Memr[impl2r(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	# Compute the mean from the sum of the output pixels.
+	if (findmean == YES)
+	    MEAN(ccd) = mean / ncols / nlines
+
+	if (CORS(ccd, FIXPIX) == YES)
+	    call lfixfreer ()
+end
+
diff --git a/noao/imred/quadred/src/ccdproc/hdrmap.com b/noao/imred/quadred/src/ccdproc/hdrmap.com
new file mode 100644
index 00000000..5aa74185
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/hdrmap.com
@@ -0,0 +1,4 @@
+# Common for HDRMAP package.
+
+pointer	stp			# Symbol table pointer
+common	/hdmcom/ stp
diff --git a/noao/imred/quadred/src/ccdproc/hdrmap.x b/noao/imred/quadred/src/ccdproc/hdrmap.x
new file mode 100644
index 00000000..ebcb253e
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/hdrmap.x
@@ -0,0 +1,544 @@
+include	<error.h>
+include	<syserr.h>
+
+.help hdrmap
+.nf-----------------------------------------------------------------------------
+HDRMAP -- Map translation between task parameters and image header parameters.
+
+In order for tasks to be partially independent of the image header
+parameter names used by different instruments and observatories a
+translation is made between task parameters and image header
+parameters.  This translation is given in a file consisting of the task
+parameter name, the image header parameter name, and an optional
+default value.  This file is turned into a symbol table.  If the
+translation file is not found a null pointer is returned.  The package will
+then use the task parameter names directly.  Also if there is no
+translation given in the file for a particular parameter it is passed
+on directly.  If a parameter is not in the image header then the symbol
+table default value, if given, is returned.  This package is layered on
+the IMIO header package.
+
+	        hdmopen (fname)
+		hdmclose ()
+		hdmwrite (fname, mode)
+		hdmname (parameter, str, max_char)
+		hdmgdef (parameter, str, max_char)
+		hdmpdef (parameter, str, max_char)
+	  y/n = hdmaccf (im, parameter)
+		hdmgstr (im, parameter, str, max_char)
+	 ival = hdmgeti (im, parameter)
+	 rval = hdmgetr (im, parameter)
+		hdmpstr (im, parameter, str)
+		hdmputi (im, parameter, value)
+		hdmputr (im, parameter, value)
+		hdmgstp (stp)
+		hdmpstp (stp)
+		hdmdelf (im, parameter)
+		hdmparm (name, parameter, max_char)
+
+hdmopen  -- Open the translation file and map it into a symbol table pointer.
+hdmclose -- Close the symbol table pointer.
+hdmwrite -- Write out translation file.
+hdmname  -- Return the image header parameter name.
+hdmpname -- Put the image header parameter name.
+hdmgdef  -- Get the default value as a string (null if none).
+hdmpdef  -- Put the default value as a string.
+hdmaccf  -- Return whether the image header parameter exists (regardless of
+	    whether there is a default value).
+hdmgstr  -- Get a string valued parameter.  Return default value if not in the
+	    image header.  Return null string if no default or image value.
+hdmgeti  -- Get an integer valued parameter.  Return default value if not in
+	    the image header and error condition if no default or image value.
+hdmgetr  -- Get a real valued parameter.  Return default value if not in
+	    the image header or error condition if no default or image value.
+hdmpstr  -- Put a string valued parameter in the image header.
+hdmputi  -- Put an integer valued parameter in the image header.
+hdmputr  -- Put a real valued parameter in the image header.
+hdmgstp  -- Get the symbol table pointer to save it while another map is used.
+hdmpstp  -- Put the symbol table pointer to restore a map.
+hdmdelf  -- Delete a field.
+hdmparm  -- Return the parameter name corresponding to an image header name.
+.endhelp -----------------------------------------------------------------------
+
+# Symbol table definitions.
+define	LEN_INDEX	32		# Length of symtab index
+define	LEN_STAB	1024		# Length of symtab string buffer
+define	SZ_SBUF		128		# Size of symtab string buffer
+
+define	SZ_NAME		79		# Size of translation symbol name
+define	SZ_DEFAULT	79		# Size of default string
+define	SYMLEN		80		# Length of symbol structure
+
+# Symbol table structure
+define	NAME		Memc[P2C($1)]		# Translation name for symbol
+define	DEFAULT		Memc[P2C($1+40)]	# Default value of parameter
+
+
+# HDMOPEN -- Open the translation file and map it into a symbol table pointer.
+
+procedure hdmopen (fname)
+
+char	fname[ARB]		# Image header map file
+
+int	fd, open(), fscan(), nscan(), errcode()
+pointer	sp, parameter, sym, stopen(), stenter()
+include	"hdrmap.com"
+
+begin
+	# Create an empty symbol table.
+	stp = stopen (fname, LEN_INDEX, LEN_STAB, SZ_SBUF)
+
+	# Return if file not found.
+	iferr (fd = open (fname, READ_ONLY, TEXT_FILE)) {
+	    if (errcode () != SYS_FNOFNAME)
+		call erract (EA_WARN)
+	    return
+	}
+
+	call smark (sp)
+	call salloc (parameter, SZ_NAME, TY_CHAR)
+
+	# Read the file an enter the translations in the symbol table.
+	while (fscan(fd) != EOF) {
+	    call gargwrd (Memc[parameter], SZ_NAME)
+	    if ((nscan() == 0) || (Memc[parameter] == '#'))
+		next
+	    sym = stenter (stp, Memc[parameter], SYMLEN)
+	    call gargwrd (NAME(sym), SZ_NAME)
+	    call gargwrd (DEFAULT(sym), SZ_DEFAULT)
+	}
+
+	call close (fd)
+	call sfree (sp)
+end
+
+
+# HDMCLOSE -- Close the symbol table pointer.
+
+procedure hdmclose ()
+
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    call stclose (stp)
+end
+
+
+# HDMWRITE -- Write out translation file.
+
+procedure hdmwrite (fname, mode)
+
+char	fname[ARB]		# Image header map file
+int	mode			# Access mode (APPEND, NEW_FILE)
+
+int	fd, open(), stridxs()
+pointer	sym, sthead(), stnext(), stname()
+errchk	open
+include	"hdrmap.com"
+
+begin
+	# If there is no symbol table do nothing.
+	if (stp == NULL)
+	    return
+
+	fd = open (fname, mode, TEXT_FILE)
+
+	sym = sthead (stp)
+	for (sym = sthead (stp); sym != NULL; sym = stnext (stp, sym)) {
+	    if (stridxs (" 	", Memc[stname (stp, sym)]) > 0)
+		call fprintf (fd, "'%s'%30t")
+	    else
+		call fprintf (fd, "%s%30t")
+	    call pargstr (Memc[stname (stp, sym)])
+	    if (stridxs (" 	", NAME(sym)) > 0)
+		call fprintf (fd, " '%s'%10t")
+	    else
+		call fprintf (fd, " %s%10t")
+	    call pargstr (NAME(sym))
+	    if (DEFAULT(sym) != EOS) {
+		if (stridxs (" 	", DEFAULT(sym)) > 0)
+		    call fprintf (fd, " '%s'")
+		else
+		    call fprintf (fd, " %s")
+		call pargstr (DEFAULT(sym))
+	    }
+	    call fprintf (fd, "\n")
+	}
+
+	call close (fd)
+end
+
+
+# HDMNAME -- Return the image header parameter name
+
+procedure hdmname (parameter, str, max_char)
+
+char	parameter[ARB]		# Parameter name
+char	str[max_char]		# String containing mapped parameter name
+int	max_char		# Maximum characters in string
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call strcpy (NAME(sym), str, max_char)
+	else
+	    call strcpy (parameter, str, max_char)
+end
+
+
+# HDMPNAME -- Put the image header parameter name
+
+procedure hdmpname (parameter, str)
+
+char	parameter[ARB]		# Parameter name
+char	str[ARB]		# String containing mapped parameter name
+
+pointer	sym, stfind(), stenter()
+include	"hdrmap.com"
+
+begin
+	if (stp == NULL)
+	    return
+
+	sym = stfind (stp, parameter)
+	if (sym == NULL) {
+	    sym = stenter (stp, parameter, SYMLEN)
+	    DEFAULT(sym) = EOS
+	}
+
+	call strcpy (str, NAME(sym), SZ_NAME)
+end
+
+
+# HDMGDEF -- Get the default value as a string (null string if none).
+
+procedure hdmgdef (parameter, str, max_char)
+
+char	parameter[ARB]		# Parameter name
+char	str[max_char]		# String containing default value
+int	max_char		# Maximum characters in string
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call strcpy (DEFAULT(sym), str, max_char)
+	else
+	    str[1] = EOS
+end
+
+
+# HDMPDEF -- PUt the default value as a string.
+
+procedure hdmpdef (parameter, str)
+
+char	parameter[ARB]		# Parameter name
+char	str[ARB]		# String containing default value
+
+pointer	sym, stfind(), stenter()
+include	"hdrmap.com"
+
+begin
+	if (stp == NULL)
+	    return
+
+	sym = stfind (stp, parameter)
+	if (sym == NULL) {
+	    sym = stenter (stp, parameter, SYMLEN)
+	    call strcpy (parameter, NAME(sym), SZ_NAME)
+	}
+
+	call strcpy (str, DEFAULT(sym), SZ_DEFAULT)
+end
+
+
+# HDMACCF -- Return whether the image header parameter exists (regardless of
+# whether there is a default value).
+
+int procedure hdmaccf (im, parameter)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+
+int	imaccf()
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    return (imaccf (im, NAME(sym)))
+	else
+	    return (imaccf (im, parameter))
+end
+
+
+# HDMGSTR -- Get a string valued parameter.  Return default value if not in
+# the image header.  Return null string if no default or image value.
+
+procedure hdmgstr (im, parameter, str, max_char)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+char	str[max_char]		# String value to return
+int	max_char		# Maximum characters in returned string
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL) {
+	    iferr (call imgstr (im, NAME(sym), str, max_char))
+		call strcpy (DEFAULT(sym), str, max_char)
+	} else {
+	    iferr (call imgstr (im, parameter, str, max_char))
+		str[1] = EOS
+	}
+end
+
+
+# HDMGETR -- Get a real valued parameter.  Return default value if not in
+# the image header.  Return error condition if no default or image value.
+
+real procedure hdmgetr (im, parameter)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+
+int	ip, ctor()
+real	value, imgetr()
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL) {
+	    iferr (value = imgetr (im, NAME(sym))) {
+		ip = 1
+		if (ctor (DEFAULT(sym), ip, value) == 0)
+		    call error (0, "HDMGETR: No value found")
+	    }
+	} else
+	    value = imgetr (im, parameter)
+
+	return (value)
+end
+
+
+# HDMGETI -- Get an integer valued parameter.  Return default value if not in
+# the image header.  Return error condition if no default or image value.
+
+int procedure hdmgeti (im, parameter)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+
+int	ip, ctoi()
+int	value, imgeti()
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL) {
+	    iferr (value = imgeti (im, NAME(sym))) {
+		ip = 1
+		if (ctoi (DEFAULT(sym), ip, value) == 0)
+		    call error (0, "HDMGETI: No value found")
+	    }
+	} else
+	    value = imgeti (im, parameter)
+
+	return (value)
+end
+
+
+# HDMPSTR -- Put a string valued parameter in the image header.
+
+procedure hdmpstr (im, parameter, str)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+char	str[ARB]		# String value
+
+int	imaccf(), imgftype()
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL) {
+	    if (imaccf (im, NAME(sym)) == YES)
+	        if (imgftype (im, NAME(sym)) != TY_CHAR)
+		    call imdelf (im, NAME(sym))
+	    call imastr (im, NAME(sym), str)
+	} else {
+	    if (imaccf (im, parameter) == YES)
+	        if (imgftype (im, parameter) != TY_CHAR)
+		    call imdelf (im, parameter)
+	    call imastr (im, parameter, str)
+	}
+end
+
+
+# HDMPUTI -- Put an integer valued parameter in the image header.
+
+procedure hdmputi (im, parameter, value)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+int	value			# Integer value to put
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call imaddi (im, NAME(sym), value)
+	else
+	    call imaddi (im, parameter, value)
+end
+
+
+# HDMPUTR -- Put a real valued parameter in the image header.
+
+procedure hdmputr (im, parameter, value)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+real	value			# Real value to put
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call imaddr (im, NAME(sym), value)
+	else
+	    call imaddr (im, parameter, value)
+end
+
+
+# HDMGSTP -- Get the symbol table pointer to save a translation map.
+# The symbol table is restored with HDMPSTP.
+
+procedure hdmgstp (ptr)
+
+pointer	ptr		# Symbol table pointer to return
+
+include	"hdrmap.com"
+
+begin
+	ptr = stp
+end
+
+
+# HDMPSTP -- Put a symbol table pointer to restore a header map.
+# The symbol table is optained with HDMGSTP.
+
+procedure hdmpstp (ptr)
+
+pointer	ptr		# Symbol table pointer to restore
+
+include	"hdrmap.com"
+
+begin
+	stp = ptr
+end
+
+
+# HDMDELF -- Delete a field.  It is an error if the field does not exist.
+
+procedure hdmdelf (im, parameter)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call imdelf (im, NAME(sym))
+	else
+	    call imdelf (im, parameter)
+end
+
+
+# HDMPARAM -- Get parameter given the image header name.
+
+procedure hdmparam (name, parameter, max_char)
+
+char	name[ARB]		# Image header name
+char	parameter[max_char]	# Parameter
+int	max_char		# Maximum size of parameter string
+
+bool	streq()
+pointer	sym, sthead(), stname(), stnext()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = sthead (stp)
+	else
+	    sym = NULL
+
+	while (sym != NULL) {
+	    if (streq (NAME(sym), name)) {
+		call strcpy (Memc[stname(stp, sym)], parameter, max_char)
+		return
+	    }
+	    sym = stnext (stp, sym)
+	}
+	call strcpy (name, parameter, max_char)
+end
diff --git a/noao/imred/quadred/src/ccdproc/mkpkg b/noao/imred/quadred/src/ccdproc/mkpkg
new file mode 100644
index 00000000..7f263c15
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/mkpkg
@@ -0,0 +1,78 @@
+# Make QUADRED Package.
+
+$call	relink
+$exit
+
+update:
+        $call   relink
+        $call   install
+        ;
+
+relink:
+        $update libpkg.a
+        $call   quadred
+        ;
+
+install:
+        $move   xx_quadred.e noaobin$x_quadred.e
+        ;
+
+quadred:
+        $omake  x_quadred.x
+        $link   x_quadred.o libpkg.a -lxtools -lcurfit -lgsurfit -lncar -lgks\
+                -o xx_quadred.e
+        ;
+
+generic:
+	$set	GEN = "$$generic -k"
+
+        $ifolder (generic/ccdred.h, ccdred.h)
+	    $copy ccdred.h generic/ccdred.h $endif
+        $ifolder (generic/proc.x,  proc.gx)
+	    $(GEN) proc.gx -o generic/proc.x $endif
+        $ifolder (generic/cor.x,  cor.gx)
+	    $(GEN) cor.gx -o generic/cor.x $endif
+        $ifolder (generic/corinput.x,  corinput.gx)
+	    $(GEN) corinput.gx -o generic/corinput.x $endif
+	;
+
+libpkg.a:
+	$ifeq (USE_GENERIC, yes) $call generic $endif
+	@generic
+
+	calimage.x	ccdtypes.h <error.h> <imset.h>
+	ccdcache.x	ccdcache.com ccdcache.h <imhdr.h> <imset.h> <mach.h>\
+			ccdcache.com
+	ccdcheck.x	ccdtypes.h <imhdr.h>
+	ccdcmp.x	
+	ccddelete.x	
+	ccdflag.x	
+	ccdlog.x	<imhdr.h> <imset.h>
+	ccdmean.x	<imhdr.h>
+	ccdnscan.x	ccdtypes.h
+	ccdproc.x	ccdred.h ccdtypes.h <error.h>
+	ccdsection.x	<ctype.h>
+	ccdsubsets.x	
+	ccdtypes.x	ccdtypes.h
+	doproc.x	ccdred.h
+	hdrmap.x	hdrmap.com <error.h>
+	readcor.x	<imhdr.h>
+	scancor.x	<imhdr.h> <imset.h>
+	setdark.x	ccdred.h ccdtypes.h <imhdr.h>
+	setfixpix.x	ccdred.h <imhdr.h>
+	setflat.x	ccdred.h ccdtypes.h <imhdr.h>
+	setfringe.x	ccdred.h ccdtypes.h <imhdr.h>
+	setheader.x	ccdred.h <imhdr.h>
+	setillum.x	ccdred.h ccdtypes.h <imhdr.h>
+	setinput.x	ccdtypes.h <error.h>
+	setinteract.x	<pkg/xtanswer.h>
+	setoutput.x	<imhdr.h> <imset.h>
+	setoverscan.x	ccdred.h <imhdr.h> <imset.h> <pkg/xtanswer.h>\
+			<pkg/gtools.h>
+	setproc.x	ccdred.h <imhdr.h>
+	setsections.x	ccdred.h <imhdr.h>
+	settrim.x	ccdred.h <imhdr.h> <imset.h>
+	setzero.x	ccdred.h ccdtypes.h <imhdr.h>
+	t_ccdproc.x	ccdred.h ccdtypes.h <error.h> <imhdr.h>
+	timelog.x	<time.h>
+	;
diff --git a/noao/imred/quadred/src/ccdproc/proc.gx b/noao/imred/quadred/src/ccdproc/proc.gx
new file mode 100644
index 00000000..b6604179
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/proc.gx
@@ -0,0 +1,379 @@
+include	<imhdr.h>
+include	"ccdred.h"
+
+
+.help proc Feb87 noao.imred.ccdred
+.nf ----------------------------------------------------------------------------
+proc -- Process CCD images
+
+These are the main CCD reduction procedures.  There is one for each
+readout axis (lines or columns) and one for short and real image data.
+They apply corrections for bad pixels, overscan levels, zero levels,
+dark counts, flat field response, illumination response, and fringe
+effects.  The image is also trimmed if it was mapped with an image
+section.  The mean value for the output image is computed when the flat
+field or illumination image is processed to form the scale factor for
+these calibrations in order to avoid reading through these image a
+second time.
+
+The processing information and parameters are specified in the CCD
+structure. The processing operations to be performed are specified by
+the correction array CORS in the ccd structure.  There is one array
+element for each operation with indices defined symbolically by macro
+definitions (see ccdred.h); i.e.  FLATCOR.  The value of the array
+element is an integer bit field in which the bit set is the same as the
+array index; i.e element 3 will have the third bit set for an operation
+with array value 2**(3-1)=4.  If an operation is not to be performed
+the bit is not set and the array element has the numeric value zero.
+Note that the addition of several correction elements gives a unique
+bit field describing a combination of operations.  For efficiency the
+most common combinations are implemented as separate units.
+
+The CCD structure also contains the correction or calibration data
+consisting either pointers to data, IMIO pointers for the calibration
+images, and scale factors.
+
+The processing is performed line-by-line.  The procedure CORINPUT is
+called to get an input line.  This procedure trims and fixes bad pixels by
+interpolation.  The output line and lines from the various calibration
+images are read.  The image vectors as well as the overscan vector and
+the scale factors are passed to the procedure COR (which also
+dereferences the pointer data into simple arrays and variables).  That
+procedure does the actual corrections apart from bad pixel
+corrections.
+
+The final optional step is to add each corrected output line to form a
+mean.  This adds efficiency since the operation is done only if desired
+and the output image data is already in memory so there is no I/O
+penalty.
+
+SEE ALSO
+    ccdred.h, cor, fixpix, setfixpix, setoverscan, settrim,
+    setzero, setdark, setflat, setillum, setfringe
+.endhelp ----------------------------------------------------------------------
+
+
+$for (sr)
+# PROC1 -- Process CCD images with readout axis 1 (lines).
+
+procedure proc1$t (ccd)
+
+pointer	ccd		# CCD structure
+
+int	i, line, nlin, ncols, nlines, findmean, rep
+int	c1, c2, l1, l2
+real	overscan, darkscale, flatscale, illumscale, frgscale, mean
+PIXEL	minrep
+pointer	in, out, zeroim, darkim, flatim, illumim, fringeim
+pointer	outbuf, overscan_vec, zerobuf, darkbuf, flatbuf, illumbuf, fringebuf
+
+$if (datatype == csir)
+real	asum$t()
+$else $if (datatype == ld)
+double	asum$t()
+$else
+PIXEL	asum$t()
+$endif $endif
+pointer	imgl2$t(), impl2$t(), ccd_gl$t()
+
+begin
+	# Initialize.  If the correction image is 1D then just get the
+	# data once.
+
+	in = IN_IM(ccd)
+	out = OUT_IM(ccd)
+	nlin = IM_LEN(in,2)
+	ncols = OUT_C2(ccd) - OUT_C1(ccd) + 1
+	nlines = OUT_L2(ccd) - OUT_L1(ccd) + 1
+
+	if (CORS(ccd, FIXPIX) == YES)
+	    call lfixinit$t (in)
+
+	findmean = CORS(ccd, FINDMEAN)
+	if (findmean == YES)
+	    mean = 0.
+	rep = CORS(ccd, MINREP)
+	if (rep == YES)
+	    minrep = MINREPLACE(ccd)
+
+	overscan_vec = OVERSCAN_VEC(ccd)
+
+	if (CORS(ccd, ZEROCOR) == 0) {
+	    zeroim = NULL
+	    zerobuf = 1
+	} else if (IM_LEN(ZERO_IM(ccd),2) == 1) {
+	    zeroim = NULL
+	    zerobuf = ccd_gl$t (ZERO_IM(ccd), ZERO_C1(ccd), ZERO_C2(ccd), 1)
+	} else
+	    zeroim = ZERO_IM(ccd)
+
+	if (CORS(ccd, DARKCOR) == 0) {
+	    darkim = NULL
+	    darkbuf = 1
+	} else if (IM_LEN(DARK_IM(ccd),2) == 1) {
+	    darkim = NULL
+	    darkbuf = ccd_gl$t (DARK_IM(ccd), DARK_C1(ccd), DARK_C2(ccd), 1)
+	    darkscale = FLATSCALE(ccd)
+	} else {
+	    darkim = DARK_IM(ccd)
+	    darkscale = DARKSCALE(ccd)
+	}
+
+	if (CORS(ccd, FLATCOR) == 0) {
+	    flatim = NULL
+	    flatbuf = 1
+	} else if (IM_LEN(FLAT_IM(ccd),2) == 1) {
+	    flatim = NULL
+	    flatbuf = ccd_gl$t (FLAT_IM(ccd), FLAT_C1(ccd), FLAT_C2(ccd), 1)
+	    flatscale = FLATSCALE(ccd)
+	} else {
+	    flatim = FLAT_IM(ccd)
+	    flatscale = FLATSCALE(ccd)
+	}
+
+	if (CORS(ccd, ILLUMCOR) == 0) {
+	    illumim = NULL
+	    illumbuf = 1
+	} else {
+	    illumim = ILLUM_IM(ccd)
+	    illumscale = ILLUMSCALE(ccd)
+	}
+
+	if (CORS(ccd, FRINGECOR) == 0) {
+	    fringeim = NULL
+	    fringebuf = 1
+	} else {
+	    fringeim = FRINGE_IM(ccd)
+	    frgscale = FRINGESCALE(ccd)
+	}
+
+	# For each line read lines from the input.  Procedure CORINPUT
+	# replaces bad pixels by interpolation and applies a trim to the
+	# input.  Get lines from the output image and from the zero level,
+	# dark count, flat field, illumination, and fringe images.
+	# Call COR1 to do the actual pixel corrections.  Finally, add the
+	# output pixels to a sum for computing the mean.
+	# We must copy data outside of the output data section.
+
+	do line = 2 - OUT_L1(ccd), 0
+	    call amov$t (
+		Mem$t[imgl2$t(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mem$t[impl2$t(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	do line = 1, nlines {
+	    outbuf = impl2$t (out, OUT_L1(ccd)+line-1)
+	    call corinput$t (in, line, ccd, Mem$t[outbuf], IM_LEN(out,1))
+
+	    outbuf = outbuf + OUT_C1(ccd) - 1
+	    if (overscan_vec != NULL)
+		overscan = Memr[overscan_vec+line-1]
+	    if (zeroim != NULL)
+		zerobuf = ccd_gl$t (zeroim, ZERO_C1(ccd), ZERO_C2(ccd),
+		    ZERO_L1(ccd)+line-1)
+	    if (darkim != NULL)
+		darkbuf = ccd_gl$t (darkim, DARK_C1(ccd), DARK_C2(ccd),
+		    DARK_L1(ccd)+line-1)
+	    if (flatim != NULL)
+		flatbuf = ccd_gl$t (flatim, FLAT_C1(ccd), FLAT_C2(ccd),
+		    FLAT_L1(ccd)+line-1)
+	    if (illumim != NULL)
+		illumbuf = ccd_gl$t (illumim, ILLUM_C1(ccd), ILLUM_C2(ccd),
+		    ILLUM_L1(ccd)+line-1)
+	    if (fringeim != NULL)
+		fringebuf = ccd_gl$t (fringeim, FRINGE_C1(ccd), FRINGE_C2(ccd),
+		    FRINGE_L1(ccd)+line-1)
+
+	    if (OUT_SEC(ccd) == NULL) {
+		call cor1$t (CORS(ccd,1), Mem$t[outbuf],
+		    overscan, Mem$t[zerobuf], Mem$t[darkbuf],
+		    Mem$t[flatbuf], Mem$t[illumbuf], Mem$t[fringebuf], ncols,
+		    darkscale, flatscale, illumscale, frgscale)
+	    } else {
+		do i = 1, IN_NSEC(ccd) {
+		    l1 = OUT_SL1(ccd,i)
+		    l2 = OUT_SL2(ccd,i)
+		    if (line < l1 || line > l2)
+			next
+		    c1 = OUT_SC1(ccd,i) - 1
+		    c2 = OUT_SC2(ccd,i) - 1
+		    ncols = c2 - c1 + 1
+		    if (overscan_vec != NULL)
+			overscan = Memr[overscan_vec+(i-1)*nlin+line-l1]
+		    
+		    call cor1$t (CORS(ccd,1), Mem$t[outbuf+c1],
+			overscan, Mem$t[zerobuf+c1], Mem$t[darkbuf+c1],
+			Mem$t[flatbuf+c1], Mem$t[illumbuf+c1],
+			Mem$t[fringebuf+c1], ncols,
+			darkscale, flatscale, illumscale, frgscale)
+		}
+	    }
+
+	    if (rep == YES)
+		call amaxk$t (Mem$t[outbuf], minrep, Mem$t[outbuf], ncols)
+	    if (findmean == YES)
+		mean = mean + asum$t (Mem$t[outbuf], ncols)
+	}
+
+	do line = nlines+1, IM_LEN(out,2)-OUT_L1(ccd)+1
+	    call amov$t (
+		Mem$t[imgl2$t(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mem$t[impl2$t(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	# Compute the mean from the sum of the output pixels.
+	if (findmean == YES)
+	    MEAN(ccd) = mean / ncols / nlines
+
+	if (CORS(ccd, FIXPIX) == YES)
+	    call lfixfree$t ()
+end
+
+
+# PROC2 -- Process CCD images with readout axis 2 (columns).
+
+procedure proc2$t (ccd)
+
+pointer	ccd		# CCD structure
+
+int	line, ncols, nlines, findmean, rep
+real	darkscale, flatscale, illumscale, frgscale, mean
+PIXEL	minrep
+pointer	in, out, zeroim, darkim, flatim, illumim, fringeim
+pointer	outbuf, overscan_vec, zerobuf, darkbuf, flatbuf, illumbuf, fringebuf
+
+$if (datatype == csir)
+real	asum$t()
+$else $if (datatype == ld)
+double	asum$t()
+$else
+PIXEL	asum$t()
+$endif $endif
+pointer	imgl2$t(), impl2$t(), imgs2$t(), ccd_gl$t()
+
+begin
+	# Initialize.  If the correction image is 1D then just get the
+	# data once.
+
+	in = IN_IM(ccd)
+	out = OUT_IM(ccd)
+	ncols = OUT_C2(ccd) - OUT_C1(ccd) + 1
+	nlines = OUT_L2(ccd) - OUT_L1(ccd) + 1
+
+	if (CORS(ccd, FIXPIX) == YES)
+	    call lfixinit$t (in)
+
+	findmean = CORS(ccd, FINDMEAN)
+	if (findmean == YES)
+	    mean = 0.
+	rep = CORS(ccd, MINREP)
+	if (rep == YES)
+	    minrep = MINREPLACE(ccd)
+
+	overscan_vec = OVERSCAN_VEC(ccd)
+
+	if (CORS(ccd, ZEROCOR) == 0) {
+	    zeroim = NULL
+	    zerobuf = 1
+	} else if (IM_LEN(ZERO_IM(ccd),1) == 1) {
+	    zeroim = NULL
+	    zerobuf = imgs2$t (ZERO_IM(ccd), 1, 1, ZERO_L1(ccd), ZERO_L2(ccd))
+	} else
+	    zeroim = ZERO_IM(ccd)
+
+	if (CORS(ccd, DARKCOR) == 0) {
+	    darkim = NULL
+	    darkbuf = 1
+	} else if (IM_LEN(DARK_IM(ccd),1) == 1) {
+	    darkim = NULL
+	    darkbuf = imgs2$t (DARK_IM(ccd), 1, 1, DARK_L1(ccd), DARK_L2(ccd))
+	    darkscale = DARKSCALE(ccd)
+	} else {
+	    darkim = DARK_IM(ccd)
+	    darkscale = DARKSCALE(ccd)
+	}
+
+	if (CORS(ccd, FLATCOR) == 0) {
+	    flatim = NULL
+	    flatbuf = 1
+	} else if (IM_LEN(FLAT_IM(ccd),1) == 1) {
+	    flatim = NULL
+	    flatbuf = imgs2$t (FLAT_IM(ccd), 1, 1, FLAT_L1(ccd), FLAT_L2(ccd))
+	    flatscale = FLATSCALE(ccd)
+	} else {
+	    flatim = FLAT_IM(ccd)
+	    flatscale = FLATSCALE(ccd)
+	}
+
+	if (CORS(ccd, ILLUMCOR) == 0) {
+	    illumim = NULL
+	    illumbuf = 1
+	} else {
+	    illumim = ILLUM_IM(ccd)
+	    illumscale = ILLUMSCALE(ccd)
+	}
+
+	if (CORS(ccd, FRINGECOR) == 0) {
+	    fringeim = NULL
+	    fringebuf = 1
+	} else {
+	    fringeim = FRINGE_IM(ccd)
+	    frgscale = FRINGESCALE(ccd)
+	}
+
+	# For each line read lines from the input.  Procedure CORINPUT
+	# replaces bad pixels by interpolation and applies a trim to the
+	# input.  Get lines from the output image and from the zero level,
+	# dark count, flat field, illumination, and fringe images.
+	# Call COR2 to do the actual pixel corrections.  Finally, add the
+	# output pixels to a sum for computing the mean.
+	# We must copy data outside of the output data section.
+
+	do line = 2 - OUT_L1(ccd), 0
+	    call amov$t (
+		Mem$t[imgl2$t(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mem$t[impl2$t(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	do line = 1, nlines {
+	    outbuf = impl2$t (out, OUT_L1(ccd)+line-1)
+	    call corinput$t (in, line, ccd, Mem$t[outbuf], IM_LEN(out,1))
+
+	    outbuf = outbuf + OUT_C1(ccd) - 1
+	    if (zeroim != NULL)
+		zerobuf = ccd_gl$t (zeroim, ZERO_C1(ccd), ZERO_C2(ccd),
+		    ZERO_L1(ccd)+line-1)
+	    if (darkim != NULL)
+		darkbuf = ccd_gl$t (darkim, DARK_C1(ccd), DARK_C2(ccd),
+		    DARK_L1(ccd)+line-1)
+	    if (flatim != NULL)
+		flatbuf = ccd_gl$t (flatim, FLAT_C1(ccd), FLAT_C2(ccd),
+		    FLAT_L1(ccd)+line-1)
+	    if (illumim != NULL)
+		illumbuf = ccd_gl$t (illumim, ILLUM_C1(ccd), ILLUM_C2(ccd),
+		    ILLUM_L1(ccd)+line-1)
+	    if (fringeim != NULL)
+		fringebuf = ccd_gl$t (fringeim, FRINGE_C1(ccd), FRINGE_C2(ccd),
+		    FRINGE_L1(ccd)+line-1)
+
+	    call cor2$t (line, CORS(ccd,1), Mem$t[outbuf],
+		Memr[overscan_vec], Mem$t[zerobuf], Mem$t[darkbuf],
+		Mem$t[flatbuf], Mem$t[illumbuf], Mem$t[fringebuf], ncols,
+		zeroim, flatim, darkscale, flatscale, illumscale, frgscale)
+
+	    if (rep == YES)
+		call amaxk$t (Mem$t[outbuf], minrep, Mem$t[outbuf], ncols)
+	    if (findmean == YES)
+		mean = mean + asum$t (Mem$t[outbuf], ncols)
+	}
+
+	do line = nlines+1, IM_LEN(out,2)-OUT_L1(ccd)+1
+	    call amov$t (
+		Mem$t[imgl2$t(in,IN_L1(ccd)+line-1)+IN_C1(ccd)-OUT_C1(ccd)],
+		Mem$t[impl2$t(out,OUT_L1(ccd)+line-1)], IM_LEN(out,1))
+
+	# Compute the mean from the sum of the output pixels.
+	if (findmean == YES)
+	    MEAN(ccd) = mean / ncols / nlines
+
+	if (CORS(ccd, FIXPIX) == YES)
+	    call lfixfree$t ()
+end
+$endfor
diff --git a/noao/imred/quadred/src/ccdproc/readcor.x b/noao/imred/quadred/src/ccdproc/readcor.x
new file mode 100644
index 00000000..61fbd836
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/readcor.x
@@ -0,0 +1,138 @@
+include	<imhdr.h>
+
+# READCOR -- Create a readout image.
+# Assume it is appropriate to perform this operation on the input image.
+# There is no CCD type checking.
+
+procedure readcor (input)
+
+char	input[ARB]		# Input image
+int	readaxis		# Readout axis
+
+int	i, nc, nl, c1, c2, cs, l1, l2, ls
+int	in_c1, in_c2, in_l1, in_l2, ccd_c1, ccd_c2, ccd_l1, ccd_l2
+pointer	sp, output, str, in, out, data
+
+real	asumr()
+int	clgwrd()
+bool	clgetb(), ccdflag()
+pointer	immap(), imgl2r(), impl2r(), imps2r()
+errchk	immap, ccddelete
+
+begin
+	# Check if this operation is desired.
+	if (!clgetb ("readcor"))
+	    return
+
+	# Check if this operation has been done.  Unfortunately this requires
+	# mapping the image.
+
+	in = immap (input, READ_ONLY, 0)
+	if (ccdflag (in, "readcor")) {
+	    call imunmap (in)
+	    return
+	}
+
+	if (clgetb ("noproc")) {
+	    call eprintf (
+		"  [TO BE DONE] Convert %s to readout correction\n")
+		call pargstr (input)
+	    call imunmap (in)
+	    return
+	}
+
+	call smark (sp)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# The default data section is the entire image.
+	nc = IM_LEN(in,1)
+	nl = IM_LEN(in,2)
+	c1 = 1
+	c2 = nc
+	cs = 1
+	l1 = 1
+	l2 = nl
+	ls = 1
+	call hdmgstr (in, "datasec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1))
+	    call error (0, "Error in DATASEC parameter")
+	in_c1 = c1
+	in_c2 = c2
+	in_l1 = l1
+	in_l2 = l2
+
+	# The default ccd section is the data section.
+	call hdmgstr (in, "ccdsec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((cs != 1) || (ls != 1))
+	    call error (0, "Error in CCDSEC parameter")
+	ccd_c1 = c1
+	ccd_c2 = c2
+	ccd_l1 = l1
+	ccd_l2 = l2
+	if ((in_c2-in_c1 != ccd_c2-ccd_c1) || (in_l2-in_l1 != ccd_l2-ccd_l1))
+	    call error (0, "Size of DATASEC and CCDSEC do not agree")
+
+	# Determine the readout axis.
+	readaxis = clgwrd ("readaxis", Memc[str], SZ_LINE, "|lines|columns|")
+
+	# Create output.
+	call mktemp ("tmp", Memc[output], SZ_FNAME)
+	call set_output (in, out, Memc[output])
+
+	# Average across the readout axis.
+	switch (readaxis) {
+	case 1:
+	    IM_LEN(out,2) = 1
+	    data = impl2r (out, 1)
+	    call aclrr (Memr[data], nc)
+	    nc = in_c2 - in_c1 + 1
+	    nl = in_l2 - in_l1 + 1
+	    data = data + in_c1 - 1
+	    do i = in_l1, in_l2
+		call aaddr (Memr[imgl2r(in,i)+in_c1-1], Memr[data],
+		    Memr[data], nc)
+	    call adivkr (Memr[data], real (nl), Memr[data], nc)
+	    call sprintf (Memc[str], SZ_LINE, "[%d:%d,1:1]")
+		call pargi (in_c1)
+		call pargi (in_c2)
+	    call hdmpstr (out, "datasec", Memc[str])
+	    call sprintf (Memc[str], SZ_LINE, "[%d:%d,*]")
+		call pargi (ccd_c1)
+		call pargi (ccd_c2)
+	    call hdmpstr (out, "ccdsec", Memc[str])
+	case 2:
+	    IM_LEN(out,1) = 1
+	    data = imps2r (out, 1, 1, 1, nl)
+	    call aclrr (Memr[data], nl)
+	    nc = in_c2 - in_c1 + 1
+	    nl = in_l2 - in_l1 + 1
+	    do i = in_l1, in_l2
+		Memr[data+i-1] = asumr (Memr[imgl2r(in,i)+in_c1-1], nc) / nc
+	    call sprintf (Memc[str], SZ_LINE, "[1:1,%d:%d]")
+		call pargi (in_l1)
+		call pargi (in_l2)
+	    call hdmpstr (out, "datasec", Memc[str])
+	    call sprintf (Memc[str], SZ_LINE, "[*,%d:%d]")
+		call pargi (ccd_l1)
+		call pargi (ccd_l2)
+	    call hdmpstr (out, "ccdsec", Memc[str])
+	}
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE,
+	    "Converted to readout format")
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (in, Memc[str])
+	call hdmpstr (out, "readcor", Memc[str])
+
+	# Replace the input image by the output image.
+	call imunmap (in)
+	call imunmap (out)
+	call ccddelete (input)
+	call imrename (Memc[output], input)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/scancor.x b/noao/imred/quadred/src/ccdproc/scancor.x
new file mode 100644
index 00000000..6a5eb84c
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/scancor.x
@@ -0,0 +1,340 @@
+include	<imhdr.h>
+include	<imset.h>
+
+define	SCANTYPES	"|shortscan|longscan|"
+define	SHORTSCAN	1	# Short scan accumulation, normal readout
+define	LONGSCAN	2	# Long scan continuous readout
+
+# SCANCOR -- Create a scanned image from an unscanned image.
+
+procedure scancor (input, output, nscan, minreplace)
+
+char	input[ARB]		# Input image
+char	output[ARB]		# Output image (must be new image)
+int	nscan			# Number of scan lines
+real	minreplace		# Minmum value of output
+
+int	scantype		# Type of scan format
+int	readaxis		# Readout axis
+
+int	clgwrd()
+pointer	sp, str, in, out, immap()
+errchk	immap
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Determine readout axis and create the temporary output image.
+	scantype = clgwrd ("scantype", Memc[str], SZ_LINE, SCANTYPES)
+	readaxis = clgwrd ("readaxis", Memc[str], SZ_LINE, "|lines|columns|")
+
+	# Make the output scanned image.
+	in = immap (input, READ_ONLY, 0)
+	call set_output (in, out, output)
+
+	switch (scantype) {
+	case SHORTSCAN:
+	    call shortscan (in, out, nscan, minreplace, readaxis)
+	case LONGSCAN:
+	    call longscan (in, out, readaxis)
+	}
+		
+	# Log the operation.
+	switch (scantype) {
+	case SHORTSCAN:
+	    call sprintf (Memc[str], SZ_LINE,
+		"Converted to shortscan from %s with nscan=%d")
+	    call pargstr (input)
+	    call pargi (nscan)
+	    call hdmputi (out, "nscanrow", nscan)
+	case LONGSCAN:
+	    call sprintf (Memc[str], SZ_LINE, "Converted to longscan from %s")
+	    call pargstr (input)
+	}
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (out, Memc[str])
+	call hdmpstr (out, "scancor", Memc[str])
+
+	call imunmap (in)
+	call imunmap (out)
+
+	call sfree (sp)
+end
+
+
+# SHORTSCAN -- Make a shortscan mode image by using a moving average.
+#
+# NOTE!! The value of nscan used here is increased by 1 because the
+# current information in the image header is actually the number of
+# scan steps and NOT the number of rows.
+
+procedure shortscan (in, out, nscan, minreplace, readaxis)
+
+pointer	in		# Input image
+pointer	out		# Output image
+int	nscan		# Number of lines scanned before readout
+real	minreplace	# Minimum output value
+int	readaxis	# Readout axis
+
+bool	replace
+real	nscanr, sum, mean, asumr()
+int	i, j, k, l, len1, len2, nc, nl, nscani, c1, c2, cs, l1, l2, ls
+pointer	sp, str, bufs, datain, dataout, data, imgl2r(), impl2r()
+long	clktime()
+errchk	malloc, calloc
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# The default data section is the entire image.
+	len1 = IM_LEN(in,1)
+	len2 = IM_LEN(in,2)
+	c1 = 1
+	c2 = len1
+	cs = 1
+	l1 = 1
+	l2 = len2
+	ls = 1
+	call hdmgstr (in, "datasec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>len1)||(l1<1)||(l2>len2)||(cs!=1)||(ls!=1))
+	    call error (0, "Error in DATASEC parameter")
+	nc = c2 - c1 + 1
+	nl = l2 - l1 + 1
+
+	# Copy initial lines.
+	do i = 1, l1 - 1
+	    call amovr (Memr[imgl2r(in,i)], Memr[impl2r(out,i)], len1)
+
+	replace = !IS_INDEF(minreplace)
+	mean = 0.
+	switch (readaxis) {
+	case 1:
+	    nscani = max (1, min (nscan, nl) + 1)
+	    nscanr = nscani
+	    call imseti (in, IM_NBUFS, nscani)
+	    call malloc (bufs, nscani, TY_INT)
+	    call calloc (data, nc, TY_REAL)
+	    j = 1
+	    k = 1
+	    l = 1
+
+	    # Ramp up
+	    while (j <= nscani) {
+		i = j + l1 - 1
+		datain = imgl2r (in, i)
+		if (nc < len1)
+		    call amovr (Memr[datain], Memr[impl2r(out,i)], len1)
+		datain = datain + c1 - 1
+		Memi[bufs+mod(j,nscani)] = datain
+	        call aaddr (Memr[data], Memr[datain], Memr[data], nc)
+	        j = j + 1
+	    }
+	    dataout = impl2r (out, l+l1-1) + c1 - 1
+	    call adivkr (Memr[data], nscanr, Memr[dataout], nc)
+	    if (replace)
+		call amaxkr (Memr[dataout], minreplace, Memr[dataout], nc)
+	    mean = mean + asumr (Memr[dataout], nc)
+	    l = l + 1
+
+	    # Moving average
+	    while (j <= nl) {
+		datain = Memi[bufs+mod(k,nscani)]
+	        call asubr (Memr[data], Memr[datain], Memr[data], nc)
+		i = j + l1 - 1
+		datain = imgl2r (in, i)
+		if (nc < len1)
+		    call amovr (Memr[datain], Memr[impl2r(out,i)], len1)
+		datain = datain + c1 - 1
+		Memi[bufs+mod(j,nscani)] = datain
+	        call aaddr (Memr[data], Memr[datain], Memr[data], nc)
+		dataout = impl2r (out, l+l1-1) + c1 - 1
+		call adivkr (Memr[data], nscanr, Memr[dataout], nc)
+		if (replace)
+		    call amaxkr (Memr[dataout], minreplace, Memr[dataout], nc)
+		mean = mean + asumr (Memr[dataout], nc)
+
+	        j = j + 1
+	        k = k + 1
+	        l = l + 1
+	    }
+
+	    # Ramp down.
+	    while (l <= nl) {
+		datain = Memi[bufs+mod(k,nscani)]
+	        call asubr (Memr[data], Memr[datain], Memr[data], nc)
+		dataout = impl2r (out, l+l1-1) + c1 - 1
+		call adivkr (Memr[data], nscanr, Memr[dataout], nc)
+		if (replace)
+		    call amaxkr (Memr[dataout], minreplace, Memr[dataout], nc)
+		mean = mean + asumr (Memr[dataout], nc)
+
+	        k = k + 1
+	        l = l + 1
+	    }
+
+	    call mfree (bufs, TY_INT)
+	    call mfree (data, TY_REAL)
+
+	case 2:
+	    nscani = max (1, min (nscan, nc) + 1)
+	    nscanr = nscani
+	    do i = 1, nl {
+	        datain = imgl2r (in, i + l1 - 1)
+		datain = datain + c1 - 1
+	        data = impl2r (out, i + l1 - 1)
+		call amovr (Memr[datain], Memr[data], len1)
+		datain = datain + c1 - 1
+		data = data + c1 - 1
+		sum = 0
+		j = 0
+		k = 0
+		l = 0
+
+		# Ramp up
+		while (j < nscani) {
+		    sum = sum + Memr[datain+j]
+		    j = j + 1
+		}
+		if (replace)
+		    Memr[data] = max (minreplace, sum / nscani)
+		else
+		    Memr[data] = sum / nscani
+		mean = mean + Memr[data]
+		l = l + 1
+
+		# Moving average
+		while (j < nl) {
+		    sum = sum + Memr[datain+j] - Memr[datain+k]
+		    if (replace)
+			Memr[data+l] = max (minreplace, sum / nscani)
+		    else
+			Memr[data+l] = sum / nscani
+		    mean = mean + Memr[data+l]
+		    j = j + 1
+		    k = k + 1
+		    l = l + 1
+		}
+
+		# Ramp down
+		while (l < nl) {
+		    sum = sum - Memr[datain+k]
+		    if (replace)
+			Memr[data+l] = max (minreplace, sum / nscani)
+		    else
+			Memr[data+l] = sum / nscani
+		    mean = mean + Memr[data+l]
+		    k = k + 1
+		    l = l + 1
+		}
+	    }
+	}
+
+	# Copy final lines.
+	do i = l2+1, len2
+	    call amovr (Memr[imgl2r(in,i)], Memr[impl2r(out,i)], len1)
+
+	mean = mean / nc / nl
+	call hdmputr (out, "ccdmean", mean)
+	call hdmputi (out, "ccdmeant", int (clktime (long (0))))
+
+	call sfree (sp)
+end
+
+
+# LONGSCAN -- Make a longscan mode readout flat field correction by averaging
+# across the readout axis.
+
+procedure longscan (in, out, readaxis)
+
+pointer	in		# Input image
+pointer	out		# Output image
+int	readaxis	# Readout axis
+
+int	i, nc, nl, c1, c2, cs, l1, l2, ls
+int	in_c1, in_c2, in_l1, in_l2, ccd_c1, ccd_c2, ccd_l1, ccd_l2
+real	mean, asumr()
+long	clktime()
+pointer	sp, str, data, imgl2r(), impl2r(), imps2r()
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# The default data section is the entire image.
+	nc = IM_LEN(in,1)
+	nl = IM_LEN(in,2)
+	c1 = 1
+	c2 = nc
+	cs = 1
+	l1 = 1
+	l2 = nl
+	ls = 1
+	call hdmgstr (in, "datasec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1))
+	    call error (0, "Error in DATASEC parameter")
+	in_c1 = c1
+	in_c2 = c2
+	in_l1 = l1
+	in_l2 = l2
+
+	# The default ccd section is the data section.
+	call hdmgstr (in, "ccdsec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((cs != 1) || (ls != 1))
+	    call error (0, "Error in CCDSEC parameter")
+	ccd_c1 = c1
+	ccd_c2 = c2
+	ccd_l1 = l1
+	ccd_l2 = l2
+	if ((in_c2-in_c1 != ccd_c2-ccd_c1) || (in_l2-in_l1 != ccd_l2-ccd_l1))
+	    call error (0, "Size of DATASEC and CCDSEC do not agree")
+
+	switch (readaxis) {
+	case 1:
+	    IM_LEN(out,2) = 1
+	    data = impl2r (out, 1)
+	    call aclrr (Memr[data], nc)
+	    nc = in_c2 - in_c1 + 1
+	    nl = in_l2 - in_l1 + 1
+	    data = data + in_c1 - 1
+	    do i = in_l1, in_l2
+		call aaddr (Memr[imgl2r(in,i)+in_c1-1], Memr[data],
+		    Memr[data], nc)
+	    call adivkr (Memr[data], real (nl), Memr[data], nc)
+	    call sprintf (Memc[str], SZ_LINE, "[%d:%d,1:1]")
+		call pargi (in_c1)
+		call pargi (in_c2)
+	    call hdmpstr (out, "datasec", Memc[str])
+	    call sprintf (Memc[str], SZ_LINE, "[%d:%d,*]")
+		call pargi (ccd_c1)
+		call pargi (ccd_c2)
+	    call hdmpstr (out, "ccdsec", Memc[str])
+	    mean = asumr (Memr[data], nc) / nl
+	case 2:
+	    IM_LEN(out,1) = 1
+	    data = imps2r (out, 1, 1, 1, nl)
+	    call aclrr (Memr[data], nl)
+	    nc = in_c2 - in_c1 + 1
+	    nl = in_l2 - in_l1 + 1
+	    do i = in_l1, in_l2
+		Memr[data+i-1] = asumr (Memr[imgl2r(in,i)+in_c1-1], nc) / nc
+	    call sprintf (Memc[str], SZ_LINE, "[1:1,%d:%d]")
+		call pargi (in_l1)
+		call pargi (in_l2)
+	    call hdmpstr (out, "datasec", Memc[str])
+	    call sprintf (Memc[str], SZ_LINE, "[*,%d:%d]")
+		call pargi (ccd_l1)
+		call pargi (ccd_l2)
+	    call hdmpstr (out, "ccdsec", Memc[str])
+	    mean = asumr (Memr[data], nl) / nc
+	}
+
+	call hdmputr (out, "ccdmean", mean)
+	call hdmputi (out, "ccdmeant", int (clktime (long (0))))
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/setdark.x b/noao/imred/quadred/src/ccdproc/setdark.x
new file mode 100644
index 00000000..bf3c7354
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setdark.x
@@ -0,0 +1,155 @@
+include	<imhdr.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+
+# SET_DARK -- Set parameters for dark count correction.
+#
+#   1.  Return immediately if the dark count correction is not requested or
+#	if the image has been previously corrected.
+#   2.  Get the dark count correction image and return an error if not found.
+#   3.  If the dark count image has not been processed call PROC.
+#   4.  Compute the dark count integration time scale factor.
+#   5.  Set the processing flags.
+#   6.  Log the operation (to user, logfile, and output image header).
+
+procedure set_dark (ccd)
+
+pointer	ccd			# CCD structure
+
+int	nscan, nc, nl, c1, c2, cs, l1, l2, ls, data_c1, ccd_c1, data_l1, ccd_l1
+real	darktime1, darktime2
+pointer	sp, image, str, im
+
+bool	clgetb(), ccdflag(), ccdcheck()
+int	ccdnscan(), ccdtypei()
+real	hdmgetr()
+pointer	ccd_cache()
+errchk	cal_image, ccd_cache, ccdproc, hdmgetr
+
+begin
+	# Check if the user wants this operation or it has already been done.
+	if (!clgetb ("darkcor") || ccdflag (IN_IM(ccd), "darkcor"))
+	    return
+
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the dark count correction image name.
+	if (clgetb ("scancor"))
+	    nscan = ccdnscan (IN_IM(ccd), ccdtypei(IN_IM(ccd)))
+	else
+	    nscan = 1
+	call cal_image (IN_IM(ccd), DARK, nscan, Memc[image], SZ_FNAME)
+
+	# If no processing is desired print dark count image and return.
+	if (clgetb ("noproc")) {
+	    call eprintf ("  [TO BE DONE] Dark count correction image is %s.\n")
+	        call pargstr (Memc[image])
+	    call sfree (sp)
+	    return
+	}
+
+	# Map the image and return on an error.
+	# Process the dark count image if necessary.
+	# If nscan > 1 then the dark may not yet exist so create it
+	# from the unscanned dark.
+
+	iferr (im = ccd_cache (Memc[image], DARK)) {
+	    call cal_image (IN_IM(ccd), DARK, 1, Memc[str], SZ_LINE)
+	    im = ccd_cache (Memc[str], DARK)
+	    if (ccdcheck (im, DARK)) {
+		call ccd_flush (im)
+		call ccdproc (Memc[str], DARK)
+	    }
+	    call scancor (Memc[str], Memc[image], nscan, INDEF)
+	    im = ccd_cache (Memc[image], DARK)
+	}
+
+	if (ccdcheck (im, DARK)) {
+	    call ccd_flush (im)
+	    call ccdproc (Memc[image], DARK)
+	    im = ccd_cache (Memc[image], DARK)
+	}
+
+	# Set the processing parameters in the CCD structure.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	c1 = 1
+	c2 = nc
+	l1 = 1
+	l2 = nl
+	cs = 1
+	ls = 1
+	call hdmgstr (im, "datasec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1)) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Data section error: image=%s[%d,%d], datasec=[%d:%d,%d:%d]")
+		call pargstr (Memc[image])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+	data_c1 = c1
+	data_l1 = l1
+	call hdmgstr (im, "ccdsec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if (nc == 1) {
+	    c1 = CCD_C1(ccd)
+	    c2 = CCD_C2(ccd)
+	}
+	if (nl == 1) {
+	    l1 = CCD_L1(ccd)
+	    l2 = CCD_L2(ccd)
+	}
+	ccd_c1 = c1
+	ccd_l1 = l1
+	if ((c1 > CCD_C1(ccd)) || (c2 < CCD_C2(ccd)) ||
+	    (l1 > CCD_L1(ccd)) || (l2 < CCD_L2(ccd))) {
+	    call sprintf (Memc[str], SZ_LINE,
+	        "CCD section error: input=[%d:%d,%d:%d], %s=[%d:%d,%d:%d]")
+		call pargi (CCD_C1(ccd))
+		call pargi (CCD_C2(ccd))
+		call pargi (CCD_L1(ccd))
+		call pargi (CCD_L2(ccd))
+		call pargstr (Memc[image])
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+
+	DARK_IM(ccd) = im
+	DARK_C1(ccd) = CCD_C1(ccd) - ccd_c1 + data_c1
+	DARK_C2(ccd) = CCD_C2(ccd) - ccd_c1 + data_c1
+	DARK_L1(ccd) = CCD_L1(ccd) - ccd_l1 + data_l1
+	DARK_L2(ccd) = CCD_L2(ccd) - ccd_l1 + data_l1
+
+	# Get the dark count integration times.  Return an error if not found.
+	iferr (darktime1 = hdmgetr (IN_IM(ccd), "darktime"))
+	    darktime1 = hdmgetr (IN_IM(ccd), "exptime")
+	iferr (darktime2 = hdmgetr (im, "darktime"))
+	    darktime2 = hdmgetr (im, "exptime")
+
+	DARKSCALE(ccd) = darktime1 / darktime2
+	CORS(ccd, DARKCOR) = D
+	COR(ccd) = YES
+
+	# Record the operation in the output image and write a log record.
+	call sprintf (Memc[str], SZ_LINE,
+	    "Dark count correction image is %s with scale=%g")
+	    call pargstr (Memc[image])
+	    call pargr (DARKSCALE(ccd))
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "darkcor", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/setfixpix.x b/noao/imred/quadred/src/ccdproc/setfixpix.x
new file mode 100644
index 00000000..05866bed
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setfixpix.x
@@ -0,0 +1,181 @@
+include	<imhdr.h>
+include	"ccdred.h"
+
+# SET_FIXPIX -- Setup for fixing bad pixels.
+#
+#   1.  Return immediately if the bad pixel correction is not requested or
+#	if the image has been previously corrected.
+#   2.  Determine the bad pixel correction file.  This may be specified
+#	directly or indirectly through the image header or symbol table.
+#	Return warning if not found.
+#   3.  Read through the file collecting the bad pixel regions into a
+#       bad column array (regions to be interpolated across columns) and
+#	a bad line array (regions to be interpolated across lines).
+#   4.  Set the processing flag.
+#   5.  Log the operation (to user, logfile, and output image header).
+
+procedure set_fixpix (ccd)
+
+pointer	ccd			# CCD structure
+
+int	fd, nc, nl, c1, c2, l1, l2, dc, dl, nbadcols, nbadlines
+pointer	sp, image, str, badcols, badlines
+
+int	open(), fscan(), nscan(), strmatch()
+bool	clgetb(), streq(), ccdflag()
+errchk	open
+
+begin
+	# Check if the user wants this operation or it has been done.
+	if (!clgetb ("fixpix") || ccdflag (IN_IM(ccd), "fixpix"))
+	    return
+
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the bad pixel file.  If the name is "image" then get the file
+	# name from the image header or symbol table.
+
+	call clgstr ("fixfile", Memc[image], SZ_FNAME)
+	if (streq (Memc[image], "image"))
+	    call hdmgstr (IN_IM(ccd), "fixfile", Memc[image], SZ_FNAME)
+
+	# If no processing is desired print message and return.
+	if (clgetb ("noproc")) {
+	    call eprintf ("  [TO BE DONE] Bad pixel file is %s\n")
+		call pargstr (Memc[image])
+	    call sfree (sp)
+	    return
+	}
+
+	# Open the file and read the bad pixel regions.  Use dynamic memory.
+	# Set the bad pixel coordinates.  By default the bad pixel coordinates
+	# refer to the image directly but if the word "untrimmed" appears
+	# in a comment then the coordinates refer to the CCD coordinates.
+
+	fd = open (Memc[image], READ_ONLY, TEXT_FILE)
+	dc = 0
+	dl = 0
+	nc = IM_LEN(IN_IM(ccd),1)
+	nl = IM_LEN(IN_IM(ccd),2)
+	nbadcols = 0
+	nbadlines = 0
+	while (fscan (fd) != EOF) {
+	    call gargwrd (Memc[str], SZ_LINE)
+	    if (Memc[str] == '#') {
+		call gargstr (Memc[str], SZ_LINE)
+		if (strmatch (Memc[str], "{untrimmed}") != 0) {
+		    dc = IN_C1(ccd) - CCD_C1(ccd)
+		    dl = IN_L1(ccd) - CCD_L1(ccd)
+		}
+	        next
+	    }
+		    
+	    call reset_scan()
+	    call gargi (c1)
+	    call gargi (c2)
+	    call gargi (l1)
+	    call gargi (l2)
+
+	    # Ignore badly specified lines.
+	    if (nscan() != 4) {
+		if (nscan() == 2) {
+		    l1 = c2
+		    c2 = c1
+		    l2 = l1
+		} else
+		    next
+	    }
+
+	    # Do the coordinate conversion.
+	    c1 = max (IN_C1(ccd), c1 + dc)
+	    c2 = min (IN_C2(ccd), c2 + dc)
+	    l1 = max (IN_L1(ccd), l1 + dl)
+	    l2 = min (IN_L2(ccd), l2 + dl)
+
+	    # Ignore an inproperly specified region.
+	    if ((c1 > c2) || (l1 > l2))
+		next
+
+	    # Interpolate across the shortest direction.
+	    if ((l2 - l1) < (c2 - c1)) {
+		nbadlines = nbadlines + 1
+		if (nbadlines == 1)
+		    call calloc (badlines, 2*nl*nbadlines, TY_SHORT)
+		else {
+		    call realloc (badlines, 2*nl*nbadlines, TY_SHORT)
+		    call aclrs (Mems[badlines+2*nl*(nbadlines-1)], 2*nl)
+		}
+		call set_badcols (c1, c2, l1, l2, Mems[badlines],
+		    nl, nbadlines)
+
+	    } else {
+		nbadcols = nbadcols + 1
+		if (nbadcols == 1)
+		    call calloc (badcols, 2*nl*nbadcols, TY_SHORT)
+		else {
+		    call realloc (badcols, 2*nl*nbadcols, TY_SHORT)
+		    call aclrs (Mems[badcols+2*nl*(nbadcols-1)], 2*nl)
+		}
+		call set_badcols (c1, c2, l1, l2, Mems[badcols],
+		    nl, nbadcols)
+	    }
+	}
+	call close (fd)
+
+	# Set structure parameters and the correction flags.
+	if (nbadcols != 0) {
+	    NBADCOLS(ccd) = nbadcols
+	    BADCOLS(ccd) = badcols
+	    CORS(ccd, FIXPIX) = YES
+	    COR(ccd) = YES
+	}
+	if (nbadlines != 0) {
+	    NBADLINES(ccd) = nbadlines
+	    BADLINES(ccd) = badlines
+	    CORS(ccd, FIXPIX) = YES
+	    COR(ccd) = YES
+	}
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE, "Bad pixel file is %s")
+	    call pargstr (Memc[image])
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "fixpix", Memc[str])
+
+	call sfree (sp)
+end
+
+
+# SET_BADCOLS -- Enter bad columns in a bad column array.
+# This procedure is used both for the line and column interpolation arrays.
+# The bad column array contains the starting and ending bad columns for
+# each line.  This allows quick look up when processing the image at the
+# expense of memory.  A column index of zero indicates no further bad columns
+# in the line.
+
+procedure set_badcols (c1, c2, l1, l2, array, nl, nbadcols)
+
+int	c1, c2, l1, l2			# Bad column
+short	array[2,nl,nbadcols]		# Bad column array
+int	nl				# Number of image lines
+int	nbadcols			# Number of bad column areas
+
+int	i, j
+
+begin
+	# For each line in the bad columns set the columns
+	# in the first unused entry in the array.
+
+	do i = l1, l2 {
+	    do j = 1, nbadcols {
+		if (array[1,i,j] == 0) {
+		    array[1,i,j] = c1
+		    array[2,i,j] = c2
+		    break
+		}
+	    }
+	}
+end
diff --git a/noao/imred/quadred/src/ccdproc/setflat.x b/noao/imred/quadred/src/ccdproc/setflat.x
new file mode 100644
index 00000000..87713404
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setflat.x
@@ -0,0 +1,146 @@
+include	<imhdr.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+# SET_FLAT -- Set parameters for flat field correction.
+#
+#   1.  Return immediately if the flat field correction is not requested or
+#	if the image has been previously corrected.
+#   2.  Get the flat field image and return on an error.
+#   3.  If the flat field image has not been processed call PROC.
+#   4.  Set the processing flags and record the operation in the output
+#   	image and write a log record.
+
+procedure set_flat (ccd)
+
+pointer	ccd			# CCD structure
+
+int	nc, nl, c1, c2, cs, l1, l2, ls, data_c1, ccd_c1, data_l1, ccd_l1
+pointer	sp, str, image, im, ccd_cache()
+bool	clgetb(), ccdflag(), ccdcheck()
+int	nscan, ccdnscan(), ccdtypei()
+real	hdmgetr()
+errchk	cal_image, ccd_cache, ccdproc, hdmgetr
+
+begin
+	# Check if the user wants this operation or if it has been done.
+	if (!clgetb ("flatcor") || ccdflag (IN_IM(ccd), "flatcor"))
+	    return
+
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the flat field correction image.
+	if (clgetb ("scancor"))
+	    nscan = ccdnscan (IN_IM(ccd), ccdtypei(IN_IM(ccd)))
+	else
+	    nscan = 1
+	call cal_image (IN_IM(ccd), FLAT, nscan, Memc[image], SZ_FNAME)
+
+	# If no processing is desired print flat field image name and return.
+	if (clgetb ("noproc")) {
+	    call eprintf ("  [TO BE DONE] Flat correction image is %s.\n")
+		call pargstr (Memc[image])
+	    call sfree (sp)
+	    return
+	}
+
+	# Map the image and return on an error.
+	# Process the flat field image if necessary.
+	# If nscan > 1 then the flat field may not yet exist so create it
+	# from the unscanned flat field.
+
+	iferr (im = ccd_cache (Memc[image], FLAT)) {
+	    call cal_image (IN_IM(ccd), FLAT, 1, Memc[str], SZ_LINE)
+	    im = ccd_cache (Memc[str], FLAT)
+	    if (ccdcheck (im, FLAT)) {
+		call ccd_flush (im)
+		call ccdproc (Memc[str], FLAT)
+	    }
+	    call scancor (Memc[str], Memc[image], nscan, MINREPLACE(ccd))
+	    im = ccd_cache (Memc[image], FLAT)
+	}
+
+	if (ccdcheck (im, FLAT)) {
+	    call ccd_flush (im)
+	    call ccdproc (Memc[image], FLAT)
+	    im = ccd_cache (Memc[image], FLAT)
+	}
+
+	# Set the processing parameters in the CCD structure.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	c1 = 1
+	c2 = nc
+	l1 = 1
+	l2 = nl
+	cs = 1
+	ls = 1
+	call hdmgstr (im, "datasec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1)) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Data section error: image=%s[%d,%d], datasec=[%d:%d,%d:%d]")
+		call pargstr (Memc[image])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+	data_c1 = c1
+	data_l1 = l1
+	call hdmgstr (im, "ccdsec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if (nc == 1) {
+	    c1 = CCD_C1(ccd)
+	    c2 = CCD_C2(ccd)
+	}
+	if (nl == 1) {
+	    l1 = CCD_L1(ccd)
+	    l2 = CCD_L2(ccd)
+	}
+	ccd_c1 = c1
+	ccd_l1 = l1
+	if ((c1 > CCD_C1(ccd)) || (c2 < CCD_C2(ccd)) ||
+	    (l1 > CCD_L1(ccd)) || (l2 < CCD_L2(ccd))) {
+	    call sprintf (Memc[str], SZ_LINE,
+	        "CCD section error: input=[%d:%d,%d:%d], %s=[%d:%d,%d:%d]")
+		call pargi (CCD_C1(ccd))
+		call pargi (CCD_C2(ccd))
+		call pargi (CCD_L1(ccd))
+		call pargi (CCD_L2(ccd))
+		call pargstr (Memc[image])
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+
+	FLAT_IM(ccd) = im
+	FLAT_C1(ccd) = CCD_C1(ccd) - ccd_c1 + data_c1
+	FLAT_C2(ccd) = CCD_C2(ccd) - ccd_c1 + data_c1
+	FLAT_L1(ccd) = CCD_L1(ccd) - ccd_l1 + data_l1
+	FLAT_L2(ccd) = CCD_L2(ccd) - ccd_l1 + data_l1
+
+	# If no mean value use 1 as the scale factor.
+	iferr (FLATSCALE(ccd) = hdmgetr (im, "ccdmean"))
+	    FLATSCALE(ccd) = 1.
+	CORS(ccd, FLATCOR) = F
+	COR(ccd) = YES
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE,
+	    "Flat field image is %s with scale=%g")
+	    call pargstr (Memc[image])
+	    call pargr (FLATSCALE(ccd))
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "flatcor", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/setfringe.x b/noao/imred/quadred/src/ccdproc/setfringe.x
new file mode 100644
index 00000000..7055f35f
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setfringe.x
@@ -0,0 +1,123 @@
+include	<imhdr.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+# SET_FRINGE -- Set parameters for fringe correction.
+#
+#   1.  Return immediately if the fringe correction is not requested or
+#	if the image has been previously corrected.
+#   2.  Get the fringe image and return error if the mkfringe flag is missing.
+#   3.  Set the processing flags and record the operation in the output
+#   	image and write a log record.
+
+procedure set_fringe (ccd)
+
+pointer	ccd			# CCD structure
+
+int	nc, nl, c1, c2, cs, l1, l2, ls, data_c1, ccd_c1, data_l1, ccd_l1
+real	exptime1, exptime2, fringescale
+pointer	sp, str, image, im
+
+bool	clgetb(), ccdflag()
+real	hdmgetr()
+pointer	ccd_cache()
+errchk	cal_image, ccd_cache, ccdproc, hdmgetr
+
+begin
+	# Check if the user wants this operation or if it has been done.
+	if (!clgetb ("fringecor") || ccdflag (IN_IM(ccd), "fringcor"))
+	    return
+
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the fringe correction image.
+	call cal_image (IN_IM(ccd), FRINGE, 1, Memc[image], SZ_FNAME)
+
+	# If no processing is desired print fringe image name and return.
+	if (clgetb ("noproc")) {
+	    call eprintf (
+		"  [TO BE DONE] Fringe correction image is %s.\n")
+		call pargstr (Memc[image])
+	    call sfree (sp)
+	    return
+	}
+
+	# Return an error if the fringe flag is missing.
+	im = ccd_cache (Memc[image], FRINGE)
+	if (!ccdflag (im, "mkfringe"))
+	    call error (0, "MKFRINGE flag missing from fringe image.")
+
+	# Set the processing parameters in the CCD structure.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	c1 = 1
+	c2 = nc
+	l1 = 1
+	l2 = nl
+	cs = 1
+	ls = 1
+	call hdmgstr (im, "datasec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1)) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Data section error: image=%s[%d,%d], datasec=[%d:%d,%d:%d]")
+		call pargstr (Memc[image])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+	data_c1 = c1
+	data_l1 = l1
+	call hdmgstr (im, "ccdsec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	ccd_c1 = c1
+	ccd_l1 = l1
+	if ((c1 > CCD_C1(ccd)) || (c2 < CCD_C2(ccd)) ||
+	    (l1 > CCD_L1(ccd)) || (l2 < CCD_L2(ccd))) {
+	    call sprintf (Memc[str], SZ_LINE,
+	        "CCD section error: input=[%d:%d,%d:%d], %s=[%d:%d,%d:%d]")
+		call pargi (CCD_C1(ccd))
+		call pargi (CCD_C2(ccd))
+		call pargi (CCD_L1(ccd))
+		call pargi (CCD_L2(ccd))
+		call pargstr (Memc[image])
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+
+	FRINGE_IM(ccd) = im
+	FRINGE_C1(ccd) = CCD_C1(ccd) - ccd_c1 + data_c1
+	FRINGE_C2(ccd) = CCD_C2(ccd) - ccd_c1 + data_c1
+	FRINGE_L1(ccd) = CCD_L1(ccd) - ccd_l1 + data_l1
+	FRINGE_L2(ccd) = CCD_L2(ccd) - ccd_l1 + data_l1
+
+	# Get the scaling factors.  If no fringe scale factor assume 1.
+	exptime1 = hdmgetr (IN_IM(ccd), "exptime")
+	exptime2 = hdmgetr (im, "exptime")
+	iferr (fringescale = hdmgetr (im, "fringscl"))
+	    fringescale = 1.
+
+	FRINGESCALE(ccd) = exptime1 / exptime2 * fringescale
+	CORS(ccd, FRINGECOR) = Q
+	COR(ccd) = YES
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE,
+	    "Fringe image is %s with scale=%g")
+	    call pargstr (Memc[image])
+	    call pargr (FRINGESCALE(ccd))
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "fringcor", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/setheader.x b/noao/imred/quadred/src/ccdproc/setheader.x
new file mode 100644
index 00000000..5687612d
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setheader.x
@@ -0,0 +1,76 @@
+include	<imhdr.h>
+include	"ccdred.h"
+
+# SET_HEADER -- Set the output image header.
+
+procedure set_header (ccd)
+
+pointer	ccd			# CCD structure
+
+int	nc, nl
+pointer	sp, str, out
+long	clktime()
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	out = OUT_IM(ccd)
+	nc = IM_LEN(out,1)
+	nl = IM_LEN(out,2)
+
+	# Set the data section if it is not the whole image.
+	if ((OUT_C1(ccd) != 1) || (OUT_C2(ccd) != nc) ||
+	    (OUT_L1(ccd) != 1) || (OUT_L2(ccd) != nl)) {
+	    call sprintf (Memc[str], SZ_LINE, "[%d:%d,%d:%d]")
+	        call pargi (OUT_C1(ccd))
+	        call pargi (OUT_C2(ccd))
+	        call pargi (OUT_L1(ccd))
+	        call pargi (OUT_L2(ccd))
+	    call hdmpstr (out, "datasec", Memc[str])
+	} else {
+	    iferr (call hdmdelf (out, "datasec"))
+		;
+	}
+
+	# Set the CCD section.
+	call sprintf (Memc[str], SZ_LINE, "[%d:%d,%d:%d]")
+	    call pargi (CCD_C1(ccd))
+	    call pargi (CCD_C2(ccd))
+	    call pargi (CCD_L1(ccd))
+	    call pargi (CCD_L2(ccd))
+	call hdmpstr (out, "ccdsec", Memc[str])
+
+	# If trimming update the trim and bias section parameters.
+	if (CORS(ccd, TRIM) == YES) {
+	    iferr (call hdmdelf (out, "trimsec"))
+	        ;
+	    iferr (call hdmdelf (out, "biassec"))
+	        ;
+	    BIAS_C1(ccd) = max (1, BIAS_C1(ccd) - TRIM_C1(ccd) + 1)
+	    BIAS_C2(ccd) = min (nc, BIAS_C2(ccd) - TRIM_C1(ccd) + 1)
+	    BIAS_L1(ccd) = max (1, BIAS_L1(ccd) - TRIM_L1(ccd) + 1)
+	    BIAS_L2(ccd) = min (nl, BIAS_L2(ccd) - TRIM_L1(ccd) + 1)
+	    if ((BIAS_C1(ccd)<=BIAS_C2(ccd)) && (BIAS_L1(ccd)<=BIAS_L2(ccd))) {
+		call sprintf (Memc[str], SZ_LINE, "[%d:%d,%d:%d]")
+		    call pargi (BIAS_C1(ccd))
+		    call pargi (BIAS_C2(ccd))
+		    call pargi (BIAS_L1(ccd))
+		    call pargi (BIAS_L2(ccd))
+		call hdmpstr (out, "biassec", Memc[str])
+	    }
+	}
+
+	# Set mean value if desired.
+	if (CORS(ccd, FINDMEAN) == YES) {
+	    call hdmputr (out, "ccdmean", MEAN(ccd))
+	    call hdmputi (out, "ccdmeant", int (clktime (long (0))))
+	}
+
+	# Mark image as processed.
+	call sprintf (Memc[str], SZ_LINE, "CCD processing done")
+	call timelog (Memc[str], SZ_LINE)
+	call hdmpstr (out, "ccdproc", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/setillum.x b/noao/imred/quadred/src/ccdproc/setillum.x
new file mode 100644
index 00000000..d1677301
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setillum.x
@@ -0,0 +1,132 @@
+include	<imhdr.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+# SET_ILLUM -- Set parameters for illumination correction.
+#
+#   1.  Return immediately if the illumination correction is not requested or
+#	if the image has been previously corrected.
+#   2.  Get the illumination image and return error if mkillum flag missing.
+#   3.  Set the processing flags and record the operation in the output
+#   	image and write a log record.
+
+procedure set_illum (ccd)
+
+pointer	ccd			# CCD structure
+
+int	nc, nl, c1, c2, cs, l1, l2, ls, data_c1, ccd_c1, data_l1, ccd_l1
+long	time
+pointer	sp, str, image, im
+
+bool	clgetb(), ccdflag()
+long	hdmgeti()
+real	hdmgetr()
+pointer	ccd_cache()
+errchk	cal_image, ccd_cache, ccdproc, hdmgetr, hdmgeti
+
+begin
+	# Check if the user wants this operation or if it has been done.
+	if (!clgetb ("illumcor") || ccdflag (IN_IM(ccd), "illumcor"))
+	    return
+
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the illumcor correction image.
+	call cal_image (IN_IM(ccd), ILLUM, 1, Memc[image], SZ_FNAME)
+
+	# If no processing is desired print illumination image name and return.
+	if (clgetb ("noproc")) {
+	    call eprintf (
+		"  [TO BE DONE] Illumination correction image is %s.\n")
+		call pargstr (Memc[image])
+	    call sfree (sp)
+	    return
+	}
+
+	# Return a warning if the illumination flag is missing.
+	im = ccd_cache (Memc[image], ILLUM)
+	if (!ccdflag (im, "mkillum")) {
+	    call ccd_flush (im)
+	    call error (0, "MKILLUM flag missing from illumination image")
+	}
+
+	# If no mean value for the scale factor compute it.
+	iferr (ILLUMSCALE(ccd) = hdmgetr (im, "ccdmean"))
+	    ILLUMSCALE(ccd) = INDEF
+	iferr (time = hdmgeti (im, "ccdmeant"))
+	    time = IM_MTIME(im)
+	if (IS_INDEF(ILLUMSCALE(ccd)) || time < IM_MTIME(im)) {
+	    call ccd_flush (im)
+	    call ccdmean (Memc[image])
+	    im = ccd_cache (Memc[image], ILLUM)
+	}
+	iferr (ILLUMSCALE(ccd) = hdmgetr (im, "ccdmean"))
+	    ILLUMSCALE(ccd) = 1.
+ 
+	# Set the processing parameters in the CCD structure.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	c1 = 1
+	c2 = nc
+	l1 = 1
+	l2 = nl
+	cs = 1
+	ls = 1
+	call hdmgstr (im, "datasec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1)) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Data section error: image=%s[%d,%d], datasec=[%d:%d,%d:%d]")
+		call pargstr (Memc[image])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+	data_c1 = c1
+	data_l1 = l1
+	call hdmgstr (im, "ccdsec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	ccd_c1 = c1
+	ccd_l1 = l1
+	if ((c1 > CCD_C1(ccd)) || (c2 < CCD_C2(ccd)) ||
+	    (l1 > CCD_L1(ccd)) || (l2 < CCD_L2(ccd))) {
+	    call sprintf (Memc[str], SZ_LINE,
+	        "CCD section error: input=[%d:%d,%d:%d], %s=[%d:%d,%d:%d]")
+		call pargi (CCD_C1(ccd))
+		call pargi (CCD_C2(ccd))
+		call pargi (CCD_L1(ccd))
+		call pargi (CCD_L2(ccd))
+		call pargstr (Memc[image])
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+
+	ILLUM_IM(ccd) = im
+	ILLUM_C1(ccd) = CCD_C1(ccd) - ccd_c1 + data_c1
+	ILLUM_C2(ccd) = CCD_C2(ccd) - ccd_c1 + data_c1
+	ILLUM_L1(ccd) = CCD_L1(ccd) - ccd_l1 + data_l1
+	ILLUM_L2(ccd) = CCD_L2(ccd) - ccd_l1 + data_l1
+
+	CORS(ccd, ILLUMCOR) = I
+	COR(ccd) = YES
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE,
+	    "Illumination image is %s with scale=%g")
+	    call pargstr (Memc[image])
+	    call pargr (ILLUMSCALE(ccd))
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "illumcor", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/setinput.x b/noao/imred/quadred/src/ccdproc/setinput.x
new file mode 100644
index 00000000..3d3170db
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setinput.x
@@ -0,0 +1,48 @@
+include	<error.h>
+include	"ccdtypes.h"
+
+# SET_INPUT -- Set the input image and image type.
+#
+# 1.  Open the input image.  Return warning and NULL pointer for an error.
+# 2.  Get the requested CCD image type.
+#	a. If no type is requested then accept the image.
+#	b. If a type is requested then match against the image type.
+#	   Unmap the image if no match.
+# 3.  If the image is acceptable then get the CCD type code.
+
+procedure set_input (image, im, ccdtype)
+
+char	image[ARB]	# Input image name
+pointer	im		# IMIO pointer (returned)
+int	ccdtype		# CCD image type
+
+bool	strne()
+int	ccdtypei()
+pointer	sp, str1, str2, immap()
+
+begin
+	# Open the image.  Return a warning and NULL pointer for an error.
+	iferr (im = immap (image, READ_ONLY, 0)) {
+	    call erract (EA_WARN)
+	    im = NULL
+	    return
+	}
+
+	call smark (sp)
+	call salloc (str1, SZ_LINE, TY_CHAR)
+	call salloc (str2, SZ_LINE, TY_CHAR)
+
+	# Get the requested CCD type.
+	call clgstr ("ccdtype", Memc[str1], SZ_LINE)
+	call xt_stripwhite (Memc[str1])
+	if (Memc[str1] != EOS) {
+	    call ccdtypes (im, Memc[str2], SZ_LINE)
+	    if (strne (Memc[str1], Memc[str2]))
+		call imunmap (im)
+	}
+
+	if (im != NULL)
+	    ccdtype = ccdtypei (im)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/setinteract.x b/noao/imred/quadred/src/ccdproc/setinteract.x
new file mode 100644
index 00000000..05bc0f71
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setinteract.x
@@ -0,0 +1,31 @@
+include	<pkg/xtanswer.h>
+
+# SET_INTERACTIVE -- Set the interactive flag.  Query the user if necessary.
+#
+# This procedure initializes the interactive flag if there is no query.
+# If there is a query it is issued by XT_ANSWER.   The four valued
+# interactive flag is returned.
+
+procedure set_interactive (query, interactive)
+
+char	query[ARB]		# Query prompt
+int	interactive		# Fit overscan interactively?  (returned)
+
+int	interact		# Saves last value of interactive flag
+bool	clgetb()
+
+begin
+	# If the query is null then initialize from the CL otherwise
+	# query the user.  This response is four valued to allow the user
+	# to turn off the query when processing multiple images.
+
+	if (query[1] == EOS) {
+	    if (clgetb ("interactive"))
+	        interact = YES
+	    else
+	        interact = ALWAYSNO
+	} else
+	    call xt_answer (query, interact)
+
+	interactive = interact
+end
diff --git a/noao/imred/quadred/src/ccdproc/setoutput.x b/noao/imred/quadred/src/ccdproc/setoutput.x
new file mode 100644
index 00000000..0c4e608f
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setoutput.x
@@ -0,0 +1,51 @@
+include	<imhdr.h>
+include	<imset.h>
+
+# SET_OUTPUT -- Setup the output image.
+# The output image is a NEW_COPY of the input image.
+# The user may select a pixel datatype with higher precision though not
+# lower.
+
+procedure set_output (in, out, output)
+
+pointer	in			# Input IMIO pointer to copy
+pointer	out			# Output IMIO pointer
+char	output[SZ_FNAME]	# Output image name
+
+int	i, clscan(), nscan()
+char	type[1]
+pointer	immap()
+errchk	immap
+
+begin
+	out = immap (output, NEW_COPY, in)
+	IM_PIXTYPE(out) = TY_REAL
+	if (clscan ("pixeltype")  != EOF) {
+	    call gargwrd (type, 1)
+	    if (nscan() == 1) {
+		i = IM_PIXTYPE(in)
+		IM_PIXTYPE(out) = i
+		switch (type[1]) {
+		case 's':
+		    ;
+		case 'u':
+		    if (i == TY_SHORT)
+			IM_PIXTYPE(out) = TY_USHORT
+		case 'i':
+		    if (i == TY_SHORT || i == TY_USHORT)
+			IM_PIXTYPE(out) = TY_INT
+		case 'l':
+		    if (i == TY_SHORT || i == TY_USHORT || i == TY_INT)
+			IM_PIXTYPE(out) = TY_LONG
+		case 'r':
+		    if (i != TY_DOUBLE)
+			IM_PIXTYPE(out) = TY_REAL
+		case 'd':
+		    IM_PIXTYPE(out) = TY_DOUBLE
+		default:
+		    call imunmap (out)
+		    call error (0, "Unknown pixel type")
+		}
+	    }
+	}
+end
diff --git a/noao/imred/quadred/src/ccdproc/setoverscan.x b/noao/imred/quadred/src/ccdproc/setoverscan.x
new file mode 100644
index 00000000..2fef378a
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setoverscan.x
@@ -0,0 +1,344 @@
+include	<imhdr.h>
+include	<imset.h>
+include <pkg/gtools.h>
+include	<pkg/xtanswer.h>
+include	"ccdred.h"
+
+
+# SET_OVERSCAN -- Set the overscan vector.
+#
+#   1.  Return immediately if the overscan correction is not requested or
+#	if the image has been previously corrected.
+#   2.	Determine the overscan columns or lines.  This may be specifed
+#	directly or indirectly through the image header or symbol table.
+#   3.	Average the overscan columns or lines.
+#   4.	Fit a function with the ICFIT routines to smooth the overscan vector.
+#   5.  Set the processing flag.
+#   6.  Log the operation (to user, logfile, and output image header).
+
+procedure set_overscan (ccd)
+
+pointer	ccd			# CCD structure pointer
+
+int	i, j, nsec, navg, npts, first, last
+int	nc, nl, c1, c2, l1, l2
+pointer	sp, str, errstr, buf, overscan, x, y, z
+
+real	asumr()
+bool	clgetb(), ccdflag()
+pointer	imgl2r()
+errchk	imgl2r, fit_overscan
+
+begin
+	# Check if the user wants this operation or if it has been done.
+	if (!clgetb ("overscan") || ccdflag (IN_IM(ccd), "overscan"))
+	    return
+
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+	call salloc (errstr, SZ_LINE, TY_CHAR)
+	call imstats (IN_IM(ccd), IM_IMAGENAME, Memc[str], SZ_LINE)
+
+	# Check bias section.
+	nc = IM_LEN(IN_IM(ccd),1)
+	nl = IM_LEN(IN_IM(ccd),2)
+
+	c1 = BIAS_C1(ccd)
+	c2 = BIAS_C2(ccd)
+	l1 = BIAS_L1(ccd)
+	l2 = BIAS_L2(ccd)
+	navg = c2 - c1 + 1
+	npts = CCD_L2(ccd) - CCD_L1(ccd) + 1
+
+	nsec = max (1, IN_NSEC(ccd))
+	do i = 1, nsec {
+	    if (BIAS_SEC(ccd) != NULL) {
+		c1 = BIAS_SC1(ccd,i)
+		c2 = BIAS_SC2(ccd,i)
+		l1 = BIAS_SL1(ccd,i)
+		l2 = BIAS_SL2(ccd,i)
+	    }
+	    if ((c1 < 1) || (c2 > nc) || (l1 < 1) || (l2 > nl)) {
+		call sprintf (Memc[errstr], SZ_LINE,
+		"Error in bias section: image=%s[%d,%d], biassec=[%d:%d,%d:%d]")
+		    call pargstr (Memc[str])
+		    call pargi (nc)
+		    call pargi (nl)
+		    call pargi (c1)
+		    call pargi (c2)
+		    call pargi (l1)
+		    call pargi (l2)
+		call error (0, Memc[errstr])
+	    }
+	    if ((c1 == 1) && (c2 == nc) && (l1 == 1) && (l2 == nl)) {
+		call error (0,
+		    "Bias section not specified or given as full image")
+	    }
+
+	    # If no processing is desired then print overscan strip and return.
+	    if (clgetb ("noproc")) {
+		call eprintf (
+		    "  [TO BE DONE] Overscan section is [%d:%d,%d:%d].\n")
+		    call pargi (c1)
+		    call pargi (c2)
+		    call pargi (l1)
+		    call pargi (l2)
+		    call sfree (sp)
+		    return
+	    }
+	}
+
+	# Determine the overscan section parameters. The readout axis
+	# determines the type of overscan.  The step sizes are ignored.
+	# The limits in the long dimension are replaced by the trim limits.
+
+	if (READAXIS(ccd) == 1) {
+	    call salloc (buf, nsec*nl, TY_REAL)
+	    z = buf
+	    do i = 1, nl {
+		y = imgl2r (IN_IM(ccd), i)
+		do j = 1, nsec {
+		    if (BIAS_SEC(ccd) != NULL) {
+			l1 = BIAS_SL1(ccd,j)
+			l2 = BIAS_SL2(ccd,j)
+			if (i < l1 || i > l2)
+			    next
+			c1 = BIAS_SC1(ccd,j)
+			c2 = BIAS_SC2(ccd,j)
+			navg = c2 - c1 + 1
+			z = buf + (j - 1) * nl
+		    }
+		    Memr[z+i-1] = asumr (Memr[y+c1-1], navg)
+		}
+	    }
+
+	    # Trim the overscan vector and set the pixel coordinate.
+	    call salloc (x, nl, TY_REAL)
+	    call malloc (overscan, nsec*nl, TY_REAL)
+	    y = overscan
+	    do i = 1, nsec {
+		if (BIAS_SEC(ccd) != NULL) {
+		    c1 = BIAS_SC1(ccd,i)
+		    c2 = BIAS_SC2(ccd,i)
+		    l1 = BIAS_SL1(ccd,i)
+		    l2 = BIAS_SL2(ccd,i)
+		    navg = c2 - c1 + 1
+		    npts = l2 - l1 + 1
+		    y = overscan + (i - 1) * nl
+		    z = buf + (i - 1) * nl
+		}
+		if (navg > 1)
+		    call adivkr (Memr[z+l1-1], real (navg), Memr[z+l1-1],
+			npts)
+		call trim_overscan (Memr[z], npts, l1, Memr[x], Memr[y])
+		call fit_overscan (Memc[str], c1, c2, l1, l2, Memr[x],
+		    Memr[y], npts)
+	    }
+
+	} else {
+	    first = l1
+	    last = l2
+	    navg = last - first + 1
+	    npts = nc
+	    call salloc (buf, npts, TY_REAL)
+	    call aclrr (Memr[buf], npts)
+	    do i = first, last
+	        call aaddr (Memr[imgl2r(IN_IM(ccd),i)], Memr[buf], Memr[buf],
+		    npts)
+	    if (navg > 1)
+	        call adivkr (Memr[buf], real (navg), Memr[buf], npts)
+
+	    # Trim the overscan vector and set the pixel coordinate.
+	    npts = CCD_C2(ccd) - CCD_C1(ccd) + 1
+	    call malloc (overscan, npts, TY_REAL)
+	    call salloc (x, npts, TY_REAL)
+	    call trim_overscan (Memr[buf], npts, IN_C1(ccd), Memr[x],
+		Memr[overscan])
+
+	    call fit_overscan (Memc[str], c1, c2, l1, l2, Memr[x],
+		Memr[overscan], npts)
+	}
+	
+	# Set the CCD structure overscan parameters.
+	CORS(ccd, OVERSCAN) = O
+	COR(ccd) = YES
+	OVERSCAN_VEC(ccd) = overscan
+
+	# Log the operation.
+	call strcpy ("overscan", Memc[errstr], SZ_LINE)
+	y = overscan
+	do i = 1, nsec {
+	    if (BIAS_SEC(ccd) != NULL) {
+		c1 = BIAS_SC1(ccd,i)
+		c2 = BIAS_SC2(ccd,i)
+		l1 = BIAS_SL1(ccd,i)
+		l2 = BIAS_SL2(ccd,i)
+		y = overscan + (i - 1) * nl
+		npts = c2 - c1 + 1
+		if (i > 1) {
+		    call sprintf (Memc[errstr], SZ_LINE, "ovrscn%d")
+			call pargi (i)
+		}
+	    }
+	    call sprintf (Memc[str], SZ_LINE,
+		"Overscan section is [%d:%d,%d:%d] with mean=%g")
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+		call pargr (asumr (Memr[y], npts) / npts)
+	    call timelog (Memc[str], SZ_LINE)
+	    call ccdlog (IN_IM(ccd), Memc[str])
+	    call hdmpstr (OUT_IM(ccd), Memc[errstr], Memc[str])
+	}
+
+	call sfree (sp)
+end
+
+
+# FIT_OVERSCAN -- Fit a function to smooth the overscan vector.
+#   The fitting uses the ICFIT procedures which may be interactive.
+#   Changes to these parameters are "learned".  The user is queried with a four
+#   valued logical query (XT_ANSWER routine) which may be turned off when
+#   multiple images are processed.
+
+procedure fit_overscan (image, c1, c2, l1, l2, x, overscan, npts)
+
+char	image[ARB]		# Image name for query and title
+int	c1, c2, l1, l2		# Overscan strip
+real	x[npts]			# Pixel coordinates of overscan
+real	overscan[npts]		# Input overscan and output fitted overscan
+int	npts			# Number of data points
+
+int	interactive, fd
+pointer	sp, str, w, ic, cv, gp, gt
+
+int	clgeti(), ic_geti(), open()
+real	clgetr(), ic_getr()
+pointer	gopen(), gt_init()
+errchk	gopen, open
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+	call salloc (w, npts, TY_REAL)
+	call amovkr (1., Memr[w], npts)
+
+	# Open the ICFIT procedures, get the fitting parameters, and
+	# set the fitting limits.
+
+	call ic_open (ic)
+	call clgstr ("function", Memc[str], SZ_LINE)
+	call ic_pstr (ic, "function", Memc[str])
+	call ic_puti (ic, "order", clgeti ("order"))
+	call clgstr ("sample", Memc[str], SZ_LINE)
+	call ic_pstr (ic, "sample", Memc[str])
+	call ic_puti (ic, "naverage", clgeti ("naverage"))
+	call ic_puti (ic, "niterate", clgeti ("niterate"))
+	call ic_putr (ic, "low", clgetr ("low_reject"))
+	call ic_putr (ic, "high", clgetr ("high_reject"))
+	call ic_putr (ic, "grow", clgetr ("grow"))
+	call ic_putr (ic, "xmin", min (x[1], x[npts]))
+	call ic_putr (ic, "xmax", max (x[1], x[npts]))
+	call ic_pstr (ic, "xlabel", "Pixel")
+	call ic_pstr (ic, "ylabel", "Overscan")
+
+	# If the fitting is done interactively set the GTOOLS and GIO
+	# pointers.  Also "learn" the fitting parameters since they may
+	# be changed when fitting interactively.
+
+	call sprintf (Memc[str], SZ_LINE,
+	    "Fit overscan vector for %s[%d:%d,%d:%d] interactively")
+	    call pargstr (image)
+	    call pargi (c1)
+	    call pargi (c2)
+	    call pargi (l1)
+	    call pargi (l2)
+	call set_interactive (Memc[str], interactive)
+	if ((interactive == YES) || (interactive == ALWAYSYES)) {
+	    gt = gt_init ()
+	    call sprintf (Memc[str], SZ_LINE,
+	        "Overscan vector for %s from section [%d:%d,%d:%d]\n")
+	        call pargstr (image)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call gt_sets (gt, GTTITLE, Memc[str])
+	    call gt_sets (gt, GTTYPE, "line")
+	    call gt_setr (gt, GTXMIN, x[1])
+	    call gt_setr (gt, GTXMAX, x[npts])
+	    call clgstr ("graphics", Memc[str], SZ_FNAME)
+	    gp = gopen (Memc[str], NEW_FILE, STDGRAPH)
+
+	    call icg_fit (ic, gp, "cursor", gt, cv, x, overscan, Memr[w], npts)
+
+	    call ic_gstr (ic, "function", Memc[str], SZ_LINE)
+	    call clpstr ("function", Memc[str])
+	    call clputi ("order", ic_geti (ic, "order"))
+	    call ic_gstr (ic, "sample", Memc[str], SZ_LINE)
+	    call clpstr ("sample", Memc[str])
+	    call clputi ("naverage", ic_geti (ic, "naverage"))
+	    call clputi ("niterate", ic_geti (ic, "niterate"))
+	    call clputr ("low_reject", ic_getr (ic, "low"))
+	    call clputr ("high_reject", ic_getr (ic, "high"))
+	    call clputr ("grow", ic_getr (ic, "grow"))
+
+	    call gclose (gp)
+	    call gt_free (gt)
+	} else
+	    call ic_fit (ic, cv, x, overscan, Memr[w], npts, YES, YES, YES, YES)
+
+	# Make a log of the fit in the plot file if given.
+	call clgstr ("plotfile", Memc[str], SZ_LINE)
+	call xt_stripwhite (Memc[str])
+	if (Memc[str] != EOS) {
+	    fd = open (Memc[str], APPEND, BINARY_FILE)
+	    gp = gopen ("stdvdm", NEW_FILE, fd)
+	    gt = gt_init ()
+	    call sprintf (Memc[str], SZ_LINE,
+	        "Overscan vector for %s from section [%d:%d,%d:%d]\n")
+	        call pargstr (image)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call gt_sets (gt, GTTITLE, Memc[str])
+	    call gt_sets (gt, GTTYPE, "line")
+	    call gt_setr (gt, GTXMIN, 1.)
+	    call gt_setr (gt, GTXMAX, real (npts))
+	    call icg_graphr (ic, gp, gt, cv, x, overscan, Memr[w], npts)
+	    call gclose (gp)
+	    call close (fd)
+	    call gt_free (gt)
+	}
+
+	# Replace the raw overscan vector with the smooth fit.
+	call cvvector (cv, x, overscan, npts)
+
+	# Finish up.
+	call ic_closer (ic)
+	call cvfree (cv)
+	call sfree (sp)
+end
+
+
+# TRIM_OVERSCAN -- Trim the overscan vector.
+
+procedure trim_overscan (data, npts, start, x, overscan)
+
+real	data[ARB]		# Full overscan vector
+int	npts			# Length of trimmed vector
+int	start			# Trim start
+real	x[npts]			# Trimmed pixel coordinates (returned)
+real	overscan[npts]		# Trimmed overscan vector (returned)
+
+int	i, j
+
+begin
+	do i = 1, npts {
+	    j = start + i - 1
+	    x[i] = j
+	    overscan[i] = data[j]
+	}
+end
diff --git a/noao/imred/quadred/src/ccdproc/setproc.x b/noao/imred/quadred/src/ccdproc/setproc.x
new file mode 100644
index 00000000..595acd76
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setproc.x
@@ -0,0 +1,80 @@
+include	<imhdr.h>
+include	"ccdred.h"
+
+# SET_PROC -- Set the processing parameter structure pointer.
+
+procedure set_proc (in, out, ccd)
+
+pointer	in			# Input IMIO pointer
+pointer	out			# Output IMIO pointer
+pointer	ccd			# CCD structure (returned)
+
+int	clgwrd(), clscan(), nscan()
+real	clgetr()
+pointer	sp, str
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Allocate the ccd structure.
+	call calloc (ccd, LEN_CCD, TY_STRUCT)
+
+	IN_IM(ccd) = in
+	OUT_IM(ccd) = out
+	COR(ccd) = NO
+	CORS(ccd, FIXPIX) = NO
+	CORS(ccd, OVERSCAN) = NO
+	CORS(ccd, TRIM) = NO
+	READAXIS(ccd) = clgwrd ("readaxis",Memc[str],SZ_LINE,"|line|columns|")
+	MINREPLACE(ccd) = clgetr ("minreplace")
+
+	CALCTYPE(ccd) = TY_REAL
+	if (clscan ("pixeltype") != EOF) {
+	    call gargwrd (Memc[str], SZ_LINE)
+	    call gargwrd (Memc[str], SZ_LINE)
+	    if (nscan() == 2) {
+	        if (Memc[str] == 'r')
+		    CALCTYPE(ccd) = TY_REAL
+		else if (Memc[str] == 's')
+		    CALCTYPE(ccd) = TY_SHORT
+		else
+		    call error (1, "Invalid calculation datatype")
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# FREE_PROC -- Free the processing structure pointer.
+
+procedure free_proc (ccd)
+
+pointer	ccd			# CCD structure
+
+begin
+	# Unmap calibration images.
+	if (ZERO_IM(ccd) != NULL)
+	    call ccd_unmap (ZERO_IM(ccd))
+	if (DARK_IM(ccd) != NULL)
+	    call ccd_unmap (DARK_IM(ccd))
+	if (FLAT_IM(ccd) != NULL)
+	    call ccd_unmap (FLAT_IM(ccd))
+	if (ILLUM_IM(ccd) != NULL)
+	    call ccd_unmap (ILLUM_IM(ccd))
+	if (FRINGE_IM(ccd) != NULL)
+	    call ccd_unmap (FRINGE_IM(ccd))
+
+	# Free memory
+	if (BADCOLS(ccd) != NULL)
+	    call mfree (BADCOLS(ccd), TY_SHORT)
+	if (BADLINES(ccd) != NULL)
+	    call mfree (BADLINES(ccd), TY_SHORT)
+	if (OVERSCAN_VEC(ccd) != NULL)
+	    call mfree (OVERSCAN_VEC(ccd), TY_REAL)
+	call mfree (IN_SEC(ccd), TY_INT)
+	call mfree (OUT_SEC(ccd), TY_INT)
+	call mfree (BIAS_SEC(ccd), TY_INT)
+	call mfree (ccd, TY_STRUCT)
+end
diff --git a/noao/imred/quadred/src/ccdproc/setsections.x b/noao/imred/quadred/src/ccdproc/setsections.x
new file mode 100644
index 00000000..b83a9d13
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setsections.x
@@ -0,0 +1,327 @@
+include	<imhdr.h>
+include	"ccdred.h"
+
+# SET_SECTIONS -- Set the data section, ccd section, trim section and
+# bias section.
+
+procedure set_sections (ccd)
+
+pointer	ccd			# CCD structure (returned)
+
+pointer	sp, str
+int	nc, nl, c1, c2, cs, l1, l2, ls
+bool	streq()
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	nc = IM_LEN(IN_IM(ccd),1)
+	nl = IM_LEN(IN_IM(ccd),2)
+
+	# The default data section is the entire image.
+	c1 = 1
+	c2 = nc
+	cs = 1
+	l1 = 1
+	l2 = nl
+	ls = 1
+	call hdmgstr (IN_IM(ccd), "datasec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1))
+	    call error (0, "Error in DATASEC parameter")
+	IN_C1(ccd) = c1
+	IN_C2(ccd) = c2
+	IN_L1(ccd) = l1
+	IN_L2(ccd) = l2
+
+	# The default trim section is the data section.
+	# Defer limit checking until actually used.
+	c1 = IN_C1(ccd)
+	c2 = IN_C2(ccd)
+	l1 = IN_L1(ccd)
+	l2 = IN_L2(ccd)
+	call clgstr ("trimsec", Memc[str], SZ_LINE)
+	if (streq (Memc[str], "image"))
+	    call hdmgstr (IN_IM(ccd), "trimsec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((cs!=1)||(ls!=1))
+	    call error (0, "Error in TRIMSEC parameter")
+	TRIM_C1(ccd) = c1
+	TRIM_C2(ccd) = c2
+	TRIM_L1(ccd) = l1
+	TRIM_L2(ccd) = l2
+
+	# The default bias section is the whole image.
+	# Defer limit checking until actually used.
+	c1 = 1
+	c2 = nc
+	l1 = 1
+	l2 = nl
+	call clgstr ("biassec", Memc[str], SZ_LINE)
+	if (streq (Memc[str], "image"))
+	    call hdmgstr (IN_IM(ccd), "biassec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((cs!=1)||(ls!=1))
+	    call error (0, "Error in BIASSEC parameter")
+	BIAS_C1(ccd) = c1
+	BIAS_C2(ccd) = c2
+	BIAS_L1(ccd) = l1
+	BIAS_L2(ccd) = l2
+
+	# The default ccd section is the size of the data section.
+	c1 = 1
+	c2 = IN_C2(ccd) - IN_C1(ccd) + 1
+	l1 = 1
+	l2 = IN_L2(ccd) - IN_L1(ccd) + 1
+	call hdmgstr (IN_IM(ccd), "ccdsec", Memc[str], SZ_LINE)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((cs != 1) || (ls != 1))
+	    call error (0, "Error in CCDSEC parameter")
+	CCD_C1(ccd) = c1
+	CCD_C2(ccd) = c2
+	CCD_L1(ccd) = l1
+	CCD_L2(ccd) = l2
+	if ((IN_C2(ccd)-IN_C1(ccd) != CCD_C2(ccd)-CCD_C1(ccd)) ||
+	    (IN_L2(ccd)-IN_L1(ccd) != CCD_L2(ccd)-CCD_L1(ccd)))
+	    call error (0, "Size of DATASEC and CCDSEC do not agree")
+
+	# The default output data section is the input data section.
+	OUT_C1(ccd) = IN_C1(ccd)
+	OUT_C2(ccd) = IN_C2(ccd)
+	OUT_L1(ccd) = IN_L1(ccd)
+	OUT_L2(ccd) = IN_L2(ccd)
+
+	# Set ARCON style sections.
+	call set_arcon (ccd)
+
+	call sfree (sp)
+end
+
+
+# SET_ARCON -- Set the data section, ccd section, trim section and
+# bias section.
+
+procedure set_arcon (ccd)
+
+pointer	ccd			# CCD structure (returned)
+
+pointer	sp, amplist, amp, key, str
+int	i, ip, nc, nl, c1, c2, cs, l1, l2, ls, ctowrd()
+int	xt1, xt2, yt1, yt2
+bool	trim, clgetb()
+
+begin
+	call smark (sp)
+	call salloc (amplist, SZ_LINE, TY_CHAR)
+	call salloc (amp, SZ_LINE, TY_CHAR)
+	call salloc (key, SZ_LINE, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	trim = clgetb ("trim")
+
+	# Get AMPLIST and determine the number of amplifiers.
+	# If there is no AMPLIST or missing BSEC keywords return.
+	call hdmgstr (IN_IM(ccd), "amplist", Memc[amplist], SZ_LINE)
+	if (Memc[amplist] == EOS) {
+	    call sfree (sp)
+	    return
+	}
+
+	ip = 1
+	for (i=0; ctowrd(Memc[amplist],ip,Memc[amp],SZ_LINE)!=0; i=i+1) {
+	    call sprintf (Memc[key], SZ_LINE, "bsec%s")
+		call pargstr (Memc[amp])
+	    call hdmgstr (IN_IM(ccd), Memc[key], Memc[str], SZ_LINE)
+	    if (Memc[str] == EOS) {
+		call sfree (sp)
+		return
+	    }
+	}
+	if (i == 0) {
+	    call sfree (sp)
+	    return
+	}
+
+	IN_NSEC(ccd) = i
+	call malloc (IN_SEC(ccd), 4*i, TY_INT)
+	call malloc (OUT_SEC(ccd), 4*i, TY_INT)
+	call malloc (BIAS_SEC(ccd), 4*i, TY_INT)
+
+	nc = IM_LEN(IN_IM(ccd),1)
+	nl = IM_LEN(IN_IM(ccd),2)
+
+	ip = 1
+	for (i=1; ctowrd(Memc[amplist],ip,Memc[amp],SZ_LINE)!=0; i=i+1) {
+
+	    # Use amp section if no trim and data section if trim.
+	    c1 = 1; c2 = nc; cs = 1; l1 = 1; l2 = nl; ls = 1
+	    if (trim)
+		call sprintf (Memc[key], SZ_LINE, "dsec%s")
+	    else
+		call sprintf (Memc[key], SZ_LINE, "asec%s")
+		call pargstr (Memc[amp])
+	    call hdmgstr (IN_IM(ccd), Memc[key], Memc[str], SZ_LINE)
+	    if (Memc[str] == EOS) {
+		call sprintf (Memc[str], SZ_LINE, "Keyword %s not found")
+		    call pargstr (Memc[key])
+		call error (0, Memc[str])
+	    }
+	    call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	    if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)) {
+		call sprintf (Memc[str], SZ_LINE, "Error in %s parameter")
+		    call pargstr (Memc[key])
+		call error (0, Memc[str])
+	    }
+	    IN_SC1(ccd,i) = c1
+	    IN_SC2(ccd,i) = c2
+	    IN_SL1(ccd,i) = l1
+	    IN_SL2(ccd,i) = l2
+
+	    # If trimming match dsec with csec and then use tsec.
+	    if (trim) {
+		c1 = IN_SC1(ccd,i); c2 = IN_SC2(ccd,i); cs = 1
+		l1 = IN_SL1(ccd,i); l2 = IN_SL2(ccd,i); ls = 1
+		call sprintf (Memc[key], SZ_LINE, "tsec%s")
+		    call pargstr (Memc[amp])
+		call hdmgstr (IN_IM(ccd), Memc[key], Memc[str], SZ_LINE)
+		if (Memc[str] != EOS)
+		    call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+		if ((c1<IN_SC1(ccd,i))||(c2>IN_SC2(ccd,i))||
+		    (l1<IN_SL1(ccd,i))||(l2>IN_SL2(ccd,i))) {
+		    call sprintf (Memc[str], SZ_LINE, "Error in %s parameter")
+			call pargstr (Memc[key])
+		    call error (0, Memc[str])
+		}
+		xt1 = max (0, c1 - IN_SC1(ccd,i))
+		xt2 = min (0, c2 - IN_SC2(ccd,i))
+		yt1 = max (0, l1 - IN_SL1(ccd,i))
+		yt2 = min (0, l2 - IN_SL2(ccd,i))
+
+		call sprintf (Memc[key], SZ_LINE, "csec%s")
+		    call pargstr (Memc[amp])
+		call hdmgstr (IN_IM(ccd), Memc[key], Memc[str], SZ_LINE)
+		if (Memc[str] == EOS) {
+		    call sprintf (Memc[str], SZ_LINE, "Keyword %s not found")
+			call pargstr (Memc[key])
+		    call error (0, Memc[str])
+		}
+		call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+		if ((c2-c1) != (IN_SC2(ccd,i)-IN_SC1(ccd,i)) ||
+		    (l2-l1) != (IN_SL2(ccd,i)-IN_SL1(ccd,i)))
+		    call error (1, "DSEC and CSEC are different sizes")
+
+		IN_SC1(ccd,i) = IN_SC1(ccd,i) + xt1
+		IN_SC2(ccd,i) = IN_SC2(ccd,i) + xt2
+		IN_SL1(ccd,i) = IN_SL1(ccd,i) + yt1
+		IN_SL2(ccd,i) = IN_SL2(ccd,i) + yt2
+		OUT_SC1(ccd,i) = c1 + xt1
+		OUT_SC2(ccd,i) = c2 + xt2
+		OUT_SL1(ccd,i) = l1 + yt1
+		OUT_SL2(ccd,i) = l2 + yt2
+
+	    } else {
+		OUT_SC1(ccd,i) = c1
+		OUT_SC2(ccd,i) = c2
+		OUT_SL1(ccd,i) = l1
+		OUT_SL2(ccd,i) = l2
+	    }
+
+	    # The default bias section is the whole image.
+	    # Defer limit checking until actually used.
+	    c1 = 1
+	    c2 = nc
+	    l1 = 1
+	    l2 = nl
+	    call sprintf (Memc[key], SZ_LINE, "bsec%s")
+		call pargstr (Memc[amp])
+	    call hdmgstr (IN_IM(ccd), Memc[key], Memc[str], SZ_LINE)
+	    if (Memc[str] == EOS) {
+		call sprintf (Memc[str], SZ_LINE, "Keyword %s not found")
+		    call pargstr (Memc[key])
+		call error (0, Memc[str])
+	    }
+	    call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	    if ((cs!=1)||(ls!=1))
+		call error (0, "Error in BSEC parameter")
+	    BIAS_SC1(ccd,i) = c1
+	    BIAS_SC2(ccd,i) = c2
+	    BIAS_SL1(ccd,i) = l1
+	    BIAS_SL2(ccd,i) = l2
+
+	    if (trim) {
+		#iferr (call hdmdelf (OUT_IM(ccd), "amplist"))
+		#    ;
+		#call sprintf (Memc[key], SZ_LINE, "asec%s")
+		#    call pargstr (Memc[amp])
+		#iferr (call hdmdelf (OUT_IM(ccd), Memc[key]))
+		#    ;
+		call sprintf (Memc[key], SZ_LINE, "bsec%s")
+		    call pargstr (Memc[amp])
+		iferr (call hdmdelf (OUT_IM(ccd), Memc[key]))
+		    ;
+		call sprintf (Memc[key], SZ_LINE, "csec%s")
+		    call pargstr (Memc[amp])
+		iferr (call hdmdelf (OUT_IM(ccd), Memc[key]))
+		    ;
+		call sprintf (Memc[key], SZ_LINE, "dsec%s")
+		    call pargstr (Memc[amp])
+		iferr (call hdmdelf (OUT_IM(ccd), Memc[key]))
+		    ;
+		call sprintf (Memc[key], SZ_LINE, "tsec%s")
+		    call pargstr (Memc[amp])
+		iferr (call hdmdelf (OUT_IM(ccd), Memc[key]))
+		    ;
+	    }
+	}
+
+	# Set global sections.
+	IN_C1(ccd) = IN_SC1(ccd,1)
+	IN_C2(ccd) = IN_SC2(ccd,1)
+	IN_L1(ccd) = IN_SL1(ccd,1)
+	IN_L2(ccd) = IN_SL2(ccd,1)
+	CCD_C1(ccd) = OUT_SC1(ccd,1)
+	CCD_C2(ccd) = OUT_SC2(ccd,1)
+	CCD_L1(ccd) = OUT_SL1(ccd,1)
+	CCD_L2(ccd) = OUT_SL2(ccd,1)
+	do i = 2, IN_NSEC(ccd) {
+	    IN_C1(ccd) = min (IN_SC1(ccd,i), IN_C1(ccd))
+	    IN_C2(ccd) = max (IN_SC2(ccd,i), IN_C2(ccd))
+	    IN_L1(ccd) = min (IN_SL1(ccd,i), IN_L1(ccd))
+	    IN_L2(ccd) = max (IN_SL2(ccd,i), IN_L2(ccd))
+	    CCD_C1(ccd) = min (OUT_SC1(ccd,i), CCD_C1(ccd))
+	    CCD_C2(ccd) = max (OUT_SC2(ccd,i), CCD_C2(ccd))
+	    CCD_L1(ccd) = min (OUT_SL1(ccd,i), CCD_L1(ccd))
+	    CCD_L2(ccd) = max (OUT_SL2(ccd,i), CCD_L2(ccd))
+	}
+	if (trim) {
+	    OUT_C1(ccd) = CCD_C1(ccd) - CCD_C1(ccd) + 1
+	    OUT_C2(ccd) = CCD_C2(ccd) - CCD_C1(ccd) + 1
+	    OUT_L1(ccd) = CCD_L1(ccd) - CCD_L1(ccd) + 1
+	    OUT_L2(ccd) = CCD_L2(ccd) - CCD_L1(ccd) + 1
+	    ip = 1
+	    for (i=1; ctowrd(Memc[amplist],ip,Memc[amp],SZ_LINE)!=0; i=i+1) {
+		OUT_SC1(ccd,i) = OUT_SC1(ccd,i) - CCD_C1(ccd) + 1
+		OUT_SC2(ccd,i) = OUT_SC2(ccd,i) - CCD_C1(ccd) + 1
+		OUT_SL1(ccd,i) = OUT_SL1(ccd,i) - CCD_L1(ccd) + 1
+		OUT_SL2(ccd,i) = OUT_SL2(ccd,i) - CCD_L1(ccd) + 1
+		call sprintf (Memc[key], SZ_LINE, "asec%s")
+		    call pargstr (Memc[amp])
+		call sprintf (Memc[str], SZ_LINE, "[%d:%d,%d:%d]")
+		    call pargi (OUT_SC1(ccd,i))
+		    call pargi (OUT_SC2(ccd,i))
+		    call pargi (OUT_SL1(ccd,i))
+		    call pargi (OUT_SL2(ccd,i))
+		call hdmpstr (OUT_IM(ccd), Memc[key], Memc[str])
+	    }
+	    IM_LEN(OUT_IM(ccd),1) = OUT_C2(ccd)
+	    IM_LEN(OUT_IM(ccd),2) = OUT_L2(ccd)
+	} else {
+	    OUT_C1(ccd) = IN_C1(ccd)
+	    OUT_C2(ccd) = IN_C2(ccd)
+	    OUT_L1(ccd) = IN_L1(ccd)
+	    OUT_L2(ccd) = IN_L2(ccd)
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/settrim.x b/noao/imred/quadred/src/ccdproc/settrim.x
new file mode 100644
index 00000000..1aef62c3
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/settrim.x
@@ -0,0 +1,115 @@
+include	<imhdr.h>
+include	<imset.h>
+include	"ccdred.h"
+
+# SET_TRIM -- Set the trim parameters.
+#
+#   1.  Return immediately if the trim correction is not requested or
+#	if the image has been previously corrected.
+#   2.	Determine the trim section.  This may be specifed directly or
+#	indirectly through the image header or symbol table.
+#   3.  Parse the trim section and apply it to the output image.
+#   4.  If the image is trimmed then log the operation and reset the output
+#	image size.
+
+procedure set_trim (ccd)
+
+pointer	ccd			# CCD structure
+
+int	xt1, xt2, yt1, yt2
+int	nc, nl, c1, c2, l1, l2
+pointer	sp, str, image
+bool	clgetb(), ccdflag()
+define	log_	10
+
+begin
+	# Check if the user wants this operation or it has been done.
+	if (!clgetb ("trim") || ccdflag (IN_IM(ccd), "trim"))
+	    return
+
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	if (IN_SEC(ccd) != NULL)
+	    goto log_
+
+	# Check trim section.
+	nc = IM_LEN(IN_IM(ccd),1)
+	nl = IM_LEN(IN_IM(ccd),2)
+	c1 = TRIM_C1(ccd)
+	c2 = TRIM_C2(ccd)
+	l1 = TRIM_L1(ccd)
+	l2 = TRIM_L2(ccd)
+	if ((c1 < 1) || (c2 > nc) || (l1 < 1) || (l2 > nl)) {
+	    call salloc (image, SZ_LINE, TY_CHAR)
+	    call imstats (IN_IM(ccd), IM_IMAGENAME, Memc[image], SZ_FNAME)
+	    call sprintf (Memc[str], SZ_LINE,
+		"Error in trim section: image=%s[%d,%d], trimsec=[%d:%d,%d:%d]")
+		call pargstr (Memc[image])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+
+	# If no processing is desired print trim section and return.
+	if (clgetb ("noproc")) {
+	    call eprintf ("  [TO BE DONE] Trim section is [%d:%d,%d:%d].\n")
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call sfree (sp)
+	    return
+	}
+
+	xt1 = max (0, c1 - IN_C1(ccd))
+	xt2 = min (0, c2 - IN_C2(ccd))
+	yt1 = max (0, l1 - IN_L1(ccd))
+	yt2 = min (0, l2 - IN_L2(ccd))
+
+	CCD_C1(ccd) = CCD_C1(ccd) + xt1
+	CCD_C2(ccd) = CCD_C2(ccd) + xt2
+	CCD_L1(ccd) = CCD_L1(ccd) + yt1
+	CCD_L2(ccd) = CCD_L2(ccd) + yt2
+	IN_C1(ccd) = IN_C1(ccd) + xt1
+	IN_C2(ccd) = IN_C2(ccd) + xt2
+	IN_L1(ccd) = IN_L1(ccd) + yt1
+	IN_L2(ccd) = IN_L2(ccd) + yt2
+	OUT_C1(ccd) = IN_C1(ccd) - c1 + 1
+	OUT_C2(ccd) = IN_C2(ccd) - c1 + 1
+	OUT_L1(ccd) = IN_L1(ccd) - l1 + 1
+	OUT_L2(ccd) = IN_L2(ccd) - l1 + 1
+	IM_LEN(OUT_IM(ccd),1) = c2 - c1 + 1
+	IM_LEN(OUT_IM(ccd),2) = l2 - l1 + 1
+
+log_
+	if (IN_SEC(ccd) == NULL) {
+	    CORS(ccd, TRIM) = YES
+	    COR(ccd) = YES
+
+	    call sprintf (Memc[str], SZ_LINE,
+		"Trim data section is [%d:%d,%d:%d]")
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call timelog (Memc[str], SZ_LINE)
+	    call ccdlog (IN_IM(ccd), Memc[str])
+	    call hdmpstr (OUT_IM(ccd), "trim", Memc[str])
+	} else {
+	    CORS(ccd, TRIM) = NO
+	    COR(ccd) = YES
+
+	    call sprintf (Memc[str], SZ_LINE,
+		"Trim multiple overscan sections")
+	    call timelog (Memc[str], SZ_LINE)
+	    call ccdlog (IN_IM(ccd), Memc[str])
+	    call hdmpstr (OUT_IM(ccd), "trim", Memc[str])
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/setzero.x b/noao/imred/quadred/src/ccdproc/setzero.x
new file mode 100644
index 00000000..610aeee7
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/setzero.x
@@ -0,0 +1,141 @@
+# Copyright(c) 1986 Association of Universities for Research in Astronomy Inc.
+
+include	<imhdr.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+# SET_ZERO -- Set parameters for zero level correction.
+#   1.  Return immediately if the zero level correction is not requested or
+#	if the image has been previously corrected.
+#   2.	Get the zero level correction image.  Return an error if not found.
+#   3.	If the zero level image has not been processed call ZEROPROC.
+#   4.	Set the processing flag.
+#   5.  Log the operation (to user, logfile, and output image header).
+
+procedure set_zero (ccd)
+
+pointer	ccd			# CCD structure
+
+int	nscan, nc, nl, c1, c2, cs, l1, l2, ls, data_c1, ccd_c1, data_l1, ccd_l1
+pointer	sp, str, image, im, ccd_cache()
+bool	clgetb(), ccdflag(), ccdcheck()
+int	ccdtypei(), ccdnscan()
+errchk	cal_image, ccd_cache, ccdproc
+
+begin
+	# Check if the user wants this operation or it has been done.
+	if (!clgetb ("zerocor") || ccdflag (IN_IM(ccd), "zerocor"))
+	    return
+
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the zero level correction image.
+	if (clgetb ("scancor"))
+	    nscan = ccdnscan (IN_IM(ccd), ccdtypei(IN_IM(ccd)))
+	else
+	    nscan = 1
+	call cal_image (IN_IM(ccd), ZERO, nscan, Memc[image], SZ_FNAME)
+
+	# If no processing is desired print zero correction image and return.
+	if (clgetb ("noproc")) {
+	    call eprintf ("  [TO BE DONE] Zero level correction image is %s.\n")
+		call pargstr (Memc[image])
+	    call sfree (sp)
+	    return
+	}
+
+	# Map the image and return on an error.
+	# Process the zero image if necessary.
+	# If nscan > 1 then the zero may not yet exist so create it
+	# from the unscanned zero.
+
+	iferr (im = ccd_cache (Memc[image], ZERO)) {
+	    call cal_image (IN_IM(ccd), ZERO, 1, Memc[str], SZ_LINE)
+	    im = ccd_cache (Memc[str], ZERO)
+	    if (ccdcheck (im, ZERO)) {
+		call ccd_flush (im)
+		call ccdproc (Memc[str], ZERO)
+	    }
+	    call scancor (Memc[str], Memc[image], nscan, INDEF)
+	    im = ccd_cache (Memc[image], ZERO)
+	}
+
+	if (ccdcheck (im, ZERO)) {
+	    call ccd_flush (im)
+	    call ccdproc (Memc[image], ZERO)
+	    im = ccd_cache (Memc[image], ZERO)
+	}
+
+	# Set the processing parameters in the CCD structure.
+	nc = IM_LEN(im,1)
+	nl = IM_LEN(im,2)
+	c1 = 1
+	c2 = nc
+	l1 = 1
+	l2 = nl
+	cs = 1
+	ls = 1
+	call hdmgstr (im, "datasec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if ((c1<1)||(c2>nc)||(l1<1)||(l2>nl)||(cs!=1)||(ls!=1)) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Data section error: image=%s[%d,%d], datasec=[%d:%d,%d:%d]")
+		call pargstr (Memc[image])
+		call pargi (nc)
+		call pargi (nl)
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+	data_c1 = c1
+	data_l1 = l1
+	call hdmgstr (im, "ccdsec", Memc[str], SZ_FNAME)
+	call ccd_section (Memc[str], c1, c2, cs, l1, l2, ls)
+	if (nc == 1) {
+	    c1 = CCD_C1(ccd)
+	    c2 = CCD_C2(ccd)
+	}
+	if (nl == 1) {
+	    l1 = CCD_L1(ccd)
+	    l2 = CCD_L2(ccd)
+	}
+	ccd_c1 = c1
+	ccd_l1 = l1
+	if ((c1 > CCD_C1(ccd)) || (c2 < CCD_C2(ccd)) ||
+	    (l1 > CCD_L1(ccd)) || (l2 < CCD_L2(ccd))) {
+	    call sprintf (Memc[str], SZ_LINE,
+	        "CCD section error: input=[%d:%d,%d:%d], %s=[%d:%d,%d:%d]")
+		call pargi (CCD_C1(ccd))
+		call pargi (CCD_C2(ccd))
+		call pargi (CCD_L1(ccd))
+		call pargi (CCD_L2(ccd))
+		call pargstr (Memc[image])
+		call pargi (c1)
+		call pargi (c2)
+		call pargi (l1)
+		call pargi (l2)
+	    call error (0, Memc[str])
+	}
+
+	ZERO_IM(ccd) = im
+	ZERO_C1(ccd) = CCD_C1(ccd) - ccd_c1 + data_c1
+	ZERO_C2(ccd) = CCD_C2(ccd) - ccd_c1 + data_c1
+	ZERO_L1(ccd) = CCD_L1(ccd) - ccd_l1 + data_l1
+	ZERO_L2(ccd) = CCD_L2(ccd) - ccd_l1 + data_l1
+
+	CORS(ccd, ZEROCOR) = Z
+	COR(ccd) = YES
+
+	# Log the operation.
+	call sprintf (Memc[str], SZ_LINE, "Zero level correction image is %s")
+	    call pargstr (Memc[image])
+	call timelog (Memc[str], SZ_LINE)
+	call ccdlog (IN_IM(ccd), Memc[str])
+	call hdmpstr (OUT_IM(ccd), "zerocor", Memc[str])
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/t_ccdproc.x b/noao/imred/quadred/src/ccdproc/t_ccdproc.x
new file mode 100644
index 00000000..8d256046
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/t_ccdproc.x
@@ -0,0 +1,155 @@
+include	<imhdr.h>
+include	<error.h>
+include	"ccdred.h"
+include	"ccdtypes.h"
+
+define	CACHEUNIT	1000000.	# Units of max_cache parameter
+
+# T_CCDPROC -- Process CCD images
+#
+# This is the main procedure for processing CCD images.  The images are
+# corrected for bad pixels, overscan levels, zero levels, dark counts,
+# flat field response, illumination errors, and fringe response.  They
+# may also be trimmed.  The input is a list of images to be processed.
+# Each image must match any image type requested.  The checking of
+# whether to apply each correction, getting the required parameters, and
+# logging the operations is left to separate procedures, one for each
+# correction.  The actual processing is done by a specialized procedure
+# designed to be very efficient.  These procedures may also process
+# calibration images if necessary.  There are two data type paths; one
+# for short pixel types and one for all other pixel types (usually
+# real).
+
+procedure t_ccdproc ()
+
+int	list			# List of CCD images to process
+int	ccdtype			# CCD image type
+int	interactive		# Fit overscan interactively?
+int	max_cache		# Maximum image cache size
+
+bool	clgetb()
+real	clgetr()
+int	imtopenp(), imtgetim(), imtlen()
+pointer	sp, input, output, str, in, out, ccd
+errchk	set_input, set_output, ccddelete, cal_open
+errchk	set_fixpix, set_zero, set_dark, set_flat, set_illum, set_fringe
+
+begin
+	call smark (sp)
+	call salloc (input, SZ_FNAME, TY_CHAR)
+	call salloc (output, SZ_FNAME, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the list and instrument translation file.  Open the translation
+	# file.  Initialize the interactive flag and the calibration images.
+
+	list = imtopenp ("images")
+	call clgstr ("instrument", Memc[input], SZ_FNAME)
+	call hdmopen (Memc[input])
+	call set_interactive ("", interactive)
+	call cal_open (list)
+	if (imtlen (list) < 3)
+	    max_cache = 0.
+	else
+	    max_cache = CACHEUNIT * clgetr ("max_cache")
+	call ccd_open (max_cache)
+
+	# Process each image.
+	while (imtgetim (list, Memc[input], SZ_FNAME) != EOF) {
+	    if (clgetb ("noproc")) {
+		call printf ("%s:\n")
+		    call pargstr (Memc[input])
+	    }
+	    call set_input (Memc[input], in, ccdtype)
+	    if (in == NULL)
+		next
+
+	    # Use a temporary image for output which will replace the input
+	    # image after processing.
+
+	    call mktemp ("tmp", Memc[output], SZ_FNAME)
+	    call set_output (in, out, Memc[output])
+
+	    # Set processing parameters applicable to all images.
+	    call set_proc (in, out, ccd)
+	    call set_sections (ccd)
+	    call set_trim (ccd)
+	    call set_fixpix (ccd)
+	    call set_overscan (ccd)
+
+	    # Set processing parameters for the standard CCD image types.
+	    switch (ccdtype) {
+	    case ZERO:
+	    case DARK:
+	        call set_zero (ccd)
+	    case FLAT:
+	        call set_zero (ccd)
+	        call set_dark (ccd)
+		CORS(ccd, FINDMEAN) = YES
+		CORS(ccd, MINREP) = YES
+	    case ILLUM:
+	        call set_zero (ccd)
+	        call set_dark (ccd)
+	        call set_flat (ccd)
+	    case OBJECT, COMP:
+	        call set_zero (ccd)
+	        call set_dark (ccd)
+	        call set_flat (ccd)
+		iferr {
+	            call set_illum (ccd)
+	            call set_fringe (ccd)
+		} then
+		    call erract (EA_WARN)
+	    default:
+	        call set_zero (ccd)
+	        call set_dark (ccd)
+	        call set_flat (ccd)
+		iferr {
+		    call set_illum (ccd)
+	            call set_fringe (ccd)
+	        } then
+		    call erract (EA_WARN)
+		CORS(ccd, FINDMEAN) = YES
+	    }
+
+	    # Do the processing if the COR flag is set.
+
+	    if (COR(ccd) == YES) {
+		call doproc (ccd)
+		call set_header (ccd)
+
+		# Replace the input image by the corrected image.
+	        call imunmap (in)
+	        call imunmap (out)
+		iferr (call ccddelete (Memc[input])) {
+		    call imdelete (Memc[output])
+		    call error (1,
+			"Can't delete or make backup of original image")
+		}
+	        call imrename (Memc[output], Memc[input])
+	    } else {
+		# Delete the temporary output image leaving the input unchanged.
+	        call imunmap (in)
+	        iferr (call imunmap (out))
+		    ;
+		iferr (call imdelete (Memc[output]))
+		    ;
+	    }
+	    call free_proc (ccd)
+
+	    # Do special processing on certain image types.
+	    switch (ccdtype) {
+	    case ZERO:
+		call readcor (Memc[input])
+	    case FLAT:
+		call ccdmean (Memc[input])
+	    }
+	}
+
+	# Finish up.
+	call hdmclose ()
+	call imtclose (list)
+	call cal_close ()
+	call ccd_close ()
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/timelog.x b/noao/imred/quadred/src/ccdproc/timelog.x
new file mode 100644
index 00000000..7a8d969f
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/timelog.x
@@ -0,0 +1,29 @@
+include	<time.h>
+
+
+# TIMELOG -- Prepend a time stamp to the given string.
+#
+# For the purpose of a history logging prepend a short time stamp to the
+# given string.  Note that the input string is modified.
+
+procedure timelog (str, max_char)
+
+char	str[max_char]		# String to be time stamped
+int	max_char		# Maximum characters in string
+
+pointer	sp, time, temp
+long	clktime()
+
+begin
+	call smark (sp)
+	call salloc (time, SZ_DATE, TY_CHAR)
+	call salloc (temp, max_char, TY_CHAR)
+
+	call cnvdate (clktime(0), Memc[time], SZ_DATE)
+	call sprintf (Memc[temp], max_char, "%s %s")
+	    call pargstr (Memc[time])
+	    call pargstr (str)
+	call strcpy (Memc[temp], str, max_char)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/ccdproc/x_quadred.x b/noao/imred/quadred/src/ccdproc/x_quadred.x
new file mode 100644
index 00000000..a603d0d5
--- /dev/null
+++ b/noao/imred/quadred/src/ccdproc/x_quadred.x
@@ -0,0 +1 @@
+task	ccdproc		= t_ccdproc
diff --git a/noao/imred/quadred/src/mkpkg b/noao/imred/quadred/src/mkpkg
new file mode 100644
index 00000000..bd2bdbc0
--- /dev/null
+++ b/noao/imred/quadred/src/mkpkg
@@ -0,0 +1,4 @@
+update:
+	$call update@ccdproc
+	$call update@quad
+	;
diff --git a/noao/imred/quadred/src/quad/Revisions b/noao/imred/quadred/src/quad/Revisions
new file mode 100644
index 00000000..55b490ed
--- /dev/null
+++ b/noao/imred/quadred/src/quad/Revisions
@@ -0,0 +1,92 @@
+---------------------------------------+--------------------------------------
+	     Revisions started with version 1.1 of the QUAD package
+				   19/Mar/93
+
+                  This package was written by Steve Heathcote!
+---------------------------------------+--------------------------------------
+
+quadgeom.x
+	Modified call to the ccd_section() routine (SH 19/Mar/93).
+
+ccdtypes.h
+ccdtypes.x
+ccdgetparam.x
+	Added routines to retrieve the image type from the image header,
+	and added special case to translate the image type to the
+	corresponding package name in ccdgetparam() (SH 19/May/93).
+
+quadproc.cl
+	Added check to see if image is of type to be processed (SH 24/May/93).
+
+mkpkg
+quad.cl
+quadscale.x
+x_quad.x
+	Installed QUADSCALE task (SH,PG 24/May/93).
+
+
+________________________________________________________________________________
+			Version 2.0 29 March 94
+
+________________________________________________________________________________
+
+quadproc.cl
+qproc.cl
+	Fitting parameters adjusted interactively where not being saved if
+	quadproc aborted at a later stage. In interactive mode these parameters
+	are now written in qproc after each image has been processed and are
+	updated on disk. (SRH 30/Mar/94)
+
+quadproc.cl
+	When running with noproc+, if the calibration images supplied in the
+	input list, and these have already been processed through [OT] task 
+	would complain that the calibration images where missing when the test
+	for second stage [ZF...] procesing was performed. Added calibration 
+	images to list to be considered.n this case.  This means that the 
+	calibration images may appear twice in the output list but ....
+	(SRH 30/Mar/94)
+
+quadproc.cl
+	complained about missing calibration images if the process flags
+	where set and no calibrations where specified, even when no images in
+	the list required the calibration step (e.g. all were zeros). Switched
+	off the check for existance in the qpcalimage call. This means the
+	task will not report the absence of required calibration images until
+	they come to be used but ccdproc does that too.  (SRH 30/Mar/94)
+
+ccddb/ctio/instruments.men
+	  /Xfccd_f1.dat
+	  /Xfccd_f2.dat
+	  /Xfccd_bith.dat
+	Added specific instrument files for the different filter subsets.
+	(SRH 30/Mar/94)
+
+qghdr2.x, quadsections.x
+	All quadrants in reduced images were being flagged as phantoms
+	causing quadsections to return no sections. (SRH 10/Jun/94)
+
+quad/ccdproc.par
+	Updated for V2.11.2.  This should be backwards compatible.
+	(10/8/99, Valdes)
+
+________________________________________________________________________________
+			Version 2.1 29 October 99
+
+________________________________________________________________________________
+
+qnoproc.cl
+qproc.cl
+	Removed explicit dependence on "imh".  The image extension is that
+	given by the imtype environment variable.  (FV 20/Oct/99)
+
+________________________________________________________________________________
+			Version 2.2 20 June 00
+
+________________________________________________________________________________
+
+qnoproc.cl
+qproc.cl
+	Changed "len" to "i" in the clause that is executed when
+	imtype contains a ','.  This caused the error
+	"Attempt to access undefined local variable `len'.
+	(6/20/00, Valdes)
diff --git a/noao/imred/quadred/src/quad/ccd.dat b/noao/imred/quadred/src/quad/ccd.dat
new file mode 100644
index 00000000..9ed9a970
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccd.dat
@@ -0,0 +1,27 @@
+# CCD.DAT -- Instrument file to be used with ccdred when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+#subset			filters
+#subset			filter1
+subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		other
+COMPARISON		other
+ZERO			zero			# New software
+#BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
+FOCUS			object
diff --git a/noao/imred/quadred/src/quad/ccddb/ctio/cfccd_both.dat b/noao/imred/quadred/src/quad/ccddb/ctio/cfccd_both.dat
new file mode 100644
index 00000000..37991738
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccddb/ctio/cfccd_both.dat
@@ -0,0 +1,27 @@
+# CFCCD.DAT -- Instrument file to be used with quad when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+subset			filters
+#subset			filter1
+#subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/quadred/src/quad/ccddb/ctio/cfccd_f1.dat b/noao/imred/quadred/src/quad/ccddb/ctio/cfccd_f1.dat
new file mode 100644
index 00000000..68cd2063
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccddb/ctio/cfccd_f1.dat
@@ -0,0 +1,27 @@
+# CFCCD.DAT -- Instrument file to be used with quad when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+#subset			filters
+subset			filter1
+#subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/quadred/src/quad/ccddb/ctio/cfccd_f2.dat b/noao/imred/quadred/src/quad/ccddb/ctio/cfccd_f2.dat
new file mode 100644
index 00000000..c4d03cb8
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccddb/ctio/cfccd_f2.dat
@@ -0,0 +1,27 @@
+# CFCCD.DAT -- Instrument file to be used with quad when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+#subset			filters
+#subset			filter1
+subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/quadred/src/quad/ccddb/ctio/csccd.dat b/noao/imred/quadred/src/quad/ccddb/ctio/csccd.dat
new file mode 100644
index 00000000..000f8c07
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccddb/ctio/csccd.dat
@@ -0,0 +1,23 @@
+# CCD.DAT -- Instrument file to be used with ccdred when reducing spectroscopic
+# data obtained with ArCon.
+
+subset			none
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		object
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/quadred/src/quad/ccddb/ctio/echccd.dat b/noao/imred/quadred/src/quad/ccddb/ctio/echccd.dat
new file mode 100644
index 00000000..90d08173
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccddb/ctio/echccd.dat
@@ -0,0 +1,23 @@
+# ECHCCD.DAT -- Instrument file to be used with ccdred when reducing echelle
+# spectroscopic data obtained with ArCon.
+
+subset			none
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
+FOCUS			object
diff --git a/noao/imred/quadred/src/quad/ccddb/ctio/instruments.men b/noao/imred/quadred/src/quad/ccddb/ctio/instruments.men
new file mode 100644
index 00000000..144c41d5
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccddb/ctio/instruments.men
@@ -0,0 +1,9 @@
+cfccd_f1	- Cassegrain focus CCD direct subset=filter1
+cfccd_f2	- Cassegrain focus CCD direct subset=filter2
+cfccd_both	- Cassegrain focus CCD direct subset=filters
+csccd		- Cassegrain focus spectroscopy
+echccd		- Echelle spectroscopy
+nfccd		- Newtonian focus CCD direct (Schmidt)
+pfccd_f1	- Prime focus CCD direct subset=filter1
+pfccd_f2	- Prime focus CCD direct subset=filter2
+pfccd_both	- Prime focus CCD direct subset=filters
diff --git a/noao/imred/quadred/src/quad/ccddb/ctio/nfccd.dat b/noao/imred/quadred/src/quad/ccddb/ctio/nfccd.dat
new file mode 100644
index 00000000..06a173cf
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccddb/ctio/nfccd.dat
@@ -0,0 +1,23 @@
+# NFCCD.DAT -- Instrument file to be used with ccdred when reducing direct
+# imageing data obtained with ArCon.
+
+subset			filter1
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/quadred/src/quad/ccddb/ctio/pfccd_both.dat b/noao/imred/quadred/src/quad/ccddb/ctio/pfccd_both.dat
new file mode 100644
index 00000000..ac8e03a6
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccddb/ctio/pfccd_both.dat
@@ -0,0 +1,27 @@
+# PFCCD.DAT -- Instrument file to be used with quad when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+subset			filters
+#subset			filter1
+#subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/quadred/src/quad/ccddb/ctio/pfccd_f1.dat b/noao/imred/quadred/src/quad/ccddb/ctio/pfccd_f1.dat
new file mode 100644
index 00000000..9893d7f1
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccddb/ctio/pfccd_f1.dat
@@ -0,0 +1,27 @@
+# PFCCD.DAT -- Instrument file to be used with quad when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+#subset			filters
+subset			filter1
+#subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/quadred/src/quad/ccddb/ctio/pfccd_f2.dat b/noao/imred/quadred/src/quad/ccddb/ctio/pfccd_f2.dat
new file mode 100644
index 00000000..89028468
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccddb/ctio/pfccd_f2.dat
@@ -0,0 +1,27 @@
+# PFCCD.DAT -- Instrument file to be used with quad when reducing direct
+# imageing data obtained with ArCon.
+
+# Uncomment ONE of the following 3 lines to select the
+# header keyword to use when grouping images into subsets by filter.
+#subset			filters
+#subset			filter1
+subset			filter2
+
+exptime 		exptime
+darktime		darktime
+imagetyp		imagetyp
+biassec			biassec
+datasec			datasec
+trimsec			trimsec
+fixfile			fixfile
+ 
+FOCUS			object
+OBJECT			object
+DARK			dark
+"PROJECTOR FLAT"	flat
+"SKY FLAT"		flat
+COMPARISON		other
+ZERO			zero			# New software
+BIAS			zero			# Old software
+"DOME FLAT"		flat
+MASK			other
diff --git a/noao/imred/quadred/src/quad/ccddelete.par b/noao/imred/quadred/src/quad/ccddelete.par
new file mode 100644
index 00000000..eaa63a22
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccddelete.par
@@ -0,0 +1 @@
+image,s,a,"",,,Image to be delete (backed up)
diff --git a/noao/imred/quadred/src/quad/ccddelete.x b/noao/imred/quadred/src/quad/ccddelete.x
new file mode 100644
index 00000000..8a72796d
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccddelete.x
@@ -0,0 +1,65 @@
+procedure t_ccddelete ()
+
+char	image[SZ_LINE]		# Image to delete (backup)
+
+begin
+
+	call clgstr ("image", image, SZ_LINE)
+	call ccddelete (image)
+end
+
+# CCDDELETE -- Delete an image by renaming it to a backup image.
+#
+#   1.	Get the backup prefix which may be a path name.
+#   2.  If no prefix is specified then delete the image without a backup.
+#   3.  If there is a prefix then make a backup image name.
+#       Rename the image to the backup image name.
+#
+#   The backup image name is formed by prepending the backup prefix to the
+#   image name.  If a previous backup exist append integers to the backup
+#   prefix until a nonexistant image name is created.
+
+procedure ccddelete (image)
+
+char	image[ARB]		# Image to delete (backup)
+
+int	i, imaccess()
+pointer	sp, prefix, backup
+errchk	imdelete, imrename
+
+begin
+	call smark (sp)
+	call salloc (prefix, SZ_FNAME, TY_CHAR)
+	call salloc (backup, SZ_FNAME, TY_CHAR)
+
+	# Get the backup prefix.
+	call clgstr ("backup", Memc[prefix], SZ_FNAME)
+	call xt_stripwhite (Memc[prefix])
+
+	# If there is no prefix then simply delete the image.
+	if (Memc[prefix] == EOS)
+	    call imdelete (image)
+
+	# Otherwise create a backup image name which does not exist and
+	# rename the image to the backup image.
+
+	else {
+	    i = 0
+	    repeat {
+		if (i == 0) {
+	    	    call sprintf (Memc[backup], SZ_FNAME, "%s%s")
+		        call pargstr (Memc[prefix])
+		        call pargstr (image)
+		} else {
+	            call sprintf (Memc[backup], SZ_FNAME, "%s%d%s")
+			call pargstr (Memc[prefix])
+			call pargi (i)
+			call pargstr (image)
+		}
+	        i = i + 1
+	    } until (imaccess (Memc[backup], READ_ONLY) == NO)
+	    call imrename (image, Memc[backup])
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/quad/ccdgetparam.par b/noao/imred/quadred/src/quad/ccdgetparam.par
new file mode 100644
index 00000000..8647c9a9
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdgetparam.par
@@ -0,0 +1,2 @@
+image,s,a,"",,,Image whose parameter is to be fetched
+parameter,s,a,"",,,Parameter to be listed
diff --git a/noao/imred/quadred/src/quad/ccdgetparam.x b/noao/imred/quadred/src/quad/ccdgetparam.x
new file mode 100644
index 00000000..a032b553
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdgetparam.x
@@ -0,0 +1,48 @@
+procedure ccdgetparam ()
+
+char	image[SZ_FNAME]		# Image whose parameter is to be fetched
+char	parameter[SZ_LINE]	# Parameter whose value is required.
+char	instrument[SZ_FNAME]	# CCD intrument file.
+
+char	buffer[SZ_LINE]
+pointer	im
+
+pointer	immap()
+int	hdmaccf()
+bool	streq()
+
+begin
+
+	call clgstr ("image", image, SZ_FNAME)
+	im = immap (image, READ_ONLY, 0)
+
+	call clgstr ("instrument", instrument, SZ_FNAME)
+	call hdmopen (instrument)
+
+	call clgstr ("parameter", parameter, SZ_LINE)
+
+	# Handle special cases where we must translate the parameter value
+	# to the corresponding package name.
+	if (streq (parameter, "imagetyp")) {
+	    call ccdtypes (im, buffer, SZ_LINE)
+	    call printf ("%s\n")
+		call pargstr (buffer)
+
+	} else if (streq (parameter, "subset")) {
+	    call ccdsubset (im, buffer, SZ_LINE)
+	    call printf ("%s\n")
+		call pargstr (buffer)
+
+	} else {
+
+	    if (hdmaccf (im, parameter) == NO) {
+		call printf ("UNDEFINED!\n")
+	    } else {
+		call hdmgstr (im, parameter, buffer, SZ_LINE)
+		call printf ("%s\n")
+		    call pargstr (buffer)
+	    }
+	}
+
+	call imunmap (im)
+end
diff --git a/noao/imred/quadred/src/quad/ccdlog.x b/noao/imred/quadred/src/quad/ccdlog.x
new file mode 100644
index 00000000..61bbff10
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdlog.x
@@ -0,0 +1,42 @@
+
+# CCDLOG -- Log information about the processing with the image name.
+#
+#   1.  If the package "verbose" parameter is set print the string preceded
+#	by the image name.
+#   2.  If the package "logfile" parameter is not null append the string,
+#	preceded by the image name, to the file.
+
+procedure ccdlog (image, str)
+
+char	image[ARB]		# Image name
+char	str[ARB]		# Log string
+
+int	fd, open()
+bool	clgetb()
+pointer	sp, fname
+errchk	open
+
+begin
+	call smark (sp)
+	call salloc (fname, SZ_FNAME, TY_CHAR)
+
+	# Write to the standard error output if "verbose".
+	if (clgetb ("verbose")) {
+	    call eprintf ("%s: %s\n")
+		call pargstr (image)
+		call pargstr (str)
+	}
+
+	# Append to the "logfile" if not null.
+	call clgstr ("logfile", Memc[fname], SZ_FNAME)
+	call xt_stripwhite (Memc[fname])
+	if (Memc[fname] != EOS) {
+	    fd = open (Memc[fname], APPEND, TEXT_FILE)
+	    call fprintf (fd, "%s: %s\n")
+		call pargstr (image)
+		call pargstr (str)
+	    call close (fd)
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/quad/ccdprcselect.par b/noao/imred/quadred/src/quad/ccdprcselect.par
new file mode 100644
index 00000000..453f4b4d
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdprcselect.par
@@ -0,0 +1,4 @@
+input,s,a,"",,,Input image list
+output,s,h,"STDOUT",,,Output image list
+procflag,s,h,"",,,Processing flag for filter action
+ccdtype,s,h,"",,,CCD image type to be listed
diff --git a/noao/imred/quadred/src/quad/ccdprcselect.x b/noao/imred/quadred/src/quad/ccdprcselect.x
new file mode 100644
index 00000000..11b4e2ef
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdprcselect.x
@@ -0,0 +1,90 @@
+# CCD_PRCSELECT -- Filter a list of image names passing on only those that
+# do (or don't) have a specified processing flag set.
+
+include "ccdtypes.h"
+
+define	PROCFLAGS "|fixpix|overscan|trim|zerocor|darkcor|flatcor|illumcor\
+	|fringecor|ccdproc|"
+
+procedure t_ccdprcselect ()
+
+pointer	inlist			#TI List of input image name.
+char	output[SZ_FNAME]	#TI List of output image names.
+char	instrument[SZ_FNAME]	#TI Instrument translation file.
+char	procflag[SZ_LINE]	#TI List of proc flags.
+char	ccdtype[SZ_LINE]	#TI ccdtype to select.
+
+int	flag, ip, type
+char	image[SZ_LINE], buffer[SZ_LINE]
+pointer	fdout, im
+
+int	strdic(), imtopenp(), imtgetim(), hdmaccf(), ctowrd(), imaccess()
+int	ccdtypei()
+
+pointer	open(), immap()
+
+begin
+	# Open input and output image lists
+	inlist = imtopenp ("input")
+	call clgstr ("output", output, SZ_LINE)
+	fdout = open (output, APPEND, TEXT_FILE)
+
+	# Open instrument file
+	call clgstr    ("instrument",  instrument,  SZ_FNAME)
+	call hdmopen   (instrument)
+
+	# Get processing flag. 
+	# If the first character is "!" pass all images for which the specified
+	# flag is not set. If the processing flag is "" we pass al images.
+	flag = 0
+	call clgstr ("procflag", buffer, SZ_LINE)
+	ip = 1
+	if (ctowrd (buffer, ip, procflag, SZ_LINE) != 0) {
+	    if (procflag[1] == '!') {
+		flag =  -1 * strdic (procflag[2], procflag, SZ_LINE, PROCFLAGS)
+	    } else {
+		flag = strdic (procflag, procflag, SZ_LINE, PROCFLAGS)
+	    }
+	    if (flag == 0)
+		call error (0, "Unknown processing flag")
+	}
+
+	# Get ccdtype to select.
+	call clgstr   ("ccdtype", ccdtype, SZ_LINE)
+	type = strdic (ccdtype, ccdtype, SZ_LINE, CCDTYPES)
+
+	while (imtgetim (inlist, image, SZ_LINE) != EOF) {
+
+	    # Silently skip any non-existant images
+	    if (imaccess (image, READ_ONLY) == NO)
+		next
+
+	    im = immap (image, READ_ONLY, 0)
+
+	    if ((ccdtype[1] != EOS) && (type != ccdtypei (im))) {
+		call imunmap (im)
+		next
+	    }
+
+	    if (flag < 0) {
+		if (hdmaccf (im, procflag) == NO) {
+		    call fprintf (fdout, "%s\n")
+			call pargstr (image)
+		}
+	    } else if (flag > 0) {
+		if (hdmaccf (im, procflag) == YES) {
+		    call fprintf (fdout, "%s\n")
+			call pargstr (image)
+		}
+	    } else {
+		call fprintf (fdout, "%s\n")
+		    call pargstr (image)
+	    }
+	    call imunmap (im)
+	}
+
+	# Tidy up
+	call close (fdout)
+	call hdmclose ()
+	call imtclose (inlist)
+end
diff --git a/noao/imred/quadred/src/quad/ccdproc.par b/noao/imred/quadred/src/quad/ccdproc.par
new file mode 100644
index 00000000..01065e28
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdproc.par
@@ -0,0 +1,43 @@
+images,s,a,"",,,List of CCD images to correct
+output,s,h,"",,,List of output CCD images
+ccdtype,s,h,"other",,,CCD image type to correct
+max_cache,i,h,0,0,,Maximum image caching memory (in Mbytes)
+noproc,b,h,no,,,"List processing steps only?
+"
+fixpix,b,h,no,,,Fix bad CCD lines and columns?
+overscan,b,h,no,,,Apply overscan strip correction?
+trim,b,h,no,,,Trim the image?
+zerocor,b,h,no,,,Apply zero level correction?
+darkcor,b,h,no,,,Apply dark count correction?
+flatcor,b,h,no,,,Apply flat field correction?
+illumcor,b,h,no,,,Apply illumination correction?
+fringecor,b,h,no,,,Apply fringe correction?
+readcor,b,h,no,,,Convert zero level image to readout correction?
+scancor,b,h,no,,,"Convert flat field image to scan correction?
+"
+readaxis,s,h,"line","column|line",, Read out axis (column|line)
+fixfile,s,h,"",,,File describing the bad lines and columns
+biassec,s,h,"",,,Overscan strip image section
+trimsec,s,h,"",,,Trim data section
+zero,s,h,"",,,Zero level calibration image
+dark,s,h,"",,,Dark count calibration image
+flat,s,h,"",,,Flat field images
+illum,s,h,"",,,Illumination correction images
+fringe,s,h,"",,,Fringe correction images
+minreplace,r,h,1.,,,Minimum flat field value
+scantype,s,h,"shortscan","shortscan|longscan",,Scan type (shortscan|longscan)
+nscan,i,h,1,1,,"Number of short scan lines
+"
+interactive,b,h,no,,,Fit overscan interactively?
+function,s,h,"legendre",,,Fitting function
+order,i,h,1,1,,Number of polynomial terms or spline pieces
+sample,s,h,"*",,,Sample points to fit
+naverage,i,h,1,,,Number of sample points to combine
+niterate,i,h,1,0,,Number of rejection iterations
+low_reject,r,h,3.,0.,,Low sigma rejection factor
+high_reject,r,h,3.,0.,,High sigma rejection factor
+grow,r,h,0.,0.,,"Rejection growing radius
+"
+backup,s,h,"",,,Backup directory or prefix
+logfile,s,h,"",,,Text log file
+verbose,b,h,no,,,Print log information to the standard output?
diff --git a/noao/imred/quadred/src/quad/ccdsection.par b/noao/imred/quadred/src/quad/ccdsection.par
new file mode 100644
index 00000000..ff8ae7ed
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdsection.par
@@ -0,0 +1 @@
+section,s,a,,,,Section to decode
diff --git a/noao/imred/quadred/src/quad/ccdsection.x b/noao/imred/quadred/src/quad/ccdsection.x
new file mode 100644
index 00000000..d6b0d6a7
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdsection.x
@@ -0,0 +1,119 @@
+include	<ctype.h>
+
+# CCD_SECTION -- Parse a 2D image section into its elements.
+# 1. The default values must be set by the caller.
+# 2. A null image section is OK.
+# 3. The first nonwhitespace character must be '['.
+# 4. The last interpreted character must be ']'.
+#
+# This procedure should be replaced with an IMIO procedure at some
+# point.
+
+
+# Cl callable entry point
+
+procedure t_ccdsection ()
+
+char	section[SZ_LINE]		#T Section to parse
+
+int	x1, x2, y1, y2, xstep, ystep
+
+begin
+	call clgstr ("section", section, SZ_LINE)
+	call ccd_section (section, x1, x2, xstep, y1, y2, ystep)
+	call printf ("%d %d %d %d \n")
+	    call pargi (x1)
+	    call pargi (x2)
+	    call pargi (y1)
+	    call pargi (y2)
+end
+
+procedure ccd_section (section, x1, x2, xstep, y1, y2, ystep)
+
+char	section[ARB]		# Image section
+int	x1, x2, xstep		# X image section parameters
+int	y1, y2, ystep		# X image section parameters
+
+int	i, ip, a, b, c, temp, ctoi()
+define	error_	99
+
+begin
+	# Decode the section string.
+	ip = 1
+	while (IS_WHITE(section[ip]))
+	    ip = ip + 1
+	if (section[ip] == '[')
+	    ip = ip + 1
+	else if (section[ip] == EOS)
+	    return
+	else
+	    goto error_
+
+	do i = 1, 2 {
+	    while (IS_WHITE(section[ip]))
+	        ip = ip + 1
+
+	    # Default values
+	    if (i == 1) {
+	        a = x1
+	        b = x2
+	        c = xstep
+	    } else {
+	        a = y1
+	        b = y2
+	        c = ystep
+	    }
+
+	    # Get a:b:c.  Allow notation such as "-*:c"
+	    # (or even "-:c") where the step is obviously negative.
+
+	    if (ctoi (section, ip, temp) > 0) {			# a
+		a = temp
+	        if (section[ip] == ':') {	
+		    ip = ip + 1
+		    if (ctoi (section, ip, b) == 0)		# a:b
+		        goto error_
+	        } else
+		    b = a
+	    } else if (section[ip] == '-') {			# -*
+		temp = a
+		a = b
+		b = temp
+	        ip = ip + 1
+	        if (section[ip] == '*')
+		    ip = ip + 1
+	    } else if (section[ip] == '*')			# *
+	        ip = ip + 1
+	    if (section[ip] == ':') {				# ..:step
+	        ip = ip + 1
+	        if (ctoi (section, ip, c) == 0)
+		    goto error_
+	        else if (c == 0)
+		    goto error_
+	    }
+	    if (a > b && c > 0)
+	        c = -c
+
+	    if (i == 1) {
+		x1 = a
+		x2 = b
+		xstep = c
+	    } else {
+		y1 = a
+		y2 = b
+		ystep = c
+	    }
+
+	    while (IS_WHITE(section[ip]))
+	        ip = ip + 1
+	    if (section[ip] == ',')
+		ip = ip + 1
+	}
+
+	if (section[ip] != ']')
+	    goto error_
+
+	return
+error_
+	call error (0, "Error in image section specification")
+end
diff --git a/noao/imred/quadred/src/quad/ccdssselect.par b/noao/imred/quadred/src/quad/ccdssselect.par
new file mode 100644
index 00000000..8499900d
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdssselect.par
@@ -0,0 +1,4 @@
+input,s,a,"",,,Input image list
+output,s,h,"STDOUT",,,Output image list
+subset,s,h,"",,,Subset to be listed
+ccdtype,s,h,"",,,CCD image type to be listed
diff --git a/noao/imred/quadred/src/quad/ccdssselect.x b/noao/imred/quadred/src/quad/ccdssselect.x
new file mode 100644
index 00000000..65a7248f
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdssselect.x
@@ -0,0 +1,73 @@
+# CCDSUBSETSELECT -- Filter a list of image names passing on only those that
+# belong to a specified subset.
+
+include "ccdtypes.h"
+
+procedure t_ccdssselect ()
+
+pointer	inlist			#TI List of input image name.
+char	output[SZ_FNAME]	#TI List of output image names.
+char	instrument[SZ_FNAME]	#TI Instrument translation file.
+char	subset[SZ_LINE]		#TI Subset required.
+char	ccdtype[SZ_LINE]	#TI ccdtype required.
+
+int	type
+char	image[SZ_LINE], buffer[SZ_LINE]
+pointer	fdout, im
+
+int	strdic(), imtopenp(), imtgetim(), ccdtypei(), imaccess()
+pointer	open(), immap()
+bool	strne()
+
+begin
+	# Open input and output image lists
+	inlist = imtopenp ("input")
+	call clgstr ("output", output, SZ_LINE)
+	fdout = open (output, APPEND, TEXT_FILE)
+
+	# Open instrument file
+	call clgstr    ("instrument",  instrument,  SZ_FNAME)
+	call hdmopen   (instrument)
+
+	# Get subset required. 
+	call clgstr ("subset", subset, SZ_LINE)
+
+	# Get ccdtype required.
+	call clgstr   ("ccdtype", ccdtype, SZ_LINE)
+	type = strdic (ccdtype, ccdtype, SZ_LINE, CCDTYPES)
+
+	while (imtgetim (inlist, image, SZ_LINE) != EOF) {
+
+	    # Silently skip non-existant images
+	    if (imaccess (image, READ_ONLY) == NO)
+		next
+
+	    im = immap (image, READ_ONLY, 0)
+
+	    # Skip images of the wrong type
+	    if ((ccdtype[1] != EOS) && (type != ccdtypei (im))) {
+		call imunmap (im)
+		next
+	    }
+	    
+	    # Skip images of the wrong subset
+	    if (subset[1] != EOS) {
+		call ccdsubset (im, buffer, SZ_LINE)
+		if (strne (subset, buffer)) {
+		    call imunmap (im)
+		    next
+		}
+	    }
+
+	    # print names of any images which pass the test.
+	    call fprintf (fdout, "%s\n")
+		call pargstr (image)
+
+	    call imunmap (im)
+	}
+
+	# Tidy up
+	call close (fdout)
+	call hdmclose ()
+	call imtclose (inlist)
+end
diff --git a/noao/imred/quadred/src/quad/ccdsubsets.x b/noao/imred/quadred/src/quad/ccdsubsets.x
new file mode 100644
index 00000000..6152897f
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdsubsets.x
@@ -0,0 +1,92 @@
+# CCDSUBSET -- Return the CCD subset identifier.
+#
+# 1. Get the subset string and search the subset record file for the ID string.
+# 2. If the subset string is not in the record file define a default ID string
+#    based on the first word of the subset string.  If the first word is not
+#    unique append a integer to the first word until it is unique.
+# 3. Add the new subset string and identifier to the record file.
+# 4. Since the ID string is used to generate image names replace all
+#    nonimage name characters with '_'.
+#
+# It is an error if the record file cannot be created or written when needed.
+
+procedure ccdsubset (im, subset, sz_name)
+
+pointer	im			# Image
+char	subset[sz_name]		# CCD subset identifier
+int	sz_name			# Size of subset string
+
+bool	streq()
+int	i, fd, ctowrd(), open(), fscan()
+pointer	sp, fname, str1, str2, subset1, subset2, subset3
+errchk	open
+
+begin
+	call smark (sp)
+	call salloc (fname, SZ_FNAME, TY_CHAR)
+	call salloc (str1, SZ_LINE, TY_CHAR)
+	call salloc (str2, SZ_LINE, TY_CHAR)
+	call salloc (subset1, SZ_LINE, TY_CHAR)
+	call salloc (subset2, SZ_LINE, TY_CHAR)
+	call salloc (subset3, SZ_LINE, TY_CHAR)
+
+	# Get the subset record file and the subset string.
+	call clgstr ("ssfile", Memc[fname], SZ_LINE)
+	call hdmgstr (im, "subset", Memc[str1], SZ_LINE)
+
+	# The default subset identifier is the first word of the subset string.
+	i = 1
+	i = ctowrd (Memc[str1], i, Memc[subset1], SZ_LINE)
+
+	# A null subset string is ok.  If not null check for conflict
+	# with previous subset IDs.
+	if (Memc[str1] != EOS) {
+	    call strcpy (Memc[subset1], Memc[subset3], SZ_LINE)
+
+	    # Search the subset record file for the same subset string.
+	    # If found use the ID string.  If the subset ID has been
+	    # used for another subset string then increment an integer
+	    # suffix to the default ID and check the list again.
+
+	    i = 1
+	    ifnoerr (fd = open (Memc[fname], READ_ONLY, TEXT_FILE)) {
+		while (fscan (fd) != EOF) {
+		    call gargwrd (Memc[str2], SZ_LINE)
+		    call gargwrd (Memc[subset2], SZ_LINE)
+		    if (streq (Memc[str1], Memc[str2])) {
+			i = 0
+			call strcpy (Memc[subset2], Memc[subset1], SZ_LINE)
+			break
+		    } if (streq (Memc[subset1], Memc[subset2])) {
+			call sprintf (Memc[subset1], SZ_LINE, "%s%d")
+			    call pargstr (Memc[subset3])
+			    call pargi (i)
+			i = i + 1
+			call seek (fd, BOF)
+		    }
+		}
+		call close (fd)
+	    }
+
+	    # If the subset is not in the record file add it.
+	    if (i > 0) {
+		fd = open (Memc[fname], APPEND, TEXT_FILE)
+		call fprintf (fd, "'%s'\t%s\n")
+		    call pargstr (Memc[str1])
+		    call pargstr (Memc[subset1])
+		call close (fd)
+	    }
+	}
+
+	# Set the subset ID string and replace magic characters by '_'
+	# since the subset ID is used in forming image names.
+
+	call strcpy (Memc[subset1], subset, sz_name)
+	for (i=1; subset[i]!=EOS; i=i+1)
+	    switch (subset[i]) {
+	    case '-','+','?','*','[',']',' ','\t':
+		subset[i] = '_'
+	    }
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/quad/ccdtypes.h b/noao/imred/quadred/src/quad/ccdtypes.h
new file mode 100644
index 00000000..0d5d4caf
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdtypes.h
@@ -0,0 +1,14 @@
+# Standard CCD image types.
+
+define	CCDTYPES "|object|zero|dark|flat|illum|fringe|other|comp|"
+
+define	NONE		-1
+define	UNKNOWN		0
+define	OBJECT		1
+define	ZERO		2
+define	DARK		3
+define	FLAT		4
+define	ILLUM		5
+define	FRINGE		6
+define	OTHER		7
+define	COMP		8
diff --git a/noao/imred/quadred/src/quad/ccdtypes.x b/noao/imred/quadred/src/quad/ccdtypes.x
new file mode 100644
index 00000000..bf6d29e2
--- /dev/null
+++ b/noao/imred/quadred/src/quad/ccdtypes.x
@@ -0,0 +1,72 @@
+include	"ccdtypes.h"
+
+# CCDTYPES -- Return the CCD type name string.
+# CCDTYPEI -- Return the CCD type code.
+
+
+# CCDTYPES -- Return the CCD type name string.
+
+procedure ccdtypes (im, name, sz_name)
+
+pointer	im			# Image
+char	name[sz_name]		# CCD type name
+int	sz_name			# Size of name string
+
+int	strdic()
+pointer	sp, str
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	# Get the image type string.  If none then return "none".
+	# Otherwise get the corresponding package image type string.
+	# If the image type is unknown return "unknown" otherwise return
+	# the package name.
+
+	call hdmgstr (im, "imagetyp", Memc[str], SZ_LINE)
+	if (Memc[str] == EOS) {
+	    call strcpy ("none", name, sz_name)
+	} else {
+	    call hdmname (Memc[str], name, sz_name)
+	    if (name[1] == EOS)
+		call strcpy (Memc[str], name, sz_name)
+	    if (strdic (name, name, sz_name, CCDTYPES) == UNKNOWN)
+	    	call strcpy ("unknown", name, sz_name)
+	}
+
+	call sfree (sp)
+end
+
+
+# CCDTYPEI -- Return the CCD type code.
+
+int procedure ccdtypei (im)
+
+pointer	im			# Image
+int	ccdtype			# CCD type (returned)
+
+pointer	sp, str1, str2
+int	strdic()
+
+begin
+	call smark (sp)
+	call salloc (str1, SZ_LINE, TY_CHAR)
+	call salloc (str2, SZ_LINE, TY_CHAR)
+
+	# Get the image type and if there is none then return the NONE code.
+	call hdmgstr (im, "imagetyp", Memc[str1], SZ_LINE)
+	if (Memc[str1] == EOS) {
+	    ccdtype = NONE
+
+	# Otherwise get the package type and convert to an image type code.
+	} else {
+	    call hdmname (Memc[str1], Memc[str2], SZ_LINE)
+	    if (Memc[str2] == EOS)
+		call strcpy (Memc[str1], Memc[str2], SZ_LINE)
+	    ccdtype = strdic (Memc[str2], Memc[str2], SZ_LINE, CCDTYPES)
+	}
+
+	call sfree (sp)
+	return (ccdtype)
+end
diff --git a/noao/imred/quadred/src/quad/detpars.par b/noao/imred/quadred/src/quad/detpars.par
new file mode 100644
index 00000000..bbb9f8aa
--- /dev/null
+++ b/noao/imred/quadred/src/quad/detpars.par
@@ -0,0 +1,6 @@
+xskip1,i,h,INDEF,0,,X pixels to skip at start of overscan
+xskip2,i,h,INDEF,0,,X pixels to skip at end of overscan
+xtrim1,i,h,INDEF,0,,X pixels to trim at start of data
+xtrim2,i,h,INDEF,0,,X pixels to trim at end   of data
+ytrim1,i,h,INDEF,0,,Y pixels to trim at start of data
+ytrim2,i,h,INDEF,0,,Y pixels to trim at end   of data
diff --git a/noao/imred/quadred/src/quad/doc/Geometry.fig b/noao/imred/quadred/src/quad/doc/Geometry.fig
new file mode 100644
index 00000000..429d987f
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/Geometry.fig
@@ -0,0 +1,91 @@
+# The following diagrams show the CCD geometry for the different readout modes.
+#
+# Single readout:
+#				G
+#		<-------------------------------->
+#			    A		    F	 
+#		<----------------------><-------->
+#		 B 	     	     C   D      E
+#		<->                 <--><>      <>
+#	^   ^	+-----------------------+--------+  ^	^
+#	|   |	|   		     	| 	 |  | e	|
+#	| c |	|   		     	|--------|  v  	|
+#	|   v	|  +----------------+   ||      ||      |
+#	|    	|  |		    |	||  o	||    	|
+#	|    	|  |		    |	||  v	||    	|
+#	|    	|  |		    |	||  e	||    	|
+#     a	|    	|  |		    |	||  r	||      | f
+#	|    	|  |		    |	||  s	||    	|
+#	|    	|  |		    |	||  c	||    	|
+#	|    	|  |		    |	||  a	||    	|
+#	|    	|  +----------------+   ||  n   ||    	|
+#	|   ^	|   		     	|--------|   	|
+#	| b |   |                       |        |  ^	|
+#	|   |	|   		     	| 	 |  | d	|
+#	v   V	*-----------------------+--------+  v	v
+#
+# Quad readout (single frame):
+#				G'
+#		<--------------------------------->
+#		     A/2    F/2  F/2      A/2
+#		<---------><---><---><----------->
+#		 B 	   D   2*E   D         C
+#		<->        <>  < >  <> 	     <-->
+#	^   ^	*----------+----.----+------------* ^	^
+#	|   |	|   	   |    .    |            | | e	|
+#	| c |	|   	   |----.----|            | v	|
+#	|   v	|  +-------+|  |.|  |+--------+   |   	|
+#  a/2	|    	|  |	   ||o |.|o ||        |   |  	| f/2
+#	|    	|  |   3   ||v |.|v ||   4    |   |   	|
+#	|    	|  |	   ||  |.|  ||        |   |  	|
+#	|    	|  |	   ||3 |.|4 ||        |   |  	|
+#       V    	...................................   	v
+#	^    	|  |	   ||o |.|o ||        |   |  	^
+#	|    	|  |   1   ||v |.|v ||   2    |   |  	|
+#	|    	|  |	   ||  |.|  ||        |   |   	|
+#   a/2	|    	|  +-------+|1 |.|2 |+--------+   |  	| f/2
+#	|   ^	|          ||  |.|  ||            |  	|
+#	| b |	|   	   |----.----|            | ^	|
+#	|   |	|   	   |    .    |            | | d	|
+#	v   v	*----------+----.----+------------* v	V
+#
+#
+# Quad readout (four frames):
+#
+#		       G"			G"
+#		<-------------->        <---------------->
+#		     A/2     F/2         F/2      A/2
+#		<---------><---->       <----><---------->
+#		 B 	   D   E        E   D          C
+#		<->        <>  <>	<>  <>	      <-->
+#	^   ^	*----------+----+	+----+------------* ^	^
+#	|   |	|   	   |    |	|    |            | | e	|
+#	| c |	|   	   |----|	|----|            | v	|
+#   a/2	|   v	|  +-------+|  ||	||  |+--------+   | ^ 	|
+#	|    	|  |	   ||o ||	||o ||        |   | |	| f/2
+#	|    	|  |   3   ||v ||	||v ||   4    |   | |	|
+#	|    	|  |	   ||  ||	||  ||        |   | |	|
+#	V    	|  |	   ||3 ||	||4 ||        |   | |	|
+#		+---------------+       +-----------------+ v	v
+#
+#
+#            	+---------------+	+-----------------+ ^	^
+#	^    	|  |	   ||o ||	||o ||        |   | |	|
+#	|    	|  |   1   ||v ||	||v ||   2    |   | |	|
+#	|    	|  |	   ||  ||	||  ||        |   | |	|
+#	|    	|  +-------+|1 ||	||2 |+--------+   | |	| f/2
+#   a/2	|   ^	|          ||  ||	||  ||            | v	|
+#	| b |	|   	   |----|	|----|            | ^	|
+#	|   |	|   	   |    |	|    |            | | d	|
+#	v   v	*----------+----+	+----+------------* v	v
+#
+# Where
+#		A  = xdata			a = ydata
+#		B  = txskip1			b = tyskip1
+#		C  = txskip2			c = tyskip2
+#		D  = bxskip1			d = byskip1
+#		E  = bxskip2			e = byskip2
+#		F  = xover			f = yover = a
+#		G  =  A + F
+#		G' =  A + F
+#		G" = (A + F) / 2
diff --git a/noao/imred/quadred/src/quad/doc/badpiximage.hlp b/noao/imred/quadred/src/quad/doc/badpiximage.hlp
new file mode 100644
index 00000000..46e13160
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/badpiximage.hlp
@@ -0,0 +1,51 @@
+.help badpiximage Jun87 noao.imred.ccdred
+.ih
+NAME
+badpiximage -- Create a bad pixel mask image from a bad pixel file
+.ih
+USAGE
+badpiximage fixfile template image
+.ih
+PARAMETERS
+.ls fixfile
+Bad pixel file.
+.le
+.ls template
+Template image used to define the size of the bad pixel mask image.
+.le
+.ls image
+Bad pixel mask image to be created.
+.le
+.ls goodvalue = 1
+Integer value assigned to the good pixels.
+.le
+.ls badvalue = 0
+Integer value assigned to the bad pixels.
+.le
+.ih
+DESCRIPTION
+A bad pixel mask image is created from the specified bad pixel file.
+The format of the bad pixel file is that used by \fBccdproc\fR to
+correct CCD defects (see instruments).  The bad pixel image is of pixel type short and
+has the value given by the parameter \fBgoodvalue\fR for the good
+pixels and the value given by the parameter \fBbadvalue\fR for the bad pixels.
+The image size and header parameters are taken from the specified
+template image.  The bad pixel mask image may be used to view the
+location of the bad pixels and blink against an data image using an
+image display, to mask or flag bad pixels later by image arithmetic,
+and to propagate the positions of the bad pixels through the
+reductions.
+.ih
+EXAMPLES
+1. To make a bad pixel mask image from the bad pixel file "cryocambp.dat"
+using the image "ccd005" as the template:
+
+	cl> badpiximage cryocambp.dat ccd005 cryocambp
+
+2. To make the bad pixel mask image with good values of 0 and bad values of 1:
+
+	cl> badpixim cryomapbp.dat ccd005 cryocambp good=0 bad=1
+.ih
+SEE ALSO
+ccdproc, instruments
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/ccdgeometry.hlp b/noao/imred/quadred/src/quad/doc/ccdgeometry.hlp
new file mode 100644
index 00000000..c01a09c8
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/ccdgeometry.hlp
@@ -0,0 +1,70 @@
+.help ccdgeometry Sep87 noao.imred.ccdred
+.ih
+NAME
+ccdgeometry - Discussion of CCD geometry and header parameters
+.ih
+DESCRIPTION
+The \fBccdred\fR package maintains and updates certain geometry
+information about the images.  This geometry is described by four image
+header parameters which may be present.  These are defined below by the
+parameter names used in the package.  Note that these names may be
+different in the image header using the image header translation
+feature of the package.
+
+.ls DATASEC
+The section of the image containing the CCD data.  If absent the
+entire image is assumed to be data.  Only the pixels within the
+data section are modified during processing.  Therefore, there may be
+additional calibration or observation information in the image.
+If after processing, the data section is the entire image it is
+not recorded in the image header.
+.le
+.ls CCDSEC
+The section of the CCD to corresponding to the data section.  This
+refers to the physical format, columns and lines, of the detector.  This is
+the coordinate system used during processing to relate calibration
+data to the image data; i.e. image data pixels are calibrated by
+calibration pixels at the same CCD coordinates regardless of image pixel
+coordinates.  This allows recording only parts of the CCD during data
+taking and calibrating with calibration frames covering some or all of
+the CCD.  The CCD section is maintained during trimming operations.
+Note that changing the format of the images by image operators outside
+of the \fBccdred\fR package will invalidate this coordinate system.
+The size of the CCD section must agree with that of the data section.
+If a CCD section is absent then it defaults to the data section such
+that the first pixel of the data section has CCD coordinate (1,1).
+.le
+.ls BIASSEC
+The section of the image containing prescan or overscan bias information.
+It consists of a strip perpendicular to the readout axis.  There may be
+both a prescan and overscan but the package currently only uses one.
+This parameter may be overridden during processing by the parameter
+\fIccdproc.biassec\fR.
+.le
+.ls TRIMSEC
+The section of the image extracted during processing when the trim
+operation is selected (\fIccdproc.trim\fR).  If absent when the trim
+operation is selected it defaults to the data section; i.e. the processed
+image consists only of the data section.  This parameter may be overridden
+during processing by the parameter \fIccdproc.trimsec\fR.  After trimming
+this parameter, if present, is removed from the image header.  The
+CCD section, data section, and bias section parameters are also modified
+by trimming.
+.le
+
+The geometry is as follows.  When a CCD image is recorded it consists
+of a data section corresponding to part or all of the CCD detector.
+Regions outside of the data section may contain additional information
+which are not affected except by trimming.  Most commonly this consists
+of prescan and overscan bias data.  When recording only part of the
+full CCD detector the package maintains information about that part and
+correctly applies calibrations for that part of the detector.  Also any
+trimming operation updates the CCD coordinate information.  If the
+images include the data section, bias section, trim section, and ccd
+section the processing may be performed entirely automatically.
+
+The sections are specified using the notation [c1:c2,l1:l2] where c1
+and c2 are the first and last columns and l1 and l2 are the first and
+last lines.  Currently c1 and l1 must be less than c2 and l2
+respectively and no subsampling is allowed.  This may be added later.
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/ccdgroups.hlp b/noao/imred/quadred/src/quad/doc/ccdgroups.hlp
new file mode 100644
index 00000000..48c29b99
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/ccdgroups.hlp
@@ -0,0 +1,163 @@
+.help ccdgroups Jun87 noao.imred.ccdred
+.ih
+NAME
+ccdgroups -- Group CCD images into image lists
+.ih
+USAGE
+ccdgroups images output
+.ih
+PARAMETERS
+.ls images
+List of CCD images to be grouped.
+.le
+.ls output
+Output root group filename.  The image group lists will be put in files
+with this root name followed by a number.
+.le
+.ls group = "ccdtype"
+Group type.  There are currently four grouping types:
+.ls ccdtype
+Group by CCD image type.
+.le
+.ls subset
+Group by subset parameter.
+.le
+.ls position
+Group by position in right ascension (in hours) and declination (in degrees).
+The groups are defined by a radius parameter (in arc seconds).
+.le
+.ls title
+Group by identical titles.
+.le
+.ls date
+Group by identical dates.
+.le
+.le
+.ls radius = 60.
+Grouping radius when grouping by positions.  This is given in arc seconds.
+.le
+.ls ccdtype = ""
+CCD image types to select from the input image list.  If null ("") then
+all image types are used.
+.le
+.ih
+DESCRIPTION
+The input images, possible restricted to a particular CCD image type,
+are grouped into image lists.  The "ccdtype" or "subset" groups
+produce output image lists with the given root name and the CCD type
+or subset as an extension (without a period).  For the other group
+types the
+image lists have file names given by
+the root output name and a numeric extension (without a period).
+If the package parameter \fIccdred.verbose\fR is yes then the
+image name and output group list is printed for each image.  The image lists can
+be used with the @ list feature for processing separate groups of observations.
+Note that grouping by CCD image type and subset is often not necessary since
+the \fBccdred\fR tasks automatically use this information (see
+\fBccdtypes\fR and \fBsubsets\fR).
+
+Besides CCD image type and subsets there are currently three ways to
+group images.  These are by position in the sky, by title, and by
+date.  Further groups may be added as suggested.  The title grouping is
+useful if consistent titles are used when taking data.  The date
+grouping is useful if multiple nights of observations are not organized
+by directories (it is recommended that data from separate nights be
+kept in separate directories).  The position grouping finds
+observations within a given radius on the sky of the first member of
+the group (this is not a clustering algorithm).  The right ascension
+and declination coordinates must be in standard units, hours and
+degrees respectively.  The grouping radius is in arc seconds.  This
+grouping type is useful for making sets of data in which separate
+calibration images are taken at each position.
+
+The date, title, and coordinates are accessed through the instrument
+translation file.  The standard names used are "date-obs", "title", "ra",
+and "dec".
+.ih
+EXAMPLES
+1. For each object 5 exposures were taken to be combined in order to remove
+cosmic rays.  If the titles are the same then (with ccdred.verbose=yes):
+
+.nf
+    cl> ccdgroups *.imh group group=title ccdtype=object
+    ccd005.imh  --> group1
+    ccd006.imh  --> group1
+    ccd007.imh  --> group1
+    ccd008.imh  --> group1
+    ccd009.imh  --> group1
+    ccd012.imh  --> group2
+    ccd013.imh  --> group2
+    ccd014.imh  --> group2
+    ccd015.imh  --> group2
+    ccd016.imh  --> group2
+    [... etc ...]
+    cl> combine @group1 obj1 proc+
+    cl> combine @group2 obj2 proc+
+    [... etc ...]
+.fi
+
+Note the numeric suffixes to the output root name "group".
+ 
+2. CCD observations were made in groups with a flat field, the object, and
+a comparison spectrum at each position.  To group and process this data:
+
+.nf
+    cl> ccdgroups *.imh obs group=position >> logfile
+    cl> ccdproc @obs1
+    cl> ccdproc @obs2
+    cl> ccdproc @obs3
+.fi
+
+Since no flat field is specified for the parameter \fIccdproc.flat\fR
+the flat field is taken from the input image list.
+
+3. If for some reason you want to group by date and position it is possible
+to use two steps.
+
+.nf
+    cl> ccdgroups *.imh date group=date
+    cl> ccdgroups @data1 pos1
+    cl> ccdgroups @data2 pos2
+.fi
+ 
+4. To get groups by CCD image type:
+ 
+.nf
+    cl> ccdgroups *.imh "" group=ccdtype
+    ccd005.imh  --> zero
+    ccd006.imh  --> zero
+    ccd007.imh  --> zero
+    ccd008.imh  --> dark
+    ccd009.imh  --> flat
+    ccd012.imh  --> flat
+    ccd013.imh  --> object
+    ccd014.imh  --> object
+    ccd015.imh  --> object
+    ccd016.imh  --> object
+    [... etc ...]
+.fi
+ 
+Note the use of a null root name and the extension is the standard
+CCDRED types (not necessarily those used in the image header).
+ 
+5. To get groups by subset:
+ 
+.nf
+    cl> ccdgroups *.imh filt group=subset
+    ccd005.imh  --> filt
+    ccd006.imh  --> filtB
+    ccd007.imh  --> filtB
+    ccd008.imh  --> filtB
+    ccd009.imh  --> filtV
+    ccd012.imh  --> filtV
+    ccd013.imh  --> filtV
+    ccd014.imh  --> filtB
+    ccd015.imh  --> filtB
+    ccd016.imh  --> filtB
+    [... etc ...]
+.fi
+ 
+.ih
+SEE ALSO
+ccdlist, ccdtypes, instruments, subsets
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/ccdhedit.hlp b/noao/imred/quadred/src/quad/doc/ccdhedit.hlp
new file mode 100644
index 00000000..1bc27d29
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/ccdhedit.hlp
@@ -0,0 +1,108 @@
+.help ccdhedit Jun87 noao.imred.ccdred
+.ih
+NAME
+ccdhedit -- CCD image header editor
+.ih
+USAGE
+ccdhedit images parameter value
+.ih
+PARAMETERS
+.ls images
+List of CCD images to be edited.
+.le
+.ls parameter
+Image header parameter.  The image header parameter will be translated by
+the header translation file for the images.
+.le
+.ls value
+The parameter value.  If the null string ("") is specified then the
+parameter is deleted from the image header, otherwise it is added or
+modified.  If the parameter is "imagetyp" then the value string giving
+the CCD image type is translated from the package CCD type to the
+instrument specific string.
+.le
+.ls type = "string"
+The parameter type.  The parameter types are "string", "real", or "integer".
+.le
+.ih
+DESCRIPTION
+The image headers of the specified CCD images are edited to add, modify,
+or delete a parameter.  The parameters may be those used by the \fBccdred\fR
+package.  The parameter name is translated to an image header parameter by the
+instrument translation file (see \fBinstruments\fR) if a translation is
+given.  Otherwise the parameter is that in the image header.  If the parameter
+is "imagetyp" the parameter value for the CCD image type may be that
+used by the package; i.e. dark, object, flat, etc.  The value string will be
+translated to the instrument image string in this case.  The translation
+facility allows use of this task in an instrument independent way.
+
+The value string is used to determine whether to delete or modify the
+image parameter.  If the null string, "", is given the specified parameter
+is deleted.  If parameters are added the header type must be specified
+as a string, real, or integer parameter.  The numeric types convert the
+value string to a number.
+.ih
+EXAMPLES
+The \fBccdred\fR package is usable even with little image header information.
+However, if desired the header information can be added to images which
+lack it.  In all the examples the parameters used are those of the package
+and apply equally well to any image header format provided there is an
+instrument translation file.
+
+.nf
+1.   cl> ccdhedit obj* imagetyp object
+2.   cl> ccdhedit flat* imagetyp flat
+3.   cl> ccdhedit zero* imagetyp zero
+4.   cl> ccdhedit obj0![1-3]* subset "V filter"
+5.   cl> ccdhedit obj0![45]* subset "R filter"
+6.   cl> ccdhedit flat001 subset "R filter"
+7.   cl> ccdhedit obj* exptime 500 type=integer
+.fi
+
+8. The following is an example of a CL script which sets the CCD image type,
+the subset, and the exposure time simultaneously.  The user may expand
+on this example to include other parameters or other initialization
+operations.
+
+.nf
+    cl> edit ccdheader.cl
+
+    ----------------------------------------------------------------
+    # Program to set CCD header parameters.
+
+    procedure ccdheader (images)
+
+    string	images			{prompt="CCD images"}
+    string	imagetyp		{prompt="CCD image type"}
+    string	subset			{prompt="CCD subset"}
+    string	exptime			{prompt="CCD exposure time"}
+
+    begin
+	    string	ims
+
+	    ims = images
+	    ccdhedit (ims, "imagetyp", imagetyp, type="string")
+	    ccdhedit (ims, "subset", subset, type="string")
+	    ccdhedit (ims, "exptime", exptime, type="real")
+    end
+    ----------------------------------------------------------------
+
+    cl> task ccdheader=ccdheader.cl
+    cl> ccdheader obj* imagetyp=object subset="V" exptime=500
+.fi
+
+9. The image header may be changed to force processing a calibration image
+as an object.  For example to flatten a flat field:
+
+.nf
+    cl> ccdhedit testflat imagetyp other
+    cl> ccdproc testflat
+.fi
+
+10. To delete processing flags:
+
+    cl> ccdhedit obj042 flatcor ""
+.ih
+SEE ALSO
+hedit, instruments, ccdtypes, subsets
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/ccdinst.hlp b/noao/imred/quadred/src/quad/doc/ccdinst.hlp
new file mode 100644
index 00000000..23ebea60
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/ccdinst.hlp
@@ -0,0 +1,389 @@
+.help ccdinstrument Nov90 noao.imred.ccdred
+.ih
+NAME
+ccdinstrument -- Setup and verify CCD instrument translation files
+.ih
+USAGE	
+ccdinstrument images
+.ih
+PARAMETERS
+.ls images
+List of images to be verified or used to setup a CCD instrument translation
+file.
+.le
+.ls instrument = ")_.instrument"
+CCD instrument translation file.  The default is to use the translation
+file defined in the \fBccdred\fR package parameters.  Note that one would
+need write permission to update this file though the task has a write
+command to save any changes to a different file.
+.le
+.ls ssfile = ")_.ssfile"
+Subset translation file.  The default is to use the file defined in
+the \fBccdred\fR package parameters.
+.le
+.ls edit = yes
+Edit the instrument translation file?  If "yes" an interactive
+mode is entered allowing translation parameters to be modified while if
+"no" the task is simply used to verify the translations noninteractively.
+.le
+.ls parameters = "basic"
+Parameters to be displayed.  The choices are "basic" to display only the
+most basic parameters (those needed for the simplest automation of
+\fBccdred\fR tasks),  "common" to display the common parameters used
+by the package (most of these are keywords to be written to the image
+rather than translated), and "all" to display all the parameters
+referenced by the package including the most obscure.  For most uses
+the "basic" set is all that is important and the other options are
+included for completeness.
+.le
+.ih
+DESCRIPTION
+The purpose of this task is to provide an interface to simplify setting
+up CCD instrument translation files and to verify the translations
+for a set of images.  Before this task was written users who needed to
+set up translation files for new instruments and observatories had
+to directly create the files with an editor.  Many people encountered
+difficulties and were prone to errors.  Also there was no task that
+directly verified the translations though \fBccdlist\fR provided some
+clues.
+
+The \fBccdred\fR package was designed to make intelligent use of
+information in image headers for determining things such as image
+calibration or object type and exposure times.  While the package may
+be used without this capability it is much more convenient to be
+able to use information from the image.  The package was also intended
+to be used with many different instruments, detectors, and observatories.
+The key to providing image header access across different observatories
+is the ability to translate the needs of the package to the appropriate
+keywords in the image header.  This is done through a file called
+an "instrument translation file".  For a complete description of
+this file and other instrument setup features of the package see
+\fBccdred.instruments\fR.
+
+The instrument translation file translates the parameter names used by
+the \fBccdred\fR package into image specific parameters and also
+supplies default values for parameters.  The translation proceeds as
+follows.  When a package task needs a parameter for an image, for
+example "imagetyp", it looks in the instrument translation file.  If
+the file is not found or none is specified then the image header
+keyword that is requested is assumed to have the same name.  If an
+instrument translation file is defined then the requested parameter is
+translated to an image header keyword, provided a translation entry is
+given.  If no translation is given the package name is used.  For
+example the package parameter "imagetyp" might be translated to
+"data-typ" (the old NOAO CCD keyword).  If the parameter is not found
+then the default value specified in the translation file, if present,
+is returned.
+
+For recording parameter information in the header, such
+as processing flags, translation is also used.  For example, if the
+flag specifying that the image has been corrected by a flat field is to
+be set then the package parameter name "flatcor" might be translated to
+"ff-flag".  If no translation is given then the new image header
+parameter is entered as "flatcor".
+
+The CCD image type requires a second level of translation also defined
+in the translation file.  Once the image keyword which identifies the
+type of CCD image, for example a flat field or object, is translated
+to an imahe keyword the specific
+string value must be translated to one of the CCD image types used
+by the package.  The translation works in the same way, the specific
+string found is translated to the \fBccdred\fR type and returned to
+the task.  This translation is tricky in that the exact string
+including all spaces and capitalizations must be correctly defined
+in the translation file.  The \fBccdinstrument\fR allows doing
+this automatically thus minimizing typing errors.
+
+The basic display format of the task is a table of five columns
+giving the parameter name used by the package, the image keyword
+to which it is translated, the default value (if any), the value
+the task will receive for the current image after translation,
+and the actual keyword value in the image.  A "?" is printed if
+a value cannot be determined.  The idea of the task is to make sure
+that the value a \fBccdred\fR task sees is the correct one and if not
+to modify the translation appropriately.  In verify mode when the
+\fBedit\fR parameter is not set the translation table is simply
+printed for each input image.
+
+In edit mode the user interactively gives commands at the ccdinstrument
+prompt to display or modify keywords.  The modifications can then be
+written to the instrument file or saved in a private copy.  The
+list of commands is shown below and may be printed using ? or help.
+
+.in 4
+.nf
+			CCDINSTRUMENT COMMANDS
+
+?	    Print command summary
+help	    Print command summary
+imheader    Page image header
+instrument  Print current instrument translation file
+next	    Next image
+newimage    Select a new image
+quit	    Quit
+read	    Read instrument translation file
+show	    Show current translations
+write	    Write instrument translation file
+
+translate   Translate image string selected by the imagetyp
+	    parameter to one of the CCDRED types given as an
+	    argument or queried:
+	    object, zero, dark, flat, comp, illum, fringe, other
+
+.fi
+The following are CCDRED parameters which may be translated.  You are
+queried for the image keyword to use or it may be typed after the command.
+An optional default value (returned if the image does not contain the
+keyword) may be typed as the second argument of the command.
+.nf
+
+	BASIC PARAMETERS
+imagetyp	Image type parameter (see also translate)
+subset		Subset or filter parameter
+exptime		Exposure time
+darktime	Dark time (may be same as the exposure time)
+.fi
+.in -4
+
+The commands may be followed by values such as file names for some of
+the general commands or the keyword and default value for the parameters
+to be translated.  Note this is the only way to specify a default value.
+If no arguments are given the user is prompted with the current value
+which may then be changed.
+
+The set of parameters shown above are only those considered "basic".
+In order to avoid confusion the task can limit the set of parameters
+displayed.  Without going into great detail, it is only the basic
+parameters which are generally required to have valid translations to
+allow the package to work well.  However, for completeness, and if someone
+wants to go wild with translations, further parameters may be displayed
+and changed.  The parameters displayed is controlled by the \fIparameters\fR
+keyword.  The additional parameters not shown above are:
+
+.in 4
+.nf
+	USEFUL DEFAULT GEOMETRY PARAMETERS
+biassec		Bias section (often has a default value)
+trimsec		Trim section (often has a default value)
+
+	COMMON PROCESSING FLAGS
+fixpix		Bad pixel replacement flag
+overscan	Overscan correction flag
+trim		Trim flag
+zerocor		Zero level correction flag
+darkcor		Dark count correction flag
+flatcor		Flat field correction flag
+
+	RARELY TRANSLATED PARAMETERS
+ccdsec		CCD section
+datasec		Data section
+fixfile		Bad pixel file
+
+fringcor	Fringe correction flag
+illumcor	Ilumination correction flag
+readcor		One dimensional zero level read out correction
+scancor		Scan mode correction flag
+
+illumflt	Ilumination flat image
+mkfringe	Fringe image
+mkillum		Iillumination image
+skyflat		Sky flat image
+
+ccdmean		Mean value
+fringscl	Fringe scale factor
+ncombine	Number of images combined
+date-obs	Date of observations
+dec		Declination
+ra		Right Ascension
+title		Image title
+.fi
+.in -4
+.ih
+EXAMPLES
+1. To verify the translations for a set of images using the default
+translation file:
+
+.nf
+	cl> setinst "" review-
+	cl> ccdinst dev$pix edit-
+	Image: dev$pix
+	Instrument file: 
+	Subset file: subsets
+
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	--------------------------------
+	imagetyp  imagetyp            none      ?
+	subset    subset                        ?
+	exptime   exptime             ?         ?
+	darktime  darktime            ?         ?
+
+	cl> setinst "" site=kpno dir=ccddb$ review-
+	cl> ccdinst dev$pix edit-
+	Image: dev$pix
+
+	Instrument file: ccddb$kpno/camera.dat
+	Subset file: subsets
+
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	--------------------------------
+	imagetyp  data-typ            object    OBJECT (0)
+	subset    f1pos               2         2
+	exptime   otime               600       600
+	darktime  ttime               600       600
+.fi
+
+2.  Set up an  instrument translation file from scratch.
+
+.nf
+	ccdinst ech???.imh instr=myccd edit+
+	Warning: OPEN: File does not exist (myccd)
+	Image: ech001.imh
+	Instrument file: myccd
+	Subset file: subsets
+	
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	------------------------------------------------------
+	imagetyp  imagetyp            none      ?
+	subset    subset                        ?
+	exptime   exptime             ?         ?
+	darktime  darktime            ?         ?
+	
+	ccdinstrument> imagetyp
+	Image keyword for image type (imagetyp): ccdtype
+	imagetyp  ccdtype             unknown   BIAS
+	ccdinstrument> translate
+	CCDRED image type for 'BIAS' (unknown): zero
+	imagetyp  ccdtype             zero      BIAS
+	ccdinstrument> subset
+	Image keyword for subset parameter (subset): filters
+	subset    filters             1         1 0
+	ccdinstrument> exptime integ
+	exptime   integ               0.        0.
+	ccdinstrument> darktime integ
+	darktime  integ               0.        0.
+	ccdinstrument> show
+	Image: ech001.imh
+	Instrument file: myccd
+	Subset file: subsets
+	
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	------------------------------------------------------
+	imagetyp  ccdtype             zero      BIAS
+	subset    filters             1         1 0
+	exptime   integ               0.        0.
+	darktime  integ               0.        0.
+	
+	ccdinstrument> next
+	Image: ech002.imh
+	Instrument file: myccd
+	Subset file: subsets
+	
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	------------------------------------------------------
+	imagetyp  ccdtype             unknown   PROJECTOR FLAT
+	subset    filters             1         1 0
+	exptime   integ               20.       20.
+	darktime  integ               20.       20.
+	
+	ccdinstrument> trans
+	CCDRED image type for 'PROJECTOR FLAT' (unknown): flat
+	imagetyp  ccdtype             flat      PROJECTOR FLAT
+	ccdinstrument> next
+	Image: ech003.imh
+	Instrument file: myccd
+	Subset file: subsets
+	
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	------------------------------------------------------
+	imagetyp  ccdtype             unknown   COMPARISON
+	subset    filters             1         1 0
+	exptime   integ               300       300
+	darktime  integ               300       300
+	
+	ccdinstrument> translate comp
+	imagetyp  ccdtype             comp      COMPARISON
+	ccdinstrument> next
+	Image: ech004.imh
+	Instrument file: myccd
+	Subset file: subsets
+	
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	------------------------------------------------------
+	imagetyp  ccdtype             unknown   OBJECT
+	subset    filters             1         1 0
+	exptime   integ               3600      3600
+	darktime  integ               3600      3600
+	
+	ccdinstrument> translate object
+	imagetyp  ccdtype             object    OBJECT
+	ccdinstrument> inst
+	imagetyp                      ccdtype 
+	BIAS                          zero    
+	subset                        filters 
+	exptime                       integ   
+	darktime                      integ   
+	'PROJECTOR FLAT'              flat    
+	COMPARISON                    comp    
+	OBJECT                        object  
+
+	ccdinstrument> next
+	Update instrument file myccd (yes)? 
+.fi
+
+3.  Set default geometry parameters.  Note that to set a default the
+arguments must be on the command line.
+
+.nf
+	cc> ccdinst ech001 instr=myccd param=common edit+
+	Image: ech001
+	Instrument file: myccd
+	Subset file: subsets
+	
+	CCDRED    IMAGE     DEFAULT   CCDRED    IMAGE   
+	PARAM     KEYWORD   VALUE     VALUE     VALUE   
+	------------------------------------------------------
+	imagetyp  ccdtype             zero      BIAS
+	subset    filters             1         1 0
+	exptime   integ               0.        0.
+	darktime  integ               0.        0.
+	
+	biassec   biassec             ?         ?
+	trimsec   trimsec             ?         ?
+	
+	fixpix    fixpix              no        ?
+	overscan  overscan            no        ?
+	trim      trim                no        ?
+	zerocor   zerocor             no        ?
+	darkcor   darkcor             no        ?
+	flatcor   flatcor             no        ?
+	
+	ccdinstrument> biassec biassec [803:830,*]
+	biassec   biassec   [803:830,*]  [803:830,*]  ?
+	ccdinstrument> trimsec trimsec [2:798,2:798]
+	trimsec   trimsec   [2:798,2:798]  [2:798,2:798]  ?
+	ccdinstrument> instr
+	trimsec                       trimsec  [2:798,2:798]
+	biassec                       biassec  [803:830,*]
+	imagetyp                      ccdtype 
+	BIAS                          zero    
+	subset                        filters 
+	exptime                       integ   
+	darktime                      integ   
+	'PROJECTOR FLAT'              flat    
+	COMPARISON                    comp    
+	OBJECT                        object  
+	
+	ccdinstrument> q
+	Update instrument file myccd (yes)? 
+.fi
+.ih
+SEE ALSO
+instruments, setinstrument
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/ccdlist.hlp b/noao/imred/quadred/src/quad/doc/ccdlist.hlp
new file mode 100644
index 00000000..9ce7dfdd
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/ccdlist.hlp
@@ -0,0 +1,133 @@
+.help ccdlist Jun87 noao.imred.ccdred
+.ih
+NAME
+ccdlist -- List CCD processing information
+.ih
+USAGE
+ccdlist images
+.ih
+PARAMETERS
+.ls images
+CCD images to be listed.  A subset of the these may be selected using the
+CCD image type parameter.
+.le
+.ls ccdtype = ""
+CCD image type to be listed.  If no type is specified then all the images
+are listed.  If an image type is specified then only images
+of that type are listed.  See \fBccdtypes\fR for a list of the package
+image types.
+.le
+.ls names = no
+List the image names only?  Used with the CCD image type parameter to make
+a list of the images of the specified type.
+.le
+.ls long = no
+Long format listing?  The images are listed in a long format containing some
+image parameters and the processing history.
+.le
+.ls ccdproc (pset)
+CCD processing parameter set.
+.le
+.ih
+DESCRIPTION
+Information from the specified input images is listed on the standard
+output.  A specific CCD image type may be selected from the input
+images by the parameter \fIccdtype\fR.  There are three list formats;
+the default one line per image format, an image name only format, and a
+multi-line long format.  The default one line format consists of the
+image name, image size, image pixel type, CCD image type, subset ID (if
+defined), processing flags, and title.  This format contains the same
+information as that produced by \fBimheader\fR as well as CCD specific
+information.  The processing flags identifying the processing operations
+performed on the image are given by the following single letter codes.
+
+.nf
+	B - Bad pixel replacement
+	O - Overscan bias subtraction
+	T - Trimming
+	Z - Zero level subtraction
+	D - Dark count subtraction
+	F - Flat field calibration
+	I - Iillumination correction
+	Q - Fringe correction
+.fi
+
+The long format has the same first line as the default format plus additional
+instrument information such as the exposure time and the full processing
+history.  In addition to listing the completed processing, the operations
+not yet done (as specified by the \fBccdproc\fR parameters) are also
+listed.
+
+The image name only format is intended to be used to generate lists of
+images of the same CCD image type.  These lists may be used as "@" file
+lists in IRAF tasks.
+.ih
+EXAMPLES
+1. To list the default format for all images:
+
+.nf
+    cl> ccdlist *.imh
+    ccd001.imh[544,512][short][unknown][V]:FOCUS L98-193
+    ccd007.imh[544,512][short][object][V]:N2968 V 600s
+    ccd015.imh[544,512][short][object][B]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R]:N4036 R 600s
+    ccd045.imh[544,512][short][flat][V]:dflat 6v+blue 5s
+    ccd066.imh[544,512][short][flat][B]:dflat 6v+blue 5s
+    ccd103.imh[544,512][short][flat][R]:dflat 6v+blue 5s
+    ccd104.imh[544,512][short][zero][]:bias
+    ccd105.imh[544,512][short][dark][]:dark 3600s
+.fi
+
+These images have not been processed.
+
+2. To restrict the listing to just the object images:
+
+.nf
+    cl> ccdlist *.imh ccdtype=object
+    ccd007.imh[544,512][short][object][V]:N2968 V 600s
+    ccd015.imh[544,512][short][object][B]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R]:N4036 R 600s
+.fi
+
+3. The long list for image "ccd007" is obtained by:
+
+.nf
+    cl> ccdlist ccd007 l+
+    ccd007[544,512][short][object][V]:N2968 R 600s
+	exptime = 200. darktime = 200.
+        [TO BE DONE] Overscan strip is [520:540,*]
+        [TO BE DONE] Trim image section is [3:510,3:510]
+        [TO BE DONE] Flat field correction
+.fi
+
+4. After processing the images have the short listing:
+
+.nf
+    cl> ccdlist *.imh ccdtype=object
+    ccd007.imh[508,508][real][object][V][OTF]:N2968 V 600s
+    ccd015.imh[508,508][real][object][B][OTF]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R][OTF]:N4036 R 600s
+.fi
+
+The processing indicated is overscan subtraction, trimming, and flat fielding.
+
+5. The long listing for "ccd007" after processing is:
+
+.nf
+    cl> ccdlist ccd007 l+
+    ccd007[508,508][real][object][V][OTF]:N2968 R 600s
+	exptime = 200. darktime = 200.
+        Jun  2 18:18 Overscan section is [520:540,*] with mean=481.8784
+        Jun  2 18:18 Trim data section is [3:510,3:510]
+        Jun  2 18:19 Flat field image is FlatV.imh with scale=138.2713
+.fi
+
+6. To make a list file containing all the flat field images:
+
+    cl> ccdlist *.imh ccdtype=flat name+ > flats
+
+This file can be used as an @ file for processing.
+.ih
+SEE ALSO
+ccdtypes ccdgroups
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/ccdproc.hlp b/noao/imred/quadred/src/quad/doc/ccdproc.hlp
new file mode 100644
index 00000000..4be65f73
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/ccdproc.hlp
@@ -0,0 +1,720 @@
+.help ccdproc Oct90 noao.imred.ccdred
+.ih
+NAME
+ccdproc -- Process CCD images
+.ih
+USAGE	
+ccdproc images
+.ih
+PARAMETERS
+.ls images
+List of input CCD images to process.  The list may include processed
+images and calibration images.
+.le
+.ls ccdtype = ""
+CCD image type to select from the input image list.  If no type is given
+then all input images will be selected.  The recognized types are described
+in \fBccdtypes\fR.
+.le
+.ls max_cache = 0
+Maximum image caching memory (in Mbytes).  If there is sufficient memory
+the calibration images, such as zero level, dark count, and flat fields,
+will be cached in memory when processing many input images.  This
+reduces the disk I/O and makes the task run a little faster.  If the
+value is zero image caching is not used.
+.le
+.ls noproc = no
+List processing steps only?
+.le
+
+.ce
+PROCESSING SWITCHES
+.ls fixpix = yes
+Fix bad CCD lines and columns by linear interpolation from neighboring
+lines and columns?  If yes then a bad pixel file must be specified.
+.le
+.ls overscan = yes
+Apply overscan or prescan bias correction?  If yes then the overscan
+image section and the readout axis must be specified.
+.le
+.ls trim = yes
+Trim the image of the overscan region and bad edge lines and columns?
+If yes then the data section must be specified.
+.le
+.ls zerocor = yes
+Apply zero level correction?  If yes a zero level image must be specified.
+.le
+.ls darkcor = yes
+Apply dark count correction?  If yes a dark count image must be specified.
+.le
+.ls flatcor = yes
+Apply flat field correction?  If yes flat field images must be specified.
+.le
+.ls illumcor = no
+Apply iillumination correction?  If yes iillumination images must be specified.
+.le
+.ls fringecor = no
+Apply fringe correction?  If yes fringe images must be specified.
+.le
+.ls readcor = no
+Convert zero level images to readout correction images?  If yes then
+zero level images are averaged across the readout axis to form one
+dimensional zero level readout correction images.
+.le
+.ls scancor = no
+Convert flat field images to scan mode flat field images?  If yes then the
+form of scan mode correction is specified by the parameter \fIscantype\fR.
+.le
+
+.ce
+PROCESSING PARAMETERS
+.ls readaxis = "line"
+Read out axis specified as "line" or "column".
+.le
+.ls fixfile
+File describing the bad lines and columns.  If "image" is specified then
+the file is specified in the image header or instrument translation file.
+.le
+.ls biassec
+Overscan bias strip image section.  If "image" is specified then the overscan
+bias section is specified in the image header or instrument translation file.
+.le
+.ls trimsec
+image section for trimming.  If "image" is specified then the trim
+image section is specified in the image header or instrument translation file.
+.le
+.ls zero = ""
+Zero level calibration image.  The zero level image may be one or two
+dimensional.  The CCD image type and subset are not checked for these
+images and they take precedence over any zero level calibration images
+given in the input list.
+.le
+.ls dark = ""
+Dark count calibration image.  The CCD image type and subset are not checked
+for these images and they take precedence over any dark count calibration
+images given in the input list.
+.le
+.ls flat = ""
+Flat field calibration images.  The flat field images may be one or
+two dimensional.  The CCD image type is not checked for these
+images and they take precedence over any flat field calibration images given
+in the input list.  The flat field image with the same subset as the
+input image being processed is selected.
+.le
+.ls illum = ""
+Iillumination correction images.  The CCD image type is not checked for these
+images and they take precedence over any iillumination correction images given
+in the input list.  The iillumination image with the same subset as the
+input image being processed is selected.
+.le
+.ls fringe = ""
+Fringe correction images.  The CCD image type is not checked for these
+images and they take precedence over any fringe correction images given
+in the input list.  The fringe image with the same subset as the
+input image being processed is selected.
+.le
+.ls minreplace = 1.
+When processing flat fields, pixel values below this value (after
+all other processing such as overscan, zero, and dark corrections) are
+replaced by this value.  This allows flat fields processed by \fBccdproc\fR
+to be certain to avoid divide by zero problems when applied to object
+images.
+.le
+.ls scantype = "shortscan"
+Type of scan format used in creating the CCD images.  The modes are:
+.ls "shortscan"
+The CCD is scanned over a number of lines and then read out as a regular
+two dimensional image.  In this mode unscanned flat fields are numerically
+scanned to form scanned flat fields comparable to the observations.  If
+the flat field calibration images are taken in scanned mode then
+\fIscancor\fR should be no and the processing performed in the same manner
+as in unscanned mode.
+.le
+.ls "longscan"
+In this mode the CCD is clocked and read out continuously to form a long
+strip.  Flat fields are averaged across the readout axis to
+form a one dimensional flat field readout correction image.  This assumes
+that all recorded image lines are clocked over the entire active area of the
+CCD.
+.le
+.le
+.ls nscan
+Number of scan readout lines used in short scan mode.  This parameter is used
+when the scan type is "shortscan".
+.le
+
+
+.ce
+OVERSCAN FITTING PARAMETERS
+.ls interactive = no
+Fit the overscan vector interactively?  If yes the overscan vector is fit
+interactively using the \fBicfit\fR package.  If no then the fitting parameters
+given below are used.
+.le
+.ls function = "legendre"
+Overscan fitting function.  The function types are "legendre" polynomial,
+"chebyshev" polynomial, "spline1" linear spline, and "spline3" cubic
+spline.
+.le
+.ls order = 1
+Number of polynomial terms or spline pieces in the overscan fit.
+.le
+.ls sample = "*"
+Sample points to use in the overscan fit.  The string "*" specified all
+points otherwise an \fBicfit\fR range string is used.
+.le
+.ls naverage = 1
+Number of points to average or median to form fitting points.  Positive
+numbers specify averages and negative numbers specify medians.
+.le
+.ls niterate = 1
+Number of rejection iterations to remove deviant points from the overscan fit.
+If 0 then no points are rejected.
+.le
+.ls low_reject = 3., high_reject = 3.
+Low and high sigma rejection factors for rejecting deviant points from the
+overscan fit.
+.le
+.ls grow = 0.
+One dimensional growing radius for rejection of neighbors to deviant points.
+.le
+.ih
+DESCRIPTION
+\fBCcdproc\fR processes CCD images to correct and calibrate for
+detector defects, readout bias, zero level bias, dark counts,
+response, iillumination, and fringing.  It also trims unwanted
+lines and columns and changes the pixel datatype.  It is efficient
+and easy to use; all one has to do is set the parameters and then
+begin processing the images.  The task takes care of most of the
+record keeping and automatically does the prerequisite processing
+of calibration images.  Beneath this simplicity there is much that
+is going on.  In this section a simple description of the usage is
+given.  The following sections present more detailed discussions
+on the different operations performed and the order and logic
+of the processing steps.  For a user's guide to the \fBccdred\fR
+package see \fBguide\fR.  Much of the ease of use derives from using
+information in the image header.  If this information is missing
+see section 13.
+
+One begins by setting the task parameters.  There are many parameters
+but they may be easily reviewed and modified using the task \fBeparam\fR.
+The input CCD images to be processed are given as an image list.
+Previously processed images are ignored and calibration images are
+recognized, provided the CCD image types are in the image header (see
+\fBinstruments\fR and \fBccdtypes\fR).  Therefore it is permissible to
+use simple image templates such as "*.imh".  The \fIccdtype\fR parameter
+may be used to select only certain types of CCD images to process
+(see \fBccdtypes\fR).
+
+The processing operations are selected by boolean (yes/no) parameters.
+Because calibration images are recognized and processed appropriately,
+the processing operations for object images should be set.
+Any combination of operations may be specified and the operations are
+performed simultaneously.  While it is possible to do operations in
+separate steps this is much less efficient.  Two of the operation
+parameters apply only to zero level and flat field images.  These
+are used for certain types of CCDs and modes of operation.
+
+The processing steps selected have related parameters which must be
+set.  These are things like image sections defining the overscan and
+trim regions and calibration images.  There are a number of parameters
+used for fitting the overscan or prescan bias section.  These are
+parameters used by the standard IRAF curve fitting package \fBicfit\fR.
+The parameters are described in more detail in the following sections.
+
+In addition to the task parameters there are package parameters
+which affect \fBccdproc\fR.  These include the instrument and subset
+files, the text and plot log files, the output pixel datatype,
+the amount of memory available for calibration image caching,
+the verbose parameter for logging to the terminal, and the backup
+prefix.  These are described in \fBccdred\fR.
+
+Calibration images are specified by task parameters and/or in the
+input image list.  If more than one calibration image is specified
+then the first one encountered is used and a warning is issued for the
+extra images.  Calibration images specified by
+task parameters take precedence over calibration images in the input list.
+These images also need not have a CCD image type parameter since the task
+parameter identifies the type of calibration image.  This method is
+best if there is only one calibration image for all images
+to be processed.  This is almost always true for zero level and dark
+count images.  If no calibration image is specified by task parameter
+then calibration images in the input image list are identified and
+used.  This requires that the images have CCD image types recognized
+by the package.  This method is useful if one may simply say "*.imh"
+as the image list to process all images or if the images are broken
+up into groups, in "@" files for example, each with their own calibration
+frames.
+
+When an input image is processed the task first determines the processing
+parameters and calibration images.  If a requested operation has been
+done it is skipped and if all requested operations have been completed then
+no processing takes place.  When it determines that a calibration image
+is required it checks for the image from the task parameter and then
+for a calibration image of the proper type in the input list.
+
+Having
+selected a calibration image it checks if it has been processed by
+looking for the image header flag CCDPROC.  If it is not present then
+the calibration image is processed.  When any image has been processed
+the CCDPROC flag is added.  For images processed directly by \fBccdproc\fR
+the individual processing flags are checked even if the CCDPROC flag is
+present.  However, the automatic processing of the calibration images is
+only done if the CCDPROC flag is absent!  This is to make the task more
+efficient by not having to check every flag for every calibration image
+for every input image.  Thus, if additional processing
+steps are added after images have been partially reduced then input images
+will be processed for the new steps but calibration images will not be
+processed automatically.
+
+After the calibration images have been identified, and processed if
+necessary, the images may be cached in memory.  This is done when there
+are more than two input images (it is actually less efficient to
+cache the calibration images for one or two input images) and the parameter
+\fImax_cache\fR is greater than zero.  When caching, as many calibration
+images as allowed by the specified memory are read into memory and
+kept there for all the input images.  Cached images are, therefore,
+only read once from disk which reduces the amount of disk I/O.  This
+makes a modest decrease in the execution time.  It is not dramatic
+because the actual processing is fairly CPU intensive.
+
+Once the processing parameters and calibration images have been determined
+the input image is processed for all the desired operations in one
+step; i.e. there are no intermediate results or images.  This makes
+the task efficient.  The corrected image is output as a temporary image
+until the entire image has been processed.  When the image has been
+completely processed then the original image is deleted (or renamed
+using the specified backup prefix) and the corrected image replaces
+the original image.  Using a temporary image protects the data in the
+event of an abort or computer failure.  Keeping the original image name
+eliminates much of the record keeping and the need to generate new
+image names.
+.sh
+1. Fixpix
+Regions of bad lines and columns may be replaced by linear
+interpolation from neighboring lines and columns when the parameter
+\fIfixpix\fR is set.  The bad regions are specified in a bad pixel
+file.  The file consists of lines with four fields, the starting and
+ending columns and the starting and ending lines.  Any number of
+regions may be specified.  Comment lines beginning with the character
+'#' may be included.  If a comment line preceding the bad regions
+contains the word "untrimmed" then the coordinate system refers to the
+original format of the images; i.e.  before trimming.  If an image has
+been trimmed previously then the trim region specified in the image
+header is used to convert the coordinates in the bad pixel file to
+those of the trimmed image.  If the file does not contain the word
+"untrimmed" then the coordinate system must match that of the image
+being corrected; i.e. untrimmed coordinates if the image has not been
+trimmed and trimmed coordinates if the image has been trimmed.
+Standard bad pixel files should always be specified in terms of the
+original format.
+
+The bad pixel file may be specified explicitly with the parameter \fIfixfile\fR
+or indirectly if the parameter has the value "image".  In the latter case
+the instrument file must contain the name of the file.
+.sh
+2. Overscan
+If an overscan or prescan correction is specified (\fIoverscan\fR
+parameter) then the image section (\fIbiassec\fR parameter) is averaged
+along the readout axis (\fIreadaxis\fR parameter) to form a
+correction vector.  A function is fit to this vector and for each readout
+line (image line or column) the function value for that line is
+subtracted from the image line.  The fitting function is generally
+either a constant (polynomial of 1 term) or a high order function
+which fits the large scale shape of the overscan vector.  Bad pixel
+rejection is also used to eliminate cosmic ray events.  The function
+fitting may be done interactively using the standard \fBicfit\fR
+iteractive graphical curve fitting tool.  Regardless of whether the fit
+is done interactively, the overscan vector and the fit may be recorded
+for later review in a metacode plot file named by the parameter
+\fIccdred.plotfile\fR.  The mean value of the bias function is also recorded in
+the image header and log file.
+.sh
+3. Trim
+When the parameter \fItrim\fR is set the input image will be trimmed to
+the image section given by the parameter \fItrimsec\fR.  This trim
+should, of course, be the same as that used for the calibration images.
+.sh
+4. Zerocor
+After the readout bias is subtracted, as defined by the overscan or prescan
+region, there may still be a zero level bias.  This level may be two
+dimensional or one dimensional (the same for every readout line).  A
+zero level calibration is obtained by taking zero length exposures;
+generally many are taken and combined.  To apply this zero
+level calibration the parameter \fIzerocor\fR is set.  In addition if
+the zero level bias is only readout dependent then the parameter \fIreadcor\fR
+is set to reduce two dimensional zero level images to one dimensional
+images.  The zero level images may be specified by the parameter \fIzero\fR
+or given in the input image list (provided the CCD image type is defined).
+
+When the zero level image is needed to correct an input image it is checked
+to see if it has been processed and, if not, it is processed automatically.
+Processing of zero level images consists of bad pixel replacement,
+overscan correction, trimming, and averaging to one dimension if the
+readout correction is specified.
+.sh
+5. Darkcor
+Dark counts are subtracted by scaling a dark count calibration image to
+the same exposure time as the input image and subtracting.  The
+exposure time used is the dark time which may be different than the
+actual integration or exposure time.  A dark count calibration image is
+obtained by taking a very long exposure with the shutter closed; i.e.
+an exposure with no light reaching the detector.  The dark count
+correction is selected with the parameter \fIdarkcor\fR and the dark
+count calibration image is specified either with the parameter
+\fIdark\fR or as one of the input images.  The dark count image is
+automatically processed as needed.  Processing of dark count images
+consists of bad pixel replacement, overscan and zero level correction,
+and trimming.
+.sh
+6. Flatcor
+The relative detector pixel response is calibrated by dividing by a
+scaled flat field calibration image.  A flat field image is obtained by
+exposure to a spatially uniform source of light such as an lamp or
+twilight sky.  Flat field images may be corrected for the spectral
+signature in spectroscopic images (see \fBresponse\fR and
+\fBapnormalize\fR), or for iillumination effects (see \fBmkillumflat\fR
+or \fBmkskyflat\fR).  For more on flat fields and iillumination corrections
+see \fBflatfields\fR.  The flat field response is dependent on the
+wavelength of light so if different filters or spectroscopic wavelength
+coverage are used a flat field calibration for each one is required.
+The different flat fields are  automatically selected by a subset
+parameter (see \fBsubsets\fR).
+
+Flat field calibration is selected with the parameter \fBflatcor\fR
+and the flat field images are specified with the parameter \fBflat\fR
+or as part of the input image list.  The appropriate subset is automatically
+selected for each input image processed.  The flat field image is
+automatically processed as needed.  Processing consists of bad pixel
+replacement, overscan subtraction, zero level subtraction, dark count
+subtraction, and trimming.  Also if a scan mode is used and the
+parameter \fIscancor\fR is specified then a scan mode correction is
+applied (see below).  The processing also computes the mean of the
+flat field image which is used later to scale the flat field before
+division into the input image.  For scan mode flat fields the ramp
+part is included in computing the mean which will affect the level
+of images processed with this flat field.  Note that there is no check for
+division by zero in the interest of efficiency.  If division by zero
+does occur a fatal error will occur.  The flat field can be fixed by
+replacing small values using a task such as \fBimreplace\fR or
+during processing using the \fIminreplace\fR parameter.  Note that the
+\fIminreplace\fR parameter only applies to flat fields processed by
+\fBccdproc\fR.
+.sh
+7. Illumcor
+CCD images processed through the flat field calibration may not be
+completely flat (in the absence of objects).  In particular, a blank
+sky image may still show gradients.  This residual nonflatness is called
+the iillumination pattern.  It may be introduced even if the detector is
+uniformly illuminated by the sky because the flat field lamp
+iillumination may be nonuniform.  The iillumination pattern is found from a
+blank sky, or even object image, by heavily smoothing and rejecting
+objects using sigma clipping.  The iillumination calibration image is
+divided into the data being processed to remove the iillumination
+pattern.  The iillumination pattern is a function of the subset so there
+must be an iillumination correction image for each subset to be
+processed.  The tasks \fBmkillumcor\fR and \fBmkskycor\fR are used to
+create the iillumination correction images.  For more on iillumination
+corrections see \fBflatfields\fR.
+
+An alternative to treating the iillumination correction as a separate
+operation is to combine the flat field and iillumination correction
+into a corrected flat field image before processing the object
+images.  This will save some processing time but does require creating
+the flat field first rather than correcting the images at the same
+time or later.  There are two methods, removing the large scale
+shape of the flat field and combining a blank sky image iillumination
+with the flat field.  These methods are discussed further in the
+tasks which create them; \fBmkillumcor\fR and \fBmkskycor\fR.
+.sh
+8. Fringecor
+There may be a fringe pattern in the images due to the night sky lines.
+To remove this fringe pattern a blank sky image is heavily smoothed
+to produce an iillumination image which is then subtracted from the
+original sky image.  The residual fringe pattern is scaled to the
+exposure time of the image to be fringe corrected and then subtracted.
+Because the intensity of the night sky lines varies with time an
+additional scaling factor may be given in the image header.
+The fringe pattern is a function of the subset so there must be
+a fringe correction image for each subset to be processed.
+The task \fBmkfringecor\fR is used to create the fringe correction images.
+.sh
+9. Readcor
+If a zero level correction is desired (\fIzerocor\fR parameter)
+and the parameter \fIreadcor\fR is yes then a single zero level
+correction vector is applied to each readout line or column.  Use of a
+readout correction rather than a two dimensional zero level image
+depends on the nature of the detector or if the CCD is operated in
+longscan mode (see below).  The readout correction is specified by a
+one dimensional image (\fIzero\fR parameter) and the readout axis
+(\fIreadaxis\fR parameter).  If the zero level image is two dimensional
+then it is automatically processed to a one dimensional image by
+averaging across the readout axis.  Note that this modifies the zero
+level calibration image.
+.sh
+10. Scancor
+CCD detectors may be operated in several modes in astronomical
+applications.  The most common is as a direct imager where each pixel
+integrates one point in the sky or spectrum.  However, the design of most CCD's
+allows the sky to be scanned across the CCD while shifting the
+accumulating signal at the same rate.  \fBCcdproc\fR provides for two
+scanning modes called "shortscan" and "longscan".  The type of scan
+mode is set with the parameter \fIscanmode\fR.
+
+In "shortscan" mode the detector is scanned over a specified number of
+lines (not necessarily at sideral rates).  The lines that scroll off
+the detector during the integration are thrown away.  At the end of the
+integration the detector is read out in the same way as an unscanned
+observation.  The advantage of this mode is that the small scale flat
+field response is averaged in one dimension over the number of lines
+scanned.  A flat field may be observed in the same way in which case
+there is no difference in the processing from unscanned imaging and the
+parameter \fIscancor\fR should be no.  However, one obtains an increase
+in the statistical accuracy of the flat fields if they are not scanned
+during the observation but digitally scanned during the processing.  In
+shortscan mode with \fIscancor\fR set to yes, flat field images are
+digitally scanned, if needed, by the specified number of scan lines
+(\fInscan\fR parameter).
+
+In "longscan" mode the detector is continuously read out to produce
+an arbitrarily long strip.  Provided data which has not passed over
+the entire detector is thrown away, the flat field corrections will
+be one dimensional.  If \fIscancor\fR is specified and the
+scan mode is "longscan" then a one dimensional flat field correction
+will be applied.  If the specified flat field (\fIflat\fR parameter)
+is a two dimensional image then when the flat field image is processed
+it will be averaged across the readout axis to form a one dimensional
+correction image.
+.sh
+11. Processing Steps
+The following describes the steps taken by the task.  This detailed
+outline provides the most detailed specification of the task.
+
+.ls 5 (1)
+An image to be processed is first checked that it is of the specified
+CCD image type.  If it is not the desired type then go on to the next image.
+.le
+.ls (2)
+A temporary output image is created of the specified pixel data type
+(\fBccdred.pixeltype\fR).  The header parameters are copied from the
+input image.
+.le
+.ls (3)
+If trimming is specified and the image has not been trimmed previously,
+the trim section is determined.
+.le
+.ls (4)
+If bad pixel replacement is specified and this has not been done
+previously, the bad pixel file is determined either from the task
+parameter or the instrument translation file.  The bad pixel regions
+are read.  If the image has been trimmed previously and the bad pixel
+file contains the word "untrimmed" then the bad pixel coordinates are
+translated to those of the trimmed image.
+.le
+.ls (5)
+If an overscan correction is specified and this correction has not been
+applied, the overscan section is averaged along the readout axis.  If
+trimming is to be done the overscan section is trimmed to the same
+limits.  A function is fit either interactively or noninteractively to
+the overscan vector.  The function is used to produce the overscan
+vector to be subtracted from the image.  This is done in real
+arithmetic.
+.le
+.ls (6)
+If the image is a zero level image go to processing step 12.
+If a zero level correction is desired and this correction has not been
+performed, find the zero level calibration image.  If the zero level
+calibration image has not been processed it is processed at this point.
+This is done by going to processing step 1 for this image.  After the
+calibration image has been processed, processing of the input image
+continues from this point.
+The processed calibration image may be
+cached in memory if it has not been previously and if there is enough memory.
+.le
+.ls (7)
+If the image is a dark count image go to processing step 12.
+If a dark count correction is desired and this correction has not been
+performed, find the dark count calibration image.  If the dark count
+calibration image has not been processed it is processed at this point.
+This is done by going to processing step 1 for this image.  After the
+calibration image has been processed, processing of the input image
+continues from this point.  The ratio of the input image dark time
+to the dark count image dark time is determined to be multiplied with
+each pixel of the dark count image before subtracting from the input
+image.
+The processed calibration image may be
+cached in memory if it has not been previously and if there is enough memory.
+.le
+.ls (8)
+If the image is a flat field image go to processing step 12.  If a flat
+field correction is desired and this correction has not been performed,
+find the flat field calibration image of the appropriate subset.  If
+the flat field calibration image has not been processed it is processed
+at this point.  This is done by going to processing step 1 for this
+image.  After the calibration image has been processed, processing of
+the input image continues from this point.  The mean of the image
+is determined from the image header to be used for scaling.  If no
+mean is found then a unit scaling is used.
+The processed calibration image may be
+cached in memory if it has not been previously and if there is enough memory.
+.le
+.ls (9)
+If the image is an iillumination image go to processing step 12.  If an
+iillumination correction is desired and this correction has not been performed,
+find the iillumination calibration image of the appropriate subset.
+The iillumination image must have the "mkillum" processing flag or the
+\fBccdproc\fR will abort with an error.  The mean of the image
+is determined from the image header to be used for scaling.  If no
+mean is found then a unit scaling is used.  The processed calibration
+image may be
+cached in memory if it has not been previously and there is enough memory.
+.le
+.ls (10)
+If the image is a fringe image go to processing step 12.  If a fringe
+correction is desired and this correction has not been performed,
+find the fringe calibration image of the appropriate subset.
+The iillumination image must have the "mkfringe" processing flag or the
+\fBccdproc\fR will abort with an error.  The ratio of the input
+image exposure time to the fringe image exposure time is determined.
+If there is a fringe scaling in the image header then this factor
+is multiplied by the exposure time ratio.  This factor is used
+for scaling.  The processed calibration image may be
+cached in memory if it has not been previously and there is enough memory.
+.le
+.ls (11)
+If there are no processing operations flagged, delete the temporary output
+image, which has been opened but not used, and go to 14.
+.le
+.ls (12)
+The input image is processed line by line with trimmed lines ignored.
+A line of the input image is read.  Bad pixel replacement and trimming
+is applied to the image.  Image lines from the calibration images
+are read from disk or the image cache.  If the calibration is one
+dimensional (such as a readout zero
+level correction or a longscan flat field correction) then the image
+vector is read only once.  Note that IRAF image I/O is buffered for
+efficiency and accessing a line at a time does not mean that image
+lines are read from disk a line at a time.  Given the input line, the
+calibration images, the overscan vector, and the various scale factors
+a special data path for each combination of corrections is used to
+perform all the processing in the most efficient manner.  If the
+image is a flat field any pixels less than the \fIminreplace\fR
+parameter are replaced by that minimum value.  Also a mean is
+computed for the flat field and stored as the CCDMEAN keyword.
+.le
+.ls (13)
+The input image is deleted or renamed to a backup image.  The temporary
+output image is renamed to the input image name.
+.le
+.ls (14)
+If the image is a zero level image and the readout correction is specified
+then it is averaged to a one dimensional readout correction.
+.le
+.ls (15)
+If the image is a flat field image and the scan mode correction is specified
+then the correction is applied.  For shortscan mode a
+modified two dimensional image is produced while for longscan mode a
+one dimensional average image is produced.
+.le
+.ls (16)
+The processing is completed and either the next input image is processed
+beginning at step 1 or, if it is a calibration image which is being
+processed for an input image, control returns to the step which initiated
+the calibration image processing.
+.le
+.sh
+12. Processing Arithmetic
+The \fBccdproc\fR task has two data paths, one for real image pixel datatypes
+and one for short integer pixel datatype.  In addition internal arithmetic
+is based on the rules of FORTRAN.  For efficiency there is
+no checking for division by zero in the flat field calibration.
+The following rules describe the processing arithmetic and data paths.
+
+.ls (1)
+If the input, output, or any calibration image is of type real the
+real data path is used.  This means all image data is converted to
+real on input.  If all the images are of type short all input data
+is kept as short integers.  Thus, if all the images are of the same type
+there is no datatype conversion on input resulting in greater
+image I/O efficiency.
+.le
+.ls (2)
+In the real data path the processing arithmetic is always real and,
+if the output image is of short pixel datatype, the result
+is truncated.
+.le
+.ls (3)
+The overscan vector and the scale factors for dark count, flat field,
+iillumination, and fringe calibrations are always of type real.  Therefore,
+in the short data path any processing which includes these operations
+will be coerced to real arithmetic and the result truncated at the end
+of the computation.
+.le
+.sh
+13. In the Absence of Image Header Information
+The tasks in the \fBccdred\fR package are most convenient to use when
+the CCD image type, subset, and exposure time are contained in the
+image header.  The ability to redefine which header parameters contain
+this information makes it possible to use the package at many different
+observatories (see \fBinstruments\fR).  However, in the absence of any
+image header information the tasks may still be used effectively.
+There are two ways to proceed.  One way is to use \fBccdhedit\fR
+to place the information in the image header.
+
+The second way is to specify the processing operations more explicitly
+than is needed when the header information is present.  The parameter
+\fIccdtype\fR is set to "" or to "none".  The calibration images are
+specified explicitly by task parameter since they cannot be recognized
+in the input list.  Only one subset at a time may be processed.
+
+If dark count and fringe corrections are to be applied the exposure
+times must be added to all the images.  Alternatively, the dark count
+and fringe images may be scaled explicitly for each input image.  This
+works because the exposure times default to 1 if they are not given in
+the image header.
+.ih
+EXAMPLES
+The user's \fBguide\fR presents a tutorial in the use of this task.
+
+1. In general all that needs to be done is to set the task parameters
+and enter
+
+	cl> ccdproc *.imh &
+
+This will run in the background and process all images which have not
+been processed previously.
+.ih
+TIME REQUIREMENTS
+.nf
+o SUN-3, 15 MHz 68020 with 68881 floating point hardware (no FPA)
+o 8 Mb RAM, 2 Fuji Eagle disks.
+o Input images = 544 x 512 short
+o Output image = 500 x 500 real
+o Operations are overscan subtraction (O), trimming to 500x500 (T),
+  zero level subtraction (Z), dark count scaling and subtraction (D),
+  and flat field scaling and subtraction (F).
+o UNIX statistics
+  (user, system, and clock time, and misc. memory and i/o statistics):
+
+[OTF] One calibration image and 9 object images:
+No caching:  110.6u 25.5s 3:18 68% 28+ 40K 3093+1645io   9pf+0w
+Caching:     111.2u 23.0s 2:59 74% 28+105K 2043+1618io   9pf+0w
+
+[OTZF] Two calibration images and 9 object images:
+No caching:  119.2u 29.0s 3:45 65% 28+ 50K 4310+1660io   9pf+0w
+Caching:     119.3u 23.0s 3:07 75% 28+124K 2179+1601io   9pf+0w
+
+[OTZDF] Three calibration images and 9 object images:
+No caching:  149.4u 31.6s 4:41 64% 28+ 59K 5501+1680io  19pf+0w
+Caching:     151.5u 29.0s 4:14 70% 27+227K 2346+1637io 148pf+0w
+
+[OTZF] 2 calibration images and 20 images processed:
+No caching:  272.7u 63.8u 8:47 63% 28+ 50K 9598+3713io  12pf+0w
+Caching:     271.2u 50.9s 7:00 76% 28+173K 4487+3613io  51pf+0w
+.fi
+.ih
+SEE ALSO
+.nf
+instruments, ccdtypes, flatfields, icfit, ccdred, guide, mkillumcor,
+mkskycor, mkfringecor
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/ccdred.hlp b/noao/imred/quadred/src/quad/doc/ccdred.hlp
new file mode 100644
index 00000000..0300bd38
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/ccdred.hlp
@@ -0,0 +1,98 @@
+.help package Jun87 noao.imred
+.ih
+NAME
+ccdred -- CCD image reduction package
+.ih
+USAGE
+ccdred
+.ih
+PARAMETERS
+.ls pixeltype = "real real"
+Output pixel datatype and calculation datatype.  When images are processed
+or created the output pixel datatype is determined by this parameter.
+The allowed types are "short" for short integer, and "real" for real
+floating point.  Note that if short input images are processed into
+real images the disk space required will generally increase.
+The calculation datatypes are also short and real with a default of
+real if none is specified.
+.le
+.ls verbose = no
+Print log information to the standard output?
+.le
+.ls logfile = "logfile"
+Text log file.  If no filename is specified then no log file is kept.
+.le
+.ls plotfile = ""
+Log metacode plot file for the overscan bias vector fits.  If
+no filename is specified then no metacode plot file is kept.
+.le
+.ls backup = ""
+Backup prefix for backup images.  If no prefix is specified then no backup
+images are kept when processing.  If specified then the backup image
+has the specified prefix.
+.le
+.ls instrument = ""
+CCD instrument translation file.  This is usually set with \fBsetinstrument\fR.
+.le
+.ls ssfile = "subsets"
+Subset translation file used to define the subset identifier.  See
+\fBsubsets\fR for more.
+.le
+.ls graphics = "stdgraph"
+Interactive graphics output device when fitting the overscan bias vector.
+.le
+.ls cursor = ""
+Graphics cursor input.  The default is the standard graphics cursor.
+.le
+.ls version = "June 1987"
+Package version.
+.le
+.ih
+DESCRIPTION
+The CCD reduction package is loaded when this command is entered.  The
+package contains parameters which affect the operation of the tasks
+it defines.  When images are processed or new image are created the
+output pixel datatype is that specified by the parameter \fBpixeltype\fR.
+Note that CCD processing replaces the original image by the processed
+image so the pixel type of the CCD images may change during processing.
+It is unlikely that real images will be processed to short images but
+the reverse is quite likely.  Processing images from short to real
+pixel datatypes will generally increase the amount of disk space
+required (a factor of 2 on most computers).
+
+The tasks produce log output which may be printed on the standard
+output (the terminal unless redirected) and appended to a file.  The
+parameter \fIverbose\fR determines whether processing information
+is printed.  This may be desirable initially, but when using background
+jobs the verbose output should be turned off.  The user may look at
+the end of the log file (for example with \fBtail\fR) to determine
+the status of the processing.
+
+The package was designed to work with data from many different observatories
+and instruments.  In order to accomplish this an instrument translation
+file is used to define a mapping between the package parameters and
+the particular image header format.  The instrument translation file
+is specified to the package by the parameter \fIinstrument\fR.  This
+parameter is generally set by the task \fBsetinstrument\fR.  The other
+file used is a subset file.  This is generally created and maintained
+by the package and the user need not do anything.  For more sophisticated
+users see \fBinstruments\fR and \fBsubsets\fR.
+
+The package has very little graphics
+output.  The exception is the overscan bias subtraction.  The bias
+vector is logged in the metacode plot file if given.  The plot file
+may be examined with the tasks in the \fBplot\fR package such as
+\fBgkimosaic\fR.  When interactively fitting the overscan vector
+the graphics input and output devices must be specified.  The defaults
+should apply in most cases.
+
+Because processing replaces the input image by the processed image it
+may be desired to save the original image.  This may be done by
+specifying a backup prefix with the parameter \fIbackup\fR.  For
+example, if the prefix is "orig" and the image is "ccd001", the backup
+image will be "origccd001".  The prefix may be a directory but it must
+end with '/' or '$' (for logical directories).
+.ih
+SEE ALSO
+instruments, setinstrument, subsets
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/ccdred.ms b/noao/imred/quadred/src/quad/doc/ccdred.ms
new file mode 100644
index 00000000..645514ec
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/ccdred.ms
@@ -0,0 +1,787 @@
+.RP
+.TL
+The IRAF CCD Reduction Package -- CCDRED
+.AU
+Francisco Valdes
+.AI
+IRAF Group - Central Computer Services
+.K2
+P.O. Box 26732, Tucson, Arizona 85726
+September 1987
+.AB
+The IRAF\(dg CCD reduction package, \fBccdred\fR, provides tools
+for the easy and efficient reduction of CCD images.  The standard
+reduction operations are replacement of bad pixels, subtraction of an
+overscan or prescan bias, subtraction of a zero level image,
+subtraction of a dark count image, division by a flat field calibration
+image, division by an illumination correction, subtraction of a fringe
+image, and trimming unwanted lines or columns.  Another common
+operation provided by the package is scaling and combining images with
+a number of algorithms for rejecting cosmic rays.  Data in the image
+header is used to make the reductions largely automated and
+self-documenting though the package may still be used in the absence of
+this data.  Also a translation mechanism is used to relate image header
+parameters to those used by the package to allow data from a variety of
+observatories and instruments to be processed.  This paper describes
+the design goals for the package and the main tasks and algorithms
+which satisfy these goals.
+.PP
+This paper is to be published as part of the proceedings of the
+Santa Cruz Summer Workshop in Astronomy and Astrophysics,
+\fIInstrumentation for Ground-Based Optical Astronomy:  Present and
+Future\fR, edited by Lloyd B. Robinson and published by
+Springer-Verlag.
+.LP
+\(dgImage Reduction and Analysis Facility (IRAF), a software system
+distributed by the National Optical Astronomy Observatories (NOAO).
+.AE
+.NH
+Introduction
+.PP
+The IRAF CCD reduction package, \fBccdred\fR, provides tools
+for performing the standard instrumental corrections and calibrations
+to CCD images.  The major design goals were:
+.IP
+.nf
+\(bu To be easy to use
+\(bu To be largely automated
+\(bu To be image header driven if the data allows
+\(bu To be usable for a variety of instruments and observatories
+\(bu To be efficient and capable of processing large volumes of data
+.fi
+.LP
+This paper describes the important tasks and algorithms and shows how
+these design goals were met.  It is not intended to describe every
+task, parameter, and usage in detail; the package has full
+documentation on each task plus a user's guide.
+.PP
+The standard CCD correction and calibration operations performed are
+replacement of bad columns and lines by interpolation from neighboring
+columns and lines, subtraction of a bias level determined from overscan
+or prescan columns or lines, subtraction of a zero level using a zero
+length exposure calibration image, subtraction of a dark count
+calibration image appropriately scaled to the dark time exposure of the
+image, division by a scaled flat field calibration image, division by
+an illumination image (derived from a blank sky image), subtraction of
+a scaled fringe image (also derived from a blank sky image), and
+trimming the image of unwanted lines or columns such as the overscan
+strip.  The processing may change the pixel datatype on disk (IRAF allows
+seven image datatypes); usually from 16 bit integer to real format.
+Two special operations are also supported for scan mode and one
+dimensional zero level and flat field calibrations; i.e. the same
+calibration is applied to each CCD readout line.  Any set of operations
+may be done simultaneously over a list of images in a highly efficient
+manner.  The reduction operations are recorded in the image header and
+may also be logged on the terminal and in a log file.
+.PP
+The package also provides tools for combining multiple exposures
+of object and calibration images to improve the statistical accuracy of
+the observations and to remove transient bad pixels.  The combining
+operation scales images of different exposure times, adjusts for
+variable sky background, statistically weights the images by their
+signal-to-noise, and provides a number of useful algorithms for
+detecting and rejecting transient bad pixels.
+.PP
+Other tasks are provided for listing reduction information about
+the images, deriving secondary calibration images (such as sky
+corrected flat fields or illumination correction images), and easily
+setting the package parameters for different instruments.
+.PP
+This paper is organized as follows.  There is a section giving an
+overview of how the package is used to reduce CCD data.  This gives the
+user's perspective and illustrates the general ease of use.  The next
+section describes many of the features of the package contributing to
+its ease of use, automation, and generality.  The next two sections
+describe the major tools and algorithms in some detail.  This includes
+discussions about achieving high efficiency.  Finally the status of the
+package and its use at NOAO is given.  References to additional
+documentation about IRAF and the CCD reduction package and an appendix
+listing the individual tasks in the package are found at the end of
+this paper.
+.NH
+A User's Overview
+.PP
+This section provides an overview of reducing data with the IRAF CCD
+reduction package.  There are many variations in usage depending on the
+type of data, whether the image headers contain information about the
+data which may be used by the tasks, and the scientific goal.  Only a
+brief example is given.  A more complete discussion of usage and
+examples is given in \fIA User's Guide to the IRAF CCDRED Package\fR.
+The package was developed within the IRAF system and so makes use of
+all the sophisticated features provided.  These features are also
+summarized here for those not familiar with IRAF since they are an
+important part of using the package.
+.PP
+Since the IRAF system is widely distributed and runs on a wide variety
+of computers, the site of the CCD reductions might be at the telescope,
+a system at the observatory provided for this purpose, or at the
+user's home computer.  The CCD images to be processed are either
+available immediately as the data is taken, transferred from the data taking
+computer via a network link (the method adopted at NOAO), or transferred
+to the reduction computer via a medium such as magnetic tape in FITS
+format.  The flexibility in reduction sites and hardware is one of the
+virtues of the IRAF-based CCD reduction package.
+.PP
+IRAF tasks typically have a number of parameters which give the user
+control over most aspects of the program.  This is possible since the
+parameters are kept in parameter files so that the user need not enter
+a large number of parameters every time the task is run.  The user may
+change any of these parameters as desired in several ways, such as by
+explicit assignment and using an easy to learn and use,
+fill-in-the-value type of screen editor.  The parameter values are
+\fIlearned\fR so that once a user sets the values they are maintained
+until the user changes them again; even between login sessions.
+.PP
+The first step in using the CCD reduction package is to set the default
+processing parameters for the data to be reduced.  These parameters include
+a database file describing the image header keyword translations and
+default values, the processing operations desired (operations
+required vary with instrument and observer), the calibration image names,
+and certain special parameters for special types of observations such
+as scan mode.  A special script task (a command procedure) is available
+to automatically set the default values, given the instrument name, to standard
+values defined by the support staff.  Identifying the instrument in this
+way may be all the novice user need do though most people quickly learn
+to adjust parameters at will.
+.PP
+As an example suppose there is an instrument identified as \fLrca4m\fR
+for an RCA CCD at the NOAO 4 meter telescope.  The user gives the command
+
+.ft L
+    cl> setinstrument rca4m
+.ft R
+
+which sets the default parameters to values suggested by the support staff
+for this instrument.  The user may then change these suggested values if
+desired.  In this example the processing switches are set to perform
+overscan bias subtraction, zero level image subtraction, flat fielding,
+and trimming.
+.PP
+The NOAO image headers contain information identifying the type of
+image, such as object, zero level, and flat field, the filter used to
+match flat fields with object images, the location of the overscan bias
+data, the trim size for the data, and whether the image has been
+processed.  With this information the user need not worry about
+selecting images, pairing object images with calibration images, or
+inadvertently reprocessing an image.
+.PP
+The first step is to combine multiple zero level and flat field observations
+to reduce the effects of statistical noise.  This is done by the
+commands
+
+.nf
+.ft L
+	cl> zerocombine *.imh
+	cl> flatcombine *.imh
+.ft R
+.fi
+
+The "cl> " is the IRAF command language prompt.  The first command says
+look through all the images and combine the zero level images.  The
+second command says look through all the images and combine the flat
+field images by filter.  What could be simpler?  Some \fIhidden\fR (default)
+parameters the user may modify are the combined image name, whether to
+process the images first, and the type of combining algorithm to use.
+.PP
+The next step is to process the images using the combined calibration
+images.  The command is
+
+.ft L
+	cl> ccdproc *.imh
+.ft R
+
+This command says look through all the images, find the object images,
+find the overscan data based on the image header and subtract the
+bias, subtract the zero level calibration image, divide by the flat field
+calibration image, and trim the bias data and edge lines and columns.
+During this operation the task recognizes that the
+zero level and flat field calibration images have not been processed
+and automatically processes them when they are needed.  The log output
+of this task, which may be to the terminal, to a file, or both, shows
+how this works.
+
+.nf
+.ft L
+  ccd003: Jun  1 15:12 Trim data section is [3:510,3:510]
+  ccd003: Jun  1 15:12 Overscan section is [520:540,*], mean=485.0
+  Dark:   Jun  1 15:12 Trim data section is [3:510,3:510]
+  Dark:   Jun  1 15:13 Overscan section is [520:540,*], mean=484.6
+  ccd003: Jun  1 15:13 Dark count image is Dark.imh
+  FlatV:  Jun  1 15:13 Trim data section is [3:510,3:510]
+  FlatV:  Jun  1 15:14 Overscan section is [520:540,*], mean=486.4
+  ccd003: Jun  1 15:15 Flat field image is FlatV.imh, scale=138.2
+  ccd004: Jun  1 15:16 Trim data section is [3:510,3:510]
+  ccd004: Jun  1 15:16 Overscan section is [520:540,*], mean=485.2
+  ccd004: Jun  1 15:16 Dark count image is Dark.imh
+  ccd004: Jun  1 15:16 Flat field image is FlatV.imh, scale=138.2
+                \fI<... more ...>\fL
+  ccd013: Jun  1 15:22 Trim data section is [3:510,3:510]
+  ccd013: Jun  1 15:23 Overscan section is [520:540,*], mean=482.4
+  ccd013: Jun  1 15:23 Dark count image is Dark.imh
+  FlatB:  Jun  1 15:23 Trim data section is [3:510,3:510]
+  FlatB:  Jun  1 15:23 Overscan section is [520:540,*], mean=486.4
+  ccd013: Jun  1 15:24 Flat field image is FlatB.imh, scale=132.3
+                \fI<... more ...>\fL
+.ft R
+.fi
+
+.PP
+The log gives the name of the image and a time stamp for each entry.
+The first image is ccd003.  It is to be trimmed to the specified
+size given as an \fIimage section\fR, an array notation used commonly
+in IRAF to specify subsections of images.  The location of the
+overscan data is also given by an image section which, in this case,
+was found in the image header.  The mean bias level of the overscan
+is also logged though the overscan is actually a function of the
+readout line with the order of the function selected by the user.
+.PP
+When the task comes to subtracting the zero level image it first
+notes that the calibration image has not been processed and switches
+to processing the zero level image.  Since it knows it is a zero level
+image the task does not attempt to zero level or flat field correct
+this image.  After the zero level image has been processed the task
+returns to the object image only to find that the flat field image
+also has not been processed.  It determines that the object image was
+obtained with a V filter and selects the flat field image having the same
+filter.  The flat field image is processed through the zero level correction
+and then the task again returns to the object image, ccd003, which it
+finishes processing.
+.PP
+The next image, ccd004, is also a V filter
+observation.  Since the zero level and V filter flat field have been
+processed the object image is processed directly.  This continues
+for all the object images except for a detour to process the B filter flat
+field when the task first encounters a B filter object image.
+.PP
+In summary, the basic usage of the CCD reduction package is quite simple.
+First, the instrument is identified and some parameters for the data
+are set.  Calibration images are then combined if needed.  Finally,
+the processing is done with the simple command
+
+.ft L
+    cl> ccdproc *.imh&
+.ft R
+
+where the processing is performed as a \fIbackground job\fR in this example.
+This simplicity was a major goal of the package.
+.NH
+Features of the Package
+.PP
+This section describes some of the special features of the package
+which contribute to its ease of use, generality, and efficiency.
+The major criteria for ease of use are to minimize the user's record keeping
+involving input and output image names, the types of images, subset
+parameters such as filters which must be kept separate, and the state
+of processing of each image.  The goal is to allow input images to
+be specified using simple wildcards, such as "*.imh" to specify all
+images, with the knowledge that the task will only operate on images
+for which it makes sense.  To accomplish this the tasks must be able to
+determine the type of image, subset, and the state of processing from
+the image itself.  This is done by making use of image header parameters.
+.PP
+For generality the package does not require any image header information
+except the exposure time.  It is really not very much more difficult to
+reduce such data.  Mainly, the user must be more explicit about specifying
+images and setting task parameters or add the information to the image
+headers.  Some default header information may also be set in the image
+header translation file (discussed below).
+.PP
+One important image header parameter is the image type.  This
+discriminates between object images and various types of calibration
+images such as flat field, zero level, dark count, comparison arcs,
+illumination, and fringe images.  This information is used in two
+ways.  For most of the tasks the user may select that only one type of
+image be considered.  Thus, all the flat field images may be selected
+for combining or only the processing status of the object images be
+listed.  The second usage is to allow the processing tasks to identify
+the standard calibration images and apply only those operations which
+make sense.  For example, flat field images are not divided by a
+flat field.  This allows the user to set the processing operations
+desired for the object images without fear of misprocessing the
+calibration images.  The image type is also used to automatically
+select calibration images from a list of images to be processed instead
+of explicitly identifying them.
+.PP
+A related parameter specifies the subset.  For certain operations the
+images must have a common value for this parameter.  This parameter is
+often the filter but it may also apply to a grating or aperture, for example.
+The subset parameter is used to identify the appropriate flat field
+image to apply to an image or to select common flat fields to be combined
+into a higher quality flat field.  This is automatic and the user need not
+keep track of which image was taken with which filter or grating.
+.PP
+The other important image header parameters are the processing flags.
+These identify when an image has been processed and also act as a history
+of the operation including calibration images used and other parameter
+information.  The usage of these parameters is obvious; it allows the
+user to include processed images in a wildcard list knowing that the
+processing will not be repeated and to quickly determine the processing
+status of the image.
+.PP
+Use of image header parameters often ties the software to the a
+particular observatory.  To maintain generality and usefulness for data
+other than that at NOAO, the CCD reduction package was designed to
+provide a translation between parameters requested by the package and
+those actually found in the image header.  This translation is defined
+in a simple text file which maps one keyword to another and also gives
+a default value to be used if the image header does not include a
+value.  In addition the translation file maps the arbitrary strings
+which may identify image types to the standard types which the package
+recognizes.  This is a relatively simple scheme and does not allow for
+forming combinations or for interpreting values which are not simple
+such as embedding an exposure time as part of a string.  A more complex
+translation scheme may prove desirable as experience is gained with
+other types of image header formats, but by then a general header translation
+ability and/or new image database structure may be a standard IRAF
+feature.
+.PP
+This feature has proven useful at NOAO.  During the course of
+developing the package the data taking system was modernized by
+updating keywords and adding new information in the image headers,
+generally following the lines laid out by the \fBccdred\fR package.
+However, there is a period of transition and it is also desirable to
+reduce preexisting data.  There are several different formats for this
+data.  The header translation files make coping with these different
+formats relatively easy.
+.PP
+A fundamental aspect of the package is that the processing
+modifies the images.  In other words, the reduction operations are
+performed directly on the image.  This "feature" further simplifies
+record keeping, frees the user from having to form unique output image
+names, and minimizes the amount of disk space required.  There
+are two safety features in this process.  First, the modifications do
+not take effect until the operation is completed on the image.  This
+allows the user to abort the task without leaving the image data in a
+partially processed state and protects data if the computer
+crashes.  The second feature is that there is a parameter which may be
+set to make a backup of the input data with a particular prefix; for
+example "b", "orig", or "imdir$" (a logical directory prefix).  This
+backup feature may be used when there is sufficient disk space, when
+learning to use the package, or just to be cautious.
+.PP
+In a similar effort to efficiently manage disk space, when combining
+images into a master object or calibration image, there is an option to
+delete the input images upon completion of the combining operation.
+Generally this is desirable when there are many calibration exposures,
+such as zero level or flat field images, which are not used after they
+are combined into a final calibration image.
+.PP
+The goal of generality for many instruments at
+different observatories inherently conflicts with the goal of ease of
+use.  Generality requires many parameters and options.  This is
+feasible in the CCD reduction package, as well as the other IRAF packages,
+because of the IRAF parameter handling mechanism.  In \fBccdred\fR
+there still remains the problem of setting the parameters appropriately
+for a particular instrument, image header format, and observatory.
+.PP
+To make this convenient there is a task, \fBsetinstrument\fR, that,
+based on an instrument name, runs a setup script for the instrument.
+An example of this task was given in the previous section.
+The script may do any type of operation but mainly it sets default
+parameters.  The setup scripts are generally created by the support staff
+for the instrument.  The combination of the setup script and the
+instrument translation file make the package, in a sense, programmable
+and achieves the desired instrument/observatory generality with ease of use.
+.NH
+CCD Processing
+.PP
+This section describes in some detail how the CCD processing is performed.
+The task which does the basic CCD processing is call \fBccdproc\fR.
+From the point of view of usage the task is very simple but a great deal
+is required to achieve this simplicity.  The approach we take in describing
+the task is to follow the flow of control as the task runs with digressions
+as appropriate.
+.PP
+The highest level of control is a loop over the input images; all the
+operations are performed successively on each image.  It is common for
+IRAF tasks which operate on individual images to allow the operation to
+be repeated automatically over a list of input images.  This is important
+in the \fBccdred\fR package because data sets are often large and the
+processing is generally the same for each image.  It would be tedious
+to have to give the processing command for each image to be processed.
+If an error occurs while processing an image the error is
+printed as a warning and processing continues with the next image.
+This provides protection primarily against mistyped or nonexistent images.
+.PP
+Before the first image is processed the calibration images are
+identified.  There are two ways to specify calibration images;
+explicitly via task parameters or implicitly as part of the list of
+images to be processed.  Explicitly identifying calibration images
+takes precedence over calibration images in the input list.  Specifying
+calibration images as part of the input image list requires that the
+image types can be determined from the image header.  Using the input
+list provides a mechanism for breaking processing up into sets of
+images (possibly using files containing the image names for each set)
+each having their own calibration images.  One can, of course,
+selectively specify input and calibration images, but whenever possible
+one would like to avoid having to specify explicit images to process
+since this requires record keeping by the user.
+.PP
+The first step in processing an image is to check that it is of the
+appropriate image type.  The user may select to process images of only
+one type.  Generally this is object images since calibration images are
+automatically processed as needed.  Images which are not of the desired
+type are skipped and the next image is considered.
+.PP
+A temporary output image is created next.  The output pixel datatype on
+disk may be changed at this point as selected by the user.
+For example it is common for the raw CCD images to be digitized as 16
+bit integers but after calibration it is sometimes desirable to have
+real format pixels.  If no output pixel datatype is specified the
+output image takes the same pixel datatype as the input image.  The
+processing is done by operating on the input image and writing the
+results to a temporary output image.  When the processing is complete
+the output image replaces the input image.  This gives the effect of
+processing the images in place but with certain safeguards.  If the
+computer crashes or the processing is interrupted the integrity of the
+input image is maintained.  The reasons for chosing to process the
+images in this way are to avoid having to generate new image names (a
+tiresome record keeping process for the user), to minimize disk
+usage, and generally the unprocessed images are not used once they have
+been processed.  When dealing with large volumes of data these reasons
+become fairly important.  However, the user may specify a backup prefix
+for the images in which case, once the processing is completed, the
+original input image is renamed by appending it to the prefix (or with
+an added digit if a previous backup image of the same name exits)
+before the processed output image takes the original input name.
+.PP
+The next step is to determine the image geometry.  Only a subsection of
+the raw image may contain the CCD data.  If this region is specified by
+a header parameter then the processing will affect only this region.
+This allows calibration and other data to be part of the image.
+Normally, the only other data in a image is overscan or prescan data.
+The location of this bias data is determined from the image header or
+from a task parameter (which overrides the image header value).  To
+relate calibration images of different sizes and to allow for readout
+of only a portion of the CCD detector, a header parameter may relate
+the image data coordinates to the full CCD coordinates.  Application of
+calibration image data and identifying bad pixel regions via a bad
+pixel file is done in this CCD coordinate system.  The final
+geometrical information is the region of the input image to be output
+after processing; an operation called trimming.  This is defined by an
+image header parameter or a task parameter.  Trimming of the image is
+selected by the user.  Any or all of this geometry information may be
+absent from the image and appropriate defaults are used.
+.PP
+Each selected operation which is appropriate for the image type is then
+considered.  If the operation has been performed previously it will not
+be repeated.  If all selected operations have been performed then the
+temporary output image is deleted and the input image is left
+unchanged.  The next image is then processed.
+.PP
+For each selected operation to be performed the pertinent data is
+determined.  This consists of such things as the name of the
+calibration image, scaling factors, the overscan bias function, etc.
+Note that at this point only the parameters are determined, the
+operation is not yet performed.  This is because operations are not
+performed sequentially but simultaneously as described below.  Consider
+flat fielding as an example.  First the input image is checked to see
+if it has been flat fielded.  Then the flat field calibration image is
+determined.  The flat field image is checked to see if it has been
+processed.  If it has not been processed then it is processed by
+calling a procedure which is essentially a copy of the main processing
+program.  After the flat field image has been processed, parameters
+affecting the processing, such as the flat field scale factor
+(essentially the mean of the flat field image), are determined.  A log
+of the operation is then printed if desired.
+.PP
+Once all the processing operations and parameters have been defined the
+actual processing begins.  One of the key design goals was that the
+processing be efficient.  There are two primary methods used to achieve
+this goal; separate processing paths for 16 bit integer data and
+floating point data and simultaneous operations.  If the image, the
+calibration images, and the output image (as selected by the user) are
+16 bit integer pixel datatypes then the image data is read and written
+as integer data.  This eliminates internal datatype conversions both
+during I/O and during computations.  However, many operations include
+use of real factors such as the overscan bias, dark count exposure
+scaling, and flat field scaling which causes the computation to be done
+in real arithmetic before the result is stored again as an integer
+value.  In any case there is never any loss of precision except when
+converting the output pixel to short integer.  If any of the images are
+not integer then a real internal data path is used in which input and
+output image data are converted to real as necessary.
+.PP
+For each data path the processing proceeds line-by-line.  For each line
+in the output image data region (ignoring pixels outside the data area
+and pixels which are trimmed) the appropriate input data and
+calibration data are obtained.  The calibration data is determined from
+the CCD coordinates of the output image and are not necessarily from
+the same image line or columns.  The input data is copied to the output
+array while applying bad pixel corrections and trimming.  The line is
+then processed using a specially optimized procedure.  This procedure
+applies all operations simultaneously for all combinations of
+operations.  As an example, consider subtracting an overscan bias,
+subtracting a zero level, and dividing by a flat field.  The basic
+kernel of the task, where the bulk of the CPU time is used, is
+
+.nf
+.ft L
+  do i = 1, n
+      out[i] = (out[i] - overscan - zero[i]) * flatscale / flat[i]
+.ft R
+.fi
+
+Here, \fIn\fR is the number of pixels in the line, \fIoverscan\fR is
+the overscan bias value for the line, \fIzero\fR is the zero level data
+from the zero level image, \fIflatscale\fR is the mean of the flat
+field image, and \fIflat\fR is the flat field data from the flat
+field image.  Note the operations are not applied sequentially but
+in a single statement.  This is the most efficient method and there is
+no need for intermediate images.
+.PP
+Though the processing is logically performed line-by-line in the program,
+the image I/O from the disk is not done this way.  The IRAF virtual
+operating system image interface automatically provides multi-line
+buffering for maximal I/O efficiency.
+.PP
+In many image processing systems it has been standard to apply operations
+sequentially over an image.  This requires producing intermediate images.
+Since this is clearly inefficient in terms of I/O it has been the practice
+to copy the images into main memory and operate upon them there until
+the final image is ready to be saved.  This has led to the perception
+that in order to be efficient an image processing system \fImust\fR
+store images in memory.  This is not true and the IRAF CCD reduction
+package illustrates this.  The CCD processing does not use intermediate
+images and does not need to keep the entire image in main memory.
+Furthermore, though of lesser importance than I/O, the single statement method
+illustrated above is more efficient than multiple passes through the
+images even when the images are kept in main memory.  Finally, as CCD
+detectors increase in size and small, fast, and cheap processors become
+common it is a distinct advantage to not require the large amounts of
+memory needed to keep entire images in memory.
+.PP
+There is one area in which use of main memory can improve performance
+and \fBccdproc\fR does take advantage of it if desired.  The calibration
+images usually are the same for many input images.  By specifying the
+maximum amount of memory available for storing images in memory
+the calibration images may be stored in memory up to that amount.
+By parameterizing the memory requirement there is no builtin dependence
+on large memory!
+.PP
+After processing the input image the last steps are to log the operations
+in the image header using processing keywords and replace the input
+image by the output image as described earlier.  The CCD coordinates
+of the data are recorded in the header, even if not there previously, to
+allow further processing on the image after the image has been trimmed.
+.NH
+Combining Images
+.PP
+The second important tool in the CCD reduction package is a task to combine
+many images into a single, higher quality image.  While this may also be
+done with more general image processing tools (the IRAF task \fBimsum\fR
+for example) the \fBccdred\fR tasks include special CCD dependent features such
+as recognizing the image types and using the image header translation
+file.  Combining images is often done
+with calibration images, which are easy to obtain in number, where it
+is important to minimize the statistical noise so as to not affect the
+object images.  Sometimes object images also are combined.
+The task is called \fBcombine\fR and there are special versions of
+this task called \fBzerocombine, darkcombine\fR, and \fBflatcombine\fR
+for the standard calibration images.
+.PP
+The task takes a list of input images to be combined.  As output there
+is the combined image, an optional sigma image, and optional log output either
+to the terminal, to a log file, or both.  A subset or subsets
+of the input images may be selected based on the image type and a
+subset parameter such as the filter.  As with the processing task,
+this allows selecting images without having to explicitly list each
+image from a large data set.  When combining based on a subset parameter
+there is an output image, and possibly a sigma image, for each separate subset.
+The output image pixel datatype may also be changed during combining;
+usually from 16 bit integer input to real output.
+The sigma image is the standard deviation of the input images about the
+output image.
+.PP
+Except for summing the images together,
+combining images may require correcting for variations between the images
+due to differing exposure times, sky background, extinctions, and
+positions.  Currently, extinction corrections and registration are
+not included but scaling and shifting corrections are included.
+The scaling corrections may be done by exposure times or by computing
+the mode in each image.  Additive shifting is also done by computing
+the mode in the images.  The region of the image in which the mode
+is computed can be specified but by default the whole image is used.
+A scaling correction is used when the flux level or sensitivity is varying.
+The offset correction is used when the sky brightness is varying independently
+of the object brightness.  If the images are not scaled then special
+data paths combine the images more efficiently.
+.PP
+Except for medianing and summing, the images are combined by averaging.
+The average may be weighted by
+
+.nf
+.ft L
+	weight = (N * scale / mode) ** 2
+.ft R
+.fi
+
+where \fIN\fR is the number of images previously combined (the task
+records the number of images combined in the image header), \fIscale\fR
+is the relative scale (applied by dividing) from the exposure time or
+mode, and \fImode\fR is the background mode estimate used when adding a
+variable offset.
+.PP
+The combining operation is the heart of the task.  There are a number
+algorithms which may be used as well as applying statistical weights.
+The algorithms are used to detect and reject deviant pixels, such as
+cosmic rays.
+The choice of algorithm depends on the data, the number of images,
+and the importance of rejecting cosmic rays.  The more complex the
+algorithm the more time consuming the operation.
+The list below summarizes the algorithms.
+Further algorithms may be added in time.
+
+.IP "Sum - sum the input images"
+.br
+The input images are combined by summing.  Care must be taken
+not to exceed the range of the 16 bit integer datatype when summing if the
+output datatype is of this type.  Summing is the only algorithm in which
+scaling and weighting are not used.  Also no sigma image is produced.
+.IP "Average - average the input images"
+.br
+The input images are combined by averaging.  The images may be scaled
+and weighted.  There is no pixel rejection.  A sigma image is produced
+if more than one image is combined.
+.IP "Median - median the input images"
+.br
+The input images are combined by medianing each pixel.  Unless the images
+are at the same exposure level they should be scaled.  The sigma image
+is based on all the input images and is only an approximation to the
+uncertainty in the median estimates.
+.IP "Minreject, maxreject, minmaxreject - reject extreme pixels"
+.br
+At each pixel the minimum, maximum, or both are excluded from the
+average.  The images should be scaled and the average may be
+weighted.  The sigma image requires at least two pixels after rejection
+of the extreme values.  These are relatively fast algorithms and are
+a good choice if there are many images (>15).
+.IP "Threshold - reject pixels above and below specified thresholds"
+.br
+The input images are combined with pixels above and below specified
+threshold values (before scaling) excluded.  The images may be scaled
+and the average weighted.  The sigma image also has the rejected
+pixels excluded.
+.IP "Sigclip - apply a sigma clipping algorithm to each pixel"
+.br
+The input images are combined by applying a sigma clipping algorithm
+at each pixel.  The images should be scaled.  This only rejects highly
+deviant points and so
+includes more of the data than the median or minimum and maximum 
+algorithms.  It requires many images (>10-15) to work effectively.
+Otherwise the bad pixels bias the sigma significantly.  The mean
+used to determine the sigmas is based on the "minmaxrej" algorithm
+to eliminate the effects of bad pixels on the mean.  Only one
+iteration is performed and at most one pixel is rejected at each
+point in the output image.  After the deviant pixels are rejected the final
+mean is computed from all the data.  The sigma image excludes the
+rejected pixels.
+.IP "Avsigclip - apply a sigma clipping algorithm to each pixel"
+.br
+The input images are combined with a variant of the sigma clipping
+algorithm which works well with only a few images.  The images should
+be scaled.  For each line the mean is first estimated using the
+"minmaxrej" algorithm.  The sigmas at each point in the line are scaled
+by the square root of the mean, that is a Poisson scaling of the noise
+is assumed.  These sigmas are averaged to get a line estimate of the
+sigma.  Then the sigma at each point in the line is estimated by
+multiplying the line sigma by the square root of the mean at that point.  As
+with the sigma clipping algorithm only one iteration is performed and
+at most one pixel is rejected at each point.  After the deviant pixels
+are rejected the file mean is computed from all the data.  The sigma
+image excludes the rejected pixels.
+.RE
+.PP
+The "avsigclip" algorithm is the best algorithm for rejecting cosmic
+rays, especially with a small number of images, but it is also the most
+time consuming.  With many images (>10-15) it might be advisable to use
+one of the other algorithms ("maxreject", "median", "minmaxrej") because
+of their greater speed.
+.PP
+This task also has several design features to make it efficient and
+versatile.  There are separate data paths for integer data and real
+data; as with processing, if all input images and the output image are
+of the same datatype then the I/O is done with no internal conversions.
+With mixed datatypes the operations are done as real.  Even in the
+integer path the operations requiring real arithmetic to preserve the
+accuracy of the calculation are performed in that mode.  There is
+effectively no limit to the number of images which may be combined.
+Also, the task determines the amount of memory available and buffers
+the I/O as much as possible.  This is a case where operating on images
+from disk rather than in memory is essential.
+.NH
+Status and Conclusion
+.PP
+The initial implementation of the IRAF \fBccdred\fR package was
+completed in June 1987.  It has been in use at the National Optical
+Astronomy Observatories since April 1987.  The package was not
+distributed with Version 2.5 of IRAF (released in August 1987) but is
+available as a separate installation upon request.  It will be part of
+future releases of IRAF.
+.PP
+At NOAO the CCD reduction package is available at the telescopes as the
+data is obtained.  This is accomplished by transferring the images from
+the data taking computer to a Sun workstation (Sun Microsystems, Inc.)
+initially via tape and later by a direct link.  There are several
+reasons for adopting this architecture.  First, the data acquisition
+system is well established and is dedicated to its real-time function.
+The second computer was phased in without disrupting the essential
+operation of the telescopes and if it fails data taking may continue
+with data being stored on tape.  The role of the second computer is to
+provide faster and more powerful reduction and analysis capability not
+required in a data acquisition system.  In the future it can be more
+easily updated to  follow the state of the art in small computers.  As
+CCD detectors get larger the higher processing speeds will be essential
+to keep up with the data flow.
+.PP
+By writing the reduction software in the high level, portable, IRAF
+system the users have the capability to process their data from the
+basic CCD reductions to a full analysis at the telescope.  Furthermore,
+the same software is widely available on a variety of computers if
+later processing or reprocessing is desired; staff and visitors at NOAO
+may also reduce their data at the headquarters facilities.  The use of
+a high level system was also essential in achieving the design goals;
+it would be difficult to duplicate this complex package without
+the rich programming environment provided by the IRAF system.
+.NH
+References
+.PP
+The following documentation is distributed by the National Optical
+Astronomy Observatories, Central Computer Services, P.O. Box 26732,
+Tucson, Arizona, 85726.  A comprehensive description of the IRAF system
+is given in \fIThe IRAF Data Reduction and Analysis System\fR by Doug
+Tody (also appearing in \fIProceedings of the SPIE - Instrumentation in
+Astronomy VI\fR, Vol. 627, 1986).  A general guide to using IRAF is \fIA
+User's Introduction to the IRAF Command Language\fR by Peter Shames
+and Doug Tody.  Both these documents are also part of the IRAF
+documentation distributed with the system.
+.PP
+A somewhat more tutorial description of the \fBccdred\fR package is
+\fIA User's Guide to the IRAF CCDRED Package\fR by the author.
+Detailed task descriptions and supplementary documentation are
+given in the on-line help library and are part of the user's guide.
+.NH
+Appendix
+.PP
+The current set of tasks making up the IRAF CCD Reduction Package,
+\fBccdred\fR, are summarized below.
+
+.nf
+.ft L
+  badpiximage - Create a bad pixel mask image from a bad pixel file
+    ccdgroups - Group CCD images into image lists
+     ccdhedit - CCD image header editor
+      ccdlist - List CCD processing information
+      ccdproc - Process CCD images
+      combine - Combine CCD images
+  darkcombine - Combine and process dark count images
+  flatcombine - Combine and process flat field images
+  mkfringecor - Make fringe correction images from sky images
+   mkillumcor - Make flat field illumination correction images
+  mkillumflat - Make illumination corrected flat fields
+     mkskycor - Make sky illumination correction images
+    mkskyflat - Make sky corrected flat field images
+setinstrument - Set instrument parameters
+  zerocombine - Combine and process zero level images
+.fi
+.ft R
diff --git a/noao/imred/quadred/src/quad/doc/ccdtypes.hlp b/noao/imred/quadred/src/quad/doc/ccdtypes.hlp
new file mode 100644
index 00000000..2cec33ea
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/ccdtypes.hlp
@@ -0,0 +1,124 @@
+.help ccdtypes Jun87 noao.imred.ccdred
+.ih
+NAME
+ccdtypes -- Description of the CCD image types
+.ih
+CCDTYPES
+The following CCD image types may be specified as the value of the parameter
+\fIccdtype\fR:
+
+.nf
+	""	- (the null string) all image types
+	object	- object images
+	zero	- zero level images such as a bias or preflash
+	dark	- dark count images
+	flat	- flat field images
+	illum	- iillumination images
+	fringe	- fringe correction images
+	other   - other image types defined in the translation file
+	none	- images without an image type parameter
+	unknown - image types not defined in the translation file
+.fi
+.ih
+DESCRIPTION
+The \fBccdred\fR package recognizes certain standard CCD image types
+identified in the image header.  The tasks may select images of a
+particular CCD image type from image lists with the parameter
+\fIccdtype\fR and also recognize and take special actions for
+calibration images.
+
+In order to make use of CCD image type information the header keyword
+identifying the image type must be specified in the instrument
+translation file.  This entry has the form
+
+	imagetyp keyword
+
+where keyword is the image header keyword.  This allows the package to
+access the image type string.  There must also be a translation between
+the image type strings and the CCD types as recognized by the package.
+This information consists of lines in the instrument translation file
+of the form
+
+	header	package
+
+where header is the exact string given in the image header and package
+is one of the types recognized by the package.  The image header string
+can be virtually anything and if it contains blanks it must be
+quoted.  The package image types are those given above except for
+the null string, "none", and "unknown".  That is, these types may
+be specified as a CCD image type in selecting images but not as a translations
+of image type strings.
+
+There may be more than one image type that maps to the same package
+type.  In particular other standard CCD image types, such as comparison
+spectra, multiple exposure, standard star, etc., should be mapped to
+object or other.  There may also be more than one type of flat field, i.e. dome
+flat, sky flat, and lamp flat.  For more on the instrument translation
+file see the help for \fBinstruments\fR.
+.ih
+EXAMPLES
+1. The example entries in the instrument translation file are from the 1986
+NOAO CCD image header format produced by the CAMERA format tape writer.
+
+.nf
+    imagetyp			data-typ
+
+    'OBJECT (0)'		object
+    'DARK (1)'			dark
+    'PROJECTOR FLAT (2)'	flat
+    'SKY FLAT (3)'		other
+    'COMPARISON LAMP (4)'	other
+    'BIAS (5)'			zero
+    'DOME FLAT (6)'		flat
+.fi
+
+The image header keyword describing the image type is "data-typ".
+The values of the image type strings in the header contain blanks so they
+are quoted.  Also the case of the strings is important.  Note that there
+are two types of flat field images and two types of other images.
+
+2. One way to check the image types is with the task \fBccdlist\fR.
+
+.nf
+    cl> ccdlist *.imh
+    Zero.imh[504,1][real][zero][1][OT]:FOCUS L98-193
+    Flat1.imh[504,1][real][flat][1][OTZ]:dflat 6v+blue 5s
+    ccd002.imh[504,504][real][unknown][1][OTZF]:FOCUS L98-193
+    ccd003.imh[544,512][short][object][1]:L98-193
+    ccd004.imh[544,512][short][object][1]:L98-193
+    ccd005.imh[544,512][short][object][1]:L98-193
+    oldformat.imh[544,512][short][none][1]:M31 V
+.fi
+
+The unknown type has a header image type of "MUL (8)".  The old format
+image does not have any header type.
+
+3. To select only images of a particular type:
+
+.nf
+    cl> ccdlist *.imh ccdtype=object
+    ccd003.imh[544,512][short][object][1]:L98-193
+    ccd004.imh[544,512][short][object][1]:L98-193
+    ccd005.imh[544,512][short][object][1]:L98-193
+    cl> ccdlist *.imh ccdtype=unknown
+    ccd002.imh[504,504][real][unknown][1][OTZF]:FOCUS L98-193
+    cl> ccdlist *.imh ccdtype=none
+    oldformat.imh[544,512][short][none][1]:M31 V
+.fi
+
+4. To process images with \fBccdproc\fR:
+
+.nf
+    cl> ccdproc *.imh
+    cl> ccdproc *.imh ccdtype=object
+.fi
+
+In the first case all the images will be processed (the default value of
+\fIccdtype\fR is "").  However, the task recognizes the calibration
+images, such as zero level and flat fields, and processes them appropriately.
+In the second case only object images are processed and all other images
+are ignored (except if needed as a calibration image).
+.ih
+SEE ALSO
+instruments
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/combine.hlp b/noao/imred/quadred/src/quad/doc/combine.hlp
new file mode 100644
index 00000000..b3c0848e
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/combine.hlp
@@ -0,0 +1,1030 @@
+.help combine Sep92 noao.imred.ccdred
+.ih
+NAME
+combine -- Combine CCD images using various algorithms
+.ih
+USAGE	
+combine input output
+.ih
+PARAMETERS
+.ls input
+List of CCD images to combine.  Images of a particular CCD image type may be
+selected with the parameter \fIccdtype\fR with the remaining images ignored.
+.le
+.ls output
+Output combined image or list of images.  If the \fIproject\fR parameter is
+no (the typical case for CCD acquisition) then there will be one output image
+or, if the \fIsubsets\fR parameter is selected, one output image per subset.
+If the images consist of stacks then the \fIproject\fR option allows combining
+each input stack into separate output images as given by the image list.
+.le
+.ls plfile = "" (optional)
+Output pixel list file or list of files.  If no name is given or the
+list ends prematurely then no file is produced.  The pixel list file
+is a map of the number of pixels rejected or, equivalently,
+the total number of input images minus the number of pixels actually used.
+The file name is also added to the output image header under the
+keyword BPM.
+.le
+.ls sigma = "" (optional)
+Output sigma image or list of images.  If no name is given or the list ends
+prematurely then no image is produced.  The sigma is standard deviation,
+corrected for a finite population, of the input pixel values (excluding
+rejected pixels) about the output combined pixel values.
+.le
+
+.ls ccdtype = ""
+CCD image type to combine.  If specified only input images of the specified
+type are combined.  See \fBccdtypes\fR for the possible image types.
+.le
+.ls subsets = no
+Combine images by subset parameter?  If yes then the input images are
+grouped by subset parameter and each group combined into a separate output
+image.  The subset identifier is appended to the output image
+name(s).  See \fBsubsets\fR for more on the subset parameter.
+.le
+.ls delete = no
+Delete input images after combining?  Only those images combined are deleted.
+.le
+.ls clobber = no
+Clobber existing output images?
+.le
+
+.ls combine = "average" (average|median)
+Type of combining operation performed on the final set of pixels (after
+offsetting, masking, thresholding, and rejection).  The choices are
+"average" or "median".  The median uses the average of the two central
+values when the number of pixels is even.
+.le
+.ls reject = "none" (none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip)
+Type of rejection operation performed on the pixels remaining after offsetting,
+masking and thresholding.  The algorithms are discussed in the
+DESCRIPTION section.  The rejection choices are:
+
+.nf
+      none - No rejection
+    minmax - Reject the nlow and nhigh pixels
+   ccdclip - Reject pixels using CCD noise parameters
+  crreject - Reject only positive pixels using CCD noise parameters
+   sigclip - Reject pixels using a sigma clipping algorithm
+ avsigclip - Reject pixels using an averaged sigma clipping algorithm
+     pclip - Reject pixels using sigma based on percentiles
+.fi
+
+.le
+.ls project = no
+Project (combine) across the highest dimension of the input images?  If
+no then all  the input images are combined to a single output image.  If
+yes then the highest dimension elements of each input image are combined to
+an output image and optional pixel list and sigma images.  Each element of
+the highest dimension may have a separate offset but there can only be one
+mask image.
+.le
+.ls outtype = "real" (short|integer|long|real|double)
+Output image pixel datatype.  The pixel datatypes are "double",
+"real", "long", "integer", and "short" with highest precedence first.
+If none is specified then the highest precedence datatype of the input
+images is used.  The datatypes may be abbreviated to a single character.
+.le
+.ls offsets = "none" (none|grid|<filename>)
+Input image offsets.  The offsets may be specified in a file consisting
+of one line per image with the offsets in each dimension forming the
+columns.  The special case of a grid may be specified by the string:
+
+.nf
+	grid [n1] [s1] [n2] [s2] ...
+.fi
+
+where ni is the number of images in dimension i and si is the step
+in dimension i.  For example "grid 5 100 5 100" specifies a 5x5
+grid with origins offset by 100 pixels.
+.le
+.ls masktype = "none" (none|goodvalue|badvalue|goodbits|badbits)
+Type of pixel masking to use.  If "none" then no pixel masking is done
+even if an image has an associated  pixel mask.  The other choices
+are to select the value in the pixel mask to be treated as good
+(goodvalue) or bad (badvalue) or the bits (specified as a value)
+to be treated as good (goodbits) or bad (badbits).  The pixel mask
+file name comes from the image header keyword BPM.
+.le
+.ls maskvalue = 0
+Mask value used with the \fImasktype\fR parameter.  If the mask type
+selects good or bad bits the value may be specified using IRAF notation
+for decimal, octal, or hexadecimal; i.e 12, 14b, 0cx to select bits 3
+and 4.
+.le
+.ls blank = 0.
+Output value to be used when there are no pixels.
+.le
+
+.ls scale = "none" (none|mode|median|mean|exposure|@<file>|!<keyword>)
+Multiplicative image scaling to be applied.  The choices are none, scale
+by the mode, median, or mean of the specified statistics section, scale
+by the exposure time in the image header, scale by the values in a specified
+file, or scale by a specified image header keyword.  When specified in
+a file the scales must be one per line in the order of the input
+images.
+.le
+.ls zero = "none" (none|mode|median|mean|@<file>|!<keyword>)
+Additive zero level image shifts to be applied.  The choices are none or
+shift by the mode, median, or mean of the specified statistics section,
+shift by values given in a file, or shift by values given by an image
+header keyword.  When specified in a file the zero values must be one
+per line in the order of the input images.
+.le
+.ls weight = "none" (none|mode|median|mean|exposure|@<file>|!<keyword>)
+Weights to be applied during the final averaging.  The choices are none,
+the mode, median, or mean of the specified statistics section, the exposure
+time, values given in a file, or values given by an image header keyword.
+When specified in a file the weights must be one per line in the order of
+the input images.
+.le
+.ls statsec = ""
+Section of images to use in computing image statistics for scaling and
+weighting.  If no section is given then the entire region of the input is
+sampled (for efficiency the images are sampled if they are big enough).
+When the images are offset relative to each other one can precede the image
+section with one of the modifiers "input", "output", "overlap".  The first
+interprets the section relative to the input image (which is equivalent to
+not specifying a modifier), the second interprets the section relative to
+the output image, and the last selects the common overlap and any following
+section is ignored.
+.le
+
+.ce
+Algorithm Parameters
+.ls lthreshold = INDEF, hthreshold = INDEF
+Low and high thresholds to be applied to the input pixels.  This is done
+before any scaling, rejection, and combining.  If INDEF the thresholds
+are not used.
+.le
+.ls nlow = 1,  nhigh = 1 (minmax)
+The number of low and high pixels to be rejected by the "minmax" algorithm.
+These numbers are converted to fractions of the total number of input images
+so that if no rejections have taken place the specified number of pixels
+are rejected while if pixels have been rejected by masking, thresholding,
+or nonoverlap, then the fraction of the remaining pixels, truncated
+to an integer, is used.
+.le
+.ls nkeep = 1
+The minimum number of pixels to retain or the maximum number to reject
+when using the clipping algorithms (ccdclip, crreject, sigclip,
+avsigclip, or pclip).  When given as a positive value this is the minimum
+number to keep.  When given as a negative value the absolute value is
+the maximum number to reject.  This is actually converted to a number
+to keep by adding it to the number of images.
+.le
+.ls mclip = yes (ccdclip, crreject, sigclip, avsigcliip)
+Use the median as the estimate for the true intensity rather than the
+average with high and low values excluded in the "ccdclip", "crreject",
+"sigclip", and "avsigclip" algorithms?  The median is a better estimator
+in the presence of data which one wants to reject than the average.
+However, computing the median is slower than the average.
+.le
+.ls lsigma = 3., hsigma = 3. (ccdclip, crreject, sigclip, avsigclip, pclip)
+Low and high sigma clipping factors for the "ccdclip", "crreject", "sigclip",
+"avsigclip", and "pclip" algorithms.  They multiply a "sigma" factor
+produced by the algorithm to select a point below and above the average or
+median value for rejecting pixels.  The lower sigma is ignored for the
+"crreject" algorithm.
+.le
+.ls rdnoise = "0.", gain = "1.", snoise = "0." (ccdclip, crreject)
+CCD readout noise in electrons, gain in electrons/DN, and sensitivity noise
+as a fraction.  These parameters are used with the "ccdclip" and "crreject"
+algorithms.  The values may be either numeric or an image header keyword
+which contains the value.
+.le
+.ls sigscale = 0.1 (ccdclip, crreject, sigclip, avsigclip)
+This parameter determines when poisson corrections are made to the
+computation of a sigma for images with different scale factors.  If all
+relative scales are within this value of unity and all relative zero level
+offsets are within this fraction of the mean then no correction is made.
+The idea is that if the images are all similarly though not identically
+scaled, the extra computations involved in making poisson corrections for
+variations in the sigmas can be skipped.  A value of zero will apply the
+corrections except in the case of equal images and a large value can be
+used if the sigmas of pixels in the images are independent of scale and
+zero level.
+.le
+.ls pclip = -0.5 (pclip)
+Percentile clipping algorithm parameter.  If greater than
+one in absolute value then it specifies a number of pixels above or
+below the median to use for computing the clipping sigma.  If less
+than one in absolute value then it specifies the fraction of the pixels
+above or below the median to use.  A positive value selects a point
+above the median and a negative value selects a point below the median.
+The default of -0.5 selects approximately the quartile point.
+See the DESCRIPTION section for further details.
+.le
+.ls grow = 0
+Number of pixels to either side of a rejected pixel along image lines
+to also be rejected.  This applies only to pixels rejected by one of
+the rejection algorithms and not the masked or threshold rejected pixels.
+.le
+
+PACKAGE PARAMETERS
+
+The package parameters are used to specify verbose and log output and the
+instrument and header definitions.
+.ih
+DESCRIPTION
+A set of CCD images are combined by weighted averaging or medianing.  Pixels
+may be rejected from the combining by using pixel masks, threshold levels,
+and rejection algorithms.  The images may be scaled multiplicatively or
+additively based on image statistics, image header keywords, or text files
+before rejection.  The images may be combined with integer pixel coordinate
+offsets to produce an image bigger than any of the input images.
+This task is a variant of the \fBimages.imcombine\fR task specialized
+for CCD images.
+
+The input images to be combined are specified by a list.  A subset or
+subsets of the input list may be selected using the parameters
+\fIccdtype\fR and  \fIsubsets\fR.  The \fIccdtype\fR parameter selects only
+images of a specified standard CCD image type.  The \fIsubsets\fR parameter
+breaks up the input list into sublists of common subset parameter (filter,
+grating, etc.).  For more information see \fBccdtypes\fR and
+\fBsubsets\fR.  This selection process is useful with wildcard templates to
+combine, for example, the flat field images for each filter in one step
+(see \fBflatcombine\fR).  When subsets of the input list are used the
+output image and optional pixel file and sigma image are given by root names
+with a subset identifier appended by the task.
+
+If the \fBproject\fR parameter is yes then the highest dimension elements
+of each input image are combined to make an output image of one lower
+dimension.  There is no limit to the number of elements combined in this
+case.  This case is If the \fBproject\fR is no then the entire input list
+is combined to form a single output image per subset.   In this case the
+images must all have the same dimensionality but they may have different
+sizes.  There is a software limit of approximately 100 images in this
+case.
+
+The output image header is a copy of the first image in the combined set.
+In addition, the number of  images combined is recorded under the keyword
+NCOMBINE, the exposure time is updated as the weighted average of the input
+exposure times, and any pixel list file created is recorded under the
+keyword BPM.  The output pixel type is set by the parameter \fIouttype\fR.
+If left blank then the input datatype of highest precision is used.
+
+In addition to one or more output combined images there may also be a pixel
+list image containing the number of pixels rejected at each point in the
+output image, an image containing the sigmas of the pixels combined about
+the final output combined pixels, and a log file.  The pixel list image is
+in the compact pixel list format which can be used as an image in other
+programs.  The sigma computation is the standard deviation corrected for a
+finite population (the n/(n-1) factor) including weights if a weighted
+average is used.
+
+Other input/output parameters are \fIdelete\fR and \fIclobber\fR.  The
+\fIdelete\fR parameter may be set to "yes" to delete the input images
+used in producing an output image after it has been created.  This is
+useful for minimizing disk space, particularly with large
+sets of calibration images needed to achieve high statistical accuracy
+in the final calibration image.  The \fBclobber\fR parameter allows
+the output image names to be existing images which are overwritten (at
+the end of the operation).
+
+An outline of the steps taken by the program is given below and the
+following sections elaborate on the steps.
+
+.nf
+o   Set the input image offsets and the final output image size.
+o   Set the input image scales and weights
+o   Write the log file output
+.fi
+
+For each output image line:
+
+.nf
+o   Get input image lines that overlap the output image line
+o   Reject masked pixels
+o   Reject pixels outside the threshold limits
+o   Reject pixels using the specified algorithm
+o   Reject neighboring pixels along each line
+o   Combine remaining pixels using the weighted average or median
+o   Compute sigmas of remaining pixels about the combined values
+o   Write the output image line, rejected pixel list, and sigmas
+.fi
+
+
+OFFSETS
+
+The images to be combined need not be of the same size or overlap.  They
+do have to have the same dimensionality which will also be the dimensionality
+of the output image.  Any dimensional images supported by IRAF may be
+used.  Note that if the \fIproject\fR flag is yes then the input images
+are the elements of the highest dimension; for example the planes of a
+three dimensional image.
+
+The overlap of the images is determined by a set of integer pixel offsets
+with an offset for each dimension of each input image.  For example
+offsets of 0, 10, and 20 in the first dimension of three images will
+result in combining the three images with only the first image in the
+first 10 colums, the first two images in the next 10 columns and
+all three images starting in the 31st column.  At the 31st output column
+the 31st column of the first image will be combined with the 21st column
+of the second image and the 1st column of the third image.
+
+The output image size is set by the maximum extent in each dimension
+of any input image after applying the offsets.  In the above example if
+all the images have 100 columns then the output image will have 130
+columns corresponding to the 30 column offset in the third image.
+
+The input image offsets are set using the \fIoffset\fR parameter.  There
+are three ways to specify the offsets.  If the word "none" or the empty
+string "" are used then all offsets will be zero and all pixels with the
+same coordinates will be combined.  The output image size will be equal to
+the biggest dimensions of the input images.
+
+If the input images have offsets in a regular grid or one wants to make
+an output image in which the input images are "mosaiced" together in
+a grid then the special offset string  beginning with the word "grid"
+is used.  The format is
+
+.nf
+	grid [n1] [s1] [n2] [s2] ...
+.fi
+
+where ni is the number of images in dimension i and si is the step in
+dimension i.  For example "grid 5 100 5 100" specifies a 5x5 grid with
+origins offset by 100 pixels.  Note that one must insure that the input
+images are specified in the correct order.  This may best be accomplished
+using a "@" list.  One useful application of the grid is to make a
+nonoverlapping mosaic of a number of images for display purposes.  Suppose
+there are 16 images which are 100x100.  The offset string "grid 4 101 4
+101" will produce a mosaic with a one pixel border having the value set
+by \fIblank\fR parameter between the images.
+
+The offsets may be defined in a file by specifying the file name
+in the \fIoffset\fR parameter.  (Note that the special file name STDIN
+may be used to type in the values terminated by the end-of-file
+character).  The file consists of a line for each input image.  The lines
+must be in the same order as the input images and so an "@" list may
+be useful.  The lines consist of whitespace separated offsets one for
+each dimension of the images.  In the first example cited above the
+offset file might contain:
+
+.nf
+	0 0
+	10 0
+	20 0
+.fi
+
+where we assume the second dimension has zero offsets.
+
+The offsets need not have zero for one of the images.  The offsets may
+include negative values or refer to some arbitrary common point.
+When the offsets are read by the program it will find the minimum
+value in each dimension and subtract it from all the other offsets
+in that dimension.  The above example could also be specified as:
+
+.nf
+	225 15
+	235 15
+	245 15
+.fi
+
+There may be cases where one doesn't want the minimum offsets reset
+to zero.  If all the offsets are positive and the comment "# Absolute"
+appears in the offset file then the images will be combined with
+blank values between the first output pixel and the first overlapping
+input pixel.  Continuing with the above example, the file
+
+.nf
+	# Absolute
+	10 10
+	20 10
+	30 10
+.fi
+
+will have the first pixel of the first image in the 11th pixel of the
+output image.  Note that there is no way to "pad" the other side of
+the output image.
+
+
+SCALES AND WEIGHTS
+
+In order to combine images with rejection of pixels based on deviations
+from some average or median they must be scaled to a common level.  There
+are two types of scaling available, a multiplicative intensity scale and an
+additive zero point shift.  The intensity scaling is defined by the
+\fIscale\fR parameter and the zero point shift by the \fIzero\fR
+parameter.  These parameters may take the values "none" for no scaling,
+"mode", "median", or "mean" to scale by statistics of the image pixels,
+"exposure" (for intensity scaling only) to scale by the exposure time
+keyword in the image header, any other image header keyword specified by
+the keyword name prefixed by the character '!', and the name of a file
+containing the scale factors for the input image prefixed by the
+character '@'.
+
+Examples of the possible parameter values are shown below where
+"myval" is the name of an image header keyword and "scales.dat" is
+a text file containing a list of scale factors.
+
+.nf
+	scale = none		No scaling
+	zero = mean		Intensity offset by the mean
+	scale = exposure	Scale by the exposure time
+	zero = !myval		Intensity offset by an image keyword
+	scale = @scales.dat	Scales specified in a file
+.fi
+
+The image statistics factors are computed by sampling a uniform grid
+of points with the smallest grid step that yields less than 10000
+pixels; sampling is used to reduce the time need to compute the statistics.
+If one wants to restrict the sampling to a region of the image the
+\fIstatsec\fR parameter is used.  This parameter has the following
+syntax:
+
+.nf
+	[input|output|overlap] [image section]
+.fi
+
+The initial modifier defaults to "input" if absent.  The modifiers are useful
+if the input images have offsets.  In that case "input" specifies
+that the image section refers to each input image, "output" specifies
+that the image section refers to the output image coordinates, and
+"overlap" specifies the mutually overlapping region of the input images.
+In the latter case an image section is ignored.
+
+The statistics are as indicated by their names.  In particular, the
+mode is a true mode using a bin size which is a fraction of the
+range of the pixels and is not based on a relationship between the
+mode, median, and mean.  Also masked pixels are excluded from the
+computations as well as during the rejection and combining operations.
+
+The "exposure" option in the intensity scaling uses the exposure time
+from the image header.  If one wants to use a nonexposure time image
+header keyword the !<keyword> syntax is available.
+
+If both an intensity scaling and zero point shift are selected the
+multiplicative scaling is done first.  Use of both makes sense
+if the intensity scaling is the exposure time to correct for
+different exposure times and then the zero point shift allows for
+sky brightness changes.
+
+The image statistics and scale factors are recorded in the log file
+unless they are all equal, which is equivalent to no scaling.  The
+intensity scale factors are normalized to a unit mean and the zero
+point shifts are adjust to a zero mean.
+
+Scaling affects not only the mean values between images but also the
+relative pixel uncertainties.  For example scaling an image by a
+factor of 0.5 will reduce the effective noise sigma of the image
+at each pixel by the square root of 0.5.  Changes in the zero
+point also changes the noise sigma if the image noise characteristics
+are Poissonian.  In the various rejection algorithms based on
+identifying a noise sigma and clipping large deviations relative to
+the scaled median or mean, one may need to account for the scaling induced
+changes in the image noise characteristics.
+
+In those algorithms it is possible to eliminate the "sigma correction"
+while still using scaling.  The reasons this might be desirable are 1) if
+the scalings are similar the corrections in computing the mean or median
+are important but the sigma corrections may not be important and 2) the
+image statistics may not be Poissonian, either inherently or because the
+images have been processed in some way that changes the statistics.  In the
+first case because computing square roots and making corrections to every
+pixel during the iterative rejection operation may be a significant
+computational speed limit the parameter \fIsigscale\fR selects how
+dissimilar the scalings must be to require the sigma corrections.  This
+parameter is a fractional deviation which, since the scale factors are
+normalized to unity, is the actual minimum deviation in the scale factors.
+For the zero point shifts the shifts are normalized by the mean shift
+before adjusting the shifts to a zero mean.  To always use sigma scaling
+corrections the parameter is set to zero and to eliminate the correction in
+all cases it is set to a very large number.
+
+If the final combining operation is "average" then the images may be
+weighted during the averaging.  The weights are specified in the
+same way as the scale factors.  In addition
+the NCOMBINE keyword, if present, will be used in the weights.
+The weights, scaled to a unit sum, are printed in the log output.
+
+The weights are only used for the final weighted average and sigma image
+output.  They are not used to form averages in the various rejection
+algorithms.
+
+
+PIXEL MASKS
+
+A pixel mask is a type of IRAF file having the extension ".pl" which
+identifies an integer value with each pixel of the images to which it is
+applied.  The integer values may denote regions, a weight, a good or bad
+flag, or some other type of integer or integer bit flag.  In the common
+case where many values are the same this file is compacted to be small and
+efficient to use.  It is also most compact and efficient if the majority of
+the pixels have a zero mask value so frequently zero is the value for good
+pixels.  Note that these files, while not stored as a strict pixel array,
+may be treated as images in programs.  This means they may be created by
+programs such as \fBmkpattern\fR, edited by \fBimedit\fR, examined by
+\fBimexamine\fR, operated upon by \fBimarith\fR, graphed by \fBimplot\fR,
+and displayed by \fBdisplay\fR.
+
+At the time of introducing this task, generic tools for creating
+pixel masks have yet to be written.  There are two ways to create a
+mask in V2.10.  First if a regular integer image can be created
+then it can be converted to pixel list format with \fBimcopy\fR:
+
+.nf
+	cl> imcopy template plfile.pl
+.fi
+
+by specifically using the .pl extension on output.  Other programs that
+can create integer images (such \fBmkpattern\fR or \fBccdred.badpiximage\fR)
+can create the pixel list file directly by simply using the ".pl"
+extension in the output image name.
+
+To use pixel masks with \fBcombine\fR one must associate a pixel
+mask file with an image by entering the pixel list file name in the
+image header under the keyword BPM (bad pixel mask).  This can be
+done with \fBhedit\fR.  Note that the same pixel mask may be associated
+with more than one image as might be the case if the mask represents
+defects in the detector used to obtain the images.
+
+If a pixel mask is associated with an image the mask is used when the
+\fImasktype\fR parameter is set to a value other than "none".  Note that
+when it is set to "none" mask information is not used even if it exists for
+the image.  The values of \fImasktype\fR which apply masks are "goodvalue",
+"badvalue", "goodbits", and "badbits".  They are used in conjunction with
+the \fImaskvalue\fR parameter.  When the mask type is "goodvalue" the
+pixels with mask values matching the specified value are included in
+combining and all others are rejected.  Similarly, for a mask type of
+"badvalue" the pixels with mask values matching the specified value are
+rejected and all others are accepted.  The bit types are useful for
+selecting a combination of attributes in a mask consisting of bit flags.
+The mask value is still an integer but is interpreted by bitwise comparison
+with the values in the mask file.
+
+If a mask operation is specified and an image has no mask image associated
+with it then the mask values are taken as all zeros.  In those cases be
+careful that zero is an accepted value otherwise the entire image will be
+rejected.
+
+
+THRESHOLD REJECTION
+
+In addition to rejecting masked pixels, pixels in the unscaled input
+images which are below or above the thresholds given by the parameters
+\fIlthreshold\fR and \fIhthreshold\fR are rejected.  Values of INDEF
+mean that no threshold value is applied.  Threshold rejection may be used
+to exclude very bad pixel values or as an alternative way of masking
+images.  In the latter case one can use a task like \fBimedit\fR
+or \fBimreplace\fR to set parts of the images to be excluded to some
+very low or high magic value.
+
+
+REJECTION ALGORITHMS
+
+The \fIreject\fR parameter selects a type of rejection operation to
+be applied to pixels not masked or thresholded.  If no rejection
+operation is desired the value "none" is specified.
+
+MINMAX
+.in 4
+A specified fraction of the highest and lowest pixels are rejected.
+The fraction is specified as the number of high and low pixels, the
+\fInhigh\fR and \fInlow\fR parameters, when data from all the input images
+are used.  If pixels have been rejected by offseting, masking, or
+thresholding then a matching fraction of the remaining pixels, truncated
+to an integer, are used.  Thus,
+
+.nf
+	nl = n * nlow/nimages + 0.001 
+	nh = n * nhigh/nimages + 0.001 
+.fi
+
+where n is the number of pixels surviving offseting, masking, and
+thresholding, nimages is the number of input images, nlow and nhigh
+are task parameters and nl and nh are the final number of low and
+high pixels rejected by the algorithm.  The factor of 0.001 is to
+adjust for rounding of the ratio.
+
+As an example with 10 input images and specifying one low and two high
+pixels to be rejected the fractions to be rejected are 0.1 and 0.2
+and the number rejected as a function of n is:
+
+.nf
+	 n   0  1  2  3  4  5  6  7  8  9 10
+	 nl  0  0  0  0  0  1  1  1  1  1  2
+	 nh  0  0  0  0  0  0  0  0  0  0  1
+.fi
+
+.in -4
+CCDCLIP
+.in 4
+If the images are obtained using a CCD with known read out noise, gain, and
+sensitivity noise parameters and they have been processed to preserve the
+relation between data values and photons or electrons then the noise
+characteristics of the images are well defined.  In this model the sigma in
+data values at a pixel with true value <I>, as approximated by the median
+or average with the lowest and highest value excluded, is given by:
+
+.nf
+	sigma = ((rn / g) ** 2 + <I> / g + (s * <I>) ** 2) ** 1/2
+.fi
+
+where rn is the read out noise in electrons, g is the gain in
+electrons per data value, s is a sensitivity noise given as a fraction,
+and ** is the exponentiation operator.  Often the sensitivity noise,
+due to uncertainties in the pixel sensitivities (for example from the
+flat field), is not known in which case a value of zero can be used.
+See the task \fBstsdas.wfpc.noisemodel\fR for a way to determine
+these vaues (though that task expresses the read out noise in data
+numbers and the sensitivity noise parameter as a percentage).
+
+The read out noise is specified by the \fIrdnoise\fR parameter.  The value
+may be a numeric value to be applied to all the input images or a image
+header keyword containing the value for each image.  Similarly, the
+parameter \fIgain\fR specifies the gain as either a value or image header
+keyword and the parameter \fIsnoise\fR specifies the sensitivity
+noise parameter as either a value or image header keyword.
+
+The algorithm operates on each output pixel independently.  It starts by
+taking the median or unweighted average (excluding the minimum and maximum)
+of the unrejected pixels provided there are at least two input pixels.  The
+expected sigma is computed from the CCD noise parameters and pixels more
+that \fIlsigma\fR times this sigma below or \fIhsigma\fR times this sigma
+above the median or average are rejected.  The process is then iterated
+until no further pixels are rejected.  If the average is used as the
+estimator of the true value then after the first round of rejections the
+highest and lowest values are no longer excluded.  Note that it is possible
+to reject all pixels if the average is used and is sufficiently skewed by
+bad pixels such as cosmic rays.
+
+If there are different CCD noise parameters for the input images
+(as might occur using the image header keyword specification) then
+the sigmas are computed for each pixel from each image using the
+same estimated true value.
+
+If the images are scaled and shifted and the \fIsigscale\fR threshold
+is exceedd then a sigma is computed for each pixel based on the
+image scale parameters; i.e. the median or average is scaled to that of the
+original image before computing the sigma and residuals.
+
+After rejection the number of retained pixels is checked against the
+\fInkeep\fR parameter.  If there are fewer pixels retained than specified
+by this parameter the pixels with the smallest residuals in absolute
+value are added back.  If there is more than one pixel with the same
+absolute residual (for example the two pixels about an average
+or median of two will have the same residuals) they are all added
+back even if this means more than \fInkeep\fR pixels are retained.
+Note that the \fInkeep\fR parameter only applies to the pixels used
+by the clipping rejection algorithm and does not apply to threshold
+or bad pixel mask rejection.
+
+This is the best clipping algorithm to use if the CCD noise parameters are
+adequately known.  The parameters affecting this algorithm are \fIreject\fR
+to select this algorithm, \fImclip\fR to select the median or average for
+the center of the clipping, \fInkeep\fR to limit the number of pixels
+rejected, the CCD noise parameters \fIrdnoise, gain\fR and \fIsnoise\fR,
+\fIlsigma\fR and \fIhsigma\fR to select the clipping thresholds,
+and \fIsigscale\fR to set the threshold for making corrections to the sigma
+calculation for different image scale factors.
+
+.in -4
+CRREJECT
+.in 4
+This algorithm is identical to "ccdclip" except that only pixels above
+the average are rejected based on the \fIhsigma\fR parameter.  This
+is appropriate for rejecting cosmic ray events and works even with
+two images.
+
+.in -4
+SIGCLIP
+.in 4
+The sigma clipping algorithm computes at each output pixel the median or
+average excluding the high and low values and the sigma about this
+estimate.  There must be at least three input pixels, though for this method
+to work well there should be at least 10 pixels.  Values deviating by more
+than the specified sigma threshold factors are rejected.  These steps are
+repeated, except that after the first time the average includes all values,
+until no further pixels are rejected or there are fewer than three pixels.
+
+After rejection the number of retained pixels is checked against the
+\fInkeep\fR parameter.  If there are fewer pixels retained than specified
+by this parameter the pixels with the smallest residuals in absolute
+value are added back.  If there is more than one pixel with the same
+absolute residual (for example the two pixels about an average
+or median of two will have the same residuals) they are all added
+back even if this means more than \fInkeep\fR pixels are retained.
+Note that the \fInkeep\fR parameter only applies to the pixels used
+by the clipping rejection algorithm and does not apply to threshold
+or bad pixel mask rejection.
+
+The  parameters affecting this algorithm are \fIreject\fR to select
+this algorithm, \fImclip\fR to select the median or average for the
+center of the clipping, \fInkeep\fR to limit the number of pixels
+rejected, \fIlsigma\fR and \fIhsigma\fR to select the
+clipping thresholds, and \fIsigscale\fR to set the threshold for
+making corrections to the sigma calculation for different image scale
+factors.
+
+.in -4
+AVSIGCLIP
+.in 4
+The averaged sigma clipping algorithm assumes that the sigma about the
+median or mean (average excluding the low and high values) is proportional
+to the square root of the median or mean at each point.  This is
+described by the equation:
+
+.nf
+	sigma(column,line) = sqrt (gain(line) * signal(column,line))
+.fi
+
+where the \fIestimated\fR signal is the mean or median (hopefully excluding
+any bad pixels) and the gain is the \fIestimated\fR proportionality
+constant having units of photons/data number.
+
+This noise model is valid for images whose values are proportional to the
+number of photons recorded.  In effect this algorithm estimates a
+detector gain for each line with no read out noise component when
+information about the detector noise parameters are not known or
+available.  The gain proportionality factor is computed
+independently for each output line by averaging the square of the residuals
+(at points having three or more input values) scaled by the median or
+mean.  In theory the proportionality should be the same for all rows but
+because of the estimating process will vary somewhat.
+
+Once the proportionality factor is determined, deviant pixels exceeding the
+specified thresholds are rejected at each point by estimating the sigma
+from the median or mean.  If any values are rejected the median or mean
+(this time not excluding the extreme values) is recomputed and further
+values rejected.  This is repeated until there are no further pixels
+rejected or the number of remaining input values falls below three.  Note
+that the proportionality factor is not recomputed after rejections.
+
+If the images are scaled differently and the sigma scaling correction
+threshold is exceedd then a correction is made in the sigma
+calculations for these differences, again under the assumption that
+the noise in an image scales as the square root of the mean intensity.
+
+After rejection the number of retained pixels is checked against the
+\fInkeep\fR parameter.  If there are fewer pixels retained than specified
+by this parameter the pixels with the smallest residuals in absolute
+value are added back.  If there is more than one pixel with the same
+absolute residual (for example the two pixels about an average
+or median of two will have the same residuals) they are all added
+back even if this means more than \fInkeep\fR pixels are retained.
+Note that the \fInkeep\fR parameter only applies to the pixels used
+by the clipping rejection algorithm and does not apply to threshold
+or bad pixel mask rejection.
+
+This algorithm works well for even a few input images.  It works better if
+the median is used though this is slower than using the average.  Note that
+if the images have a known read out noise and gain (the proportionality
+factor above) then the "ccdclip" algorithm is superior.  The two algorithms
+are related in that the average sigma proportionality factor is an estimate
+of the gain.
+
+The  parameters affecting this algorithm are \fIreject\fR to select
+this algorithm, \fImclip\fR to select the median or average for the
+center of the clipping, \fInkeep\fR to limit the number of pixels
+rejected, \fIlsigma\fR and \fIhsigma\fR to select the
+clipping thresholds, and \fIsigscale\fR to set the threshold for
+making corrections to the sigma calculation for different image scale
+factors.
+
+.in -4
+PCLIP
+.in 4
+The percentile clipping algorithm is similar to sigma clipping using the
+median as the center of the distribution except that, instead of computing
+the sigma of the pixels from the CCD noise parameters or from the data
+values, the width of the distribution is characterized by the difference
+between the median value and a specified "percentile" pixel value.  This
+width is then multipled by the scale factors \fIlsigma\fR and \fIhsigma\fR
+to define the clipping thresholds above and below the median.  The clipping
+is not iterated.
+
+The pixel values at each output point are ordered in magnitude and the
+median is determined.  In the case of an even number of pixels the average
+of the two middle values is used as the median value and the lower or upper
+of the two is the median pixel when counting from the median pixel to
+selecting the percentile pixel.  The parameter \fIpclip\fR selects the
+percentile pixel as the number (if the absolute value is greater
+than unity) or fraction of the pixels from the median in the ordered set.
+The direction of the percentile pixel from the median is set by the sign of
+the \fIpclip\fR parameter with a negative value signifying pixels with
+values less than the median.  Fractional values are internally converted to
+the appropriate number of pixels for the number of input images.  A minimum
+of one pixel and a maximum corresponding to the extreme pixels from the
+median are enforced.  The value used is reported in the log output.  Note
+that the same percentile pixel is used even if pixels have been rejected by
+offseting, masking, or thresholding; for example, if the 3nd pixel below
+the median is specified then the 3rd pixel will be used whether there are
+10 pixels or 5 pixels remaining after the preliminary steps.
+
+Some examples help clarify the definition of the percentile pixel.  In the
+examples assume 10 pixels.  The median is then the average of the
+5th and 6th pixels.  A \fIpclip\fR value of 2 selects the 2nd pixel
+above the median (6th) pixel which is the 8th pixel.  A \fIpclip\fR
+value of -0.5 selects the point halfway between the median and the
+lowest pixel.  In this case there are 4 pixels below the median,
+half of that is 2 pixels which makes the percentile pixel the 3rd pixel.
+
+The percentile clipping algorithm is most useful for clipping small
+excursions, such as the wings of bright objects when combining
+disregistered observations for a sky flat field, that are missed when using
+the pixel values to compute a sigma.  It is not as powerful, however, as
+using the CCD noise parameters (provided they are accurately known) to clip
+about the median.
+
+The  parameters affecting this algorithm are \fIreject\fR to select this
+algorithm, \fIpclip\fR to select the percentile pixel, \fInkeep\fR to limit
+the number of pixels rejected, and \fIlsigma\fR and \fIhsigma\fR to select
+the clipping thresholds.
+
+.in -4
+GROW REJECTION
+
+Neighbors of pixels rejected by the rejection algorithms along image lines
+may also be rejected.  The number of neighbors to be rejected on either
+side is specified by the \fIgrow\fR parameter.  The rejection only
+applies to neighbors along each image line.  This is because the
+task operates independently on each image line and does not have the
+ability to go back to previous lines or maintain a list of rejected
+pixels to later lines.
+
+This rejection step is also checked against the \fInkeep\fR parameter
+and only as many pixels as would not violate this parameter are
+rejected.  Unlike it's application in the rejection algorithms at
+this stage there is no checking on the magnitude of the residuals
+and the pixels retained which would otherwise be rejected are randomly
+selected.
+
+
+COMBINING
+
+After all the steps of offsetting the input images, masking pixels,
+threshold rejection, scaling, and applying a rejection algorithms the
+remaining pixels are combined and output.  The pixels may be combined
+by computing the median or by computing a weighted average.
+
+
+SIGMA OUTPUT
+
+In addition to the combined image and optional sigma image may be
+produced.  The sigma computed is the standard deviation, corrected for a
+finite population by a factor of n/(n-1), of the unrejected input pixel
+values about the output combined pixel values.
+.ih
+EXAMPLES
+1.  To average and median images without any other features:
+
+.nf
+	cl> combine obj* avg combine=average reject=none
+	cl> combine obj* med combine=median reject=none
+.fi
+
+2.  To reject cosmic rays:
+
+.nf
+	cl> combine obs1,obs2 Obs reject=crreject rdnoise=5.1, gain=4.3
+.fi
+
+3.  To make a grid for display purposes with 21 64x64 images:
+
+.nf
+	cl> combine @list grid offset="grid 5 65 5 65"
+.fi
+
+4.  To apply a mask image with good pixels marked with a zero value and
+    bad pixels marked with a value of one:
+
+.nf
+	cl> hedit ims* bpm badpix.pl add+ ver-
+	cl> combine ims* final combine=median masktype=goodval
+.fi
+
+5.  To scale image by the exposure time and then adjust for varying
+    sky brightness and make a weighted average:
+
+.nf
+	cl> combine obj* avsig combine=average reject=avsig \
+	>>> scale=exp zero=mode weight=exp  expname=exptime
+.fi
+.ih
+TIME REQUIREMENTS
+The following times were obtain with a Sun 4/470.  The tests combine
+1000x200 images consisting of Poisson noise and cosmic rays generated
+with the \fBartdata\fR package.  The times, especially the total time,
+are approximate and depend on user loads.
+
+.nf
+IMAGES:   Number of images (1000x200) and datatype (R=real, S=short)
+COMBINE:  Combine option
+REJECT:   Rejection option with grow = 0
+	      minmax:    nlow = 1, nhigh = 1
+	      ccdclip:   lsigma = 3., hsigma = 3, sigscale = 0.
+	      sigclip:   lsigma = 3., hsigma = 3, sigscale = 0.
+	      avsigclip: lsigma = 3., hsigma = 3, sigscale = 0.
+	      pclip:     lsigma = 3., hsigma = 3, pclip = -0.5
+	      /a:        mclip = no  (clip about the average)
+	      /m:        mclip = yes (clip about the median)
+O M T S:  Features used (Y=yes, N=no)
+O:        offset = "grid 5 10 2 10"
+M:        masktype = goodval, maskval = 0
+	      Pixel mask has 2 bad lines and 20 bad columns 
+T:        lthreshold = INDEF, hthreshold = 1100.
+S:        scale = mode, zero = none, weight = mode
+TIME:     cpu time in seconds, total time in minutes and seconds
+
+
+IMAGES  COMBINE  REJECT        O M T S     TIME
+
+  10R   average  none          N N N N    1.3 0:08
+  10R   average  minmax        N N N N    4.3 0:10
+  10R   average  pclip         N N N N   17.9 0:32
+  10R   average  ccdclip/a     N N N N   11.6 0:21
+  10R   average  crreject/a    N N N N   11.4 0:21
+  10R   average  sigclip/a     N N N N   13.6 0:29
+  10R   average  avsigclip/a   N N N N   15.9 0:35
+  10R   average  ccdclip/m     N N N N   16.9 0:32
+  10R   average  crreject/m    N N N N   17.0 0:28
+  10R   average  sigclip/m     N N N N   19.6 0:42
+  10R   average  avsigclip/m   N N N N   20.6 0:43
+
+  10R   median   none          N N N N    6.8 0:17
+  10R   median   minmax        N N N N    7.8 0:15
+  10R   median   pclip         N N N N   16.9 1:00
+  10R   median   ccdclip/a     N N N N   18.0 0:34
+  10R   median   crreject/a    N N N N   17.7 0:30
+  10R   median   sigclip/a     N N N N   21.1 1:13
+  10R   median   avsigclip/a   N N N N   23.1 0:41
+  10R   median   ccdclip/m     N N N N   16.1 0:27
+  10R   median   crreject/m    N N N N   16.0 0:27
+  10R   median   sigclip/m     N N N N   18.1 0:29
+  10R   median   avsigclip/m   N N N N   19.6 0:32
+
+  10R   average  none          N N N Y    6.1 0:36
+  10R   median   none          N N N Y   10.4 0:49
+  10R   median   pclip         N N N Y   20.4 1:10
+  10R   median   ccdclip/m     N N N Y   19.5 0:36
+  10R   median   avsigclip/m   N N N Y   23.0 1:06
+
+  10R   average  none          N Y N N    3.5 0:12
+  10R   median   none          N Y N N    8.9 0:21
+  10R   median   pclip         N Y N N   19.9 0:45
+  10R   median   ccdclip/m     N Y N N   18.0 0:44
+  10R   median   avsigclip/m   N Y N N   20.9 0:28
+
+  10R   average  none          Y N N N    4.3 0:13
+  10R   median   none          Y N N N    9.6 0:21
+  10R   median   pclip         Y N N N   21.8 0:54
+  10R   median   ccdclip/m     Y N N N   19.3 0:44
+  10R   median   avsigclip/m   Y N N N   22.8 0:51
+
+  10R   average  none          Y Y Y Y   10.8 0:22
+  10R   median   none          Y Y Y Y   16.1 0:28
+  10R   median   pclip         Y Y Y Y   27.4 0:42
+  10R   median   ccdclip/m     Y Y Y Y   25.5 0:39
+  10R   median   avsigclip/m   Y Y Y Y   28.9 0:44
+
+  10S   average  none          N N N N    2.2 0:06
+  10S   average  minmax        N N N N    4.6 0:12
+  10S   average  pclip         N N N N   18.1 0:33
+.fi
+.ih
+REVISIONS
+.ls COMBINE V2.10.2
+The weighting was changed from using the square root of the exposure time
+or image statistics to using the values directly.  This corresponds
+to variance weighting.  Other options for specifying the scaling and
+weighting factors were added; namely from a file or from a different
+image header keyword.  The \fInkeep\fR parameter was added to allow
+controlling the maximum number of pixels to be rejected by the clipping
+algorithms.  The \fIsnoise\fR parameter was added to include a sensitivity
+or scale noise component to the noise model.  Errors will now delete
+the output images.
+.le
+.ls COMBINE V2.10
+This task was greatly revised to provide many new features.  These features
+are:
+
+.nf
+    o Bad pixel masks
+    o Combining offset and different size images
+    o Blank value for missing data
+    o Combining across the highest dimension (the project option)
+    o Separating threshold rejection, the rejection algorithms,
+      and the final combining statistic
+    o New CCDCLIP, CRREJECT, and PCLIP algorithms
+    o Rejection now may reject more than one pixel per output pixel
+    o Choice of a central median or average for clipping
+    o Choice of final combining operation
+    o Simultaneous multiplicative and zero point scaling
+.fi
+.le
+.ih
+LIMITATIONS
+Though this task is essentially not limited by the physical
+limits of the host (number of open files, amount of memory) there is a
+software limit in the IRAF virtual operating system of about 120 separate
+images which may be combined.  To combine more images one may combine smaller
+groups and then combine those or one may stack the images into a higher
+dimensional image using \fBimstack\fR and use the \fIproject\fR option.
+.ih
+SEE ALSO
+image.imcombine, instruments, ccdtypes, icfit, ccdred, guide, darkcombine,
+flatcombine, zerocombine, onedspec.scombine wfpc.noisemodel
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/contents.ms b/noao/imred/quadred/src/quad/doc/contents.ms
new file mode 100644
index 00000000..8ba2624a
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/contents.ms
@@ -0,0 +1,34 @@
+.sp 1i
+.ps +2
+.ft B
+.ce
+Contents
+.sp 3
+.ps -2
+.ft R
+.sp
+1.\h'|0.4i'\fBIntroduction\fP\l'|5.6i.'\0\01
+.sp
+2.\h'|0.4i'\fBGetting Started\fP\l'|5.6i.'\0\02
+.sp
+3.\h'|0.4i'\fBProcessing Your Data\fP\l'|5.6i.'\0\05
+.br
+\h'|0.4i'3.1.\h'|0.9i'Combining Calibration Images\l'|5.6i.'\0\06
+.br
+\h'|0.4i'3.2.\h'|0.9i'Calibrations and Corrections\l'|5.6i.'\0\07
+.sp
+4.\h'|0.4i'\fBSpecial Processing Operations\fP\l'|5.6i.'\0\08
+.br
+\h'|0.4i'4.1.\h'|0.9i'Spectroscopic Flat Fields\l'|5.6i.'\0\08
+.br
+\h'|0.4i'4.2.\h'|0.9i'Illumination Corrections\l'|5.6i.'\0\09
+.br
+\h'|0.4i'4.3.\h'|0.9i'Sky Flat Fields\l'|5.6i.'\010
+.br
+\h'|0.4i'4.4.\h'|0.9i'Illumination Corrected Flat Fields\l'|5.6i.'\010
+.br
+\h'|0.4i'4.5.\h'|0.9i'Fringe Corrections\l'|5.6i.'\010
+.sp
+5.\h'|0.4i'\fBSummary\fP\l'|5.6i.'\011
+.sp
+\h'|0.4i'\fBReferences\fP\l'|5.6i.'\011
diff --git a/noao/imred/quadred/src/quad/doc/cosmicrays.hlp b/noao/imred/quadred/src/quad/doc/cosmicrays.hlp
new file mode 100644
index 00000000..c50a129f
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/cosmicrays.hlp
@@ -0,0 +1,220 @@
+.help cosmicrays Dec87 noao.imred.ccdred
+.ih
+NAME
+cosmicrays -- Detect and replace cosmic rays
+.ih
+USAGE
+cosmicrays input output
+.ih
+PARAMETERS
+.ls input
+List of input images in which to detect cosmic rays.
+.le
+.ls output
+List of output images in which the detected cosmic rays will be replaced
+by an average of neighboring pixels.  If the output image name differs
+from the input image name then a copy of the input image is made with
+the detected cosmic rays replaced.  If no output images are specified
+then the input images are modified in place.  In place modification of
+an input image also occurs when the output image name is the same as
+the input image name.
+.le
+.ls badpix = ""
+List of bad pixel files to be created, one for each input image.  If no
+file names are given then no bad pixel file is created.  The bad pixel 
+file is a simple list of pixel coordinates for each replaced cosmic ray.
+This file may be used in conjunction with \fBbadpixelimage\fR to create
+a mask image.
+.le
+.ls ccdtype = ""
+If specified only the input images of the desired CCD image type will be
+selected.
+.le
+.ls threshold = 25.
+Detection threshold above the mean of the surrounding pixels for cosmic
+rays.  The threshold will depend on the noise characteristics of the
+image and how weak the cosmic rays may be for detection.  A typical value
+is 5 or more times the sigma of the background.
+.le
+.ls fluxratio = 2.
+The ratio (as a percent) of the mean neighboring pixel flux to the candidate
+cosmic ray pixel for rejection.  The value depends on the seeing and the
+characteristics of the cosmic rays.  Typical values are in the range
+2 to 10 percent.
+.le
+.ls npasses = 5
+Number of cosmic ray detection passes.  Since only the locally strongest
+pixel is considered a cosmic ray, multiple detection passes are needed to
+detect and replace multiple pixel cosmic ray events.
+.le
+.ls window = 5
+Size of cosmic ray detection window.  A square window of either 5 by 5 or
+7 by 7 is used to detect cosmic rays.  The smaller window allows detection
+in the presence of greater background gradients but is less sensitive at
+discriminating multiple event cosmic rays from stars.  It is also marginally
+faster.
+.le
+.ls interactive = yes
+Examine parameters interactively?  A plot of the mean flux within the
+detection window (x100) vs the flux ratio (x100) is plotted and the user may
+set the flux ratio threshold, delete and undelete specific events, and
+examine specific events.  This is useful for new data in which one is
+uncertain of an appropriate flux ratio threshold.  Once determined the
+task need not be used interactively.
+.le
+.ls answer
+This parameter is used for interactive queries when processing a list of
+images.  The responses may be "no", "yes", "NO", or "YES".  The upper case
+responses permanently enable or disable the interactive review while
+the lower case reponses allow selective examination of certain input
+images.
+.le
+.ih
+OTHER PARAMETERS
+There are other parameters which may be defined by the package, as is the
+case with \fBccdred\fR, or as part of the task, as is the case with
+standalone version in the \fBgeneric\fR package.
+
+.ls verbose
+If yes then a time stamped log of the operation is printed on the standard
+output.
+.le
+.ls logfile
+If a log file is specified then a time stamped log of the operation is
+recorded.
+.le
+.ls plotfile
+If a plot file is specified then the graph of the flux ratio (x100) vs
+the mean flux (x100) is recorded as metacode.  This may be spooled or examined
+later.
+.le
+.ls graphics = "stdgraph"
+Interactive graphic output device for interactive examination of the
+detection parameters.
+.le
+.ls cursor = ""
+Interactive graphics cursor input.  If null the graphics display cursor
+is used, otherwise a file containing cursor input may be specified.
+.le
+.ls instrument
+The \fBccdred\fR instrument file is used for mapping header keywords and
+CCD image types.
+.le
+.ih
+CURSOR COMMANDS
+
+.nf
+d	Mark candidate for replacement (applys to '+' points)
+q	Quit and replace the selected pixels
+r	Redraw the graph
+s	Make a surface plot for the candidate nearest the cursor
+t	Set the flux ratio threshold at the y cursor position
+u	Mark candidate to not be replaced (applys to 'x' points)
+w	Adjust the graph window (see \fBgtools\fR)
+.fi
+
+There are no colon commands except those for the windowing options (type
+:\help or see \fBgtools\fR).
+.ih
+DESCRIPTION
+Cosmic ray events in each input image are detected and replaced by the
+average of the four neighbors.  The replacement may be performed
+directly on the input image if no output image is specified or if the
+output image name is the same as the input image name.  If a new image
+is created it is a copy of the input image except for the replaced
+pixels.  The processing keyword CRCOR is added to the output image
+header.  Optional output includes a log file to which a processing log
+is appended, a verbose log output to the standard output (the same as
+that in the log file), a plot file showing the parameters of the
+detected cosmic ray candidates and the flux ratio threshold used, and a
+bad pixel file containing the coordinates of the replaced pixels.  The
+bad pixel file may be used for plotting purposes or to create a mask
+image for display and analysis using the task \fBbadpiximage\fR.  This
+bad pixel file will be replaced by the IRAF bad pixel facility when it
+becomes available.  If one wants more than a simple mask image then by
+creating a different output image a difference image between the
+original and the modified image may be made using \fBimarith\fR.
+
+This task may be applied to an image previously processed to detect
+additional cosmic rays.  A warning will be given (because of the
+CRCOR header parameter) and the previous processing header keyword will
+be overwritten.
+
+The cosmic ray detection algorithm consists of the following steps.
+First a pixel must be the brightest pixel within the specified
+detection window (either 5x5 or 7x7).  The mean flux in the surrounding
+pixels with the second brightest pixel excluded (which may also be a
+cosmic ray event) is computed and the candidate pixel must exceed this
+mean by the amount specified by the parameter \fIthreshold\fR.  A plane
+is fit to the border pixels of the window and the fitted background is
+subtracted.  The mean flux (now background subtracted) and the ratio of
+this mean to the cosmic ray candidate (the brightest pixel) are
+computed.  The mean flux (x100) and the ratio (x100) are recorded for
+interactive examination if desired.
+
+Once the list of cosmic ray candidates has been created and a threshold
+for the flux ratio established (either by the parameter \fIfluxratio\fR
+or modified interactively) the pixels with ratios below the threshold
+are replaced in the output by the average of the four neighboring pixels
+(with the second strongest pixel in the detection window excluded if it is
+one of these pixels).  Additonal pixels may then be detected and replaced
+in further passes as specified by the parameter \fInpasses\fR.  Note that
+only pixels in the vicinity of replaced pixels need be considered in
+further passes.
+
+The division between the peaks of real objects and cosmic rays is made
+based on the flux ratio between the mean flux (excluding the center
+pixel and the second strongest pixel) and the candidate pixel.  This
+threshold depends on the point spread function and the distribution of
+multiple cosmic ray events and any additional neighboring light caused
+by the events.  This threshold is not strongly coupled to small changes
+in the data so that once it is set for a new type of image data it may
+be used for similar images.  To set it initially one may examine the
+scatter plot of the flux ratio as a function of the mean flux.  This
+may be done interactively or from the optional plot file produced.
+
+When the interactive flag is set the user is queried for each image.
+Responses may be made for specific images or for all images by using
+lower or upper case answers respectively.  When the parameters are
+examined interactively the user may change the flux ratio threshold
+('t' key).  Changes made are stored in the parameter file and, thus,
+learned for further images.  Pixels to be deleted are marked by crosses
+and pixels which are peaks of objects are marked by pluses.  The user
+may explicitly delete or undelete any point if desired but this is only
+for special cases near the threshold.  In the future keys for
+interactive display of the specific detections will be added.
+Currently a surface plot of any candidate may be displayed graphically
+in four 90 degree rotated views using the 's' key.  Note that the
+initial graph does not show all the points some of which are clearly
+cosmic rays because they have negative mean flux or flux ratio.  To
+view all data one must rewindow the graph with the 'w' key or ":/"
+commands (see \fBgtools\fR).
+.ih
+EXAMPLES
+1. To replace cosmic rays in a set of images ccd*:
+
+.nf
+	cl> cosmicrays ccd* new//ccd*
+	ccd001: Examine parameters interactively? (yes):
+	[A scatter plot graph is made.  One can adjust the threshold.]
+	[Looking at a few points using the 's' key can be instructive.]
+	[When done type 'q'.]
+	ccd002: Examine parameters interactively? (yes): NO
+	[No further interactive examination is done.]
+.fi
+
+After cleaning one typically displays the images and  possibly blinks them.
+A difference image or mask image may also be created.
+
+2.  To create a mask image a bad pixel file must be specified.  In the
+following we replace the cosmic rays in place and create a bad pixel
+file and mask image:
+
+.nf
+	cl> cosmicrays ccd001 ccd001 badpix=ccd001.bp
+	cl> badpiximage ccd001.bp ccd001 ccd001bp
+.fi
+.ih
+SEE ALSO
+badpixelimage gtools
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/darkcombine.hlp b/noao/imred/quadred/src/quad/doc/darkcombine.hlp
new file mode 100644
index 00000000..ef9eb81c
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/darkcombine.hlp
@@ -0,0 +1,125 @@
+.help darkcombine Sept93 arcon.quad
+.ih
+NAME
+darkcombine -- Combine and process dark count images
+.ih
+USAGE
+darkcombine input
+.ih
+PARAMETERS
+.ls input
+List of dark count images to combine.  The \fIccdtype\fR parameter
+may be used to select the zero level images from a list containing all
+types of data.
+.le
+.ls output = "Dark"
+Output dark count root image name.
+.le
+.ls combine = "average" (average|median)
+Type of combining operation performed on the final set of pixels (after
+rejection).  The choices are
+"average" or "median".  The median uses the average of the two central
+values when the number of pixels is even.
+.le
+.ls reject = "avsigclip" (none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip)
+Type of rejection operation.  See \fBcombine\fR for details.
+.le
+.ls ccdtype = "zero"
+CCD image type to combine.  If no image type is given then all input images
+are combined.
+.le
+.ls process = no
+Process the input images before combining?
+.le
+.ls delete = no
+Delete input images after combining?  Only those images combined are deleted.
+.le
+.ls clobber = no
+Clobber existing output images?
+.le
+.ls scale = "none" (none|mode|median|mean|exposure)
+Multiplicative image scaling to be applied.  The choices are none, scale
+by the mode, median, or mean of the specified statistics section, or scale
+by the exposure time given in the image header.
+.le
+.ls statsec = ""
+Section of images to use in computing image statistics for scaling.
+If no section is given then the entire region of the image is
+sampled (for efficiency the images are sampled if they are big enough).
+.le
+
+.ce
+Algorithm Parameters
+.ls nlow = 1,  nhigh = 1 (minmax)
+The number of low and high pixels to be rejected by the "minmax" algorithm.
+.le
+.ls nkeep = 1
+The minimum number of pixels to retain or the maximum number to reject
+when using the clipping algorithms (ccdclip, crreject, sigclip,
+avsigclip, or pclip).  When given as a positive value this is the minimum
+number to keep.  When given as a negative value the absolute value is
+the maximum number to reject.  This is actually converted to a number
+to keep by adding it to the number of images.
+.le
+.ls mclip = yes (ccdclip, crreject, sigclip, avsigcliip)
+Use the median as the estimate for the true intensity rather than the
+average with high and low values excluded in the "ccdclip", "crreject",
+"sigclip", and "avsigclip" algorithms?  The median is a better estimator
+in the presence of data which one wants to reject than the average.
+However, computing the median is slower than the average.
+.le
+.ls lsigma = 3., hsigma = 3. (ccdclip, crreject, sigclip, avsigclip, pclip)
+Low and high sigma clipping factors for the "ccdclip", "crreject", "sigclip",
+"avsigclip", and "pclip" algorithms.  They multiply a "sigma" factor
+produced by the algorithm to select a point below and above the average or
+median value for rejecting pixels.  The lower sigma is ignored for the
+"crreject" algorithm.
+.le
+.ls rdnoise = "0.", gain = "1.", snoise = "0." (ccdclip, crreject)
+CCD readout noise in electrons, gain in electrons/DN, and sensitivity noise
+as a fraction.  These parameters are used with the "ccdclip" and "crreject"
+algorithms.  The values may be either numeric or an image header keyword
+which contains the value.
+.le
+.ls pclip = -0.5 (pclip)
+Percentile clipping algorithm parameter.  If greater than
+one in absolute value then it specifies a number of pixels above or
+below the median to use for computing the clipping sigma.  If less
+than one in absolute value then it specifies the fraction of the pixels
+above or below the median to use.  A positive value selects a point
+above the median and a negative value selects a point below the median.
+The default of -0.5 selects approximately the quartile point.
+See \fBcombine\fR for further details.
+.le
+.ls blank = 0.
+Output value to be used when there are no pixels.
+.le
+.ih
+DESCRIPTION
+The dark count images in the input image list are combined.
+The input images may be processed first if desired.
+The original images may be deleted automatically if desired.
+
+This task is a script which applies \fBquadproc\fR and \fBcombine\fR.  The
+parameters and combining algorithms are described in detail in the help for
+\fBcombine\fR.  This script has default parameters specifically set for
+dark count images and simplifies the combining parameters.  There are other
+combining options not included in this task.  For these additional
+features, such as thresholding, offseting, masking, and projecting, use
+\fBcombine\fR.
+
+The version of \fBdarkcombine\fR in the \fBquad\fR package differs from that
+in \fBccdred\fR in that \fBquadproc\fR rather than \fBccdproc\fR is used to
+process the images if this is requested. The \fBquad\fR version MUST be
+used if process=yes and the input list contains any multi-readout images which
+have not been overscan corrected and trimmed.
+.ih
+EXAMPLES
+1. The image data contains four dark count images.  To automatically select
+them and combine them as a background job using the default combining algorithm:
+
+    cl> darkcombine ccd*.imh&
+.ih
+SEE ALSO
+quadproc, combine
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/flatcombine.hlp b/noao/imred/quadred/src/quad/doc/flatcombine.hlp
new file mode 100644
index 00000000..c463655d
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/flatcombine.hlp
@@ -0,0 +1,139 @@
+.help flatcombine Sept93 arcon.quad
+.ih
+NAME
+flatcombine -- Combine and process flat field images
+.ih
+USAGE
+flatcombine input
+.ih
+PARAMETERS
+.ls input
+List of flat field images to combine.  The \fIccdtype\fR parameter
+may be used to select the flat field images from a list containing all
+types of data.
+.le
+.ls output = "Flat"
+Output flat field root image name.  The subset ID is appended.
+.le
+.ls combine = "average" (average|median)
+Type of combining operation performed on the final set of pixels (after
+rejection).  The choices are
+"average" or "median".  The median uses the average of the two central
+values when the number of pixels is even.
+.le
+.ls reject = "avsigclip" (none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip)
+Type of rejection operation.  See \fBcombine\fR for details.
+.le
+.ls ccdtype = "flat"
+CCD image type to combine.  If no image type is given then all input images
+are combined.
+.le
+.ls process = no
+Process the input images before combining?
+.le
+.ls subsets = yes
+Combine images by subset parameter?  If yes then the input images are
+grouped by subset parameter and each group combined into a separate output
+image.  The subset identifier is appended to the output and sigma image
+names.  See \fBsubsets\fR for more on the subset parameter.  This is generally
+used with flat field images.
+.le
+.ls delete = no
+Delete input images after combining?  Only those images combined are deleted.
+.le
+.ls clobber = no
+Clobber existing output images?
+.le
+.ls scale = "none" (none|mode|median|mean|exposure)
+Multiplicative image scaling to be applied.  The choices are none, scale
+by the mode, median, or mean of the specified statistics section, or scale
+by the exposure time given in the image header.
+.le
+.ls statsec = ""
+Section of images to use in computing image statistics for scaling.
+If no section is given then the entire region of the image is
+sampled (for efficiency the images are sampled if they are big enough).
+.le
+
+.ce
+Algorithm Parameters
+.ls nlow = 1,  nhigh = 1 (minmax)
+The number of low and high pixels to be rejected by the "minmax" algorithm.
+.le
+.ls nkeep = 1
+The minimum number of pixels to retain or the maximum number to reject
+when using the clipping algorithms (ccdclip, crreject, sigclip,
+avsigclip, or pclip).  When given as a positive value this is the minimum
+number to keep.  When given as a negative value the absolute value is
+the maximum number to reject.  This is actually converted to a number
+to keep by adding it to the number of images.
+.le
+.ls mclip = yes (ccdclip, crreject, sigclip, avsigcliip)
+Use the median as the estimate for the true intensity rather than the
+average with high and low values excluded in the "ccdclip", "crreject",
+"sigclip", and "avsigclip" algorithms?  The median is a better estimator
+in the presence of data which one wants to reject than the average.
+However, computing the median is slower than the average.
+.le
+.ls lsigma = 3., hsigma = 3. (ccdclip, crreject, sigclip, avsigclip, pclip)
+Low and high sigma clipping factors for the "ccdclip", "crreject", "sigclip",
+"avsigclip", and "pclip" algorithms.  They multiply a "sigma" factor
+produced by the algorithm to select a point below and above the average or
+median value for rejecting pixels.  The lower sigma is ignored for the
+"crreject" algorithm.
+.le
+.ls rdnoise = "0.", gain = "1.", snoise = "0." (ccdclip, crreject)
+CCD readout noise in electrons, gain in electrons/DN, and sensitivity noise
+as a fraction.  These parameters are used with the "ccdclip" and "crreject"
+algorithms.  The values may be either numeric or an image header keyword
+which contains the value.
+.le
+.ls pclip = -0.5 (pclip)
+Percentile clipping algorithm parameter.  If greater than
+one in absolute value then it specifies a number of pixels above or
+below the median to use for computing the clipping sigma.  If less
+than one in absolute value then it specifies the fraction of the pixels
+above or below the median to use.  A positive value selects a point
+above the median and a negative value selects a point below the median.
+The default of -0.5 selects approximately the quartile point.
+See \fBcombine\fR for further details.
+.le
+.ls blank = 1.
+Output value to be used when there are no pixels.
+.le
+.ih
+DESCRIPTION
+The flat field images in the input image list are combined.  If there
+is more than one subset (such as a filter or grating) then the input
+flat field images are grouped by subset and an combined separately.
+The input images may be processed first if desired.  However if all
+zero level bias effects are linear then this is not necessary and some
+processing time may be saved.  The original images may be deleted
+automatically if desired.
+
+This task is a script which applies \fBquadproc\fR and \fBcombine\fR.  The
+parameters and combining algorithms are described in detail in the help for
+\fBcombine\fR.  This script has default parameters specifically set for
+flat field images and simplifies the combining parameters.  There are other
+combining options not included in this task.  For these additional
+features, such as thresholding, offseting, masking, and projecting, use
+\fBcombine\fR.
+
+The version of \fBzerocombine\fR in the \fBquad\fR package differs from that
+in \fBccdred\fR in that \fBquadproc\fR rather than \fBccdproc\fR is used to
+process the images if this is requested. The \fBquad\fR version MUST be
+used if process=yes and the input list contains any multi-readout images which
+have not been overscan corrected and trimmed.
+.ih
+EXAMPLES
+1. The image data contains four flat field images for three filters.
+To automatically select them and combine them as a background job
+using the default combining algorithm:
+
+    cl> flatcombine ccd*.imh&
+
+The final images are "FlatV", "FlatB", and "FlatR".
+.ih
+SEE ALSO
+quadproc, combine, subsets
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/flatfields.hlp b/noao/imred/quadred/src/quad/doc/flatfields.hlp
new file mode 100644
index 00000000..94766960
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/flatfields.hlp
@@ -0,0 +1,177 @@
+.help flatfields Jun87 noao.imred.ccdred
+
+.ih
+NAME
+flatfields -- Discussion of CCD flat field calibrations
+.ih
+DESCRIPTION
+This topic describes the different types of CCD flat fields and
+the tasks available in the \fBccdred\fR and spectroscopy packages for
+creating them.  Flat field calibration is the most important operation
+performed on CCD data.  This operation calibrates the relative response
+of the detector at each pixel.  In some cases this is as simple as
+taking a special type of observation called a flat field.  However, in
+many cases this calibration observation must be corrected for
+iillumination, scanning, wavelength, and aperture effects.
+
+The discussion is in three sections; direct imaging, scan mode,
+and spectroscopy.  Though there are many similarities between these
+modes of operation there are important differences in how corrections
+are applied to the basic flat field observations.  The application of
+the flat field calibrations to the observations using \fBccdproc\fR is
+the same in all cases, however.
+.sh
+1. Direct Imaging
+The starting point for determining the flat field calibration is an
+observation of something which should have uniform response at all
+points on the detector.  In addition the color of the light falling at
+each pixel should be the same as that in an observation so the same
+filter must be used when determining the flat field (the issue of the
+matching the color of the objects observed at the appropriate pixels is
+ignored here).  The best calibration observation is of a blank sky.  If
+an accurate blank sky observation can be obtained then this is all that
+is needed for a flat field calibration.  This type of flat field might
+be called a \fIsky flat\fR, though this term is more often used for a
+type of flat field described below.  There are two difficulties with
+this type of calibration; finding a really blank sky and getting a
+sufficiently accurate measurement without using all the observing
+time.
+
+It is usually not possible to get a blank sky observation accurate
+enough to calibrate the individual pixels without introducing
+undesirable noise.  What is generally done is to use a lamp to either
+uniformly illuminate a part of the dome or directly illuminate the
+field of view.  The first type of observation is called a \fIdome
+flat\fR and the second is called a \fIprojection flat\fR.  We shall call
+both of these types of observations \fBlamp flat fields\fR.  If the
+iillumination is truely uniform then these types of observations are
+sufficient for flat field calibration.  To get a very accurate flat
+field many observations are made and then combined (see
+\fBflatcombine\fR).
+
+Unfortunately, it is sometimes the case that the lamp flat fields
+do not illuminate the telescope/detector in the same way as the actual
+observations.  Calibrating with these flat fields will introduce a
+residual large scale iillumination pattern, though it will correctly
+calibrate the relative pixel responses locally.  There are two ways to
+correct for this effect.  The first is to correct the flat field
+observation.  The second is to apply the uncorrected flat field to the
+observations and then apply an \fIiillumination\fR correction as a
+separate operation.  The first is more efficient since it consists of a
+single correction applied to each observation but in some cases the
+approximate correction is desired immediately, the observation needed
+to make the correction has not been taken yet, or the residual
+iillumination error is not discovered until later.
+
+For the two methods there are two types of correction.  One is to
+use a blank sky observation to correct for the residual iillumination
+pattern.  This is different than using the sky observation directly as
+a flat field calibration in that only the large scale pattern is
+needed.  Determining the large scale iillumination does not require high
+signal-to-noise at each pixel and faint objects in the image can be
+either eliminated or ignored.  The second method is to remove the large
+scale shape from the lamp flat field.  This is not as good as using a
+blank sky observation but, if there is no such observation and the
+iillumination pattern is essentially only in the lamp flat field, this
+may be sufficient.
+
+From the above two paragraphs one sees there are four options.
+There is a task in the \fBccdred\fR package for each of these options.
+To correct a lamp flat field observation by a blank sky observation,
+called a \fIsky flat\fR, the task is \fBmkskyflat\fR.  To correct the
+flat field for its own large scale gradients, called an \fIiillumination
+flat\fR, the task is \fBmkillumflat\fR.  To create a secondary
+correction to be applied to data processed with the lamp flat field
+image the tasks are \fBmkskycor\fR and \fBmkillumcor\fR which are,
+respectively, based on a blank sky observation and the lamp flat field
+iillumination pattern.
+
+With this introduction turn to the individual documentation for these
+four tasks for further details.
+.sh
+2. Scan Mode
+There are two types of scan modes supported by the \fBccdred\fR
+package; \fIshortscan\fR and \fIlongscan\fR (see \fBccdproc\fR for
+further details).  They both affect the manner in which flat field
+calibrations are handled.  The shortscan mode produces images which are
+the same as direct images except that the light recorded at each pixel
+was collected by a number of different pixels.  This improves the flat
+field calibration.  If the flat field images, of the same types
+described in the direct imaging section, are observed in the same way
+as all other observations, i.e. in scan mode, then there is no
+difference from direct imaging (except in the quality of the flat
+fields).  There is a statistical advantage to observing the lamp or sky
+flat field without scanning and then numerically averaging to simulate
+the result of the scanning.  This improves the accuracy of
+the flat fields and might possibly allow direct blank sky observations
+to be used for flat fields.  The numerical scanning is done in
+\fBccdproc\fR by setting the appropriate scanning parameters.
+
+In longscan mode the CCD detector is read out in such a way that
+each output image pixel is the sum of the light falling on all pixels
+along the direction of the scan.  This reduces the flat field calibration
+to one dimension, one response value for each point across the scan.
+The one dimensional calibration is obtained from a longscan observation
+by averaging all the readout lines.
+This is done automatically in \fBccdproc\fR by setting the appropriate
+parameters.  In this case very good flat fields can be obtained from
+one or more blank sky observations or an unscanned lamp observation.  Other
+corrections are not generally used.
+.sh
+3. Spectroscopy
+Spectroscopic flat fields differ from direct imaging in that the
+spectrum of the sky or lamp and transmission variations with wavelength
+are part of the observation.  Application of such images will introduce
+the inverse of the spectrum and transmission into the observation.  It
+also distorts the observed counts making signal-to-noise estimates
+invalid.  This, and the low signal in the dispersed light, makes it
+difficult to use blank sky observations directly as flat fields.  As
+with direct imaging, sky observation may be used to correct for
+iillumination errors if necessary.  At sufficiently high dispersion the
+continuous lamp spectrum may be flat enough that the spectral signature
+of the lamp is not a problem.  Alternatively, flux calibrating the
+spectra will also remove the flat field spectral signature.  The
+spectroscopic flat fields also have to be corrected for regions outside
+of the slit or apertures to avoid bad response effects when applying
+the flat field calibration to the observations.
+
+The basic scheme for removing the spectral signature is to average
+all the lines or columns across the dispersion and within the aperture
+to form an estimate of the spectrum.  In addition to the averaging, a
+smooth curve is fit to the lamp spectrum to remove noise.  This smooth
+shape is then divided back into each line or column to eliminate the
+shape of the spectrum without changing the shape of the spectrum
+in the spatial direction or the small scale response variations.
+Regions outside of the apertures are replaced by unity.
+This method requires that the dispersion be aligned fairly close to
+either the CCD lines or columns.
+
+This scheme is used in both longslit and multiaperture spectra.
+The latter includes echelle, slitlets, aperture masks, and fiber feeds.
+For narrow apertures which do not have wider slits for the lamp
+exposures there may be problems with flexure and defining a good
+composite spectrum.  The algorithm for longslit spectra is simpler and
+is available in the task \fBresponse\fR in the \fBlongslit\fR package.
+For multiaperture data there are problems of defining where the spectra
+lie and avoiding regions off of the aperture where there is no signal.
+The task which does this is \fBapnormalize\fR in the \fBapextract\fR
+package.   Note that the lamp observations must first be processed
+explicitly for bias and dark count corrections.
+
+Longslit spectra may also suffer the same types of iillumination
+problems found in direct imaging.  However, in this case the iillumination
+pattern is determined from sky observations (or the flat field itself)
+by finding the large scale pattern across the dispersion and at a number
+of wavelengths while avoiding the effects of night sky spectrum.  The
+task which makes this type of correction in the \fBlongslit\fR package
+is \fBiillumination\fR.  This produces an iillumination correction.
+To make sky flats or the other types of corrections image arithmetic
+is used.  Note also that the sky observations must be explicitly
+processed through the flat field stage before computing the iillumination.
+.ih
+SEE ALSO
+.nf
+ccdproc, guide, mkillumcor, mkillumflat, mkskycor, mkskyflat
+apextract.apnormalize, longslit.response, longslit.iillumination
+.fi
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/guide.hlp b/noao/imred/quadred/src/quad/doc/guide.hlp
new file mode 100644
index 00000000..d7639a6f
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/guide.hlp
@@ -0,0 +1,715 @@
+.help guide Sept93 arcon.quad
+.ce
+User's Guide to the QUAD Package
+.sh
+1. Introduction
+
+     This guide provides a brief description of the \fBquad\fR package including
+examples of its use for reducing simple CCD data. The \fBquad\fR package 
+contains all the basic tasks necessary for the reduction of CCD data obtained
+using the CTIO array controller Arcon. It is based on the IRAF CCD reduction
+package \fBccdred\fR written by Frank Valdes. It incorporates a few special
+tasks needed to deal with the peculiarities of Arcon data but most of the
+routines are taken directly from the standard package. The way in which one
+uses the routines and the basic reduction recipe is unchanged.
+
+This guide is generic in that it is not tied to any particular type of data.
+There may be more specific guides (or "cookbooks") for your data. Detailed
+descriptions of the tasks and features of the package are provided in the help
+documentation for the package.
+
+With Arcon the CCD is often readout using four ("quad") or two ("dual")
+amplifiers in order to reduce readout time. A feature of such images is that
+each readout typically has a slightly different, DC bias level, gain, and
+readout noise. As a result both zero frames and uniformly illuminated
+exposures show a characteristic chequer board pattern, the sections of the
+image read through each amplifier having different levels. In addition, there
+will be a separate overscan strip, used to monitor the zero level, for each
+readout. The location of these overscan strips in the raw frame depends on
+which amplifiers are used (for more on this see \fBquadreadout\fR). Because
+of these peculiarities the \fBquad\fR package must be used for the first
+reduction steps, overscan correction and trimming, of multi-readout images; 
+subsequent steps can be performed using \fBquad\fR or \fBccdred\fR. Either
+package can be used for the complete reduction of conventional single readout
+CCD images.
+
+     The purpose of \fBquad\fR package is to provide tools for the removal of 
+all the "instrumental signatures" from CCD data taken with Arcon. The standard
+reduction operations are: replacement of bad columns and lines by interpolation
+from neighboring columns and lines; subtraction of a bias level
+determined from overscan or prescan columns or lines; subtraction of a
+zero level using a zero exposure time calibration image; subtraction
+of a dark count calibration image appropriately scaled to the dark time
+exposure; division by a scaled flat field calibration image; division
+by an iillumination image (derived from a blank sky image); subtraction
+of a scaled fringe image (also derived from a blank sky image); and
+trimming the image of unwanted lines or columns such as the overscan
+strip.  Any set of these operations may be done simultaneously over a list of
+images in a highly efficient manner.  The reduction operations are
+recorded in the image header and may also be logged on the terminal and
+in a log file.
+
+     The package also provides tools for combining multiple exposures
+of object and calibration images to improve the statistical accuracy of
+the observations and to remove transient bad pixels.  The combining
+operation scales images of different exposure times, adjusts for
+variable sky background, statistically weights the images by their
+signal-to-noise, and provides a number of useful algorithms for
+detecting and rejecting transient bad pixels.
+
+     Other tasks are provided for listing reduction information about
+the images, deriving secondary calibration images (such as sky
+corrected flat fields or iillumination correction images), and easily
+setting the package parameters for different instruments.
+
+The \fBquad\fR package also includes some tasks which can be used for the
+examination of multi-readout images, prior to reducing them, by for instance
+calculating simple image statistics, generating histograms, etc. 
+
+     There are several important features provided by the \fBccdred\fR package 
+underpining \fBquad\fR,  which makes the reduction of CCD images convenient;
+particularly to minimize record keeping.  One of these is the ability to 
+recognize the different types of CCD images.  This ability allows the user to 
+select a certain class of images to be processed or listed and allows the
+processing tasks to identify calibration images and process them differently 
+from object images.  The standard CCD image types are \fIobject\fR,
+\fIzero\fR level, \fIdark\fR count, and \fIflat\fR field.  For more on
+the image types see \fBccdtypes\fR.
+
+     The tasks can also identify the different filters (or other subset
+parameter) which require different flat field images.  This means you don't
+have to separate the images by filter and process each set separately.
+This feature is discussed further in \fBsubsets\fR.
+
+     The tasks keep track of the reduction steps completed on each
+image and ignore images which have been processed.  This feature,
+along with recognizing the image types and subsets, makes it possible to
+specify all the images to a task with a wildcard template, such as
+"*.imh", rather than indicating each image by name.  You will find this
+extremely important with large sets of observations.
+
+     A fundamental aspect of the package is that the processing
+modifies the images.  In other words, the reduction operations are
+performed directly on the image.  This "feature" further simplifies
+record keeping, frees the user from having to form unique output image
+names, and minimizes the amount of disk space required.  There
+are two safety features in this process.  First, the modifications do
+not take effect until the operation is completed on the image.  This
+allows you to abort the task without messing up the image data and
+protects data if the computer crashes.  The second feature is that
+there is a package parameter which may be set to make a backup of the
+input data with a particular prefix such as "orig" or "imdir$".  This
+backup feature may be used when there is sufficient disk space, when learning
+to use the package, or just to be cautious.
+
+     In a similar effort to efficiently manage disk space, when combining
+images into a master object or calibration image there is an option to
+delete the input images upon completion of the combining operation.
+Generally this is desirable when there are many calibration exposures,
+such as zero level or flat field images, which are not used after they
+are combined into a final calibration image.
+
+     The following sections guide you through the basic use of the
+\fBquad\fR package.  Only the important parameters which you might
+want to change are described.  It is assumed that the support personnel
+have created the necessary instrument files (see \fBinstruments\fR)
+which will set the default parameters for the data you will be
+reducing.  If this is not the case you may need to delve more deeply
+into the details of the tasks.  Information about all the parameters
+and how the various tasks operate are given in the help documentation
+for the tasks and in additional special help topics.  Some useful help
+documentation is indicated in the discussion and also in the
+\fBReferences\fR section.
+.sh
+2. Getting Started
+
+     The first step is to load \fBquad\fR.  This is done by loading
+the \fBarcon\fR package, and then the \fBquad\fR package.  Loading a
+package consists of typing its name. 
+
+     When you load the \fBquad\fR package the menu of tasks or commands
+is listed.  This appears as follows:
+
+.nf
+  cl> quad
+      badpiximage       combine           mkillumcor        qstatistics
+      ccdgroups         cosmicrays        mkillumflat       quadproc
+      ccdhedit          darkcombine       mkskycor          quadscale
+      ccdinstrument     flatcombine       mkskyflat         setinstrument
+      ccdlist           mkfringecor       qhistogram        zerocombine
+.fi
+
+A summary of the tasks and additional help topics is obtained by typing:
+
+    cl> help
+
+This list and how to get additional help on specific topics is described
+in the \fBReferences\fR section at the end of this guide.
+
+     The first command to use is \fBsetinstrument\fR, which sets the package
+appropriately for the CCD images to be reduced.  The support personnel
+should tell you the instrument identification, but if not a list
+of known instruments may be listed by using '?' for the instrument name.
+
+.nf
+    cl> setinstrument
+    Instrument ID (type ? for a list) \fI<enter instrument id or ?>\fR
+        <Set quad package parameters using eparam>
+        <Set quadproc task parameters using eparam>
+.fi
+
+This task sets the default parameters and then allows you to modify the
+package parameters and the processing parameters using the parameter
+editor \fBeparam\fR.  If you are not familiar with \fBeparam\fR see the
+help or CL introduction documentation.  For most terminals you move up
+and down through the parameters with the terminal arrow keys, you
+change the parameters by simply typing the desired value, and you exit
+with control Z or control D.  Note that you can change parameters for
+any task at any time with \fBeparam\fR and you do not have to run
+\fBsetinstrument\fR again, even if you logout, until you need to reduce
+data from a different instrument.
+
+     The \fBquad\fR package parameters control general I/O functions of
+the tasks in the package.  The parameters you might wish to change are
+the output pixel type and the verbose option.  Except when the input
+images are short integers, the noise is significantly greater than one
+digital unit, and disk space is critical, it is probably better to
+allow the processing to convert the images to real pixel datatype.  The
+verbose parameter simply prints the information written to the log file
+on the terminal.  This can be useful when little else is being done and
+you are just beginning.  However, when doing background processing and
+other IRAF reduction tasks it is enough to simply look at the end of
+the logfile with the task \fBtail\fR to see the current state of the
+processing.
+
+     The \fBquadproc\fR parameters control the CCD processing.  There are
+many parameters but they all may be conveniently set at this point.
+Many of the parameters have default values set appropriately for the
+instrument you specified.  The images to be processed can be specified
+later.  What needs to be set are the processing operations that you
+want done and the parameters required for each operation.  The
+processing operations are selected by entering yes or no for each one.
+The following items briefly describe each of the possible processing
+operations and the additional parameters required.
+
+.ls \fIfixpix\fR - Fix bad CCD lines and columns?
+The bad pixels (cosmetic defects) in the detector are given in a file
+specified by the parameter \fIfixfile\fR.  This information is used
+to replace the pixels by interpolating from the neighboring pixels.
+A standard file for your instrument may be set by \fBsetinstrument\fR
+or if the word "image" is given then the file is defined in the instrument
+data file.  For more on the bad pixel file see \fBinstruments\fR.
+.le
+.ls \fIoverscan\fR - Apply overscan strip correction?
+The overscan or prescan region is specified by the parameter
+\fIbiassec\fR.  This is given as an IRAF image section. For guidance on 
+seting this parameter see the help page for \fBquadproc\fR. The overscan
+region is averaged along the readout axis, specified by the parameter
+\fIreadaxis\fR, to create a one dimensional bias vector.  This bias is
+fit by a function to remove cosmic rays and noise.  There are a number
+of parameters at the end of the parameter list which control the
+fitting.
+.le
+.ls \fItrim\fR - Trim the image?
+The image is trimmed to the image section given by the parameter
+\fItrimsec\fR. For guidance on setting this parameter see the help page
+for \fBquadproc\fR.
+.le
+.ls \fIzerocor\fR - Apply zero level correction?
+The zero level image to be subtracted is specified by the parameter
+\fIzero\fR.  If none is given then the calibration image will be sought
+in the list of images to be processed.
+.le
+.ls \fIdarkcor\fR - Apply dark count correction?
+The dark count image to be subtracted is specified by the parameter
+\fIdark\fR.  If none is given then the calibration image will be sought
+in the list of images to be processed.
+.le
+.ls \fIflatcor\fR - Apply flat field correction?
+The flat field images to be used are specified by the parameter
+\fIflat\fR.  There must be one flat field image for each filter
+or subset (see \fBsubsets\fR) to be processed.  If a flat field
+image is not given then the calibration image will be sought
+in the list of images to be processed.
+.le
+.ls \fIreadcor\fR - Convert zero level image to readout correction?
+If a one dimensional zero level readout correction vector is to be subtracted
+instead of a two dimensional zero level image then, when this parameter is set,
+the zero level images will be averaged to one dimension.  The readout axis
+must be specified by the parameter \fIreadaxis\fR.  The default for your
+instrument is set by \fBsetinstrument\fR.
+.le
+.ls \fIscancor\fR - Convert flat field image to scan correction?
+If the instrument is operated in a scan mode then a correction to the
+flat field may be required.  There are two types of scan modes, "shortscan"
+and "longscan".  In longscan mode flat field images will be averaged
+to one dimension and the readout axis must be specified.  Shortscan mode
+is a little more complicated.  The scan correction is used if the flat
+field images are not observed in scan mode.  The number of scan lines
+must be specified by the parameter \fInscan\fR.  If they are observed in
+scan mode, like the object observations, then the scan correction
+operations should \fInot\fR be specified.  For details of scan mode operations
+see \fBquadproc\fR.  The scan parameters
+should be set by \fBsetinstrument\fR.  If in doubt consult someone
+familiar with the instrument and mode of operation.
+.le
+
+     This description of the parameters is longer than the actual operation of
+setting the parameters.  The only parameters likely to change during processing
+are the calibration image parameters.
+
+     When processing many images using the same calibration files a modest
+performance improvement can be achieved by keeping (caching) the
+calibration images in memory to avoid disk accesses.  This option
+is available by specifying the amount of memory available for image
+caching with the parameter \fImax_cache\fR.  If the value is zero then
+the images are accessed from disk as needed while if there is
+sufficient memory the calibration images may be kept in memory during
+the task execution.
+.sh
+3. Processing Your Data
+
+     The processing path depends on the type of data, the type of
+instrument, types of calibration images, and the observing
+sequence.  In this section we describe two types of operations common
+in reducing most data; combining calibration images and performing the
+standard calibration and correction operations.  Some additional special
+operations are described in the following section.
+
+     However, the first thing you might want to try before any
+processing is to get a listing of the CCD images showing the CCD image
+types, subsets, and processing flags.  The task for this is
+\fBccdlist\fR.  It has three types of output; a short one line per
+image format, a longer format which shows the state of the processing,
+and a format which prints the image names only (used to create files
+containing lists of images of a particular CCD image type).  To get a
+quick listing type:
+
+.nf
+    cl> ccdlist *.imh
+    ccd001.imh[544,512][short][unknown][V]:FOCUS L98-193
+    ccd007.imh[544,512][short][object][V]:N2968 V 600s
+    ccd015.imh[544,512][short][object][B]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R]:N4036 R 600s
+    ccd045.imh[544,512][short][flat][V]:dflat 5s
+    ccd066.imh[544,512][short][flat][B]:dflat 5s
+    ccd103.imh[544,512][short][flat][R]:dflat 5s
+    ccd104.imh[544,512][short][zero][]:bias
+    ccd105.imh[544,512][short][dark][]:dark 3600s
+.fi
+
+     The example shows only a sample of the images.  The short format
+listing tells you the name of the image, its size and pixel type, the
+CCD image type as seen by the package, the subset identifier (in this
+case the filter), and the title.  If the data had been processed then
+there would also be processing flags.  If the CCD image types do not
+seem right then there may be a problem with the instrument
+specification.
+
+     Many of the tasks in the \fBquad\fR package have the parameter
+\fIccdtype\fR which selects a particular type of image.  To list
+only the object images from the previous example:
+
+.nf
+    cl> ccdlist *.imh ccdtype=object
+    ccd007.imh[544,512][short][object][V]:N2968 V 600s
+    ccd015.imh[544,512][short][object][B]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R]:N4036 R 600s
+.fi
+
+If no CCD image type is specified (by using the null string "")
+then all image types are selected.  This may be
+necessary if your instrument data does not contain image type identifications.
+.sh
+3.1 Combining Calibration Images
+
+     If you do not need to combine calibration images because you only
+have one image of each type, you can skip this section.  Calibration
+images, particularly zero level and flat field images, are combined in
+order to minimize the effects of noise and reject cosmic ray hits in the
+calibrations.  The basic tool for combining images is the task
+\fBcombine\fR.  There are simple variants of this task whose default
+parameters are set appropriately for each type of calibration image.
+These are the ones you will use for calibration images leaving
+\fBcombine\fR for combining object images.  Zero level images are
+combined with \fBzerocombine\fR, dark count images with
+\fBdarkcombine\fR, and flat field images with \fBflatcombine\fR.
+
+     For example, to combine flat field images the command is:
+
+.nf
+    cl> flatcombine *.imh
+    Jun  1 14:26 combine: maxreject
+            Images      N    Exp   Mode  Scale Offset Weight
+        ccd045.imh      1    5.0  INDEF  1.000     0.  0.048
+        ccd046.imh      1    5.0  INDEF  1.000     0.  0.048
+        	<... list of files ...>
+        ccd065.imh      1    5.0  INDEF  1.000     0.  0.048
+        ----------- ------ ------
+         FlatV.imh     21    5.0
+.fi
+
+This output is printed when verbose mode is set.  The same information
+is recorded in the log file.  In this case the flat fields are combined
+by rejecting the maximum value at each point in the image (the
+"maxreject" algorithm).  The images are scaled by the exposure times,
+which are all the same in this example.  The mode is not evaluated for
+exposure scaling and the relative weights are the same because the
+exposure times are the same.  The example only shows part of the
+output; \fBflatcombine\fR automatically groups the flat field images by
+filter to produce the calibration images "FlatV", "FlatB", and
+"FlatR".
+.sh
+3.2 Calibrations and Corrections
+
+     Processing the CCD data is easy and largely automated.
+First, set the task parameters with the following command:
+
+    cl> eparam quadproc
+
+You may have already set the parameters when you ran
+\fBsetinstrument\fR, though the calibration image parameters
+\fIzero\fR, \fIdark\fR, and \fIflat\fR may still need to be set or
+changed.  Once this is done simply give the command
+
+.nf
+    cl> quadproc *.imh
+    ccd003: Jun  1 15:13 Overscan section is [520:540,*] with mean=485.0
+    ccd003: Jun  1 15:14 Trim data section is [3:510,3:510]
+    ccd003: Jun  1 15:14 Overscan section is [520:540,*] with mean=485.0
+    FlatV:  Jun  1 15:14 Trim data section is [3:510,3:510]
+    FlatV:  Jun  1 15:15 Overscan section is [520:540,*] with mean=486.4
+    ccd003: Jun  1 15:15 Flat field image is FlatV.imh with scale=138.2
+    ccd004: Jun  1 15:16 Trim data section is [3:510,3:510]
+    ccd004: Jun  1 15:16 Overscan section is [520:540,*] with mean=485.2
+    ccd004: Jun  1 15:16 Flat field image is FlatV.imh with scale=138.2
+                <... more ...>
+    ccd013: Jun  1 15:22 Trim data section is [3:510,3:510]
+    ccd013: Jun  1 15:23 Overscan section is [520:540,*] with mean=482.4
+    FlatB:  Jun  1 15:23 Trim data section is [3:510,3:510]
+    FlatB:  Jun  1 15:23 Overscan section is [520:540,*] with mean=486.4
+    ccd013: Jun  1 15:24 Flat field image is FlatB.imh with scale=132.3
+                <... more ...>
+.fi
+
+     The output shown is with verbose mode set.  It is the same as
+recorded in the log file.  It illustrates the principle of automatic
+calibration image processing.  The first object image, "ccd003", was
+being processed when the flat field image was required.  Since the
+image was taken with the V filter the appropriate flat field was
+determined to be "FlatV".  Since it had not been processed, the
+processing of "ccd003" was interrupted to process "FlatV".  The
+processed calibration image may have been cached if there was enough
+memory.  Once "FlatV" was processed (note that the flat field was not
+flattened because the task knows this image is a flat field) the
+processing of "ccd003" was completed.  The next image, "ccd004", is
+also a V filter image so the already processed, and possibly cached,
+flat field "FlatV" is used again.  The first B band image is "ccd013"
+and, as before, the B filter flat field calibration image is processed
+automatically.  The same automatic calibration processing and image
+caching occurs when using zero level and dark count calibration
+images.
+
+     Commonly the processing is done with the verbose mode turned off
+and the task run as a background job.  This is done with the commands
+
+.nf
+    cl> quad.verbose=no
+    cl> quadproc *.imh &
+.fi
+
+The already processed images in the input list are recognized as having been
+processed and are not affected.  To check the status of the processing we
+can look at the end of the log file with:
+
+    cl> tail logfile
+
+After processing we can repeat the \fBccdlist\fR command to find:
+
+.nf
+    cl> ccdlist *.imh ccdtype=object
+    ccd007.imh[508,508][real][object][V][OTF]:N2968 V 600s
+    ccd015.imh[508,508][real][object][B][OTF]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R][OTF]:N4036 R 600s
+.fi
+
+The processing flags indicate the images have been overscan corrected,
+trimmed, and flat fielded.
+
+     As you can see, processing images is very easy.  There is one source
+of minor confusion for beginning users and that is dealing with calibration
+images.  First, there is no reason that calibration images
+may not be processed explicitly with \fBquadproc\fR, just remember to set
+the \fIccdtype\fR to the calibration image type or to "".  When processing
+object images the calibration images to be used may be specified either
+with the task parameter for the particular calibration image or by
+including the calibration image in the list of input images.  Calibration
+images specified by parameter value take precedence and the task
+does not check its CCD image type.  Calibration images given in the
+input list must have a valid CCD image type.  In case too many
+calibration images are specified, say because the calibration images
+combined to make the master calibration images were not deleted and
+so are part of the image list "*.imh", only the first one will be used.
+Another point to know is that flat field, iillumination, and fringe images
+are subset (filter) dependent and so a calibration image for each filter
+must be specified.
+.sh
+4. Special Processing Operations
+
+     The special processing operations are mostly concerned with the
+flat field response correction.  There are also special processing
+operations available in \fBquadproc\fR for one dimensional readout
+corrections in the zero level and flat field calibrations.  These
+were described briefly above and in more detail in \fBquadproc\fR
+and are not discussed further in this guide.  The processing
+operations described in this section are for preparing flat fields
+for two dimensional spectroscopic data, for correcting flat fields
+for iilluminations effects, for making a separate iillumination correction,
+and for applying corrections for fringe effects.  For additional
+discussion about flat fields and iillumination corrections see the
+help topic \fBflatfields\fR.
+.sh
+4.1 Spectroscopic Flat Fields
+
+     For spectroscopic data the flat fields may have to be processed to
+remove the general shape of the lamp spectrum and to replace regions outside
+of the aperture where there is no flat field information with values that
+will not cause bad response effects when the flat field is applied to the
+data.  If the shape of the lamp spectrum is not important and if the
+longslit spectra have the regions outside of the slit either off the
+detector or trimmed then you may use the flat field without special
+processing.
+
+   First you must process the flat field images explicitly with
+
+    cl> quadproc *.imh ccdtype=flat
+
+where "*.imh" may be replaced with any list containing the flat fields.
+If zero level and dark count corrections are required these calibration
+images must be available at this time.
+
+     Load the \fBtwodspec\fR package and then either the \fBlongslit\fR
+package, for longslit data, or the \fBapextract\fR package, for
+multiaperture data such as echelles, multifiber, or aperture mask
+spectra.  The task for removing the longslit quartz spectrum is
+\fBresponse\fR.  There is also a task for removing iillumination
+effects, including the slit profile, from longslit spectra called
+\fBiillumination\fR.  For more about processing longslit spectra see the
+help for these tasks and the paper \fIReduction of Longslit Spectra
+with IRAF\fR.  The cookbook \fIReduction of Longslit Spectroscopic
+Data Using IRAF (KPNO ICCD and Cryogenic Camera Data)\fR also provides
+a very good discussion even if your data is from a different instrument.
+
+     For multiaperture data the task for removing the relative shapes of
+the spectra is called \fBapnormalize\fR.  Again, consult the help documentation
+for this task for further details.  Since you will probably also be
+using the package for extracting the spectra you may be interested
+in the document \fIThe IRAF APEXTRACT Package\fR.
+.sh
+4.2 Iillumination Corrections
+
+     The flat field calibration images may not have the same iillumination
+pattern as the observations of the sky due to the way the lamp illuminates the
+optical system.  In this case when the flat field correction is applied
+to the data there will be gradients in the sky background.  To remove
+these gradients a blank sky calibration image is heavily smoothed
+to produce an iillumination image.  The iillumination image
+is then divided into the images during processing to correct for the
+iillumination difference between the flat field and the objects.
+Like the flat fields, the iillumination corrections images may be subset
+dependent so there should be an iillumination image for each subset.
+
+The task which makes iillumination correction images is \fBmkskycor\fR.
+Some examples are
+
+.nf
+    cl> mkskycor sky004 Illum004
+    cl> mkskycor sky*.imh ""
+.fi
+
+In the first example the sky image "sky004" is used to make the iillumination
+correction image "Illum004".  In the second example the sky images are
+converted to iillumination correction images by specifying no output image
+names.  Like \fBquadproc\fR if the input images have not been processed they
+are first processed automatically.
+
+To apply the iillumination correction
+
+.nf
+    cl> quadproc *.imh ccdtype=object illumcor+ illum=Illum004
+    cl> quadproc *.imh ccdtype=object illumcor+ illum=sky*.imh
+.fi
+
+The iillumination images could also be set using \fBeparam\fR or given
+on the command line.
+.sh
+4.3 Sky Flat Fields
+
+    You will notice that when you process images with an iillumination
+correction you are dividing each image by a flat field calibration and
+an iillumination correction.  If the iillumination corrections are not
+done as a later step but at the same time as the rest of the processing
+one will get the same calibration by multiplying the flat field by
+the iillumination correction and using this product alone as the
+flat field.  Such an image is called a \fIsky flat\fR since it is
+a flat field which has been corrected to yield a flat sky when applied
+to the observations.  This approach has the advantage of one less
+calibration image and two less computations (scaling and dividing the
+iillumination correction).  As an added short cut, rather than compute
+the iillumination image with \fBmkskycor\fR and then multiplying, the
+task \fBmkskyflat\fR does all this in one step.  Thus, \fBmkskyflat\fR
+takes an input blank sky image, processes it if needed, determines the
+appropriate flat field (sky flats are also subset dependent) from the
+\fBquadproc\fR parameters or the input image list, and produces an
+output sky flat.  Further if no output image is specified the task
+converts the input blank sky calibration image into a sky flat.
+
+     Two examples in which a new image is created and in which the
+input images are converted to sky flats are
+
+.nf
+    cl> mkskyflat sky004 Skyflat
+    cl> mkskyflat sky*.imh ""
+.fi
+.sh
+4.4 Iillumination Corrected Flat Fields
+
+     A third method to account for iillumination problems in the flat fields
+is to remove the large scale pattern from the flat field itself.  This is
+useful if there are no reasonable blank sky calibration images and the
+astronomical exposures are evenly illuminated but the flat fields are not.
+This is done by smoothing the flat field images instead of blank sky
+images.  As with using the sky images there are two methods, creating
+an iillumination correction to be applied as a separate step or fixing
+the original flat field.  The smoothing algorithm is
+the same as that used in the other tasks.  The tasks to make these types
+of corrections are \fBmkillumcor\fR and \fBmkillumflat\fR.  The usage
+is pretty much the same as the other iillumination correction tasks
+except that it is more reasonable to replace the original flat fields
+by the corrected flat fields when fixing the flat field.  Examples
+of an iillumination correction and removing the iillumination pattern
+from the flat field are
+
+.nf
+    cl> mkillumcor flat025 Illum025
+    cl> mkillumflat flat*.imh ""
+.fi
+
+As with the other tasks, the input images are processed if necessary.
+.sh
+4.5 Fringe Corrections
+
+    Some CCD detectors suffer from fringing effects due to the night
+sky emission lines which are not removed by the other calibration
+and correction operations.  To correct for the fringing you need a
+really blank sky image.  There is not yet a task to remove objects from
+sky images because this is often done with an interactive image display
+tool (which will soon be added).  The blank sky image is heavily smoothed
+to determine the mean sky background and then this is subtracted from the
+original image.  The image should then be essentially zero except for the
+fringe pattern.  This fringe correction image is scaled to the same
+exposure time as the image to be corrected and then subtracted to remove
+the fringing.  Note that since the night sky lines are variable there
+may need to be an additional scaling applied.  Determining this scaling
+requires either an interactive display tool or a very clever task.
+Such tasks will also be added in the future.
+
+     The task to make a fringe correction image is \fBmkfringecor\fR.
+the sky background is determined in exactly the same way as the iillumination
+pattern, in fact the same sky image may be used for both the sky
+iillumination and for the fringe correction.  The task works consistently
+with the "mk" tasks in that the input images are processed first if needed
+and then the output correction image is produced with the specified name
+or replaces the input image if no output image is specified.
+As examples,
+
+.nf
+    cl> mkfringecor sky004 Fringe
+    cl> mkfringecor sky*.imh ""
+.fi
+.sh
+6. Summary
+
+     The \fBquad\fR package is very easy to use.  First load the package;
+it is in the \fBarcon\fR package.  If this is your first time reducing data
+from a particular instrument or if you have changed instruments then run
+\fBsetinstrument\fR. Set the processing parameters for the operations you want
+performed.  If you need to combine calibration images to form a master 
+calibration image use one of the combine tasks.  Spectroscopic flat fields may
+need to be processed first in order to remove the lamp spectrum.
+Finally, just type
+
+    cl> quadproc *.imh&
+.sh
+7. References
+
+     A general guide to using IRAF is \fIA User's Introduction to the IRAF
+Command Language\fR.  This document may be found in the IRAF documentation
+sets and is available from the National Optical Astronomy Observatories,
+Central Computer Services (NOAO-CCS).
+
+     A more detailed description of the \fBccdred\fR package, on which
+\fBquad\fR is based,  including a discussion of the design and some of the
+algorithms see \fIThe IRAF CCD Reduction Package -- CCDRED\fR by F. Valdes.
+This paper is available from NOAO-CCS and appears in the proceedings of the 
+Santa Cruz Summer Workshop in Astronomy and Astrophysics, \fIInstrumentation
+for Ground-Based Optical Astronomy: Present and Future\fR, edited by 
+Lloyd B. Robinson and published by Springer-Verlag.
+
+     The task descriptions and supplementary documentation are available
+on-line through the help task by typing
+
+    cl> help \fItopic\fR
+
+where \fItopic\fR is one of the following.
+
+.nf
+             SPECIAL TASKS FOR MULTI-READOUT CCD IMAGES
+ 
+       quadproc - Process multi-readout CCD images
+      quadscale - Apply correction for amplifier dependent gain differences
+    qstatistics - Calculate image statistics for multi-readout CCD images
+     qhistogram - Make histogram of multi-readout CCD image
+    darkcombine - Combine and process dark count images
+    flatcombine - Combine and process flat field images
+    zerocombine - Combine and process zero level images
+ 
+ 
+            STANDARD CCDRED TASKS
+ 
+    badpiximage - Create a bad pixel mask image from a bad pixel file
+      ccdgroups - Group CCD images into image lists
+       ccdhedit - CCD image header editor
+  ccdinstrument - Review and edit instrument translation files
+        ccdlist - List CCD processing information
+        combine - Combine CCD images
+     cosmicrays - Detect and replace cosmic rays
+    mkfringecor - Make fringe correction images from sky images
+     mkillumcor - Make flat field iillumination correction images
+    mkillumflat - Make iillumination corrected flat fields
+       mkskycor - Make sky iillumination correction images
+      mkskyflat - Make sky corrected flat field images
+  setinstrument - Set instrument parameters
+ 
+              ADDITIONAL HELP TOPICS
+ 
+    ccdgeometry - Discussion of CCD coordinate/geometry keywords
+       ccdtypes - Description of the CCD image types
+     flatfields - Discussion of CCD flat field calibrations
+          guide - Introductory guide to using the CCDRED package
+    instruments - Instrument specific data files
+        package - CCD image reduction package
+    quadreadout - Description of multi-readout CCD data
+        subsets - Description of CCD subsets
+.fi
+
+Printed copies of the on-line help documentation may be made with the
+command
+
+    cl> help topic | lprint
+
+     In addition to the package documentation for \fBquad\fR,
+\fBlongslit\fR, and \fBapextract\fR there may be specific guides for
+certain instruments.  These specific guides, called "cookbooks", give
+specific examples and parameter values for the CCD data.
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/guide.ms b/noao/imred/quadred/src/quad/doc/guide.ms
new file mode 100644
index 00000000..62d87bb9
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/guide.ms
@@ -0,0 +1,794 @@
+.RP
+.TL
+User's Guide to the CCDRED Package
+.AU
+Francisco Valdes
+.AI
+IRAF Group - Central Computer Services
+.K2
+P.O. Box 26732, Tucson, Arizona 85726
+June 1987
+Revised February 1988
+.AB
+The IRAF CCD reduction package, \fBccdred\fR, provides tools
+for the easy and efficient reduction of CCD images.  The standard
+reduction operations are replacement of bad pixels, subtraction of an
+overscan or prescan bias, subtraction of a zero level image,
+subtraction of a dark count image, division by a flat field calibration
+image, division by an illumination correction, subtraction of a fringe
+image, and trimming unwanted lines or columns.  Another common
+operation provided by the package is scaling and combining images with
+a number of algorithms for rejecting cosmic rays.  Data in the image
+header is used to make the reductions largely automated and
+self-documenting though the package may still be used in the absence of
+this data.  Also a translation mechanism is used to relate image header
+parameters to those used by the package to allow data from a variety of
+observatories and instruments to be processed.  This guide provides a brief
+description of the IRAF CCD reduction package and examples of reducing
+simple CCD data.
+.AE
+.NH
+Introduction
+.LP
+     This guide provides a brief description of the IRAF CCD reduction
+package \fBccdred\fR and examples of reducing simple CCD data.  It is a
+generic guide in that it is not tied to any particular type of data.
+There may be more specific guides (or "cookbooks") for your data.
+Detailed descriptions of the tasks and features of the package are
+provided in the help documentation for the package.
+
+     The purpose of the CCDRED package is to provide tools for the easy
+and efficient reduction of CCD images.  The standard reduction
+operations are replacement of bad columns and lines by interpolation
+from neighboring columns and lines, subtraction of a bias level
+determined from overscan or prescan columns or lines, subtraction of a
+zero level using a zero length exposure calibration image, subtraction
+of a dark count calibration image appropriately scaled to the dark time
+exposure, division by a scaled flat field calibration image, division
+by an illumination image (derived from a blank sky image), subtraction
+of a scaled fringe image (also derived from a blank sky image), and
+trimming the image of unwanted lines or columns such as the overscan
+strip.  Any set of operations may be done simultaneously over a list of
+images in a highly efficient manner.  The reduction operations are
+recorded in the image header and may also be logged on the terminal and
+in a log file.
+
+     The package also provides tools for combining multiple exposures
+of object and calibration images to improve the statistical accuracy of
+the observations and to remove transient bad pixels.  The combining
+operation scales images of different exposure times, adjusts for
+variable sky background, statistically weights the images by their
+signal-to-noise, and provides a number of useful algorithms for
+detecting and rejecting transient bad pixels.
+
+     Other tasks are provided for listing reduction information about
+the images, deriving secondary calibration images (such as sky
+corrected flat fields or illumination correction images), and easily
+setting the package parameters for different instruments.
+
+     There are several important features provided by the package to
+make the reduction of CCD images convenient; particularly to minimize
+record keeping.  One of these is the ability to recognize the different
+types of CCD images.  This ability allows the user to select a certain
+class of images to be processed or listed and allows the processing
+tasks to identify calibration images and process them differently from
+object images.  The standard CCD image types are \fIobject\fR,
+\fIzero\fR level, \fIdark\fR count, and \fIflat\fR field.  For more on
+the image types see \fBccdtypes\fR.
+
+     The tasks can also identify the different filters (or other subset
+parameter) which require different flat field images.  This means you don't
+have to separate the images by filter and process each set separately.
+This feature is discussed further in \fBsubsets\fR.
+
+     The tasks keep track of the reduction steps completed on each
+image and ignore images which have been processed.  This feature,
+along with recognizing the image types and subsets, makes it possible to
+specify all the images to a task with a wildcard template, such as
+"*.imh", rather than indicating each image by name.  You will find this
+extremely important with large sets of observations.
+
+     A fundamental aspect of the package is that the processing
+modifies the images.  In other words, the reduction operations are
+performed directly on the image.  This "feature" further simplifies
+record keeping, frees the user from having to form unique output image
+names, and minimizes the amount of disk space required.  There
+are two safety features in this process.  First, the modifications do
+not take effect until the operation is completed on the image.  This
+allows you to abort the task without messing up the image data and
+protects data if the computer crashes.  The second feature is that
+there is a package parameter which may be set to make a backup of the
+input data with a particular prefix such as "orig" or "imdir$".  This
+backup feature may be used when there is sufficient disk space, when learning
+to use the package, or just to be cautious.
+
+     In a similar effort to efficiently manage disk space, when combining
+images into a master object or calibration image there is an option to
+delete the input images upon completion of the combining operation.
+Generally this is desirable when there are many calibration exposures,
+such as zero level or flat field images, which are not used after they
+are combined into a final calibration image.
+
+     The following sections guide you through the basic use of the
+\fBccdred\fR package.  Only the important parameters which you might
+want to change are described.  It is assumed that the support personnel
+have created the necessary instrument files (see \fBinstruments\fR)
+which will set the default parameters for the data you will be
+reducing.  If this is not the case you may need to delve more deeply
+into the details of the tasks.  Information about all the parameters
+and how the various tasks operate are given in the help documentation
+for the tasks and in additional special help topics.  Some useful help
+documentation is indicated in the discussion and also in the
+\fBReferences\fR section.
+.NH
+Getting Started
+.LP
+     The first step is to load \fBccdred\fR.  This is done by loading
+the \fBnoao\fR package, followed by the image reduction package
+\fBimred\fR, and finally the \fBccdred\fR package.  Loading a
+package consists of typing its name.  Note that some of these packages may be
+loaded automatically when you logon to IRAF.
+
+     When you load the \fBccdred\fR package the menu of tasks or commands
+is listed.  This appears as follows:
+
+.nf
+.KS
+.ft L
+    cl> ccdred
+      badpiximage       ccdtest           mkfringecor       setinstrument
+      ccdgroups         combine           mkillumcor        zerocombine
+      ccdhedit          cosmicrays        mkillumflat       
+      ccdlist           darkcombine       mkskycor          
+      ccdproc           flatcombine       mkskyflat         
+.ft R
+.KE
+.fi
+
+A summary of the tasks and additional help topics is obtained by typing:
+
+.ft L
+    cl> help
+.ft R
+
+This list and how to get additional help on specific topics is described
+in the \fBReferences\fR section at the end of this guide.
+
+     The first command to use is \fBsetinstrument\fR, which sets the package
+appropriately for the CCD images to be reduced.  The support personnel
+should tell you the instrument identification, but if not a list
+of known instruments may be listed by using '?' for the instrument name.
+
+.nf
+.ft L
+    cl> setinstrument
+    Instrument ID (type ? for a list) \fI<enter instrument id or ?>
+        <Set ccdred package parameters using eparam>
+        <Set ccdproc task parameters using eparam>
+.ft R
+.fi
+
+This task sets the default parameters and then allows you to modify the
+package parameters and the processing parameters using the parameter
+editor \fBeparam\fR.  If you are not familiar with \fBeparam\fR see the
+help or CL introduction documentation.  For most terminals you move up
+and down through the parameters with the terminal arrow keys, you
+change the parameters by simply typing the desired value, and you exit
+with control Z or control D.  Note that you can change parameters for
+any task at any time with \fBeparam\fR and you do not have to run
+\fBsetinstrument\fR again, even if you logout, until you need to reduce
+data from a different instrument.
+
+     The \fBccdred\fR package parameters control general I/O functions of
+the tasks in the package.  The parameters you might wish to change are
+the output pixel type and the verbose option.  Except when the input
+images are short integers, the noise is significantly greater than one
+digital unit, and disk space is critical, it is probably better to
+allow the processing to convert the images to real pixel datatype.  The
+verbose parameter simply prints the information written to the log file
+on the terminal.  This can be useful when little else is being done and
+you are just beginning.  However, when doing background processing and
+other IRAF reduction tasks it is enough to simply look at the end of
+the logfile with the task \fBtail\fR to see the current state of the
+processing.
+
+     The \fBccdproc\fR parameters control the CCD processing.  There are
+many parameters but they all may be conveniently set at this point.
+Many of the parameters have default values set appropriately for the
+instrument you specified.  The images to be processed can be specified
+later.  What needs to be set are the processing operations that you
+want done and the parameters required for each operation.  The
+processing operations are selected by entering yes or no for each one.
+The following items briefly describe each of the possible processing
+operations and the additional parameters required.
+
+.LP
+\fIfixpix\fR - Fix bad CCD lines and columns?
+.IP
+The bad pixels (cosmetic defects) in the detector are given in a file
+specified by the parameter \fIfixfile\fR.  This information is used
+to replace the pixels by interpolating from the neighboring pixels.
+A standard file for your instrument may be set by \fBsetinstrument\fR
+or if the word "image" is given then the file is defined in the instrument
+data file.  For more on the bad pixel file see \fBinstruments\fR.
+.LP
+\fIoverscan\fR - Apply overscan strip correction?
+.IP
+The overscan or prescan region is specified by the parameter
+\fIbiassec\fR.  This is given as an IRAF image section.  The overscan
+region is averaged along the readout axis, specified by the parameter
+\fIreadaxis\fR, to create a one dimensional bias vector.  This bias is
+fit by a function to remove cosmic rays and noise.  There are a number
+of parameters at the end of the parameter list which control the
+fitting.  The default overscan bias section and fitting parameters for
+your instrument should be set by \fBsetinstrument\fR.  If the word
+"image" is given the overscan bias section is defined in the image
+header or the instrument translation file.  If an overscan section is
+not set you can use \fBimplot\fR to determine the columns or rows for
+the bias region and define an overscan image section.  If you are
+unsure about image sections consult with someone or read the
+introductory IRAF documentation.
+.LP
+\fItrim\fR - Trim the image?
+.IP
+The image is trimmed to the image section given by the parameter
+\fItrimsec\fR.  A default trim section for your instrument should be
+set by \fBsetinstrument\fR, however, you may override this default if
+desired.  If the word "image" is given the data
+image section is given in the image header or the instrument
+translation file.  As with the overscan image section it is
+straightforward to specify, but if you are unsure consult someone.
+.LP
+\fIzerocor\fR - Apply zero level correction?
+.IP
+The zero level image to be subtracted is specified by the parameter
+\fIzero\fR.  If none is given then the calibration image will be sought
+in the list of images to be processed.
+.LP
+\fIdarkcor\fR - Apply dark count correction?
+.IP
+The dark count image to be subtracted is specified by the parameter
+\fIdark\fR.  If none is given then the calibration image will be sought
+in the list of images to be processed.
+.LP
+\fIflatcor\fR - Apply flat field correction?
+.IP
+The flat field images to be used are specified by the parameter
+\fIflat\fR.  There must be one flat field image for each filter
+or subset (see \fBsubsets\fR) to be processed.  If a flat field
+image is not given then the calibration image will be sought
+in the list of images to be processed.
+.LP
+\fIreadcor\fR - Convert zero level image to readout correction?
+.IP
+If a one dimensional zero level readout correction vector is to be subtracted
+instead of a two dimensional zero level image then, when this parameter is set,
+the zero level images will be averaged to one dimension.  The readout axis
+must be specified by the parameter \fIreadaxis\fR.  The default for your
+instrument is set by \fBsetinstrument\fR.
+.LP
+\fIscancor\fR - Convert flat field image to scan correction?
+.IP
+If the instrument is operated in a scan mode then a correction to the
+flat field may be required.  There are two types of scan modes, "shortscan"
+and "longscan".  In longscan mode flat field images will be averaged
+to one dimension and the readout axis must be specified.  Shortscan mode
+is a little more complicated.  The scan correction is used if the flat
+field images are not observed in scan mode.  The number of scan lines
+must be specified by the parameter \fInscan\fR.  If they are observed in
+scan mode, like the object observations, then the scan correction
+operations should \fInot\fR be specified.  For details of scan mode operations
+see \fBccdproc\fR.  The scan parameters
+should be set by \fBsetinstrument\fR.  If in doubt consult someone
+familiar with the instrument and mode of operation.
+.LP
+
+     This description of the parameters is longer than the actual operation of
+setting the parameters.  The only parameters likely to change during processing
+are the calibration image parameters.
+
+     When processing many images using the same calibration files a modest
+performance improvement can be achieved by keeping (caching) the
+calibration images in memory to avoid disk accesses.  This option
+is available by specifying the amount of memory available for image
+caching with the parameter \fImax_cache\fR.  If the value is zero then
+the images are accessed from disk as needed while if there is
+sufficient memory the calibration images may be kept in memory during
+the task execution.
+.NH
+Processing Your Data
+.LP
+     The processing path depends on the type of data, the type of
+instrument, types of calibration images, and the observing
+sequence.  In this section we describe two types of operations common
+in reducing most data; combining calibration images and performing the
+standard calibration and correction operations.  Some additional special
+operations are described in the following section.
+
+     However, the first thing you might want to try before any
+processing is to get a listing of the CCD images showing the CCD image
+types, subsets, and processing flags.  The task for this is
+\fBccdlist\fR.  It has three types of of output; a short one line per
+image format, a longer format which shows the state of the processing,
+and a format which prints the image names only (used to create files
+containing lists of images of a particular CCD image type).  To get a
+quick listing type:
+
+.nf
+.ft L
+    cl> ccdlist *.imh
+    ccd001.imh[544,512][short][unknown][V]:FOCUS L98-193
+    ccd007.imh[544,512][short][object][V]:N2968 V 600s
+    ccd015.imh[544,512][short][object][B]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R]:N4036 R 600s
+    ccd045.imh[544,512][short][flat][V]:dflat 5s
+    ccd066.imh[544,512][short][flat][B]:dflat 5s
+    ccd103.imh[544,512][short][flat][R]:dflat 5s
+    ccd104.imh[544,512][short][zero][]:bias
+    ccd105.imh[544,512][short][dark][]:dark 3600s
+.ft R
+.fi
+
+     The example shows only a sample of the images.  The short format
+listing tells you the name of the image, its size and pixel type, the
+CCD image type as seen by the package, the subset identifier (in this
+case the filter), and the title.  If the data had been processed then
+there would also be processing flags.  If the CCD image types do not
+seem right then there may be a problem with the instrument
+specification.
+
+     Many of the tasks in the \fBccdred\fR package have the parameter
+\fIccdtype\fR which selects a particular type of image.  To list
+only the object images from the previous example:
+
+.nf
+.ft L
+    cl> ccdlist *.imh ccdtype=object
+    ccd007.imh[544,512][short][object][V]:N2968 V 600s
+    ccd015.imh[544,512][short][object][B]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R]:N4036 R 600s
+.ft R
+.fi
+
+If no CCD image type is specified (by using the null string "")
+then all image types are selected.  This may be
+necessary if your instrument data does not contain image type identifications.
+.NH 2
+Combining Calibration Images
+.LP
+     If you do not need to combine calibration images because you only
+have one image of each type, you can skip this section.  Calibration
+images, particularly zero level and flat field images, are combined in
+order to minimize the effects of noise and reject bad pixels in the
+calibrations.  The basic tool for combining images is the task
+\fBcombine\fR.  There are simple variants of this task whose default
+parameters are set appropriately for each type of calibration image.
+These are the ones you will use for calibration images leaving
+\fBcombine\fR for combining object images.  Zero level images are
+combined with \fBzerocombine\fR, dark count images with
+\fBdarkcombine\fR, and flat field images with \fBflatcombine\fR.
+
+     For example, to combine flat field images the command is:
+
+.nf
+.ft L
+    cl> flatcombine *.imh
+    Jun  1 14:26 combine: maxreject
+            Images      N    Exp   Mode  Scale Offset Weight
+        ccd045.imh      1    5.0  INDEF  1.000     0.  0.048
+        ccd046.imh      1    5.0  INDEF  1.000     0.  0.048
+        	\fI<... list of files ...>\fL
+        ccd065.imh      1    5.0  INDEF  1.000     0.  0.048
+        ----------- ------ ------
+         FlatV.imh     21    5.0
+.ft R
+.fi
+
+This output is printed when verbose mode is set.  The same information
+is recorded in the log file.  In this case the flat fields are combined
+by rejecting the maximum value at each point in the image (the
+"maxreject" algorithm).  The images are scaled by the exposure times,
+which are all the same in this example.  The mode is not evaluated for
+exposure scaling and the relative weights are the same because the
+exposure times are the same.  The example only shows part of the
+output; \fBflatcombine\fR automatically groups the flat field images by
+filter to produce the calibration images "FlatV", "FlatB", and
+"FlatR".
+.NH 2
+Calibrations and Corrections
+.LP
+     Processing the CCD data is easy and largely automated.
+First, set the task parameters with the following command:
+
+.ft L
+    cl> eparam ccdproc
+.ft R
+
+You may have already set the parameters when you ran
+\fBsetinstrument\fR, though the calibration image parameters
+\fIzero\fR, \fIdark\fR, and \fIflat\fR may still need to be set or
+changed.  Once this is done simply give the command
+
+.nf
+.ft L
+    cl> ccdproc *.imh
+    ccd003: Jun  1 15:13 Overscan section is [520:540,*] with mean=485.0
+    ccd003: Jun  1 15:14 Trim data section is [3:510,3:510]
+    ccd003: Jun  1 15:14 Overscan section is [520:540,*] with mean=485.0
+    FlatV:  Jun  1 15:14 Trim data section is [3:510,3:510]
+    FlatV:  Jun  1 15:15 Overscan section is [520:540,*] with mean=486.4
+    ccd003: Jun  1 15:15 Flat field image is FlatV.imh with scale=138.2
+    ccd004: Jun  1 15:16 Trim data section is [3:510,3:510]
+    ccd004: Jun  1 15:16 Overscan section is [520:540,*] with mean=485.2
+    ccd004: Jun  1 15:16 Flat field image is FlatV.imh with scale=138.2
+                \fI<... more ...>\fL
+    ccd013: Jun  1 15:22 Trim data section is [3:510,3:510]
+    ccd013: Jun  1 15:23 Overscan section is [520:540,*] with mean=482.4
+    FlatB:  Jun  1 15:23 Trim data section is [3:510,3:510]
+    FlatB:  Jun  1 15:23 Overscan section is [520:540,*] with mean=486.4
+    ccd013: Jun  1 15:24 Flat field image is FlatB.imh with scale=132.3
+                \fI<... more ...>\fL
+.ft R
+.fi
+
+     The output shown is with verbose mode set.  It is the same as
+recorded in the log file.  It illustrates the principle of automatic
+calibration image processing.  The first object image, "ccd003", was
+being processed when the flat field image was required.  Since the
+image was taken with the V filter the appropriate flat field was
+determined to be "FlatV".  Since it had not been processed, the
+processing of "ccd003" was interrupted to process "FlatV".  The
+processed calibration image may have been cached if there was enough
+memory.  Once "FlatV" was processed (note that the flat field was not
+flattened because the task knows this image is a flat field) the
+processing of "ccd003" was completed.  The next image, "ccd004", is
+also a V filter image so the already processed, and possibly cached,
+flat field "FlatV" is used again.  The first B band image is "ccd013"
+and, as before, the B filter flat field calibration image is processed
+automatically.  The same automatic calibration processing and image
+caching occurs when using zero level and dark count calibration
+images.
+
+     Commonly the processing is done with the verbose mode turned off
+and the task run as a background job.  This is done with the commands
+
+.nf
+.ft L
+    cl> ccdred.verbose=no
+    cl> ccdproc *.imh &
+.ft R
+.fi
+
+The already processed images in the input list are recognized as having been
+processed and are not affected.  To check the status of the processing we
+can look at the end of the log file with:
+
+.ft L
+    cl> tail logfile
+.ft R
+
+After processing we can repeat the \fBccdlist\fR command to find:
+
+.nf
+.ft L
+    cl> ccdlist *.imh ccdtype=object
+    ccd007.imh[508,508][real][object][V][OTF]:N2968 V 600s
+    ccd015.imh[508,508][real][object][B][OTF]:N3098 B 500s
+    ccd024.imh[544,512][short][object][R][OTF]:N4036 R 600s
+.ft R
+.fi
+
+The processing flags indicate the images have been overscan corrected,
+trimmed, and flat fielded.
+
+     As you can see, processing images is very easy.  There is one source
+of minor confusion for beginning users and that is dealing with calibration
+images.  First, there is no reason that calibration images
+may not be processed explicitly with \fBccdproc\fR, just remember to set
+the \fIccdtype\fR to the calibration image type or to "".  When processing
+object images the calibration images to be used may be specified either
+with the task parameter for the particular calibration image or by
+including the calibration image in the list of input images.  Calibration
+images specified by parameter value take precedence and the task
+does not check its CCD image type.  Calibration images given in the
+input list must have a valid CCD image type.  In case too many
+calibration images are specified, say because the calibration images
+combined to make the master calibration images were not deleted and
+so are part of the image list "*.imh", only the first one will be used.
+Another point to know is that flat field, illumination, and fringe images
+are subset (filter) dependent and so a calibration image for each filter
+must be specified.
+.NH
+Special Processing Operations
+.LP
+     The special processing operations are mostly concerned with the
+flat field response correction.  There are also special processing
+operations available in \fBccdproc\fR for one dimensional readout
+corrections in the zero level and flat field calibrations.  These
+were described briefly above and in more detail in \fBccdproc\fR
+and are not discussed further in this guide.  The processing
+operations described in this section are for preparing flat fields
+for two dimensional spectroscopic data, for correcting flat fields
+for illuminations effects, for making a separate illumination correction,
+and for applying corrections for fringe effects.  For additional
+discussion about flat fields and illumination corrections see the
+help topic \fBflatfields\fR.
+.NH 2
+Spectroscopic Flat Fields
+.LP
+     For spectroscopic data the flat fields may have to be processed to
+remove the general shape of the lamp spectrum and to replace regions outside
+of the aperture where there is no flat field information with values that
+will not cause bad response effects when the flat field is applied to the
+data.  If the shape of the lamp spectrum is not important and if the
+longslit spectra have the regions outside of the slit either off the
+detector or trimmed then you may use the flat field without special
+processing.
+
+   First you must process the flat field images explicitly with
+
+.ft L
+    cl> ccdproc *.imh ccdtype=flat
+.ft R
+
+where "*.imh" may be replaced with any list containing the flat fields.
+If zero level and dark count corrections are required these calibration
+images must be available at this time.
+
+     Load the \fBtwodspec\fR package and then either the \fBlongslit\fR
+package, for longslit data, or the \fBapextract\fR package, for
+multiaperture data such as echelles, multifiber, or aperture mask
+spectra.  The task for removing the longslit quartz spectrum is
+\fBresponse\fR.  There is also a task for removing illumination
+effects, including the slit profile, from longslit spectra called
+\fBillumination\fR.  For more about processing longslit spectra see the
+help for these tasks and the paper \fIReduction of Longslit Spectra
+with IRAF\fR.  The cookbook \fIReduction of Longslit Spectroscopic
+Data Using IRAF (KPNO ICCD and Cryogenic Camera Data)\fR also provides
+a very good discussion even if your data is from a different instrument.
+
+     For multiaperture data the task for removing the relative shapes of
+the spectra is called \fBapnormalize\fR.  Again, consult the help documentation
+for this task for further details.  Since you will probably also be
+using the package for extracting the spectra you may be interested
+in the document \fIThe IRAF APEXTRACT Package\fR.
+.NH 2
+Illumination Corrections
+.LP
+     The flat field calibration images may not have the same illumination
+pattern as the observations of the sky due to the way the lamp illuminates the
+optical system.  In this case when the flat field correction is applied
+to the data there will be gradients in the sky background.  To remove
+these gradients a blank sky calibration image is heavily smoothed
+to produce an illumination image.  The illumination image
+is then divided into the images during processing to correct for the
+illumination difference between the flat field and the objects.
+Like the flat fields, the illumination corrections images may be subset
+dependent so there should be an illumination image for each subset.
+
+The task which makes illumination correction images is \fBmkskycor\fR.
+Some examples are
+
+.nf
+.ft L
+    cl> mkskycor sky004 Illum004
+    cl> mkskycor sky*.imh ""
+.ft R
+.fi
+
+In the first example the sky image "sky004" is used to make the illumination
+correction image "Illum004".  In the second example the sky images are
+converted to illumination correction images by specifying no output image
+names.  Like \fBccdproc\fR if the input images have not been processed they
+are first processed automatically.
+
+To apply the illumination correction
+
+.nf
+.ft L
+    cl> ccdproc *.imh ccdtype=object illumcor+ illum=Illum004
+    cl> ccdproc *.imh ccdtype=object illumcor+ illum=sky*.imh
+.ft R
+.fi
+
+The illumination images could also be set using \fBeparam\fR or given
+on the command line.
+.NH 2
+Sky Flat Fields
+.LP
+    You will notice that when you process images with an illumination
+correction you are dividing each image by a flat field calibration and
+an illumination correction.  If the illumination corrections are not
+done as a later step but at the same time as the rest of the processing
+one will get the same calibration by multiplying the flat field by
+the illumination correction and using this product alone as the
+flat field.  Such an image is called a \fIsky flat\fR since it is
+a flat field which has been corrected to yield a flat sky when applied
+to the observations.  This approach has the advantage of one less
+calibration image and two less computations (scaling and dividing the
+illumination correction).  As an added short cut, rather than compute
+the illumination image with \fBmkskycor\fR and then multiplying, the
+task \fBmkskyflat\fR does all this in one step.  Thus, \fBmkskyflat\fR
+takes an input blank sky image, processes it if needed, determines the
+appropriate flat field (sky flats are also subset dependent) from the
+\fBccdproc\fR parameters or the input image list, and produces an
+output sky flat.  Further if no output image is specified the task
+converts the input blank sky calibration image into a sky flat.
+
+     Two examples in which a new image is created and in which the
+input images are converted to sky flats are
+
+.nf
+.ft L
+    cl> mkskyflat sky004 Skyflat
+    cl> mkskyflat sky*.imh ""
+.ft R
+.fi
+.NH 2
+Illumination Corrected Flat Fields
+.LP
+     A third method to account for illumination problems in the flat fields
+is to remove the large scale pattern from the flat field itself.  This is
+useful if there are no reasonable blank sky calibration images and the
+astronomical exposures are evenly illuminated but the flat fields are not.
+This is done by smoothing the flat field images instead of blank sky
+images.  As with using the sky images there are two methods, creating
+an illumination correction to be applied as a separate step or fixing
+the original flat field.  The smoothing algorithm is
+the same as that used in the other tasks.  The tasks to make these types
+of corrections are \fBmkillumcor\fR and \fBmkillumflat\fR.  The usage
+is pretty much the same as the other illumination correction tasks
+except that it is more reasonable to replace the original flat fields
+by the corrected flat fields when fixing the flat field.  Examples
+of an illumination correction and removing the illumination pattern
+from the flat field are
+
+.nf
+.ft L
+    cl> mkillumcor flat025 Illum025
+    cl> mkillumflat flat*.imh ""
+.ft R
+.fi
+
+As with the other tasks, the input images are processed if necessary.
+.NH 2
+Fringe Corrections
+.LP
+    Some CCD detectors suffer from fringing effects due to the night
+sky emission lines which are not removed by the other calibration
+and correction operations.  To correct for the fringing you need a
+really blank sky image.  There is not yet a task to remove objects from
+sky images because this is often done with an interactive image display
+tool (which will soon be added).  The blank sky image is heavily smoothed
+to determine the mean sky background and then this is subtracted from the
+original image.  The image should then be essentially zero except for the
+fringe pattern.  This fringe correction image is scaled to the same
+exposure time as the image to be corrected and then subtracted to remove
+the fringing.  Note that since the night sky lines are variable there
+may need to be an additional scaling applied.  Determining this scaling
+requires either an interactive display tool or a very clever task.
+Such tasks will also be added in the future.
+
+     The task to make a fringe correction image is \fBmkfringecor\fR.
+the sky background is determined in exactly the same way as the illumination
+pattern, in fact the same sky image may be used for both the sky
+illumination and for the fringe correction.  The task works consistently
+with the "mk" tasks in that the input images are processed first if needed
+and then the output correction image is produced with the specified name
+or replaces the input image if no output image is specified.
+As examples,
+
+.nf
+.ft L
+    cl> mkfringecor sky004 Fringe
+    cl> mkfringecor sky*.imh ""
+.ft R
+.fi
+.NH
+Demonstration
+.LP
+     A simple demonstration task is available.  To run this demonstration
+load the \fBccdtest\fR package; this is a subpackage of the main
+\fBccdred\fR package.  Then simply type
+
+.ft L
+	cl> demo
+.ft R
+
+The demonstration will then create some artificial CCD data and reduce
+them giving descriptive comments as it goes along.  This demonstration uses
+the "playback" facility of the command language and is actually substituting
+it's own commands for terminal input.  Initially you must type carriage return
+or space after each comment ending with "...".  If you wish to have the
+demonstration run completely automatically at it's own speed then type 'g'
+a the "..." prompt.  Thereafter, it will simple pause long enough to give
+you a chance to read the comments.  When the demo is finished you will
+need to remove the files created.  However, feel free to examine the reduced
+images, the log file, etc.  \fINote that the demonstration changes the
+setup parameters so be sure to run \fBsetinstrument\fI again and check
+the setup parameters.\fR
+.NH
+Summary
+.LP
+     The \fBccdred\fR package is very easy to use.  First load the package;
+it is in the \fBimred\fR package which is in the \fBnoao\fR package.
+If this is your first time reducing data from a particular instrument
+or if you have changed instruments then run \fBsetinstrument\fR.
+Set the processing parameters for the operations you want performed.
+If you need to combine calibration images to form a master calibration
+image use one of the combine tasks.  Spectroscopic flat fields may
+need to be processed first in order to remove the lamp spectrum.
+Finally, just type
+
+.ft L
+    cl> ccdproc *.imh&
+.ft R
+.SH
+References
+.LP
+     A general guide to using IRAF is \fIA User's Introduction to the IRAF
+Command Language\fR.  This document may be found in the IRAF documentation
+sets and is available from the National Optical Astronomy Observatories,
+Central Computer Services (NOAO-CCS).
+
+     A more detailed description of the \fBccdred\fR package including
+a discussion of the design and some of the algorithms see \fIThe IRAF
+CCD Reduction Package -- CCDRED\fR" by F. Valdes.  This paper is available
+from NOAO-CCS and appears in the proceedings of the Santa Cruz Summer
+Workshop in Astronomy and Astrophysics, \fIInstrumentation for Ground-Based
+Optical Astronomy: Present and Future\fR, edited by Lloyd B. Robinson and
+published by Springer-Verlag.
+
+     The task descriptions and supplementary documentation are available
+in printed form in the IRAF documentation sets, a special set
+containing documentation for just the \fBccdred\fR package, and on-line
+through the help task by typing
+
+.ft L
+    cl> help \fItopic\fR
+.ft R
+
+where \fItopic\fR is one of the following.
+
+.nf
+.ft L
+  badpiximage - Create a bad pixel mask image from a bad pixel file
+    ccdgroups - Group CCD images into image lists
+     ccdhedit - CCD image header editor
+      ccdlist - List CCD processing information
+      ccdproc - Process CCD images
+      ccdtest - CCD test and demonstration package
+      combine - Combine CCD images
+   cosmicrays - Detect and replace cosmic rays
+  darkcombine - Combine and process dark count images
+  flatcombine - Combine and process flat field images
+  mkfringecor - Make fringe correction images from sky images
+   mkillumcor - Make flat field illumination correction images
+  mkillumflat - Make illumination corrected flat fields
+     mkskycor - Make sky illumination correction images
+    mkskyflat - Make sky corrected flat field images
+setinstrument - Set instrument parameters
+  zerocombine - Combine and process zero level images
+
+          ADDITIONAL HELP TOPICS
+
+       ccdred - CCD image reduction package
+     ccdtypes - Description of the CCD image types
+   flatfields - Discussion of CCD flat field calibrations
+        guide - Introductory guide to using the CCDRED package
+  instruments - Instrument specific data files
+      subsets - Description of CCD subsets
+.ft R
+.fi
+
+Printed copies of the on-line help documentation may be made with the
+command
+
+.ft L
+    cl> help \fItopic\fL | lprint
+.ft R
+
+     In addition to the package documentation for \fBccdred\fR,
+\fBlongslit\fR, and \fBapextract\fR there may be specific guides for
+certain instruments.  These specific guides, called "cookbooks", give
+specific examples and parameter values for the CCD data.
diff --git a/noao/imred/quadred/src/quad/doc/instruments.hlp b/noao/imred/quadred/src/quad/doc/instruments.hlp
new file mode 100644
index 00000000..2b2c92f7
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/instruments.hlp
@@ -0,0 +1,248 @@
+.help instruments Jun87 noao.imred.ccdred
+
+.ih
+NAME
+instruments -- Instrument specific data files
+.ih
+DESCRIPTION
+The \fBccdred\fR package has been designed to accommodate many different
+instruments, detectors, and observatories.  This is done by having
+instrument specific data files.  Note that by instrument we mean a
+combination of detector, instrument, application, and observatory, so
+there might be several "instruments" associated with a particular CCD
+detector.  Creating and maintaining the instrument files is generally
+the responsibility of the support staff, though the user may create or
+copy and modify his/her own instrument/application specific files.  The
+task \fBsetinstrument\fR makes this information available to the user
+and package easily.
+
+There are three instrument data files, all of which are optional.  The
+package may be used without the instrument files but much of the
+convenience of the package, particularly with respect to using the CCD
+image types, will be lost.  The three files are an instrument image
+header translation file, an initialization task which mainly sets
+default task parameters, and a bad pixel file identifying the cosmic
+bad pixels in the detector.  These files are generally stored in a
+system data directory which is a subdirectory of the logical
+directory "ccddb$".  Each file has a root name which identifies the
+instrument.
+.sh
+1. Instrument Translation File
+The instrument translation file translates the parameter names used by
+the \fBccdred\fR pacakge into instrument specific parameters and also
+supplies instrument specific default values.  The package parameter
+\fIccdred.instrument\fR specifies this file to the package.  The task
+\fBsetinstrument\fR sets this parameter, though it can be set
+explicitly like any other parameter.  For the standard instrument
+translation file the root name is the instrument identification and the
+extension is "dat" ("*.dat" files are protected from being removed in a
+"stripped" system, i.e. when all nonessential files are removed).
+Private instrument files may be given any name desired.
+
+The instrument translation proceeds as follows.  When a package task needs
+a parameter for an image, for example "imagetyp", it looks in the instrument
+translation file.  If the file is not found or none is specified then the
+image header keyword that is requested has the same name.  If an
+instrument translation file is defined then the requested
+parameter is translated to an image header keyword, provided a translation
+entry is given.  If no translation is given the package name is used.  For
+example the package parameter "imagetyp" might be translated to "data-typ"
+(the old NOAO CCD keyword).  If the parameter is not found then the default
+value specified in the translation file, if present, is returned.  For recording
+parameter information in the header, such as processing flags, the
+translation is also used.  The default value has no meaning in this case.
+For example, if the flag specifying that the image has been corrected
+by a flat field is to be set then the package parameter name "flatcor"
+might be translated to "ff-flag".  If no translation is given then the
+new image header parameter is entered as "flatcor".
+
+The format of the translation file are lines consisting of the package
+parameter name, followed by the image header keyword, followed by the
+default value.  The first two fields are parameter names.  The fields
+are separated by whitespace (blanks and tabs).  String  default values
+containing blanks must be quoted.  An example is given below.
+
+.nf
+    exptime     itime
+    darktime    itime
+    imagetyp    data-typ
+    subset      f1pos
+    biassec     biassec    [411:431,2:573]
+    datasec     datasec    [14:385,2:573]
+
+    fixpix      bp-flag    0
+    overscan    bt-flag    0
+    zerocor     bi-flag    0
+    darkcor     dk-flag    0
+    flatcor     ff-flag    0
+    fringcor    fr-flag    0 
+.fi
+
+The first two lines translate the CCD image type, and the subset parameter
+without default values (see \fBccdtypes\fR and \fBsubsets\fR for more
+information).  The next two lines give the overscan bias strip
+section and the data section with default values for the instrument.
+Note that these parameters may be overridden in the task \fBccdproc\fR.
+The blank line is ignored.
+
+The next set of translations requires further discussion.  For processing
+flags the package assumes that the absence of a keyword means that the
+processing has not been done.  If processing is always to be done with
+the \fBCCDRED\fR package and no processing keywords are recorded in the raw data
+then these parameters should be absent (unless you don't like the names
+used by the package).  However, for compatibility with the original NOAO
+CCD images, which may be processed outside of IRAF and which use 0 as the
+no processing value, the processing flags are translated and the false values
+are indicated by the default values.
+
+In addition to the parameter name translations the translation file
+contains translations between the value of the image type parameter
+and the image types used by the package.  These lines
+consist of the image header type string as the first field (with quotes
+if there are blanks) and the image type as recognized by the package.  The
+following example will make this clearer.
+
+.nf
+	'OBJECT (0)'		object
+	'DARK (1)'		dark
+	'PROJECTOR FLAT (2)'	flat
+	'SKY FLAT (3)'		other
+	'COMPARISON LAMP (4)'	other
+	'BIAS (5)'		zero
+	'DOME FLAT (6)'		flat
+.fi
+
+The values of the image type strings in the header contain blanks so they
+are quoted.  Also the case of the strings is important.  Note that there
+are two types of flat field images and three types of object images.
+
+The CCD image types recognized by the package are:
+
+.nf
+	zero   - zero level image such as a bias or preflash
+	dark   - dark count image
+	flat   - flat field image
+	illum  - iillumination image such as a sky image
+	fringe - fringe correction image
+	object - object image
+.fi
+
+There may be more than one image type that maps to the same package
+type.  In particular other standard CCD image types, such as comparison
+spectra, multiple exposure, standard star, etc., should be mapped to
+object or other.  There may also be more than one type of flat field,
+i.e. dome flat, sky flat, and lamp flat.  For more on the CCD image
+types see \fBccdtypes\fR.
+
+The complete set of package parameters are given below.
+The package parameter names are generally the same as the
+standard image header keywords being adopted by NOAO.
+
+.nf
+	General Image Header and Default Parameters
+    ccdmean		darktime	exptime		fixfile
+    imagetyp		ncombine	biassec		subset
+    title		datasec
+
+	       CCDRED Processing Flags
+    ccdproc		darkcor		fixpix		flatcor
+    fringcor		illumcor	overscan	trim
+    zerocor
+
+	       CCDRED CCD Image Types
+    dark		flat		fringe		illum
+    none		object		unknown		zero
+.fi
+
+The translation mechanism described here may become more
+sophisticated in the future and a general IRAF system facility may be
+implemented eventually.  For the present the translation mechanism is
+quite simple.
+.sh
+2. Instrument Setup Script
+The task \fBsetinstrument\fR translates an instrument ID into a
+CL script in the instrument directory.  This script is then executed.
+Generally this script simply sets the task parameters for an
+instrument/application.  However, it could do anything else the support
+staff desires.  Below are the first few lines of a typical instrument setup
+script.
+
+.nf
+	ccdred.instrument = "ccddb$kpno/example.dat"
+	ccdred.pixeltype = "real"
+	ccdproc.fixpix = yes
+	ccdproc.overscan = yes
+	ccdproc.trim = yes
+	ccdproc.zerocor = no
+	ccdproc.darkcor = no
+	ccdproc.flatcor = yes
+	ccdproc.biassec = "[411:431,2:573]"
+	ccdproc.datasec = "[14:385,2:573]"
+.fi
+
+The instrument parameter should always be set unless there is no
+translation file for the instrument.  The \fBccdproc\fR parameters
+illustrate setting the appropriate processing flags for the
+instrument.  The overscan bias and trim data sections show an alternate
+method of setting these instrument specific parameters.  They may be
+set in the setup script in which case they are given explicitly in the
+user parameter list for \fBccdproc\fR.  If the value is "image" then
+the parameters may be determined either through the default value in
+the instrument translation file, as illustrated in the previous
+section, or from the image header itself.
+
+The instrument setup script for setting default task parameters may be
+easily created by the support person as follows.  Set the package
+parameters using \fBeparam\fR or with CL statements.  Setting the
+parameters might involve testing.  When satisfied with the way the
+package is set then the parameters may be dumped to a setup script
+using the task \fBdparam\fR.  The final step is editing this script to
+delete unimportant and query parameters.  For example,
+
+.nf
+	cl> dparam ccdred >> file.cl
+	cl> dparam ccdproc >> file.cl
+	cl> dparam combine >> file.cl
+		...
+	cl> ed file.cl
+.fi
+.sh
+3. Instrument Bad Pixel File
+The bad pixel file describes the bad pixels, columns, and lines in the
+detector which are to be replaced by interpolation when processing the
+images.  This file is clearly detector specific.  The file consists of
+lines describing rectangular regions of the image.
+The regions are specified by four numbers giving the starting and ending
+columns followed by the starting and ending lines.  The starting and
+ending points may be the same to specify a single column or line.  The
+example below illustrates a bad pixel file.
+
+.nf
+	# RCA1 CCD untrimmed
+	25 25 1 512
+	108 108 1 512
+	302 302 403 512
+	1 512 70 70
+	245 246 312 315
+.fi
+
+If there is a comment line in the file containing the word "untrimmed"
+then the coordinates of the bad pixel regions apply to the original image.
+If the image has been trimmed and the bad pixels are replaced at a later
+stage then this word indicates that the trim region be determined from the
+image header and the necessary coordinate conversion made.  If the word
+"untrimmed" does not appear then the coordinates are assumed to apply to
+the image directly; i.e. the trimmed coordinates if the image has been
+trimmed or the original coordinates if the image has not been trimmed.
+The standard bad pixel files should always refer to the original, untrimmed
+coordinates.
+
+The first two bad pixel regions are complete bad columns (the image
+is 512 x 512), the next line is a partial bad column, the next line is
+a bad line, and the last line is a small bad region.  These files are
+easy to create, provided you have a good image to work from and a way
+to measure the positions with an image or graphics display.
+.ih
+SEE ALSO
+ccdtypes, subsets, setinstrument
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/mkfringecor.hlp b/noao/imred/quadred/src/quad/doc/mkfringecor.hlp
new file mode 100644
index 00000000..797f4d11
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/mkfringecor.hlp
@@ -0,0 +1,90 @@
+.help mkfringecor Feb88 noao.imred.ccdred
+.ih
+NAME
+mkfringecor -- Make fringe correction images from sky images
+.ih
+USAGE
+mkfringecor input output
+.ih
+PARAMETERS
+.ls input
+List of input images for making fringe correction images.
+.le
+.ls output
+List of output fringe correction images.  If none is
+specified or if the name is the same as the input image then the output
+image replaces the input image.
+.le
+.ls ccdtype = ""
+CCD image type to select from the input images.  If none is specified
+then all types are used.
+.le
+.ls xboxmin = 5, xboxmax = 0.25, yboxmin = 5, yboxmax = 0.25
+Minimum and maximum smoothing box size along the x and y axes.  The
+minimum box size is used at the edges and grows to the maximum size in
+the middle of the image.  This allows the smoothed image to better
+represent gradients at the edge of the image.  If a size is less then 1
+then it is interpreted as a fraction of the image size.  If a size is
+greater than or equal to 1 then it is the box size in pixels.  A size
+greater than the size of image selects a box equal to the size of the
+image.
+.le
+.ls clip = yes
+Clean the input images of objects?  If yes then a clipping algorithm is
+used to detect and exclude objects from the smoothing.
+.le
+.ls lowsigma = 2.5, highsigma = 2.5
+Sigma clipping thresholds above and below the smoothed background.
+.le
+.ls ccdproc (parameter set)
+CCD processing parameters.
+.le
+.ih
+DESCRIPTION
+The input blank sky images are automatically processed up through the
+iillumination correction before computing the fringe correction images.
+The fringe corrections are subset dependent.
+The slowly varying background is determined and subtracted leaving only
+the fringe pattern caused by the sky emission lines.  These fringe images
+are then scaled and subtracted from the observations by \fBccdproc\fR.
+The background is determined by heavily smoothing the image using a
+moving "boxcar" average.  The effects of the objects and fringes in the
+image is minimized by using a sigma clipping algorithm to detect and
+exclude them from the average.  Note, however, that objects left in the
+fringe image will affect the fringe corrected observations.  Any objects
+in the sky image should be removed using \fBskyreplace\fR (not yet
+available).
+
+The smoothing algorithm is a moving average over a two dimensional
+box.  The algorithm is unconvential in that the box size is not fixed.
+The box size is increased from the specified minimum at the edges to
+the maximum in the middle of the image.  This permits a better estimate
+of the background at the edges, while retaining the very large scale
+smoothing in the center of the image.  Note that the sophisticated
+tools of the \fBimages\fR package may be used for smoothing but this
+requires more of the user and, for the more sophisticated smoothing
+algorithms such as surface fitting, more processing time.
+
+To minimize the effects of the fringes and any objects in the blank sky
+calibration images a sigma clipping algorithm is used to detect and
+exclude features from the background.  This is done by computing the
+rms of the image lines relative to the smoothed background and
+excluding points exceeding the specified threshold factors times the
+rms.  This is done before each image line is added to the moving
+average, except for the first few lines where an iterative process is
+used.
+.ih
+EXAMPLES
+1. The two examples below make an fringe correction image from a blank
+sky image, "sky017".  In the first example a separate fringe
+image is created and in the second the fringe image replaces the
+sky image.
+
+.nf
+    cl> mkskycor sky017 Fringe
+    cl> mkskycor sky017 frg017
+.fi
+.ih
+SEE ALSO
+ccdproc
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/mkillumcor.hlp b/noao/imred/quadred/src/quad/doc/mkillumcor.hlp
new file mode 100644
index 00000000..0effd7a2
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/mkillumcor.hlp
@@ -0,0 +1,92 @@
+.help mkillumcor Oct88 noao.imred.ccdred
+.ih
+NAME
+mkillumcor -- Make flat field iillumination correction images
+.ih
+USAGE
+mkillumcor input output
+.ih
+PARAMETERS
+.ls input
+List of input images for making flat field iillumination correction images.
+.le
+.ls output
+List of output flat field iillumination correction images.  If none is
+specified or if the name is the same as the input image then the output
+image replaces the input image.
+.le
+.ls ccdtype = "flat"
+CCD image type to select from the input images.  If none is specified
+then all types are used.
+.le
+.ls xboxmin = 5, xboxmax = 0.25, yboxmin = 5, yboxmax = 0.25
+Minimum and maximum smoothing box size along the x and y axes.  The
+minimum box size is used at the edges and grows to the maximum size in
+the middle of the image.  This allows the smoothed image to better
+represent gradients at the edge of the image.  If a size is less then 1
+then it is interpreted as a fraction of the image size.  If a size is
+greater than or equal to 1 then it is the box size in pixels.  A size
+greater than the size of image selects a box equal to the size of the
+image.
+.le
+.ls clip = yes
+Clean the input images of objects?  If yes then a clipping algorithm is
+used to detect and exclude deviant points from the smoothing.
+.le
+.ls lowsigma = 2.5, highsigma = 2.5
+Sigma clipping thresholds above and below the smoothed iillumination.
+.le
+.ls divbyzero = 1.
+The iillumination correction is the inverse of the smoothed flat field.
+This may produce division by zero.  A warning is given if division
+by zero takes place and the result (the iillumination correction value)
+is replaced by the value of this parameter.
+.le
+.ls ccdproc (parameter set)
+CCD processing parameters.
+.le
+.ih
+DESCRIPTION
+First, the input flat field images are automatically processed if
+needed.  Then, the large scale iillumination pattern of the images is
+determined by heavily smoothing them using a moving "boxcar" average.
+The iillumination correction, the inverse of the iillumination pattern,
+is applied by \fBccdproc\fR to CCD images to remove the iillumination
+pattern introduced by the flat field.  The combination of the flat
+field calibration and the iillumination correction based on the flat
+field is equivalent to removing the iillumination from the flat field
+(see \fBmkillumflat\fR).  This two step calibration is generally used
+when the observations have been previously flat field calibrated.  This
+task is closely related to \fBmkskycor\fR which determines the
+iillumination correction from a blank sky image; this is preferable to
+using the iillumination from the flat field as it corrects for the
+residual iillumination error.  For a general discussion of the options
+for flat fields and iillumination corrections see \fBflatfields\fR.
+
+The smoothing algorithm is a moving average over a two dimensional
+box.  The algorithm is unconvential in that the box size is not fixed.
+The box size is increased from the specified minimum at the edges to
+the maximum in the middle of the image.  This permits a better estimate
+of the background at the edges, while retaining the very large scale
+smoothing in the center of the image.  Note that the sophisticated
+tools of the \fBimages\fR package may be used for smoothing but this
+requires more of the user and, for the more sophisticated smoothing
+algorithms such as surface fitting, more processing time.
+
+To minimize the effects of bad pixels a sigma clipping algorithm is
+used to detect and reject these pixels from the iillumination.  This is
+done by computing the rms of the image lines relative to the smoothed
+iillumination and excluding points exceeding the specified threshold
+factors times the rms.  This is done before each image line is added to
+the moving average, except for the first few lines where an iterative
+process is used.
+.ih
+EXAMPLES
+1. The example below makes an iillumination correction image from the
+flat field image, "flat017".
+
+    cl> mkillumcor flat017 Illum
+.ih
+SEE ALSO
+ccdproc, flatfields, mkillumflat, mkskycor, mkskyflat
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/mkillumflat.hlp b/noao/imred/quadred/src/quad/doc/mkillumflat.hlp
new file mode 100644
index 00000000..8288fb85
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/mkillumflat.hlp
@@ -0,0 +1,101 @@
+.help mkillumflat Oct88 noao.imred.ccdred
+.ih
+NAME
+mkillumflat -- Make illumination corrected flat fields
+.ih
+USAGE
+mkillumflat input output
+.ih
+PARAMETERS
+.ls input
+List of input flat field images to be illumination corrected.
+.le
+.ls output
+List of output illumination corrected flat field images.
+If none is specified or if the name is the same as the
+input image then the output image replaces the input image.
+.le
+.ls ccdtype = "flat"
+CCD image type to select from the input images.
+.le
+.ls xboxmin = 5, xboxmax = 0.25, yboxmin = 5, yboxmax = 0.25
+Minimum and maximum smoothing box size along the x and y axes.  The
+minimum box size is used at the edges and grows to the maximum size in
+the middle of the image.  This allows the smoothed image to better
+represent gradients at the edge of the image.  If a size is less then 1
+then it is interpreted as a fraction of the image size.  If a size is
+greater than or equal to 1 then it is the box size in pixels.  A size
+greater than the size of image selects a box equal to the size of the
+image.
+.le
+.ls clip = yes
+Clean the input images of objects?  If yes then a clipping algorithm is
+used to detect and exclude objects from the smoothing.
+.le
+.ls lowsigma = 2.5, highsigma = 2.5
+Sigma clipping thresholds above and below the smoothed illumination.
+.le
+.ls divbyzero = 1.
+The illumination flat field is the ratio of the flat field to a
+smoothed flat field.  This may produce division by zero.  A warning is
+given if division by zero takes place and the result (the illumination
+corrected flat field value) is replaced by the value of this
+parameter.
+.le
+.ls ccdproc (parameter set)
+CCD processing parameters.
+.le
+.ih
+DESCRIPTION
+First, the input flat field images are processed as needed.  Then the
+large scale illumination pattern of the images is removed.  The
+illumination pattern is determined by heavily smoothing the image using
+a moving "boxcar" average.  The output image is the ratio of the input
+image to the illumination pattern.  The illumination pattern is
+normalized by its mean to preserve the mean level of the input image.
+
+When this task is applied to flat field images only the small scale
+response effects are retained.  This is appropriate if the flat field
+images have illumination effects which differ from the astronomical
+images and blank sky images are not available for creating sky
+corrected flat fields.  When a high quality blank sky image is
+available the related task \fBmkskyflat\fR should be used.  Note that
+the illumination correction, whether from the flat field or a sky
+image, may be applied as a separate step by using the task
+\fBmkillumcor\fR or \fBmkskycor\fR and applying the illumination
+correction as a separate operation in \fBccdproc\fR.  However, creating
+an illumination corrected flat field image before processing is more
+efficient since one less operation per image processed is needed.  For
+more discussion about flat fields and illumination corrections see
+\fBflatfields\fR.
+
+The smoothing algorithm is a moving average over a two dimensional
+box.  The algorithm is unconvential in that the box size is not fixed.
+The box size is increased from the specified minimum at the edges to
+the maximum in the middle of the image.  This permits a better estimate
+of the background at the edges, while retaining the very large scale
+smoothing in the center of the image.  Note that the sophisticated
+tools of the \fBimages\fR package may be used for smoothing but this
+requires more of the user and, for the more sophisticated smoothing
+algorithms such as surface fitting, more processing time.
+
+To minimize the effects of bad pixels a sigma clipping algorithm is
+used to detect and reject these pixels from the illumination.  This is
+done by computing the rms of the image lines relative to the smoothed
+illumination and excluding points exceeding the specified threshold
+factors times the rms.  This is done before each image line is added to
+the moving average, except for the first few lines where an iterative
+process is used.
+.ih
+EXAMPLES
+1. Two examples in which a new image is created and in which the
+input flat fields are corrected in place are:
+
+.nf
+    cl> mkllumflat flat004 FlatV
+    cl> mkillumflat flat* ""
+.fi
+.ih
+SEE ALSO
+ccdproc, flatfields, mkfringecor, mkillumcor, mkskycor, mkskyflat
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/mkskycor.hlp b/noao/imred/quadred/src/quad/doc/mkskycor.hlp
new file mode 100644
index 00000000..15cfacf6
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/mkskycor.hlp
@@ -0,0 +1,103 @@
+.help mkskycor Feb88 noao.imred.ccdred
+.ih
+NAME
+mkskycor -- Make sky iillumination correction images
+.ih
+USAGE
+mkskycor input output
+.ih
+PARAMETERS
+.ls input
+List of input images for making sky iillumination correction images.
+.le
+.ls output
+List of output flat field iillumination correction images.  If none is
+specified or if the name is the same as the input image then the output
+image replaces the input image.
+.le
+.ls ccdtype = ""
+CCD image type to select from the input images.  If none is specified
+then all types are used.
+.le
+.ls xboxmin = 5, xboxmax = 0.25, yboxmin = 5, yboxmax = 0.25
+Minimum and maximum smoothing box size along the x and y axes.  The
+minimum box size is used at the edges and grows to the maximum size in
+the middle of the image.  This allows the smoothed image to better
+represent gradients at the edge of the image.  If a size is less then 1
+then it is interpreted as a fraction of the image size.  If a size is
+greater than or equal to 1 then it is the box size in pixels.  A size
+greater than the size of image selects a box equal to the size of the
+image.
+.le
+.ls clip = yes
+Clean the input images of objects?  If yes then a clipping algorithm is
+used to detect and exclude objects from the smoothing.
+.le
+.ls lowsigma = 2.5, highsigma = 2.5
+Sigma clipping thresholds above and below the smoothed iillumination.
+.le
+.ls ccdproc (parameter set)
+CCD processing parameters.
+.le
+.ih
+DESCRIPTION
+The large scale iillumination pattern of the input images, generally
+blank sky calibration images, is determined by heavily smoothing
+the image using a moving "boxcar" average.  The effects of objects in
+the image may be minimized by using a sigma clipping algorithm to
+detect and exclude the objects from the average.  This
+iillumination image is applied by \fBccdproc\fR to CCD images to remove
+the iillumination pattern.
+
+The input images are automatically processed up through flat field
+calibration before computing the iillumination.  The iillumination
+correction is that needed to make the processed images flat
+over large scales.  The input images are generally blank sky calibration
+images which have the same iillumination and instrumental effects
+as the object observations.  Object images may be used but removal
+of the objects may not be very good; particularly large, bright objects.
+For further discussion of flat fields and iillumination corrections
+see \fBflatfields\fR.
+
+You will notice that when you process images with an iillumination
+correction you are dividing each image by a flat field calibration and
+an iillumination correction.  If the iillumination corrections are not
+done as a later step but at the same time as the rest of the processing
+one will get the same calibration by multiplying the flat field by the
+iillumination correction and using this product alone as the flat
+field.  This approach has the advantage of one less calibration image
+and two less computations (scaling and dividing the iillumination
+correction).  Such an image, called a \fIsky flat\fR, may be created by
+\fBmkskyflat\fR as an alternative to this task.
+
+The smoothing algorithm is a moving average over a two dimensional
+box.  The algorithm is unconvential in that the box size is not fixed.
+The box size is increased from the specified minimum at the edges to
+the maximum in the middle of the image.  This permits a better estimate
+of the background at the edges, while retaining the very large scale
+smoothing in the center of the image.  Note that the sophisticated
+tools of the \fBimages\fR package may be used for smoothing but this
+requires more of the user and, for the more sophisticated smoothing
+algorithms such as surface fitting, more processing time.
+
+Blank sky images may not be completely blank so a sigma clipping
+algorithm may be used to detect and exclude objects from the
+iillumination pattern.  This is done by computing the rms of the image
+lines relative to the smoothed background and excluding points
+exceeding the specified threshold factors times the rms.  This is done
+before each image line is added to the moving average, except for the
+first few lines where an iterative process is used.
+.ih
+EXAMPLES
+1. The two examples below make an iillumination image from a blank sky image,
+"sky017".  In the first example a separate iillumination image is created
+and in the second the iillumination image replaces the sky image.
+
+.nf
+    cl> mkskycor sky017 Illum
+    cl> mkskycor sky017 sky017
+.fi
+.ih
+SEE ALSO
+ccdproc, flatfields, mkillumcor, mkillumflat, mkskyflat
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/mkskyflat.hlp b/noao/imred/quadred/src/quad/doc/mkskyflat.hlp
new file mode 100644
index 00000000..3d9ac1ca
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/mkskyflat.hlp
@@ -0,0 +1,111 @@
+.help mkskyflat Feb88 noao.imred.ccdred
+.ih
+NAME
+mkskyflat -- Make sky corrected flat field images
+.ih
+USAGE
+mkskyflat input output
+.ih
+PARAMETERS
+.ls input
+List of blank sky images to be used to create sky corrected flat field
+calibration images.
+.le
+.ls output
+List of output sky corrected flat field calibration images (called
+sky flats).  If none is specified or if the name is the same as the
+input image then the output image replaces the input image.
+.le
+.le
+.ls ccdtype = ""
+CCD image type to select from the input images.
+.le
+.ls xboxmin = 5, xboxmax = 0.25, yboxmin = 5, yboxmax = 0.25
+Minimum and maximum smoothing box size along the x and y axes.  The
+minimum box size is used at the edges and grows to the maximum size in
+the middle of the image.  This allows the smoothed image to better
+represent gradients at the edge of the image.  If a size is less then 1
+then it is interpreted as a fraction of the image size.  If a size is
+greater than or equal to 1 then it is the box size in pixels.  A size
+greater than the size of image selects a box equal to the size of the
+image.
+.le
+.ls clip = yes
+Clean the input images of objects?  If yes then a clipping algorithm is
+used to detect and exclude objects from the smoothing.
+.le
+.ls lowsigma = 2.5, highsigma = 2.5
+Sigma clipping thresholds above and below the smoothed iillumination.
+.le
+.ls ccdproc (pset)
+CCD processing parameter set.
+.le
+.ih
+DESCRIPTION
+A sky corrected flat field calibration image, called a sky flat, is a
+flat field that when applied to observations of the sky have no large
+scale gradients.  Flat field images are generally obtained by exposures
+to lamps either illuminating the telescope field or a surface in the dome
+at which the telescope is pointed.  Because the detector is not illuminated
+in the same way as an observation of the sky there may be large
+scale iillumination patterns introduced into the observations with such
+a flat field.  To correct this type of flat field a blank sky observation
+(which has been divided by the original flat field) is heavily smoothed
+to remove the noise leaving only the residual large scale iillumination
+pattern.  This iillumination pattern is divided into the original flat
+field to remove this residual.
+
+The advantage of creating a sky flat field is that when processing
+the observations no additional operations are required.  However,
+if the observations have already been processed with the original
+flat field then the residual iillumination pattern of blank sky
+calibration images may be created as an iillumination correction
+to be applied by \fBccdproc\fR.  Such a correction is created by the
+task \fBmkskycor\fR.  If a good blank sky image is not
+available then it may be desirable to remove the iillumination pattern
+of the flat field image using \fBmkillumflat\fR or \fBmkillumcor\fR
+provided the sky observations are truly uniformly illuminated.
+For more on flat fields and iillumination corrections see \fBflatfields\fR.
+
+The input, blank sky images are first processed, based on the
+\fBccdproc\fR parameters, if needed.  These parameters also determine
+the flat field image to be used in making the sky flat.  The residual
+iillumination pattern is determined by heavily smoothing the image using
+a moving "boxcar" average.  The effects of objects in the input image
+may be minimized by using a sigma clipping algorithm to detect and
+exclude the objects from the average.  The output image is ratio of the
+flat field image, for the same subset as the input image, to the
+residual iillumination pattern determined from the processed blank sky
+input image.  The iillumination pattern is normalized by its mean to
+preserve the mean level of the flat field image.
+
+The smoothing algorithm is a moving average over a two dimensional
+box.  The algorithm is unconvential in that the box size is not fixed.
+The box size is increased from the specified minimum at the edges to
+the maximum in the middle of the image.  This permits a better estimate
+of the background at the edges, while retaining the very large scale
+smoothing in the center of the image.  Note that the sophisticated
+tools of the \fBimages\fR package may be used for smoothing but this
+requires more of the user and, for the more sophisticated smoothing
+algorithms such as surface fitting, more processing time.
+
+Blank sky images may not be completely blank so a sigma clipping
+algorithm may be used to detect and exclude objects from the
+iillumination pattern.  This is done by computing the rms of the image
+lines relative to the smoothed background and excluding points
+exceeding the specified threshold factors times the rms.  This is done
+before each image line is added to the moving average, except for the
+first few lines where an iterative process is used.
+.ih
+EXAMPLES
+1. Two examples in which a new image is created and in which the
+input sky images are converted to sky flats are:
+
+.nf
+    cl> mkskyflat sky004 Skyflat
+    cl> mkskyflat sky* ""
+.fi
+.ih
+SEE ALSO
+ccdproc, flatfields, mkfringecor, mkillumcor, mkillumflat, mkskycor
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/quad.hlp b/noao/imred/quadred/src/quad/doc/quad.hlp
new file mode 100644
index 00000000..7f8754ee
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/quad.hlp
@@ -0,0 +1,121 @@
+.help package Sep93 arcon.quad
+.ih
+NAME
+quad -- reduction package for CCD images obtained with Arcon
+
+.ih
+USAGE
+quad
+
+This package \fBmust\fR be used in place of \fBccdred\fR for the first steps
+(overscan correction and trimming) of multi-readout (quad or dual) images.
+Either package can be used for the subsequent stages, and for the complete
+reduction of single readout images.
+
+.ih
+PARAMETERS
+.ls pixeltype = "real real"
+Output pixel datatype and calculation datatype.  When images are processed
+or created the output pixel datatype is determined by this parameter.
+The allowed types are "short" for short integer, and "real" for real
+floating point.  The calculation datatypes are also short and real with a
+default of real if none is specified. Note that Arcon generates images of type
+"ushort" (unsigned 16-bit integers). In general both the output and calculation
+types should, therefore, be set to "real" to avoid truncation and wrap
+around errors, although this means that the reduced images will occupy twice as
+much disk space.
+.le
+.ls verbose = no
+Print log information to the standard output?
+.le
+.ls logfile = "logfile"
+Text log file.  If no filename is specified then no log file is kept.
+.le
+.ls plotfile = ""
+Log metacode plot file for the overscan bias vector fits.  If
+no filename is specified then no metacode plot file is kept.
+.le
+.ls backup = ""
+Backup prefix for backup images.  If no prefix is specified then no backup
+images are kept when processing.  If specified then the backup image
+has the specified prefix.
+.le
+.ls instrument = ""
+CCD instrument translation file.  This is usually set with \fBsetinstrument\fR.
+.le
+.ls ssfile = "subsets"
+Subset translation file used to define the subset identifier.  See
+\fBsubsets\fR for more.
+.le
+.ls graphics = "stdgraph"
+Interactive graphics output device when fitting the overscan bias vector.
+.le
+.ls cursor = ""
+Graphics cursor input.  The default is the standard graphics cursor.
+.le
+.ls version = "Version 2.0 - Sept 93"
+Package version.
+.le
+.ih
+DESCRIPTION
+The \fBquad\fR package contains all the basic tasks necessary for the
+reduction of CCD data obtained with Arcon. With Arcon images are often readout
+using four ("quad") or two ("dual") amplifiers in order to reduce readout time.
+The \fBquad\fR package includes the few special tasks needed to deal with such
+multi-readout data, as well as many standard tasks taken directly from the 
+\fBccdred\fR package. The \fBquad\fR package must be used for the first
+reduction steps, overscan correction and trimming, of multi-readout images;
+subsequent steps can be performed using \fBquad\fR or \fBccdred\fR. Either
+package can be used for the complete reduction of conventional single readout
+CCD images.
+
+The \fBquad\fR package also contains the tasks \fBqstatistics\fR and 
+\fBqhistogram\fR which can be used for examining raw multi-readout images. 
+
+The \fBquad\fR package task itself has several parameters which are common to 
+many of the tasks in the package.  When images are processed or new image are
+created the output pixel datatype is that specified by the parameter
+\fBpixeltype\fR. Note that CCD processing replaces the original image by the
+processed image so the pixel type of the CCD images may change during
+processing.  It is unlikely that real images will be processed to short images
+but the reverse is quite likely.  Processing images from short to real
+pixel datatypes will generally increase the amount of disk space
+required (a factor of 2 on most computers).
+
+The tasks produce log output which may be printed on the standard
+output (the terminal unless redirected) and appended to a file.  The
+parameter \fIverbose\fR determines whether processing information
+is printed.  This may be desirable initially, but when using background
+jobs the verbose output should be turned off.  The user may look at
+the end of the log file (for example with \fBtail\fR) to determine
+the status of the processing.
+
+The package was designed to work with data from many different observatories
+and instruments.  In order to accomplish this an instrument translation
+file is used to define a mapping between the package parameters and
+the particular image header format.  The instrument translation file
+is specified to the package by the parameter \fIinstrument\fR.  This
+parameter is generally set by the task \fBsetinstrument\fR.  The other
+file used is a subset file.  This is generally created and maintained
+by the package and the user need not do anything.  For more sophisticated
+users see \fBinstruments\fR and \fBsubsets\fR.
+
+The package has very little graphics
+output.  The exception is the overscan bias subtraction.  The bias
+vector is logged in the metacode plot file if given.  The plot file
+may be examined with the tasks in the \fBplot\fR package such as
+\fBgkimosaic\fR.  When interactively fitting the overscan vector
+the graphics input and output devices must be specified.  The defaults
+should apply in most cases.
+
+Because processing replaces the input image by the processed image it
+may be desired to save the original image.  This may be done by
+specifying a backup prefix with the parameter \fIbackup\fR.  For
+example, if the prefix is "orig" and the image is "ccd001", the backup
+image will be "origccd001".  The prefix may be a directory but if so it must
+end with '/' or '$' (for logical directories) and the directory must already
+exist.
+.ih
+SEE ALSO
+instruments, setinstrument, subsets
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/quadman.hlp b/noao/imred/quadred/src/quad/doc/quadman.hlp
new file mode 100644
index 00000000..55bfe10d
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/quadman.hlp
@@ -0,0 +1,1330 @@
+.help quadman Sep93 Version-0.0
+.ce
+\fIV-ARCON. Reduction of CCD data obtained with Arcon\fR
+
+.nf
+     1. Introduction
+     2. Getting the Data
+     3. Reducing the Data
+          3.1   Introduction
+          3.2   Reading the Data from Tape
+          3.3   Setting Up the Translation File
+                3.3.1  Setinstrument for CCD Used
+                3.3.2  Setting the Subsets Parameter and Preparations 
+          3.4   Preparing Individual Calibration Frames
+	  3.5   Processing the calibration frames
+          3.6   Preparing a Final Flat Field
+          3.7   Processing the Images
+          3.8   Creating the Bad Pixel File
+          3.9   Writing the Data to Tape
+
+
+
+
+
+
+					A thinly disguised version of CCDMAN
+
+
+						     Lisa Wells
+
+                                                    Mario Hamuy
+
+						 September 30, 1993
+.fi
+.bp
+.ls \fI1. Introduction\fR
+
+CCDRED is a package in IRAF used for CCD data reduction. It is primarily used
+for CCD imaging although various aspects are also used for spectral reduction.
+This document is intended as a guideline to reducing direct CCD images using
+IRAF. If you are reducing spectra, see Section III or IV of
+this manual. If you do not have experience using IRAF we suggest that
+you start by
+reading "An Introduction to IRAF" which will give you a general idea of IRAF
+structure as well as a few fundamental tools. If you plan to use this package
+extensively, there is a demo on the computer as well which will run through
+the reduction process interactively. Once you login and enter IRAF
+type the following:
+
+.nf
+      cl> noao
+      no> imred
+      im> ccdred
+      cc> ccdtest
+      cc>
+.fi
+
+The cc> prompt indicates the package has been loaded. 'ccdtest' contains several
+tasks one of which is 'demo'. Now type 'demo' and follow the instructions. It
+will prompt you, from time to time, to continue to the next section.
+
+The examples shown here are just that, examples. The user must decide
+upon the reduction procedure, naming, convention, etc..., appropriate for
+his/her own data and use the cookbook and examples as guidelines only. The
+examples are shown with prompts, for the package containing the tasks (do not
+type the prompts, of course). It is strongly recommended that you perform an
+'lpar' on every task immediately before using it, unless you are familiar with
+all of its parameters. This is not always shown in the examples, but is normal
+practice even among seasoned IRAF users.
+
+IRAF uses two conventions that you should always keep in mind. 
+First, images consist of lines and columns (not rows and columns). Keep in mind
+that the mountain Forth systems for the CCDs are zero-indexed and use rows and
+lines. IRAF uses one-indexed coordinates for images (see figure 1). Second,
+the "order" of a function is the number of independent coefficients for a
+polynomial, or the number of intervals for a spline curve. For example, a cubic
+(third-degree) polynomial is described as "order=4" (four coefficients).
+
+If you require personal assistance in your reductions please contact
+either Mauricio Navarrete or Nelson Saavedra on Tololo (ex 422),
+or Mario Hamuy(ex 210) in La Serena.
+.le
+.bp
+.ls \fI2. Getting the Data\fR
+
+Many observers often get confused about the number and kind of calibration
+frames that must be taken to properly reduce their data. During a whole
+run you should get the following:
+
+1) Bias frames for each night are essential no matter what setup and chip
+you are using. 20-30 of these should be taken and combined.
+
+2) Dome flats should be taken for each filter you are using. Preferably
+this should be done every day, but you can get by with just one per run,
+as long as you take a sufficient number of them, say 20-30.
+
+3) Twilight sky flats are necessary if you want to do photometry to better
+than 2%-3%, if you are doing surface photometry of extended objects,
+or if sky subtraction is critical. We suggest that everyone take sky flats
+since it is a good check of your dome flat iillumination. For some CCDs it
+is better to use a sky flat to flatten your objects and this may depend
+upon the filters being used.
+It was found at the 0.9-m and 1.5-m telescopes that
+sky flats do better in flattening your
+images in the U and B filters. It is therefore
+suggested that you concentrate on getting many U and B sky flats (10 or more)
+since you will probably process your data using them.
+These will be combined in the first steps of the reduction.
+
+4) Darks are worth taking to check that things are working but dark correction
+is not necessary for any of the CCDs now used at CTIO. The dark current
+should be <10 e-/hour/pixel, if greater, then something is wrong and you
+should get it fixed.
+
+5) Photometric standard stars should be taken when needed and as many as
+necessary (>20) to properly calibrate your objects.
+
+You should refer to the instrument manual for more details. We
+suggest that you start taking your calibration frames early in the afternoon so
+that you have enough time left for supper. It is important to note on your
+calibration frames, the positions of bad pixels and then avoid observing
+your objects on these regions of the CCD, especially if you plan to do
+photometry. At the end of the reductions, you may wish to use a bad pixel map
+to correct the bad pixels. This will be discussed later (section 3.8)
+in more detail.
+.le
+.bp
+.ce
+\fI3. Reducing the Data\fR
+.ls \fI3.1 Introduction\fR
+
+A full reduction of CCD data requires the following operations (see the
+flow diagram on the next page):
+
+.nf
+      1) Combine the bias, flats and darks.
+      2) Fit and subtract a readout bias given by the overscan strip.
+      3) Trim the image of overscan strip and border rows and columns.
+      4) Subtract the dark, if appropriate.
+      5) Prepare a final flat.
+      6) Divide by the flat field.
+      7) Fix the bad pixels in all the images.
+      8) Fringing corrections may be done at the end.
+.fi
+
+The most general processing, described in this manual, consists of
+overscan subtracting, trimming, bias subtracting, dark subtracting,
+and flat fielding your data. Although dark subtraction is rarely used,
+it is included in this example for generality.
+
+Individual bias, darks, dome and sky flats must be properly combined to give
+good signal to noise calibration frames and to remove cosmic rays. The
+algorithm used to combine the images must have 10 or more frames to do a good
+job of cleaning the cosmic rays. IRAF offers several algorithms for combining
+the individual frames. You should always carefully inspect all the individual
+frames, and the final image to check
+for potential problems.
+
+Having obtained the combined calibration images you should flatten your sky flat
+using the dome flat and examine the result for any significant iillumination 
+variation. If these variations are significant they may be fit in order to
+correct your dome flat. 
+Fringing corrections may be
+applied. This should be done separately. This is only needed for the RCA
+chips at the 4 meter PF/CCD and the TI chips in the I band. We do not
+currently support this but direction can be given as to what might possibly
+work.
+
+At this level
+the images should be finished except for fixing any bad pixels that may not
+have been taken care of in the flat fielding. Once this is done you may
+do photometry. A photometry manual is available to do your analysis,
+see section VI of this manual, which describe the use of the
+aperture photometry routines in IRAF and the transformation from
+instrumental to standard magnitudes. There is also a manual which was
+written by the IRAF group in Tucson which is a good guide; "A User's
+Guide to Stellar CCD Photometry with IRAF".
+.bp
+.nf
+
+                   ==========================
+                   =      Set Instrument    =
+                   =  and Translation File  =
+                   ==========================
+                             *****
+                              ***
+                               *
+               ==================================
+               =  Combining Calibration Frames  =
+               =    and Removing Cosmic Rays    =
+               ==================================
+                             *****
+                              ***
+                               *
+		===============================
+		=          Processing         =
+		=      Calibration Frames     =
+		===============================
+			     *****
+			      ***
+			       *
+                ================================
+                =    Preparing a Flat Field    =
+                ================================
+                             *****
+                              ***
+                               *
+		   ==========================
+		   =  Processing the data   =
+		   ==========================
+			     *****
+			      ***
+			       *
+		   ==========================
+		   =   Fixing bad pixels    =
+		   ==========================
+			     *****
+			      ***
+			       *
+                   ==========================
+                   =   Fringe Corrections   =
+                   =       (optional)       =
+                   ==========================
+.fi
+.le
+.bp
+.ls \fI3.2 Reading the data from Tape\fR
+
+Load the 'dataio' package and allocate the appropriate tape drive:
+
+.nf
+      cl> dataio
+      da> alloc mta
+.fi
+
+If you wish to read fits files from an exabyte, use 'mtx' as the device
+designation. Now mount your tape on the tape drive and be sure you've
+removed the write ring. It is best to create a separate directory for
+each night. This is done using the command 'mkdir night1'. Now change
+to this directory by typing 'cd night1'. Read the data using the task
+'rfits'. You must specify the tape drive name, the list of files you wish
+to read and the "root" file name. If you transferred your data to the
+SUN using 'getpix' then you may wish to use the naming convention given
+to your files, in this case just set the parameter 'oldirafname' to yes.
+In choosing the root file name, it is usually a good idea to include a
+digit in the name to indicate the tape number (eg, "tape1" for the
+first tape; files would be called "tape10001, tape10002,.."); alternatively,
+an offset may be added (eg, offset=89 means the first files would be
+called "tape10090, tape10091,.." or 1+89, 2+89,..).
+
+.nf
+      da> epar rfits          (check the parameter list)
+      da> rfits mta 1-999 tape1
+.fi
+
+The file list "1-999" should more than cover the number of files on tape;
+the task will end gracefully at the end of the tape. When finished,
+rewind the tape and deallocate the drive,
+
+.nf
+      da> rew mta
+      da> dealloc mta
+.fi
+
+and remove your tape from the drive. We assume that you kept the old IRAF
+name given to your files throughout the rest of this manual.
+
+.nf
+                     \fIrfits\fR
+
+    fits_file = "mta"       FITS data source
+    file_list = "1-999"     File list
+    iraf_file = "tape1"     IRAF filename
+  (make_image = yes)        Create an IRAF image?
+ (long_header = no)         Print FITS header cards?
+(short_header = yes)        Print short header?
+    (datatype = "")         IRAF data type
+       (blank = 0.)         Blank value
+       (scale = yes)        Scale the data?
+ (oldirafname = no)         Use old IRAF name in place of iraf_file?
+      (offset = 0)          Tape file offset
+        (mode = "ql")           
+.fi
+.le
+.bp
+.ce
+\fI3.3 Setting Up the Translation File\fR
+.ls \fI3.3.1 Setinstrument for CCD Used\fR
+
+Start by loading the 'imred' and 'ccdred' packages.
+
+.nf
+      cl> noao
+      no> imred
+      im> ccdred
+      cc>
+.fi
+
+Because the 'ccdred' package was
+designed to work with data from many different observatories and instruments,
+an \fIinstrument translation file\fR is required to define a mapping
+between the package parameters and the particular image header format.
+An example of a translation file is shown on the next page.
+You must define a translation file using the task 'setinstrument'.
+Edit the parameters for the task 'setinstrument' according to the
+list given below and run it.
+The choices for instrument can be found in Appendix A. If the CCD you
+used is not listed, use the generic "ccd" or "cfccd" in the instrument
+parameter in the task.
+
+.nf
+      cc> epar setinstrument       (check the parameter list)
+      cc> setinstrument
+.fi
+
+The task will run and prompt you for the instrument ID (a "?" will list
+the possible choices). Answer 'cfccd' and the task will send you into 
+the parameter editing mode for
+the task 'ccdred'. It will automatically set the \fIinstrument\fR
+(translation) parameter
+so do not change it. It is a good idea while processing your calibration
+frames to save a copy of the unprocessed images. This will be done
+by the package 'ccdred' if you specify a prefix or subdirectory in the
+parameter 'backup'. In our example, the files will be saved with the prefix
+'B'. When you type 'ctrl-z' to exit you will then be sent to 'ccdproc'
+to edit its parameters. We will edit
+'ccdproc' later so don't worry about it for now.
+
+.nf
+               \fIsetinstrument parameters\fR
+
+   \fIinstrument\fR = "cfccd"     Instrument ID (type ? for a list)
+        (\fIsite\fR = "ctio")     Site ID
+   (\fIdirectory\fR = "ccddb$")   Instrument directory
+      (review = yes)        Review instrument parameters?
+        query = ""          Instrument ID (type q to quit)
+        (mode = "ql")           
+
+                 \fIccdred parameters\fR
+
+   (pixeltype = "real real") Output and calculation pixel datatypes
+     (verbose = no)         Print log information to the standard output?
+     (logfile = "ccdlog")   Text log file
+    (plotfile = "ccdplot")  Log metacode plot file
+      (\fIbackup\fR = "B")        Backup directory or prefix
+  (\fIinstrument\fR = "ccddb$ctio/cfccd.dat") CCD instrument file
+      (\fIssfile\fR = "subsets")  Subset translation file
+    (graphics = "stdgraph") Interactive graphics output device
+      (cursor = "")         Graphics cursor input
+     (version = "2: October 1987") 
+        (mode = "ql")           
+      ($nargs = 0)              
+
+.fi
+
+An example of the \fIinstrument translation file\fR follows.
+
+.nf
+
+          exptime exptime
+          darktime darktime
+          imagetyp imagetyp
+          subset filters
+          biassec biassec
+          datasec datasec
+	  trimsec trimsec
+          fixfile fixfile
+
+          fixpix                bp-flag 0
+          overscan              bt-flag 0
+          zerocor               bi-flag 0
+          darkcor               dk-flag 0
+          flatcor               ff-flag 0
+          fringcor              fr-flag 0
+
+          OBJECT		object
+          DARK			dark
+          "PROJECTOR FLAT"	flat
+          "SKY FLAT"		other
+          COMPARISON		other
+          BIAS			zero
+          "DOME FLAT"		flat
+          MASK			other
+.fi
+
+
+The instrument file consists of first, the IRAF parameter and its associated
+image header keyword from the objects. These header values may vary depending
+upon the instrument being used.
+The second section is the
+header flag section which is added to the object as it is being processed to
+mark that the operation has been done. Once an image is zero corrected, the
+keyword bi-flag parameter is added to the image header and set to '0' so that
+the process is not repeated later. The last section is the image-type 
+specification. This is used when the imagetyp parameter is read. The header
+value 'OBJECT' is translated to 'object', and a 'SKY FLAT' becomes 'other'.
+If you need to modify the translation file you may copy this file to your
+directory and change the appropriate parameters. If the name of the imagetype
+contains 2 words, then you must put quotes around the designation, for example,
+look at the 'SKY FLAT' line in the above file. Comparison arcs are not used
+in direct imaging and are not needed.
+
+Without the proper translation file, the task 'ccdlist' will give the following:
+
+.nf
+  cc> ccdlist *.imh
+
+  bias001.imh[400,420][short][unknown][]:median of 4 ave of 6 bias 
+  flat002.imh[400,420][short][unknown][]:median of 4 ave of 6 flat
+  flat003.imh[400,420][short][unknown][]:median of 4 ave of 6 flat
+  obj004.imh[400,420][short][unknown][]:IC 481  V-filter ........
+  obj005.imh[400,420][short][unknown][]:IC 481  B-filter.........
+         :	:	:	:	:	:	:	:
+  obj036.imh[400,420][short][unknown][]:Sky flat B-filter .......
+  obj037.imh[400,420][short][unknown][]:Sky flat V-filter .......
+         :	:	:	:	:	:	:	:
+.fi
+
+The [unknown] in the listing means that the frame type is unknown, ie, if
+it is a dark, flat, bias,... etc. The blank brackets should contain the
+filter type and will be taken care of in the next section.
+.le
+.bp
+.ls \fI3.3.2 Setting the Subsets Parameter and Preparing for Processing\fR
+
+The 'ccdred' package groups observations into subsets. The image header
+parameter used to identify the subsets is defined in the \fIinstrument
+translation file\fR. For example, to select subsets by the header parameter
+'filters' the instrument translation file would contain the line
+
+.nf
+     subset filters
+.fi
+
+Now do a 'ccdlist' and you should see the
+correct image type specified for each frame:
+
+.nf
+  cc> ccdlist *.imh
+
+  bias001.imh[400,420][short][zero][]:median of 4 ave of 6 bias
+  flat002.imh[400,420][short][flat][]:median of 4 ave of 6 flat
+  flat003.imh[400,420][short][flat][]:median of 4 ave of 6 flat
+  obj004.imh[400,420][short][object][]:IC 481  V-filter ......
+  obj005.imh[400,420][short][object][]:IC 481  B-filter.......
+	:          :        :        :        :    :       :
+	:          :        :        :        :    :       :
+  obj036.imh[400,420][short][object][]:Sky flat B-filter .....
+  obj037.imh[400,420][short][object][]:Sky flat V-filter .....
+	:          :        :        :        :    :       :
+.fi
+
+Doing this will create a file in your directory called 'subsets'. This is a
+file with a listing of the filter type read from the image header consisting
+of the combination of the upper and lower filter bolt positions. The flats
+were taken with a color balance filter so they have different values from the
+objects in the list. Therefore, you need to edit this file to set the filter
+types properly. The bias and dark were probably taken with a setting that
+corresponds to one of the filters, but it will be ignored. If however, the
+filter type set in the header corresponds to something other than a standard
+filter, set this to some arbitrary value, for example below it is assumed that
+the filter positions for the bias were '0 1', so this is set to '0'.
+
+.nf
+      cc> edit subsets
+.fi
+
+An example of the necessary changes is:
+
+.nf
+       \fISubsets Before     |        Subsets After\fR
+      '1 0'      1        |       '1 0'      U
+      '2 0'      2        |       '2 0'      B
+      '3 0'      3        |       '3 0'      V
+      '4 0'      4        |       '4 0'      R
+      '5 0'      5        |       '5 0'      I
+      '0 1'     01        |       '0 1'      0
+      '1 1'     11        |       '1 1'      U
+      '2 1'     21        |       '2 1'      B
+      '3 1'     31        |       '3 1'      V
+      '4 1'     41        |       '4 1'      R
+      '5 1'     51        |       '5 1'      I
+.fi
+
+If any of the parameters are not specified properly after doing 'ccdlist',
+then the translation file may be set up improperly. Consult
+Mauricio Navarrete, Nelson Saavedra, or Mario Hamuy.
+
+You must also specify the overscan and trim region.
+The overscan is the region to the far right of the image when plotting a line
+of the image (see figure 2a). The overscan region should be
+specified by the beginning and ending column followed by the beginning and
+ending line. This region should begin at least 5-10 pixels from the edge of
+the active region of the CCD. The correct position can be found by plotting
+several lines using ':l #1 #2' (#1 and #2 specify a range of lines to be
+averaged and plotted) in 'implot', and expanding the right side (see figure 2b).
+Notice the signal decays toward the right just the other side of the step with
+an e-folding distance of a few pixels. The overscan strip should begin in 3 to
+4 e-folding distances from the break. You want to fit this region all along
+the image so the range of lines should include everything. Be sure to write
+down these values so you don't forget them.
+
+The trim region is the section of the image to be kept after processing.
+Choose this area excluding the overscan region
+and any bad lines or columns at the edges of the image. Figures 2c and 2d show
+a plot of a line and column, respectively. They show the edges which should be
+trimmed from the image. Later (section 3.5)
+you will edit the parameters for 'ccdproc' and enter the overscan and trim
+section.
+
+The bad pixel file will be used after the images have been flattened. In many
+cases the flatfielding will correct the bad pixel regions also so it is best
+left until the end. If you specify the bad pixel file during the processing
+be aware that the corrections are done on the file first.
+.le
+.bp
+.ls \fI3.4 Preparing Individual Calibration Frames\fR
+
+If you have taken many calibration frames (bias, dome flats, darks
+and sky flats) that you wish to combine in order to remove cosmic
+rays, we suggest you to perform a combination of images separately for
+each night. In some cases, when the instrument response remains
+stable during your run, it is worth combining data from many nights,
+especially the darks and sky flats, to improve the signal-to-noise
+ratio. If you have already combined the data on the mountain skip
+over this section and go on to the next one.
+
+Most likely you used "getpix" to transfer your data from the LSI
+to the SUN so you have preserved the naming convention. This makes
+it very easy to combine your images.
+
+There are tasks which combine each type of object together. For the
+bias do an 'epar' on the 'zerocombine' task, and fill the parameters
+according to the list given below. We suggest selecting the 'avsigclip'
+rejection operation which applies a
+sigma clipping algorithm to each pixel to remove cosmic rays. This
+algorithm requires at least three input images (best with
+more than 10) to work effectively. According to your particular needs you may
+select other options to combine the data like minmax, ccdclip, etc.
+No scaling is performed on the biases.
+If your bias frames vary greatly, then there
+is something wrong with your setup. In this case, have someone check
+out the electronics.
+
+.nf
+      cc> epar zerocombine           (check the list given below)
+.fi
+
+Then combine the bias frames. Optionally you may add a '&' at the end
+of the command line to submit the task as a background job.
+
+.nf
+      cc> zerocombine bias*.imh output=zero1 &
+.fi
+
+Now, proceed with the combination of the darks.
+
+.nf
+      cc> epar darkcombine            (check the list given below)
+      cc> darkcombine dark*.imh output=dark1 &
+.fi
+
+Before combining the flat frames, you must
+find a region free of bad pixels to be used to scale the individual
+flat frames. The box should be chosen where there is signal.
+Once you have determined the position of the box, you
+should first run 'imstat' for all your images using this region.
+
+.nf
+      cc>  imstat flat*[200:250,300:330]
+
+      #          IMAGE             NPIX   MEAN   STDDEV  MIN   MAX
+      flat001.imh[200:250,300:330] 37901  5489.  1510.   678.  9020.
+      flat002.imh[200:250,300:330] 37901  5485.  1508.   694.  8484.
+      flat003.imh[200:250,300:330] 37901  5478.  1507.   691.  8472.
+      flat004.imh[200:250,300:330] 37901  5475.  1506.   671.  8397.
+      flat005.imh[200:250,300:330] 37901  5474.  1506.   659.  8540.
+      flat006.imh[200:250,300:330] 37901  5472.  1505.   663.  8422.
+      flat007.imh[200:250,300:330] 37901  5467.  1504.   655. 15513.
+      flat008.imh[200:250,300:330] 37901  5464.  1502.   673.  8471.
+      flat009.imh[200:250,300:330] 37901  5458.  1501.   684.  8503.
+.fi
+
+If the mean varies by a large amount, say greater than a few percent, then
+you should use the mode section for the scaling.
+In the example below the flats are combined with scaling.
+Enter this region in the 'statsec' parameter in the following format,
+
+.nf
+      [x1:x2,y1:y2]
+.fi
+      
+where the values x1 and x2 are the limits of the box in the x-axis, y1
+and y2 are the limits along the y-axis. This will only be
+used if 'median' is specified in the 'scale' parameter of the task
+'flatcombine'. In this example we have chosen to combine the individual
+flats using the 'ccdclip' option, which rejects pixels using the CCD noise
+parameters, namely the read-out-noise and the gain. You must enter these
+values in the parameters 'rdnoise' and 'gain' in 'flatcombine'. In this
+example we have entered a read-out-noise of 5 electrons, and a gain of
+2.5 electrons/ADU.
+
+.nf
+       cc> epar flatcombine          (check the list given below)
+.fi
+
+Proceed with the combination of the flats.
+
+.nf
+       cc> flatcombine flat.*imh output=flat1 &
+.fi
+
+If you have 3 or more sky flats, they may be combined in the same manner
+as the dome flats (change the 'ccdtype' parameter to 'other').
+
+.nf
+      cc> epar flatcombine        (check the list given below)
+      cc> flatcombine sky.*imh output=sky1 &
+.fi
+
+The output at this point is a set of images clean of cosmic rays called zero1,
+dark1, flat1, and sky1, where the 1 stands for the first night and the flats
+and skys end in their respective filter type ie, flat1U, flat1B,... Using the
+parameter subsets, the combination occurred for all the flats and skys of the
+same filter type (subset). We suggest that you examine these images, either by
+displaying, or imploting them. For example;
+
+.nf
+      cc> display zero1
+      cc> implot zero1
+.fi
+
+We suggest also to look at the logfile created by the package 'ccdred' in
+order to check that the images were properly combined by the same filter
+type.
+
+.nf
+      cc> page ccdlog
+.fi
+.bp
+
+.nf
+                         \fIzerocombine\fR
+
+        input = "bias*.imh"     List of zero level images to combine
+      (output = "zero1")        Output zero level name
+     (\fIcombine\fR = "average")      Type of combine operation
+      (\fIreject\fR = "avsigclip")    Type of rejection
+     (\fIccdtype\fR = "zero")         CCD image type to combine
+     (process = no)             Process images before combining?
+      (delete = no)             Delete input images after combining?
+     (clobber = no)             Clobber existing output image?
+       (\fIscale\fR = "none")         Image scaling
+     (statsec = "")             Image section for computing statistics
+        (nlow = 0)              minmax: Number of low pixels to reject
+       (nhigh = 1)              minmax: Number of high pixels to reject
+       (nkeep = 1)              Minimum to keep (pos) or maximum to reject
+       (mclip = yes)            Use median in sigma clipping algorithms?
+      (lsigma = 3.)             Lower sigma clipping factor
+      (hsigma = 3.)             Upper sigma clipping factor
+     (rdnoise = "0")            ccdclip: CCD readout noise (electrons)
+        (gain = "1")            ccdclip: CCD gain (electrons/DN)
+      (snoise = "0.")           ccdclip: Sensitivity noise (fraction)
+       (pclip = -0.5)           pclip: Percentile clipping parameter
+       (blank = 0.)             Value if there are no pixels
+        (mode = "ql")           
+
+                         \fIdarkcombine\fR
+
+        input = "dark.*imh"     List of dark images to combine
+      (output = "dark1")        Output flat field root name
+     (\fIcombine\fR = "average")      Type of combine operation
+      (\fIreject\fR = "avsigclip")    Type of rejection
+     (\fIccdtype\fR = "dark")         CCD image type to combine
+     (process = no)             Process images before combining?
+      (delete = no)             Delete input images after combining?
+     (clobber = no)             Clobber existing output image?
+       (\fIscale\fR = "exposure")     Image scaling
+     (statsec = "")             Image section for computing statistics
+        (nlow = 1)              minmax: Number of low pixels to reject
+       (nhigh = 1)              minmax: Number of high pixels to reject
+       (nkeep = 1)              Minimum to keep (pos) or maximum to reject
+       (mclip = yes)            Use median in sigma clipping algorithms?
+      (lsigma = 3.)             Lower sigma clipping factor
+      (hsigma = 3.)             Upper sigma clipping factor
+     (rdnoise = "0.")           ccdclip: CCD readout noise (electrons)
+        (gain = "1.")           ccdclip: CCD gain (electrons/DN)
+      (snoise = "0.")           ccdclip: Sensitivity noise (fraction)
+       (pclip = -0.5)           pclip: Percentile clipping parameter
+       (blank = 0.)             Value if there are no pixels
+        (mode = "ql")           
+
+                    \fIflatcombine for dome flats\fR
+
+        input = "flat.*imh"     List of flat field images to combine
+      (output = "flat1")        Output flat field root name
+     (combine = "median")       Type of combine operation
+      (reject = "ccdclip")      Type of rejection
+     (ccdtype = "flat")         CCD image type to combine
+     (process = no)             Process images before combining?
+     (subsets = yes)            Combine images by subset parameter?
+      (delete = no)             Delete input images after combining?
+     (clobber = no)             Clobber existing output image?
+       (scale = "median")       Image scaling
+     (statsec = "[m:n,p:q]")    Image section for computing statistics
+        (nlow = 1)              minmax: Number of low pixels to reject
+       (nhigh = 1)              minmax: Number of high pixels to reject
+       (nkeep = 1)              Minimum to keep (pos) or maximum to reject
+       (mclip = yes)            Use median in sigma clipping algorithms?
+      (lsigma = 3.)             Lower sigma clipping factor
+      (hsigma = 3.)             Upper sigma clipping factor
+     (rdnoise = "5")            ccdclip: CCD readout noise (electrons)
+        (gain = "2.5")          ccdclip: CCD gain (electrons/DN)
+      (snoise = "0.")           ccdclip: Sensitivity noise (fraction)
+       (pclip = -0.5)           pclip: Percentile clipping parameter
+       (blank = 1.)             Value if there are no pixels
+        (mode = "ql")           
+
+                   \fIflatcombine for sky flats\fR
+
+        input = "sky.*imh"      List of flat field images to combine
+      (output = "sky1")         Output flat field root name
+     (combine = "median")       Type of combine operation
+      (reject = "ccdclip")      Type of rejection
+     (ccdtype = "other")        CCD image type to combine
+     (process = no)             Process images before combining?
+     (subsets = yes)            Combine images by subset parameter?
+      (delete = no)             Delete input images after combining?
+     (clobber = no)             Clobber existing output image?
+       (scale = "median")       Image scaling
+     (statsec = "[m:n,p:q]")    Image section for computing statistics
+        (nlow = 1)              minmax: Number of low pixels to reject
+       (nhigh = 1)              minmax: Number of high pixels to reject
+       (nkeep = 1)              Minimum to keep (pos) or maximum to reject
+       (mclip = yes)            Use median in sigma clipping algorithms?
+      (lsigma = 3.)             Lower sigma clipping factor
+      (hsigma = 3.)             Upper sigma clipping factor
+     (rdnoise = "5")            ccdclip: CCD readout noise (electrons)
+        (gain = "2.5")          ccdclip: CCD gain (electrons/DN)
+      (snoise = "0.")           ccdclip: Sensitivity noise (fraction)
+       (pclip = -0.5)           pclip: Percentile clipping parameter
+       (blank = 1.)             Value if there are no pixels
+        (mode = "ql")           
+.fi
+.le
+.bp
+.ls \fI3.5 Processing the calibration frames\fR
+
+Although all the following steps may be done only in one step, our
+approach is to do them separately to allow you to start at any point in
+this section in case you have already started reducing the images on
+the mountain.
+
+You must start by overscan subtracting and trimming 'zero1'. Edit the
+parameters for the 'ccdproc' task according to the list given below.
+There is a series of parameters that are set to 'yes' and 'no'. You must set
+only 'overscan' and 'trim' to 'yes' and the rest to 'no'. Also
+'ccdtype' must be
+set to 'zero'. Be sure to properly specify the parameters 
+'biassec' and 'trimsec' which you determined while reading section 3.3.2.
+The range of columns comes first separated by a ':' and the range of lines
+is again separated by a ':', i.e., [29:425,21:402].
+
+\fIDo not change these parameters until having
+processed all your images\fR.
+
+.nf
+      cc> epar ccdproc        (check the list given below)
+      cc> ccdproc zero1
+.fi
+
+If the parameter 'interactive' was set to 'yes' you will be required to
+fit interactively the overscan region with a certain function. Once
+presented by the task with the plot of the overscan region (see figure 3)
+you may change the fitting function, for example, with ':function chebyshev'
+and its order with
+':order 4'. To try a new fit type 'f'.  We suggest a spline3 of order 2.
+You may also select the sample to be fit using the 's' command twice.
+If you are happy with
+the fit type 'q' to quit. The task will then process 'zero1' accordingly.
+
+Continue by overscan subtracting, trimming and bias subtracting 'dark1'.
+In this case you have to change in 'ccdproc' the 'ccdtype' parameter
+to 'dark' and the
+'zerocor' parameter to 'yes'.
+
+.nf
+      cc> epar ccdproc        (check the list given below)
+      cc> ccdproc dark1
+.fi
+
+The dark image must be examined before proceeding. \fIFor instance, if the
+dark level is low enough (<10 counts/hour/pixel)
+compared to the flats, you will
+probably disregard dark subtracting your images, to avoid
+introducing noise in your data.\fR
+However, if you notice some structure in the dark image, it would be
+worth trying to dark correct the data. In the following examples, for
+generality's sake, we consider dark subtraction as part of the overall
+processing.  If this is not your case, do not forget to set the 'darkcor'
+parameter in 'ccdproc' to 'no' and leave it alone.
+
+Then process the flats. Check that the 'ccdtype' parameter is set
+to 'flat', that 'overscan', 'trim', 'zerocor' and 'darkcor' are all set
+to 'yes' and execute the task.
+
+.nf
+      cc> epar ccdproc        (check the list given below)
+      cc> ccdproc flat1*imh
+.fi
+
+IRAF records all the reduction operations in the image headers.  You
+may check from the headers of 'zero1', 'dark1', 'sky1' and 'flat1' that
+BT-FLAG, BI-FLAG, DK-FLAG are properly set. For instance,
+
+.nf
+      cc> imheader flat1R l+
+.fi
+
+It is also possible to check this by using the 'ccdlist' task which will check
+the header automatically and list the operations which have been performed on
+the image.
+
+.nf
+      cc> ccdlist flat1R
+
+.fi
+You should get the following,
+
+.nf
+        flat1R[496,501][real][flat][R][OTZ]:dflat R
+
+.fi
+'ccdlist' should tell you the image name (flat1R), the image size [496,501]
+left after trimming, the pixel type [real] of the image (the processed
+images should normally have pixels in real format, as opposed to
+the raw images which generally have pixels in 'short' format),
+the image type [flat], the filter used in the observation
+[R], the level of processing of the image [OTZ], and the image title (dflat R).
+
+At this level you should have the flats processed up through [OTZ] which
+means that the image has been [O]verscan subtracted, [T]rimmed, and
+[Z]ero subtracted. Additional codes for other operations in 'ccdproc'
+are [F]lat correction, [B]ad pixel correction, [I]illumination correction.
+
+.nf
+			\fIccdproc for zero1\fR
+
+       images = "zero1"         List of CCD images to correct
+     (\fIccdtype\fR = "zero")         CCD image type to correct
+   (max_cache = 0)              Maximum image caching memory (in Mbytes)
+      (noproc = no)             List processing steps only?
+      (fixpix = no)             Fix bad CCD lines and columns?
+    (\fIoverscan\fR = yes)            Apply overscan strip correction?
+        (\fItrim\fR = yes)            Trim the image?
+     (\fIzerocor\fR = no)             Apply zero level correction?
+     (\fIdarkcor\fR = no)             Apply dark count correction?
+     (\fIflatcor\fR = no)             Apply flat field correction?
+    (illumcor = no)             Apply iillumination correction?
+   (fringecor = no)             Apply fringe correction?
+     (readcor = no)             Convert zero level image to readout cor?
+     (scancor = no)             Convert flat field image to scan correction?
+    (readaxis = "line")         Read out axis (column|line)
+     (fixfile = "")             File describing the bad lines and columns
+     (\fIbiassec\fR = "[m:n,*]")      Overscan strip image section
+     (\fItrimsec\fR = "[r:s,t:u]")    Trim data section
+        (\fIzero\fR = "zero1")        Zero level calibration image
+        (\fIdark\fR = "dark1")        Dark count calibration image
+        (\fIflat\fR = "")             Flat field images
+       (illum = "")             Iillumination correction images
+      (fringe = "")             Fringe correction images
+  (minreplace = 1.)             Minimum flat field value
+    (scantype = "shortscan")    Scan type (shortscan|longscan)
+       (nscan = 1)              Number of short scan lines\n
+ (interactive = yes)            Fit overscan interactively?
+    (function = "spline3")      Fitting function
+       (order = 2)              Number of polynomial terms or spline pieces
+      (sample = "*")            Sample points to fit
+    (naverage = 1)              Number of sample points to combine
+    (niterate = 1)              Number of rejection iterations
+  (low_reject = 3.)             Low sigma rejection factor
+ (high_reject = 3.)             High sigma rejection factor
+        (grow = 0.)             Rejection growing radius
+        (mode = "ql")           
+
+			\fIccdproc for dark1\fR
+
+       images = "dark1"         List of CCD images to correct
+     (\fIccdtype\fR = "dark")         CCD image type to correct
+   (max_cache = 0)              Maximum image caching memory (in Mbytes)
+      (noproc = no)             List processing steps only?
+      (fixpix = no)             Fix bad CCD lines and columns?
+    (\fIoverscan\fR = yes)            Apply overscan strip correction?
+        (\fItrim\fR = yes)            Trim the image?
+     (\fIzerocor\fR = yes)            Apply zero level correction?
+     (\fIdarkcor\fR = no)             Apply dark count correction?
+     (\fIflatcor\fR = no)             Apply flat field correction?
+    (illumcor = no)             Apply iillumination correction?
+   (fringecor = no)             Apply fringe correction?
+     (readcor = no)             Convert zero level image to readout corr?
+     (scancor = no)             Convert flat field image to scan correction?
+    (readaxis = "line")         Read out axis (column|line)
+     (fixfile = "")             File describing the bad lines and columns
+     (\fIbiassec\fR = "[m:n,*]")      Overscan strip image section
+     (\fItrimsec\fR = "[r:s,t:u]")    Trim data section
+        (\fIzero\fR = "zero1")        Zero level calibration image
+        (\fIdark\fR = "dark1")        Dark count calibration image
+        (\fIflat\fR = "")             Flat field images
+       (illum = "")             Iillumination correction images
+      (fringe = "")             Fringe correction images
+  (minreplace = 1.)             Minimum flat field value
+    (scantype = "shortscan")    Scan type (shortscan|longscan)
+       (nscan = 1)              Number of short scan lines\n
+ (interactive = yes)            Fit overscan interactively?
+    (function = "spline3")      Fitting function
+       (order = 2)              Number of polynomial terms or spline pieces
+      (sample = "*")            Sample points to fit
+    (naverage = 1)              Number of sample points to combine
+    (niterate = 1)              Number of rejection iterations
+  (low_reject = 3.)             Low sigma rejection factor
+ (high_reject = 3.)             High sigma rejection factor
+        (grow = 0.)             Rejection growing radius
+        (mode = "ql")           
+
+			\fIccdproc for flat1\fR
+
+       images = "flat1*imh"     List of CCD images to correct
+     (\fIccdtype\fR = "flat")         CCD image type to correct
+   (max_cache = 0)              Maximum image caching memory (in Mbytes)
+      (noproc = no)             List processing steps only?
+      (fixpix = no)             Fix bad CCD lines and columns?
+    (\fIoverscan\fR = yes)            Apply overscan strip correction?
+        (\fItrim\fR = yes)            Trim the image?
+     (\fIzerocor\fR = yes)            Apply zero level correction?
+     (\fIdarkcor\fR = yes)            Apply dark count correction?
+     (\fIflatcor\fR = no)             Apply flat field correction?
+    (illumcor = no)             Apply iillumination correction?
+   (fringecor = no)             Apply fringe correction?
+     (readcor = no)             Convert zero level image to readout corr?
+     (scancor = no)             Convert flat field image to scan correction?
+    (readaxis = "line")         Read out axis (column|line)
+     (fixfile = "")             File describing the bad lines and columns
+     (\fIbiassec\fR = "[m:n,*]")      Overscan strip image section
+     (\fItrimsec\fR = "[r:s,t:u]")    Trim data section
+        (\fIzero\fR = "zero1")        Zero level calibration image
+        (\fIdark\fR = "dark1")        Dark count calibration image
+        (\fIflat\fR = "")             Flat field images
+       (illum = "")             Iillumination correction images
+      (fringe = "")             Fringe correction images
+  (minreplace = 1.)             Minimum flat field value
+    (scantype = "shortscan")    Scan type (shortscan|longscan)
+       (nscan = 1)              Number of short scan lines\n
+ (interactive = yes)            Fit overscan interactively?
+    (function = "spline3")      Fitting function
+       (order = 2)              Number of polynomial terms or spline pieces
+      (sample = "*")            Sample points to fit
+    (naverage = 1)              Number of sample points to combine
+    (niterate = 1)              Number of rejection iterations
+  (low_reject = 3.)             Low sigma rejection factor
+ (high_reject = 3.)             High sigma rejection factor
+        (grow = 0.)             Rejection growing radius
+        (mode = "ql")           
+.fi
+.le
+.bp
+.ls \fI3.6 Preparing a Final Flat Field\fR
+
+Next we want to check the iillumination of the flat by applying it to the sky
+flat. Load the 'imred' and 'ccdred' packages if they are
+not already loaded.
+There is no tried and true method for testing the iillumination of
+the sky flats except for applying them on a long exposure taken in the same
+filter and implotting it or doing image statistics.
+
+We must use 'ccdproc' to overscan subtract, trim, bias subtract, dark subtract
+(if needed), and flat field the sky images. Again, we assume here
+that the dark is
+necessary for the reductions. Be sure that the images you are using for
+the flat field division have the proper filter identification.
+First edit the parameters for 'ccdproc', and then run
+this task to process your skys to see if the iillumination of the dome
+flat is uniform;
+
+.nf
+      cl> noao
+      im> imred
+      im> ccdred
+      cc> epar ccdproc        (check the parameter list)
+      cc> ccdproc sky1R
+.fi
+
+Now we must check the sky to see if it really is flat. This is done
+using 'implot' and plotting some lines or a group of lines,
+
+.nf
+      cc> implot sky1R
+            :l 150 200
+            :c 200 250
+	    q
+.fi
+
+Ideally if the iillumination was uniform, sky1R should not show any variation.
+In plotting several lines together, you may get a small slope (see figure 4).
+If you see any    
+variations, including a slope even near the edges of the image, then you must
+run the task 'mkskyflat'. Select a smoothing box size which preserves the large
+scale features while adequately suppressing the noise.  The scale of the
+largest features expected shouldn't be smaller than say 1/10 to 1/12 the
+image size.
+
+.nf
+      cc> epar mkskyflat      (check the parameter list)
+      cc> mkskyflat sky1R finalflat1R
+.fi
+
+The output image is the corrected flat image so call it "finalflat1R".
+We need to recopy the sky flat to process it again. Do an imcopy of the sky1R
+from the backup image after deleting the processed one.
+
+.nf
+      cc> imdel sky1R
+      cc> imcopy Bsky1R sky1R
+      cc> epar ccdproc        (change the parameter 'flat' from
+			       flat1R to finalflat1R)
+      cc> ccdproc sky1R
+.fi
+
+Again, check to see if the sky is really flat. If it is flat
+(see figure 5), then you are
+done and must process the flats for your other filters. If it is not flat,
+go back to the beginning and ask for help. It may be that you need to play
+with the smoothing parameters. Repeat these steps until you are satisfied.
+Now you can process your images.
+
+.nf
+
+			\fIccdproc for sky flats\fR
+
+       images = "sky1*imh"      List of CCD images to correct
+     (\fIccdtype\fR = "other")        CCD image type to correct
+   (max_cache = 0)              Maximum image caching memory (in Mbytes)
+      (noproc = no)             List processing steps only?
+      (fixpix = no)             Fix bad CCD lines and columns?
+    (\fIoverscan\fR = yes)            Apply overscan strip correction?
+        (\fItrim\fR = yes)            Trim the image?
+     (\fIzerocor\fR = yes)            Apply zero level correction?
+     (\fIdarkcor\fR = yes)            Apply dark count correction?
+     (\fIflatcor\fR = yes)            Apply flat field correction?
+    (illumcor = no)             Apply iillumination correction?
+   (fringecor = no)             Apply fringe correction?
+     (readcor = no)             Convert zero level image to readout corr?
+     (scancor = no)             Convert flat field image to scan correction?
+    (readaxis = "line")         Read out axis (column|line)
+     (fixfile = "")             File describing the bad lines and columns
+     (\fIbiassec\fR = "[m:n,*]")      Overscan strip image section
+     (\fItrimsec\fR = "[r:s,t:u]")    Trim data section
+        (\fIzero\fR = "zero1")        Zero level calibration image
+        (\fIdark\fR = "dark1")        Dark count calibration image
+        (\fIflat\fR = "flat1*imh")    Flat field images
+       (illum = "")             Iillumination correction images
+      (fringe = "")             Fringe correction images
+  (minreplace = 1.)             Minimum flat field value
+    (scantype = "shortscan")    Scan type (shortscan|longscan)
+       (nscan = 1)              Number of short scan lines\n
+ (interactive = yes)            Fit overscan interactively?
+    (function = "spline3")      Fitting function
+       (order = 2)              Number of polynomial terms or spline pieces
+      (sample = "*")            Sample points to fit
+    (naverage = 1)              Number of sample points to combine
+    (niterate = 1)              Number of rejection iterations
+  (low_reject = 3.)             Low sigma rejection factor
+ (high_reject = 3.)             High sigma rejection factor
+        (grow = 0.)             Rejection growing radius
+        (mode = "ql")           
+.fi
+.bp
+.nf
+                      \fImkskyflat\fR
+
+        input = "sky1R"     Input CCD images
+       output = "finalflat1R"     Output images (same as input if none)
+     (ccdtype = "")         CCD image type to select
+     (\fIxboxmin\fR = 0.1)        Minimum smoothing box size in x at edges
+     (\fIxboxmax\fR = 0.1)        Maximum smoothing box size in x
+     (\fIyboxmin\fR = 0.1)        Minimum smoothing box size in y at edges
+     (\fIyboxmax\fR = 0.1)        Maximum smoothing box size in y
+        (clip = yes)        Clip input pixels?
+    (lowsigma = 2.5)        Low clipping sigma
+   (highsigma = 2.5)        High clipping sigma
+     (ccdproc = "")         CCD processing parameters
+        (mode = "ql")
+.fi
+.le
+.bp
+.ls \fI3.7 Processing the Images\fR
+
+This can be setup to be done all at once. The final flat has been made so now
+we divide it into your objects.
+If the calibration frames themselves
+have not been processed it will do this as well. The program takes into
+account the differing filters. Be sure that you have deleted all the individual
+calibration frames that were combined. Edit the parameters for 'ccdproc' and run
+it. For tasks that take a long time, it is a good idea to set them going as a
+background job and send the output to a file which you can watch to keep track
+of the progress. You may wish to make a list of the objects to be processed
+to avoid reprocessing your sky flats.
+
+.nf
+      cc> epar ccdproc        (check the parameter list)
+      cc> ccdproc obj*.imh
+.fi
+
+To check the progress of the task, just type 
+
+.nf
+      cc> tail ccdlog
+.fi
+
+This will print out the last lines of the file named 'ccdlog'
+which is the latest 
+operation done by the task 'ccdproc'.
+Once this is done, check your images to see
+that they have been properly flat fielded. If you are satisfied, then you may
+now check your images for bad pixel regions, the structure of which may not have
+been processed out of your images.
+
+We suggest also to do a 'ccdlist' on the objects in order to
+check whether the frames have been duly processed, i.e.,
+
+.nf
+     cc> ccdlist obj*.imh
+.fi
+
+You should get a listing of your images in the format that follows,
+
+.nf
+
+      obj1010.imh[496,501][real][object][R][OTZF]:rubin 152 R
+      obj1011.imh[496,501][real][object][I][OTZF]:rubin 152 I
+      obj1012.imh[496,501][real][object][B][OTZF]:rubin 149 B
+      obj1013.imh[496,501][real][object][V][OTZF]:rubin 149 V
+      obj1014.imh[496,501][real][object][R][OTZF]:rubin 149 R
+      obj1015.imh[496,501][real][object][I][OTZF]:rubin 149 I
+      obj1016.imh[496,501][real][object][B][OTZF]:rubin 149 B
+      obj1017.imh[496,501][real][object][V][OTZF]:rubin 149 V
+      obj1018.imh[496,501][real][object][R][OTZF]:rubin 149 R
+      obj1019.imh[496,501][real][object][I][OTZF]:rubin 149 I
+.fi
+
+where the [OTZF] code reveals the degree of processing of the images.
+
+.nf
+                   \fIccdproc for objects\fR
+
+       images = "obj*imh)"      List of CCD images to correct
+     (\fIccdtype\fR = "object")       CCD image type to correct
+   (max_cache = 0)              Maximum image caching memory (in Mbytes)
+      (noproc = no)             List processing steps only?
+      (fixpix = no)             Fix bad CCD lines and columns?
+    (\fIoverscan\fR = yes)            Apply overscan strip correction?
+        (\fItrim\fR = yes)            Trim the image?
+     (\fIzerocor\fR = yes)            Apply zero level correction?
+     (\fIdarkcor\fR = yes)            Apply dark count correction?
+     (\fIflatcor\fR = yes)            Apply flat field correction?
+    (illumcor = no)             Apply iillumination correction?
+   (fringecor = no)             Apply fringe correction?
+     (readcor = no)             Convert zero level image to readout corr?
+     (scancor = no)             Convert flat field image to scan correction?
+    (readaxis = "line")         Read out axis (column|line)
+     (fixfile = "")             File describing the bad lines and columns
+     (\fIbiassec\fR = "[m:n,*]")      Overscan strip image section
+     (\fItrimsec\fR = "[r:s,t:u]")    Trim data section
+        (\fIzero\fR = "zero1")        Zero level calibration image
+        (\fIdark\fR = "dark1")        Dark count calibration image
+        (\fIflat\fR = "finalflat1*imh")    Flat field images
+       (illum = "")             Iillumination correction images
+      (fringe = "")             Fringe correction images
+  (minreplace = 1.)             Minimum flat field value
+    (scantype = "shortscan")    Scan type (shortscan|longscan)
+       (nscan = 1)              Number of short scan lines\n
+ (interactive = yes)            Fit overscan interactively?
+    (function = "spline3")      Fitting function
+       (order = 2)              Number of polynomial terms or spline pieces
+      (sample = "*")            Sample points to fit
+    (naverage = 1)              Number of sample points to combine
+    (niterate = 1)              Number of rejection iterations
+  (low_reject = 3.)             Low sigma rejection factor
+ (high_reject = 3.)             High sigma rejection factor
+        (grow = 0.)             Rejection growing radius
+        (mode = "ql")           
+
+.fi
+
+.le
+.bp
+.ls \fI3.8 Creating the Bad Pixel File\fR
+
+Now it is time to check your images to see if structure remains in the bad
+pixel regions. If you were careful to observe your objects far away from any
+obvious bad regions then you may only need to 'fix' pixels for cosmetic reasons.
+We suggest you to examine these files using the display window,
+imtool (this can only be done at one of the SUN consoles), and then plotting
+them using 'implot'. Start by loading the 'noao', 'images', 'tv', 'imred',
+and 'ccdred' packages. Display
+a processed image and plot it using 'implot',
+
+.nf
+      cl> noao
+      no> images
+      im> tv
+      tv> imred
+      im> ccdred
+      cc> display obj002 1
+      cc> implot obj002
+.fi
+
+Do not exit from implot, but move the cursor to the imtool window and press
+'F6'. The cursor coordinates are now visible at the bottom of the screen.
+Find the position of a bad pixel using this, return to the graph and
+plot it using 'implot' with the ':l #'(line) and ':c #'(column) commands.
+You can define them more precisely using 'implot' by overplotting lines and
+columns around the center of the bad regions. Do this by typing 'o' followed
+by ':c #' and ':l #'. Once you have these regions written down, check some of
+your images to see if the bad pixels are a problem, ie >1% in signal. If it is
+a problem then create a file called 'badpix' with the listing of
+the pixels you wish to fix;
+
+.nf
+      cc> edit badpix           (according to the following format)
+.fi
+
+The following example is to illustrate the format of a bad pixel file.
+
+.nf
+      84 87 1 450
+      87 90 105 109
+      87 89 110 111
+      124 126 112 116
+      206 206 80 80
+.fi
+
+Each line stands for a rectangular region of the image to be fixed. The regions
+are specified by four numbers giving the starting and ending columns followed
+by the starting and ending lines. The starting and ending points may be the
+same to specify a single column, line or pixel. Note that each region is
+"fixed" by interpolating across its shortest dimension and that regions are
+processed in the order that they appear in the bad pixel list. For bad regions
+of complex shape, some care may be required in specifying the regions in order
+to achieve an optimal result. \fIIt is strongly recommended that you test your
+bad pixel file by using it to correct a copy of one of your images before going
+into production\fR. This bad pixel file will be specified in the task 'ccdproc'
+in the parameter 'fixfile'. So now edit and run the task:
+
+.nf
+       cc> epar ccdproc
+       cc> ccdproc obj*.imh
+.fi
+
+Remember that 'ccdproc' already knows that the images
+have been processed so those
+operations will not be performed again. Now you have final images that are ready
+to be used. If you plan to do photometry in IRAF see section VI of this manual.
+
+.nf
+                             \fIccdproc\fR
+
+       images = "obj*imh)"      List of CCD images to correct
+     (\fIccdtype\fR = "object")       CCD image type to correct
+   (max_cache = 0)              Maximum image caching memory (in Mbytes)
+      (noproc = no)             List processing steps only?
+      (\fIfixpix\fR = yes)            Fix bad CCD lines and columns?
+    (\fIoverscan\fR = yes)            Apply overscan strip correction?
+        (\fItrim\fR = yes)            Trim the image?
+     (\fIzerocor\fR = yes)            Apply zero level correction?
+     (\fIdarkcor\fR = yes)            Apply dark count correction?
+     (\fIflatcor\fR = yes)            Apply flat field correction?
+    (illumcor = no)             Apply iillumination correction?
+   (fringecor = no)             Apply fringe correction?
+     (readcor = no)             Convert zero level image to readout corr?
+     (scancor = no)             Convert flat field image to scan correction?
+    (readaxis = "line")         Read out axis (column|line)
+     (\fIfixfile\fR = "badpix")       File describing the bad lines and columns
+     (\fIbiassec\fR = "[m:n,*]")      Overscan strip image section
+     (\fItrimsec\fR = "[r:s,t:u]")    Trim data section
+        (\fIzero\fR = "zero1")        Zero level calibration image
+        (\fIdark\fR = "dark1")        Dark count calibration image
+        (\fIflat\fR = "finalflat1*imh")    Flat field images
+       (illum = "")             Iillumination correction images
+      (fringe = "")             Fringe correction images
+  (minreplace = 1.)             Minimum flat field value
+    (scantype = "shortscan")    Scan type (shortscan|longscan)
+       (nscan = 1)              Number of short scan lines\n
+ (interactive = yes)            Fit overscan interactively?
+    (function = "spline3")      Fitting function
+       (order = 2)              Number of polynomial terms or spline pieces
+      (sample = "*")            Sample points to fit
+    (naverage = 1)              Number of sample points to combine
+    (niterate = 1)              Number of rejection iterations
+  (low_reject = 3.)             Low sigma rejection factor
+ (high_reject = 3.)             High sigma rejection factor
+        (grow = 0.)             Rejection growing radius
+        (mode = "ql")           
+
+.fi
+.le
+.bp
+.ls \fI3.9 Writing the Data to Tape\fR
+
+Allocate the device, for the SUNs it is "mta". Then mount your tape, don't
+forget to put in a write ring. If you wish to use the exabyte drive, use "mtx"
+for the device name. Load the package 'dataio' and do an epar on 'wfits'.
+
+.nf
+      cl> dataio
+      da> epar wfits
+      da> wfits *.imh mta.6250 new+ 
+.fi
+
+The parameter newtape should be "yes"
+if you are starting on a new tape. Otherwise you will not want to overwrite
+data which has already been placed on a tape, so use "no". 
+
+After writing all the desired files to tape, deallocate the drive and retrieve
+your tape.
+
+.nf
+      da> dealloc mta
+.fi
+.le
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/quadproc.hlp b/noao/imred/quadred/src/quad/doc/quadproc.hlp
new file mode 100644
index 00000000..8d445097
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/quadproc.hlp
@@ -0,0 +1,672 @@
+.help quadproc Sept93 arcon.quad
+.ih
+NAME
+quadproc -- Process multi-readout CCD images
+.ih
+USAGE	
+quadproc images
+.ih
+PARAMETERS
+.ls images
+List of input CCD images to process.  The list may include processed
+images and calibration images.
+.le
+.ls ccdtype = ""
+CCD image type to select from the input image list.  If no type is given
+then all input images will be selected.  The recognized types are described
+in \fBccdtypes\fR.
+.le
+.ls max_cache = 0
+Maximum image caching memory (in Mbytes).  If there is sufficient memory
+the calibration images, such as zero level, dark count, and flat fields,
+will be cached in memory when processing many input images.  This
+reduces the disk I/O and makes the task run a little faster.  If the
+value is zero image caching is not used.
+.le
+.ls noproc = no
+List processing steps only?
+.le
+
+.ce
+PROCESSING SWITCHES
+.ls fixpix = yes
+Fix bad CCD lines and columns by linear interpolation from neighboring
+lines and columns?  If yes then a bad pixel file must be specified.
+.le
+.ls overscan = yes
+Apply overscan or prescan bias correction?  If yes then the overscan
+image section and the readout axis must be specified.
+.le
+.ls trim = yes
+Trim the image of the overscan region and bad edge lines and columns?
+If yes then the trim section must be specified.
+.le
+.ls zerocor = yes
+Apply zero level correction?  If yes a zero level image must be specified.
+.le
+.ls darkcor = yes
+Apply dark count correction?  If yes a dark count image must be specified.
+.le
+.ls flatcor = yes
+Apply flat field correction?  If yes flat field images must be specified.
+.le
+.ls illumcor = no
+Apply iillumination correction?  If yes iillumination images must be specified.
+.le
+.ls fringecor = no
+Apply fringe correction?  If yes fringe images must be specified.
+.le
+.ls readcor = no
+Convert zero level images to readout correction images?  If yes then
+zero level images are averaged across the readout axis to form one
+dimensional zero level readout correction images.
+.le
+.ls scancor = no
+Convert flat field images to scan mode flat field images?  If yes then the
+form of scan mode correction is specified by the parameter \fIscantype\fR.
+.le
+
+.ce
+PROCESSING PARAMETERS
+.ls readaxis = "line"
+Read out axis specified as "line" or "column".
+.le
+.ls fixfile
+File describing the bad lines and columns.  If "image" is specified then
+the file is specified in the image header or instrument translation file.
+See Section 2. of Description for further information on bad pixel files.
+.le
+.ls biassec
+Overscan bias strip image section.  If "image" is specified then the overscan
+bias section is specified in the image header or instrument translation file.
+See Section 3. of Description for further information on setting this parmeter.
+.le
+.ls trimsec
+image section for trimming.  If "image" is specified then the trim
+image section is specified in the image header or instrument translation file.
+See Section 4. of Description for further information on setting this parmeter.
+.le
+.ls zero = ""
+Zero level calibration image.  The zero level image may be one or two
+dimensional.  The CCD image type and subset are not checked for these
+images and they take precedence over any zero level calibration images
+given in the input list.
+.le
+.ls dark = ""
+Dark count calibration image.  The CCD image type and subset are not checked
+for these images and they take precedence over any dark count calibration
+images given in the input list.
+.le
+.ls flat = ""
+Flat field calibration images.  The flat field images may be one or
+two dimensional.  The CCD image type is not checked for these
+images and they take precedence over any flat field calibration images given
+in the input list.  The flat field image with the same subset as the
+input image being processed is selected.
+.le
+.ls illum = ""
+Iillumination correction images.  The CCD image type is not checked for these
+images and they take precedence over any iillumination correction images given
+in the input list.  The iillumination image with the same subset as the
+input image being processed is selected.
+.le
+.ls fringe = ""
+Fringe correction images.  The CCD image type is not checked for these
+images and they take precedence over any fringe correction images given
+in the input list.  The fringe image with the same subset as the
+input image being processed is selected.
+.le
+.ls minreplace = 1.
+When processing flat fields, pixel values below this value (after
+all other processing such as overscan, zero, and dark corrections) are
+replaced by this value.  This allows flat fields processed by \fBquadproc\fR
+to be certain to avoid divide by zero problems when applied to object
+images.
+.le
+.ls scantype = "shortscan"
+Type of scan format used in creating the CCD images.  The modes are:
+.ls "shortscan"
+The CCD is scanned over a number of lines and then read out as a regular
+two dimensional image.  In this mode unscanned flat fields are numerically
+scanned to form scanned flat fields comparable to the observations.  If
+the flat field calibration images are taken in scanned mode then
+\fIscancor\fR should be no and the processing performed in the same manner
+as in unscanned mode.
+.le
+.ls "longscan"
+In this mode the CCD is clocked and read out continuously to form a long
+strip.  Flat fields are averaged across the readout axis to
+form a one dimensional flat field readout correction image.  This assumes
+that all recorded image lines are clocked over the entire active area of the
+CCD.
+.le
+.le
+.ls nscan
+Number of scan readout lines used in short scan mode.  This parameter is used
+when the scan type is "shortscan".
+.le
+
+.ce
+OVERSCAN FITTING PARAMETERS
+.ls interactive = no
+Fit the overscan vector interactively?  If yes the overscan vector is fit
+interactively using the \fBicfit\fR package.  If no then the fitting parameters
+given below are used.
+.le
+.ls function = "legendre"
+Overscan fitting function.  The function types are "legendre" polynomial,
+"chebyshev" polynomial, "spline1" linear spline, and "spline3" cubic
+spline.
+.le
+.ls order = 1
+Number of polynomial terms or spline pieces in the overscan fit.
+.le
+.ls sample = "*"
+Sample points to use in the overscan fit.  The string "*" specified all
+points otherwise an \fBicfit\fR range string is used.
+.le
+.ls naverage = 1
+Number of points to average or median to form fitting points.  Positive
+numbers specify averages and negative numbers specify medians.
+.le
+.ls niterate = 1
+Number of rejection iterations to remove deviant points from the overscan fit.
+If 0 then no points are rejected.
+.le
+.ls low_reject = 3., high_reject = 3.
+Low and high sigma rejection factors for rejecting deviant points from the
+overscan fit.
+.le
+.ls grow = 0.
+One dimensional growing radius for rejection of neighbors to deviant points.
+.le
+.ih
+DESCRIPTION
+\fBQuadproc\fR processes CCD images to remove all "instrumental signatures" from
+the data. The operations performed are:
+.ls
+.nf
+o correct detector defects (bad lines and columns)
+o determine readout bias level using overscan and subtract it
+o trim off the overscan regions and unwanted border pixels
+o subtract zero level bias
+o subtract dark counts
+o correct for pixel-to-pixel sensitivity variations
+o correct for non-uniform iillumination
+o correct for fringing
+.fi
+.le
+.sp 1
+\fBQuadproc\fR is a cl script based on the task \fBccdproc\fR in the
+\fBccdred\fR package. It is specifically designed to deal with Arcon data
+obtained in multi-readout mode (see \fBquadformat\fR). A feature of such
+images is that each readout typically has a slightly different, DC bias
+level, gain, and readout noise. As a result both zero frames and uniformly 
+illuminated exposures show a characteristic chequer board pattern, the
+sections of the image read through each amplifier having different levels.
+In addition, there will be a separate overscan strip, used to monitor the zero
+level, for each readout. The location of these overscan strips in the raw
+frame depends on which amplifiers are used. \fBQuadproc\fR splits each 
+multi-readout image into subimages, one for each amplifier, and also calculates
+the biassec and trimsec appropriately for each. It then calls \fBccdproc\fR to
+perform the first three operations listed above. The sub-images are then glued
+back together. Finaly, \fBccdproc\fR is called a second time to perform all the
+remaining reduction steps. 
+
+\fBQuadproc\fR MUST be used for the reduction of multi-readout data up to and
+including the trimming step, and it is convenient to use it for the entire
+reduction process. However, once ALL images have been trimmed it is possible
+to finish the reductions using \fBccdproc\fR if the \fBquad\fR package is not
+available at your home institution. \fBQuadproc\fR recognizes mono-readout
+images and processes them directly using \fBccdproc\fR. If your images are a
+mixture of multi- and mono- readout use \fBquadproc\fR; if you only have
+mono-readout data use \fBccdproc\fR.
+
+\fBQuadproc\fR is identical to \fBccdproc\fR in the way it is used, and has
+exactly the same parameters; as far as possible it also behaves in the same way.
+To run it, all one has to do is set the parameters and then begin processing
+the images.  The task takes care of most of the record keeping and
+automatically does the prerequisite processing of calibration images. For
+ease of reference, the following sections provide a simple outline of how to
+use the task, together with a description of the operations performed. They 
+are taken almost verbatim from the help page for \fBccdproc\fR. If you are 
+already familiar with that task you should read sections 2., 3. and 4. below,
+which include information on the preparation of the badpixel file, and on how
+to specify \fBbiassec\fR and \fBtrimsec\fR parameters. See section 12. for a
+description of the differences between the two tasks. For a user's guide and 
+cookbook for the \fBquad\fR package see \fBguide\fR.
+.sh
+1. Parameters
+There are many parameters but they may be easily reviewed and modified using
+the task \fBeparam\fR.
+The input CCD images to be processed are given as an image list.
+Previously processed images are ignored and calibration images are
+recognized, provided the CCD image types are in the image header (see
+\fBinstruments\fR and \fBccdtypes\fR).  \fBQuadproc\fR separates multi- and
+mono-readout images in the input list and handles them accordingly.
+Therefore it is permissible to use simple image templates such as "*.imh".
+The \fIccdtype\fR parameter may be used to select only certain types of CCD
+images to process (see \fBccdtypes\fR).
+
+The processing operations are selected by boolean (yes/no) parameters.
+Because calibration images are recognized and processed appropriately,
+the processing operations for object images should be set. Any combination of
+operations may be specified. Two of the operations, \fBreadcor\fR and \fBscancor\fR, are only applicable to zero level and flat field images respectively. These
+are used for certain types of CCDs and modes of operation.
+
+The processing steps selected have related parameters which must be
+set.  These are things like image sections defining the overscan and
+trim regions and calibration images.  There are a number of parameters
+used for fitting the overscan or prescan bias section.  These are
+parameters used by the standard IRAF curve fitting package \fBicfit\fR.
+The parameters are described in more detail in the following sections.
+
+In addition to the task parameters there are package parameters
+which affect \fBquadproc\fR.  These include the instrument and subset
+files, the text and plot log files, the output pixel datatype,
+the verbose parameter for logging to the terminal, and the backup
+prefix.  These are described in \fBquad\fR.
+
+Calibration images are specified by task parameters and/or in the
+input image list.  If more than one calibration image is specified
+then the first one encountered is used. Calibration images specified by
+task parameters take precedence over calibration images in the input list.
+These images also need not have a CCD image type parameter since the task
+parameter identifies the type of calibration image.  This method is
+best if there is only one calibration image for all images
+to be processed, almost always true for zero level and dark
+count images.  If no calibration image is specified by task parameter
+then calibration images in the input image list are identified and
+used.  This requires that the images have CCD image types recognized
+by the package.  This method is useful if one may simply say "*.imh"
+as the image list to process all images or if the images are broken
+up into groups, in "@" files for example, each with their own calibration
+frames.
+.sh
+2. Fixpix
+Regions of bad lines and columns may be replaced by linear
+interpolation from neighboring lines and columns when the parameter
+\fIfixpix\fR is set.  The bad regions are specified in a bad pixel
+file.  The file consists of lines with four fields, the starting and
+ending columns and the starting and ending lines.  Any number of
+regions may be specified. Currently, the coordinates given for the bad regions
+must be those that would be applicable if the CCD was used in SINGLE READOUT
+MODE, even if multi-readout images are being reduced. A task is being written
+to aid in the preparation of an appropriate bad-pixel file given measurements
+made on a raw multi-readout image.
+
+Comment lines beginning with the character '#' may be included. If a comment
+line preceding the bad regions contains the word "untrimmed" then the
+coordinate system refers to the original format of the images; i.e.  before 
+trimming.  If an image has been trimmed previously then the trim region
+specified in the image header is used to convert the coordinates in the bad
+pixel file to those of the trimmed image.  If the file does not contain the
+word "untrimmed" then the coordinate system must match that of the image
+being corrected; i.e. untrimmed coordinates if the image has not been
+trimmed and trimmed coordinates if the image has been trimmed.
+Standard bad pixel files should always be specified in terms of the original
+format.
+
+The bad pixel file may be specified explicitly with the parameter \fIfixfile\fR
+or indirectly if the parameter has the value "image".  In the latter case
+the instrument file must contain the name of the file.
+.sh
+3. Overscan
+The portion of the image used to determine the readout bias level is specified
+with the parameter \fBbiassec\fR. This may be an explicit image section, or it
+may be set to the special value "image". In the latter case the value given in
+the image header is used.  The image header value uses the entire overscan 
+strip without allowing any margin between the data section and the bias
+section.  Because Arcon uses a DC-coupled preamplifier the transition
+between data and overscan is very sharp indeed. Nonetheless, we recommend that
+you do skip the first few pixels of the overscan strip. To decide this issue
+for yourself, use implot to plot the average of several lines from a high 
+exposure level image such as a flat field. Expand the transition region 
+between data and overscan and decide how many pixels of the overscan are
+contaminated.
+
+In the case of multi-readout images, the way in which an explicit value for
+\fBbiassec\fR must be set, is unfortunately somewhat non-intuitive.  Currently,
+the value recorded in the image header is that which would be appropriate had
+the detector been read out using a single amplifier; an explicit image section
+must be specified in the same way. \fBQuadproc\fR calculates the sections
+to use for the sub-images corresponding to each readout based on such "single
+readout" sections. To determine the section you must enter, use \fBimhead\fR
+or \fBhselect\fR to determine the value of \fBbiassec\fR stored in the image 
+header. If this is, for instance,  "[1025:1060,1:1028]" then setting 
+\fBbiassec\fR = "[1029:1060,1:1028]" would leave  a margin of 4 pixels
+(1029 - 1025).  Note that if two readouts are used in the horizontal direction 
+(quad or serial-split dual readout) the overscan strip for each amplifier is
+only half as wide as that in single readout mode. Thus in the example a 15
+pixel (36 / 2 - 3) wide strip is used for each readout.
+
+If an overscan or prescan correction is specified (\fIoverscan\fR
+parameter) then the specified image section is averaged
+along the readout axis (\fIreadaxis\fR parameter) to form a
+correction vector.  A function is fit to this vector and for each readout
+line (image line or column) the function value for that line is
+subtracted from the image line.  The fitting function is generally
+either a constant (polynomial of 1 term) or a high order function
+which fits the large scale shape of the overscan vector.  Bad pixel
+rejection is also used to eliminate cosmic ray events.  The function
+fitting may be done interactively using the standard \fBicfit\fR
+iteractive graphical curve fitting tool.  Regardless of whether the fit
+is done interactively, the overscan vector and the fit may be recorded
+for later review in a metacode plot file named by the parameter
+\fIquad.plotfile\fR.  The mean value of the bias function is also recorded in
+the image header and log file.
+
+The overscan subtraction performed by \fBquadproc\fR corrects the 
+amplifier-to-amplifier differences in the bias level, so that no
+readout structure should be visible in processed zero images. However, you
+will still see the chequer board structure in flatfield and object exposures
+(unless the sky level is zero) because of gain difference between the
+amplifiers.
+.sh
+4. Trim
+When the parameter \fItrim\fR is set the input image will be trimmed to
+the image section given by the parameter \fItrimsec\fR. This may be an explicit
+image section, or it may be set to the special value "image". In the latter
+case the value given in the image header is used.  The image header value keeps
+the entire imaging section of the CCD.
+
+In the case of multi-readout images, the way in which an explicit value for
+\fBtrimsec\fR must be set, is unfortunately somewhat non-intuitive.  Currently,
+the value recorded in the image header is that which would be appropriate had
+the detector been read out using a single amplifier; an explicit image section
+must be specified in the same way. \fBQuadproc\fR calculates the sections
+to use for the sub-images corresponding to each readout based on such "single
+readout" sections. In addition one is currently restricted to trimming exactly
+the same number of columns from each side of the CCD; there is no such 
+restriction on the number of lines which can be trimmed from the top and bottom
+edges of the image. To determine the section you must enter, use \fBimhead\fR
+or \fBhselect\fR to determine the value of \fBtrimsec\fR stored in the image
+header. If this is, for instance, "[1:1024,1:1028]" then setting
+\fBtrimsec\fR = "[10:1015,20:998]" would trim 9 columns from the left and right
+edges and 19 and 29 lines from the bottom and top edges respectively. If you
+need to perform an asymmetric trim in the horizontal direction this can be
+done, after processing, by using \fBimcopy\fR to copy the required portion of
+the image.
+
+The trim section used for science images should, of course, be the same as 
+that used for the calibration images.
+.sh
+5. Zerocor
+After the readout bias is subtracted, as defined by the overscan or prescan
+region, there may still be a zero level bias.  This level may be two
+dimensional or one dimensional (the same for every readout line).  A
+zero level calibration is obtained by taking zero length exposures;
+generally many are taken and combined.  To apply this zero
+level calibration the parameter \fIzerocor\fR is set.  In addition if
+the zero level bias is only readout dependent then the parameter \fIreadcor\fR
+is set to reduce two dimensional zero level images to one dimensional
+images.  The zero level images may be specified by the parameter \fIzero\fR
+or given in the input image list (provided the CCD image type is defined).
+
+When the zero level image is needed to correct an input image it is checked
+to see if it has been processed and, if not, it is processed automatically.
+Processing of zero level images consists of bad pixel replacement,
+overscan correction, trimming, and averaging to one dimension if the
+readout correction is specified.
+.sh
+6. Darkcor
+Dark counts are subtracted by scaling a dark count calibration image to
+the same exposure time as the input image and subtracting.  The
+exposure time used is the dark time which may be different than the
+actual integration or exposure time.  A dark count calibration image is
+obtained by taking a very long exposure with the shutter closed; i.e.
+an exposure with no light reaching the detector.  The dark count
+correction is selected with the parameter \fIdarkcor\fR and the dark
+count calibration image is specified either with the parameter
+\fIdark\fR or as one of the input images.  The dark count image is
+automatically processed as needed.  Processing of dark count images
+consists of bad pixel replacement, overscan and zero level correction,
+and trimming.
+.sh
+7. Flatcor
+The relative detector pixel response is calibrated by dividing by a
+scaled flat field calibration image.  A flat field image is obtained by
+exposure to a spatially uniform source of light such as an lamp or
+twilight sky.  Flat field images may be corrected for the spectral
+signature in spectroscopic images (see \fBresponse\fR and
+\fBapnormalize\fR), or for iillumination effects (see \fBmkillumflat\fR
+or \fBmkskyflat\fR).  For more on flat fields and iillumination corrections
+see \fBflatfields\fR.  The flat field response is dependent on the
+wavelength of light so if different filters or spectroscopic wavelength
+coverage are used a flat field calibration for each one is required.
+The different flat fields are  automatically selected by a subset
+parameter (see \fBsubsets\fR).
+
+Flat field calibration is selected with the parameter \fBflatcor\fR
+and the flat field images are specified with the parameter \fBflat\fR
+or as part of the input image list.  The appropriate subset is automatically
+selected for each input image processed.  The flat field image is
+automatically processed as needed.  Processing consists of bad pixel
+replacement, overscan subtraction, zero level subtraction, dark count
+subtraction, and trimming.  Also if a scan mode is used and the
+parameter \fIscancor\fR is specified then a scan mode correction is
+applied (see below).  The processing also computes the mean of the
+flat field image which is used later to scale the flat field before
+division into the input image.  For scan mode flat fields the ramp
+part is included in computing the mean which will affect the level
+of images processed with this flat field.  Note that there is no check for
+division by zero in the interest of efficiency.  If division by zero
+does occur a fatal error will occur.  The flat field can be fixed by
+replacing small values using a task such as \fBimreplace\fR or
+during processing using the \fIminreplace\fR parameter.  Note that the
+\fIminreplace\fR parameter only applies to flat fields processed by
+\fBquadproc\fR.
+.sh
+8. Illumcor
+CCD images processed through the flat field calibration may not be
+completely flat (in the absence of objects).  In particular, a blank
+sky image may still show gradients.  This residual nonflatness is called
+the iillumination pattern.  It may be introduced even if the detector is
+uniformly illuminated by the sky because the flat field lamp
+iillumination may be nonuniform.  The iillumination pattern is found from a
+blank sky, or even object image, by heavily smoothing and rejecting
+objects using sigma clipping.  The iillumination calibration image is
+divided into the data being processed to remove the iillumination
+pattern.  The iillumination pattern is a function of the subset so there
+must be an iillumination correction image for each subset to be
+processed.  The tasks \fBmkillumcor\fR and \fBmkskycor\fR are used to
+create the iillumination correction images.  For more on iillumination
+corrections see \fBflatfields\fR.
+
+An alternative to treating the iillumination correction as a separate
+operation is to combine the flat field and iillumination correction
+into a corrected flat field image before processing the object
+images.  This will save some processing time but does require creating
+the flat field first rather than correcting the images at the same
+time or later.  There are two methods, removing the large scale
+shape of the flat field and combining a blank sky image iillumination
+with the flat field.  These methods are discussed further in the
+tasks which create them; \fBmkillumcor\fR and \fBmkskycor\fR.
+.sh
+9. Fringecor
+There may be a fringe pattern in the images due to the night sky lines.
+To remove this fringe pattern a blank sky image is heavily smoothed
+to produce an iillumination image which is then subtracted from the
+original sky image.  The residual fringe pattern is scaled to the
+exposure time of the image to be fringe corrected and then subtracted.
+Because the intensity of the night sky lines varies with time an
+additional scaling factor may be given in the image header.
+The fringe pattern is a function of the subset so there must be
+a fringe correction image for each subset to be processed.
+The task \fBmkfringecor\fR is used to create the fringe correction images.
+.sh
+10. Readcor
+If a zero level correction is desired (\fIzerocor\fR parameter)
+and the parameter \fIreadcor\fR is yes then a single zero level
+correction vector is applied to each readout line or column.  Use of a
+readout correction rather than a two dimensional zero level image
+depends on the nature of the detector or if the CCD is operated in
+longscan mode (see below).  The readout correction is specified by a
+one dimensional image (\fIzero\fR parameter) and the readout axis
+(\fIreadaxis\fR parameter).  If the zero level image is two dimensional
+then it is automatically processed to a one dimensional image by
+averaging across the readout axis.  Note that this modifies the zero
+level calibration image.
+.sh
+11. Scancor
+CCD detectors may be operated in several modes in astronomical
+applications.  The most common is as a direct imager where each pixel
+integrates one point in the sky or spectrum.  However, the design of most CCD's
+allows the sky to be scanned across the CCD while shifting the
+accumulating signal at the same rate.  \fBQuadproc\fR provides for two
+scanning modes called "shortscan" and "longscan".  The type of scan
+mode is set with the parameter \fIscanmode\fR.
+
+In "shortscan" mode the detector is scanned over a specified number of
+lines (not necessarily at sideral rates).  The lines that scroll off
+the detector during the integration are thrown away.  At the end of the
+integration the detector is read out in the same way as an unscanned
+observation.  The advantage of this mode is that the small scale flat
+field response is averaged in one dimension over the number of lines
+scanned.  A flat field may be observed in the same way in which case
+there is no difference in the processing from unscanned imaging and the
+parameter \fIscancor\fR should be no.  However, one obtains an increase
+in the statistical accuracy of the flat fields if they are not scanned
+during the observation but digitally scanned during the processing.  In
+shortscan mode with \fIscancor\fR set to yes, flat field images are
+digitally scanned, if needed, by the specified number of scan lines
+(\fInscan\fR parameter).
+
+In "longscan" mode the detector is continuously read out to produce
+an arbitrarily long strip.  Provided data which has not passed over
+the entire detector is thrown away, the flat field corrections will
+be one dimensional.  If \fIscancor\fR is specified and the
+scan mode is "longscan" then a one dimensional flat field correction
+will be applied.  If the specified flat field (\fIflat\fR parameter)
+is a two dimensional image then when the flat field image is processed
+it will be averaged across the readout axis to form a one dimensional
+correction image.
+.sh
+12. Outline of Processing Steps
+
+Because of the special handling required for multi-readout data
+\fBquadproc\fR internally reduces the data in two stages.
+
+.ls Stage one
+The operations which may be performed in the first stage are badpixel
+correction, determination and subtraction of the readout bias level, and
+trimming. This stage is only performed if one or more of the \fBfixpix\fR,
+\fBoverscan\fR or \fBtrim\fR flags is set to yes.
+
+First, all the calibration images which will be needed are identified. Any
+which were obtained in multi-readout mode AND which have not already been
+trimmed are selected for processing during this stage. This is necessary to
+ensure that the calibration images will be reduced properly. Similarly, the
+input list is searched and all multi-readout images, which have not already
+been trimmed are selected for processing.
+
+The images selected in this way are then processed sequentially. Each is split
+into separate images one for each amplifier. The values of the trimsec and
+biassec header keywords for each of these sub-images are set as required. 
+\fBccdproc\fR is then run to correct bad pixels, determine and subtract the
+readout bias and trim each sub-image. Finaly, the pieces are glued back 
+together again to form the complete image and the header information is 
+tidied up. The resulting image is initialy created as a temporary image.
+When stage one processing is complete the original image is deleted (or
+renamed using the specified backup prefix) and the corrected image replaces
+the original image.  Using a temporary image protects the data in the
+event of an abort or computer failure.  Keeping the original image name
+eliminates much of the record keeping and the need to generate new
+image names.
+.le
+.ls Stage two
+\fBCcdproc\fR is now run a second time to process ALL input images. For those
+images which were NOT selected for processing during stage one all the selected
+processing steps are carried out during this second pass. For those which were
+selected in stage one only the remaining processing steps will be performed.
+Again the output processed image is initialy created as a temporary image.
+When stage two processing is complete the original image is deleted (or
+renamed using the specified backup prefix) and the corrected image replaces
+the original image.
+.le
+
+The following difference in the behaviour of \fBquadproc\fB and \fBccdproc\fR
+should be noted:
+.ls
+Because it is a script, and because it is reads and writes each image several
+times during processing \fBquadproc\fR is not very efficiant. This will be 
+rectified when the present prototype code is replaced by the final version.
+.le
+.ls
+If backups are enable then \fBquadproc\fR will produce two intermediate 
+images for every input image which is modified in both processing stages.
+These backup images may quickly fill up the available disk space.
+.le
+.ls
+Images may not be processed in the order they appear in the input list. Stage
+one processing is performed (if necessary) on all calibration images, then on
+all images in the input list. Any images which have already been trimmed, or
+which were taken in mono-readout mode will be skipped. Stage two processing is 
+then done sequentially on all images in the input list.
+.le
+.sh
+13. Processing Arithmetic
+The \fBquadproc\fR task has two data paths, one for real image pixel datatypes
+and one for short integer pixel datatype.  In addition internal arithmetic
+is based on the rules of FORTRAN.  For efficiency there is
+no checking for division by zero in the flat field calibration.
+The following rules describe the processing arithmetic and data paths.
+
+.ls (1)
+If the input, output, or any calibration image is of type real the
+real data path is used.  This means all image data is converted to
+real on input.  If all the images are of type short all input data
+is kept as short integers.  Thus, if all the images are of the same type
+there is no datatype conversion on input resulting in greater
+image I/O efficiency.
+.le
+.ls (2)
+In the real data path the processing arithmetic is always real and,
+if the output image is of short pixel datatype, the result
+is truncated.
+.le
+.ls (3)
+The overscan vector and the scale factors for dark count, flat field,
+iillumination, and fringe calibrations are always of type real.  Therefore,
+in the short data path any processing which includes these operations
+will be coerced to real arithmetic and the result truncated at the end
+of the computation.
+.le
+.sh
+14. In the Absence of Image Header Information
+The tasks in the \fBquad\fR package are most convenient to use when
+the CCD image type, subset, and exposure time are contained in the
+image header. This is true for all data obtained with Arcon.  The ability to
+redefine which header parameters contain this information makes it possible
+to use the package at many different observatories (see \fBinstruments\fR). 
+However, in the absence of any image header information the tasks may still
+be used effectively.  There are two ways to proceed.  One way is to use
+\fBccdhedit\fR to place the information in the image header.
+
+The second way is to specify the processing operations more explicitly
+than is needed when the header information is present.  The parameter
+\fIccdtype\fR is set to "" or to "none".  The calibration images are
+specified explicitly by task parameter since they cannot be recognized
+in the input list.  Only one subset at a time may be processed.
+
+If dark count and fringe corrections are to be applied the exposure
+times must be added to all the images.  Alternatively, the dark count
+and fringe images may be scaled explicitly for each input image.  This
+works because the exposure times default to 1 if they are not given in
+the image header.
+.ih
+EXAMPLES
+The user's \fBguide\fR presents a tutorial in the use of this task.
+
+1. In general all that needs to be done is to set the task parameters
+and enter
+
+	cl> quadproc *.imh &
+
+This will run in the background and process all images which have not
+been processed previously.
+.ih
+SEE ALSO
+quadformat, ccdproc, instruments, ccdtypes, flatfields, icfit, quad, guide,
+mkillumcor, mkskycor, mkfringecor
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/quadreadout.hlp b/noao/imred/quadred/src/quad/doc/quadreadout.hlp
new file mode 100644
index 00000000..355fdb61
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/quadreadout.hlp
@@ -0,0 +1,19 @@
+With Arcon it is possible to read out a CCD using more than one amplifier in
+parallel, leading to a substantial reduction in readout time.  Once properly
+reduced, such data is indistinguishable from that obtained when reading out
+through only a single amplifier.  However, the raw images are rather different
+and consequently must be processed somewhat differently. Firstly, each readout
+will typically have a slightly different, zero level, gain, and readout noise,
+and may differ slightly in its departures from perfect linearity. As a result
+both zero frames and uniformly illuminated exposures will show a characteristic
+chequer board pattern, the sections of the data read through each amplifier
+having different levels.  Secondly, there will be a separate overscan strip,
+used to monitor the zero level, for each readout. The location of these overscan
+strips in the raw frame depends on which amplifiers are used. When all four 
+amplifiers are used the four overscan regions form a vertical stripe down the
+centre of the raw image. A CCD read out through two amplifiers can have its
+two overscan strips, running side by side down the center of the picture; or 
+they may be one above the other, on the same side of the picture; or the strip
+for the upper and lower halves of the CCD can be at opposited sides of the
+image (in which case there will also be a horizontal displacement of the data
+in the two sections).
diff --git a/noao/imred/quadred/src/quad/doc/setinstrument.hlp b/noao/imred/quadred/src/quad/doc/setinstrument.hlp
new file mode 100644
index 00000000..410dd20f
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/setinstrument.hlp
@@ -0,0 +1,97 @@
+.help setinstrument Oct87 noao.imred.ccdred
+.ih
+NAME
+setinstrument -- Set instrument parameters
+.ih
+USAGE	
+setinstrument instrument
+.ih
+PARAMETERS
+.ls instrument
+Instrument identification for instrument parameters to be set.  If '?'
+then a list of the instrument identifiers is printed.
+.le
+.ls site = "kpno"
+Site ID.
+.le
+.ls directory = "ccddb$"
+Instrument directory containing instrument files.  The instrument files
+are found in the subdirectory given by the site ID. 
+.le
+.ls review = yes
+Review the instrument parameters?  If yes then \fBeparam\fR is run for
+the parameters of \fBccdred\fR and \fBccdproc\fR.
+.le
+.ls query
+Parameter query if initial instrument is not found.
+.le
+.ih
+DESCRIPTION
+The purpose of the task is to allow the user to easily set default
+parameters for a new instrument.  The default parameters are generally
+defined by support personal in an instrument directory for a particular
+site.  The instrument directory is the concatenation of the specified
+directory and the site.  For example if the directory is "ccddb$" and
+the site is "kpno" then the instrument directory is "ccddb$kpno/".
+The user may have his own set of instrument files in a local directory.
+The current directory is used by setting the directory and site to the
+null string ("").
+
+The user specifies an instrument identifier.  This instrument may
+be specific to a particular observatory, telescope, instrument, and
+detector.  If the character '?' is specified or the instrument file is
+not found then a list of instruments
+in the instrument directory is produced by paging the file "instruments.men".
+The task then performs the following operations:
+.ls (1)
+If an instrument translation file with the name given by the instrument
+ID and the extension ".dat" is found then the instrument translation
+file parameter, \fIccdred.instrument\fR, is set to this file.
+If it does not exist then the user is queried again.  Note that a
+null instrument, "", is allowed to set no translation file.
+.le
+.ls (2)
+If an instrument setup script with the name given by the instrument ID
+and the extension ".cl" is found then the commands in the file are
+executed (using the command \fIcl < script\fR.  This script generally
+sets default parameters.
+.le
+.ls (3)
+If the review flag is set the task \fBeparam\fR is run to allow the user
+to examine and modify the parameters for the package \fBccdred\fR and task
+\fBccdproc\fR.
+.le
+.ih
+EXAMPLES
+1. To get a list of the instruments;
+
+.nf
+	cl> setinstrument ?
+	[List of instruments]
+
+2. To set the instrument and edit the processing parameters:
+
+	cl> setinstrument ccdlink
+	[Edit CCDRED parameters]
+	[Edit CCDPROC parameters]
+
+3. To use your own instrument translation file and/or setup script in
+your working directory.
+
+	cl> setinst.site=""
+	cl> setinst.dir=""
+	cl> setinst myinstrument
+
+To make these files see help under \fBinstruments\fR.  Copying and modifying
+system files is also straightforward.
+
+	cl> copy ccddb$kpno/fits.dat .
+	cl> edit fits.dat
+	cl> setinst.site=""
+	cl> setinst.dir=""
+	cl> setinst fits
+.fi
+.ih
+SEE ALSO
+instruments, ccdred, ccdproc
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/subsets.hlp b/noao/imred/quadred/src/quad/doc/subsets.hlp
new file mode 100644
index 00000000..2823bd6d
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/subsets.hlp
@@ -0,0 +1,97 @@
+.help subsets Jun87 noao.imred.ccdred
+.ih
+NAME
+subsets -- Description of CCD subsets
+.ih
+DESCRIPTION
+The \fBccdred\fR package groups observation into subsets.
+The image header parameter used to identify the subsets is defined
+in the instrument translation file (see help for \fBinstruments\fR).
+For example to select subsets by the header parameter "filters" the
+instrument translation file would contain the line:
+
+	subset	filters
+
+Observations are generally grouped into subsets based on a common
+instrument configuration such as a filter, aperture mask,
+grating setting, etc.  This allows combining images from several
+different subsets automatically and applying the appropriate
+flat field image when processing the observations.  For example
+if the subsets are by filter then \fBflatcombine\fR will search
+through all the images, find the flat field images (based on the
+CCD type parameter), and combine the flat field images from
+each filter separately.  Then when processing the images the
+flat field with the same filter as the observation is used.
+
+Each subset is assigned a short identifier.  This is listed when
+using \fBccdlist\fR and is appended to a root name when combining
+images.  Because the subset parameter in the image header may be
+any string there must be a mapping applied to generate unique
+identifiers.  This mapping is defined in the file given by
+the package parameter \fIccdred.ssfile\fR.  The file consists of
+lines with two fields:
+
+	'subset string'	subset_id
+
+where the subset string is the image header string and the subset_id is
+the identifier.  A field must be quoted if it contains blanks.  The
+user may create this file but generally it is created by the tasks.  The
+tasks use the first word of the subset string as the default identifier
+and a number is appended if the first word is not unique.  The
+following steps define the subset identifier:
+
+.ls (1)
+Search the subset file, if present, for a matching subset string and
+use the defined subset identifier.
+.le
+.ls (2)
+If there is no matching subset string use the first word of the
+image header subset string and, if it is not unique,
+add successive integers until it is unique.
+.le
+.ls (3)
+If the identifier is not in the subset file create the file and add an
+entry if necessary.
+.le
+.ih
+EXAMPLES
+1. The subset file is "subsets" (the default).  The subset parameter is
+translated to "f1pos" in the image header (the old NOAO CCD parameter)
+which is an integer filter position.  After running a task, say
+"ccdlist *.imh" to cause all filters to be checked, the subset file contains:
+
+.nf
+	'2'	2
+	'5'	5
+	'3'	3
+.fi
+
+The order reflects the order in which the filters were encountered.
+Suppose the user wants to have more descriptive names then the subset
+file can be created or edited to the form:
+
+.nf
+	'2'	U
+	'3'	B
+	'4'	V
+.fi
+
+(This is only an example and does not mean these are standard filters.)
+
+2. As another example suppose the image header parameter is "filter" and
+contains more descriptive strings.  The subset file might become:
+
+.nf
+	'GG 385 Filter'	GG
+	'GG 495 Filter'	GG1
+	'RG 610 Filter'	RG
+	'H-ALPHA'	H_ALPHA
+.fi
+
+In this case use of the first word was not very good but it is unique.
+It is better if the filters are encoded with the thought that the first
+word will be used by \fBccdred\fR; it should be short and unique.
+.ih
+SEE ALSO
+instruments
+.endhelp
diff --git a/noao/imred/quadred/src/quad/doc/zerocombine.hlp b/noao/imred/quadred/src/quad/doc/zerocombine.hlp
new file mode 100644
index 00000000..ad1b021d
--- /dev/null
+++ b/noao/imred/quadred/src/quad/doc/zerocombine.hlp
@@ -0,0 +1,127 @@
+.help zerocombine Sep93 arcon.quad
+.ih
+NAME
+zerocombine -- Combine and process zero level images
+.ih
+USAGE
+zerocombine input
+.ih
+PARAMETERS
+.ls input
+List of zero level images to combine.  The \fIccdtype\fR parameter
+may be used to select the zero level images from a list containing all
+types of data.
+.le
+.ls output = "Zero"
+Output zero level root image name.
+.le
+.ls combine = "average" (average|median)
+Type of combining operation performed on the final set of pixels (after
+rejection).  The choices are
+"average" or "median".  The median uses the average of the two central
+values when the number of pixels is even.
+.le
+.ls reject = "minmax" (none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip)
+Type of rejection operation.  See \fBcombine\fR for details.
+.le
+.ls ccdtype = "zero"
+CCD image type to combine.  If no image type is given then all input images
+are combined.
+.le
+.ls process = no
+Process the input images before combining?
+.le
+.ls delete = no
+Delete input images after combining?  Only those images combined are deleted.
+.le
+.ls clobber = no
+Clobber existing output images?
+.le
+.ls scale = "none" (none|mode|median|mean|exposure)
+Multiplicative image scaling to be applied.  The choices are none, scale
+by the mode, median, or mean of the specified statistics section, or scale
+by the exposure time given in the image header.
+.le
+.ls statsec = ""
+Section of images to use in computing image statistics for scaling.
+If no section is given then the entire region of the image is
+sampled (for efficiency the images are sampled if they are big enough).
+.le
+
+.ce
+Algorithm Parameters
+.ls nlow = 0,  nhigh = 1 (minmax)
+The number of low and high pixels to be rejected by the "minmax" algorithm.
+.le
+.ls nkeep = 1
+The minimum number of pixels to retain or the maximum number to reject
+when using the clipping algorithms (ccdclip, crreject, sigclip,
+avsigclip, or pclip).  When given as a positive value this is the minimum
+number to keep.  When given as a negative value the absolute value is
+the maximum number to reject.  This is actually converted to a number
+to keep by adding it to the number of images.
+.le
+.ls mclip = yes (ccdclip, crreject, sigclip, avsigcliip)
+Use the median as the estimate for the true intensity rather than the
+average with high and low values excluded in the "ccdclip", "crreject",
+"sigclip", and "avsigclip" algorithms?  The median is a better estimator
+in the presence of data which one wants to reject than the average.
+However, computing the median is slower than the average.
+.le
+.ls lsigma = 3., hsigma = 3. (ccdclip, crreject, sigclip, avsigclip, pclip)
+Low and high sigma clipping factors for the "ccdclip", "crreject", "sigclip",
+"avsigclip", and "pclip" algorithms.  They multiply a "sigma" factor
+produced by the algorithm to select a point below and above the average or
+median value for rejecting pixels.  The lower sigma is ignored for the
+"crreject" algorithm.
+.le
+.ls rdnoise = "0.", gain = "1.", snoise = "0." (ccdclip, crreject)
+CCD readout noise in electrons, gain in electrons/DN, and sensitivity noise
+as a fraction.  These parameters are used with the "ccdclip" and "crreject"
+algorithms.  The values may be either numeric or an image header keyword
+which contains the value.
+.le
+.ls pclip = -0.5 (pclip)
+Percentile clipping algorithm parameter.  If greater than
+one in absolute value then it specifies a number of pixels above or
+below the median to use for computing the clipping sigma.  If less
+than one in absolute value then it specifies the fraction of the pixels
+above or below the median to use.  A positive value selects a point
+above the median and a negative value selects a point below the median.
+The default of -0.5 selects approximately the quartile point.
+See \fBcombine\fR for further details.
+.le
+.ls blank = 0.
+Output value to be used when there are no pixels.
+.le
+.ih
+DESCRIPTION
+The zero level images in the input image list are combined.
+The input images may be processed first if desired.
+The original images may be deleted automatically if desired.
+
+This task is a script which applies \fBquadproc\fR and \fBcombine\fR.  The
+parameters and combining algorithms are described in detail in the help for
+\fBcombine\fR.  This script has default parameters specifically set for
+zero level images and simplifies the combining parameters.  There are other
+combining options not included in this task.  For these additional
+features, such as thresholding, offseting, masking, and projecting, use
+\fBcombine\fR.
+
+The version of \fBzerocombine\fR in the \fBquad\fR package differs from that
+in \fBccdred\fR in that \fBquadproc\fR rather than \fBccdproc\fR is used to
+process the images if this is requested. The \fBquad\fR version MUST be
+used if process=yes and the input list contains any multi-readout images which
+have not been overscan corrected and trimmed.
+
+.ih
+EXAMPLES
+1. The image data contains four zero level images.
+To automatically select them and combine them as a background job
+using the default combining algorithm:
+
+    cl> zerocombine ccd*.imh&
+.ih
+SEE ALSO
+quadproc, combine
+.endhelp
diff --git a/noao/imred/quadred/src/quad/gainmeasure.par b/noao/imred/quadred/src/quad/gainmeasure.par
new file mode 100644
index 00000000..00e183af
--- /dev/null
+++ b/noao/imred/quadred/src/quad/gainmeasure.par
@@ -0,0 +1,6 @@
+flat1,s,a,"",,,First   high level exposure
+flat2,s,a,"",,,Second  high level exposure
+zero1,s,a,"",,,First   zero level exposure
+zero2,s,a,"",,,Second  zero level exposure
+section,s,a,"",,,Image section for calculations
+print_headers,b,h,yes,,,Print column headers
diff --git a/noao/imred/quadred/src/quad/gainmeasure.x b/noao/imred/quadred/src/quad/gainmeasure.x
new file mode 100644
index 00000000..592cf7cf
--- /dev/null
+++ b/noao/imred/quadred/src/quad/gainmeasure.x
@@ -0,0 +1,170 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+define  OPT_REFLECT     4
+
+# GAINMEASURE -- Calculate the gain (e/ADU) and RON of a CCD using the CTIO
+# (Bruce Attwood) algorithm.
+# Input are a pair of high signal level exposures (Flat1, Flat2) and a pair of
+# zero exposures (Zero1, Zero2). We then calculate:
+#
+#    epadu = <Flat1> + <Flat2> - (<Zero1> + <Zero2>) / var{Diff_F} - Var{Diff_Z}
+#    RON   = RMS {Diff_Z} * epadu / sqrt(2)
+#
+# Where:
+#
+#    diff_Z = Zero1 - Zero2
+#    diff_F = Flat1 - Flat2
+#
+# The statistics must be calculated for regions free of bad pixels and other
+# defects, and with reasonably uniform illumination. 
+
+procedure t_gainmeasure ()
+
+pointer	flat1, flat2		#TI High level images
+pointer	zero1, zero2		#TI Zero level images
+char	section[SZ_LINE]	#TI Section for calculation
+
+char	buffer[SZ_LINE]
+int	npix, x1, x2, y1, y2, amp
+pointer	sp, f1, f2, z1, z2, fd, zd, qg
+real	f1bar,   f2bar,   z1bar,   z2bar,   fdbar,   zdbar
+real	f1sigma, f2sigma, z1sigma, z2sigma, fdsigma, zdsigma
+real	div, epadu, ron
+bool	headers
+
+pointer	immap(), imgs2r()
+bool	clgetb(), quadsect()
+int	hdmaccf()
+
+begin
+        # Open instrument file
+        call clgstr    ("instrument",  buffer,  SZ_FNAME)
+        call hdmopen   (buffer)
+
+	# Map input images
+	call clgstr ("flat1",   buffer, SZ_LINE)
+	flat1 = immap (buffer,  READ_ONLY, 0)
+
+	call clgstr ("flat2",   buffer, SZ_LINE)
+	flat2 = immap (buffer,  READ_ONLY, 0)
+
+	call clgstr ("zero1",   buffer, SZ_LINE)
+	zero1 = immap (buffer,  READ_ONLY, 0)
+
+	call clgstr ("zero2",   buffer, SZ_LINE)
+	zero2 = immap (buffer,  READ_ONLY, 0)
+
+        # Get section over which measurement is to be made.
+        call clgstr ("section", section, SZ_LINE)
+
+	# See if headers are to be printed
+	headers = clgetb ("print_headers")
+
+        # Set-up quadgeom structure. We blithely assume all images are the same.
+        call quadalloc (qg)
+
+	if (hdmaccf (flat1, "HDR_REV") == NO) {
+	    call quadgeom  (flat1, qg, "", "")
+	} else {
+	    call qghdr2 (flat1, qg)
+	}
+#       call quaddump  (qg)
+
+	if (headers) {
+	    call printf ("#")
+	    do amp = 1, QG_NAMPS (qg) {
+		call printf ("%9wAmp%2s%5w")
+		    call pargstr (Memc[QG_AMPID (qg, amp)])
+	    }
+	    call printf ("\n")
+
+	    call printf ("#")
+	    do amp = 1, QG_NAMPS (qg) {
+		call printf ("%5wGain%4wRON%3w")
+	    }
+	    call printf ("\n")
+	    call printf ("#")
+	    do amp = 1, QG_NAMPS (qg) {
+		call printf ("%3w(e-/ADU)%2w(e-)%2w")
+	    }
+	    call printf ("\n")
+	}
+
+	call printf ("%1w")
+        do amp = 1, QG_NAMPS (qg) {
+ 
+            if (quadsect (qg, section, OPT_REFLECT, amp, x1, x2, y1, y2)) {
+
+		npix = (abs(y2 - y1) + 1) * (abs(x2 - x1) + 1)
+
+		# Allocate working arrays
+		call smark  (sp)
+		call salloc (fd, npix, TY_REAL)
+		call salloc (zd, npix, TY_REAL)
+
+		# Read data 
+		f1 = imgs2r (flat1, x1, x2, y1, y2)
+		f2 = imgs2r (flat2, x1, x2, y1, y2)
+		z1 = imgs2r (zero1, x1, x2, y1, y2)
+		z2 = imgs2r (zero2, x1, x2, y1, y2)
+
+		# Calculate differences
+		call asubr (Memr[f1], Memr[f2], Memr[fd], npix)
+		call asubr (Memr[z1], Memr[z2], Memr[zd], npix)
+
+		# Calculate means and standard deviations
+		call aavgr (Memr[f1], npix, f1bar, f1sigma)
+		call aavgr (Memr[f2], npix, f2bar, f2sigma)
+		call aavgr (Memr[z1], npix, z1bar, z1sigma)
+		call aavgr (Memr[z2], npix, z2bar, z2sigma)
+		call aavgr (Memr[fd], npix, fdbar, fdsigma)
+		call aavgr (Memr[zd], npix, zdbar, zdsigma)
+
+#		call eprintf ("f1bar=%g f1sigma=%g\n")
+#		    call pargr (f1bar)
+#		    call pargr (f1sigma)
+#		call eprintf ("f2bar=%g f2sigma=%g\n")
+#		    call pargr (f2bar)
+#		    call pargr (f2sigma)
+#		call eprintf ("z1bar=%g z1sigma=%g\n")
+#		    call pargr (z1bar)
+#		    call pargr (z1sigma)
+#		call eprintf ("z2bar=%g z2sigma=%g\n")
+#		    call pargr (z2bar)
+#		    call pargr (z2sigma)
+#		call eprintf ("fdbar=%g fdsigma=%g\n")
+#		    call pargr (fdbar)
+#		    call pargr (fdsigma)
+#		call eprintf ("zdbar=%g zdsigma=%g\n")
+#		    call pargr (zdbar)
+#		    call pargr (zdsigma)
+
+		div  = fdsigma**2 - zdsigma**2
+		if (div > 0.0) {
+		    epadu = ((f1bar + f2bar) - (z1bar + z2bar)) / div
+		    ron   = epadu * zdsigma / 1.41421356
+		} else {
+		    epadu = INDEF
+		    ron   = INDEF
+		}
+
+		# Print results
+		call printf ("%3w%6.2f%2w%6.2f%2w")
+		    call pargr (epadu)
+		    call pargr (ron)
+
+	    # Free working arrays
+	    call sfree (sp)
+
+	    }
+	}
+
+	call printf ("\n")
+
+	# Tidy up
+	call imunmap (flat1)
+	call imunmap (flat2)
+	call imunmap (zero1)
+	call imunmap (zero2)
+end
diff --git a/noao/imred/quadred/src/quad/hdrmap.com b/noao/imred/quadred/src/quad/hdrmap.com
new file mode 100644
index 00000000..5aa74185
--- /dev/null
+++ b/noao/imred/quadred/src/quad/hdrmap.com
@@ -0,0 +1,4 @@
+# Common for HDRMAP package.
+
+pointer	stp			# Symbol table pointer
+common	/hdmcom/ stp
diff --git a/noao/imred/quadred/src/quad/hdrmap.x b/noao/imred/quadred/src/quad/hdrmap.x
new file mode 100644
index 00000000..ebcb253e
--- /dev/null
+++ b/noao/imred/quadred/src/quad/hdrmap.x
@@ -0,0 +1,544 @@
+include	<error.h>
+include	<syserr.h>
+
+.help hdrmap
+.nf-----------------------------------------------------------------------------
+HDRMAP -- Map translation between task parameters and image header parameters.
+
+In order for tasks to be partially independent of the image header
+parameter names used by different instruments and observatories a
+translation is made between task parameters and image header
+parameters.  This translation is given in a file consisting of the task
+parameter name, the image header parameter name, and an optional
+default value.  This file is turned into a symbol table.  If the
+translation file is not found a null pointer is returned.  The package will
+then use the task parameter names directly.  Also if there is no
+translation given in the file for a particular parameter it is passed
+on directly.  If a parameter is not in the image header then the symbol
+table default value, if given, is returned.  This package is layered on
+the IMIO header package.
+
+	        hdmopen (fname)
+		hdmclose ()
+		hdmwrite (fname, mode)
+		hdmname (parameter, str, max_char)
+		hdmgdef (parameter, str, max_char)
+		hdmpdef (parameter, str, max_char)
+	  y/n = hdmaccf (im, parameter)
+		hdmgstr (im, parameter, str, max_char)
+	 ival = hdmgeti (im, parameter)
+	 rval = hdmgetr (im, parameter)
+		hdmpstr (im, parameter, str)
+		hdmputi (im, parameter, value)
+		hdmputr (im, parameter, value)
+		hdmgstp (stp)
+		hdmpstp (stp)
+		hdmdelf (im, parameter)
+		hdmparm (name, parameter, max_char)
+
+hdmopen  -- Open the translation file and map it into a symbol table pointer.
+hdmclose -- Close the symbol table pointer.
+hdmwrite -- Write out translation file.
+hdmname  -- Return the image header parameter name.
+hdmpname -- Put the image header parameter name.
+hdmgdef  -- Get the default value as a string (null if none).
+hdmpdef  -- Put the default value as a string.
+hdmaccf  -- Return whether the image header parameter exists (regardless of
+	    whether there is a default value).
+hdmgstr  -- Get a string valued parameter.  Return default value if not in the
+	    image header.  Return null string if no default or image value.
+hdmgeti  -- Get an integer valued parameter.  Return default value if not in
+	    the image header and error condition if no default or image value.
+hdmgetr  -- Get a real valued parameter.  Return default value if not in
+	    the image header or error condition if no default or image value.
+hdmpstr  -- Put a string valued parameter in the image header.
+hdmputi  -- Put an integer valued parameter in the image header.
+hdmputr  -- Put a real valued parameter in the image header.
+hdmgstp  -- Get the symbol table pointer to save it while another map is used.
+hdmpstp  -- Put the symbol table pointer to restore a map.
+hdmdelf  -- Delete a field.
+hdmparm  -- Return the parameter name corresponding to an image header name.
+.endhelp -----------------------------------------------------------------------
+
+# Symbol table definitions.
+define	LEN_INDEX	32		# Length of symtab index
+define	LEN_STAB	1024		# Length of symtab string buffer
+define	SZ_SBUF		128		# Size of symtab string buffer
+
+define	SZ_NAME		79		# Size of translation symbol name
+define	SZ_DEFAULT	79		# Size of default string
+define	SYMLEN		80		# Length of symbol structure
+
+# Symbol table structure
+define	NAME		Memc[P2C($1)]		# Translation name for symbol
+define	DEFAULT		Memc[P2C($1+40)]	# Default value of parameter
+
+
+# HDMOPEN -- Open the translation file and map it into a symbol table pointer.
+
+procedure hdmopen (fname)
+
+char	fname[ARB]		# Image header map file
+
+int	fd, open(), fscan(), nscan(), errcode()
+pointer	sp, parameter, sym, stopen(), stenter()
+include	"hdrmap.com"
+
+begin
+	# Create an empty symbol table.
+	stp = stopen (fname, LEN_INDEX, LEN_STAB, SZ_SBUF)
+
+	# Return if file not found.
+	iferr (fd = open (fname, READ_ONLY, TEXT_FILE)) {
+	    if (errcode () != SYS_FNOFNAME)
+		call erract (EA_WARN)
+	    return
+	}
+
+	call smark (sp)
+	call salloc (parameter, SZ_NAME, TY_CHAR)
+
+	# Read the file an enter the translations in the symbol table.
+	while (fscan(fd) != EOF) {
+	    call gargwrd (Memc[parameter], SZ_NAME)
+	    if ((nscan() == 0) || (Memc[parameter] == '#'))
+		next
+	    sym = stenter (stp, Memc[parameter], SYMLEN)
+	    call gargwrd (NAME(sym), SZ_NAME)
+	    call gargwrd (DEFAULT(sym), SZ_DEFAULT)
+	}
+
+	call close (fd)
+	call sfree (sp)
+end
+
+
+# HDMCLOSE -- Close the symbol table pointer.
+
+procedure hdmclose ()
+
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    call stclose (stp)
+end
+
+
+# HDMWRITE -- Write out translation file.
+
+procedure hdmwrite (fname, mode)
+
+char	fname[ARB]		# Image header map file
+int	mode			# Access mode (APPEND, NEW_FILE)
+
+int	fd, open(), stridxs()
+pointer	sym, sthead(), stnext(), stname()
+errchk	open
+include	"hdrmap.com"
+
+begin
+	# If there is no symbol table do nothing.
+	if (stp == NULL)
+	    return
+
+	fd = open (fname, mode, TEXT_FILE)
+
+	sym = sthead (stp)
+	for (sym = sthead (stp); sym != NULL; sym = stnext (stp, sym)) {
+	    if (stridxs (" 	", Memc[stname (stp, sym)]) > 0)
+		call fprintf (fd, "'%s'%30t")
+	    else
+		call fprintf (fd, "%s%30t")
+	    call pargstr (Memc[stname (stp, sym)])
+	    if (stridxs (" 	", NAME(sym)) > 0)
+		call fprintf (fd, " '%s'%10t")
+	    else
+		call fprintf (fd, " %s%10t")
+	    call pargstr (NAME(sym))
+	    if (DEFAULT(sym) != EOS) {
+		if (stridxs (" 	", DEFAULT(sym)) > 0)
+		    call fprintf (fd, " '%s'")
+		else
+		    call fprintf (fd, " %s")
+		call pargstr (DEFAULT(sym))
+	    }
+	    call fprintf (fd, "\n")
+	}
+
+	call close (fd)
+end
+
+
+# HDMNAME -- Return the image header parameter name
+
+procedure hdmname (parameter, str, max_char)
+
+char	parameter[ARB]		# Parameter name
+char	str[max_char]		# String containing mapped parameter name
+int	max_char		# Maximum characters in string
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call strcpy (NAME(sym), str, max_char)
+	else
+	    call strcpy (parameter, str, max_char)
+end
+
+
+# HDMPNAME -- Put the image header parameter name
+
+procedure hdmpname (parameter, str)
+
+char	parameter[ARB]		# Parameter name
+char	str[ARB]		# String containing mapped parameter name
+
+pointer	sym, stfind(), stenter()
+include	"hdrmap.com"
+
+begin
+	if (stp == NULL)
+	    return
+
+	sym = stfind (stp, parameter)
+	if (sym == NULL) {
+	    sym = stenter (stp, parameter, SYMLEN)
+	    DEFAULT(sym) = EOS
+	}
+
+	call strcpy (str, NAME(sym), SZ_NAME)
+end
+
+
+# HDMGDEF -- Get the default value as a string (null string if none).
+
+procedure hdmgdef (parameter, str, max_char)
+
+char	parameter[ARB]		# Parameter name
+char	str[max_char]		# String containing default value
+int	max_char		# Maximum characters in string
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call strcpy (DEFAULT(sym), str, max_char)
+	else
+	    str[1] = EOS
+end
+
+
+# HDMPDEF -- PUt the default value as a string.
+
+procedure hdmpdef (parameter, str)
+
+char	parameter[ARB]		# Parameter name
+char	str[ARB]		# String containing default value
+
+pointer	sym, stfind(), stenter()
+include	"hdrmap.com"
+
+begin
+	if (stp == NULL)
+	    return
+
+	sym = stfind (stp, parameter)
+	if (sym == NULL) {
+	    sym = stenter (stp, parameter, SYMLEN)
+	    call strcpy (parameter, NAME(sym), SZ_NAME)
+	}
+
+	call strcpy (str, DEFAULT(sym), SZ_DEFAULT)
+end
+
+
+# HDMACCF -- Return whether the image header parameter exists (regardless of
+# whether there is a default value).
+
+int procedure hdmaccf (im, parameter)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+
+int	imaccf()
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    return (imaccf (im, NAME(sym)))
+	else
+	    return (imaccf (im, parameter))
+end
+
+
+# HDMGSTR -- Get a string valued parameter.  Return default value if not in
+# the image header.  Return null string if no default or image value.
+
+procedure hdmgstr (im, parameter, str, max_char)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+char	str[max_char]		# String value to return
+int	max_char		# Maximum characters in returned string
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL) {
+	    iferr (call imgstr (im, NAME(sym), str, max_char))
+		call strcpy (DEFAULT(sym), str, max_char)
+	} else {
+	    iferr (call imgstr (im, parameter, str, max_char))
+		str[1] = EOS
+	}
+end
+
+
+# HDMGETR -- Get a real valued parameter.  Return default value if not in
+# the image header.  Return error condition if no default or image value.
+
+real procedure hdmgetr (im, parameter)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+
+int	ip, ctor()
+real	value, imgetr()
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL) {
+	    iferr (value = imgetr (im, NAME(sym))) {
+		ip = 1
+		if (ctor (DEFAULT(sym), ip, value) == 0)
+		    call error (0, "HDMGETR: No value found")
+	    }
+	} else
+	    value = imgetr (im, parameter)
+
+	return (value)
+end
+
+
+# HDMGETI -- Get an integer valued parameter.  Return default value if not in
+# the image header.  Return error condition if no default or image value.
+
+int procedure hdmgeti (im, parameter)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+
+int	ip, ctoi()
+int	value, imgeti()
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL) {
+	    iferr (value = imgeti (im, NAME(sym))) {
+		ip = 1
+		if (ctoi (DEFAULT(sym), ip, value) == 0)
+		    call error (0, "HDMGETI: No value found")
+	    }
+	} else
+	    value = imgeti (im, parameter)
+
+	return (value)
+end
+
+
+# HDMPSTR -- Put a string valued parameter in the image header.
+
+procedure hdmpstr (im, parameter, str)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+char	str[ARB]		# String value
+
+int	imaccf(), imgftype()
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL) {
+	    if (imaccf (im, NAME(sym)) == YES)
+	        if (imgftype (im, NAME(sym)) != TY_CHAR)
+		    call imdelf (im, NAME(sym))
+	    call imastr (im, NAME(sym), str)
+	} else {
+	    if (imaccf (im, parameter) == YES)
+	        if (imgftype (im, parameter) != TY_CHAR)
+		    call imdelf (im, parameter)
+	    call imastr (im, parameter, str)
+	}
+end
+
+
+# HDMPUTI -- Put an integer valued parameter in the image header.
+
+procedure hdmputi (im, parameter, value)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+int	value			# Integer value to put
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call imaddi (im, NAME(sym), value)
+	else
+	    call imaddi (im, parameter, value)
+end
+
+
+# HDMPUTR -- Put a real valued parameter in the image header.
+
+procedure hdmputr (im, parameter, value)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+real	value			# Real value to put
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call imaddr (im, NAME(sym), value)
+	else
+	    call imaddr (im, parameter, value)
+end
+
+
+# HDMGSTP -- Get the symbol table pointer to save a translation map.
+# The symbol table is restored with HDMPSTP.
+
+procedure hdmgstp (ptr)
+
+pointer	ptr		# Symbol table pointer to return
+
+include	"hdrmap.com"
+
+begin
+	ptr = stp
+end
+
+
+# HDMPSTP -- Put a symbol table pointer to restore a header map.
+# The symbol table is optained with HDMGSTP.
+
+procedure hdmpstp (ptr)
+
+pointer	ptr		# Symbol table pointer to restore
+
+include	"hdrmap.com"
+
+begin
+	stp = ptr
+end
+
+
+# HDMDELF -- Delete a field.  It is an error if the field does not exist.
+
+procedure hdmdelf (im, parameter)
+
+pointer	im			# IMIO pointer
+char	parameter[ARB]		# Parameter name
+
+pointer	sym, stfind()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = stfind (stp, parameter)
+	else
+	    sym = NULL
+
+	if (sym != NULL)
+	    call imdelf (im, NAME(sym))
+	else
+	    call imdelf (im, parameter)
+end
+
+
+# HDMPARAM -- Get parameter given the image header name.
+
+procedure hdmparam (name, parameter, max_char)
+
+char	name[ARB]		# Image header name
+char	parameter[max_char]	# Parameter
+int	max_char		# Maximum size of parameter string
+
+bool	streq()
+pointer	sym, sthead(), stname(), stnext()
+include	"hdrmap.com"
+
+begin
+	if (stp != NULL)
+	    sym = sthead (stp)
+	else
+	    sym = NULL
+
+	while (sym != NULL) {
+	    if (streq (NAME(sym), name)) {
+		call strcpy (Memc[stname(stp, sym)], parameter, max_char)
+		return
+	    }
+	    sym = stnext (stp, sym)
+	}
+	call strcpy (name, parameter, max_char)
+end
diff --git a/noao/imred/quadred/src/quad/irlincor.par b/noao/imred/quadred/src/quad/irlincor.par
new file mode 100644
index 00000000..77739715
--- /dev/null
+++ b/noao/imred/quadred/src/quad/irlincor.par
@@ -0,0 +1,12 @@
+# irlincor parameter file
+input,s,a,"",,,Input  images
+output,s,a,"",,,Output images
+section,s,h,"",,,Image section to correct
+coeff1,r,h,1.0,,,First coefficient of correction equation
+coeff2,r,h,0.0,,,Second coefficient of correction equation
+coeff3,r,h,0.0,,,Third coefficient of correction equation
+coeff4,r,h,0.0,,,Fourth coefficient of correction equation
+coeff5,r,h,0.0,,,Fifth coefficient of correction equation
+coeff6,r,h,0.0,,,Sixth coefficient of correction equation
+coeff7,r,h,0.0,,,Seventh coefficient of correction equation
+maxadu,r,h,INDEF,0,,Maximum number of ADU
diff --git a/noao/imred/quadred/src/quad/mkpkg b/noao/imred/quadred/src/quad/mkpkg
new file mode 100644
index 00000000..9243e633
--- /dev/null
+++ b/noao/imred/quadred/src/quad/mkpkg
@@ -0,0 +1,56 @@
+# QUAD mkpkg file (Mon Mar 28 14:07:29 CST 1994)
+
+$call	relink
+$exit
+
+update:
+	$call	relink
+	$call	install
+	;
+
+relink:
+	$update	libpkg.a
+	$omake	x_quad.x
+	$link	x_quad.o libpkg.a -lxtools -o xx_quad.e
+	;
+
+install:
+	$move	xx_quad.e noaobin$x_quad.e
+	;
+
+libpkg.a:
+
+	$ifolder (qsplits.x, qsplit.gx) $generic -k -t silrd qsplit.gx $endif
+
+	ccddelete.x	
+	ccdgetparam.x	
+	ccdlog.x	
+	ccdprcselect.x	"ccdtypes.h"
+	ccdsection.x	<ctype.h>
+	ccdssselect.x	"ccdtypes.h"
+	ccdsubsets.x	
+	ccdtypes.x	"ccdtypes.h"
+	gainmeasure.x	"quadgeom.h" <imhdr.h>
+	hdrmap.x	"hdrmap.com" <error.h> <syserr.h>
+	qghdr2.x	"quadgeom.h" <imhdr.h>
+	qguser.x	"quadgeom.h"
+	qpcalimage.x	"ccdtypes.h" <error.h> <imset.h>
+	qpselect.x	"ccdtypes.h"
+	qsplitd.x	"quadgeom.h" <imhdr.h>
+	qspliti.x	"quadgeom.h" <imhdr.h>
+	qsplitl.x	"quadgeom.h" <imhdr.h>
+	qsplitr.x	"quadgeom.h" <imhdr.h>
+	qsplits.x	"quadgeom.h" <imhdr.h>
+	quadalloc.x	"quadgeom.h" <imhdr.h>
+	quaddelete.x	"quadgeom.h"
+	quadgeom.x	"quadgeom.h" <imhdr.h>
+	quadgeomred.x	"quadgeom.h" <imhdr.h>
+	quadjoin.x	"quadgeom.h" <imhdr.h>
+	quadmap.x	"quadgeom.h" <error.h> <imhdr.h>
+	quadmerge.x	"quadgeom.h" <imhdr.h>
+	quadscale.x	"quadgeom.h" <imhdr.h>
+	quadsections.x	"quadgeom.h" <imhdr.h>
+	quadsplit.x	"quadgeom.h" <imhdr.h>
+	test.x		"quadgeom.h"
+	timelog.x	<time.h>
+	;
diff --git a/noao/imred/quadred/src/quad/new.par b/noao/imred/quadred/src/quad/new.par
new file mode 100644
index 00000000..8700d447
--- /dev/null
+++ b/noao/imred/quadred/src/quad/new.par
@@ -0,0 +1,8 @@
+input,s,a,"",,,Input image name
+instrument,s,a,"",,,Instrument file
+xtrim1,i,h,0,0,,
+xtrim2,i,h,0,0,,
+ytrim1,i,h,0,0,,
+ytrim2,i,h,0,0,,
+xskip1,i,h,0,0,,
+xskip2,i,h,0,0,,
diff --git a/noao/imred/quadred/src/quad/old.par b/noao/imred/quadred/src/quad/old.par
new file mode 100644
index 00000000..e77315b3
--- /dev/null
+++ b/noao/imred/quadred/src/quad/old.par
@@ -0,0 +1,2 @@
+input,s,a,"",,,Input image name
+instrument,s,a,"",,,Instrument file
diff --git a/noao/imred/quadred/src/quad/qccdproc.par b/noao/imred/quadred/src/quad/qccdproc.par
new file mode 100644
index 00000000..f20207a7
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qccdproc.par
@@ -0,0 +1,43 @@
+images,s,a,"",,,List of CCD images to correct
+ccdtype,s,h,"",,,CCD image type to correct
+max_cache,i,h,0,0,,Maximum image caching memory (in Mbytes)
+noproc,b,h,no,,,"List processing steps only?
+"
+fixpix,b,h,yes,,,Fix bad CCD lines and columns?
+overscan,b,h,yes,,,Apply overscan strip correction?
+trim,b,h,yes,,,Trim the image?
+zerocor,b,h,yes,,,Apply zero level correction?
+darkcor,b,h,no,,,Apply dark count correction?
+flatcor,b,h,yes,,,Apply flat field correction?
+illumcor,b,h,no,,,Apply illumination correction?
+fringecor,b,h,no,,,Apply fringe correction?
+readcor,b,h,no,,,Convert zero level image to readout correction?
+scancor,b,h,no,,,"Convert flat field image to scan correction?
+"
+readaxis,s,h,"line","column|line",, Read out axis (column|line)
+fixfile,s,h,"",,,File describing the bad lines and columns
+biassec,s,h,"",,,Overscan strip image section
+trimsec,s,h,"",,,Trim data section
+zero,s,h,"",,,Zero level calibration image
+dark,s,h,"",,,Dark count calibration image
+flat,s,h,"",,,Flat field images
+illum,s,h,"",,,Illumination correction images
+fringe,s,h,"",,,Fringe correction images
+minreplace,r,h,1.,,,Minimum flat field value
+scantype,s,h,"shortscan","shortscan|longscan",,Scan type (shortscan|longscan)
+nscan,i,h,1,1,,"Number of short scan lines
+"
+interactive,b,h,no,,,Fit overscan interactively?
+function,s,h,"legendre",,,Fitting function
+order,i,h,1,1,,Number of polynomial terms or spline pieces
+sample,s,h,"*",,,Sample points to fit
+naverage,i,h,1,,,Number of sample points to combine
+niterate,i,h,1,0,,Number of rejection iterations
+low_reject,r,h,3.,0.,,Low sigma rejection factor
+high_reject,r,h,3.,0.,,High sigma rejection factor
+grow,r,h,0.,0.,,"Rejection growing radius
+"
+verbose,b,h,)_.verbose,,,Print log information to the standard output?
+logfile,f,h,)_.logfile,,,Text log file
+backup,s,h,)_.backup,,,Backup directory or prefix
+output,s,h,"",,,Not used
diff --git a/noao/imred/quadred/src/quad/qdarkcombine.cl b/noao/imred/quadred/src/quad/qdarkcombine.cl
new file mode 100644
index 00000000..7f0ef6e7
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qdarkcombine.cl
@@ -0,0 +1,48 @@
+# DARKCOMBINE -- Process and combine dark count CCD images.
+
+procedure darkcombine (input)
+
+string	input			{prompt="List of dark images to combine"}
+file	output="Dark"		{prompt="Output dark image root name"}
+string	combine="average"	{prompt="Type of combine operation",
+				 enum="average|median"}
+string	reject="avsigclip"	{prompt="Type of rejection",
+		enum="none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip"}
+string	ccdtype="dark"	{prompt="CCD image type to combine"}
+bool	process=yes	{prompt="Process images before combining?"}
+bool	delete=no	{prompt="Delete input images after combining?"}
+bool	clobber=no	{prompt="Clobber existing output image?"}
+string	scale="exposure"	{prompt="Image scaling",
+			 enum="none|mode|median|mean|exposure"}
+string	statsec=""	{prompt="Image section for computing statistics"}
+int	nlow=1		{prompt="minmax: Number of low pixels to reject"}
+int	nhigh=1		{prompt="minmax: Number of high pixels to reject"}
+int	nkeep=1		{prompt="Minimum to keep (pos) or maximum to reject (neg)"}
+bool	mclip=yes	{prompt="Use median in sigma clipping algorithms?"}
+real	lsigma=3.	{prompt="Lower sigma clipping factor"}
+real	hsigma=3.	{prompt="Upper sigma clipping factor"}
+string	rdnoise="0."	{prompt="ccdclip: CCD readout noise (electrons)"}
+string	gain="1."	{prompt="ccdclip: CCD gain (electrons/DN)"}
+string	snoise="0."	{prompt="ccdclip: Sensitivity noise (fraction)"}
+real	pclip=-0.5	{prompt="pclip: Percentile clipping parameter"}
+real	blank=0.	{prompt="Value if there are no pixels"}
+
+begin
+	string	ims
+
+	ims = input
+
+	# Process images first if desired.
+	if (process == YES)
+	    quadproc (ims, ccdtype=ccdtype)
+
+	# Combine the dark images.
+	combine (ims, output=output, plfile="", sigma="", combine=combine,
+	    reject=reject, ccdtype=ccdtype, subsets=no, delete=delete,
+	    clobber=clobber, project=no, outtype="real", offsets="none",
+	    masktype="none", blank=blank, scale=scale, zero="none", weight=no,
+	    statsec=statsec, lthreshold=INDEF, hthreshold=INDEF, nlow=nlow,
+	    nhigh=nhigh, nkeep=nkeep, mclip=mclip, lsigma=lsigma, hsigma=hsigma,
+	    rdnoise=rdnoise, gain=gain, snoise=snoise, sigscale=0.1,
+	    pclip=pclip, grow=0)
+end
diff --git a/noao/imred/quadred/src/quad/qflatcombine.cl b/noao/imred/quadred/src/quad/qflatcombine.cl
new file mode 100644
index 00000000..7a0eb7ce
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qflatcombine.cl
@@ -0,0 +1,49 @@
+# FLATCOMBINE -- Process and combine flat field CCD images.
+
+procedure flatcombine (input)
+
+string	input			{prompt="List of flat field images to combine"}
+file	output="Flat"		{prompt="Output flat field root name"}
+string	combine="average"	{prompt="Type of combine operation",
+				 enum="average|median"}
+string	reject="avsigclip"	{prompt="Type of rejection",
+		enum="none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip"}
+string	ccdtype="flat"	{prompt="CCD image type to combine"}
+bool	process=yes	{prompt="Process images before combining?"}
+bool	subsets=yes	{prompt="Combine images by subset parameter?"}
+bool	delete=no	{prompt="Delete input images after combining?"}
+bool	clobber=no	{prompt="Clobber existing output image?"}
+string	scale="mode"	{prompt="Image scaling",
+			 enum="none|mode|median|mean|exposure"}
+string	statsec=""	{prompt="Image section for computing statistics"}
+int	nlow=1		{prompt="minmax: Number of low pixels to reject"}
+int	nhigh=1		{prompt="minmax: Number of high pixels to reject"}
+int	nkeep=1		{prompt="Minimum to keep (pos) or maximum to reject (neg)"}
+bool	mclip=yes	{prompt="Use median in sigma clipping algorithms?"}
+real	lsigma=3.	{prompt="Lower sigma clipping factor"}
+real	hsigma=3.	{prompt="Upper sigma clipping factor"}
+string	rdnoise="0."	{prompt="ccdclip: CCD readout noise (electrons)"}
+string	gain="1."	{prompt="ccdclip: CCD gain (electrons/DN)"}
+string	snoise="0."	{prompt="ccdclip: Sensitivity noise (fraction)"}
+real	pclip=-0.5	{prompt="pclip: Percentile clipping parameter"}
+real	blank=1.	{prompt="Value if there are no pixels"}
+
+begin
+	string	ims
+
+	ims = input
+
+	# Process images first if desired.
+	if (process == YES)
+	    quadproc (ims, ccdtype=ccdtype)
+
+	# Combine the flat field images.
+	combine (ims, output=output, plfile="", sigma="", combine=combine,
+	    reject=reject, ccdtype=ccdtype, subsets=subsets, delete=delete,
+	    clobber=clobber, project=no, outtype="real", offsets="none",
+	    masktype="none", blank=blank, scale=scale, zero="none", weight=no,
+	    statsec=statsec, lthreshold=INDEF, hthreshold=INDEF, nlow=nlow,
+	    nhigh=nhigh, nkeep=nkeep, mclip=mclip, lsigma=lsigma, hsigma=hsigma,
+	    rdnoise=rdnoise, gain=gain, snoise=snoise, sigscale=0.1,
+	    pclip=pclip, grow=0)
+end
diff --git a/noao/imred/quadred/src/quad/qghdr2.x b/noao/imred/quadred/src/quad/qghdr2.x
new file mode 100644
index 00000000..6a483a5b
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qghdr2.x
@@ -0,0 +1,216 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+define	SZ_KEYWRD	8		# Chars in FITS keyword
+
+# QGHDR2 -- Set up section information in quadgeom structure based on 
+# information in the image header.
+
+procedure qghdr2 (im, qg)
+
+pointer	im			#I  Pointer to input image.
+pointer	qg			#IO Pointer to open quadgeom structure.
+
+pointer sp, keyword, hdrvalue, section
+int	amp
+int	ax1, ax2, axs, ay1, ay2, ays
+int	bx1, bx2, bxs, by1, by2, bys
+int	cx1, cx2, cxs, cy1, cy2, cys
+int	dx1, dx2, dxs, dy1, dy2, dys
+int	tx1, tx2, txs, ty1, ty2, tys
+
+int	hdmaccf()
+
+begin
+
+	# Get stack space
+	call smark (sp)
+	call salloc (keyword,  SZ_KEYWRD, TY_CHAR)
+	call salloc (hdrvalue, SZ_LINE,   TY_CHAR)
+	call salloc (section,  SZ_LINE,   TY_CHAR)
+
+	# Get input image dimensions.
+	QG_NX (qg, 0) = IM_LEN(im, 1)
+	QG_NY (qg, 0) = IM_LEN(im, 2)
+
+	# Get number of active amplifiers in Y and X.
+	call hdmgstr (im, "nampsyx", Memc[hdrvalue], SZ_LINE)
+	call sscan (Memc[hdrvalue])
+	    call gargi (QG_NAMPSY(qg))
+	    call gargi (QG_NAMPSX(qg))
+	
+	QG_NAMPS(qg) = QG_NAMPSY(qg) * QG_NAMPSX(qg)
+	if (QG_NAMPS(qg) > QG_MAXAMPS)
+	    call error (0, "CCD has too many read-outs for this program")
+
+	# Get decode and order list of active amplifiers.
+	call hdmgstr (im, "amplist", Memc[hdrvalue], SZ_LINE)
+	call ampnames (qg, Memc[hdrvalue])
+
+	# Read geometry keywords for each amplifier from header.
+	do amp = 1, QG_NAMPS (qg) {
+
+	    # Ampsec (ASECyx keyword)
+	    #
+	    call sprintf (Memc[keyword], SZ_KEYWRD, "ASEC%2s")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+	    call hdmgstr (im, Memc[keyword], Memc[section], SZ_LINE)
+
+	    ax1 = 1
+	    ax2 = QG_NX(qg, 0) / QG_NAMPSX(qg)
+	    axs = 1
+	    ay1 = 1
+	    ay2 = QG_NY(qg, 0) / QG_NAMPSY(qg)
+	    ays = 1
+
+	    call ccd_section (Memc[section], ax1, ax2, axs, ay1, ay2, ays)
+	    QG_AX1(qg, amp) = ax1
+	    QG_AX2(qg, amp) = ax2
+	    QG_AY1(qg, amp) = ay1
+	    QG_AY2(qg, amp) = ay2
+	    
+	    # Set X and Y dimensions of subimage read out by each amplifier
+	    QG_NX(qg, amp) = ax2 - ax1 + 1
+	    QG_NY(qg, amp) = ay2 - ay1 + 1
+
+	    # Datasec (DSECyx keyword)
+	    #
+	    call sprintf (Memc[keyword], SZ_KEYWRD, "DSEC%2s")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+	    call hdmgstr (im, Memc[keyword], Memc[section], SZ_LINE)
+
+	    dx1 = ax1
+	    dx2 = ax2
+	    dxs = 1
+	    dy1 = ay1
+	    dy2 = ay2
+	    dys = 1
+	    call ccd_section (Memc[section], dx1, dx2, dxs, dy1, dy2, dys)
+	    QG_DX1(qg, amp) = dx1 - ax1 + 1
+	    QG_DX2(qg, amp) = dx2 - ax1 + 1
+	    QG_DY1(qg, amp) = dy1 - ay1 + 1
+	    QG_DY2(qg, amp) = dy2 - ay1 + 1
+
+	    # CCDsec (CSECyx keyword)
+	    #
+	    call sprintf (Memc[keyword], SZ_KEYWRD, "CSEC%2s")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+	    call hdmgstr (im, Memc[keyword], Memc[section], SZ_LINE)
+
+	    cx1 = dx1
+	    cx2 = dx2
+	    cxs = 1
+	    cy1 = dy1
+	    cy2 = dy2
+	    cys = 1
+	    call ccd_section (Memc[section], cx1, cx2, cxs, cy1, cy2, cys)
+	    QG_CX1(qg, amp) = cx1
+	    QG_CX2(qg, amp) = cx2
+	    QG_CY1(qg, amp) = cy1
+	    QG_CY2(qg, amp) = cy2
+
+	    # Trimsec (TSECyx keyword)
+	    #
+	    call sprintf (Memc[keyword], SZ_KEYWRD, "TSEC%2s")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+
+	    if (hdmaccf (im, Memc[keyword]) == YES) {
+		call hdmgstr (im, Memc[keyword], Memc[section], SZ_LINE)
+
+		tx1 = dx1
+		tx2 = dx2
+		txs = 1
+		ty1 = dy1
+		ty2 = dy2
+		tys = 1
+		call ccd_section (Memc[section], tx1, tx2, txs, ty1, ty2, tys)
+		QG_TX1(qg, amp) = tx1 - ax1 + 1
+		QG_TX2(qg, amp) = tx2 - ax1 + 1
+		QG_TY1(qg, amp) = ty1 - ay1 + 1
+		QG_TY2(qg, amp) = ty2 - ay1 + 1
+
+		QG_PHANTOM(qg, amp) = NO
+
+	    } else {
+		QG_TX1(qg, amp) = 0
+		QG_TX2(qg, amp) = 0
+		QG_TY1(qg, amp) = 0
+		QG_TY2(qg, amp) = 0
+
+		# If the image has not been reduced this must be a phantom
+		if (hdmaccf (im, "trim") == NO) {
+		    QG_PHANTOM(qg, amp) = YES
+		} else {
+		    QG_PHANTOM(qg, amp) = NO
+		}
+	    }
+
+	    # Biassec (BSECyx keyword)
+	    #
+	    call sprintf (Memc[keyword], SZ_KEYWRD, "BSEC%2s")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+
+	    if (hdmaccf (im, Memc[keyword]) == YES) {
+		call hdmgstr (im, Memc[keyword], Memc[section], SZ_LINE)
+
+		bx1 = 0
+		bx2 = 0
+		bxs = 1
+		by1 = 0
+		by2 = 0
+		bys = 1
+		call ccd_section (Memc[section], bx1, bx2, bxs, by1, by2, bys)
+		QG_BX1(qg, amp) = bx1 - ax1 + 1
+		QG_BX2(qg, amp) = bx2 - ax1 + 1
+		QG_BY1(qg, amp) = by1 - ay1 + 1
+		QG_BY2(qg, amp) = by2 - ay1 + 1
+	    } else {
+		QG_BX1(qg, amp) = 0
+		QG_BX2(qg, amp) = 0
+		QG_BY1(qg, amp) = 0
+		QG_BY2(qg, amp) = 0
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+procedure ampnames (qg, amplist)
+
+pointer	qg			#I/O Pointer to open quadgeom structure
+char	amplist[ARB]		#I List of active amplifiers
+
+int	amp, nch
+pointer	sp, ampnum
+
+int	strdic(), itoc()
+
+begin
+	call smark (sp)
+	call salloc (ampnum, QG_NAMPS (qg), TY_INT)
+
+	# parse amplist into array of ordinal numbers
+	call sscan (amplist)
+	do amp = 1, QG_NAMPS (qg) {
+	    call gargi (Memi[ampnum+amp-1])
+	}
+
+	# Sort ordinal numbers into increasing order
+	call asrti (Memi[ampnum], Memi[ampnum], QG_NAMPS(qg))
+
+	# Convert ordinal numbers back into id strings
+	do amp = 1, QG_NAMPS (qg) {
+	    call malloc (QG_AMPID(qg, amp), SZ_AMPID, TY_CHAR)
+	    nch = itoc (Memi[ampnum+amp-1], Memc[QG_AMPID(qg, amp)], SZ_AMPID)
+	}
+
+	# Set AMPTYPE codes
+	do amp = 1, QG_NAMPS (qg) {
+	    QG_AMPTYPE (qg, amp) = strdic (Memc[QG_AMPID (qg, amp)], 
+	    Memc[QG_AMPID (qg, amp)], SZ_AMPID, AMPDICT)
+	}
+
+	call sfree (sp)
+
+end
diff --git a/noao/imred/quadred/src/quad/qguser.x b/noao/imred/quadred/src/quad/qguser.x
new file mode 100644
index 00000000..5d4bf349
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qguser.x
@@ -0,0 +1,126 @@
+include "quadgeom.h"
+
+# QGUSER -- modify open quadgeom structure for user specified trim and
+# overscan.
+
+procedure qguser (qg, xtrim1, xtrim2, ytrim1, ytrim2, xskip1, xskip2)
+
+pointer	qg		# Pointer to open quadgeom structure.
+int	xtrim1		# Number of pixels to trim at right.
+int	xtrim2		# Number of pixels to trim at left.
+int	ytrim1		# Number of pixels to trim at bottom.
+int	ytrim2		# Number of pixels to trim at top.
+int	xskip1		# Number of pixels to skip at start of overscan in X.
+int	xskip2		# Number of pixels to skip at end   of overscan in X.
+
+int	amp, x, y
+int	bx1, bx2, by1, by2
+
+begin
+
+	# Modify overscan margins
+	Do amp = 1, QG_NAMPS (qg) {
+
+	    switch (QG_AMPTYPE(qg, amp)) {
+	    case AMP11, AMP21:  # Left hand side
+		if (IS_INDEFI (xskip1)) {
+		    bx1 = QG_BX1(qg, amp)
+		} else {
+		    bx1 = QG_DX2(qg, amp) + xskip1 + 1
+		}
+
+		if (IS_INDEFI (xskip2)) {
+		    bx2 = QG_BX2(qg, amp)
+		} else {
+		    bx2 = QG_AX2(qg, amp) - QG_AX1(qg, amp) - xskip2 + 1
+		}
+
+	    case AMP12, AMP22:  # Right hand side
+		if (IS_INDEFI (xskip2)) {
+		    bx1 = QG_BX1(qg, amp)
+		} else {
+		    bx1 = 1 + xskip2 
+		}
+		if (IS_INDEFI (xskip1)) {
+		    bx2 = QG_BX2(qg, amp)
+		} else {
+		    bx2 = QG_DX1(qg, amp) - xskip1 - 1
+		}
+
+	    }
+	    by1 = QG_BY1(qg, amp)
+	    by2 = QG_BY2(qg, amp)
+
+	    if (bx1 > bx2) {
+		bx1 = 0
+		bx2 = 0
+		by1 = 0
+		by2 = 0
+	    }
+
+	    QG_BX1(qg, amp) = bx1
+	    QG_BX2(qg, amp) = bx2
+	    QG_BY1(qg, amp) = by1
+	    QG_BY2(qg, amp) = by2
+
+	}
+
+	# Modify trim margins
+
+	# Set left hand edge
+	if (! IS_INDEFI(xtrim1)) {
+	    do y = 1, QG_NAMPSY(qg) {
+		do x = 1, QG_NAMPSX(qg) {
+
+		    amp = QG_AMP(qg, x, y)
+		    if (QG_PHANTOM(qg, amp) == NO) {
+			QG_TX1(qg, amp) = QG_DX1(qg, amp) + xtrim1
+			break
+		    }
+		}
+	    }
+	}
+
+	# Set right hand edge
+	if (! IS_INDEFI(xtrim2)) {
+	    do y = 1, QG_NAMPSY(qg) {
+		do x = QG_NAMPSX(qg), 1, -1 {
+
+		    amp = QG_AMP(qg, x, y)
+		    if (QG_PHANTOM(qg, amp) == NO) {
+			QG_TX2(qg, amp) = QG_DX2(qg, amp) - xtrim2
+			break
+		    }
+		}
+	    }
+	}
+
+
+	# Set lower edge
+	if (! IS_INDEFI(ytrim1)) {
+	    do x = 1, QG_NAMPSX(qg) {
+		do y = 1, QG_NAMPSY(qg) {
+
+		    amp = QG_AMP(qg, x, y)
+		    if (QG_PHANTOM(qg, amp) == NO) {
+			QG_TY1(qg, amp) = QG_DY1(qg, amp) + ytrim1
+			break
+		    }
+		}
+	    }
+	}
+
+	# Set upper edge
+	if (! IS_INDEFI(ytrim2)) {
+	    do x = 1, QG_NAMPSX(qg) {
+		do y = QG_NAMPSY(qg), 1, -1 {
+
+		    amp = QG_AMP(qg, x, y)
+		    if (QG_PHANTOM(qg, amp) == NO) {
+			QG_TY2(qg, amp) = QG_DY2(qg, amp) - ytrim2
+			break
+		    }
+		}
+	    }
+	}
+end
diff --git a/noao/imred/quadred/src/quad/qhistogram.cl b/noao/imred/quadred/src/quad/qhistogram.cl
new file mode 100644
index 00000000..4b5c1958
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qhistogram.cl
@@ -0,0 +1,58 @@
+procedure qhistogram (image)
+
+begin
+	string	tmp, meta, im, subimage, amp, section
+	int	nx, ny
+#	real	zz1, zz2, mean, mode, min, max, sigma
+
+	im = image
+
+	tmp   = mktemp ("uparm$tmp")
+	fdtmp = tmp
+	meta  = mktemp ("uparm$meta")
+
+	# Project image section on to quadrant boundaries.
+	#quadsections (im, window=window, section="", template="$I$S $A $S\n", 
+	#xskip1=INDEF, xskip2=INDEF, xtrim1=INDEF, xtrim2=INDEF,
+	#ytrim1=INDEF, ytrim2=INDEF, >> tmp)
+	quadsections (im, window=window, section="", template="$I$S $A $S\n", 
+	    >> tmp)
+
+#	# Set up histogram limits
+#	switch (substr (scaling, 1, 1) {
+#	case "s":	set
+#	    zz1 = z1
+#	    zz2 = z2
+
+#	case minmax"
+
+
+	if (listout) {
+	    printf ("%s\n", im)
+	    while (fscan (fdtmp, subimage, amp, section) != EOF) {
+
+		printf ("\tAmp%s: section=%s\n\n", amp, section)
+
+		imhist (subimage, z1=z1, z2=z2, binwidth=binwidth, nbins=nbins, 
+		autoscale=autoscale, top_closed=top_closed, hist_type=hist_type,
+		listout=listout, plot_type=plot_type, logy=logy, device=device)
+	    }
+
+	} else {
+	    while (fscan (fdtmp, subimage) != EOF) {
+
+		imhist (subimage, z1=z1, z2=z2, binwidth=binwidth, nbins=nbins, 
+		autoscale=autoscale, top_closed=top_closed, hist_type=hist_type,
+		listout=listout, plot_type=plot_type, logy=logy, device=device,
+		>>G meta)
+
+	    }
+	    ccdgetparam (im, "nampsyx") | scan (ny, nx)
+	    gkim (meta, device=device, output=plotfile, nx=nx, ny=ny, rotate=no,
+	    fill=yes, interactive=no, cursor="")
+
+	    delete (meta, ver-)
+	}
+
+	delete (tmp,  ver-)
+end
diff --git a/noao/imred/quadred/src/quad/qhistogram.par b/noao/imred/quadred/src/quad/qhistogram.par
new file mode 100644
index 00000000..1ba40ec1
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qhistogram.par
@@ -0,0 +1,17 @@
+image,s,a,,,,Image name
+window,s,h,"datasec","|datasec|trimsec|biassec|reflect|duplicate|",,Window to apply to image
+z1,r,h,INDEF,,,Minimum histogram intensity
+z2,r,h,INDEF,,,Maximum histogram intensity
+binwidth,r,h,INDEF,,,Resolution of histogram in intensity units
+nbins,i,h,512,1,,Number of bins in histogram
+autoscale,b,h,yes,,,Adjust nbins and z2 for integer data?
+top_closed,b,h,no,,,Include z2 in the top bin?
+hist_type,s,h,"normal","normal|cumulative|difference|second_difference",,"Type of histogram"
+listout,b,h,no,,,List instead of plot histogram?
+plot_type,s,h,"line","line|box",,Type of vectors to plot
+logy,b,h,yes,,,Log scale y-axis?
+device,s,h,"stdgraph",,,Output graphics device
+plotfile,s,h,"",,,"Output graphics file
+"
+fdtmp,*s,h,,,,Internal use only
+mode,s,h,ql,,,
diff --git a/noao/imred/quadred/src/quad/qnoproc.cl b/noao/imred/quadred/src/quad/qnoproc.cl
new file mode 100644
index 00000000..9f7d048f
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qnoproc.cl
@@ -0,0 +1,77 @@
+procedure qnoproc (image_list)
+
+begin
+	string	image, buffer, imtype
+	int	i, len, nampsx, nampsy, nlines
+	bool	dofix, dotrim, doover
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	i = strlen (imtype)
+
+	dofix  = fixpix
+	doover = overscan
+	dotrim = trim
+
+	fd = image_list
+	while (fscan (fd, image) != EOF) {
+
+	    len = strlen (image)
+	    if (substr(image, len-i+1, len) == imtype) {
+		image = substr (image, 1, len-i)
+	    }
+
+	    # Report what processing steps will be performed by qproc
+	    printf ("%s:", image)
+
+	    if (fixpix) {
+		ccdgetparam (image, "fixpix") | scan (buffer)
+		dofix =  (buffer == "UNDEFINED!")
+	    }
+
+	    if (overscan) {
+		ccdgetparam (image, "overscan") | scan (buffer)
+		doover = (buffer == "UNDEFINED!") 
+	    }
+
+	    if (trim) {
+		ccdgetparam (image, "trim") | scan (buffer)
+		dotrim = (buffer == "UNDEFINED!") 
+	    }
+
+	    if (dofix || dotrim || doover) {
+		ccdgetparam (image, "nampsyx") | scan (nampsy, nampsx)
+		if (nampsx == 2 && nampsy == 2) {
+		    printf (" (Quad-readout image)\n")
+		} else if (nampsx == 2 || nampsy == 2) {
+		    printf (" (Dual-readout image: nampsx=%d nampsy=%d)\n",
+		    nampsx, nampsy)
+		} else {
+		    printf ("\n")
+		}
+		
+		if (doover) {
+		    printf ("  [TO BE DONE] Trim section is:\n")
+		    #quadsections (image, window="trimsec", section="", 
+		    #template="%18tAMP$A $S\n", xskip1=xskip1, xskip2=xskip2,
+		    #xtrim1=xtrim1, xtrim2=xtrim2, ytrim1=ytrim1, ytrim2=ytrim2)
+		    quadsections (image, window="trimsec", section="", 
+		    template="%18tAMP$A $S\n")
+		}
+
+		if (dofix)
+		    printf ("  [TO BE DONE] Bad pixel file is %s\n", fixfile)
+
+		if (doover) {
+		    printf ("  [TO BE DONE] Overscan section is:\n")
+		    #quadsections (image, window="biassec", section="", 
+		    #template="%18tAMP$A $S\n", xskip1=xskip1, xskip2=xskip2,
+		    #xtrim1=xtrim1, xtrim2=xtrim2, ytrim1=ytrim1, ytrim2=ytrim2)
+		    quadsections (image, window="biassec", section="", 
+		    template="%18tAMP$A $S\n")
+		}
+	    }
+	}
+end
diff --git a/noao/imred/quadred/src/quad/qnoproc.par b/noao/imred/quadred/src/quad/qnoproc.par
new file mode 100644
index 00000000..7e01c141
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qnoproc.par
@@ -0,0 +1,15 @@
+image_list,s,a,"",,,List of CCD images to correct
+fixpix,b,h,yes,,,Fix bad CCD lines and columns?
+overscan,b,h,yes,,,Apply overscan strip correction?
+trim,b,h,yes,,,Trim the image?
+fixfile,s,h,"",,,"File describing the bad lines and columns
+
+# TRIM AND OVERSCAN MARGINS (overide header values)"
+xskip1,i,h,INDEF,0,,X pixels to skip at start of overscan
+xskip2,i,h,INDEF,0,,X pixels to skip at end of overscan
+xtrim1,i,h,INDEF,0,,X pixels to trim at start of data
+xtrim2,i,h,INDEF,0,,X pixels to trim at end   of data
+ytrim1,i,h,INDEF,0,,Y pixels to trim at start of data
+ytrim2,i,h,INDEF,0,,"Y pixels to trim at end   of data
+"
+fd,*s,h,,,,Internal use only
diff --git a/noao/imred/quadred/src/quad/qpcalimage.par b/noao/imred/quadred/src/quad/qpcalimage.par
new file mode 100644
index 00000000..ddeb506d
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qpcalimage.par
@@ -0,0 +1,3 @@
+quadproc,pset,h,,,,CCD processing parameters
+only_param,b,h,no,,,Only return calibration images from parameters
+check,b,h,yes,,,Complain if any calibration images are unspecified
diff --git a/noao/imred/quadred/src/quad/qpcalimage.x b/noao/imred/quadred/src/quad/qpcalimage.x
new file mode 100644
index 00000000..2e0ee40b
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qpcalimage.x
@@ -0,0 +1,525 @@
+include	<error.h>
+include	<imset.h>
+include	"ccdtypes.h"
+
+define	SZ_SUBSET	16			# Maximum size of subset string
+define	IMAGE	Memc[$1+($2-1)*SZ_FNAME]	# Image string
+define	SUBSET	Memc[$1+($2-1)*SZ_SUBSET]	# Subset string
+
+procedure t_qpcalimage ()
+
+pointer	im, subsets, list
+int	i, j
+bool	flatcor, illumcor, fringecor, found, check
+char	instrument[SZ_LINE], image[SZ_FNAME], buffer[SZ_SUBSET-1]
+
+pointer	immap(), imtopenp()
+int	imtgetim()
+bool	clgetb(), streq()
+
+begin
+	# Open list of images and instrument file
+	list = imtopenp ("images")
+	call clgstr ("instrument", instrument, SZ_LINE)
+	call hdmopen (instrument)
+
+	if (clgetb ("only_param")) {
+	    call cal_open (NULL)
+	} else {
+	    call cal_open (list)
+	}
+
+	check = clgetb ("check")
+
+	if (clgetb ("zerocor")) {
+	    iferr (call cal_find (ZERO, "", image, SZ_FNAME)) {
+		if (check) {
+		    call erract (EA_WARN)
+		}
+
+	    } else {
+		call printf ("%s\n")
+		    call pargstr (image)
+	    }
+	}
+
+	if (clgetb ("darkcor")) {
+	    iferr (call cal_find (DARK, "", image, SZ_FNAME)) {
+		if (check) 
+		    call erract (EA_WARN)
+
+	    } else {
+		call printf ("%s\n")
+		    call pargstr (image)
+	    }
+	}
+
+	flatcor   = clgetb ("flatcor")
+	illumcor  = clgetb ("illumcor")
+	fringecor = clgetb ("fringecor")
+
+	if (flatcor || illumcor || fringecor) {
+
+	    i = 1
+	    found = false
+	    while (imtgetim (list, image, SZ_FNAME) != EOF) {
+		# Open the image.  Silently skip any non-existant images
+		iferr (im = immap (image, READ_ONLY, 0)) 
+		    next
+
+		call ccdsubset (im, buffer, SZ_SUBSET-1)
+		call imunmap (im)
+
+		# Check to see if we have already dealt with this subset
+		do j = 1, i - 1 {
+		    found = (streq (buffer, SUBSET (subsets, j)))
+		    if (found)
+			break
+		}
+
+		if (!found) {
+
+		    # Add subset to list of processed subsets
+		    if (i == 1) 
+			call malloc  (subsets, i * SZ_SUBSET, TY_CHAR)
+		    else 
+			call realloc (subsets, i * SZ_SUBSET, TY_CHAR)
+
+		    call strcpy (buffer, SUBSET(subsets, i), SZ_SUBSET-1)
+		    i = i + 1
+
+		    # Find and print names of associated calibration images
+		    if (flatcor) {
+			iferr (call cal_find (FLAT, buffer, image, SZ_FNAME)) {
+			    if (check) 
+				call erract (EA_WARN)
+
+			} else {
+			    call printf ("%s\n")
+				call pargstr (image)
+			}
+		    }
+
+		    if (illumcor) {
+			iferr (call cal_find (ILLUM, buffer, image, SZ_FNAME)) {
+			    if (check) 
+				call erract (EA_WARN)
+
+			} else {
+			    call printf ("%s\n")
+				call pargstr (image)
+			}
+		    }
+
+		    if (fringecor) {
+			iferr (call cal_find (FRINGE, buffer, image, SZ_FNAME)){
+			    if (check) 
+				call erract (EA_WARN)
+
+			} else {
+			    call printf ("%s\n")
+				call pargstr (image)
+			}
+		    }
+		}
+	    }
+	}
+
+	call hdmclose ()
+	call imtclose (list)
+	call mfree (subsets, TY_CHAR)
+	call cal_close ()
+
+end
+
+# CAL_FIND  -- Return a calibration image of the specified type and subset
+# CAL_IMAGE -- Return a calibration image for a specified input image.
+# CAL_OPEN  -- Open the calibration image list.
+# CAL_CLOSE -- Close the calibration image list.
+# CAL_LIST  -- Add images to the calibration image list.
+#
+# The open procedure is called first to get the calibration image
+# lists and add them to an internal list.  Calibration images from the
+# input list are also added so that calibration images may be specified
+# either from the calibration image list parameters or in the input image list.
+# Existence errors and duplicate calibration images are ignored.
+# Validity checks are made when the calibration images are requested.
+#
+# During processing the calibration image names are requested for each input
+# image.  The calibration image list is searched for a calibration image of
+# the right type and subset.  If more than one is found the first one is
+# returned and a warning given for the others.  The warning is only issued
+# once.  If no calibration image is found then an error is returned.
+#
+# The calibration image list must be closed at the end of processing the
+# input images.
+
+# CAL_FIND -- Return a calibration image of a particular type and subset.
+# Search the calibration list for the first calibration image of the desired
+# type and subset.  Print a warning if there  is more than one possible
+# calibration image and return an error if there is no calibration image. 
+
+procedure cal_find (ccdtype, subset, image, maxchars)
+
+int	ccdtype			#I Callibration CCD image type
+char	subset[ARB]		#I Calibration image subset
+char	image[maxchars]		#O Calibration image (returned)
+int	maxchars		#I Maximum number chars in image name
+
+int	i
+char	errmsg[SZ_LINE]
+bool	strne()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subsets
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, images, nimages
+
+begin
+
+	switch (ccdtype) {
+	case ZERO, DARK:
+	    do i = 1, nimages {
+		if (Memi[ccdtypes+i-1] != ccdtype)
+		    next
+
+		call strcpy (IMAGE(images,i), image, maxchars)
+		return
+	    }
+
+	case FLAT, ILLUM, FRINGE:
+	    do i = 1, nimages {
+		if (Memi[ccdtypes+i-1] != ccdtype)
+		    next
+		if (strne (SUBSET(subsets,i), subset))
+		    next
+
+		call strcpy (IMAGE(images,i), image, maxchars)
+		return
+	    }
+	}
+
+	# If no calibration image is found then it is an error.
+	switch (ccdtype) {
+	case ZERO:
+	    call error (0, "No zero level calibration image found")
+	case DARK:
+	    call error (0, "No dark count calibration image found")
+	case FLAT:
+	    call sprintf (errmsg, SZ_LINE,
+		 "No flat field calibration image of subset %s found")
+		 call pargstr (subset)
+	    call error (0, errmsg)
+	case ILLUM:
+	    call sprintf (errmsg, SZ_LINE,
+		 "No illumination calibration image of subset %s found")
+		 call pargstr (subset)
+	    call error (0, errmsg)
+	case FRINGE:
+	    call sprintf (errmsg, SZ_LINE,
+		 "No fringe calibration image of subset %s found")
+		 call pargstr (subset)
+	    call error (0, errmsg)
+	}
+end
+
+# CAL_IMAGE -- Return a calibration image of a particular type.
+# Search the calibration list for the first calibration image of the desired
+# type and subset.  Print a warning if there  is more than one possible
+# calibration image and return an error if there is no calibration image. 
+
+procedure cal_image (im, ccdtype, image, maxchars)
+
+pointer	im		# Image to be processed
+int	ccdtype		# Callibration CCD image type
+char	image[maxchars]	# Calibration image (returned)
+int	maxchars	# Maximum number chars in image name
+
+int	i, n
+pointer	sp, subset, str
+bool	strne(), ccd_cmp()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subsets
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, images, nimages
+
+begin
+	call smark (sp)
+	call salloc (subset, SZ_SUBSET, TY_CHAR)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	switch (ccdtype) {
+	case ZERO, DARK:
+	    n = 0
+	    do i = 1, nimages {
+		if (Memi[ccdtypes+i-1] != ccdtype)
+		    next
+		n = n + 1
+		if (n == 1)
+		    call strcpy (IMAGE(images,i), image, maxchars)
+		else {
+#		    call eprintf (
+#			"Warning: Extra calibration image %s ignored\n")
+#		        call pargstr (IMAGE(images,i))
+
+		    # Reset the image type to eliminate further warnings.
+		    Memi[ccdtypes+i-1] = UNKNOWN
+		}
+	    }
+	case FLAT, ILLUM, FRINGE:
+	    call ccdsubset (im, Memc[subset], SZ_SUBSET)
+
+	    n = 0
+	    do i = 1, nimages {
+		if (Memi[ccdtypes+i-1] != ccdtype)
+		    next
+		if (strne (SUBSET(subsets,i), Memc[subset]))
+		    next
+		n = n + 1
+		if (n == 1)
+		    call strcpy (IMAGE(images,i), image, maxchars)
+		else {
+#		    call eprintf (
+#			"Warning: Extra calibration image %s ignored\n")
+#		        call pargstr (IMAGE(images,i))
+
+		    # Reset the image type to eliminate further warnings.
+		    Memi[ccdtypes+i-1] = UNKNOWN
+		}
+	    }
+	}
+
+	# If no calibration image is found then it is an error.
+	if (n == 0)
+	    switch (ccdtype) {
+	    case ZERO:
+	        call error (0, "No zero level calibration image found")
+	    case DARK:
+	        call error (0, "No dark count calibration image found")
+	    case FLAT:
+		call sprintf (Memc[str], SZ_LINE,
+	             "No flat field calibration image of subset %s found")
+		     call pargstr (Memc[subset])
+	        call error (0, Memc[str])
+	    case ILLUM:
+		call sprintf (Memc[str], SZ_LINE,
+	             "No illumination calibration image of subset %s found")
+		     call pargstr (Memc[subset])
+	        call error (0, Memc[str])
+	    case FRINGE:
+		call sprintf (Memc[str], SZ_LINE,
+	             "No fringe calibration image of subset %s found")
+		     call pargstr (Memc[subset])
+	        call error (0, Memc[str])
+	    }
+
+	# Check that the input image is not the same as the calibration image.
+	call imstats (im, IM_IMAGENAME, Memc[str], SZ_LINE)
+	if (ccd_cmp (Memc[str], image)) {
+	    call sprintf (Memc[str], SZ_LINE,
+		"Calibration image %s is the same as the input image")
+		call pargstr (image)
+	    call error (0, Memc[str])
+	}
+
+	call sfree (sp)
+end
+
+
+# CAL_OPEN -- Create a list of calibration images from the input image list
+# and the calibration image lists.
+
+procedure cal_open (list)
+
+int	list		# List of input images
+int	list1		# List of calibration images
+
+pointer	sp, str
+int	ccdtype, strdic(), imtopenp()
+bool	clgetb()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subset numbers
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, images, nimages
+
+errchk	cal_list
+
+begin
+	call smark (sp)
+	call salloc (str, SZ_LINE, TY_CHAR)
+
+	call clgstr ("ccdtype", Memc[str], SZ_LINE)
+	call xt_stripwhite (Memc[str])
+	if (Memc[str] == EOS)
+	    ccdtype = NONE
+	else
+	    ccdtype = strdic (Memc[str], Memc[str], SZ_LINE, CCDTYPES)
+
+	# Add calibration images to list.
+	nimages = 0
+	if (ccdtype != ZERO && clgetb ("zerocor")) {
+	    list1 = imtopenp ("zero")
+	    call cal_list (list1, ZERO)
+	    call imtclose (list1)
+	}
+	if (ccdtype != ZERO && ccdtype != DARK && clgetb ("darkcor")) {
+	    list1 = imtopenp ("dark")
+	    call cal_list (list1, DARK)
+	    call imtclose (list1)
+	}
+	if (ccdtype != ZERO && ccdtype != DARK && ccdtype != FLAT &&
+	    clgetb ("flatcor")) {
+	    list1 = imtopenp ("flat")
+	    call cal_list (list1, FLAT)
+	    call imtclose (list1)
+	}
+	if (ccdtype != ZERO && ccdtype != DARK && ccdtype != FLAT &&
+	    ccdtype != ILLUM && clgetb ("illumcor")) {
+	    list1 = imtopenp ("illum")
+	    call cal_list (list1, ILLUM)
+	    call imtclose (list1)
+	}
+	if (ccdtype != ZERO && ccdtype != DARK && ccdtype != FLAT &&
+	    ccdtype != FRINGE && clgetb ("fringecor")) {
+	    list1 = imtopenp ("fringe")
+	    call cal_list (list1, FRINGE)
+	    call imtclose (list1)
+	}
+	if (list != NULL) {
+	    call cal_list (list, UNKNOWN)
+	    call imtrew (list)
+	}
+
+	call sfree (sp)
+end
+
+
+# CAL_CLOSE -- Free memory from the internal calibration image list.
+
+procedure cal_close ()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subset
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, images, nimages
+
+begin
+	if (nimages > 0) {
+	    call mfree (ccdtypes, TY_INT)
+	    call mfree (subsets, TY_CHAR)
+	    call mfree (images, TY_CHAR)
+	}
+end
+
+
+# CAL_LIST -- Add calibration images to an internal list.
+# Map each image and get the CCD image type and subset.
+# If the ccdtype is given as a procedure argument this overrides the
+# image header type.  For the calibration images add the type, subset,
+# and image name to dynamic arrays.  Ignore duplicate names.
+
+procedure cal_list (list, listtype)
+
+pointer	list		# Image list
+int	listtype	# CCD type of image in list.
+			# Overrides header type if not UNKNOWN.
+
+int	i, ccdtype, ccdtypei(), imtgetim()
+pointer	sp, image, im, immap()
+bool	streq()
+
+pointer	ccdtypes	# Pointer to array of calibration ccdtypes
+pointer	subsets		# Pointer to array of calibration subsets
+pointer	images		# Pointer to array of calibration image names
+int	nimages		# Number of images
+common	/calib/ ccdtypes, subsets, images, nimages
+
+begin
+	call smark (sp)
+	call salloc (image, SZ_FNAME, TY_CHAR)
+
+	while (imtgetim (list, Memc[image], SZ_FNAME) != EOF) {
+	    # Open the image.  If an explicit type is given it is an
+	    # error if the image can't be opened.
+	    iferr (im = immap (Memc[image], READ_ONLY, 0)) {
+		if (listtype == UNKNOWN)
+		    next
+		else
+		    call erract (EA_ERROR)
+	    }
+
+	    # Override image header CCD type if a list type is given.
+	    if (listtype == UNKNOWN)
+	        ccdtype = ccdtypei (im)
+	    else
+		ccdtype = listtype
+		
+	    switch (ccdtype) {
+	    case ZERO, DARK, FLAT, ILLUM, FRINGE:
+		# Check for duplication.
+		for (i=1; i<=nimages; i=i+1)
+		    if (streq (Memc[image], IMAGE(images,i)))
+			break
+		if (i <= nimages)
+		    break
+
+		# Allocate memory for a new image.
+		if (i == 1) {
+		    call malloc (ccdtypes, i, TY_INT)
+		    call malloc (subsets, i * SZ_SUBSET, TY_CHAR)
+		    call malloc (images, i * SZ_FNAME, TY_CHAR)
+		} else {
+		    call realloc (ccdtypes, i, TY_INT)
+		    call realloc (subsets, i * SZ_FNAME, TY_CHAR)
+		    call realloc (images, i * SZ_FNAME, TY_CHAR)
+		}
+
+		# Enter the ccdtype, subset, and image name.
+		Memi[ccdtypes+i-1] = ccdtype
+		call ccdsubset (im, SUBSET(subsets,i), SZ_SUBSET-1)
+		call strcpy (Memc[image], IMAGE(images,i), SZ_FNAME-1)
+		nimages = i
+	    }
+	    call imunmap (im)
+	}
+#	call eprintf ("nimages=%d\n")
+#	    call pargi (nimages)
+#	do i = 1, nimages {
+#	    call eprintf ("ccdtype=%d subset=%s image=%s\n")
+#		call pargi (Memi[ccdtypes+i-1])
+#		call pargstr (SUBSET (subsets, i))
+#		call pargstr (IMAGE (images, i))
+#	}
+
+	call sfree (sp)
+end
+
+# CCD_CMP -- Compare two image names with extensions ignored.
+
+bool procedure ccd_cmp (image1, image2)
+
+char	image1[ARB]		# First image
+char	image2[ARB]		# Second image
+
+int	i, j, strmatch(), strlen(), strncmp()
+bool	streq()
+
+begin
+	if (streq (image1, image2))
+	    return (true)
+
+	i = max (strmatch (image1, ".imh"), strmatch (image1, ".hhh"))
+	if (i == 0)
+	    i = strlen (image1)
+	j = max (strmatch (image2, ".imh"), strmatch (image2, ".hhh"))
+	if (j == 0)
+	    j = strlen (image2)
+
+	return (strncmp (image1, image2, max (i, j)) == 0)
+end
diff --git a/noao/imred/quadred/src/quad/qproc.cl b/noao/imred/quadred/src/quad/qproc.cl
new file mode 100644
index 00000000..d0040d18
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qproc.cl
@@ -0,0 +1,109 @@
+procedure qproc (image_list)
+
+begin
+	struct	buffer
+	string	image, answr, imtype
+	int	i, len, nampsx, nampsy
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	i = strlen (imtype)
+
+	cache ("quadsplit", "quadjoin", "qccdproc", "quadproc")
+
+
+	# Validate fixfile
+	if (fixpix) {
+	    match ("single_readout", fixfile) | scan (buffer)
+	    if (stridx ("#", buffer) == 0) {
+		buffer = "fixfile " // fixfile // 
+		" cannot be used with multi-readout images"
+		error (0, buffer)
+	    }
+	}
+
+	# Initialise interactive query
+	if (qccdproc.interactive) {
+	    answer.p_value = "yes"
+	    answr = "yes"
+	} else {
+	    answr = "NO"
+	}
+
+	fd = image_list
+	while (fscan (fd, image) != EOF) {
+
+	    len = strlen (image)
+	    if (substr(image, len-i+1, len) == imtype) {
+		image = substr (image, 1, len-i)
+	    }
+
+	    # Split out one image for each quadrant and set header sections
+	    #quadsplit (image, output="",
+	    #xskip1=xskip1, xskip2=xskip2, xtrim1=xtrim1, xtrim2=xtrim2,
+	    #ytrim1=ytrim1, ytrim2=ytrim2, clobber=yes)
+	    quadsplit (image, output="", clobber=yes)
+
+
+	    # Find out of interactive fit is required for this image
+	    if (answr == "yes" || answr == "no") {
+		printf ("Fit overscan vector for %s interactively\n", image) | 
+		scan (buffer)
+		answer.p_prompt=buffer
+		answr = answer
+	    }
+
+	    # Overscan correct and trim
+	    if (answr == "yes" || answr == "YES") {
+		qccdproc.interactive = yes
+
+		print ("YES") | qccdproc (image//".??"//imtype, fixpix=fixpix,
+		overscan=overscan, trim=trim, readaxis=readaxis,
+		fixfile=fixfile, biassec="image", trimsec="image",
+		ccdtype="", max_cache=0, noproc=no, zerocor=no, darkcor=no,
+		flatcor=no, illumcor=no, fringecor=no, readcor=no,
+		scancor=no, zero="", dark="", flat="", illum="", fringe="",
+		minreplace=1., scantype="shortscan", nscan=1, backup="", 
+		logfile="", verbose=no, >> "dev$null")
+
+		# Set parameters of quadproc used for overscan fitting to match
+                # the ccdproc values which may have been adjusted interactively.
+		# We do this on every pass in case there is a later interupt
+		# of task execution. 
+		quadproc.function.p_value    = qccdproc.function
+		quadproc.order.p_value       = qccdproc.order
+		quadproc.sample.p_value      = qccdproc.sample
+		quadproc.naverage.p_value    = qccdproc.naverage
+		quadproc.niterate.p_value    = qccdproc.niterate
+		quadproc.low_reject.p_value  = qccdproc.low_reject
+		quadproc.high_reject.p_value = qccdproc.high_reject
+		quadproc.grow.p_value        = qccdproc.grow
+
+		# Force the parameter update
+		update ("quadproc")
+
+	    } else {
+		qccdproc.interactive = no
+
+		qccdproc (image//".??"//imtype, fixpix=fixpix,
+		overscan=overscan, trim=trim, readaxis=readaxis,
+		fixfile=fixfile, biassec="image", trimsec="image",
+		ccdtype="", max_cache=0, noproc=no, zerocor=no, darkcor=no,
+		flatcor=no, illumcor=no, fringecor=no, readcor=no,
+		scancor=no, zero="", dark="", flat="", illum="", fringe="",
+		minreplace=1., scantype="shortscan", nscan=1, backup="",
+		logfile="", verbose=no)
+	    }
+
+	    # Combine processed quadrants into single image
+	    quadjoin (image, output="", delete=yes)
+
+	}
+
+	# Reset interactive flag if we haven't recieved a definative NO
+	if (answr == "no") {
+	    qccdproc.interactive = yes
+	}
+end
diff --git a/noao/imred/quadred/src/quad/qproc.par b/noao/imred/quadred/src/quad/qproc.par
new file mode 100644
index 00000000..6a713a5d
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qproc.par
@@ -0,0 +1,15 @@
+image_list,s,a,"",,,List of CCD images to correct
+fixpix,b,h,yes,,,Fix bad CCD lines and columns?
+overscan,b,h,yes,,,Apply overscan strip correction?
+trim,b,h,yes,,,Trim the image?
+readaxis,s,h,"line","column|line",, Read out axis (column|line)
+fixfile,s,h,"",,,File describing the bad lines and columns
+xskip1,i,h,INDEF,0,,X pixels to skip at start of overscan
+xskip2,i,h,INDEF,0,,X pixels to skip at end of overscan
+xtrim1,i,h,INDEF,0,,X pixels to trim at start of data
+xtrim2,i,h,INDEF,0,,X pixels to trim at end   of data
+ytrim1,i,h,INDEF,0,,Y pixels to trim at start of data
+ytrim2,i,h,INDEF,0,,Y pixels to trim at end   of data
+answer,s,ql,"yes","|yes|no|YES|NO|",,"Fit overscan vector for xxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxxx interactively
+"
+fd,*s,h,,,,Internal use only
diff --git a/noao/imred/quadred/src/quad/qpselect.par b/noao/imred/quadred/src/quad/qpselect.par
new file mode 100644
index 00000000..d1a7aa56
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qpselect.par
@@ -0,0 +1,4 @@
+input,s,a,"",,,Input image list
+output,s,h,"STDOUT",,,Output image list
+ccdtype,s,h,"",,,CCD image type to be listed
+stop,b,h,"no",,,"Stop, rather than pass, selected images"
diff --git a/noao/imred/quadred/src/quad/qpselect.x b/noao/imred/quadred/src/quad/qpselect.x
new file mode 100644
index 00000000..8bd2acb2
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qpselect.x
@@ -0,0 +1,108 @@
+# QPSELECT -- Filter a list of image names passing on only those that are of 
+# the specified ccdtype -AND-
+#
+# If stop = yes
+#       1) Are multi-readout		-AND-
+# 	2) Have not been trimmed
+# If stop = no
+#	1) Are single-readout		-OR-
+#	2) Have been trimmed
+
+include "ccdtypes.h"
+
+procedure t_qpselect ()
+
+pointer	inlist			#TI List of input image name.
+char	output[SZ_FNAME]	#TI List of output image names.
+char	instrument[SZ_FNAME]	#TI Instrument translation file.
+char	ccdtype[SZ_LINE]	#TI ccdtype to select.
+bool	stop			#TI stop rather than pass selected images
+
+int	type, nampx, nampy
+char	image[SZ_LINE], nampsyx[SZ_LINE]
+pointer	fdout, im
+
+int	strdic(), imtopenp(), imtgetim(), hdmaccf(), imaccess()
+int	ccdtypei()
+bool	clgetb()
+
+pointer	open(), immap()
+
+begin
+	# Open input and output image lists
+	inlist = imtopenp ("input")
+	call clgstr ("output", output, SZ_LINE)
+	fdout = open (output, APPEND, TEXT_FILE)
+
+	# Open instrument file
+	call clgstr    ("instrument",  instrument,  SZ_FNAME)
+	call hdmopen   (instrument)
+
+	# Get ccdtype to select.
+	call clgstr   ("ccdtype", ccdtype, SZ_LINE)
+	type = strdic (ccdtype, ccdtype, SZ_LINE, CCDTYPES)
+
+	# Get stop
+	stop = clgetb ("stop")
+
+	while (imtgetim (inlist, image, SZ_LINE) != EOF) {
+
+	    # Silently skip any non-existant images
+	    if (imaccess (image, READ_ONLY) == NO)
+		next
+
+	    im = immap (image, READ_ONLY, 0)
+
+	    if ((ccdtype[1] != EOS) && (type != ccdtypei (im))) {
+		call imunmap (im)
+		next
+	    }
+
+	    if (stop) {
+
+		if (hdmaccf (im, "trim") == YES) {
+		    call fprintf (fdout, "%s\n")
+			call pargstr (image)
+
+		} else if (hdmaccf (im, "nampsyx") == NO) {
+		    call fprintf (fdout, "%s\n")
+			call pargstr (image)
+
+		} else {
+
+		    call hdmgstr (im, "nampsyx", nampsyx, SZ_LINE)
+		    call sscan (nampsyx)
+			call gargi (nampx)
+			call gargi (nampy)
+
+		    if (nampx == 1 && nampy == 1) {
+			call fprintf (fdout, "%s\n")
+			    call pargstr (image)
+		    }
+		}
+
+	    } else {
+
+		if ((hdmaccf (im, "trim")    == NO) &&
+		    (hdmaccf (im, "nampsyx") == YES)) {
+
+		    call hdmgstr (im, "nampsyx", nampsyx, SZ_LINE)
+		    call sscan (nampsyx)
+			call gargi (nampx)
+			call gargi (nampy)
+
+		    if (nampx != 1 || nampy != 1) {
+			call fprintf (fdout, "%s\n")
+			    call pargstr (image)
+		    }
+		}
+	    }
+
+	    call imunmap (im)
+	}
+
+	# Tidy up
+	call close (fdout)
+	call hdmclose ()
+	call imtclose (inlist)
+end
diff --git a/noao/imred/quadred/src/quad/qsplit.gx b/noao/imred/quadred/src/quad/qsplit.gx
new file mode 100644
index 00000000..3d5b1873
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qsplit.gx
@@ -0,0 +1,97 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+# QSPLITx -- Split multi-readout image into separate images one for each 
+# readout.
+
+procedure qsplit$t (in, out, qg)
+
+pointer	in			#I Image pointer for input image
+pointer	out[ARB]		#I Image pointer for output images
+pointer	qg			#I pointer to quadgeom structure
+
+long	ivec[IM_MAXDIM], ovec[IM_MAXDIM, QG_MAXAMPS]
+int	amp, amp2, x, y, line, junk
+pointer	ibuf, obuf, ptr
+bool	all_phantom
+
+int	imgnl$t(), impnl$t()
+
+begin
+	# Setup start vectors for sequential reads ...
+	call amovkl (long(1), ivec, IM_MAXDIM)
+	# ... and writes
+	do amp = 1, QG_NAMPS (qg)
+	    call amovkl (long(1), ovec[1, amp], IM_MAXDIM)
+
+	do y = 1, QG_NAMPSY(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+
+	    # Check to see if there are any non phantom regions in this tier
+	    all_phantom = true
+	    do x = 1, QG_NAMPSX(qg) {
+		amp = QG_AMP(qg, x, y)
+		if (QG_PHANTOM (qg, amp) == NO) {
+		    all_phantom = false 
+		    break
+		}
+	    }
+
+	    if (all_phantom) {
+
+		# Reset start vector for reads to skip phantom data
+		ivec[2] = ivec[2] + long (QG_NY (qg, amp2))
+
+	    } else {
+
+		do line = 1, QG_NY(qg, amp2) {
+		    junk = imgnl$t (in, ibuf, ivec)
+		    ptr = ibuf
+		    do x = 1, QG_NAMPSX(qg) {
+			amp = QG_AMP(qg, x, y)
+			if (QG_PHANTOM (qg, amp) == NO) {
+			    junk = impnl$t (out[amp], obuf, ovec[1, amp])
+			    call amov$t (Mem$t[ptr], Mem$t[obuf], QG_NX(qg, amp))
+			}
+			ptr  = ptr + QG_NX(qg, amp)
+		    }
+		}
+	    }
+	}
+end
+
+# QJOINx -- Join multi-readout sub-images into a single image.
+
+procedure qjoin$t (in, out, qg)
+
+pointer	in[ARB]			#I Image pointer for input images.
+pointer	out			#I Image pointer for output image.
+pointer	qg			#I pointer to quadgeom structure.
+
+long	ivec[IM_MAXDIM, QG_MAXAMPS], ovec[IM_MAXDIM]
+int	amp, amp2, x, y, line, junk
+pointer	ibuf, obuf, ptr
+
+int	imgnl$t(), impnl$t()
+
+begin
+	# Setup start vectors for sequential reads ...
+	do amp = 1, QG_NAMPS (qg)
+	    call amovkl (long(1), ivec[1, amp], IM_MAXDIM)
+	# ... and writes
+	call amovkl (long(1), ovec, IM_MAXDIM)
+
+	do y = 1, QG_NAMPSY(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+	    do line = 1, QG_NY(qg, amp2) {
+		junk = impnl$t (out, obuf, ovec)
+		ptr = obuf
+		do x = 1, QG_NAMPSX(qg) {
+		    amp = QG_AMP(qg, x, y)
+		    junk = imgnl$t (in[amp], ibuf, ivec[1, amp])
+		    call amov$t (Mem$t[ibuf], Mem$t[ptr], QG_NX(qg, amp))
+		    ptr  = ptr + QG_NX(qg, amp)
+		}
+	    }
+	}
+end
diff --git a/noao/imred/quadred/src/quad/qsplitd.x b/noao/imred/quadred/src/quad/qsplitd.x
new file mode 100644
index 00000000..b7680f4d
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qsplitd.x
@@ -0,0 +1,97 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+# QSPLITx -- Split multi-readout image into separate images one for each 
+# readout.
+
+procedure qsplitd (in, out, qg)
+
+pointer	in			#I Image pointer for input image
+pointer	out[ARB]		#I Image pointer for output images
+pointer	qg			#I pointer to quadgeom structure
+
+long	ivec[IM_MAXDIM], ovec[IM_MAXDIM, QG_MAXAMPS]
+int	amp, amp2, x, y, line, junk
+pointer	ibuf, obuf, ptr
+bool	all_phantom
+
+int	imgnld(), impnld()
+
+begin
+	# Setup start vectors for sequential reads ...
+	call amovkl (long(1), ivec, IM_MAXDIM)
+	# ... and writes
+	do amp = 1, QG_NAMPS (qg)
+	    call amovkl (long(1), ovec[1, amp], IM_MAXDIM)
+
+	do y = 1, QG_NAMPSY(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+
+	    # Check to see if there are any non phantom regions in this tier
+	    all_phantom = true
+	    do x = 1, QG_NAMPSX(qg) {
+		amp = QG_AMP(qg, x, y)
+		if (QG_PHANTOM (qg, amp) == NO) {
+		    all_phantom = false 
+		    break
+		}
+	    }
+
+	    if (all_phantom) {
+
+		# Reset start vector for reads to skip phantom data
+		ivec[2] = ivec[2] + long (QG_NY (qg, amp2))
+
+	    } else {
+
+		do line = 1, QG_NY(qg, amp2) {
+		    junk = imgnld (in, ibuf, ivec)
+		    ptr = ibuf
+		    do x = 1, QG_NAMPSX(qg) {
+			amp = QG_AMP(qg, x, y)
+			if (QG_PHANTOM (qg, amp) == NO) {
+			    junk = impnld (out[amp], obuf, ovec[1, amp])
+			    call amovd (Memd[ptr], Memd[obuf], QG_NX(qg, amp))
+			}
+			ptr  = ptr + QG_NX(qg, amp)
+		    }
+		}
+	    }
+	}
+end
+
+# QJOINx -- Join multi-readout sub-images into a single image.
+
+procedure qjoind (in, out, qg)
+
+pointer	in[ARB]			#I Image pointer for input images.
+pointer	out			#I Image pointer for output image.
+pointer	qg			#I pointer to quadgeom structure.
+
+long	ivec[IM_MAXDIM, QG_MAXAMPS], ovec[IM_MAXDIM]
+int	amp, amp2, x, y, line, junk
+pointer	ibuf, obuf, ptr
+
+int	imgnld(), impnld()
+
+begin
+	# Setup start vectors for sequential reads ...
+	do amp = 1, QG_NAMPS (qg)
+	    call amovkl (long(1), ivec[1, amp], IM_MAXDIM)
+	# ... and writes
+	call amovkl (long(1), ovec, IM_MAXDIM)
+
+	do y = 1, QG_NAMPSY(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+	    do line = 1, QG_NY(qg, amp2) {
+		junk = impnld (out, obuf, ovec)
+		ptr = obuf
+		do x = 1, QG_NAMPSX(qg) {
+		    amp = QG_AMP(qg, x, y)
+		    junk = imgnld (in[amp], ibuf, ivec[1, amp])
+		    call amovd (Memd[ibuf], Memd[ptr], QG_NX(qg, amp))
+		    ptr  = ptr + QG_NX(qg, amp)
+		}
+	    }
+	}
+end
diff --git a/noao/imred/quadred/src/quad/qspliti.x b/noao/imred/quadred/src/quad/qspliti.x
new file mode 100644
index 00000000..84aa5fc7
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qspliti.x
@@ -0,0 +1,97 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+# QSPLITx -- Split multi-readout image into separate images one for each 
+# readout.
+
+procedure qspliti (in, out, qg)
+
+pointer	in			#I Image pointer for input image
+pointer	out[ARB]		#I Image pointer for output images
+pointer	qg			#I pointer to quadgeom structure
+
+long	ivec[IM_MAXDIM], ovec[IM_MAXDIM, QG_MAXAMPS]
+int	amp, amp2, x, y, line, junk
+pointer	ibuf, obuf, ptr
+bool	all_phantom
+
+int	imgnli(), impnli()
+
+begin
+	# Setup start vectors for sequential reads ...
+	call amovkl (long(1), ivec, IM_MAXDIM)
+	# ... and writes
+	do amp = 1, QG_NAMPS (qg)
+	    call amovkl (long(1), ovec[1, amp], IM_MAXDIM)
+
+	do y = 1, QG_NAMPSY(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+
+	    # Check to see if there are any non phantom regions in this tier
+	    all_phantom = true
+	    do x = 1, QG_NAMPSX(qg) {
+		amp = QG_AMP(qg, x, y)
+		if (QG_PHANTOM (qg, amp) == NO) {
+		    all_phantom = false 
+		    break
+		}
+	    }
+
+	    if (all_phantom) {
+
+		# Reset start vector for reads to skip phantom data
+		ivec[2] = ivec[2] + long (QG_NY (qg, amp2))
+
+	    } else {
+
+		do line = 1, QG_NY(qg, amp2) {
+		    junk = imgnli (in, ibuf, ivec)
+		    ptr = ibuf
+		    do x = 1, QG_NAMPSX(qg) {
+			amp = QG_AMP(qg, x, y)
+			if (QG_PHANTOM (qg, amp) == NO) {
+			    junk = impnli (out[amp], obuf, ovec[1, amp])
+			    call amovi (Memi[ptr], Memi[obuf], QG_NX(qg, amp))
+			}
+			ptr  = ptr + QG_NX(qg, amp)
+		    }
+		}
+	    }
+	}
+end
+
+# QJOINx -- Join multi-readout sub-images into a single image.
+
+procedure qjoini (in, out, qg)
+
+pointer	in[ARB]			#I Image pointer for input images.
+pointer	out			#I Image pointer for output image.
+pointer	qg			#I pointer to quadgeom structure.
+
+long	ivec[IM_MAXDIM, QG_MAXAMPS], ovec[IM_MAXDIM]
+int	amp, amp2, x, y, line, junk
+pointer	ibuf, obuf, ptr
+
+int	imgnli(), impnli()
+
+begin
+	# Setup start vectors for sequential reads ...
+	do amp = 1, QG_NAMPS (qg)
+	    call amovkl (long(1), ivec[1, amp], IM_MAXDIM)
+	# ... and writes
+	call amovkl (long(1), ovec, IM_MAXDIM)
+
+	do y = 1, QG_NAMPSY(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+	    do line = 1, QG_NY(qg, amp2) {
+		junk = impnli (out, obuf, ovec)
+		ptr = obuf
+		do x = 1, QG_NAMPSX(qg) {
+		    amp = QG_AMP(qg, x, y)
+		    junk = imgnli (in[amp], ibuf, ivec[1, amp])
+		    call amovi (Memi[ibuf], Memi[ptr], QG_NX(qg, amp))
+		    ptr  = ptr + QG_NX(qg, amp)
+		}
+	    }
+	}
+end
diff --git a/noao/imred/quadred/src/quad/qsplitl.x b/noao/imred/quadred/src/quad/qsplitl.x
new file mode 100644
index 00000000..5e1d0e7e
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qsplitl.x
@@ -0,0 +1,97 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+# QSPLITx -- Split multi-readout image into separate images one for each 
+# readout.
+
+procedure qsplitl (in, out, qg)
+
+pointer	in			#I Image pointer for input image
+pointer	out[ARB]		#I Image pointer for output images
+pointer	qg			#I pointer to quadgeom structure
+
+long	ivec[IM_MAXDIM], ovec[IM_MAXDIM, QG_MAXAMPS]
+int	amp, amp2, x, y, line, junk
+pointer	ibuf, obuf, ptr
+bool	all_phantom
+
+int	imgnll(), impnll()
+
+begin
+	# Setup start vectors for sequential reads ...
+	call amovkl (long(1), ivec, IM_MAXDIM)
+	# ... and writes
+	do amp = 1, QG_NAMPS (qg)
+	    call amovkl (long(1), ovec[1, amp], IM_MAXDIM)
+
+	do y = 1, QG_NAMPSY(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+
+	    # Check to see if there are any non phantom regions in this tier
+	    all_phantom = true
+	    do x = 1, QG_NAMPSX(qg) {
+		amp = QG_AMP(qg, x, y)
+		if (QG_PHANTOM (qg, amp) == NO) {
+		    all_phantom = false 
+		    break
+		}
+	    }
+
+	    if (all_phantom) {
+
+		# Reset start vector for reads to skip phantom data
+		ivec[2] = ivec[2] + long (QG_NY (qg, amp2))
+
+	    } else {
+
+		do line = 1, QG_NY(qg, amp2) {
+		    junk = imgnll (in, ibuf, ivec)
+		    ptr = ibuf
+		    do x = 1, QG_NAMPSX(qg) {
+			amp = QG_AMP(qg, x, y)
+			if (QG_PHANTOM (qg, amp) == NO) {
+			    junk = impnll (out[amp], obuf, ovec[1, amp])
+			    call amovl (Meml[ptr], Meml[obuf], QG_NX(qg, amp))
+			}
+			ptr  = ptr + QG_NX(qg, amp)
+		    }
+		}
+	    }
+	}
+end
+
+# QJOINx -- Join multi-readout sub-images into a single image.
+
+procedure qjoinl (in, out, qg)
+
+pointer	in[ARB]			#I Image pointer for input images.
+pointer	out			#I Image pointer for output image.
+pointer	qg			#I pointer to quadgeom structure.
+
+long	ivec[IM_MAXDIM, QG_MAXAMPS], ovec[IM_MAXDIM]
+int	amp, amp2, x, y, line, junk
+pointer	ibuf, obuf, ptr
+
+int	imgnll(), impnll()
+
+begin
+	# Setup start vectors for sequential reads ...
+	do amp = 1, QG_NAMPS (qg)
+	    call amovkl (long(1), ivec[1, amp], IM_MAXDIM)
+	# ... and writes
+	call amovkl (long(1), ovec, IM_MAXDIM)
+
+	do y = 1, QG_NAMPSY(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+	    do line = 1, QG_NY(qg, amp2) {
+		junk = impnll (out, obuf, ovec)
+		ptr = obuf
+		do x = 1, QG_NAMPSX(qg) {
+		    amp = QG_AMP(qg, x, y)
+		    junk = imgnll (in[amp], ibuf, ivec[1, amp])
+		    call amovl (Meml[ibuf], Meml[ptr], QG_NX(qg, amp))
+		    ptr  = ptr + QG_NX(qg, amp)
+		}
+	    }
+	}
+end
diff --git a/noao/imred/quadred/src/quad/qsplitr.x b/noao/imred/quadred/src/quad/qsplitr.x
new file mode 100644
index 00000000..adba483d
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qsplitr.x
@@ -0,0 +1,97 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+# QSPLITx -- Split multi-readout image into separate images one for each 
+# readout.
+
+procedure qsplitr (in, out, qg)
+
+pointer	in			#I Image pointer for input image
+pointer	out[ARB]		#I Image pointer for output images
+pointer	qg			#I pointer to quadgeom structure
+
+long	ivec[IM_MAXDIM], ovec[IM_MAXDIM, QG_MAXAMPS]
+int	amp, amp2, x, y, line, junk
+pointer	ibuf, obuf, ptr
+bool	all_phantom
+
+int	imgnlr(), impnlr()
+
+begin
+	# Setup start vectors for sequential reads ...
+	call amovkl (long(1), ivec, IM_MAXDIM)
+	# ... and writes
+	do amp = 1, QG_NAMPS (qg)
+	    call amovkl (long(1), ovec[1, amp], IM_MAXDIM)
+
+	do y = 1, QG_NAMPSY(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+
+	    # Check to see if there are any non phantom regions in this tier
+	    all_phantom = true
+	    do x = 1, QG_NAMPSX(qg) {
+		amp = QG_AMP(qg, x, y)
+		if (QG_PHANTOM (qg, amp) == NO) {
+		    all_phantom = false 
+		    break
+		}
+	    }
+
+	    if (all_phantom) {
+
+		# Reset start vector for reads to skip phantom data
+		ivec[2] = ivec[2] + long (QG_NY (qg, amp2))
+
+	    } else {
+
+		do line = 1, QG_NY(qg, amp2) {
+		    junk = imgnlr (in, ibuf, ivec)
+		    ptr = ibuf
+		    do x = 1, QG_NAMPSX(qg) {
+			amp = QG_AMP(qg, x, y)
+			if (QG_PHANTOM (qg, amp) == NO) {
+			    junk = impnlr (out[amp], obuf, ovec[1, amp])
+			    call amovr (Memr[ptr], Memr[obuf], QG_NX(qg, amp))
+			}
+			ptr  = ptr + QG_NX(qg, amp)
+		    }
+		}
+	    }
+	}
+end
+
+# QJOINx -- Join multi-readout sub-images into a single image.
+
+procedure qjoinr (in, out, qg)
+
+pointer	in[ARB]			#I Image pointer for input images.
+pointer	out			#I Image pointer for output image.
+pointer	qg			#I pointer to quadgeom structure.
+
+long	ivec[IM_MAXDIM, QG_MAXAMPS], ovec[IM_MAXDIM]
+int	amp, amp2, x, y, line, junk
+pointer	ibuf, obuf, ptr
+
+int	imgnlr(), impnlr()
+
+begin
+	# Setup start vectors for sequential reads ...
+	do amp = 1, QG_NAMPS (qg)
+	    call amovkl (long(1), ivec[1, amp], IM_MAXDIM)
+	# ... and writes
+	call amovkl (long(1), ovec, IM_MAXDIM)
+
+	do y = 1, QG_NAMPSY(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+	    do line = 1, QG_NY(qg, amp2) {
+		junk = impnlr (out, obuf, ovec)
+		ptr = obuf
+		do x = 1, QG_NAMPSX(qg) {
+		    amp = QG_AMP(qg, x, y)
+		    junk = imgnlr (in[amp], ibuf, ivec[1, amp])
+		    call amovr (Memr[ibuf], Memr[ptr], QG_NX(qg, amp))
+		    ptr  = ptr + QG_NX(qg, amp)
+		}
+	    }
+	}
+end
diff --git a/noao/imred/quadred/src/quad/qsplits.x b/noao/imred/quadred/src/quad/qsplits.x
new file mode 100644
index 00000000..b4eaba80
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qsplits.x
@@ -0,0 +1,97 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+# QSPLITx -- Split multi-readout image into separate images one for each 
+# readout.
+
+procedure qsplits (in, out, qg)
+
+pointer	in			#I Image pointer for input image
+pointer	out[ARB]		#I Image pointer for output images
+pointer	qg			#I pointer to quadgeom structure
+
+long	ivec[IM_MAXDIM], ovec[IM_MAXDIM, QG_MAXAMPS]
+int	amp, amp2, x, y, line, junk
+pointer	ibuf, obuf, ptr
+bool	all_phantom
+
+int	imgnls(), impnls()
+
+begin
+	# Setup start vectors for sequential reads ...
+	call amovkl (long(1), ivec, IM_MAXDIM)
+	# ... and writes
+	do amp = 1, QG_NAMPS (qg)
+	    call amovkl (long(1), ovec[1, amp], IM_MAXDIM)
+
+	do y = 1, QG_NAMPSY(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+
+	    # Check to see if there are any non phantom regions in this tier
+	    all_phantom = true
+	    do x = 1, QG_NAMPSX(qg) {
+		amp = QG_AMP(qg, x, y)
+		if (QG_PHANTOM (qg, amp) == NO) {
+		    all_phantom = false 
+		    break
+		}
+	    }
+
+	    if (all_phantom) {
+
+		# Reset start vector for reads to skip phantom data
+		ivec[2] = ivec[2] + long (QG_NY (qg, amp2))
+
+	    } else {
+
+		do line = 1, QG_NY(qg, amp2) {
+		    junk = imgnls (in, ibuf, ivec)
+		    ptr = ibuf
+		    do x = 1, QG_NAMPSX(qg) {
+			amp = QG_AMP(qg, x, y)
+			if (QG_PHANTOM (qg, amp) == NO) {
+			    junk = impnls (out[amp], obuf, ovec[1, amp])
+			    call amovs (Mems[ptr], Mems[obuf], QG_NX(qg, amp))
+			}
+			ptr  = ptr + QG_NX(qg, amp)
+		    }
+		}
+	    }
+	}
+end
+
+# QJOINx -- Join multi-readout sub-images into a single image.
+
+procedure qjoins (in, out, qg)
+
+pointer	in[ARB]			#I Image pointer for input images.
+pointer	out			#I Image pointer for output image.
+pointer	qg			#I pointer to quadgeom structure.
+
+long	ivec[IM_MAXDIM, QG_MAXAMPS], ovec[IM_MAXDIM]
+int	amp, amp2, x, y, line, junk
+pointer	ibuf, obuf, ptr
+
+int	imgnls(), impnls()
+
+begin
+	# Setup start vectors for sequential reads ...
+	do amp = 1, QG_NAMPS (qg)
+	    call amovkl (long(1), ivec[1, amp], IM_MAXDIM)
+	# ... and writes
+	call amovkl (long(1), ovec, IM_MAXDIM)
+
+	do y = 1, QG_NAMPSY(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+	    do line = 1, QG_NY(qg, amp2) {
+		junk = impnls (out, obuf, ovec)
+		ptr = obuf
+		do x = 1, QG_NAMPSX(qg) {
+		    amp = QG_AMP(qg, x, y)
+		    junk = imgnls (in[amp], ibuf, ivec[1, amp])
+		    call amovs (Mems[ibuf], Mems[ptr], QG_NX(qg, amp))
+		    ptr  = ptr + QG_NX(qg, amp)
+		}
+	    }
+	}
+end
diff --git a/noao/imred/quadred/src/quad/qstatistics.cl b/noao/imred/quadred/src/quad/qstatistics.cl
new file mode 100644
index 00000000..a20f373f
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qstatistics.cl
@@ -0,0 +1,19 @@
+procedure qstatistics (images)
+
+begin
+	string	tmp
+
+	tmp = mktemp ("uparm$tmp")
+
+	#quadsections (image, window=window, section="", template="",
+	#xskip1=INDEF, xskip2=INDEF, xtrim1=INDEF, xtrim2=INDEF, ytrim1=INDEF,
+	#ytrim2=INDEF, >> tmp)
+	quadsections (image, window=window, section="", template="", >> tmp)
+
+	# Calculate image statistics
+	imstatistics ("@"//tmp, fields=fields, lower=lower, upper=upper,
+	binwidth=binwidth, format=format)
+
+
+	delete (tmp, ver-)
+end
diff --git a/noao/imred/quadred/src/quad/qstatistics.par b/noao/imred/quadred/src/quad/qstatistics.par
new file mode 100644
index 00000000..92a32f66
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qstatistics.par
@@ -0,0 +1,7 @@
+images,s,a,,,,Images
+window,s,h,"datasec","|datasec|trimsec|biassec|reflect|duplicate|",,Window to apply to image
+fields,s,h,"image,npix,mean,stddev,min,max",,,Fields to be printed
+lower,r,h,INDEF,,,Lower cutoff for pixel values
+upper,r,h,INDEF,,,Upper cutoff for pixel values
+binwidth,r,h,0.1,,,Bin width of histogram in sigma
+format,b,h,yes,,,Format output and print column labels?
diff --git a/noao/imred/quadred/src/quad/quad.cl b/noao/imred/quadred/src/quad/quad.cl
new file mode 100644
index 00000000..b08434c0
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quad.cl
@@ -0,0 +1,64 @@
+#{ QUAD -- Quad CCD reduction package
+
+noao
+imred
+
+set	ccddb			= "quad$ccddb/"
+set	quadtest 		= "quad$quadtest/"
+
+package quad
+
+task	quadtest.pkg		= "quadtest$quadtest.cl"
+
+task	quadsplit,
+	quadjoin,
+	quadscale,
+	quadsections,
+	ccddelete,
+	ccdprcselect,
+	ccdssselect,
+	ccdsection,
+	qpcalimage,
+	qpselect,
+	irlincor,
+	gainmeasure,
+#	ccdgetparam		= "quad$xx_quad.e"
+	ccdgetparam		= "quad$x_quad.e"
+
+task	quadproc		= "quad$quadproc.cl"
+task	qproc			= "quad$qproc.cl"
+task	qnoproc			= "quad$qnoproc.cl"
+task	qstatistics		= "quad$qstatistics.cl"
+task	qhistogram		= "quad$qhistogram.cl"
+
+hidetask ccdgetparam, ccddelete, ccdprcselect, ccdssselect, ccdsection
+hidetask qpcalimage, qpselect, qproc, qnoproc, quadsplit, quadjoin, quadsections
+
+# CCDRED tasks.
+task	badpiximage,
+	ccdgroups,
+	ccdhedit,
+	ccdinstrument,
+	ccdlist,
+	combine,
+	cosmicrays = ccdred$x_ccdred.e
+#	cosmicrays,
+#	mkfringecor,
+#	mkillumcor,
+#	mkillumflat,
+#	mkskycor,
+#	mkskyflat = ccdred$x_ccdred.e
+
+task	setinstrument	= quad$setinstrument.cl
+
+# Different default parameters
+task	qccdproc	= quad$x_ccdred.e
+
+# Special versions which run quadproc rather than ccdproc
+task	darkcombine	= quad$darkcombine.cl
+task	flatcombine	= quad$flatcombine.cl
+task	zerocombine	= quad$zerocombine.cl
+
+hidetask ccdproc
+
+clbye()
diff --git a/noao/imred/quadred/src/quad/quad.hd b/noao/imred/quadred/src/quad/quad.hd
new file mode 100644
index 00000000..b8526c66
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quad.hd
@@ -0,0 +1,33 @@
+# Help directory for the QUAD package.
+
+$defdir		= "quad$"
+$doc 		= "quad$doc/"
+
+badpiximage	hlp=doc$badpiximage.hlp	
+ccdgroups	hlp=doc$ccdgroups.hlp
+ccdhedit	hlp=doc$ccdhedit.hlp
+ccdlist		hlp=doc$ccdlist.hlp
+combine		hlp=doc$combine.hlp
+cosmicrays	hlp=doc$cosmicrays.hlp
+darkcombine	hlp=doc$darkcombine.hlp
+flatcombine	hlp=doc$flatcombine.hlp
+mkfringecor	hlp=doc$mkfringecor.hlp
+mkillumcor	hlp=doc$mkillumcor.hlp
+mkillumflat	hlp=doc$mkillumflat.hlp
+mkskycor	hlp=doc$mkskycor.hlp
+mkskyflat	hlp=doc$mkskyflat.hlp
+quadproc	hlp=doc$quadproc.hlp
+quadscale	hlp=doc$quadscale.hlp
+qhistogram	hlp=doc$qhistogram.hlp
+qstatistics	hlp=doc$qstatistics.hlp
+setinstrument	hlp=doc$setinstrument.hlp
+zerocombine	hlp=doc$zerocombine.hlp
+
+ccdgeometry	hlp=doc$ccdgeometry.hlp
+ccdinstrument	hlp=doc$ccdinst.hlp
+ccdtypes	hlp=doc$ccdtypes.hlp
+flatfields	hlp=doc$flatfields.hlp
+guide		hlp=doc$guide.hlp
+instruments	hlp=doc$instruments.hlp
+package		hlp=doc$quad.hlp
+subsets		hlp=doc$subsets.hlp
diff --git a/noao/imred/quadred/src/quad/quad.men b/noao/imred/quadred/src/quad/quad.men
new file mode 100644
index 00000000..6b323daf
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quad.men
@@ -0,0 +1,36 @@
+	     SPECIAL TASKS FOR MULTI-READOUT CCD IMAGES
+
+       quadproc - Process multi-readout CCD images
+      quadscale - 
+    qstatistics - Calculate image statistics for multi-readout CCD images
+     qhistogram - Make histogram of multi-readout CCD image
+    darkcombine - Combine and process dark count images
+    flatcombine - Combine and process flat field images
+    zerocombine - Combine and process zero level images
+
+
+	    STANDARD CCDRED TASKS
+
+    badpiximage - Create a bad pixel mask image from a bad pixel file
+      ccdgroups - Group CCD images into image lists
+       ccdhedit - CCD image header editor
+  ccdinstrument - Review and edit instrument translation files
+        ccdlist - List CCD processing information
+        combine - Combine CCD images
+     cosmicrays - Detect and replace cosmic rays
+    mkfringecor - Make fringe correction images from sky images
+     mkillumcor - Make flat field illumination correction images
+    mkillumflat - Make illumination corrected flat fields
+       mkskycor - Make sky illumination correction images
+      mkskyflat - Make sky corrected flat field images
+  setinstrument - Set instrument parameters
+
+    	      ADDITIONAL HELP TOPICS
+
+    ccdgeometry - Discussion of CCD coordinate/geometry keywords
+       ccdtypes - Description of the CCD image types
+     flatfields - Discussion of CCD flat field calibrations
+          guide - Introductory guide to using the CCDRED package
+    instruments - Instrument specific data files
+        package - CCD image reduction package
+        subsets - Description of CCD subsets
diff --git a/noao/imred/quadred/src/quad/quad.par b/noao/imred/quadred/src/quad/quad.par
new file mode 100644
index 00000000..74267f31
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quad.par
@@ -0,0 +1,12 @@
+# QUAD package parameter file
+
+pixeltype,s,h,"real real",,,Output and calculation pixel datatypes
+verbose,b,h,no,,,Print log information to the standard output?
+logfile,f,h,"logfile",,,Text log file
+plotfile,f,h,"",,,Log metacode plot file
+backup,s,h,"",,,Backup directory or prefix
+instrument,s,h,"",,,CCD instrument file
+ssfile,s,h,"subsets",,,Subset translation file
+graphics,s,h,"stdgraph",,,Interactive graphics output device
+cursor,*gcur,h,"",,,Graphics cursor input
+version,s,h,"Version 2.0 - Mar 94","Version 2.0 - Mar 94"  
diff --git a/noao/imred/quadred/src/quad/quadalloc.x b/noao/imred/quadred/src/quad/quadalloc.x
new file mode 100644
index 00000000..9373340a
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadalloc.x
@@ -0,0 +1,165 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+# QUADOPEN -- Allocate space for quadgeom structure
+# Note: The various arrays are dimensioned as QG_MAXAMPS+1 and are ZERO indexed.
+
+procedure quadalloc (qg)
+
+pointer	qg			#O Pointer to opened quadgeom structure
+
+begin
+
+	call malloc (qg, QG_LENSTRUCT, TY_STRUCT)
+
+	# Zero readout counters
+	QG_NAMPS(qg)  = 0
+	QG_NAMPSX(qg) = 0
+	QG_NAMPSY(qg) = 0
+
+	# Allocate and zero arrays.
+	call calloc (QG_AMPIDPTR(qg), QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_AMPTYPTR(qg), QG_MAXAMPS+1, TY_INT)
+
+	call calloc (QG_NXPTR(qg),    QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_NYPTR(qg),    QG_MAXAMPS+1, TY_INT)
+
+	call calloc (QG_DX1PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_DX2PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_DY1PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_DY2PTR(qg),   QG_MAXAMPS+1, TY_INT)
+
+	call calloc (QG_TX1PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_TX2PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_TY1PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_TY2PTR(qg),   QG_MAXAMPS+1, TY_INT)
+
+	call calloc (QG_BX1PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_BX2PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_BY1PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_BY2PTR(qg),   QG_MAXAMPS+1, TY_INT)
+ 
+	call calloc (QG_CX1PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_CX2PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_CY1PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_CY2PTR(qg),   QG_MAXAMPS+1, TY_INT)
+
+	call calloc (QG_AX1PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_AX2PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_AY1PTR(qg),   QG_MAXAMPS+1, TY_INT)
+	call calloc (QG_AY2PTR(qg),   QG_MAXAMPS+1, TY_INT)
+
+	call calloc (QG_PHPTR(qg),    QG_MAXAMPS+1, TY_INT)
+
+end
+
+# QUADFREE -- Free quadgeom structure
+
+procedure quadfree (qg)
+
+pointer	qg			#O Pointer to open quadgeom structure
+
+begin
+
+	if (qg != NULL) {
+	   
+	    call mfree (QG_AMPIDPTR(qg), TY_INT)
+	    call mfree (QG_AMPTYPTR(qg), TY_INT)
+
+	    call mfree (QG_NXPTR(qg),    TY_INT)
+	    call mfree (QG_NYPTR(qg),    TY_INT)
+
+	    call mfree (QG_DX1PTR(qg),   TY_INT)
+	    call mfree (QG_DX2PTR(qg),   TY_INT)
+	    call mfree (QG_DY1PTR(qg),   TY_INT)
+	    call mfree (QG_DY2PTR(qg),   TY_INT)
+
+	    call mfree (QG_TX1PTR(qg),   TY_INT)
+	    call mfree (QG_TX2PTR(qg),   TY_INT)
+	    call mfree (QG_TY1PTR(qg),   TY_INT)
+	    call mfree (QG_TY2PTR(qg),   TY_INT)
+
+	    call mfree (QG_BX1PTR(qg),   TY_INT)
+	    call mfree (QG_BX2PTR(qg),   TY_INT)
+	    call mfree (QG_BY1PTR(qg),   TY_INT)
+	    call mfree (QG_BY2PTR(qg),   TY_INT)
+
+	    call mfree (QG_CX1PTR(qg),   TY_INT)
+	    call mfree (QG_CX2PTR(qg),   TY_INT)
+	    call mfree (QG_CY1PTR(qg),   TY_INT)
+	    call mfree (QG_CY2PTR(qg),   TY_INT)
+
+	    call mfree (QG_AX1PTR(qg),   TY_INT)
+	    call mfree (QG_AX2PTR(qg),   TY_INT)
+	    call mfree (QG_AY1PTR(qg),   TY_INT)
+	    call mfree (QG_AY2PTR(qg),   TY_INT)
+
+	    call mfree (QG_PHPTR(qg),    TY_INT)
+
+	    call mfree (qg, TY_STRUCT)
+	}
+end
+
+# QUADDUMP -- Print contents of quadgeom structure on STDERR
+procedure quaddump (qg)
+
+pointer	qg			#O Pointer to open quadgeom structure
+
+int	amp
+
+begin
+
+	call eprintf ("Active amps: %d (%d in x, %d in y)\n")
+	    call pargi (QG_NAMPS(qg))
+	    call pargi (QG_NAMPSX(qg))
+	    call pargi (QG_NAMPSY(qg))
+
+	do amp = 0, QG_NAMPS(qg) {
+	    switch (amp) {
+	    case 0:
+		call eprintf ("Entire image\n")
+	    default:
+		call eprintf ("Amp %s")
+		    call pargstr (Memc[QG_AMPID(qg, amp)])
+
+		if (QG_PHANTOM (qg, amp) == YES)
+		    call eprintf (" [Phantom]")
+
+		call eprintf ("\n")
+	    }
+
+	    call eprintf ("\tnx = %d \tny = %d \n")
+		call pargi (QG_NX(qg, amp))
+		call pargi (QG_NY(qg, amp))
+
+	    call eprintf ("\tdx1 = %d \tdx2 = %d \tdy1 = %d \tdy2 = %d\n")
+		call pargi (QG_DX1(qg, amp))
+		call pargi (QG_DX2(qg, amp))
+		call pargi (QG_DY1(qg, amp))
+		call pargi (QG_DY2(qg, amp))
+
+	    call eprintf ("\ttx1 = %d \ttx2 = %d \tty1 = %d \tty2 = %d\n")
+		call pargi (QG_TX1(qg, amp))
+		call pargi (QG_TX2(qg, amp))
+		call pargi (QG_TY1(qg, amp))
+		call pargi (QG_TY2(qg, amp))
+
+	    call eprintf ("\tbx1 = %d \tbx2 = %d \tby1 = %d \tby2 = %d\n")
+		call pargi (QG_BX1(qg, amp))
+		call pargi (QG_BX2(qg, amp))
+		call pargi (QG_BY1(qg, amp))
+		call pargi (QG_BY2(qg, amp))
+
+	    call eprintf ("\tcx1 = %d \tcx2 = %d \tcy1 = %d \tcy2 = %d\n")
+		call pargi (QG_CX1(qg, amp))
+		call pargi (QG_CX2(qg, amp))
+		call pargi (QG_CY1(qg, amp))
+		call pargi (QG_CY2(qg, amp))
+
+	    call eprintf ("\tax1 = %d \tax2 = %d \tay1 = %d \tay2 = %d\n")
+		call pargi (QG_AX1(qg, amp))
+		call pargi (QG_AX2(qg, amp))
+		call pargi (QG_AY1(qg, amp))
+		call pargi (QG_AY2(qg, amp))
+	}
+end
diff --git a/noao/imred/quadred/src/quad/quaddelete.x b/noao/imred/quadred/src/quad/quaddelete.x
new file mode 100644
index 00000000..bdee65b2
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quaddelete.x
@@ -0,0 +1,39 @@
+include "quadgeom.h"
+
+# QUADDELETE --  Delete subimages, one for each readout.
+
+procedure quaddelete (qg, rootname)
+
+pointer	qg		#I Pointer to open quadgeom structure
+char	rootname[ARB]	#I Root name for subimages.
+
+int	amp
+pointer	fullname
+
+pointer	sp
+int	imaccess()
+
+begin
+	call smark (sp)
+	call salloc (fullname, SZ_LINE, TY_CHAR)
+
+	# Loop over active readouts
+	do amp = 1, QG_NAMPS(qg) {
+
+	    # The sub-section image will only exist if this is not a phantom
+	    if (QG_PHANTOM (qg, amp) == NO) {
+
+		# Make sub-image name
+		call sprintf (Memc[fullname], SZ_LINE, "%s.%s")
+		    call pargstr (rootname)
+		    call pargstr (Memc[QG_AMPID(qg, amp)])
+
+		# Delete the sub-image (if it exists)
+		if (imaccess (Memc[fullname], READ_ONLY) == YES) {
+		    call imdelete (Memc[fullname])
+		}
+	    }
+	}
+	
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/quad/quadgeom.h b/noao/imred/quadred/src/quad/quadgeom.h
new file mode 100644
index 00000000..090b4bf2
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadgeom.h
@@ -0,0 +1,99 @@
+# QUADGEOM - Structure definitions and macros for quadgeom structure.
+
+define QG_LENSTRUCT    28		# Length of structure.
+define QG_MAXAMPS	4		# Maximum possible number of readouts.
+# The various arrays are dimensioned as QG_MAXAMPS+1.
+# QG_AAAA(0) contains quantities refering to the entire image
+# QG_AAAA(z) contains quantities refering to the zth sub-image
+
+define QG_NAMPS		Memi[$1]	# Total number of active readouts.
+define QG_NAMPSX	Memi[$1+1]	# Number of active readouts in X.
+define QG_NAMPSY	Memi[$1+2]	# Number of active readouts in Y.
+
+# Array of pointers to names of active readouts.
+define QG_AMPIDPTR	Memi[$1+3]			# --> ampid  array.
+define QG_AMPID		Memi[QG_AMPIDPTR($1)+$2]	# ampid  array.
+
+# Array of pointers to names of active readouts.
+define QG_AMPTYPTR	Memi[$1+4]			# --> amptype  array.
+define QG_AMPTYPE	Memi[QG_AMPTYPTR($1)+$2]	# amptype  array.
+
+# Dimensions of image from each readout.
+define QG_NXPTR		Memi[$1+5]			# --> X dimension array.
+define QG_NX		Memi[QG_NXPTR($1)+$2]		# X dimension.
+define QG_NYPTR		Memi[$1+6]			# --> Y dimension array.
+define QG_NY		Memi[QG_NYPTR($1)+$2]		# Y dimension.
+
+# datasec = "[dx1:dx2,dy1:dy2]"
+define QG_DOFF		7
+define QG_DX1PTR	Memi[$1+QG_DOFF]		# --> dx1 array.
+define QG_DX2PTR	Memi[$1+QG_DOFF+1]		# --> dx2 array.
+define QG_DY1PTR	Memi[$1+QG_DOFF+2]		# --> dy1 array.
+define QG_DY2PTR	Memi[$1+QG_DOFF+3]		# --> dy2 array.
+define QG_DX1		Memi[QG_DX1PTR($1)+$2]		# dx1.
+define QG_DX2		Memi[QG_DX2PTR($1)+$2]		# dx2.
+define QG_DY1		Memi[QG_DY1PTR($1)+$2]		# dy1..
+define QG_DY2		Memi[QG_DY2PTR($1)+$2]		# dy2.
+
+# trimsec = "[tx1:tx2,ty1:ty2]"
+define QG_TOFF		11				# QG_DOFF+4.
+define QG_TX1PTR	Memi[$1+QG_TOFF]		# --> tx1 array.
+define QG_TX2PTR	Memi[$1+QG_TOFF+1]		# --> tx2 array.
+define QG_TY1PTR	Memi[$1+QG_TOFF+2]		# --> ty1 array.
+define QG_TY2PTR	Memi[$1+QG_TOFF+3]		# --> ty2 array.
+define QG_TX1		Memi[QG_TX1PTR($1)+$2]		# tx1.
+define QG_TX2		Memi[QG_TX2PTR($1)+$2]		# tx2.
+define QG_TY1		Memi[QG_TY1PTR($1)+$2]		# ty1.
+define QG_TY2		Memi[QG_TY2PTR($1)+$2]		# ty2.
+
+# biassec = "[bx1:bx2,by1:by2]"
+define QG_BOFF		15				# QG_TOFF+4.
+define QG_BX1PTR	Memi[$1+QG_BOFF]		# --> bx1 array.
+define QG_BX2PTR	Memi[$1+QG_BOFF+1]		# --> bx2 array.
+define QG_BY1PTR	Memi[$1+QG_BOFF+2]		# --> by1 array.
+define QG_BY2PTR	Memi[$1+QG_BOFF+3]		# --> by2 array.
+define QG_BX1		Memi[QG_BX1PTR($1)+$2]		# bx1.
+define QG_BX2		Memi[QG_BX2PTR($1)+$2]		# bx2.
+define QG_BY1		Memi[QG_BY1PTR($1)+$2]		# by1.
+define QG_BY2		Memi[QG_BY2PTR($1)+$2]		# by2.
+
+# ccdsec = "[cx1:cx2,cy1:cy2]"
+define QG_COFF		19				# QG_BOFF+4.
+define QG_CX1PTR	Memi[$1+QG_COFF]		# --> cx1 array.
+define QG_CX2PTR	Memi[$1+QG_COFF+1]		# --> cx2 array.
+define QG_CY1PTR	Memi[$1+QG_COFF+2]		# --> cy1 array.
+define QG_CY2PTR	Memi[$1+QG_COFF+3]		# --> cy2 array.
+define QG_CX1		Memi[QG_CX1PTR($1)+$2]		# cx1.
+define QG_CX2		Memi[QG_CX2PTR($1)+$2]		# cx2.
+define QG_CY1		Memi[QG_CY1PTR($1)+$2]		# cy1.
+define QG_CY2		Memi[QG_CY2PTR($1)+$2]		# cy2.
+
+# ampsec = "[ax1:ax2,ay1:ay2]"
+define QG_AOFF		23				# QG_COFF+4.
+define QG_AX1PTR	Memi[$1+QG_AOFF]		# --> ax1 array.
+define QG_AX2PTR	Memi[$1+QG_AOFF+1]		# --> ax2 array.
+define QG_AY1PTR	Memi[$1+QG_AOFF+2]		# --> ay1 array.
+define QG_AY2PTR	Memi[$1+QG_AOFF+3]		# --> ay2 array.
+define QG_AX1		Memi[QG_AX1PTR($1)+$2]		# ax1.
+define QG_AX2		Memi[QG_AX2PTR($1)+$2]		# ax2.
+define QG_AY1		Memi[QG_AY1PTR($1)+$2]		# ay1.
+define QG_AY2		Memi[QG_AY2PTR($1)+$2]		# ay2.
+
+# Phantom markers
+define QG_PHOFF		27				# QG_AOFF+4
+define QG_PHPTR		Memi[$1+QG_PHOFF]		# --> Phantom array
+define QG_PHANTOM	Memi[QG_PHPTR($1)+$2]		# Phantom value
+
+# Macros to convert between array offset and grid position
+define	QG_GRIDX	($2 - (($2-1)/QG_NAMPSX($1))*QG_NAMPSX($1))
+define	QG_GRIDY	(($2-1)/QG_NAMPSX($1)+1)
+define	QG_AMP		($2 + ($3-1) * QG_NAMPSX($1))
+
+# Symbolic values for AMPTYPE codes
+define	AMPDICT		"|11|12|21|22|"
+define	AMP11		1		# BLHC
+define	AMP12		2		# BRHC
+define	AMP21		3		# TLHC
+define	AMP22		4		# TRHC
+
+define	SZ_AMPID	2
diff --git a/noao/imred/quadred/src/quad/quadgeom.x b/noao/imred/quadred/src/quad/quadgeom.x
new file mode 100644
index 00000000..3ce173ff
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadgeom.x
@@ -0,0 +1,304 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+# QUADGEOM -- Set up section information in quadgeom structure based on 
+# information in the image header. The sections given in the image header are
+# "whole image" sections (i.e. those that would be appropriate for single
+# readout. From these we must calculate the sections to apply to the data 
+# read through each readout. The values of datasec and ccdsec are taken from 
+# the header. The values of trimsec and biassec can be supplied explicitly
+# via the corresponding arguments. If these are given as "image" or "" then the
+# image header values are used.
+
+procedure quadgeom (im, qg, trimsec, biassec)
+
+pointer	im			#I  Pointer to input image.
+pointer	qg			#IO Pointer to open quadgeom structure.
+char	trimsec[SZ_LINE]	#I  Trimsec may be used to overide header value.
+char	biassec[SZ_LINE]	#I  Biassec may be used to overide header value.
+
+char	section[SZ_LINE], nampsyx[SZ_LINE]
+int	nx, ny, xdata, ydata, xover, yover, amp, xamp, yamp, pre
+int	dx1, dx2, dxs, dy1, dy2, dys
+int	ddx1, ddx2, ddy1, ddy2
+int	cx1, cx2, cxs, cy1, cy2, cys
+int	ccx1, ccx2, ccy1, ccy2
+int	tx1, tx2, txs, txskip1, txskip2
+int	ty1, ty2, tys, tyskip1, tyskip2
+int	ttx1, ttx2, tty1, tty2
+int	bx1, bx2, bxs, bxskip1, bxskip2
+int	by1, by2, bys, byskip1, byskip2
+int	bbx1, bbx2, bby1, bby2
+
+bool	streq()
+
+begin
+
+	# Get input image dimensions.
+	nx  = IM_LEN(im, 1)
+	ny  = IM_LEN(im, 2)
+
+	# Get number of active amplifiers in Y and X.
+	call hdmgstr (im, "nampsyx", nampsyx, SZ_LINE)
+	call sscan (nampsyx)
+	    call gargi (QG_NAMPSY(qg))
+	    call gargi (QG_NAMPSX(qg))
+	
+	QG_NAMPS(qg) = QG_NAMPSY(qg) * QG_NAMPSX(qg)
+	if (QG_NAMPS(qg) > QG_MAXAMPS)
+	    call error (0, "CCD has two many read-outs for this program")
+
+	# Get list of active amplifiers.
+	# Presently the header doesn't contain this information so we fake it
+	# since we know all the posibilities.
+	do amp = 1, QG_NAMPS(qg)
+	    call malloc (QG_AMPID(qg, amp), SZ_AMPID, TY_CHAR)
+
+	switch (QG_NAMPSX(qg)) {
+	case 1:
+	    switch (QG_NAMPSY(qg)) {
+	    case 1:	# Mono
+		QG_AMPTYPE (qg, 1) = AMP11
+		call strcpy ("11", Memc[QG_AMPID(qg, 1)], SZ_AMPID)
+
+	    case 2:	# Split parallels
+		call error (0, "Unsuported read-out configuration")
+	    }
+
+	case 2:
+
+	    switch (QG_NAMPSY(qg)) {
+	    case 1:	# Split serials
+		QG_AMPTYPE (qg, 1) = AMP11
+		call strcpy ("11", Memc[QG_AMPID(qg, 1)], SZ_AMPID)
+		QG_AMPTYPE (qg, 2) = AMP12
+		call strcpy ("12", Memc[QG_AMPID(qg, 2)], SZ_AMPID)
+
+	    case 2:	# Quad
+		QG_AMPTYPE (qg, 1) = AMP11
+		call strcpy ("11", Memc[QG_AMPID(qg, 1)], SZ_AMPID)
+		QG_AMPTYPE (qg, 2) = AMP12
+		call strcpy ("12", Memc[QG_AMPID(qg, 2)], SZ_AMPID)
+		QG_AMPTYPE (qg, 3) = AMP21
+		call strcpy ("21", Memc[QG_AMPID(qg, 3)], SZ_AMPID)
+		QG_AMPTYPE (qg, 4) = AMP22
+		call strcpy ("22", Memc[QG_AMPID(qg, 4)], SZ_AMPID)
+	    }
+	}
+
+	# Set X and Y dimensions of subimage read out by each amplifier
+	QG_NX (qg, 0) = nx
+	QG_NY (qg, 0) = ny
+	do amp = 1, QG_NAMPS (qg) {
+	    QG_NX(qg, amp) = nx / QG_NAMPSX (qg)
+	    QG_NY(qg, amp) = ny / QG_NAMPSY (qg)
+	}
+
+	# Get datasec, trimsec and biassec parameters from image header.
+	# trimsec and biassec may be overidden by supplying an explicit
+	# section in the biassec and trimsec arguments.
+	call hdmgstr (im, "datasec", section, SZ_LINE)
+	dx1 = 1
+	dx2 = nx
+	dxs = 1
+	dy1 = 1
+	dy2 = ny
+	dys = 1
+	call ccd_section (section, dx1, dx2, dxs, dy1, dy2, dys)
+	QG_DX1(qg, 0) = dx1
+	QG_DX2(qg, 0) = dx2
+	QG_DY1(qg, 0) = dy1
+	QG_DY2(qg, 0) = dy2
+
+	if (streq (trimsec, "image") || streq (trimsec, "")) {
+	    call hdmgstr (im, "trimsec", section, SZ_LINE)
+	} else {
+	    call strcpy (trimsec, section, SZ_LINE)
+	}
+	tx1 = dx1
+	tx2 = dx2
+	txs = 1
+	ty1 = dy1
+	ty2 = dy2
+	tys = 1
+	call ccd_section (section, tx1, tx2, txs, ty1, ty2, tys)
+	QG_TX1(qg, 0) = tx1
+	QG_TX2(qg, 0) = tx2
+	QG_TY1(qg, 0) = ty1
+	QG_TY2(qg, 0) = ty2
+
+	if (streq (biassec, "image") || streq (biassec, "")) {
+	    call hdmgstr (im, "biassec", section, SZ_LINE)
+	} else {
+	    call strcpy (biassec, section, SZ_LINE)
+	}
+	bx1 = dx2 + 1
+	bx2 = nx
+	bxs = 1
+	by1 = 1
+	by2 = ny
+	bys = 1
+	call ccd_section (section, bx1, bx2, bxs, by1, by2, bys)
+	QG_BX1(qg, 0) = bx1
+	QG_BX2(qg, 0) = bx2
+	QG_BY1(qg, 0) = by1
+	QG_BY2(qg, 0) = by2
+
+	call hdmgstr (im, "ccdsec", section, SZ_LINE)
+	cx1 = dx1
+	cx2 = dx2
+	cxs = 1
+	cy1 = dy1
+	cy2 = dy2
+	cys = 1
+	call ccd_section (section, cx1, cx2, cxs, cy1, cy2, cys)
+	QG_CX1(qg, 0) = cx1
+	QG_CX2(qg, 0) = cx2
+	QG_CY1(qg, 0) = cy1
+	QG_CY2(qg, 0) = cy2
+
+	# Calculate number of data pixels and margins to leave around
+	# trimsection.
+	xdata = dx2 - dx1 + 1
+	ydata = dy2 - dy1 + 1
+	txskip1 = tx1 - dx1
+	# *************			KLUDGE!		*********************
+	# The datasec is the whole image. We have no way of knowing where the
+	# division between data and overscan is supposed to be so we assume 
+	# that trimsec leaves an equal margin on both sides of the true datasec.
+	if ((dx1 == 1 ) && (dx2 == nx)) {	
+	    dx2 = tx2 + txskip1 	
+	    xdata = dx2 - dx1 + 1
+	    cx2 = cx1 + xdata - 1
+	    QG_DX2(qg, 0) = dx2
+	    QG_CX2(qg, 0) = cx2
+	}
+	txskip2 = dx2 - tx2
+	tyskip1 = ty1 - dy1
+	tyskip2 = dy2 - ty2
+
+	# Calculate number of overscan pixels and margins to leave around
+	# biassec.
+	xover   = nx  - xdata
+	yover   = ny
+	bxskip1 = bx1 - dx2 - 1
+	bxskip2 = nx  - bx2
+	byskip1 = by1 - dy1
+	byskip2 = ny  - by2
+
+	# Calculate number of data and overscan pixels in subimages
+	xdata = xdata / QG_NAMPSX(qg)
+	ydata = ydata / QG_NAMPSY(qg)
+	xover = xover / QG_NAMPSX(qg)
+	yover = yover / QG_NAMPSY(qg)
+
+	# Calculate datasec, trimsec, etc. for each amplifier
+	do amp = 1, QG_NAMPS(qg) {
+
+	    # Assume there are no phantoms
+	    QG_PHANTOM (qg, amp) = NO
+
+	    # X coordinates
+	    switch (QG_AMPTYPE(qg, amp)) {
+	    case AMP11, AMP21:	# Left hand side
+		ddx1 = dx1
+		ddx2 = ddx1 + xdata - 1
+		ttx1 = ddx1 + txskip1
+		ttx2 = ddx2 
+		bbx1 = ddx2 + bxskip1 + 1
+		bbx2 = ddx2 + xover - bxskip2
+		ccx1 = cx1
+		ccx2 = cx1  + xdata - 1
+
+	    case AMP12, AMP22:	# Right hand side
+		bbx1 = bxskip2 + 1
+		bbx2 = xover - bxskip1 
+		ddx1 = xover + 1
+		ddx2 = ddx1 + xdata - 1
+		ttx1 = ddx1
+		ttx2 = ddx2 - txskip2 
+		ccx1 = cx1 +  xdata 
+		ccx2 = cx2
+	    }
+
+	    # Y Coordinates
+	    switch (QG_AMPTYPE(qg, amp)) {
+	    case AMP11, AMP12:	# Lower row
+		ddy1 = dy1
+		ddy2 = ddy1 + ydata - 1
+		tty1 = ddy1 + tyskip1
+		bby1 = ddy1 + byskip1 
+		if (QG_NAMPSY(qg) == 1) {
+		    tty2 = ddy2 - tyskip2
+		    bby2 = ddy2 - byskip2
+		} else {
+		    tty2 = ddy2
+		    bby2 = ddy2
+		}
+		ccy1 = cy1
+		ccy2 = cy1  + ydata - 1
+
+	    case AMP21, AMP22:	# Upper row
+		ddy1 = 1
+		ddy2 = ddy1 + ydata - 1
+		if (QG_NAMPSY(qg) == 1) {
+		    tty1 = ddy1 + tyskip1
+		    bby1 = ddy1 + byskip1 
+		} else {
+		    tty1 = 1
+		    bby1 = 1
+		}
+		tty2 = ddy2 - tyskip2
+		bby2 = ddy2 - byskip2
+		ccy1 = cy1  + ydata 
+		ccy2 = cy2
+	    }
+
+
+	    QG_DX1(qg, amp) = ddx1
+	    QG_DX2(qg, amp) = ddx2
+	    QG_DY1(qg, amp) = ddy1
+	    QG_DY2(qg, amp) = ddy2
+
+	    QG_TX1(qg, amp) = ttx1
+	    QG_TX2(qg, amp) = ttx2
+	    QG_TY1(qg, amp) = tty1
+	    QG_TY2(qg, amp) = tty2
+
+	    QG_BX1(qg, amp) = bbx1
+	    QG_BX2(qg, amp) = bbx2
+	    QG_BY1(qg, amp) = bby1
+	    QG_BY2(qg, amp) = bby2
+
+	    QG_CX1(qg, amp) = ccx1
+	    QG_CX2(qg, amp) = ccx2
+	    QG_CY1(qg, amp) = ccy1
+	    QG_CY2(qg, amp) = ccy2
+	}
+
+	# Set up "ampsec" - the section of the composite image derived from
+	# each sub-image.
+	do yamp = 1, QG_NAMPSY(qg) {
+	    amp = QG_AMP (qg, 1, yamp)
+	    QG_AX1(qg, amp) = 1
+	    QG_AX2(qg, amp) = QG_NX(qg, amp)
+	    do xamp = 2, QG_NAMPSX(qg) {
+		amp = QG_AMP (qg, xamp,   yamp)
+		pre = QG_AMP (qg, xamp-1, yamp)
+		QG_AX1(qg, amp) = QG_AX2(qg, pre) + 1
+		QG_AX2(qg, amp) = QG_AX1(qg, amp) + QG_NX(qg, amp) - 1
+	    }
+	}
+	do xamp = 1, QG_NAMPSX(qg) {
+	    amp = QG_AMP (qg, xamp, 1)
+	    QG_AY1(qg, amp) = 1
+	    QG_AY2(qg, amp) = QG_NY(qg, amp)
+	    do yamp = 2, QG_NAMPSY(qg) {
+		amp = QG_AMP (qg, xamp, yamp)
+		pre = QG_AMP (qg, xamp, yamp-1)
+		QG_AY1(qg, amp) = QG_AY2(qg, pre) + 1
+		QG_AY2(qg, amp) = QG_AY1(qg, amp) + QG_NY(qg, amp) - 1
+	    }
+	}
+
+end
diff --git a/noao/imred/quadred/src/quad/quadgeomred.x b/noao/imred/quadred/src/quad/quadgeomred.x
new file mode 100644
index 00000000..ff5d043c
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadgeomred.x
@@ -0,0 +1,165 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+# QUADGEOMRED -- Set up section information in quadgeom structure based on 
+# information in the image header for a reduced image. The sections given in the
+# image header are "whole image" sections (i.e. those that would be appropriate
+# for single  readout. From these we must calculate the sections to apply to
+# the data read through each readout.
+
+procedure quadgeomred (im, qg)
+
+pointer	im			#I  Pointer to input image.
+pointer	qg			#IO Pointer to open quadgeom structure.
+
+char	section[SZ_LINE], keyword[SZ_LINE], nampsyx[SZ_LINE]
+int	nx, ny, x, y, amp, pre
+int	dx1, dx2, dxs, dy1, dy2, dys
+int	cx1, cx2, cxs, cy1, cy2, cys
+int	ax1, ax2, axs, ay1, ay2, ays
+
+begin
+
+	# Get input image dimensions.
+	nx  = IM_LEN(im, 1)
+	ny  = IM_LEN(im, 2)
+	QG_NX (qg, 0) = nx
+	QG_NY (qg, 0) = ny
+
+	# Get number of active amplifiers in Y and X.
+	call hdmgstr (im, "nampsyx", nampsyx, SZ_LINE)
+	call sscan (nampsyx)
+	    call gargi (QG_NAMPSY(qg))
+	    call gargi (QG_NAMPSX(qg))
+	
+	QG_NAMPS(qg) = QG_NAMPSY(qg) * QG_NAMPSX(qg)
+	if (QG_NAMPS(qg) > QG_MAXAMPS)
+	    call error (0, "CCD has two many read-outs for this program")
+
+	# Get list of active amplifiers.
+	# Presently the header doesn't contain this information so we fake it
+	# since we know all the posibilities.
+	do amp = 1, QG_NAMPS(qg)
+	    call malloc (QG_AMPID(qg, amp), SZ_AMPID, TY_CHAR)
+
+	switch (QG_NAMPSX(qg)) {
+	case 1:
+	    switch (QG_NAMPSY(qg)) {
+	    case 1:	# Mono
+		QG_AMPTYPE (qg, 1) = AMP11
+		call strcpy ("11", Memc[QG_AMPID(qg, 1)], SZ_AMPID)
+
+	    case 2:	# Split parallels
+		call error (0, "Unsuported read-out configuration")
+	    }
+
+	case 2:
+
+	    switch (QG_NAMPSY(qg)) {
+	    case 1:	# Split serials
+		QG_AMPTYPE (qg, 1) = AMP11
+		call strcpy ("11", Memc[QG_AMPID(qg, 1)], SZ_AMPID)
+		QG_AMPTYPE (qg, 2) = AMP12
+		call strcpy ("12", Memc[QG_AMPID(qg, 2)], SZ_AMPID)
+
+	    case 2:	# Quad
+		QG_AMPTYPE (qg, 1) = AMP11
+		call strcpy ("11", Memc[QG_AMPID(qg, 1)], SZ_AMPID)
+		QG_AMPTYPE (qg, 2) = AMP12
+		call strcpy ("12", Memc[QG_AMPID(qg, 2)], SZ_AMPID)
+		QG_AMPTYPE (qg, 3) = AMP21
+		call strcpy ("21", Memc[QG_AMPID(qg, 3)], SZ_AMPID)
+		QG_AMPTYPE (qg, 4) = AMP22
+		call strcpy ("22", Memc[QG_AMPID(qg, 4)], SZ_AMPID)
+	    }
+	}
+
+
+	# Get datasec.
+	call hdmgstr (im, "datasec", section, SZ_LINE)
+	dx1 = 1
+	dx2 = nx
+	dxs = 1
+	dy1 = 1
+	dy2 = ny
+	dys = 1
+	call ccd_section (section, dx1, dx2, dxs, dy1, dy2, dys)
+	QG_DX1(qg, 0) = dx1
+	QG_DX2(qg, 0) = dx2
+	QG_DY1(qg, 0) = dy1
+	QG_DY2(qg, 0) = dy2
+
+	# Get ccdsec.
+	call hdmgstr (im, "ccdsec", section, SZ_LINE)
+	cx1 = dx1
+	cx2 = dx2
+	cxs = 1
+	cy1 = dy1
+	cy2 = dy2
+	cys = 1
+	call ccd_section (section, cx1, cx2, cxs, cy1, cy2, cys)
+	QG_CX1(qg, 0) = cx1
+	QG_CX2(qg, 0) = cx2
+	QG_CY1(qg, 0) = cy1
+	QG_CY2(qg, 0) = cy2
+
+
+	do amp = 1, QG_NAMPS (qg) {
+
+	    # Get AMPSECmn for each readout
+	    call sprintf (keyword, SZ_LINE, "AMPSEC%s")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+	    call hdmgstr (im, keyword, section, SZ_LINE)
+	    ax1 = 1
+	    ax2 = nx
+	    axs = 1
+	    ay1 = 1
+	    ay2 = ny
+	    ays = 1
+	    call ccd_section (section, ax1, ax2, axs, ay1, ay2, ays)
+	    QG_AX1(qg, amp) = ax1
+	    QG_AX2(qg, amp) = ax2
+	    QG_AY1(qg, amp) = ay1
+	    QG_AY2(qg, amp) = ay2
+
+
+	    # Set X and Y dimensions of subimage read out by each amplifier
+	    QG_NX(qg, amp) = ax2 - ax1 + 1
+	    QG_NY(qg, amp) = ay2 - ay1 + 1
+
+	    # Set datsec and trimsec for each sub image
+	    QG_DX1(qg, amp) = 1
+	    QG_DX2(qg, amp) = QG_NX(qg, amp)
+	    QG_DY1(qg, amp) = 1
+	    QG_DY2(qg, amp) = QG_NY(qg, amp)
+
+	    QG_TX1(qg, amp) = 1
+	    QG_TX2(qg, amp) = QG_NX(qg, amp)
+	    QG_TY1(qg, amp) = 1
+	    QG_TY2(qg, amp) = QG_NY(qg, amp)
+	}
+
+	# Determine ccdsec for each each sub-image.
+	do y = 1, QG_NAMPSY(qg) {
+	    amp = QG_AMP (qg, 1, y)
+	    QG_CX1(qg, amp) = QG_CX1(qg, 0)
+	    QG_CX2(qg, amp) = QG_CX1(qg, amp) + QG_NX(qg, amp) - 1
+	    do x = 2, QG_NAMPSX(qg) {
+		amp = QG_AMP (qg, x,   y)
+		pre = QG_AMP (qg, x-1, y)
+		QG_CX1(qg, amp) = QG_CX2(qg, pre) + 1
+		QG_CX2(qg, amp) = QG_CX1(qg, amp) + QG_NX(qg, amp) - 1
+	    }
+	}
+	do x = 1, QG_NAMPSX(qg) {
+	    amp = QG_AMP (qg, x, 1)
+	    QG_CY1(qg, amp) = QG_CY1(qg, 0)
+	    QG_CY2(qg, amp) = QG_CY1(qg, amp) + QG_NY(qg, amp) - 1
+	    do y = 2, QG_NAMPSY(qg) {
+		amp = QG_AMP (qg, x, y)
+		pre = QG_AMP (qg, x, y-1)
+		QG_CY1(qg, amp) = QG_CY2(qg, pre) + 1
+		QG_CY2(qg, amp) = QG_CY1(qg, amp) + QG_NY(qg, amp) - 1
+	    }
+	}
+end
diff --git a/noao/imred/quadred/src/quad/quadjoin.par b/noao/imred/quadred/src/quad/quadjoin.par
new file mode 100644
index 00000000..8ebf6582
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadjoin.par
@@ -0,0 +1,4 @@
+input,s,a,"",,,Input root name
+output,s,h,"",,,"Output image name
+"
+delete,b,h,yes,,,"Delete sub-images on completion"
diff --git a/noao/imred/quadred/src/quad/quadjoin.x b/noao/imred/quadred/src/quad/quadjoin.x
new file mode 100644
index 00000000..0ef94394
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadjoin.x
@@ -0,0 +1,638 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+procedure t_quadjoin ()
+
+char	input[SZ_FNAME]			#TI Input image root name.
+char	output[SZ_FNAME]		#TI Output image name.
+char	instrument[SZ_FNAME]		#TI Instrument translation file.
+bool	delete				#TI delete sub-images when done.
+
+int	namps, amp
+pointer	in[QG_MAXAMPS], out, qg
+char	logstr[SZ_LINE]
+bool	inplace
+
+pointer	immap()
+int	quadmap(), imaccess()
+bool	streq(), clgetb()
+
+errchk	ccddelete()
+
+begin
+	# Open instrument file
+	call clgstr    ("instrument",  instrument,  SZ_FNAME)
+	call hdmopen   (instrument)
+
+	# Get input image name and output image names.
+	call clgstr ("input", input, SZ_FNAME)
+	call xt_imroot (input, input, SZ_FNAME)
+	call clgstr ("output", output, SZ_FNAME)
+
+	# If the output name is null the opperation is "done in place one 
+	# removed". That is:
+	#	the sub-images are combined to form a temporary image
+	#	the ORIGINAL PARENT IMAGE is deleted or copied to a backup image
+	#       the temporary image is renamed to the original parent image
+	#
+	if (streq (output, "")) {
+	    call mktemp ("tmp", output, SZ_FNAME)
+	    inplace = true
+	} else {
+	    inplace = false
+	}
+
+	# Get delete sub-image flag
+	delete = clgetb ("delete")
+
+	# Allocate quadgeom structure
+	call quadalloc (qg)
+
+	# Open input sub-images
+	namps = quadmap (input, READ_ONLY, false, 0, qg, in)
+
+#	call quaddump (qg)
+
+	# Open output image
+	out = immap (output, NEW_COPY, in[1])
+
+	# Merge header information to form header for composite image.
+#	call quadjoinhdr (in, out, qg)
+	call quadjoinhdr2 (in, out, qg)
+
+        switch (IM_PIXTYPE(out)) {
+        case TY_USHORT, TY_SHORT:
+	    call qjoins (in, out, qg)
+
+        case TY_INT:
+	    call qjoini (in, out, qg)
+
+        case TY_LONG:
+	    call qjoinl (in, out, qg)
+
+        case TY_REAL:
+	    call qjoinr (in, out, qg)
+
+        case TY_DOUBLE:
+	    call qjoind (in, out, qg)
+
+        default:
+            call error (1, "unsupported pixel datatype")
+        }
+
+	# Log opperation
+	if (QG_NAMPSX(qg) == 2 && QG_NAMPSY(qg) == 2) {
+	    call sprintf (logstr, SZ_LINE, "Quad-readout image")
+	} else if (QG_NAMPSX(qg) == 2 || QG_NAMPSY(qg) == 2) {
+	    call sprintf (logstr, SZ_LINE, "Dual-readout image: nampsx=%d nampsy=%d")
+		call pargi (QG_NAMPSX(qg))
+		call pargi (QG_NAMPSY(qg))
+	} else {
+	    call sprintf (logstr, SZ_LINE, "Single-readout image")
+	}
+	call timelog (logstr, SZ_LINE)
+	call ccdlog (input, logstr)
+
+	# Tidy up
+	call imunmap (out)
+	do amp = 1, namps
+	    call imunmap (in[amp])
+
+	# Delete sub-images
+	if (delete)
+	    call quaddelete (qg, input)
+
+	if (inplace) {
+  	    # Replace the input by the output image.
+	    if (imaccess (input, READ_ONLY) == YES) {
+		iferr (call ccddelete (input)) {
+		    call imdelete (output)
+		    call error (0, "Can't delete or make backup of original image")
+		}
+	    }
+	    call imrename (output, input)
+	}
+
+	call quadfree (qg)
+	call hdmclose ()
+end
+
+# Merge header information and write to header of output image.
+
+procedure quadjoinhdr (in, out, qg)
+
+pointer	in[ARB]		#I Pointer to input sub-images.
+pointer	out		#I Pointer to output image.
+pointer	qg		#I Pointer to quadgeom structure.
+
+char	keyword[SZ_LINE], section[SZ_LINE], buffer[SZ_LINE]
+real	rval, ccdmean
+int	amp, brk
+
+int	hdmaccf(), strsearch()
+real	hdmgetr()
+
+begin
+	# Set image dimensions
+	IM_LEN (out, 1) = QG_NX(qg, 0)
+	IM_LEN (out, 2) = QG_NY(qg, 0)
+
+	# Add defined sections to output image header.
+	if ((QG_DX1 (qg, 0) != 0) && (hdmaccf (out, "trim") == NO)) {
+	    call sprintf (section, SZ_LINE, "[%d:%d,%d:%d]")
+		call pargi (QG_DX1(qg, 0))
+		call pargi (QG_DX2(qg, 0))
+		call pargi (QG_DY1(qg, 0))
+		call pargi (QG_DY2(qg, 0))
+	    call hdmpstr (out, "datasec", section)
+
+	    call sprintf (section, SZ_LINE, "[%d:%d,%d:%d]")
+		call pargi (QG_TX1(qg, 0))
+		call pargi (QG_TX2(qg, 0))
+		call pargi (QG_TY1(qg, 0))
+		call pargi (QG_TY2(qg, 0))
+	    call hdmpstr (out, "trimsec", section)
+
+	    call sprintf (section, SZ_LINE, "[%d:%d,%d:%d]")
+		call pargi (QG_BX1(qg, 0))
+		call pargi (QG_BX2(qg, 0))
+		call pargi (QG_BY1(qg, 0))
+		call pargi (QG_BY2(qg, 0))
+	    call hdmpstr (out, "biassec", section)
+	}
+
+	if (QG_CX1 (qg, 0) != 0) {
+	    call sprintf (section, SZ_LINE, "[%d:%d,%d:%d]")
+		call pargi (QG_CX1(qg, 0))
+		call pargi (QG_CX2(qg, 0))
+		call pargi (QG_CY1(qg, 0))
+		call pargi (QG_CY2(qg, 0))
+	    call hdmpstr (out, "ccdsec", section)
+	}
+
+	# Set AMPSECnm 
+	do amp = 1, QG_NAMPS(qg) {
+	    call sprintf (keyword, SZ_LINE, "ampsec%s")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+
+	    call sprintf (section, SZ_LINE, "[%d:%d,%d:%d]")
+		call pargi (QG_AX1(qg, amp))
+		call pargi (QG_AX2(qg, amp))
+		call pargi (QG_AY1(qg, amp))
+		call pargi (QG_AY2(qg, amp))
+
+	    call hdmpstr (out, keyword, section)
+	}
+
+	# Tidy up processing history
+	if (hdmaccf (out, "trim") == YES) {
+	    do amp = 1, QG_NAMPS(qg) 
+		call mergehist (in[amp], out, "trim", Memc[QG_AMPID(qg, amp)])
+	    call hdmdelf (out, "trim")
+	    call strcpy ("Trimmed", buffer, SZ_LINE)
+	    call timelog (buffer, SZ_LINE)
+	    call hdmpstr (out, "trim", buffer)
+	}
+
+	if (hdmaccf (out, "overscan") == YES) {
+	    do amp = 1, QG_NAMPS(qg) 
+		call mergehist (in[amp], out, "overscan", Memc[QG_AMPID(qg, amp)])
+	    call hdmdelf (out, "overscan")
+	    call strcpy ("Overscan corrected", buffer, SZ_LINE)
+	    call timelog (buffer, SZ_LINE)
+	    call hdmpstr (out, "overscan", buffer)
+	}
+
+	if (hdmaccf (out, "ccdmean") == YES) {
+	    ccdmean = 0.0
+	    do amp = 1, QG_NAMPS(qg) {
+		rval = hdmgetr (in[amp], "ccdmean")
+		ccdmean = ccdmean + rval
+		call sprintf (keyword, SZ_LINE, "ccdmea%s")
+		    call pargstr (Memc[QG_AMPID(qg, amp)])
+		call hdmputr (out, keyword, rval)
+	    }
+	    ccdmean = ccdmean / QG_NAMPS(qg)
+	    call hdmdelf (out, "ccdmean")
+	    call hdmputr (out, "ccdmean", ccdmean)
+	}
+
+	# Move CCDPROC keyword to end of header
+	if (hdmaccf (out, "ccdproc") == YES) {
+	    call hdmgstr (in, "ccdproc", buffer, SZ_LINE)
+	    call hdmdelf (out, "ccdproc")
+	    brk = strsearch (buffer, "CCD")
+	    if (brk !=0)
+		call strcpy (buffer[brk-3], buffer, SZ_LINE)
+	    call timelog (buffer, SZ_LINE)
+	    call hdmpstr (out, "ccdproc", buffer)
+	}
+end
+
+define	SZ_KEYWRD	8		# Number of chars in FITS keyword
+
+define	REVSTRING	"1.000	09Mar94 (Included amplifier geometry keywords)"
+
+# Merge header information and write to header of output image.
+
+procedure quadjoinhdr2 (in, out, qg)
+
+pointer	in[ARB]		#I Pointer to input sub-images.
+pointer	out		#I Pointer to output image.
+pointer	qg		#I Pointer to quadgeom structure.
+
+pointer	sp, keyword, section, buffer
+real	rval, ccdmean
+int	amp, brk, ch
+
+int	ax1, ax2, ay1, ay2
+int	bx1, bx2, by1, by2
+int	dx1, dx2, dy1, dy2
+int	tx1, tx2, ty1, ty2
+
+int	hdmaccf(), strsearch()
+real	hdmgetr()
+
+begin
+	call smark (sp)
+	call salloc (keyword, SZ_KEYWRD, TY_CHAR)
+	call salloc (section, SZ_LINE,   TY_CHAR)
+	call salloc (buffer,  SZ_LINE,   TY_CHAR)
+
+	# Set image dimensions
+	IM_LEN (out, 1) = QG_NX(qg, 0)
+	IM_LEN (out, 2) = QG_NY(qg, 0)
+
+	# Set the header revision level if not already set.
+	if (hdmaccf (out, "HDR_REV") == NO) {
+	    call hdmpstr (out, "HDR_REV", REVSTRING)
+	}
+
+	# Update nampsyx and amplist
+	call sprintf (Memc[buffer], SZ_LINE, "%d %d")
+	    call pargi (QG_NAMPSY(qg))
+	    call pargi (QG_NAMPSX(qg))
+	call hdmpstr (out, "nampsyx", Memc[buffer])
+
+	ch = 1
+	do amp = 1, QG_NAMPS(qg) {
+	    call sprintf (Memc[buffer+ch-1], 3, "%2s ")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+	    ch = ch + 3
+	}
+	call hdmpstr (out, "amplist", Memc[buffer])
+
+	# Update geometry keywords for each amplifier in the header.
+	# If the corresponding section is undefined any old keywords are deleted
+	# The TSECyx, DSECyx and BSECyx keywords are only retained if the image
+	# has not been trimmed.
+	do amp = 1, QG_NAMPS (qg) {
+
+	    # Ampsec (ASECyx keyword)
+	    #
+	    call sprintf (Memc[keyword], SZ_LINE, "ASEC%2s")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+
+	    ax1 = QG_AX1 (qg, amp)
+	    ax2 = QG_AX2 (qg, amp)
+	    ay1 = QG_AY1 (qg, amp)
+	    ay2 = QG_AY2 (qg, amp)
+
+	    call sprintf (Memc[section], SZ_LINE, "[%d:%d,%d:%d]")
+		call pargi (ax1)
+		call pargi (ax2)
+		call pargi (ay1)
+		call pargi (ay2)
+
+	    call hdmpstr (out, Memc[keyword], Memc[section])
+
+	    # Biassec (BSECyx keyword)
+	    #
+	    call sprintf (Memc[keyword], SZ_LINE, "BSEC%2s")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+
+	    if ((hdmaccf (out, "trim") == NO) && (QG_BX1 (qg, amp) != 0)) {
+
+
+		bx1 = QG_BX1 (qg, amp) + ax1 - 1
+		bx2 = QG_BX2 (qg, amp) + ax1 - 1
+		by1 = QG_BY1 (qg, amp) + ay1 - 1
+		by2 = QG_BY2 (qg, amp) + ay1 - 1
+
+		call sprintf (Memc[section], SZ_LINE, "[%d:%d,%d:%d]")
+		    call pargi (bx1)
+		    call pargi (bx2)
+		    call pargi (by1)
+		    call pargi (by2)
+
+		call hdmpstr (out, Memc[keyword], Memc[section])
+
+	    } else if (hdmaccf (out, Memc[keyword]) == YES) {
+
+		call hdmdelf (out, Memc[keyword])
+
+	    }
+
+	    # CCDsec (CSECyx keyword)
+	    #
+	    call sprintf (Memc[keyword], SZ_LINE, "CSEC%2s")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+
+	    if ((hdmaccf (out, "trim") == NO) && (QG_CX1 (qg, amp) != 0)) {
+
+		call sprintf (Memc[section], SZ_LINE, "[%d:%d,%d:%d]")
+		    call pargi (QG_CX1(qg, amp))
+		    call pargi (QG_CX2(qg, amp))
+		    call pargi (QG_CY1(qg, amp))
+		    call pargi (QG_CY2(qg, amp))
+
+		call hdmpstr (out, Memc[keyword], Memc[section])
+
+	    } else if (hdmaccf (out, Memc[keyword]) == YES) {
+
+		call hdmdelf (out, Memc[keyword])
+
+	    }
+
+	    # Datasec (DSECyx keyword)
+	    #
+	    call sprintf (Memc[keyword], SZ_LINE, "DSEC%2s")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+
+	    if ((hdmaccf (out, "trim") == NO) && (QG_DX1 (qg, amp) != 0)) {
+
+		dx1 = QG_DX1 (qg, amp) + ax1 - 1
+		dx2 = QG_DX2 (qg, amp) + ax1 - 1
+		dy1 = QG_DY1 (qg, amp) + ay1 - 1
+		dy2 = QG_DY2 (qg, amp) + ay1 - 1
+
+		call sprintf (Memc[section], SZ_LINE, "[%d:%d,%d:%d]")
+		    call pargi (dx1)
+		    call pargi (dx2)
+		    call pargi (dy1)
+		    call pargi (dy2)
+		call hdmpstr (out, Memc[keyword], Memc[section])
+
+	    } else if (hdmaccf (out, Memc[keyword]) == YES) {
+
+		call hdmdelf (out, Memc[keyword])
+
+	    }
+
+	    # Trimsec (TSECyx keyword)
+	    #
+	    call sprintf (Memc[keyword], SZ_LINE, "TSEC%2s")
+		call pargstr (Memc[QG_AMPID(qg, amp)])
+
+	    if ((hdmaccf (out, "trim") == NO) && (QG_TX1 (qg, amp) != 0)) {
+
+
+		tx1 = QG_TX1 (qg, amp) + ax1 - 1
+		tx2 = QG_TX2 (qg, amp) + ax1 - 1
+		ty1 = QG_TY1 (qg, amp) + ay1 - 1
+		ty2 = QG_TY2 (qg, amp) + ay1 - 1
+
+		call sprintf (Memc[section], SZ_LINE, "[%d:%d,%d:%d]")
+		    call pargi (tx1)
+		    call pargi (tx2)
+		    call pargi (ty1)
+		    call pargi (ty2)
+		call hdmpstr (out, Memc[keyword], Memc[section])
+
+	    } else if (hdmaccf (out, Memc[keyword]) == YES) {
+
+		call hdmdelf (out, Memc[keyword])
+
+	    }
+
+	}
+
+	# Delete biassec, ccdsec, datasec and trimsec if present.
+	if (hdmaccf (out, "biassec") == YES) {
+	    call hdmdelf (out, "biassec")
+	}
+
+	if (hdmaccf (out, "datasec") == YES) {
+	    call hdmdelf (out, "datasec")
+	}
+
+	if (hdmaccf (out, "trimsec") == YES) {
+	    call hdmdelf (out, "trimsec")
+	}
+
+	if (hdmaccf (out, "ccdsec") == YES) {
+	    call hdmdelf (out, "ccdsec")
+	}
+
+	# If image has been trimmed insert CCDSEC for entire image. This is 
+	# derived from the CCDSEC's for the sub-images in the BLH and TRH
+	# corners.
+	if (hdmaccf (out, "trim") == YES) {
+	    call sprintf (Memc[section], SZ_LINE, "[%d:%d,%d:%d]")
+		call pargi (QG_CX1(qg, 1))
+		call pargi (QG_CX2(qg, QG_NAMPS(qg)))
+		call pargi (QG_CY1(qg, 1))
+		call pargi (QG_CY2(qg, QG_NAMPS(qg)))
+ 
+	    call hdmpstr (out, "CCDSEC", Memc[section])
+	}
+
+	# Tidy up processing history as appropriate
+
+	# Overscan Subtraction
+	if (hdmaccf (out, "overscan") == YES) {
+	    do amp = 1, QG_NAMPS(qg) 
+		call merge_overscan (in[amp], out, Memc[QG_AMPID(qg, amp)])
+	    
+	    call hdmdelf (out, "overscan")
+	    call strcpy ("Overscan corrected", Memc[buffer], SZ_LINE)
+	    call timelog (Memc[buffer], SZ_LINE)
+	    call hdmpstr (out, "overscan", Memc[buffer])
+	}
+
+	# Triming.
+	if (hdmaccf (out, "trim") == YES) {
+
+	    do amp = 1, QG_NAMPS(qg) 
+		call merge_trim (in[amp], out, Memc[QG_AMPID(qg, amp)])
+
+	    call hdmdelf (out, "trim")
+	    call strcpy ("Trimmed", Memc[buffer], SZ_LINE)
+	    call timelog (Memc[buffer], SZ_LINE)
+	    call hdmpstr (out, "trim", Memc[buffer])
+
+	}
+
+	# CCDMEAN
+	if (hdmaccf (out, "ccdmean") == YES) {
+	    ccdmean = 0.0
+	    do amp = 1, QG_NAMPS(qg) {
+		rval = hdmgetr (in[amp], "ccdmean")
+		ccdmean = ccdmean + rval
+		call sprintf (Memc[keyword], SZ_LINE, "ccdmea%s")
+		    call pargstr (Memc[QG_AMPID(qg, amp)])
+		call hdmputr (out, Memc[keyword], rval)
+	    }
+	    ccdmean = ccdmean / QG_NAMPS(qg)
+	    call hdmdelf (out, "ccdmean")
+	    call hdmputr (out, "ccdmean", ccdmean)
+	}
+
+	# Move CCDPROC keyword to end of header
+	if (hdmaccf (out, "ccdproc") == YES) {
+	    call hdmgstr (in, "ccdproc", Memc[buffer], SZ_LINE)
+	    call hdmdelf (out, "ccdproc")
+	    brk = strsearch (Memc[buffer], "CCD")
+	    if (brk !=0)
+		call strcpy (Memc[buffer+brk-4], Memc[buffer], SZ_LINE)
+	    call timelog (Memc[buffer], SZ_LINE)
+	    call hdmpstr (out, "ccdproc", Memc[buffer])
+	}
+
+	call sfree (sp)
+end
+
+define	OVSC_FMT1	"Overscan section is %s with mean=%g"
+define	OVSC_FMT2	"Overscan section is %s"
+define	OVSC_FMT3	"Overscan section is %s with function=%s" 
+
+procedure merge_overscan (in, out, ampid)
+
+pointer	in		# Input quadrant image
+pointer	out		# Output image
+char	ampid[2]	# Label for readout
+
+pointer	sp, buffer, amplifier, biassec, func, rootname, fullname
+real	mean
+int	idx
+
+int	hdmaccf(), stridx(), nscan()
+
+
+begin
+	call smark (sp)
+	call salloc (buffer,    SZ_LINE,   TY_CHAR)
+	call salloc (amplifier, SZ_LINE,   TY_CHAR)
+	call salloc (biassec,   SZ_LINE,   TY_CHAR)
+	call salloc (func,      SZ_LINE,   TY_CHAR)
+	call salloc (rootname,  SZ_KEYWRD, TY_CHAR)
+	call salloc (fullname,  SZ_KEYWRD, TY_CHAR)
+
+	if (hdmaccf (out, "overscan") == YES) {
+
+	    # Get BSECyx 
+	    call sprintf (Memc[fullname], SZ_LINE, "BSEC%2s")
+		call pargstr (ampid)
+	    call hdmgstr (in, Memc[fullname], Memc[biassec], SZ_LINE)
+
+	    # Get overscan flag and retrieve the mean value if present
+	    call hdmgstr (in, "overscan", Memc[buffer], SZ_LINE)
+	    idx = stridx ("=", Memc[buffer])
+	    if (idx == 0) {
+		call sprintf (Memc[buffer], SZ_LINE, OVSC_FMT2)
+		    call pargstr (Memc[biassec])
+
+	    } else {
+		call sscan (Memc[buffer+idx])
+		    call gargr (mean)
+	        if (nscan() == 1) {
+		    call sprintf (Memc[buffer], SZ_LINE, OVSC_FMT1)
+			call pargstr (Memc[biassec])
+			call pargr (mean)
+		} else {
+		    call strcpy (Memc[buffer+idx], Memc[func], SZ_LINE)
+		    call sprintf (Memc[buffer], SZ_LINE, OVSC_FMT3)
+			call pargstr (Memc[biassec])
+			call pargstr (Memc[func])
+		}
+	    }
+
+	    # Get overscan keyword name and append AMP_ID
+	    call hdmname ("overscan", Memc[rootname], 6)
+	    call strcpy (Memc[rootname], Memc[fullname], 6)
+	    call strcat (ampid, Memc[fullname], SZ_KEYWRD)
+
+	    # Write new overscan keyword.
+	    call timelog (Memc[buffer], SZ_LINE)
+	    call hdmpstr (out, Memc[fullname], Memc[buffer])
+	
+	    # And record opperation in logfile
+	    call sprintf (Memc[amplifier], SZ_LINE, "    AMP%s")
+		call pargstr (ampid)
+	    call ccdlog (Memc[amplifier], Memc[buffer])
+
+	}
+
+	call sfree (sp)
+end
+
+define	TRIM_FMT	"Trim data section is %s"
+
+procedure merge_trim (in, out, ampid)
+
+pointer	in		# Input quadrant image
+pointer	out		# Output image
+char	ampid[2]	# Label for readout
+
+pointer	sp, buffer, amplifier, trimsec, rootname, fullname
+
+int	hdmaccf()
+
+
+begin
+	call smark (sp)
+	call salloc (buffer,   SZ_LINE,   TY_CHAR)
+	call salloc (amplifier, SZ_LINE,   TY_CHAR)
+	call salloc (trimsec,  SZ_LINE,   TY_CHAR)
+	call salloc (rootname, SZ_KEYWRD, TY_CHAR)
+	call salloc (fullname, SZ_KEYWRD, TY_CHAR)
+
+	if (hdmaccf (out, "trim") == YES) {
+
+	    # Get BSECyx 
+	    call sprintf (Memc[fullname], SZ_LINE, "TSEC%2s")
+		call pargstr (ampid)
+	    call hdmgstr (in, Memc[fullname], Memc[trimsec], SZ_LINE)
+
+	    call sprintf (Memc[buffer], SZ_LINE, TRIM_FMT)
+		    call pargstr (Memc[trimsec])
+
+	    # Get overscan keyword name and append AMP_ID
+	    call hdmname ("trim", Memc[rootname], 6)
+	    call strcpy (Memc[rootname], Memc[fullname], 6)
+	    call strcat (ampid, Memc[fullname], SZ_KEYWRD)
+
+	    # Write new overscan keyword.
+	    call timelog (Memc[buffer], SZ_LINE)
+	    call hdmpstr (out, Memc[fullname], Memc[buffer])
+
+	    # And record opperation in logfile
+	    call sprintf (Memc[amplifier], SZ_LINE, "    AMP%s")
+		call pargstr (ampid)
+	    call ccdlog (Memc[amplifier], Memc[buffer])
+	}
+
+	call sfree (sp)
+end
+
+procedure mergehist (in, out, keyword, ampid)
+
+pointer	in		# Input quadrant image
+pointer	out		# Output image
+char	keyword[ARB]	# Header keyword to modify
+char	ampid[2]	# Label for readout
+
+char	rootname[6], fullname[8]
+char	buffer[SZ_LINE]
+
+int	hdmaccf()
+
+begin
+	if (hdmaccf (out, keyword) == YES) {
+	    call hdmgstr (in, keyword, buffer, SZ_LINE)
+	    call hdmname (keyword, rootname, 6)
+	    call strcpy (rootname, fullname, 6)
+	    call strcat (ampid, fullname, 8)
+	    call hdmpstr (out, fullname, buffer)
+	}
+end
diff --git a/noao/imred/quadred/src/quad/quadmap.x b/noao/imred/quadred/src/quad/quadmap.x
new file mode 100644
index 00000000..db0a052b
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadmap.x
@@ -0,0 +1,297 @@
+include <imhdr.h>
+include <error.h>
+include "quadgeom.h"
+
+# QUADMAP --  Map subimages, one for each readout, for input or output
+
+int procedure quadmap (rootname, mode, clobber, in, qg, out)
+
+char	rootname[SZ_FNAME]	#I Root name for output images.
+int	mode			#I Access mode.
+bool	clobber			#I Clobber existing output images.
+pointer	in			#I Input image pointer (for NEW_COPY).
+pointer	qg			#I Pointer to quadgeom structure.
+pointer	out[ARB]		#O Array of imio pointers for sub-images.
+
+int	nopen			#O Number of subimages mapped.
+
+int	i, j, x, y, nx[QG_MAXAMPS], nampsx, nampsy
+char	fullname[SZ_LINE], id[SZ_AMPID]
+
+pointer	immap()
+int	ahivi(), imaccess()
+
+begin
+	switch (mode) {
+	case NEW_COPY, NEW_IMAGE:
+
+	    # Loop over active readouts
+	    nopen = 0
+	    do i = 1, QG_NAMPS(qg) {
+
+		nopen = nopen + 1
+
+		# The sub-section image need only be written if this is not a 
+		# phantom
+		if (QG_PHANTOM (qg, i) == NO) {
+
+		    # Make sub-image name
+		    call sprintf (fullname, SZ_LINE, "%s.%s")
+			call pargstr (rootname)
+			call pargstr (Memc[QG_AMPID(qg, nopen)])
+
+		    # If clobber is set then we can delete any pre-existing
+		    # sub-images. Otherwise it is an error if the sub-image already
+		    # exists. However we leave it to the immap call to find out.
+		    if (clobber) {
+			if (imaccess (fullname, READ_ONLY) == YES) 
+			    call imdelete (fullname)
+		    }
+
+		    iferr (out[nopen] = immap (fullname, mode, in)) {
+			nopen = nopen - 1
+			do j = 1, nopen 
+			    call imunmap (out[j])
+			call erract (EA_ERROR)
+		    }
+
+		    call quadwritehdr (qg, out[nopen], i)
+
+		} else {
+		    out[nopen] = NULL
+		}
+	    }
+
+
+	case READ_ONLY, READ_WRITE:
+
+	    # Loop over full grid of possible readout positions.
+	    nopen = 0
+	    do y = 1, QG_MAXAMPS {
+		nx[y] = 0
+		do x = 1, QG_MAXAMPS {
+
+		    # Make readout id string
+		    call sprintf (id, SZ_AMPID, "%1d%1d")
+			call pargi (y)
+			call pargi (x)
+
+		    # Make sub-image name
+		    call sprintf (fullname, SZ_LINE, "%s.%s")
+			call pargstr (rootname)
+			call pargstr (id)
+
+		    # Attempt to map it.
+		    nopen = nopen + 1
+		    if (nopen > QG_MAXAMPS) {
+			nopen = nopen - 1
+			next
+		    }
+
+		    # Skip to next grid position if sub-image does not exist.
+		    iferr (out[nopen] = immap (fullname, mode, in)) {
+			nopen = nopen - 1
+			next
+		    }
+		    nx[y] = nx[y] + 1
+		    call quadreadhdr (qg, out[nopen], nopen, id)
+		}
+	    }
+
+	    nampsx = ahivi (nx, QG_MAXAMPS)
+	    nampsy = nopen / nampsx
+	    QG_NAMPS(qg)  = nopen
+	    QG_NAMPSX(qg) = nampsx
+	    QG_NAMPSY(qg) = nampsy
+
+	    # Consolidate quadgeom structure and perform consistancy checks
+#	    call quaddump (qg)
+	    call quadmerge (qg)
+
+	}
+
+	return (nopen)
+end
+
+# QUADWRITEHDR -- Add dimensions and section information to image header.
+
+procedure quadwritehdr (qg, im, readout)
+
+pointer	im			#I Pointer to output sub-image image.
+pointer	qg			#I Pointer to open quadgeom structure.
+int	readout			#I readout number.
+
+int	amp
+pointer	sp, section, keyword
+
+int	hdmaccf()
+
+begin
+	call smark (sp)
+	call salloc (section, SZ_LINE, TY_CHAR)
+	call salloc (keyword, SZ_LINE, TY_CHAR)
+
+	IM_LEN (im, 1) = QG_NX(qg, readout)
+	IM_LEN (im, 2) = QG_NY(qg, readout)
+
+	call sprintf (Memc[section], SZ_LINE, "[%d:%d,%d:%d]")
+	    call pargi (QG_DX1(qg, readout))
+	    call pargi (QG_DX2(qg, readout))
+	    call pargi (QG_DY1(qg, readout))
+	    call pargi (QG_DY2(qg, readout))
+	call hdmpstr (im, "datasec", Memc[section])
+
+	call sprintf (Memc[section], SZ_LINE, "[%d:%d,%d:%d]")
+	    call pargi (QG_TX1(qg, readout))
+	    call pargi (QG_TX2(qg, readout))
+	    call pargi (QG_TY1(qg, readout))
+	    call pargi (QG_TY2(qg, readout))
+	call hdmpstr (im, "trimsec", Memc[section])
+
+	call sprintf (Memc[section], SZ_LINE, "[%d:%d,%d:%d]")
+	    call pargi (QG_BX1(qg, readout))
+	    call pargi (QG_BX2(qg, readout))
+	    call pargi (QG_BY1(qg, readout))
+	    call pargi (QG_BY2(qg, readout))
+	call hdmpstr (im, "biassec", Memc[section])
+
+	call sprintf (Memc[section], SZ_LINE, "[%d:%d,%d:%d]")
+	    call pargi (QG_CX1(qg, readout))
+	    call pargi (QG_CX2(qg, readout))
+	    call pargi (QG_CY1(qg, readout))
+	    call pargi (QG_CY2(qg, readout))
+	call hdmpstr (im, "ccdsec", Memc[section])
+
+	# Delete zSECyx keywords for all other amps from header
+	do amp = 1, QG_NAMPS(qg) {
+	    if (amp != readout) {
+	       call sprintf (Memc[keyword], SZ_LINE, "ASEC%2s")
+		   call pargstr (Memc[QG_AMPID(qg, amp)])
+		if (hdmaccf (im, Memc[keyword]) == YES)
+		     call hdmdelf (im, Memc[keyword])
+
+	       call sprintf (Memc[keyword], SZ_LINE, "BSEC%2s")
+		   call pargstr (Memc[QG_AMPID(qg, amp)])
+		if (hdmaccf (im, Memc[keyword]) == YES)
+		     call hdmdelf (im, Memc[keyword])
+
+	       call sprintf (Memc[keyword], SZ_LINE, "CSEC%2s")
+		   call pargstr (Memc[QG_AMPID(qg, amp)])
+		if (hdmaccf (im, Memc[keyword]) == YES)
+		     call hdmdelf (im, Memc[keyword])
+
+	       call sprintf (Memc[keyword], SZ_LINE, "DSEC%2s")
+		   call pargstr (Memc[QG_AMPID(qg, amp)])
+		if (hdmaccf (im, Memc[keyword]) == YES)
+		     call hdmdelf (im, Memc[keyword])
+
+	       call sprintf (Memc[keyword], SZ_LINE, "TSEC%2s")
+		   call pargstr (Memc[QG_AMPID(qg, amp)])
+		if (hdmaccf (im, Memc[keyword]) == YES)
+		     call hdmdelf (im, Memc[keyword])
+	    }
+	}
+
+	call sfree (sp)
+
+end
+
+# QUADREADHDR -- Get dimensions and section information from image header.
+
+procedure quadreadhdr (qg, im, readout, id)
+
+pointer	qg			#I Pointer to open quadgeom structure.
+pointer	im			#I Pointer to input sub-image image.
+int	readout			#I Readout number.
+char	id[SZ_AMPID]		#I Readout identifier.
+
+int	nx, ny
+int	dx1, dx2, dxs, dy1, dy2, dys
+int	tx1, tx2, txs, ty1, ty2, tys
+int	bx1, bx2, bxs, by1, by2, bys
+int	cx1, cx2, cxs, cy1, cy2, cys
+pointer	sp, section
+
+int	hdmaccf(), strdic()
+
+begin
+	call smark (sp)
+	call salloc (section, SZ_LINE, TY_CHAR)
+
+	# Store QG_AMPID and set QG_AMPTYPE
+	call malloc (QG_AMPID(qg, readout), SZ_AMPID, TY_CHAR)
+
+	call strcpy (id, Memc[QG_AMPID(qg, readout)], SZ_AMPID)
+
+	QG_AMPTYPE (qg, readout) = strdic (id, id, SZ_AMPID, AMPDICT)
+
+	# Get input image dimensions.
+	nx = IM_LEN (im, 1)
+	ny = IM_LEN (im, 2)
+	QG_NX(qg, readout) = nx
+	QG_NY(qg, readout) = ny
+
+	# Get datasec, trimsec etc. from image header, setting a null value
+	# for any missing sections.
+	if (hdmaccf (im, "datasec") == YES) {
+	    call hdmgstr (im, "datasec", Memc[section], SZ_LINE)
+	    dx1 = 1
+	    dx2 = nx
+	    dxs = 1
+	    dy1 = 1
+	    dy2 = ny
+	    dys = 1
+	    call ccd_section (Memc[section], dx1, dx2, dxs, dy1, dy2, dys)
+	}
+	QG_DX1(qg, readout) = dx1
+	QG_DX2(qg, readout) = dx2
+	QG_DY1(qg, readout) = dy1
+	QG_DY2(qg, readout) = dy2
+
+	if (hdmaccf (im, "trimsec") == YES) {
+	    call hdmgstr (im, "trimsec", Memc[section], SZ_LINE)
+	    tx1 = dx1
+	    tx2 = dx2
+	    txs = 1
+	    ty1 = dy1
+	    ty2 = dy2
+	    tys = 1
+	    call ccd_section (Memc[section], tx1, tx2, txs, ty1, ty2, tys)
+	}
+	QG_TX1(qg, readout) = tx1
+	QG_TX2(qg, readout) = tx2
+	QG_TY1(qg, readout) = ty1
+	QG_TY2(qg, readout) = ty2
+
+	if (hdmaccf (im, "biassec") == YES) {
+	    call hdmgstr (im, "biassec", Memc[section], SZ_LINE)
+	    bx1 = dx2 + 1
+	    bx2 = nx
+	    bxs = 1
+	    by1 = 1
+	    by2 = ny
+	    bys = 1
+	    call ccd_section (Memc[section], bx1, bx2, bxs, by1, by2, bys)
+	}
+	QG_BX1(qg, readout) = bx1
+	QG_BX2(qg, readout) = bx2
+	QG_BY1(qg, readout) = by1
+	QG_BY2(qg, readout) = by2
+
+	if (hdmaccf (im, "ccdsec") == YES) {
+	    call hdmgstr (im, "ccdsec", Memc[section], SZ_LINE)
+	    cx1 = dx1
+	    cx2 = dx2
+	    cxs = 1
+	    cy1 = dy1
+	    cy2 = dy2
+	    cys = 1
+	    call ccd_section (Memc[section], cx1, cx2, cxs, cy1, cy2, cys)
+	}
+	QG_CX1(qg, readout) = cx1
+	QG_CX2(qg, readout) = cx2
+	QG_CY1(qg, readout) = cy1
+	QG_CY2(qg, readout) = cy2
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/quad/quadmerge.x b/noao/imred/quadred/src/quad/quadmerge.x
new file mode 100644
index 00000000..ec75d286
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadmerge.x
@@ -0,0 +1,122 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+procedure quadmerge (qg)
+
+pointer	qg		#I Pointer to quadgeom structure.
+
+int	nx, ny, xdata, ydata, txskip1, txskip2, tyskip1, tyskip2
+int	bxskip1, bxskip2, byskip1, byskip2
+int	x, y, amp, pre, namps, nampsx, nampsy
+
+begin
+	namps  = QG_NAMPS(qg)
+	nampsx = QG_NAMPSX(qg)
+	nampsy = QG_NAMPSY(qg)
+
+	# Check consistancy of number of active readouts.
+	if (namps == 0)
+	    call error (0, "No input images")
+	if (namps != nampsx * nampsy)
+	    call error (0, "Incomplete or inconsistant set of sub-images")
+
+	# Determine dimensions of the composite image.
+	# We just sum the dimensions of the first row and column of sub-images
+	# We should realy check that the sub-images do form a regular grid.
+	nx = 0
+	do x = 1, nampsx {
+	    nx = nx + QG_NX(qg, QG_AMP(qg, x, 1))
+	}
+	ny = 0
+	do y = 1, nampsy {
+	    ny = ny + QG_NY(qg, QG_AMP(qg, 1, y))
+	}
+	QG_NX(qg, 0) = nx 
+	QG_NY(qg, 0) = ny 
+
+	# Calculate datasec, trimsec, and biassec, ccdsec for composite image.
+	# The required sections are those for the equivalent mono-readout image.
+	# If datasec is uninitialised assume all these sections are absent as 
+	# will be the case for processed [OT] images.
+	if (QG_DX1 (qg, 1) != 0) {
+	    # Calculate number of data pixels.
+	    xdata = 0
+	    do x = 1, nampsx {
+		amp   = QG_AMP(qg, x, 1)
+		xdata = xdata + QG_DX2(qg, amp) - QG_DX1(qg, amp) + 1
+	    }
+	    ydata = 0
+	    do y = 1, nampsy {
+		amp   = QG_AMP(qg, 1, y)
+		ydata = ydata + QG_DY2(qg, amp) - QG_DY1(qg, amp) + 1
+	    }
+	    txskip1 = QG_TX1(qg, 1)     - QG_DX1(qg, 1)
+	    txskip2 = QG_DX2(qg, namps) - QG_TX2(qg, namps)
+	    tyskip1 = QG_TY1(qg, 1)     - QG_DY1(qg, 1)
+	    tyskip2 = QG_DY2(qg, namps) - QG_TY2(qg, namps)
+
+	    # Calculate width of bias strip margins.
+	    switch (QG_AMPTYPE(qg, 1)) {
+	    case AMP11, AMP21:		# "Left amp"
+		bxskip1 = QG_BX1(qg, 1) - QG_DX2(qg, 1) - 1
+		bxskip2 = QG_NX(qg, 1)  - QG_BX2(qg, 1)
+
+	    case AMP12, AMP22:		# "Right amp"
+		bxskip1 = QG_DX1(qg, 1) - QG_BX2(qg, 1) - 1
+		bxskip2 = QG_BX1(qg, 1) - 1
+	    }
+
+	    byskip1 = QG_BY1(qg, 1)    - 1
+	    byskip2 = QG_NY(qg, namps) - QG_BY2(qg, namps)
+
+	    QG_DX1(qg, 0) = QG_DX1(qg, 1)
+	    QG_DX2(qg, 0) = QG_DX1(qg, 0) + xdata - 1
+	    QG_DY1(qg, 0) = QG_DY1(qg, 1)
+	    QG_DY2(qg, 0) = QG_DY1(qg, 0) + ydata - 1
+
+	    QG_TX1(qg, 0) = QG_DX1(qg, 0) + txskip1
+	    QG_TX2(qg, 0) = QG_DX2(qg, 0) - txskip2
+	    QG_TY1(qg, 0) = QG_DY1(qg, 0) + tyskip1
+	    QG_TY2(qg, 0) = QG_DY2(qg, 0) - tyskip2
+
+	    QG_BX1(qg, 0) = QG_DX2(qg, 0) + bxskip1 + 1
+	    QG_BX2(qg, 0) = nx - bxskip2
+	    QG_BY1(qg, 0) = 1  + byskip1
+	    QG_BY2(qg, 0) = ny - byskip2
+	}
+
+	# Calculate ccdsec for composite image using sub-images in BLH and TRH
+	# corners.
+	if (QG_CX1 (qg, 1) != 0) {
+	    QG_CX1(qg, 0) = QG_CX1(qg, 1)
+	    QG_CX2(qg, 0) = QG_CX2(qg, nampsx)
+	    QG_CY1(qg, 0) = QG_CY1(qg, 1)
+	    QG_CY2(qg, 0) = QG_CY2(qg, namps)
+	}
+
+	# Set up "ampsec" - the section of the composite image derived from
+	# each sub-image.
+	do y = 1, nampsy {
+	    amp = QG_AMP (qg, 1, y)
+	    QG_AX1(qg, amp) = 1
+	    QG_AX2(qg, amp) = QG_NX(qg, amp)
+	    do x = 2, nampsx {
+		amp = QG_AMP (qg, x,   y)
+		pre = QG_AMP (qg, x-1, y)
+		QG_AX1(qg, amp) = QG_AX2(qg, pre) + 1
+		QG_AX2(qg, amp) = QG_AX1(qg, amp) + QG_NX(qg, amp) - 1
+	    }
+	}
+	do x = 1, nampsx {
+	    amp = QG_AMP (qg, x, 1)
+	    QG_AY1(qg, amp) = 1
+	    QG_AY2(qg, amp) = QG_NY(qg, amp)
+	    do y = 2, nampsy {
+		amp = QG_AMP (qg, x, y)
+		pre = QG_AMP (qg, x, y-1)
+		QG_AY1(qg, amp) = QG_AY2(qg, pre) + 1
+		QG_AY2(qg, amp) = QG_AY1(qg, amp) + QG_NY(qg, amp) - 1
+	    }
+	}
+
+end
diff --git a/noao/imred/quadred/src/quad/quadproc.cl b/noao/imred/quadred/src/quad/quadproc.cl
new file mode 100644
index 00000000..3a881cd7
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadproc.cl
@@ -0,0 +1,173 @@
+procedure quadproc (images)
+
+begin
+	string	ims, in_list, cal_list, qp_list
+	int	nims
+	struct	buffer
+
+	# Freeze input image list 
+	in_list = mktemp ("uparm$tmp")
+	ccdlist (images, ccdtype="", names+, > in_list)
+	ims = "@"//in_list
+
+	# Check that the input list contains some images of the specified type.
+	ccdssselect (ims, ccdtype=ccdtype, subset="") | count | scan (nims)
+	if (nims == 0) {	# Nothing to do !
+	    delete (in_list, ver-)
+	    return
+	}
+
+	# Set initial values for the ccdproc parameters used for fitting the
+	# overscan. These parameters may be modified during the interactive
+	# fitting process, the new values being used for all subsequent fits.
+	qccdproc.function    = function
+	qccdproc.order       = order
+	qccdproc.sample	     = sample
+	qccdproc.naverage    = naverage
+	qccdproc.niterate    = niterate
+	qccdproc.low_reject  = low_reject
+	qccdproc.high_reject = high_reject
+	qccdproc.grow        = grow
+	qccdproc.interactive = interactive
+
+	if (overscan || trim || fixpix) {
+	    # Only those images which must be treated specialy are processed
+	    # with qproc:
+	    #	1) Multiple readout
+	    # 	2) Not already trimmed
+
+	    # First process [OT] any calibration images which WILL BE USED so
+	    # that we can be sure they will be reduced explicitly by qproc
+	    # rather than automaticaly within ccdproc.
+	    qp_list = mktemp ("uparm$tmp")
+
+	    if (noproc) {
+
+		cal_list = mktemp ("uparm$tmp")
+		qpcalimage (images=ims, only_param=yes, check=no, > cal_list)
+		qpselect ("@"//cal_list, ccdtype="", stop=no, > qp_list)
+		delete (cal_list, ver-)
+		count (qp_list) | scan (nims)
+		if (nims > 0) {
+		    printf ("Calibration images which will be processed:\n")
+		    qnoproc (qp_list, fixpix=fixpix, overscan=overscan,
+		    trim=trim, fixfile=fixfile, xskip1=xskip1, xskip2=xskip2,
+		    xtrim1=xtrim1, xtrim2=xtrim2, ytrim1=ytrim1, ytrim2=ytrim2)
+
+		    printf ("\nImages from the input list:\n")
+		}
+
+	    } else {
+
+		cal_list = mktemp ("uparm$tmp")
+		qpcalimage (images=ims, only_param=no, check=no, > cal_list)
+		qpselect ("@"//cal_list, ccdtype="", stop=no, > qp_list)
+		delete (cal_list, ver-)
+		count (qp_list) | scan (nims)
+		if (nims > 0) {
+		    qproc (qp_list, fixpix=fixpix, overscan=overscan, trim=trim,
+		    readaxis=readaxis, fixfile=fixfile, xskip1=xskip1,
+		    xskip2=xskip2, xtrim1=xtrim1, xtrim2=xtrim2, ytrim1=ytrim1,
+		    ytrim2=ytrim2)
+
+		}
+	    }
+
+	    delete (qp_list, ver-)
+
+	    # Now process all the remaining images.
+	    qpselect (ims, ccdtype=ccdtype, stop=no, >> qp_list) 
+
+	    if (noproc) {
+		qnoproc (qp_list, fixpix=fixpix, overscan=overscan,
+		trim=trim, fixfile=fixfile, xskip1=xskip1, xskip2=xskip2,
+		xtrim1=xtrim1, xtrim2=xtrim2, ytrim1=ytrim1, ytrim2=ytrim2)
+	    } else {
+		qproc (qp_list, fixpix=fixpix, overscan=overscan, trim=trim,
+		readaxis=readaxis, fixfile=fixfile, xskip1=xskip1,
+		xskip2=xskip2, xtrim1=xtrim1, xtrim2=xtrim2, ytrim1=ytrim1,
+		ytrim2=ytrim2)
+	    }
+
+	    delete (qp_list, ver-)
+
+	}
+
+	# Do all other operations with the standard ccdproc.
+
+	if (noproc) {
+
+	    # Handle those images that will be processed with qproc ....
+	    qpselect (ims, ccdtype=ccdtype, stop=no, >> qp_list) 
+
+	    # We must also include the calibration images or ccdproc will
+	    # complain about missing calibrations.
+	    qpcalimage (images=ims, only_param=no, check=no, > cal_list)
+	    qpselect ("@"//cal_list, ccdtype="", stop=yes, >> qp_list)
+
+	    if (zerocor || darkcor || flatcor || illumcor || fringecor ||
+	    readcor || scancor) {
+		qccdproc ("@"//qp_list, noproc=yes, 
+		fixpix=no, overscan=no, trim=no, zerocor=zerocor,
+		darkcor=darkcor, flatcor=flatcor, illumcor=illumcor,
+		fringecor=fringecor, readcor=readcor, scancor=scancor, 
+		ccdtype=ccdtype, max_cache=max_cache, readaxis=readaxis,
+		fixfile=fixfile, biassec="image", trimsec="image", zero=zero,
+		dark=dark, flat=flat, illum=illum, fringe=fringe,
+		minreplace=minreplace, scantype=scantype, nscan=nscan)
+	    }
+
+	    printf ("\n")
+	    delete (qp_list, ver-)
+
+	    # ..... and those that won't
+	    qpselect (ims, ccdtype=ccdtype, stop=yes, >> qp_list) 
+
+	    qccdproc ("@"//qp_list, noproc=yes, 
+	    fixpix=fixpix, overscan=overscan, trim=trim, zerocor=zerocor,
+	    darkcor=darkcor, flatcor=flatcor, illumcor=illumcor,
+	    fringecor=fringecor, readcor=readcor, scancor=scancor, 
+	    ccdtype=ccdtype, max_cache=max_cache, readaxis=readaxis,
+	    fixfile=fixfile, biassec="image", trimsec="image", zero=zero,
+	    dark=dark, flat=flat, illum=illum, fringe=fringe,
+	    minreplace=minreplace, scantype=scantype, nscan=nscan)
+
+	    delete (qp_list, ver-)
+
+	} else {
+
+	    # Validate fixfile
+	    if (fixpix) {
+		match ("single_readout", fixfile) | scan (buffer)
+		if (stridx ("#", buffer) == 0) {
+		    buffer = "fixfile " // fixfile // 
+		    " cannot be used with multi-readout images"
+		    error (0, buffer)
+		}
+	    }
+
+	    qccdproc (ims, ccdtype=ccdtype, max_cache=max_cache, noproc=no,
+	    fixpix=fixpix, overscan=overscan, trim=trim, zerocor=zerocor,
+	    darkcor=darkcor, flatcor=flatcor, illumcor=illumcor, 
+	    fringecor=fringecor, readcor=readcor, scancor=scancor, 
+	    readaxis=readaxis, fixfile=fixfile, biassec="image",
+	    trimsec="image", zero=zero, dark=dark, flat=flat, illum=illum,
+	    fringe=fringe, minreplace=minreplace, scantype=scantype,
+	    nscan=nscan, backup=backup, interactive=interactive,
+	    verbose=verbose, logfile=logfile)
+
+	    # Set task parameters used for overscan fitting to the ccdproc
+	    # values which may have been adjusted interactively
+	    function.p_value    = qccdproc.function
+	    order.p_value       = qccdproc.order
+	    sample.p_value      = qccdproc.sample
+	    naverage.p_value    = qccdproc.naverage
+	    niterate.p_value    = qccdproc.niterate
+	    low_reject.p_value  = qccdproc.low_reject
+	    high_reject.p_value = qccdproc.high_reject
+	    grow.p_value        = qccdproc.grow
+
+	}
+
+	delete (in_list,   ver-)
+end
diff --git a/noao/imred/quadred/src/quad/quadproc.par b/noao/imred/quadred/src/quad/quadproc.par
new file mode 100644
index 00000000..edc70514
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadproc.par
@@ -0,0 +1,42 @@
+images,s,a,"",,,List of CCD images to correct
+ccdtype,s,h,"",,,CCD image type to correct
+max_cache,i,h,0,0,,Maximum image caching memory (in Mbytes)
+noproc,b,h,no,,,"List processing steps only?
+"
+fixpix,b,h,yes,,,Fix bad CCD lines and columns?
+overscan,b,h,yes,,,Apply overscan strip correction?
+trim,b,h,yes,,,Trim the image?
+zerocor,b,h,yes,,,Apply zero level correction?
+darkcor,b,h,yes,,,Apply dark count correction?
+flatcor,b,h,yes,,,Apply flat field correction?
+illumcor,b,h,no,,,Apply illumination correction?
+fringecor,b,h,no,,,Apply fringe correction?
+readcor,b,h,no,,,Convert zero level image to readout correction?
+scancor,b,h,no,,,"Convert flat field image to scan correction?
+"
+readaxis,s,h,"line","column|line",, Read out axis (column|line)
+fixfile,s,h,"",,,File describing the bad lines and columns
+xskip1,i,h,INDEF,0,,X pixels to skip at start of overscan
+xskip2,i,h,INDEF,0,,X pixels to skip at end of overscan
+xtrim1,i,h,INDEF,0,,X pixels to trim at start of data
+xtrim2,i,h,INDEF,0,,X pixels to trim at end   of data
+ytrim1,i,h,INDEF,0,,Y pixels to trim at start of data
+ytrim2,i,h,INDEF,0,,Y pixels to trim at end   of data
+zero,s,h,"",,,Zero level calibration image
+dark,s,h,"",,,Dark count calibration image
+flat,s,h,"",,,Flat field images
+illum,s,h,"",,,Illumination correction images
+fringe,s,h,"",,,Fringe correction images
+minreplace,r,h,1.,,,Minimum flat field value
+scantype,s,h,"shortscan","shortscan|longscan",,Scan type (shortscan|longscan)
+nscan,i,h,1,1,,"Number of short scan lines
+"
+interactive,b,h,no,,,Fit overscan interactively?
+function,s,h,"legendre",,,Fitting function
+order,i,h,1,1,,Number of polynomial terms or spline pieces
+sample,s,h,"*",,,Sample points to fit
+naverage,i,h,1,,,Number of sample points to combine
+niterate,i,h,1,0,,Number of rejection iterations
+low_reject,r,h,3.,0.,,Low sigma rejection factor
+high_reject,r,h,3.,0.,,High sigma rejection factor
+grow,r,h,0.,0.,,Rejection growing radius
diff --git a/noao/imred/quadred/src/quad/quadscale.par b/noao/imred/quadred/src/quad/quadscale.par
new file mode 100644
index 00000000..9241c2b1
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadscale.par
@@ -0,0 +1,7 @@
+input,s,a,,,,Input image
+output,s,a,,,,Output image
+gain11,r,h,1,,,"Gain for quadrant y=1, x=1"
+gain12,r,h,1,,,"Gain for quadrant y=1, x=2"
+gain21,r,h,1,,,"Gain for quadrant y=2, x=1"
+gain22,r,h,1,,,"Gain for quadrant y=2, x=2"
+opperation,s,h,"multiply","multiply|divide",,Multiply or divide by gains
diff --git a/noao/imred/quadred/src/quad/quadscale.x b/noao/imred/quadred/src/quad/quadscale.x
new file mode 100644
index 00000000..5e594eb4
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadscale.x
@@ -0,0 +1,159 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+define	OPPERATIONS	"|multiply|divide|"
+define	OPMULTIPLY	1
+define	OPDIVIDE	2
+define	TOL1		 1.0e-7
+define	TOL2		-1.0e-7
+
+procedure t_quadscale ()
+
+char	input[SZ_FNAME]		#TI Input image name.
+char	output[SZ_FNAME]	#TI Output image name.
+char    instrument[SZ_FNAME]    #TI Instrument translation file
+
+real	gain[QG_MAXAMPS]	#TI Gain factor for each quadrant
+int	op			#TI Multiply or divide by gain factors
+
+int	i
+pointer	in, out, qg
+char	buffer[SZ_LINE]
+
+real	clgetr()
+int	clgwrd(), hdmaccf()
+pointer	immap()
+
+begin
+        # Open instrument file
+        call clgstr ("instrument",  instrument,  SZ_FNAME)
+        call hdmopen (instrument)
+
+	# Open input image
+	call clgstr ("input",  input,  SZ_FNAME)
+	in = immap  (input, READ_ONLY, 0)
+
+	# Allocate quadgeom structure and initialise it from image header
+	call quadalloc (qg)
+
+
+	# Fill out quadgeom structure from header depending on revision level
+	if (hdmaccf (in, "HDR_REV") == NO) {
+
+	    # Check to see if the image has been processed or not
+	    if (hdmaccf (in, "ccdproc") == YES) {
+		call quadgeomred (in, qg)
+	    } else {
+		call quadgeom (in, qg, "", "")
+	    }
+
+	} else {
+	    call qghdr2 (in, qg)
+	}
+
+	# Open output image
+	call clgstr ("output",  output,  SZ_FNAME)
+	out = immap (output, NEW_COPY, in)
+	IM_PIXTYPE(out) = TY_REAL
+
+	# Get gain factors
+	gain[1] = clgetr ("gain11")
+	gain[2] = clgetr ("gain12")
+	gain[3] = clgetr ("gain21")
+	gain[4] = clgetr ("gain22")
+
+	# Get direction of opperation
+	op = clgwrd ("opperation", buffer, SZ_LINE, OPPERATIONS)
+
+	switch (op) {
+	case OPMULTIPLY:
+	    call quadmult (in, out, gain, qg)
+
+	case OPDIVIDE:
+	    # Check for zero gain --> divide by zero
+	    do i = 1, 4 {
+		if ((gain[i] < TOL1) && (gain[i] > TOL2)) {
+		    call error (0, "Attempt to divide by gain value of zero")
+		}
+	    }
+	    call quaddiv (in, out, gain, qg)
+
+	}
+
+	call imunmap (in)
+	call imunmap (out)
+	call quadfree (qg)
+	call hdmclose ()
+end
+
+procedure quadmult (in, out, gain, qg)
+
+pointer	in				#I imio pointer for input image.
+pointer	out				#I imio pointer for output image.
+real	gain[ARB]			#I Array of gain factors.
+pointer	qg				#I Pointer to quadgeom structure.
+
+pointer	inbuf, obuf
+int	junk, nx, x, y, line, amp, amp2, off
+long	invec[IM_MAXDIM], ovec[IM_MAXDIM]
+
+int	imgnlr(), impnlr()
+
+begin
+
+	# Setup start vector for sequential reads
+	call amovkl (long(1), invec, IM_MAXDIM)
+	call amovkl (long(1), ovec,  IM_MAXDIM)
+
+	do y = 1, QG_NAMPS(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+	    do line = 1, QG_NY(qg, amp2) {
+		junk = imgnlr (in,  inbuf, invec)
+		junk = impnlr (out, obuf,  ovec) 
+		off = 0
+		do x = 1, QG_NAMPSX(qg) {
+		    amp = QG_AMP(qg, x, y)
+		    nx = QG_NX(qg, amp)
+		    call amulkr (Memr[inbuf+off], gain[amp], Memr[obuf+off], nx)
+		    off = off + nx
+		}
+	    }
+	}
+
+end
+
+procedure quaddiv (in, out, gain, qg)
+
+pointer	in				#I imio pointer for input image.
+pointer	out				#I imio pointer for output image.
+real	gain[ARB]			#I Array of gain factors.
+pointer	qg				#I Pointer to quadgeom structure.
+
+pointer	inbuf, obuf
+int	junk, nx, x, y, line, amp, amp2, off
+long	invec[IM_MAXDIM], ovec[IM_MAXDIM]
+
+int	imgnlr(), impnlr()
+
+begin
+
+	# Setup start vector for sequential reads
+	call amovkl (long(1), invec, IM_MAXDIM)
+	call amovkl (long(1), ovec,  IM_MAXDIM)
+
+	do y = 1, QG_NAMPS(qg) {
+	    amp2 = QG_AMP(qg, 1, y)
+	    do line = 1, QG_NY(qg, amp2) {
+		junk = imgnlr (in,  inbuf, invec)
+		junk = impnlr (out, obuf,  ovec) 
+		off = 0
+		do x = 1, QG_NAMPSX(qg) {
+		    amp = QG_AMP(qg, x, y)
+		    nx = QG_NX(qg, amp)
+		    call adivkr (Memr[inbuf+off], gain[amp], Memr[obuf+off], nx)
+		    off = off + nx
+		}
+	    }
+	}
+
+end
diff --git a/noao/imred/quadred/src/quad/quadsections.par b/noao/imred/quadred/src/quad/quadsections.par
new file mode 100644
index 00000000..aa6ae59d
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadsections.par
@@ -0,0 +1,14 @@
+images,s,a,"",,,Input image name
+window,s,h,"datasec","|datasec|trimsec|biassec|reflect|duplicate|",,Window to apply to section
+section,s,h,"",,,Default Image section
+template,s,h,"",,,Template for formating results
+#
+## TRIM AND OVERSCAN MARGINS (override header values)"
+#xskip1,i,h,INDEF,0,,X pixels to skip at start of overscan
+#xskip2,i,h,INDEF,0,,X pixels to skip at end of overscan
+#xtrim1,i,h,INDEF,0,,X pixels to trim at start of data
+#xtrim2,i,h,INDEF,0,,X pixels to trim at end   of data
+#ytrim1,i,h,INDEF,0,,Y pixels to trim at start of data
+#ytrim2,i,h,INDEF,0,,"Y pixels to trim at end   of data
+#"
+#mode,s,h,"ql"
diff --git a/noao/imred/quadred/src/quad/quadsections.x b/noao/imred/quadred/src/quad/quadsections.x
new file mode 100644
index 00000000..1d21d94c
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadsections.x
@@ -0,0 +1,447 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+# QUADSECTIONS.X -- File header comment.
+
+define	OPTION_DICT	"|biassec|datasec|trimsec|reflect|duplicate|"
+
+define	OPT_BIASSEC	1
+define	OPT_DATASEC	2
+define	OPT_TRIMSEC	3
+define	OPT_REFLECT	4
+define	OPT_DUPLICATE	5
+
+define	DEFAULT_MACRO	"$I$S\\n"
+
+
+# QUADSECTIONS -- Quadsections task.
+
+procedure t_quadsections ()
+
+pointer	inlist			#TI List of input image name.
+char	instrument[SZ_FNAME]	#TI Instrument translation file
+char	section[SZ_LINE]	#TI Section of CCD required
+int	option			#TI Type of section required
+char	format[SZ_LINE]		#TI strmac macro string for building output
+int	xtrim1			#TI X pixels to trim at start of data
+int	xtrim2			#TI X pixels to trim at end   of data
+int	ytrim1			#TI Y pixels to trim at start of data
+int	ytrim2			#TI Y pixels to trim at end   of data
+int	xskip1			#TI X pixels to skip at start of overscan
+int	xskip2			#TI X pixels to skip at end   of overscan
+ 
+char	buffer[SZ_LINE], input[SZ_LINE]
+
+int	clgwrd(), imtopenp(), imtgetim()
+
+begin
+	# Open input image
+	inlist = imtopenp ("images")
+
+	# Open instrument file
+	call clgstr    ("instrument",  instrument,  SZ_FNAME)
+	call hdmopen   (instrument)
+
+	# Get option.
+	option = clgwrd ("window", buffer, SZ_LINE, OPTION_DICT)
+
+	# Get default section
+	call clgstr ("section", section, SZ_LINE)
+
+	# Get user defined trim and overscan margins
+	#xtrim1 = clgeti ("xtrim1")
+	#xtrim2 = clgeti ("xtrim2")
+	#ytrim1 = clgeti ("ytrim1")
+	#ytrim2 = clgeti ("ytrim2")
+	#xskip1 = clgeti ("xskip1")
+	#xskip2 = clgeti ("xskip2")
+	xtrim1 = INDEFI
+	xtrim2 = INDEFI
+	ytrim1 = INDEFI
+	ytrim2 = INDEFI
+	xskip1 = INDEFI
+	xskip2 = INDEFI
+
+	# Get format string and convert to a strmac macro string.
+	call clgstr ("template", format, SZ_LINE)
+	if (format[1] == EOS)
+	    call sprintf (format, SZ_LINE, "%s")
+		call pargstr (DEFAULT_MACRO)
+	call qsmkmacro (format, format, SZ_LINE)
+
+	while (imtgetim (inlist, input, SZ_LINE) != EOF)  {
+	    call quadsections (input, section, xtrim1, xtrim2, ytrim1, ytrim2,
+	    xskip1, xskip2, option, format)
+	}
+
+	# Tidy up
+	call hdmclose ()
+	call imtclose (inlist)
+end
+
+
+# QUADSECTIONS -- ???
+
+procedure quadsections (input, section, xtrim1, xtrim2, ytrim1, ytrim2,
+	xskip1, xskip2, option, format)
+
+char	input[SZ_FNAME]		#I Input image name.
+char	section[SZ_LINE]	#I Default section specification
+int	xtrim1			#I X pixels to trim at start of data
+int	xtrim2			#I X pixels to trim at end   of data
+int	ytrim1			#I Y pixels to trim at start of data
+int	ytrim2			#I Y pixels to trim at end   of data
+int	xskip1			#I X pixels to skip at start of overscan
+int	xskip2			#I X pixels to skip at end   of overscan
+int	option			#I Type of section required
+char	format[SZ_LINE]		#I strmac macro string for building output
+
+char	image[SZ_LINE], argstr[SZ_LINE], buffer[SZ_LINE]
+char	insection[SZ_LINE], outsection[SZ_LINE]
+int	amp, arg[9], len
+int	i, x1,  x2,  y1,  y2
+
+pointer	in, qg
+bool	reduced
+
+pointer	immap()
+int	hdmaccf(), gstrcpy(), strlen(), strmac()
+bool	quadsect()
+
+begin
+	# Parse input into an image name and an image section.
+	call imgimage   (input, image,     SZ_LINE)
+	call imgsection (input, insection, SZ_LINE)
+	# if no section was supplied in the image name use the default section.
+	if (insection[1] == EOS) {
+	    call strcpy (section, insection, SZ_LINE)
+	}
+
+	# Open input image
+	in = immap  (image, READ_ONLY, 0)
+
+	# Determine if image has been trimmed or not
+	reduced = (hdmaccf (in, "trim") == YES)
+
+	if (reduced) { 
+	    # OPT_BIASSEC does not make sense for reduced images.
+	    if (option == OPT_BIASSEC)
+		return
+	    # Trimsec and datasec are identical for reduced images
+	    if (option == OPT_TRIMSEC)
+		option = OPT_DATASEC
+	}
+
+	# Set-up quadgeom structure
+	call quadalloc (qg)
+        if (hdmaccf (in, "HDR_REV") == NO) {
+	    if (reduced) {
+		call quadgeomred (in, qg)
+	    } else {
+		call quadgeom (in, qg, "", "")
+	    }
+        } else {
+            call qghdr2 (in, qg)
+        }
+
+#	call quaddump (qg)
+
+	# Adjust quadgeom structure for user trim and overscan margins
+	if (! reduced) {
+	    call qguser (qg, xtrim1, xtrim2, ytrim1, ytrim2, xskip1, xskip2)
+	}
+#	call quaddump (qg)
+
+
+	# Store image name as first argument in macro argument string "argstr"
+	arg[1] = 1
+	arg[2] = 1 + arg[1] + gstrcpy (image, argstr, SZ_LINE)
+
+	# Blank output string
+	buffer[1] = EOS
+
+	# Determine the intersection of the specified section with the portion
+	# of the image read through each readout.
+	do amp = 1, QG_NAMPS (qg) {
+
+	    # skip any phantoms in raw images
+	    if (QG_PHANTOM (qg, amp) == NO) {
+
+		if (quadsect (qg, insection, option, amp, x1, x2, y1, y2)) {
+		    # Build resulting section string ...
+		    call sprintf (outsection, SZ_LINE, "[%d:%d,%d:%d]")
+			call pargi (x1)
+			call pargi (x2)
+			call pargi (y1)
+			call pargi (y2)
+
+		    # ... and save it as second argument
+		    arg[3] = 1 + arg[2] + gstrcpy (outsection, argstr[arg[2]],
+		    SZ_LINE-arg[2]+1)
+
+		    # Save Ampid as third argument
+		    call strcpy (Memc[QG_AMPID(qg, amp)], argstr[arg[3]],
+		    SZ_LINE-arg[3]+1)
+
+		    # Process macro string
+		    i = strmac (format, argstr, buffer, SZ_LINE)
+		    call printf (buffer)
+		}
+	    }
+	}
+
+	# Output <lf> if format does not explicitly include one.
+	len = strlen (buffer)
+	if ((len > 2) && !(buffer[len-1]=='\\' && buffer[len]=='n')) {
+	    call printf ("\n")
+	}
+
+	call flush (STDOUT)
+
+	# Tidy up
+	call quadfree (qg)
+	call imunmap (in)
+end
+
+
+# QSMKMACRO -- Perform the following substitutions on the given macro string
+#
+# $I --> $1
+# $S --> $2
+# $A --> $3
+# $? --> $?
+
+procedure qsmkmacro (instr, outstr, maxchars)
+
+char	instr[ARB]			#I Input macro string.
+char	outstr[maxchars]		#O Output macro string.
+int	maxchars			#I Maximum length of outstr
+
+char	ch
+int	ip, op
+
+begin
+
+	op = 1
+	for (ip=1; instr[ip] != EOS; ip=ip+1) {
+	    ch = instr[ip]
+	    outstr[op] = ch
+	    op = op + 1
+	    if (op > maxchars)
+		call error (0, "qsmkmacro: Output buffer overflow")
+	    
+	    if (ch == '$') {
+		ip = ip + 1
+		ch = instr[ip]
+
+		if (ch == 'I') {
+		    outstr (op) = '1'
+		    op = op + 1
+		} else if (ch == 'S') {
+		    outstr (op) = '2'
+		    op = op + 1
+		} else if (ch == 'A') {
+		    outstr (op) = '3'
+		    op = op + 1
+		} else {
+		    outstr (op) = ch
+		    op = op + 1
+		}
+		if (op > maxchars)
+		    call error (0, "qsmkmacro: Output buffer overflow")
+	    }
+	}
+end
+
+
+# QUADSECT -- ??
+
+bool procedure quadsect (qg, section, option, amp, x1, x2, y1, y2)
+
+pointer	qg			#I Pointer to initialised quadgeom structure.
+char	section[SZ_LINE]	#I Default section specification.
+int	option			#I Type of section required.
+int	amp			#I Amplifier for which section is required.
+int	x1, x2, y1, y2		#O Corners of specified section.
+bool	overlap			#O true if part of section read through amp.
+
+int	xskip, xsize, yskip, ysize
+int	sx1, sx2, sy1, sy2, sxs, sys
+int	dx1, dx2, dy1, dy2
+int	tx1, tx2, ty1, ty2
+int	bx1, bx2, by1, by2
+
+begin
+
+	# Decode input section
+	x1  = 1
+	x2  = QG_NX(qg, 0)
+	sxs = 1
+	y1  = 1
+	y2  = QG_NY(qg, 0)
+	sys = 1
+	call ccd_section (section, x1, x2, sxs, y1, y2, sys)
+	sx1 = min (x1, x2)
+	sx2 = max (x1, x2)
+	sy1 = min (y1, y2)
+	sy2 = max (y1, y2)
+
+	# Set up null return (overlap) values in case no part of section was
+	# read with this amplifier.
+	overlap = false
+	x1 = 0
+	x2 = 0
+	y1 = 0
+	y2 = 0
+
+	# Calculate suplimentary quantitiies as required.
+	switch (option) {
+
+	case OPT_REFLECT, OPT_DUPLICATE:
+	    xskip = sx1 - QG_DX1(qg, 0)
+	    xsize = sx2 - sx1 + 1
+	    yskip = sy1 - QG_DY1(qg, 0)
+	    ysize = sy2 - sy1 + 1
+	}
+
+	# Determine the intersection of the specified section with the portion
+	# of the image read through the specified readout.
+	switch (option) {
+
+	case OPT_BIASSEC:
+	    bx1 = QG_AX1(qg, amp) + QG_BX1(qg, amp) - 1
+	    bx2 = QG_AX1(qg, amp) + QG_BX2(qg, amp) - 1
+	    by1 = QG_AY1(qg, amp) + QG_BY1(qg, amp) - 1
+	    by2 = QG_AY1(qg, amp) + QG_BY2(qg, amp) - 1
+
+	    if (sx1 > bx2)
+		return (overlap)
+	    if (sx2 < bx1)
+		return (overlap)
+	    if (sy1 > by2)
+		return (overlap)
+	    if (sy2 < by1)
+		return (overlap)
+
+	    x1 = max (sx1, bx1)
+	    x2 = min (sx2, bx2)
+	    y1 = max (sy1, by1)
+	    y2 = min (sy2, by2)
+
+	case OPT_DATASEC:
+	    dx1 = QG_AX1(qg, amp) + QG_DX1(qg, amp) - 1
+	    dx2 = QG_AX1(qg, amp) + QG_DX2(qg, amp) - 1
+	    dy1 = QG_AY1(qg, amp) + QG_DY1(qg, amp) - 1
+	    dy2 = QG_AY1(qg, amp) + QG_DY2(qg, amp) - 1
+
+	    if (sx1 > dx2)
+		return (overlap)
+	    if (sx2 < dx1)
+		return (overlap)
+	    if (sy1 > dy2)
+		return (overlap)
+	    if (sy2 < dy1)
+		return (overlap)
+
+	    x1 = max (sx1, dx1)
+	    x2 = min (sx2, dx2)
+	    y1 = max (sy1, dy1)
+	    y2 = min (sy2, dy2)
+
+	case OPT_TRIMSEC:
+	    tx1 = QG_AX1(qg, amp) + QG_TX1(qg, amp) - 1
+	    tx2 = QG_AX1(qg, amp) + QG_TX2(qg, amp) - 1
+	    ty1 = QG_AY1(qg, amp) + QG_TY1(qg, amp) - 1
+	    ty2 = QG_AY1(qg, amp) + QG_TY2(qg, amp) - 1
+
+	    if (sx1 > tx2)
+		return (overlap)
+	    if (sx2 < tx1)
+		return (overlap)
+	    if (sy1 > ty2)
+		return (overlap)
+	    if (sy2 < ty1)
+		return (overlap)
+
+	    x1 = max (sx1, tx1)
+	    x2 = min (sx2, tx2)
+	    y1 = max (sy1, ty1)
+	    y2 = min (sy2, ty2)
+
+	case OPT_REFLECT:
+	    dx1 = QG_AX1(qg, amp) + QG_DX1(qg, amp) - 1
+	    dx2 = QG_AX1(qg, amp) + QG_DX2(qg, amp) - 1
+	    dy1 = QG_AY1(qg, amp) + QG_DY1(qg, amp) - 1
+	    dy2 = QG_AY1(qg, amp) + QG_DY2(qg, amp) - 1
+
+	    switch (QG_AMPTYPE(qg, amp)) {
+	    case AMP11:
+		x1  = dx1 + xskip
+		x2  = x1  + xsize - 1
+		y1  = dy1 + yskip
+		y2  = y1  + ysize - 1
+
+	    case AMP12:
+		x2  = dx2 - xskip
+		x1  = x2  - xsize + 1
+		y1  = dy1 + yskip
+		y2  = y1  + ysize - 1
+
+	    case AMP21:
+		x1  = dx1 + xskip
+		x2  = x1  + xsize - 1
+		y2  = dy2 - yskip
+		y1  = y2  - ysize + 1
+
+	    case AMP22:
+		x2  = dx2 - xskip
+		x1  = x2  - xsize + 1
+		y2  = dy2 - yskip
+		y1  = y2  - ysize + 1
+	    }
+		
+	    if (x1 > dx2)
+		return (overlap)
+	    if (x2 < dx1)
+		return (overlap)
+	    if (y1 > dy2)
+		return (overlap)
+	    if (y2 < dy1)
+		return (overlap)
+
+	    x1 = max (x1, dx1)
+	    x2 = min (x2, dx2)
+	    y1 = max (y1, dy1)
+	    y2 = min (y2, dy2)
+
+	case OPT_DUPLICATE:
+	    dx1 = QG_AX1(qg, amp) + QG_DX1(qg, amp) - 1
+	    dx2 = QG_AX1(qg, amp) + QG_DX2(qg, amp) - 1
+	    dy1 = QG_AY1(qg, amp) + QG_DY1(qg, amp) - 1
+	    dy2 = QG_AY1(qg, amp) + QG_DY2(qg, amp) - 1
+
+	    x1  = dx1 + xskip
+	    x2  = x1  + xsize - 1
+	    y1  = dy1 + yskip
+	    y2  = y1  + ysize - 1
+
+	    if (x1 > dx2)
+		return (overlap)
+	    if (x2 < dx1)
+		return (overlap)
+	    if (y1 > dy2)
+		return (overlap)
+	    if (y2 < dy1)
+		return (overlap)
+
+	    x1 = max (x1, dx1)
+	    x2 = min (x2, dx2)
+	    y1 = max (y1, dy1)
+	    y2 = min (y2, dy2)
+
+	}
+
+	overlap = true
+	return (overlap)
+
+end
diff --git a/noao/imred/quadred/src/quad/quadsplit.par b/noao/imred/quadred/src/quad/quadsplit.par
new file mode 100644
index 00000000..274018c0
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadsplit.par
@@ -0,0 +1,9 @@
+input,s,a,"",,,Input image name
+output,s,h,"",,,Output root name
+clobber,b,h,"yes",,,Clobber prexisting subimages
+#xskip1,i,h,INDEF,0,,X pixels to skip at start of overscan
+#xskip2,i,h,INDEF,0,,X pixels to skip at end of overscan
+#xtrim1,i,h,INDEF,0,,X pixels to trim at start of data
+#xtrim2,i,h,INDEF,0,,X pixels to trim at end   of data
+#ytrim1,i,h,INDEF,0,,Y pixels to trim at start of data
+#ytrim2,i,h,INDEF,0,,Y pixels to trim at end   of data
diff --git a/noao/imred/quadred/src/quad/quadsplit.x b/noao/imred/quadred/src/quad/quadsplit.x
new file mode 100644
index 00000000..a6ffc95f
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadsplit.x
@@ -0,0 +1,115 @@
+include <imhdr.h>
+include "quadgeom.h"
+
+procedure t_quadsplit ()
+
+char	input[SZ_FNAME]		#TI Input image name.
+char	output[SZ_FNAME]	#TI Output image root name.
+char	instrument[SZ_FNAME]	#TI Instrument translation file.
+bool	clobber			#TI Clobber any existing sub-images.
+int     xtrim1         	#TI Number of pixels to trim at right.
+int     xtrim2         	#TI Number of pixels to trim at left.
+int     ytrim1         	#TI Number of pixels to trim at bottom.
+int     ytrim2         	#TI Number of pixels to trim at top.
+int     xskip1         	#TI Number of pixels to skip at start of overscan in X
+int     xskip2         	#TI Number of pixels to skip at end   of overscan in X
+
+pointer	in, qg, out[QG_MAXAMPS]
+int	amp, namps
+char	logstr[SZ_LINE]
+
+pointer	immap()
+bool	streq(), clgetb()
+int	quadmap(), hdmaccf()
+
+begin
+
+	# Open instrument file
+	call clgstr    ("instrument",  instrument,  SZ_FNAME)
+	call hdmopen   (instrument)
+
+	# Map input image
+	call clgstr ("input",  input,  SZ_FNAME)
+	in = immap  (input, READ_ONLY, 0)
+
+	# Get root name for output image
+	call clgstr  ("output", output, SZ_FNAME)
+	if (streq (output, ""))
+	    call strcpy (input, output, SZ_FNAME)
+	call xt_imroot (output, output, SZ_FNAME)
+
+	# Set-up section translation
+	call quadalloc (qg)
+
+	if (hdmaccf (in, "HDR_REV") == NO) {
+	    call quadgeom  (in, qg, "", "")
+	} else {
+	    call qghdr2 (in, qg)
+	}
+
+	# Adjust quadgeom structure for user trim and overscan margins
+	#xtrim1 = clgeti ("xtrim1")
+	#xtrim2 = clgeti ("xtrim2")
+	#ytrim1 = clgeti ("ytrim1")
+	#ytrim2 = clgeti ("ytrim2")
+	#xskip1 = clgeti ("xskip1")
+	#xskip2 = clgeti ("xskip2")
+	xtrim1 = INDEFI
+	xtrim2 = INDEFI
+	ytrim1 = INDEFI
+	ytrim2 = INDEFI
+	xskip1 = INDEFI
+	xskip2 = INDEFI
+	call qguser (qg, xtrim1, xtrim2, ytrim1, ytrim2, xskip1, xskip2)
+
+#	call quaddump  (qg)
+
+	# Map output images one for each readout
+	clobber = clgetb ("clobber")
+	namps = quadmap (output, NEW_COPY, clobber, in, qg, out)
+
+	# Split the image using the appropriately typed routine
+        switch (IM_PIXTYPE(in)) {
+        case TY_USHORT, TY_SHORT:
+	    call qsplits (in, out, qg)
+
+        case TY_LONG:
+	    call qsplitl (in, out, qg)
+
+	case TY_INT:
+	    call qspliti (in, out, qg)
+
+        case TY_REAL:
+	    call qsplitr (in, out, qg)
+
+        case TY_DOUBLE:
+	    call qsplitd (in, out, qg)
+
+        default:
+            call error (1, "unsupported pixel datatype")
+        }
+
+	# Log opperation
+	if (QG_NAMPSX(qg) == 2 && QG_NAMPSY(qg) == 2) {
+	    call sprintf (logstr, SZ_LINE, "Quad-readout image")
+	} else if (QG_NAMPSX(qg) == 2 || QG_NAMPSY(qg) == 2) {
+	    call sprintf (logstr, SZ_LINE,
+	    "Dual-readout image: nampsx=%d nampsy=%d")
+		call pargi (QG_NAMPSX(qg))
+		call pargi (QG_NAMPSY(qg))
+	} else {
+	    call sprintf (logstr, SZ_LINE, "Single-readout image")
+	}
+	call timelog (logstr, SZ_LINE)
+	call ccdlog (input, logstr)
+
+	# Tidy up
+	call imunmap (in)
+	do amp = 1, namps {
+	    if (out[amp] != NULL) {
+		call imunmap (out[amp])
+	    }
+	}
+	call quadfree (qg)
+	call hdmclose ()
+end
diff --git a/noao/imred/quadred/src/quad/quadtest/artobs.cl b/noao/imred/quadred/src/quad/quadtest/artobs.cl
new file mode 100644
index 00000000..292ed8c6
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadtest/artobs.cl
@@ -0,0 +1,68 @@
+# ARTOBS -- Simulate observe command using artificial data.
+
+procedure artobs ()
+
+begin
+	string	image, oim, ccdt
+	int	picnum, nexps, i
+	real	exptime
+	string	imtitle
+
+	# Get ccdtype
+	ccdt = obspars.ccdtype
+
+	# Get number of pictures to take
+	nexps   = npics
+
+	# Get next picture number
+	if (obspars.autopicnum) {
+	    picnum = obspars.picture.p_value
+	} else {
+	    picnum = obspars.picture
+	}
+
+	# Get exposure time
+	if (ccdt != "zero") {
+	    exptime = obspars.exposure
+	} else {
+	    exptime = 0.0
+	}
+
+	# Set filter
+	if (obspars.setfilter != "none" && ccdt != "zero" && ccdt != "dark") {
+	    if (instrpars.instrname != "")
+		mkquad.filter = instrpars.filter1
+	}
+
+	# Get imtitle. This MUST always be the last interactive prompt!
+	imtitle = title
+
+	for (i = picnum; i < picnum+nexps; i = i+1) {
+
+	    # Make image name
+	    if (ccdt == "object") {
+		printf ("obj%03d\n", i) | scan (image)
+	    } else {
+		printf ("%s%03d\n", ccdt, i) | scan (image)
+	    }
+	    if (access (image//".imh")) {
+		oim = image
+		image = mktemp (image//".")
+		printf ("Output image %s already exists...  %s used \n", oim, 
+		image)
+	    }
+
+	    if (ccdt == "dflat" || ccdt == "pflat")
+		ccdt = "flat"
+
+	    if (ccdt == "sflat" || ccdt == "comp" )
+	       ccdt = "other"
+
+	    # Call MKQUAD task
+	    mkquad (image, exptime, ccdt)
+	    hedit  (image, "i_title", imtitle, add+, ver-, show-)
+	    obspars.picture.p_value = i + 1
+	    printf ("Image %s written to disk\n", image, > "STDERR")
+	}
+
+end
diff --git a/noao/imred/quadred/src/quad/quadtest/artobs.par b/noao/imred/quadred/src/quad/quadtest/artobs.par
new file mode 100644
index 00000000..d9611ef5
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadtest/artobs.par
@@ -0,0 +1,5 @@
+# observe parameter file
+obspars,pset,h,,,,Observing parameters
+detpars,pset,h,,,,Detector parameters
+instrpars,pset,h,,,,Instrument parameters
+telpars,pset,h,,,,Telescope parameters
diff --git a/noao/imred/quadred/src/quad/quadtest/ccdpars.par b/noao/imred/quadred/src/quad/quadtest/ccdpars.par
new file mode 100644
index 00000000..b30fbb99
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadtest/ccdpars.par
@@ -0,0 +1,29 @@
+ncols,i,h,1060,,,"Number of columns"
+nlines,i,h,1024,,,"Number of lines
+"
+datasec,s,h,"[1:1024,1:1024]",,,"Data section"
+trimsec,s,h,"[1:1024,1:1024]",,,"Trim section"
+biassec,s,h,"[1025:1060,1:1024]",,,"Bias section
+"
+amplifiers,s,h,"Quad","|Quad|UpperPair|LowerPair|LowerLeft|",,"Amplifiers to use
+"
+gain1,r,h,1.0,,,gain (e-/ADU) for Amp12
+ron1,r,h,4.0,,,readout noise for Amp11
+zero1,i,h,1000,,,"zero level for Amp11"
+nlin1,s,h,"",,,"Non-linearity coefficants
+"
+gain2,r,h,1.0,,,gain (e-/ADU) for Amp12
+ron2,r,h,4.0,,,readout noise for Amp12
+zero2,i,h,1000,,,"zero level for Amp12"
+nlin2,s,h,"",,,"Non-linearity coefficants
+"
+gain3,r,h,1.0,,,gain (e-/ADU) for Amp21
+ron3,r,h,4.0,,,readout noise for Amp21
+zero3,i,h,1000,,,"zero level for Amp21"
+nlin3,s,h,"",,,"Non-linearity coefficants
+"
+gain4,r,h,1.0,,,gain (e-/ADU) for Amp22
+ron4,r,h,4.0,,,readout noise for Amp22
+zero4,i,h,1000,,,"zero level for Amp22"
+nlin4,s,h,"",,,"Non-linearity coefficants
+"
diff --git a/noao/imred/quadred/src/quad/quadtest/logfile b/noao/imred/quadred/src/quad/quadtest/logfile
new file mode 100644
index 00000000..ddf97f0a
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadtest/logfile
@@ -0,0 +1 @@
+obj99999: Dec  9 12:21 Quadjoin: nampsx=2 nampsy=2
diff --git a/noao/imred/quadred/src/quad/quadtest/mkamp.cl b/noao/imred/quadred/src/quad/quadtest/mkamp.cl
new file mode 100644
index 00000000..98cd8468
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadtest/mkamp.cl
@@ -0,0 +1,166 @@
+# MKAMP -- Make a CCD observation
+
+procedure mkamp (image, exptime, ccdtype)
+
+string	image			{prompt="Image name"}
+real	exptime			{prompt="Exposure time"}
+string	ccdtype			{prompt="CCD type"}
+
+int	ncols=132		{prompt="Number of columns"}
+int	nlines=100		{prompt="Number of lines"}
+string	filter=""		{prompt="Filter"}
+string	datasec=""		{prompt="Data section"}
+string	trimsec=""		{prompt="Trim section"}
+string	biassec=""		{prompt="Bias section"}
+
+file	imdata=""		{prompt="Image data"}
+real	skyrate=0.		{prompt="Sky count rate"}
+real	zeroval=0.		{prompt="Zero level value"}
+real	zeroslope=0.		{prompt="Slope of zero level"}
+real	flashval=0.		{prompt="Preflash value"}
+real	flashslope=0.		{prompt="Slope of preflash value"}
+real	darkrate=0.		{prompt="Dark count rate"}
+real	darkslope=0.		{prompt="Slope of dark count rate"}
+real	flatslope=0.		{prompt="Flat field slope"}
+file	badpix=""		{prompt="Bad pixel regions"}
+real	badval=0.		{prompt="Bad pixel value"}
+real	gain=1.			{prompt="Gain (e-/adu)", min=1.0e-9}
+real	ron=0.			{prompt="Read out noise e-"}
+string	nonlin			{prompt="Non-linearity coefficiants"}
+bool	poisson=yes		{prompt="Add poisson noise?"}
+bool	overwrite=no		{prompt="Overwrite existing image?"}
+struct	*fdnl			{prompt="Internal use"}
+
+begin
+	int	c1, c2, l1, l2, rseed, i, dummy
+	real	exp, value, valslope, invgain, date, rval, coef[7]
+	string	im, type, s, lincoefs, ampsec
+
+	im = image
+	exp = exptime
+	type = ccdtype
+
+	# Check for zero (or very small) gain
+	if (abs (gain) < 1.0e-9)
+	    call error (0, "zero (or very small) gain specified")
+
+	invgain = 1.0 / gain
+
+	if (access (im//".imh") == yes)
+	    im = im // ".imh"
+	if (access (im//".hhh") == yes)
+	    im = im // ".hhh"
+	if (access (im) == yes) {
+	    if (overwrite == yes)
+		imdelete (im, verify=no)
+	    else
+	        return
+	}
+
+	# Create the image.
+	s = str (ncols) // " " // str (nlines)
+	mkimage (im, "make", 0., 2, s, pixtype="real", slope=0., sigma=0.)
+
+	# Add a data image.
+	if (access (imdata//".imh") == yes)
+	    imdata = imdata // ".imh"
+	if (access (imdata//".hhh") == yes)
+	    imdata = imdata // ".hhh"
+	if (access (imdata) == yes)
+	    imcopy (imdata//datasec, im//datasec, verbose=no)
+
+	# Add sky.
+	value = exp * skyrate
+	if (value != 0.)
+	    mkimage (im//datasec, "add", value, slope=0., sigma=0.)
+
+	# Add flat field response.
+	if (flatslope != 0.)
+	    mkimage (im//datasec, "mul", 1., slope=flatslope, sigma=0.)
+	    
+	# Add preflash level and dark count.
+	value = flashval + exp * darkrate
+	valslope = flashslope + exp * darkslope
+	if ((value != 0.) && (valslope != 0.))
+	    mkimage (im//datasec, "add", value, slope=valslope, sigma=0.)
+
+	# Convert to ADU
+	mkimage (im//datasec, "mul", invgain, slope=0., sigma=0.)
+
+	# Add poisson and readout noise
+	# if seed is 0 pick a fairly arbitrary value
+	if (seed == 0) {
+	    date | translit ("STDIN", from_string="a-zA-Z: ", delete+) |
+	    scan (date)
+	    rseed = abs (date / 10000)
+	} else {
+	    rseed = seed
+	}
+
+	# Add non-linearity
+	if (nonlin != "") {
+	    lincoefs = mktemp ("uparm$tmp")
+	    files (nonlin, >> lincoefs)
+	    fdnl = lincoefs
+	    coef[1] = 1.0
+	    for (i=2; i <= 7; i = i+1) {
+		dummy = fscan (fdnl, rval)
+		if (dummy == EOF) {
+		   coef[i] = 0.0
+		} else {
+		    coef[i] = rval
+		}
+	    }
+
+	    irlincor (im, im, section= "", coeff1=coef[1], coeff2=coef[2],
+	    coeff3=coef[3], coeff4=coef[4], coeff5=coef[5], coeff6=coef[6],
+	    coeff7=coef[7], maxadu=65535.0)
+	    delete (lincoefs, ver-)
+	}
+
+	mknoise (im, background=0., gain=gain, rdnoise=ron, poisson=poisson, 
+	seed=rseed, cosrays="", ncosrays=0, comments=no)
+
+	# decrement seed for next use
+	if (seed < 0) 
+	    seed.p_value = seed - 1
+
+	# Add zero level
+	# We add an extra 0.5 so that we nint rather than truncate when 
+	# converting to short integer.
+	zeroval = zeroval + 0.5
+	mkimage (im, "add", zeroval, slope=zeroslope, sigma=0.)
+
+	# Set bad pixels.
+	if (access (badpix)) {
+	    list = badpix
+	    while (fscan (list, c1, c2, l1, l2) != EOF) {
+	        if (nscan() != 4)
+		    next
+	        c1 = max (1, c1)
+	        c2 = min (ncols, c2)
+	        l1 = max (1, l1)
+	        l2 = min (nlines, l2)
+	        s = "["//c1//":"//c2//","//l1//":"//l2//"]"
+	        mkimage (im//s, "replace", badval, slope=0., sigma=0.)
+	    }
+	}
+
+	# Convert to ushort data type
+	chpixtype (im, im, "ushort", oldpixtype="all", ver-)
+
+	# Set image header
+	ccdhedit (im, "exptime", exp, type="real")
+	if (type != "")
+	    ccdhedit (im, "imagetyp", type, type="string")
+
+	if (datasec != "") {
+	    ccdhedit (im, "datasec", datasec, type="string")
+	}
+	if (trimsec != "")
+	    ccdhedit (im, "trimsec", trimsec, type="string")
+	if (biassec != "")
+	    ccdhedit (im, "biassec", biassec, type="string")
+	if (filter != "")
+	    ccdhedit (im, "subset", filter, type="string")
+end
diff --git a/noao/imred/quadred/src/quad/quadtest/mkimage.par b/noao/imred/quadred/src/quad/quadtest/mkimage.par
new file mode 100644
index 00000000..148bf7ea
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadtest/mkimage.par
@@ -0,0 +1,10 @@
+image,s,a,,,,Image to make or modify
+option,s,a,,"make|replace|add|multiply",,Editing option
+value,r,a,,,,Mean pixel value
+slope,r,h,0.,,,Slope of pixel values
+sigma,r,h,0.,0.,,Noise sigma
+seed,i,h,0,0,,Seed for noise generator
+
+ndim,i,a,,1,7,Number of dimensions
+dims,s,a,,,,Image dimensions
+pixtype,s,h,"real","short|real",,Pixel datatype
diff --git a/noao/imred/quadred/src/quad/quadtest/mkquad.cl b/noao/imred/quadred/src/quad/quadtest/mkquad.cl
new file mode 100644
index 00000000..391d1a61
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadtest/mkquad.cl
@@ -0,0 +1,222 @@
+# MKQUAD -- Make an artifical multi-readout image
+
+procedure mkquad (image, exptime, ccdtype)
+
+begin
+	string	im, ccdt
+	real	exp, sky
+
+	string	amps, as, bs, cs, ds, ts, nampsyx, amplist
+	int	tx1, tx2, ty1, ty2
+	int	bx1, bx2, by1, by2
+	int	cx1, cx2, cy1, cy2
+	int	dx1, dx2, dy1, dy2
+	int	txs1, txs2, tys1, tys2
+	int	bxs1, bxs2, bys1, bys2
+	int	nx, ny, dnx, dny, onx, ony
+	int	nampx, nampy
+	bool	use_amp[4]
+
+	im   = image
+	if (access (im//".imh"))
+	    error (0, "Output image already exists")
+
+	exp  = exptime
+	ccdt = ccdtype
+	sky  = skyrate
+	amps = ccdpars.amplifiers
+
+	nx = ccdpars.ncols
+	ny = ccdpars.nlines
+
+	# Set number of amplifiers and use_amp. This is a bit kludgy
+	if (amps == "Quad") {
+	    nampx = 2
+	    nampy = 2
+	    use_amp[1] = yes
+	    use_amp[2] = yes
+	    use_amp[3] = yes
+	    use_amp[4] = yes
+	    amplist = "11 12 21 22"
+	} else if (amps == "LowerPair") {
+	    nampx = 2
+	    nampy = 1
+	    use_amp[1] = yes
+	    use_amp[2] = yes
+	    use_amp[3] = no
+	    use_amp[4] = no
+	    amplist = "11 12"
+	} else if (amps == "UpperPair") {
+	    nampx = 2
+	    nampy = 1
+	    use_amp[1] = no
+	    use_amp[2] = no
+	    use_amp[3] = yes
+	    use_amp[4] = yes
+	    amplist = "21 22"
+	} else if (amps == "LowerLeft") {
+	    nampx = 1
+	    nampy = 1
+	    use_amp[1] = yes
+	    use_amp[2] = no
+	    use_amp[3] = no
+	    use_amp[4] = no
+	    amplist = "11"
+	}
+
+	# Parse sections strings.
+	ccdsection (ccdpars.trimsec) | scan (tx1, tx2, ty1, ty2)
+	tx1 = max (1,  tx1)
+	tx2 = min (nx, tx2)
+	ty1 = max (1,  ty1)
+	ty2 = min (ny, ty2)
+
+	ccdsection (ccdpars.biassec) | scan (bx1, bx2, by1, by2)
+	bx1 = max (1,  bx1)
+	bx2 = min (nx, bx2)
+	by1 = max (1,  by1)
+	by2 = min (ny, by2)
+
+	ccdsection (ccdpars.datasec) | scan (dx1, dx2, dy1, dy2)
+	dx1 = max (1,  dx1)
+	dx2 = min (nx, dx2)
+	dy1 = max (1,  dy1)
+	dy2 = min (ny, dy2)
+
+	# Number of pixels to trim
+	txs1 = tx1 - 1
+	txs2 = dx2 - tx2
+	tys1 = ty1 - 1
+	tys2 = dy2 - ty2
+
+	# Number of pixels to skip before overscan strip
+	bxs1 = bx1 - dx2 - 1
+	bxs2 = nx  - bx2
+	bys1 = by1 - 1
+	bys2 = ny  - by2
+
+	# Number of pixels in subimages
+	nx  = nx / nampx
+	ny  = ny / nampy
+	dnx = (dx2 - dx1 + 1) / nampx
+	dny = (dy2 - dy1 + 1) / nampy
+	onx = nx - dnx
+	ony = ny
+
+	# Set ampsec for all amps
+	printf ("[1:%d,1:%d]\n", nx, ny) | scan (as)
+
+	# Set sections for Amp11 & Amp21
+	dx1 = 1
+	dx2 = dx1 + dnx - 1
+	dy1 = 1
+	dy2 = dy1 + dny - 1
+	printf ("[%d:%d,%d:%d]\n", dx1, dx2, dy1, dy2) | scan (ds)
+
+	tx1 = dx1 + txs1 
+	tx2 = dx2
+	ty1 = dy1 + tys1
+	ty2 = dy2
+	printf ("[%d:%d,%d:%d]\n", tx1, tx2, ty1, ty2) | scan (ts)
+
+	bx1 = dx2 + bxs1 + 1
+	bx2 = nx  - bxs2
+	by1 = 1 + bys1
+	by2 = ny
+	printf ("[%d:%d,%d:%d]\n", bx1, bx2, by1, by2) | scan (bs)
+
+	if (use_amp[1]) {
+	    mkamp (im//".11", exp, ccdt, ncols=nx, nlines=ny,
+	    filter=filter, datasec=ds, trimsec=ts, biassec=bs, imdata=imdata,
+	    skyrate=sky, zeroval=ccdpars.zero1, zeroslope=zeroslope,
+	    badpix=badpix, badval=badval, flashval=flashval,
+	    flashslope=flashslope, darkrate=darkrate, darkslope=darkslope,
+	    flatslope=flatslope, gain=ccdpars.gain1, ron=ccdpars.ron1,
+	    nonlin=ccdpars.nlin1, poisson=poisson, overwrite=yes)
+	    hedit (im//".11", "asec11", as, show-, ver-, add+)
+	    cx1 = 1 
+	    cx2 = cx1 + dnx - 1
+	    cy1 = 1
+	    cy2 = cy1 + dny - 1
+	    printf ("[%d:%d,%d:%d]\n", cx1, cx2, cy1, cy2) | scan (cs)
+	    hedit (im//".11", "ccdsec", cs, show-, ver-, add+)
+	}
+
+	if (use_amp[3]) {
+	    mkamp (im//".21", exp, ccdt, ncols=nx, nlines=ny,
+	    filter=filter, datasec=ds, trimsec=ts, biassec=bs, imdata=imdata,
+	    skyrate=sky, zeroval=ccdpars.zero3, zeroslope=zeroslope,
+	    badpix=badpix, badval=badval, flashval=flashval,
+	    flashslope=flashslope, darkrate=darkrate, darkslope=darkslope,
+	    flatslope=flatslope, gain=ccdpars.gain3, ron=ccdpars.ron3,
+	    nonlin=ccdpars.nlin3, poisson=poisson, overwrite=yes)
+	    hedit (im//".21", "asec21", as, show-, ver-, add+)
+	    cx1 = 1 
+	    cx2 = cx1 + dnx - 1
+	    cy1 = dny + 1
+	    cy2 = cy1 + dny - 1
+	    printf ("[%d:%d,%d:%d]\n", cx1, cx2, cy1, cy2) | scan (cs)
+	    hedit (im//".21", "ccdsec", cs, show-, ver-, add+)
+	}
+
+	# Set sections for Amp12 & Amp22
+	dx1 = onx + 1
+	dx2 = nx
+	dy1 = 1
+	dy2 = dy1 + dny - 1
+	printf ("[%d:%d,%d:%d]\n", dx1, dx2, dy1, dy2) | scan (ds)
+
+	tx1 = dx1 + txs1
+	tx2 = dx2
+	ty1 = dy1 + tys1
+	ty2 = dy2
+	printf ("[%d:%d,%d:%d]\n", tx1, tx2, ty1, ty2) | scan (ts)
+
+	bx1 = 1 + bxs1
+	bx2 = onx - bxs2
+	by1 = 1 + bys1
+	by2 = ny
+	printf ("[%d:%d,%d:%d]\n", bx1, bx2, by1, by2) | scan (bs)
+
+	if (use_amp[2]) {
+	    mkamp (im//".12", exp, ccdt, ncols=nx, nlines=ny,
+	    filter=filter, datasec=ds, trimsec=ts, biassec=bs, imdata=imdata,
+	    skyrate=sky, zeroval=ccdpars.zero2, zeroslope=zeroslope,
+	    badpix=badpix, badval=badval, flashval=flashval,
+	    flashslope=flashslope, darkrate=darkrate, darkslope=darkslope,
+	    flatslope=flatslope, gain=ccdpars.gain2, ron=ccdpars.ron2,
+	    nonlin=ccdpars.nlin2, poisson=poisson, overwrite=yes)
+	    hedit (im//".12", "asec12", as, show-, ver-, add+)
+	    cx1 = dnx + 1 
+	    cx2 = cx1 + dnx - 1
+	    cy1 = 1
+	    cy2 = cy1 + dny - 1
+	    printf ("[%d:%d,%d:%d]\n", cx1, cx2, cy1, cy2) | scan (cs)
+	    hedit (im//".12", "ccdsec", cs, show-, ver-, add+)
+	}
+
+	if (use_amp[4]) {
+	    mkamp (im//".22", exp, ccdt, ncols=nx, nlines=ny,
+	    filter=filter, datasec=ds, trimsec=ts, biassec=bs, imdata=imdata,
+	    skyrate=sky, zeroval=ccdpars.zero4, zeroslope=zeroslope,
+	    badpix=badpix, badval=badval, flashval=flashval,
+	    flashslope=flashslope, darkrate=darkrate, darkslope=darkslope,
+	    flatslope=flatslope, gain=ccdpars.gain4, ron=ccdpars.ron4,
+	    nonlin=ccdpars.nlin4, poisson=poisson, overwrite=yes)
+	    hedit (im//".22", "asec22", as, show-, ver-, add+)
+	    cx1 = dnx + 1 
+	    cx2 = cx1 + dnx - 1
+	    cy1 = dny + 1
+	    cy2 = cy1 + dny - 1
+	    printf ("[%d:%d,%d:%d]\n", cx1, cx2, cy1, cy2) | scan (cs)
+	    hedit (im//".22", "ccdsec", cs, show-, ver-, add+)
+	}
+
+	# Set NAMPSYX  and amplistin header
+	nampsyx = str (nampy) // " " // str (nampx)
+	hedit (im//".??.imh", "nampsyx", nampsyx, show-, ver-, add+)
+	hedit (im//".??.imh", "amplist", amplist, show-, ver-, add+)
+
+	quadjoin (im, output="", delete=yes)
+
+end
diff --git a/noao/imred/quadred/src/quad/quadtest/mkquad.par b/noao/imred/quadred/src/quad/quadtest/mkquad.par
new file mode 100644
index 00000000..662f315f
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadtest/mkquad.par
@@ -0,0 +1,4 @@
+image,s,a,,,,"Image name"
+exptime,r,a,,,,"Exposure time"
+ccdtype,s,a,,,,"CCD type"
+filter,s,h,"",,,"Filter"
diff --git a/noao/imred/quadred/src/quad/quadtest/quadtest.cl b/noao/imred/quadred/src/quad/quadtest/quadtest.cl
new file mode 100644
index 00000000..3129f636
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadtest/quadtest.cl
@@ -0,0 +1,14 @@
+# QUADTEST -- QUAD Test package
+
+# load artdata package (mknoise)
+artdata
+
+package quadtest
+
+task	mkimage		= quadtest$x_ccdred.e
+task	mkamp		= quadtest$mkamp.cl
+task	mkquad		= quadtest$mkquad.cl
+task	artobs		= quadtest$artobs.cl
+task	ccdpars		= quadtest$ccdpars.par
+
+clbye()
diff --git a/noao/imred/quadred/src/quad/quadtest/quadtest.par b/noao/imred/quadred/src/quad/quadtest/quadtest.par
new file mode 100644
index 00000000..efe72ef5
--- /dev/null
+++ b/noao/imred/quadred/src/quad/quadtest/quadtest.par
@@ -0,0 +1,20 @@
+# QUADTEST -- package parameter file
+imdata,f,h,"",,,"Image data"
+skyrate,r,h,0.,,,"Sky count rate
+"
+zeroslope,r,h,0.,,,"Slope of zero value"
+flatslope,r,h,0.,,,"Flat field slope
+"
+badpix,f,h,"",,,"Bad pixel regions"
+badval,r,h,0.,,,"Bad pixel value
+"
+flashval,r,h,0.,,,"Preflash level value"
+flashslope,r,h,0.,,,"Slope of preflash level
+"
+darkrate,r,h,0.,,,"Dark count rate"
+darkslope,r,h,0.,,,"Slope of dark count rate
+"
+poisson,b,h,yes,,,"Add Poisson noise"
+seed,i,h,0,,,"Random number seed
+"
+version,s,h,"Version 1.0 - Oct 93","Version 1.0 - Oct 93"  
diff --git a/noao/imred/quadred/src/quad/qzerocombine.cl b/noao/imred/quadred/src/quad/qzerocombine.cl
new file mode 100644
index 00000000..b8d554ae
--- /dev/null
+++ b/noao/imred/quadred/src/quad/qzerocombine.cl
@@ -0,0 +1,48 @@
+# ZEROCOMBINE -- Process and combine zero level CCD images.
+
+procedure zerocombine (input)
+
+string	input			{prompt="List of zero level images to combine"}
+file	output="Zero"		{prompt="Output zero level name"}
+string	combine="average"	{prompt="Type of combine operation",
+				 enum="average|median"}
+string	reject="minmax"		{prompt="Type of rejection",
+		enum="none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip"}
+string	ccdtype="zero"	{prompt="CCD image type to combine"}
+bool	process=no	{prompt="Process images before combining?"}
+bool	delete=no	{prompt="Delete input images after combining?"}
+bool	clobber=no	{prompt="Clobber existing output image?"}
+string	scale="none"	{prompt="Image scaling",
+			 enum="none|mode|median|mean|exposure"}
+string	statsec=""	{prompt="Image section for computing statistics"}
+int	nlow=0		{prompt="minmax: Number of low pixels to reject"}
+int	nhigh=1		{prompt="minmax: Number of high pixels to reject"}
+int	nkeep=1		{prompt="Minimum to keep (pos) or maximum to reject (neg)"}
+bool	mclip=yes	{prompt="Use median in sigma clipping algorithms?"}
+real	lsigma=3.	{prompt="Lower sigma clipping factor"}
+real	hsigma=3.	{prompt="Upper sigma clipping factor"}
+string	rdnoise="0."	{prompt="ccdclip: CCD readout noise (electrons)"}
+string	gain="1."	{prompt="ccdclip: CCD gain (electrons/DN)"}
+string	snoise="0."	{prompt="ccdclip: Sensitivity noise (fraction)"}
+real	pclip=-0.5	{prompt="pclip: Percentile clipping parameter"}
+real	blank=0.	{prompt="Value if there are no pixels"}
+
+begin
+	string	ims
+
+	ims = input
+
+	# Process images first if desired.
+	if (process == YES)
+	    quadproc (ims, ccdtype=ccdtype)
+
+	# Combine the flat field images.
+	combine (ims, output=output, plfile="", sigma="", combine=combine,
+	    reject=reject, ccdtype=ccdtype, subsets=no, delete=delete,
+	    clobber=clobber, project=no, outtype="real", offsets="none",
+	    masktype="none", blank=blank, scale=scale, zero="none", weight=no,
+	    statsec=statsec, lthreshold=INDEF, hthreshold=INDEF, nlow=nlow,
+	    nhigh=nhigh, nkeep=nkeep, mclip=mclip, lsigma=lsigma, hsigma=hsigma,
+	    rdnoise=rdnoise, gain=gain, snoise=snoise, sigscale=0.1,
+	    pclip=pclip, grow=0)
+end
diff --git a/noao/imred/quadred/src/quad/setinstrument.cl b/noao/imred/quadred/src/quad/setinstrument.cl
new file mode 100644
index 00000000..72361f89
--- /dev/null
+++ b/noao/imred/quadred/src/quad/setinstrument.cl
@@ -0,0 +1,58 @@
+# SETINSTRUMENT -- Set up instrument parameters for the CCD reduction tasks.
+#
+# This task sets default parameters based on an instrument ID.
+
+procedure setinstrument (instrument)
+
+char	instrument		{prompt="Instrument ID (type ? for a list)"}
+char	site="ctio"		{prompt="Site ID"}
+char	directory="ccddb$"	{prompt="Instrument directory"}
+bool	review=yes		{prompt="Review instrument parameters?"}
+char	query			{prompt="Instrument ID (type q to quit)",
+				 mode="q"}
+
+begin
+	string	inst, instdir, instmen, instfile
+
+	# Define instrument directory, menu, and file
+	instdir = directory
+	if (site != "")
+	    instdir = instdir // site // "/"
+	instmen = instdir // "instruments.men"
+	inst = instrument
+	instfile = instdir // inst // ".dat"
+
+	# Loop until a valid instrument file is given.
+	while (inst != "" && !access (instfile)) {
+	    if (access (instmen))
+		page (instmen)
+	    else if (inst == "?")
+		print ("Instrument list ", instmen, " not found")
+	    else
+	        print ("Instrument file ", instfile, " not found")
+	    print ("")
+	    inst = query
+	    if (inst == "q")
+		return
+	    instrument = inst
+	    instfile = instdir // inst // ".dat"
+	}
+
+	# Set instrument parameter.
+	if (access (instfile))
+	    quadred.instrument = instfile
+	else
+	    quadred.instrument = ""
+
+	# Run instrument setup script.
+	instfile = instdir // inst // ".cl"
+	if (access (instfile))
+	    cl (< instfile)
+
+	# Review parameters if desired.
+	if (review) {
+	    eparam ("quadred")
+	    eparam ("qccdproc")
+	    eparam ("quadproc")
+	}
+end
diff --git a/noao/imred/quadred/src/quad/test.x b/noao/imred/quadred/src/quad/test.x
new file mode 100644
index 00000000..3df5240a
--- /dev/null
+++ b/noao/imred/quadred/src/quad/test.x
@@ -0,0 +1,71 @@
+include	"quadgeom.h"
+
+procedure new ()
+
+char    input[SZ_FNAME]         #TI Input image name.
+char    instrument[SZ_FNAME]    #TI Instrument translation file
+ 
+pointer in, qg
+int	xtrim1, xtrim2, ytrim1, ytrim2, xskip1, xskip2
+ 
+int	clgeti
+pointer immap()
+ 
+begin
+ 
+        # Open instrument file
+        call clgstr    ("instrument",  instrument,  SZ_FNAME)
+        call hdmopen   (instrument)
+ 
+        # Open input image
+        call clgstr ("input",  input,  SZ_FNAME)
+        in = immap  (input, READ_ONLY, 0)
+
+	xtrim1 = clgeti ("xtrim1")
+	xtrim2 = clgeti ("xtrim2")
+	ytrim1 = clgeti ("ytrim1")
+	ytrim2 = clgeti ("ytrim2")
+	xskip1 = clgeti ("xskip1")
+	xskip2 = clgeti ("xskip2")
+ 
+        # Set-up section translation
+        call quadalloc (qg)
+        call qghdr2  (in, qg)
+	call qguser (qg, xtrim1, xtrim2, ytrim1, ytrim2, xskip1, xskip2)
+        call quaddump  (qg)
+ 
+        # Tidy up
+        call imunmap (in)
+        call quadfree (qg)
+        call hdmclose ()
+end
+
+procedure old ()
+
+char    input[SZ_FNAME]         #TI Input image name.
+char    instrument[SZ_FNAME]    #TI Instrument translation file
+ 
+pointer in, qg
+ 
+pointer immap()
+ 
+begin
+ 
+        # Open instrument file
+        call clgstr    ("instrument",  instrument,  SZ_FNAME)
+        call hdmopen   (instrument)
+ 
+        # Open input image
+        call clgstr ("input",  input,  SZ_FNAME)
+        in = immap  (input, READ_ONLY, 0)
+ 
+        # Set-up section translation
+        call quadalloc (qg)
+        call quadgeom  (in, qg, "", "")
+        call quaddump  (qg)
+ 
+        # Tidy up
+        call imunmap (in)
+        call quadfree (qg)
+        call hdmclose ()
+end
diff --git a/noao/imred/quadred/src/quad/timelog.x b/noao/imred/quadred/src/quad/timelog.x
new file mode 100644
index 00000000..7a8d969f
--- /dev/null
+++ b/noao/imred/quadred/src/quad/timelog.x
@@ -0,0 +1,29 @@
+include	<time.h>
+
+
+# TIMELOG -- Prepend a time stamp to the given string.
+#
+# For the purpose of a history logging prepend a short time stamp to the
+# given string.  Note that the input string is modified.
+
+procedure timelog (str, max_char)
+
+char	str[max_char]		# String to be time stamped
+int	max_char		# Maximum characters in string
+
+pointer	sp, time, temp
+long	clktime()
+
+begin
+	call smark (sp)
+	call salloc (time, SZ_DATE, TY_CHAR)
+	call salloc (temp, max_char, TY_CHAR)
+
+	call cnvdate (clktime(0), Memc[time], SZ_DATE)
+	call sprintf (Memc[temp], max_char, "%s %s")
+	    call pargstr (Memc[time])
+	    call pargstr (str)
+	call strcpy (Memc[temp], str, max_char)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/quadred/src/quad/x_quad.x b/noao/imred/quadred/src/quad/x_quad.x
new file mode 100644
index 00000000..8000dabf
--- /dev/null
+++ b/noao/imred/quadred/src/quad/x_quad.x
@@ -0,0 +1,14 @@
+task	ccdsection	= t_ccdsection,
+	quadsplit   	= t_quadsplit,
+	quadjoin    	= t_quadjoin,
+	ccddelete   	= t_ccddelete,
+	ccdgetparam 	= ccdgetparam,
+	ccdprcselect 	= t_ccdprcselect,
+	ccdssselect	= t_ccdsubsetselect,
+	qpcalimage	= t_qpcalimage,
+	qpselect	= t_qpselect,
+	quadscale   	= t_quadscale,
+	quadsections    = t_quadsections,
+	gainmeasure	= t_gainmeasure,
+	new		= new,
+	old		= old
diff --git a/noao/imred/specred/Revisions b/noao/imred/specred/Revisions
new file mode 100644
index 00000000..890668dc
--- /dev/null
+++ b/noao/imred/specred/Revisions
@@ -0,0 +1,167 @@
+.help revisions Jun88 noao.imred.msred
+.nf
+
+=======
+V2.12.3
+=======
+
+specred.cl
+specred.men
+    1.  Added ODCOMBINE and LSCOMBINE to the package.
+    2.  Modified SCOMBINE to point to new executable.
+    (6/21/04, Valdes)
+
+=====
+V2.12
+=====
+
+imred$specred/msresp1d.cl
+    Modified to use "imtype" rather than hardwired to "imh".  This uses
+    the same code as srcfibers$fibresponse.cl.
+    (2/29/00, Valdes)
+
+=========
+V2.11.3p1
+=========
+=======
+V2.11.3
+=======
+
+imred$specred/doc/msresp1d.hlp
+    The package was incorrect and the requirement that the unextracted
+    spectrum must be present even if the extracted spectrum is present
+    was made clearer.  (9/20/99, Valdes)
+
+=======
+V2.11.2
+=======
+
+imred$specred/doc/dofibers.hlp
+imred$specred/doc/doslit.hlp
+imred$specred/doc/dofibers.ms
+imred$specred/doc/doslit.ms
+    Updated for change where if both crval and cdelt are INDEF then the
+    automatic identification is not done.  (5/2/96, Valdes)
+
+imred$specred/specred.cl
+    Increased the minimum min_lenuserarea from 40000 to 100000.
+    (7/31/96, Valdes)
+
+imred$specred/doc/doslit.hlp
+imred$specred/doc/doslit.ms
+    Updated for the addition of automatic arc line identification.  (4/9/96)
+
+imred$specred/sparams.par
+    Changed match from 10 to -3.  (4/5/96, Valdes)
+
+imred$specred/dofibers.cl
+imred$specred/dofibers.par
+imred$specred/params.par
+imred$specred/doc/dofibers.hlp
+imred$specred/doc/dofibers.ms
+imred$specred/doc/doslit.hlp
+imred$specred/doc/doslit.ms
+    Added crval/cdelt parameters used in new version with automatic arc
+    line identification.  (4/5/96, Valdes)
+
+imred$specred/doc/msresp1d.hlp
+    Added a sentence to say that extracted throughput (sky) spectra are
+    flat fielded before computing the throughput values.  (1/9/96, Valdes)
+
+imred$specred/doc/dofibers.hlp
+imred$specred/doc/dofibers.ms
+    Describes the new header option for the aperture identification table.
+    (7/25/95, Valdes)
+
+imred$specred/specred.cl
+imred$specred/dofibers.cl
+imred$specred/dofibers.par
+imred$specred/doc/dofibers.hlp
+imred$specred/doc/dofibers.ms
+    Added sky alignment option.  (7/19/95, Valdes)
+
+=======
+V2.10.4
+=======
+
+specred/specred.cl
+specred/specred.men
+    1.  Added background, illumination, and response.
+    2.  Renamed the fiber response task to "fibresponse".
+    (12/29/94, Valdes)
+
+imred$specred/dofibers.cl
+    There was an incorrect default value for the dispaxis parameter:
+	)_dispaxis --> )_.dispaxis.  (8/24/92, Valdes)
+
+=============
+V2.10-V2.10.1
+=============
+
+imred$msred --> imred$specred
+    Renamed the package to a more generic name since it is for both
+    multiple aperture/fiber data as well as generic slit data.
+    (2/20/92, Valdes)
+
+imred$msred/msred.cl
+imred$msred/msred.hd
+    Added generic slit and fiber reduction tasks to make this a complete
+    generic package.  (2/19/92, Valdes)
+
+imred$msred/msresp1d.cl
+    Improved task to include throughput file (2/18/92, Valdes)
+
+imred$msred/msresp1d.cl +
+imred$msred/doc/msresp1d.hlp +
+imred$msred/msred.cl
+imred$msred/msred.hd
+    1.  Added new task MSRESP1D modeled after imred$src/fibers/response but
+	using APALL instead of APSCRIPT and all the connections to PARAMS.
+    2.  Added new task SKYSUB from imred$src/fibers.
+
+imred$msred/msbplot.cl -
+imred$msred/doc/msdispcor.hlp -
+imred$msred/doc/msbplot.hlp -
+imred$msred/msred.hd
+    1.  Moved help to ONEDSPEC.
+
+imred$msred/*
+    Updated to new APEXTRACT and ONEDSPEC packages.
+    (7/13/90, Valdes)
+
+====
+V2.9
+====
+
+imred$msred/msbplot.cl +
+imred$msred/doc/msbplot.hlp +
+imred$msred/msred.cl
+imred$msred/msred.men
+imred$msred/msred.hd
+    Added a version of ECBPLOT (written by Rob Seaman) to the package with
+    appropriate changes to refer to lines and apertures instead of
+    orders.  (10/27/89, Valdes)
+
+imred$msred/doc/msdispcor.hlp
+    Tried to make the description of the global parameter clearer.  Also
+    fixed an incorrect example.  (8/29/89, Valdes)
+
+====
+V2.8
+====
+
+imred$msred/apnormalize.par +
+imred$msred/msred.cl
+imred$msred/msred.men
+    Added APNORMALIZE to the package. (6/1/89, Valdes)
+
+imred$msred/standard.par
+    Removed ennumerated list.  (4/10/89, Valdes)
+
+imred$msred/* +
+imred$msred/doc/* +
+    New package specialized for reducing spectra in "multispec" format.
+    It includes new tasks for doing dispersion solutions in multispec
+    format spectra.  (3/29/89, Valdes)
+
+.endhelp
diff --git a/noao/imred/specred/doc/dofibers.hlp b/noao/imred/specred/doc/dofibers.hlp
new file mode 100644
index 00000000..d5a893a7
--- /dev/null
+++ b/noao/imred/specred/doc/dofibers.hlp
@@ -0,0 +1,1531 @@
+.help dofibers Jul95 noao.imred.specred
+.ih
+NAME
+dofibers -- Multifiber data reduction task
+.ih
+USAGE
+dofibers objects
+.ih
+SUMMARY
+The \fBdofibers\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, fiber throughput correction, wavelength calibration, and sky
+subtraction of multifiber spectra.  It is a
+command language script which collects and combines the functions and
+parameters of many general purpose tasks to provide a single complete data
+reduction path.  The task provides a degree of guidance, automation, and
+record keeping necessary when dealing with the large amount of data
+generated by multifiber instruments.  Variants of this task are
+\fBdoargus\fR, \fBdofoe\fR, \fBdohydra\fR, and \fBdo3fiber\fR.
+.ih
+PARAMETERS
+.ls objects
+List of object spectra to be processed.  Previously processed spectra are
+ignored unless the \fIredo\fR flag is set or the \fIupdate\fR flag is set and
+dependent calibration data has changed.  Extracted spectra are ignored.
+.le
+.ls apref = ""
+Aperture reference spectrum.  This spectrum is used to define the basic
+extraction apertures and is typically a flat field spectrum.
+.le
+.ls flat = "" (optional)
+Flat field spectrum.  If specified the one dimensional flat field spectra
+are extracted and used to make flat field calibrations.  If a separate
+throughput file or image is not specified the flat field is also used
+for computing a fiber throughput correction.
+.le
+.ls throughput = "" (optional)
+Throughput file or image.  If an image is specified, typically a blank
+sky observation, the total flux through
+each fiber is used to correct for fiber throughput.  If a file consisting
+of lines with the aperture number and relative throughput is specified
+then the fiber throughput will be corrected by those values.  If neither
+is specified but a flat field image is given it is used to compute the
+throughput.  
+.le
+.ls arcs1 = "" (at least one if dispersion correcting)
+List of primary arc spectra.  These spectra are used to define the dispersion
+functions for each fiber apart from a possible zero point correction made
+with secondary shift spectra or arc calibration fibers in the object spectra.
+One fiber from the first spectrum is used to mark lines and set the dispersion
+function interactively and dispersion functions for all other fibers and
+arc spectra are derived from it.
+.le
+.ls arcs2 = "" (optional)
+List of optional shift arc spectra.  Features in these secondary observations
+are used to supply a wavelength zero point shift through the observing
+sequence.  One type of observation is dome lamps containing characteristic
+emission lines.
+.le
+.ls arctable = "" (optional) (refspectra)
+Table defining arc spectra to be assigned to object
+spectra (see \fBrefspectra\fR).  If not specified an assignment based
+on a header parameter, \fIparams.sort\fR, such as the observation time is made.
+.le
+
+.ls readnoise = "0." (apsum)
+Read out noise in photons.  This parameter defines the minimum noise
+sigma.  It is defined in terms of photons (or electrons) and scales
+to the data values through the gain parameter.  A image header keyword
+(case insensitive) may be specified to get the value from the image.
+.le
+.ls gain = "1." (apsum)
+Detector gain or conversion factor between photons/electrons and
+data values.  It is specified as the number of photons per data value.
+A image header keyword (case insensitive) may be specified to get the value
+from the image.
+.le
+.ls datamax = INDEF (apsum.saturation)
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the flat field or
+arc spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.le
+.ls fibers = 97 (apfind)
+Number of fibers.  This number is used during the automatic definition of
+the apertures from the aperture reference spectrum.  It is best if this
+reflects the actual number of fibers which may be found in the aperture
+reference image.  The interactive
+review of the aperture assignments allows verification and adjustments
+to the automatic aperture definitions.
+.le
+.ls width = 12. (apedit)
+Approximate base full width of the fiber profiles.  This parameter is used
+for the profile centering algorithm.
+.le
+.ls minsep = 8. (apfind)
+Minimum separation between fibers.  Weaker spectra or noise within this
+distance of a stronger spectrum are rejected.
+.le
+.ls maxsep = 15. (apfind)
+Maximum separation between adjacent fibers.  This parameter
+is used to identify missing fibers.  If two adjacent spectra exceed this
+separation then it is assumed that a fiber is missing and the aperture
+identification assignments will be adjusted accordingly.
+.le
+.ls apidtable = "" (apfind)
+Aperture identification table.  This may be either a text file or an
+image.  A text file contains the fiber number, beam number defining object
+(1), sky (0), and arc (2) fibers, and a object title.  An image contains
+the keywords SLFIBnnn with string value consisting of the fiber number,
+beam number, optional right ascension and declination, and an object
+title.  Unassigned and broken fibers (beam of -1) should be included in the
+identification information since they will automatically be excluded.
+.le
+.ls crval = INDEF, cdelt = INDEF (autoidentify)
+These parameters specify an approximate central wavelength and dispersion.
+They may be specified as numerical values, INDEF, or image header keyword
+names whose values are to be used.
+If both these parameters are INDEF then the automatic identification will
+not be done.
+.le
+.ls objaps = "", skyaps = "", arcaps = ""
+List of object, sky, and arc aperture numbers.  These are used to
+identify arc apertures for wavelength calibration and object and sky
+apertures for sky subtraction.  Note sky apertures may be identified as
+both object and sky if one wants to subtract the mean sky from the
+individual sky spectra.  Typically the different spectrum types are
+identified by their beam numbers and the default, null string,
+lists select all apertures.
+.le
+.ls objbeams = "0,1", skybeams = "0", arcbeams = 2
+List of object, sky, and arc beam numbers.  The convention is that sky
+fibers are given a beam number of 0, object fibers a beam number of 1, and
+arc fibers a beam number of 2.  The beam numbers are typically set in the
+\fIapidtable\fR.  Unassigned or broken fibers may be given a beam number of
+-1 in the aperture identification table since apertures with negative beam
+numbers are not extracted.  Note it is valid to identify sky fibers as both
+object and sky.
+.le
+
+.ls scattered = no (apscatter)
+Smooth and subtracted scattered light from the object and flat field
+images.  This operation consists of fitting independent smooth functions
+across the dispersion using data outside the fiber apertures and then
+smoothing the individual fits along the dispersion.  The initial
+flat field, or if none is given the aperture reference image, are
+done interactively to allow setting the fitting parameters.  All
+subsequent subtractions use the same fitting parameters.
+.le
+.ls fitflat = yes (flat1d)
+Fit the composite flat field spectrum by a smooth function and divide each
+flat field spectrum by this function?  This operation removes the average
+spectral signature of the flat field lamp from the sensitivity correction to
+avoid modifying the object fluxes.
+.le
+.ls clean = yes (apsum)
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction and requires reasonably good values
+for the readout noise and gain.  In addition the datamax parameters
+can be useful.
+.le
+.ls dispcor = yes
+Dispersion correct spectra?  Depending on the \fIparams.linearize\fR
+parameter this may either resample the spectra or insert a dispersion
+function in the image header.
+.le
+.ls skyalign = no
+Align sky lines?  If yes then for the first object spectrum you are asked
+to mark one or more sky lines to use for alignment.  Then these lines will
+be found in all spectra and an average zeropoint shift computed and applied
+to the dispersion solution to align these lines.  Note that this assumes
+the sky lines are seen in all fibers.
+.le
+.ls savearcs = yes
+Save any simultaneous arc apertures?  If no then the arc apertures will
+be deleted after use.
+.le
+.ls skysubtract = yes
+Subtract sky from the object spectra?  If yes the sky spectra are combined
+and subtracted from the object spectra as defined by the object and sky
+aperture/beam parameters.
+.le
+.ls skyedit = yes
+Overplot all the sky spectra and allow contaminated sky spectra to be
+deleted?
+.le
+.ls saveskys = yes
+Save the combined sky spectrum?  If no then the sky spectrum will be
+deleted after sky subtraction is completed.
+.le
+.ls splot = no
+Plot the final spectra with the task \fBsplot\fR?
+.le
+.ls redo = no
+Redo operations previously done?  If no then previously processed spectra
+in the objects list will not be processed (unless they need to be updated).
+.le
+.ls update = yes
+Update processing of previously processed spectra if aperture, flat
+field, or dispersion reference definitions are changed?
+.le
+.ls batch = no
+Process spectra as a background or batch job provided there are no interactive
+options (\fIskyedit\fR and \fIsplot\fR) selected.
+.le
+.ls listonly = no
+List processing steps but don't process?
+.le
+
+.ls params = "" (pset)
+Name of parameter set containing additional processing parameters.  The
+default is parameter set \fBparams\fR.  The parameter set may be examined
+and modified in the usual ways (typically with "epar params" or ":e params"
+from the parameter editor).  Note that using a different parameter file
+is not allowed.  The parameters are described below.
+.le
+
+.ce
+-- PACKAGE PARAMETERS
+
+Package parameters are those which generally apply to all task in the
+package.  This is also true of \fBdofibers\fR.
+.ls dispaxis = 2
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.  The default value defers to the
+package parameter of the same name.
+.le
+.ls observatory = "observatory"
+Observatory at which the spectra were obtained if not specified in the
+image header by the keyword OBSERVAT.  See \fBobservatory\fR for more
+details.
+.le
+.ls interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc)
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.nf
+	nearest - nearest neighbor
+	 linear - linear
+	  poly3 - 3rd order polynomial
+	  poly5 - 5th order polynomial
+	spline3 - cubic spline
+	   sinc - sinc function
+.fi
+.le
+.ls database = "database"
+Database (directory) used for storing aperture and dispersion information.
+.le
+.ls verbose = no
+Print verbose information available with various tasks.
+.le
+.ls logfile = "logfile", plotfile = ""
+Text and plot log files.  If a filename is not specified then no log is
+kept.  The plot file contains IRAF graphics metacode which may be examined
+in various ways such as with \fBgkimosaic\fR.
+.le
+.ls records = ""
+Dummy parameter to be ignored.
+.le
+.ls version = "SPECRED: ..."
+Version of the package.
+.le
+
+.ce
+PARAMS PARAMETERS
+
+The following parameters are part of the \fBparams\fR parameter set and
+define various algorithm parameters for \fBdofibers\fR.
+
+.ce
+--  GENERAL PARAMETERS --
+.ls line = INDEF, nsum = 10
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, recentering, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.le
+.ls order = "decreasing" (apfind)
+When assigning aperture identifications order the spectra "increasing"
+or "decreasing" with increasing pixel position (left-to-right or
+right-to-left in a cross-section plot of the image).
+.le
+.ls extras = no (apsum)
+Include extra information in the output spectra?  When cleaning or using
+variance weighting the cleaned and weighted spectra are recorded in the
+first 2D plane of a 3D image, the raw, simple sum spectra are recorded in
+the second plane, and the estimated sigmas are recorded in the third plane.
+.le
+
+.ce
+-- DEFAULT APERTURE LIMITS --
+.ls lower = -5., upper = 5. (apdefault)
+Default lower and upper aperture limits relative to the aperture center.
+These limits are used when the apertures are first found and may be
+resized automatically or interactively.
+.le
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+.ls ylevel = 0.05 (apresize)
+Data level at which to set aperture limits during automatic resizing.
+It is a fraction of the peak relative to a local background.
+.le
+
+.ce
+-- TRACE PARAMETERS --
+.ls t_step = 10 (aptrace)
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \fInsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.le
+.ls t_function = "spline3", t_order = 3 (aptrace)
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.le
+.ls t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+Default number of rejection iterations and rejection sigma thresholds.
+.le
+
+.ce
+-- SCATTERED LIGHT PARAMETERS --
+.ls buffer = 1. (apscatter)
+Buffer distance from the aperture edges to be excluded in selecting the
+scattered light pixels to be used.
+.le
+.ls apscat1 = "" (apscatter)
+Fitting parameters across the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat1"
+parameter set.
+.le
+.ls apscat2 = "" (apscatter)
+Fitting parameters along the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat2"
+parameter set.
+.le
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+.ls weights = "none" (apsum)
+Type of extraction weighting.  Note that if the \fIclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+.ls "none"
+The pixels are summed without weights except for partial pixels at the
+ends.
+.le
+.ls "variance"
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \fIgain\fR and \fIreadnoise\fR
+parameters.
+.le
+.le
+.ls pfit = "fit1d" (apsum) (fit1d|fit2d)
+Profile fitting algorithm for cleaning and variance weighted extractions.
+The default is generally appropriate for multifiber data but users
+may try the other algorithm.  See \fBapprofiles\fR for further information.
+.le
+.ls lsigma = 3., usigma = 3. (apsum)
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.le
+.ls nsubaps = 1 (apsum)
+During extraction it is possible to equally divide the apertures into
+this number of subapertures.
+.le
+
+.ce
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --
+.ls f_interactive = yes (fit1d)
+Fit the composite one dimensional flat field spectrum interactively?
+This is used if \fIfitflat\fR is set and a two dimensional flat field
+spectrum is specified.
+.le
+.ls f_function = "spline3", f_order = 10 (fit1d)
+Function and order used to fit the composite one dimensional flat field
+spectrum.  The functions are "legendre", "chebyshev", "spline1", and
+"spline3".  The spline functions are linear and cubic splines with the
+order specifying the number of pieces.
+.le
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+.ls threshold = 10. (autoidentify/identify/reidentify)
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.le
+.ls coordlist = "linelists$idhenear.dat" (autoidentify/identify)
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelists$".
+.le
+.ls match = -3. (autoidentify/identify)
+The maximum difference for a match between the dispersion function prediction
+value and a wavelength in the coordinate list.
+.le
+.ls fwidth = 4. (autoidentify/identify)
+Approximate full base width (in pixels) of arc lines.
+.le
+.ls cradius = 10. (reidentify)
+Radius from previous position to reidentify arc line.
+.le
+.ls i_function = "spline3", i_order = 3 (autoidentify/identify)
+The default function and order to be fit to the arc wavelengths as a
+function of the pixel coordinate.  The functions choices are "chebyshev",
+"legendre", "spline1", or "spline3".
+.le
+.ls i_niterate = 2, i_low = 3.0, i_high = 3.0 (autoidentify/identify)
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.le
+.ls refit = yes (reidentify)
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.le
+.ls addfeatures = no (reidentify)
+Add new features from a line list during each reidentification?
+This option can be used to compensate for lost features from the
+reference solution.  Care should be exercised that misidentified features
+are not introduced.
+.le
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+.ls select = "interp" (refspectra)
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+.ls average
+Average two reference spectra without regard to any sort parameter.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.
+This option is used to assign two reference spectra, with equal weights,
+independent of any sorting parameter.
+.le
+.ls following
+Select the nearest following spectrum in the reference list based on the
+sorting parameter.  If there is no following spectrum use the nearest preceding
+spectrum.
+.le
+.ls interp
+Interpolate between the preceding and following spectra in the reference
+list based on the sorting parameter.  If there is no preceding and following
+spectrum use the nearest spectrum.  The interpolation is weighted by the
+relative distances of the sorting parameter.
+.le
+.ls match
+Match each input spectrum with the reference spectrum list in order.
+This overrides the reference aperture check.
+.le
+.ls nearest
+Select the nearest spectrum in the reference list based on the sorting
+parameter.
+.le
+.ls preceding
+Select the nearest preceding spectrum in the reference list based on the
+sorting parameter.  If there is no preceding spectrum use the nearest following
+spectrum.
+.le
+.le
+.ls sort = "jd", group = "ljd" (refspectra)
+Image header keywords to be used as the sorting parameter for selection
+based on order and to group spectra.
+A null string, "", or the word "none" may be use to disable the sorting
+or grouping parameters.
+The sorting parameter
+must be numeric but otherwise may be anything.  The grouping parameter
+may be a string or number and must simply be the same for all spectra within
+the same group (say a single night).
+Common sorting parameters are times or positions.
+In \fBdofibers\fR the Julian date (JD) and the local Julian day number (LJD)
+at the middle of the exposure are automatically computed from the universal
+time at the beginning of the exposure and the exposure time.  Also the
+parameter UTMIDDLE is computed.
+.le
+.ls time = no, timewrap = 17. (refspectra)
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.le
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+.ls linearize = yes (dispcor)
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling
+If no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data are not interpolated.
+.le
+.ls log = no (dispcor)
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.le
+.ls flux = yes (dispcor)
+Conserve the total flux during interpolation?  If \fIno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \fIyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.le
+
+.ce
+-- SKY SUBTRACTION PARAMETERS --
+.ls combine = "average" (scombine) (average|median)
+Option for combining sky pixels at the same dispersion coordinate after any
+rejection operation.  The options are to compute the  "average" or "median"
+of the pixels.  The median uses the average of the two central
+values when the number of pixels is even.
+.le
+.ls reject = "none" (scombine) (none|minmax|avsigclip)
+Type of rejection operation performed on the pixels which overlap at each
+dispersion coordinate.  The algorithms are discussed in the
+help for \fBscombine\fR.  The rejection choices are:
+
+.nf
+      none - No rejection
+    minmax - Reject the low and high pixels
+ avsigclip - Reject pixels using an averaged sigma clipping algorithm
+.fi
+
+.le
+.ls scale = "none" (none|mode|median|mean)
+Multiplicative scaling to be applied to each spectrum.  The choices are none
+or scale by the mode, median, or mean.  This should not be necessary if the
+flat field and throughput corrections have been properly made. 
+.le
+.ih
+ENVIRONMENT PARAMETERS
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
+.ih
+DESCRIPTION
+The \fBdofibers\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, fiber throughput correction, wavelength calibration, and sky
+subtraction of multifiber spectra.  It is a command language script
+which collects and combines the functions and parameters of many general
+purpose tasks to provide a single complete data reduction path.  The task
+provides a degree of guidance, automation, and record keeping necessary
+when dealing with the large amount of data generated by multifiber
+instruments.  Variants of this task are \fBdoargus\fR, \fBdofoe\fR,
+\fBdohydra\fR, and \fBdo3fiber\fR.
+
+The general organization of the task is to do the interactive setup steps
+first using representative calibration data and then perform the majority
+of the reductions automatically, and possibly as a background process, with
+reference to the setup data.  In addition, the task determines which setup
+and processing operations have been completed in previous executions of the
+task and, contingent on the \fIredo\fR and \fIupdate\fR options, skip or
+repeat some or all the steps.
+
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage Since
+\fBdofibers\fR combines many separate, general purpose tasks the
+description given here refers to these tasks and leaves some of the details
+to their help documentation.
+
+\fBUsage Outline\fR
+
+.ls 6 [1]
+The images are first processed with \fBccdproc\fR for overscan,
+bias, and dark corrections.
+The \fBdofibers\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+.le
+.ls [2]
+Set the \fBdofibers\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed, the flat field image as the aperture reference and
+the flat field, and one or more arc images.  A throughput file or image,
+such as a blank sky observation, may also be specified.  If there are many
+object or arc spectra per setup you might want to prepare "@ files".
+Specify the aperture identification table for the configuration
+if one has been created.  If the image headers contain the SLFIB keywords
+specify an image name; typically the same as the aperture reference
+image.
+You might wish to verify the geometry parameters,
+separations, dispersion direction, etc., which may
+change with different detector setups.  The processing parameters are set
+for complete reductions but for quicklook you might not use the clean
+option or dispersion calibration and sky subtraction.
+
+The parameters are set for a particular configuration and different
+configurations may use different flat fields, arcs, and aperture
+identification tables.
+.le
+.ls [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the execution and no further queries of that
+type will be made.
+.le
+.ls [4]
+The apertures are defined using the specified aperture reference image.
+The spectra are found automatically and apertures assigned based on
+task parameters and the aperture identification table.  Unassigned
+fibers may have a negative beam number and will be ignored in subsequent
+processing.  The resize option sets the aperture size to the widths of
+the profiles at a fixed fraction of the peak height.  The interactive
+review of the apertures is recommended.  If the identifications are off
+by a shift the 'o' key is used.  To exit the aperture review type 'q'.
+.le
+.ls [5]
+The fiber positions at a series of points along the dispersion are measured
+and a function is fit to these positions.  This may be done interactively to
+adjust the fitting parameters.  Not all fibers need be examined and the "NO"
+response will quit the interactive fitting.  To exit the interactive
+fitting type 'q'.
+.le
+.ls [6]
+If scattered light subtraction is to be done the flat field image is
+used to define the scattered light fitting parameters interactively.
+If one is not specified then the aperture reference image is used for
+this purpose.
+
+There are two queries for the interactive fitting.  A graph of the
+data between the defined reference apertures separated by a specified
+buffer distance is first shown.  The function order and type may be
+adjusted.  After quiting with 'q' the user has the option of changing
+the buffer value and returning to the fitting, changing the image line
+or column to check if the fit parameters are satisfactory at other points,
+or to quit and accept the fit parameters.  After fitting all points
+across the dispersion another graph showing the scattered light from
+the individual fits is shown and the smoothing parameters along the
+dispersion may be adjusted.  Upon quiting with 'q' you have the option
+of checking other cuts parallel to the dispersion or quiting and finishing
+the scattered light function smoothing and subtraction.
+
+If there is a throughput image then this is corrected for scattered light
+noninteractively using the previous fitting parameters.
+.le
+.ls [7]
+If flat fielding is to be done the flat field spectra are extracted.  The
+average spectrum over all fibers is determined and a function is fit
+interactively (exit with 'q').  This function is generally of sufficiently
+high order that the overall shape is well fit.  This function is then used
+to normalize the individual flat field spectra.  If a throughput image, a
+sky flat, is specified then the total sky counts through each fiber are
+used to correct the total flat field counts.  Alternatively, a separately
+derived throughput file can be used for specifying throughput corrections.
+If neither type of throughput is used the flat field also provides the
+throughput correction.  The final response spectra are normalized to a unit
+mean over all fibers.  The relative average throughput for each fiber is
+recorded in the log and possibly printed to the terminal.
+.le
+.ls [8]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  The middle fiber is used to identify the arc lines and define
+the dispersion function using the task \fBautoidentify\fR.  The
+\fIcrval\fR and \fIcdelt\fR parameters are used in the automatic
+identification.  Whether or not the automatic identification is
+successful you will be shown the result of the arc line identification.
+If the automatic identification is not successful identify a few arc
+lines with 'm' and use the 'l' line list identification command to
+automatically add additional lines and fit the dispersion function.  Check
+the quality of the dispersion function fit with 'f'.  When satisfied exit
+with 'q'.
+.le
+.ls [9]
+The remaining fibers are automatically reidentified.  You have the option
+to review the line identifications and dispersion function for each fiber
+and interactively add or delete arc lines and change fitting parameters.
+This can be done selectively, such as when the reported RMS increases
+significantly.
+.le
+.ls [10]
+If the spectra are to be resampled to a linear dispersion system
+(which will be the same for all spectra) default dispersion parameters
+are printed and you are allowed to adjust these as desired.
+.le
+.ls [11]
+If the sky line alignment option is selected and the sky lines have not
+been identified for a particular aperture identification table then you are
+asked to mark one or more sky lines.  You may simply accept the wavelengths
+of these lines as defined by the dispersion solution for this spectrum and
+fiber or you may specify knowns wavelengths for the lines. These lines will
+be reidentified in all object spectra extracted and a mean zeropoint shift
+will be added to the dispersion solution.  This has the effect of aligning
+these lines to optimize sky subtraction.
+.le
+.ls [12]
+The object spectra are now automatically scattered light subtracted,
+ extracted, flat fielded, and dispersion corrected.
+.le
+.ls [13]
+When sky subtracting, the individual sky spectra may be reviewed and some
+spectra eliminated using the 'd' key.  The last deleted spectrum may be
+recovered with the 'e' key.  After exiting the review with 'q' you are
+asked for the combining option.  The type of combining is dictated by the
+number of sky fibers.
+.le
+.ls [14]
+The option to examine the final spectra with \fBsplot\fR may be given.
+To exit type 'q'.
+.le
+.ls [15]
+If scattered light is subtracted from the input data a copy of the
+original image is made by appending "noscat" to the image name.
+If the data are reprocessed with the \fIredo\fR flag the original
+image will be used again to allow modification of the scattered
+light parameters.
+
+The final spectra will have the same name as the original 2D images
+with a ".ms" extension added.  The flat field and arc spectra will
+also have part of the aperture identification table name added to
+allow different configurations to use the same 2D flat field and arcs
+but with different aperture definitions.  If using the sky alignment
+option an image "align" with the aperture identification table name
+applied will also be created.
+.le
+
+\fBSpectra and Data Files\fR
+
+The basic input consists of multifiber object and
+calibration spectra stored as IRAF images.
+The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+The raw CCD images must
+be processed to remove overscan, bias, and dark count effects.  This
+is generally done using the \fBccdred\fR package.
+The \fBdofibers\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+Flat fielding is
+generally not done at this stage but as part of \fBdofibers\fR.
+If flat fielding is done as part of the basic CCD processing then
+a flattened flat field, blank sky observation, or throughput file
+should still be created for applying fiber throughput corrections.
+
+The task \fBdofibers\fR uses several types of calibration spectra.  These
+are flat fields, blank sky flat fields, comparison lamp spectra, auxiliary
+mercury line (from the dome lights) or sky line spectra, and simultaneous
+arc spectra taken during the object observation.  The flat field,
+throughput image or file, auxiliary emission line spectra, and simultaneous
+comparison fibers are optional.  If a flat field is used then the sky flat
+or throughput file is optional assuming the flat field has the same fiber
+iillumination.  It is legal to specify only a throughput image or file and
+leave the flat field blank in order to simply apply a throughput
+correction.  Because only the total counts through each fiber are used from
+a throughput image, sky flat exposures need not be of high signal per
+pixel.
+
+There are three types of arc calibration methods.  One is to take arc
+calibration exposures through all fibers periodically and apply the
+dispersion function derived from one or interpolated between pairs to the
+object fibers.  This is the most common method.  Another method is to
+use only one or two all-fiber arcs to define the shape of the dispersion
+function and track zero point wavelength shifts with \fIsimultaneous arc\fR
+fibers taken during the object exposure.  The simultaneous arcs may or may
+not be available at the instrument but \fBdofibers\fR can use this type of
+observation.  The arc fibers are identified by their beam or aperture
+numbers.  A related and mutually exclusive method is to use \fIauxiliary
+line spectra\fR such as lines in the dome lights or sky lines to monitor
+shifts relative to a few actual arc exposures.  The main reason to do this
+is if taking arc exposures through all fibers is inconvenient.
+
+The assignment of arc or auxiliary line calibration exposures to object
+exposures is generally done by selecting the nearest in time and
+interpolating.  There are other options possible which are described under
+the task \fBrefspectra\fR.  The most general option is to define a table
+giving the object image name and the one or two arc spectra to be assigned
+to that object.  That file is called an \fIarc assignment table\fR and it
+is one of the optional setup files which can used with \fBdofibers\fR.
+
+The first step in the processing is identifying the spectra in the images.
+The \fIaperture identification table\fR contains information about the fiber
+assignments.  The identification table is not mandatory, sequential numbering
+will be used, but it is highly recommended for keeping track of the objects
+assigned to the fibers.  The aperture identification table may be
+a file containing lines
+specifying an aperture number, a beam number, and an object
+identification.  It may also be an image whose header contains the keywords
+SLFIB with strings consisting of an aperture number, beam number, optional
+right ascension and declination, and a tile.  The file lines or keywords
+must be in the same order as the fibers in the
+image.  The aperture number may be any unique number but it is recommended
+that the fiber number be used.  The beam number is used to flag object,
+sky, arc, or other types of spectra.  The default beam numbers used by the
+task are 0 for sky, 1 for object, and 2 for arc.  The object
+identifications are optional but it is good practice to include them so
+that the data will contain the object information independent of other
+records.  Figure 1 shows an example identification file called M33Sch2.
+.nf
+
+    Figure 1: Example Aperture Identification File
+
+    cl> type m33sch2
+    1 1 143
+    2 1 254
+    3 0 sky
+    4 -1 Broken
+    5 2 arc
+       .
+       .
+       .
+    44 1 s92
+    45 -1 Unassigned
+    46 2 arc
+    47 0 sky
+    48 1 phil2
+
+.fi
+Note the identification of the sky fibers with beam number 0, the object
+fibers with 1, and the arc fibers with 2.
+The broken and unassigned fiber entries, given beam
+number -1, are optional but recommended to give the automatic spectrum
+finding operation the best chance to make the correct identifications.  The
+identification table will vary for each plugboard setup.  Additional
+information about the aperture identification table may be found in the
+description of the task \fBapfind\fR.
+
+An alternative to using an aperture identification table is to give no
+name, the "" empty string, and to explicitly give a range of
+aperture numbers for the skys and possibly for the sky subtraction
+object list in the parameters \fIobjaps, skyaps, arcaps, objbeams,
+skybeams,\fR and \fIarcbeams\fR.  This is reasonable if the fibers always
+have a fixed typed.  As an example the CTIO Argus instrument always
+alternates object and sky fibers so the object apertures can be given
+as 1x2 and the sky fibers as 2x2; i.e. objects are the odd numbered
+apertures and skys are the even numbered apertures.
+
+The final reduced spectra are recorded in two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ms" extension.  Each line in the reduced image is a one dimensional
+spectrum with associated aperture, wavelength, and identification
+information.  When the \fIextras\fR parameter is set the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tools such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.  The special task \fBscopy\fR may be used to extract
+specific apertures or to change format to individual one dimensional
+images.
+
+\fBPackage Parameters\fR
+
+The \fBspecred\fR package parameters set parameters affecting all the
+tasks in the package.
+The dispersion axis parameter defines the image axis along which the
+dispersion runs.  This is used if the image header doesn't define the
+dispersion axis with the DISPAXIS keyword.
+The observatory parameter is used if there is no
+OBSERVAT keyword in the image header (see \fBobservatory\fR for more
+details).  The spectrum interpolation type might be changed to "sinc" but
+with the cautions given in \fBonedspec.package\fR.
+The other parameters define the standard I/O functions.
+The verbose parameter selects whether to print everything which goes
+into the log file on the terminal.  It is useful for monitoring
+what the \fBdofibers\fR task does.  The log and plot files are useful for
+keeping a record of the processing.  A log file is highly recommended.
+A plot file provides a record of apertures, traces, and extracted spectra
+but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+
+\fBProcessing Parameters\fR
+
+The list of objects and arcs can be @ files if desired.  The aperture
+reference spectrum is usually the same as the flat field spectrum though it
+could be any exposure with enough signal to accurately define the positions
+and trace the spectra.  The first list of arcs are the standard Th-Ar or
+HeNeAr comparison arc spectra (they must all be of the same type).  The
+second list of arcs are the auxiliary emission line exposures mentioned
+previously.
+
+The detector read out noise and gain are used for cleaning and variance
+(optimal) extraction.  This is specified either explicitly or by reference
+to an image header keyword.
+The dispersion axis defines the wavelength direction of spectra in
+the image if not defined in the image header by the keyword DISPAXIS.  The
+width and separation parameters define the dimensions (in pixels) of the
+spectra (fiber profile) across the dispersion.  The width parameter
+primarily affects the centering.  The maximum separation parameter is
+important if missing spectra from the aperture identification table are to
+be correctly skipped.  The number of fibers is either the actual number
+of fibers or the number in the aperture identification table.  An attempt
+is made to account for unassigned or missing fibers.  As a recommendation
+the actual number of fibers should be specified.
+
+The approximate central wavelength and dispersion are used for the
+automatic identification of the arc reference.  They may be specified
+as image header keywords or values.  The INDEF values search the
+entire range of the coordinate reference file but the automatic
+line identification algorithm works much better and faster if
+approximate values are given.
+
+The task needs to know which fibers are object, sky if sky subtraction is
+to be done, and simultaneous arcs if used.  One could explicitly give the
+aperture numbers but the recommended way, provided an aperture
+identification table is used, is to select the apertures based on the beam
+numbers.  The default values are recommended beam numbers.  Sky
+subtracted sky spectra are useful for evaluating the sky subtraction.
+Since only the spectra identified as objects are sky subtracted one can
+exclude fibers from the sky subtraction.  For example, if the
+\fIobjbeams\fR parameter is set to 1 then only those fibers with a beam of
+1 will be sky subtracted.  All other fibers will remain in the extracted
+spectra but will not be sky subtracted.
+
+The next set of parameters select the processing steps and options.  The
+scattered light option allows fitting and subtracting a scattered light
+surface from the input object and flat field.  If there is significant
+scattered light which is not subtracted the fiber throughput correction
+will not be accurate.  The
+flat fitting option allows fitting and removing the overall shape of the
+flat field spectra while preserving the pixel-to-pixel response
+corrections.  This is useful for maintaining the approximate object count
+levels and not introducing the reciprocal of the flat field spectrum into
+the object spectra.  The \fIclean\fR option invokes a profile fitting and
+deviant point rejection algorithm as well as a variance weighting of points
+in the aperture.  These options require knowing the effective (i.e.
+accounting for any image combining) read out noise and gain.  For a
+discussion of cleaning and variance weighted extraction see
+\fBapvariance\fR and \fBapprofiles\fR.
+
+The dispersion correction option selects whether to extract arc spectra,
+determine a dispersion function, assign them to the object spectra, and,
+possibly, resample the spectra to a linear (or log-linear) wavelength
+scale.  If simultaneous arc fibers are defined there is an option to delete
+them from the final spectra when they are no longer needed.
+
+The sky alignment option allows applying a zeropoint dispersion shift
+to all fibers based on one or more sky lines.  This requires all fibers
+to have the sky lines visible.  When there are sky lines this will
+improve the sky subtraction if there is a systematic error in the
+fiber iillumination between the sky and the arc calibration.
+
+The sky subtraction option selects whether to combine the sky fiber spectra
+and subtract this sky from the object fiber spectra.  \fIDispersion
+correction and sky subtraction are independent operations.\fR  This means
+that if dispersion correction is not done then the sky subtraction will be
+done with respect to pixel coordinates.  This might be desirable in some
+quick look cases though it is incorrect for final reductions.
+
+The sky subtraction option has two additional options.  The individual sky
+spectra may be examined and contaminated spectra deleted interactively
+before combining.  This can be a useful feature in crowded regions.  The
+final combined sky spectrum may be saved for later inspection in an image
+with the spectrum name prefixed by \fBsky\fR.
+
+After a spectrum has been processed it is possible to examine the results
+interactively using the \fBsplot\fR tasks.  This option has a query which
+may be turned off with "YES" or "NO" if there are multiple spectra to be
+processed.
+
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\fIupdate\fR flag is set.  The changes which will cause an update are a new
+aperture identification table, a new reference image, new flat fields, and a
+new arc reference.  If all input spectra are to be processed regardless of
+previous processing the \fIredo\fR flag may be used.  Note that
+reprocessing clobbers the previously processed output spectra.
+
+The \fIbatch\fR processing option allows object spectra to be processed as
+a background or batch job.  This will only occur if sky spectra editing and
+\fBsplot\fR review (interactive operations) are turned off, either when the
+task is run or by responding with "NO" to the queries during processing.
+
+The \fIlistonly\fR option prints a summary of the processing steps which
+will be performed on the input spectra without actually doing anything.
+This is useful for verifying which spectra will be affected if the input
+list contains previously processed spectra.  The listing does not include
+any arc spectra which may be extracted to dispersion calibrate an object
+spectrum.
+
+The last parameter (excluding the task mode parameter) points to another
+parameter set for the algorithm parameters.  The way \fBdofibers\fR works
+this may not have any value and the parameter set \fBparams\fR is always
+used.  The algorithm parameters are discussed further in the next section.
+
+\fBAlgorithms and Algorithm Parameters\fR
+
+This section summarizes the various algorithms used by the \fBdofibers\fR
+task and the parameters which control and modify the algorithms.  The
+algorithm parameters available to the user are collected in the parameter
+set \fBparams\fR.  These parameters are taken from the various general
+purpose tasks used by the \fBdofibers\fR processing task.  Additional
+information about these parameters and algorithms may be found in the help
+for the actual task executed.  These tasks are identified in the parameter
+section listing in parenthesis.  The aim of this parameter set organization
+is to collect all the algorithm parameters in one place separate from the
+processing parameters and include only those which are relevant for
+multifiber data.  The parameter values can be changed from the
+defaults by using the parameter editor,
+.nf
+
+	cl> epar params
+
+.fi
+or simple typing \fIparams\fR.  The parameter editor can also be
+entered when editing the \fBdofibers\fR parameters by typing \fI:e
+params\fR or simply \fI:e\fR if positioned at the \fIparams\fR
+parameter.
+
+\fBExtraction\fR
+
+The identification of the spectra in the two dimensional images and their
+scattered light subtraction and extraction to one dimensional spectra
+in multispec format is accomplished
+using the tasks from the \fBapextract\fR package.  The first parameters
+through \fInsubaps\fR control the extractions.
+
+The dispersion line is that used for finding the spectra, for plotting in
+the aperture editor, and as the starting point for tracing.  The default
+value of \fBINDEF\fR selects the middle of the image.  The aperture
+finding, adjusting, editing, and tracing operations also allow summing a
+number of dispersion lines to improve the signal.  The number of lines is
+set by the \fInsum\fR parameter.
+
+The order parameter defines whether the order of the aperture
+identifications in the aperture identification table (or the default
+sequential numbers if no table is used) is in the same sense as the image
+coordinates (increasing) or the opposite sense (decreasing).  If the
+aperture identifications turn out to be opposite to what is desired when
+viewed in the aperture editing graph then simply change this parameter.
+
+The basic data output by the spectral extraction routines are the one
+dimensional spectra.  Additional information may be output when the
+\fIextras\fR option is selected and the cleaning or variance weighting
+options are also selected.  In this case a three dimensional image is
+produced with the first element of the third dimension being the cleaned
+and/or weighted spectra, the second element being the uncleaned and
+unweighted spectra, and the third element being an estimate of the sigma
+of each pixel in the extracted spectrum.  Currently the sigma data is not
+used by any other tasks and is only for reference.
+
+The initial step of finding the fiber spectra in the aperture reference
+image consists of identifying the peaks in a cut across the dispersion,
+eliminating those which are closer to each other than the \fIminsep\fR
+distance, and then keeping the specified \fInfibers\fR highest peaks.  The
+centers of the profiles are determined using the \fBcenter1d\fR algorithm
+which uses the \fIwidth\fR parameter.
+
+Apertures are then assigned to each spectrum.  The initial edges of the
+aperture relative to the center are defined by the \fIlower\fR and
+\fIupper\fR parameters.  The trickiest part of assigning the apertures is
+relating the aperture identification from the aperture identification table
+to automatically selected fiber profiles.  The first aperture id in the
+file is assigned to the first spectrum found using the \fIorder\fR parameter to
+select the assignment direction.  The numbering proceeds in this way except
+that if a gap greater than a multiple of the \fImaxsep\fR parameter is
+encountered then assignments in the file are skipped under the assumption
+that a fiber is missing (broken).  If unassigned fibers are still
+visible in a flat field, either by design or by scattered light, the
+unassigned fibers can be included in the number of fibers to find and
+then the unassigned (negative beam number) apertures are excluded from
+any extraction.  For more on the finding and
+assignment algorithms see \fBapfind\fR.
+
+The initial apertures are the same for all spectra but they can each be
+automatically resized.  The automatic resizing sets the aperture limits
+at a fraction of the peak relative to the interfiber minimum.
+The default \fIylevel\fR is to resize the apertures to 5% of the peak.
+See the description for the task \fBapresize\fR for further details.
+
+The user is given the opportunity to graphically review and adjust the
+aperture definitions.  This is recommended.  As mentioned previously, the
+correct identification of the fibers is tricky and it is fundamentally
+important that this be done correctly; otherwise the spectrum
+identifications will not be for the objects they say.  An important command in
+this regard is the 'o' key which allows reordering the identifications
+based on the aperture identification table.  This is required if the first
+fiber is actually missing since the initial assignment begins assigning the
+first spectrum found with the first entry in the aperture file.  The
+aperture editor is a very powerful tool and is described in detail as
+\fBapedit\fR.
+
+The next set of parameters control the tracing and function fitting of the
+aperture reference positions along the dispersion direction.  The position
+of a spectrum across the dispersion is determined by the centering
+algorithm (see \fBcenter1d\fR) at a series of evenly spaced steps, given by
+the parameter \fIt_step\fR, along the dispersion.  The step size should be
+fine enough to follow position changes but it is not necessary to measure
+every point.  The fitted points may jump around a little bit due to noise
+and cosmic rays even when summing a number of lines.  Thus, a smooth
+function is fit.  The function type, order, and iterative rejection of
+deviant points is controlled by the other trace parameters.  For more
+discussion consult the help pages for \fBaptrace\fR and \fBicfit\fR.  The
+default is to fit a cubic spline of three pieces with a single iteration of
+3 sigma rejection.
+
+The actual extraction of the spectra by summing across the aperture at each
+point along the dispersion is controlled by the next set of parameters.
+The default extraction simply sums the pixels using partial pixels at the
+ends.  The options allow selection of a weighted sum based on a Poisson
+variance model using the \fIreadnoise\fR and \fIgain\fR detector
+parameters.  Note that if the \fIclean\fR option is selected the variance
+weighted extraction is used regardless of the \fIweights\fR parameter.  The
+sigma thresholds for cleaning are also set in the \fBparams\fR parameters.
+For more on the variance weighted extraction and cleaning see
+\fBapvariance\fR and \fBapprofiles\fR as well as \fBapsum\fR.
+
+The last parameter, \fInsubaps\fR, is used only in special cases when it is
+desired to subdivide the fiber profiles into subapertures prior to
+dispersion correction.  After dispersion correction the subapertures are
+then added together.  The purpose of this is to correct for wavelength
+shifts across a fiber.
+
+\fBScattered Light Subtraction\fR
+
+Scattered light may be subtracted from the input two dimensional image as
+the first step.  This is done using the algorithm described in
+\fBapscatter\fR.  This can be important if there is significant scattered
+light since the flat field/throughput correction will otherwise be
+incorrect.  The algorithm consists of fitting a function to the data
+outside the defined apertures by a specified \fIbuffer\fR at each line or
+column across the dispersion.  The function fitting parameters are the same
+at each line.  Because the fitted functions are independent at each line or
+column a second set of one dimensional functions are fit parallel to the
+dispersion using the evaluated fit values from the cross-dispersion step.
+This produces a smooth scattered light surface which is finally subtracted
+from the input image.  Again the function fitting parameters are the
+same at each line or column though they may be different than the parameters
+used to fit across the dispersion.
+
+The first time the task is run with a particular flat field (or aperture
+reference image if no flat field is used) the scattered light fitting
+parameters are set interactively using that image.  The interactive step
+selects a particular line or column upon which the fitting is done
+interactively with the \fBicfit\fR commands.  A query is first issued
+which allows skipping this interactive stage.  Note that the interactive
+fitting is only for defining the fitting functions and orders.  When
+the graphical \fBicfit\fR fitting is exited (with 'q') there is a second prompt
+allowing you to change the buffer distance (in the first cross-dispersion
+stage) from the apertures, change the line/column, or finally quit.
+
+The initial fitting parameters and the final set parameters are recorded
+in the \fBapscat1\fR and \fBapscat2\fR hidden parameter sets.  These
+parameters are then used automatically for every subsequent image
+which is scattered light corrected.
+
+The scattered light subtraction modifies the input 2D images.  To preserve
+the original data a copy of the original image is made with the same
+root name and the word "noscat" appended.  The scattered light subtracted
+images will have the header keyword "APSCATTE" which is how the task
+avoids repeating the scattered light subtraction during any reprocessing.
+However if the \fIredo\fR option is selected the scattered light subtraction
+will also be redone by first restoring the "noscat" images to the original
+input names.
+
+\fBFlat Field and Fiber Throughput Corrections\fR
+
+Flat field corrections may be made during the basic CCD processing; i.e.
+direct division by the two dimensional flat field observation.  In that
+case do not specify a flat field spectrum; use the null string "".  The
+\fBdofibers\fR task provides an alternative flat field response correction
+based on division of the extracted object spectra by the extracted flat field
+spectra.  A discussion of the theory and merits of flat fielding directly
+verses using the extracted spectra will not be made here.  The
+\fBdofibers\fR flat fielding algorithm is the \fIrecommended\fR method for
+flat fielding since it works well and is not subject to the many problems
+involved in two dimensional flat fielding.
+
+In addition to correcting for pixel-to-pixel response the flat field step
+also corrects for differences in the fiber throughput.  Thus, even if the
+pixel-to-pixel flat field corrections have been made in some other way it
+is desirable to use a sky or dome flat observation for determining a fiber
+throughput correction.  Alternatively, a separately derived throughput
+file may be specified.  This file consists of the aperture numbers
+(the same as used for the aperture reference) and relative throughput
+numbers.
+
+The first step is extraction of the flat field spectrum, if specified,
+using the reference apertures.  Only one flat field is allowed so if
+multiple flat fields are required the data must be reduced in groups.
+After extraction one or more corrections are applied.  If the \fIfitflat\fR
+option is selected (the default) the extracted flat field spectra are
+averaged together and a smooth function is fit.  The default fitting
+function and order are given by the parameters \fIf_function\fR and
+\fIf_order\fR.  If the parameter \fIf_interactive\fR is "yes" then the
+fitting is done interactively using the \fBfit1d\fR task which uses the
+\fBicfit\fR interactive fitting commands.
+
+The fitted function is divided into the individual flat field spectra to
+remove the basic shape of the spectrum while maintaining the relative
+individual pixel responses and any fiber to fiber differences.  This step
+avoids introducing the flat field spectrum shape into the object spectra
+and closely preserves the object counts.
+
+If a throughput image is available (an observation of blank sky
+usually at twilight) it is extracted.  If no flat field is used the average
+signal through each fiber is computed and this becomes the response
+normalization function.  Note that a dome flat may be used in place of a
+sky in the sky flat field parameter for producing throughput only
+corrections.  If a flat field is specified then each sky spectrum is
+divided by the appropriate flat field spectrum.  The total counts through
+each fiber are multiplied into the flat field spectrum thus making the sky
+throughput of each fiber the same.  This correction is important if the
+iillumination of the fibers differs between the flat field source and the
+sky.  Since only the total counts are required the sky or dome flat field
+spectra need not be particularly strong though care must be taken to avoid
+objects.
+
+Instead of a sky flat or other throughput image a separately derived
+throughput file may be used.  It may be used with or without a
+flat field.
+
+The final step is to normalize the flat field spectra by the mean counts of
+all the fibers.  This normalization step is simply to preserve the average
+counts of the extracted object and arc spectra after division by the
+response spectra.  The final relative throughput values are recorded in the
+log and possibly printed on the terminal.
+
+These flat field response steps and algorithm are available as a separate
+task called \fBmsresp1d\fR.
+
+\fBDispersion Correction\fR
+
+Dispersion corrections are applied to the extracted spectra if the
+\fBdispcor\fR parameter is set.  This can be a complicated process which
+the \fBdofibers\fR task tries to simplify for you.  There are three basic
+steps involved; determining the dispersion functions relating pixel
+position to wavelength, assigning the appropriate dispersion function to a
+particular observation, and resampling the spectra to evenly spaced pixels
+in wavelength.
+
+The comparison arc spectra are used to define dispersion functions for the
+fibers using the tasks \fBautoidentify\fR and \fBreidentify\fR.  The
+interactive \fBautoidentify\fR task is only used on the central fiber of the
+first arc spectrum to define the basic reference dispersion solution from
+which all other fibers and arc spectra are automatically derived using
+\fBreidentify\fR. \fBAutoidentify\fR attempts to automatically identify
+the arc lines using the \fIcrval\fR and \fIcdelt\fR parameters.  Whether
+or not it is successful the user is presented with the interactive
+identification graph.  The automatic identifications can be reviewed and a
+new solution or corrections to the automatic solution may be performed.
+
+The set of arc dispersion function parameters are from \fBautoidentify\fR and
+\fBreidentify\fR.  The parameters define a line list for use in
+automatically assigning wavelengths to arc lines, a parameter controlling
+the width of the centering window (which should match the base line
+widths), the dispersion function type and order, parameters to exclude bad
+lines from function fits, and parameters defining whether to refit the
+dispersion function, as opposed to simply determining a zero point shift,
+and the addition of new lines from the line list when reidentifying
+additional arc spectra.  The defaults should generally be adequate and the
+dispersion function fitting parameters may be altered interactively.  One
+should consult the help for the two tasks for additional details of these
+parameters and the operation of \fBautoidentify\fR.
+
+Generally, taking a number of comparison arc lamp exposures interspersed
+with the program spectra is sufficient to accurately dispersion calibrate
+multifiber spectra.  However, there are some other calibration options
+which may be of interest.  These options apply additional calibration data
+consisting either of auxiliary line spectra, such as from dome lights or
+night sky lines, or simultaneous arc lamp spectra taken through a few
+fibers during the object exposure.  These options add complexity to the
+dispersion calibration process.
+
+When only arc comparison lamp spectra are used, dispersion functions are
+determined independently for each fiber of each arc image and then assigned
+to the matching fibers in the program object observations.  The assignment
+consists of selecting one or two arc images to calibrate each object
+image.  When two bracketing arc spectra are used the dispersion functions
+are linearly interpolated (usually based on the time of the observations).
+
+If taking comparison exposures is time-consuming, possibly requiring
+reconfiguration to illuminate the fibers, and the spectrograph is
+expected to be fairly stable apart from small shifts, there are two
+mutually exclusive methods for monitoring
+shifts in the dispersion zero point from the basic arc lamp spectra other
+than taking many arc lamp exposures.  One is to use some fibers to take a
+simultaneous arc spectrum while observing the program objects.  The fibers
+are identified by aperture or beam numbers.  The second method is to use
+\fIauxiliary line spectra\fR, such as mercury lines from the dome lights.
+These spectra are specified with an auxiliary shift arc list, \fIarc2\fR.
+
+When using auxiliary line spectra for monitoring zero point shifts one of
+these spectra is plotted interactively by \fBidentify\fR with the
+reference dispersion function from the reference arc spectrum.  The user
+marks one or more lines which will be used to compute zero point wavelength
+shifts in the dispersion functions automatically.  The actual wavelengths
+of the lines need not be known.  In this case accept the wavelength based
+on the reference dispersion function.  As other observations of the same
+features are made the changes in the positions of the features will be
+tracked as zero point wavelength changes such that wavelengths of the
+features remain constant.
+
+When using auxiliary line spectra the only arc lamp spectrum used is the
+initial arc reference spectrum (the first image in the \fIarcs1\fR list).
+The master dispersion functions are then shifted based on the spectra in
+the \fIarcs2\fR list (which must all be of the same type).  The dispersion
+function assignments made by \fBrefspectra\fR using either the arc
+assignment file or based on header keywords is done in the same way as
+described for the arc lamp images except using the auxiliary spectra.
+
+If simultaneous arcs are used the arc lines are reidentified to determine a
+zero point shift relative to the comparison lamp spectra selected, by
+\fBrefspectra\fR, of the same fiber.  A linear function of aperture
+position on the image across the dispersion verses the zero point shifts
+from the arc fibers is determined and applied to the dispersion functions
+from the assigned calibration arcs for the non-arc fibers.  Note that if
+there are two comparison lamp spectra (before and after the object
+exposure) then there will be two shifts applied to two dispersion functions
+which are then combined using the weights based on the header parameters
+(usually the observation time).
+
+The arc assignments may be done either explicitly with an arc assignment
+table (parameter \fIarctable\fR) or based on a header parameter.  The task
+used is \fBrefspectra\fR and the user should consult this task if the
+default behavior is not what is desired.  The default is to interpolate
+linearly between the nearest arcs based on the Julian date (corrected to
+the middle of the exposure).  The Julian date and a local Julian day number
+(the day number at local noon) are computed automatically by the task
+\fBsetjd\fR and recorded in the image headers under the keywords JD and
+LJD.  In addition the universal time at the middle of the exposure, keyword
+UTMIDDLE, is computed by the task \fBsetairmass\fR and this may also be used
+for ordering the arc and object observations.
+
+An optional step is to use sky lines in the spectra to compute a zeropoint
+dispersion shift that will align the sky lines.  This may improve sky
+subtraction if the iillumination is not the same between the arc calibration
+and the sky.  When selected the object spectrum is dispersion corrected
+using a non-linear dispersion function to avoid resampling the spectrum.
+The sky lines are then reidentified in wavelength space from a template
+list of sky lines.  The mean shift in the lines for each fiber relative to
+the template in that fiber is computed to give the zeropoint shift.  The
+database file is created when the first object is extracted.  You are asked
+to mark the sky lines in one fiber and then the lines are automatically
+reidentified in all other fibers.  Note that this technique requires the
+sky lines be found in all fibers.
+
+The last step of dispersion correction (resampling the spectrum to evenly
+spaced pixels in wavelength) is optional and relatively straightforward.
+If the \fIlinearize\fR parameter is no then the spectra are not resampled
+and the nonlinear dispersion information is recorded in the image header.
+Other IRAF tasks (the coordinate description is specific to IRAF) will use
+this information whenever wavelengths are needed.  If linearizing is
+selected a linear dispersion relation, either linear in the wavelength or
+the log of the wavelength, is defined once and applied to every extracted
+spectrum.  The resampling algorithm  parameters allow selecting the
+interpolation function type, whether to conserve flux per pixel by
+integrating across the extent of the final pixel, and whether to linearize
+to equal linear or logarithmic intervals.  The latter may be appropriate
+for radial velocity studies.  The default is to use a fifth order
+polynomial for interpolation, to conserve flux, and to not use logarithmic
+wavelength bins.  These parameters are described fully in the help for the
+task \fBdispcor\fR which performs the correction.  The interpolation
+function options and the nonlinear dispersion coordinate system is
+described in the help topic \fBonedspec.package\fR.
+
+\fBSky Subtraction\fR
+
+Sky subtraction is selected with the \fIskysubtract\fR processing option.
+The sky spectra are selected by their aperture and beam numbers and
+combined into a single master sky spectrum
+which is then subtracted from each object spectrum.  If the \fIskyedit\fR
+option is selected the sky spectra are plotted using the task
+\fBspecplot\fR.  By default they are superposed to allow identifying
+spectra with unusually high signal due to object contamination.  To
+eliminate a sky spectrum from consideration point at it with the cursor and
+type 'd'.  The last deleted spectrum may be undeleted with 'e'.  This
+allows recovery of incorrect or accidental deletions.
+
+The sky combining algorithm parameters define how the individual sky fiber
+spectra, after interactive editing, are combined before subtraction from
+the object fibers.  The goals of combining are to reduce noise, eliminate
+cosmic-rays, and eliminate fibers with inadvertent objects.  The common
+methods for doing this to use a median and/or a special sigma clipping
+algorithm (see \fBscombine\fR for details).  The scale
+parameter determines whether the individual skys are first scaled to a
+common mode.  The scaling should be used if the throughput is uncertain,
+but in that case you probably did the wrong thing in the throughput
+correction.  If the sky subtraction is done interactively, i.e. with the
+\fIskyedit\fR option selected, then after selecting the spectra to be
+combined a query is made for the combining algorithm.  This allows
+modifying the default algorithm based on the number of sky spectra
+selected since the "avsigclip" rejection algorithm requires at least
+three spectra.
+
+The combined sky spectrum is subtracted from only those spectra specified
+by the object aperture and beam numbers.  Other spectra, such as comparison
+arc spectra, are retained unchanged.  One may include the sky spectra as
+object spectra to produce residual sky spectra for analysis.  The combined
+master sky spectra may be saved if the \fIsaveskys\fR parameter is set.
+The saved sky is given the name of the object spectrum with the prefix
+"sky".
+.ih
+EXAMPLES
+1.  The following example uses artificial data and may be executed
+at the terminal (with IRAF V2.10).  This is also the sequence performed
+by the test procedure "demos dohydra" from the \fBhydra\fR package..
+
+.nf
+sp> hydra
+hy> demos mkhydra
+Creating image demoobj ...
+Creating image demoflat ...
+Creating image demoarc ...
+hy> bye
+sp> type demoapid
+===> demoapid <===
+36 1
+37 0
+38 1
+39 1
+41 0
+42 1
+43 1
+44 0
+45 1
+46 -1
+47 0
+48 1
+sp> specred.verbose = yes
+sp> dofibers demoobj apref=demoflat flat=demoflat arcs1=demoarc \
+>>> fib=12 apid=demoapid width=4. minsep=5. maxsep=7. clean- splot+
+Set reference apertures for demoflat
+Resize apertures for demoflat?  (yes):
+Edit apertures for demoflat?  (yes):
+<Exit with 'q'>
+Fit curve to aperture 36 of demoflat interactively  (yes):
+<Exit with 'q'>
+Fit curve to aperture 37 of demoflat interactively  (yes): N
+Create response function demoflatdemoad.ms
+Extract flat field demoflat
+Fit and ratio flat field demoflat
+<Exit with 'q'>
+Create the normalized response demoflatdemoad.ms
+demoflatdemoad.ms -> demoflatdemoad.ms  using bzero: 0.
+    and bscale: 1.000001
+    mean: 1.000001  median: 1.052665  mode: 1.273547
+    upper: INDEF  lower: INDEF
+Average fiber response:
+1.  1.151023
+2.  0.4519709
+3.  1.250614
+4.  1.287281
+5.  1.271358
+6.  0.6815334
+7.  1.164336
+8.  0.7499605
+9.  1.008654
+10.  1.053296
+11.  0.929967
+Extract arc reference image demoarc
+Determine dispersion solution for demoarc
+<A solution is found and presented.>
+<Type 'f' to look at fit.  Type 'q' to exit fit.>
+<Exit with 'q'>
+
+REIDENTIFY: NOAO/IRAF V2.10BETA valdes@puppis Tue 16:01:07 11-Feb-92
+  Reference image = d....ms.imh, New image = d....ms, Refit = yes
+     Image Data Found    Fit Pix Shift User Shift  Z Shift     RMS
+d....ms - Ap 41 16/20  16/16   0.00796     0.0682  8.09E-6    3.86
+Fit dispersion function interactively? (no|yes|NO|YES) (NO): y
+<Exit with 'q'>
+d....ms - Ap 41 16/20  16/16   0.00796     0.0682  8.09E-6    3.86
+d....ms - Ap 39 19/20  19/19     0.152        1.3  1.95E-4    3.89
+Fit dispersion function interactively? (no|yes|NO|YES) (yes): N
+d....ms - Ap 39 19/20  19/19     0.152        1.3  1.95E-4    3.89
+d....ms - Ap 38 18/20  18/18     0.082      0.697  9.66E-5    3.64
+d....ms - Ap 37 19/20  19/19    0.0632      0.553  1.09E-4    6.05
+d....ms - Ap 36 18/20  18/18    0.0112     0.0954  1.35E-5    4.12
+d....ms - Ap 43 17/20  17/17    0.0259      0.221  3.00E-5    3.69
+d....ms - Ap 44 19/20  19/19     0.168       1.44  2.22E-4    4.04
+d....ms - Ap 45 20/20  20/20      0.18       1.54  2.35E-4    3.95
+d....ms - Ap 47 18/20  18/18  -2.02E-4    0.00544  9.86E-6     4.4
+d....ms - Ap 48 16/20  16/16   0.00192     0.0183  1.44E-6    3.82
+
+Dispersion correct demoarc
+d....ms.imh: w1 = 5748.07..., w2 = 7924.62..., dw = 8.50..., nw = 257
+  Change wavelength coordinate assignments? (yes|no|NO): n
+Extract object spectrum demoobj
+Assign arc spectra for demoobj
+[demoobj] refspec1='demoarc'
+Dispersion correct demoobj
+demoobj.ms.imh: w1 = 5748.078, w2 = 7924.622, dw = 8.502127, nw = 257
+Sky subtract demoobj:  skybeams=0
+Edit the sky spectra? (yes):
+<Exit with 'q'>
+Sky rejection option (none|minmax|avsigclip) (avsigclip):
+demoobj.ms.imh:
+Splot spectrum? (no|yes|NO|YES) (yes):
+Image line/aperture to plot (1:) (1):
+<Look at spectra and change apertures with # key>
+<Exit with 'q'>
+.fi
+.ih
+REVISIONS
+.ls DOFIBERS V2.11
+A sky alignment option was added.
+
+The aperture identification can now be taken from image header keywords.
+
+The initial arc line identifications is done with the automatic line
+identification algorithm.
+.le
+.ls DOFIBERS V2.10.3
+The usual output WCS format is "equispec".  The image format type to be
+processed is selected with the \fIimtype\fR environment parameter.  The
+dispersion axis parameter is now a package parameter.  Images will only
+be processed if the have the CCDPROC keyword.  A \fIdatamax\fR parameter
+has been added to help improve cosmic ray rejection.  A scattered
+light subtraction processing option has been added.
+.le
+.ih
+SEE ALSO
+apedit, apfind, approfiles, aprecenter, apresize, apsum, aptrace,
+apvariance, ccdred, center1d, doargus, dohydra, dofoe, do3fiber, dispcor,
+fit1d, icfit, identify, msresp1d, observatory, onedspec.package,
+refspectra, reidentify, scombine, setairmass, setjd, specplot, splot
+.endhelp
diff --git a/noao/imred/specred/doc/dofibers.ms b/noao/imred/specred/doc/dofibers.ms
new file mode 100644
index 00000000..c0196563
--- /dev/null
+++ b/noao/imred/specred/doc/dofibers.ms
@@ -0,0 +1,1807 @@
+.nr PS 9
+.nr VS 11
+.de V1
+.ft CW
+.nf
+..
+.de V2
+.fi
+.ft R
+..
+.de LS
+.br
+.in +2
+..
+.de LE
+.br
+.sp .5v
+.in -2
+..
+.ND July 1995
+.TL
+Guide to the Multifiber Reduction Task DOFIBERS
+.AU
+Francisco Valdes
+.AI
+IRAF Group - Central Computer Services
+.K2
+.DY
+
+.AB
+The \fBdofibers\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, fiber throughput correction, wavelength calibration, and sky
+subtraction of multifiber spectra.  It is a
+command language script which collects and combines the functions and
+parameters of many general purpose tasks to provide a single complete data
+reduction path.  The task provides a degree of guidance, automation, and
+record keeping necessary when dealing with the large amount of data
+generated by multifiber instruments.  Variants of this task are
+\fBdoargus\fR, \fBdofoe\fR, \fBdohydra\fR, and \fBdo3fiber\fR.
+.AE
+.NH
+Introduction
+.LP
+The \fBdofibers\fR reduction task is specialized for scattered light
+subtraction, extraction, flat
+fielding, fiber throughput correction, wavelength calibration, and sky
+subtraction of multifiber spectra.  It is a command language script
+which collects and combines the functions and parameters of many general
+purpose tasks to provide a single complete data reduction path.  The task
+provides a degree of guidance, automation, and record keeping necessary
+when dealing with the large amount of data generated by multifiber
+instruments.  Variants of this task are \fBdoargus\fR, \fBdofoe\fR,
+\fBdohydra\fR, and \fBdo3fiber\fR.
+.LP
+The general organization of the task is to do the interactive setup steps
+first using representative calibration data and then perform the majority
+of the reductions automatically, and possibly as a background process, with
+reference to the setup data.  In addition, the task determines which setup
+and processing operations have been completed in previous executions of the
+task and, contingent on the \f(CWredo\fR and \f(CWupdate\fR options, skip or
+repeat some or all the steps.
+.LP
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage Since
+\fBdofibers\fR combines many separate, general purpose tasks the
+description given here refers to these tasks and leaves some of the details
+to their help documentation.
+.NH
+Usage Outline
+.LP
+.IP [1] 6
+The images are first processed with \fBccdproc\fR for overscan,
+bias, and dark corrections.
+The \fBdofibers\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+.IP [2]
+Set the \fBdofibers\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed, the flat field image as the aperture reference and
+the flat field, and one or more arc images.  A throughput file or image,
+such as a blank sky observation, may also be specified.  If there are many
+object or arc spectra per setup you might want to prepare "@ files".
+Specify the aperture identification table for the configuration
+if one has been created.  If the image headers contain the SLFIB keywords
+specify an image name; typically the same as the aperture reference
+image.
+You might wish to verify the geometry parameters,
+separations, dispersion direction, etc., which may
+change with different detector setups.  The processing parameters are set
+for complete reductions but for quicklook you might not use the clean
+option or dispersion calibration and sky subtraction.
+
+The parameters are set for a particular configuration and different
+configurations may use different flat fields, arcs, and aperture
+identification tables.
+.IP [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the execution and no further queries of that
+type will be made.
+.IP [4]
+The apertures are defined using the specified aperture reference image.
+The spectra are found automatically and apertures assigned based on
+task parameters and the aperture identification table.  Unassigned
+fibers may have a negative beam number and will be ignored in subsequent
+processing.  The resize option sets the aperture size to the widths of
+the profiles at a fixed fraction of the peak height.  The interactive
+review of the apertures is recommended.  If the identifications are off
+by a shift the 'o' key is used.  To exit the aperture review type 'q'.
+.IP [5]
+The fiber positions at a series of points along the dispersion are measured
+and a function is fit to these positions.  This may be done interactively to
+adjust the fitting parameters.  Not all fibers need be examined and the "NO"
+response will quit the interactive fitting.  To exit the interactive
+fitting type 'q'.
+.IP [6]
+If scattered light subtraction is to be done the flat field image is
+used to define the scattered light fitting parameters interactively.
+If one is not specified then the aperture reference image is used for
+this purpose.
+
+There are two queries for the interactive fitting.  A graph of the
+data between the defined reference apertures separated by a specified
+buffer distance is first shown.  The function order and type may be
+adjusted.  After quiting with 'q' the user has the option of changing
+the buffer value and returning to the fitting, changing the image line
+or column to check if the fit parameters are satisfactory at other points,
+or to quit and accept the fit parameters.  After fitting all points
+across the dispersion another graph showing the scattered light from
+the individual fits is shown and the smoothing parameters along the
+dispersion may be adjusted.  Upon quiting with 'q' you have the option
+of checking other cuts parallel to the dispersion or quiting and finishing
+the scattered light function smoothing and subtraction.
+
+If there is a throughput image then this is corrected for scattered light
+noninteractively using the previous fitting parameters.
+.IP [7]
+If flat fielding is to be done the flat field spectra are extracted.  The
+average spectrum over all fibers is determined and a function is fit
+interactively (exit with 'q').  This function is generally of sufficiently
+high order that the overall shape is well fit.  This function is then used
+to normalize the individual flat field spectra.  If a throughput image, a
+sky flat, is specified then the total sky counts through each fiber are
+used to correct the total flat field counts.  Alternatively, a separately
+derived throughput file can be used for specifying throughput corrections.
+If neither type of throughput is used the flat field also provides the
+throughput correction.  The final response spectra are normalized to a unit
+mean over all fibers.  The relative average throughput for each fiber is
+recorded in the log and possibly printed to the terminal.
+.IP [8]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  The middle fiber is used to identify the arc lines and define
+the dispersion function using the task \fBautoidentify\fR.  The
+\fIcrval\fR and \fIcdelt\fR parameters are used in the automatic
+identification.  Whether or not the automatic identification is
+successful you will be shown the result of the arc line identification.
+If the automatic identification is not successful identify a few arc
+lines with 'm' and use the 'l' line list identification command to
+automatically add additional lines and fit the dispersion function.  Check
+the quality of the dispersion function fit with 'f'.  When satisfied exit
+with 'q'.
+.IP [9]
+The remaining fibers are automatically reidentified.  You have the option
+to review the line identifications and dispersion function for each fiber
+and interactively add or delete arc lines and change fitting parameters.
+This can be done selectively, such as when the reported RMS increases
+significantly.
+.IP [10]
+If the spectra are to be resampled to a linear dispersion system
+(which will be the same for all spectra) default dispersion parameters
+are printed and you are allowed to adjust these as desired.
+.IP [11]
+If the sky line alignment option is selected and the sky lines have not
+been identified for a particular aperture identification table then you are
+asked to mark one or more sky lines.  You may simply accept the wavelengths
+of these lines as defined by the dispersion solution for this spectrum and
+fiber or you may specify knowns wavelengths for the lines. These lines will
+be reidentified in all object spectra extracted and a mean zeropoint shift
+will be added to the dispersion solution.  This has the effect of aligning
+these lines to optimize sky subtraction.
+.IP [12]
+The object spectra are now automatically scattered light subtracted,
+ extracted, flat fielded, and dispersion corrected.
+.IP [13]
+When sky subtracting, the individual sky spectra may be reviewed and some
+spectra eliminated using the 'd' key.  The last deleted spectrum may be
+recovered with the 'e' key.  After exiting the review with 'q' you are
+asked for the combining option.  The type of combining is dictated by the
+number of sky fibers.
+.IP [14]
+The option to examine the final spectra with \fBsplot\fR may be given.
+To exit type 'q'.
+.IP [15]
+If scattered light is subtracted from the input data a copy of the
+original image is made by appending "noscat" to the image name.
+If the data are reprocessed with the \fIredo\fR flag the original
+image will be used again to allow modification of the scattered
+light parameters.
+
+The final spectra will have the same name as the original 2D images
+with a ".ms" extension added.  The flat field and arc spectra will
+also have part of the aperture identification table name added to
+allow different configurations to use the same 2D flat field and arcs
+but with different aperture definitions.  If using the sky alignment
+option an image "align" with the aperture identification table name
+applied will also be created.
+.NH
+Spectra and Data Files
+.LP
+The basic input consists of multifiber object and
+calibration spectra stored as IRAF images.
+The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+The raw CCD images must
+be processed to remove overscan, bias, and dark count effects.  This
+is generally done using the \fBccdred\fR package.
+The \fBdofibers\fR task will abort if the image header keyword CCDPROC,
+which is added by \fBccdproc\fR, is missing.  If the data processed outside
+of the IRAF \fBccdred\fR package then a dummy CCDPROC keyword should be
+added to the image headers; say with \fBhedit\fR.
+Flat fielding is
+generally not done at this stage but as part of \fBdofibers\fR.
+If flat fielding is done as part of the basic CCD processing then
+a flattened flat field, blank sky observation, or throughput file
+should still be created for applying fiber throughput corrections.
+.LP
+The task \fBdofibers\fR uses several types of calibration spectra.  These
+are flat fields, blank sky flat fields, comparison lamp spectra, auxiliary
+mercury line (from the dome lights) or sky line spectra, and simultaneous
+arc spectra taken during the object observation.  The flat field,
+throughput image or file, auxiliary emission line spectra, and simultaneous
+comparison fibers are optional.  If a flat field is used then the sky flat
+or throughput file is optional assuming the flat field has the same fiber
+illumination.  It is legal to specify only a throughput image or file and
+leave the flat field blank in order to simply apply a throughput
+correction.  Because only the total counts through each fiber are used from
+a throughput image, sky flat exposures need not be of high signal per
+pixel.
+.LP
+There are three types of arc calibration methods.  One is to take arc
+calibration exposures through all fibers periodically and apply the
+dispersion function derived from one or interpolated between pairs to the
+object fibers.  This is the most common method.  Another method is to
+use only one or two all-fiber arcs to define the shape of the dispersion
+function and track zero point wavelength shifts with \fIsimultaneous arc\fR
+fibers taken during the object exposure.  The simultaneous arcs may or may
+not be available at the instrument but \fBdofibers\fR can use this type of
+observation.  The arc fibers are identified by their beam or aperture
+numbers.  A related and mutually exclusive method is to use \fIauxiliary
+line spectra\fR such as lines in the dome lights or sky lines to monitor
+shifts relative to a few actual arc exposures.  The main reason to do this
+is if taking arc exposures through all fibers is inconvenient.
+.LP
+The assignment of arc or auxiliary line calibration exposures to object
+exposures is generally done by selecting the nearest in time and
+interpolating.  There are other options possible which are described under
+the task \fBrefspectra\fR.  The most general option is to define a table
+giving the object image name and the one or two arc spectra to be assigned
+to that object.  That file is called an \fIarc assignment table\fR and it
+is one of the optional setup files which can used with \fBdofibers\fR.
+.LP
+The first step in the processing is identifying the spectra in the images.
+The \fIaperture identification table\fR contains information about the fiber
+assignments.  The identification table is not mandatory, sequential numbering
+will be used, but it is highly recommended for keeping track of the objects
+assigned to the fibers.  The aperture identification table may be
+a file containing lines
+specifying an aperture number, a beam number, and an object
+identification.  It may also be an image whose header contains the keywords
+SLFIB with strings consisting of an aperture number, beam number, optional
+right ascension and declination, and a tile.  The file lines or keywords
+must be in the same order as the fibers in the
+image.  The aperture number may be any unique number but it is recommended
+that the fiber number be used.  The beam number is used to flag object,
+sky, arc, or other types of spectra.  The default beam numbers used by the
+task are 0 for sky, 1 for object, and 2 for arc.  The object
+identifications are optional but it is good practice to include them so
+that the data will contain the object information independent of other
+records.  Figure 1 shows an example aperture identification file
+called M33Sch2.
+.V1
+
+.ce
+Figure 1: Example Aperture Identification File
+
+    cl> type m33sch2
+    1 1 143
+    2 1 254
+    3 0 sky
+    4 -1 Broken
+    5 2 arc
+       .
+       .
+       .
+    44 1 s92
+    45 -1 Unassigned
+    46 2 arc
+    47 0 sky
+    48 1 phil2
+
+.V2
+Note the identification of the sky fibers with beam number 0, the object
+fibers with 1, and the arc fibers with 2.
+The broken and unassigned fiber entries, given beam
+number -1, are optional but recommended to give the automatic spectrum
+finding operation the best chance to make the correct identifications.  The
+identification table will vary for each plugboard setup.  Additional
+information about the aperture identification table may be found in the
+description of the task \fBapfind\fR.
+.LP
+An alternative to using an aperture identification table is to give no
+name, the "" empty string, and to explicitly give a range of
+aperture numbers for the skys and possibly for the sky subtraction
+object list in the parameters \f(CWobjaps, skyaps, arcaps, objbeams,
+skybeams,\fR and \f(CWarcbeams\fR.  This is reasonable if the fibers always
+have a fixed typed.  As an example the CTIO Argus instrument always
+alternates object and sky fibers so the object apertures can be given
+as 1x2 and the sky fibers as 2x2; i.e. objects are the odd numbered
+apertures and skys are the even numbered apertures.
+.LP
+The final reduced spectra are recorded in two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ms" extension.  Each line in the reduced image is a one dimensional
+spectrum with associated aperture, wavelength, and identification
+information.  When the \f(CWextras\fR parameter is set the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tools such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.  The special task \fBscopy\fR may be used to extract
+specific apertures or to change format to individual one dimensional
+images.
+.NH
+Package Parameters
+.LP
+The \fBspecred\fR package parameters, shown in Figure 2, set parameters
+affecting all the tasks in the package.
+.KS
+.V1
+
+.ce
+Figure 2: Package Parameter Set for SPECRED
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = imred
+   TASK = specred
+
+(extinct= onedstds$kpnoextinct.dat) Extinction file
+(caldir = onedstds$spec16redcal/) Standard star calibration directory
+(observa=  observatory) Observatory of data
+(interp =        poly5) Interpolation type
+(dispaxi=            2) Image axis for 2D images
+(nsum   =            1) Number of lines/columns to sum for 2D images
+
+(databas=     database) Database
+(verbose=           no) Verbose output?
+(logfile=      logfile) Log file
+(plotfil=             ) Plot file
+
+(records=             ) Record number extensions
+(version= SPECRED V3: April 1992)
+
+.KE
+.V2
+The dispersion axis parameter defines the image axis along which the
+dispersion runs.  This is used if the image header doesn't define the
+dispersion axis with the DISPAXIS keyword.
+The observatory parameter is used if there is no
+OBSERVAT keyword in the image header (see \fBobservatory\fR for more
+details).  The spectrum interpolation type might be changed to "sinc" but
+with the cautions given in \fBonedspec.package\fR.
+The other parameters define the standard I/O functions.
+The verbose parameter selects whether to print everything which goes
+into the log file on the terminal.  It is useful for monitoring
+what the \fBdofibers\fR task does.  The log and plot files are useful for
+keeping a record of the processing.  A log file is highly recommended.
+A plot file provides a record of apertures, traces, and extracted spectra
+but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+.NH
+Processing Parameters
+.LP
+The \fBdofibers\fR parameters are shown in Figure 3.
+.KS
+.V1
+
+.ce
+Figure 3: Parameter Set for DOFIBERS
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = specred
+   TASK = dofibers
+
+objects =               List of object spectra
+(apref  =             ) Aperture reference spectrum
+(flat   =             ) Flat field spectrum
+(through=             ) Throughput file or image (optional)
+(arcs1  =             ) List of arc spectra
+(arcs2  =             ) List of shift arc spectra
+(arctabl=             ) Arc assignment table (optional)
+
+.KE
+.V1
+(readnoi=           0.) Read out noise sigma (photons)
+(gain   =           1.) Photon gain (photons/data number)
+(datamax=        INDEF) Max data value / cosmic ray threshold
+(fibers =           97) Number of fibers
+(width  =          12.) Width of profiles (pixels)
+(minsep =           8.) Minimum separation between fibers (pixels)
+(maxsep =          15.) Maximum separation between fibers (pixels)
+(apidtab=             ) Aperture identifications
+(crval  =        INDEF) Approximate wavelength
+(cdelt  =        INDEF) Approximate dispersion
+(objaps =             ) Object apertures
+(skyaps =             ) Sky apertures
+(arcaps =             ) Arc apertures
+(objbeam=          0,1) Object beam numbers
+(skybeam=            0) Sky beam numbers
+(arcbeam=             ) Arc beam numbers
+
+(scatter=           no) Subtract scattered light?
+(fitflat=          yes) Fit and ratio flat field spectrum?
+(clean  =          yes) Detect and replace bad pixels?
+(dispcor=          yes) Dispersion correct spectra?
+(savearc=          yes) Save simultaneous arc apertures?
+(skysubt=          yes) Subtract sky?
+(skyedit=          yes) Edit the sky spectra?
+(savesky=          yes) Save sky spectra?
+(splot  =           no) Plot the final spectrum?
+(redo   =           no) Redo operations if previously done?
+(update =          yes) Update spectra if cal data changes?
+(batch  =           no) Extract objects in batch?
+(listonl=           no) List steps but don't process?
+
+(params =             ) Algorithm parameters
+
+.V2
+The list of objects and arcs can be @ files if desired.  The aperture
+reference spectrum is usually the same as the flat field spectrum though it
+could be any exposure with enough signal to accurately define the positions
+and trace the spectra.  The first list of arcs are the standard Th-Ar or
+HeNeAr comparison arc spectra (they must all be of the same type).  The
+second list of arcs are the auxiliary emission line exposures mentioned
+previously.
+.LP
+The detector read out noise and gain are used for cleaning and variance
+(optimal) extraction.  This is specified either explicitly or by reference
+to an image header keyword.
+The variance
+weighting and cosmic-ray cleanning are sensitive to extremely strong
+cosmic-rays; ones which are hundreds of times brighter than the
+spectrum.  The \fIdatamax\fR is used to set an upper limit for any
+real data.  Any pixels above this value will be flagged as cosmic-rays
+and will not affect the extractions.
+The dispersion axis defines the wavelength direction of spectra in
+the image if not defined in the image header by the keyword DISPAXIS.  The
+width and separation parameters define the dimensions (in pixels) of the
+spectra (fiber profile) across the dispersion.  The width parameter
+primarily affects the centering.  The maximum separation parameter is
+important if missing spectra from the aperture identification table are to
+be correctly skipped.  The number of fibers is either the actual number
+of fibers or the number in the aperture identification table.  An attempt
+is made to account for unassigned or missing fibers.  As a recommendation
+the actual number of fibers should be specified.
+.LP
+The approximate central wavelength and dispersion are used for the
+automatic identification of the arc reference.  They may be specified
+as image header keywords or values.  The INDEF values search the
+entire range of the coordinate reference file but the automatic
+line identification algorithm works much better and faster if
+approximate values are given.
+.LP
+The task needs to know which fibers are object, sky if sky subtraction is
+to be done, and simultaneous arcs if used.  One could explicitly give the
+aperture numbers but the recommended way, provided an aperture
+identification table is used, is to select the apertures based on the beam
+numbers.  The default values are recommended beam numbers.  Sky
+subtracted sky spectra are useful for evaluating the sky subtraction.
+Since only the spectra identified as objects are sky subtracted one can
+exclude fibers from the sky subtraction.  For example, if the
+\f(CWobjbeams\fR parameter is set to 1 then only those fibers with a beam of
+1 will be sky subtracted.  All other fibers will remain in the extracted
+spectra but will not be sky subtracted.
+.LP
+The next set of parameters select the processing steps and options.  The
+scattered light option allows fitting and subtracting a scattered light
+surface from the input object and flat field.  If there is significant
+scattered light which is not subtracted the fiber throughput correction
+will not be accurate.  The
+flat fitting option allows fitting and removing the overall shape of the
+flat field spectra while preserving the pixel-to-pixel response
+corrections.  This is useful for maintaining the approximate object count
+levels and not introducing the reciprocal of the flat field spectrum into
+the object spectra.  The \f(CWclean\fR option invokes a profile fitting and
+deviant point rejection algorithm as well as a variance weighting of points
+in the aperture.  These options require knowing the effective (i.e.
+accounting for any image combining) read out noise and gain.  For a
+discussion of cleaning and variance weighted extraction see
+\fBapvariance\fR and \fBapprofiles\fR.
+.LP
+The dispersion correction option selects whether to extract arc spectra,
+determine a dispersion function, assign them to the object spectra, and,
+possibly, resample the spectra to a linear (or log-linear) wavelength
+scale.  If simultaneous arc fibers are defined there is an option to delete
+them from the final spectra when they are no longer needed.
+.LP
+The sky alignment option allows applying a zeropoint dispersion shift
+to all fibers based on one or more sky lines.  This requires all fibers
+to have the sky lines visible.  When there are sky lines this will
+improve the sky subtraction if there is a systematic error in the
+fiber illumination between the sky and the arc calibration.
+.LP
+The sky subtraction option selects whether to combine the sky fiber spectra
+and subtract this sky from the object fiber spectra.  \fIDispersion
+correction and sky subtraction are independent operations.\fR  This means
+that if dispersion correction is not done then the sky subtraction will be
+done with respect to pixel coordinates.  This might be desirable in some
+quick look cases though it is incorrect for final reductions.
+.LP
+The sky subtraction option has two additional options.  The individual sky
+spectra may be examined and contaminated spectra deleted interactively
+before combining.  This can be a useful feature in crowded regions.  The
+final combined sky spectrum may be saved for later inspection in an image
+with the spectrum name prefixed by \fBsky\fR.
+.LP
+After a spectrum has been processed it is possible to examine the results
+interactively using the \fBsplot\fR tasks.  This option has a query which
+may be turned off with "YES" or "NO" if there are multiple spectra to be
+processed.
+.LP
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\f(CWupdate\fR flag is set.  The changes which will cause an update are a new
+aperture identification table, a new reference image, new flat fields, and a
+new arc reference.  If all input spectra are to be processed regardless of
+previous processing the \f(CWredo\fR flag may be used.  Note that
+reprocessing clobbers the previously processed output spectra.
+.LP
+The \f(CWbatch\fR processing option allows object spectra to be processed as
+a background or batch job.  This will only occur if sky spectra editing and
+\fBsplot\fR review (interactive operations) are turned off, either when the
+task is run or by responding with "NO" to the queries during processing.
+.LP
+The \f(CWlistonly\fR option prints a summary of the processing steps which
+will be performed on the input spectra without actually doing anything.
+This is useful for verifying which spectra will be affected if the input
+list contains previously processed spectra.  The listing does not include
+any arc spectra which may be extracted to dispersion calibrate an object
+spectrum.
+.LP
+The last parameter (excluding the task mode parameter) points to another
+parameter set for the algorithm parameters.  The way \fBdofibers\fR works
+this may not have any value and the parameter set \fBparams\fR is always
+used.  The algorithm parameters are discussed further in the next section.
+.NH
+Algorithms and Algorithm Parameters
+.LP
+This section summarizes the various algorithms used by the \fBdofibers\fR
+task and the parameters which control and modify the algorithms.  The
+algorithm parameters available to the user are collected in the parameter
+set \fBparams\fR.  These parameters are taken from the various general
+purpose tasks used by the \fBdofibers\fR processing task.  Additional
+information about these parameters and algorithms may be found in the help
+for the actual task executed.  These tasks are identified in the parameter
+section listing in parenthesis.  The aim of this parameter set organization
+is to collect all the algorithm parameters in one place separate from the
+processing parameters and include only those which are relevant for
+multifiber data.  The parameter values can be changed from the
+defaults by using the parameter editor,
+.V1
+
+	cl> epar params
+
+.V2
+or simple typing \f(CWparams\fR.  The parameter editor can also be
+entered when editing the \fBdofibers\fR parameters by typing \f(CW:e
+params\fR or simply \f(CW:e\fR if positioned at the \f(CWparams\fR
+parameter.  Figure 4 shows the parameter set.
+.KS
+.V1
+
+.ce
+Figure 4: Algorithm Parameter Set
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = specred
+   TASK = params
+
+(line   =        INDEF) Default dispersion line
+(nsum   =           10) Number of dispersion lines to sum
+(order  =   decreasing) Order of apertures
+(extras =           no) Extract sky, sigma, etc.?
+
+                        -- DEFAULT APERTURE LIMITS --
+(lower  =          -5.) Lower aperture limit relative to center
+(upper  =           5.) Upper aperture limit relative to center
+
+                        -- AUTOMATIC APERTURE RESIZING PARAMETERS --
+(ylevel =         0.05) Fraction of peak or intensity for resizing
+
+.KE
+.KS
+.V1
+                        -- TRACE PARAMETERS --
+(t_step =           10) Tracing step
+(t_funct=      spline3) Trace fitting function
+(t_order=            3) Trace fitting function order
+(t_niter=            1) Trace rejection iterations
+(t_low  =           3.) Trace lower rejection sigma
+(t_high =           3.) Trace upper rejection sigma
+
+.KE
+.KS
+.V1
+                        -- SCATTERED LIGHT PARAMETERS --
+(buffer =           1.) Buffer distance from apertures
+(apscat1=             ) Fitting parameters across the dispersion
+(apscat2=             ) Fitting parameters along the dispersion
+
+.KE
+.KS
+.V1
+                        -- APERTURE EXTRACTION PARAMETERS --
+(weights=         none) Extraction weights (none|variance)
+(pfit   =        fit1d) Profile fitting algorithm (fit1d|fit2d)
+(weights=         none) Extraction weights (none|variance)
+(pfit   =        fit1d) Profile fitting algorithm (fit1d|fit2d)
+(lsigma =           3.) Lower rejection threshold
+(usigma =           3.) Upper rejection threshold
+(nsubaps=            1) Number of subapertures
+
+.KE
+.KS
+.V1
+                        -- FLAT FIELD FUNCTION FITTING PARAMETERS --
+(f_inter=          yes) Fit flat field interactively?
+(f_funct=      spline3) Fitting function
+(f_order=           10) Fitting function order
+
+.KE
+.KS
+.V1
+                        -- ARC DISPERSION FUNCTION PARAMETERS --
+(coordli=linelists$idhenear.dat) Line list
+(match  =          -3.) Line list matching limit in Angstroms
+(fwidth =           4.) Arc line widths in pixels
+(cradius=          10.) Centering radius in pixels
+(i_funct=      spline3) Coordinate function
+(i_order=            3) Order of dispersion function
+(i_niter=            2) Rejection iterations
+(i_low  =           3.) Lower rejection sigma
+(i_high =           3.) Upper rejection sigma
+(refit  =          yes) Refit coordinate function when reidentifying?
+(addfeat=           no) Add features when reidentifying?
+
+.KE
+.KS
+.V1
+                        -- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+(select =       interp) Selection method for reference spectra
+(sort   =           jd) Sort key
+(group  =          ljd) Group key
+(time   =           no) Is sort key a time?
+(timewra=          17.) Time wrap point for time sorting
+
+.KE
+.KS
+.V1
+                        -- DISPERSION CORRECTION PARAMETERS --
+(lineari=          yes) Linearize (interpolate) spectra?
+(log    =           no) Logarithmic wavelength scale?
+(flux   =          yes) Conserve flux?
+
+.KE
+.KS
+.V1
+                        -- SKY SUBTRACTION PARAMETERS --
+(combine=      average) Type of combine operation
+(reject =    avsigclip) Sky rejection option
+(scale  =         none) Sky scaling option
+
+.KE
+.V2
+.NH 2
+Extraction
+.LP
+The identification of the spectra in the two dimensional images and their
+scattered light subtraction and extraction to one dimensional spectra
+in multispec format is accomplished
+using the tasks from the \fBapextract\fR package.  The first parameters
+through \f(CWnsubaps\fR control the extractions.
+.LP
+The dispersion line is that used for finding the spectra, for plotting in
+the aperture editor, and as the starting point for tracing.  The default
+value of \fBINDEF\fR selects the middle of the image.  The aperture
+finding, adjusting, editing, and tracing operations also allow summing a
+number of dispersion lines to improve the signal.  The number of lines is
+set by the \f(CWnsum\fR parameter.
+.LP
+The order parameter defines whether the order of the aperture
+identifications in the aperture identification table (or the default
+sequential numbers if no file is used) is in the same sense as the image
+coordinates (increasing) or the opposite sense (decreasing).  If the
+aperture identifications turn out to be opposite to what is desired when
+viewed in the aperture editing graph then simply change this parameter.
+.LP
+The basic data output by the spectral extraction routines are the one
+dimensional spectra.  Additional information may be output when the
+\f(CWextras\fR option is selected and the cleaning or variance weighting
+options are also selected.  In this case a three dimensional image is
+produced with the first element of the third dimension being the cleaned
+and/or weighted spectra, the second element being the uncleaned and
+unweighted spectra, and the third element being an estimate of the sigma
+of each pixel in the extracted spectrum.  Currently the sigma data is not
+used by any other tasks and is only for reference.
+.LP
+The initial step of finding the fiber spectra in the aperture reference
+image consists of identifying the peaks in a cut across the dispersion,
+eliminating those which are closer to each other than the \f(CWminsep\fR
+distance, and then keeping the specified \f(CWnfibers\fR highest peaks.  The
+centers of the profiles are determined using the \fBcenter1d\fR algorithm
+which uses the \f(CWwidth\fR parameter.
+.LP
+Apertures are then assigned to each spectrum.  The initial edges of the
+aperture relative to the center are defined by the \f(CWlower\fR and
+\f(CWupper\fR parameters.  The trickiest part of assigning the apertures is
+relating the aperture identification from the aperture identification table
+to automatically selected fiber profiles.  The first aperture id in the
+file is assigned to the first spectrum found using the \f(CWorder\fR
+parameter to select the assignment direction.  The numbering proceeds in
+this way except that if a gap greater than a multiple of the \f(CWmaxsep\fR
+parameter is encountered then assignments in the file are skipped under the
+assumption that a fiber is missing (broken).  If unassigned fibers are
+still visible in a flat field, either by design or by scattered light, the
+unassigned fibers can be included in the number of fibers to find and then
+the unassigned (negative beam number) apertures are excluded from any
+extraction.  For more on the finding and assignment algorithms see
+\fBapfind\fR.
+.LP
+The initial apertures are the same for all spectra but they can each be
+automatically resized.  The automatic resizing sets the aperture limits
+at a fraction of the peak relative to the interfiber minimum.
+The default \f(CWylevel\fR is to resize the apertures to 5% of the peak.
+See the description for the task \fBapresize\fR for further details.
+.LP
+The user is given the opportunity to graphically review and adjust the
+aperture definitions.  This is recommended.  As mentioned previously, the
+correct identification of the fibers is tricky and it is fundamentally
+important that this be done correctly; otherwise the spectrum
+identifications will not be for the objects they say.  An important command in
+this regard is the 'o' key which allows reordering the identifications
+based on the aperture identification table.  This is required if the first
+fiber is actually missing since the initial assignment begins assigning the
+first spectrum found with the first entry in the aperture file.  The
+aperture editor is a very powerful tool and is described in detail as
+\fBapedit\fR.
+.LP
+The next set of parameters control the tracing and function fitting of the
+aperture reference positions along the dispersion direction.  The position
+of a spectrum across the dispersion is determined by the centering
+algorithm (see \fBcenter1d\fR) at a series of evenly spaced steps, given by
+the parameter \f(CWt_step\fR, along the dispersion.  The step size should be
+fine enough to follow position changes but it is not necessary to measure
+every point.  The fitted points may jump around a little bit due to noise
+and cosmic rays even when summing a number of lines.  Thus, a smooth
+function is fit.  The function type, order, and iterative rejection of
+deviant points is controlled by the other trace parameters.  For more
+discussion consult the help pages for \fBaptrace\fR and \fBicfit\fR.  The
+default is to fit a cubic spline of three pieces with a single iteration of
+3 sigma rejection.
+.LP
+The actual extraction of the spectra by summing across the aperture at each
+point along the dispersion is controlled by the next set of parameters.
+The default extraction simply sums the pixels using partial pixels at the
+ends.  The options allow selection of a weighted sum based on a Poisson
+variance model using the \f(CWreadnoise\fR and \f(CWgain\fR detector
+parameters.  Note that if the \f(CWclean\fR option is selected the variance
+weighted extraction is used regardless of the \f(CWweights\fR parameter.  The
+sigma thresholds for cleaning are also set in the \fBparams\fR parameters.
+For more on the variance weighted extraction and cleaning see
+\fBapvariance\fR and \fBapprofiles\fR as well as \fBapsum\fR.
+.LP
+The last parameter, \f(CWnsubaps\fR, is used only in special cases when it is
+desired to subdivide the fiber profiles into subapertures prior to
+dispersion correction.  After dispersion correction the subapertures are
+then added together.  The purpose of this is to correct for wavelength
+shifts across a fiber.
+.NH 2
+Scattered Light Subtraction
+.LP
+Scattered light may be subtracted from the input two dimensional image as
+the first step.  This is done using the algorithm described in
+\fBapscatter\fR.  This can be important if there is significant scattered
+light since the flat field/throughput correction will otherwise be
+incorrect.  The algorithm consists of fitting a function to the data
+outside the defined apertures by a specified \fIbuffer\fR at each line or
+column across the dispersion.  The function fitting parameters are the same
+at each line.  Because the fitted functions are independent at each line or
+column a second set of one dimensional functions are fit parallel to the
+dispersion using the evaluated fit values from the cross-dispersion step.
+This produces a smooth scattered light surface which is finally subtracted
+from the input image.  Again the function fitting parameters are the
+same at each line or column though they may be different than the parameters
+used to fit across the dispersion.
+.LP
+The first time the task is run with a particular flat field (or aperture
+reference image if no flat field is used) the scattered light fitting
+parameters are set interactively using that image.  The interactive step
+selects a particular line or column upon which the fitting is done
+interactively with the \fBicfit\fR commands.  A query is first issued
+which allows skipping this interactive stage.  Note that the interactive
+fitting is only for defining the fitting functions and orders.  When
+the graphical \fBicfit\fR fitting is exited (with 'q') there is a second prompt
+allowing you to change the buffer distance (in the first cross-dispersion
+stage) from the apertures, change the line/column, or finally quit.
+.LP
+The initial fitting parameters and the final set parameters are recorded
+in the \fBapscat1\fR and \fBapscat2\fR hidden parameter sets.  These
+parameters are then used automatically for every subsequent image
+which is scattered light corrected.
+.LP
+The scattered light subtraction modifies the input 2D images.  To preserve
+the original data a copy of the original image is made with the same
+root name and the word "noscat" appended.  The scattered light subtracted
+images will have the header keyword "APSCATTE" which is how the task
+avoids repeating the scattered light subtraction during any reprocessing.
+However if the \fIredo\fR option is selected the scattered light subtraction
+will also be redone by first restoring the "noscat" images to the original
+input names.
+.NH 2
+Flat Field and Fiber Throughput Corrections
+.LP
+Flat field corrections may be made during the basic CCD processing; i.e.
+direct division by the two dimensional flat field observation.  In that
+case do not specify a flat field spectrum; use the null string "".  The
+\fBdofibers\fR task provides an alternative flat field response correction
+based on division of the extracted object spectra by the extracted flat field
+spectra.  A discussion of the theory and merits of flat fielding directly
+verses using the extracted spectra will not be made here.  The
+\fBdofibers\fR flat fielding algorithm is the \fIrecommended\fR method for
+flat fielding since it works well and is not subject to the many problems
+involved in two dimensional flat fielding.
+.LP
+In addition to correcting for pixel-to-pixel response the flat field step
+also corrects for differences in the fiber throughput.  Thus, even if the
+pixel-to-pixel flat field corrections have been made in some other way it
+is desirable to use a sky or dome flat observation for determining a fiber
+throughput correction.  Alternatively, a separately derived throughput
+file may be specified.  This file consists of the aperture numbers
+(the same as used for the aperture reference) and relative throughput
+numbers.
+.LP
+The first step is extraction of the flat field spectrum, if specified,
+using the reference apertures.  Only one flat field is allowed so if
+multiple flat fields are required the data must be reduced in groups.
+After extraction one or more corrections are applied.  If the \f(CWfitflat\fR
+option is selected (the default) the extracted flat field spectra are
+averaged together and a smooth function is fit.  The default fitting
+function and order are given by the parameters \f(CWf_function\fR and
+\f(CWf_order\fR.  If the parameter \f(CWf_interactive\fR is "yes" then the
+fitting is done interactively using the \fBfit1d\fR task which uses the
+\fBicfit\fR interactive fitting commands.
+.LP
+The fitted function is divided into the individual flat field spectra to
+remove the basic shape of the spectrum while maintaining the relative
+individual pixel responses and any fiber to fiber differences.  This step
+avoids introducing the flat field spectrum shape into the object spectra
+and closely preserves the object counts.
+.LP
+If a throughput image is available (an observation of blank sky
+usually at twilight) it is extracted.  If no flat field is used the average
+signal through each fiber is computed and this becomes the response
+normalization function.  Note that a dome flat may be used in place of a
+sky in the sky flat field parameter for producing throughput only
+corrections.  If a flat field is specified then each sky spectrum is
+divided by the appropriate flat field spectrum.  The total counts through
+each fiber are multiplied into the flat field spectrum thus making the sky
+throughput of each fiber the same.  This correction is important if the
+illumination of the fibers differs between the flat field source and the
+sky.  Since only the total counts are required the sky or dome flat field
+spectra need not be particularly strong though care must be taken to avoid
+objects.
+.LP
+Instead of a sky flat or other throughput image a separately derived
+throughput file may be used.  It may be used with or without a
+flat field.
+.LP
+The final step is to normalize the flat field spectra by the mean counts of
+all the fibers.  This normalization step is simply to preserve the average
+counts of the extracted object and arc spectra after division by the
+response spectra.  The final relative throughput values are recorded in the
+log and possibly printed on the terminal.
+.LP
+These flat field response steps and algorithm are available as a separate
+task called \fBmsresp1d\fR.
+.NH
+Dispersion Correction
+.LP
+Dispersion corrections are applied to the extracted spectra if the
+\fBdispcor\fR parameter is set.  This can be a complicated process which
+the \fBdofibers\fR task tries to simplify for you.  There are three basic
+steps involved; determining the dispersion functions relating pixel
+position to wavelength, assigning the appropriate dispersion function to a
+particular observation, and resampling the spectra to evenly spaced pixels
+in wavelength.
+.LP
+The comparison arc spectra are used to define dispersion functions for the
+fibers using the tasks \fBautoidentify\fR and \fBreidentify\fR.  The
+interactive \fBautoidentify\fR task is only used on the central fiber of the
+first arc spectrum to define the basic reference dispersion solution from
+which all other fibers and arc spectra are automatically derived using
+\fBreidentify\fR. \fBAutoidentify\fR attempts to automatically identify
+the arc lines using the \fIcrval\fR and \fIcdelt\fR parameters.  Whether
+or not it is successful the user is presented with the interactive
+identification graph.  The automatic identifications can be reviewed and a
+new solution or corrections to the automatic solution may be performed.
+.LP
+The set of arc dispersion function parameters are from \fBautoidentify\fR and
+\fBreidentify\fR.  The parameters define a line list for use in
+automatically assigning wavelengths to arc lines, a parameter controlling
+the width of the centering window (which should match the base line
+widths), the dispersion function type and order, parameters to exclude bad
+lines from function fits, and parameters defining whether to refit the
+dispersion function, as opposed to simply determining a zero point shift,
+and the addition of new lines from the line list when reidentifying
+additional arc spectra.  The defaults should generally be adequate and the
+dispersion function fitting parameters may be altered interactively.  One
+should consult the help for the two tasks for additional details of these
+parameters and the operation of \fBautoidentify\fR.
+.LP
+Generally, taking a number of comparison arc lamp exposures interspersed
+with the program spectra is sufficient to accurately dispersion calibrate
+multifiber spectra.  However, there are some other calibration options
+which may be of interest.  These options apply additional calibration data
+consisting either of auxiliary line spectra, such as from dome lights or
+night sky lines, or simultaneous arc lamp spectra taken through a few
+fibers during the object exposure.  These options add complexity to the
+dispersion calibration process.
+.LP
+When only arc comparison lamp spectra are used, dispersion functions are
+determined independently for each fiber of each arc image and then assigned
+to the matching fibers in the program object observations.  The assignment
+consists of selecting one or two arc images to calibrate each object
+image.  When two bracketing arc spectra are used the dispersion functions
+are linearly interpolated (usually based on the time of the observations).
+.LP
+If taking comparison exposures is time-consuming, possibly requiring
+reconfiguration to illuminate the fibers, and the spectrograph is
+expected to be fairly stable apart from small shifts, there are two
+mutually exclusive methods for monitoring
+shifts in the dispersion zero point from the basic arc lamp spectra other
+than taking many arc lamp exposures.  One is to use some fibers to take a
+simultaneous arc spectrum while observing the program objects.  The fibers
+are identified by aperture or beam numbers.  The second method is to use
+\fIauxiliary line spectra\fR, such as mercury lines from the dome lights.
+These spectra are specified with an auxiliary shift arc list, \f(CWarc2\fR.
+.LP
+When using auxiliary line spectra for monitoring zero point shifts one of
+these spectra is plotted interactively by \fBidentify\fR with the
+reference dispersion function from the reference arc spectrum.  The user
+marks one or more lines which will be used to compute zero point wavelength
+shifts in the dispersion functions automatically.  The actual wavelengths
+of the lines need not be known.  In this case accept the wavelength based
+on the reference dispersion function.  As other observations of the same
+features are made the changes in the positions of the features will be
+tracked as zero point wavelength changes such that wavelengths of the
+features remain constant.
+.LP
+When using auxiliary line spectra the only arc lamp spectrum used is the
+initial arc reference spectrum (the first image in the \f(CWarcs1\fR list).
+The master dispersion functions are then shifted based on the spectra in
+the \f(CWarcs2\fR list (which must all be of the same type).  The dispersion
+function assignments made by \fBrefspectra\fR using either the arc
+assignment file or based on header keywords is done in the same way as
+described for the arc lamp images except using the auxiliary spectra.
+.LP
+If simultaneous arcs are used the arc lines are reidentified to determine a
+zero point shift relative to the comparison lamp spectra selected, by
+\fBrefspectra\fR, of the same fiber.  A linear function of aperture
+position on the image across the dispersion verses the zero point shifts
+from the arc fibers is determined and applied to the dispersion functions
+from the assigned calibration arcs for the non-arc fibers.  Note that if
+there are two comparison lamp spectra (before and after the object
+exposure) then there will be two shifts applied to two dispersion functions
+which are then combined using the weights based on the header parameters
+(usually the observation time).
+.LP
+The arc assignments may be done either explicitly with an arc assignment
+table (parameter \f(CWarctable\fR) or based on a header parameter.  The task
+used is \fBrefspectra\fR and the user should consult this task if the
+default behavior is not what is desired.  The default is to interpolate
+linearly between the nearest arcs based on the Julian date (corrected to
+the middle of the exposure).  The Julian date and a local Julian day number
+(the day number at local noon) are computed automatically by the task
+\fBsetjd\fR and recorded in the image headers under the keywords JD and
+LJD.  In addition the universal time at the middle of the exposure, keyword
+UTMIDDLE, is computed by the task \fBsetairmass\fR and this may also be used
+for ordering the arc and object observations.
+.LP
+.LP
+An optional step is to use sky lines in the spectra to compute a zeropoint
+dispersion shift that will align the sky lines.  This may improve sky
+subtraction if the illumination is not the same between the arc calibration
+and the sky.  When selected the object spectrum is dispersion corrected
+using a non-linear dispersion function to avoid resampling the spectrum.
+The sky lines are then reidentified in wavelength space from a template
+list of sky lines.  The mean shift in the lines for each fiber relative to
+the template in that fiber is computed to give the zeropoint shift.  The
+database file is created when the first object is extracted.  You are asked
+to mark the sky lines in one fiber and then the lines are automatically
+reidentified in all other fibers.  Note that this technique requires the
+sky lines be found in all fibers.
+.LP
+The last step of dispersion correction (resampling the spectrum to evenly
+spaced pixels in wavelength) is optional and relatively straightforward.
+If the \f(CWlinearize\fR parameter is no then the spectra are not resampled
+and the nonlinear dispersion information is recorded in the image header.
+Other IRAF tasks (the coordinate description is specific to IRAF) will use
+this information whenever wavelengths are needed.  If linearizing is
+selected a linear dispersion relation, either linear in the wavelength or
+the log of the wavelength, is defined once and applied to every extracted
+spectrum.  The resampling algorithm  parameters allow selecting the
+interpolation function type, whether to conserve flux per pixel by
+integrating across the extent of the final pixel, and whether to linearize
+to equal linear or logarithmic intervals.  The latter may be appropriate
+for radial velocity studies.  The default is to use a fifth order
+polynomial for interpolation, to conserve flux, and to not use logarithmic
+wavelength bins.  These parameters are described fully in the help for the
+task \fBdispcor\fR which performs the correction.  The interpolation
+function options and the nonlinear dispersion coordinate system is
+described in the help topic \fBonedspec.package\fR.
+.NH
+Sky Subtraction
+.LP
+Sky subtraction is selected with the \f(CWskysubtract\fR processing option.
+The sky spectra are selected by their aperture and beam numbers and
+combined into a single master sky spectrum
+which is then subtracted from each object spectrum.  If the \f(CWskyedit\fR
+option is selected the sky spectra are plotted using the task
+\fBspecplot\fR.  By default they are superposed to allow identifying
+spectra with unusually high signal due to object contamination.  To
+eliminate a sky spectrum from consideration point at it with the cursor and
+type 'd'.  The last deleted spectrum may be undeleted with 'e'.  This
+allows recovery of incorrect or accidental deletions.
+.LP
+The sky combining algorithm parameters define how the individual sky fiber
+spectra, after interactive editing, are combined before subtraction from
+the object fibers.  The goals of combining are to reduce noise, eliminate
+cosmic-rays, and eliminate fibers with inadvertent objects.  The common
+methods for doing this to use a median and/or a special sigma clipping
+algorithm (see \fBscombine\fR for details).  The scale
+parameter determines whether the individual skys are first scaled to a
+common mode.  The scaling should be used if the throughput is uncertain,
+but in that case you probably did the wrong thing in the throughput
+correction.  If the sky subtraction is done interactively, i.e. with the
+\f(CWskyedit\fR option selected, then after selecting the spectra to be
+combined a query is made for the combining algorithm.  This allows
+modifying the default algorithm based on the number of sky spectra
+selected since the "avsigclip" rejection algorithm requires at least
+three spectra.
+.LP
+The combined sky spectrum is subtracted from only those spectra specified
+by the object aperture and beam numbers.  Other spectra, such as comparison
+arc spectra, are retained unchanged.  One may include the sky spectra as
+object spectra to produce residual sky spectra for analysis.  The combined
+master sky spectra may be saved if the \f(CWsaveskys\fR parameter is set.
+The saved sky is given the name of the object spectrum with the prefix
+"sky".
+.NH
+References
+.NH 2
+IRAF Introductory References
+.LP
+Work is underway on a new introductory guide to IRAF.  Currently, the
+work below is the primary introduction.
+.IP
+P. Shames and D. Tody, \fIA User's Introduction to the IRAF Command
+Language\fR, Central Computer Services, NOAO, 1986.
+.NH 2
+CCD Reductions
+.IP
+F. Valdes, \fIThe IRAF CCD Reduction Package -- CCDRED\fR, Central
+Computer Services, NOAO, 1987.
+.IP
+F. Valdes, \fIUser's Guide to the CCDRED Package\fR, Central
+Computer Services, NOAO, 1988.  Also on-line as \f(CWhelp ccdred.guide\fR.
+.IP
+P. Massey, \fIA User's Guide to CCD Reductions with IRAF\fR, Central
+Computer Services, NOAO, 1989.
+.NH 2
+Aperture Extraction Package
+.IP
+F. Valdes, \fIThe IRAF APEXTRACT Package\fR, Central Computer Services,
+NOAO, 1987 (out-of-date).
+.NH 2
+Task Help References
+.LP
+Each task in the \fBspecred\fR packages and tasks used by \fBdofibers\fR have
+help pages describing the parameters and task in some detail.  To get
+on-line help type
+.V1
+
+cl> help \fItaskname\fR
+
+.V2
+The output of this command can be piped to \fBlprint\fR to make a printed
+copy.
+
+.V1
+      apall - Extract 1D spectra (all parameters in one task)
+  apdefault - Set the default aperture parameters and apidtable
+     apedit - Edit apertures interactively
+     apfind - Automatically find spectra and define apertures
+      apfit - Fit 2D spectra and output the fit, difference, or ratio
+  apflatten - Remove overall spectral and profile shapes from flat fields
+     apmask - Create and IRAF pixel list mask of the apertures
+apnormalize - Normalize 2D apertures by 1D functions
+ aprecenter - Recenter apertures
+   apresize - Resize apertures
+  apscatter - Fit and subtract scattered light
+      apsum - Extract 1D spectra
+    aptrace - Trace positions of spectra
+
+      bplot - Batch plot of spectra with SPLOT
+  calibrate - Extinction and flux calibrate spectra
+  continuum - Fit the continuum in spectra
+   deredden - Apply interstellar extinction correction
+    dispcor - Dispersion correct spectra
+     dopcor - Doppler correct spectra
+   fitprofs - Fit gaussian profiles
+   identify - Identify features in spectrum for dispersion solution
+   msresp1d - Create 1D response spectra from flat field and sky spectra
+ refspectra - Assign wavelength reference spectra to other spectra
+ reidentify - Automatically reidentify features in spectra
+ sapertures - Set or change aperture header information
+     sarith - Spectrum arithmetic
+   scombine - Combine spectra
+      scopy - Select and copy apertures in different spectral formats
+   sensfunc - Compute instrumental sensitivity from standard stars
+ setairmass - Compute effective airmass and middle UT for an exposure
+      setjd - Compute and set Julian dates in images
+       sfit - Fit spectra and output fit, ratio, or difference
+     skysub - Sky subtract extracted multispec spectra
+      slist - List spectrum header parameters
+   specplot - Scale, stack, and plot multiple spectra
+      splot - Preliminary spectral plot/analysis
+   standard - Tabulate standard star counts and fluxes
+
+   dofibers - Process multifiber spectra
+      demos - Demonstrations and tests
+
+	    Additional help topics
+
+   onedspec.package - Package parameters and general description of package
+  apextract.package - Package parameters and general description of package
+ approfiles - Profile determination algorithms
+ apvariance - Extractions, variance weighting, cleaning, and noise model
+   center1d - One dimensional centering algorithm
+      icfit - Interactive one dimensional curve fitting
+.V2
+.SH
+Appendix A: DOFIBERS Parameters
+.LP
+.nr PS 8
+.nr VS 10
+objects
+.LS
+List of object spectra to be processed.  Previously processed spectra are
+ignored unless the \fIredo\fR flag is set or the \fIupdate\fR flag is set and
+dependent calibration data has changed.  Extracted spectra are ignored.
+.LE
+apref = ""
+.LS
+Aperture reference spectrum.  This spectrum is used to define the basic
+extraction apertures and is typically a flat field spectrum.
+.LE
+flat = "" (optional)
+.LS
+Flat field spectrum.  If specified the one dimensional flat field spectra
+are extracted and used to make flat field calibrations.  If a separate
+throughput file or image is not specified the flat field is also used
+for computing a fiber throughput correction.
+.LE
+throughput = "" (optional)
+.LS
+Throughput file or image.  If an image is specified, typically a blank
+sky observation, the total flux through
+each fiber is used to correct for fiber throughput.  If a file consisting
+of lines with the aperture number and relative throughput is specified
+then the fiber throughput will be corrected by those values.  If neither
+is specified but a flat field image is given it is used to compute the
+throughput.  
+.LE
+arcs1 = "" (at least one if dispersion correcting)
+.LS
+List of primary arc spectra.  These spectra are used to define the dispersion
+functions for each fiber apart from a possible zero point correction made
+with secondary shift spectra or arc calibration fibers in the object spectra.
+One fiber from the first spectrum is used to mark lines and set the dispersion
+function interactively and dispersion functions for all other fibers and
+arc spectra are derived from it.
+.LE
+arcs2 = "" (optional)
+.LS
+List of optional shift arc spectra.  Features in these secondary observations
+are used to supply a wavelength zero point shift through the observing
+sequence.  One type of observation is dome lamps containing characteristic
+emission lines.
+.LE
+arctable = "" (optional) (refspectra)
+.LS
+Table defining arc spectra to be assigned to object
+spectra (see \fBrefspectra\fR).  If not specified an assignment based
+on a header parameter, \fIparams.sort\fR, such as the observation time is made.
+.LE
+
+readnoise = "0." (apsum)
+.LS
+Read out noise in photons.  This parameter defines the minimum noise
+sigma.  It is defined in terms of photons (or electrons) and scales
+to the data values through the gain parameter.  A image header keyword
+(case insensitive) may be specified to get the value from the image.
+.LE
+gain = "1." (apsum)
+.LS
+Detector gain or conversion factor between photons/electrons and
+data values.  It is specified as the number of photons per data value.
+A image header keyword (case insensitive) may be specified to get the value
+from the image.
+.LE
+datamax = INDEF (apsum.saturation)
+.LS
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the flat field or
+arc spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.LE
+fibers = 97 (apfind)
+.LS
+Number of fibers.  This number is used during the automatic definition of
+the apertures from the aperture reference spectrum.  It is best if this
+reflects the actual number of fibers which may be found in the aperture
+reference image.  The interactive
+review of the aperture assignments allows verification and adjustments
+to the automatic aperture definitions.
+.LE
+width = 12. (apedit)
+.LS
+Approximate base full width of the fiber profiles.  This parameter is used
+for the profile centering algorithm.
+.LE
+minsep = 8. (apfind)
+.LS
+Minimum separation between fibers.  Weaker spectra or noise within this
+distance of a stronger spectrum are rejected.
+.LE
+maxsep = 15. (apfind)
+.LS
+Maximum separation between adjacent fibers.  This parameter
+is used to identify missing fibers.  If two adjacent spectra exceed this
+separation then it is assumed that a fiber is missing and the aperture
+identification assignments will be adjusted accordingly.
+.LE
+apidtable = "" (apfind)
+.LS
+Aperture identification table.  This may be either a text file or an
+image.  A text file contains the fiber number, beam number defining object
+(1), sky (0), and arc (2) fibers, and a object title.  An image contains
+the keywords SLFIBnnn with string value consisting of the fiber number,
+beam number, optional right ascension and declination, and an object
+title.  Unassigned and broken fibers (beam of -1) should be included in the
+identification information since they will automatically be excluded.
+.LE
+crval = INDEF, cdelt = INDEF (autoidentify)
+.LS
+These parameters specify an approximate central wavelength and dispersion.
+They may be specified as numerical values, INDEF, or image header keyword
+names whose values are to be used.
+If both these parameters are INDEF then the automatic identification will
+not be done.
+.LE
+objaps = "", skyaps = "", arcaps = ""
+.LS
+List of object, sky, and arc aperture numbers.  These are used to
+identify arc apertures for wavelength calibration and object and sky
+apertures for sky subtraction.  Note sky apertures may be identified as
+both object and sky if one wants to subtract the mean sky from the
+individual sky spectra.  Typically the different spectrum types are
+identified by their beam numbers and the default, null string,
+lists select all apertures.
+.LE
+objbeams = "0,1", skybeams = "0", arcbeams = 2
+.LS
+List of object, sky, and arc beam numbers.  The convention is that sky
+fibers are given a beam number of 0, object fibers a beam number of 1, and
+arc fibers a beam number of 2.  The beam numbers are typically set in the
+\fIapidtable\fR.  Unassigned or broken fibers may be given a beam number of
+-1 in the aperture identification table since apertures with negative beam
+numbers are not extracted.  Note it is valid to identify sky fibers as both
+object and sky.
+.LE
+
+scattered = no (apscatter)
+.LS
+Smooth and subtracted scattered light from the object and flat field
+images.  This operation consists of fitting independent smooth functions
+across the dispersion using data outside the fiber apertures and then
+smoothing the individual fits along the dispersion.  The initial
+flat field, or if none is given the aperture reference image, are
+done interactively to allow setting the fitting parameters.  All
+subsequent subtractions use the same fitting parameters.
+.LE
+fitflat = yes (flat1d)
+.LS
+Fit the composite flat field spectrum by a smooth function and divide each
+flat field spectrum by this function?  This operation removes the average
+spectral signature of the flat field lamp from the sensitivity correction to
+avoid modifying the object fluxes.
+.LE
+clean = yes (apsum)
+.LS
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction and requires reasonably good values
+for the readout noise and gain.  In addition the datamax parameters
+can be useful.
+.LE
+dispcor = yes
+.LS
+Dispersion correct spectra?  Depending on the \fIparams.linearize\fR
+parameter this may either resample the spectra or insert a dispersion
+function in the image header.
+.LE
+skyalign = no
+.LS
+Align sky lines?  If yes then for the first object spectrum you are asked
+to mark one or more sky lines to use for alignment.  Then these lines will
+be found in all spectra and an average zeropoint shift computed and applied
+to the dispersion solution to align these lines.  Note that this assumes
+the sky lines are seen in all fibers.
+.LE
+savearcs = yes
+.LS
+Save any simultaneous arc apertures?  If no then the arc apertures will
+be deleted after use.
+.LE
+skysubtract = yes
+.LS
+Subtract sky from the object spectra?  If yes the sky spectra are combined
+and subtracted from the object spectra as defined by the object and sky
+aperture/beam parameters.
+.LE
+skyedit = yes
+.LS
+Overplot all the sky spectra and allow contaminated sky spectra to be
+deleted?
+.LE
+saveskys = yes
+.LS
+Save the combined sky spectrum?  If no then the sky spectrum will be
+deleted after sky subtraction is completed.
+.LE
+splot = no
+.LS
+Plot the final spectra with the task \fBsplot\fR?
+.LE
+redo = no
+.LS
+Redo operations previously done?  If no then previously processed spectra
+in the objects list will not be processed (unless they need to be updated).
+.LE
+update = yes
+.LS
+Update processing of previously processed spectra if aperture, flat
+field, or dispersion reference definitions are changed?
+.LE
+batch = no
+.LS
+Process spectra as a background or batch job provided there are no interactive
+options (\fIskyedit\fR and \fIsplot\fR) selected.
+.LE
+listonly = no
+.LS
+List processing steps but don't process?
+.LE
+
+params = "" (pset)
+.LS
+Name of parameter set containing additional processing parameters.  The
+default is parameter set \fBparams\fR.  The parameter set may be examined
+and modified in the usual ways (typically with "epar params" or ":e params"
+from the parameter editor).  Note that using a different parameter file
+is not allowed.  The parameters are described below.
+.LE
+
+.ce
+-- PACKAGE PARAMETERS
+
+Package parameters are those which generally apply to all task in the
+package.  This is also true of \fBdofibers\fR.
+
+dispaxis = 2
+.LS
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.  The default value defers to the
+package parameter of the same name.
+.LE
+observatory = "observatory"
+.LS
+Observatory at which the spectra were obtained if not specified in the
+image header by the keyword OBSERVAT.  See \fBobservatory\fR for more
+details.
+.LE
+interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc)
+.LS
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.nf
+	nearest - nearest neighbor
+	 linear - linear
+	  poly3 - 3rd order polynomial
+	  poly5 - 5th order polynomial
+	spline3 - cubic spline
+	   sinc - sinc function
+.fi
+.LE
+database = "database"
+.LS
+Database (directory) used for storing aperture and dispersion information.
+.LE
+verbose = no
+.LS
+Print verbose information available with various tasks.
+.LE
+logfile = "logfile", plotfile = ""
+.LS
+Text and plot log files.  If a filename is not specified then no log is
+kept.  The plot file contains IRAF graphics metacode which may be examined
+in various ways such as with \fBgkimosaic\fR.
+.LE
+records = ""
+.LS
+Dummy parameter to be ignored.
+.LE
+version = "SPECRED: ..."
+.LS
+Version of the package.
+.LE
+
+.ce
+PARAMS PARAMETERS
+
+The following parameters are part of the \fBparams\fR parameter set and
+define various algorithm parameters for \fBdofibers\fR.
+
+.ce
+--  GENERAL PARAMETERS --
+
+line = INDEF, nsum = 10
+.LS
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, recentering, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.LE
+order = "decreasing" (apfind)
+.LS
+When assigning aperture identifications order the spectra "increasing"
+or "decreasing" with increasing pixel position (left-to-right or
+right-to-left in a cross-section plot of the image).
+.LE
+extras = no (apsum)
+.LS
+Include extra information in the output spectra?  When cleaning or using
+variance weighting the cleaned and weighted spectra are recorded in the
+first 2D plane of a 3D image, the raw, simple sum spectra are recorded in
+the second plane, and the estimated sigmas are recorded in the third plane.
+.LE
+
+.ce
+-- DEFAULT APERTURE LIMITS --
+
+lower = -5., upper = 5. (apdefault)
+.LS
+Default lower and upper aperture limits relative to the aperture center.
+These limits are used when the apertures are first found and may be
+resized automatically or interactively.
+.LE
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+
+ylevel = 0.05 (apresize)
+.LS
+Data level at which to set aperture limits during automatic resizing.
+It is a fraction of the peak relative to a local background.
+.LE
+
+.ce
+-- TRACE PARAMETERS --
+
+t_step = 10 (aptrace)
+.LS
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \fInsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.LE
+t_function = "spline3", t_order = 3 (aptrace)
+.LS
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.LE
+t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+.LS
+Default number of rejection iterations and rejection sigma thresholds.
+
+.ce
+-- SCATTERED LIGHT PARAMETERS --
+
+buffer = 1. (apscatter)
+.LS
+Buffer distance from the aperture edges to be excluded in selecting the
+scattered light pixels to be used.
+.LE
+apscat1 = "" (apscatter)
+.LS
+Fitting parameters across the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat1"
+parameter set.
+.LE
+apscat2 = "" (apscatter)
+.LS
+Fitting parameters along the dispersion.  This references an additional
+set of parameters for the ICFIT package.  The default is the "apscat2"
+parameter set.
+.LE
+.LE
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+
+weights = "none" (apsum)
+.LS
+Type of extraction weighting.  Note that if the \fIclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+
+"none"
+.LS
+The pixels are summed without weights except for partial pixels at the
+ends.
+.LE
+"variance"
+.LS
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \fIgain\fR and \fIreadnoise\fR
+parameters.
+.LE
+.LE
+pfit = "fit1d" (apsum) (fit1d|fit2d)
+.LS
+Profile fitting algorithm for cleaning and variance weighted extractions.
+The default is generally appropriate for multifiber data but users
+may try the other algorithm.  See \fBapprofiles\fR for further information.
+.LE
+lsigma = 3., usigma = 3. (apsum)
+.LS
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.LE
+nsubaps = 1 (apsum)
+.LS
+During extraction it is possible to equally divide the apertures into
+this number of subapertures.
+.LE
+
+.ce
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --
+
+f_interactive = yes (fit1d)
+.LS
+Fit the composite one dimensional flat field spectrum interactively?
+This is used if \fIfitflat\fR is set and a two dimensional flat field
+spectrum is specified.
+.LE
+f_function = "spline3", f_order = 10 (fit1d)
+.LS
+Function and order used to fit the composite one dimensional flat field
+spectrum.  The functions are "legendre", "chebyshev", "spline1", and
+"spline3".  The spline functions are linear and cubic splines with the
+order specifying the number of pieces.
+.LE
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+
+threshold = 10. (autoidentify/identify/reidentify)
+.LS
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.LE
+coordlist = "linelists$idhenear.dat" (autoidentify/identify)
+.LS
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelists$".
+.LE
+match = -3. (autoidentify/identify)
+.LS
+The maximum difference for a match between the dispersion function prediction
+value and a wavelength in the coordinate list.
+.LE
+fwidth = 4. (autoidentify/identify)
+.LS
+Approximate full base width (in pixels) of arc lines.
+.LE
+cradius = 10. (reidentify)
+.LS
+Radius from previous position to reidentify arc line.
+.LE
+i_function = "spline3", i_order = 3 (autoidentify/identify)
+.LS
+The default function and order to be fit to the arc wavelengths as a
+function of the pixel coordinate.  The functions choices are "chebyshev",
+"legendre", "spline1", or "spline3".
+.LE
+i_niterate = 2, i_low = 3.0, i_high = 3.0 (autoidentify/identify)
+.LS
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.LE
+refit = yes (reidentify)
+.LS
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.LE
+addfeatures = no (reidentify)
+.LS
+Add new features from a line list during each reidentification?
+This option can be used to compensate for lost features from the
+reference solution.  Care should be exercised that misidentified features
+are not introduced.
+.LE
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+
+select = "interp" (refspectra)
+.LS
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+
+average
+.LS
+Average two reference spectra without regard to any sort parameter.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.
+This option is used to assign two reference spectra, with equal weights,
+independent of any sorting parameter.
+.LE
+following
+.LS
+Select the nearest following spectrum in the reference list based on the
+sorting parameter.  If there is no following spectrum use the nearest preceding
+spectrum.
+.LE
+interp
+.LS
+Interpolate between the preceding and following spectra in the reference
+list based on the sorting parameter.  If there is no preceding and following
+spectrum use the nearest spectrum.  The interpolation is weighted by the
+relative distances of the sorting parameter.
+.LE
+match
+.LS
+Match each input spectrum with the reference spectrum list in order.
+This overrides the reference aperture check.
+.LE
+nearest
+.LS
+Select the nearest spectrum in the reference list based on the sorting
+parameter.
+.LE
+preceding
+.LS
+Select the nearest preceding spectrum in the reference list based on the
+sorting parameter.  If there is no preceding spectrum use the nearest following
+spectrum.
+.LE
+.LE
+sort = "jd", group = "ljd" (refspectra)
+.LS
+Image header keywords to be used as the sorting parameter for selection
+based on order and to group spectra.
+A null string, "", or the word "none" may be use to disable the sorting
+or grouping parameters.
+The sorting parameter
+must be numeric but otherwise may be anything.  The grouping parameter
+may be a string or number and must simply be the same for all spectra within
+the same group (say a single night).
+Common sorting parameters are times or positions.
+In \fBdofibers\fR the Julian date (JD) and the local Julian day number (LJD)
+at the middle of the exposure are automatically computed from the universal
+time at the beginning of the exposure and the exposure time.  Also the
+parameter UTMIDDLE is computed.
+.LE
+time = no, timewrap = 17. (refspectra)
+.LS
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.LE
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+
+linearize = yes (dispcor)
+.LS
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling
+If no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data are not interpolated.
+.LE
+log = no (dispcor)
+.LS
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.LE
+flux = yes (dispcor)
+.LS
+Conserve the total flux during interpolation?  If \fIno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \fIyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.LE
+
+.ce
+-- SKY SUBTRACTION PARAMETERS --
+
+combine = "average" (scombine) (average|median)
+.LS
+Option for combining sky pixels at the same dispersion coordinate after any
+rejection operation.  The options are to compute the  "average" or "median"
+of the pixels.  The median uses the average of the two central
+values when the number of pixels is even.
+.LE
+reject = "none" (scombine) (none|minmax|avsigclip)
+.LS
+Type of rejection operation performed on the pixels which overlap at each
+dispersion coordinate.  The algorithms are discussed in the
+help for \fBscombine\fR.  The rejection choices are:
+
+.nf
+      none - No rejection
+    minmax - Reject the low and high pixels
+ avsigclip - Reject pixels using an averaged sigma clipping algorithm
+.fi
+
+.LE
+scale = "none" (none|mode|median|mean)
+.LS
+Multiplicative scaling to be applied to each spectrum.  The choices are none
+or scale by the mode, median, or mean.  This should not be necessary if the
+flat field and throughput corrections have been properly made. 
+.LE
+
+.ce
+ENVIRONMENT PARAMETERS
+.LP
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
diff --git a/noao/imred/specred/doc/doslit.hlp b/noao/imred/specred/doc/doslit.hlp
new file mode 100644
index 00000000..2bcf7294
--- /dev/null
+++ b/noao/imred/specred/doc/doslit.hlp
@@ -0,0 +1,1201 @@
+.help doslit Feb93 noao.imred.specred
+.ih
+NAME
+doslit -- Slit spectra data reduction task
+.ih
+USAGE
+doslit objects
+.ih
+SUMMARY
+\fBDoslit\fR extracts, sky subtracts, wavelength calibrates, and flux
+calibrates simple two dimensional slit spectra which have been processed to
+remove the detector characteristics; i.e. CCD images have been bias, dark
+count, and flat field corrected.  It is primarily intended for
+spectrophotometry or radial velocities of stellar spectra with the spectra
+aligned with one of the image axes; i.e. the assumption is that extractions
+can be done by summing along image lines or columns.  The alignment does
+not have to be precise but only close enough that the wavelength difference
+across the spectrum profiles is insignificant.  The task is available
+in the \fBctioslit\fR, \fBkpnoslit\fR, \fBkpnocoude\fR, and \fBspecred\fR
+packages.
+.ih
+PARAMETERS
+.ls objects
+List of object images to be processed.  Previously processed spectra are
+ignored unless the \fIredo\fR flag is set or the \fIupdate\fR flag is set
+and dependent calibration data has changed.  If the images contain the
+keyword IMAGETYP then only those with a value of "object" or "OBJECT"
+are used and those with a value of "comp" or "COMPARISON" are added
+to the list of arcs.  Extracted spectra are ignored.
+.le
+.ls arcs = "" (at least one if dispersion correcting)
+List of arc calibration spectra.  These spectra are used to define
+the dispersion functions.  The first spectrum is used to mark lines
+and set the dispersion function interactively and dispersion functions
+for all other arc spectra are derived from it.  If the images contain
+the keyword IMAGETYP then only those with a value of "comp" or
+"COMPARISON" are used.  All others are ignored as are extracted spectra.
+.le
+.ls arctable = "" (optional) (refspectra)
+Table defining which arc spectra are to be assigned to which object
+spectra (see \fBrefspectra\fR).  If not specified an assignment based
+on a header parameter, \fIsparams.sort\fR, such as the Julian date
+is made.
+.le
+.ls standards = "" (at least one if flux calibrating)
+List of standard star spectra.  The standard stars must have entries in
+the calibration database (package parameter \fIcaldir\fR).
+.le
+
+.ls readnoise = "rdnoise", gain = "gain" (apsum)
+Read out noise in photons and detector gain in photons per data value.
+This parameter defines the minimum noise sigma and the conversion between
+photon Poisson statistics and the data number statistics.  Image header
+keywords (case insensitive) may be specified to obtain the values from the
+image header.
+.le
+.ls datamax = INDEF (apsum.saturation)
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the standard star or
+arc spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.le
+.ls width = 5. (apedit)
+Approximate full width of the spectrum profiles.  This parameter is used
+to define a width and error radius for the profile centering algorithm.
+.le
+.ls crval = INDEF, cdelt = INDEF (autoidentify)
+These parameters specify an approximate central wavelength and dispersion.
+They may be specified as numerical values, INDEF, or image header keyword
+names whose values are to be used.
+If both these parameters are INDEF then the automatic identification will
+not be done.
+.le
+
+.ls dispcor = yes
+Dispersion correct spectra?  This may involve either defining a nonlinear
+dispersion coordinate system in the image header or resampling the
+spectra to uniform linear wavelength coordinates as selected by
+the parameter \fIsparams.linearize\fR.
+.le
+.ls extcor = no
+Extinction correct the spectra?
+.le
+.ls fluxcal = no
+Flux calibrate the spectra using standard star observations?
+.le
+.ls resize = no (apresize)
+Resize the default aperture for each object based on the spectrum profile?
+.le
+.ls clean = no (apsum)
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction.  In addition the datamax parameters
+can be useful.
+.le
+.ls splot = no
+Plot the final spectra with the task \fBsplot\fR?  In quicklook mode
+this is automatic and in non-quicklook mode it is queried.
+.le
+.ls redo = no
+Redo operations previously done?  If no then previously processed spectra
+in the object list will not be processed unless required by the
+update option.
+.le
+.ls update = no
+Update processing of previously processed spectra if the
+dispersion reference image or standard star calibration data are changed?
+.le
+.ls quicklook = no
+Extract and calibrate spectra with minimal interaction?  In quicklook mode
+only the initial dispersion function solution and standard star setup are
+done interactively.  Normally the \fIsplot\fR option is set in this mode to
+produce an automatic final spectrum plot for each object.  It is
+recommended that this mode not be used for final reductions.
+.le
+.ls batch = yes
+Process spectra as a background or batch job provided there are no interactive
+steps remaining.
+.le
+.ls listonly = no
+List processing steps but don't process?
+.le
+
+.ls sparams = "" (pset)
+Name of parameter set containing additional processing parameters.  This
+parameter is only for indicating the link to the parameter set
+\fBsparams\fR and should not be given a value.  The parameter set may be
+examined and modified in the usual ways (typically with "epar sparams"
+or ":e sparams" from the parameter editor).  The parameters are
+described below.
+.le
+
+.ce
+-- GENERAL PARAMETERS --
+.ls line = INDEF, nsum = 10
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.le
+.ls extras = no (apsum)
+Include raw unweighted and uncleaned spectra, the background spectra, and
+the estimated sigmas in a three dimensional output image format.
+See the discussion in the \fBapextract\fR package for further information.
+.le
+
+.ce
+-- DEFAULT APERTURE LIMITS --
+.ls lower = -3., upper = 3. (apdefault)
+Default lower and upper aperture limits relative to the aperture center.
+These limits are used when the apertures are first defined.
+.le
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+.ls ylevel = 0.05 (apresize)
+Fraction of the peak to set aperture limits during automatic resizing.
+.le
+
+.ce
+-- TRACE PARAMETERS --
+.ls t_step = 10 (aptrace)
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \fInsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.le
+.ls t_function = "spline3", t_order = 1 (aptrace)
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of terms in the
+polynomial functions or the number of spline pieces in the spline
+functions.
+.le
+.ls t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+Default number of rejection iterations and rejection sigma thresholds.
+.le
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+.ls weights = "none" (apsum) (none|variance)
+Type of extraction weighting.  Note that if the \fIclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+.ls "none"
+The pixels are summed without weights except for partial pixels at the
+ends.
+.le
+.ls "variance"
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \fIgain\fR and \fIreadnoise\fR
+parameters.
+.le
+.le
+.ls pfit = "fit1d" (apsum and approfile) (fit1d|fit2d)
+Type of profile fitting algorithm to use.  The "fit1d" algorithm is
+preferred except in cases of extreme tilt.
+.le
+.ls lsigma = 3., usigma = 3. (apsum)
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.le
+
+.ce
+-- DEFAULT BACKGROUND PARAMETERS --
+.ls background = "fit" (apsum) (none|average|median|minimum|fit)
+Type of background subtraction.  The choices are "none" for no background
+subtraction, "average" to average the background within the background
+regions, "median" to use the median in the background regions, "minimum" to
+use the minimum in the background regions, or "fit" to fit across the
+dispersion using the background within the background regions.  Note that
+the "average" option does not do any medianing or bad pixel checking,
+something which is recommended.  The fitting option is slower than the
+other options and requires additional fitting parameter.
+.le
+.ls b_function = "legendre", b_order = 1 (apsum)
+Default background fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.le
+.ls b_sample = "-10:-6,6:10" (apsum)
+Default background sample.  The sample is given by a set of colon separated
+ranges each separated by either whitespace or commas.  The string "*" refers
+to all points.  Note that the background coordinates are relative to the
+aperture center and not image pixel coordinates so the endpoints need not
+be integer.  It is recommended that the background regions be examined
+and set interactively with the 'b' key in the interactive aperture
+definition mode.  This requires \fIquicklook\fR to be no.
+.le
+.ls b_naverage = -100 (apsum)
+Default number of points to average or median.  Positive numbers
+average that number of sequential points to form a fitting point.
+Negative numbers median that number, in absolute value, of sequential
+points.  A value of 1 does no averaging and each data point is used in the
+fit.
+.le
+.ls b_niterate = 1 (apsum)
+Default number of rejection iterations.  If greater than zero the fit is
+used to detect deviant fitting points and reject them before repeating the
+fit.  The number of iterations of this process is given by this parameter.
+.le
+.ls b_low_reject = 3., b_high_reject = 3. (apsum)
+Default background lower and upper rejection sigmas.  If greater than zero
+points deviating from the fit below and above the fit by more than this
+number of times the sigma of the residuals are rejected before refitting.
+.le
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+.ls threshold = 10. (autoidentify/identify/reidentify)
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.le
+.ls coordlist = "linelists$idhenear.dat" (autoidentify/identify)
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelists$".
+.le
+.ls match = -3. (autoidentify/identify)
+The maximum difference for a match between the dispersion function computed
+value and a wavelength in the coordinate list.
+.le
+.ls fwidth = 4. (autoidentify/identify)
+Approximate full base width (in pixels) of arc lines.
+.le
+.ls cradius = 10. (reidentify)
+Radius from previous position to reidentify arc line.
+.le
+.ls i_function = "spline3", i_order = 1 (autoidentify/identify)
+The default function and order to be fit to the arc wavelengths as a
+function of the pixel coordinate.  The functions choices are "chebyshev",
+"legendre", "spline1", or "spline3".
+.le
+.ls i_niterate = 0, i_low = 3.0, i_high = 3.0 (autoidentify/identify)
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.le
+.ls refit = yes (reidentify)
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the initial arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.le
+.ls addfeatures = no (reidentify)
+Add new features from a line list during each reidentification?
+This option can be used to compensate for lost features from the
+reference solution.  Care should be exercised that misidentified features
+are not introduced.
+.le
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+.ls select = "interp" (refspectra)
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+.ls average
+Average two reference spectra without regard to any
+sort or group parameters.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.  There is no checking of the
+group values.
+.le
+.ls following
+Select the nearest following spectrum in the reference list based on the
+sort and group parameters.  If there is no following spectrum use the
+nearest preceding spectrum.
+.le
+.ls interp
+Interpolate between the preceding and following spectra in the reference
+list based on the sort and group parameters.  If there is no preceding and
+following spectrum use the nearest spectrum.  The interpolation is weighted
+by the relative distances of the sorting parameter (see cautions in
+DESCRIPTION section).
+.le
+.ls match
+Match each input spectrum with the reference spectrum list in order.
+This overrides any group values.
+.le
+.ls nearest
+Select the nearest spectrum in the reference list based on the sort and
+group parameters.
+.le
+.ls preceding
+Select the nearest preceding spectrum in the reference list based on the
+sort and group parameters.  If there is no preceding spectrum use the
+nearest following spectrum.
+.le
+.le
+.ls sort = "jd" (setjd and refspectra)
+Image header keyword to be used as the sorting parameter for selection
+based on order.  The header parameter must be numeric but otherwise may
+be anything.  Common sorting parameters are times or positions.
+.le
+.ls group = "ljd" (setjd and refspectra)
+Image header keyword to be used to group spectra.  For those selection
+methods which use the group parameter the reference and object
+spectra must have identical values for this keyword.  This can
+be anything but it must be constant within a group.  Common grouping
+parameters are the date of observation "date-obs" (provided it does not
+change over a night) or the local Julian day number.
+.le
+.ls time = no, timewrap = 17. (refspectra)
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.le
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+.ls linearize = yes (dispcor)
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling using
+the linear dispersion parameters specified by other parameters.  If
+no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data is not interpolated.  Note the interpolation
+function type is set by the package parameter \fIinterp\fR.
+.le
+.ls log = no (dispcor)
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.le
+.ls flux = yes (dispcor)
+Conserve the total flux during interpolation?  If \fIno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \fIyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.le
+
+.ce
+-- SENSITIVITY CALIBRATION PARAMETERS --
+.ls s_function = "spline3", s_order = 1 (sensfunc)
+Function and order used to fit the sensitivity data.  The function types
+are "chebyshev" polynomial, "legendre" polynomial, "spline3" cubic spline,
+and "spline1" linear spline.  Order of the sensitivity fitting function.
+The value corresponds to the number of polynomial terms or the number of
+spline pieces.  The default values may be changed interactively.
+.le
+.ls fnu = no (calibrate)
+The default calibration is into units of F-lambda. If \fIfnu\fR = yes then
+the calibrated spectrum will be in units of F-nu.
+.le
+
+.ce
+PACKAGE PARAMETERS
+
+The following package parameters are used by this task.  The default values
+may vary depending on the package.
+.ls dispaxis = 2
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.  The default value defers to the
+package parameter of the same name.
+.le
+.ls extinction (standard, sensfunc, calibrate)
+Extinction file for a site.  There are two extinction files in the
+NOAO standards library, onedstds$, for KPNO and CTIO.  These extinction
+files are used for extinction and flux calibration.
+.le
+.ls caldir (standard)
+Standard star calibration directory.  A directory containing standard
+star data files.  Note that the directory name must end with '/'.
+There are a number of standard star calibrations directories in the NOAO
+standards library, onedstds$.
+.le
+.ls observatory = "observatory" (observatory)
+The default observatory to use for latitude dependent computations.
+If the OBSERVAT keyword in the image header it takes precedence over
+this parameter.
+.le
+.ls interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc) (dispcor)
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.nf
+	nearest - nearest neighbor
+	 linear - linear
+	  poly3 - 3rd order polynomial
+	  poly5 - 5th order polynomial
+	spline3 - cubic spline
+	   sinc - sinc function
+.fi
+.le
+.ls database = "database"
+Database name used by various tasks.  This is a directory which is created
+if necessary.
+.le
+.ls verbose = no
+Verbose output?  If set then almost all the information written to the
+logfile is also written to the terminal except when the task is a
+background or batch process.
+.le
+.ls logfile = "logfile"
+If specified detailed text log information is written to this file.
+.le
+.ls plotfile = ""
+If specified metacode plots are recorded in this file for later review.
+Since plot information can become large this should be used only if
+really desired.
+.le
+.ih
+ENVIRONMENT PARAMETERS
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
+.ih
+DESCRIPTION
+\fBDoslit\fR extracts, sky subtracts, wavelength calibrates, and flux
+calibrates simple two dimensional slit spectra which have been processed to
+remove the detector characteristics; i.e. CCD images have been bias, dark
+count, and flat field corrected.  It is primarily intended for
+spectrophotometry or radial velocities of stellar spectra with the spectra
+aligned with one of the image axes; i.e. the assumption is that extractions
+can be done by summing along image lines or columns.  The alignment does
+not have to be precise but only close enough that the wavelength difference
+across the spectrum profiles is insignificant.  Extended objects requiring
+accurate geometric alignment over many pixels are reduced using the
+\fBlongslit\fR package.
+
+The task is a command language script which collects and combines the
+functions and parameters of many general purpose tasks to provide a single,
+complete data reduction path and a degree of guidance, automation, and
+record keeping.  In the following description and in the parameter section
+the various general tasks used are identified.  Further
+information about those tasks and their parameters may be found in their
+documentation.  \fBDoslit\fR also simplifies and consolidates parameters
+from those tasks and keeps track of previous processing to avoid
+duplications.
+
+The general organization of the task is to do the interactive setup steps,
+such as the reference dispersion function
+determination, first using representative calibration data and then perform
+the majority of the reductions automatically, possibly as a background
+process, with reference to the setup data.  In addition, the task
+determines which setup and processing operations have been completed in
+previous executions of the task and, contingent on the \fIredo\fR and
+\fIupdate\fR options, skip or repeat some or all the steps.
+
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage
+since there are many variations possible.
+
+\fBUsage Outline\fR
+
+.ls 6 [1]
+The images are first processed with \fBccdproc\fR for overscan,
+zero level, dark count, and flat field corrections.
+.le
+.ls [2]
+Set the \fBdoslit\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed,
+one or more arc images, and one or more standard
+star images.  If there are many object, arc, or standard star images
+you might prepare "@ files".  Set the detector and data
+specific parameters.  Select the processing options desired.
+Finally you might wish to review the \fIsparams\fR algorithm parameters
+though the defaults are probably adequate.
+.le
+.ls [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the current execution and no further queries of that
+type will be made.
+.le
+.ls [4]
+Apertures are defined for all the standard and object images.  This is only
+done if there are no previous aperture definitions for the image.
+The highest peak is found and centered and the default aperture limits
+are set.  If the resize option is set the aperture is resized by finding
+the level which  is 5% (the default) of the peak above local background.
+If not using the quicklook option you now have the option
+of entering the aperture editing loop to check the aperture position,
+size, and background fitting parameters, and possibly add additional
+apertures.  This is step is highly recommended.
+It is important to check the background regions with the 'b'
+key.  To exit the background mode and then
+to exit the review mode use 'q'.
+
+The spectrum positions at a series of points along the dispersion are
+measured and a function is fit to these positions.  If not using the
+quicklook option the traced positions may be examined interactively and the
+fitting parameters adjusted.  To exit the interactive fitting type 'q'.
+.le
+.ls [5]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  The dispersion function is defined using the task
+\fBautoidentify\fR.  The \fIcrval\fR and \fIcdelt\fR parameters are used in
+the automatic identification.  Whether or not the automatic identification
+is successful you will be shown the result of the arc line identification.
+If the automatic identification is not successful identify a few arc lines
+with with 'm' and use the 'l' line list identification command to
+automatically add additional lines and fit the dispersion function.  Check
+the quality of the dispersion function fit with 'f'.  When satisfied exit
+with 'q'.
+.le
+.ls [6]
+If the flux calibration option is selected the standard star spectra are
+processed (if not done previously).  The images are
+extracted and wavelength calibrated.  The appropriate arc
+calibration spectra are extracted and the dispersion function refit
+using the arc reference spectrum as a starting point.  The standard star
+fluxes through the calibration bandpasses are compiled.  You are queried
+for the name of the standard star calibration data file.
+
+After all the standard stars are processed a sensitivity function is
+determined using the interactive task \fBsensfunc\fR.  Finally, the
+standard star spectra are extinction corrected and flux calibrated
+using the derived sensitivity function.
+.le
+.ls [7]
+The object spectra are now automatically
+extracted, wavelength calibrated, and flux calibrated.
+.le
+.ls [8]
+The option to examine the final spectra with \fBsplot\fR may be given.
+To exit type 'q'.  In quicklook mode the spectra are plotted
+noninteractively with \fBbplot\fR.
+.le
+.ls [9]
+The final spectra will have the same name as the original 2D images
+with a ".ms" extension added.
+.le
+
+\fBSpectra and Data Files\fR
+
+The basic input consists of two dimensional slit object, standard star, and
+arc calibration spectra stored as IRAF images.
+The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+The raw CCD images must be
+processed to remove overscan, bias, dark count, and flat field effects.
+This is generally done using the \fBccdred\fR package.  Lines of constant
+wavelength should be closely aligned with one of the image axes though a
+small amount of misalignment only causes a small loss of resolution.  For
+large misalignments one may use the \fBrotate\fR task.  More complex
+geometric problems and observations of extended objects should be handled
+by the \fBlongslit\fR package.
+
+The arc
+spectra are comparison arc lamp observations (they must all be of the same
+type).  The assignment of arc calibration exposures to object exposures is
+generally done by selecting the nearest in time and interpolating.
+However, the optional \fIarc assignment table\fR may be used to explicitly
+assign arc images to specific objects.  The format of this file is
+described in task \fBrefspectra\fR.
+
+The final reduced spectra are recorded in one, two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ms" extension.  Each line in the reduced image is a one dimensional
+spectrum with associated aperture, wavelength, and identification
+information.  With a single aperture the image will be one dimensional
+and with multiple apertures the image will be two dimensional.
+When the \fIextras\fR parameter is set the images will be three
+dimensional (regardless of the number of apertures) and the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tasks such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.
+
+\fBPackage Parameters\fR
+
+The package parameters set parameters which change
+infrequently and set the standard I/O functions.  The extinction file
+is used for making extinction corrections and the standard star
+calibration directory is used for determining flux calibrations from
+standard star observations.  The calibration directories contain data files
+with standard star fluxes and band passes.  The available extinction
+files and flux calibration directories may be listed using the command:
+.nf
+
+	cl> help onedstds
+
+.fi
+
+The extinction correction requires computation of an air mass using the
+task \fBsetairmass\fR.  The air mass computation needs information
+about the observation and, in particular, the latitude of the observatory.
+This is determined using the OBSERVAT image header keyword.  If this
+keyword is not present the observatory parameter is used.  See the
+task \fBobservatory\fR for more on defining the observatory parameters.
+
+The spectrum interpolation type is used whenever a spectrum needs to be
+resampled for linearization or performing operations between spectra
+with different sampling.  The "sinc" interpolation may be of interest
+as an alternative but see the cautions given in \fBonedspec.package\fR.
+
+The general direction in which the spectra run is specified by the
+dispersion axis parameter.  Recall that ideally it is the direction
+of constant wavelength which should be aligned with an image axis and
+the dispersion direction may not be exactly aligned because atmospheric
+dispersion.
+
+The verbose parameter selects whether to print everything which goes
+into the log file on the terminal.  It is useful for monitoring
+what the \fBdoslit\fR task does.  The log and plot files are useful for
+keeping a record of the processing.  A log file is highly recommended.
+A plot file provides a record of the apertures, traces, and extracted
+spectra but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+
+\fBProcessing Parameters\fR
+
+The input images are specified by image lists.  The lists may be
+a list of explicit comma separate image names, @ files, or image
+templates using pattern matching against file names in the directory.
+To allow wildcard image lists to be used safely and conveniently the
+image lists are checked to remove extracted images (the .ms images)
+and to automatically identify object and arc spectra.  Object and arc
+images are identified by the keyword IMAGETYP with values of "object",
+"OBJECT", "comp", or "COMPARISON" (the current practice at NOAO).
+If arc images are found in the object list they are transferred to the
+arc list while if object images are found in the arc list they are ignored.
+All other image types, such as biases, darks, or flat fields, are
+ignored.  This behavior allows simply specifying all images with a wildcard
+in the object list with automatic selections of arc spectra or a
+wildcard in the arc list to automatically find the arc spectra.
+If the data lack the identifying information it is up to the user
+to explicitly set the proper lists.
+
+The arc assignment table is a file which may be used to assign
+specific arc spectra to specific object and standard star spectra.
+For more on this option see \fBrefspectra\fR.
+
+The next set of parameters describe the noise characteristics and
+spectrum characteristics.  The read out noise and gain are used when
+"cleaning" cosmic rays and when using variance or optimal weighting.  These
+parameters must be fairly accurate.  Note that these are the effective
+parameters and must be adjusted if previous processing has modified the
+pixel values; such as with an unnormalized flat field.
+The variance
+weighting and cosmic-ray cleanning are sensitive to extremely strong
+cosmic-rays; ones which are hundreds of times brighter than the
+spectrum.  The \fIdatamax\fR is used to set an upper limit for any
+real data.  Any pixels above this value will be flagged as cosmic-rays
+and will not affect the extractions.
+
+The profile width should be approximately the full width
+at the profile base.  This parameter is used for centering and tracing
+of the spectrum profiles.
+
+The approximate central wavelength and dispersion are used for the
+automatic identification of the arc reference.  They may be specified
+as image header keywords or values.  The INDEF values search the
+entire range of the coordinate reference file but the automatic
+line identification algorithm works much better and faster if
+approximate values are given.
+
+The next set of parameters select the processing steps and options.  The
+various calibration steps may be done simultaneously, that is at the same
+time as the basic extractions, or in separate executions of the task.
+Typically, all the desired operations are done at the same time.
+Dispersion correction requires at least one arc spectrum and flux
+calibration requires dispersion correction and at least one standard star
+observation.
+
+The \fIresize\fR option resets the edges of the extraction aperture based
+on the profile for each object and standard star image.  The default
+resizing is to the 5% point relative to the peak measured above the
+background.  This allows following changes in the seeing.  However, one
+should consider the consequences of this if attempting to flux calibrate
+the observations.  Except in quicklook mode, the apertures for each object
+and standard star observation may be reviewed graphically and
+adjustments made to the aperture width and background regions.
+
+The \fIclean\fR option invokes a profile
+fitting and deviant point rejection algorithm as well as a variance weighting
+of points in the aperture.  See the next section for more about
+requirements to use this option.
+
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\fIupdate\fR flag is set.  The changes which will cause an update are a
+new arc reference image and new standard stars.  If all input spectra are to be
+processed regardless of previous processing the \fIredo\fR flag may be
+used.  Note that reprocessing clobbers the previously processed output
+spectra.
+
+The final step is to plot the spectra if the \fIsplot\fR option is
+selected.  In non-quicklook mode there is a query which may be
+answered either in lower or upper case.  The plotting uses the interactive
+task \fBsplot\fR.  In quicklook mode the plot appears noninteractively
+using the task \fBbplot\fR.  
+
+The \fIquicklook\fR option provides a simpler, less interactive, mode.
+In quicklook mode a single aperture is defined using default parameters
+without interactive aperture review or trace fitting and
+the \fIsplot\fR option selects a noninteractive plot to be
+shown at the end of processing of each object and standard star
+spectrum.  While the algorithms used in quicklook mode are nearly the same
+as in non-quicklook mode and the final results may be the same it is
+recommended that the greater degree of monitoring and review in
+non-quicklook mode be used for careful final reductions.
+
+The batch processing option allows object spectra to be processed as a
+background or batch job.  This will occur only if the interactive
+\fIsplot\fR option is not active; either not set, turned off during
+processing with "NO", or in quicklook mode.  In batch processing the
+terminal output is suppressed.
+
+The \fIlistonly\fR option prints a summary of the processing steps
+which will be performed on the input spectra without actually doing
+anything.  This is useful for verifying which spectra will be affected
+if the input list contains previously processed spectra.  The listing
+does not include any arc spectra which may be extracted to dispersion
+calibrate an object spectrum.
+
+The last parameter (excluding the task mode parameter) points to
+another parameter set for the algorithm parameters.  The default
+parameter set is called \fIsparams\fR.  The algorithm parameters are
+discussed further in the next section.
+
+\fBAlgorithms and Algorithm Parameters\fR
+
+This section summarizes the various algorithms used by the
+\fBdoslit\fR task and the parameters which control and modify the
+algorithms.  The algorithm parameters available to you are
+collected in the parameter set \fBsparams\fR.  These parameters are
+taken from the various general purpose tasks used by the \fBdoslit\fR
+processing task.  Additional information about these parameters and
+algorithms may be found in the help for the actual
+task executed.  These tasks are identified below.  The aim of this
+parameter set organization is to collect all the algorithm parameters
+in one place separate from the processing parameters and include only
+those which are relevant for slit data.  The parameter values
+can be changed from the defaults by using the parameter editor,
+.nf
+
+cl> epar sparams
+
+.fi
+or simple typing \fIsparams\fR.
+The parameter editor can also be entered when editing the \fBdoslit\fR
+parameters by typing \fI:e\fR when positioned at the \fIsparams\fR
+parameter.
+
+\fBAperture Definitions\fR
+
+The first operation is to define the extraction apertures, which include the
+aperture width, background regions, and position dependence with
+wavelength, for the input slit spectra and, if flux calibration is
+selected, the standard star spectra.  This is done only for spectra which
+do not have previously defined apertures unless the \fIredo\fR option is
+set to force all definitions to be redone.  Thus, apertures may be
+defined separately using the \fBapextract\fR tasks.  This is particularly
+useful if one needs to use reference images to define apertures for very
+weak spectra which are not well centered or traced by themselves.
+
+Initially a single spectrum is found and a default aperture defined
+automatically.  If the \fIresize\fR parameter is set the aperture width is
+adjusted to a specified point on the spectrum profile (see
+\fBapresize\fR).  If not in "quicklook" mode (set by the \fIquicklook\fR
+parameter) a query is printed to select whether to inspect and modify the
+aperture and background aperture definitions using the commands described
+for \fBapedit\fR.  This option allows adding
+apertures for other objects on the slit and adjusting
+background regions to avoid contaminating objects.  The query may be
+answered in lower case for a single spectrum or in upper case to
+permanently set the response for the duration of the task execution.  This
+convention for query responses is used throughout the task.  It is
+recommended that quicklook only be used for initial quick extractions and
+calibration and that for final reductions one at least review the aperture
+definitions and traces.
+
+The initial spectrum finding and aperture definitions are done at a specified
+line or column.  The positions of the spectrum at a set of other lines or
+columns is done next and a smooth function is fit to define the aperture
+centers at all points in the image.  In non-quicklook mode the user has the
+option to review and adjust the function fitting parameters and delete bad
+position determinations.  As with the initial aperture review there is a
+query which may be answered either in lower or upper case.
+
+The above steps are all performed using tasks from the \fBapextract\fR
+package and parameters from the \fBsparams\fR parameters.  As a quick
+summary, the dispersion direction of the spectra are determined from the
+package \fBdispaxis\fR parameter if not defined in the image header.  The default
+line or column for finding the object position on the slit and the number
+of image lines or columns to sum are set by the \fIline\fR and \fInsum\fR
+parameters.  A line of INDEF (the default) selects the middle of the image.
+The automatic finding algorithm is described for the task
+\fBapfind\fR and is basically finds the strongest peak.  The default
+aperture size, background parameters, and resizing are described in
+the tasks \fBapdefault\fR and \fBapresize\fR and the
+parameters used are also described there.
+The tracing is done as described in \fBaptrace\fR and consists of
+stepping along the image using the specified \fIt_step\fR parameter.  The
+function fitting uses the \fBicfit\fR commands with the other parameters
+from the tracing section.
+
+\fBExtraction\fR
+
+The actual extraction of the spectra is done by summing across the
+fixed width apertures at each point along the dispersion.
+The default is to simply sum the pixels using
+partial pixels at the ends.  There is an option to weight the
+sum based on a Poisson variance model using the \fIreadnoise\fR and
+\fIgain\fR detector parameters.  Note that if the \fIclean\fR
+option is selected the variance weighted extraction is used regardless
+of the \fIweights\fR parameter.  The sigma thresholds for cleaning
+are also set in the \fBsparams\fR parameters.
+
+The cleaning and variance weighting options require knowing the effective
+(i.e. accounting for any image combining) read out noise and gain.  These
+numbers need to be adjusted if the image has been processed such that the
+intensity scale has a different origin (such as applying a separate
+background subtraction operation) or scaling (such as caused by
+unnormalized flat fielding).  These options also require using background
+subtraction if the profile does not go to zero.  For optimal extraction and
+cleaning to work it is recommended that any flat fielding be done using
+normalized flat fields (as is done in \fBccdproc\fR) and using background
+subtraction if there is any appreciable sky.  For further discussion of
+cleaning and variance weighted extraction see \fBapvariance\fR and
+\fBapprofiles\fR as well as  \fBapsum\fR.
+
+Background sky subtraction is done during the extraction based on
+background regions and parameters defined by the default parameters or
+changed during the interactive setting of the apertures.  The background
+subtraction options are to do no background subtraction, subtract the
+average, median, or minimum of the pixels in the background regions, or to
+fit a function and subtract the function from under the extracted object
+pixels.  The background regions are specified in pixels from
+the aperture center and follow changes in center of the spectrum along the
+dispersion.  The syntax is colon separated ranges with multiple ranges
+separated by a comma or space.  The background fitting uses the \fBicfit\fR
+routines which include medians, iterative rejection of deviant points, and
+a choice of function types and orders.  Note that it is important to use a
+method which rejects cosmic rays such as using either medians over all the
+background regions (\fIbackground\fR = "median") or median samples during
+fitting (\fIb_naverage\fR < -1).  The background subtraction algorithm and
+options are described in greater detail in \fBapsum\fR and
+\fBapbackground\fR.
+
+\fBDispersion Correction\fR
+
+If dispersion correction is not selected, \fIdispcor\fR=no, then the object
+spectra are simply extracted.  The extracted spectra may be plotted
+by setting the \fIsplot\fR option.  This produces a query and uses
+the interactive \fBsplot\fR task in non-quicklook mode and uses the
+noninteractive \fBbplot\fR task in quicklook mode.
+
+Dispersion corrections are applied to the extracted spectra if the
+\fIdispcor\fR processing parameter is set.  There are three basic steps
+involved; determining the dispersion functions relating pixel position to
+wavelength, assigning the appropriate dispersion function to a particular
+observation, and either storing the nonlinear dispersion function in the
+image headers or resampling the spectra to evenly spaced pixels in
+wavelength.
+
+The first arc spectrum in the arc list is used to define the reference
+dispersion solution.  It is extracted at middle of the image with no
+tracing.  Note extractions of arc spectra are not background subtracted.
+The task \fBautoidentify\fR is attempts to define the dispersion function
+automatically using the \fIcrval\fR and \fIcdelt\fR parameters.  Whether or
+not it is successful the user is presented with the interactive
+identification graph.  The automatic identifications can be reviewed and a
+new solution or corrections to the automatic solution may be performed.
+
+The arc dispersion function parameters are for \fBautoidentify\fR and it's
+related partner \fBreidentify\fR.  The parameters define a line list for
+use in automatically assigning wavelengths to arc lines, a centering width
+(which should match the line widths at the base of the lines), the
+dispersion function type and orders, parameters to exclude bad lines from
+function fits, and defining whether to refit the dispersion function as
+opposed to simply determining a zero point shift.  The defaults should
+generally be adequate and the dispersion function fitting parameters may be
+altered interactively.  One should consult the help for the two tasks for
+additional details of these parameters and the interactive operation of
+\fBautoidentify\fR.
+
+The extracted reference arc spectrum is then dispersion corrected.
+If the spectra are to be linearized, as set by the \fIlinearize\fR
+parameter, the default linear wavelength parameters are printed and
+you have the option to adjust them.  The dispersion system defined at
+this point will be applied automatically to all other spectra as they
+are dispersion corrected.
+
+Once the reference dispersion function is defined other arc spectra are
+extracted as required by the object spectra.  The assignment of arcs is
+done either explicitly with an arc assignment table (parameter
+\fIarctable\fR) or based on a header parameter such as a time.
+This assignments are made by the task
+\fBrefspectra\fR.  When two arcs are assigned to an object spectrum an
+interpolation is done between the two dispersion functions.  This makes an
+approximate correction for steady drifts in the dispersion.
+
+The tasks \fBsetjd\fR and \fBsetairmass\fR are automatically run on all
+spectra.  This computes and adds the header parameters for the Julian date
+(JD), the local Julian day number (LJD), the universal time (UTMIDDLE), and
+the air mass at the middle of the exposure.  The default arc assignment is
+to use the Julian date grouped by the local Julian day number.  The
+grouping allows multiple nights of data to be correctly assigned at the
+same time.
+
+The assigned arc spectra are then extracted using the object aperture
+definitions (but without background subtraction or cleaning) so that the
+same pixels on the detector are used.  The extracted arc spectra are then
+reidentified automatically against the reference arc spectrum.  Some
+statistics of the reidentification are printed (if not in batch mode) and
+the user has the option of examining the lines and fits interactively if
+not in quicklook mode.  The task which does the reidentification is called
+\fBreidentify\fR.
+
+The last step of dispersion correction is setting the dispersion
+of the object image from the arc images.  There are two choices here.
+If the \fIlinearize\fR parameter is not set the nonlinear dispersion
+function is stored in the image header.  Other IRAF tasks interpret
+this information when dispersion coordinates are needed for plotting
+or analysis.  This has the advantage of not requiring the spectra
+to be interpolated and the disadvantage that the dispersion
+information is only understood by IRAF tasks and cannot be readily
+exported to other analysis software.
+
+If the \fIlinearize\fR parameter is set then the spectra are resampled to a
+linear dispersion relation either in wavelength or the log of the
+wavelength using the dispersion coordinate system defined previously
+for the arc reference spectrum.
+
+The linearization algorithm parameters allow selecting the interpolation
+function type, whether to conserve flux per pixel by integrating across the
+extent of the final pixel, and whether to linearize to equal linear or
+logarithmic intervals.  The latter may be appropriate for radial velocity
+studies.  The default is to use a fifth order polynomial for interpolation,
+to conserve flux, and to not use logarithmic wavelength bins.  These
+parameters are described fully in the help for the task \fBdispcor\fR which
+performs the correction.
+
+\fBFlux Calibration\fR
+
+Flux calibration consists of an extinction correction and an instrumental
+sensitivity calibration.  The extinction correction only depends on the
+extinction function defined by the package parameter \fIextinct\fR and
+determination of the airmass from the header parameters (the air mass is
+computed by \fBsetairmass\fR as mentioned earlier).  The sensitivity
+calibration depends on a sensitivity calibration spectrum determined from
+standard star observations for which there are tabulated absolute fluxes.
+The task that applies both the extinction correction and sensitivity
+calibration to each extracted object spectrum is \fBcalibrate\fR.  Consult
+the manual page for this task for more information.
+
+Generation of the sensitivity calibration spectrum is done before
+processing any object spectra since it has two interactive steps and
+requires all the standard star observations.  The first step is tabulating
+the observed fluxes over the same bandpasses as the calibrated absolute
+fluxes.  The standard star tabulations are done after each standard star is
+extracted and dispersion corrected.  You are asked for the name of the
+standard star as tabulated in the absolute flux data files in the directory
+\fIcaldir\fR defined by the package parameters.
+The tabulation of the standard star
+observations over the standard bandpasses is done by the task
+\fBstandard\fR.  The tabulated data is stored in the file \fIstd\fR.  Note
+that if the \fIredo\fR flag is not set any new standard stars specified in
+subsequent executions of \fBdoslit\fR are added to the previous data in
+the data file, otherwise the file is first deleted.  Modification of the
+tabulated standard star data, such as by adding new stars, will cause any
+spectra in the input list which have been previously calibrated to be
+reprocessed if the \fIupdate\fR flag is set.
+
+After the standard star calibration bandpass fluxes are tabulated the
+information from all the standard stars is combined to produce a
+sensitivity function for use by \fBcalibrate\fR.  The sensitivity function
+determination is interactive and uses the task \fBsensfunc\fR.  This task
+allows fitting a smooth sensitivity function to the ratio of the observed
+to calibrated fluxes verses wavelength.  The types of manipulations one
+needs to do include deleting bad observations, possibly removing variable
+extinction (for poor data), and possibly deriving a revised extinction
+function.  This is a complex operation and one should consult the manual
+page for \fBsensfunc\fR.  The sensitivity function is saved as a one
+dimensional spectrum with the name \fIsens\fR.  Deletion of this image
+will also cause reprocessing to occur if the \fIupdate\fR flag is set.
+.ih
+EXAMPLES
+1.  The following example uses artificial data and may be executed
+at the terminal (with IRAF V2.10).  This is similar to the sequence
+performed by the test procedure "demos doslit".  The output is with
+the verbose package parameter set.  Normally users use \fBeparam\fR
+rather than the long command line.  All parameters not shown
+for \fBsparams\fR and \fBdoslit\fR are the default.
+
+.nf
+cl> demos mkdoslit
+Creating example longslit in image demoarc1 ...
+Creating example longslit in image demoobj1 ...
+Creating example longslit in image demostd1 ...
+Creating example longslit in image demoarc2 ...
+cl> doslit demoobj1 arcs=demoarc1,demoarc2 stand=demostd1 \
+>>> extcor=yes, fluxcal=yes resize=yes
+Searching aperture database ...
+Finding apertures ...
+Jan 17 15:52: FIND - 1 apertures found for demoobj1
+Resizing apertures ...
+Jan 17 15:52: APRESIZE  - 1 apertures resized for demoobj1 (-3.50, 3.49)
+Edit apertures for demostd1?  (yes):
+<Check aperture and background definitions ('b').  Exit with 'q'>
+Fit traced positions for demostd1 interactively?  (yes):  
+Tracing apertures ...
+Fit curve to aperture 1 of demostd1 interactively  (yes):
+<Exit with 'q'>
+Searching aperture database ...
+Finding apertures ...
+Jan 17 15:54: FIND - 1 apertures found for demostd1
+Resizing apertures ...
+Jan 17 15:54: APRESIZE  - 1 apertures resized for demostd1 (-3.35, 3.79)
+Edit apertures for demostd1?  (yes):
+<Exit with 'q'>
+Fit traced positions for demostd1 interactively?  (yes): n
+Tracing apertures ...
+Jan 17 15:55: TRACE - 1 apertures traced in demostd1.
+Jan 17 15:55: DATABASE - 1 apertures for demostd1 written to database
+Extract arc reference image demoarc1
+Searching aperture database ...
+Finding apertures ...
+Jan 17 15:55: FIND - 1 apertures found for demoarc1
+Jan 17 15:55: DATABASE - 1 apertures for demoarc1 written to database
+Extracting apertures ...
+Jan 17 15:55: EXTRACT - Aperture 1 from demoarc1 --> demoarc1.ms
+Determine dispersion solution for demoarc1
+<A dispersion function is automatically determined.>
+<Type 'f' to see the fit residuals>
+<Type 'd' to delete the two deviant lines>
+<Type 'f' to refit with the bad points deleted>
+<Type 'q' to quit fit and then 'q' to exit>
+demoarc1.ms.imh: w1 = 4204.18..., w2 = 7355.37..., dw = 6.16..., nw = 512
+  Change wavelength coordinate assignments? (yes|no|NO) (no): n
+Extract standard star spectrum demostd1
+Searching aperture database ...
+Jan 17 15:59: DATABASE  - 1 apertures read for demostd1 from database
+Extracting apertures ...
+Jan 17 15:59: EXTRACT - Aperture 1 from demostd1 --> demostd1.ms
+Assign arc spectra for demostd1
+[demostd1] refspec1='demoarc1 0.403'
+[demostd1] refspec2='demoarc2 0.597'
+Extract and reidentify arc spectrum demoarc1
+Searching aperture database ...
+Jan 17 15:59: DATABASE  - 1 apertures read for demostd1 from database
+Jan 17 15:59: DATABASE - 1 apertures for demoarc1 written to database
+Extracting apertures ...
+Jan 17 15:59: EXTRACT - Aperture 1 from demoarc1 --> demostd1demoarc1.ms
+
+REIDENTIFY: NOAO/IRAF V2.10BETA valdes@puppis Fri 15:59:21 17-Jan-92
+  Reference image = demoarc1.ms, New image = demostd1..., Refit = yes
+Image Data    Found     Fit Pix Shift  User Shift  Z Shift      RMS
+demo...       48/48   48/48    2.22E-4     0.00184  5.09E-7    0.225
+Fit dispersion function interactively? (no|yes|NO|YES) (yes):
+demoarc1.ms: w1 = 4211.81, w2 = 7353.58, dw = 6.148, nw = 512, log = no
+  Change wavelength coordinate assignments? (yes|no|NO): N
+demo... 48/48   48/48    2.22E-4     0.00184  5.09E-7    0.225
+Extract and reidentify arc spectrum demoarc2
+Searching aperture database ...
+Jan 17 16:01: DATABASE  - 1 apertures read for demostd1 from database
+Jan 17 16:01: DATABASE - 1 apertures for demoarc2 written to database
+Extracting apertures ...
+Jan 17 16:01: EXTRACT - Aperture 1 from demoarc2 --> demostd1demoarc2.ms
+
+REIDENTIFY: NOAO/IRAF V2.10BETA valdes@puppis Fri 16:01:54 17-Jan-92
+  Reference image = demoarc1.ms, New image = demostd1..., Refit = yes
+Image Data    Found     Fit Pix Shift  User Shift  Z Shift      RMS
+demo...       48/48   48/48    0.00302      0.0191  3.82E-6    0.244
+Dispersion correct demostd1
+demostd1.ms: ap = 1, w1 = 4204.181, w2 = 7355.375, dw = 6.16..., nw = 512
+Compile standard star fluxes for demostd1
+Star name in calibration list: hz2 <in kpnoslit package>
+demostd1.ms.imh[1]: Example artificial long slit image
+Compute sensitivity function
+Fit aperture 1 interactively? (no|yes|NO|YES) (no|yes|NO|YES) (yes):
+<Exit with 'q'>
+Sensitivity function for all apertures --> sens
+Flux and/or extinction calibrate standard stars
+[demostd1.ms.imh][1]: Example artificial long slit image
+  Extinction correction applied
+  Flux calibration applied
+Extract object spectrum demoobj1
+Searching aperture database ...
+Jan 17 16:05: DATABASE  - 1 apertures read for demoobj1 from database
+Extracting apertures ...
+Jan 17 16:05: EXTRACT - Aperture 1 from demoobj1 --> demoobj1.ms
+Assign arc spectra for demoobj1
+[demoobj1] refspec1='demoarc1 0.403'
+[demoobj1] refspec2='demoarc2 0.597'
+Extract and reidentify arc spectrum demoarc1
+Searching aperture database ...
+Jan 17 16:05: DATABASE  - 1 apertures read for demoobj1 from database
+Jan 17 16:05: DATABASE - 1 apertures for demoarc1 written to database
+Extracting apertures ...
+Jan 17 16:05: EXTRACT - Aperture 1 from demoarc1 --> demoobj1demoarc1.ms
+
+REIDENTIFY: NOAO/IRAF V2.10BETA valdes@puppis Fri 16:05:39 17-Jan-92
+  Reference image = demoarc1.ms, New image = demoobj1..., Refit = yes
+Image Data    Found     Fit Pix Shift  User Shift  Z Shift      RMS
+demo...       48/48   48/48   -2.49E-4    -0.00109  -1.1E-7    0.227
+Extract and reidentify arc spectrum demoarc2
+Searching aperture database ...
+Jan 17 16:05: DATABASE  - 1 apertures read for demoobj1 from database
+Jan 17 16:05: DATABASE - 1 apertures for demoarc2 written to database
+Extracting apertures ...
+Jan 17 16:05: EXTRACT - Aperture 1 from demoarc2 --> demoobj1demoarc2.ms
+
+REIDENTIFY: NOAO/IRAF V2.10BETA valdes@puppis Fri 16:05:42 17-Jan-92
+  Reference image = demoarc1.ms, New image = demoobj1..., Refit = yes
+Image Data    Found     Fit Pix Shift  User Shift  Z Shift      RMS
+demo...       48/48   48/48    0.00266      0.0169  3.46E-6     0.24
+Dispersion correct demoobj1
+demoobj1.ms: ap = 1, w1 = 4204.181, w2 = 7355.375, dw = 6.16..., nw = 512
+Extinction correct demoobj1
+Flux calibrate demoobj1
+[demoobj1.ms.imh][1]: Example artificial long slit image
+  Extinction correction applied
+  Flux calibration applied
+.fi
+
+2.  To redo the above:
+
+.nf
+cl> doslit demoobj1 arcs=demoarc1,demoarc2 stand=demostd1 \
+>>> extcor=yes, fluxcal=yes resize=yes redo+
+.fi
+.ih
+REVISIONS
+.ls DOSLIT V2.11
+The initial arc line identifications is done with the automatic line
+identification algorithm.
+.le
+.ls DOSLIT V2.10.3
+The usual output WCS format is "equispec".  The image format type to be
+processed is selected with the \fIimtype\fR environment parameter.  The
+dispersion axis parameter is now a package parameter.  Images will only
+be processed if the have the CCDPROC keyword.  A \fIdatamax\fR parameter
+has been added to help improve cosmic ray rejection.  The arc reference
+is no longer taken from the center of the image but using the first object
+aperture.  A bug which alphabetized the arc list was fixed.
+.le
+.ih
+SEE ALSO
+apbackground, apedit, apfind, approfiles, aprecenter, apresize, apsum,
+aptrace, apvariance, calibrate, ccdred, center1d, ctioslit, dispcor,
+echelle.doecslit, icfit, autoidentify, identify, kpnocoude, kpnoslit,
+specred, observatory, onedspec.package, refspectra, reidentify, sensfunc,
+setairmass, setjd, splot, standard
+.endhelp
diff --git a/noao/imred/specred/doc/doslit.ms b/noao/imred/specred/doc/doslit.ms
new file mode 100644
index 00000000..03ad0ab5
--- /dev/null
+++ b/noao/imred/specred/doc/doslit.ms
@@ -0,0 +1,1401 @@
+.nr PS 9
+.nr VS 11
+.de V1
+.ft CW
+.nf
+..
+.de V2
+.fi
+.ft R
+..
+.de LS
+.br
+.in +2
+..
+.de LE
+.br
+.sp .5v
+.in -2
+..
+.ND February 1993
+.TL
+Guide to the Slit Spectra Reduction Task DOSLIT
+.AU
+Francisco Valdes
+.AI
+IRAF Group - Central Computer Services
+.K2
+.DY
+
+.AB
+\fBDoslit\fR extracts, sky subtracts, wavelength calibrates, and flux
+calibrates simple two dimensional slit spectra which have been processed to
+remove the detector characteristics; i.e. CCD images have been bias, dark
+count, and flat field corrected.  It is primarily intended for
+spectrophotometry or radial velocities of stellar spectra with the spectra
+aligned with one of the image axes; i.e. the assumption is that extractions
+can be done by summing along image lines or columns.  The alignment does
+not have to be precise but only close enough that the wavelength difference
+across the spectrum profiles is insignificant.  The task is available
+in the \fBctioslit\fR, \fBkpnoslit\fR, \fBkpnocoude\fR, and \fBspecred\fR
+packages.
+.AE
+.NH
+Introduction
+.LP
+\fBDoslit\fR extracts, sky subtracts, wavelength calibrates, and flux
+calibrates simple two dimensional slit spectra which have been processed to
+remove the detector characteristics; i.e. CCD images have been bias, dark
+count, and flat field corrected.  It is primarily intended for
+spectrophotometry or radial velocities of stellar spectra with the spectra
+aligned with one of the image axes; i.e. the assumption is that extractions
+can be done by summing along image lines or columns.  The alignment does
+not have to be precise but only close enough that the wavelength difference
+across the spectrum profiles is insignificant.  Extended objects requiring
+accurate geometric alignment over many pixels are reduced using the
+\fBlongslit\fR package.
+.LP
+The task is a command language script which collects and combines the
+functions and parameters of many general purpose tasks to provide a single,
+complete data reduction path and a degree of guidance, automation, and
+record keeping.  In the following description and in the parameter section
+the various general tasks used are identified.  Further
+information about those tasks and their parameters may be found in their
+documentation.  \fBDoslit\fR also simplifies and consolidates parameters
+from those tasks and keeps track of previous processing to avoid
+duplications.
+.LP
+The general organization of the task is to do the interactive setup steps,
+such as the reference dispersion function
+determination, first using representative calibration data and then perform
+the majority of the reductions automatically, possibly as a background
+process, with reference to the setup data.  In addition, the task
+determines which setup and processing operations have been completed in
+previous executions of the task and, contingent on the \f(CWredo\fR and
+\f(CWupdate\fR options, skip or repeat some or all the steps.
+.LP
+The description is divided into a quick usage outline followed by details
+of the parameters and algorithms.  The usage outline is provided as a
+checklist and a refresher for those familiar with this task and the
+component tasks.  It presents only the default or recommended usage
+since there are many variations possible.
+.NH
+Usage Outline
+.LP
+.IP [1] 6
+The images are first processed with \fBccdproc\fR for overscan,
+zero level, dark count, and flat field corrections.
+.IP [2]
+Set the \fBdoslit\fR parameters with \fBeparam\fR.  Specify the object
+images to be processed,
+one or more arc images, and one or more standard
+star images.  If there are many object, arc, or standard star images
+you might prepare "@ files".  Set the detector and data
+specific parameters.  Select the processing options desired.
+Finally you might wish to review the \f(CWsparams\fR algorithm parameters
+though the defaults are probably adequate.
+.IP [3]
+Run the task.  This may be repeated multiple times with different
+observations and the task will generally only do the setup steps
+once and only process new images.  Queries presented during the
+execution for various interactive operations may be answered with
+"yes", "no", "YES", or "NO".  The lower case responses apply just
+to that query while the upper case responses apply to all further
+such queries during the current execution and no further queries of that
+type will be made.
+.IP [4]
+Apertures are defined for all the standard and object images.  This is only
+done if there are no previous aperture definitions for the image.
+The highest peak is found and centered and the default aperture limits
+are set.  If the resize option is set the aperture is resized by finding
+the level which  is 5% (the default) of the peak above local background.
+If not using the quicklook option you now have the option
+of entering the aperture editing loop to check the aperture position,
+size, and background fitting parameters, and possibly add additional
+apertures.  This is step is highly recommended.
+It is important to check the background regions with the 'b'
+key.  To exit the background mode and then
+to exit the review mode use 'q'.
+.IP
+The spectrum positions at a series of points along the dispersion are
+measured and a function is fit to these positions.  If not using the
+quicklook option the traced positions may be examined interactively and the
+fitting parameters adjusted.  To exit the interactive fitting type 'q'.
+.IP [5]
+If dispersion correction is selected the first arc in the arc list is
+extracted.  The dispersion function is defined using the task
+\fBautoidentify\fR.  The \fIcrval\fR and \fIcdelt\fR parameters are used in
+the automatic identification.  Whether or not the automatic identification
+is successful you will be shown the result of the arc line identification.
+If the automatic identification is not successful identify a few arc lines
+with with 'm' and and use the 'l' line list identification command to
+automatically add additional lines and fit the dispersion function.  Check
+the quality of the dispersion function fit with 'f'.  When satisfied exit
+with 'q'.
+.IP [6]
+If the flux calibration option is selected the standard star spectra are
+processed (if not done previously).  The images are
+extracted and wavelength calibrated.  The appropriate arc
+calibration spectra are extracted and the dispersion function refit
+using the arc reference spectrum as a starting point.  The standard star
+fluxes through the calibration bandpasses are compiled.  You are queried
+for the name of the standard star calibration data file.
+.IP
+After all the standard stars are processed a sensitivity function is
+determined using the interactive task \fBsensfunc\fR.  Finally, the
+standard star spectra are extinction corrected and flux calibrated
+using the derived sensitivity function.
+.IP [7]
+The object spectra are now automatically
+extracted, wavelength calibrated, and flux calibrated.
+.IP [8]
+The option to examine the final spectra with \fBsplot\fR may be given.
+To exit type 'q'.  In quicklook mode the spectra are plotted
+noninteractively with \fBbplot\fR.
+.IP [9]
+The final spectra will have the same name as the original 2D images
+with a ".ms" extension added.
+.NH
+Spectra and Data Files
+.LP
+The basic input consists of two dimensional slit object, standard star, and
+arc calibration spectra stored as IRAF images.
+The type of image format is defined by the
+environment parameter \fIimtype\fR.  Only images with that extension will
+be processed and created.
+The raw CCD images must be
+processed to remove overscan, bias, dark count, and flat field effects.
+This is generally done using the \fBccdred\fR package.  Lines of constant
+wavelength should be closely aligned with one of the image axes though a
+small amount of misalignment only causes a small loss of resolution.  For
+large misalignments one may use the \fBrotate\fR task.  More complex
+geometric problems and observations of extended objects should be handled
+by the \fBlongslit\fR package.
+.LP
+The arc
+spectra are comparison arc lamp observations (they must all be of the same
+type).  The assignment of arc calibration exposures to object exposures is
+generally done by selecting the nearest in time and interpolating.
+However, the optional \fIarc assignment table\fR may be used to explicitly
+assign arc images to specific objects.  The format of this file is
+described in task \fBrefspectra\fR.
+.LP
+The final reduced spectra are recorded in one, two or three dimensional IRAF
+images.  The images have the same name as the original images with an added
+".ms" extension.  Each line in the reduced image is a one dimensional
+spectrum with associated aperture, wavelength, and identification
+information.  With a single aperture the image will be one dimensional
+and with multiple apertures the image will be two dimensional.
+When the \f(CWextras\fR parameter is set the images will be three
+dimensional (regardless of the number of apertures) and the lines in the
+third dimension contain additional information (see
+\fBapsum\fR for further details).  These spectral formats are accepted by the
+one dimensional spectroscopy tasks such as the plotting tasks \fBsplot\fR
+and \fBspecplot\fR.
+.NH
+Package Parameters
+.LP
+The package parameters, shown in Figure 1 for the \fBspecred\fR package,
+set parameters which change infrequently and define the standard I/O functions.
+.KS
+.V1
+
+.ce
+Figure 1: Package Parameter Set for DOSLIT Packages
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = imred
+   TASK = specred
+
+(extinct= onedstds$kpnoextinct.dat) Extinction file
+(caldir = onedstds$spec16redcal/) Standard star calibration directory
+(observa=  observatory) Observatory of data
+(interp =        poly5) Interpolation type
+(dispaxi=            2) Image axis for 2D images
+(nsum   =            1) Number of lines/columns to sum for 2D images
+
+(databas=     database) Database
+(verbose=           no) Verbose output?
+(logfile=      logfile) Log file
+(plotfil=             ) Plot file
+
+(records=             ) Record number extensions
+(version= SPECRED V3: April 1992)
+
+.KE
+.V2
+The extinction file
+is used for making extinction corrections and the standard star
+calibration directory is used for determining flux calibrations from
+standard star observations.  The calibration directories contain data files
+with standard star fluxes and band passes.  The available extinction
+files and flux calibration directories may be listed using the command:
+.V1
+
+	cl> help onedstds
+
+.V2
+The extinction correction requires computation of an air mass using the
+task \fBsetairmass\fR.  The air mass computation needs information
+about the observation and, in particular, the latitude of the observatory.
+This is determined using the OBSERVAT image header keyword.  If this
+keyword is not present the observatory parameter is used.  See the
+task \fBobservatory\fR for more on defining the observatory parameters.
+.LP
+The spectrum interpolation type is used whenever a spectrum needs to be
+resampled for linearization or performing operations between spectra
+with different sampling.  The "sinc" interpolation may be of interest
+as an alternative but see the cautions given in \fBonedspec.package\fR.
+.LP
+The general direction in which the spectra run is specified by the
+dispersion axis parameter.  Recall that ideally it is the direction
+of constant wavelength which should be aligned with an image axis and
+the dispersion direction may not be exactly aligned because atmospheric
+dispersion.
+.LP
+The verbose parameter selects whether to print everything which goes
+into the log file on the terminal.  It is useful for monitoring
+what the \fBdoslit\fR task does.  The log and plot files are useful for
+keeping a record of the processing.  A log file is highly recommended.
+A plot file provides a record of the apertures, traces, and extracted
+spectra but can become quite large.
+The plotfile is most conveniently viewed and printed with \fBgkimosaic\fR.
+.NH
+Processing Parameters
+.LP
+The \fBdoslit\fR parameters are shown in Figure 2.
+.KS
+.V1
+
+.ce
+Figure 2: Parameter Set for DOSLIT
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = specred
+   TASK = doslit
+
+objects =               List of object spectra
+(arcs   =             ) List of arc spectra
+(arctabl=             ) Arc assignment table (optional)
+(standar=             ) List of standard star spectra
+
+.KE
+.V1
+(readnoi=      rdnoise) Read out noise sigma (photons)
+(gain   =         gain) Photon gain (photons/data number)
+(datamax=        INDEF) Max data value / cosmic ray threshold
+(width  =           5.) Width of profiles (pixels)
+(crval  =        INDEF) Approximate wavelength
+(cdelt  =        INDEF) Approximate dispersion
+
+(dispcor=          yes) Dispersion correct spectra?
+(extcor =           no) Extinction correct spectra?
+(fluxcal=           no) Flux calibrate spectra?
+(resize =           no) Automatically resize apertures?
+(clean  =           no) Detect and replace bad pixels?
+(splot  =           no) Plot the final spectrum?
+(redo   =           no) Redo operations if previously done?
+(update =           no) Update spectra if cal data changes?
+(quicklo=           no) Minimally interactive quick-look?
+(batch  =           no) Extract objects in batch?
+(listonl=           no) List steps but don't process?
+
+(sparams=             ) Algorithm parameters
+
+.V2
+The input images are specified by image lists.  The lists may be
+explicit comma separate image names, @ files, or image
+templates using pattern matching against file names in the directory.
+To allow wildcard image lists to be used safely and conveniently the
+image lists are checked to remove extracted images (the .ms images)
+and to automatically identify object and arc spectra.  Object and arc
+images are identified by the keyword IMAGETYP with values of "object",
+"OBJECT", "comp", or "COMPARISON" (the current practice at NOAO).
+If arc images are found in the object list they are transferred to the
+arc list while if object images are found in the arc list they are ignored.
+All other image types, such as biases, darks, or flat fields, are
+ignored.  This behavior allows simply specifying all images with a wildcard
+in the object list with automatic selections of arc spectra or a
+wildcard in the arc list to automatically find the arc spectra.
+If the data lack the identifying information it is up to the user
+to explicitly set the proper lists.
+.LP
+The arc assignment table is a file which may be used to assign
+specific arc spectra to specific object and standard star spectra.
+For more on this option see \fBrefspectra\fR.
+.LP
+The next set of parameters describe the noise characteristics and
+spectrum characteristics.  The read out noise and gain are used when
+"cleaning" cosmic rays and when using variance or optimal weighting.  These
+parameters must be fairly accurate.  Note that these are the effective
+parameters and must be adjusted if previous processing has modified the
+pixel values; such as with an unnormalized flat field.
+The variance
+weighting and cosmic-ray cleanning are sensitive to extremely strong
+cosmic-rays; ones which are hundreds of times brighter than the
+spectrum.  The \fIdatamax\fR is used to set an upper limit for any
+real data.  Any pixels above this value will be flagged as cosmic-rays
+and will not affect the extractions.
+.LP
+The profile width should be approximately the full width
+at the profile base.  This parameter is used for centering and tracing
+of the spectrum profiles.
+.LP
+The approximate central wavelength and dispersion are used for the
+automatic identification of the arc reference.  They may be specified
+as image header keywords or values.  The INDEF values search the
+entire range of the coordinate reference file but the automatic
+line identification algorithm works much better and faster if
+approximate values are given.
+.LP
+The next set of parameters select the processing steps and options.  The
+various calibration steps may be done simultaneously, that is at the same
+time as the basic extractions, or in separate executions of the task.
+Typically, all the desired operations are done at the same time.
+Dispersion correction requires at least one arc spectrum and flux
+calibration requires dispersion correction and at least one standard star
+observation.
+.LP
+The \f(CWresize\fR option resets the edges of the extraction aperture based
+on the profile for each object and standard star image.  The default
+resizing is to the 5% point relative to the peak measured above the
+background.  This allows following changes in the seeing.  However, one
+should consider the consequences of this if attempting to flux calibrate
+the observations.  Except in quicklook mode, the apertures for each object
+and standard star observation may be reviewed graphically and
+adjustments made to the aperture width and background regions.
+.LP
+The \f(CWclean\fR option invokes a profile
+fitting and deviant point rejection algorithm as well as a variance weighting
+of points in the aperture.  See the next section for more about
+requirements to use this option.
+.LP
+Generally once a spectrum has been processed it will not be reprocessed if
+specified as an input spectrum.  However, changes to the underlying
+calibration data can cause such spectra to be reprocessed if the
+\f(CWupdate\fR flag is set.  The changes which will cause an update are a
+new arc reference image and new standard stars.  If all input spectra are to be
+processed regardless of previous processing the \f(CWredo\fR flag may be
+used.  Note that reprocessing clobbers the previously processed output
+spectra.
+.LP
+The final step is to plot the spectra if the \f(CWsplot\fR option is
+selected.  In non-quicklook mode there is a query which may be
+answered either in lower or upper case.  The plotting uses the interactive
+task \fBsplot\fR.  In quicklook mode the plot appears noninteractively
+using the task \fBbplot\fR.  
+.LP
+The \f(CWquicklook\fR option provides a simpler, less interactive, mode.
+In quicklook mode a single aperture is defined using default parameters
+without interactive aperture review or trace fitting and
+the \f(CWsplot\fR option selects a noninteractive plot to be
+shown at the end of processing of each object and standard star
+spectrum.  While the algorithms used in quicklook mode are nearly the same
+as in non-quicklook mode and the final results may be the same it is
+recommended that the greater degree of monitoring and review in
+non-quicklook mode be used for careful final reductions.
+.LP
+The batch processing option allows object spectra to be processed as a
+background or batch job.  This will occur only if the interactive
+\f(CWsplot\fR option is not active; either not set, turned off during
+processing with "NO", or in quicklook mode.  In batch processing the
+terminal output is suppressed.
+.LP
+The \f(CWlistonly\fR option prints a summary of the processing steps
+which will be performed on the input spectra without actually doing
+anything.  This is useful for verifying which spectra will be affected
+if the input list contains previously processed spectra.  The listing
+does not include any arc spectra which may be extracted to dispersion
+calibrate an object spectrum.
+.LP
+The last parameter (excluding the task mode parameter) points to
+another parameter set for the algorithm parameters.  The default
+parameter set is called \f(CWsparams\fR.  The algorithm parameters are
+discussed further in the next section.
+.NH
+Algorithms and Algorithm Parameters
+.LP
+This section summarizes the various algorithms used by the
+\fBdoslit\fR task and the parameters which control and modify the
+algorithms.  The algorithm parameters available to you are
+collected in the parameter set \fBsparams\fR.  These parameters are
+taken from the various general purpose tasks used by the \fBdoslit\fR
+processing task.  Additional information about these parameters and
+algorithms may be found in the help for the actual
+task executed.  These tasks are identified below.  The aim of this
+parameter set organization is to collect all the algorithm parameters
+in one place separate from the processing parameters and include only
+those which are relevant for slit data.  The parameter values
+can be changed from the defaults by using the parameter editor,
+.V1
+
+cl> epar sparams
+
+.V2
+or simple typing \f(CWsparams\fR.
+The parameter editor can also be entered when editing the \fBdoslit\fR
+parameters by typing \f(CW:e\fR when positioned at the \f(CWsparams\fR
+parameter.  Figure 3 shows the parameter set.
+.KS
+.V1
+
+.ce
+Figure 3: Algorithm Parameter Set
+
+                           I R A F
+            Image Reduction and Analysis Facility
+PACKAGE = specred
+   TASK = sparams
+
+(line   =        INDEF) Default dispersion line
+(nsum   =           10) Number of dispersion lines to sum
+(extras =           no) Extract sky, sigma, etc.?
+
+                        -- DEFAULT APERTURE LIMITS --
+(lower  =          -3.) Lower aperture limit relative to center
+(upper  =           3.) Upper aperture limit relative to center
+
+                        -- AUTOMATIC APERTURE RESIZING PARAMETERS --
+(ylevel =         0.05) Fraction of peak or intensity for resizing
+
+.KE
+.KS
+.V1
+                        -- TRACE PARAMETERS --
+(t_step =           10) Tracing step
+(t_funct=      spline3) Trace fitting function
+(t_order=            1) Trace fitting function order
+(t_niter=            1) Trace rejection iterations
+(t_low  =           3.) Trace lower rejection sigma
+(t_high =           3.) Trace upper rejection sigma
+
+.KE
+.KS
+.V1
+                        -- APERTURE EXTRACTION PARAMETERS --
+(weights=         none) Extraction weights (none|variance)
+(pfit   =        fit1d) Profile fitting algorithm (fit1d|fit2d)
+(lsigma =           3.) Lower rejection threshold
+(usigma =           3.) Upper rejection threshold
+
+.KE
+.KS
+.V1
+                        -- BACKGROUND SUBTRACTION PARAMETERS --
+(backgro=          fit) Background to subtract
+(b_funct=     legendre) Background function
+(b_order=            1) Background function order
+(b_sampl=  -10:-6,6:10) Background sample regions
+(b_naver=         -100) Background average or median
+(b_niter=            1) Background rejection iterations
+(b_low  =           3.) Background lower rejection sigma
+(b_high =           3.) Background upper rejection sigma
+
+.KE
+.KS
+.V1
+                        -- ARC DISPERSION FUNCTION PARAMETERS --
+(coordli=linelists$idhenear.dat) Line list
+(match  =          -3.) Line list matching limit in Angstroms
+(fwidth =           4.) Arc line widths in pixels
+(cradius=          10.) Centering radius in pixels
+(i_funct=      spline3) Coordinate function
+(i_order=            1) Order of dispersion function
+(i_niter=            0) Rejection iterations
+(i_low  =           3.) Lower rejection sigma
+(i_high =           3.) Upper rejection sigma
+(refit  =          yes) Refit coordinate function when reidentifying?
+(addfeat=           no) Add features when reidentifying?
+
+.KE
+.KS
+.V1
+                        -- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+(select =       interp) Selection method for reference spectra
+(sort   =           jd) Sort key
+(group  =          ljd) Group key
+(time   =           no) Is sort key a time?
+(timewra=          17.) Time wrap point for time sorting
+
+.KE
+.KS
+.V1
+                        -- DISPERSION CORRECTION PARAMETERS --
+(lineari=          yes) Linearize (interpolate) spectra?
+(log    =           no) Logarithmic wavelength scale?
+(flux   =          yes) Conserve flux?
+
+.KE
+.KS
+.V1
+                        -- SENSITIVITY CALIBRATION PARAMETERS --
+(s_funct=      spline3) Fitting function
+(s_order=            1) Order of sensitivity function
+(fnu    =           no) Create spectra having units of FNU?
+
+.KE
+.V2
+.NH 2
+Aperture Definitions
+.LP
+The first operation is to define the extraction apertures, which include the
+aperture width, background regions, and position dependence with
+wavelength, for the input slit spectra and, if flux calibration is
+selected, the standard star spectra.  This is done only for spectra which
+do not have previously defined apertures unless the \f(CWredo\fR option is
+set to force all definitions to be redone.  Thus, apertures may be
+defined separately using the \fBapextract\fR tasks.  This is particularly
+useful if one needs to use reference images to define apertures for very
+weak spectra which are not well centered or traced by themselves.
+.LP
+Initially a single spectrum is found and a default aperture defined
+automatically.  If the \f(CWresize\fR parameter is set the aperture width is
+adjusted to a specified point on the spectrum profile (see
+\fBapresize\fR).  If not in "quicklook" mode (set by the \f(CWquicklook\fR
+parameter) a query is printed to select whether to inspect and modify the
+aperture and background aperture definitions using the commands described
+for \fBapedit\fR.  This option allows adding
+apertures for other objects on the slit and adjusting
+background regions to avoid contaminating objects.  The query may be
+answered in lower case for a single spectrum or in upper case to
+permanently set the response for the duration of the task execution.  This
+convention for query responses is used throughout the task.  It is
+recommended that quicklook only be used for initial quick extractions and
+calibration and that for final reductions one at least review the aperture
+definitions and traces.
+.LP
+The initial spectrum finding and aperture definitions are done at a specified
+line or column.  The positions of the spectrum at a set of other lines or
+columns is done next and a smooth function is fit to define the aperture
+centers at all points in the image.  In non-quicklook mode the user has the
+option to review and adjust the function fitting parameters and delete bad
+position determinations.  As with the initial aperture review there is a
+query which may be answered either in lower or upper case.
+.LP
+The above steps are all performed using tasks from the \fBapextract\fR
+package and parameters from the \fBsparams\fR parameters.  As a quick
+summary, the dispersion direction of the spectra are determined from the
+package \fBdispaxis\fR parameter if not defined in the image header.  The default
+line or column for finding the object position on the slit and the number
+of image lines or columns to sum are set by the \f(CWline\fR and \f(CWnsum\fR
+parameters.  A line of INDEF (the default) selects the middle of the image.
+The automatic finding algorithm is described for the task
+\fBapfind\fR and is basically finds the strongest peak.  The default
+aperture size, background parameters, and resizing are described in
+the tasks \fBapdefault\fR and \fBapresize\fR and the
+parameters used are also described there.
+The tracing is done as described in \fBaptrace\fR and consists of
+stepping along the image using the specified \f(CWt_step\fR parameter.  The
+function fitting uses the \fBicfit\fR commands with the other parameters
+from the tracing section.
+.NH 2
+Extraction
+.LP
+The actual extraction of the spectra is done by summing across the
+fixed width apertures at each point along the dispersion.
+The default is to simply sum the pixels using
+partial pixels at the ends.  There is an option to weight the
+sum based on a Poisson variance model using the \f(CWreadnoise\fR and
+\f(CWgain\fR detector parameters.  Note that if the \f(CWclean\fR
+option is selected the variance weighted extraction is used regardless
+of the \f(CWweights\fR parameter.  The sigma thresholds for cleaning
+are also set in the \fBsparams\fR parameters.
+.LP
+The cleaning and variance weighting options require knowing the effective
+(i.e. accounting for any image combining) read out noise and gain.  These
+numbers need to be adjusted if the image has been processed such that the
+intensity scale has a different origin (such as applying a separate
+background subtraction operation) or scaling (such as caused by
+unnormalized flat fielding).  These options also require using background
+subtraction if the profile does not go to zero.  For optimal extraction and
+cleaning to work it is recommended that any flat fielding be done using
+normalized flat fields (as is done in \fBccdproc\fR) and using background
+subtraction if there is any appreciable sky.  For further discussion of
+cleaning and variance weighted extraction see \fBapvariance\fR and
+\fBapprofiles\fR as well as  \fBapsum\fR.
+.LP
+Background sky subtraction is done during the extraction based on
+background regions and parameters defined by the default parameters or
+changed during the interactive setting of the apertures.  The background
+subtraction options are to do no background subtraction, subtract the
+average, median, or minimum of the pixels in the background regions, or to
+fit a function and subtract the function from under the extracted object
+pixels.  The background regions are specified in pixels from
+the aperture center and follow changes in center of the spectrum along the
+dispersion.  The syntax is colon separated ranges with multiple ranges
+separated by a comma or space.  The background fitting uses the \fBicfit\fR
+routines which include medians, iterative rejection of deviant points, and
+a choice of function types and orders.  Note that it is important to use a
+method which rejects cosmic rays such as using either medians over all the
+background regions (\f(CWbackground\fR = "median") or median samples during
+fitting (\f(CWb_naverage\fR < -1).  The background subtraction algorithm and
+options are described in greater detail in \fBapsum\fR and
+\fBapbackground\fR.
+.NH 2
+Dispersion Correction
+.LP
+If dispersion correction is not selected, \f(CWdispcor\fR=no, then the object
+spectra are simply extracted.  The extracted spectra may be plotted
+by setting the \f(CWsplot\fR option.  This produces a query and uses
+the interactive \fBsplot\fR task in non-quicklook mode and uses the
+noninteractive \fBbplot\fR task in quicklook mode.
+.LP
+Dispersion corrections are applied to the extracted spectra if the
+\f(CWdispcor\fR processing parameter is set.  There are three basic steps
+involved; determining the dispersion functions relating pixel position to
+wavelength, assigning the appropriate dispersion function to a particular
+observation, and either storing the nonlinear dispersion function in the
+image headers or resampling the spectra to evenly spaced pixels in
+wavelength.
+.LP
+The first arc spectrum in the arc list is used to define the reference
+dispersion solution.  It is extracted at middle of the image with no
+tracing.  Note extractions of arc spectra are not background subtracted.
+The task \fBautoidentify\fR is attempts to define the dispersion function
+automatically using the \fIcrval\fR and \fIcdelt\fR parameters.  Whether or
+not it is successful the user is presented with the interactive
+identification graph.  The automatic identifications can be reviewed and a
+new solution or corrections to the automatic solution may be performed.
+.LP
+The arc dispersion function parameters are for \fBautoidentify\fR and it's
+related partner \fBreidentify\fR.  The parameters define a line list for
+use in automatically assigning wavelengths to arc lines, a centering width
+(which should match the line widths at the base of the lines), the
+dispersion function type and orders, parameters to exclude bad lines from
+function fits, and defining whether to refit the dispersion function as
+opposed to simply determining a zero point shift.  The defaults should
+generally be adequate and the dispersion function fitting parameters may be
+altered interactively.  One should consult the help for the two tasks for
+additional details of these parameters and the interactive operation of
+\fBautoidentify\fR.
+.LP
+The extracted reference arc spectrum is then dispersion corrected.
+If the spectra are to be linearized, as set by the \f(CWlinearize\fR
+parameter, the default linear wavelength parameters are printed and
+you have the option to adjust them.  The dispersion system defined at
+this point will be applied automatically to all other spectra as they
+are dispersion corrected.
+.LP
+Once the reference dispersion function is defined other arc spectra are
+extracted as required by the object spectra.  The assignment of arcs is
+done either explicitly with an arc assignment table (parameter
+\f(CWarctable\fR) or based on a header parameter such as a time.
+This assignments are made by the task
+\fBrefspectra\fR.  When two arcs are assigned to an object spectrum an
+interpolation is done between the two dispersion functions.  This makes an
+approximate correction for steady drifts in the dispersion.
+.LP
+The tasks \fBsetjd\fR and \fBsetairmass\fR are automatically run on all
+spectra.  This computes and adds the header parameters for the Julian date
+(JD), the local Julian day number (LJD), the universal time (UTMIDDLE), and
+the air mass at the middle of the exposure.  The default arc assignment is
+to use the Julian date grouped by the local Julian day number.  The
+grouping allows multiple nights of data to be correctly assigned at the
+same time.
+.LP
+The assigned arc spectra are then extracted using the object aperture
+definitions (but without background subtraction or cleaning) so that the
+same pixels on the detector are used.  The extracted arc spectra are then
+reidentified automatically against the reference arc spectrum.  Some
+statistics of the reidentification are printed (if not in batch mode) and
+the user has the option of examining the lines and fits interactively if
+not in quicklook mode.  The task which does the reidentification is called
+\fBreidentify\fR.
+.LP
+The last step of dispersion correction is setting the dispersion
+of the object image from the arc images.  There are two choices here.
+If the \f(CWlinearize\fR parameter is not set the nonlinear dispersion
+function is stored in the image header.  Other IRAF tasks interpret
+this information when dispersion coordinates are needed for plotting
+or analysis.  This has the advantage of not requiring the spectra
+to be interpolated and the disadvantage that the dispersion
+information is only understood by IRAF tasks and cannot be readily
+exported to other analysis software.
+.LP
+If the \f(CWlinearize\fR parameter is set then the spectra are resampled to a
+linear dispersion relation either in wavelength or the log of the
+wavelength using the dispersion coordinate system defined previously
+for the arc reference spectrum.
+.LP
+The linearization algorithm parameters allow selecting the interpolation
+function type, whether to conserve flux per pixel by integrating across the
+extent of the final pixel, and whether to linearize to equal linear or
+logarithmic intervals.  The latter may be appropriate for radial velocity
+studies.  The default is to use a fifth order polynomial for interpolation,
+to conserve flux, and to not use logarithmic wavelength bins.  These
+parameters are described fully in the help for the task \fBdispcor\fR which
+performs the correction.
+.NH 2
+Flux Calibration
+.LP
+Flux calibration consists of an extinction correction and an instrumental
+sensitivity calibration.  The extinction correction only depends on the
+extinction function defined by the package parameter \f(CWextinct\fR and
+determination of the airmass from the header parameters (the air mass is
+computed by \fBsetairmass\fR as mentioned earlier).  The sensitivity
+calibration depends on a sensitivity calibration spectrum determined from
+standard star observations for which there are tabulated absolute fluxes.
+The task that applies both the extinction correction and sensitivity
+calibration to each extracted object spectrum is \fBcalibrate\fR.  Consult
+the manual page for this task for more information.
+.LP
+Generation of the sensitivity calibration spectrum is done before
+processing any object spectra since it has two interactive steps and
+requires all the standard star observations.  The first step is tabulating
+the observed fluxes over the same bandpasses as the calibrated absolute
+fluxes.  The standard star tabulations are done after each standard star is
+extracted and dispersion corrected.  You are asked for the name of the
+standard star as tabulated in the absolute flux data files in the directory
+\f(CWcaldir\fR defined by the package parameters.
+The tabulation of the standard star
+observations over the standard bandpasses is done by the task
+\fBstandard\fR.  The tabulated data is stored in the file \f(CWstd\fR.  Note
+that if the \f(CWredo\fR flag is not set any new standard stars specified in
+subsequent executions of \fBdoslit\fR are added to the previous data in
+the data file, otherwise the file is first deleted.  Modification of the
+tabulated standard star data, such as by adding new stars, will cause any
+spectra in the input list which have been previously calibrated to be
+reprocessed if the \f(CWupdate\fR flag is set.
+.LP
+After the standard star calibration bandpass fluxes are tabulated the
+information from all the standard stars is combined to produce a
+sensitivity function for use by \fBcalibrate\fR.  The sensitivity function
+determination is interactive and uses the task \fBsensfunc\fR.  This task
+allows fitting a smooth sensitivity function to the ratio of the observed
+to calibrated fluxes verses wavelength.  The types of manipulations one
+needs to do include deleting bad observations, possibly removing variable
+extinction (for poor data), and possibly deriving a revised extinction
+function.  This is a complex operation and one should consult the manual
+page for \fBsensfunc\fR.  The sensitivity function is saved as a one
+dimensional spectrum with the name \f(CWsens\fR.  Deletion of this image
+will also cause reprocessing to occur if the \f(CWupdate\fR flag is set.
+.NH
+References
+.NH 2
+IRAF Introductory References
+.LP
+Work is underway on a new introductory guide to IRAF.  Currently, the
+work below is the primary introduction.
+.IP
+P. Shames and D. Tody, \fIA User's Introduction to the IRAF Command
+Language\fR, Central Computer Services, NOAO, 1986.
+.NH 2
+CCD Reductions
+.IP
+F. Valdes, \fIThe IRAF CCD Reduction Package -- CCDRED\fR, Central
+Computer Services, NOAO, 1987.
+.IP
+F. Valdes, \fIUser's Guide to the CCDRED Package\fR, Central
+Computer Services, NOAO, 1988.  Also on-line as \f(CWhelp ccdred.guide\fR.
+.IP
+P. Massey, \fIA User's Guide to CCD Reductions with IRAF\fR, Central
+Computer Services, NOAO, 1989.
+.NH 2
+Aperture Extraction Package
+.IP
+F. Valdes, \fIThe IRAF APEXTRACT Package\fR, Central Computer Services,
+NOAO, 1987 (out-of-date).
+.NH 2
+DOSLIT Task
+.IP
+P. Massey, \fIUser's Guide to Slit Spectra Reductions\fR,
+Central Computer Services, NOAO, 1992.
+.NH 2
+Task Help References
+.LP
+Each task in the \fBspecred\fR packages and tasks used by \fBdoslit\fR have
+help pages describing the parameters and task in some detail.  To get
+on-line help type
+.V1
+
+cl> help \fItaskname\fR
+
+.V2
+The output of this command can be piped to \fBlprint\fR to make a printed
+copy.
+
+.V1
+       apall - Extract 1D spectra (all parameters in one task)
+   apdefault - Set the default aperture parameters and apidtable
+      apedit - Edit apertures interactively
+      apfind - Automatically find spectra and define apertures
+       apfit - Fit 2D spectra and output the fit, difference, or ratio
+   apflatten - Remove overall spectral and profile shapes from flat fields
+      apmask - Create and IRAF pixel list mask of the apertures
+ apnormalize - Normalize 2D apertures by 1D functions
+  aprecenter - Recenter apertures
+    apresize - Resize apertures
+   apscatter - Fit and subtract scattered light
+       apsum - Extract 1D spectra
+     aptrace - Trace positions of spectra
+ 
+autoidentify - Automatically identify arc lines and a dispersion function
+       bplot - Batch plot of spectra with SPLOT
+   calibrate - Extinction and flux calibrate spectra
+   continuum - Fit the continuum in spectra
+    deredden - Apply interstellar extinction correction
+     dispcor - Dispersion correct spectra
+      dopcor - Doppler correct spectra
+    fitprofs - Fit gaussian profiles
+    identify - Identify features in spectrum for dispersion solution
+    msresp1d - Create 1D response spectra from flat field and sky spectra
+  refspectra - Assign wavelength reference spectra to other spectra
+  reidentify - Automatically reidentify features in spectra
+  sapertures - Set or change aperture header information
+      sarith - Spectrum arithmetic
+    scombine - Combine spectra
+       scopy - Select and copy apertures in different spectral formats
+    sensfunc - Compute instrumental sensitivity from standard stars
+  setairmass - Compute effective airmass and middle UT for an exposure
+       setjd - Compute and set Julian dates in images
+        sfit - Fit spectra and output fit, ratio, or difference
+      skysub - Sky subtract extracted multispec spectra
+       slist - List spectrum header parameters
+    specplot - Scale, stack, and plot multiple spectra
+       splot - Preliminary spectral plot/analysis
+    standard - Tabulate standard star counts and fluxes
+ 
+      doslit - Process slit spectra
+       demos - Demonstrations and tests
+
+	    Additional help topics
+
+   onedspec.package - Package parameters and general description of package
+  apextract.package - Package parameters and general description of package
+ approfiles - Profile determination algorithms
+ apvariance - Extractions, variance weighting, cleaning, and noise model
+   center1d - One dimensional centering algorithm
+      icfit - Interactive one dimensional curve fitting
+.V2
+.SH
+Appendix A: DOSLIT Parameters
+.LP
+.nr PS 8
+.nr VS 10
+objects
+.LS
+List of object images to be processed.  Previously processed spectra are
+ignored unless the \f(CWredo\fR flag is set or the \f(CWupdate\fR flag is set
+and dependent calibration data has changed.  If the images contain the
+keyword IMAGETYP then only those with a value of "object" or "OBJECT"
+are used and those with a value of "comp" or "COMPARISON" are added
+to the list of arcs.  Extracted spectra are ignored.
+.LE
+arcs = "" (at least one if dispersion correcting)
+.LS
+List of arc calibration spectra.  These spectra are used to define
+the dispersion functions.  The first spectrum is used to mark lines
+and set the dispersion function interactively and dispersion functions
+for all other arc spectra are derived from it.  If the images contain
+the keyword IMAGETYP then only those with a value of "comp" or
+"COMPARISON" are used.  All others are ignored as are extracted spectra.
+.LE
+arctable = "" (optional) (refspectra)
+.LS
+Table defining which arc spectra are to be assigned to which object
+spectra (see \fBrefspectra\fR).  If not specified an assignment based
+on a header parameter, \f(CWsparams.sort\fR, such as the Julian date
+is made.
+.LE
+standards = "" (at least one if flux calibrating)
+.LS
+List of standard star spectra.  The standard stars must have entries in
+the calibration database (package parameter \f(CWcaldir\fR).
+.LE
+
+readnoise = "rdnoise", gain = "gain" (apsum)
+.LS
+Read out noise in photons and detector gain in photons per data value.
+This parameter defines the minimum noise sigma and the conversion between
+photon Poisson statistics and the data number statistics.  Image header
+keywords (case insensitive) may be specified to obtain the values from the
+image header.
+.LE
+datamax = INDEF (apsum.saturation)
+.LS
+The maximum data value which is not a cosmic ray.
+When cleaning cosmic rays and/or using variance weighted extraction
+very strong cosmic rays (pixel values much larger than the data) can
+cause these operations to behave poorly.  If a value other than INDEF
+is specified then all data pixels in excess of this value will be
+excluded and the algorithms will yield improved results.
+This applies only to the object spectra and not the standard star or
+arc spectra.  For more
+on this see the discussion of the saturation parameter in the
+\fBapextract\fR package.
+.LE
+width = 5. (apedit)
+.LS
+Approximate full width of the spectrum profiles.  This parameter is used
+to define a width and error radius for the profile centering algorithm.
+.LE
+crval = INDEF, cdelt = INDEF (autoidentify)
+.LS
+These parameters specify an approximate central wavelength and dispersion.
+They may be specified as numerical values, INDEF, or image header keyword
+names whose values are to be used.
+If both these parameters are INDEF then the automatic identification will
+not be done.
+.LE
+
+dispcor = yes
+.LS
+Dispersion correct spectra?  This may involve either defining a nonlinear
+dispersion coordinate system in the image header or resampling the
+spectra to uniform linear wavelength coordinates as selected by
+the parameter \f(CWsparams.linearize\fR.
+.LE
+extcor = no
+.LS
+Extinction correct the spectra?
+.LE
+fluxcal = no
+.LS
+Flux calibrate the spectra using standard star observations?
+.LE
+resize = no (apresize)
+.LS
+Resize the default aperture for each object based on the spectrum profile?
+.LE
+clean = no (apsum)
+.LS
+Detect and correct for bad pixels during extraction?  This is the same
+as the clean option in the \fBapextract\fR package.  If yes this also
+implies variance weighted extraction.  In addition the datamax parameters
+can be useful.
+.LE
+splot = no
+.LS
+Plot the final spectra with the task \fBsplot\fR?  In quicklook mode
+this is automatic and in non-quicklook mode it is queried.
+.LE
+redo = no
+.LS
+Redo operations previously done?  If no then previously processed spectra
+in the object list will not be processed unless required by the
+update option.
+.LE
+update = no
+.LS
+Update processing of previously processed spectra if the
+dispersion reference image or standard star calibration data are changed?
+.LE
+quicklook = no
+.LS
+Extract and calibrate spectra with minimal interaction?  In quicklook mode
+only the initial dispersion function solution and standard star setup are
+done interactively.  Normally the \f(CWsplot\fR option is set in this mode to
+produce an automatic final spectrum plot for each object.  It is
+recommended that this mode not be used for final reductions.
+.LE
+batch = yes
+.LS
+Process spectra as a background or batch job provided there are no interactive
+steps remaining.
+.LE
+listonly = no
+.LS
+List processing steps but don't process?
+.LE
+
+sparams = "" (pset)
+.LS
+Name of parameter set containing additional processing parameters.  This
+parameter is only for indicating the link to the parameter set
+\fBsparams\fR and should not be given a value.  The parameter set may be
+examined and modified in the usual ways (typically with "eparam sparams"
+or ":e sparams" from the parameter editor).  The parameters are
+described below.
+.LE
+
+.ce
+-- GENERAL PARAMETERS --
+
+line = INDEF, nsum = 10
+.LS
+The dispersion line (line or column perpendicular to the dispersion
+axis) and number of adjacent lines (half before and half after unless
+at the end of the image) used in finding, resizing,
+editing, and tracing operations.  A line of INDEF selects the middle of the
+image along the dispersion axis.
+.LE
+extras = no (apsum)
+.LS
+Include raw unweighted and uncleaned spectra, the background spectra, and
+the estimated sigmas in a three dimensional output image format.
+See the discussion in the \fBapextract\fR package for further information.
+.LE
+
+.ce
+-- DEFAULT APERTURE LIMITS --
+
+lower = -3., upper = 3. (apdefault)
+.LS
+Default lower and upper aperture limits relative to the aperture center.
+These limits are used when the apertures are first defined.
+.LE
+
+.ce
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --
+
+ylevel = 0.05 (apresize)
+.LS
+Fraction of the peak to set aperture limits during automatic resizing.
+.LE
+
+.ce
+-- TRACE PARAMETERS --
+
+t_step = 10 (aptrace)
+.LS
+Step along the dispersion axis between determination of the spectrum
+positions.  Note the \f(CWnsum\fR parameter is also used to enhance the
+signal-to-noise at each step.
+.LE
+t_function = "spline3", t_order = 1 (aptrace)
+.LS
+Default trace fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of terms in the
+polynomial functions or the number of spline pieces in the spline
+functions.
+.LE
+t_niterate = 1, t_low = 3., t_high = 3. (aptrace)
+.LS
+Default number of rejection iterations and rejection sigma thresholds.
+.LE
+
+.ce
+-- APERTURE EXTRACTION PARAMETERS --
+
+weights = "none" (apsum) (none|variance)
+.LS
+Type of extraction weighting.  Note that if the \f(CWclean\fR parameter is
+set then the weights used are "variance" regardless of the weights
+specified by this parameter.  The choices are:
+
+"none"
+.LS
+The pixels are summed without weights except for partial pixels at the
+ends.
+.LE
+"variance"
+.LS
+The extraction is weighted by the variance based on the data values
+and a poisson/ccd model using the \f(CWgain\fR and \f(CWreadnoise\fR
+parameters.
+.LE
+.LE
+pfit = "fit1d" (apsum and approfile) (fit1d|fit2d)
+.LS
+Type of profile fitting algorithm to use.  The "fit1d" algorithm is
+preferred except in cases of extreme tilt.
+.LE
+lsigma = 3., usigma = 3. (apsum)
+.LS
+Lower and upper rejection thresholds, given as a number of times the
+estimated sigma of a pixel, for cleaning.
+.LE
+
+.ce
+-- DEFAULT BACKGROUND PARAMETERS --
+
+background = "fit" (apsum) (none|average|median|minimum|fit)
+.LS
+Type of background subtraction.  The choices are "none" for no background
+subtraction, "average" to average the background within the background
+regions, "median" to use the median in the background regions, "minimum" to
+use the minimum in the background regions, or "fit" to fit across the
+dispersion using the background within the background regions.  Note that
+the "average" option does not do any medianing or bad pixel checking,
+something which is recommended.  The fitting option is slower than the
+other options and requires additional fitting parameter.
+.LE
+b_function = "legendre", b_order = 1 (apsum)
+.LS
+Default background fitting function and order.  The fitting function types are
+"chebyshev" polynomial, "legendre" polynomial, "spline1" linear spline, and
+"spline3" cubic spline.  The order refers to the number of
+terms in the polynomial functions or the number of spline pieces in the spline
+functions.
+.LE
+b_sample = "-10:-6,6:10" (apsum)
+.LS
+Default background sample.  The sample is given by a set of colon separated
+ranges each separated by either whitespace or commas.  The string "*" refers
+to all points.  Note that the background coordinates are relative to the
+aperture center and not image pixel coordinates so the endpoints need not
+be integer.  It is recommended that the background regions be examined
+and set interactively with the 'b' key in the interactive aperture
+definition mode.  This requires \f(CWquicklook\fR to be no.
+.LE
+b_naverage = -100 (apsum)
+.LS
+Default number of points to average or median.  Positive numbers
+average that number of sequential points to form a fitting point.
+Negative numbers median that number, in absolute value, of sequential
+points.  A value of 1 does no averaging and each data point is used in the
+fit.
+.LE
+b_niterate = 1 (apsum)
+.LS
+Default number of rejection iterations.  If greater than zero the fit is
+used to detect deviant fitting points and reject them before repeating the
+fit.  The number of iterations of this process is given by this parameter.
+.LE
+b_low_reject = 3., b_high_reject = 3. (apsum)
+.LS
+Default background lower and upper rejection sigmas.  If greater than zero
+points deviating from the fit below and above the fit by more than this
+number of times the sigma of the residuals are rejected before refitting.
+.LE
+
+.ce
+-- ARC DISPERSION FUNCTION PARAMETERS --
+
+threshold = 10. (autoidentify/reidentify)
+.LS
+In order for a feature center to be determined the range of pixel intensities
+around the feature must exceed this threshold.
+.LE
+coordlist = "linelists$idhenear.dat" (autoidentify)
+.LS
+Arc line list consisting of an ordered list of wavelengths.
+Some standard line lists are available in the directory "linelists$".
+.LE
+match = -3. (autoidentify)
+.LS
+The maximum difference for a match between the dispersion function computed
+value and a wavelength in the coordinate list.
+.LE
+fwidth = 4. (autoidentify)
+.LS
+Approximate full base width (in pixels) of arc lines.
+.LE
+cradius = 10. (reidentify)
+.LS
+Radius from previous position to reidentify arc line.
+.LE
+i_function = "spline3", i_order = 1 (autoidentify)
+.LS
+The default function and order to be fit to the arc wavelengths as a
+function of the pixel coordinate.  The functions choices are "chebyshev",
+"legendre", "spline1", or "spline3".
+.LE
+i_niterate = 0, i_low = 3.0, i_high = 3.0 (autoidentify)
+.LS
+Number of rejection iterations and sigma thresholds for rejecting arc
+lines from the dispersion function fits.
+.LE
+refit = yes (reidentify)
+.LS
+Refit the dispersion function?  If yes and there is more than 1 line
+and a dispersion function was defined in the initial arc reference then a new
+dispersion function of the same type as in the reference image is fit
+using the new pixel positions.  Otherwise only a zero point shift is
+determined for the revised fitted coordinates without changing the
+form of the dispersion function.
+.LE
+addfeatures = no (reidentify)
+.LS
+Add new features from a line list during each reidentification?
+This option can be used to compensate for lost features from the
+reference solution.  Care should be exercised that misidentified features
+are not introduced.
+.LE
+
+.ce
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --
+
+select = "interp" (refspectra)
+.LS
+Selection method for assigning wavelength calibration spectra.
+Note that an arc assignment table may be used to override the selection
+method and explicitly assign arc spectra to object spectra.
+The automatic selection methods are:
+
+average
+.LS
+Average two reference spectra without regard to any
+sort or group parameters.
+If only one reference spectrum is specified then it is assigned with a
+warning.  If more than two reference spectra are specified then only the
+first two are used and a warning is given.  There is no checking of the
+group values.
+.LE
+following
+.LS
+Select the nearest following spectrum in the reference list based on the
+sort and group parameters.  If there is no following spectrum use the
+nearest preceding spectrum.
+.LE
+interp
+.LS
+Interpolate between the preceding and following spectra in the reference
+list based on the sort and group parameters.  If there is no preceding and
+following spectrum use the nearest spectrum.  The interpolation is weighted
+by the relative distances of the sorting parameter (see cautions in
+DESCRIPTION section).
+.LE
+match
+.LS
+Match each input spectrum with the reference spectrum list in order.
+This overrides any group values.
+.LE
+nearest
+.LS
+Select the nearest spectrum in the reference list based on the sort and
+group parameters.
+.LE
+preceding
+.LS
+Select the nearest preceding spectrum in the reference list based on the
+sort and group parameters.  If there is no preceding spectrum use the
+nearest following spectrum.
+.LE
+.LE
+sort = "jd" (setjd and refspectra)
+.LS
+Image header keyword to be used as the sorting parameter for selection
+based on order.  The header parameter must be numeric but otherwise may
+be anything.  Common sorting parameters are times or positions.
+.LE
+group = "ljd" (setjd and refspectra)
+.LS
+Image header keyword to be used to group spectra.  For those selection
+methods which use the group parameter the reference and object
+spectra must have identical values for this keyword.  This can
+be anything but it must be constant within a group.  Common grouping
+parameters are the date of observation "date-obs" (provided it does not
+change over a night) or the local Julian day number.
+.LE
+time = no, timewrap = 17. (refspectra)
+.LS
+Is the sorting parameter a 24 hour time?  If so then the time origin
+for the sorting is specified by the timewrap parameter.  This time
+should precede the first observation and follow the last observation
+in a 24 hour cycle.
+.LE
+
+.ce
+-- DISPERSION  CORRECTION PARAMETERS --
+
+linearize = yes (dispcor)
+.LS
+Interpolate the spectra to a linear dispersion sampling?  If yes the
+spectra will be interpolated to a linear or log linear sampling using
+the linear dispersion parameters specified by other parameters.  If
+no the nonlinear dispersion function(s) from the dispersion function
+database are assigned to the input image world coordinate system
+and the spectral data is not interpolated.  Note the interpolation
+function type is set by the package parameter \f(CWinterp\fR.
+.LE
+log = no (dispcor)
+.LS
+Use linear logarithmic wavelength coordinates?  Linear logarithmic
+wavelength coordinates have wavelength intervals which are constant
+in the logarithm of the wavelength.
+.LE
+flux = yes (dispcor)
+.LS
+Conserve the total flux during interpolation?  If \f(CWno\fR the output
+spectrum is interpolated from the input spectrum at each output
+wavelength coordinate.  If \f(CWyes\fR the input spectrum is integrated
+over the extent of each output pixel.  This is slower than
+simple interpolation.
+.LE
+
+.ce
+-- SENSITIVITY CALIBRATION PARAMETERS --
+
+s_function = "spline3", s_order = 1 (sensfunc)
+.LS
+Function and order used to fit the sensitivity data.  The function types
+are "chebyshev" polynomial, "legendre" polynomial, "spline3" cubic spline,
+and "spline1" linear spline.  Order of the sensitivity fitting function.
+The value corresponds to the number of polynomial terms or the number of
+spline pieces.  The default values may be changed interactively.
+.LE
+fnu = no (calibrate)
+.LS
+The default calibration is into units of F-lambda. If \f(CWfnu\fR = yes then
+the calibrated spectrum will be in units of F-nu.
+.LE
+
+.ce
+PACKAGE PARAMETERS
+
+The following package parameters are used by this task.  The default values
+may vary depending on the package.
+
+dispaxis = 2
+.LS
+Default dispersion axis.  The dispersion axis is 1 for dispersion
+running along image lines and 2 for dispersion running along image
+columns.  If the image header parameter DISPAXIS is defined it has
+precedence over this parameter.  The default value defers to the
+package parameter of the same name.
+.LE
+extinction (standard, sensfunc, calibrate)
+.LS
+Extinction file for a site.  There are two extinction files in the
+NOAO standards library, onedstds$, for KPNO and CTIO.  These extinction
+files are used for extinction and flux calibration.
+.LE
+caldir (standard)
+.LS
+Standard star calibration directory.  A directory containing standard
+star data files.  Note that the directory name must end with '/'.
+There are a number of standard star calibrations directories in the NOAO
+standards library, onedstds$.
+.LE
+observatory = "observatory" (observatory)
+.LS
+The default observatory to use for latitude dependent computations.
+If the OBSERVAT keyword in the image header it takes precedence over
+this parameter.
+.LE
+interp = "poly5" (nearest|linear|poly3|poly5|spline3|sinc) (dispcor)
+.LS
+Spectrum interpolation type used when spectra are resampled.  The choices are:
+
+.V1
+	nearest - nearest neighbor
+	 linear - linear
+	  poly3 - 3rd order polynomial
+	  poly5 - 5th order polynomial
+	spline3 - cubic spline
+	   sinc - sinc function
+.V2
+.LE
+database = "database"
+.LS
+Database name used by various tasks.  This is a directory which is created
+if necessary.
+.LE
+verbose = no
+.LS
+Verbose output?  If set then almost all the information written to the
+logfile is also written to the terminal except when the task is a
+background or batch process.
+.LE
+logfile = "logfile"
+.LS
+If specified detailed text log information is written to this file.
+.LE
+plotfile = ""
+.LS
+If specified metacode plots are recorded in this file for later review.
+Since plot information can become large this should be used only if
+really desired.
+.LE
+
+.ce
+ENVIRONMENT PARAMETERS
+.LP
+The environment parameter \fIimtype\fR is used to determine the extension
+of the images to be processed and created.  This allows use with any
+supported image extension.  For STF images the extension has to be exact;
+for example "d1h".
diff --git a/noao/imred/specred/doc/msresp1d.hlp b/noao/imred/specred/doc/msresp1d.hlp
new file mode 100644
index 00000000..cc3dfed2
--- /dev/null
+++ b/noao/imred/specred/doc/msresp1d.hlp
@@ -0,0 +1,191 @@
+.help msresp1d Feb92 noao.imred.specred
+.ih
+NAME
+msresp1d -- Create 1D aperture response from flat and throughput data
+.ih
+USAGE
+msresp1d flat throughput apreference response
+.ih
+PARAMETERS
+.ls flat
+Flat field image to extract and normalize to create a one dimensional
+aperture response image.  If no flat field is specified then a throughput
+image or file must be specified and only a throughput correction will be
+created.  Note that the two dimensional unextracted image is specified.
+If an extracted image of the same name with the ".ms" extension is present
+it is used without reextraction though the unextracted image must also
+be present.
+.le
+.ls throughput
+Throughput file or image.  If an image is specified, typically a blank sky
+observation, the total flux through each aperture is used to correct for
+the aperture throughput.  If a file consisting of lines with the aperture
+number and relative throughput is specified then the aperture throughput
+will be generated by those values.  If neither is specified but a flat
+field image is given the flat field is used to compute the throughput.
+Note that the image is a two dimensional unextracted image.  If an
+extracted image of the same name with the ".ms" extension is present
+it is used without reextraction though the unextracted image must also
+be present.
+.le
+.ls apreference
+Aperture reference spectrum.  If not specified the apertures are defined
+using the flat field or throughput images.  If only a throughput file
+is used then an aperture reference spectrum must be specified to define
+the apertures and dimensions of the final response image.
+.le
+.ls response
+Response spectrum to be created.
+.le
+
+.ls recenter = no
+Recenter throughput image apertures?
+.le
+.ls edit = yes
+Edit and review apertures?
+.le
+.ls trace = no
+Trace spectra?
+.le
+.ls clean = no
+Detect and replace bad pixels?
+.le
+.ls fitflat = yes
+Fit and ratio flat field spectrum?
+.le
+.ls interactive = yes
+Interactive flat field fit?
+.le
+.ls function = "spline3", order = 20
+Flat field fitting function and order.  The functions may be one of
+"chebyshev", "legendre", "spline1" (linear spline), or "spline3" (cubic spline).
+The order is either the number of polynomial terms or the number of spline
+pieces.
+.le
+.ih
+OTHER PARAMETERS
+The package parameters control logging of the operations performed and
+the verbose option allows printing of some progress information.  The
+graphics use the device defined by the STDGRAPH variable and cursor
+input is with the parameter \fIcl.gcur\fR.
+
+Aperture extraction is done using the task \fBapall\fR and any parameters
+not overridden by task parameters will be used; for example the detector
+noise parameters.
+.ih
+DESCRIPTION
+For multiaperture or multifiber spectra a throughput aperture correction 
+must be applied to extracted object spectra.  Also it is often better to
+divide by a one dimensional flat field than a two dimensional one.  This
+is valid provided the pixels sampled by the flat field and object are
+essentially the same.  The advantages are that interspectrum pixels where
+there is little signal are not used and small shifts (fractions of a pixel)
+can be tolerated.  The task \fBmsresp1d\fR creates a multiaperture image
+containing one dimensional flat field and throughput corrections which
+can be directly divided into extracted object spectra.
+
+If a one dimensional flat field is to be determined the flat field spectra
+are extracted unless an extracted image having the specified flat field
+name with the ".ms" extension is present.  If the \fIfitflat\fR parameter
+is set then all the spectra are averaged and a smooth function is fit to
+this composite flat field spectrum.  The smooth fit is divided into the
+individual flat field spectra.  This removes the mean flat field spectrum
+shape, thus avoiding introducing the inverse of the flat field spectrum
+into the object spectra and changing the approximate count levels in the
+object.  This procedure is recommended.  Note that it does not matter if
+the individual fibers have differing spectral shapes (such as might happen
+with a combination of fibers with differing spectral throughput) because
+only a common function is used.  The fitting is done using the \fBfit1d\fR
+task based on the \fBicfit\fR function fitting routines.  When the
+\fIinteractive\fR flag is set the fitting may be done interactively
+allowing iteration on the fitting function and other fitting parameters.
+Note that the function fit should follow the overall shape using a fairly
+high order.
+
+If no throughput image or file is specified the relative strengths
+of the flat field spectra define a throughput correction.  If a
+separate throughput image or file is given then the individual
+flat field spectra are normalized to unity and then scaled by the
+throughput determined from the image or file.
+
+If a throughput image, such as a blank sky observation, is specified it is
+extracted if needed.  The extracted sky spectra are divided by the flat
+field which is not yet corrected for throughput variations.  The total flux
+through each aperture is then found to define the relative throughputs of
+the apertures.  If a flat field was also specified the throughput values
+are multiplied into the normalized flat field otherwise the response image
+will consist of constant spectra with the relative throughputs derived from
+the image.
+
+If a throughput file is specified the throughput values for each aperture
+are defined from this file.  The file consists of lines with two columns,
+the aperture number and the relative throughput.  All apertures should
+be represented.  If a flat field was also specified the throughput values
+are multiplied into the normalized flat field.  If no flat field
+is given then the aperture reference image must be specified and it
+will be extracted, if necessary, to provide the template for the response
+image having constant values for each aperture spectrum.
+
+It is an error unless one or both of the flat field and throughput
+are specified.
+
+The last stage is to normalize of the response spectra over
+all apertures to a global unit mean.  Because of this step the throughput
+values derived from the flat field, throughput image, or throughput
+file need only be relative.  Log information is recorded and printed
+which includes the final relative throughputs values.
+
+Aperture extraction is done using the task \fBapall\fR and any parameters
+not overridden by task parameters will be used; for example the detector
+noise parameters.  Task parmeters control whether recentering,
+aperture review, and tracing are done.  If no aperture reference is
+specified the apertures will be defined as the task is run.
+The aperture reference, if defined, is often the same as the flat field.
+.ih
+EXAMPLES
+1.  To make a flat field response and apply it to an extracted object:
+
+.nf
+    ms> msred.verbose=yes
+    ms> msresp1d flat005 "" "" resp005.ms
+    Extract flat field flat005
+    Searching aperture database ...
+    Sep  7 14:36: DATABASE  - 44 apertures read for flat005.
+    Resize apertures for flat005?  (yes): n
+    Edit apertures for flat005?  (yes): n
+    Extract aperture spectra for flat005?  (yes): 
+    Review extracted spectra from flat005?  (yes): n
+    Extracting apertures ...
+    Sep  7 14:37: EXTRACT - Aperture 1 from flat005 --> flat005.ms
+    Sep  7 14:37: EXTRACT - Aperture 2 from flat005 --> flat005.ms
+    Sep  7 14:37: EXTRACT - Aperture 3 from flat005 --> flat005.ms
+    Sep  7 14:37: EXTRACT - Aperture 4 from flat005 --> flat005.ms
+    Sep  7 14:37: EXTRACT - Aperture 5 from flat005 --> flat005.ms
+    <etc>
+    Fit and ratio flat field flat005
+    <Interactive fitting of average extracted flat field>
+    Create the normalized response resp005.ms
+    Sep  7 14:38 BSCALE: image = resp005.ms
+      bzero=0.  bscale=1.0  mean=1.0  median=1.02386  mode=1.07141
+    Average fiber response:
+      1  0.8049859
+      2  0.6428247
+      3  0.9014022
+      4  0.7955039
+      5  0.9898984
+      <etc>
+    ms> imarith obj006.ms / resp005.ms obj006.ms
+.fi
+
+Of course the extracted object spectra must be the same in terms of apertures,
+wavelength coverage, etc.
+
+2.  To make only a throughput correction:
+
+.nf
+    ms> msresp1d "" obj005 "" resp005
+.fi
+.ih
+SEE ALSO
+icfit, fit1d, apflatten, apnormalize, dofibers
+.endhelp
diff --git a/noao/imred/specred/doc/skysub.hlp b/noao/imred/specred/doc/skysub.hlp
new file mode 100644
index 00000000..75392822
--- /dev/null
+++ b/noao/imred/specred/doc/skysub.hlp
@@ -0,0 +1,98 @@
+.help skysub Mar94 noao.imred.specred
+.ih
+NAME
+skysub -- Sky subtract extracted multispec spectra
+.ih
+USAGE
+skysub input
+.ih
+PARAMETERS
+.ls input
+List of input multispec spectra to sky subtract.
+.le
+.ls output = ""
+List of output sky subtracted spectra.  If no output is specified then
+the output replaces the input spectra.
+.le
+.ls objaps = "", objbeams = ""
+Object aperture and beam numbers.  An empty list selects all aperture
+or beam numbers.  Only the selected apertures are sky subtracted.
+Other apertures are left unmodified.  Note that it is valid to include
+the sky apertures in the object selection which results in residual
+sky spectra after subtraction by a mean sky.
+.le
+.ls skyaps = "", skybeams = ""
+Sky aperture and beam numbers.  An empty list selects all aperture or
+beam numbers.
+.le
+.ls skyedit = yes
+Edit the sky spectra?  If yes the sky spectra are graphed using the
+task \fBspecplot\fR and the user may delete contaminated sky spectra with
+the 'd' key and exit with 'q'.
+.le
+.ls combine = "average" (average|median|sum)
+Option for combining pixels at the same dispersion coordinate after any
+rejection operation.  The options are to compute the  "average", "median",
+or "sum" of the pixels.  The median uses the average of the two central
+values when the number of pixels is even.
+.le
+.ls reject = "none" (none|minmax|avsigclip)
+Type of rejection operation performed on the pixels which overlap at each
+dispersion coordinate.  The algorithms are discussed in the
+DESCRIPTION section.  The rejection choices are:
+
+.nf
+      none - No rejection
+    minmax - Reject the nlow and nhigh pixels
+ avsigclip - Reject pixels using an averaged sigma clipping algorithm
+.fi
+
+.le
+.ls scale = no
+Scale the sky spectra by the mode?
+.le
+.ls saveskys = yes
+Save the sky spectra?  If no then the mean sky spectra will be deleted after
+sky subtraction is completed.  Otherwise a one dimensional image with
+the prefix "sky" and then the output name is created.
+.le
+.ls logfile = ""
+Logfile for making a record of the sky subtraction operation.
+.le
+.ih
+DESCRIPTION
+This task selects a subset of aperture spectra from a multispec
+format image, called sky spectra though they could be anything,
+and combines them into a master spectrum which is subtracted
+from another subset of spectra called the objects.  Options include
+saving the master sky spectrum and reviewing the selected sky spectra
+graphically and deleting some of them.
+
+The sky apertures are selected using the aperture and beam numbers
+defined during extraction (see the \fBapextract\fR package).  In
+some applications the beam numbers are used to code object and sky
+apertures and selection by beam number is quite easy.  Otherwise one
+must list the aperture numbers explicitly.
+
+The object apertures are also selected using an aperture and beam
+number list.  Spectra not selected to be objects are not modified
+by the sky subtraction.  Note that it is perfectly valid to include
+the sky spectra in the object list to produce residual sky spectra.
+
+When interactively editing the sky spectra the task \fBspecplot\fR
+is used.  To delete a spectrum type 'd'.  To undelete the last deleted
+spectrum type 'e'.  When finished type 'e'.
+
+The sky spectra are combined using one of combining and rejection options from
+the task \fBscombine\fR except for the option "none".
+.ih
+EXAMPLES
+1.  To median and subtract apertures 1,10,15,20 from all apertures:
+
+.nf
+    ms> skysub obj010.ms out=skysub010.ms skyaps="1,10,15,20"
+.fi
+.ih
+SEE ALSO
+specplot, scombine
+.endhelp
diff --git a/noao/imred/specred/dofibers.cl b/noao/imred/specred/dofibers.cl
new file mode 100644
index 00000000..90a10b7e
--- /dev/null
+++ b/noao/imred/specred/dofibers.cl
@@ -0,0 +1,74 @@
+# DOFIBERS -- Process fiber spectra from 2D to wavelength calibrated 1D.
+#
+# The task PROC does all of the interactive work and BATCH does the
+# background work.  This procedure is organized this way to minimize the
+# dictionary space when the background task is submitted.
+
+procedure dofibers (objects)
+
+string	objects = ""		{prompt="List of object spectra"}
+
+file	apref = ""		{prompt="Aperture reference spectrum"}
+file	flat = ""		{prompt="Flat field spectrum"}
+file	throughput = ""		{prompt="Throughput file or image (optional)"}
+string	arcs1 = ""		{prompt="List of arc spectra"}
+string	arcs2 = ""		{prompt="List of shift arc spectra"}
+file	arctable = ""		{prompt="Arc assignment table (optional)\n"}
+
+string	readnoise = "0."	{prompt="Read out noise sigma (photons)"}
+string	gain = "1."		{prompt="Photon gain (photons/data number)"}
+real	datamax = INDEF		{prompt="Max data value / cosmic ray threshold"}
+int	fibers = 97		{prompt="Number of fibers"}
+real	width = 12.		{prompt="Width of profiles (pixels)"}
+real	minsep = 8.	{prompt="Minimum separation between fibers (pixels)"}
+real	maxsep = 15.	{prompt="Maximum separation between fibers (pixels)"}
+file	apidtable = ""		{prompt="Aperture identifications"}
+string	crval = "INDEF"		{prompt="Approximate central wavelength"}
+string	cdelt = "INDEF"		{prompt="Approximate dispersion"}
+string	objaps = ""		{prompt="Object apertures"}
+string	skyaps = ""		{prompt="Sky apertures"}
+string	arcaps = ""		{prompt="Arc apertures"}
+string	objbeams = "0,1"	{prompt="Object beam numbers"}
+string	skybeams = "0"		{prompt="Sky beam numbers"}
+string	arcbeams = ""		{prompt="Arc beam numbers\n"}
+
+bool	scattered = no		{prompt="Subtract scattered light?"}
+bool	fitflat = yes		{prompt="Fit and ratio flat field spectrum?"}
+bool	clean = yes		{prompt="Detect and replace bad pixels?"}
+bool	dispcor = yes		{prompt="Dispersion correct spectra?"}
+bool	skyalign = no		{prompt="Align sky lines?"}
+bool	savearcs = yes		{prompt="Save simultaneous arc apertures?"}
+bool	skysubtract = yes	{prompt="Subtract sky?"}
+bool	skyedit = yes		{prompt="Edit the sky spectra?"}
+bool	saveskys = yes		{prompt="Save sky spectra?"}
+bool	splot = no		{prompt="Plot the final spectrum?"}
+bool	redo = no		{prompt="Redo operations if previously done?"}
+bool	update = yes		{prompt="Update spectra if cal data changes?"}
+bool	batch = no		{prompt="Extract objects in batch?"}
+bool	listonly = no		{prompt="List steps but don't process?\n"}
+
+pset	params = ""		{prompt="Algorithm parameters"}
+
+begin
+	apscript.readnoise = readnoise
+	apscript.gain = gain
+	apscript.nfind = fibers
+	apscript.width = width
+	apscript.t_width = width
+	apscript.minsep = minsep
+	apscript.maxsep = maxsep
+	apscript.radius = minsep
+	apscript.clean = clean
+	proc.datamax = datamax
+
+	proc (objects, apref, flat, throughput, arcs1, arcs2, "",
+	    arctable, fibers, apidtable, crval, cdelt, objaps, skyaps,
+	    arcaps, objbeams, skybeams, arcbeams, scattered, fitflat, no,
+	    no, no, no, clean, dispcor, savearcs, skyalign, skysubtract,
+	    skyedit, saveskys, splot, redo, update, batch, listonly)
+
+	if (proc.dobatch) {
+	    print ("-- Do remaining spectra as a batch job --")
+	    print ("batch&batch") | cl
+	}
+end
diff --git a/noao/imred/specred/dofibers.par b/noao/imred/specred/dofibers.par
new file mode 100644
index 00000000..cbe2e2a0
--- /dev/null
+++ b/noao/imred/specred/dofibers.par
@@ -0,0 +1,42 @@
+objects,s,a,"",,,"List of object spectra"
+apref,f,h,"",,,"Aperture reference spectrum"
+flat,f,h,"",,,"Flat field spectrum"
+throughput,f,h,"",,,"Throughput file or image (optional)"
+arcs1,s,h,"",,,"List of arc spectra"
+arcs2,s,h,"",,,"List of shift arc spectra"
+arctable,f,h,"",,,"Arc assignment table (optional)
+"
+readnoise,s,h,"0.",,,"Read out noise sigma (photons)"
+gain,s,h,"1.",,,"Photon gain (photons/data number)"
+datamax,r,h,INDEF,,,"Max data value / cosmic ray threshold"
+fibers,i,h,97,,,"Number of fibers"
+width,r,h,12.,,,"Width of profiles (pixels)"
+minsep,r,h,8.,,,"Minimum separation between fibers (pixels)"
+maxsep,r,h,15.,,,"Maximum separation between fibers (pixels)"
+apidtable,f,h,"",,,"Aperture identifications"
+crval,s,h,INDEF,,,"Approximate central wavelength"
+cdelt,s,h,INDEF,,,"Approximate dispersion"
+objaps,s,h,"",,,"Object apertures"
+skyaps,s,h,"",,,"Sky apertures"
+arcaps,s,h,"",,,"Arc apertures"
+objbeams,s,h,"0,1",,,"Object beam numbers"
+skybeams,s,h,"0",,,"Sky beam numbers"
+arcbeams,s,h,"",,,"Arc beam numbers
+"
+scattered,b,h,no,,,"Subtract scattered light?"
+fitflat,b,h,yes,,,"Fit and ratio flat field spectrum?"
+clean,b,h,yes,,,"Detect and replace bad pixels?"
+dispcor,b,h,yes,,,"Dispersion correct spectra?"
+skyalign,b,h,no,,,"Align sky lines?"
+savearcs,b,h,yes,,,"Save simultaneous arc apertures?"
+skysubtract,b,h,yes,,,"Subtract sky?"
+skyedit,b,h,yes,,,"Edit the sky spectra?"
+saveskys,b,h,yes,,,"Save sky spectra?"
+splot,b,h,no,,,"Plot the final spectrum?"
+redo,b,h,no,,,"Redo operations if previously done?"
+update,b,h,yes,,,"Update spectra if cal data changes?"
+batch,b,h,no,,,"Extract objects in batch?"
+listonly,b,h,no,,,"List steps but don\'t process?
+"
+params,pset,h,"",,,"Algorithm parameters"
+mode,s,h,"ql",,,
diff --git a/noao/imred/specred/msresp1d.cl b/noao/imred/specred/msresp1d.cl
new file mode 100644
index 00000000..1083c64d
--- /dev/null
+++ b/noao/imred/specred/msresp1d.cl
@@ -0,0 +1,234 @@
+# MSRESP1D -- Make a aperture response spectrum using a flat field
+# and a throughput file or image.
+
+procedure msresp1d (flat, throughput, apreference, response)
+
+string	flat			{prompt="Flat field spectrum"}
+string	throughput		{prompt="Throughput file or image"}
+string	apreference		{prompt="Aperture reference spectrum"}
+string	response		{prompt="Response spectrum"}
+
+bool	recenter = no		{prompt="Recenter apertures?"}
+bool	edit = yes		{prompt="Edit/review apertures?"}
+bool	trace = no		{prompt="Trace spectra?"}
+bool	clean = no		{prompt="Detect and replace bad pixels?"}
+bool	fitflat = no		{prompt="Fit and ratio flat field spectrum?"}
+bool	interactive = yes	{prompt="Fit flat field interactively?"}
+string	function = "spline3"	{prompt="Fitting function",
+				 enum="spline3|legendre|chebyshev|spline1"}
+int	order = 20		{prompt="Fitting function order", min=1}
+
+begin
+	file	flat2d, skyflat2d, apref, resp
+	file	temp1, temp2, log1, log2
+	string	imtype, mstype
+	int	i, n, ap, naxis
+	real	respval
+
+	flat2d = flat
+	skyflat2d = throughput
+	apref = apreference
+	resp = response
+	temp1 = mktemp ("tmp")
+	temp2 = mktemp ("tmp")
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	mstype = ".ms" // imtype
+	n = strlen (imtype)
+
+	# Check required input and output.
+ 	if (resp == "" || resp == flat2d || resp == skyflat2d)
+ 	    error (1, "Bad response image name")
+	if (flat2d == "" && skyflat2d == "")
+	    error (1, "No flat field or throughput specified")
+
+	if (flat2d != "") {
+	    i = strlen (flat2d)
+	    if (i > n && substr (flat2d, i-n+1, i) == imtype)
+		flat2d = substr (flat2d, 1, i-n)
+	    if (!access (flat2d // imtype))
+		error (1, "Flat field spectrum not found - " // flat2d)
+	}
+	if (skyflat2d != "") {
+	    i = strlen (skyflat2d)
+	    if (i > n && substr (skyflat2d, i-n+1, i) == imtype)
+	        skyflat2d = substr (skyflat2d, 1, i-n)
+	    if (!access (skyflat2d // imtype)) {
+		if (!access (skyflat2d))
+		    error (1,
+			"Throughput file or image not found - " // skyflat2d)
+
+		if (flat2d == "") {
+		    i = strlen (apref)
+		    if (i > n && substr (apref, i-n+1, i) == imtype)
+			apref = substr (apref, 1, i-n)
+		    if (!access (apref // imtype))
+			error (1, "Aperture reference image required")
+		}
+	    }
+	}
+
+	# Set logging
+	tee.append = yes
+	if (logfile == "")
+	    log1 = "dev$null"
+	else
+	    log1 = logfile
+	if (verbose)
+	    log2 = "STDOUT"
+	else
+	    log2 = "dev$null"
+
+	# If using a flat field extract it if necessary and possibly fit it
+	# and ratio the individual apertures by an overall smooth function
+
+	if (flat2d != "") {
+	    if (!access (flat2d // mstype)) {
+		print ("Extract flat field ", flat2d) | tee (log1)
+		if (flat2d != apref)
+		    apall (flat2d, output=resp, references=apref, profiles="",
+			interactive=yes, find=yes, recenter=recenter,
+			resize=no, edit=edit, trace=trace, fittrace=yes,
+			extract=yes, review=no, background="none", clean=clean,
+			extras=no)
+		else
+		    apall (flat2d, output=resp, references=apref, profiles="",
+			interactive=no, find=yes, recenter=no, resize=no,
+			edit=edit, trace=no, fittrace=yes, extract=yes,
+			review=no, background="none", clean=clean, extras=no)
+	    } else
+		imcopy (flat2d//".ms", resp, verbose=no)
+
+	    if (fitflat) {
+		print ("Fit and ratio flat field ", flat2d) | tee (log1)
+		blkavg (resp, temp1, option="average", b1=1, b2=10000)
+		imcopy (temp1//"[*,1]", temp1, verbose=no)
+		fit1d (temp1, temp1, "fit", axis=1, interactive=interactive,
+		    sample="*", naverage=1, function=function, order=order,
+		    low_reject=0., high_reject=0., niterate=1, grow=0.,
+		    graphics="stdgraph")
+		sarith (resp, "/", temp1, resp, w1=INDEF, w2=INDEF,
+		    apertures="", beams="", apmodulus=0, reverse=no,
+		    ignoreaps=yes, format="multispec", renumber=no, offset=0,
+		    clobber=yes, merge=no, errval=0, verbose=no)
+		imdelete (temp1, verify=no)
+	    }
+	}
+
+	# If using a throughput image extract it if necessary.
+	# Apply it to the flat field if given and otherwise only
+	# compute the throughput through each aperture.
+
+	if (skyflat2d != "") {
+	    if (access (skyflat2d // imtype)) {
+		if (!access (skyflat2d // mstype)) {
+		    print ("Extract throughput image ", skyflat2d) | tee (log1)
+		    apall (skyflat2d, output=temp1, references=apref,
+			profiles="", interactive=yes, find=yes,
+			recenter=recenter, resize=no, edit=edit,
+			trace=trace, fittrace=yes, extract=yes, review=no,
+			background="none", clean=clean, extras=no)
+		    temp2 = temp1
+		} else
+		    temp2 = skyflat2d // ".ms"
+
+		if (flat2d != "") {
+		    print ("Correct flat field to throughput image") |
+			tee (log1)
+		    sarith (temp2, "/", resp, temp1, w1=INDEF, w2=INDEF,
+			apertures="", beams="", apmodulus=0, reverse=no,
+			ignoreaps=no, format="multispec", renumber=no, offset=0,
+			clobber=yes, merge=no, errval=0, verbose=no)
+		    fit1d (temp1, temp1, type="fit", axis=1,
+			interactive=no, sample="*", naverage=1,
+			function="legendre", order=1, niterate=0)
+		    sarith (resp, "*", temp1, resp, w1=INDEF, w2=INDEF,
+			apertures="", beams="", apmodulus=0, reverse=no,
+			ignoreaps=yes, format="multispec", renumber=no,
+			offset=0, clobber=yes, merge=no, errval=0, verbose=no)
+		    imdelete (temp1, verify=no)
+		} else {
+		    print ("Compute aperture throughput from image") |
+			tee (log1)
+		    fit1d (temp2, resp, type="fit", axis=1,
+			interactive=no, sample="*", naverage=1,
+			function="legendre", order=1, niterate=0)
+		    if (temp2 == temp1)
+			imdelete (temp2, verify=no)
+		}
+
+	    # If a flat field and throughput file are used scale the average
+	    # flat field in each aperture to those values
+
+	    } else if (flat2d != "") {
+		print ("Correct flat field with throughput file ", skyflat2d) |
+		    tee (log1)
+		fit1d (resp, resp, type="ratio", axis=1,
+		    interactive=no, sample="*", naverage=1,
+		    function="legendre", order=1, niterate=0)
+
+		list = skyflat2d
+		while (fscan (list, ap, respval) != EOF) {
+		    sarith (resp, "*", respval, resp, w1=INDEF, w2=INDEF,
+		        apertures=ap, beams="", apmodulus=0, reverse=no,
+		        ignoreaps=no, format="multispec", renumber=no,
+			offset=0, clobber=yes, merge=yes, errval=0.,
+			verbose=no)
+		}
+		list = ""
+
+	    # If only a throughput file is given create the response from the
+	    # aperture reference and set the aperture response to the specified
+	    # values.
+
+	    } else {
+		print ("Set aperture throughput using ", skyflat2d) | tee (log1)
+		if (!access (apref // mstype)) {
+		    apall (apref, output=resp, references=apref,
+			profiles="", interactive=no, find=yes, recenter=no,
+			resize=no, edit=edit, trace=no, fittrace=yes,
+			extract=yes, review=no, background="none", clean=no,
+			extras=no)
+		    sarith (resp, "replace", "0", resp, w1=INDEF, w2=INDEF,
+			apertures="", beams="", apmodulus=0, reverse=no,
+			ignoreaps=no, format="multispec", renumber=no,
+			offset=0, clobber=yes, merge=yes, errval=0., verbose=no)
+		} else
+		    sarith (apref//".ms", "replace", "0", resp, w1=INDEF,
+			w2=INDEF, apertures="", beams="", apmodulus=0,
+			reverse=no, ignoreaps=no, format="multispec",
+			renumber=no, offset=0, clobber=yes, merge=yes,
+			errval=0., verbose=no)
+
+		list = skyflat2d
+		while (fscan (list, ap, respval) != EOF) {
+		    sarith (resp, "replace", respval, resp, w1=INDEF, w2=INDEF,
+		        apertures=ap, beams="", apmodulus=0, reverse=no,
+		        ignoreaps=no, format="multispec", renumber=no,
+			offset=0, clobber=yes, merge=yes, errval=0.,
+			verbose=no)
+		}
+		list = ""
+	    }
+	}
+
+	# The final response is normalized to overall unit mean and the
+	# average aperture response is printed.
+
+	print ("Create the normalized response ", resp) | tee (log1)
+	bscale (resp, resp, bzero="0.", bscale="mean", section="",
+	    step=1, upper=INDEF, lower=INDEF, verbose=yes) | tee (log1, >log2)
+	blkavg (resp, temp1, option="average", b1=10000, b2=1)
+	print ("Average aperture response:") | tee (log1, >log2)
+	hselect (temp1, "naxis", yes, > temp2)
+	list = temp2; ap = fscan (list, naxis)
+	if (naxis == 1)
+	    listpixels (temp1) | tee (log1, >log2)
+	else
+	    listpixels (temp1//"[1,*]") | tee (log1, >log2)
+	list = ""; delete (temp2, verify=no)
+	imdelete (temp1, verify=no)
+end
diff --git a/noao/imred/specred/msresp1d.par b/noao/imred/specred/msresp1d.par
new file mode 100644
index 00000000..9a59eb46
--- /dev/null
+++ b/noao/imred/specred/msresp1d.par
@@ -0,0 +1,13 @@
+flat,s,a,,,,"Flat field spectrum"
+throughput,s,a,,,,"Throughput file or image"
+apreference,s,a,,,,"Aperture reference spectrum"
+response,s,a,,,,"Response spectrum"
+recenter,b,h,no,,,"Recenter apertures?"
+edit,b,h,yes,,,"Edit/review apertures?"
+trace,b,h,no,,,"Trace spectra?"
+clean,b,h,no,,,"Detect and replace bad pixels?"
+fitflat,b,h,no,,,"Fit and ratio flat field spectrum?"
+interactive,b,h,yes,,,"Fit flat field interactively?"
+function,s,h,"spline3",spline3|legendre|chebyshev|spline1,,"Fitting function"
+order,i,h,20,1,,"Fitting function order"
+mode,s,h,"ql",,,
diff --git a/noao/imred/specred/params.par b/noao/imred/specred/params.par
new file mode 100644
index 00000000..fab14009
--- /dev/null
+++ b/noao/imred/specred/params.par
@@ -0,0 +1,67 @@
+line,i,h,INDEF,,,"Default dispersion line"
+nsum,i,h,10,,,"Number of dispersion lines to sum or median"
+order,s,h,"decreasing","increasing|decreasing",,"Order of apertures"
+extras,b,h,no,,,"Extract sky, sigma, etc.?
+
+-- DEFAULT APERTURE LIMITS --"
+lower,r,h,-5.,,,"Lower aperture limit relative to center"
+upper,r,h,5.,,,"Upper aperture limit relative to center
+
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --"
+ylevel,r,h,0.05,,,"Fraction of peak or intensity for resizing
+
+-- TRACE PARAMETERS --"
+t_step,i,h,10,,,"Tracing step"
+t_function,s,h,"spline3","chebyshev|legendre|spline1|spline3",,"Trace fitting function"
+t_order,i,h,3,,,"Trace fitting function order"
+t_niterate,i,h,1,0,,"Trace rejection iterations"
+t_low,r,h,3.,0.,,"Trace lower rejection sigma"
+t_high,r,h,3.,0.,,"Trace upper rejection sigma
+
+-- SCATTERED LIGHT PARAMETERS --"
+buffer,r,h,1.,0.,,Buffer distance from apertures
+apscat1,pset,h,"",,,Fitting parameters across the dispersion
+apscat2,pset,h,"",,,"Fitting parameters along the dispersion
+
+-- APERTURE EXTRACTION PARAMETERS --"
+weights,s,h,"none","none|variance",,Extraction weights (none|variance)
+pfit,s,h,"fit1d","fit1d|fit2d",,Profile fitting algorithm (fit1d|fit2d)
+lsigma,r,h,3.,,,Lower rejection threshold
+usigma,r,h,3.,,,Upper rejection threshold
+nsubaps,i,h,1,1,,"Number of subapertures
+
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --"
+f_interactive,b,h,yes,,,"Fit flat field interactively?"
+f_function,s,h,"spline3",spline3|legendre|chebyshev|spline1,,"Fitting function"
+f_order,i,h,10,1,,"Fitting function order
+
+-- ARC DISPERSION FUNCTION PARAMETERS --"
+threshold,r,h,10.,0.,,"Minimum line contrast threshold"
+coordlist,f,h,linelists$idhenear.dat,,,"Line list"
+match,r,h,-3.,,,"Line list matching limit in Angstroms"
+fwidth,r,h,4.,,,"Arc line widths in pixels"
+cradius,r,h,10.,,,Centering radius in pixels
+i_function,s,h,"spline3","legendre|chebyshev|spline1|spline3",,"Coordinate function"
+i_order,i,h,3,1,,"Order of dispersion function"
+i_niterate,i,h,2,0,,"Rejection iterations"
+i_low,r,h,3.,0.,,"Lower rejection sigma"
+i_high,r,h,3.,0.,,"Upper rejection sigma"
+refit,b,h,yes,,,"Refit coordinate function when reidentifying?"
+addfeatures,b,h,no,,,"Add features when reidentifying?
+
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --"
+select,s,h,"interp",,,"Selection method for reference spectra"
+sort,s,h,"jd",,,"Sort key"
+group,s,h,"ljd",,,"Group key"
+time,b,h,no,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting
+
+-- DISPERSION CORRECTION PARAMETERS --"
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+log,b,h,no,,,"Logarithmic wavelength scale?"
+flux,b,h,yes,,,"Conserve flux?
+
+-- SKY SUBTRACTION PARAMETERS --"
+combine,s,h,"average","average|median",,Type of combine operation
+reject,s,h,"avsigclip","none|minmax|avsigclip",,"Sky rejection option"
+scale,s,h,"none","none|mode|median|mean",,"Sky scaling option"
diff --git a/noao/imred/specred/sparams.par b/noao/imred/specred/sparams.par
new file mode 100644
index 00000000..1cc001d8
--- /dev/null
+++ b/noao/imred/specred/sparams.par
@@ -0,0 +1,65 @@
+line,i,h,INDEF,,,"Default dispersion line"
+nsum,i,h,10,,,"Number of dispersion lines to sum or median"
+extras,b,h,no,,,"Extract sky, sigma, etc.?
+
+-- DEFAULT APERTURE PARAMETERS -- "
+lower,r,h,-3.,,,Lower aperture limit relative to center
+upper,r,h,3.,,,"Upper aperture limit relative to center
+
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --"
+ylevel,r,h,0.05,,,"Fraction of peak or intensity for resizing
+
+-- TRACE PARAMETERS --"
+t_step,i,h,10,,,"Tracing step"
+t_function,s,h,"spline3","chebyshev|legendre|spline1|spline3",,"Trace fitting function"
+t_order,i,h,1,,,"Trace fitting function order"
+t_niterate,i,h,1,0,,"Trace rejection iterations"
+t_low,r,h,3.,0.,,"Trace lower rejection sigma"
+t_high,r,h,3.,0.,,"Trace upper rejection sigma
+
+-- APERTURE EXTRACTION PARAMETERS --"
+weights,s,h,"none",,,Extraction weights (none|variance)
+pfit,s,h,"fit1d","fit1d|fit2d",,Profile fitting algorithm (fit1d|fit2d)
+lsigma,r,h,3.,,,Lower rejection threshold
+usigma,r,h,3.,,,"Upper rejection threshold
+
+-- BACKGROUND SUBTRACTION PARAMETERS --"
+background,s,h,"fit","none|average|median|minimum|fit",,Background to subtract
+b_function,s,h,"legendre","chebyshev|legendre|spline1|spline3",,"Background function"
+b_order,i,h,1,,,"Background function order"
+b_sample,s,h,"-10:-6,6:10",,,"Background sample regions"
+b_naverage,i,h,-100,,,"Background average or median"
+b_niterate,i,h,1,0,,"Background rejection iterations"
+b_low,r,h,3.,0.,,"Background lower rejection sigma"
+b_high,r,h,3.,0.,,"Background upper rejection sigma
+
+-- ARC DISPERSION FUNCTION PARAMETERS --"
+threshold,r,h,10.,0.,,"Minimum line contrast threshold"
+coordlist,f,h,linelists$idhenear.dat,,,"Line list"
+match,r,h,-3.,,,"Line list matching limit in Angstroms"
+fwidth,r,h,4.,,,"Arc line widths in pixels"
+cradius,r,h,10.,,,Centering radius in pixels
+i_function,s,h,"spline3","legendre|chebyshev|spline1|spline3",,"Coordinate function"
+i_order,i,h,1,1,,"Order of dispersion function"
+i_niterate,i,h,1,0,,"Rejection iterations"
+i_low,r,h,3.,0.,,"Lower rejection sigma"
+i_high,r,h,3.,0.,,"Upper rejection sigma"
+refit,b,h,yes,,,"Refit coordinate function when reidentifying?"
+addfeatures,b,h,no,,,"Add features when reidentifying?
+
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --"
+select,s,h,"interp",,,"Selection method for reference spectra"
+sort,s,h,"jd",,,"Sort key"
+group,s,h,"ljd",,,"Group key"
+time,b,h,no,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting
+
+-- DISPERSION CORRECTION PARAMETERS --"
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+log,b,h,no,,,"Logarithmic wavelength scale?"
+flux,b,h,yes,,,"Conserve flux?
+
+-- SENSITIVITY CALIBRATION PARAMETERS --"
+s_function,s,h,"spline3","chebyshev|legendre|spline3|spline1",,"Fitting function"
+s_order,i,h,1,1,,"Order of sensitivity function"
+fnu,b,h,no,,,"Create spectra having units of FNU?"
diff --git a/noao/imred/specred/specred.cl b/noao/imred/specred/specred.cl
new file mode 100644
index 00000000..ab859853
--- /dev/null
+++ b/noao/imred/specred/specred.cl
@@ -0,0 +1,103 @@
+#{ SPECRED package definition
+
+proto		# bscale
+
+s1 = envget ("min_lenuserarea")
+if (s1 == "")
+    reset min_lenuserarea = 100000
+else if (int (s1) < 100000)
+    reset min_lenuserarea = 100000
+ 
+package specred
+
+# Slitproc
+cl < doslit$doslittasks.cl
+task	sparams		= "specred$sparams.par"
+
+# Dofibers
+task	dofibers	= "specred$dofibers.cl"
+task	params		= "specred$params.par"
+
+task	proc		= "srcfibers$proc.cl"
+task	fibresponse	= "srcfibers$fibresponse.cl"
+task	arcrefs		= "srcfibers$arcrefs.cl"
+task	doarcs		= "srcfibers$doarcs.cl"
+task	doalign		= "srcfibers$doalign.cl"
+task	skysub		= "srcfibers$skysub.cl"
+task	batch		= "srcfibers$batch.cl"
+task	getspec		= "srcfibers$getspec.cl"
+task	listonly	= "srcfibers$listonly.cl"
+task	apscript	= "srcfibers$x_apextract.e"
+
+# Generic fiber reduction tasks
+task	msresp1d	= "specred$msresp1d.cl"
+
+# Onedspec tasks
+task	autoidentify,
+	calibrate,
+	continuum,
+	deredden,
+	dispcor,
+	dopcor,
+	fitprofs,
+	identify,
+	odcombine,
+	refspectra,
+	reidentify,
+	sapertures,
+	sarith,
+	sensfunc,
+	sfit,
+	sflip,
+	slist,
+	skytweak,
+	specplot,
+	specshift,
+	splot,
+	standard,
+	telluric	= "onedspec$x_onedspec.e"
+task	scombine	= "onedspec$scombine/x_scombine.e"
+task	aidpars		= "onedspec$aidpars.par"
+task	bplot		= "onedspec$bplot.cl"
+task	scopy		= "onedspec$scopy.cl"
+task	dispcor1	= "onedspec$dispcor1.par"
+ 
+# Apextract tasks
+task	apall,
+	apedit,
+	apfind,
+	apfit,
+	apflatten,
+	apmask,
+	apnormalize,
+	aprecenter,
+	apresize,
+	apscatter,
+	apsum,
+	aptrace		= "apextract$x_apextract.e"
+task	apparams	= "apextract$apparams.par"
+task	apall1		= "apextract$apall1.par"
+task	apfit1		= "apextract$apfit1.par"
+task	apflat1		= "apextract$apflat1.par"
+task	apnorm1		= "apextract$apnorm1.par"
+task	apdefault	= "apextract$apdefault.par"
+task	apscat1		= "apextract$apscat1.par"
+task	apscat2		= "apextract$apscat2.par"
+
+# Longslit tasks
+task	illumination,
+	lscombine,
+	response,
+	transform	= "twodspec$longslit/x_longslit.e"
+task	background	= "generic$background.cl"
+
+# Astutil tasks
+task	setairmass,
+	setjd		= "astutil$x_astutil.e"
+
+# Hide tasks from the user
+hidetask apparams, apall1, apfit1, apflat1, apnorm1, apscat1, apscat2, dispcor1
+hidetask sparams, params, doalign
+hidetask apscript, proc, batch, arcrefs, doarcs, getspec, listonly, fibresponse
+
+clbye
diff --git a/noao/imred/specred/specred.hd b/noao/imred/specred/specred.hd
new file mode 100644
index 00000000..94f4609b
--- /dev/null
+++ b/noao/imred/specred/specred.hd
@@ -0,0 +1,11 @@
+# Help directory for the SPECRED package.
+ 
+$doc		=	"./doc/"
+$doslit		=	"noao$imred/src/doslit/"
+
+dofibers	hlp=doc$dofibers.hlp,	src=dofibers.cl
+doslit		hlp=doc$doslit.hlp,	src=doslit$doslit.cl
+msresp1d	hlp=doc$msresp1d.hlp,	src=msresp1d.cl
+skysub		hlp=doc$skysub.hlp,	src=srcfibers$skysub.cl
+ 
+revisions	sys=Revisions
diff --git a/noao/imred/specred/specred.men b/noao/imred/specred/specred.men
new file mode 100644
index 00000000..3e2b0130
--- /dev/null
+++ b/noao/imred/specred/specred.men
@@ -0,0 +1,51 @@
+          apall - Extract 1D spectra (all parameters in one task)
+      apdefault - Set the default aperture parameters and apidtable
+         apedit - Edit apertures interactively
+	 apfind - Automatically find spectra and define apertures
+	  apfit - Fit 2D spectra and output the fit, difference, or ratio
+      apflatten - Remove overall spectral and profile shapes from flat fields
+         apmask - Create and IRAF pixel list mask of the apertures
+    apnormalize - Normalize 2D apertures by 1D functions
+     aprecenter - Recenter apertures
+       apresize - Resize apertures
+      apscatter - Fit and subtract scattered light
+          apsum - Extract 1D spectra
+	aptrace - Trace positions of spectra
+
+     background - Fit and subtract a line or column background
+	  bplot - Batch plot of spectra with SPLOT
+      calibrate - Extinction and flux calibrate spectra
+      continuum - Fit the continuum in spectra
+       deredden - Apply interstellar extinction correction
+        dispcor - Dispersion correct spectra
+	 dopcor - Doppler correct spectra
+       fitprofs - Fit gaussian profiles
+       identify - Identify features in spectrum for dispersion solution
+   illumination - Determine illumination calibration
+      lscombine - Combine longslit spectra
+       msresp1d - Create 1D response spectra from flat field and sky spectra
+      odcombine - Combine spectra (new version)
+     refspectra - Assign wavelength reference spectra to other spectra
+     reidentify - Automatically reidentify features in spectra
+       response - Determine response calibration
+     sapertures - Set or change aperture header information
+	 sarith - Spectrum arithmetic
+       scombine - Combine spectra
+          scopy - Select and copy apertures in different spectral formats
+       sensfunc - Compute instrumental sensitivity from standard stars
+     setairmass - Compute effective airmass and middle UT for an exposure
+          setjd - Compute and set Julian dates in images
+	   sfit - Fit spectra and output fit, ratio, or difference
+	  sflip - Flip data and/or dispersion coordinates in spectra
+         skysub - Sky subtract extracted multispec spectra
+       skytweak - Sky subtract 1D spectra after tweaking sky spectra
+          slist - List spectrum header parameters
+       specplot - Scale, stack, and plot multiple spectra
+      specshift - Shift spectral dispersion coordinate systems
+          splot - Preliminary spectral plot/analysis
+       standard - Tabulate standard star counts and fluxes
+       telluric - Remove telluric features from 1D spectra
+      transform - Resample longslit spectra
+
+       dofibers - Process fiber spectra
+         doslit - Process slit spectra
diff --git a/noao/imred/specred/specred.par b/noao/imred/specred/specred.par
new file mode 100644
index 00000000..15471412
--- /dev/null
+++ b/noao/imred/specred/specred.par
@@ -0,0 +1,15 @@
+# SPECRED parameter file
+extinction,s,h,onedstds$kpnoextinct.dat,,,Extinction file
+caldir,s,h,onedstds$spec16redcal/,,,Standard star calibration directory
+observatory,s,h,"observatory",,,Observatory of data
+interp,s,h,"poly5","nearest|linear|poly3|poly5|spline3|sinc",,Interpolation type
+dispaxis,i,h,2,1,3,Image axis for 2D/3D images
+nsum,s,h,"1",,,"Number of lines/columns/bands to sum for 2D/3D images
+"
+database,f,h,"database",,,Database
+verbose,b,h,no,,,Verbose output?
+logfile,s,h,"logfile",,,Log file
+plotfile,s,h,"",,,"Plot file
+"
+records,s,h,"",,,Record number extensions
+version,s,h,"SPECRED V3: April 1992"
diff --git a/noao/imred/src/doecslit/Revisions b/noao/imred/src/doecslit/Revisions
new file mode 100644
index 00000000..c4e6ee16
--- /dev/null
+++ b/noao/imred/src/doecslit/Revisions
@@ -0,0 +1,93 @@
+.help revisions Dec94 noao.imred.src.doecslit
+.nf
+
+=======
+V2.12.3
+=======
+
+doecslit$sdoarcs.cl
+    The sparams.refit parameter was being ignored and the ecreidentify
+    step has refit=yes hardwired.  The parameter reference is now used.
+    (11/14/05, Valdes)
+
+doecslit$sbatch.cl
+doecslit$sproc.cl
+doecslit$fibresponse.cl
+    Error messages now hint to check imtype setting.
+    (4/15/05, Valdes)
+
+========
+V2.12.2b
+========
+
+doecslit$sproc.cl
+    Modified code to eliminate goto.  This is for use with pyraf.
+    (11/21/00, Valdes)
+
+========
+V2.11.3a
+========
+
+doecslit$sproc.cl
+    The arcref and arcrefs variables were not initialized if dispcor=no
+    and if the user goes directly to batch mode there is an undefined
+    local variable error.  Added initialization.  (1/27/98, Valdes)
+
+=======
+V2.11.1
+=======
+
+doecslit$sarcrefs.cl
+doecslit$sbatch.cl
+doecslit$sfluxcal.cl
+doecslit$sgetspec.cl
+doecslit$slistonly.cl
+doecslit$sproc.cl
+doecslit$sdoarcs.cl
+    Any additional qualifiers in the imtype string are stripped.
+    (8/14/97, Valdes)
+
+doecslit$sgetspec.cl
+    Added the field parameter to the RENAME call.  (8/12/97, Valdes)
+
+=========
+V2.11Beta
+=========
+
+doecslit$sbatch.cl
+    Fixed typo bugs in this script.  (10/3/96, Valdes)
+
+doecslit$apslitproc.par
+    Made changes for the new aperture selection option.  (9/5/96, Valdes)
+
+=======
+V2.10.4
+=======
+
+doecslit$sgetspec.cl
+doecslit$doecslit.cl
+    The arc table will now be checked for arc spectra. (5/1/95, Valdes)
+
+doecslit$sparams.par
+doecslit$sdoarcs.cl
+doecslit$sarcrefs.cl
+    Added "threshold" as a user parameter.  (1/16/95, Valdes)
+
+doecslit$sproc.cl
+doecslit$sbatch.cl
+doecslit$sfluxcal.cl
+doecslit$sproc.par
+doecslit$sbatch.par
+doecslit$sfluxcal.par
+    SETAIRMASS and SETJD are only called if the required keywords are
+    present.  Errors from missing airmass or JD are then reported from
+    the task that actually uses them.  (12/31/94, Valdes)
+
+doecslit$sgetspec.cl
+doecslit$sgetspec.par
+    Added warning and query for missing CCDPROC keyword.  (12/31/94, Valdes)
+
+=======
+V2.10.3
+=======
+.endhelp
diff --git a/noao/imred/src/doecslit/apslitproc.par b/noao/imred/src/doecslit/apslitproc.par
new file mode 100644
index 00000000..3233960a
--- /dev/null
+++ b/noao/imred/src/doecslit/apslitproc.par
@@ -0,0 +1,145 @@
+# APSCRIPT
+
+input,s,a,,,,List of input images
+output,s,h,"",,,List of output spectra
+apertures,s,h,"",,,Apertures
+scatter,s,h,"",,,List of scattered light images (optional)
+references,s,h,"",,,List of aperture reference images
+profiles,s,h,"",,,"List of aperture profile images
+"
+interactive,b,h,yes,,,Run task interactively?
+find,b,h,yes,,,Find apertures?
+recenter,b,h,yes,,,Recenter apertures?
+resize,b,h,yes,,,Resize apertures?
+edit,b,h,yes,,,Edit apertures?
+trace,b,h,yes,,,Trace apertures?
+fittrace,b,h,yes,,,Fit the traced points interactively?
+extract,b,h,yes,,,Extract spectra?
+review,b,h,yes,,,Review extractions?
+subtract,b,h,yes,,,Subtract scattered light?
+smooth,b,h,yes,,,Smooth scattered light along the dispersion?
+fitscatter,b,h,yes,,,Fit scattered light interactively?
+fitsmooth,b,h,yes,,,"Smooth the scattered light interactively?
+"
+line,i,h,)sparams.line,,,>sparams.line
+nsum,i,h,)sparams.nsum,,,>sparams.nsum
+buffer,r,h,)sparams.buffer,,,">sparams.buffer
+
+# OUTPUT PARAMETERS
+"
+format,s,h,"echelle",,,Extracted spectra format
+extras,b,h,)sparams.extras,,,"Extract sky, sigma, etc.?"
+dbwrite,s,h,"YES",,,Write to database?
+initialize,b,h,no,,,Initialize answers?
+verbose,b,h,)_.verbose,,,"Verbose output?
+
+# DEFAULT APERTURE PARAMETERS
+"
+lower,r,h,,,,Lower aperture limit relative to center
+upper,r,h,,,,Upper aperture limit relative to center
+apidtable,s,h,"",,,"Aperture ID table (optional)
+
+# DEFAULT BACKGROUND PARAMETERS
+"
+b_function,s,h,)sparams.b_function,,,>sparams.b_function
+b_order,i,h,)sparams.b_order,,,>sparams.b_order
+b_sample,s,h,)sparams.b_sample,,,>sparams.b_sample
+b_naverage,i,h,)sparams.b_naverage,,,>sparams.b_naverage
+b_niterate,i,h,)sparams.b_niterate,,,>sparams.b_niterate
+b_low_reject,r,h,)sparams.b_low,,,>sparams.b_low
+b_high_reject,r,h,)sparams.b_high,,,>sparams.b_high
+b_grow,r,h,0.,0.,,"Background rejection growing radius
+
+# APERTURE CENTERING PARAMETERS
+"
+width,r,h,,,,Profile centering width
+radius,r,h,,,,Profile centering radius
+threshold,r,h,10.,0.,,"Detection threshold for profile centering
+
+# AUTOMATIC FINDING AND ORDERING PARAMETERS
+"
+nfind,i,h,,,,Number of apertures to be found automatically
+minsep,r,h,,,,Minimum separation between spectra
+maxsep,r,h,100000.,,,Maximum separation between spectra
+order,s,h,"increasing",,,"Order of apertures
+
+# RECENTERING PARAMETERS
+"
+aprecenter,s,h,"",,,Apertures for recentering calculation
+npeaks,r,h,INDEF,,,Select brightest peaks
+shift,b,h,yes,,,"Use average shift instead of recentering?
+
+# RESIZING PARAMETERS
+"
+llimit,r,h,INDEF,,,Lower aperture limit relative to center
+ulimit,r,h,INDEF,,,Upper aperture limit relative to center
+ylevel,r,h,)sparams.ylevel,,,>sparams.ylevel
+peak,b,h,yes,,,Is ylevel a fraction of the peak?
+bkg,b,h,yes,,,Subtract background in automatic width?
+r_grow,r,h,0.,,,Grow limits by this factor
+avglimits,b,h,no,,,"Average limits over all apertures?
+
+# EDITING PARAMETERS
+"
+e_output,s,q,,,,Output spectra rootname
+e_profiles,s,q,,,,"Profile reference image
+
+# TRACING PARAMETERS
+"
+t_nsum,i,h,)sparams.nsum,,,>sparams.nsum
+t_step,i,h,)sparams.t_step,,,>sparams.t_step
+t_nlost,i,h,3,1,,Number of consecutive times profile is lost before quitting
+t_width,r,h,)sparams.width,,,>sparams.width
+t_function,s,h,)sparams.t_function,,,>sparams.t_function
+t_sample,s,h,"*",,,Trace sample regions
+t_order,i,h,)sparams.t_order,,,>sparams.t_order
+t_naverage,i,h,1,,,Trace average or median
+t_niterate,i,h,)sparams.t_niterate,,,>sparams.t_niterate
+t_low_reject,r,h,)sparams.t_low,,,>sparams.t_low
+t_high_reject,r,h,)sparams.t_high,,,>sparams.t_high
+t_grow,r,h,0.,0.,,"Trace rejection growing radius
+
+# EXTRACTION PARAMETERS
+"
+background,s,h,,,,Background to subtract
+skybox,i,h,1,,,Box car smoothing length for sky
+weights,s,h,)sparams.weights,,,>sparams.weights
+pfit,s,h,)sparams.pfit,,,>sparams.pfit
+clean,b,h,no,,,Detect and replace bad pixels?
+nclean,r,h,0.5,,,Maximum number of pixels to clean
+niterate,i,h,5,0,,Number of profile fitting iterations
+saturation,r,h,INDEF,,,Saturation level
+readnoise,s,h,,,,Read out noise sigma (photons)
+gain,s,h,,,,Photon gain (photons/data number)
+lsigma,r,h,)sparams.lsigma,,,>sparams.lsigma
+usigma,r,h,)sparams.usigma,,,>sparams.usigma
+polysep,r,h,0.95,0.1,0.95,Marsh algorithm polynomial spacing
+polyorder,i,h,10,1,,Marsh algorithm polynomial order
+nsubaps,i,h,1,1,,"Number of subapertures per aperture
+
+# ANSWER PARAMETERS
+"
+ansclobber,s,h,"NO",,," "
+ansclobber1,s,h,"NO",,," "
+ansdbwrite,s,h,"YES",,," "
+ansdbwrite1,s,h,"NO",,," "
+ansedit,s,h,"NO",,," "
+ansextract,s,h,"NO",,," "
+ansfind,s,h,"NO",,," "
+ansfit,s,h,"NO",,," "
+ansfitscatter,s,h,"NO",,," "
+ansfitsmooth,s,h,"NO",,," "
+ansfitspec,s,h,"NO",,," "
+ansfitspec1,s,h,"NO",,," "
+ansfittrace,s,h,"NO",,," "
+ansfittrace1,s,h,"NO",,," "
+ansflat,s,h,"NO",,," "
+ansnorm,s,h,"NO",,," "
+ansrecenter,s,h,"NO",,," "
+ansresize,s,h,"NO",,," "
+ansreview,s,h,"NO",,," "
+ansreview1,s,h,"NO",,," "
+ansscat,s,h,"NO",,," "
+ansskyextract,s,h,"NO",,," "
+anssmooth,s,h,"NO",,," "
+anstrace,s,h,"NO",,," "
diff --git a/noao/imred/src/doecslit/doecslit.cl b/noao/imred/src/doecslit/doecslit.cl
new file mode 100644
index 00000000..a3675416
--- /dev/null
+++ b/noao/imred/src/doecslit/doecslit.cl
@@ -0,0 +1,106 @@
+# DOECSLIT -- Process Echelle slit spectra from 2D to wavelength calibrated
+# and flux calibrated 1D spectra.
+#
+# The task PROC does all of the interactive work and BATCH does the
+# background work.  This procedure is organized this way to minimize the
+# dictionary space when the background task is submitted.
+
+procedure doecslit (objects)
+
+string	objects = ""		{prompt="List of object spectra"}
+
+file	apref = ""		{prompt="Aperture reference spectrum"}
+string	arcs = ""		{prompt="List of arc spectra"}
+file	arctable = ""		{prompt="Arc assignment table (optional)"}
+string	standards = ""		{prompt="List of standard star spectra\n"}
+
+string	readnoise = "0."	{prompt="Read out noise sigma (photons)"}
+string	gain = "1."		{prompt="Photon gain (photons/data number)"}
+real	datamax = INDEF		{prompt="Max data value / cosmic ray threshold"}
+int	norders = 10		{prompt="Number of orders"}
+real	width = 5.		{prompt="Width of profiles (pixels)\n"}
+
+bool	dispcor = yes		{prompt="Dispersion correct spectra?"}
+bool	extcor = no		{prompt="Extinction correct spectra?"}
+bool	fluxcal = no		{prompt="Flux calibrate spectra?"}
+bool	resize = no		{prompt="Resize object apertures?"}
+bool	clean = no		{prompt="Detect and replace bad pixels?"}
+bool	trace = yes		{prompt="Trace object spectra?"}
+string	background = "none"	{prompt="Background to subtract",
+			 enum="none|scattered|average|median|minimum|fit"}
+bool	splot = no		{prompt="Plot the final spectra?"}
+bool	redo = no		{prompt="Redo operations if previously done?"}
+bool	update = no		{prompt="Update spectra if cal data changes?"}
+bool	quicklook = no		{prompt="Approximate quicklook reductions?"}
+bool	batch = no		{prompt="Extract objects in batch?"}
+bool	listonly = no		{prompt="List steps but don't process?\n"}
+
+pset	sparams = ""		{prompt="Algorithm parameters"}
+
+begin
+	bool	recenter, arcap, tr, scat
+
+	int	i, j
+	file	obj, arc, std
+
+	# Expand image lists
+	obj = mktemp ("tmp$iraf") 
+	arc = mktemp ("tmp$iraf")
+	std = mktemp ("tmp$iraf")
+	sgetspec (objects, arcs, arctable, standards, obj, arc, std)
+
+	# Remove any leading whitespace from parameters that might be null.
+	if (logfile != "") {
+	    j = strlen (logfile)
+	    for (i=1; i<=j && substr(logfile,i,i)==" "; i+=1);
+	    logfile = substr (logfile, i, j)
+	}
+	if (arctable != "") {
+	    j = strlen (arctable)
+	    for (i=1; i<=j && substr(arctable,i,i)==" "; i+=1);
+	    arctable = substr (arctable, i, j)
+	}
+
+	apslitproc.readnoise = readnoise
+	apslitproc.gain = gain
+	apslitproc.nfind = norders
+	apslitproc.width = width
+	apslitproc.lower = -width / 2.
+	apslitproc.upper = width / 2.
+	apslitproc.b_sample = \
+	    str(-2*width)//":"//str(-width)//","//str(width)//":"//str(2*width)
+	apslitproc.t_width = width
+	apslitproc.radius = width
+	apslitproc.minsep = width
+	apslitproc.clean = clean
+	if (background == "scattered") {
+	    scat = yes
+	    apslitproc.background = "none"
+	} else {
+	    scat = no
+	    apslitproc.background = background
+	}
+	sproc.datamax = datamax
+
+	recenter = yes
+	tr = trace
+	arcap = yes
+	if (quicklook) {
+	    tr = no
+	    scat = no
+	    arcap = no
+	}
+
+	sproc (obj, apref, arc, arctable, std, recenter,
+	    resize, quicklook, tr, scat, arcap, dispcor,
+	    extcor, fluxcal, splot, redo, update, batch, listonly)
+	delete (std, verify=no)
+
+	if (sproc.dobatch) {
+	    print ("-- Do remaining spectra as a batch job --")
+	    print ("sbatch&batch") | cl
+	} else {
+	    delete (obj, verify=no)
+	    delete (arc, verify=no)
+	}
+end
diff --git a/noao/imred/src/doecslit/doecslit.par b/noao/imred/src/doecslit/doecslit.par
new file mode 100644
index 00000000..1d68f729
--- /dev/null
+++ b/noao/imred/src/doecslit/doecslit.par
@@ -0,0 +1,28 @@
+objects,s,a,"",,,"List of object spectra"
+apref,f,h,"",,,"Aperture reference spectrum"
+arcs,s,h,"",,,"List of arc spectra"
+arctable,f,h,"",,,"Arc assignment table (optional)"
+standards,s,h,"",,,"List of standard star spectra
+"
+readnoise,s,h,"0.",,,"Read out noise sigma (photons)"
+gain,s,h,"1.",,,"Photon gain (photons/data number)"
+datamax,r,h,INDEF,,,"Max data value / cosmic ray threshold"
+norders,i,h,10,,,"Number of orders"
+width,r,h,5.,,,"Width of profiles (pixels)
+"
+dispcor,b,h,yes,,,"Dispersion correct spectra?"
+extcor,b,h,no,,,"Extinction correct spectra?"
+fluxcal,b,h,no,,,"Flux calibrate spectra?"
+resize,b,h,no,,,"Resize object apertures?"
+clean,b,h,no,,,"Detect and replace bad pixels?"
+trace,b,h,yes,,,"Trace object spectra?"
+background,s,h,"none",none|scattered|average|median|minimum|fit,,"Background to subtract"
+splot,b,h,no,,,"Plot the final spectra?"
+redo,b,h,no,,,"Redo operations if previously done?"
+update,b,h,no,,,"Update spectra if cal data changes?"
+quicklook,b,h,no,,,"Approximate quicklook reductions?"
+batch,b,h,no,,,"Extract objects in batch?"
+listonly,b,h,no,,,"List steps but don\'t process?
+"
+sparams,pset,h,"",,,"Algorithm parameters"
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/doecslit/sarcrefs.cl b/noao/imred/src/doecslit/sarcrefs.cl
new file mode 100644
index 00000000..907b446f
--- /dev/null
+++ b/noao/imred/src/doecslit/sarcrefs.cl
@@ -0,0 +1,77 @@
+# SARCREFS -- Determine dispersion relation for reference arc.
+
+procedure sarcrefs (arcref, done, log1, log2)
+
+file	arcref
+file	done
+file	log1
+file	log2
+
+struct	*fd
+
+begin
+	string	arcrefec, arcec, temp
+	int	i, dc
+	bool	log
+
+	temp = mktemp ("tmp$iraf")
+
+	# Extract the primary arc reference spectrum.  Determine the
+	# dispersion function with IDENTIFY/REIDENTIFY.  Set the wavelength
+	# parameters with ECDISPCOR.
+
+	arcrefec = arcref // ".ec." // envget ("imtype")
+	i = stridx (",", arcrefec)
+	if (i > 0)
+	    arcrefec = substr (arcrefec, 1, i-1)
+	if (!access (arcrefec)) {
+	    print ("Extract arc reference image ", arcref) | tee (log1)
+	    apslitproc (arcref, background="none", clean=no, weights="none")
+	}
+
+	# Get the dispersion parameters from the header.  These are
+	# used for all further spectra and also flag whether this
+	# spectrum has been processed.  If the parameters are missing
+	# the spectrum needs to have the dispersion function and
+	# wavelength scale determined.  The HEDIT is needed because
+	# in some cases the user may exit ECIDENTIFY without updating
+	# the database (if the image was deleted but the database
+	# entry was not).
+
+	hselect (arcrefec, "dc-flag", yes, > temp)
+	fd = temp
+	dc = -1
+	i = fscan (fd, dc)
+	fd = ""; delete (temp, verify=no)
+	if (i < 1) {
+	    print ("Determine dispersion solution for ", arcref) | tee (log1)
+	    #delete (database//"/ec"//arcref//".ec*", verify=no)
+	    ecidentify (arcrefec, database=database,
+		coordlist=sparams.coordlist, match=sparams.match,
+		maxfeatures=100, zwidth=10., ftype="emission",
+		fwidth=sparams.fwidth, cradius=sparams.cradius,
+		threshold=sparams.threshold, minsep=2.,
+		function=sparams.i_function, xorder=sparams.i_xorder,
+		yorder=sparams.i_yorder, niterate=sparams.i_niterate,
+		lowreject=sparams.i_low, highreject=sparams.i_high,
+		autowrite=yes)
+	    hedit (arcrefec, "refspec1", arcref // ".ec", add=yes,
+		show=no, verify=no, update=yes)
+	}
+
+	# Dispersion correct the reference arc.  This step is required to
+	# to set the wavelength scale for all further spectra.
+
+	if (i < 1) {
+	    dispcor (arcrefec, "", linearize=sparams.linearize,
+		database=database, table="", w1=INDEF, w2=INDEF, dw=INDEF,
+		nw=INDEF, log=sparams.log, flux=sparams.flux, samedisp=no,
+		global=no, ignoreaps=no, confirm=no, listonly=no, verbose=yes,
+		logfile=log1, > log2)
+	    hedit (arcrefec, "dc-flag", 0, add=yes, show=no,
+		verify=no, update=yes)
+	    sproc.newdisp = yes
+	}
+
+	print (arcref, >> done)
+end
diff --git a/noao/imred/src/doecslit/sarcrefs.par b/noao/imred/src/doecslit/sarcrefs.par
new file mode 100644
index 00000000..38b81646
--- /dev/null
+++ b/noao/imred/src/doecslit/sarcrefs.par
@@ -0,0 +1,6 @@
+arcref,f,a,"",,,
+done,f,a,"",,,
+log1,f,a,"",,,
+log2,f,a,"",,,
+fd,*struct,h,"",,,
+mode,s,h,"q",,,
diff --git a/noao/imred/src/doecslit/sbatch.cl b/noao/imred/src/doecslit/sbatch.cl
new file mode 100644
index 00000000..062ac3e5
--- /dev/null
+++ b/noao/imred/src/doecslit/sbatch.cl
@@ -0,0 +1,216 @@
+# SBATCH -- Process spectra in batch.
+# This task is called in batch mode.  It only processes objects
+# not previously processed unless the update or redo flags are set.
+
+procedure sbatch ()
+
+file	objects		{prompt="Object spectra"}
+real	datamax 	{prompt="Max data value / cosmic ray threshold"}
+
+file	arcs		{prompt="List of arc spectra"}
+file	arcref		{prompt="Arc reference for dispersion solution"}
+string	arcrefs		{prompt="Arc references\n"}
+
+file	done		{prompt="File of spectra already done"}
+file	logfile		{prompt="Logfile"}
+bool	redo		{prompt="Redo operations?"}
+bool	update		{prompt="Update spectra?\n"}
+
+bool	scattered	{prompt="Subtract scattered light?"}
+bool	arcap		{prompt="Use object apertures for arcs?"}
+bool	dispcor		{prompt="Dispersion correct spectra?"}
+bool	extcor		{prompt="Extinction correct spectra?"}
+bool	fluxcal1	{prompt="Flux calibrate spectra?"}
+
+bool	newaps, newdisp, newsens, newarcs
+
+struct	*fd1, *fd2, *fd3
+
+begin
+	file	temp, spec, specec, arc
+	bool	reextract, extract, scat, disp, ext, flux, log, disperr
+	string	imtype, ectype, str1, str2, str3, str4
+	int	i
+	str1 = ""
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	ectype = ".ec" // imtype
+
+	temp = mktemp ("tmp$iraf")
+
+	reextract = redo || (update && (newaps || newdisp))
+
+	fd1 = objects
+	while (fscan (fd1, spec) != EOF) {
+	    if (access (done)) {
+	        fd2 = done
+	        while (fscan (fd2, specec) != EOF)
+		    if (spec == specec)
+		        break
+	        if (spec == specec)
+		    next
+	        fd2 = ""
+	    }
+	    if (!access (spec // imtype)) {
+		print ("Object spectrum not found - " // spec // imtype,
+		    >> logfile)
+		print ("Check setting of imtype", >> logfile)
+		next
+	    }
+	    specec = spec // ectype
+
+	    scat = no
+	    extract = no
+	    disp = no
+	    ext = no
+	    flux = no
+	    if (scattered) {
+		hselect (spec, "apscatte", yes, > temp)
+		fd2 = temp
+		if (fscan (fd2, str1) < 1)
+		    scat = yes
+		fd2 = ""; delete (temp, verify=no)
+	    }
+	    if (reextract || !access (specec) || (update && scat))
+		extract = yes
+	    else {
+		hselect (specec, "dc-flag", yes, > temp)
+		hselect (specec, "ex-flag", yes, >> temp)
+		hselect (specec, "ca-flag", yes, >> temp)
+		fd2 = temp
+		if (fscan (fd2, str1) == 1) {
+		    extract = update && newdisp
+		    if (update && !newdisp)
+		        # We really should check if REFSPEC will assign
+			# different reference spectra.
+			;
+		} else
+		    disp = dispcor
+		if (fscan (fd2, str1) == 1)
+		    extract = update && !extcor
+		else
+		    ext = extcor
+		if (fscan (fd2, str1) == 1)
+		    extract = update && (!fluxcal1 || newsens)
+		else
+		    flux = fluxcal1
+		fd2 = ""; delete (temp, verify=no)
+	    }
+
+	    if (extract) {
+		disp = dispcor
+		ext = extcor
+		flux = fluxcal1
+	    }
+		
+	    if (extract) {
+		if (access (specec))
+		    imdelete (specec, verify=no)
+
+		if (scat) {
+		    print ("Subtract scattered light in ", spec, >> logfile)
+		    apslitproc (spec, ansextract="NO", ansscat="YES")
+		}
+
+		print ("Extract object spectrum ", spec, >> logfile)
+		hselect (spec, "date-obs,ut,exptime", yes, > temp)
+		hselect (spec, "ra,dec,epoch,st", yes, >> temp)
+		fd3 = temp
+		if (fscan (fd3, str1, str2, str3) == 3) {
+		    setjd (spec, observatory=observatory, date="date-obs",
+			time="ut", exposure="exptime", jd="jd", hjd="",
+			ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+			>> logfile)
+		    if (fscan (fd3, str1, str2, str3, str4) == 4)
+			setairmass (spec, intype="beginning",
+			    outtype="effective", exposure="exptime",
+			    observatory=observatory, show=no, update=yes,
+			    override=yes, >> logfile)
+		}
+		fd3 = ""; delete (temp, verify=no)
+		apslitproc (spec, saturation=datamax, verbose=no)
+	    }
+
+	    disperr = no
+	    if (disp) {
+		# Fix arc headers if necessary.
+		if (newarcs) {
+	    	    fd2 = arcs
+	    	    while (fscan (fd2, arc) != EOF) {
+			hselect (arc, "date-obs,ut,exptime", yes, > temp)
+			hselect (arc, "ra,dec,epoch,st", yes, >> temp)
+			fd3 = temp
+			if (fscan (fd3, str1, str2, str3) == 3) {
+			    setjd (arc, observatory=observatory,
+				date="date-obs", time="ut", exposure="exptime",
+				jd="jd", hjd="", ljd="ljd", utdate=yes,
+				uttime=yes, listonly=no, >> logfile)
+			    if (fscan (fd3, str1, str2, str3, str4) == 4)
+				setairmass (arc, intype="beginning",
+				    outtype="effective", exposure="exptime",
+				    observatory=observatory, show=no,
+				    update=yes, override=yes, >> logfile)
+			}
+			fd3 = ""; delete (temp, verify=no)
+	        	hedit (arc, "refspec1", arc, add=yes, verify=no,
+		    	    show=no, update=yes)
+		    }
+	    	    fd2 = ""
+		    newarcs = no
+		}
+
+		print ("Assign arc spectra for ", spec, >> logfile)
+		refspectra (spec, references=arcrefs,
+		    apertures="", refaps="", ignoreaps=no,
+		    select=sparams.select, sort=sparams.sort,
+		    group=sparams.group, time=sparams.time,
+		    timewrap=sparams.timewrap, override=yes, confirm=no,
+		    assign=yes, logfiles="STDOUT", verbose=no,
+		    >> logfile)
+
+		sdoarcs (spec, arcref, reextract, arcap, logfile, yes)
+
+	        hselect (specec, "refspec1", yes, > temp)
+	        fd2 = temp
+	        i = fscan (fd2, arc)
+	        fd2 = ""; delete (temp, verify=no)
+		if (i < 1) {
+		    print ("No arc reference assigned for ", spec, >> logfile)
+		    disperr = yes
+		} else {
+	            print ("Dispersion correct ", spec, >> logfile)
+		    dispcor (specec, "", linearize=sparams.linearize,
+			database=database, table=arcref//ectype,
+			w1=INDEF, w2=INDEF, dw=INDEF, nw=INDEF,
+			log=sparams.log, flux=sparams.flux, samedisp=no,
+			global=no, ignoreaps=no, confirm=no, listonly=no,
+			logfile=logfile, > "dev$null")
+		    hedit (specec, "dc-flag", 0, add=yes, show=no,
+			verify=no, update=yes)
+		}
+	    }
+
+	    if (!disperr && (extract || disp)) {
+	        if (ext)
+		    print ("Extinction correct ", spec, >> logfile)
+	        if (flux)
+		    print ("Flux calibrate ", spec, >> logfile)
+	        if (flux || ext)
+		    calibrate (specec, "", extinct=extcor, flux=fluxcal1,
+			extinction=extinction, observatory=observatory,
+			ignoreaps=no, sensitivity="sens", fnu=sparams.fnu,
+			>> logfile)
+	    }
+	}
+	fd1 = ""
+	delete (objects, verify=no)
+	delete (arcs, verify=no)
+
+	if (access (done))
+	    delete (done, verify=no)
+
+	flprcache (0)
+end
diff --git a/noao/imred/src/doecslit/sbatch.par b/noao/imred/src/doecslit/sbatch.par
new file mode 100644
index 00000000..9bb5239d
--- /dev/null
+++ b/noao/imred/src/doecslit/sbatch.par
@@ -0,0 +1,24 @@
+objects,f,h,"",,,"Object spectra"
+datamax,r,h,,,,"Max data value / cosmic ray threshold"
+arcs,f,h,"",,,"List of arc spectra"
+arcref,f,h,"",,,"Arc reference for dispersion solution"
+arcrefs,s,h,,,,"Arc references
+"
+done,f,h,"",,,"File of spectra already done"
+logfile,f,h,"",,,"Logfile"
+redo,b,h,,,,"Redo operations?"
+update,b,h,,,,"Update spectra?
+"
+scattered,b,h,,,,"Subtract scattered light?"
+arcap,b,h,,,,"Use object apertures for arcs?"
+dispcor,b,h,,,,"Dispersion correct spectra?"
+extcor,b,h,,,,"Extinction correct spectra?"
+fluxcal1,b,h,,,,"Flux calibrate spectra?"
+newaps,b,h,,,,
+newdisp,b,h,,,,
+newsens,b,h,,,,
+newarcs,b,h,,,,
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+fd3,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/doecslit/sdoarcs.cl b/noao/imred/src/doecslit/sdoarcs.cl
new file mode 100644
index 00000000..76ccaab8
--- /dev/null
+++ b/noao/imred/src/doecslit/sdoarcs.cl
@@ -0,0 +1,102 @@
+# SDOARCS -- Determine dispersion relation for spectrum based on reference arcs.
+
+procedure sdoarcs (spec, arcref, reextract, arcap, logfile, batch)
+
+file	spec
+file	arcref
+bool	reextract
+bool	arcap
+file	logfile
+bool	batch
+
+struct	*fd
+
+begin
+	string	imtype, ectype
+	int	i, j, k, n
+	file	temp, arc1, arc2, str1, str2, arctype, apref, arc, arcec, logs
+	file	specec, specarc
+	bool	verbose1
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	ectype = ".ec" // imtype
+	n = strlen (imtype)
+
+	temp = mktemp ("tmp$iraf")
+
+	if (batch)
+	    verbose1 = no
+	else
+	    verbose1 = verbose
+	if (verbose1)
+	    logs = logfile//",STDOUT"
+	else
+	    logs = logfile
+
+	for (j=1; j<=2; j+=1) {
+	    # The reference spectra refer initially to the 2D image.  At the
+	    # end we will reset them to refer to the 1D spectra.
+
+	    hselect (spec, "refspec"//j, yes, > temp)
+	    fd = temp
+	    k = fscan (fd, arc1, str1)
+	    fd = ""; delete (temp, verify=no)
+	    if (k < 1)
+		break
+
+	    # Strip possible image extension.
+	    i = strlen (arc1)
+	    if (i > n && substr (arc1, i-n+1, i) == imtype)
+		arc1 = substr (arc1, 1, i-n)
+
+	    # Set extraction output and aperture reference depending on whether
+	    # the arcs are to be rextracted using recentered or retraced object
+	    # apertures.
+
+	    if (arcap) {
+		arc2 = spec // arc1
+		apref = spec
+		if (access (arc2//ectype))
+		    imdelete (arc2//ectype, verify=no)
+		delete (database//"/ec"//arc2//".ec*", verify = no)
+	    } else {
+		arc2 = arc1
+		apref = apslitproc.references
+		if (reextract && access (arc2//ectype)) {
+		    if (arc2 != arcref)
+			imdelete (arc2//ectype, verify=no)
+		}
+	    }
+
+	    # Extract and determine dispersion function if necessary.
+	    if (!access (arc2//ectype)) {
+		delete (database//"/ec"//arc2//".ec*", verify = no)
+		if (!batch)
+		    print ("Extract and reidentify arc spectrum ", arc1)
+		print ("Extract and reidentify arc spectrum ", arc1, >> logfile)
+		apslitproc (arc1, output=arc2//".ec", references=apref,
+		    background="none", clean=no, weights="none",
+		    verbose=verbose1)
+		ecreidentify (arc2//".ec", arcref//".ec", shift=0.,
+		    cradius=sparams.cradius, threshold=sparams.threshold,
+		    refit=sparams.refit, database=database, logfiles=logs)
+
+		# If not reextracting arcs based on object apertures
+		# then save the extracted arc to avoid doing it again.
+
+		if (arc1 != arc2)
+		    imdelete (arc2//".ec", verify=no)
+	    }
+    
+	    # Set the REFSPEC parameters for echelle spectrum.
+	    if (k == 1)
+		hedit (spec//".ec", "refspec"//j, arc2//".ec", add=yes,
+		    verify=no, show=no, update=yes)
+	    else
+		hedit (spec//".ec", "refspec"//j, arc2//".ec "//str1, add=yes,
+		    verify=no, show=no, update=yes)
+	}
+end
diff --git a/noao/imred/src/doecslit/sdoarcs.par b/noao/imred/src/doecslit/sdoarcs.par
new file mode 100644
index 00000000..648bacaf
--- /dev/null
+++ b/noao/imred/src/doecslit/sdoarcs.par
@@ -0,0 +1,8 @@
+spec,f,a,"",,,
+arcref,f,a,"",,,
+reextract,b,a,,,,
+arcap,b,a,,,,
+logfile,f,a,"",,,
+batch,b,a,,,,
+fd,*struct,h,"",,,
+mode,s,h,"q",,,
diff --git a/noao/imred/src/doecslit/sfluxcal.cl b/noao/imred/src/doecslit/sfluxcal.cl
new file mode 100644
index 00000000..b8b7fd80
--- /dev/null
+++ b/noao/imred/src/doecslit/sfluxcal.cl
@@ -0,0 +1,214 @@
+# SFLUXCAL -- Extract standard stars and determine sensitivity function.
+# If flux calibrating, extract and dispersion correct the standard star
+# spectra.  Compile the standard star fluxes from the calibration
+# directory.  The user is queried for the star name but the band passes
+# are not allow to change interactively.  Next compute the sensitivity
+# function using SENSFUNC.  This is interactive.  Once the sensitivity
+# function images are created, flux and extinction calibrate the standard
+# stars.  This is done in such a way that if new standard stars are added
+# in a later execution only the new stars are added and then a new
+# sensitivity function is computed.  If the update flag is set all
+# spectra which are specified are reprocessed if they were previously
+# processed.  In a redo the "std" file is deleted, otherwise additions
+# are appended to this file.
+
+procedure sfluxcal (stds, arcs, arcref, arcrefs, redo, update,
+	scattered, arcap, extcor, done, log1, log2)
+
+file	stds
+file	arcs
+file	arcref
+string	arcrefs
+bool	redo
+bool	update
+bool	scattered
+bool	arcap
+bool	extcor
+file	done
+file	log1
+file	log2
+
+struct	*fd1, *fd2, *fd3
+
+begin
+	string	imtype, ectype
+	string	spec, specec, arc, str1, str2, str3, str4
+	file	temp1, temp2
+	int	i, j
+	bool	reextract, log, scat
+	str1 = ""
+	str2 = ""
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	ectype = ".ec" // imtype
+
+	temp1 = mktemp ("tmp$iraf")
+	temp2 = mktemp ("tmp$iraf")
+
+	reextract = redo || (update && (sproc.newaps || sproc.newdisp))
+	sproc.newsens = no
+
+	if (redo && access ("std"))
+	    delete ("std", verify=no)
+
+        fd1 = stds
+        while (fscan (fd1, spec) != EOF) {
+	    specec = spec // ectype
+
+	    scat = no
+	    if (scattered) {
+		hselect (spec, "apscatte", yes, > temp1)
+		fd2 = temp1
+		if (fscan (fd2, str1) < 1)
+		    scat = yes
+		fd2 = ""; delete (temp1, verify=no)
+	    }
+	    if (reextract || !access (specec) || (update && scat)) {
+		if (access (specec))
+		    imdelete (specec, verify=no)
+
+		if (scat) {
+		    print ("Subtract scattered light in ", spec) | tee (log1)
+		    apslitproc (spec, ansextract="NO", ansscat="YES")
+		}
+
+	        print ("Extract standard star spectrum ", spec) | tee (log1)
+		hselect (spec, "date-obs,ut,exptime", yes, > temp1)
+		hselect (spec, "ra,dec,epoch,st", yes, >> temp1)
+		fd2 = temp1
+		if (fscan (fd2, str1, str2, str3) == 3) {
+		    setjd (spec, observatory=observatory, date="date-obs",
+			time="ut", exposure="exptime", jd="jd", hjd="",
+			ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+			>> log1)
+		    if (fscan (fd2, str1, str2, str3, str4) == 4)
+			setairmass (spec, intype="beginning",
+			    outtype="effective", exposure="exptime",
+			    observatory=observatory, show=no, update=yes,
+			    override=yes, >> log1)
+		}
+		fd2 = ""; delete (temp1, verify=no)
+		apslitproc (spec)
+	    }
+
+	    hselect (specec, "dc-flag,std-flag", yes, > temp1)
+	    fd2 = temp1
+	    j = fscan (fd2, str1, str2)
+	    fd2 = ""; delete (temp1, verify=no)
+	    if (j < 1) {
+		# Fix arc headers if necessary.
+		if (sproc.newarcs) {
+	    	    fd2 = arcs
+	    	    while (fscan (fd2, arc) != EOF) {
+			hselect (arc, "date-obs,ut,exptime", yes, > temp1)
+			hselect (arc, "ra,dec,epoch,st", yes, >> temp1)
+			fd3 = temp1
+			if (fscan (fd3, str1, str2, str3) == 3) {
+			    setjd (arc, observatory=observatory,
+				date="date-obs", time="ut", exposure="exptime",
+				jd="jd", hjd="", ljd="ljd", utdate=yes,
+				uttime=yes, listonly=no, >> log1)
+			    if (fscan (fd3, str1, str2, str3, str4) == 4)
+				setairmass (arc, intype="beginning",
+				    outtype="effective", exposure="exptime",
+				    observatory=observatory, show=no,
+				    update=yes, override=yes, >> log1)
+			}
+			fd3 = ""; delete (temp1, verify=no)
+	        	hedit (arc, "refspec1", arc, add=yes, verify=no,
+		    	    show=no, update=yes)
+		    }
+	    	    fd2 = ""
+		    sproc.newarcs = no
+		}
+
+		print ("Assign arc spectra for ", spec) | tee (log1)
+		refspectra (spec, references=arcrefs,
+		    apertures="", refaps="", ignoreaps=no,
+		    select=sparams.select, sort=sparams.sort,
+		    group=sparams.group, time=sparams.time,
+		    timewrap=sparams.timewrap, override=yes, confirm=no,
+		    assign=yes, logfiles="STDOUT", verbose=no) |
+		    tee (log1, > log2)
+
+		sdoarcs (spec, arcref, reextract, arcap, log1, no)
+
+	        hselect (specec, "refspec1", yes, > temp1)
+	        fd2 = temp1
+	        i = fscan (fd2, arc)
+	        fd2 = ""; delete (temp1, verify=no)
+		if (i < 1) {
+		    print ("No arc reference assigned for ", spec) | tee (log1)
+		    next
+		} else {
+	            print ("Dispersion correct ", spec) | tee (log1)
+		    dispcor (specec, "", linearize=sparams.linearize,
+			database=database, table=arcref//ectype,
+			w1=INDEF, w2=INDEF, dw=INDEF, nw=INDEF, log=sparams.log,
+			flux=sparams.flux, global=no, ignoreaps=no, confirm=no,
+			listonly=no, logfile=logfile)
+		    hedit (specec, "dc-flag", 0, add=yes, show=no,
+			verify=no, update=yes)
+		}
+	    }
+
+	    if (j < 2 || !access ("std")) {
+                print ("Compile standard star fluxes for ", spec) | tee (log1)
+	        standard (specec, output="std", samestar=yes, beam_switch=no,
+		    apertures="", bandwidth=sparams.bandwidth,
+		    bandsep=sparams.bandsep, fnuzero=3.68E-20,
+		    extinction=extinction, caldir=caldir,
+		    observatory=observatory, interact=sparams.s_interact)
+	        hedit (specec, "std-flag", "yes", add=yes, verify=no,
+		    show=no, update=yes)
+	        print (specec, >> temp2)
+	        sproc.newsens = yes
+            }
+        }
+        fd1 = ""
+
+        sections ("sens.????"//imtype, option="nolist")
+        if (sproc.newsens || sections.nimages == 0) {
+	    if (!access ("std")) {
+	        print ("No standard star data") | tee (log1)
+	        sproc.fluxcal1 = no
+	    } else {
+	        imdelete ("sens.????"//imtype, verify=no)
+                print ("Compute sensitivity function") | tee (log1)
+                sensfunc ("std", "sens", apertures="", ignoreaps=no,
+		    logfile=logfile, extinction=extinction,
+		    newextinction="extinct.dat", observatory=observatory,
+		    function=sparams.s_function, order=sparams.s_order,
+		    interactive=yes, graphs="sr", marks="plus cross box")
+	        sproc.newsens = yes
+	    }
+        }
+
+        # Note that if new standard stars are added the old standard
+        # stars are not recalibrated unless the redo flag is used.
+
+        if (sproc.fluxcal1 && sproc.newsens) {
+            print ("Flux and/or extinction calibrate standard stars") |
+	        tee (log1)
+	    calibrate ("@"//temp2, "", extinct=extcor, flux=sproc.fluxcal1,
+		extinction=extinction, observatory=observatory, ignoreaps=no,
+		sensitivity="sens", fnu=sparams.fnu) | tee (log1, > log2)
+	    if (sproc.splot1) {
+	        print ("Standard stars:")
+	        str1 = sproc.anssplot
+	        if (str1 == "NO" || str1 == "YES")
+		    sproc.splot1 = no
+	        if (str1 == "no" || str1 == "NO")
+		    sproc.splot2 = no
+	        else
+		    sproc.splot2 = yes
+	    }
+	    if (sproc.splot2)
+		splot ("@"//temp2)
+	    sections (temp2, option="fullname", >> done)
+            delete (temp2, verify=no)
+        }
+end
diff --git a/noao/imred/src/doecslit/sfluxcal.par b/noao/imred/src/doecslit/sfluxcal.par
new file mode 100644
index 00000000..b750d265
--- /dev/null
+++ b/noao/imred/src/doecslit/sfluxcal.par
@@ -0,0 +1,16 @@
+stds,s,a,,,,
+arcs,s,a,,,,
+arcref,f,a,"",,,
+arcrefs,s,a,,,,
+redo,b,a,,,,
+update,b,a,,,,
+scattered,b,a,,,,
+arcap,b,a,,,,
+extcor,b,a,,,,
+done,f,a,"",,,
+log1,f,a,"",,,
+log2,f,a,"",,,
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+fd3,*struct,h,"",,,
+mode,s,h,"q",,,
diff --git a/noao/imred/src/doecslit/sgetspec.cl b/noao/imred/src/doecslit/sgetspec.cl
new file mode 100644
index 00000000..7038dcb2
--- /dev/null
+++ b/noao/imred/src/doecslit/sgetspec.cl
@@ -0,0 +1,177 @@
+# SGETSPEC -- Get spectra which are CCD processed and not extracted.
+# This task also recognizes the arc spectra in the object list and arc table.
+# This task also strips the image type extension.
+
+procedure sgetspec (objects, arcs, arctable, standards, obj, arc, std)
+
+string	objects			{prompt="List of object images"}
+string	arcs			{prompt="List of arc images"}
+file	arctable		{prompt="Arc table"}
+string	standards		{prompt="List of standard images"}
+file	obj			{prompt="File of object images"}
+file	arc			{prompt="File of arc images"}
+file	std			{prompt="File of standard images"}
+bool	ccdproc			{prompt="Add CCDPROC keyword and continue?",
+				 mode="q"}
+struct	*fd1, *fd2
+
+begin
+	string	imtype, temp, image, itype
+	int	n, n1, narcs
+
+	imtype = "." // envget ("imtype")
+	n = stridx (",", imtype)
+	if (n > 0)
+	    imtype = substr (imtype, 1, n-1)
+	n1 = strlen (imtype)
+
+	temp = mktemp ("tmp$iraf")
+
+	# Initialize files
+	set clobber=yes
+	sleep (> obj)
+	sleep (> arc)
+	sleep (> std)
+	set clobber=no
+
+	# Do arcs
+	narcs = 0
+	sections (arcs, option="fullname", > temp)
+	fd1 = temp
+	while (fscan (fd1, image) != EOF) {
+	    hselect (image, "ccdproc", yes) | scan (itype)
+	    if (nscan() == 0) {
+		printf ("%s: CCDPROC keyword not found.\n", image)
+		printf ("  Either run CCDPROC or add CCDPROC keyword with HEDIT.\n")
+		if (!ccdproc)
+		    error (1, "Exit")
+		hedit (image, "ccdproc", "DOSLIT", add=yes, update=yes,
+		    verify=no, show=no)
+	    }
+	    hselect (image, "wat0_001", yes) | scanf ("system=%s", itype)
+	    if (itype == "equispec" || itype == "multispec")
+		next
+	    hselect (image, "imagetyp", yes) | scan (itype)
+	    if (nscan() == 0)
+		itype = "comp"
+	    if (itype != "comp" && itype != "COMPARISON" &&
+		itype != "comparison" && itype != "COMP")
+		next
+	    n = strlen (image)
+	    if (n > n1 && substr (image, n-n1+1, n) == imtype)
+		image = substr (image, 1, n-n1)
+	    narcs = narcs + 1
+	    printf ("%s %02d\n", image, narcs, >> arc)
+	}
+	fd1 = ""; delete (temp, verify=no)
+
+	# Do arc table.
+	if (arctable != "") {
+	    fd2 = arctable
+	    while (fscan (fd2, image, image) != EOF) {
+		if (nscan() != 2)
+		    next
+		sections (image, option="fullname", > temp)
+		fd1 = temp
+		while (fscan (fd1, image) != EOF) {
+		    hselect (image, "ccdproc", yes) | scan (itype)
+		    if (nscan() == 0) {
+			printf ("%s: CCDPROC keyword not found.\n", image)
+			printf ("  Either run CCDPROC or add CCDPROC keyword with HEDIT.\n")
+			if (!ccdproc)
+			    error (1, "Exit")
+			hedit (image, "ccdproc", "DOSLIT", add=yes, update=yes,
+			    verify=no, show=no)
+		    }
+		    hselect (image, "wat0_001", yes) | scanf ("system=%s", itype)
+		    if (itype == "equispec" || itype == "multispec")
+			next
+		    hselect (image, "imagetyp", yes) | scan (itype)
+		    if (nscan() == 0)
+			itype = "comp"
+		    if (itype != "comp" && itype != "COMPARISON" &&
+			itype != "comparison" && itype != "COMP")
+			next
+		    n = strlen (image)
+		    if (n > n1 && substr (image, n-n1+1, n) == imtype)
+			image = substr (image, 1, n-n1)
+		    narcs = narcs + 1
+		    printf ("%s %02d\n", image, narcs, >> arc)
+		}
+		fd1 = ""; delete (temp, verify=no)
+	    }
+	}
+
+	# Do standards
+	sections (standards, option="fullname", > temp)
+	fd1 = temp
+	while (fscan (fd1, image) != EOF) {
+	    hselect (image, "ccdproc", yes) | scan (itype)
+	    if (nscan() == 0) {
+		printf ("%s: CCDPROC keyword not found.\n", image)
+		printf ("  Either run CCDPROC or add CCDPROC keyword with HEDIT.\n")
+		if (!ccdproc)
+		    error (1, "Exit")
+		hedit (image, "ccdproc", "DOSLIT", add=yes, update=yes,
+		    verify=no, show=no)
+	    }
+	    hselect (image, "wat0_001", yes) | scanf ("system=%s", itype)
+	    if (itype == "equispec" || itype == "multispec")
+		next
+	    n = strlen (image)
+	    if (n > n1 && substr (image, n-n1+1, n) == imtype)
+		image = substr (image, 1, n-n1)
+	    print (image, >> std)
+	}
+	fd1 = ""; delete (temp, verify=no)
+
+	# Do objects
+	sections (objects, option="fullname", > temp)
+	fd1 = temp
+	while (fscan (fd1, image) != EOF) {
+	    hselect (image, "ccdproc", yes) | scan (itype)
+	    if (nscan() == 0) {
+		printf ("%s: CCDPROC keyword not found.\n", image)
+		printf ("  Either run CCDPROC or add CCDPROC keyword with HEDIT.\n")
+		if (!ccdproc)
+		    error (1, "Exit")
+		hedit (image, "ccdproc", "DOSLIT", add=yes, update=yes,
+		    verify=no, show=no)
+	    }
+	    hselect (image, "wat0_001", yes) | scanf ("system=%s", itype)
+	    if (itype == "equispec" || itype == "multispec")
+		next
+	    hselect (image, "imagetyp", yes) | scan (itype)
+	    if (nscan() == 0)
+		itype = "object"
+
+	    n = strlen (image)
+	    if (n > n1 && substr (image, n-n1+1, n) == imtype)
+		image = substr (image, 1, n-n1)
+	    if (itype == "object" || itype == "OBJECT")
+		print (image, >> obj)
+	    else if (itype == "comp" || itype == "COMPARISON" ||
+		itype == "comparison" || itype == "COMP") {
+		narcs = narcs + 1
+		printf ("%s %02d\n", image, narcs, >> arc)
+	    }
+	}
+	fd1 = ""; delete (temp, verify=no)
+
+	if (narcs > 0) {
+	    sort (arc, column=0, ignore=yes, numeric=no, reverse=no, > temp)
+	    delete (arc, verify=no)
+	    rename (temp, arc, field="all")
+	    itype = ""
+	    fd1 = arc
+	    while (fscan (fd1, image, narcs) != EOF) {
+		if (image != itype)
+		    printf ("%s %02d\n", image, narcs, >> temp)
+		itype = image
+	    }
+	    delete (arc, verify=no)
+	    sort (temp, column=2, ignore=yes, numeric=yes, reverse=no) |
+	    fields ("STDIN", "1", lines="1-99", > arc)
+	    delete (temp, verify=no)
+	}
+end
diff --git a/noao/imred/src/doecslit/sgetspec.par b/noao/imred/src/doecslit/sgetspec.par
new file mode 100644
index 00000000..1f5387cc
--- /dev/null
+++ b/noao/imred/src/doecslit/sgetspec.par
@@ -0,0 +1,11 @@
+objects,s,a,,,,"List of object images"
+arcs,s,a,,,,"List of arc images"
+arctable,f,a,"",,,"Arc table"
+standards,s,a,,,,"List of standard images"
+obj,f,a,"",,,"File of object images"
+arc,f,a,"",,,"File of arc images"
+std,f,a,"",,,"File of standard images"
+ccdproc,b,q,,,,"Add CCDPROC keyword and continue?"
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/doecslit/slistonly.cl b/noao/imred/src/doecslit/slistonly.cl
new file mode 100644
index 00000000..f765af36
--- /dev/null
+++ b/noao/imred/src/doecslit/slistonly.cl
@@ -0,0 +1,241 @@
+# SLISTONLY -- List processing to be done.
+#
+# This follows pretty much the same logic as the full procedure but doesn't
+# do anything but list the operations.
+
+procedure slistonly (objects, apref, arcs, standards, scattered, dispcor,
+	extcor, fluxcal, redo, update)
+
+string	objects
+file	apref
+string	arcs
+string	standards
+
+bool	scattered
+bool	dispcor
+bool	extcor
+bool	fluxcal
+bool	redo
+bool	update
+
+struct	*fd1
+struct	*fd2
+
+begin
+	string	imtype, ectype
+	string	spec, arcref
+	string	specec, arcrefec
+	string	temp1, temp2, done, str
+	bool	newaps, newdisp, newsens
+	bool	extract, disp, ext, flux, scat, reextract, fluxcal1, stdfile
+	int	i, j, n
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	ectype = ".ec" // imtype
+	n = strlen (imtype)
+
+	temp1 = mktemp ("tmp$iraf")
+	temp2 = mktemp ("tmp$iraf")
+	done = mktemp ("tmp$iraf")
+
+	newaps = no
+	newdisp = no
+	newsens = no
+	fluxcal1 = fluxcal
+
+	i = strlen (apref)
+	if (i > n && substr (apref, i-n+1, i) == imtype)
+	    apref = substr (apref, 1, i-n)
+
+	reextract = redo
+	if (reextract || !access (database // "/ap" // apref)) {
+	    print ("Set reference aperture for ", apref)
+	    newaps = yes
+	}
+
+	scat = no
+	if (scattered) {
+	    hselect (apref, "apscatte", yes, > temp1)
+	    fd1 = temp1
+	    if (fscan (fd1, str1) < 1)
+		scat = yes
+	    fd1 = ""; delete (temp1, verify=no)
+	}
+	if (scat)
+	    print ("Subtract scattered light in ", apref) | tee (log1)
+
+	if (dispcor) {
+	    hselect (arcs, "$I,wat0_001", yes, > temp1)
+	    fd1 = temp1; s1 = ""
+	    i = fscanf (fd1, "%s\tsystem=%s", arcref, s1)
+	    if (i < 1 || (i == 2 && (s1 == "equispec" || s1 == "multispec")))
+		error (1, "No reference arcs")
+	    fd1 = ""; delete (temp1, verify=no)
+	    i = strlen (arcref)
+	    if (i > n && substr (arcref, i-n+1, i) == imtype)
+	        arcref = substr (arcref, 1, i-n)
+	    arcrefec = arcref // ectype
+
+	    reextract = redo || (update && newaps)
+	    if (reextract || !access (arcrefec)) {
+	        print ("Extract arc reference image ", arcref)
+	        print ("Determine dispersion solution for ", arcref)
+	        newdisp = yes
+	    } else {
+		hselect (arcrefec, "refspec1,dc-flag", yes, > temp1)
+	        fd1 = temp1
+	        i = fscan (fd1, str, j)
+	        fd1 = ""; delete (temp1, verify=no)
+	        if (i < 1) {
+	            print ("Determine dispersion solution for ", arcref)
+	            newdisp = yes
+	        }
+	    }
+	    print (arcref, > done)
+
+	    if (fluxcal1) {
+		stdfile = access ("std")
+		if (redo && stdfile)
+		    stdfile = no
+
+	        reextract = redo || (update && (newaps || newdisp))
+		hselect (standards, "$I,ctype1", yes, >temp1)
+	        fd1 = temp1
+	        while (fscan (fd1, spec, s1) != EOF) {
+		    if (nscan() == 2 && s1 == "MULTISPE")
+			next
+		    i = strlen (spec)
+		    if (i > n && substr (spec, i-n+1, i) == imtype)
+		        spec = substr (spec, 1, i-n)
+		    specec = spec // ectype
+
+		    scat = no
+		    if (scattered) {
+			hselect (spec, "apscatte", yes, > temp2)
+			fd2 = temp2
+			if (fscan (fd2, str) < 1)
+			    scat = yes
+			fd2 = ""; delete (temp2, verify=no)
+		    }
+	            if (reextract || !access (specec) || (update && scat)) {
+			if (scat)
+			    print ("Subtract scattered light from ", spec)
+		        print ("Extract standard star spectrum ", spec)
+	                print ("Dispersion correct ", spec)
+	                print ("Compile standard star fluxes for ", spec)
+		        stdfile = yes
+		        newsens = yes
+		    } else {
+		        hselect (specec, "dc-flag,std-flag", yes, > temp2)
+		        fd2 = temp2
+		        i = fscan (fd2, str1, str2)
+		        fd2 = ""; delete (temp2, verify=no)
+		        if (i < 1)
+		            print ("Dispersion correct ", spec)
+		        if (i < 2) {
+		            print ("Compile standard star fluxes for ", spec)
+		            stdfile = yes
+		            newsens = yes
+		        }
+	            }
+		    print (spec, >> done)
+	        }
+	        fd1 = ""; delete (temp1, verify=no)
+
+	        sections ("sens.????"//imtype, option="nolist")
+	        if (newsens || sections.nimages == 0) {
+		    if (!stdfile) {
+		        print ("No standard stars")
+		        fluxcal1 = no
+		    } else {
+	                print ("Compute sensitivity function")
+		        newsens = yes
+		    }
+	        }
+
+	        if (fluxcal1 && newsens)
+	            print ("Flux and/or extinction calibrate standard stars")
+	    }
+	}
+
+	reextract = redo || (update && (newaps || newdisp))
+	hselect (objects, "$I,ctype1", yes, > temp1)
+	fd1 = temp1
+	while (fscan (fd1, spec, s1) != EOF) {
+	    if (nscan() == 2 && s1 == "MULTISPE")
+		next
+	    if (i > n && substr (spec, i-n+1, i) == imtype)
+	        spec = substr (spec, 1, i-n)
+
+	    if (access (done)) {
+	        fd2 = done
+	        while (fscan (fd2, specec) != EOF)
+		    if (spec == specec)
+		        break
+	        if (spec == specec)
+		    next
+	        fd2 = ""
+	    }
+
+	    specec = spec // ectype
+
+	    scat = no
+	    extract = no
+	    disp = no
+	    ext = no
+	    flux = no
+	    if (scattered) {
+		hselect (spec, "apscatte", yes, > temp2)
+		fd2 = temp2
+		if (fscan (fd2, str) < 1)
+		    scat = yes
+		fd2 = ""; delete (temp2, verify=no)
+	    }
+	    if (reextract || !access (specec) || (update && scat)) {
+		extract = yes
+	    } else {
+		hselect (specec, "dc-flag", yes, > temp2)
+		hselect (specec, "ex-flag", yes, >> temp2)
+		hselect (specec, "ca-flag", yes, >> temp2)
+		fd2 = temp2
+		extract = update && newaps
+		if (fscan (fd2, str1) == 1)
+		    extract = update && newdisp
+		else
+		    disp = yes
+		if (fscan (fd2, str1) == 1)
+		    extract = update && !extcor
+		else
+		    ext = extcor
+		if (fscan (fd2, str1) == 1)
+		    extract = update && (!fluxcal1 || newsens)
+		else
+		    flux = fluxcal1
+		fd2 = ""; delete (temp2, verify=no)
+	    }
+		
+	    if (extract) {
+		disp = dispcor
+		ext = extcor
+		flux = fluxcal1
+	    }
+		    
+	    if (scat)
+		print ("Subtract scattered light from ", spec)
+	    if (extract)
+		print ("Extract object spectrum ", spec)
+	    if (disp)
+	        print ("Dispersion correct ", spec)
+	    if (ext)
+		print ("Extinction correct ", spec)
+	    if (flux)
+		print ("Flux calibrate ", spec)
+	}
+	fd1 = ""; delete (temp1, verify=no)
+
+	if (access (done))
+	    delete (done, verify=no)
+end
diff --git a/noao/imred/src/doecslit/slistonly.par b/noao/imred/src/doecslit/slistonly.par
new file mode 100644
index 00000000..f0986d61
--- /dev/null
+++ b/noao/imred/src/doecslit/slistonly.par
@@ -0,0 +1,13 @@
+objects,s,a,,,,
+apref,f,a,"",,,
+arcs,s,a,,,,
+standards,s,a,,,,
+scattered,b,a,,,,
+dispcor,b,a,,,,
+extcor,b,a,,,,
+fluxcal,b,a,,,,
+redo,b,a,,,,
+update,b,a,,,,
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+mode,s,h,"q",,,
diff --git a/noao/imred/src/doecslit/slittasks.cl b/noao/imred/src/doecslit/slittasks.cl
new file mode 100644
index 00000000..ada92452
--- /dev/null
+++ b/noao/imred/src/doecslit/slittasks.cl
@@ -0,0 +1,19 @@
+#{ ECSLITPROC tasks
+
+task	doecslit	= "doecslit$doecslit.cl"
+task	sproc		= "doecslit$sproc.cl"
+task	sarcrefs	= "doecslit$sarcrefs.cl"
+task	sdoarcs		= "doecslit$sdoarcs.cl"
+task	sfluxcal	= "doecslit$sfluxcal.cl"
+task	sbatch		= "doecslit$sbatch.cl"
+task	slistonly	= "doecslit$slistonly.cl"
+task	sgetspec	= "doecslit$sgetspec.cl"
+
+task	sparams		= "doecslit$sparams.par"
+
+task	apslitproc	= "doecslit$x_apextract.e"
+
+hidetask sproc, sbatch, sarcrefs, sdoarcs, sfluxcal, slistonly, sgetspec
+hidetask sparams, apslitproc
+
+keep
diff --git a/noao/imred/src/doecslit/sparams.par b/noao/imred/src/doecslit/sparams.par
new file mode 100644
index 00000000..62868ed8
--- /dev/null
+++ b/noao/imred/src/doecslit/sparams.par
@@ -0,0 +1,65 @@
+line,i,h,INDEF,,,"Default dispersion line"
+nsum,i,h,10,,,"Number of dispersion lines to sum or median"
+extras,b,h,no,,,"Extract sky, sigma, etc.?
+
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --"
+ylevel,r,h,0.05,,,"Fraction of peak or intensity for resizing
+
+-- TRACE PARAMETERS --"
+t_step,i,h,10,,,"Tracing step"
+t_function,s,h,"spline3","chebyshev|legendre|spline1|spline3",,"Trace fitting function"
+t_order,i,h,2,,,"Trace fitting function order"
+t_niterate,i,h,1,0,,"Trace rejection iterations"
+t_low,r,h,3.,0.,,"Trace lower rejection sigma"
+t_high,r,h,3.,0.,,"Trace upper rejection sigma
+
+-- BACKGROUND AND SCATTERED LIGHT PARAMETERS --"
+b_function,s,h,"legendre","chebyshev|legendre|spline1|spline3",,Background function
+b_order,i,h,1,,,Background function order
+b_naverage,i,h,-100,,,Background average or median
+b_niterate,i,h,0,0,,Background rejection iterations
+b_low,r,h,3.,0.,,Background lower rejection sigma
+b_high,r,h,3.,0.,,Background upper rejection sigma
+buffer,r,h,1.,0.,,Buffer distance from apertures
+apscat1,pset,h,"",,,Fitting parameters across the dispersion
+apscat2,pset,h,"",,,"Fitting parameters along the dispersion
+
+-- APERTURE EXTRACTION PARAMETERS --"
+weights,s,h,"none","none|variance",,Extraction weights (none|variance)
+pfit,s,h,"fit1d","fit1d|fit2d",,Profile fitting algorithm (fit1d|fit2d)
+lsigma,r,h,3.,,,Lower rejection threshold
+usigma,r,h,3.,,,"Upper rejection threshold
+
+-- ARC DISPERSION FUNCTION PARAMETERS --"
+threshold,r,h,10.,0.,,"Minimum line contrast threshold"
+coordlist,f,h,linelists$thar.dat,,,"Line list"
+match,r,h,1.,,,"Line list matching limit in Angstroms"
+fwidth,r,h,4,,,"Arc line widths in pixels"
+cradius,r,h,10.,,,"Centering radius in pixels"
+i_function,s,h,"legendre","legendre|chebyshev",,"Echelle coordinate function"
+i_xorder,i,h,3,1,,Order of coordinate function along dispersion
+i_yorder,i,h,3,1,,Order of coordinate function across dispersion
+i_niterate,i,h,3,0,,"Rejection iterations"
+i_low,r,h,3.,0.,,"Lower rejection sigma"
+i_high,r,h,3.,0.,,"Upper rejection sigma"
+refit,b,h,yes,,,"Refit coordinate function when reidentifying
+
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --"
+select,s,h,"interp",,,"Selection method for reference spectra"
+sort,s,h,"jd",,,"Sort key"
+group,s,h,"ljd",,,"Group key"
+time,b,h,no,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting
+
+-- DISPERSION CORRECTION PARAMETERS --"
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+log,b,h,no,,,"Logarithmic wavelength scale?"
+flux,b,h,yes,,,"Conserve flux?
+
+-- SENSITIVITY CALIBRATION PARAMETERS --"
+bandwidth,r,h,10.,,,Bandpass widths
+bandsep,r,h,10.,,,Bandpass separation
+s_interact,b,h,yes,,,Graphic interaction to examine/define bandpasses
+s_function,s,h,"spline3","chebyshev|legendre|spline3|spline1",,"Fitting function"
+s_order,i,h,1,1,,"Order of sensitivity function"
+fnu,b,h,no,,,"Create spectra having units of FNU?"
diff --git a/noao/imred/src/doecslit/sproc.cl b/noao/imred/src/doecslit/sproc.cl
new file mode 100644
index 00000000..8caeadd9
--- /dev/null
+++ b/noao/imred/src/doecslit/sproc.cl
@@ -0,0 +1,490 @@
+# SPROC -- Process echelle slit spectra
+# This program combines all the operations of scattered light
+# subtraction, extraction, dispersion correction, extinction correction,
+# and flux calibration in as simple and noninteractive manner as
+# possible.  The data must all share the same position on the 2D image
+# and the same dispersion solution apart from small instrumental changes
+# which can be followed automatically.
+
+procedure sproc (objects, apref, arcs, arctable, standards, recenter,
+	resize, quicklook, trace, scattered, arcap, dispcor, extcor,
+	fluxcal, splot, redo, update, batch, listonly)
+
+file	objects			{prompt="List of object spectra"}
+
+file	apref			{prompt="Aperture reference spectrum"}
+file	arcs			{prompt="List of arc spectra"}
+file	arctable		{prompt="Arc assignment table (optional)"}
+file	standards		{prompt="List of standard star spectra\n"}
+
+bool	recenter		{prompt="Recenter object apertures?"}
+bool	resize			{prompt="Resize object apertures?"}
+bool	quicklook		{prompt="Edit/review object apertures?"}
+bool	trace			{prompt="Trace object spectra?"}
+bool	scattered		{prompt="Subtract scattered light?"}
+bool	arcap			{prompt="Use object apertures for arcs?"}
+bool	dispcor			{prompt="Dispersion correct spectra?"}
+bool	extcor			{prompt="Extinction correct spectra?"}
+bool	fluxcal			{prompt="Flux calibrate spectra?"}
+bool	splot			{prompt="Plot the final spectrum?"}
+bool	redo			{prompt="Redo operations if previously done?"}
+bool	update			{prompt="Update spectra if cal data changes?"}
+bool	batch			{prompt="Extract objects in batch?"}
+bool	listonly		{prompt="List steps but don't process?\n"}
+
+real	datamax = INDEF		{prompt="Max data value / cosmic ray threshold"}
+
+string	anssplot = "yes"	{prompt="Splot spectrum?", mode="q",
+				 enum="no|yes|NO|YES"}
+bool	newaps, newdisp, newsens, newarcs
+bool	fluxcal1, splot1, splot2
+bool	dobatch
+
+struct	*fd1, *fd2, *fd3
+
+begin
+	string	imtype, ectype
+	string	arcref, spec, arc
+	string	arcrefec, specec, arcec
+	string	temp, done
+	string	str1, str2, str3, str4, arcrefs, log1, log2
+	bool	reextract, extract, scat, disp, ext, flux, log, disperr
+	int	i, j, n
+	struct	err
+	str1 = ""
+
+	# Call a separate task to do the listing to minimize the size of
+	# this script and improve it's readability.
+
+	dobatch = no
+	if (listonly) {
+	    slistonly (objects, apref, arcs, standards, scattered,
+		dispcor, extcor, fluxcal, redo, update)
+	    bye
+	}
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	ectype = ".ec" // imtype
+	n = strlen (imtype)
+
+	# Temporary files used repeatedly in this script.  Under some
+	# abort circumstances these files may be left behind.
+
+	temp = mktemp ("tmp$iraf")
+	done = mktemp ("tmp$iraf")
+
+	# Rather than always have switches on the logfile and verbose flags
+	# we use TEE and set a file to "dev$null" if output is not desired.
+	# We must check for the null string to signify no logfile.
+
+	tee.append = yes
+	if (logfile == "")
+	    log1 = "dev$null"
+	else
+	    log1 = logfile
+	if (verbose)
+	    log2 = "STDOUT"
+	else
+	    log2 = "dev$null"
+
+	# If the update switch is used changes in the calibration data
+	# can cause images to be reprocessed (if they are in the object
+	# list).  Possible changes are in the aperture definitions,
+	# dispersion solution, and sensitivity function.  The newarcs
+	# flag is used to only go through the arc image headers once
+	# setting the reference spectrum, airmass, and UT.
+
+	newaps = no
+	newdisp = no
+	newsens = no
+	newarcs = yes
+	fluxcal1 = fluxcal
+
+	# Check if there are aperture definitions in the database and
+	# define them if needed.  This is usually somewhat interactive.
+	# Set the newaps flag in case an update is desired.
+
+	# Initialize APSCRIPT for aperture reference.
+	apslitproc.saturation = INDEF
+	apslitproc.references = ""
+	apslitproc.ansfind = "YES"
+	if (recenter)
+	    apslitproc.ansrecenter = "YES"
+	else
+	    apslitproc.ansrecenter = "NO"
+	if (resize)
+	    apslitproc.ansresize = "YES"
+	else
+	    apslitproc.ansresize = "NO"
+	apslitproc.ansedit = "yes"
+	apslitproc.anstrace = "YES"
+	apslitproc.ansfittrace = "yes"
+	apslitproc.ansextract = "NO"
+
+	i = strlen (apref)
+	if (i > n && substr (apref, i-n+1, i) == imtype)
+	    apref = substr (apref, 1, i-n)
+
+	reextract = redo
+	if (reextract || !access (database // "/ap" // apref)) {
+	    if (!access (apref // imtype)) {
+		printf ("Aperture reference spectrum not found - %s%s\n",
+		    apref, imtype) | scan (err)
+		error (1, err // "\nCheck setting of imtype")
+	    }
+	    scat = no
+	    if (scattered) {
+		hselect (apref, "apscatte", yes, > temp)
+		fd1 = temp
+		if (fscan (fd1, str1) < 1)
+		    scat = yes
+		fd1 = ""; delete (temp, verify=no)
+	    }
+
+	    print ("Set reference aperture for ", apref) | tee (log1)
+	    delete (database//"/ap"//apref, verify=no, >& "dev$null")
+	    apslitproc (apref)
+	    newaps = yes
+	}
+
+	# Initialize APSCRIPT for aperture definitions.
+	if (quicklook) {
+	    apslitproc.ansedit = "NO"
+	    apslitproc.ansfittrace = "NO"
+	}
+	if (trace) {
+	    apslitproc.anstrace = "yes"
+	} else {
+	    apslitproc.anstrace = "NO"
+	}
+	apslitproc.ansextract = "NO"
+	apslitproc.ansscat = "NO"
+
+	print ("Define object apertures", >> log1)
+	if (redo)
+	    apslitproc ("@"//objects, references=apref)
+	else
+	    apslitproc ("@"//objects, references="NEW"//apref)
+	if (dispcor && fluxcal1) {
+	    if (redo)
+		apslitproc ("@"//standards, references=apref)
+	    else
+		apslitproc ("@"//standards, references="NEW"//apref)
+	}
+
+	# Initialize APSCRIPT for extraction and SPLOT.
+	apslitproc.ansrecenter = "NO"
+	apslitproc.ansresize = "NO"
+	apslitproc.ansedit = "NO"
+	apslitproc.anstrace = "NO"
+	apslitproc.ansextract = "YES"
+	apslitproc.ansreview = "NO"
+	apslitproc.ansscat = "NO"
+	apslitproc.anssmooth = "YES"
+
+	if (splot && !quicklook) {
+	    splot1 = yes
+	    splot2 = yes
+	} else {
+	    splot1 = no
+	    splot2 = no
+	}
+
+	# The next step is to setup the scattered light correction if needed.
+	# We use the aperture reference image for the interactive setting.
+	# If this image has been  scattered light corrected we assume the
+	# scattered light functions parameters are correctly set.
+
+	scat = no
+	if (scattered) {
+	    hselect (apref, "apscatte", yes, > temp)
+	    fd1 = temp
+	    if (fscan (fd1, str1) < 1)
+		scat = yes
+	    fd1 = ""; delete (temp, verify=no)
+	}
+	if (scat) {
+	    print ("Setup and do scattered light subtraction in ", apref) |
+		tee (log1)
+	    apslitproc.ansfitscatter = "yes"
+	    apslitproc.ansfitsmooth = "yes"
+	    apslitproc (apref, ansextract="NO", ansscat="YES")
+	    apslitproc.ansfitscatter = "NO"
+	    apslitproc.ansfitsmooth = "NO"
+	}
+
+	# If not dispersion correcting we can go directly to extracting
+	# the object spectra.  The reference arcs are the first on
+	# the arc lists.  The processing of the reference arcs is done
+	# by the task ARCREFS.
+
+	arcref = ""
+	arcrefs = ""
+	if (dispcor) {
+	    if (arctable == "")
+		arcrefs = "@"//arcs
+	    else
+		arcrefs = arctable
+
+	    fd1 = arcs
+	    if (fscan (fd1, arcref) == EOF)
+		error (1, "No reference arcs")
+	    fd1 = ""
+	    if (!access (arcref // imtype)) {
+		printf ("Arc reference spectrum not found - %s%s\n",
+		    arcref, imtype) | scan (err)
+		error (1, err // "\nCheck setting of imtype")
+	    }
+	    arcrefec = arcref // ectype
+	    reextract = redo || (update && newaps)
+	    if (reextract && access (arcrefec))
+	        imdelete (arcrefec, verify=no)
+
+	    apslitproc.references = apref
+	    sarcrefs (arcref, done, log1, log2)
+	    apslitproc.references = ""
+
+	    if (fluxcal1)
+		sfluxcal (standards, arcs, arcref, arcrefs, redo, update,
+		    scattered, arcap, extcor, done, log1, log2)
+	}
+
+	# Now we are ready to process the object spectra.
+
+	reextract = redo || (update && (newaps || newdisp))
+	fd1 = objects
+	while (fscan (fd1, spec) != EOF) {
+	    # Check if previously done; i.e. arc.
+	    if (access (done)) {
+	        fd2 = done
+	        while (fscan (fd2, specec) != EOF)
+		    if (spec == specec)
+		        break
+	        if (spec == specec)
+		    next
+	        fd2 = ""
+	    }
+	    if (!access (spec // imtype)) {
+		printf ("Object spectrum not found - %s%s\n",
+		    spec, imtype) | scan (err)
+		print (err) | tee (log1)
+		print ("Check setting of imtype")
+		next
+	    }
+	    specec = spec // ectype
+
+	    # Determine required operations from the flags and image header.
+	    scat = no
+	    extract = no
+	    disp = no
+	    ext = no
+	    flux = no
+	    if (scattered) {
+		hselect (spec, "apscatte", yes, > temp)
+		fd2 = temp
+		if (fscan (fd2, str1) < 1)
+		    scat = yes
+		fd2 = ""; delete (temp, verify=no)
+	    }
+	    if (reextract || !access (specec) || (update && scat))
+		extract = yes
+	    else {
+		hselect (specec, "dc-flag", yes, > temp)
+		hselect (specec, "ex-flag", yes, >> temp)
+		hselect (specec, "ca-flag", yes, >> temp)
+		fd2 = temp
+		if (fscan (fd2, str1) == 1) {
+		    extract = update && newdisp
+		    if (update && !newdisp)
+		        # We really should check if REFSPEC will assign
+			# different reference spectra.
+			;
+		} else
+		    disp = dispcor
+		if (fscan (fd2, str1) == 1)
+		    extract = update && !extcor
+		else
+		    ext = extcor
+		if (fscan (fd2, str1) == 1)
+		    extract = update && (!fluxcal1 || newsens)
+		else
+		    flux = fluxcal1
+		fd2 = ""; delete (temp, verify=no)
+	    }
+
+	    if (extract) {
+		disp = dispcor
+		ext = extcor
+		flux = fluxcal1
+	    }
+
+	    # If fully processed go to the next object.
+	    if (!extract && !disp && !extcor && !flux)
+		next
+
+	    # If not interactive and the batch flag is set submit rest to batch.
+	    if (batch && !splot1 && !splot2) {
+		fd1 = ""
+		flprcache
+		sbatch.objects = objects
+		sbatch.datamax = datamax
+		sbatch.arcs = arcs
+		sbatch.arcref = arcref
+		sbatch.arcrefs = arcrefs
+		sbatch.done = done
+		sbatch.logfile = log1
+		sbatch.redo = reextract
+		sbatch.update = update
+		sbatch.scattered = scattered
+		sbatch.arcap = arcap
+		sbatch.dispcor = dispcor
+		sbatch.fluxcal1 = fluxcal1
+		sbatch.extcor = extcor
+		sbatch.newaps = newaps
+		sbatch.newdisp = newdisp
+		sbatch.newsens = newsens
+		sbatch.newarcs = newarcs
+		dobatch = yes
+		return
+	    }
+
+	    # Process the spectrum in foreground.
+	    if (extract) {
+		if (access (specec))
+		    imdelete (specec, verify=no)
+
+		if (scat) {
+		    print ("Subtract scattered light in ", spec) | tee (log1)
+		    apslitproc (spec, ansextract="NO", ansscat="YES")
+		}
+
+		print ("Extract object spectrum ", spec) | tee (log1)
+		hselect (spec, "date-obs,ut,exptime", yes, > temp)
+		hselect (spec, "ra,dec,epoch,st", yes, >> temp)
+		fd2 = temp
+		if (fscan (fd2, str1, str2, str3) == 3) {
+		    setjd (spec, observatory=observatory, date="date-obs",
+			time="ut", exposure="exptime", jd="jd", hjd="",
+			ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+			>> log1)
+		    if (fscan (fd2, str1, str2, str3, str4) == 4)
+			setairmass (spec, intype="beginning",
+			    outtype="effective", exposure="exptime",
+			    observatory=observatory, show=no, update=yes,
+			    override=yes, >> log1)
+		}
+		fd2 = ""; delete (temp, verify=no)
+		apslitproc (spec, saturation=datamax)
+	    }
+
+	    disperr = no
+	    if (disp) {
+		# Fix arc headers if necessary.
+		if (newarcs) {
+	    	    fd2 = arcs
+	    	    while (fscan (fd2, arc) != EOF) {
+			hselect (arc, "date-obs,ut,exptime", yes, > temp)
+			hselect (arc, "ra,dec,epoch,st", yes, >> temp)
+			fd3 = temp
+			if (fscan (fd3, str1, str2, str3) == 3) {
+			    setjd (arc, observatory=observatory,
+				date="date-obs", time="ut", exposure="exptime",
+				jd="jd", hjd="", ljd="ljd", utdate=yes,
+				uttime=yes, listonly=no, >> log1)
+			    if (fscan (fd3, str1, str2, str3, str4) == 4)
+				setairmass (arc, intype="beginning",
+				    outtype="effective", exposure="exptime",
+				    observatory=observatory, show=no,
+				    update=yes, override=yes, >> log1)
+			}
+			fd3 = ""; delete (temp, verify=no)
+	        	hedit (arc, "refspec1", arc, add=yes, verify=no,
+		    	    show=no, update=yes)
+		    }
+	    	    fd2 = ""
+		    newarcs = no
+		}
+
+		print ("Assign arc spectra for ", spec) | tee (log1)
+		refspectra (spec, references=arcrefs,
+		    apertures="", refaps="", ignoreaps=no,
+		    select=sparams.select, sort=sparams.sort,
+		    group=sparams.group, time=sparams.time,
+		    timewrap=sparams.timewrap, override=yes, confirm=no,
+		    assign=yes, logfiles="STDOUT", verbose=no) |
+		    tee (log1, > log2)
+
+		sdoarcs (spec, arcref, reextract, arcap, log1, no)
+
+	        hselect (specec, "refspec1", yes, > temp)
+	        fd2 = temp
+	        i = fscan (fd2, arc)
+	        fd2 = ""; delete (temp, verify=no)
+		if (i < 1) {
+		    print ("No arc reference assigned for ", spec) | tee (log1)
+		    disperr = yes
+		} else {
+	            print ("Dispersion correct ", spec) | tee (log1)
+		    dispcor (specec, "", linearize=sparams.linearize,
+			database=database, table=arcref//ectype,
+			w1=INDEF, w2=INDEF, dw=INDEF, nw=INDEF,
+			log=sparams.log, flux=sparams.flux, samedisp=no,
+			global=no, confirm=no, ignoreaps=no, listonly=no,
+			logfile=logfile)
+		    hedit (specec, "dc-flag", 0, add=yes, show=no,
+			verify=no, update=yes)
+		}
+	    }
+
+	    if (!disperr && (extract || disp)) {
+	        if (ext)
+		    print ("Extinction correct ", spec) | tee (log1)
+	        if (flux)
+		    print ("Flux calibrate ", spec) | tee (log1)
+	        if (flux || ext)
+		    calibrate (specec, "", extinct=extcor, flux=fluxcal1,
+			extinction=extinction, observatory=observatory,
+			ignoreaps=no, sensitivity="sens", fnu=sparams.fnu) |
+			tee (log1, > log2)
+	    }
+	    if (extract || disp || ext || flux) {
+		if (splot1) {
+		    print (specec, ":")
+		    str1 = anssplot
+		    if (str1 == "NO" || str1 == "YES")
+			splot1 = no
+		    if (str1 == "no" || str1 == "NO")
+			splot2 = no
+		    else
+			splot2 = yes
+		}
+		if (splot2)
+		    splot (specec)
+		else if (splot && quicklook) {
+		    if (disp) {
+			print ("q") |
+			specplot (specec, apertures="", autolayout=no,
+			    scale=1., offset=0., step=0., sysid=yes,
+			    yscale=yes, xmin=INDEF, xmax=INDEF, ymin=INDEF,
+			    ymax=INDEF, logfile="", graphics="stdgraph",
+			    cursor="STDIN")
+		    } else {
+			print ("q") |
+			specplot (specec, apertures="", autolayout=yes,
+			    autoscale=no, scale=1., offset=0., step=0.,
+			    sysid=yes, yscale=no, xmin=INDEF, xmax=INDEF,
+			    ymin=INDEF, ymax=INDEF, logfile="",
+			    graphics="stdgraph", cursor="STDIN")
+		    }
+		}
+	    }
+	    print (spec, >> done)
+	}
+	fd1 = ""
+
+	if (access (done))
+	    delete (done, verify=no)
+end
diff --git a/noao/imred/src/doecslit/sproc.par b/noao/imred/src/doecslit/sproc.par
new file mode 100644
index 00000000..a0ecbd0c
--- /dev/null
+++ b/noao/imred/src/doecslit/sproc.par
@@ -0,0 +1,35 @@
+objects,f,a,"",,,"List of object spectra"
+apref,f,a,"",,,"Aperture reference spectrum"
+arcs,f,a,"",,,"List of arc spectra"
+arctable,f,a,"",,,"Arc assignment table (optional)"
+standards,f,a,"",,,"List of standard star spectra
+"
+recenter,b,a,,,,"Recenter object apertures?"
+resize,b,a,,,,"Resize object apertures?"
+quicklook,b,a,,,,"Edit/review object apertures?"
+trace,b,a,,,,"Trace object spectra?"
+scattered,b,a,,,,"Subtract scattered light?"
+arcap,b,a,,,,"Use object apertures for arcs?"
+dispcor,b,a,,,,"Dispersion correct spectra?"
+extcor,b,a,,,,"Extinction correct spectra?"
+fluxcal,b,a,,,,"Flux calibrate spectra?"
+splot,b,a,,,,"Plot the final spectrum?"
+redo,b,a,,,,"Redo operations if previously done?"
+update,b,a,,,,"Update spectra if cal data changes?"
+batch,b,a,,,,"Extract objects in batch?"
+listonly,b,a,,,,"List steps but don\'t process?
+"
+datamax,r,h,INDEF,,,"Max data value / cosmic ray threshold"
+anssplot,s,q,"yes",no|yes|NO|YES,,"Splot spectrum?"
+newaps,b,h,,,,
+newdisp,b,h,,,,
+newsens,b,h,,,,
+newarcs,b,h,,,,
+fluxcal1,b,h,,,,
+splot1,b,h,,,,
+splot2,b,h,,,,
+dobatch,b,h,,,,
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+fd3,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/dofoe/Revisions b/noao/imred/src/dofoe/Revisions
new file mode 100644
index 00000000..25357644
--- /dev/null
+++ b/noao/imred/src/dofoe/Revisions
@@ -0,0 +1,47 @@
+.help revisions Jan95 noao.imred.src.dofoe
+.nf
+dofoe$batch.cl
+dofoe$proc.cl
+dofoe$response.cl
+    Error messages now hint to check imtype setting.
+    (4/15/05, Valdes)
+
+========
+V2.11.3b
+========
+
+dofoe$proc.cl
+    Modified code to eliminate goto.  This is for use with pyraf.
+    (11/21/00, Valdes)
+
+========
+V2.11.3a
+========
+
+dofoe$arcrefs.cl
+dofoe$batch.cl
+dofoe$doarcs.cl
+dofoe$listonly.cl
+dofoe$proc.cl
+dofoe$response.cl
+    Any additional qualifiers in the imtype string are stripped.
+    (8/14/97, Valdes)
+
+=========
+V2.11BETA
+=========
+
+dofoe$apsript.par
+    Made changes for the new aperture selection option.  (9/5/96, Valdes)
+
+dofoe$params.par
+dofoe$arcrefs.cl
+dofoe$doarcs.cl
+    Added "threshold" as a user parameter.  (1/16/95, Valdes)
+
+dofoe$proc.cl
+dofoe$batch.cl
+dofoe$listonly.cl
+    The test for extracted spectra based on the system keyword was failing
+    and so it was removed.  (1/16/95, Valdes)
+.endhelp
diff --git a/noao/imred/src/dofoe/apscript.par b/noao/imred/src/dofoe/apscript.par
new file mode 100644
index 00000000..c316829d
--- /dev/null
+++ b/noao/imred/src/dofoe/apscript.par
@@ -0,0 +1,145 @@
+# APSCRIPT
+
+input,s,a,,,,List of input images
+output,s,h,"",,,List of output spectra
+apertures,s,h,"",,,Apertures
+scatter,s,h,"",,,List of scattered light images (optional)
+references,s,h,"",,,List of aperture reference images
+profiles,s,h,"",,,"List of aperture profile images
+"
+interactive,b,h,yes,,,Run task interactively?
+find,b,h,yes,,,Find apertures?
+recenter,b,h,yes,,,Recenter apertures?
+resize,b,h,yes,,,Resize apertures?
+edit,b,h,yes,,,Edit apertures?
+trace,b,h,yes,,,Trace apertures?
+fittrace,b,h,yes,,,Fit the traced points interactively?
+extract,b,h,yes,,,Extract spectra?
+review,b,h,yes,,,Review extractions?
+subtract,b,h,yes,,,Subtract scattered light?
+smooth,b,h,yes,,,Smooth scattered light along the dispersion?
+fitscatter,b,h,yes,,,Fit scattered light interactively?
+fitsmooth,b,h,yes,,,"Smooth the scattered light interactively?
+"
+line,i,h,)params.line,,,>params.line
+nsum,i,h,)params.nsum,,,>params.nsum
+buffer,r,h,)params.buffer,,,">params.buffer
+
+# OUTPUT PARAMETERS
+"
+format,s,h,"echelle",,,Extracted spectra format
+extras,b,h,)params.extras,,,>params.extras
+dbwrite,s,h,"YES",,,Write to database?
+initialize,b,h,no,,,Initialize answers?
+verbose,b,h,)_.verbose,,,"Verbose output?
+
+# DEFAULT APERTURE PARAMETERS
+"
+lower,r,h,)params.lower,,,>params.lower
+upper,r,h,)params.upper,,,>params.upper
+apidtable,s,h,"",,,"Aperture ID table (optional)
+
+# DEFAULT BACKGROUND PARAMETERS
+"
+b_function,s,h,)params.b_function,,,>params.b_function
+b_order,i,h,)params.b_order,,,>params.b_order
+b_sample,s,h,)params.b_sample,,,>params.b_sample
+b_naverage,i,h,)params.b_naverage,,,>params.b_naverage
+b_niterate,i,h,)params.b_niterate,,,>params.b_niterate
+b_low_reject,r,h,)params.b_low,,,>params.b_low
+b_high_reject,r,h,)params.b_high,,,>params.b_high
+b_grow,r,h,)params.b_grow,,,">params.b_grow
+
+# APERTURE CENTERING PARAMETERS
+"
+width,r,h,,0.,,Profile centering width
+radius,r,h,,,,Profile centering radius
+threshold,r,h,10.,0.,,"Detection threshold for profile centering
+
+# AUTOMATIC FINDING AND ORDERING PARAMETERS
+"
+nfind,i,h,,,,Number of apertures to be found automatically
+minsep,r,h,1.,,,Minimum separation between spectra
+maxsep,r,h,100000.,,,Maximum separation between spectra
+order,s,h,"increasing","increasing|decreasing",,"Order of apertures
+
+# RECENTERING PARAMETERS
+"
+aprecenter,s,h,"",,,Apertures for recentering calculation
+npeaks,r,h,0.5,,,Select brightest peaks
+shift,b,h,yes,,,"Use average shift instead of recentering?
+
+# RESIZING PARAMETERS
+"
+llimit,r,h,INDEF,,,Lower aperture limit relative to center
+ulimit,r,h,INDEF,,,Upper aperture limit relative to center
+ylevel,r,h,)params.ylevel,,,>params.ylevel
+peak,b,h,yes,,,Is ylevel a fraction of the peak?
+bkg,b,h,yes,,,"Subtract background in automatic width?"
+r_grow,r,h,0.,,,"Grow limits by this factor"
+avglimits,b,h,no,,,"Average limits over all apertures?
+
+# EDITING PARAMETERS
+"
+e_output,s,q,,,,Output spectra rootname
+e_profiles,s,q,,,,"Profile reference image
+
+# TRACING PARAMETERS
+"
+t_nsum,i,h,)params.nsum,,,>params.nsum
+t_step,i,h,)params.t_step,,,>params.t_step
+t_nlost,i,h,3,1,,Number of consecutive times profile is lost before quitting
+t_width,r,h,,0.,,Profile centering width
+t_function,s,h,)params.t_function,,,>params.t_function
+t_sample,s,h,"*",,,Trace sample regions
+t_order,i,h,)params.t_order,,,>params.t_order
+t_naverage,i,h,1,,,Trace average or median
+t_niterate,i,h,)params.t_niterate,,,>params.t_niterate
+t_low_reject,r,h,)params.t_low,,,>params.t_low
+t_high_reject,r,h,)params.t_high,,,>params.t_high
+t_grow,r,h,0.,0.,,"Trace rejection growing radius
+
+# EXTRACTION PARAMETERS
+"
+background,s,h,,"none|average|median|minimum|fit",,Background to subtract
+skybox,i,h,)params.b_smooth,,,>params.b_smooth
+weights,s,h,)params.weights,,,>params.weights
+pfit,s,h,)params.pfit,,,>params.pfit
+clean,b,h,,,,Detect and replace bad pixels?
+nclean,r,h,0.5,,,Maximum number of pixels to clean
+niterate,i,h,5,0,,Number of profile fitting iterations
+saturation,r,h,INDEF,,,Saturation level
+readnoise,s,h,,,,Read out noise sigma (photons)
+gain,s,h,,,,Photon gain (photons/data number)
+lsigma,r,h,)params.lsigma,,,>params.lsigma
+usigma,r,h,)params.usigma,,,>params.usigma
+polysep,r,h,0.95,0.1,0.95,Marsh algorithm polynomial spacing
+polyorder,i,h,10,1,,Marsh algorithm polynomial order
+nsubaps,i,h,1,1,,"Number of subapertures per aperture
+
+# ANSWER PARAMETERS
+"
+ansclobber,s,h,"NO",,," "
+ansclobber1,s,h,"NO",,," "
+ansdbwrite,s,h,"YES",,," "
+ansdbwrite1,s,h,"NO",,," "
+ansedit,s,h,"NO",,," "
+ansextract,s,h,"NO",,," "
+ansfind,s,h,"NO",,," "
+ansfit,s,h,"NO",,," "
+ansfitscatter,s,h,"NO",,," "
+ansfitsmooth,s,h,"NO",,," "
+ansfitspec,s,h,"NO",,," "
+ansfitspec1,s,h,"NO",,," "
+ansfittrace,s,h,"NO",,," "
+ansfittrace1,s,h,"NO",,," "
+ansflat,s,h,"NO",,," "
+ansnorm,s,h,"NO",,," "
+ansrecenter,s,h,"NO",,," "
+ansresize,s,h,"NO",,," "
+ansreview,s,h,"NO",,," "
+ansreview1,s,h,"NO",,," "
+ansscat,s,h,"NO",,," "
+ansskyextract,s,h,"NO",,," "
+anssmooth,s,h,"NO",,," "
+anstrace,s,h,"NO",,," "
diff --git a/noao/imred/src/dofoe/arcrefs.cl b/noao/imred/src/dofoe/arcrefs.cl
new file mode 100644
index 00000000..fa8f950a
--- /dev/null
+++ b/noao/imred/src/dofoe/arcrefs.cl
@@ -0,0 +1,106 @@
+# ARCREFS -- Determine dispersion relation for reference arc.
+
+procedure arcrefs (arcref, arcaps, arcbeams, response, done, log1, log2)
+
+file	arcref
+string	arcaps
+string	arcbeams
+file	response
+file	done
+file	log1
+file	log2
+
+struct	*fd
+
+begin
+	string	arcrefec, arcec, temp, str, imtype
+	int	i, dc
+	bool	log
+
+	temp = mktemp ("tmp$iraf")
+
+	# Extract the primary arc reference spectrum.  Determine the
+	# dispersion function with ECIDENTIFY/ECREIDENTIFY.  Set the wavelength
+	# parameters with ECDISPCOR.
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	arcrefec = arcref // ".ec"
+	if (arcaps != "" || arcbeams  != "")
+	    arcec = arcref // "arc.ec"
+	else
+	    arcec = ""
+	if (!access (arcrefec//imtype)) {
+	    print ("Extract arc reference image ", arcref) | tee (log1)
+	    apscript (arcref, ansrecenter="NO", ansresize="NO", ansedit="NO",
+		anstrace="NO", background="none", clean=no, weights="none")
+	    if (response != "")
+		sarith (arcrefec, "/", response, arcrefec, w1=INDEF, w2=INDEF,
+		    apertures="", bands="", beams="", apmodulus=0, reverse=no,
+		    ignoreaps=no, format="multispec", renumber=no, offset=0,
+		    clobber=yes, merge=no, errval=0, verbose=no)
+	    if (arcec != "") {
+		scopy (arcrefec, arcec, w1=INDEF, w2=INDEF, apertures=arcaps,
+		    bands="", beams=arcbeams, apmodulus=0, offset=0,
+		    format="multispec", clobber=yes, merge=no, renumber=yes,
+		    verbose=no)
+		scopy (arcrefec, "", w1=INDEF, w2=INDEF, apertures="!"//arcaps,
+		    bands="", beams=arcbeams, apmodulus=0, offset=0,
+		    format="multispec", clobber=yes, merge=no, renumber=yes,
+		    verbose=no)
+	    }
+	}
+		    
+	# Get the dispersion parameters from the header.  These are
+	# used for all further spectra and also flag whether this
+	# spectrum has been processed.  If the parameters are missing
+	# the spectrum needs to have the dispersion function and
+	# wavelength scale determined.  The HEDIT is needed because
+	# in some cases the user may exit IDENTIFY without updating
+	# the database (if the image was deleted but the database
+	# entry was not).
+
+	hselect (arcrefec, "dc-flag", yes, > temp)
+	fd = temp
+	dc = -1
+	i = fscan (fd, dc)
+	fd = ""; delete (temp, verify=no)
+	if (dc == -1) {
+	    print ("Determine dispersion solution for ", arcref) | tee (log1)
+	    delete (database//"/ec"//arcref//".ec*", verify=no)
+	    ecidentify (arcrefec, database=database,
+		coordlist=params.coordlist, match=params.match,
+		maxfeatures=100, zwidth=10., ftype="emission",
+		fwidth=params.fwidth, cradius=params.cradius,
+		threshold=params.threshold, minsep=2.,
+		function=params.i_function, xorder=params.i_xorder,
+		yorder=params.i_yorder, niterate=params.i_niterate,
+		lowreject=params.i_low, highreject=params.i_high,
+		autowrite=yes)
+	    if (arcec != "") {
+		ecreidentify (arcec, arcrefec, shift=0., cradius=params.cradius,
+		    threshold=params.threshold, refit=yes, database=database,
+		    logfiles=log1//","//log2)
+		imdelete (arcec, verify=no)
+	    }
+	    hedit (arcrefec, "refspec1", arcref // ".ec", add=yes,
+		show=no, verify=no, update=yes)
+	}
+
+	# Dispersion correct the reference arc.  Set the newdisp flag.
+
+	if (dc == -1) {
+	    dispcor (arcrefec, "", linearize=params.linearize,
+		database=database, table="", w1=INDEF, w2=INDEF, dw=INDEF,
+		nw=INDEF, log=params.log, flux=params.flux, samedisp=no,
+		global=no, ignoreaps=no, confirm=no, listonly=no, verbose=yes,
+		logfile=log1, > log2)
+	    hedit (arcrefec, "dc-flag", 0, add=yes, verify=no,
+		show=no, update=yes)
+	    proc.newdisp = yes
+	}
+
+	print (arcref, >> done)
+end
diff --git a/noao/imred/src/dofoe/arcrefs.par b/noao/imred/src/dofoe/arcrefs.par
new file mode 100644
index 00000000..5aa35c57
--- /dev/null
+++ b/noao/imred/src/dofoe/arcrefs.par
@@ -0,0 +1,9 @@
+arcref,f,a,"",,,
+arcaps,s,a,,,,
+arcbeams,s,a,,,,
+response,f,a,"",,,
+done,f,a,"",,,
+log1,f,a,"",,,
+log2,f,a,"",,,
+fd,*struct,h,"",,,
+mode,s,h,"q",,,
diff --git a/noao/imred/src/dofoe/batch.cl b/noao/imred/src/dofoe/batch.cl
new file mode 100644
index 00000000..6adcbb04
--- /dev/null
+++ b/noao/imred/src/dofoe/batch.cl
@@ -0,0 +1,207 @@
+# BATCH -- Process spectra in batch.
+# This task is called in batch mode.  It only processes objects
+# not previously processed unless the update or redo flags are set.
+
+procedure batch ()
+
+string	objects		{prompt="Object spectra"}
+real	datamax 	{prompt="Max data value / cosmic ray threshold"}
+
+file	response	{prompt="Response spectrum"}
+string	arcs		{prompt="List of arc spectra"}
+file	arcref		{prompt="Arc reference for dispersion solution"}
+string	arcrefs		{prompt="Arc references"}
+
+string	objaps		{prompt="Object apertures"}
+string	arcaps		{prompt="Arc apertures"}
+string	objbeams	{prompt="Object beam numbers"}
+string	arcbeams	{prompt="Arc beam numbers\n"}
+
+file	done		{prompt="File of spectra already done"}
+file	logfile		{prompt="Logfile"}
+
+bool	redo		{prompt="Redo operations?"}
+bool	update		{prompt="Update spectra?"}
+bool	scattered	{prompt="Subtract scattered light?"}
+bool	arcap		{prompt="Use object apertures for arcs?"}
+bool	dispcor		{prompt="Dispersion correct spectra?"}
+
+bool	newaps, newresp, newdisp, newarcs
+
+struct	*fd1, *fd2
+
+begin
+	file	temp1, temp2, spec, specec, arc, arcec
+	bool	reextract, extract, scat, disp, log
+	string	imtype, ectype, str
+	int	i, n
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	ectype = ".ec" // imtype
+	n = strlen (imtype)
+
+	temp1 = mktemp ("tmp$iraf")
+	temp2 = mktemp ("tmp$iraf")
+
+	# Initialize extraction to be noninteractive.
+	if (apscript.ansrecenter == "yes")
+	    apscript.ansrecenter = "YES"
+	else if (apscript.ansrecenter == "no")
+	    apscript.ansrecenter = "NO"
+	apscript.ansedit = "NO"
+	if (apscript.anstrace == "yes") {
+	    apscript.anstrace = "YES"
+	    apscript.ansfittrace = "NO"
+	} else if (apscript.anstrace == "no")
+	    apscript.anstrace = "NO"
+
+	reextract = redo || (update && (newaps || newresp || newdisp))
+
+	hselect (objects, "$I", yes, > temp1)
+	#sections (objects, option="fullname", > temp1)
+	fd1 = temp1
+	while (fscan (fd1, spec) != EOF) {
+	    i = strlen (spec)
+	    if (i > n && substr (spec, i-n+1, i) == imtype)
+		spec = substr (spec, 1, i-n)
+	    
+	    if (access (done)) {
+	        fd2 = done
+	        while (fscan (fd2, specec) != EOF)
+		    if (spec == specec)
+		        break
+	        if (spec == specec)
+		    next
+	        fd2 = ""
+	    }
+	    if (!access (spec // imtype)) {
+		printf ("Object spectrum not found - %s%s\nCheck setting of imtype\n", spec, imtype) | tee (log1)
+		next
+	    }
+	    specec = spec // ectype
+
+	    scat = no
+	    extract = no
+	    disp = no
+	    if (scattered) {
+		hselect (spec, "apscatte", yes, > temp2)
+		fd2 = temp2
+		if (fscan (fd2, str) < 1)
+		    scat = yes
+		fd2 = ""; delete (temp2, verify=no)
+	    }
+	    if (reextract || !access (specec) || (update && scat))
+		extract = yes
+	    else {
+		hselect (specec, "dc-flag", yes, > temp2)
+		fd2 = temp2
+		if (fscan (fd2, str) == 1) {
+		    extract = update && newdisp
+		    if (update && !newdisp)
+		        # We really should check if REFSPEC will assign
+			# different reference spectra.
+			;
+		} else
+		    disp = dispcor
+		fd2 = ""; delete (temp2, verify=no)
+	    }
+		
+	    if (extract)
+		disp = dispcor
+
+	    if (extract) {
+		if (access (specec))
+		    imdelete (specec, verify=no)
+		if (scat) {
+		    print ("Subtract scattered light in ", spec, >> logfile)
+		    apscript (spec, output="", ansextract="NO",
+			ansscat="YES", anssmooth="YES", verbose=no)
+		}
+		print ("Extract object spectrum ", spec, >> logfile)
+		setjd (spec, observatory=observatory, date="date-obs",
+		    time="ut", exposure="exptime", jd="jd", hjd="",
+		    ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+		    >> logfile)
+	        setairmass (spec, intype="beginning",
+		    outtype="effective", exposure="exptime",
+		    observatory=observatory, show=no, update=yes,
+		    override=yes, >> logfile)
+		apscript (spec, saturation=datamax, verbose=no)
+		if (response != "")
+		    sarith (specec, "/", response, specec, w1=INDEF, w2=INDEF,
+			apertures="", bands="", beams="", apmodulus=0,
+			reverse=no, ignoreaps=no, format="multispec",
+			renumber=no, offset=0, clobber=yes, merge=no,
+			errval=0, verbose=no)
+	    }
+
+	    if (disp) {
+		# Fix arc headers if necessary.
+		if (newarcs) {
+	    	    sections (arcs, option="fullname", >temp2)
+		    setjd ("@"//temp2, observatory=observatory, date="date-obs",
+			time="ut", exposure="exptime", jd="jd", hjd="",
+			ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+			>> logfile)
+	    	    setairmass ("@"//temp2, intype="beginning",
+			outtype="effective", exposure="exptime",
+			observatory=observatory, show=no, update=yes,
+			override=yes, >> logfile)
+		    delete (temp2, verify=no)
+		    hselect (arcs, "$I", yes, >temp2)
+	    	    fd2 = temp2
+	    	    while (fscan (fd2, arc) != EOF) {
+	        	i = strlen (arc)
+	        	if (i > n && substr (arc, i-n+1, i) == imtype)
+	            	    arc = substr (arc, 1, i-n)
+	        	hedit (arc, "refspec1", arc, add=yes, verify=no,
+		    	    show=no, update=yes)
+	        	hedit (arc, "arctype", "henear", add=yes, verify=no,
+		    	    show=no, update=yes)
+	    	    }
+	    	    fd2 = ""; delete (temp2, verify=no)
+		    newarcs = no
+		}
+
+		print ("Assign arc spectra for ", spec, >> logfile)
+		refspectra (spec, references=arcrefs,
+		    apertures="", refaps="", ignoreaps=no,
+		    select=params.select, sort=params.sort,
+		    group=params.group, time=params.time,
+		    timewrap=params.timewrap, override=yes, confirm=no,
+		    assign=yes, logfiles="STDOUT", verbose=no,
+		    >> logfile)
+
+		doarcs (spec, response, arcref, arcaps, arcbeams, reextract,
+		    arcap, logfile, yes)
+
+	        hselect (specec, "refspec1", yes, > temp2)
+	        fd2 = temp2
+	        i = fscan (fd2, arc)
+	        fd2 = ""; delete (temp2, verify=no)
+		if (i < 1)
+		    print ("No arc reference assigned for ", spec, >> logfile)
+		else {
+	            print ("Dispersion correct ", spec, >> logfile)
+		    dispcor (specec, "", linearize=params.linearize,
+			database=database, table=arcref//ectype,
+			w1=INDEF, w2=INDEF, dw=INDEF, nw=INDEF,
+			log=params.log, samedisp=no, flux=params.flux,
+			global=no, ignoreaps=no, confirm=no, listonly=no,
+			verbose=no, logfile=logfile)
+		    hedit (specec, "dc-flag", 0, add=yes, verify=no,
+			show=no, update=yes)
+		    disp = no
+		}
+	    }
+	}
+	fd1 = ""; delete (temp1, verify=no)
+
+	if (access (done))
+	    delete (done, verify=no)
+
+	flprcache (0)
+end
diff --git a/noao/imred/src/dofoe/batch.par b/noao/imred/src/dofoe/batch.par
new file mode 100644
index 00000000..81b8c8ae
--- /dev/null
+++ b/noao/imred/src/dofoe/batch.par
@@ -0,0 +1,25 @@
+objects,s,h,,,,"Object spectra"
+datamax,r,h,,,,"Max data value / cosmic ray threshold"
+response,f,h,"",,,"Response spectrum"
+arcs,s,h,,,,"List of arc spectra"
+arcref,f,h,"",,,"Arc reference for dispersion solution"
+arcrefs,s,h,,,,"Arc references"
+objaps,s,h,,,,"Object apertures"
+arcaps,s,h,,,,"Arc apertures"
+objbeams,s,h,,,,"Object beam numbers"
+arcbeams,s,h,,,,"Arc beam numbers
+"
+done,f,h,"",,,"File of spectra already done"
+logfile,f,h,"",,,"Logfile"
+redo,b,h,,,,"Redo operations?"
+update,b,h,,,,"Update spectra?"
+scattered,b,h,,,,"Subtract scattered light?"
+arcap,b,h,,,,"Use object apertures for arcs?"
+dispcor,b,h,,,,"Dispersion correct spectra?"
+newaps,b,h,,,,
+newresp,b,h,,,,
+newdisp,b,h,,,,
+newarcs,b,h,,,,
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/dofoe/doarcs.cl b/noao/imred/src/dofoe/doarcs.cl
new file mode 100644
index 00000000..653146b1
--- /dev/null
+++ b/noao/imred/src/dofoe/doarcs.cl
@@ -0,0 +1,167 @@
+# DOARCS -- Determine dispersion relation for spectrum based on reference arcs.
+
+procedure doarcs (spec, response, arcref, arcaps, arcbeams, reextract,
+	arcap, logfile, batch)
+
+file	spec
+file	response
+file	arcref
+string	arcaps
+string	arcbeams
+bool	reextract
+bool	arcap
+file	logfile
+bool	batch
+
+struct	*fd
+
+begin
+	string	imtype, ectype
+	int	i, j, k, n
+	file	temp, arc1, arc2, str1, str2, arctype, apref, arc, arcec, logs
+	file	specec, specarc
+	bool	verbose1
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	ectype = ".ec" // imtype
+	n = strlen (imtype)
+
+	temp = mktemp ("tmp$iraf")
+
+	if (batch)
+	    verbose1 = no
+	else
+	    verbose1 = verbose
+	if (verbose1)
+	    logs = logfile//",STDOUT"
+	else
+	    logs = logfile
+
+	# Separate simultaneous arc from object.
+	specec = spec // ".ec"
+	if (arcaps != "" || arcbeams != "")
+	    specarc = spec // "arc1.ec"
+	else
+	     specarc = ""
+	if (specarc != "") {
+	    scopy (specec, specarc, w1=INDEF, w2=INDEF, apertures=arcaps,
+		bands="", beams="", apmodulus=0, format="multispec",
+		renumber=yes, offset=0, clobber=yes, merge=no, verbose=no)
+	    scopy (specec, "", w1=INDEF, w2=INDEF, apertures="!"//arcaps,
+		bands="", beams="", apmodulus=0, format="multispec",
+		renumber=yes, offset=0, clobber=yes, merge=no, verbose=no)
+	}
+
+	for (j=1; j<=2; j+=1) {
+	    # The reference spectra refer initially to the 2D image.  At the
+	    # end we will reset them to refer to the 1D spectra.
+
+	    hselect (spec, "refspec"//j, yes, > temp)
+	    fd = temp
+	    k = fscan (fd, arc1, str1)
+	    fd = ""; delete (temp, verify=no)
+	    if (k < 1)
+		break
+
+	    # Strip possible image extension.
+	    i = strlen (arc1)
+	    if (i > n && substr (arc1, i-n+1, i) == imtype)
+		arc1 = substr (arc1, 1, i-n)
+    
+	    # Set extraction output and aperture reference depending on whether
+	    # the arcs are to be rextracted using recentered or retraced object
+	    # apertures.
+
+	    if (arcap &&
+		(apscript.ansrecenter=="yes" || apscript.anstrace=="yes" ||
+		 apscript.ansrecenter=="YES" || apscript.anstrace=="YES")) {
+		arc2 = spec // arc1
+		apref = spec
+		if (access (arc2//ectype))
+		    imdelete (arc2//ectype, verify=no)
+		delete (database//"/ec"//arc2//".ec*", verify = no)
+	    } else {
+		arc2 = arc1
+		apref = apscript.references
+	    }
+
+	    # Arcs are reidentified using the user refit option.
+	    #	Also internal arcs are checked if HENEAR.
+
+	    hselect (arc1, "arctype", yes, > temp)
+	    fd = temp
+	    i = fscan (fd, arctype)
+	    fd = ""; delete (temp, verify=no)
+    
+	    # Extract and determine dispersion function if necessary.
+	    if (!access (arc2//ectype)) {
+		if (!batch)
+		    print ("Extract and reidentify arc spectrum ", arc1)
+		print ("Extract and reidentify arc spectrum ", arc1, >> logfile)
+		apscript (arc1, output=arc2//".ec", references=apref,
+		    ansrecenter="NO", ansresize="NO", ansedit="NO",
+		    anstrace="NO", background="none",
+		    clean=no, weights="none", verbose=verbose1)
+		if (response != "")
+		    sarith (arc2//".ec", "/", response, arc2//".ec", w1=INDEF,
+			w2=INDEF, apertures="", bands="", beams="", apmodulus=0,
+			reverse=no, ignoreaps=no, format="multispec",
+			renumber=no, offset=0, clobber=yes, merge=no, errval=0,
+			verbose=no)
+
+		if (arcaps != "") {
+		    scopy (arc2//".ec", arc2//"arc.ec", w1=INDEF, w2=INDEF,
+			apertures=arcaps, bands="",  beams="", apmodulus=0,
+			format="multispec", renumber=yes, offset=0,
+			clobber=yes, merge=no, verbose=no)
+		    scopy (arc2//".ec", "", w1=INDEF, w2=INDEF,
+			apertures="!"//arcaps, bands="",  beams="",
+			apmodulus=0, format="multispec", renumber=yes, offset=0,
+			clobber=yes, merge=no, verbose=no)
+		    ecreidentify (arc2//"arc.ec", arcref//"arc.ec", shift=0.,
+			cradius=params.cradius, threshold=params.threshold,
+			refit=yes, database=database, logfiles=logs)
+		    imdelete (arc2//"arc.ec", verify=no)
+		}
+		ecreidentify (arc2//".ec", arcref//".ec", shift=0.,
+		    cradius=params.cradius, threshold=params.threshold,
+		    refit=yes, database=database, logfiles=logs)
+
+		# If not reextracting arcs based on object apertures
+		# then save the extracted arc to avoid doing it again.
+
+		if (arc1 != arc2)
+		    imdelete (arc2//".ec", verify=no)
+	    }
+    
+	    # Set the REFSPEC parameters for echelle spectrum.
+	    if (k == 1)
+		hedit (specec, "refspec"//j, arc2//".ec", add=yes,
+		    verify=no, show=no, update=yes)
+	    else
+		hedit (specec, "refspec"//j, arc2//".ec "//str1,
+		    add=yes, verify=no, show=no, update=yes)
+
+	    # Check for arc fibers in object spectra.
+	    if (specarc != "") {
+		if (!batch)
+		    print ("Reidentify arc fibers in ", spec,
+			" with respect to ", arc1)
+		print ("Reidentify arc fibers in ", spec,
+		    " with respect to ", arc1, >> logfile)
+		delete (database//"/ec"//specarc, verify = no, >& "dev$null")
+		ecreidentify (specarc, arc2//"arc.ec", shift=0.,
+		    cradius=params.cradius, threshold=params.threshold,
+		    refit=no, database=database, logfiles=logs)
+		hedit (specec, "refshft"//j, specarc,
+		    add=yes, verify=no, show=no, update=yes)
+		imrename (specarc, spec//"arc"//j+1//".ec", verbose=no)
+		specarc = spec // "arc" // j+1 // ".ec"
+	    }
+	}
+	if (specarc != "")
+	    imdelete (specarc, verify=no)
+end
diff --git a/noao/imred/src/dofoe/doarcs.par b/noao/imred/src/dofoe/doarcs.par
new file mode 100644
index 00000000..e399380b
--- /dev/null
+++ b/noao/imred/src/dofoe/doarcs.par
@@ -0,0 +1,11 @@
+spec,f,a,"",,,
+response,f,a,"",,,
+arcref,f,a,"",,,
+arcaps,s,a,,,,
+arcbeams,s,a,,,,
+reextract,b,a,,,,
+arcap,b,a,,,,
+logfile,f,a,"",,,
+batch,b,a,,,,
+fd,*struct,h,"",,,
+mode,s,h,"q",,,
diff --git a/noao/imred/src/dofoe/dofoe.cl b/noao/imred/src/dofoe/dofoe.cl
new file mode 100644
index 00000000..ae1c2ca8
--- /dev/null
+++ b/noao/imred/src/dofoe/dofoe.cl
@@ -0,0 +1,89 @@
+# DOFOE -- Process FOE spectra from 2D to wavelength calibrated 1D.
+#
+# The task PROC does all of the interactive work and BATCH does the
+# background work.  This procedure is organized this way to minimize the
+# dictionary space when the background task is submitted.
+
+procedure dofoe (objects)
+
+string	objects = ""		{prompt="List of object spectra"}
+
+file	apref = ""		{prompt="Aperture reference spectrum"}
+file	flat = ""		{prompt="Flat field spectrum"}
+string	arcs = ""		{prompt="List of arc spectra"}
+file	arctable = ""		{prompt="Arc assignment table (optional)\n"}
+
+string	readnoise = "0."	{prompt="Read out noise sigma (photons)"}
+string	gain = "1."		{prompt="Photon gain (photons/data number)"}
+real	datamax = INDEF		{prompt="Max data value / cosmic ray threshold"}
+int	norders = 12		{prompt="Number of orders"}
+real	width = 4.		{prompt="Width of profiles (pixels)"}
+string	arcaps = "2x2"		{prompt="Arc apertures\n"}
+
+bool	fitflat = yes		{prompt="Fit and ratio flat field spectrum?"}
+string	background = "none"	{prompt="Background to subtract",
+			 enum="none|scattered|average|median|minimum|fit"}
+bool	clean = no		{prompt="Detect and replace bad pixels?"}
+bool	dispcor = yes		{prompt="Dispersion correct spectra?"}
+bool	redo = no		{prompt="Redo operations if previously done?"}
+bool	update = no		{prompt="Update spectra if cal data changes?"}
+bool	batch = no		{prompt="Extract objects in batch?"}
+bool	listonly = no		{prompt="List steps but don't process?\n"}
+
+pset	params = ""		{prompt="Algorithm parameters"}
+
+begin
+	int	i, j
+	bool	scattered
+
+	# Remove any leading whitespace from parameters that might be null.
+	if (logfile != "") {
+	    j = strlen (logfile)
+	    for (i=1; i<=j && substr(logfile,i,i)==" "; i+=1);
+	    logfile = substr (logfile, i, j)
+	}
+	if (flat != "") {
+	    j = strlen (flat)
+	    for (i=1; i<=j && substr(flat,i,i)==" "; i+=1);
+	    flat = substr (flat, i, j)
+	}
+	if (arctable != "") {
+	    j = strlen (arctable)
+	    for (i=1; i<=j && substr(arctable,i,i)==" "; i+=1);
+	    arctable = substr (arctable, i, j)
+	}
+	if (arcaps != "") {
+	    j = strlen (arcaps)
+	    for (i=1; i<=j && substr(arcaps,i,i)==" "; i+=1);
+	    arcaps = substr (arcaps, i, j)
+	}
+
+	apscript.readnoise = readnoise
+	apscript.gain = gain
+	if (arcaps != "")
+	    i = 2 * norders
+	else
+	    i = norders
+	apscript.nfind = i
+	apscript.width = width
+	apscript.t_width = width
+	apscript.radius = width
+	apscript.clean = clean
+	if (background == "scattered") {
+	    scattered = yes
+	    apscript.background = "none"
+	} else {
+	    scattered = no
+	    apscript.background = background
+	}
+	proc.datamax = datamax
+
+	proc (objects, apref, flat, arcs, arctable, i, "", arcaps,
+	    "", "", fitflat, yes, scattered, no, no, no, clean, dispcor,
+	    no, redo, update, batch, listonly)
+
+	if (proc.dobatch) {
+	    print ("-- Do remaining spectra as a batch job --")
+	    print ("batch&batch") | cl
+	}
+end
diff --git a/noao/imred/src/dofoe/dofoe.par b/noao/imred/src/dofoe/dofoe.par
new file mode 100644
index 00000000..9853b7e5
--- /dev/null
+++ b/noao/imred/src/dofoe/dofoe.par
@@ -0,0 +1,24 @@
+objects,s,a,"",,,"List of object spectra"
+apref,f,h,"",,,"Aperture reference spectrum"
+flat,f,h,"",,,"Flat field spectrum"
+arcs,s,h,"",,,"List of arc spectra"
+arctable,f,h,"",,,"Arc assignment table (optional)
+"
+readnoise,s,h,"0.",,,"Read out noise sigma (photons)"
+gain,s,h,"1.",,,"Photon gain (photons/data number)"
+datamax,r,h,INDEF,,,"Max data value / cosmic ray threshold"
+norders,i,h,12,,,"Number of orders"
+width,r,h,4.,,,"Width of profiles (pixels)"
+arcaps,s,h,"2x2",,,"Arc apertures
+"
+fitflat,b,h,yes,,,"Fit and ratio flat field spectrum?"
+background,s,h,"none",none|scattered|average|median|minimum|fit,,"Background to subtract"
+clean,b,h,no,,,"Detect and replace bad pixels?"
+dispcor,b,h,yes,,,"Dispersion correct spectra?"
+redo,b,h,no,,,"Redo operations if previously done?"
+update,b,h,no,,,"Update spectra if cal data changes?"
+batch,b,h,no,,,"Extract objects in batch?"
+listonly,b,h,no,,,"List steps but don\'t process?
+"
+params,pset,h,"",,,"Algorithm parameters"
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/dofoe/dofoetasks.cl b/noao/imred/src/dofoe/dofoetasks.cl
new file mode 100644
index 00000000..4c602be0
--- /dev/null
+++ b/noao/imred/src/dofoe/dofoetasks.cl
@@ -0,0 +1,19 @@
+#{ DOFOE tasks
+
+task	dofoe		= "dofoe$dofoe.cl"
+task	params		= "dofoe$params.par"
+
+task	proc		= "dofoe$proc.cl"
+task	response	= "dofoe$response.cl"
+task	arcrefs		= "dofoe$arcrefs.cl"
+task	doarcs		= "dofoe$doarcs.cl"
+task	batch		= "dofoe$batch.cl"
+task	listonly	= "dofoe$listonly.cl"
+
+task	apscript	= "dofoe$x_apextract.e"
+
+# Hide tasks from the user
+hidetask apscript
+hidetask params, proc, batch, arcrefs, doarcs, listonly, response
+
+keep
diff --git a/noao/imred/src/dofoe/listonly.cl b/noao/imred/src/dofoe/listonly.cl
new file mode 100644
index 00000000..bae8aff8
--- /dev/null
+++ b/noao/imred/src/dofoe/listonly.cl
@@ -0,0 +1,167 @@
+# LISTONLY -- List processing to be done.
+#
+# This follows pretty much the same logic as the full procedure but doesn't
+# do anything but list the operations.
+
+procedure listonly (objects, apref, flat, arcs, scattered, dispcor,
+	redo, update)
+
+string	objects = ""		{prompt="List of object spectra"}
+file	apref = ""		{prompt="Aperture reference spectrum"}
+file	flat = ""		{prompt="Flat field spectrum"}
+string	arcs = ""		{prompt="List of arc spectra"}
+
+bool	scattered		{prompt="Subtract scattered light?"}
+bool	dispcor			{prompt="Dispersion correct spectra?"}
+bool	redo			{prompt="Redo operations if previously done?"}
+bool	update			{prompt="Update spectra if cal data changes?"}
+
+struct	*fd1
+struct	*fd2
+
+begin
+	string	imtype, ectype
+	string	spec, arcref
+	string	specec, arcrefec, response
+	string	temp1, temp2, done, str
+	bool	reextract, newaps, newresp, newdisp, extract, disp, scat
+	int	i, j, n
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	ectype = ".ec" // imtype
+	n = strlen (imtype)
+
+	temp1 = mktemp ("tmp$iraf")
+	temp2 = mktemp ("tmp$iraf")
+	done = mktemp ("tmp$iraf")
+
+	newaps = no
+	newresp = no
+	newdisp = no
+
+	i = strlen (apref)
+	if (i > n && substr (apref, i-n+1, i) == imtype)
+	    apref = substr (apref, 1, i-n)
+
+	reextract = redo
+	if (reextract || !access (database // "/ap" // apref)) {
+	    print ("Set reference aperture for ", apref)
+	    newaps = yes
+	}
+
+	if (flat != "") {
+	    response = flat
+	    i = strlen (response)
+	    if (i > n && substr (response, i-n+1, i) == imtype)
+	        response = substr (response, 1, i-n)
+	    response = response // "norm.ec"
+
+	    reextract = redo || (update && newaps)
+	    scat = no
+	    if (scattered) {
+		hselect (flat, "apscatte", yes, > temp2)
+		fd2 = temp2
+		if (fscan (fd2, str) < 1)
+		    scat = yes
+		fd2 = ""; delete (temp2, verify=no)
+	    }
+	    if (reextract || !access (response // imtype) || (update && scat)) {
+		if (scat)
+		    print ("Subtract scattered light from ", flat)
+	        print ("Create response function ", response)
+	        newresp = yes
+	    }
+	}
+
+	if (dispcor) {
+	    hselect (arcs, "$I", yes, > temp1)
+	    #sections (arcs, option="fullname", > temp1)
+	    fd1 = temp1
+	    i = fscan (fd1, arcref)
+	    if (i < 1)
+		error (1, "No reference arcs")
+	    fd1 = ""; delete (temp1, verify=no)
+	    i = strlen (arcref)
+	    if (i > n && substr (arcref, i-n+1, i) == imtype)
+	        arcref = substr (arcref, 1, i-n)
+	    arcrefec = arcref // ectype
+
+	    reextract = redo || (update && newaps)
+	    if (reextract || !access (arcrefec)) {
+	        print ("Extract arc reference image ", arcref)
+	        print ("Determine dispersion solution for ", arcref)
+	        newdisp = yes
+	    } else {
+		hselect (arcrefec, "refspec1,dc-flag", yes, > temp1)
+	        fd1 = temp1
+	        i = fscan (fd1, str, j)
+	        fd1 = ""; delete (temp1, verify=no)
+	        if (i < 1) {
+	            print ("Determine dispersion solution for ", arcref)
+	            newdisp = yes
+	        }
+	    }
+	    print (arcref, > done)
+	}
+
+	reextract = redo || (update && (newaps || newresp || newdisp))
+	hselect (objects, "$I", yes, > temp1)
+	#sections (objects, option="fullname", > temp1)
+	fd1 = temp1
+	while (fscan (fd1, spec) != EOF) {
+	    if (i > n && substr (spec, i-n+1, i) == imtype)
+	        spec = substr (spec, 1, i-n)
+
+	    if (access (done)) {
+	        fd2 = done
+	        while (fscan (fd2, specec) != EOF)
+		    if (spec == specec)
+		        break
+	        if (spec == specec)
+		    next
+	        fd2 = ""
+	    }
+
+	    specec = spec // ectype
+
+	    scat = no
+	    extract = no
+	    disp = no
+	    if (scattered) {
+		hselect (spec, "apscatte", yes, > temp2)
+		fd2 = temp2
+		if (fscan (fd2, str) < 1)
+		    scat = yes
+		fd2 = ""; delete (temp2, verify=no)
+	    }
+	    if (reextract || !access (specec) || (update && scat)) {
+		extract = yes
+	    } else {
+		hselect (specec, "dc-flag", yes, > temp2)
+		fd2 = temp2
+		extract = update && newaps
+		if (fscan (fd2, str) == 1)
+		    extract = update && newdisp
+		else
+		    disp = yes
+		fd2 = ""; delete (temp2, verify=no)
+	    }
+		
+	    if (extract)
+		disp = dispcor
+		    
+	    if (scat)
+		print ("Subtract scattered light from ", spec)
+	    if (extract)
+		print ("Extract object spectrum ", spec)
+	    if (disp)
+	        print ("Dispersion correct ", spec)
+	}
+	fd1 = ""; delete (temp1, verify=no)
+
+	if (access (done))
+	    delete (done, verify=no)
+end
diff --git a/noao/imred/src/dofoe/listonly.par b/noao/imred/src/dofoe/listonly.par
new file mode 100644
index 00000000..a05b8f94
--- /dev/null
+++ b/noao/imred/src/dofoe/listonly.par
@@ -0,0 +1,11 @@
+objects,s,a,"",,,"List of object spectra"
+apref,f,a,"",,,"Aperture reference spectrum"
+flat,f,a,"",,,"Flat field spectrum"
+arcs,s,a,"",,,"List of arc spectra"
+scattered,b,a,,,,"Subtract scattered light?"
+dispcor,b,a,,,,"Dispersion correct spectra?"
+redo,b,a,,,,"Redo operations if previously done?"
+update,b,a,,,,"Update spectra if cal data changes?"
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+mode,s,h,"q",,,
diff --git a/noao/imred/src/dofoe/params.par b/noao/imred/src/dofoe/params.par
new file mode 100644
index 00000000..fafb71f7
--- /dev/null
+++ b/noao/imred/src/dofoe/params.par
@@ -0,0 +1,69 @@
+line,i,h,INDEF,,,"Default dispersion line"
+nsum,i,h,10,,,"Number of dispersion lines to sum or median"
+extras,b,h,no,,,"Extract sky, sigma, etc.?
+
+-- DEFAULT APERTURE LIMITS --"
+lower,r,h,-3.,,,"Lower aperture limit relative to center"
+upper,r,h,3.,,,"Upper aperture limit relative to center
+
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --"
+ylevel,r,h,0.05,,,"Fraction of peak or intensity for resizing
+
+-- TRACE PARAMETERS --"
+t_step,i,h,10,,,"Tracing step"
+t_function,s,h,"spline3","chebyshev|legendre|spline1|spline3",,"Trace fitting function"
+t_order,i,h,2,,,"Trace fitting function order"
+t_niterate,i,h,1,0,,"Trace rejection iterations"
+t_low,r,h,3.,0.,,"Trace lower rejection sigma"
+t_high,r,h,3.,0.,,"Trace upper rejection sigma
+
+-- DEFAULT BACKGROUND PARAMETERS --"
+buffer,r,h,1.,0.,,Buffer distance from apertures
+apscat1,pset,h,"",,,Fitting parameters across the dispersion
+apscat2,pset,h,"",,,Fitting parameters along the dispersion
+b_function,s,h,"legendre","chebyshev|legendre|spline1|spline3",,Background function
+b_order,i,h,2,,,Background function order
+b_sample,s,h,"-10:-6,6:10",,,Background sample regions
+b_naverage,i,h,-3,,,Background average or median
+b_niterate,i,h,0,0,,Background rejection iterations
+b_low,r,h,3.,0.,,Background lower rejection sigma
+b_high,r,h,3.,0.,,Background upper rejection sigma
+b_grow,r,h,0.,0.,,Background rejection growing radius
+b_smooth,i,h,10,,,"Background smoothing length
+
+-- APERTURE EXTRACTION PARAMETERS --"
+weights,s,h,"none","none|variance",,Extraction weights (none|variance)
+pfit,s,h,"fit1d","fit1d|fit2d",,Profile fitting algorithm (fit1d|fit2d)
+lsigma,r,h,3.,,,Lower rejection threshold
+usigma,r,h,3.,,,"Upper rejection threshold
+
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --"
+f_interactive,b,h,no,,,"Fit flat field interactively?"
+f_function,s,h,"spline3",spline3|legendre|chebyshev|spline1,,"Fitting function"
+f_order,i,h,20,1,,"Fitting function order
+
+-- ARC DISPERSION FUNCTION PARAMETERS --"
+threshold,r,h,10.,0.,,"Minimum line contrast threshold"
+coordlist,f,h,linelists$thar.dat,,,"Line list"
+match,r,h,1.,,,"Line list matching limit in Angstroms"
+fwidth,r,h,4.,,,"Arc line widths in pixels"
+cradius,r,h,4.,,,Centering radius in pixels
+i_function,s,h,"chebyshev","legendre|chebyshev",,"Echelle coordinate function"
+i_xorder,i,h,3,1,,Order of coordinate function along dispersion
+i_yorder,i,h,3,1,,Order of coordinate function across dispersion
+i_niterate,i,h,3,0,,"Rejection iterations"
+i_low,r,h,3.,0.,,"Lower rejection sigma"
+i_high,r,h,3.,0.,,"Upper rejection sigma"
+refit,b,h,yes,,,"Refit coordinate function when reidentifying?
+
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --"
+select,s,h,"interp",,,"Selection method for reference spectra"
+sort,s,h,"jd",,,"Sort key"
+group,s,h,"ljd",,,"Group key"
+time,b,h,no,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting
+
+-- DISPERSION CORRECTION PARAMETERS --"
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+log,b,h,no,,,"Logarithmic wavelength scale?"
+flux,b,h,yes,,,"Conserve flux?"
diff --git a/noao/imred/src/dofoe/proc.cl b/noao/imred/src/dofoe/proc.cl
new file mode 100644
index 00000000..75740bda
--- /dev/null
+++ b/noao/imred/src/dofoe/proc.cl
@@ -0,0 +1,464 @@
+# PROC -- Process echelle fiber spectra
+# This program combines the operations of extraction, flat fielding, and
+# dispersion correction in as simple and noninteractive way as possible.
+# It supports a second simultaneous arc fiber.  The data must all share
+# the same position on the 2D image and the same dispersion solution
+# apart from small instrumental changes which can be tracked
+# automatically.  The apertures must be identified sequentially and must
+# be properly paired if a arc fiber is used.
+# 
+# If every needed on could add sky subtraction (with a sky fiber) and
+# fluxing following the model of the multifiber packages.
+
+procedure proc (objects, apref, flat, arcs, arctable, naps, objaps, arcaps,
+	objbeams, arcbeams, fitflat, recenter, scattered, edit, trace, arcap,
+	clean, dispcor, splot, redo, update, batch, listonly)
+
+string	objects			{prompt="List of object spectra"}
+
+file	apref			{prompt="Aperture reference spectrum"}
+file	flat			{prompt="Flat field spectrum"}
+string	arcs			{prompt="List of arc spectra"}
+file	arctable		{prompt="Arc assignment table (optional)\n"}
+
+int	naps			{prompt="Number of apertures"}
+string	objaps			{prompt="Object apertures"}
+string	arcaps			{prompt="Arc apertures"}
+string	objbeams		{prompt="Object beam numbers"}
+string	arcbeams		{prompt="Arc beam numbers\n"}
+
+bool	fitflat			{prompt="Fit and ratio flat field spectrum?"}
+bool	recenter		{prompt="Recenter object apertures?"}
+bool	scattered		{prompt="Subtract scattered light?"}
+bool	edit			{prompt="Edit/review object apertures?"}
+bool	trace			{prompt="Trace object spectra?"}
+bool	arcap			{prompt="Use object apertures for arcs?"}
+bool	clean			{prompt="Detect and replace bad pixels?"}
+bool	dispcor			{prompt="Dispersion correct spectra?"}
+bool	splot			{prompt="Plot the final spectrum?"}
+bool	redo			{prompt="Redo operations if previously done?"}
+bool	update			{prompt="Update spectra if cal data changes?"}
+bool	batch			{prompt="Extract objects in batch?"}
+bool	listonly		{prompt="List steps but don't process?\n"}
+
+real	datamax = INDEF		{prompt="Max data value / cosmic ray threshold"}
+
+bool	newaps, newresp, newdisp, newarcs, dobatch
+
+string	anssplot = "yes"	{prompt="Splot spectrum?", mode="q",
+				 enum="no|yes|NO|YES"}
+
+struct	*fd1, *fd2
+
+begin
+	string	imtype, ectype
+	string	arcref, spec, arc
+	string	arcrefec, specec, arcec, response
+	string	temp1, temp2, done
+	string	str1, objs, arcrefs, log1, log2
+	bool	reextract, extract, scat, disp, disperr, log
+	bool	splot1, splot2
+	int	i, j, n, nspec
+	struct	err
+
+	# Call a separate task to do the listing to minimize the size of
+	# this script and improve it's readability.
+
+	dobatch = no
+	if (listonly) {
+	    listonly (objects, apref, flat, arcs, scattered, dispcor,
+		redo, update)
+	    bye
+	}
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	ectype = ".ec" // imtype
+	n = strlen (imtype)
+
+	# Get query parameter.
+	objs = objects
+	if (arctable == "")
+	    arcrefs = arcs
+	else
+	    arcrefs = arctable
+	arcref = ""
+
+	# Temporary files used repeatedly in this script.  Under some
+	# abort circumstances these files may be left behind.
+
+	temp1 = mktemp ("tmp$iraf")
+	temp2 = mktemp ("tmp$iraf")
+	done = mktemp ("tmp$iraf")
+
+	# Rather than always have switches on the logfile and verbose flags
+	# we use TEE and set a file to "dev$null" if output is not desired.
+	# We must check for the null string to signify no logfile.
+
+	tee.append = yes
+	if (logfile == "")
+	    log1 = "dev$null"
+	else
+	    log1 = logfile
+	if (verbose)
+	    log2 = "STDOUT"
+	else
+	    log2 = "dev$null"
+
+	# If the update switch is used changes in the calibration data
+	# can cause images to be reprocessed (if they are in the object
+	# list).  Possible changes are in the aperture definitions,
+	# response function, dispersion solution, and sensitivity
+	# function.  The newarcs flag is used to only go through the arc
+	# image headers once setting the reference spectrum, airmass, and
+	# UT.
+
+	newaps = no
+	newresp = no
+	newdisp = no
+	newarcs = yes
+
+	# Check if there are aperture definitions in the database and
+	# define them if needed.  This is usually somewhat interactive.
+	# Delete the database entry to start fresh if we enter this
+	# because of a redo.  Set the newaps flag in case an update is
+	# desired.
+
+	i = strlen (apref)
+	if (i > n && substr (apref, i-n+1, i) == imtype)
+	    apref = substr (apref, 1, i-n)
+
+	# Initialize
+	apscript.saturation = INDEF
+	apscript.references = apref
+	apscript.profiles = ""
+	apscript.nfind = naps
+	apscript.clean = clean
+	if (splot) {
+	    splot1 = yes
+	    splot2 = yes
+	} else {
+	    splot1 = no
+	    splot2 = no
+	}
+
+	reextract = redo
+	if (reextract || !access (database // "/ap" // apref)) {
+	    if (!access (apref // imtype)) {
+		printf ("Aperture reference spectrum not found - %s%s\n",
+		    apref, imtype) | scan (err)
+		error (1, err // "\nCheck setting of imtype")
+	    }
+	    print ("Set reference apertures for ", apref) | tee (log1)
+	    if (access (database // "/ap" // apref))
+		delete (database // "/ap" // apref, verify=no)
+	    apscript.ansresize = "yes"
+	    apscript.ansedit = "YES"
+	    apscript.ansfittrace = "yes"
+	    apscript (apref, references="", ansfind="YES", ansrecenter="NO",
+		anstrace="YES", ansextract="NO")
+	    newaps = yes
+	}
+
+	if (recenter)
+	    apscript.ansrecenter = "YES"
+	else
+	    apscript.ansrecenter = "NO"
+	apscript.ansresize = "NO"
+	if (edit)
+	    apscript.ansedit = "yes"
+	else
+	    apscript.ansedit = "NO"
+	if (trace)
+	    apscript.anstrace = "YES"
+	else
+	    apscript.anstrace = "NO"
+	apscript.ansfittrace = "NO"
+	apscript.ansextract = "YES"
+	apscript.ansreview = "NO"
+
+	# The next step is to setup the scattered light correction if needed.
+	# We use the flat field image for the interactive setting unless
+	# one is not used an then we use the aperture reference.
+	# If these images have been  scattered light corrected we assume the
+	# scattered light functions parameters are correctly set.
+
+	i = strlen (flat)
+	if (i > n && substr (flat, i-n+1, i) == imtype)
+	    flat = substr (flat, 1, i-n)
+
+	if (flat != "")
+	    spec = flat
+	else
+	    spec = apref
+
+	scat = no
+	if (scattered) {
+	    hselect (spec, "apscatte", yes, > temp1)
+	    fd1 = temp1
+	    if (fscan (fd1, str1) < 1)
+		scat = yes
+	    fd1 = ""; delete (temp1, verify=no)
+	}
+	if (scat) {
+	    print ("Subtract scattered light in ", spec) | tee (log1)
+	    apscript.ansfitscatter = "yes"
+	    apscript.ansfitsmooth = "yes"
+	    apscript (spec, output="", ansextract="NO", ansscat="YES",
+		anssmooth="YES")
+	    apscript.ansfitscatter = "NO"
+	    apscript.ansfitsmooth = "NO"
+	}
+
+	response = ""
+	if (flat != "") {
+	    response = flat // "norm.ec"
+	    reextract = redo || (update && newaps)
+	    if (reextract || !access (response // imtype) || (update && scat)) {
+	        print ("Create response function ", response) | tee (log1)
+
+	        if (access (response // imtype))
+		    imdelete (response, verify=no)
+	        if (access (flat //ectype))
+		    imdelete (flat//ectype, verify=no)
+
+	        response (flat, apref, response, recenter=recenter,
+		    edit=edit, trace=trace, clean=clean, fitflat=fitflat,
+		    interactive=params.f_interactive,
+		    function=params.f_function, order=params.f_order)
+
+	        newresp = yes
+	    }
+	}
+
+	# If not dispersion correcting we can go directly to extracting
+	# the object spectra.  The reference arcs are the first on
+	# the arc lists.  The processing of the reference arcs is done
+	# by the task ARCREFS.
+
+	if (dispcor) {
+	    hselect (arcs, "$I", yes, >temp1)
+	    fd1 = temp1
+	    i = fscan (fd1, arcref)
+	    if (i < 1)
+		error (1, "No reference arcs")
+	    fd1 = ""; delete (temp1, verify=no)
+	    i = strlen (arcref)
+	    if (i > n && substr (arcref, i-n+1, i) == imtype)
+	        arcref = substr (arcref, 1, i-n)
+	    if (!access (arcref // imtype)) {
+		printf ("Arc reference spectrum not found - %s%s\n",
+		    arcref, imtype) | scan (err)
+		error (1, err // "\nCheck setting of imtype")
+	    }
+	    arcrefec = arcref // ectype
+	    reextract = redo || (update && newaps)
+	    if (reextract && access (arcrefec))
+	        imdelete (arcrefec, verify=no)
+
+	    arcrefs (arcref, arcaps, arcbeams, response, done, log1, log2)
+	}
+
+	# Now we are ready to process the object spectra.
+
+	reextract = redo || (update && (newaps || newresp || newdisp))
+	hselect (objs, "$I", yes, > temp1)
+	fd1 = temp1
+	while (fscan (fd1, spec) != EOF) {
+	    i = strlen (spec)
+	    if (i > n && substr (spec, i-n+1, i) == imtype)
+		spec = substr (spec, 1, i-n)
+	    
+	    # Check if previously done; i.e. arc.
+	    if (access (done)) {
+	        fd2 = done
+	        while (fscan (fd2, specec) != EOF)
+		    if (spec == specec)
+		        break
+	        if (spec == specec)
+		    next
+	        fd2 = ""
+	    }
+	    if (!access (spec // imtype)) {
+		printf ("Object spectrum not found - %s%s\n",
+		    spec, imtype) | scan (err)
+		print (err) | tee (log1)
+		print ("Check setting of imtype")
+		next
+	    }
+	    specec = spec // ectype
+
+	    # Determine required operations from the flags and image header.
+	    scat = no
+	    extract = no
+	    disp = no
+	    if (scattered) {
+		hselect (spec, "apscatte", yes, > temp2)
+		fd2 = temp2
+		if (fscan (fd2, str1) < 1)
+		    scat = yes
+		fd2 = ""; delete (temp2, verify=no)
+	    }
+	    if (reextract || !access (specec) || (update && scat))
+		extract = yes
+	    else {
+		hselect (specec, "dc-flag", yes, > temp2)
+		fd2 = temp2
+		if (fscan (fd2, str1) == 1) {
+		    extract = update && newdisp
+		    if (update && !newdisp)
+		        # We really should check if REFSPEC will assign
+			# different reference spectra.
+			;
+		} else
+		    disp = dispcor
+
+		fd2 = ""; delete (temp2, verify=no)
+	    }
+		
+	    if (extract)
+		disp = dispcor
+
+	    # If fully processed go to the next object.
+	    if (!extract && !disp)
+		next
+
+	    # If not interactive and the batch flag is set submit rest to batch.
+	    if (batch && !splot1 && !splot2 && apscript.ansedit == "NO") {
+		fd1 = ""; delete (temp1, verify=no)
+		flprcache
+		batch.objects = objs
+		batch.datamax = datamax
+		batch.response = response
+		batch.arcs = arcs
+		batch.arcref = arcref
+		batch.arcrefs = arcrefs
+		batch.objaps = objaps
+		batch.arcaps = arcaps
+		batch.objbeams = objbeams
+		batch.arcbeams = arcbeams
+		batch.done = done
+		batch.logfile = log1
+		batch.redo = reextract
+		batch.update = update
+		batch.scattered = scattered
+		batch.arcap = arcap
+		batch.dispcor = dispcor
+		batch.newaps = newaps
+		batch.newresp = newresp
+		batch.newdisp = newdisp
+		batch.newarcs = newarcs
+		dobatch = yes
+		return
+	    }
+
+	    # Process the spectrum in foreground.
+	    if (extract) {
+		if (access (specec))
+		    imdelete (specec, verify=no)
+
+		if (scat) {
+		    print ("Subtract scattered light in ", spec) | tee (log1)
+		    apscript (spec, output="", ansextract="NO",
+			ansscat="YES", anssmooth="YES")
+		}
+
+		print ("Extract object spectrum ", spec) | tee (log1)
+		setjd (spec, observatory=observatory, date="date-obs",
+		    time="ut", exposure="exptime", jd="jd", hjd="",
+		    ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+		    >> log1)
+	        setairmass (spec, intype="beginning",
+		    outtype="effective", exposure="exptime",
+		    observatory=observatory, show=no, update=yes,
+		    override=yes, >> log1)
+		apscript (spec, saturation=datamax)
+		if (response != "")
+		    imarith (specec, "/", response, specec)
+	    }
+
+	    disperr = no
+	    if (disp) {
+		# Fix arc headers if necessary.
+		if (newarcs) {
+	    	    sections (arcs, option="fullname", >temp2)
+		    setjd ("@"//temp2, observatory=observatory, date="date-obs",
+			time="ut", exposure="exptime", jd="jd", hjd="",
+			ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+			>> log1)
+	    	    setairmass ("@"//temp2, intype="beginning",
+			outtype="effective", exposure="exptime",
+			observatory=observatory, show=no, update=yes,
+			override=yes, >> log1)
+		    delete (temp2, verify=no)
+		    hselect (arcs, "$I", yes, >temp2)
+	    	    fd2 = temp2
+	    	    while (fscan (fd2, arc) != EOF) {
+	        	i = strlen (arc)
+	        	if (i > n && substr (arc, i-n+1, i) == imtype)
+	            	    arc = substr (arc, 1, i-n)
+	        	hedit (arc, "refspec1", arc, add=yes, verify=no,
+		    	    show=no, update=yes)
+	        	hedit (arc, "arctype", "henear", add=yes, verify=no,
+		    	    show=no, update=yes)
+	    	    }
+	    	    fd2 = ""; delete (temp2, verify=no)
+		    newarcs = no
+		}
+
+		print ("Assign arc spectra for ", spec) | tee (log1)
+		refspectra (spec, references=arcrefs,
+		    apertures="", refaps="", ignoreaps=no,
+		    select=params.select, sort=params.sort,
+		    group=params.group, time=params.time,
+		    timewrap=params.timewrap, override=yes, confirm=no,
+		    assign=yes, logfiles="STDOUT", verbose=no) |
+		    tee (log1, > log2)
+
+		doarcs (spec, response, arcref, arcaps, arcbeams, reextract,
+		    arcap, log1, no)
+
+	        hselect (specec, "refspec1", yes, > temp2)
+	        fd2 = temp2
+	        i = fscan (fd2, arc)
+	        fd2 = ""; delete (temp2, verify=no)
+		if (i < 1) {
+		    print ("No arc reference assigned for ", spec) | tee (log1)
+		    disperr = yes
+		} else {
+	            print ("Dispersion correct ", spec) | tee (log1)
+		    dispcor (specec, "", linearize=params.linearize,
+			database=database, table=arcref//ectype,
+			w1=INDEF, w2=INDEF, dw=INDEF, nw=INDEF,
+			log=params.log, samedisp=no, flux=params.flux,
+			global=no, ignoreaps=no, confirm=no, listonly=no,
+			verbose=verbose, logfile=logfile)
+		    hedit (specec, "dc-flag", 0, add=yes, verify=no,
+			show=no, update=yes)
+		}
+	    }
+
+	    if (!disperr && (extract || disp)) {
+		if (splot1) {
+		    print (specec, ":")
+		    str1 = anssplot
+		    if (str1 == "NO" || str1 == "YES")
+			splot1 = no
+		    if (str1 == "no" || str1 == "NO")
+			splot2 = no
+		    else
+			splot2 = yes
+		}
+		if (splot2)
+		    splot (specec)
+	    }
+
+	    print (spec, >> done)
+	}
+	fd1 = ""; delete (temp1, verify=no)
+
+	if (access (done))
+	    delete (done, verify=no)
+end
diff --git a/noao/imred/src/dofoe/proc.par b/noao/imred/src/dofoe/proc.par
new file mode 100644
index 00000000..f74d6651
--- /dev/null
+++ b/noao/imred/src/dofoe/proc.par
@@ -0,0 +1,36 @@
+objects,s,a,,,,"List of object spectra"
+apref,f,a,"",,,"Aperture reference spectrum"
+flat,f,a,"",,,"Flat field spectrum"
+arcs,s,a,,,,"List of arc spectra"
+arctable,f,a,"",,,"Arc assignment table (optional)
+"
+naps,i,a,,,,"Number of apertures"
+objaps,s,a,,,,"Object apertures"
+arcaps,s,a,,,,"Arc apertures"
+objbeams,s,a,,,,"Object beam numbers"
+arcbeams,s,a,,,,"Arc beam numbers
+"
+fitflat,b,a,,,,"Fit and ratio flat field spectrum?"
+recenter,b,a,,,,"Recenter object apertures?"
+scattered,b,a,,,,"Subtract scattered light?"
+edit,b,a,,,,"Edit/review object apertures?"
+trace,b,a,,,,"Trace object spectra?"
+arcap,b,a,,,,"Use object apertures for arcs?"
+clean,b,a,,,,"Detect and replace bad pixels?"
+dispcor,b,a,,,,"Dispersion correct spectra?"
+splot,b,a,,,,"Plot the final spectrum?"
+redo,b,a,,,,"Redo operations if previously done?"
+update,b,a,,,,"Update spectra if cal data changes?"
+batch,b,a,,,,"Extract objects in batch?"
+listonly,b,a,,,,"List steps but don\'t process?
+"
+datamax,r,h,INDEF,,,"Max data value / cosmic ray threshold"
+newaps,b,h,,,,
+newresp,b,h,,,,
+newdisp,b,h,,,,
+newarcs,b,h,,,,
+dobatch,b,h,,,,
+anssplot,s,q,"yes",no|yes|NO|YES,,"Splot spectrum?"
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/dofoe/response.cl b/noao/imred/src/dofoe/response.cl
new file mode 100644
index 00000000..a59c5ea3
--- /dev/null
+++ b/noao/imred/src/dofoe/response.cl
@@ -0,0 +1,99 @@
+# RESPONSE -- Make a fiber response spectrum using a flat field and sky flat.
+
+procedure response (flat, apreference, response)
+
+string	flat			{prompt="Flat field spectrum"}
+string	apreference		{prompt="Aperture reference spectrum"}
+string	response		{prompt="Response spectrum"}
+
+bool	recenter = no		{prompt="Recenter sky apertures?"}
+bool	edit = no		{prompt="Edit/review sky apertures?"}
+bool	trace = no		{prompt="Trace sky spectra?"}
+bool	clean = no		{prompt="Detect and replace bad pixels?"}
+bool	fitflat = no		{prompt="Fit and ratio flat field spectrum?"}
+bool	interactive = yes	{prompt="Fit flat field interactively?"}
+string	function = "spline3"	{prompt="Fitting function",
+				 enum="spline3|legendre|chebyshev|spline1"}
+int	order = 20		{prompt="Fitting function order", min=1}
+
+begin
+	string	imtype
+	file	log1, log2, flat2d, flatec, resp
+	int	i, n
+	struct	err
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	n = strlen (imtype)
+
+	flat2d = flat
+	resp = response
+
+	if (flat2d == "")
+	    error (1, "No flat field defined")
+	if (flat2d != "") {
+	    i = strlen (flat2d)
+	    if (i > n && substr (flat2d, i-n+1, i) == imtype)
+		flat2d = substr (flat2d, 1, i-n)
+	    flatec = flat2d // ".ec"
+	    if (!access (flat2d // imtype)) {
+		printf ("Flat field spectrum not found - %s%s\n",
+		    flat2d, imtype) | scan (err)
+		error (1, err // "\nCheck setting of imtype")
+	    }
+	}
+
+	tee.append = yes
+	if (logfile == "")
+	    log1 = "dev$null"
+	else
+	    log1 = logfile
+	if (verbose)
+	    log2 = "STDOUT"
+	else
+	    log2 = "dev$null"
+
+	# Initialize APALL
+	apscript.references = apreference
+	if (recenter)
+	    apscript.ansrecenter = "YES"
+	else
+	    apscript.ansrecenter = "NO"
+	apscript.ansresize = "NO"
+	if (edit)
+	    apscript.ansedit = "yes"
+	else
+	    apscript.ansedit = "NO"
+	if (trace)
+	    apscript.anstrace = "YES"
+	else
+	    apscript.anstrace = "NO"
+	apscript.ansextract = "YES"
+
+	print ("Extract flat field ", flat2d) | tee (log1)
+	if (flat2d == apscript.references)
+	    apscript (flat2d, ansrecenter="NO", ansedit="NO", anstrace="NO",
+		background="none", clean=clean, extras=no)
+	else
+	    apscript (flat2d, clean=clean, extras=no)
+
+	if (fitflat) {
+	    print ("Fit and ratio flat field ", flat2d) | tee (log1)
+	    fit1d (flatec, resp, "fit", axis=1, interactive=interactive,
+		sample="*", naverage=1, function=function, order=order,
+		low_reject=0., high_reject=0., niterate=1, grow=0.,
+		graphics="stdgraph")
+	    sarith (flatec, "/", resp, resp, w1=INDEF, w2=INDEF, apertures="",
+		bands="", beams="", apmodulus=0, reverse=no, ignoreaps=yes,
+		format="multispec", renumber=no, offset=0, clobber=yes,
+		merge=no, errval=0, verbose=no)
+	    imdelete (flatec, verify=no)
+	} else
+	    imrename (flatec, resp, verbose=no)
+
+	print ("Create the normalized response ", resp) | tee (log1)
+	bscale (resp, resp, bzero="0.", bscale="mean", section="",
+	    step=1, upper=INDEF, lower=INDEF, verbose=yes) | tee (log1, >log2)
+end
diff --git a/noao/imred/src/dofoe/response.par b/noao/imred/src/dofoe/response.par
new file mode 100644
index 00000000..2bff1f0f
--- /dev/null
+++ b/noao/imred/src/dofoe/response.par
@@ -0,0 +1,12 @@
+flat,s,a,,,,"Flat field spectrum"
+apreference,s,a,,,,"Aperture reference spectrum"
+response,s,a,,,,"Response spectrum"
+recenter,b,h,no,,,"Recenter sky apertures?"
+edit,b,h,no,,,"Edit/review sky apertures?"
+trace,b,h,no,,,"Trace sky spectra?"
+clean,b,h,no,,,"Detect and replace bad pixels?"
+fitflat,b,h,no,,,"Fit and ratio flat field spectrum?"
+interactive,b,h,yes,,,"Fit flat field interactively?"
+function,s,h,"spline3",spline3|legendre|chebyshev|spline1,,"Fitting function"
+order,i,h,20,1,,"Fitting function order"
+mode,s,h,"q",,,
diff --git a/noao/imred/src/doslit/Revisions b/noao/imred/src/doslit/Revisions
new file mode 100644
index 00000000..5e219369
--- /dev/null
+++ b/noao/imred/src/doslit/Revisions
@@ -0,0 +1,129 @@
+.help revisions Dec94 noao.imred.src.doslit
+.nf
+
+=======
+V2.12.3
+=======
+
+doslit$sbatch.cl
+doslit$sproc.cl
+    Error messages now hint to check imtype setting.
+	(4/15/05, Valdes)
+
+========
+V2.12.2b
+========
+
+=======
+V2.12.1
+=======
+
+doslit$sproc.cl
+doslit$sbatch.cl
+doslit$sarcrefs.cl
+doslit$sfluxcal.cl
+    Added a flpr after dispcor to workaround a bug with the FITS kernel
+    header caching.  (6/24/02, Valdes)
+
+=====
+V2.12
+=====
+
+doslit$sproc.cl
+    Modified code to eliminate goto.  This is for use with pyraf.
+    (11/21/00, Valdes)
+
+========
+V2.11.3a
+========
+
+doslit$sarcrefs.cl
+     The test for INDEF values on CRVAL/CDELT did not work correctly.
+     (9/24/99, Valdes)
+
+doslit$doslit.cl
+doslit$doslit.par
+doslit$sarcrefs.cl
+doslit$sarcrefs.par
+doslit$sproc.cl
+doslit$sproc.par
+     No change made though dates were modified.  (9/24/99, Valdes)
+
+=======
+V2.11.2
+=======
+
+doslit$sarcrefs.cl
+    The test on CRVAL and CDELT would not work with header keywords.
+    (9/22/98, Valdes)
+
+doslit$sarcrefs.cl
+doslit$sbatch.cl
+doslit$sdoarcs.cl
+doslit$sfluxcal.cl
+doslit$sgetspec.cl
+doslit$slistonly.cl
+doslit$sproc.cl
+    Any additional qualifiers in the imtype string are stripped.
+    (8/14/97, Valdes)
+
+doslit$sgetspec.cl
+    Added the field parameter to the RENAME call.  (8/12/97, Valdes)
+
+=========
+V2.11Beta
+=========
+
+doslit$sarcrefs.cl
+    If both crval and cdelt are INDEF then the autoidentify option is not
+    used.  (5/2/97, Valdes)
+
+doslit$apslitproc.par
+    Made changes for the new aperture selection option.  (9/5/96, Valdes)
+
+doslit.cl
+doslit.par
+sproc.cl
+sproc.par
+sarcrefs.cl
+sarcrefs.par
+sparams.par
+    Modified to use autoidentify.  (4/5/96, Valdes)
+
+doslit$sproc.cl
+doslit$sproc.par
+    Added missing parameter declaration.  (5/25/95, Valdes)
+
+doslit$sgetspec.cl
+doslit$doslit.cl
+    The arc table will now be checked for arc spectra. (5/1/95, Valdes)
+
+doslit$sparams.par
+doslit$sdoarcs.cl
+doslit$sarcrefs.cl
+    Added "threshold" as a user parameter.  (1/16/95, Valdes)
+
+doslit$sproc.cl
+doslit$sbatch.cl
+doslit$sfluxcal.cl
+doslit$sproc.par
+doslit$sbatch.par
+doslit$sfluxcal.par
+    SETAIRMASS and SETJD are only called if the required keywords are
+    present.  Errors from missing airmass or JD are then reported from
+    the task that actually uses them.  (12/31/94, Valdes)
+
+doslit$sgetspec.cl
+doslit$sgetspec.par
+    Added warning and query for missing CCDPROC keyword.  (12/31/94, Valdes)
+
+doslit$sproc.cl
+doslit$sarcrefs.cl
+    1.	If the object apertures used for reference arc contain more than
+	one aperture then after extraction all apertures but the first
+	are removed.  This will be one reference arc aperture for the
+	master dispersion solution.
+    2.  Set ignoreaps=yes so that any new apertures added to the objects
+	will inherit the wavelength scale of the reference arc.
+    (10/12/94, Valdes)
+.endhelp
diff --git a/noao/imred/src/doslit/apslitproc.par b/noao/imred/src/doslit/apslitproc.par
new file mode 100644
index 00000000..bab5b58e
--- /dev/null
+++ b/noao/imred/src/doslit/apslitproc.par
@@ -0,0 +1,145 @@
+# APSCRIPT
+
+input,s,a,,,,List of input images
+output,s,h,"",,,List of output spectra
+apertures,s,h,"",,,Apertures
+scatter,s,h,"",,,List of scattered light images (optional)
+references,s,h,"",,,List of aperture reference images
+profiles,s,h,"",,,"List of aperture profile images
+"
+interactive,b,h,yes,,,Run task interactively?
+find,b,h,yes,,,Find apertures?
+recenter,b,h,yes,,,Recenter apertures?
+resize,b,h,yes,,,Resize apertures?
+edit,b,h,yes,,,Edit apertures?
+trace,b,h,yes,,,Trace apertures?
+fittrace,b,h,yes,,,Fit the traced points interactively?
+extract,b,h,yes,,,Extract spectra?
+review,b,h,yes,,,Review extractions?
+subtract,b,h,yes,,,Subtract scattered light?
+smooth,b,h,yes,,,Smooth scattered light along the dispersion?
+fitscatter,b,h,yes,,,Fit scattered light interactively?
+fitsmooth,b,h,yes,,,"Smooth the scattered light interactively?
+"
+line,i,h,)sparams.line,,,>sparams.line
+nsum,i,h,)sparams.nsum,,,>sparams.nsum
+buffer,r,h,)sparams.buffer,,,">sparams.buffer
+
+# OUTPUT PARAMETERS
+"
+format,s,h,"multispec",,,Extracted spectra format
+extras,b,h,)sparams.extras,,,"Extract sky, sigma, etc.?"
+dbwrite,s,h,"YES",,,Write to database?
+initialize,b,h,no,,,Initialize answers?
+verbose,b,h,)_.verbose,,,"Verbose output?
+
+# DEFAULT APERTURE PARAMETERS
+"
+lower,r,h,)sparams.lower,,,>sparams.lower
+upper,r,h,)sparams.upper,,,>sparams.upper
+apidtable,s,h,"",,,"Aperture ID table (optional)
+
+# DEFAULT BACKGROUND PARAMETERS
+"
+b_function,s,h,)sparams.b_function,,,>sparams.b_function
+b_order,i,h,)sparams.b_order,,,>sparams.b_order
+b_sample,s,h,)sparams.b_sample,,,>sparams.b_sample
+b_naverage,i,h,)sparams.b_naverage,,,>sparams.b_naverage
+b_niterate,i,h,)sparams.b_niterate,,,>sparams.b_niterate
+b_low_reject,r,h,)sparams.b_low,,,>sparams.b_low
+b_high_reject,r,h,)sparams.b_high,,,>sparams.b_high
+b_grow,r,h,0.,0.,,"Background rejection growing radius
+
+# APERTURE CENTERING PARAMETERS
+"
+width,r,h,,,,Profile centering width
+radius,r,h,,,,Profile centering radius
+threshold,r,h,10.,0.,,"Detection threshold for profile centering
+
+# AUTOMATIC FINDING AND ORDERING PARAMETERS
+"
+nfind,i,h,1,,,Number of apertures to be found automatically
+minsep,r,h,1.,,,Minimum separation between spectra
+maxsep,r,h,100000.,,,Maximum separation between spectra
+order,s,h,"increasing",,,"Order of apertures
+
+# RECENTERING PARAMETERS
+"
+aprecenter,s,h,"",,,Apertures for recentering calculation
+npeaks,r,h,INDEF,,,Select brightest peaks
+shift,b,h,yes,,,"Use average shift instead of recentering?
+
+# RESIZING PARAMETERS
+"
+llimit,r,h,INDEF,,,Lower aperture limit relative to center
+ulimit,r,h,INDEF,,,Upper aperture limit relative to center
+ylevel,r,h,)sparams.ylevel,,,>sparams.ylevel
+peak,b,h,yes,,,Is ylevel a fraction of the peak?
+bkg,b,h,yes,,,Subtract background in automatic width?
+r_grow,r,h,0.,,,Grow limits by this factor
+avglimits,b,h,no,,,"Average limits over all apertures?
+
+# EDITING PARAMETERS
+"
+e_output,s,q,,,,Output spectra rootname
+e_profiles,s,q,,,,"Profile reference image
+
+# TRACING PARAMETERS
+"
+t_nsum,i,h,)sparams.nsum,,,>sparams.nsum
+t_step,i,h,)sparams.t_step,,,>sparams.t_step
+t_nlost,i,h,3,1,,Number of consecutive times profile is lost before quitting
+t_width,r,h,)sparams.width,,,>sparams.width
+t_function,s,h,)sparams.t_function,,,>sparams.t_function
+t_sample,s,h,"*",,,Trace sample regions
+t_order,i,h,)sparams.t_order,,,>sparams.t_order
+t_naverage,i,h,1,,,Trace average or median
+t_niterate,i,h,)sparams.t_niterate,,,>sparams.t_niterate
+t_low_reject,r,h,)sparams.t_low,,,>sparams.t_low
+t_high_reject,r,h,)sparams.t_high,,,>sparams.t_high
+t_grow,r,h,0.,0.,,"Trace rejection growing radius
+
+# EXTRACTION PARAMETERS
+"
+background,s,h,)sparams.background,,,>sparams.background
+skybox,i,h,1,,,Box car smoothing length for sky
+weights,s,h,)sparams.weights,,,>sparams.weights
+pfit,s,h,)sparams.pfit,,,>sparams.pfit
+clean,b,h,no,,,Detect and replace bad pixels?
+nclean,r,h,0.5,,,Maximum number of pixels to clean
+niterate,i,h,5,0,,Number of profile fitting iterations
+saturation,r,h,INDEF,,,Saturation level
+readnoise,s,h,,,,Read out noise sigma (photons)
+gain,s,h,,,,Photon gain (photons/data number)
+lsigma,r,h,)sparams.lsigma,,,>sparams.lsigma
+usigma,r,h,)sparams.usigma,,,>sparams.usigma
+polysep,r,h,0.95,0.1,0.95,Marsh algorithm polynomial spacing
+polyorder,i,h,10,1,,Marsh algorithm polynomial order
+nsubaps,i,h,1,1,,"Number of subapertures per aperture
+
+# ANSWER PARAMETERS
+"
+ansclobber,s,h,"NO",,," "
+ansclobber1,s,h,"NO",,," "
+ansdbwrite,s,h,"YES",,," "
+ansdbwrite1,s,h,"NO",,," "
+ansedit,s,h,"NO",,," "
+ansextract,s,h,"NO",,," "
+ansfind,s,h,"NO",,," "
+ansfit,s,h,"NO",,," "
+ansfitscatter,s,h,"NO",,," "
+ansfitsmooth,s,h,"NO",,," "
+ansfitspec,s,h,"NO",,," "
+ansfitspec1,s,h,"NO",,," "
+ansfittrace,s,h,"NO",,," "
+ansfittrace1,s,h,"NO",,," "
+ansflat,s,h,"NO",,," "
+ansnorm,s,h,"NO",,," "
+ansrecenter,s,h,"NO",,," "
+ansresize,s,h,"NO",,," "
+ansreview,s,h,"NO",,," "
+ansreview1,s,h,"NO",,," "
+ansscat,s,h,"NO",,," "
+ansskyextract,s,h,"NO",,," "
+anssmooth,s,h,"NO",,," "
+anstrace,s,h,"NO",,," "
diff --git a/noao/imred/src/doslit/demologfile b/noao/imred/src/doslit/demologfile
new file mode 100644
index 00000000..a5a245c2
--- /dev/null
+++ b/noao/imred/src/doslit/demologfile
@@ -0,0 +1 @@
+Define object apertures
diff --git a/noao/imred/src/doslit/doslit.cl b/noao/imred/src/doslit/doslit.cl
new file mode 100644
index 00000000..56458435
--- /dev/null
+++ b/noao/imred/src/doslit/doslit.cl
@@ -0,0 +1,64 @@
+# DOSLIT -- Process slit spectra from 2D to wavelength calibrated 1D.
+#
+# The task SPROC does all of the interactive work and SBATCH does the
+# background work.  This procedure is organized this way to minimize the
+# dictionary space when the background task is submitted.
+
+procedure doslit (objects)
+
+string	objects = ""		{prompt="List of object spectra"}
+
+string	arcs = ""		{prompt="List of arc spectra"}
+file	arctable		{prompt="Arc assignment table (optional)"}
+string	standards = ""		{prompt="List of standard star spectra\n"}
+
+string	readnoise = "rdnoise"	{prompt="Read out noise sigma (photons)"}
+string	gain = "gain"		{prompt="Photon gain (photons/data number)"}
+real	datamax = INDEF		{prompt="Max data value / cosmic ray threshold"}
+real	width = 5.		{prompt="Width of profiles (pixels)"}
+string	crval = "INDEF"		{prompt="Approximate wavelength"}
+string	cdelt = "INDEF"		{prompt="Approximate dispersion\n"}
+
+bool	dispcor = yes		{prompt="Dispersion correct spectra?"}
+bool	extcor = no		{prompt="Extinction correct spectra?"}
+bool	fluxcal = no		{prompt="Flux calibrate spectra?"}
+bool	resize = no		{prompt="Automatically resize apertures?"}
+bool	clean = no		{prompt="Detect and replace bad pixels?"}
+bool	splot = no		{prompt="Plot the final spectrum?"}
+bool	redo = no		{prompt="Redo operations if previously done?"}
+bool	update = no		{prompt="Update spectra if cal data changes?"}
+bool	quicklook = no		{prompt="Minimally interactive quick-look?"}
+bool	batch = no		{prompt="Extract objects in batch?"}
+bool	listonly = no		{prompt="List steps but don't process?\n"}
+
+pset	sparams = ""		{prompt="Algorithm parameters"}
+
+begin
+	file	obj, arc, std
+
+	# Expand image lists
+	obj = mktemp ("tmp$iraf") 
+	arc = mktemp ("tmp$iraf")
+	std = mktemp ("tmp$iraf")
+	sgetspec (objects, arcs, arctable, standards, obj, arc, std)
+
+	apslitproc.readnoise = readnoise
+	apslitproc.gain = gain
+	apslitproc.width = width
+	apslitproc.t_width = width
+	apslitproc.radius = width
+	apslitproc.clean = clean
+	sproc.datamax = datamax
+
+	sproc (obj, arc, arctable, std, crval, cdelt, dispcor, extcor, fluxcal,
+	    resize, clean, splot, redo, update, quicklook, batch, listonly)
+	delete (std, verify=no)
+
+	if (sproc.dobatch) {
+	    print ("-- Do remaining spectra as a batch job --")
+	    print ("sbatch&batch") | cl
+	} else {
+	    delete (obj, verify=no)
+	    delete (arc, verify=no)
+	}
+end
diff --git a/noao/imred/src/doslit/doslit.par b/noao/imred/src/doslit/doslit.par
new file mode 100644
index 00000000..6e4119f6
--- /dev/null
+++ b/noao/imred/src/doslit/doslit.par
@@ -0,0 +1,26 @@
+objects,s,a,"",,,"List of object spectra"
+arcs,s,h,"",,,"List of arc spectra"
+arctable,f,h,"",,,"Arc assignment table (optional)"
+standards,s,h,"",,,"List of standard star spectra
+"
+readnoise,s,h,"rdnoise",,,"Read out noise sigma (photons)"
+gain,s,h,"gain",,,"Photon gain (photons/data number)"
+datamax,r,h,INDEF,,,"Max data value / cosmic ray threshold"
+width,r,h,5.,,,"Width of profiles (pixels)"
+crval,s,h,"INDEF",,,"Approximate wavelength"
+cdelt,s,h,"INDEF",,,"Approximate dispersion
+"
+dispcor,b,h,yes,,,"Dispersion correct spectra?"
+extcor,b,h,no,,,"Extinction correct spectra?"
+fluxcal,b,h,no,,,"Flux calibrate spectra?"
+resize,b,h,no,,,"Automatically resize apertures?"
+clean,b,h,no,,,"Detect and replace bad pixels?"
+splot,b,h,no,,,"Plot the final spectrum?"
+redo,b,h,no,,,"Redo operations if previously done?"
+update,b,h,no,,,"Update spectra if cal data changes?"
+quicklook,b,h,no,,,"Minimally interactive quick-look?"
+batch,b,h,no,,,"Extract objects in batch?"
+listonly,b,h,no,,,"List steps but don\'t process?
+"
+sparams,pset,h,"",,,"Algorithm parameters"
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/doslit/doslittasks.cl b/noao/imred/src/doslit/doslittasks.cl
new file mode 100644
index 00000000..a7b635a9
--- /dev/null
+++ b/noao/imred/src/doslit/doslittasks.cl
@@ -0,0 +1,17 @@
+#{ SLITPROC tasks
+
+task	doslit		= "doslit$doslit.cl"
+task	sproc		= "doslit$sproc.cl"
+task	sarcrefs	= "doslit$sarcrefs.cl"
+task	sdoarcs		= "doslit$sdoarcs.cl"
+task	sfluxcal	= "doslit$sfluxcal.cl"
+task	sbatch		= "doslit$sbatch.cl"
+task	slistonly	= "doslit$slistonly.cl"
+task	sgetspec	= "doslit$sgetspec.cl"
+
+task	apslitproc	= "doslit$x_apextract.e"
+
+hidetask sproc, sbatch, sarcrefs, sdoarcs, sfluxcal, slistonly, sgetspec
+hidetask apslitproc
+
+keep
diff --git a/noao/imred/src/doslit/sarcrefs.cl b/noao/imred/src/doslit/sarcrefs.cl
new file mode 100644
index 00000000..304983f1
--- /dev/null
+++ b/noao/imred/src/doslit/sarcrefs.cl
@@ -0,0 +1,118 @@
+# SARCREFS -- Determine dispersion relation for reference arcs.
+
+procedure sarcrefs (arcref1, crval, cdelt, done, log1, log2)
+
+file	arcref1
+string	crval = "INDEF"
+string	cdelt = "INDEF"
+file	done
+file	log1
+file	log2
+bool	newdisp = no
+
+struct	*fd
+
+begin
+	string	arcref, arcrefms, arc, arcms, temp, str1, str2
+	int	i, dc, nspec
+	bool	log
+	struct	str3
+
+	temp = mktemp ("tmp$iraf")
+
+	# Extract the primary arc reference spectrum.  Determine the
+	# dispersion function with IDENTIFY/REIDENTIFY.  Set the wavelength
+	# parameters with MSDISPCOR.
+
+	newdisp = no
+	arcref = arcref1
+	arcrefms = arcref1 // ".ms." // envget ("imtype")
+	i = stridx (",", arcrefms)
+	if (i > 0)
+	    arcrefms = substr (arcrefms, 1, i-1)
+	if (!access (arcrefms)) {
+	    print ("Extract arc reference image ", arcref) | tee (log1)
+	    if (apslitproc.reference == "") {
+		delete (database//"/ap"//arcref, verify=no, >& "dev$null")
+		apslitproc (arcref, nfind=-1, ansfind="YES",
+		    background="none", clean=no, weights="none")
+	    } else
+		apslitproc (arcref, background="none", clean=no, weights="none")
+
+	    nspec = 1
+	    hselect (arcrefms, "naxis2", yes) | scan (nspec)
+	    if (nspec > 1)
+		scopy (arcrefms//"[*,1]", arcrefms, w1=INDEF, w2=INDEF,
+		    apertures="", bands="", beams="", apmodulus=0,
+		    format="multispec", renumber=no, offset=0, clobber=yes,
+		    merge=no, rebin=yes, verbose=no)
+	}
+		    
+	# Check for dispersion correction.  If missing determine the
+	# dispersion function and dispersion correct.  Dispersion
+	# correction is required to define the dispersion parameters
+	# for the objects.
+
+	hselect (arcrefms, "dispcor", yes, > temp)
+	fd = temp
+	dc = -1
+	i = fscan (fd, dc)
+	fd = ""; delete (temp, verify=no)
+	if (i < 1 || dc == -1) {
+	    print ("Determine dispersion solution for ", arcref) | tee (log1)
+	    #delete (database//"/id"//arcref//".ms*", verify=no)
+	    printf ("%s %s\n", crval, cdelt) | scan (str3)
+	    if (str3 == "INDEF INDEF")
+		identify (arcrefms, section="middle line", database=database,
+		    coordlist=sparams.coordlist, nsum=1, match=sparams.match,
+		    maxfeatures=50, zwidth=100., ftype="emission",
+		    fwidth=sparams.fwidth, cradius=sparams.cradius,
+		    threshold=sparams.threshold, minsep=2.,
+		    function=sparams.i_function, order=sparams.i_order,
+		    sample="*", niterate=sparams.i_niterate,
+		    low_reject=sparams.i_low, high_reject=sparams.i_high,
+		    grow=0., autowrite=yes)
+	    else
+		autoidentify (arcrefms, crval, cdelt,
+		    coordlist=sparams.coordlist,
+		    interactive="YES", section="middle line", nsum="1",
+		    ftype="emission", fwidth=sparams.fwidth,
+		    cradius=sparams.cradius, threshold=sparams.threshold,
+		    minsep=2., match=sparams.match, function=sparams.i_function,
+		    order=sparams.i_order, sample="*",
+		    niterate=sparams.i_niterate, low_reject=sparams.i_low,
+		    high_reject=sparams.i_high, grow=0., dbwrite="YES",
+		    overwrite=yes, database="database", verbose=yes,
+		    logfile=logfile, plotfile=plotfile,
+		    reflist="", refspec="", crpix="INDEF", cddir="unknown",
+		    crsearch="-0.5", cdsearch="INDEF", aidpars="")
+
+	    hedit (arcrefms, "refspec1", arcref // ".ms", add=yes,
+		show=no, verify=no)
+
+	    dispcor (arcrefms, "", linearize=sparams.linearize,
+		database=database, table="", w1=INDEF, w2=INDEF, dw=INDEF,
+		nw=INDEF, log=sparams.log, flux=sparams.flux, samedisp=yes,
+		global=no, ignoreaps=yes, confirm=yes, verbose=no, listonly=no,
+		logfile=logfile)
+	    flpr
+
+	    hedit (arcrefms, "dispcor", 0, add=yes, verify=no,
+		show=no, update=yes)
+	    newdisp = yes
+
+#	    if (sproc.splot1) {
+#	        print (arcrefms, ":")
+#	        str1 = sproc.anssplot
+#	        if (str1 == "NO" || str1 == "YES")
+#		    sproc.splot1 = no
+#	        if (str1 == "no" || str1 == "NO")
+#		    sproc.splot2 = no
+#	        else
+#		    sproc.splot2 = yes
+#	    }
+#	    if (sproc.splot2)
+#		splot (arcrefms)
+	}
+	print (arcref, >> done)
+end
diff --git a/noao/imred/src/doslit/sarcrefs.par b/noao/imred/src/doslit/sarcrefs.par
new file mode 100644
index 00000000..012dcaf7
--- /dev/null
+++ b/noao/imred/src/doslit/sarcrefs.par
@@ -0,0 +1,9 @@
+arcref1,f,a,"",,,
+crval,s,a,"INDEF",,,
+cdelt,s,a,"INDEF",,,
+done,f,a,"",,,
+log1,f,a,"",,,
+log2,f,a,"",,,
+newdisp,b,h,no,,,
+fd,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/doslit/sbatch.cl b/noao/imred/src/doslit/sbatch.cl
new file mode 100644
index 00000000..8e01b09e
--- /dev/null
+++ b/noao/imred/src/doslit/sbatch.cl
@@ -0,0 +1,199 @@
+# SBATCH -- Process spectra in batch.
+# This task is called in batch mode.  It only processes objects
+# not previously processed unless the update or redo flags are set.
+
+procedure sbatch ()
+
+file	objects		{prompt="List of object spectra"}
+real	datamax 	{prompt="Max data value / cosmic ray threshold"}
+file	arcs1		{prompt="List of arc spectra"}
+file	arcref1		{prompt="Arc reference for dispersion solution"}
+string	arcrefs		{prompt="Arc references\n"}
+
+file	done		{prompt="File of spectra already done"}
+file	logfile		{prompt="Logfile"}
+
+bool	redo		{prompt="Redo operations?"}
+bool	update		{prompt="Update spectra?"}
+bool	dispcor		{prompt="Dispersion correct spectra?"}
+bool	extcor		{prompt="Extinction correct spectra?"}
+bool	fluxcal1	{prompt="Flux calibrate spectra?"}
+
+bool	newdisp, newsens, newarcs
+
+struct	*fd1, *fd2, *fd3
+
+begin
+	file	temp, spec, specms, arc, arcms
+	bool	reextract, extract, disp, ext, flux, log
+	string	imtype, mstype, str1, str2, str3, str4
+	int	i
+	struct	err
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	mstype = ".ms" // imtype
+	temp = mktemp ("tmp$iraf")
+
+	reextract = redo || (update && newdisp)
+
+	fd1 = objects
+	while (fscan (fd1, spec) != EOF) {
+	    if (access (done)) {
+	        fd2 = done
+	        while (fscan (fd2, specms) != EOF)
+		    if (spec == specms)
+		        break
+	        if (spec == specms)
+		    next
+	        fd2 = ""
+	    }
+	    if (!access (spec // imtype)) {
+		printf ("Object spectrum not found - %s%s\n",
+		    spec, imtype) | scan (err)
+		print (err, >> logfile)
+		print ("Check setting of imtype", >> logfile)
+		next
+	    }
+	    specms = spec // mstype
+
+	    extract = no
+	    disp = no
+	    ext = no
+	    flux = no
+	    if (reextract || !access (specms))
+		extract = yes
+	    else {
+		hselect (specms, "dispcor", yes, > temp)
+		hselect (specms, "ex-flag", yes, >> temp)
+		hselect (specms, "ca-flag", yes, >> temp)
+		fd2 = temp
+		if (fscan (fd2, str1) == 1) {
+		    extract = update && newdisp
+		    if (update && !newdisp)
+		        # We really should check if REFSPEC will assign
+			# different reference spectra.
+			;
+		} else
+		    disp = dispcor
+		if (fscan (fd2, str1) == 1)
+		    extract = update && !extcor
+		else
+		    ext = extcor
+		if (fscan (fd2, str1) == 1)
+		    extract = update && (!fluxcal1 || newsens)
+		else
+		    flux = fluxcal1
+		fd2 = ""; delete (temp, verify=no)
+	    }
+		
+	    if (extract) {
+		disp = dispcor
+		ext = extcor
+		flux = fluxcal1
+	    }
+
+	    if (extract) {
+		if (access (specms))
+		    imdelete (specms, verify=no)
+		print ("Extract object spectrum ", spec, >> logfile)
+		hselect (spec, "date-obs,ut,exptime", yes, > temp)
+		hselect (spec, "ra,dec,epoch,st", yes, >> temp)
+		fd2 = temp
+		if (fscan (fd2, str1, str2, str3) == 3) {
+		    setjd (spec, observatory=observatory, date="date-obs",
+			time="ut", exposure="exptime", jd="jd", hjd="",
+			ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+			>> logfile)
+		    if (fscan (fd2, str1, str2, str3, str4) == 4)
+			setairmass (spec, intype="beginning",
+			    outtype="effective", exposure="exptime",
+			    observatory=observatory, show=no, update=yes,
+			    override=yes, >> logfile)
+		}
+		fd2 = ""; delete (temp, verify=no)
+		apslitproc (spec, saturation=datamax, verbose=no)
+	    }
+
+	    if (disp) {
+		# Fix arc headers if necessary.
+		if (newarcs) {
+	    	    fd2 = arcs1
+	    	    while (fscan (fd2, arc) != EOF) {
+			hselect (arc, "date-obs,ut,exptime", yes, > temp)
+			hselect (arc, "ra,dec,epoch,st", yes, >> temp)
+			fd3 = temp
+			if (fscan (fd3, str1, str2, str3) == 3) {
+			    setjd (arc, observatory=observatory,
+				date="date-obs", time="ut", exposure="exptime",
+				jd="jd", hjd="", ljd="ljd", utdate=yes,
+				uttime=yes, listonly=no, >> logfile)
+			    if (fscan (fd3, str1, str2, str3, str4) == 4)
+				setairmass (arc, intype="beginning",
+				    outtype="effective", exposure="exptime",
+				    observatory=observatory, show=no,
+				    update=yes, override=yes, >> logfile)
+			}
+			fd3 = ""; delete (temp, verify=no)
+	        	hedit (arc, "refspec1", arc, add=yes, verify=no,
+		    	    show=no, update=yes)
+		    }
+	    	    fd2 = ""
+		    newarcs = no
+		}
+
+		print ("Assign arc spectra for ", spec, >> logfile)
+		refspectra (spec, references=arcrefs,
+		    apertures="", refaps="", ignoreaps=no,
+		    select=sparams.select, sort=sparams.sort,
+		    group=sparams.group, time=sparams.time,
+		    timewrap=sparams.timewrap, override=yes, confirm=no,
+		    assign=yes, logfiles="STDOUT", verbose=no,
+		    >> logfile)
+
+		sdoarcs (spec, arcref1, reextract, logfile, yes)
+
+	        hselect (specms, "refspec1", yes, > temp)
+	        fd2 = temp
+	        i = fscan (fd2, arc)
+	        fd2 = ""; delete (temp, verify=no)
+		if (i < 1)
+		    print ("No arc reference assigned for ", spec, >> logfile)
+		else {
+	            print ("Dispersion correct ", spec, >> logfile)
+		    dispcor (specms, "", linearize=sparams.linearize,
+			database=database, table=arcref1//mstype,
+			w1=INDEF, w2=INDEF, dw=INDEF, nw=INDEF,
+			log=sparams.log, flux=sparams.flux, samedisp=no,
+			global=no, ignoreaps=no, confirm=no, listonly=no,
+			verbose=no, logfile=logfile)
+		    flpr
+		    hedit (specms, "dispcor", 0, add=yes, verify=no,
+			show=no, update=yes)
+		    disp = no
+		}
+	    }
+
+	    if (!disp) {
+	        if (ext)
+		    print ("Extinction correct ", spec, >> logfile)
+	        if (flux)
+		    print ("Flux calibrate ", spec, >> logfile)
+	        if (flux || ext)
+		    calibrate (specms, "", extinct=extcor, flux=fluxcal1,
+			extinction=extinction, observatory=observatory,
+			ignoreaps=yes, sensitivity="sens", fnu=sparams.fnu,
+			>> logfile)
+	    }
+	}
+	fd1 = ""
+	delete (objects, verify=no)
+	delete (arcs1, verify=no)
+
+	if (access (done))
+	    delete (done, verify=no)
+
+	flprcache (0)
+end
diff --git a/noao/imred/src/doslit/sbatch.par b/noao/imred/src/doslit/sbatch.par
new file mode 100644
index 00000000..582bdf03
--- /dev/null
+++ b/noao/imred/src/doslit/sbatch.par
@@ -0,0 +1,20 @@
+objects,f,h,"",,,"List of object spectra"
+datamax,r,h,,,,"Max data value / cosmic ray threshold"
+arcs1,f,h,"",,,"List of arc spectra"
+arcref1,f,h,"",,,"Arc reference for dispersion solution"
+arcrefs,s,h,,,,"Arc references
+"
+done,f,h,"",,,"File of spectra already done"
+logfile,f,h,"",,,"Logfile"
+redo,b,h,,,,"Redo operations?"
+update,b,h,,,,"Update spectra?"
+dispcor,b,h,,,,"Dispersion correct spectra?"
+extcor,b,h,,,,"Extinction correct spectra?"
+fluxcal1,b,h,,,,"Flux calibrate spectra?"
+newdisp,b,h,,,,
+newsens,b,h,,,,
+newarcs,b,h,,,,
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+fd3,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/doslit/sdoarcs.cl b/noao/imred/src/doslit/sdoarcs.cl
new file mode 100644
index 00000000..19b8f3af
--- /dev/null
+++ b/noao/imred/src/doslit/sdoarcs.cl
@@ -0,0 +1,101 @@
+# SDOARCS -- Determine dispersion relation for spectrum based on refernece arcs.
+
+procedure sdoarcs (spec, arcref1, reextract, logfile, batch)
+
+file	spec
+file	arcref1
+bool	reextract
+file	logfile
+bool	batch
+
+struct	*fd
+
+begin
+	file	temp, arc1, arc2, str1
+	string	imtype, mstype, reid
+	bool	verbose1
+	int	i, n
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	mstype = ".ms" // imtype
+	n = strlen (imtype)
+
+	temp = mktemp ("tmp$iraf")
+
+	for (j=1; j<=2; j+=1) {
+
+	    # Setup interactive/batch parameters
+	    if (batch) {
+		verbose1 = no
+		reid = "no"
+	    } else {
+		verbose1 = verbose
+		reidentify.answer.p_mode = "h"
+		reid = reidentify.answer
+		reidentify.answer.p_mode = "q"
+		if (reid == "no")
+		    reid = "yes"
+	    }
+
+	    # The reference spectra refer initially to the 2D image.  At the
+	    # end we will reset them to refer to the 1D spectra.
+
+	    hselect (spec, "refspec"//j, yes, > temp)
+	    fd = temp
+	    i = fscan (fd, arc1, str1)
+	    fd = ""; delete (temp, verify=no)
+	    if (nscan() < 1)
+		break
+
+	    # Strip possible image extension.
+	    i = strlen (arc1)
+	    if (i > n && substr (arc1, i-n+1, i) == imtype)
+		arc1 = substr (arc1, 1, i-n)
+    
+	    # Set extraction output and aperture reference depending on whether
+	    # the arcs are to be rextracted using recentered or retraced object
+	    # apertures.
+
+	    arc2 = spec // arc1
+	    if (access (arc2//mstype))
+		imdelete (arc2//mstype, verify=no)
+	    delete (database//"/id"//arc2//".ms*", verify = no, >& "dev$null")
+    
+	    # Extract and determine dispersion function if necessary.
+	    if (!access (arc2//mstype)) {
+		if (!batch)
+		    print ("Extract and reidentify arc spectrum ", arc1)
+		print ("Extract and reidentify arc spectrum ", arc1, >> logfile)
+		apslitproc (arc1, output=arc2//".ms", references=spec,
+		    background="none", clean=no, weights="none",
+		    verbose=verbose1)
+		delete (database//"/id"//arc2//".ms*", verify = no,
+		    >& "dev$null")
+		reidentify (arcref1//".ms", arc2//".ms", interactive=reid,
+		    section="middle line", shift=0., step=1, nsum=1,
+		    cradius=sparams.cradius, threshold=sparams.threshold,
+		    nlost=100, refit=sparams.refit, trace=no, override=no,
+		    newaps=yes, addfeatures=sparams.addfeatures,
+		    coordlist=sparams.coordlist, match=sparams.match,
+		    maxfeatures=50, minsep=2., database=database,
+		    plotfile=plotfile, logfiles=logfile, verbose=verbose1)
+
+		# If not reextracting arcs based on object apertures
+		# then save the extracted arc to avoid doing it again.
+
+		if (arc1 != arc2)
+		    imdelete (arc2//".ms", verify=no)
+	    }
+    
+	    # Set the REFSPEC parameters for multispec spectrum.
+	    if (nscan() == 1)
+		hedit (spec//".ms", "refspec"//j, arc2//".ms", add=yes,
+		    verify=no, show=no, update=yes)
+	    else
+		hedit (spec//".ms", "refspec"//j, arc2//".ms "//str1,
+		    add=yes, verify=no, show=no, update=yes)
+	}
+end
diff --git a/noao/imred/src/doslit/sdoarcs.par b/noao/imred/src/doslit/sdoarcs.par
new file mode 100644
index 00000000..cea554c2
--- /dev/null
+++ b/noao/imred/src/doslit/sdoarcs.par
@@ -0,0 +1,7 @@
+spec,f,a,"",,,
+arcref1,f,a,"",,,
+reextract,b,a,,,,
+logfile,f,a,"",,,
+batch,b,a,,,,
+fd,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/doslit/sfluxcal.cl b/noao/imred/src/doslit/sfluxcal.cl
new file mode 100644
index 00000000..e9399ac3
--- /dev/null
+++ b/noao/imred/src/doslit/sfluxcal.cl
@@ -0,0 +1,196 @@
+# SFLUXCAL -- Extract standard stars and determine sensitivity function.
+# If flux calibrating, extract and dispersion correct the standard star
+# spectra.  Compile the standard star fluxes from the calibration
+# directory.  The user is queried for the star name but the band passes
+# are not allow to change interactively.  Next compute the sensitivity
+# function using SENSFUNC.  This is interactive.  Once the sensitivity
+# function images are created, flux and extinction calibrate the standard
+# stars.  This is done in such a way that if new standard stars are added
+# in a later execution only the new stars are added and then a new
+# sensitivity function is computed.  If the update flag is set all
+# spectra which are specified are reprocessed if they were previously
+# processed.  In a redo the "std" file is deleted, otherwise additions
+# are appended to this file.
+
+procedure sfluxcal (stds, arcs1, arcref1, arcrefs, redo, update, extcor,
+	done, log1, log2)
+
+file	stds
+file	arcs1
+file	arcref1
+string	arcrefs
+bool	redo
+bool	update
+bool	extcor
+file	done
+file	log1
+file	log2
+
+struct	*fd1, *fd2, *fd3
+
+begin
+	string	imtype, mstype
+	string	spec, specms, arc, str1, str2, str3, str4
+	file	temp1, temp2
+	int	i, j
+	bool	reextract, log
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	mstype = ".ms" // imtype
+
+	temp1 = mktemp ("tmp$iraf")
+	temp2 = mktemp ("tmp$iraf")
+
+	reextract = redo || (update && sproc.newdisp)
+	sproc.newsens = no
+
+	if (redo && access ("std"))
+	    delete ("std", verify=no)
+
+        fd1 = stds
+        while (fscan (fd1, spec) != EOF) {
+	    specms = spec // mstype
+
+	    if (reextract && access (specms))
+	        imdelete (specms, verify=no)
+            if (!access (specms)) {
+	        print ("Extract standard star spectrum ", spec) | tee (log1)
+		hselect (spec, "date-obs,ut,exptime", yes, > temp1)
+		hselect (spec, "ra,dec,epoch,st", yes, >> temp1)
+		fd2 = temp1
+		if (fscan (fd2, str1, str2, str3) == 3) {
+		    setjd (spec, observatory=observatory, date="date-obs",
+			time="ut", exposure="exptime", jd="jd", hjd="",
+			ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+			>> log1)
+		    if (fscan (fd2, str1, str2, str3, str4) == 4)
+			setairmass (spec, intype="beginning",
+			    outtype="effective", exposure="exptime",
+			    observatory=observatory, show=no, update=yes,
+			    override=yes, >> log1)
+		}
+		fd2 = ""; delete (temp1, verify=no)
+		apslitproc (spec)
+	    }
+
+	    hselect (specms, "dispcor,std-flag", yes, > temp1)
+	    fd2 = temp1
+	    j = fscan (fd2, str1, str2)
+	    fd2 = ""; delete (temp1, verify=no)
+	    if (j < 1) {
+		# Fix arc headers if necessary.
+		if (sproc.newarcs) {
+	    	    fd2 = arcs1
+	    	    while (fscan (fd2, arc) != EOF) {
+			hselect (arc, "date-obs,ut,exptime", yes, > temp1)
+			hselect (arc, "ra,dec,epoch,st", yes, >> temp1)
+			fd3 = temp1
+			if (fscan (fd3, str1, str2, str3) == 3) {
+			    setjd (arc, observatory=observatory,
+				date="date-obs", time="ut", exposure="exptime",
+				jd="jd", hjd="", ljd="ljd", utdate=yes,
+				uttime=yes, listonly=no, >> log1)
+			    if (fscan (fd3, str1, str2, str3, str4) == 4)
+				setairmass (arc, intype="beginning",
+				    outtype="effective", exposure="exptime",
+				    observatory=observatory, show=no,
+				    update=yes, override=yes, >> log1)
+			}
+			fd3 = ""; delete (temp1, verify=no)
+	        	hedit (arc, "refspec1", arc, add=yes, verify=no,
+		    	    show=no, update=yes)
+		    }
+	    	    fd2 = ""
+		    sproc.newarcs = no
+		}
+
+		print ("Assign arc spectra for ", spec) | tee (log1)
+		refspectra (spec, references=arcrefs,
+		    apertures="", refaps="", ignoreaps=no,
+		    select=sparams.select, sort=sparams.sort,
+		    group=sparams.group, time=sparams.time,
+		    timewrap=sparams.timewrap, override=yes, confirm=no,
+		    assign=yes, logfiles="STDOUT", verbose=no) |
+		    tee (log1, > log2)
+
+		sdoarcs (spec, arcref1, reextract, log1, no)
+
+	        hselect (specms, "refspec1", yes, > temp1)
+	        fd2 = temp1
+	        i = fscan (fd2, arc)
+	        fd2 = ""; delete (temp1, verify=no)
+		if (i < 1) {
+		    print ("No arc reference assigned for ", spec) | tee (log1)
+		    next
+		} else {
+	            print ("Dispersion correct ", spec) | tee (log1)
+		    dispcor (specms, "", linearize=sparams.linearize,
+			database=database, table=arcref1//mstype,
+			w1=INDEF, w2=INDEF, dw=INDEF, nw=INDEF,
+			log=sparams.log, flux=sparams.flux, samedisp=no,
+			global=no, ignoreaps=no, confirm=no, listonly=no,
+			logfile=logfile, > log2)
+		    flpr
+		    hedit (specms, "dispcor", 0, add=yes, verify=no,
+			show=no, update=yes)
+		}
+	    }
+
+	    if (j < 2 || !access ("std")) {
+                print ("Compile standard star fluxes for ", spec) | tee (log1)
+	        standard (specms, output="std", samestar=no, beam_switch=no,
+		    apertures="", bandwidth=INDEF, bandsep=INDEF,
+		    fnuzero=3.68E-20, extinction=extinction, caldir=caldir,
+		    observatory=observatory, interact=no)
+	        hedit (specms, "std-flag", "yes", add=yes, verify=no,
+		    show=no, update=yes)
+	        print (specms, >> temp2)
+	        sproc.newsens = yes
+            }
+        }
+        fd1 = ""
+
+	if (sproc.newsens || !access ("sens"//imtype)) {
+	    if (!access ("std")) {
+	        print ("No standard star data") | tee (log1)
+	        sproc.fluxcal1 = no
+	    } else {
+	        imdelete ("sens"//imtype, verify=no, >& "dev$null")
+                print ("Compute sensitivity function") | tee (log1)
+                sensfunc ("std", "sens", apertures="", ignoreaps=yes,
+		    logfile=logfile, extinction=extinction,
+		    newextinction="extinct.dat", observatory=observatory,
+		    function=sparams.s_function, order=sparams.s_order,
+		    interactive=yes, graphs="sr", marks="plus cross box")
+	        sproc.newsens = yes
+	    }
+        }
+
+        # Note that if new standard stars are added the old standard
+        # stars are not recalibrated unless the redo flag is used.
+
+        if (sproc.fluxcal1 && sproc.newsens && access (temp2)) {
+            print ("Flux and/or extinction calibrate standard stars") |
+	        tee (log1)
+	    calibrate ("@"//temp2, "", extinct=extcor, flux=sproc.fluxcal1,
+		extinction=extinction, observatory=observatory, ignoreaps=yes,
+		sensitivity="sens", fnu=sparams.fnu) | tee (log1, > log2)
+	    if (sproc.splot1) {
+	        print ("Standard stars:")
+	        str1 = sproc.anssplot
+	        if (str1 == "NO" || str1 == "YES")
+		    sproc.splot1 = no
+	        if (str1 == "no" || str1 == "NO")
+		    sproc.splot2 = no
+	        else
+		    sproc.splot2 = yes
+	    }
+	    if (sproc.splot2)
+		splot ("@"//temp2)
+	    sections (temp2, option="fullname", >> done)
+            delete (temp2, verify=no)
+        }
+end
diff --git a/noao/imred/src/doslit/sfluxcal.par b/noao/imred/src/doslit/sfluxcal.par
new file mode 100644
index 00000000..44474335
--- /dev/null
+++ b/noao/imred/src/doslit/sfluxcal.par
@@ -0,0 +1,14 @@
+stds,f,a,,,,
+arcs1,f,a,,,,
+arcref1,f,a,"",,,
+arcrefs,s,a,,,,
+redo,b,a,,,,
+update,b,a,,,,
+extcor,b,a,,,,
+done,f,a,"",,,
+log1,f,a,"",,,
+log2,f,a,"",,,
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+fd3,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/doslit/sgetspec.cl b/noao/imred/src/doslit/sgetspec.cl
new file mode 100644
index 00000000..1140e610
--- /dev/null
+++ b/noao/imred/src/doslit/sgetspec.cl
@@ -0,0 +1,178 @@
+# SGETSPEC -- Get spectra which are CCD processed and not extracted.
+# This task also recognizes the arc spectra in the object list and arc table.
+# This task also strips the image type extension.
+
+procedure sgetspec (objects, arcs, arctable, standards, obj, arc, std)
+
+string	objects			{prompt="List of object images"}
+string	arcs			{prompt="List of arc images"}
+file	arctable		{prompt="Arc table"}
+string	standards		{prompt="List of standard images"}
+file	obj			{prompt="File of object images"}
+file	arc			{prompt="File of arc images"}
+file	std			{prompt="File of standard images"}
+bool	ccdproc			{prompt="Add CCDPROC keyword and continue?",
+				 mode="q"}
+struct	*fd1, *fd2
+
+begin
+	string	imtype, temp, image, itype
+	int	n, n1, narcs
+
+	imtype = "." // envget ("imtype")
+	n = stridx (",", imtype)
+	if (n > 0)
+	    imtype = substr (imtype, 1, n-1)
+	n1 = strlen (imtype)
+
+	temp = mktemp ("tmp$iraf")
+
+	# Initialize files
+	set clobber=yes
+	sleep (> obj)
+	sleep (> arc)
+	sleep (> std)
+	set clobber=no
+
+	# Do arcs
+	itype = ""
+	narcs = 0
+	sections (arcs, option="fullname", > temp)
+	fd1 = temp
+	while (fscan (fd1, image) != EOF) {
+	    hselect (image, "ccdproc", yes) | scan (itype)
+	    if (nscan() == 0) {
+		printf ("%s: CCDPROC keyword not found.\n", image)
+		printf ("  Either run CCDPROC or add CCDPROC keyword with HEDIT.\n")
+		if (!ccdproc)
+		    error (1, "Exit")
+		hedit (image, "ccdproc", "DOSLIT", add=yes, update=yes,
+		    verify=no, show=no)
+	    }
+	    hselect (image, "wat0_001", yes) | scanf ("system=%s", itype)
+	    if (itype == "equispec" || itype == "multispec")
+		next
+	    hselect (image, "imagetyp", yes) | scan (itype)
+	    if (nscan() == 0)
+		itype = "comp"
+	    if (itype != "comp" && itype != "COMPARISON" &&
+		itype != "comparison" && itype != "COMP")
+		next
+	    n = strlen (image)
+	    if (n > n1 && substr (image, n-n1+1, n) == imtype)
+		image = substr (image, 1, n-n1)
+	    narcs = narcs + 1
+	    printf ("%s %02d\n", image, narcs, >> arc)
+	}
+	fd1 = ""; delete (temp, verify=no)
+
+	# Do arc table.
+	if (arctable != "") {
+	    fd2 = arctable
+	    while (fscan (fd2, image, image) != EOF) {
+		if (nscan() != 2)
+		    next
+		sections (image, option="fullname", > temp)
+		fd1 = temp
+		while (fscan (fd1, image) != EOF) {
+		    hselect (image, "ccdproc", yes) | scan (itype)
+		    if (nscan() == 0) {
+			printf ("%s: CCDPROC keyword not found.\n", image)
+			printf ("  Either run CCDPROC or add CCDPROC keyword with HEDIT.\n")
+			if (!ccdproc)
+			    error (1, "Exit")
+			hedit (image, "ccdproc", "DOSLIT", add=yes, update=yes,
+			    verify=no, show=no)
+		    }
+		    hselect (image, "wat0_001", yes) | scanf ("system=%s", itype)
+		    if (itype == "equispec" || itype == "multispec")
+			next
+		    hselect (image, "imagetyp", yes) | scan (itype)
+		    if (nscan() == 0)
+			itype = "comp"
+		    if (itype != "comp" && itype != "COMPARISON" &&
+			itype != "comparison" && itype != "COMP")
+			next
+		    n = strlen (image)
+		    if (n > n1 && substr (image, n-n1+1, n) == imtype)
+			image = substr (image, 1, n-n1)
+		    narcs = narcs + 1
+		    printf ("%s %02d\n", image, narcs, >> arc)
+		}
+		fd1 = ""; delete (temp, verify=no)
+	    }
+	}
+
+	# Do standards
+	sections (standards, option="fullname", > temp)
+	fd1 = temp
+	while (fscan (fd1, image) != EOF) {
+	    hselect (image, "ccdproc", yes) | scan (itype)
+	    if (nscan() == 0) {
+		printf ("%s: CCDPROC keyword not found.\n", image)
+		printf ("  Either run CCDPROC or add CCDPROC keyword with HEDIT.\n")
+		if (!ccdproc)
+		    error (1, "Exit")
+		hedit (image, "ccdproc", "DOSLIT", add=yes, update=yes,
+		    verify=no, show=no)
+	    }
+	    hselect (image, "wat0_001", yes) | scanf ("system=%s", itype)
+	    if (itype == "equispec" || itype == "multispec")
+		next
+	    n = strlen (image)
+	    if (n > n1 && substr (image, n-n1+1, n) == imtype)
+		image = substr (image, 1, n-n1)
+	    print (image, >> std)
+	}
+	fd1 = ""; delete (temp, verify=no)
+
+	# Do objects
+	sections (objects, option="fullname", > temp)
+	fd1 = temp
+	while (fscan (fd1, image) != EOF) {
+	    hselect (image, "ccdproc", yes) | scan (itype)
+	    if (nscan() == 0) {
+		printf ("%s: CCDPROC keyword not found.\n", image)
+		printf ("  Either run CCDPROC or add CCDPROC keyword with HEDIT.\n")
+		if (!ccdproc)
+		    error (1, "Exit")
+		hedit (image, "ccdproc", "DOSLIT", add=yes, update=yes,
+		    verify=no, show=no)
+	    }
+	    hselect (image, "wat0_001", yes) | scanf ("system=%s", itype)
+	    if (itype == "equispec" || itype == "multispec")
+		next
+	    hselect (image, "imagetyp", yes) | scan (itype)
+	    if (nscan() == 0)
+		itype = "object"
+
+	    n = strlen (image)
+	    if (n > n1 && substr (image, n-n1+1, n) == imtype)
+		image = substr (image, 1, n-n1)
+	    if (itype == "object" || itype == "OBJECT")
+		print (image, >> obj)
+	    else if (itype == "comp" || itype == "COMPARISON" ||
+		itype == "comparison" || itype == "COMP") {
+		narcs = narcs + 1
+		printf ("%s %02d\n", image, narcs, >> arc)
+	    }
+	}
+	fd1 = ""; delete (temp, verify=no)
+
+	if (narcs > 0) {
+	    sort (arc, column=0, ignore=yes, numeric=no, reverse=no, > temp)
+	    delete (arc, verify=no)
+	    rename (temp, arc, field="all")
+	    itype = ""
+	    fd1 = arc
+	    while (fscan (fd1, image, narcs) != EOF) {
+		if (image != itype)
+		    printf ("%s %02d\n", image, narcs, >> temp)
+		itype = image
+	    }
+	    delete (arc, verify=no)
+	    sort (temp, column=2, ignore=yes, numeric=yes, reverse=no) |
+	    fields ("STDIN", "1", lines="1-99", > arc)
+	    delete (temp, verify=no)
+	}
+end
diff --git a/noao/imred/src/doslit/sgetspec.par b/noao/imred/src/doslit/sgetspec.par
new file mode 100644
index 00000000..1f5387cc
--- /dev/null
+++ b/noao/imred/src/doslit/sgetspec.par
@@ -0,0 +1,11 @@
+objects,s,a,,,,"List of object images"
+arcs,s,a,,,,"List of arc images"
+arctable,f,a,"",,,"Arc table"
+standards,s,a,,,,"List of standard images"
+obj,f,a,"",,,"File of object images"
+arc,f,a,"",,,"File of arc images"
+std,f,a,"",,,"File of standard images"
+ccdproc,b,q,,,,"Add CCDPROC keyword and continue?"
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/doslit/slistonly.cl b/noao/imred/src/doslit/slistonly.cl
new file mode 100644
index 00000000..71ee3b40
--- /dev/null
+++ b/noao/imred/src/doslit/slistonly.cl
@@ -0,0 +1,180 @@
+# SLISTONLY -- List processing to be done.
+#
+# This follows pretty much the same logic as the full procedure but doesn't
+# do anything but list the operations.
+
+procedure slistonly (objects, arcs1, standards, dispcor, extcor, fluxcal,
+	redo, update)
+
+file	objects
+file	arcs1
+file	standards
+
+bool	dispcor
+bool	extcor
+bool	fluxcal
+bool	redo
+bool	update
+
+struct	*fd1
+struct	*fd2
+
+begin
+	string	imtype, mstype
+	string	spec, arcref1
+	string	specms, arcref1ms
+	string	temp, done, str1, str2
+	bool	reextract, fluxcal1, stdfile
+	bool	newdisp, newsens, extract, disp, ext, flux
+	int	i, dc, sf
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	mstype = ".ms" // imtype
+	temp = mktemp ("tmp$iraf")
+	done = mktemp ("tmp$iraf")
+
+	newdisp = no
+	newsens = no
+	fluxcal1 = fluxcal
+
+	print ("Check and set new object aperture definitions")
+
+	if (dispcor) {
+	    fd1 = arcs1
+	    if (fscan (fd1, arcref1) == EOF)
+		error (1, "No reference arcs")
+	    fd1 = ""
+	    arcref1ms = arcref1 // mstype
+
+	    if (redo || !access (arcref1ms)) {
+	        print ("Extract arc reference image ", arcref1)
+	        print ("Determine dispersion solution for ", arcref1)
+	        newdisp = yes
+	    } else {
+		hselect (arcref1ms, "dispcor", yes, > temp)
+	        fd1 = temp
+		dc = -1
+	        i = fscan (fd1, dc)
+	        fd1 = ""; delete (temp, verify=no)
+	        if (i < 1) {
+	            print ("Determine dispersion solution for ", arcref1)
+	            newdisp = yes
+	        }
+	    }
+	    print (arcref1, > done)
+
+	    if (fluxcal1) {
+		stdfile = access ("std")
+		if (redo && stdfile)
+		    stdfile = no
+
+	        reextract = redo || (update && newdisp)
+	        fd1 = standards
+	        while (fscan (fd1, spec) != EOF) {
+		    specms = spec // mstype
+	            if (reextract || !access (specms)) {
+		        print ("Extract standard star spectrum ", spec)
+	                print ("Dispersion correct ", spec)
+	                print ("Compile standard star fluxes for ", spec)
+		        stdfile = yes
+		        newsens = yes
+		    } else {
+		        hselect (specms, "dispcor,std-flag", yes, > temp)
+		        fd2 = temp
+			dc = -1
+			sf = -1
+		        i = fscan (fd2, dc, sf)
+		        fd2 = ""; delete (temp, verify=no)
+		        if (i < 1)
+		            print ("Dispersion correct ", spec)
+		        if (i < 2) {
+		            print ("Compile standard star fluxes for ", spec)
+		            stdfile = yes
+		            newsens = yes
+		        }
+	            }
+		    print (spec, >> done)
+	        }
+	        fd1 = ""
+
+	        sections ("sens.????" // imtype, option="nolist")
+	        if (newsens || sections.nimages == 0) {
+		    if (!stdfile) {
+		        print ("No standard stars")
+		        fluxcal1 = no
+		    } else {
+	                print ("Compute sensitivity function")
+		        newsens = yes
+		    }
+	        }
+
+	        if (fluxcal1 && newsens)
+	            print ("Flux and/or extinction calibrate standard stars")
+	    }
+	}
+
+	reextract = redo || (update && newdisp)
+	fd1 = objects
+	while (fscan (fd1, spec) != EOF) {
+	    if (access (done)) {
+	        fd2 = done
+	        while (fscan (fd2, specms) != EOF)
+		    if (spec == specms)
+		        break
+	        if (spec == specms)
+		    next
+	        fd2 = ""
+	    }
+
+	    specms = spec // mstype
+
+	    extract = no
+	    disp = no
+	    ext = no
+	    flux = no
+	    if (reextract || !access (specms))
+		extract = yes
+	    else {
+		hselect (specms, "dispcor", yes, > temp)
+		hselect (specms, "ex-flag", yes, >> temp)
+		hselect (specms, "ca-flag", yes, >> temp)
+		fd2 = temp
+		extract = update
+		if (fscan (fd2, str1) == 1)
+		    extract = update && newdisp
+		else
+		    disp = yes
+		if (fscan (fd2, str1) == 1)
+		    extract = update && !extcor
+		else
+		    ext = extcor
+		if (fscan (fd2, str1) == 1)
+		    extract = update && (!fluxcal1 || newsens)
+		else
+		    flux = fluxcal1
+		fd2 = ""; delete (temp, verify=no)
+	    }
+		
+	    if (extract) {
+		disp = dispcor
+		ext = extcor
+		flux = fluxcal1
+	    }
+		    
+	    if (extract)
+		print ("Extract object spectrum ", spec)
+	    if (disp)
+	        print ("Dispersion correct ", spec)
+	    if (ext)
+		print ("Extinction correct ", spec)
+	    if (flux)
+		print ("Flux calibrate ", spec)
+	}
+	fd1 = ""
+
+	if (access (done))
+	    delete (done, verify=no)
+end
diff --git a/noao/imred/src/doslit/slistonly.par b/noao/imred/src/doslit/slistonly.par
new file mode 100644
index 00000000..08d4e016
--- /dev/null
+++ b/noao/imred/src/doslit/slistonly.par
@@ -0,0 +1,12 @@
+objects,f,a,,,,
+arcs1,f,a,,,,
+standards,f,a,,,,
+dispcor,b,a,,,,
+extcor,b,a,,,,
+fluxcal,b,a,,,,
+redo,b,a,,,,
+update,b,a,,,,
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+fd3,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/doslit/sparams.par b/noao/imred/src/doslit/sparams.par
new file mode 100644
index 00000000..1cc001d8
--- /dev/null
+++ b/noao/imred/src/doslit/sparams.par
@@ -0,0 +1,65 @@
+line,i,h,INDEF,,,"Default dispersion line"
+nsum,i,h,10,,,"Number of dispersion lines to sum or median"
+extras,b,h,no,,,"Extract sky, sigma, etc.?
+
+-- DEFAULT APERTURE PARAMETERS -- "
+lower,r,h,-3.,,,Lower aperture limit relative to center
+upper,r,h,3.,,,"Upper aperture limit relative to center
+
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --"
+ylevel,r,h,0.05,,,"Fraction of peak or intensity for resizing
+
+-- TRACE PARAMETERS --"
+t_step,i,h,10,,,"Tracing step"
+t_function,s,h,"spline3","chebyshev|legendre|spline1|spline3",,"Trace fitting function"
+t_order,i,h,1,,,"Trace fitting function order"
+t_niterate,i,h,1,0,,"Trace rejection iterations"
+t_low,r,h,3.,0.,,"Trace lower rejection sigma"
+t_high,r,h,3.,0.,,"Trace upper rejection sigma
+
+-- APERTURE EXTRACTION PARAMETERS --"
+weights,s,h,"none",,,Extraction weights (none|variance)
+pfit,s,h,"fit1d","fit1d|fit2d",,Profile fitting algorithm (fit1d|fit2d)
+lsigma,r,h,3.,,,Lower rejection threshold
+usigma,r,h,3.,,,"Upper rejection threshold
+
+-- BACKGROUND SUBTRACTION PARAMETERS --"
+background,s,h,"fit","none|average|median|minimum|fit",,Background to subtract
+b_function,s,h,"legendre","chebyshev|legendre|spline1|spline3",,"Background function"
+b_order,i,h,1,,,"Background function order"
+b_sample,s,h,"-10:-6,6:10",,,"Background sample regions"
+b_naverage,i,h,-100,,,"Background average or median"
+b_niterate,i,h,1,0,,"Background rejection iterations"
+b_low,r,h,3.,0.,,"Background lower rejection sigma"
+b_high,r,h,3.,0.,,"Background upper rejection sigma
+
+-- ARC DISPERSION FUNCTION PARAMETERS --"
+threshold,r,h,10.,0.,,"Minimum line contrast threshold"
+coordlist,f,h,linelists$idhenear.dat,,,"Line list"
+match,r,h,-3.,,,"Line list matching limit in Angstroms"
+fwidth,r,h,4.,,,"Arc line widths in pixels"
+cradius,r,h,10.,,,Centering radius in pixels
+i_function,s,h,"spline3","legendre|chebyshev|spline1|spline3",,"Coordinate function"
+i_order,i,h,1,1,,"Order of dispersion function"
+i_niterate,i,h,1,0,,"Rejection iterations"
+i_low,r,h,3.,0.,,"Lower rejection sigma"
+i_high,r,h,3.,0.,,"Upper rejection sigma"
+refit,b,h,yes,,,"Refit coordinate function when reidentifying?"
+addfeatures,b,h,no,,,"Add features when reidentifying?
+
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --"
+select,s,h,"interp",,,"Selection method for reference spectra"
+sort,s,h,"jd",,,"Sort key"
+group,s,h,"ljd",,,"Group key"
+time,b,h,no,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting
+
+-- DISPERSION CORRECTION PARAMETERS --"
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+log,b,h,no,,,"Logarithmic wavelength scale?"
+flux,b,h,yes,,,"Conserve flux?
+
+-- SENSITIVITY CALIBRATION PARAMETERS --"
+s_function,s,h,"spline3","chebyshev|legendre|spline3|spline1",,"Fitting function"
+s_order,i,h,1,1,,"Order of sensitivity function"
+fnu,b,h,no,,,"Create spectra having units of FNU?"
diff --git a/noao/imred/src/doslit/sproc.cl b/noao/imred/src/doslit/sproc.cl
new file mode 100644
index 00000000..0b13d71a
--- /dev/null
+++ b/noao/imred/src/doslit/sproc.cl
@@ -0,0 +1,404 @@
+# SPROC -- Process spectra from 2D to 1D
+#
+# This program combines all the operations of extraction, dispersion
+# correction, extinction correction, and flux calibration in as simple
+# and noninteractive manner as possible.
+
+procedure sproc (objects, arcs1, arctable, standards, crval, cdelt, dispcor,
+	extcor, fluxcal, resize, clean, splot, redo, update, quicklook, batch,
+	listonly)
+
+file	objects = ""		{prompt="List of object spectra"}
+
+file	arcs1 = ""		{prompt="List of arc spectra"}
+file	arctable = ""		{prompt="Arc assignment table (optional)"}
+file	standards = ""		{prompt="List of standard star spectra\n"}
+
+string	crval = "INDEF"		{prompt="Approximate wavelength"}
+string	cdelt = "INDEF"		{prompt="Approximate dispersion\n"}
+
+bool	dispcor = yes		{prompt="Dispersion correct spectra?"}
+bool	extcor = no		{prompt="Extinction correct spectra?"}
+bool	fluxcal = no		{prompt="Flux calibrate spectra?"}
+bool	resize = no		{prompt="Automatically resize apertures?"}
+bool	clean = no		{prompt="Detect and replace bad pixels?"}
+bool	splot = no		{prompt="Plot the final spectrum?"}
+bool	redo = no		{prompt="Redo operations if previously done?"}
+bool	update = no		{prompt="Update spectra if cal data changes?"}
+bool	quicklook = no		{prompt="Minimally interactive quick-look?"}
+bool	batch = no		{prompt="Extract objects in batch?"}
+bool	listonly = no		{prompt="List steps but don't process?\n"}
+
+real	datamax = INDEF		{prompt="Max data value / cosmic ray threshold"}
+
+string	anssplot		{prompt="Splot spectrum?", mode="q",
+				 enum="no|yes|NO|YES"}
+bool	newdisp, newsens, newarcs
+bool	fluxcal1, splot1, splot2
+bool	dobatch
+
+struct	*fd1, *fd2, *fd3
+
+begin
+	file	arcref1, spec, arc
+	file	arcref1ms, specms, arcms
+	file	temp, done
+	string	imtype, mstype
+	string	str1, str2, str3, str4, arcrefs, log1, log2
+	bool	reextract, extract, disp, ext, flux, log
+	int	i, j, n, nspec
+	struct	err
+
+	# Call a separate task to do the listing to minimize the size of
+	# this script and improve it's readability.
+
+	dobatch = no
+	if (listonly) {
+	    slistonly (objects, arcs1, standards, dispcor, extcor,
+		fluxcal, redo, update)
+	    bye
+	}
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	mstype = ".ms" // imtype
+	n = strlen (imtype)
+
+	# Temporary files used repeatedly in this script.  Under some
+	# abort circumstances these files may be left behind.
+
+	temp = mktemp ("tmp$iraf")
+	done = mktemp ("tmp$iraf")
+
+	# Get query parameters
+	if (arctable == "")
+	    arcrefs = "@"//arcs1
+	else
+	    arcrefs = arctable
+	arcref1 = ""
+
+	# Rather than always have switches on the logfile and verbose flags
+	# we use TEE and set a file to "dev$null" if output is not desired.
+	# We must check for the null string to signify no logfile.
+
+	tee.append = yes
+	if (logfile == "")
+	    log1 = "dev$null"
+	else
+	    log1 = logfile
+	if (verbose)
+	    log2 = "STDOUT"
+	else
+	    log2 = "dev$null"
+
+	# If the update switch is used changes in the calibration data can
+	# cause images to be reprocessed (if they are in the object list).
+	# Possible changes are in the dispersion solution and sensitivity
+	# function.  The newarcs flag is used to only go through the arc
+	# image headers once setting the reference spectrum, airmass, and UT.
+
+	newdisp = no
+	newsens = no
+	newarcs = yes
+	fluxcal1 = fluxcal
+
+	# Check if there are aperture definitions in the database and
+	# define them if needed.  This is interactive.
+
+	print ("Define object apertures", >> log1)
+	if (resize)
+	    apslitproc.ansresize = "YES"
+	else
+	    apslitproc.ansresize = "NO"
+	if (quicklook) {
+	    apslitproc.ansedit = "NO"
+	    apslitproc.ansfittrace = "NO"
+	} else {
+	    apslitproc.ansedit = "yes"
+	    apslitproc.ansfittrace = "yes"
+	}
+	if (redo) {
+	    delete (database//"/ap//@"//objects, verify=no, >& "dev$null")
+	    apslitproc ("@"//objects, references="", ansfind="YES",
+		ansrecenter="NO", anstrace="YES", ansextract="NO")
+	} else
+	    apslitproc ("@"//objects, references="NEW", ansfind="YES",
+		ansrecenter="NO", anstrace="YES", ansextract="NO")
+	if (dispcor && fluxcal1) {
+	    if (redo) {
+		delete (database//"/ap//@"//standards, verify=no, >& "dev$null")
+		apslitproc ("@"//standards, references="", ansfind="YES",
+		    ansrecenter="NO", anstrace="YES", ansextract="NO")
+	    } else
+		apslitproc ("@"//standards, references="NEW", ansfind="YES",
+		    ansrecenter="NO", anstrace="YES", ansextract="NO")
+	}
+
+	# Initialize APSLITPROC.
+	apslitproc.saturation = INDEF
+	apslitproc.references = ""
+	apslitproc.profiles = ""
+	apslitproc.ansrecenter = "NO"
+	apslitproc.ansresize = "NO"
+	apslitproc.ansedit = "NO"
+	apslitproc.anstrace = "NO"
+	apslitproc.ansfittrace = "NO"
+	apslitproc.ansextract = "YES"
+	apslitproc.ansreview = "NO"
+
+	# Initialize REIDENTIFY
+	if (quicklook)
+	    reidentify.answer = "NO"
+	else
+	    reidentify.answer = "yes"
+
+	if (splot && !quicklook) {
+	    splot1 = yes
+	    splot2 = yes
+	} else {
+	    splot1 = no
+	    splot2 = no
+	}
+
+	# If not dispersion correcting we can go directly to extracting
+	# the object spectra.  The reference arcs are the first on
+	# the arc lists.  The processing of the reference arcs is done
+	# by the task SARCREFS.
+
+	if (dispcor) {
+	    fd1 = arcs1
+	    fd2 = objects
+	    if (fscan (fd1, arcref1) == EOF)
+		error (1, "No reference arcs")
+	    fd1 = ""
+	    if (fscan (fd2, spec) == EOF)
+		error (1, "No object spectra for arc reference")
+	    fd2 = ""
+	    i = strlen (arcref1)
+	    if (!access (arcref1 // imtype)) {
+		printf ("Arc reference spectrum not found - %s%s\n",
+		    arcref1, imtype) | scan (err)
+		error (1, err // "\nCheck setting of imtype")
+	    }
+	    arcref1ms = arcref1 // mstype
+	    if (redo && access (arcref1ms))
+	        imdelete (arcref1ms, verify=no)
+	    apslitproc.references = spec
+	    sarcrefs (arcref1, crval, cdelt, done, log1, log2)
+	    apslitproc.references = ""
+
+	    if (fluxcal1)
+		sfluxcal (standards, arcs1, arcref1, arcrefs,
+		    redo, update, extcor, done, log1, log2)
+	}
+
+	# Now we are ready to process the object spectra.
+
+	reextract = redo || (update && newdisp)
+	fd1 = objects
+	while (fscan (fd1, spec) != EOF) {
+	    i = strlen (spec)
+	    if (i > n && substr (spec, i-n+1, i) == imtype)
+		spec = substr (spec, 1, i-n)
+	    
+	    # Check if previously done; i.e. arc.
+	    if (access (done)) {
+	        fd2 = done
+	        while (fscan (fd2, specms) != EOF)
+		    if (spec == specms)
+		        break
+	        if (spec == specms)
+		    next
+	        fd2 = ""
+	    }
+	    if (!access (spec // imtype)) {
+		print ("Object spectrum not found - " // spec // imtype) |
+		    tee (log1)
+		print ("Check setting of imtype")
+		next
+	    }
+	    specms = spec // mstype
+
+	    # Determine required operations from the flags and image header.
+	    extract = no
+	    disp = no
+	    ext = no
+	    flux = no
+	    if (reextract || !access (specms))
+		extract = yes
+	    else {
+		hselect (specms, "dispcor", yes, > temp)
+		hselect (specms, "ex-flag", yes, >> temp)
+		hselect (specms, "ca-flag", yes, >> temp)
+		fd2 = temp
+		if (fscan (fd2, str1) == 1) {
+		    extract = update && newdisp
+		    if (update && !newdisp)
+		        # We really should check if REFSPEC will assign
+			# different reference spectra.
+			;
+		} else
+		    disp = dispcor
+		if (fscan (fd2, str1) == 1)
+		    extract = update && !extcor
+		else
+		    ext = extcor
+		if (fscan (fd2, str1) == 1)
+		    extract = update && (!fluxcal1 || newsens)
+		else
+		    flux = fluxcal1
+		fd2 = ""; delete (temp, verify=no)
+	    }
+		
+	    if (extract) {
+		disp = dispcor
+		ext = extcor
+		flux = fluxcal1
+	    }
+
+	    # If fully processed go to the next object.
+	    if (!extract && !disp && !extcor && !flux)
+		next
+
+	    # If not interactive and the batch flag is set submit rest to batch.
+	    if (batch && !splot1 && !splot2) {
+		fd1 = ""
+		flprcache
+		sbatch.objects = objects
+		sbatch.datamax = datamax
+		sbatch.arcs1 = arcs1
+		sbatch.arcref1 = arcref1
+		sbatch.arcrefs = arcrefs
+		sbatch.done = done
+		sbatch.logfile = log1
+		sbatch.redo = reextract
+		sbatch.update = update
+		sbatch.dispcor = dispcor
+		sbatch.fluxcal1 = fluxcal1
+		sbatch.extcor = extcor
+		sbatch.newdisp = newdisp
+		sbatch.newsens = newsens
+		sbatch.newarcs = newarcs
+		dobatch = yes
+		return
+	    }
+
+	    # Process the spectrum in foreground.
+	    if (extract) {
+		if (access (specms))
+		    imdelete (specms, verify=no)
+		print ("Extract object spectrum ", spec) | tee (log1)
+		hselect (spec, "date-obs,ut,exptime", yes, > temp)
+		hselect (spec, "ra,dec,epoch,st", yes, >> temp)
+		fd2 = temp
+		if (fscan (fd2, str1, str2, str3) == 3) {
+		    setjd (spec, observatory=observatory, date="date-obs",
+			time="ut", exposure="exptime", jd="jd", hjd="",
+			ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+			>> log1)
+		    if (fscan (fd2, str1, str2, str3, str4) == 4)
+			setairmass (spec, intype="beginning",
+			    outtype="effective", exposure="exptime",
+			    observatory=observatory, show=no, update=yes,
+			    override=yes, >> log1)
+		}
+		fd2 = ""; delete (temp, verify=no)
+		apslitproc (spec, saturation=datamax)
+	    }
+
+	    if (disp) {
+		# Fix arc headers if necessary.
+		if (newarcs) {
+	    	    fd2 = arcs1
+	    	    while (fscan (fd2, arc) != EOF) {
+			hselect (arc, "date-obs,ut,exptime", yes, > temp)
+			hselect (arc, "ra,dec,epoch,st", yes, >> temp)
+			fd3 = temp
+			if (fscan (fd3, str1, str2, str3) == 3) {
+			    setjd (arc, observatory=observatory,
+				date="date-obs", time="ut", exposure="exptime",
+				jd="jd", hjd="", ljd="ljd", utdate=yes,
+				uttime=yes, listonly=no, >> log1)
+			    if (fscan (fd3, str1, str2, str3, str4) == 4)
+				setairmass (arc, intype="beginning",
+				    outtype="effective", exposure="exptime",
+				    observatory=observatory, show=no,
+				    update=yes, override=yes, >> log1)
+			}
+			fd3 = ""; delete (temp, verify=no)
+	        	hedit (arc, "refspec1", arc, add=yes, verify=no,
+		    	    show=no, update=yes)
+		    }
+	    	    fd2 = ""
+		    newarcs = no
+		}
+
+		print ("Assign arc spectra for ", spec) | tee (log1)
+		refspectra (spec, references=arcrefs,
+		    apertures="", refaps="", ignoreaps=no,
+		    select=sparams.select, sort=sparams.sort,
+		    group=sparams.group, time=sparams.time,
+		    timewrap=sparams.timewrap, override=yes, confirm=no,
+		    assign=yes, logfiles="STDOUT", verbose=no) |
+		    tee (log1, > log2)
+
+		sdoarcs (spec, arcref1, reextract, log1, no)
+
+	        hselect (specms, "refspec1", yes, > temp)
+	        fd2 = temp
+	        i = fscan (fd2, arc)
+	        fd2 = ""; delete (temp, verify=no)
+		if (i < 1)
+		    print ("No arc reference assigned for ", spec) | tee (log1)
+		else {
+	            print ("Dispersion correct ", spec) | tee (log1)
+		    dispcor (specms, "", linearize=sparams.linearize,
+			database=database, table=arcref1//mstype,
+			w1=INDEF, w2=INDEF, dw=INDEF, nw=INDEF,
+			log=sparams.log, flux=sparams.flux, samedisp=no,
+			global=no, ignoreaps=yes, confirm=no, listonly=no,
+			verbose=verbose, logfile=logfile)
+		    flpr
+		    hedit (specms, "dispcor", 0, add=yes, verify=no,
+			show=no, update=yes)
+		    disp = no
+		}
+	    }
+
+	    if (!disp) {
+	        if (ext)
+		    print ("Extinction correct ", spec) | tee (log1)
+	        if (flux)
+		    print ("Flux calibrate ", spec) | tee (log1)
+	        if (flux || ext)
+		    calibrate (specms, "", extinct=extcor, flux=fluxcal1,
+			extinction=extinction, observatory=observatory,
+			ignoreaps=yes, sensitivity="sens", fnu=sparams.fnu) |
+			tee (log1, > log2)
+	    }
+	    if (extract || disp || ext || flux) {
+		if (splot1) {
+		    print (specms, ":")
+		    str1 = anssplot
+		    if (str1 == "NO" || str1 == "YES")
+			splot1 = no
+		    if (str1 == "no" || str1 == "NO")
+			splot2 = no
+		    else
+			splot2 = yes
+		}
+		if (splot2)
+		    splot (specms)
+		else if (splot && quicklook)
+		    bplot (specms, apertures="1", band=1, graphics="stdgraph",
+			cursor="onedspec$gcurval")
+	    }
+	    print (spec, >> done)
+	}
+	fd1 = ""
+
+	if (access (done))
+	    delete (done, verify=no)
+end
diff --git a/noao/imred/src/doslit/sproc.par b/noao/imred/src/doslit/sproc.par
new file mode 100644
index 00000000..536e05e4
--- /dev/null
+++ b/noao/imred/src/doslit/sproc.par
@@ -0,0 +1,33 @@
+objects,f,a,"",,,"List of object spectra"
+arcs1,f,a,"",,,"List of arc spectra"
+arctable,f,a,"",,,"Arc assignment table (optional)"
+standards,f,a,"",,,"List of standard star spectra
+"
+crval,s,a,"INDEF",,,"Approximate wavelength"
+cdelt,s,a,"INDEF",,,"Approximate dispersion
+"
+dispcor,b,a,yes,,,"Dispersion correct spectra?"
+extcor,b,a,no,,,"Extinction correct spectra?"
+fluxcal,b,a,no,,,"Flux calibrate spectra?"
+resize,b,a,no,,,"Automatically resize apertures?"
+clean,b,a,no,,,"Detect and replace bad pixels?"
+splot,b,a,no,,,"Plot the final spectrum?"
+redo,b,a,no,,,"Redo operations if previously done?"
+update,b,a,no,,,"Update spectra if cal data changes?"
+quicklook,b,a,no,,,"Minimally interactive quick-look?"
+batch,b,a,no,,,"Extract objects in batch?"
+listonly,b,a,no,,,"List steps but don\'t process?
+"
+datamax,r,h,INDEF,,,"Max data value / cosmic ray threshold"
+anssplot,s,q,,no|yes|NO|YES,,"Splot spectrum?"
+newdisp,b,h,,,,
+newsens,b,h,,,,
+newarcs,b,h,,,,
+fluxcal1,b,h,,,,
+splot1,b,h,,,,
+splot2,b,h,,,,
+dobatch,b,h,,,,
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+fd3,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/fibers/Revisions b/noao/imred/src/fibers/Revisions
new file mode 100644
index 00000000..a21892a2
--- /dev/null
+++ b/noao/imred/src/fibers/Revisions
@@ -0,0 +1,223 @@
+.help revisions Nov90 noao.imred.src.fibers
+.nf
+
+srcfibers$proc.cl
+srcfibers$listonly.cl
+    For reasons that are now lost in the mists of time, the shortening of
+    filenames can cause problems.  This has been removed.
+    (2/11/11, Valdes) (See bug log 577)
+
+=======
+V2.15.1
+=======
+
+=======
+V2.12.3
+=======
+
+srcfibers$batch.cl
+srcfibers$proc.cl
+srcfibers$fibresponse.cl
+    Error messages now hint to check imtype setting.
+    (4/15/05, Valdes)
+
+
+=======
+V2.12.2
+=======
+
+srcfibers$proc.cl
+srcfibers$batch.cl
+    Because dispcor.samedisp=yes when doing the objects any dispersion change
+    applied to the reference arc was not being applied to the objects.
+    (5/21/03, Valdes)
+
+=======
+V2.12.1
+=======
+
+srcfibers$skysub.cl
+    Added a flpr to workaround a FITS kernel caching problem.
+    (6/21/02, Valdes)
+
+=====
+V2.12
+=====
+
+srcfibers$proc.cl
+    Modified code to eliminate goto.  This is for use with pyraf.
+    (11/21/00, Valdes)
+
+========
+V2.11.3a
+========
+
+srcfibers$arcrefs.cl
+    The test for crval/cdelt both INDEF was not working.  (9/24/99, Valdes)
+
+srcfibers$mkfibers.cl
+     Had to define a dummy variable 'ar' to get rid of ambiguous parameter
+     error.  (9/14/99, Valdes)
+
+=======
+V2.11.2
+=======
+
+doslit$arcrefs.cl
+    The test on CRVAL and CDELT would not work with header keywords.
+    (9/22/98, Valdes)
+
+srcfibers$arcrefs.cl
+srcfibers$batch.cl
+srcfibers$doarcs.cl
+srcfibers$fibresponse.cl
+srcfibers$getspec.cl
+srcfibers$listonly.cl
+srcfibers$mkfibers.cl
+srcfibers$skysub.cl
+srcfibers$proc.cl
+    Any additional qualifiers in the imtype string are stripped.
+    (8/14/97, Valdes)
+
+=========
+V2.11BETA
+=========
+
+arcrefs.cl
+    If both crval and cdelt are INDEF then the autoidentify option is
+    not used.  (5/2/97, Valdes)
+
+apsript.par
+    Made changes for the new aperture selection option.  (9/5/96, Valdes)
+
+skysub.cl
+    Added package name to calls of "match", "sort", "uniq" to avoid
+    possible conflicts.  (5/6/96, Valdes)
+
+proc.cl
+proc.par
+arcrefs.cl
+arcrefs.par
+params.par
+    Modified to use autoidentify.  (4/5/96, Valdes)
+
+srcfibers$proc.cl
+srcfibers$batch.cl
+    When using subapertures the subapertures were not wavelength
+    calibrated correctly because the reference arc spectrum which
+    provides the wavelength scale does not contain the subapertures
+    and DISPCOR does not use samedisp=yes.  Changed the value of
+    samedisp to yes.  (10/27/95, Valdes)
+
+srcfibers$mkfibers.cl
+    The calls to mk1dspec did not specify the header file which would
+    then default to the task parameter which might be invalid.
+    (10/17/95, Valdes)
+
+srcfibers$proc.cl
+    Needed to initialize arcref2 in order work in batch when no dispersion
+    correction is requested.  (10/16/95, Valdes)
+
+srcfibers$mkfibers.cl
+    The calls to MK1DSPEC were changed in accordance with parameter changes
+    to that task.
+    (7/28/95, Valdes)
+
+srcfibers$proc.cl
+    Any image extension is stripped from the apidtable parameter.
+    (7/24/95, Valdes)
+
+srcfibers$doalign.cl +
+srcfibers$doalign.par +
+srcfibers$proc.cl
+srcfibers$batch.cl
+    Added the sky alignment option.  (7/19/95, Valdes)
+
+srcfibers$proc.cl
+srcfibers$batch.cl
+srcfibers$arcrefs.cl
+    The wrong range syntax is used with subapertures in SARITH/SCOPY.
+    Changed all -999 to 1-999.  (6/14/95, Valdes)
+
+=======
+V2.10.4
+=======
+
+srcfibers$proc.cl
+srcfibers$fibresponse.cl
+    1.  Need to add check for the throughput being a file rather than
+	an image when checking whether to apply a scattered light
+	correction.
+    2.	Removed a warning message when using a throughput file containing
+    	fiber values which are not in the flat field (for example, if a fiber
+    	is broken).
+    (1/25/95, Valdes)
+
+srcfibers$params.par
+srcfibers$doarcs.cl
+srcfibers$arcrefs.cl
+    Added "threshold" as a user parameter.  (1/16/95, Valdes)
+
+srcfibers$response.cl -> imred$src/fibers/fibresponse.cl
+srcfibers$response.par -> imred$src/fibers/fibresponse.par
+srcfibers$proc.par
+    Changed the fiber response task name from "response" to "fibresponse"
+    to avoid conflict with longslit.response.  (12/31/94, Valdes)
+
+srcfibers$proc.cl
+    The check for arcs2 = " " was done incorrectly.  (9/12/94, Valdes)
+
+srcfibers$proc.cl
+srcfibers$batch.cl
+srcfibers$doarcs.cl
+    A check was needed on whether the arc spectra were extracted during
+    the current execution to avoid reextracting the same arc multiple
+    times during a "redo" or the initial time.  In both those cases
+    the rextract flag is set causing spectra to be reextracted if they
+    exist.  Previously doarcs could not tell if the arc exists because
+    of a previous run or during the current run with the same arc
+    used multiple times.  (5/18/94, Valdes)
+
+===========
+V2.10.3beta
+===========
+
+srcfibers$skysub.cl
+imred$specred/doc/skysub.hlp
+    1.  The combine option was being ignored.
+    2.  The help did not mention the reject option and was otherwised
+	out of date.
+    (3/31/94, Valdes)
+
+srcfibers$proc.cl
+    The scattered light correction is now queried for all images and may
+    be turned off with NO.  (9/1/93, Valdes)
+
+===========
+V2.10.3beta
+===========
+
+srcfibers$arcrefs.cl
+     MOdified to use shift=INDEF in REIDENTIFY.
+     (2/18/93, Valdes)
+
+srcfibers$*.cl
+     Modified to use the "imtype" environment variable to define the
+     extension type.
+     (2/18/93, Valdes)
+
+=======
+V2.10.2
+=======
+
+srcfibers$proc.cl
+     The aperture reference is redone when a new aperture ID file is seen.
+     (1/11/93, Valdes)
+
+srcfibers$*
+     Updated for new ONEDSPEC.  (7/24/91, Valdes)
+
+srcfibers$*
+     All occurrences of latitude replaced by observatory as required by
+     recent changes to setairmass, etc.  (11/20/90, Valdes)
+.endhelp
diff --git a/noao/imred/src/fibers/apscript.par b/noao/imred/src/fibers/apscript.par
new file mode 100644
index 00000000..e52248de
--- /dev/null
+++ b/noao/imred/src/fibers/apscript.par
@@ -0,0 +1,145 @@
+# APSCRIPT
+
+input,s,a,,,,List of input images
+output,s,h,"",,,List of output spectra
+apertures,s,h,"",,,Apertures
+scatter,s,h,"",,,List of scattered light images (optional)
+references,s,h,"",,,List of aperture reference images
+profiles,s,h,"",,,"List of aperture profile images
+"
+interactive,b,h,yes,,,Run task interactively?
+find,b,h,yes,,,Find apertures?
+recenter,b,h,yes,,,Recenter apertures?
+resize,b,h,yes,,,Resize apertures?
+edit,b,h,yes,,,Edit apertures?
+trace,b,h,yes,,,Trace apertures?
+fittrace,b,h,yes,,,Fit the traced points interactively?
+extract,b,h,yes,,,Extract spectra?
+review,b,h,yes,,,Review extractions?
+subtract,b,h,yes,,,Subtract scattered light?
+smooth,b,h,yes,,,Smooth scattered light along the dispersion?
+fitscatter,b,h,yes,,,Fit scattered light interactively?
+fitsmooth,b,h,yes,,,"Smooth the scattered light interactively?
+"
+line,i,h,)params.line,,,>params.line
+nsum,i,h,)params.nsum,,,>params.nsum
+buffer,r,h,)params.buffer,,,">params.buffer
+
+# OUTPUT PARAMETERS
+"
+format,s,h,"multispec",,,Extracted spectra format
+extras,b,h,)params.extras,,,"Extract sky, sigma, etc.?"
+dbwrite,s,h,"YES",,,Write to database?
+initialize,b,h,no,,,Initialize answers?
+verbose,b,h,no,,,"Verbose output?
+
+# DEFAULT APERTURE PARAMETERS
+"
+lower,r,h,)params.lower,,,>params.lower
+upper,r,h,)params.upper,,,>params.upper
+apidtable,s,h,"",,,"Aperture ID table (optional)
+
+# DEFAULT BACKGROUND PARAMETERS
+"
+b_function,s,h,"legendre","chebyshev|legendre|spline1|spline3",,Background function
+b_order,i,h,1,,,Background function order
+b_sample,s,h,"-10:-6,6:10",,,Background sample regions
+b_naverage,i,h,-3,,,Background average or median
+b_niterate,i,h,0,0,,Background rejection iterations
+b_low_reject,r,h,3.,0.,,Background lower rejection sigma
+b_high_reject,r,h,3.,0.,,Background upper rejection sigma
+b_grow,r,h,0.,0.,,"Background rejection growing radius
+
+# APERTURE CENTERING PARAMETERS
+"
+width,r,h,5.,0.,,Profile centering width
+radius,r,h,10.,,,Profile centering radius
+threshold,r,h,10.,0.,,"Detection threshold for profile centering
+
+# AUTOMATIC FINDING AND ORDERING PARAMETERS
+"
+nfind,i,h,,,,Number of apertures to be found automatically
+minsep,r,h,1.,,,Minimum separation between spectra
+maxsep,r,h,100000.,,,Maximum separation between spectra
+order,s,h,)params.order,,,"Order of apertures
+
+# RECENTERING PARAMETERS
+"
+aprecenter,s,h,"",,,Apertures to use in recentering
+npeaks,r,h,0.5,,,Select brightest peaks
+shift,b,h,yes,,,"Use average shift instead of recentering?
+
+# RESIZING PARAMETERS
+"
+llimit,r,h,INDEF,,,Lower aperture limit relative to center
+ulimit,r,h,INDEF,,,Upper aperture limit relative to center
+ylevel,r,h,)params.ylevel,,,>params.ylevel
+peak,b,h,yes,,,Is ylevel a fraction of the peak?
+bkg,b,h,yes,,,"Subtract background in automatic width?"
+r_grow,r,h,0.,,,Grow limits by this factor
+avglimits,b,h,no,,,"Average limits over all apertures?
+
+# EDITING PARAMETERS
+"
+e_output,s,q,,,,Output spectra rootname
+e_profiles,s,q,,,,"Profile reference image
+
+# TRACING PARAMETERS
+"
+t_nsum,i,h,)params.nsum,,,>params.nsum
+t_step,i,h,)params.t_step,,,>params.t_step
+t_nlost,i,h,3,1,,Number of consecutive times profile is lost before quitting
+t_width,r,h,5.,0.,,Profile centering width
+t_function,s,h,)params.t_function,,,>params.t_function
+t_sample,s,h,"*",,,Trace sample regions
+t_order,i,h,)params.t_order,,,>params.t_order
+t_naverage,i,h,1,,,Trace average or median
+t_niterate,i,h,)params.t_niterate,,,>params.t_niterate
+t_low_reject,r,h,)params.t_low,,,>params.t_low
+t_high_reject,r,h,)params.t_high,,,>params.t_high
+t_grow,r,h,0.,0.,,"Trace rejection growing radius
+
+# EXTRACTION PARAMETERS
+"
+background,s,h,"none","none|average|median|minimum|fit",,Background to subtract
+skybox,i,h,1,,,Box car smoothing length for sky
+weights,s,h,)params.weights,,,>params.weights
+pfit,s,h,)params.pfit,,,>params.pfit
+clean,b,h,no,,,Detect and replace bad pixels?
+nclean,r,h,0.5,,,Maximum number of pixels to clean
+niterate,i,h,5,0,,Number of profile fitting iterations
+saturation,r,h,INDEF,,,Saturation level
+readnoise,s,h,"0.",,,Read out noise sigma (photons)
+gain,s,h,"1.",,,Photon gain (photons/data number)
+lsigma,r,h,)params.lsigma,,,>params.lsigma
+usigma,r,h,)params.usigma,,,>params.usigma
+polysep,r,h,0.95,0.1,0.95,Marsh algorithm polynomial spacing
+polyorder,i,h,10,1,,Marsh algorithm polynomial order
+nsubaps,i,h,1,1,,"Number of subapertures per aperture
+
+# ANSWER PARAMETERS
+"
+ansclobber,s,h,"NO",,," "
+ansclobber1,s,h,"NO",,," "
+ansdbwrite,s,h,"YES",,," "
+ansdbwrite1,s,h,"NO",,," "
+ansedit,s,h,"NO",,," "
+ansextract,s,h,"NO",,," "
+ansfind,s,h,"NO",,," "
+ansfit,s,h,"NO",,," "
+ansfitscatter,s,h,"NO",,," "
+ansfitsmooth,s,h,"NO",,," "
+ansfitspec,s,h,"NO",,," "
+ansfitspec1,s,h,"NO",,," "
+ansfittrace,s,h,"NO",,," "
+ansfittrace1,s,h,"NO",,," "
+ansflat,s,h,"NO",,," "
+ansnorm,s,h,"NO",,," "
+ansrecenter,s,h,"NO",,," "
+ansresize,s,h,"NO",,," "
+ansreview,s,h,"NO",,," "
+ansreview1,s,h,"NO",,," "
+ansscat,s,h,"NO",,," "
+ansskyextract,s,h,"NO",,," "
+anssmooth,s,h,"NO",,," "
+anstrace,s,h,"NO",,," "
diff --git a/noao/imred/src/fibers/arcrefs.cl b/noao/imred/src/fibers/arcrefs.cl
new file mode 100644
index 00000000..d0d6fcf1
--- /dev/null
+++ b/noao/imred/src/fibers/arcrefs.cl
@@ -0,0 +1,326 @@
+# ARCREFS -- Determine dispersion relation for reference arcs.
+
+procedure arcrefs (arcref1, arcref2, extn, arcreplace, apidtable, response,
+	crval, cdelt, done, log1, log2)
+
+file	arcref1
+file	arcref2
+string	extn
+file	arcreplace
+file	apidtable
+file	response
+string	crval = "INDEF"
+string	cdelt = "INDEF"
+file	done
+file	log1
+file	log2
+
+struct	*fd
+
+begin
+	string	imtype
+	string	arcref, arcrefms, arc, arcms
+	string	temp, temp1, temp2, str1, str2
+	int	i, n, nspec, dc
+	real	w
+	bool	log
+	struct	str3
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	n = strlen (imtype)
+
+	temp = mktemp ("tmp$iraf")
+	temp1 = mktemp ("tmp$iraf")
+	temp2 = mktemp ("tmp$iraf")
+
+	# Extract the primary arc reference spectrum.  Extract and replace
+	# any replacement arcs defined in the arcreplace file.  Determine the
+	# dispersion function with IDENTIFY/REIDENTIFY.  Set the wavelength
+	# parameters with MSDISPCOR.
+
+	arcref = arcref1
+	arcrefms = arcref1 // extn
+	if (!access (arcrefms//imtype)) {
+	    print ("Extract arc reference image ", arcref) | tee (log1)
+	    apscript (arcref, output=arcrefms, ansrecenter="NO",
+		ansresize="NO", ansedit="NO", anstrace="NO",
+		nsubaps=params.nsubaps, background="none", clean=no,
+		weights="none")
+	    sapertures (arcrefms, apertures="", apidtable=apidtable,
+		wcsreset=no, verbose=no, beam=INDEF, dtype=INDEF, w1=INDEF,
+		dw=INDEF, z=INDEF, aplow=INDEF, aphigh=INDEF, title=INDEF)
+	    if (response != "") {
+		if (params.nsubaps == 1)
+	            sarith (arcrefms, "/", response, arcrefms, w1=INDEF,
+			w2=INDEF, apertures="", bands="", beams="", apmodulus=0,
+			reverse=no, ignoreaps=no, format="multispec",
+			renumber=no, offset=0, clobber=yes, merge=no,
+			errval=0, verbose=no)
+		else {
+		    blkrep (response, temp, 1, params.nsubaps)
+	            sarith (arcrefms, "/", temp, arcrefms, w1=INDEF, w2=INDEF,
+			apertures="", bands="", beams="", apmodulus=0,
+			reverse=no, ignoreaps=yes, format="multispec",
+			renumber=no, offset=0, clobber=yes, merge=no,
+			errval=0, verbose=no)
+		    imdelete (temp, verify=no)
+		}
+	    }
+
+	    if (arcreplace != "") {
+		if (!access (arcreplace))
+		    error (1, "Can't access file "//arcreplace)
+		fd = arcreplace
+		while (fscan (fd, arc, str1, str2) != EOF) {
+		    i = strlen (arc)
+		    if (i > n && substr (arc, i-n+1, i) == imtype)
+			arc = substr (arc, 1, i-n)
+		    if (arc != arcref)
+			    next
+		    arc = str1
+		    if (i > n && substr (arc, i-n+1, i) == imtype)
+			arc = substr (arc, 1, i-n)
+		    arcms = arc // extn
+
+		    if (access (arcms//imtype))
+			imdelete (arcms, verify=no)
+
+		    print ("Extract arc reference image ", arc) | tee (log1)
+		    apscript (arc, output=arcms, ansrecenter="NO",
+			ansresize="NO", ansedit="NO", anstrace="NO",
+			nsubaps=params.nsubaps, background="none", clean=no,
+			weights="none")
+		    sapertures (arcms, apertures="", apidtable=apidtable,
+			wcsreset=no, verbose=no, beam=INDEF, dtype=INDEF,
+			w1=INDEF, dw=INDEF, z=INDEF, aplow=INDEF, aphigh=INDEF,
+			title=INDEF)
+		    if (response != "") {
+			if (params.nsubaps == 1)
+			    sarith (arcms, "/", response, arcms, w1=INDEF,
+				w2=INDEF, apertures="", bands="", beams="",
+				apmodulus=0, reverse=no, ignoreaps=no,
+				format="multispec", renumber=no, offset=0,
+				clobber=yes, merge=no, errval=0, verbose=no)
+			else {
+			    blkrep (response, temp, 1, params.nsubaps)
+			    sarith (arcms, "/", temp, arcms, w1=INDEF,
+				w2=INDEF, apertures="", bands="", beams="",
+				apmodulus=0, reverse=no, ignoreaps=yes,
+				format="multispec", renumber=no, offset=0,
+				clobber=yes, merge=no, errval=0, verbose=no)
+			    imdelete (temp, verify=no)
+			}
+		    }
+		    scopy (arcms, arcrefms, w1=INDEF, w2=INDEF, apertures=str2,
+			bands="", beams="", apmodulus=1000, offset=0,
+			format="multispec", clobber=yes, merge=yes, renumber=no,
+			verbose=yes) | tee (log1, > log2)
+		    imdelete (arcms, verify=no)
+		}
+		fd = ""
+	    }
+	}
+		    
+	# Get the dispersion parameters from the header.  These are
+	# used for all further spectra and also flag whether this
+	# spectrum has been processed.  If the parameters are missing
+	# the spectrum needs to have the dispersion function and
+	# wavelength scale determined.  The HEDIT is needed because
+	# in some cases the user may exit IDENTIFY without updating
+	# the database (if the image was deleted but the database
+	# entry was not).
+
+	hselect (arcrefms, "dclog1", yes) | scan (str1)
+	if (nscan () != 1) {
+	    print ("Determine dispersion solution for ", arcref) | tee (log1)
+	    #delete (database//"/id"//arcrefms//"*", verify=no)
+	    printf ("%s %s\n", crval, cdelt) | scan (str3)
+	    if (str3 == "INDEF INDEF")
+		identify (arcrefms, section="middle line", database=database,
+		    coordlist=params.coordlist, nsum=1, match=params.match,
+		    maxfeatures=50, zwidth=100., ftype="emission",
+		    fwidth=params.fwidth, cradius=params.cradius,
+		    threshold=params.threshold, minsep=2.,
+		    function=params.i_function, order=params.i_order,
+		    sample="*", niterate=params.i_niterate,
+		    low_reject=params.i_low, high_reject=params.i_high,
+		    grow=0., autowrite=yes)
+	    else
+		autoidentify (arcrefms, crval, cdelt,
+		    coordlist=params.coordlist,
+		    interactive="YES", section="middle line", nsum="1",
+		    ftype="emission", fwidth=params.fwidth,
+		    cradius=params.cradius, threshold=params.threshold,
+		    minsep=2., match=params.match, function=params.i_function,
+		    order=params.i_order, sample="*",
+		    niterate=params.i_niterate, low_reject=params.i_low,
+		    high_reject=params.i_high, grow=0., dbwrite="YES",
+		    overwrite=yes, database="database", verbose=yes,
+		    logfile=logfile, plotfile=plotfile,
+		    reflist="", refspec="", crpix="INDEF", cddir="unknown",
+		    crsearch="-0.5", cdsearch="INDEF", aidpars="")
+
+	    hedit (arcrefms, "refspec1", arcrefms, add=yes,
+		show=no, verify=no)
+
+	    nspec = 1
+	    hselect (arcrefms, "naxis2", yes) | scan (nspec)
+	    if (nspec > 1)
+		reidentify (arcrefms, "", interactive=yes,
+		    section="middle line", shift=0., step=1, nsum=1,
+		    cradius=params.cradius, threshold=params.threshold,
+		    nlost=100, refit=params.refit, trace=no, override=yes,
+		    addfeatures=params.addfeatures, newaps=no,
+		    coordlist=params.coordlist, match=params.match,
+		    maxfeatures=50, minsep=2., database=database,
+		    plotfile=plotfile, logfiles=logfile, verbose=yes)
+
+	    # Dispersion correct the reference arc.  This step is required to
+	    # use the confirm option of MSDISPCOR to set the wavelength scale
+	    # for all further spectra.  Set the newdisp flag.
+
+	    print ("Dispersion correct ", arcref) | tee (log1)
+	    dispcor (arcrefms, "", linearize=params.linearize,
+		database=database, table="", w1=INDEF, w2=INDEF, dw=INDEF,
+		nw=INDEF, log=params.log, flux=params.flux, samedisp=yes,
+		global=no, ignoreaps=no, confirm=yes, listonly=no, verbose=no,
+		logfile=logfile)
+	    if (params.nsubaps > 1) {
+		imrename (arcrefms, temp, verbose=no)
+		scopy (temp, arcrefms, w1=INDEF, w2=INDEF, apertures="1-999",
+		    bands="", beams="", apmodulus=0, offset=0,
+		    format="multispec", clobber=no, merge=no, renumber=no,
+		    verbose=no)
+		blkavg (temp, temp, 1, params.nsubaps, option="sum")
+		imcopy (temp, arcrefms//"[*,*]", verbose=no)
+		imdelete (temp, verify=no)
+	    }
+	    proc.newdisp = yes
+	}
+	if (extn == ".ms")
+	    print (arcref, >> done)
+
+	# Extract the alternate shift arc reference.  Transfer the dispersion
+	# function from the primary arc reference and then identify shift
+	# lines.
+
+	if (arcref2 != "") {
+	    arcref = arcref2
+	    arcrefms = arcref2 // extn
+	    if (proc.newdisp && access (arcrefms//imtype))
+		imdelete (arcrefms, verify=no)
+	    if (!access (arcrefms)) {
+		print ("Extract arc reference image ", arcref) | tee (log1)
+		apscript (arcref, output=arcrefms, ansrecenter="NO",
+		    ansresize="NO", ansedit="NO", anstrace="NO",
+		    nsubaps=params.nsubaps, background="none", clean=no,
+		    weights="none")
+		sapertures (arcrefms, apertures="", apidtable=apidtable,
+		    wcsreset=no, verbose=no, beam=INDEF, dtype=INDEF, w1=INDEF,
+		    dw=INDEF, z=INDEF, aplow=INDEF, aphigh=INDEF, title=INDEF)
+		if (response != "") {
+		    if (params.nsubaps == 1)
+			sarith (arcrefms, "/", response, arcrefms, w1=INDEF,
+			    w2=INDEF, apertures="", bands="", beams="",
+			    apmodulus=0, reverse=no, ignoreaps=no,
+			    format="multispec", renumber=no, offset=0,
+			    clobber=yes, merge=no, errval=0, verbose=no)
+		    else {
+			blkrep (response, temp, 1, params.nsubaps)
+			sarith (arcrefms, "/", temp, arcrefms, w1=INDEF,
+			    w2=INDEF, apertures="", bands="", beams="",
+			    apmodulus=0, reverse=no, ignoreaps=yes,
+			    format="multispec", renumber=no, offset=0,
+			    clobber=yes, merge=no, errval=0, verbose=no)
+			imdelete (temp, verify=no)
+		    }
+		}
+	    }
+
+	    hselect (arcrefms, "dclog1", yes) | scan (str1)
+	    if (nscan () != 1) {
+		print ("Determine dispersion solution for ", arcref) |
+		    tee (log1)
+		#delete (database//"/id"//arcrefms//"*", verify=no)
+
+		print (":r ", arcref1//extn, "\na\nd") |
+		identify (arcrefms, section="middle line", database=database,
+		    coordlist="", nsum=1, match=params.match, maxfeatures=50,
+		    zwidth=100., ftype="emission", fwidth=params.fwidth,
+		    cradius=params.cradius, threshold=params.threshold,
+		    minsep=2., function=params.i_function,
+		    order=params.i_order, sample="*",
+		    niterate=params.i_niterate, low_reject=params.i_low,
+		    high_reject=params.i_high, grow=0., autowrite=yes,
+		    cursor="STDIN", >G "dev$null", >& "dev$null")
+		identify (arcrefms, section="middle line", database=database,
+		    coordlist="", nsum=1, match=params.match, maxfeatures=50,
+		    zwidth=100., ftype="emission", fwidth=params.fwidth,
+		    cradius=params.cradius, threshold=params.threshold,
+		    minsep=2., function=params.i_function,
+		    order=params.i_order, sample="*",
+		    niterate=params.i_niterate, low_reject=params.i_low,
+		    high_reject=params.i_high, grow=0., autowrite=yes)
+		print (":feat ", temp) |
+		identify (arcrefms, section="middle line", database=database,
+		    coordlist="", nsum=1, match=params.match, maxfeatures=50,
+		    zwidth=100., ftype="emission", fwidth=params.fwidth,
+		    cradius=params.cradius, threshold=params.threshold,
+		    minsep=2., function=params.i_function,
+		    order=params.i_order, sample="*",
+		    niterate=params.i_niterate, low_reject=params.i_low,
+		    high_reject=params.i_high, grow=0., autowrite=yes,
+		    cursor="STDIN", >G "dev$null", >& "dev$null")
+		print (":r ", arcref1//extn, "\na\nd", > temp1)
+		fd = temp
+		while (fscan (fd, i, w, w, w) != EOF) {
+		    if (nscan() == 4) {
+			print (w, 1, 1, "m", >> temp1)
+			print (w, >> temp2)
+		    }
+		}
+		print ("g", >> temp1)
+		fd = ""; delete (temp, verify=no)
+
+		nspec = 1
+		hselect (arcrefms, "naxis2", yes) | scan (nspec)
+		for (i = 1; i <= nspec; i+=1)
+		    identify (arcrefms, section="line "//i,
+			database=database, coordlist="", nsum=1,
+			match=params.match, maxfeatures=50, zwidth=100.,
+			ftype="emission", fwidth=params.fwidth,
+			cradius=params.cradius, threshold=params.threshold,
+			minsep=2., function=params.i_function,
+			order=params.i_order, sample="*",
+			niterate=params.i_niterate,
+			low_reject=params.i_low, high_reject=params.i_high,
+			grow=0., autowrite=yes, cursor=temp1, < temp2,
+			>G "dev$null", >>& temp)
+		delete (temp1, verify=no); delete (temp2, verify=no)
+		system.match ("Coordinate shift", temp, stop=no, print_file_n=yes,
+		    metacharacte=yes) | tee (log1, > log2)
+		delete (temp, verify=no)
+
+		dispcor (arcrefms, "", linearize=params.linearize,
+		    database=database, table="", w1=INDEF, w2=INDEF,
+		    dw=INDEF, nw=INDEF, log=params.log, flux=params.flux,
+		    samedisp=yes, global=no, ignoreaps=no, confirm=no,
+		    listonly=no, verbose=yes, logfile=logfile, > log2)
+		if (params.nsubaps > 1) {
+		    imrename (arcrefms, temp, verbose=no)
+		    scopy (temp, arcrefms, w1=INDEF, w2=INDEF, apertures="1-999",
+			bands="", beams="", apmodulus=0, offset=0,
+			format="multispec", clobber=no, merge=no, renumber=no,
+			verbose=no)
+		    blkavg (temp, temp, 1, params.nsubaps, option="sum")
+		    imcopy (temp, arcrefms//"[*,*]", verbose=no)
+		    imdelete (temp, verify=no)
+		}
+	    }
+	    if (extn == ".ms")
+		print (arcref, >> done)
+	}
+end
diff --git a/noao/imred/src/fibers/arcrefs.par b/noao/imred/src/fibers/arcrefs.par
new file mode 100644
index 00000000..56f69145
--- /dev/null
+++ b/noao/imred/src/fibers/arcrefs.par
@@ -0,0 +1,13 @@
+arcref1,f,a,"",,,
+arcref2,f,a,"",,,
+extn,s,a,,,,
+arcreplace,f,a,"",,,
+apidtable,f,a,"",,,
+response,f,a,"",,,
+crval,s,a,INDEF,,,
+cdelt,s,a,INDEF,,,
+done,f,a,"",,,
+log1,f,a,"",,,
+log2,f,a,"",,,
+fd,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/fibers/batch.cl b/noao/imred/src/fibers/batch.cl
new file mode 100644
index 00000000..84b0a7b7
--- /dev/null
+++ b/noao/imred/src/fibers/batch.cl
@@ -0,0 +1,297 @@
+# BATCH -- Process spectra in batch.
+# This task is called in batch mode.  It only processes objects
+# not previously processed unless the update or redo flags are set.
+
+procedure batch ()
+
+string	objects		{prompt="Object spectra"}
+real	datamax		{prompt="Max data value / cosmic ray threshold"}
+
+file	response	{prompt="Response spectrum"}
+string	arcs1		{prompt="List of arc spectra"}
+string	arcs2		{prompt="List of shift arc spectra"}
+file	arcref1		{prompt="Arc reference for dispersion solution"}
+file	arcref2		{prompt="Arc reference for dispersion solution"}
+file	arcreplace	{prompt="Special aperture replacements"}
+string	arcrefs		{prompt="Arc references"}
+string	extn		{prompt="Extraction extension"}
+
+file	apidtable	{prompt="Aperture identifications"}
+string	objaps		{prompt="Object apertures"}
+string	skyaps		{prompt="Sky apertures"}
+string	arcaps		{prompt="Arc apertures"}
+string	objbeams	{prompt="Object beam numbers"}
+string	skybeams	{prompt="Sky beam numbers"}
+string	arcbeams	{prompt="Arc beam numbers\n"}
+
+file	done		{prompt="File of spectra already done"}
+file	logfile		{prompt="Logfile"}
+
+bool	redo		{prompt="Redo operations?"}
+bool	update		{prompt="Update spectra?"}
+bool	scattered	{prompt="Subtracted scattered light?"}
+bool	arcap		{prompt="Use object apertures for arcs?"}
+bool	dispcor		{prompt="Dispersion correct spectra?"}
+bool	savearcs	{prompt="Save internal arcs?"}
+bool	skyalign	{prompt="Align sky lines?"}
+bool	skysubtract	{prompt="Subtract sky?"}
+bool	saveskys	{prompt="Save sky spectra?\n"}
+
+bool	newaps, newresp, newdisp, newarcs
+
+struct	*fd1, *fd2, *fd3
+
+begin
+	file	objs, temp, temp1, spec, specms, arc
+	bool	reextract, extract, scat, disp, sky, log
+	string	imtype, mstype, str, str2, str3, str4
+	int	i
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	mstype = ".ms" // imtype
+
+	objs = mktemp ("tmp$iraf")
+	temp = mktemp ("tmp$iraf")
+	temp1 = mktemp ("tmp$iraf")
+
+	# Initialize extraction to be noninteractive.
+	if (apscript.ansrecenter == "yes")
+	    apscript.ansrecenter = "YES"
+	else if (apscript.ansrecenter == "no")
+	    apscript.ansrecenter = "NO"
+	apscript.ansedit = "NO"
+	if (apscript.anstrace == "yes") {
+	    apscript.anstrace = "YES"
+	    apscript.ansfittrace = "NO"
+	} else if (apscript.anstrace == "no")
+	    apscript.anstrace = "NO"
+
+	reextract = redo || (update && (newaps || newresp || newdisp))
+
+	getspec (objects, objs)
+	fd1 = objs
+	while (fscan (fd1, spec) != EOF) {
+	    if (access (done)) {
+	        fd2 = done
+	        while (fscan (fd2, specms) != EOF)
+		    if (spec == specms)
+		        break
+	        if (spec == specms)
+		    next
+	        fd2 = ""
+	    }
+	    if (!access (spec // imtype)) {
+		printf ("Object spectrum not found - %s%s\nCheck setting of imtype\n", spec, imtype, >> logfile)
+		next
+	    }
+	    specms = spec // mstype
+
+	    scat = no
+	    extract = no
+	    disp = no
+	    sky = no
+	    if (scattered) {
+		if (redo && access (spec//"noscat"//imtype)) {
+		    imdelete (spec, verify=no)
+		    imrename (spec//"noscat", spec)
+		}
+		hselect (spec, "apscatte", yes) | scan (str)
+		if (nscan() == 0)
+		    scat = yes
+	    }
+	    if (reextract || !access (specms) || (update && scat))
+		extract = yes
+	    else {
+		hselect (specms, "dclog1", yes) | scan (str)
+		if (nscan () == 1) {
+		    extract = update && newdisp
+		    if (update && !newdisp)
+		        # We really should check if REFSPEC will assign
+			# different reference spectra.
+			;
+		} else
+		    disp = dispcor
+
+		hselect (specms, "skysub", yes) | scan (str)
+		if (nscan() == 0)
+		    sky = skysubtract
+	    }
+		
+	    if (extract) {
+		disp = dispcor
+		sky = skysubtract
+	    }
+
+	    if (extract) {
+		if (access (specms))
+		    imdelete (specms, verify=no)
+		if (scat) {
+		    print ("Subtract scattered light from ", spec, >> logfile)
+		    imrename (spec, spec//"noscat")
+		    apscript (spec//"noscat", output=spec, ansextract="NO",
+			ansscat="YES", anssmooth="YES", verbose=no)
+		}
+		print ("Extract object spectrum ", spec, >> logfile)
+		hselect (spec, "date-obs,ut,exptime", yes, > temp1)
+		hselect (spec, "ra,dec,epoch,st", yes, >> temp1)
+		fd3 = temp1
+		if (fscan (fd3, str, str2, str3) == 3) {
+		    setjd (spec, observatory=observatory, date="date-obs",
+			time="ut", exposure="exptime", jd="jd", hjd="",
+			ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+			>> logfile)
+		    if (fscan (fd3, str, str2, str3, str4) == 4)
+			setairmass (spec, intype="beginning",
+			    outtype="effective", exposure="exptime",
+			    observatory=observatory, show=no, update=yes,
+			    override=yes, >> logfile)
+		}
+		fd3 = ""; delete (temp1, verify=no)
+		apscript (spec, nsubaps=params.nsubaps, saturation=datamax,
+		    verbose=no)
+		sapertures (specms, apertures="", apidtable=apidtable,
+		    wcsreset=no, verbose=no, beam=INDEF, dtype=INDEF, w1=INDEF,
+		    dw=INDEF, z=INDEF, aplow=INDEF, aphigh=INDEF, title=INDEF)
+		if (response != "") {
+		    if (params.nsubaps == 1)
+			sarith (specms, "/", response, specms, w1=INDEF,
+			    w2=INDEF, apertures="", bands="", beams="",
+			    apmodulus=0, reverse=no, ignoreaps=no,
+			    format="multispec", renumber=no, offset=0,
+			    clobber=yes, merge=no, errval=0, verbose=no)
+		    else {
+			blkrep (response, temp, 1, params.nsubaps)
+			sarith (specms, "/", temp, specms, w1=INDEF,
+			    w2=INDEF, apertures="", bands="", beams="",
+			    apmodulus=0, reverse=no, ignoreaps=yes,
+			    format="multispec", renumber=no, offset=0,
+			    clobber=yes, merge=no, errval=0, verbose=no)
+			imdelete (temp, verify=no)
+		    }
+		}
+	    }
+
+	    if (disp) {
+		# Fix arc headers if necessary.
+		if (newarcs) {
+		    getspec (arcs1, temp)
+	    	    fd2 = temp
+	    	    while (fscan (fd2, arc) != EOF) {
+			hselect (arc, "date-obs,ut,exptime", yes, > temp1)
+			hselect (arc, "ra,dec,epoch,st", yes, >> temp1)
+			fd3 = temp1
+			if (fscan (fd3, str, str2, str3) == 3) {
+			    setjd (arc, observatory=observatory, date="date-obs",
+				time="ut", exposure="exptime", jd="jd", hjd="",
+				ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+				>> logfile)
+			    if (fscan (fd3, str, str2, str3, str4) == 4)
+				setairmass (arc, intype="beginning",
+				    outtype="effective", exposure="exptime",
+				    observatory=observatory, show=no, update=yes,
+				    override=yes, >> logfile)
+			}
+			fd3 = ""; delete (temp1, verify=no)
+	        	hedit (arc, "refspec1", arc, add=yes, verify=no,
+		    	    show=no, update=yes)
+	        	hedit (arc, "arctype", "henear", add=yes, verify=no,
+		    	    show=no, update=yes)
+	    	    }
+	    	    fd2 = ""; delete (temp, verify=no)
+		    getspec (arcs2, temp)
+	    	    fd2 = temp
+	    	    while (fscan (fd2, arc) != EOF) {
+			hselect (arc, "date-obs,ut,exptime", yes, > temp1)
+			hselect (arc, "ra,dec,epoch,st", yes, >> temp1)
+			fd3 = temp1
+			if (fscan (fd3, str, str2, str3) == 3) {
+			    setjd (arc, observatory=observatory,
+				date="date-obs", time="ut", exposure="exptime",
+				jd="jd", hjd="", ljd="ljd", utdate=yes,
+				uttime=yes, listonly=no, >> logfile)
+			    if (fscan (fd3, str, str2, str3, str4) == 4)
+				setairmass (arc, intype="beginning",
+				    outtype="effective", exposure="exptime",
+				    observatory=observatory, show=no,
+				    update=yes, override=yes, >> logfile)
+
+			}
+			fd3 = ""; delete (temp1, verify=no)
+	        	hedit (arc, "refspec1", arc, add=yes, verify=no,
+		    	    show=no, update=yes)
+	        	hedit (arc, "arctype", "shift", add=yes, verify=no,
+		    	    show=no, update=yes)
+	    	    }
+	    	    fd2 = ""; delete (temp, verify=no)
+		    newarcs = no
+		}
+
+		print ("Assign arc spectra for ", spec, >> logfile)
+		refspectra (spec, references=arcrefs,
+		    apertures="", refaps="", ignoreaps=no,
+		    select=params.select, sort=params.sort,
+		    group=params.group, time=params.time,
+		    timewrap=params.timewrap, override=yes, confirm=no,
+		    assign=yes, logfiles="STDOUT", verbose=no,
+		    >> logfile)
+
+		doarcs (spec, response, arcref1, arcref2, extn, arcreplace,
+		    apidtable, arcaps, arcbeams, savearcs, reextract, arcap,
+		    logfile, yes, done)
+
+	        hselect (specms, "refspec1", yes, > temp)
+	        fd2 = temp
+	        i = fscan (fd2, arc)
+	        fd2 = ""; delete (temp, verify=no)
+		if (i < 1)
+		    print ("No arc reference assigned for ", spec, >> logfile)
+		else {
+		    if (skyalign)
+			doalign (spec, specms, "align"//extn//imtype,
+			    arcref1//extn, logfile, yes)
+	            print ("Dispersion correct ", spec, >> logfile)
+		    dispcor (specms, "", linearize=params.linearize,
+			database=database, table=arcref1//extn, w1=INDEF,
+			w2=INDEF, dw=INDEF, nw=INDEF, log=params.log,
+			flux=params.flux, samedisp=no, global=no,
+			ignoreaps=no, confirm=no, listonly=no, verbose=no,
+			logfile=logfile)
+		    if (params.nsubaps > 1) {
+			imrename (specms, temp, verbose=no)
+			scopy (temp, specms, w1=INDEF, w2=INDEF,
+			    apertures="1-999", bands="", beams="", apmodulus=0,
+			    offset=0, format="multispec", clobber=no, merge=no,
+			    renumber=no, verbose=no)
+			blkavg (temp, temp, 1, params.nsubaps, option="sum")
+			imcopy (temp, specms//"[*,*]", verbose=no)
+			imdelete (temp, verify=no)
+		    }
+		    disp = no
+		}
+	    }
+
+	    if (sky && !disp) {
+		str = ""
+		if (skyaps != "")
+		    str = "skyaps=" // skyaps
+		if (skybeams != "")
+		    str = str // " skybeams=" // skybeams
+	        print ("Sky subtract ", spec, ": ", str, >> logfile)
+		skysub (specms, output="", objaps=objaps, skyaps=skyaps,
+		    objbeams=objbeams, skybeams=skybeams, skyedit=no,
+		    combine=params.combine, reject=params.reject,
+		    scale=params.scale, saveskys=saveskys, logfile=logfile)
+	        hedit (specms, "skysub", str, add=yes, show=no, verify=no,
+		    update=yes)
+	    }
+	}
+	fd1 = ""; delete (objs, verify=no)
+
+	if (access (done))
+	    delete (done, verify=no)
+
+	flprcache (0)
+end
diff --git a/noao/imred/src/fibers/batch.par b/noao/imred/src/fibers/batch.par
new file mode 100644
index 00000000..54575594
--- /dev/null
+++ b/noao/imred/src/fibers/batch.par
@@ -0,0 +1,38 @@
+objects,s,h,,,,"Object spectra"
+datamax,r,h,,,,"Max data value / cosmic ray threshold"
+response,f,h,"",,,"Response spectrum"
+arcs1,s,h,,,,"List of arc spectra"
+arcs2,s,h,,,,"List of shift arc spectra"
+arcref1,f,h,"",,,"Arc reference for dispersion solution"
+arcref2,f,h,"",,,"Arc reference for dispersion solution"
+arcreplace,f,h,"",,,"Special aperture replacements"
+arcrefs,s,h,,,,"Arc references"
+extn,s,h,,,,"Extraction extension"
+apidtable,f,h,"",,,"Aperture identifications"
+objaps,s,h,,,,"Object apertures"
+skyaps,s,h,,,,"Sky apertures"
+arcaps,s,h,,,,"Arc apertures"
+objbeams,s,h,,,,"Object beam numbers"
+skybeams,s,h,,,,"Sky beam numbers"
+arcbeams,s,h,,,,"Arc beam numbers
+"
+done,f,h,"",,,"File of spectra already done"
+logfile,f,h,"",,,"Logfile"
+redo,b,h,,,,"Redo operations?"
+update,b,h,,,,"Update spectra?"
+scattered,b,h,,,,"Subtracted scattered light?"
+arcap,b,h,,,,"Use object apertures for arcs?"
+dispcor,b,h,,,,"Dispersion correct spectra?"
+savearcs,b,h,,,,"Save internal arcs?"
+skyalign,b,h,,,,"Align sky lines?"
+skysubtract,b,h,,,,"Subtract sky?"
+saveskys,b,h,,,,"Save sky spectra?
+"
+newaps,b,h,,,,
+newresp,b,h,,,,
+newdisp,b,h,,,,
+newarcs,b,h,,,,
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+fd3,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/fibers/doalign.cl b/noao/imred/src/fibers/doalign.cl
new file mode 100644
index 00000000..e3b8d4db
--- /dev/null
+++ b/noao/imred/src/fibers/doalign.cl
@@ -0,0 +1,78 @@
+# DOALIGN -- Align sky lines in objects.
+# If there is no database of features for alignment have user identify
+# them interactively.
+
+procedure doalign (spec, specms, align, table, logfile, batch)
+
+file	spec
+file	specms
+file	align
+file	table
+file	logfile
+bool	batch
+
+begin
+	file	temp
+	bool	log, verbose1
+
+	if (batch)
+	    verbose1 = no
+	else
+	    verbose1 = verbose
+
+	if (!access (align)) {
+	    print ("Identify alignment features")
+	    dispcor (specms, align, linearize=no,
+		database=database, table=table, w1=INDEF,
+		w2=INDEF, dw=INDEF, nw=INDEF, log=params.log,
+		flux=params.flux, samedisp=no, global=no,
+		ignoreaps=no, confirm=no, listonly=no,
+		verbose=no, logfile="")
+	    identify (align, section="middle line", database=database,
+		coordlist="", nsum=1, match=params.match, maxfeatures=50,
+		zwidth=100., ftype="emission", fwidth=params.fwidth,
+		cradius=params.cradius, threshold=params.threshold,
+		minsep=2., function=params.i_function,
+		order=params.i_order, sample="*",
+		niterate=params.i_niterate, low_reject=params.i_low,
+		high_reject=params.i_high, grow=0., autowrite=yes)
+	    print ("g") |
+	    identify (align, section="middle line", database=database,
+		coordlist="", nsum=1, match=params.match, maxfeatures=50,
+		zwidth=100., ftype="emission", fwidth=params.fwidth,
+		cradius=params.cradius, threshold=params.threshold,
+		minsep=2., function=params.i_function,
+		order=params.i_order, sample="*",
+		niterate=params.i_niterate, low_reject=params.i_low,
+		high_reject=params.i_high, grow=0., autowrite=yes,
+		cursor="STDIN", >G "dev$null", >& "dev$null")
+	    reidentify (align, "",
+		interactive=no, section="middle line", shift=0.,
+		step=1, nsum=1, cradius=params.cradius,
+		threshold=params.threshold, nlost=100, newaps=no,
+		refit=no, trace=no, override=yes, addfeatures=no,
+		database=database, plotfile=plotfile,
+		logfiles=logfile, verbose=verbose1)
+	}
+
+	# Set arc dispersion function in image header.
+	if (!batch)
+	    print ("Identify alignment features in ", spec)
+	print ("Identify alignment features in ", spec, >> logfile)
+	dispcor (specms, "", linearize=no,
+	    database=database, table=table, w1=INDEF,
+	    w2=INDEF, dw=INDEF, nw=INDEF, log=params.log,
+	    flux=params.flux, samedisp=no, global=no,
+	    ignoreaps=no, confirm=no, listonly=no,
+	    verbose=no, logfile="")
+	hedit (specms, "refspec1", align, add=yes,
+	    verify=no, show=no, update=yes)
+	delete (database//"/id"//spec//".ms", verify=no, >& "dev$null")
+	reidentify (align, specms,
+	    interactive=no, section="middle line", shift=0.,
+	    step=1, nsum=1, cradius=params.cradius,
+	    threshold=params.threshold, nlost=100, newaps=no,
+	    refit=no, trace=no, override=no, addfeatures=no,
+	    database=database, plotfile=plotfile,
+	    logfiles=logfile, verbose=verbose1)
+end
diff --git a/noao/imred/src/fibers/doalign.par b/noao/imred/src/fibers/doalign.par
new file mode 100644
index 00000000..0ddd375f
--- /dev/null
+++ b/noao/imred/src/fibers/doalign.par
@@ -0,0 +1,7 @@
+spec,f,a,"",,,
+specms,f,a,"",,,
+align,f,a,"",,,
+table,f,a,"",,,
+logfile,f,a,"",,,
+batch,b,a,,,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/fibers/doarcs.cl b/noao/imred/src/fibers/doarcs.cl
new file mode 100644
index 00000000..bd4e3748
--- /dev/null
+++ b/noao/imred/src/fibers/doarcs.cl
@@ -0,0 +1,264 @@
+# DOARCS -- Determine dispersion relation for spectrum based on reference arcs.
+# This procedure is complicated by:
+#    1. The need to reextract arcs if the objects spectra are being
+#	recentered or retraced.
+#    2. The use of shift spectra to track shifts in the dispersion from
+#	the reference arc spectrum.
+#    3. The use of multiple exposures to correct for illumination problems
+#	in taking the arcs.
+
+procedure doarcs (spec, response, arcref1, arcref2, extn, arcreplace, apidtable,
+	arcaps, arcbeams, savearcs, reextract, arcap, logfile, batch, done)
+
+file	spec
+file	response
+file	arcref1
+file	arcref2
+string	extn
+file	arcreplace
+file	apidtable
+string	arcaps
+string	arcbeams
+bool	savearcs
+bool	reextract
+bool	arcap
+file	logfile
+bool	batch
+file	done
+
+struct	*fd
+
+begin
+	string	imtype
+	int	i, j, k, n
+	file	temp, arc1, arc2, str1, str2, arctype, apref, arc, arcms
+	bool	verbose1
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	n = strlen (imtype)
+
+	temp = mktemp ("tmp$iraf")
+
+	if (batch)
+	    verbose1 = no
+	else
+	    verbose1 = verbose
+
+	for (j=1; j<=2; j+=1) {
+	    # The reference spectra refer initially to the 2D image.  At the
+	    # end we will reset them to refer to the 1D spectra.
+
+	    hselect (spec, "refspec"//j, yes, > temp)
+	    fd = temp
+	    k = fscan (fd, arc1, str1)
+	    fd = ""; delete (temp, verify=no)
+	    if (k < 1)
+		break
+
+	    # Strip possible image extension.
+	    i = strlen (arc1)
+	    if (i > n && substr (arc1, i-n+1, i) == imtype)
+		arc1 = substr (arc1, 1, i-n)
+    
+	    # Set extraction output and aperture reference depending on whether
+	    # the arcs are to be rextracted using recentered or retraced object
+	    # apertures.
+
+	    if (arcap &&
+		(apscript.ansrecenter=="yes" || apscript.anstrace=="yes" ||
+		 apscript.ansrecenter=="YES" || apscript.anstrace=="YES")) {
+		arc2 = spec // arc1 // ".ms"
+		apref = spec
+		if (access (arc2//imtype))
+		    imdelete (arc2//imtype, verify=no)
+		delete (database//"/id"//arc2//"*", verify = no)
+	    } else {
+		arc2 = arc1 // extn
+		apref = apscript.references
+		if (reextract && access (arc2//imtype)) {
+		    if (arc2 != arcref1 // extn && arc2 != arcref2 // extn) {
+			if (access (done)) {
+			    fd = done
+			    while (fscan (fd, arcms) != EOF)
+				if (arcms == arc2)
+				    break
+			    fd = ""
+			} else
+			    arcms = ""
+			if (arcms != arc2)
+			    imdelete (arc2, verify=no)
+		    }
+		}
+	    }
+
+	    # SHIFT arcs are reidentified with only a shift.
+	    # HENEAR arcs are reidentified using the user refit option.
+	    #	Also internal arcs are checked if HENEAR.
+
+	    hselect (arc1, "arctype", yes, > temp)
+	    fd = temp
+	    i = fscan (fd, arctype)
+	    fd = ""; delete (temp, verify=no)
+    
+	    # Extract and determine dispersion function if necessary.
+	    if (!access (arc2//imtype)) {
+		delete (database//"/id"//arc2//"*", verify = no)
+		if (!batch)
+		    print ("Extract and reidentify arc spectrum ", arc1)
+		print ("Extract and reidentify arc spectrum ", arc1, >> logfile)
+		apscript (arc1, output=arc2, references=apref,
+		    ansrecenter="NO", ansresize="NO", ansedit="NO",
+		    anstrace="NO", nsubaps=params.nsubaps, background="none",
+		    clean=no, weights="none", verbose=verbose1)
+		sapertures (arc2, apertures="", apidtable=apidtable,
+		    wcsreset=no, verbose=no, beam=INDEF, dtype=INDEF, w1=INDEF,
+		    dw=INDEF, z=INDEF, aplow=INDEF, aphigh=INDEF, title=INDEF)
+		if (response != "") {
+		    if (params.nsubaps == 1)
+			sarith (arc2, "/", response, arc2, w1=INDEF, w2=INDEF,
+			    apertures="", bands="", beams="", apmodulus=0,
+			    reverse=no, ignoreaps=no, format="multispec",
+			    renumber=no, offset=0, clobber=yes, merge=no,
+			    errval=0, verbose=no)
+		    else {
+			blkrep (response, temp, 1, params.nsubaps)
+			sarith (arc2, "/", temp, arc2, w1=INDEF, w2=INDEF,
+			    apertures="", bands="", beams="", apmodulus=0,
+			    reverse=no, ignoreaps=yes, format="multispec",
+			    renumber=no, offset=0, clobber=yes, merge=no,
+			    errval=0, verbose=no)
+			imdelete (temp, verify=no)
+		    }
+		}
+		print (arc2, >> done)
+
+		if (arctype == "shift") {
+		    reidentify (arcref2//extn, arc2,
+			interactive=no, section="middle line", shift=0.,
+			step=1, nsum=1, cradius=params.cradius,
+			threshold=params.threshold, nlost=100, newaps=no,
+			refit=no, trace=no, override=no, addfeatures=no,
+			database=database, plotfile=plotfile,
+			logfiles=logfile, verbose=verbose1)
+		} else {
+		    if (arcreplace != "") {
+			fd = arcreplace
+			while (fscan (fd, arc, arcms, str2) != EOF) {
+			    i = strlen (arc)
+			    if (i > n && substr (arc, i-n+1, i) == imtype)
+				arc = substr (arc, 1, i-n)
+			    if (arc != arc1)
+				    next
+			    arc = arcms
+			    if (i > n && substr (arc, i-n+1, i) == imtype)
+				arc = substr (arc, 1, i-n)
+			    arcms = arc // extn // imtype
+	
+			    if (access (arcms))
+				imdelete (arcms, verify=no)
+	
+			    if (!batch)
+			        print ("Extract arc spectrum ", arc)
+			    print ("Extract arc spectrum ", arc, >> logfile)
+			    apscript (arc, references=apref,
+				ansrecenter="NO", ansresize="NO", ansedit="NO",
+				anstrace="NO", nsubaps=params.nsubaps,
+				background="none", clean=no,
+				weights="none", verbose=verbose1)
+			    sapertures (arcms, apertures="",
+				apidtable=apidtable, wcsreset=no, verbose=no,
+				beam=INDEF, dtype=INDEF, w1=INDEF, dw=INDEF,
+				z=INDEF, aplow=INDEF, aphigh=INDEF, title=INDEF)
+			    if (response != "") {
+			        if (params.nsubaps == 1)
+				    sarith (arcms, "/", response, arcfms,
+					w1=INDEF, w2=INDEF,
+					apertures="", bands="", beams="",
+					apmodulus=0, reverse=no,
+					ignoreaps=no, format="multispec",
+					renumber=no, offset=0, clobber=yes,
+					merge=no, errval=0, verbose=no)
+			        else {
+				    blkrep (response, temp, 1, params.nsubaps)
+				    sarith (arcms, "/", temp, arcfms,
+					w1=INDEF, w2=INDEF,
+					apertures="", bands="", beams="",
+					apmodulus=0, reverse=no,
+					ignoreaps=yes, format="multispec",
+					renumber=no, offset=0, clobber=yes,
+					merge=no, errval=0, verbose=no)
+				    imdelete (temp, verify=no)
+			        }
+			    }
+			    scopy (arcms, arc2, w1=INDEF, w2=INDEF,
+				apertures=str2, bands="", beams="",
+				apmodulus=1000, offset=0, format="multispec",
+				clobber=yes, merge=yes, renumber=no,
+				verbose=yes, >> logfile)
+			    imdelete (arcms, verify=no)
+			}
+			fd = ""
+		    }
+		    reidentify (arcref1//extn, arc2,
+			interactive=!batch, section="middle line",
+			shift=0., step=1, nsum=1, cradius=params.cradius,
+			threshold=params.threshold, nlost=100,
+			refit=params.refit, trace=no, override=no,
+			addfeatures=params.addfeatures,
+			coordlist=params.coordlist, match=params.match,
+			maxfeatures=50, minsep=2., database=database,
+			plotfile=plotfile, logfiles=logfile,
+			verbose=verbose1)
+		}
+
+		# If not reextracting arcs based on object apertures
+		# then save the extracted arc to avoid doing it again.
+
+		if (arc1//extn != arc2)
+		    imdelete (arc2, verify=no)
+	    }
+    
+	    # Set the REFSPEC parameters for multispec spectrum.
+	    if (k == 1)
+		hedit (spec//".ms", "refspec"//j, arc2, add=yes,
+		    verify=no, show=no, update=yes)
+	    else
+		hedit (spec//".ms", "refspec"//j, arc2//" "//str1,
+		    add=yes, verify=no, show=no, update=yes)
+
+	    # Check for arc fibers in object spectra.
+	    if (arctype != "shift" && (arcaps != "" || arcbeams != "")) {
+	        scopy (spec//".ms", spec//"arc.ms", w1=INDEF, w2=INDEF,
+		    apertures=arcaps, bands="", beams=arcbeams, apmodulus=1000,
+		    offset=0, format="multispec", clobber=yes, merge=no,
+		    renumber=no, verbose=no, >& "dev$null")
+	        if (access (spec//"arc.ms"//imtype)) {
+		    if (!batch)
+		        print ("Reidentify arc fibers in ", spec,
+			    " with respect to ", arc1)
+		    print ("Reidentify arc fibers in ", spec,
+		        " with respect to ", arc1, >> logfile)
+		    delete (database//"/id"//spec//"arc.ms*", verify = no)
+		    reidentify (arc2, spec//"arc.ms", interactive=no,
+		        section="middle line", shift=0., step=1, nsum=1,
+			cradius=params.cradius, threshold=params.threshold,
+			nlost=100, refit=no, trace=no, override=no,
+			addfeatures=no, database=database,
+			plotfile=plotfile, logfiles=logfile,
+			verbose=verbose1)
+		    imdelete (spec//"arc.ms", verify=no)
+		    hedit (spec//".ms", "refshft"//j, spec//"arc.ms interp",
+		        add=yes, verify=no, show=no, update=yes)
+		    if (!savearcs)
+	                scopy (spec//".ms", "", w1=INDEF, w2=INDEF,
+			    apertures="!"//arcaps, bands="", beams=arcbeams,
+			    apmodulus=1000, offset=0, format="multispec",
+			    clobber=yes, merge=no, renumber=no,
+			    verbose=yes, >> logfile)
+	        }
+	    }
+	}
+end
diff --git a/noao/imred/src/fibers/doarcs.par b/noao/imred/src/fibers/doarcs.par
new file mode 100644
index 00000000..a93b16c6
--- /dev/null
+++ b/noao/imred/src/fibers/doarcs.par
@@ -0,0 +1,17 @@
+spec,f,a,"",,,
+response,f,a,"",,,
+arcref1,f,a,"",,,
+arcref2,f,a,"",,,
+extn,s,a,,,,
+arcreplace,f,a,"",,,
+apidtable,f,a,"",,,
+arcaps,s,a,,,,
+arcbeams,s,a,,,,
+savearcs,b,a,,,,
+reextract,b,a,,,,
+arcap,b,a,,,,
+logfile,f,a,"",,,
+batch,b,a,,,,
+done,f,a,"",,,
+fd,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/fibers/fibresponse.cl b/noao/imred/src/fibers/fibresponse.cl
new file mode 100644
index 00000000..2379fcc4
--- /dev/null
+++ b/noao/imred/src/fibers/fibresponse.cl
@@ -0,0 +1,261 @@
+# FIBRESPONSE -- Make a aperture response spectrum using a flat field
+# and a throughput file or image.
+
+procedure fibresponse (flat, throughput, apreference, response)
+
+string	flat			{prompt="Flat field spectrum"}
+string	throughput		{prompt="Throughput file or image"}
+string	apreference		{prompt="Aperture reference spectrum"}
+string	response		{prompt="Response spectrum"}
+
+bool	recenter = no		{prompt="Recenter apertures?"}
+bool	edit = yes		{prompt="Edit/review apertures?"}
+bool	trace = no		{prompt="Trace spectra?"}
+bool	clean = no		{prompt="Detect and replace bad pixels?"}
+bool	fitflat = no		{prompt="Fit and ratio flat field spectrum?"}
+bool	interactive = yes	{prompt="Fit flat field interactively?"}
+string	function = "spline3"	{prompt="Fitting function",
+				 enum="spline3|legendre|chebyshev|spline1"}
+int	order = 20		{prompt="Fitting function order", min=1}
+
+begin
+	string	imtype, mstype
+	file	flat2d, skyflat2d, apref, resp
+	file	temp1, temp2, log1, log2
+	int	n, ap, naxis
+	real	respval
+	struct	err
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	mstype = ".ms" // imtype
+	n = strlen (imtype)
+
+	flat2d = flat
+	skyflat2d = throughput
+	apref = apreference
+	resp = response
+	temp1 = mktemp ("tmp")
+	temp2 = mktemp ("tmp")
+
+	# Check required input and output.
+ 	if (resp == "" || resp == flat2d || resp == skyflat2d)
+ 	    error (1, "Bad response image name")
+	if (flat2d == "" && skyflat2d == "")
+	    error (1, "No flat field or throughput specified")
+
+	if (flat2d != "") {
+	    i = strlen (flat2d)
+	    if (i > n && substr (flat2d, i-n+1, i) == imtype)
+		flat2d = substr (flat2d, 1, i-n)
+	    if (!access (flat2d // imtype)) {
+		printf ("Flat field spectrum not found - %s%s\n",
+		    flat2d, imtype) | scan (err)
+		error (1, err // "\nCheck settting of imtype")
+	    }
+	}
+	if (skyflat2d != "") {
+	    i = strlen (skyflat2d)
+	    if (i > n && substr (skyflat2d, i-n+1, i) == imtype)
+	        skyflat2d = substr (skyflat2d, 1, i-n)
+	    if (!access (skyflat2d // imtype)) {
+		if (!access (skyflat2d)) {
+		    printf ("Throughput file or image not found - %s%s\n",
+			skyflat2d, imtype) | scan (err)
+		    error (1, err // "\nCheck settting of imtype")
+		}
+
+		if (flat2d == "") {
+		    i = strlen (apref)
+		    if (i > n && substr (apref, i-n+1, i) == imtype)
+			apref = substr (apref, 1, i-n)
+		    if (!access (apref // imtype))
+			error (1, "Aperture reference image required")
+		}
+	    }
+	}
+
+	# Set logging
+	tee.append = yes
+	if (logfile == "")
+	    log1 = "dev$null"
+	else
+	    log1 = logfile
+	if (verbose)
+	    log2 = "STDOUT"
+	else
+	    log2 = "dev$null"
+
+	# Initialize APSCRIPT
+	apscript.references = apref
+	if (recenter)
+	    apscript.ansrecenter = "YES"
+	else
+	    apscript.ansrecenter = "NO"
+	apscript.ansresize = "NO"
+	if (edit)
+	    apscript.ansedit = "yes"
+	else
+	    apscript.ansedit = "NO"
+	if (trace)
+	    apscript.anstrace = "YES"
+	else
+	    apscript.anstrace = "NO"
+	apscript.ansextract = "YES"
+
+	# If using a flat field extract it if necessary and possibly fit it
+	# and ratio the individual apertures by an overall smooth function
+
+	if (flat2d != "") {
+	    if (!access (flat2d // mstype)) {
+		print ("Extract flat field ", flat2d) | tee (log1)
+		if (flat2d != apref)
+		    apscript (flat2d, output=resp, background="none",
+			clean=clean, extras=no)
+		else
+		    apscript (flat2d, output=resp, ansrecenter="NO",
+			ansrecenter="NO", ansresize="NO", ansedit="NO",
+			anstrace="NO", background="none",
+			clean=clean, extras=no)
+	    } else
+		imcopy (flat2d//".ms", resp, verbose=no)
+
+	    if (fitflat) {
+		print ("Fit and ratio flat field ", flat2d) | tee (log1)
+		blkavg (resp, temp1, option="average", b1=1, b2=10000)
+		imcopy (temp1//"[*,1]", temp1, verbose=no)
+		fit1d (temp1, temp1, "fit", axis=1, interactive=interactive,
+		    sample="*", naverage=1, function=function, order=order,
+		    low_reject=0., high_reject=0., niterate=1, grow=0.,
+		    graphics="stdgraph")
+		sarith (resp, "/", temp1, resp, w1=INDEF, w2=INDEF,
+		    apertures="", bands="", beams="", apmodulus=0, reverse=no,
+		    ignoreaps=yes, format="multispec", renumber=no,
+		    offset=0, clobber=yes, merge=no, errval=0, verbose=no)
+		imdelete (temp1, verify=no)
+	    }
+	}
+
+	# If using a throughput image extract it if necessary.
+	# Apply it to the flat field if given and otherwise only
+	# compute the throughput through each aperture.
+
+	if (skyflat2d != "") {
+	    if (access (skyflat2d // imtype)) {
+		if (!access (skyflat2d // mstype)) {
+		    print ("Extract throughput image ", skyflat2d) | tee (log1)
+		    apscript (skyflat2d, output=temp1, background="none",
+			clean=clean, extras=no)
+		    temp2 = temp1
+		} else
+		    temp2 = skyflat2d // ".ms"
+
+		if (flat2d != "") {
+		    print ("Correct flat field to throughput image") |
+			tee (log1)
+		    sarith (temp2, "/", resp, temp1, w1=INDEF, w2=INDEF,
+			apertures="", bands="", beams="", apmodulus=0,
+			reverse=no, ignoreaps=no, format="multispec",
+			renumber=no, offset=0, clobber=yes, merge=no,
+			errval=0, verbose=no)
+		    fit1d (temp1, temp1, type="fit", axis=1,
+			interactive=no, sample="*", naverage=1,
+			function="legendre", order=1, niterate=0)
+		    sarith (resp, "*", temp1, resp, w1=INDEF, w2=INDEF,
+			apertures="", bands="", beams="", apmodulus=0,
+			reverse=no, ignoreaps=yes, format="multispec",
+			renumber=no, offset=0, clobber=yes, merge=no,
+			errval=0, verbose=no)
+		    imdelete (temp1, verify=no)
+		} else {
+		    print ("Compute aperture throughput from image") |
+			tee (log1)
+		    fit1d (temp2, resp, type="fit", axis=1,
+			interactive=no, sample="*", naverage=1,
+			function="legendre", order=1, niterate=0)
+		    if (temp2 == temp1)
+			imdelete (temp2, verify=no)
+		}
+
+	    # If a flat field and throughput file are used scale the average
+	    # flat field in each aperture to those values
+
+	    } else if (flat2d != "") {
+		print ("Correct flat field with throughput file ", skyflat2d) |
+		    tee (log1)
+		fit1d (resp, resp, type="ratio", axis=1,
+		    interactive=no, sample="*", naverage=1,
+		    function="legendre", order=1, niterate=0)
+
+		list = skyflat2d
+		while (fscan (list, ap, respval) != EOF) {
+		    sarith (resp, "*", respval, resp, w1=INDEF, w2=INDEF,
+			apertures=ap, bands="", beams="", apmodulus=0,
+			reverse=no, ignoreaps=no, format="multispec",
+			renumber=no, offset=0, clobber=yes, merge=yes,
+			errval=0., verbose=no, >& "dev$null")
+		}
+		list = ""
+
+	    # If only a throughput file is given create the response from the
+	    # aperture reference and set the aperture response to the specified
+	    # values.
+
+	    } else {
+		print ("Set aperture throughput using ", skyflat2d) | tee (log1)
+		if (!access (apref // mstype)) {
+		    apscript (apref, output=resp, ansrecenter="NO",
+			ansrecenter="NO", ansresize="NO", ansedit="NO",
+			anstrace="NO", background="none",
+			clean=no, extras=no)
+		    sarith (resp, "replace", "0", resp, w1=INDEF,
+			w2=INDEF, apertures="", bands="", beams="", apmodulus=0,
+			reverse=no, ignoreaps=no, format="multispec",
+			renumber=no, offset=0, clobber=yes, merge=yes,
+			errval=0., verbose=no)
+		} else
+		    sarith (apref//".ms", "replace", "0", resp, w1=INDEF,
+			w2=INDEF, apertures="", bands="", beams="", apmodulus=0,
+			reverse=no, ignoreaps=no, format="multispec",
+			renumber=no, offset=0, clobber=yes, merge=yes,
+			errval=0., verbose=no)
+
+		list = skyflat2d
+		while (fscan (list, ap, respval) != EOF) {
+		    sarith (resp, "replace", respval, resp, w1=INDEF, w2=INDEF,
+			apertures=ap, bands="", beams="", apmodulus=0,
+			reverse=no, ignoreaps=no, format="multispec",
+			renumber=no, offset=0, clobber=yes, merge=yes,
+			errval=0., verbose=no)
+		}
+		list = ""
+	    }
+	}
+
+	# The final response is normalized to overall unit mean and the
+	# average aperture response is printed.
+
+	print ("Create the normalized response ", resp) | tee (log1)
+	bscale (resp, resp, bzero="0.", bscale="mean", section="",
+	    step=1, upper=INDEF, lower=INDEF, verbose=yes) | tee (log1, >log2)
+	blkavg (resp, temp1, option="average", b1=10000, b2=1)
+	print ("Average aperture response:") | tee (log1, >log2)
+	naxis = 5
+	#hselect (temp1, "naxis", yes) | scan (naxis)
+	#if (naxis == 1)
+	#    listpixels (temp1) | tee (log1, >log2)
+	#else
+	#    listpixels (temp1//"[1,*]") | tee (log1, >log2)
+
+	hselect (temp1, "naxis", yes, > temp2)
+	list = temp2; ap = fscan (list, naxis)
+	if (naxis == 1)
+	    listpixels (temp1) | tee (log1, >log2)
+	else
+	    listpixels (temp1//"[1,*]") | tee (log1, >log2)
+	list = ""; delete (temp2, verify=no)
+
+	imdelete (temp1, verify=no)
+end
diff --git a/noao/imred/src/fibers/fibresponse.par b/noao/imred/src/fibers/fibresponse.par
new file mode 100644
index 00000000..9a59eb46
--- /dev/null
+++ b/noao/imred/src/fibers/fibresponse.par
@@ -0,0 +1,13 @@
+flat,s,a,,,,"Flat field spectrum"
+throughput,s,a,,,,"Throughput file or image"
+apreference,s,a,,,,"Aperture reference spectrum"
+response,s,a,,,,"Response spectrum"
+recenter,b,h,no,,,"Recenter apertures?"
+edit,b,h,yes,,,"Edit/review apertures?"
+trace,b,h,no,,,"Trace spectra?"
+clean,b,h,no,,,"Detect and replace bad pixels?"
+fitflat,b,h,no,,,"Fit and ratio flat field spectrum?"
+interactive,b,h,yes,,,"Fit flat field interactively?"
+function,s,h,"spline3",spline3|legendre|chebyshev|spline1,,"Fitting function"
+order,i,h,20,1,,"Fitting function order"
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/fibers/getspec.cl b/noao/imred/src/fibers/getspec.cl
new file mode 100644
index 00000000..84ce9a1c
--- /dev/null
+++ b/noao/imred/src/fibers/getspec.cl
@@ -0,0 +1,49 @@
+# GETSPEC -- Get spectra which are processed but are not extracted.
+# Strip the imtype extension.
+
+procedure getspec (images, output)
+
+string	images			{prompt="List of images"}
+file	output			{prompt="Output file of images"}
+bool	ccdproc			{prompt="Add CCDPROC keyword and continue?",
+				 mode="q"}
+struct	*fd
+
+begin
+	string	imtype, temp, image, system=""
+	int	n, n1
+
+	imtype = "." // envget ("imtype")
+	n = stridx (",", imtype)
+	if (n > 0)
+	    imtype = substr (imtype, 1, n-1)
+	n1 = strlen (imtype)
+
+	# Initialize files
+	set clobber=yes
+	sleep (> output)
+	set clobber=no
+
+	temp = mktemp ("tmp$iraf")
+	sections (images, option="fullname", > temp)
+	fd = temp
+	while (fscan (fd, image) != EOF) {
+	    hselect (image, "ccdproc", yes) | scan (system)
+	    if (nscan() == 0) {
+		printf ("%s: CCDPROC keyword not found.\n", image)
+		printf ("  Either run CCDPROC or add CCDPROC keyword with HEDIT.\n")
+		if (!ccdproc)
+		    error (1, "Exit")
+		hedit (image, "ccdproc", "DONE", add=yes, update=yes,
+		    verify=no, show=no)
+	    }
+	    hselect (image, "wat0_001", yes) | scanf ("system=%s", system)
+	    if (system=="equispec" || system=="multispec")
+		next
+	    n = strlen (image)
+	    if (n > n1 && substr (image, n-n1+1, n) == imtype)
+		image = substr (image, 1, n-n1)
+	    print (image, >> output)
+	}
+	fd = ""; delete (temp, verify=no)
+end
diff --git a/noao/imred/src/fibers/getspec.par b/noao/imred/src/fibers/getspec.par
new file mode 100644
index 00000000..e676c18e
--- /dev/null
+++ b/noao/imred/src/fibers/getspec.par
@@ -0,0 +1,5 @@
+images,s,a,,,,"List of images"
+output,f,a,,,,"Output file of images"
+ccdproc,b,q,,,,"Add CCDPROC keyword and continue?"
+fd,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/fibers/listonly.cl b/noao/imred/src/fibers/listonly.cl
new file mode 100644
index 00000000..ac215892
--- /dev/null
+++ b/noao/imred/src/fibers/listonly.cl
@@ -0,0 +1,237 @@
+# LISTONLY -- List processing to be done.
+#
+# This follows pretty much the same logic as the full procedure but doesn't
+# do anything but list the operations.
+
+procedure listonly (objects, apidtable, apref, flat, throughput, arcs1, arcs2,
+	scattered, dispcor, skysubtract, redo, update)
+
+string	objects = ""		{prompt="List of object spectra"}
+file	apidtable = ""		{prompt="Aperture ID table"}
+file	apref = ""		{prompt="Aperture reference spectrum"}
+file	flat = ""		{prompt="Flat field spectrum"}
+file	throughput = ""		{prompt="Throughput file or image"}
+string	arcs1 = ""		{prompt="List of arc spectra"}
+string	arcs2 = ""		{prompt="List of shift arc spectra"}
+
+bool	scattered		{prompt="Subtract scattered light?"}
+bool	dispcor			{prompt="Dispersion correct spectra?"}
+bool	skysubtract		{prompt="Subtract sky?"}
+bool	redo = no		{prompt="Redo operations if previously done?"}
+bool	update = yes		{prompt="Update spectra if cal data changes?"}
+
+struct	*fd1
+struct	*fd2
+
+begin
+	string	imtype, mstype, extn
+	string	spec, arcref1, arcref2
+	string	specms, arcref1ms, arcref2ms, response
+	string	objs, temp, done, str
+	bool	reextract, newaps, newresp, newdisp, scat, extract, disp, sky
+	int	i, j, n, dc
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	mstype = ".ms" // imtype
+	n = strlen (imtype)
+
+	objs = mktemp ("tmp$iraf")
+	temp = mktemp ("tmp$iraf")
+	done = mktemp ("tmp$iraf")
+
+	if (apidtable != "") {
+	    j = strlen (apidtable)
+	    for (i=1; i<=j && substr(apidtable,i,i)==" "; i+=1);
+	    apidtable = substr (apidtable, i, j)
+	}
+	i = strlen (apidtable)
+	if (i == 0)
+	    extn = ".ms"
+	else {
+	    extn = apidtable
+	    while (yes) {
+		i = stridx ("/$]", extn)
+		if (i == 0)
+		    break
+		j = strlen (extn)
+		extn = substr (extn, i+1, j)
+	    }
+	    extn = extn // ".ms"
+	}
+
+	newaps = no
+	newresp = no
+	newdisp = no
+
+	i = strlen (apref)
+	if (i > n && substr (apref, i-n+1, i) == imtype)
+	    apref = substr (apref, 1, i-n)
+
+	reextract = redo
+	if (reextract || !access (database // "/ap" // apref // extn)) {
+	    print ("Set reference aperture for ", apref)
+	    newaps = yes
+	}
+
+	i = strlen (flat)
+	if (i > n && substr (flat, i-n+1, i) == imtype)
+	    flat = substr (flat, 1, i-n)
+	if (flat != "") {
+	    scat = no
+	    if (scattered) {
+		if (redo && access (flat//"noscat"//imtype))
+		    hselect (flat//"noscat", "apscatte", yes) | scan (str)
+		else
+		    hselect (flat, "apscatte", yes) | scan (str)
+		if (nscan() == 0)
+		    scat = yes
+	    }
+	    if (scat)
+		print ("Subtract scattered light from ", flat)
+	}
+
+	spec = throughput
+	i = strlen (spec)
+	if (i > n && substr (spec, i-n+1, i) == imtype)
+	    spec = substr (spec, 1, i-n)
+	if (spec != "") {
+	    scat = no
+	    if (scattered) {
+		if (redo && access (flat//"noscat"//imtype))
+		    hselect (flat//"noscat", "apscatte", yes) | scan (str)
+		else
+		    hselect (flat, "apscatte", yes) | scan (str)
+		if (nscan() == 0)
+		    scat = yes
+	    }
+	    if (scat)
+		print ("Subtract scattered light from ", spec)
+	}
+
+	response = ""
+	if (flat != "" || spec != "") {
+	    if (extn == ".ms")
+		response = flat // spec // "norm.ms"
+	    else
+		response = flat // spec // extn
+
+	    reextract = redo || (update && newaps)
+	    if (reextract || !access (response // imtype) || (redo && scat)) {
+	        print ("Create response function ", response)
+	        newresp = yes
+	    }
+	}
+
+	if (dispcor) {
+	    getspec (arcs1, temp)
+	    fd1 = temp
+	    if (fscan (fd1, arcref1) == EOF)
+		error (1, "No reference arcs")
+	    fd1 = ""; delete (temp, verify=no)
+	    arcref1ms = arcref1 // extn
+
+	    getspec (arcs2, temp)
+	    fd1 = temp
+	    if (fscan (fd1, arcref2) == EOF)
+		arcref2 = ""
+	    fd1 = ""; delete (temp, verify=no)
+	    arcref2ms = arcref2 // extn
+
+	    reextract = redo || (update && newaps)
+	    if (reextract || !access (arcref1ms//imtype)) {
+	        print ("Extract arc reference image ", arcref1)
+	        print ("Determine dispersion solution for ", arcref1)
+	        newdisp = yes
+	    } else {
+	        hselect (arcref1ms, "dclog1", yes, > temp)
+	        fd1 = temp
+		dc = -1
+	        i = fscan (fd1, dc)
+	        fd1 = ""; delete (temp, verify=no)
+	        if (i < 1) {
+	            print ("Determine dispersion solution for ", arcref1)
+	            newdisp = yes
+	        }
+	    }
+	    print (arcref1, > done)
+
+	    if (arcref2 != "") {
+	        if (reextract || !access (arcref2ms//imtype) || newdisp) {
+		    print ("Extract shift arc reference image ", arcref2)
+	            print ("Determine dispersion solution for ", arcref2)
+		} else {
+		    hselect (arcref2ms, "dclog1", yes, > temp)
+		    fd1 = temp
+		    dc = -1
+		    i = fscan (fd1, dc)
+		    fd1 = ""; delete (temp, verify=no)
+		    if (i < 1)
+	                print ("Determine dispersion solution for ", arcref2)
+		}
+	    }
+	    print (arcref2, >> done)
+	}
+
+	reextract = redo || (update && (newaps || newresp || newdisp))
+	getspec (objects, objs)
+	fd1 = objs
+	while (fscan (fd1, spec) != EOF) {
+	    if (access (done)) {
+	        fd2 = done
+	        while (fscan (fd2, specms) != EOF)
+		    if (spec == specms)
+		        break
+	        if (spec == specms)
+		    next
+	        fd2 = ""
+	    }
+
+	    specms = spec // mstype
+
+	    scat = no
+	    extract = no
+	    disp = no
+	    sky = no
+	    if (scattered) {
+		if (redo && access (spec//"noscat"//imtype))
+		    hselect (spec//"noscat", "apscatte", yes) | scan (str)
+		else
+		    hselect (spec, "apscatte", yes) | scan (str)
+		if (nscan() == 0)
+		    scat = yes
+	    }
+	    if (reextract || !access (specms) || (redo && scat))
+		extract = yes
+	    else {
+		hselect (specms, "dclog1", yes) | scan (str)
+		if (nscan() == 0)
+		    disp = yes
+		else
+		    extract = update && newdisp
+		hselect (specms, "skysub", yes) | scan (str)
+		if (nscan() == 0)
+		    sky = skysubtract
+	    }
+		
+	    if (extract) {
+		disp = dispcor
+		sky = skysubtract
+	    }
+		    
+	    if (scat)
+		print ("Subtract scattered light from ", spec)
+	    if (extract)
+		print ("Extract object spectrum ", spec)
+	    if (disp)
+	        print ("Dispersion correct ", spec)
+	    if (sky)
+		print ("Sky subtract ", spec)
+	}
+	fd1 = ""; delete (objs, verify=no)
+
+	if (access (done))
+	    delete (done, verify=no)
+end
diff --git a/noao/imred/src/fibers/listonly.par b/noao/imred/src/fibers/listonly.par
new file mode 100644
index 00000000..aa52691e
--- /dev/null
+++ b/noao/imred/src/fibers/listonly.par
@@ -0,0 +1,15 @@
+objects,s,a,"",,,"List of object spectra"
+apidtable,f,a,"",,,"Aperture ID table"
+apref,f,a,"",,,"Aperture reference spectrum"
+flat,f,a,"",,,"Flat field spectrum"
+throughput,f,a,"",,,"Throughput file or image"
+arcs1,s,a,"",,,"List of arc spectra"
+arcs2,s,a,"",,,"List of shift arc spectra"
+scattered,b,a,,,,"Subtract scattered light?"
+dispcor,b,a,,,,"Dispersion correct spectra?"
+skysubtract,b,a,,,,"Subtract sky?"
+redo,b,a,no,,,"Redo operations if previously done?"
+update,b,a,yes,,,"Update spectra if cal data changes?"
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/fibers/mkfibers.cl b/noao/imred/src/fibers/mkfibers.cl
new file mode 100644
index 00000000..b7ffdac2
--- /dev/null
+++ b/noao/imred/src/fibers/mkfibers.cl
@@ -0,0 +1,167 @@
+# MKFIBERS - Make multifiber examples
+
+procedure mkfibers (image)
+
+file	image				{prompt="Image name"}
+string	type="object"			{prompt="Object type",
+		 enum="object|objnosky|sky|flat|henear|ehenear|ohenear|mercury"}
+file	fibers=""			{prompt="Fiber data file"}
+string	title="Multifiber artificial image"	{prompt="Title"}
+file	header="artdata$stdhdr.dat"	{prompt="Header keyword file"}
+int	ncols=400			{prompt="Number of columns"}
+int	nlines=512			{prompt="Number of lines"}
+real	wstart=4210.			{prompt="Starting wavelength"}
+real	wend=7362.			{prompt="Ending wavelength"}
+int	seed=1				{prompt="Noise seed"}
+
+begin
+	int	i, ap, beam
+	real	ar
+	file	out, obj, sky, arc, dat
+	string	htype, imtype
+
+	out = image
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	if (access (out) || access (out//imtype))
+	    return
+
+	print ("Creating image ", out, " ...")
+	
+	obj = mktemp ("art")
+	sky = mktemp ("art")
+	arc = mktemp ("art")
+	dat = mktemp ("art")
+	
+	list = fibers
+	if (type == "object") {		# Object spectrum + sky
+	    htype = "object"
+	    mk1dspec (obj, output="", ap=1, rv=0., z=no, ncols=nlines, naps=1,
+		wstart=wstart, wend=wend, continuum=1000., slope=0.,
+		temperature=7000., lines="", nlines=50, peak=-0.5,
+		profile="gaussian", gfwhm=24, seed=2, comments=no, header="")
+	    mk1dspec (sky, output="", ap=1, rv=0., z=no, ncols=nlines, naps=1,
+		wstart=wstart, wend=wend, continuum=1000., slope=0.,
+		temperature=5800., lines="", nlines=20, peak=1.,
+		profile="gaussian", gfwhm=12, seed=1, comments=no, header="")
+	    imarith (obj, "+", sky, obj, verbose=no, noact=no)
+	    mk1dspec (arc, output="", ap=1, rv=0., z=no, ncols=nlines, naps=1,
+		wstart=wstart, wend=wend, continuum=0.8, slope=0.,
+		temperature=0., lines="mkexamples$henear2.dat",
+		profile="gaussian", gfwhm=14, comments=no, header="")
+	    mk1dspec (arc, output="", ap=1, rv=0., z=no, continuum=20,
+		slope=0., temperature=0., lines="", nlines=0,
+		comments=no, header="")
+	    while (fscan (list, ap, beam, line) != EOF) {
+		if (beam == 0)
+		    print (sky, " ", line, >> dat)
+		else if (beam == 1)
+		    print (obj, " ", line, >> dat)
+		else if (beam == 2)
+		    print (arc, " ", line, >> dat)
+	    }
+	} else if (type == "objnosky") {	# Object spectrum
+	    htype = "object"
+	    mk1dspec (obj, output="", ap=1, rv=0., z=no, ncols=nlines, naps=1,
+		wstart=wstart, wend=wend, continuum=1000., slope=0.,
+		temperature=7000., lines="", nlines=50, peak=-0.5,
+		profile="gaussian", gfwhm=24, seed=2, comments=no, header="")
+	    mk1dspec (arc, output="", ap=1, rv=0., z=no, ncols=nlines, naps=1,
+		wstart=wstart, wend=wend, continuum=0.8, slope=0.,
+		temperature=0., lines="mkexamples$henear2.dat",
+		profile="gaussian", gfwhm=14, comments=no, header="")
+	    mk1dspec (arc, output="", ap=1, rv=0., z=no, continuum=20,
+		slope=0., temperature=0., lines="", nlines=0,
+		comments=no, header="")
+	    while (fscan (list, ap, beam, line) != EOF) {
+		if (beam == 1)
+		    print (obj, " ", line, >> dat)
+		else if (beam == 2)
+		    print (arc, " ", line, >> dat)
+	    }
+	} else if (type == "sky") {	# Sky only
+	    htype = "object"
+	    mk1dspec (sky, output="", ap=1, rv=0., z=no, ncols=nlines, naps=1,
+		wstart=wstart, wend=wend, continuum=1000., slope=0.,
+		temperature=5800., lines="", nlines=20, peak=1.,
+		profile="gaussian", gfwhm=12, seed=1, comments=no, header="")
+	    while (fscan (list, ap, beam, line) != EOF)
+		print (sky, " ", line, >> dat)
+	} else if (type == "flat") {	# Flat field
+	    htype = "flat"
+	    mk1dspec (obj, output="", ap=1, rv=0., z=no, ncols=nlines, naps=1,
+		wstart=wstart, wend=wend, continuum=10000., slope=0.,
+		temperature=8000., lines="", nlines=0, comments=no, header="")
+	    while (fscan (list, ap, beam, line) != EOF)
+		print (obj, " ", line, >> dat)
+	} else if (type == "henear") {	# HE-NE-AR
+	    htype = "comp"
+	    mk1dspec (arc, output="", ap=1, rv=0., z=no, ncols=nlines, naps=1,
+		wstart=wstart, wend=wend, continuum=0.8, slope=0.,
+		temperature=0., lines="mkexamples$henear2.dat",
+		profile="gaussian", gfwhm=14, comments=no, header="")
+	    mk1dspec (arc, output="", ap=1, rv=0., z=no, continuum=20,
+		slope=0., temperature=0., lines="", nlines=0,
+		comments=no, header="")
+	    while (fscan (list, ap, beam, line) != EOF)
+		print (arc, " ", line, >> dat)
+	} else if (type == "ehenear") {	# HE-NE-AR Even fibers
+	    htype = "comp"
+	    mk1dspec (arc, output="", ap=1, rv=0., z=no, ncols=nlines, naps=1,
+		wstart=wstart, wend=wend, continuum=0.8, slope=0.,
+		temperature=0., lines="mkexamples$henear2.dat",
+		profile="gaussian", gfwhm=14, comments=no, header="")
+	    mk1dspec (arc, output="", ap=1, rv=0., z=no, continuum=20,
+		slope=0., temperature=0., lines="", nlines=0,
+		comments=no, header="")
+	    while (fscan (list, ap, beam, line) != EOF) {
+		if (mod (ap, 2) == 0) {
+		    print (arc, " ", line, >> dat)
+		}
+	    }
+	} else if (type == "ohenear") {	# HE-NE-AR Odd fibers
+	    htype = "comp"
+	    mk1dspec (arc, output="", ap=1, rv=0., z=no, ncols=nlines, naps=1,
+		wstart=wstart, wend=wend, continuum=0.8, slope=0.,
+		temperature=0., lines="mkexamples$henear2.dat",
+		profile="gaussian", gfwhm=14, comments=no, header="")
+	    mk1dspec (arc, output="", ap=1, rv=0., z=no, continuum=20,
+		slope=0., temperature=0., lines="", nlines=0,
+		comments=no, header="")
+	    while (fscan (list, ap, beam, line) != EOF) {
+		if (mod (ap, 2) == 1) {
+		    print (arc, " ", line, >> dat)
+		}
+	    }
+	} else if (type == "mercury") {	# Emission lines
+	    htype = "comp"
+	    mk1dspec (arc, output="", ap=1, rv=0., z=no, ncols=nlines, naps=1,
+		wstart=wstart, wend=wend, continuum=0., slope=0.,
+		temperature=0., lines="", nlines=30, peak=10000.,
+		profile="gaussian", gfwhm=7, seed=i, comments=no, header="")
+	    mk1dspec (arc, output="", ap=1, rv=0., z=no, continuum=20,
+		slope=0., temperature=0., lines="", nlines=0,
+		comments=no, header="")
+	    while (fscan (list, ap, beam, line) != EOF) {
+		print (arc, " ", line, >> dat)
+	    }
+	}
+	list = ""
+	
+	mk2dspec (out, output="", model=dat, ncols=ncols, nlines=nlines,
+	    title=title, header=header, comments=no)
+	hedit (out, "imagetyp", htype, update=yes, add=no, delete=no,
+	    show=no, verify=no)
+	    
+	
+	mknoise (out, output="", background=0., gain=1., rdnoise=3.,
+	    poisson=yes, seed=seed, cosrays="", ncosrays=0, energy=30000.,
+	    radius=0.5, ar=1., pa=0., comments=no)
+	
+	imdelete (obj, verify=no, >& "dev$null")
+	imdelete (sky, verify=no, >& "dev$null")
+	imdelete (arc, verify=no, >& "dev$null")
+	delete (dat, verify=no, >& "dev$null")
+end
diff --git a/noao/imred/src/fibers/mkfibers.par b/noao/imred/src/fibers/mkfibers.par
new file mode 100644
index 00000000..9ba33353
--- /dev/null
+++ b/noao/imred/src/fibers/mkfibers.par
@@ -0,0 +1,11 @@
+image,f,a,"",,,"Image name"
+type,s,h,"object",object|objnosky|sky|flat|henear|ehenear|ohenear|mercury,,"Object type"
+fibers,f,h,"",,,"Fiber data file"
+title,s,h,"Multifiber artificial image",,,"Title"
+header,f,h,"artdata$stdhdr.dat",,,"Header keyword file"
+ncols,i,h,400,,,"Number of columns"
+nlines,i,h,512,,,"Number of lines"
+wstart,r,h,4210.,,,"Starting wavelength"
+wend,r,h,7362.,,,"Ending wavelength"
+seed,i,h,1,,,"Noise seed"
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/fibers/params.par b/noao/imred/src/fibers/params.par
new file mode 100644
index 00000000..bf41e8ec
--- /dev/null
+++ b/noao/imred/src/fibers/params.par
@@ -0,0 +1,75 @@
+line,i,h,INDEF,,,Default dispersion line
+nsum,i,h,10,,,Number of dispersion lines to sum or median
+width,r,h,,,,Width of profiles
+minsep,r,h,1.,,,Minimum separation between spectra
+maxsep,r,h,100000.,,,Maximum separation between spectra
+order,s,h,"increasing","increasing|decreasing",,"Order of apertures"
+extras,b,h,no,,,"Extract sky, sigma, etc.?
+
+-- DEFAULT APERTURE LIMITS --"
+lower,r,h,-3.,,,"Lower aperture limit relative to center"
+upper,r,h,3.,,,"Upper aperture limit relative to center
+
+-- AUTOMATIC APERTURE RESIZING PARAMETERS --"
+ylevel,r,h,0.05,,,"Fraction of peak or intensity for resizing"
+peak,b,h,yes,,,"Is ylevel a fraction of the peak?"
+bkg,b,h,yes,,,"Subtract background for resizing?"
+avglimits,b,h,no,,,"Average limits over all apertures?
+
+-- TRACE PARAMETERS --"
+t_step,i,h,10,,,"Tracing step"
+t_function,s,h,"spline3","chebyshev|legendre|spline1|spline3",,"Trace fitting function"
+t_order,i,h,2,,,"Trace fitting function order"
+t_niterate,i,h,1,0,,"Trace rejection iterations"
+t_low,r,h,3.,0.,,"Trace lower rejection sigma"
+t_high,r,h,3.,0.,,"Trace upper rejection sigma
+
+-- SCATTERED LIGHT PARAMETERS --"
+buffer,r,h,1.,0.,,Buffer distance from apertures
+apscat1,pset,h,"",,,Fitting parameters across the dispersion
+apscat2,pset,h,"",,,"Fitting parameters along the dispersion
+
+-- APERTURE EXTRACTION PARAMETERS --"
+weights,s,h,"none","none|variance",,Extraction weights (none|variance)
+pfit,s,h,"fit1d","fit1d|fit2d",,Profile fitting algorithm (fit1d|fit2d)
+readnoise,s,h,0.,,,Read out noise sigma (photons)
+gain,s,h,1.,,,Photon gain (photons/data number)
+lsigma,r,h,3.,,,Lower rejection threshold
+usigma,r,h,3.,,,Upper rejection threshold
+nsubaps,i,h,1,1,,"Number of subapertures
+
+-- FLAT FIELD FUNCTION FITTING PARAMETERS --"
+f_interactive,b,h,yes,,,"Fit flat field interactively?"
+f_function,s,h,"spline3",spline3|legendre|chebyshev|spline1,,"Fitting function"
+f_order,i,h,20,1,,"Fitting function order
+
+-- ARC DISPERSION FUNCTION PARAMETERS --"
+threshold,r,h,10.,0.,,"Minimum line contrast threshold"
+coordlist,f,h,linelist$idhenear.dat,,,"Line list"
+match,r,h,-3.,,,"Line list matching limit in Angstroms"
+fwidth,r,h,4.,,,"Arc line widths in pixels"
+cradius,r,h,10.,,,Centering radius in pixels
+i_function,s,h,"chebyshev","legendre|chebyshev|spline1|spline3",,"Coordinate function"
+i_order,i,h,3,1,,"Order of dispersion function"
+i_niterate,i,h,2,0,,"Rejection iterations"
+i_low,r,h,3.,0.,,"Lower rejection sigma"
+i_high,r,h,3.,0.,,"Upper rejection sigma"
+refit,b,h,yes,,,"Refit coordinate function when reidentifying?"
+addfeatures,b,h,no,,,"Add features when reidentifying?
+
+-- AUTOMATIC ARC ASSIGNMENT PARAMETERS --"
+select,s,h,"interp",,,"Selection method for reference spectra"
+sort,s,h,"jd",,,"Sort key"
+group,s,h,"ljd",,,"Group key"
+time,b,h,no,,,"Is sort key a time?"
+timewrap,r,h,17.,0.,24.,"Time wrap point for time sorting
+
+-- DISPERSION CORRECTION PARAMETERS --"
+linearize,b,h,yes,,,Linearize (interpolate) spectra?
+log,b,h,no,,,"Logarithmic wavelength scale?"
+flux,b,h,yes,,,"Conserve flux?
+
+-- SKY SUBTRACTION PARAMETERS --"
+combine,s,h,"average","average|median",,Type of combine operation
+reject,s,h,"avsigclip","none|minmax|avsigclip",,"Sky rejection option"
+scale,s,h,"none","none|mode|median|mean",,"Sky scaling option"
diff --git a/noao/imred/src/fibers/proc.cl b/noao/imred/src/fibers/proc.cl
new file mode 100644
index 00000000..a55039d8
--- /dev/null
+++ b/noao/imred/src/fibers/proc.cl
@@ -0,0 +1,707 @@
+# PROC -- Process spectra from 2D to wavelength calibrated 1D.
+# This program combines the operations of extraction, flat fielding,
+# fiber throughput correction, dispersion correction, and sky subtraction
+# in as simple and noninteractive way as possible.  Certain assumptions
+# are made about the data and the output.  A blank sky image, called a
+# sky flat, may be used to determine the instrument throughput.  The data
+# must all share the same position on the 2D image and the same
+# dispersion solution apart from small instrumental changes which can be
+# tracked automatically.
+
+procedure proc (objects, apref, flat, throughput, arcs1, arcs2, arcreplace,
+	arctable, fibers, apidtable, crval, cdelt, objaps, skyaps, arcaps,
+	objbeams, skybeams, arcbeams, scattered, fitflat, recenter, edit,
+	trace, arcap, clean, dispcor, savearcs, skyalign, skysubtract,
+	skyedit, saveskys, splot, redo, update, batch, listonly)
+
+string	objects			{prompt="List of object spectra"}
+
+file	apref			{prompt="Aperture reference spectrum"}
+file	flat			{prompt="Flat field spectrum"}
+file	throughput		{prompt="Throughput file or image (optional)"}
+string	arcs1			{prompt="List of arc spectra"}
+string	arcs2			{prompt="List of shift arc spectra"}
+file	arcreplace		{prompt="Special aperture replacements"}
+file	arctable		{prompt="Arc assignment table (optional)\n"}
+
+int	fibers			{prompt="Number of fibers"}
+file	apidtable		{prompt="Aperture identifications"}
+string	crval = "INDEF"		{prompt="Approximate wavelength"}
+string	cdelt = "INDEF"		{prompt="Approximate dispersion"}
+string	objaps			{prompt="Object apertures"}
+string	skyaps			{prompt="Sky apertures"}
+string	arcaps			{prompt="Arc apertures"}
+string	objbeams		{prompt="Object beam numbers"}
+string	skybeams		{prompt="Sky beam numbers"}
+string	arcbeams		{prompt="Arc beam numbers\n"}
+
+bool	scattered		{prompt="Subtract scattered light?"}
+bool	fitflat			{prompt="Fit and ratio flat field spectrum?"}
+bool	recenter		{prompt="Recenter object apertures?"}
+bool	edit			{prompt="Edit/review object apertures?"}
+bool	trace			{prompt="Trace object spectra?"}
+bool	arcap			{prompt="Use object apertures for arcs?"}
+bool	clean			{prompt="Detect and replace bad pixels?"}
+bool	dispcor			{prompt="Dispersion correct spectra?"}
+bool	savearcs		{prompt="Save internal arcs?"}
+bool	skyalign		{prompt="Align sky lines?"}
+bool	skysubtract		{prompt="Subtract sky?"}
+bool	skyedit			{prompt="Edit the sky spectra?"}
+bool	saveskys		{prompt="Save sky spectra?"}
+bool	splot			{prompt="Plot the final spectrum?"}
+bool	redo			{prompt="Redo operations if previously done?"}
+bool	update			{prompt="Update spectra if cal data changes?"}
+bool	batch			{prompt="Extract objects in batch?"}
+bool	listonly		{prompt="List steps but don't process?\n"}
+
+real	datamax = INDEF		{prompt="Max data value / cosmic ray threshold"}
+
+string	ansskyedit = "yes"	{prompt="Edit the sky spectra?", mode="q"}
+bool	newaps, newresp, newdisp, newarcs, dobatch
+
+string	anssplot = "yes"	{prompt="Splot spectrum?", mode="q",
+				 enum="no|yes|NO|YES"}
+
+string	extn = ".ms"		{prompt="Extraction extension"}
+struct	*fd1, *fd2, *fd3
+
+begin
+	string	imtype, mstype
+	string	arcref1, arcref2, spec, arc, align=""
+	string	arcref1ms, arcref2ms, specms, arcms, response
+	string	objs, temp, temp1, done
+	string	str1, str2, str3, str4, arcrefs, log1, log2
+	bool	scat, reextract, extract, disp, disperr, sky, log
+	bool	skyedit1, skyedit2, splot1, splot2
+	int	i, j, n, nspec
+	struct	err
+
+	# Call a separate task to do the listing to minimize the size of
+	# this script and improve it's readability.
+
+	dobatch = no
+	if (listonly) {
+	    listonly (objects, apidtable, apref, flat, throughput, arcs1, arcs2,
+		scattered, dispcor, skysubtract, redo, update)
+	    bye
+	}
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	mstype = ".ms" // imtype
+	n = strlen (imtype)
+
+	# Temporary files used repeatedly in this script.  Under some
+	# abort circumstances these files may be left behind.
+
+	objs = mktemp ("tmp$iraf")
+	temp = mktemp ("tmp$iraf")
+	temp1 = mktemp ("tmp$iraf")
+	done = mktemp ("tmp$iraf")
+
+	if (apidtable != "") {
+	    i = strlen (apidtable)
+	    if (i > n && substr (apidtable, i-n+1, i) == imtype) {
+		apidtable = substr (apidtable, 1, i-n)
+		i = strlen (apidtable)
+	    }
+	    for (j=1; j<=i && substr(apidtable,j,j)==" "; j+=1);
+	    apidtable = substr (apidtable, j, i)
+	}
+	i = strlen (apidtable)
+	if (i == 0)
+	    extn = ".ms"
+	else {
+	    extn = apidtable
+	    while (yes) {
+		i = stridx ("/$]", extn)
+		if (i == 0)
+		    break
+		j = strlen (extn)
+		extn = substr (extn, i+1, j)
+	    }
+	    extn = extn // ".ms"
+	}
+
+	# Get query parameter.
+	getspec (objects, objs)
+	if (arctable == "" || arctable == " ") {
+	    if (arcs2 == "" || arcs2 == " ")
+	        arcrefs = arcs1
+	    else
+		arcrefs = arcs2
+	} else
+	    arcrefs = arctable
+	arcref1 = ""
+	arcref2 = ""
+
+	# Rather than always have switches on the logfile and verbose flags
+	# we use TEE and set a file to "dev$null" if output is not desired.
+	# We must check for the null string to signify no logfile.
+
+	tee.append = yes
+	if (logfile == "")
+	    log1 = "dev$null"
+	else
+	    log1 = logfile
+	if (verbose)
+	    log2 = "STDOUT"
+	else
+	    log2 = "dev$null"
+
+	# If the update switch is used changes in the calibration data
+	# can cause images to be reprocessed (if they are in the object
+	# list).  Possible changes are in the aperture definitions,
+	# response function, dispersion solution, and sensitivity
+	# function.  The newarcs flag is used to only go through the arc
+	# image headers once setting the reference spectrum, airmass, and
+	# UT.
+
+	newaps = no
+	newresp = no
+	newdisp = no
+	newarcs = yes
+
+	# Check if there are aperture definitions in the database and
+	# define them if needed.  This is usually somewhat interactive.
+	# Delete the database entry to start fresh if we enter this
+	# because of a redo.  Set the newaps flag in case an update is
+	# desired.
+
+	i = strlen (apref)
+	if (i > n && substr (apref, i-n+1, i) == imtype)
+	    apref = substr (apref, 1, i-n)
+
+	getspec (apref, temp)
+	fd1 = temp
+	if (fscan (fd1, apref) == EOF)
+	    error (1, "No aperture reference")
+	fd1 = ""; delete (temp, verify=no)
+
+	# Initialize
+	apscript.saturation = INDEF
+	apscript.references = apref
+	apscript.profiles = ""
+	apscript.apidtable = apidtable
+	apscript.nfind = fibers
+	apscript.clean = clean
+	if (splot) {
+	    splot1 = yes
+	    splot2 = yes
+	} else {
+	    splot1 = no
+	    splot2 = no
+	}
+
+	reextract = redo
+	if (reextract || !access (database // "/ap" // apref // extn)) {
+	    if (!access (apref // imtype)) {
+		printf ("Aperture reference spectrum not found - %s%s\n",
+		    apref, imtype) | scan (err)
+		error (1, err // "\nCheck settting of imtype")
+	    }
+	    print ("Set reference apertures for ", apref) | tee (log1)
+	    if (access (database // "/ap" // apref))
+		delete (database // "/ap" // apref, verify=no)
+	    if (access (database // "/ap" // apref//extn))
+		delete (database // "/ap" // apref // extn, verify=no)
+	    apscript.ansresize = "yes"
+	    apscript.ansedit = "yes"
+	    apscript.ansfittrace = "yes"
+	    apscript (apref, references="", ansfind="YES", ansrecenter="NO",
+		anstrace="YES", ansextract="NO")
+	    newaps = yes
+	    copy (database//"/ap"//apref, database//"/ap"//apref//extn,
+		verbose=no)
+	} else {
+	    if (access (database // "/ap" // apref))
+		delete (database // "/ap" // apref, verify=no)
+	    copy (database//"/ap"//apref//extn, database//"/ap"//apref,
+		verbose=no)
+	}
+
+	if (recenter)
+	    apscript.ansrecenter = "YES"
+	else
+	    apscript.ansrecenter = "NO"
+	apscript.ansresize = "NO"
+	if (edit)
+	    apscript.ansedit = "yes"
+	else
+	    apscript.ansedit = "NO"
+	if (trace)
+	    apscript.anstrace = "YES"
+	else
+	    apscript.anstrace = "NO"
+	if (scattered) {
+	    apscript.ansfitscatter = "yes"
+	    apscript.ansfitsmooth = "yes"
+	}
+	apscript.ansfittrace = "NO"
+	apscript.ansextract = "YES"
+	apscript.ansreview = "NO"
+	if (skyedit) {
+	    skyedit1 = yes
+	    skyedit2 = yes
+	} else {
+	    skyedit1 = no
+	    skyedit2 = no
+	}
+
+	# The next step is to setup the scattered light correction if needed.
+	# We use the flat field image for the interactive setting unless
+	# one is not used and then we use the aperture reference.
+	# If these images have been  scattered light corrected we assume the
+	# scattered light functions parameters are correctly set.
+
+	i = strlen (flat)
+	if (i > n && substr (flat, i-n+1, i) == imtype)
+	    flat = substr (flat, 1, i-n)
+
+	if (flat != "")
+	    spec = flat
+	else
+	    spec = apref
+
+	getspec (spec, temp)
+	fd1 = temp
+	if (fscan (fd1, spec) == EOF)
+	    error (1, "No flat field")
+	fd1 = ""; delete (temp, verify=no)
+
+	scat = no
+	if (scattered) {
+	    if (redo && access (spec//"noscat"//imtype)) {
+		imdelete (spec, verify=no)
+		imrename (spec//"noscat", spec)
+	    }
+	    hselect (spec, "apscatte", yes) | scan (str1)
+	    if (nscan() == 0)
+		scat = yes
+	}
+	if (scat) {
+	    print ("Subtract scattered light from ", spec) | tee (log1)
+	    #apscript.ansfitscatter = "yes"
+	    #apscript.ansfitsmooth = "yes"
+	    imrename (spec, spec//"noscat")
+	    apscript (spec//"noscat", output=spec, ansextract="NO",
+		ansscat="YES", anssmooth="YES")
+	    #apscript.ansfitscatter = "NO"
+	    #apscript.ansfitsmooth = "NO"
+	}
+
+	# The next step is to process the flat field image which is used
+	# as a flat field and a throughput correction.
+
+	spec = throughput
+	i = strlen (spec)
+	if (i > n && substr (spec, i-n+1, i) == imtype)
+	    spec = substr (spec, 1, i-n)
+	specms = spec // mstype
+
+	if (spec != "" && access (spec//imtype)) {
+	    getspec (spec, temp)
+	    fd1 = temp
+	    if (fscan (fd1, spec) == EOF)
+		error (1, "No flat field")
+	    fd1 = ""; delete (temp, verify=no)
+
+	    scat = no
+	    if (scattered) {
+		if (redo && access (spec//"noscat"//imtype)) {
+		    imdelete (spec, verify=no)
+		    imrename (spec//"noscat", spec)
+		}
+		hselect (spec, "apscatte", yes) | scan (str1)
+		if (nscan() == 0)
+		    scat = yes
+	    }
+	    if (scat) {
+		print ("Subtract scattered light from ", spec) | tee (log1)
+		imrename (spec, spec//"noscat")
+		apscript (spec//"noscat", output=spec, ansextract="NO",
+		    ansscat="YES", anssmooth="YES")
+	    }
+	}
+
+	response = ""
+	if (flat != "" || spec != "") {
+	    if (extn == ".ms")
+		response = flat // spec // "norm.ms"
+	    else
+		response = flat // spec // extn
+	    reextract = redo || (update && newaps)
+	    if (reextract || !access (response // imtype) || (redo && scat)) {
+	        print ("Create response function ", response) | tee (log1)
+
+	        if (access (response // imtype))
+		    imdelete (response, verify=no)
+	        if (access (flat //mstype))
+		    imdelete (flat//mstype, verify=no)
+	        if (access (specms))
+		    imdelete (specms, verify=no)
+
+	        fibresponse (flat, spec, apref, response, recenter=recenter,
+		    edit=edit, trace=trace, clean=clean,
+		    fitflat=fitflat, interactive=params.f_interactive,
+		    function=params.f_function, order=params.f_order)
+
+	        newresp = yes
+	    }
+	}
+
+	# If not dispersion correcting we can go directly to extracting
+	# the object spectra.  The reference arcs are the first on
+	# the arc lists.  The processing of the reference arcs is done
+	# by the task ARCREFS.
+
+	if (dispcor) {
+	    getspec (arcs1, temp)
+	    fd1 = temp
+	    if (fscan (fd1, arcref1) == EOF)
+		error (1, "No reference arcs")
+	    fd1 = ""; delete (temp, verify=no)
+	    if (!access (arcref1 // imtype)) {
+		printf ("Arc reference spectrum not found - %s%s\n",
+		    arcref1, imtype) | scan (err)
+		error (1, err // "\nCheck settting of imtype")
+	    }
+	    arcref1ms = arcref1 // extn
+	    reextract = redo || (update && newaps)
+	    if (reextract && access (arcref1ms//imtype))
+	        imdelete (arcref1ms, verify=no)
+
+	    getspec (arcs2, temp)
+	    fd1 = temp
+	    if (fscan (fd1, arcref2) == EOF)
+		arcref2 = ""
+	    else {
+	        if (!access (arcref2 // imtype)) {
+		    printf ("Arc reference spectrum not found - %s%s\n",
+			arcref2, imtype) | scan (err)
+		    error (1, err // "\nCheck settting of imtype")
+		}
+	        arcref2ms = arcref2 // extn
+	        if (reextract && access (arcref2ms//imtype))
+	            imdelete (arcref2ms, verify=no)
+	    }
+	    fd1 = ""; delete (temp, verify=no)
+
+	    arcrefs (arcref1, arcref2, extn, arcreplace, apidtable, response,
+		crval, cdelt, done, log1, log2)
+
+	    # Define alignment if needed.
+	    if (skyalign) {
+		align = "align" // extn // imtype
+		if (reextract)
+		    imdelete (align, verify=no, >& "dev$null")
+	    }
+	}
+
+	# Now we are ready to process the object spectra.
+
+	reextract = redo || (update && (newaps || newresp || newdisp))
+	fd1 = objs
+	while (fscan (fd1, spec) != EOF) {
+	    # Check if previously done; i.e. arc.
+	    if (access (done)) {
+	        fd2 = done
+	        while (fscan (fd2, specms) != EOF)
+		    if (spec == specms)
+		        break
+	        if (spec == specms)
+		    next
+	        fd2 = ""
+	    }
+	    if (!access (spec // imtype)) {
+		printf ("Object spectrum not found - %s%s\n",
+		    spec, imtype) | tee (log1)
+		print ("Check settting of imtype")
+	    }
+	    specms = spec // mstype
+
+	    # Determine required operations from the flags and image header.
+	    scat = no
+	    extract = no
+	    disp = no
+	    sky = no
+	    if (scattered) {
+		if (redo && access (spec//"noscat"//imtype)) {
+		    imdelete (spec, verify=no)
+		    imrename (spec//"noscat", spec)
+		}
+		hselect (spec, "apscatte", yes) | scan (str1)
+		if (nscan() == 0)
+		    scat = yes
+	    }
+	    if (reextract || !access (specms) || (redo && scat))
+		extract = yes
+	    else {
+		hselect (specms, "dclog1", yes) | scan (str1)
+		if (nscan () == 1) {
+		    extract = update && newdisp
+		    if (update && !newdisp)
+		        # We really should check if REFSPEC will assign
+			# different reference spectra.
+			;
+		} else
+		    disp = dispcor
+
+		hselect (specms, "skysub", yes) | scan (str1)
+		if (nscan() == 0)
+		    sky = skysubtract
+	    }
+		
+	    if (extract) {
+		disp = dispcor
+		sky = skysubtract
+	    }
+
+	    # If fully processed go to the next object.
+	    if (!extract && !disp && !sky)
+		next
+
+	    # If not interactive and the batch flag is set submit rest to batch.
+	    if (batch && !skyedit1 && !skyedit2 && !splot1 && !splot2 &&
+		apscript.ansedit == "NO" && (!skyalign || access (align))) {
+		fd1 = ""; delete (objs, verify=no)
+		apscript.ansfitscatter = "NO"
+		apscript.ansfitsmooth = "NO"
+
+		flprcache
+		batch.objects = objects
+		batch.datamax = datamax
+		batch.response = response
+		batch.arcs1 = arcs1
+		batch.arcs2 = arcs2
+		batch.arcref1 = arcref1
+		batch.arcref2 = arcref2
+		batch.arcreplace = arcreplace
+		batch.apidtable = apidtable
+		batch.arcrefs = arcrefs
+		batch.extn = extn
+		batch.objaps = objaps
+		batch.skyaps = skyaps
+		batch.arcaps = arcaps
+		batch.objbeams = objbeams
+		batch.skybeams = skybeams
+		batch.arcbeams = arcbeams
+		batch.done = done
+		batch.logfile = log1
+		batch.redo = reextract
+		batch.update = update
+		batch.scattered = scattered
+		batch.arcap = arcap
+		batch.dispcor = dispcor
+		batch.savearcs = savearcs
+		batch.skyalign = skyalign
+		batch.skysubtract = skysubtract
+		batch.saveskys = saveskys
+		batch.newaps = newaps
+		batch.newresp = newresp
+		batch.newdisp = newdisp
+		batch.newarcs = newarcs
+		dobatch = yes
+		return
+	    }
+
+	    # Process the spectrum in foreground.
+	    if (extract) {
+		if (access (specms))
+		    imdelete (specms, verify=no)
+
+		if (scat) {
+		    print ("Subtract scattered light from ", spec) | tee (log1)
+		    imrename (spec, spec//"noscat")
+		    apscript (spec//"noscat", output=spec, ansextract="NO",
+			ansscat="YES", anssmooth="YES")
+		}
+
+		print ("Extract object spectrum ", spec) | tee (log1)
+		hselect (spec, "date-obs,ut,exptime", yes, > temp1)
+		hselect (spec, "ra,dec,epoch,st", yes, >> temp1)
+		fd3 = temp1
+		if (fscan (fd3, str1, str2, str3) == 3) {
+		    setjd (spec, observatory=observatory, date="date-obs",
+			time="ut", exposure="exptime", jd="jd", hjd="",
+			ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+			>> log1)
+		    if (fscan (fd3, str1, str2, str3, str4) == 4)
+			setairmass (spec, intype="beginning",
+			    outtype="effective", exposure="exptime",
+			    observatory=observatory, show=no, update=yes,
+			    override=yes, >> log1)
+		}
+		fd3 = ""; delete (temp1, verify=no)
+		apscript (spec, nsubaps=params.nsubaps, saturation=datamax)
+		sapertures (specms, apertures="", apidtable=apidtable,
+		    wcsreset=no, verbose=no, beam=INDEF, dtype=INDEF, w1=INDEF,
+		    dw=INDEF, z=INDEF, aplow=INDEF, aphigh=INDEF, title=INDEF)
+		if (response != "") {
+		    if (params.nsubaps == 1)
+			sarith (specms, "/", response, specms, w1=INDEF,
+			    w2=INDEF, apertures="", bands="", beams="",
+			    apmodulus=0, reverse=no, ignoreaps=no,
+			    format="multispec", renumber=no, offset=0,
+			    clobber=yes, merge=no, errval=0, verbose=no)
+		    else {
+			blkrep (response, temp, 1, params.nsubaps)
+			sarith (specms, "/", temp, specms, w1=INDEF,
+			    w2=INDEF, apertures="", bands="", beams="",
+			    apmodulus=0, reverse=no, ignoreaps=yes,
+			    format="multispec", renumber=no, offset=0,
+			    clobber=yes, merge=no, errval=0, verbose=no)
+			imdelete (temp, verify=no)
+		    }
+		}
+	    }
+
+	    disperr = no
+	    if (disp) {
+		# Fix arc headers if necessary.
+		if (newarcs) {
+		    getspec (arcs1, temp)
+	    	    fd2 = temp
+	    	    while (fscan (fd2, arc) != EOF) {
+			hselect (arc, "date-obs,ut,exptime", yes, > temp1)
+			hselect (arc, "ra,dec,epoch,st", yes, >> temp1)
+			fd3 = temp1
+			if (fscan (fd3, str1, str2, str3) == 3) {
+			    setjd (arc, observatory=observatory, date="date-obs",
+				time="ut", exposure="exptime", jd="jd", hjd="",
+				ljd="ljd", utdate=yes, uttime=yes, listonly=no,
+				>> log1)
+			    if (fscan (fd3, str1, str2, str3, str4) == 4)
+				setairmass (arc, intype="beginning",
+				    outtype="effective", exposure="exptime",
+				    observatory=observatory, show=no, update=yes,
+				    override=yes, >> log1)
+			}
+			fd3 = ""; delete (temp1, verify=no)
+	        	hedit (arc, "refspec1", arc, add=yes, verify=no,
+		    	    show=no, update=yes)
+	        	hedit (arc, "arctype", "henear", add=yes, verify=no,
+		    	    show=no, update=yes)
+	    	    }
+	    	    fd2 = ""; delete (temp, verify=no)
+		    getspec (arcs2, temp)
+	    	    fd2 = temp
+	    	    while (fscan (fd2, arc) != EOF) {
+			hselect (arc, "date-obs,ut,exptime", yes, > temp1)
+			hselect (arc, "ra,dec,epoch,st", yes, >> temp1)
+			fd3 = temp1
+			if (fscan (fd3, str1, str2, str3) == 3) {
+			    setjd (arc, observatory=observatory,
+				date="date-obs", time="ut", exposure="exptime",
+				jd="jd", hjd="", ljd="ljd", utdate=yes,
+				uttime=yes, listonly=no, >> log1)
+			    if (fscan (fd3, str1, str2, str3, str4) == 4)
+				setairmass (arc, intype="beginning",
+				    outtype="effective", exposure="exptime",
+				    observatory=observatory, show=no,
+				    update=yes, override=yes, >> log1)
+
+			}
+			fd3 = ""; delete (temp1, verify=no)
+	        	hedit (arc, "refspec1", arc, add=yes, verify=no,
+		    	    show=no, update=yes)
+	        	hedit (arc, "arctype", "shift", add=yes, verify=no,
+		    	    show=no, update=yes)
+	    	    }
+	    	    fd2 = ""; delete (temp, verify=no)
+		    newarcs = no
+		}
+
+		print ("Assign arc spectra for ", spec) | tee (log1)
+		refspectra (spec, references=arcrefs,
+		    apertures="", refaps="", ignoreaps=no,
+		    select=params.select, sort=params.sort,
+		    group=params.group, time=params.time,
+		    timewrap=params.timewrap, override=yes, confirm=no,
+		    assign=yes, logfiles="STDOUT", verbose=no) |
+		    tee (log1, > log2)
+
+		doarcs (spec, response, arcref1, arcref2, extn, arcreplace,
+		    apidtable, arcaps, arcbeams, savearcs, reextract, arcap,
+		    log1, no, done)
+
+	        hselect (specms, "refspec1", yes, > temp)
+	        fd2 = temp
+	        i = fscan (fd2, arc)
+	        fd2 = ""; delete (temp, verify=no)
+		if (i < 1) {
+		    print ("No arc reference assigned for ", spec) | tee (log1)
+		    disperr = yes
+		} else {
+		    if (skyalign)
+			doalign (spec, specms, align, arcref1ms, log1, no)
+	            print ("Dispersion correct ", spec) | tee (log1)
+		    dispcor (specms, "", linearize=params.linearize,
+			database=database, table=arcref1ms, w1=INDEF,
+			w2=INDEF, dw=INDEF, nw=INDEF, log=params.log,
+			flux=params.flux, samedisp=no, global=no,
+			ignoreaps=no, confirm=no, listonly=no,
+			verbose=verbose, logfile=logfile)
+		    if (params.nsubaps > 1) {
+			imrename (specms, temp, verbose=no)
+			scopy (temp, specms, w1=INDEF, w2=INDEF,
+			    apertures="1-999", bands="", beams="", apmodulus=0,
+			    offset=0, format="multispec", clobber=no, merge=no,
+			    renumber=no, verbose=no)
+			blkavg (temp, temp, 1, params.nsubaps, option="sum")
+			imcopy (temp, specms//"[*,*]", verbose=no)
+			imdelete (temp, verify=no)
+		    }
+		}
+	    }
+
+	    if (sky && !disperr) {
+		str1 = ""
+		if (skyaps != "")
+		    str1 = "skyaps=" // skyaps
+		if (skybeams != "")
+		    str1 = str1 // " skybeams=" // skybeams
+	        print ("Sky subtract ", spec, ": ", str1) | tee (log1)
+		if (skyedit1) {
+		    str1 = substr (ansskyedit, 1, 1)
+		    if (str1 == "N" || str1 == "Y")
+			skyedit1 = no
+		    if (str1 == "n" || str1 == "N")
+			skyedit2 = no
+		    else
+			skyedit2 = yes
+		}
+		skysub.reject = params.reject
+		skysub (specms, output="", objaps=objaps, skyaps=skyaps,
+		    objbeams=objbeams, skybeams=skybeams, skyedit=skyedit2,
+		    combine=params.combine, scale=params.scale,
+		    saveskys=saveskys, logfile=logfile)
+		params.reject = skysub.reject
+	        hedit (specms, "skysub", yes, add=yes, show=no, verify=no,
+		    update=yes)
+	    }
+
+	    if (!disperr && (extract || disp || sky)) {
+		if (splot1) {
+		    print (specms, ":")
+		    str1 = anssplot
+		    if (str1 == "NO" || str1 == "YES")
+			splot1 = no
+		    if (str1 == "no" || str1 == "NO")
+			splot2 = no
+		    else
+			splot2 = yes
+		}
+		if (splot2)
+		    splot (specms)
+	    }
+
+	    print (spec, >> done)
+	}
+	fd1 = ""; delete (objs, verify=no)
+
+	if (access (done))
+	    delete (done, verify=no)
+end
diff --git a/noao/imred/src/fibers/proc.par b/noao/imred/src/fibers/proc.par
new file mode 100644
index 00000000..1b3961ea
--- /dev/null
+++ b/noao/imred/src/fibers/proc.par
@@ -0,0 +1,52 @@
+objects,s,a,,,,"List of object spectra"
+apref,f,a,"",,,"Aperture reference spectrum"
+flat,f,a,"",,,"Flat field spectrum"
+throughput,f,a,"",,,"Throughput file or image (optional)"
+arcs1,s,a,,,,"List of arc spectra"
+arcs2,s,a,,,,"List of shift arc spectra"
+arcreplace,f,a,"",,,"Special aperture replacements"
+arctable,f,a,"",,,"Arc assignment table (optional)
+"
+fibers,i,a,,,,"Number of fibers"
+apidtable,f,a,"",,,"Aperture identifications"
+crval,s,a,INDEF,,,"Approximate wavelength"
+cdelt,s,a,INDEF,,,"Approximate dispersion"
+objaps,s,a,,,,"Object apertures"
+skyaps,s,a,,,,"Sky apertures"
+arcaps,s,a,,,,"Arc apertures"
+objbeams,s,a,,,,"Object beam numbers"
+skybeams,s,a,,,,"Sky beam numbers"
+arcbeams,s,a,,,,"Arc beam numbers
+"
+scattered,b,a,,,,"Subtract scattered light?"
+fitflat,b,a,,,,"Fit and ratio flat field spectrum?"
+recenter,b,a,,,,"Recenter object apertures?"
+edit,b,a,,,,"Edit/review object apertures?"
+trace,b,a,,,,"Trace object spectra?"
+arcap,b,a,,,,"Use object apertures for arcs?"
+clean,b,a,,,,"Detect and replace bad pixels?"
+dispcor,b,a,,,,"Dispersion correct spectra?"
+savearcs,b,a,,,,"Save internal arcs?"
+skyalign,b,a,,,,"Align sky lines?"
+skysubtract,b,a,,,,"Subtract sky?"
+skyedit,b,a,,,,"Edit the sky spectra?"
+saveskys,b,a,,,,"Save sky spectra?"
+splot,b,a,,,,"Plot the final spectrum?"
+redo,b,a,,,,"Redo operations if previously done?"
+update,b,a,,,,"Update spectra if cal data changes?"
+batch,b,a,,,,"Extract objects in batch?"
+listonly,b,a,,,,"List steps but don\'t process?
+"
+datamax,r,h,INDEF,,,"Max data value / cosmic ray threshold"
+ansskyedit,s,q,"yes",,,"Edit the sky spectra?"
+newaps,b,h,,,,
+newresp,b,h,,,,
+newdisp,b,h,,,,
+newarcs,b,h,,,,
+dobatch,b,h,,,,
+anssplot,s,q,"yes",no|yes|NO|YES,,"Splot spectrum?"
+extn,s,h,".ms",,,"Extraction extension"
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+fd3,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/fibers/skysub.cl b/noao/imred/src/fibers/skysub.cl
new file mode 100644
index 00000000..b7522591
--- /dev/null
+++ b/noao/imred/src/fibers/skysub.cl
@@ -0,0 +1,145 @@
+# SKYSUB -- Sky subtract fiber spectra.
+#   Subtract the selected sky apertures from the selected object apertures.
+#   The object apertures may include the sky apertures if desired.
+#   The sky apertures are combined to a single master sky which is subtracted
+#   from each selected object aperture.  match.  The subtracted sky may be
+#   saved in an image with the prefix "sky" and the same output name.  Note
+#   that existing output images are clobbered.
+
+procedure skysub (input)
+
+string	input = ""		{prompt="Input spectra to sky subtract"}
+
+string	output = ""		{prompt="Output sky subtracted spectra"}
+string	objaps = ""		{prompt="Object apertures"}
+string	skyaps = ""		{prompt="Sky apertures"}
+string	objbeams = ""		{prompt="Object beam numbers"}
+string	skybeams = ""		{prompt="Sky beam numbers"}
+bool	skyedit	= yes		{prompt="Edit the sky spectra?"}
+string	combine = "average"	{prompt="Combining option",
+				 enum="average|median|sum"}
+string	reject	= "avsigclip"	{prompt="Sky rejection option",
+				 enum="none|minmax|avsigclip"}
+string	scale = "none"		{prompt="Sky scaling option",
+				 enum="none|mode|median|mean"}
+bool	saveskys = yes		{prompt="Save sky spectra?"}
+file	logfile = ""		{prompt="Logfile"}
+
+struct	*fd1
+struct	*fd2
+struct	*fd3
+
+begin
+	string	imtype, mstype
+	string	in, out, out1, sky, log, aps, str, str2
+	file	temp1, temp2, temp3, temp4
+	int	i, j, n
+
+	imtype = "." // envget ("imtype")
+	i = stridx (",", imtype)
+	if (i > 0)
+	    imtype = substr (imtype, 1, i-1)
+	n = strlen (imtype)
+
+	temp1 = mktemp ("tmp$iraf")
+	temp2 = mktemp ("tmp$iraf")
+	temp3 = mktemp ("tmp$iraf")
+	temp4 = mktemp ("tmp$iraf")
+
+	if (logfile == "")
+	    log = "dev$null"
+	else
+	    log = logfile
+
+	sections (input, option="fullname", > temp1)
+	sections (output, option="fullname", > temp2)
+	fd1 = temp1
+	fd2 = temp2
+	while (fscan (fd1, in) != EOF) {
+	    i = strlen (in)
+	    if (i > n && substr (in, i-n+1, i) == imtype)
+		in = substr (in, 1, i-n)
+	    if (fscan (fd2, out) < 1)
+		out = in
+	    out1 = out
+	    i = strlen (out1)
+	    if (i > 3 && substr (out1, i-2, i) == ".ms")
+		out1 = substr (out1, 1, i-3)
+
+	    aps = skyaps
+	    sky = "sky" // out1
+	    if (access (sky // imtype))
+		imdelete (sky, verify=no)
+	    if (skyedit) {
+		scopy (in, sky, w1=INDEF, w2=INDEF, apertures=aps, bands="1",
+		    beams=skybeams, apmodulus=0, offset=0, clobber=yes,
+		    format="multispec", merge=no, renumber=no,
+		    verbose=yes, >> "dev$null")
+		specplot (sky, apertures="", bands="1", autolayout=no,
+		    autoscale=yes, fraction=1., scale=1., offset=0.,
+		    step=0., ptype="1", labels="user", ulabels="",
+		    sysid=yes, yscale=yes, xlpos=1.02, ylpos=0.,
+		    title="Edit sky spectra from "//in, xlabel="",
+		    ylabel="", xmin=INDEF, xmax=INDEF, ymin=INDEF,
+		    ymax=INDEF, logfile=temp4, graphics="stdgraph")
+		imdelete (sky, verify=no)
+		system.match (sky, temp4, stop=no) |
+		fields (fields="2", lines="1-9999") |
+		system.sort (column=0, ignore=yes, numeric=no,
+		    reverse_sort=no) |
+		lists.unique (> temp3)
+		delete (temp4, verify=no)
+		aps = "@" // temp4
+		fd3 = temp3
+		while (fscan (fd3, str) != EOF) {
+		    i = stridx ("(", str)
+		    j = stridx (")", str)
+		    if (i > 0 && j > i)
+			str = substr(str,i+1,j-1)
+		    else
+			str = ""
+		    print (str, >> temp4)
+		}
+		fd3 = ""; delete (temp3, verify=no)
+
+		reject.p_mode="q"
+		str = reject
+		reject.p_mode="h"
+	    }
+
+	    if (skybeams == "") {
+		scombine (in, sky, noutput="", logfile=logfile,
+		    apertures=aps, group="all", combine=combine,
+		    reject=reject, first=yes, scale=scale, zero="none",
+		    weight="none", sample="", lthreshold=INDEF,
+		    hthreshold=INDEF, nlow=1, nhigh=1, nkeep=1, mclip=yes,
+		    lsigma=3., hsigma=2., rdnoise="0.", gain="1.", snoise="0.",
+		    sigscale=0., pclip=-0.5, grow=0, blank=0.)
+	    } else {
+		temp3 = mktemp ("sky")
+		scopy (in, sky, w1=INDEF, w2=INDEF, apertures=aps, bands="",
+		    beams=skybeams, apmodulus=0, offset=0, clobber=yes,
+		    format="multispec", merge=no, renumber=no,
+		    verbose=yes, >> log)
+		scombine (sky, temp3, noutput="", logfile=logfile,
+		    apertures=aps, group="all", combine=combine,
+		    reject=reject, first=yes, scale=scale, zero="none",
+		    weight="none", sample="", lthreshold=INDEF,
+		    hthreshold=INDEF, nlow=1, nhigh=1, nkeep=1, mclip=yes,
+		    lsigma=3., hsigma=2., rdnoise="0.", gain="1.", snoise="0.",
+		    sigscale=0., pclip=-0.5, grow=0, blank=0.)
+		flpr
+		imdelete (sky, verify=no)
+		imrename (temp3, sky, verbose=yes, >> log)
+	    }
+	    sarith (in, "-", sky, out, w1=INDEF, w2=INDEF, apertures=objaps,
+		bands="", beams=objbeams, reverse=no, ignoreaps=yes,
+		format="multispec", renumber=no, offset=0, clobber=yes,
+		merge=no, errval=0., verbose=yes, >> log)
+	    if (!saveskys)
+		imdelete (sky, verify=no)
+	}
+	fd1 = ""; delete (temp1, verify=no)
+	fd2 = ""; delete (temp2, verify=no)
+	delete (temp4, verify=no, >>& "dev$null")
+end
diff --git a/noao/imred/src/fibers/skysub.par b/noao/imred/src/fibers/skysub.par
new file mode 100644
index 00000000..bf1f4c2c
--- /dev/null
+++ b/noao/imred/src/fibers/skysub.par
@@ -0,0 +1,16 @@
+input,s,a,"",,,"Input spectra to sky subtract"
+output,s,h,"",,,"Output sky subtracted spectra"
+objaps,s,h,"",,,"Object apertures"
+skyaps,s,h,"",,,"Sky apertures"
+objbeams,s,h,"",,,"Object beam numbers"
+skybeams,s,h,"",,,"Sky beam numbers"
+skyedit,b,h,yes,,,"Edit the sky spectra?"
+combine,s,h,"average",average|median|sum,,"Combining option"
+reject,s,h,"avsigclip",none|minmax|avsigclip,,"Sky rejection option"
+scale,s,h,"none",none|mode|median|mean,,"Sky scaling option"
+saveskys,b,h,yes,,,"Save sky spectra?"
+logfile,f,h,"",,,"Logfile"
+fd1,*struct,h,"",,,
+fd2,*struct,h,"",,,
+fd3,*struct,h,"",,,
+mode,s,h,"ql",,,
diff --git a/noao/imred/src/fibers/temp b/noao/imred/src/fibers/temp
new file mode 100644
index 00000000..2205597e
--- /dev/null
+++ b/noao/imred/src/fibers/temp
@@ -0,0 +1,16 @@
+Prototype Data Manager Keywords
+
+COMMAND
+STATUS
+EOF
+
+LABEL
+
+IMAGEID
+MJD-OBS
+
+FILTER
+XTALK
+BPM
+ZERO
+FLAT
diff --git a/noao/imred/src/temp b/noao/imred/src/temp
new file mode 100644
index 00000000..25086705
--- /dev/null
+++ b/noao/imred/src/temp
@@ -0,0 +1,10 @@
+doslit/sproc.cl
+fibers/batch.cl
+fibers/fibresponse.cl
+fibers/proc.cl
+doecslit/sbatch.cl
+dofoe/batch.cl
+doslit/sbatch.cl
+doecslit/sproc.cl
+dofoe/response.cl
+dofoe/proc.cl
diff --git a/noao/imred/tutor.cl b/noao/imred/tutor.cl
new file mode 100644
index 00000000..52cf6a98
--- /dev/null
+++ b/noao/imred/tutor.cl
@@ -0,0 +1,14 @@
+# TUTOR -- Tutorial Help
+
+procedure tutor (topic)
+
+string	topic		{prompt="Tutorial topic"}
+string	package=""	{prompt="Tutorial package"}
+string	tutordb="helpdb"	{prompt="Tutorial database"}
+
+begin
+	if ($nargs == 0)
+	    help (package//".Tutorial", section="topics", helpdb=tutordb)
+	else
+	    help (package//".Tutorial", section=topic, helpdb=tutordb)
+end
diff --git a/noao/imred/vtel/README b/noao/imred/vtel/README
new file mode 100644
index 00000000..8f0be8f3
--- /dev/null
+++ b/noao/imred/vtel/README
@@ -0,0 +1,81 @@
+This is the home directory for the Kitt Peak vacuum telescope
+reduction programs.
+
+README		this file
+Revisions	revisions file
+asciilook	lookup table for ascii values into the pixelfont
+d1900.x		calculate number of days since turn of century
+decodeheader.x	decode/print vacuum telescope tape header
+destreak.par	
+destreak.x	destreak 10830 full disk helium grams
+destreak5.cl	script for processing 10830 tape containing 5 grams
+destreak5.par
+dicoplot.h	header file containing defines for DICOPLOT
+dicoplot.par
+dicoplot.x	program to make Carrington rotation mape on the Dicomed
+doc		documentation directory
+ephem.x		program to calculate solar ephemeris data
+fitslogr.cl	script, make a log file of a fits tape (daily grams)
+fitslogr.par
+getsqib.par
+getsqib.x	get the squibby brightness image from a full disk gram
+gryscl.dico	greyscale lookup table for use with DICOPLOT
+imfglexr.x	Get Line with EXtension Real for use with IMFilt
+imfilt.x	convolve an image with gaussian kernel, used in destreak
+imratio.x	find the ratio between two images, used in merge
+imtext.x	subroutine to load text into an image by overwriting pixels
+lstsq.x		least squares fitting subroutine
+makehelium.cl	script to process a helium 10830 tape into daily grams (180)
+makehelium.par
+makeimages.cl	script to process a magnetogram tape into daily grams (180)
+makeimages.par
+merge.par
+merge.x		program to merge daily grams into Carrington rotation maps
+mkpkg		make the package
+mrotlogr.cl	script, make a log file of a fits tape (Carrington rotations)
+mrotlogr.par
+mscan.par
+mscan.x		read vacuum telescope area scan tapes
+numeric.h	header file for numeric subroutine
+numeric.x	subroutine to calculate derivitives of latitude and longitude
+		with respect to x and y respectively (used in rmap)
+pimtext.par
+pimtext.x	program to put text into images by overwriting pixels
+pixbit.x	subroutine that looks up text pixel format in pixelfont
+pixelfont	pixel font for use with pimtext (no lower case, no decenders)
+putsqib.par
+putsqib.x	program to put the squibby brightness back in a full disk gram
+quickfit.par
+quickfit.x	fit an ellipse to the limb of the sun
+readheader.x    read a vacuum telescope header
+readss1.x	subroutine to read a type 1 area scan
+readss2.x	subroutine to read a type 2 area scan
+readss3.x	subroutine to read a type 3 area scan
+readss4.x	subroutine to read a type 4 area scan
+readsubswath.x	subroutine to read a sub-swath
+readvt.par
+readvt.x	read full disk grams from tape
+rmap.par
+rmap.x		map full disk grams into daily grams (180x180)
+syndico.x	Make dicomed print of daily grams 18 cm across.
+tcopy.par
+tcopy.x		tape to tape copy program
+trim.par
+trim.x		trim a full disk gram using squibby brightness info
+unwrap.par
+unwrap.x	program to remove binary wrap-around from images
+vt.h
+vtblink.cl	script to blink images on the IIS to check registration
+vtblink.par
+vtel.cl		load the vacuum telescope package
+vtel.hd		info about locations of various files
+vtel.men	menu for package
+vtel.par
+vtexamine.par
+vtexamine.x	program to examine a vacuum telescope tape (tell about record
+		lengths, header info, number of files, etc.)
+writetape.cl	script to write five full disk grams to tape
+writetape.par
+writevt.par
+writevt.x	program to write a full disk gram to tape in mountain format
+x_vtel.x	package parent program
diff --git a/noao/imred/vtel/Revisions b/noao/imred/vtel/Revisions
new file mode 100644
index 00000000..054bb80e
--- /dev/null
+++ b/noao/imred/vtel/Revisions
@@ -0,0 +1,209 @@
+This is the vacuum telescope package revisions file.
+
+mkpkg
+    Added some missing file dependencies and removed unnecessary ones from
+    the mkpkg file. (9/30/99, Davis)
+
+doc/dicoplot.hlp
+doc/readvt.hlp
+doc/unwrap.hlp
+doc/pimtext.hlp
+    Fixed minor formating problems.  (4/22/99, Valdes)
+
+=======
+V2.11.1
+=======
+
+May 16, 1989 by Dyer Lytle mods to 'readvt', 'syndico', and 'mscan'
+
+Fixed readvt to work with tape drives over the network [(if (mtfile(...].
+Modified syndico to take advantage of the disk-center info in the image
+header.
+
+Modified mscan to be much faster by taking out the geometrical correction.
+Also simplified it by removing the date/time pimtext call.  Also made it
+create only the images needed.  Also made it have a short file name option.
+Also made it work on tape drives over the net.
+
+
+June 5, 1988 by Dyer Lytle modification to PUTSQIB
+
+PUTSQIB had code in it for triming the limb as well as merging the two
+images.  I simplified the program to just make the merge.  The task TRIM
+can be used to trim the limb, and do a better job of it at that.
+
+September 29, 1987 by Dyer Lytle add SYNDICO to package
+
+Added this new program for makeing dicomed prints of daily
+grams 18 cm across.
+
+July 17, 1987 by Dyer Lytle fix bug in numeric.x
+
+There was a bug in the way an error flag was being set that made
+the program fail with a 'divide by zero' error on some data sets.
+
+June 8, 1987  by Dyer Lytle  Overhaul of the package
+
+Major modifications were made to the code to make it conform to IRAF
+standards.  Dynamic memory allocation replaced fixed memory allocation
+in many places.  Readvt was modified to accept templates for input
+and output file names.  New structures were provided for the vacuum
+telescope header, the tapeio buffer, and to reduce the argument count
+for the subroutine 'numeric'.  Vtfix was dropped from the package
+since 'readvt' was modified to check for long records by doing its
+own buffering.  Unwrap was updated to a new, more general and powerful
+version.  A major bug was found and fixed in 'rmap' which was causing
+the total mapped pixel count to be off by about 20%.
+
+June 10, 1986  by Dyer Lytle  Modification of PIMTEXT
+
+Pimtext was modified to allow the user to magnify the text in x and/or y
+and to get the date and/or time from a reference image if desired.
+
+May 21, 1986  by Dyer Lytle  Addition of PIMTEXT to package
+
+Pimtext was added to the vacuum telescope package.  This program allows
+the user to insert text directly into images.  The default action of the
+program is to look up the date and time in the image headers and insert
+this information in the lower left corner of each image.  The user can
+modify the parameters to write any text string.
+
+May 15, 1986  by Dyer Lytle  Modification to Mscan
+
+Mscan was modified to write the date and time into the images using
+a pixel font.  A hidden argument controls this option.  The characters
+are written into the image itself to speed up the moviemaking process.
+Various hidden parameters were added to allow the user to specify
+things about the text such as postition, pixel value, background fill,
+and background value.
+
+May 7, 1986  by Dyer Lytle  Modification to Makeimages and Destreak5
+
+Makeimages and Destreak5 were modified to accept as another argument
+the input scratch disk on which the input files are to be expected.
+
+February 19, 1986  by Dyer Lytle  Modification to Fitslogr
+
+Rfits was changed to produce a short header by default instead of
+a long header.  I changed fitslogr to force the long header it needs.
+
+February 6, 1986  by Dyer Lytle  Modification to Dicoplot
+
+Dicoplot was plotting all of the dates in the input image header
+file.  Sometimes, this list includes dates which should appear
+off the plot, before the zero or after the 360 degree marks.
+The modification involved teaching the program to dump these
+extra dates instead of putting them on the plots.
+
+January 30, 1986  by Dyer Lytle  Modification to vtfix
+
+Vtfix was originally set up to correct extra long records on
+vacuum telescope tapes.  It looked to record lengths of 10242
+bytes and truncated them to 10240 bytes.  Today I found a tape
+with lots of different record lengths all larger than 10240 so
+I modified vtfix to look for records with lengths longer than
+10240 bytes and truncate them to 10240.
+
+January 29, 1986  by Dyer Lytle  Modification to makehelium.
+
+Makehelium was modified to automatically delete the absolute
+value image output from RMAP since this image is junk anyway.
+
+January 29, 1986  by Dyer Lytle  Bug fix and mods to dicoplot.
+
+Dicoplot had a bug which caused the Ratio (POLARITY) images to
+come out zero.  This was corrected.  Also some of the constants
+in GREYMAP were changed to increase the contrast in the weights
+image and in the abs. flux image.  The greyscale as drawn on the
+images was modified to not have white boxes around each grey level
+and to have the number associated with each grey level printed on the
+plot.
+
+January 28, 1986  by Dyer Lytle  Modifications to mscan.
+
+Mscan was using too much memory when processing large images.
+This was causing a lot of page fault errors on VMS.  A modification
+was made to mscan to use fixed size subrasters, decreasing the
+memory needs drastically.
+
+January 20, 1986  by Dyer Lytle  Modifications to readss4.x.
+
+Readss4, which is a subroutine called by mscan to read type 4
+sector scans was set up to add the average field to each pixel
+of the output image.  This was found to be useful only in the
+special case of type 4 intensity scans and was removed.
+"It wasn't a BUG, it was a FEATURE!"
+
+January 20, 1986  by Dyer Lytle  Modifications to destreak.x.
+
+Destreak was set up to use a temporary image for data storage
+between the two destreaking passes.  The temporary image was
+hardwired into the name "tempim".  This was found to unacceptable
+since two or more destreaking jobs run at the same time would have
+a collision at "tempim".  The temporary image was made into an input
+parameter.
+
+January 20, 1986  by Dyer Lytle  Modifications to CL scripts.
+
+The CL scripts makeimages.cl, makehelium.cl, destreak5.cl, and
+writetape.cl were modified to check for the existence of each file
+before it tries to use it.  An error message is output if an image
+cannot be accessed.
+
+January 20, 1986  by Dyer Lytle  Modification to vtblink.cl
+
+Vtblink was modified so that the command "stat" can be entered to the
+"next image" prompt and the script will list which images are loaded
+into which IIS memory plane.
+
+January 20, 1986  by Dyer Lytle  Modification to merge.x
+
+Merge was not set up to handle the differences between the magnetogram
+reduction and the 10830 reduction.  Magnetogram data has three(3) images
+per day and 10830 data has two(2) images per day.  The extra image for
+magnetogram data is the absolute value immage.  Merge was designed to
+expect all three images and to produce four(4) output images.  When
+10830 data is input merge should expect two input images per day and
+only produce two output images.  This modification was made.
+Also the output images were set up such that the data and absolute
+value images were output without being divided by the weight image.
+This was changed since no information is lost by doing this division
+since the weight image is also saved.  Merge was also restructured
+quite a bit but is still a mess and needs rewriting, but it works.
+
+January 20, 1986  by Dyer Lytle  Modification to rmap.x
+
+Rmap was changed to calculate the average field, the average absolute
+field, and the total number of pixels for each gram reduced.
+These parameters are stored in the reduced data image header as
+MEAN_FLD, MEANAFLD, and NUM_PIX.
+
+January 10, 1986  by Dyer Lytle  Bug fix in tcopy.
+
+Tcopy was reporting errors incorrectly.  The record number identified
+with the error was one less than the actual error record.
+
+January 10, 1986  by Dyer Lytle  Modification to decodeheader.x.
+
+Changed the format used by decodeheader to print out the date and time,
+the format was of variable width depending on the size of the number printed.
+The new format has fixed length fields.
+
+January 9, 1986   by Dyer Lytle   Modification to merge.
+
+Merge was modified to expect the images in the textfile 'mergelist' to be in the
+order (data, abs value, weights) instead of (data, weights, abs value).
+
+January 3, 1986   by Dyer Lytle   Correction to dicoplot.
+
+Dicoplot had, for some integer expressions, TRUE/FALSE instead of YES/NO.
+This works fine on the UNIX system but was found to fail on VMS.
+
+January 3, 1986   by Dyer Lytle   Correction to mscan.
+
+Mscan was not reading type one(1) area scans properly.  The error occurred
+in readss1 where a temporary array was being salloced with the wrong length.
+The correction involved replacing "ny" by "2*ny".
+Also, readss1 and readss3 had a rather contrived error recovery mechanism built
+in, I removed this and will add a more general and reliable error procedure
+based on the fset(VALIDATE) call in a later revision.
diff --git a/noao/imred/vtel/asciilook.inc b/noao/imred/vtel/asciilook.inc
new file mode 100644
index 00000000..68974d34
--- /dev/null
+++ b/noao/imred/vtel/asciilook.inc
@@ -0,0 +1,19 @@
+data	(asciilook[i], i=1,7)     / 449, 449, 449, 449, 449, 449, 449 /
+data	(asciilook[i], i=8,14)    / 449, 449, 449, 449, 449, 449, 449 /
+data	(asciilook[i], i=15,21)   / 449, 449, 449, 449, 449, 449, 449 /
+data	(asciilook[i], i=22,28)   / 449, 449, 449, 449, 449, 449, 449 /
+data	(asciilook[i], i=29,35)   / 449, 449, 449, 449, 001, 008, 015 /
+data	(asciilook[i], i=36,42)   / 022, 029, 036, 043, 050, 057, 064 /
+data	(asciilook[i], i=43,49)   / 071, 078, 085, 092, 099, 106, 113 /
+data	(asciilook[i], i=50,56)   / 120, 127, 134, 141, 148, 155, 162 /
+data	(asciilook[i], i=57,63)   / 169, 176, 183, 190, 197, 204, 211 /
+data	(asciilook[i], i=64,70)   / 218, 225, 232, 239, 246, 253, 260 /
+data	(asciilook[i], i=71,77)   / 267, 274, 281, 288, 295, 302, 309 /
+data	(asciilook[i], i=78,84)   / 316, 323, 330, 337, 344, 351, 358 /
+data	(asciilook[i], i=85,91)   / 365, 372, 379, 386, 393, 400, 407 /
+data	(asciilook[i], i=92,98)   / 414, 421, 428, 435, 442, 449, 232 /
+data	(asciilook[i], i=99,105)  / 239, 246, 253, 260, 267, 274, 281 /
+data	(asciilook[i], i=106,112) / 288, 295, 302, 309, 316, 323, 330 /
+data	(asciilook[i], i=113,119) / 337, 344, 351, 358, 365, 372, 379 /
+data	(asciilook[i], i=120,126) / 386, 393, 400, 407, 449, 449, 449 /
+data	(asciilook[i], i=127,128) / 449, 449/
diff --git a/noao/imred/vtel/d1900.x b/noao/imred/vtel/d1900.x
new file mode 100644
index 00000000..7af25a4b
--- /dev/null
+++ b/noao/imred/vtel/d1900.x
@@ -0,0 +1,15 @@
+# D1900 -- Function to return the number of days since the turn of the
+# century.
+
+int procedure d1900 (month, day, year)
+
+int	month, day, year		# m,d,y of date
+
+int	mac[12]
+data	mac/0, 31, 59, 90, 120, 151, 181, 212, 243, 273, 304, 334/
+
+begin
+	d1900 = 365 * year + (year - 1) / 4 + mac[month] + day
+	if (month >= 3 && mod(year,4) == 0)
+	    d1900 = d1900 + 1
+end
diff --git a/noao/imred/vtel/decodeheader.x b/noao/imred/vtel/decodeheader.x
new file mode 100644
index 00000000..5d54753d
--- /dev/null
+++ b/noao/imred/vtel/decodeheader.x
@@ -0,0 +1,67 @@
+include <mach.h>
+include	"vt.h"
+
+# DECODEHEADER -- Unpack date and time, and, if 'verbose' flag is set,
+# display some information to the user.
+
+procedure decodeheader (hbuf, hs, verbose)
+
+pointer	hbuf		# header data input buffer pointer (short, SZ_VTHDR)
+pointer	hs		# header data structure
+bool	verbose		# verbose flag
+
+int	hour, minute, second
+int	bitupk()
+
+begin
+	# Unpack date, time.  The constants below are explained in the
+	# description of the image header and how it is packed.  If any
+	# changes are made the following code will have to be rewritten.
+
+	# Month. The month and day are stored in the first header word.
+	VT_HMONTH[hs] = (bitupk (int(Mems[hbuf]), 13, 4)) * 10 +
+	    bitupk (int(Mems[hbuf]), 9, 4)
+
+	# Day.
+	VT_HDAY[hs] = (bitupk (int(Mems[hbuf]), 5, 4)) * 10 +
+	    bitupk (int(Mems[hbuf]), 1, 4)
+
+	# Year. The year is stored in the second header word.
+	VT_HYEAR[hs] = (bitupk (int(Mems[hbuf+1]), 13, 4)) * 10 +
+	    bitupk (int(Mems[hbuf+1]), 9, 4)
+
+	# Time (seconds since midnight).  Stored in the third and forth words.
+	VT_HTIME[hs] = (bitupk (int(Mems[hbuf+2]), 1, 2)) * 2**15 +
+	    bitupk (int(Mems[hbuf+3]), 1, 15)
+
+	# Store other header parameters. Stored one per word.
+	VT_HWVLNGTH[hs]  = Mems[hbuf+4]	# Wavelength (angstroms)
+	VT_HOBSTYPE[hs]  = Mems[hbuf+5]	# Observation type (0,1,2,3,or 4)
+	VT_HAVINTENS[hs] = Mems[hbuf+6]	# Average intensity
+	VT_HNUMCOLS[hs]  = Mems[hbuf+7]	# Number of columns
+	VT_HINTGPIX[hs]  = Mems[hbuf+8]	# Integrations per pixel
+	VT_HREPTIME[hs]  = Mems[hbuf+9]	# Repitition time
+
+	# Calculate the time in hours, minutes, and seconds instead of
+	# seconds since midnight.
+
+	hour = int(VT_HTIME[hs]/3600)
+	minute = int((VT_HTIME[hs] - hour * 3600)/60)
+	second = VT_HTIME[hs] - hour * 3600 - minute * 60
+
+	# If verbose, print out some header info on one line no <CR>.
+	if (verbose) {
+	    call printf ("%02d/%02d/%02d %02d:%02d:%02d")
+		call pargi (VT_HMONTH[hs])
+		call pargi (VT_HDAY[hs])
+		call pargi (VT_HYEAR[hs])
+		call pargi (hour)
+		call pargi (minute)
+		call pargi (second)
+	    call printf (" wvlngth %d obstype %d numcols %d")
+		call pargi (VT_HWVLNGTH[hs])
+		call pargi (VT_HOBSTYPE[hs])
+		call pargi (VT_HNUMCOLS[hs])
+	    call flush (STDOUT)
+	}
+end
diff --git a/noao/imred/vtel/dephem.x b/noao/imred/vtel/dephem.x
new file mode 100644
index 00000000..6c8c315d
--- /dev/null
+++ b/noao/imred/vtel/dephem.x
@@ -0,0 +1,139 @@
+# EPHEM -- Calculate ephemeris data for the sun, return latitude and
+# longitude of sub-earth point.
+
+procedure ephem (month, day, year, hour, minute, second, image_r,
+	bn_degrees, cldc_degrees, verbose)
+ 
+int	month			# time of observation
+int	day			#
+int	year			#
+int	hour			#
+int	minute			#
+int	second			#
+real	image_r			# image radius
+real	bn_degrees		# solar latitude of sub-earth point (degrees)
+real	cldc_degrees		# Carrington longitude of disk center
+bool	verbose			# verbose flag
+
+double	radians_per_degree, pi, two_pi, st, d, dd
+double	ma, sin_ma, sin_two_ma, ml, e, e_squared, e_cubed
+double	ep, ea, r, image_r_squared, tl
+double	lan, bn, p, p_degrees
+double	sl1, sl2, cldc, cos_bn, x, cl1
+double	sin_three_ma, sec_bn, y
+double	dd_squared, dd_cubed, c, s, cl2, sln
+int	mac[12]
+
+data	mac/0, 31, 59, 90, 120, 151, 181, 212, 243, 273, 304, 334/
+
+begin
+	# This version ignores lunar and planetary perturbations.
+	radians_per_degree = .017453292519943d+0
+	pi = 3.1415926536d+0
+	two_pi = pi + pi
+
+	d = double(365 * year + (year - 1)/4 + mac[month] + day)
+	if (month >= 3 && mod(year, 4) == 0)
+	    d = d + 1.d+0
+	st = double(second / 3600. + minute / 60. + hour)
+	d = d + st/24.d+0 -.5d+0
+	dd = d / 10000.d+0
+	dd_squared = dd * dd
+	dd_cubed = dd * dd * dd
+
+	# Mean anomaly.
+	ma = radians_per_degree * (358.475845d+0 + .985600267d+0 *
+	    d - 1.12d-5 * dd_squared - 7.d-8 * dd_cubed)
+	ma = mod(ma, two_pi)
+	sin_ma = sin(ma)
+	sin_two_ma = sin(2.d+0 * ma)
+	sin_three_ma = sin(3.d+0 * ma)
+
+	# Mean longitude.
+	ml = radians_per_degree *
+	    (279.696678d+0 + .9856473354d+0 * d + 2.267d-5 *  dd_squared)
+	ml = mod(ml, two_pi)
+
+	# Ecentricity.
+	e = 0.01675104d+0 - 1.1444d-5 * dd - 9.4d-9 * dd_squared
+	e_squared = e * e
+	e_cubed = e_squared * e
+
+	# Obliquity.
+	ep = radians_per_degree * (23.452294d+0 -
+	    3.5626d-3 * dd - 1.23d-7 * dd_squared + 1.03d-8 * dd_cubed)
+
+	# Eccentric anomaly.
+	ea = ma + (e - e_cubed/8.d+0) * sin_ma + e_squared * sin_two_ma/2.d+0 +
+	    3.d+0 * e_cubed * sin_three_ma/8.d+0
+
+	# Radius vector.
+	r = 1.00000003d+0 * (1.d+0 - e * cos(ea))
+
+	# Image radius.
+	image_r = real(961.18d+0 / r)
+	image_r_squared = double(image_r * image_r)
+
+	# True longitude.
+	tl = ml + (2.d+0 * e - e_cubed/4.d+0) * sin_ma + 5.d+0 * e_squared *
+	    sin_two_ma/4.d+0 + 13.d+0 * e_cubed * sin_three_ma/12.d+0
+	tl = mod(tl, two_pi)
+
+	# Longitude of ascending node of solar equator.
+	lan = radians_per_degree * (73.666667d+0 + 0.0139583d+0 *
+	    (year + 50.d+0))
+
+	# Solar latitude of sub-earth point.
+	bn = asin(sin(tl - lan) * .12620d+0)
+	bn_degrees = real(bn / radians_per_degree)
+	if (verbose) {
+	    call printf("B0 (degrees) = %10.5f\n")
+	        call pargr(bn_degrees)
+	}
+
+	# Position angle of rotation axis.
+	p = atan(-cos(tl) * tan(ep)) + atan(-cos(tl - lan) * .12722d+0)
+	p_degrees = p/radians_per_degree
+	if (verbose) {
+	    call printf("P-angle (degrees) = %10.5f\n")
+	        call pargr(real(p_degrees))
+	}
+
+	# Carrington longitude of disk center.
+	sl1 = (d + 16800.d+0) * 360.d+0/25.38d+0
+	sl2 = mod(sl1, 360.d+0)
+	sln = 360.d+0 - sl2
+	sln = radians_per_degree * sln
+
+	cos_bn = cos(bn)
+	sec_bn = 1.d+0/cos_bn
+	c = +1.d+0
+	s = +1.d+0
+	x = -sec_bn * cos(tl - lan)
+	if (x < 0.)
+	    c = -1.d+0
+	y = -sec_bn * sin(tl - lan) * .99200495d+0
+	if (y < 0.)
+	    s = -1.d+0
+
+	cl1 = tan(tl - lan) * 0.99200495d+0
+	cl2 = atan(cl1)
+	if (s == 1.d+0 && c == 1.d+0)
+	    cldc = sln + cl2
+	if (s == -1.d+0 && c == -1.d+0)
+	    cldc = sln + cl2 + pi
+	if (s == 1.d+0 && c == -1.d+0)
+	    cldc = sln + cl2 + pi
+	if (s == -1.d+0 && c == 1.d+0)
+	    cldc = sln + cl2
+	if (cldc < 0.d+0)
+	    cldc = cldc + two_pi
+	if (cldc > two_pi)
+	    cldc = mod(cldc, two_pi)
+
+	cldc_degrees = real(cldc / radians_per_degree)
+	if (verbose) {
+	    call printf ("L0 (degrees) = %10.5f\n")
+	        call pargr (cldc_degrees)
+	}
+end
diff --git a/noao/imred/vtel/destreak.par b/noao/imred/vtel/destreak.par
new file mode 100644
index 00000000..4b03ee85
--- /dev/null
+++ b/noao/imred/vtel/destreak.par
@@ -0,0 +1,5 @@
+heimage,s,q,,,,Helium 10830 image to be destreaked
+heout,s,q,,,,Output image
+tempim,s,q,,,,Temporary image
+verbose,b,h,no,,,Print out header data and give progress reports
+threshold,i,h,3,,,Squibby brightness threshold defining the limb
diff --git a/noao/imred/vtel/destreak.x b/noao/imred/vtel/destreak.x
new file mode 100644
index 00000000..5002bab9
--- /dev/null
+++ b/noao/imred/vtel/destreak.x
@@ -0,0 +1,432 @@
+include <mach.h>
+include <imhdr.h>
+include <imset.h>
+include "vt.h"
+
+define	WINDEXC		800.	# constant for weight index calculation
+define	WINDEX6TH	75.	# constant for weight index calculation
+define	LIMBR		.97	# Limb closeness rejection coefficient.
+define	SOWTHRESH	20.	# Sum of weights threshold.
+define	SZ_WT10830	1024	# size of weight table for destreak
+define	FCORRECT	.9375	# fractional term for lattitude correction
+
+# Structure for least square fitting parameters.
+
+define	VT_LENSQSTRUCT	8		# Length of VT sq structure
+
+# Pointers
+define	VT_SQ1P		Memi[$1]	# pointers to arrays for least
+define	VT_SQ1Q1P	Memi[$1+1]	# squares fit
+define	VT_SQ1Q2P	Memi[$1+2]	#
+define	VT_SQ1Q3P	Memi[$1+3]	#
+define	VT_SQ2Q2P	Memi[$1+4]	#
+define	VT_SQ2Q3P	Memi[$1+5]	#
+define	VT_SQ3Q3P	Memi[$1+6]	#
+define	VT_NUMDATAP	Memi[$1+7]	#
+
+# Macro definitions
+define	VT_SQ1		Memr[VT_SQ1P($1)+$2-1]
+define	VT_SQ1Q1	Memr[VT_SQ1Q1P($1)+$2-1]
+define	VT_SQ1Q2	Memr[VT_SQ1Q2P($1)+$2-1]
+define	VT_SQ1Q3	Memr[VT_SQ1Q3P($1)+$2-1]
+define	VT_SQ2Q2	Memr[VT_SQ2Q2P($1)+$2-1]
+define	VT_SQ2Q3	Memr[VT_SQ2Q3P($1)+$2-1]
+define	VT_SQ3Q3	Memr[VT_SQ3Q3P($1)+$2-1]
+define	VT_NUMDATA	Memi[VT_NUMDATAP($1)+$2-1]
+
+
+# DESTREAK -- Destreak 10830 grams.  On a 10830 full disk image.  For
+# each diode, based on the data from that diode calculate coefficients for
+# a best fit function and subtract this function from the data.  Apply a
+# spatial filter to the resulting image.
+
+procedure t_destreak()
+
+char	heimage[SZ_FNAME]		# input image
+char	heout[SZ_FNAME]	    		# output image
+char	tempim[SZ_FNAME]	    	# temporary image
+bool	verbose				# verbose flag
+real	el[LEN_ELSTRUCT]		# ellipse parameters data structure
+int	threshold			# squibby brightness threshold
+
+int	diode, npix, i, line
+int	kxdim, kydim
+real	kernel[3,9]
+pointer	weights
+pointer	lgp1, lpp
+pointer	heim, heoutp
+pointer	a, c
+pointer	sqs, sp
+
+bool	clgetb()
+int	clgeti()
+real	imgetr()
+pointer	imgl2s(), impl2s(), immap()
+errchk	immap, imgl2s, impl2s, imfilt
+
+begin
+	call smark (sp)
+	call salloc (sqs, VT_LENSQSTRUCT, TY_STRUCT)
+	call salloc (VT_SQ1P(sqs), DIM_VTFD, TY_REAL)
+	call salloc (VT_SQ1Q1P(sqs), DIM_VTFD, TY_REAL)
+	call salloc (VT_SQ1Q2P(sqs), DIM_VTFD, TY_REAL)
+	call salloc (VT_SQ1Q3P(sqs), DIM_VTFD, TY_REAL)
+	call salloc (VT_SQ2Q2P(sqs), DIM_VTFD, TY_REAL)
+	call salloc (VT_SQ2Q3P(sqs), DIM_VTFD, TY_REAL)
+	call salloc (VT_SQ3Q3P(sqs), DIM_VTFD, TY_REAL)
+	call salloc (VT_NUMDATAP(sqs), DIM_VTFD, TY_INT)
+	call salloc (a, DIM_VTFD, TY_REAL)
+	call salloc (c, DIM_VTFD, TY_REAL)
+	call salloc (weights, SZ_WT10830, TY_REAL)
+	
+	# Get parameters from the cl.
+
+	call clgstr ("heimage", heimage, SZ_FNAME)
+	call clgstr ("heout", heout, SZ_FNAME)
+	call clgstr ("tempim", tempim, SZ_FNAME)
+	verbose = clgetb ("verbose")
+	threshold = clgeti("threshold")
+
+	# Open the images
+	heim = immap (heimage, READ_WRITE, 0)
+	heoutp = immap (tempim, NEW_COPY, heim)
+
+	# Ellipse parameters.
+	E_XCENTER[el] = imgetr (heim, "E_XCEN")
+	E_YCENTER[el] = imgetr (heim, "E_YCEN")
+	E_XSEMIDIAMETER[el] = imgetr (heim, "E_XSMD")
+	E_YSEMIDIAMETER[el] = imgetr (heim, "E_XSMD")
+
+	# Generate the weight array.
+	do i = 1, SZ_WT10830
+	    Memr[weights+i-1] = exp((real(i) - WINDEXC)/WINDEX6TH)
+
+	# Set the sq arrays and the a and c arrays to zero.
+	call aclrr (VT_SQ1(sqs,1), DIM_VTFD)
+	call aclrr (VT_SQ1Q1(sqs,1), DIM_VTFD)
+	call aclrr (VT_SQ1Q2(sqs,1), DIM_VTFD)
+	call aclrr (VT_SQ1Q3(sqs,1), DIM_VTFD)
+	call aclrr (VT_SQ2Q2(sqs,1), DIM_VTFD)
+	call aclrr (VT_SQ2Q3(sqs,1), DIM_VTFD)
+	call aclrr (VT_SQ3Q3(sqs,1), DIM_VTFD)
+	call aclri (VT_NUMDATA(sqs,1), DIM_VTFD)
+	call aclrr (Memr[a], DIM_VTFD)
+	call aclrr (Memr[c], DIM_VTFD)
+
+	# for all lines in the image {
+	#    calculate which diode this line corresponds to
+	#    get the line from the image
+	#    sum the q's for this line
+	# }
+
+	npix = IM_LEN(heim,1)
+	do line = 1, DIM_VTFD {
+	    diode = mod((line - 1), SWTH_HIGH) + 1
+	    lgp1 = imgl2s (heim, line)
+	    call qsumq (Mems[lgp1], npix, el, threshold, weights, LIMBR,
+		line, sqs)
+	}
+
+	# Fit the function to the data for each line. 
+	do line = 1, DIM_VTFD {
+	    call qfitdiode(sqs, line, npix, Memr[a+line-1], Memr[c+line-1],
+		threshold, verbose)
+	    if (verbose) {
+		call printf ("line = %d\n")
+		    call pargi (line)
+		call flush (STDOUT)
+	    }
+	}
+
+	# For each image line subtract the function from the data.
+	do line = 1, DIM_VTFD {
+	    diode = mod((line - 1), SWTH_HIGH) + 1
+	    lgp1 = imgl2s (heim, line)
+	    lpp  = impl2s (heoutp, line)
+	    call qrfunct(Mems[lgp1], Mems[lpp], npix, el, threshold,
+		Memr[a+line-1], Memr[c+line-1], LIMBR, line)
+	}
+
+	# Switch images
+	call imunmap (heim)
+	call imunmap (heoutp)
+	heim = immap (tempim, READ_WRITE, 0)
+	heoutp = immap (heout, NEW_COPY, heim)
+
+	# Call the spacial filter program.
+
+	# First we have to load up the filter kernel
+	kxdim = 3
+	kydim = 9
+	kernel[1,1] = .017857
+	kernel[1,2] = .017857
+	kernel[1,3] = .035714
+	kernel[1,4] = .035714
+	kernel[1,5] = .035714
+	kernel[1,6] = .035714
+	kernel[1,7] = .035714
+	kernel[1,8] = .017857
+	kernel[1,9] = .017857
+	kernel[2,1] = .017857
+	kernel[2,2] = .053571
+	kernel[2,3] = .071428
+	kernel[2,4] = .071428
+	kernel[2,5] = .071428
+	kernel[2,6] = .071428
+	kernel[2,7] = .071428
+	kernel[2,8] = .053571
+	kernel[2,9] = .017857
+	kernel[3,1] = .017857
+	kernel[3,2] = .017857
+	kernel[3,3] = .035714
+	kernel[3,4] = .035714
+	kernel[3,5] = .035714
+	kernel[3,6] = .035714
+	kernel[3,7] = .035714
+	kernel[3,8] = .017857
+	kernel[3,9] = .017857
+
+	if (verbose) {
+	    call printf ("filtering\n")
+	    call flush(STDOUT)
+	}
+	call imfilt(heim, heoutp, kernel, kxdim, kydim, el)
+
+	# Unmap the images.
+	call imunmap(heim)
+	call imunmap(heoutp)
+
+	call sfree (sp)
+
+end
+
+
+# QFITDIODE -- Calculate the coefficients of the best fit functions.
+
+procedure qfitdiode (sqs, line, npix, a, c, threshold, verbose)
+
+pointer	sqs						# q's structure
+int	line						# line in image
+int	npix						# number of pixels
+real	a, c						# returned coeffs
+int	threshold					# sqib threshold
+bool	verbose						# verbose flag
+
+int	i, j
+real	zz[4,4], limbr
+
+begin
+	# If the number of points is insufficient, skip.
+	if (VT_NUMDATA(sqs,line) < 50) {
+	    a = 0.0
+	    c = 0.0
+	    return
+	}
+
+	# First set the out arrays equal to the in arrays, initialize limbr.
+	limbr = LIMBR
+
+
+	# Clear the z array.
+	do i = 1,4 
+	    do j = 1,4
+		zz[i,j] = 0.0
+
+	# Fill the z array.
+	zz[1,2] = VT_SQ1Q1(sqs,line)
+	zz[1,3] = VT_SQ1Q2(sqs,line)
+	zz[1,4] = VT_SQ1Q3(sqs,line)
+	zz[2,3] = VT_SQ2Q2(sqs,line)
+	zz[2,4] = VT_SQ2Q3(sqs,line)
+	zz[3,4] = VT_SQ3Q3(sqs,line)
+
+	# Do the fit if the sum of weights is sufficient.
+	if (VT_SQ1(sqs,line) > SOWTHRESH)
+	    call lstsq(zz,4,VT_SQ1(sqs,line))
+	else {
+	    zz[3,1] = 0.0
+	    zz[3,2] = 0.0
+	}
+
+	# Coefficients are:
+	if (verbose) {
+	    call printf ("a = %g, c = %g ")
+	    call pargr(zz[3,1])
+	    call pargr(zz[3,2])
+	    call flush(STDOUT)
+	}
+	c = zz[3,1]
+	a = zz[3,2]
+end
+
+
+# SUMQ -- Sum up the values of the Qs for the least squares fit.
+
+procedure qsumq (in, npix, el, threshold, weights, limbr, y, sqs)
+
+short	in[npix]			# array to sum from
+pointer	weights				# weights
+real	el[LEN_ELSTRUCT]		# limb fit ellipse struct
+real	limbr				# limb closeness rejection coefficient
+int	npix				# numpix in im line
+int	threshold			# sqib threshold
+int	y				# line in image
+pointer	sqs				# pointer to q's structure
+
+real	q1, q2, q3
+int	i, windex, itemp
+real	rsq, r4th, r6th, r8th
+real	x, xfr, yfr, data
+short	k
+
+int	and()
+short	shifts()
+
+begin
+	k = -4
+
+	# First, calculate the y fractional radius squared.
+	yfr = (abs(real(y) - E_YCENTER[el]))**2 / (E_YSEMIDIAMETER[el]**2)
+
+	# Do this for all the pixels in this row.
+	do i = 1, npix {
+	    # Calculate the x fractional radius squared.
+	    x = real(i)
+	    xfr = (abs(x - E_XCENTER[el]))**2 / E_XSEMIDIAMETER[el]**2
+
+	    # If off the disk, skip.
+	    if (xfr > 1.0) {
+		next
+	    }
+
+	    # Check to see if the brightness of this data point is above the
+	    # threshold, if not, skip.
+
+	    itemp = in[i]
+	    if (and(itemp,17B) < threshold)
+		next
+
+	    # Strip off the squibby brightness, if data too big skip.
+	    data = real(shifts(in[i], k))
+	    if (data > 100.)
+		next
+	    
+	    # Calculate the radius squared. (fractional)
+	    rsq = xfr + yfr
+
+	    # Check to see if the data point is on the disk.
+	    if (rsq > limbr)
+		next
+
+	    r4th = rsq * rsq
+	    r6th = rsq * r4th
+	    r8th = r4th * r4th
+
+	    # Calculate the weight index.
+	    windex = WINDEXC + data + WINDEX6TH * r6th
+	    if (windex < 1)
+		windex = 1
+	    if (windex > SZ_WT10830)
+		windex = SZ_WT10830
+
+	    # Calculate the Qs.
+	    q1 = Memr[weights+windex-1]
+	    q2 = q1 * r6th
+	    q3 = q1 * data
+	    VT_SQ1(sqs,y) = VT_SQ1(sqs,y) + q1
+	    VT_SQ1Q1(sqs,y) = VT_SQ1Q1(sqs,y) + q1 * q1
+	    VT_SQ1Q2(sqs,y) = VT_SQ1Q2(sqs,y) + q1 * q2
+	    VT_SQ1Q3(sqs,y) = VT_SQ1Q3(sqs,y) + q1 * q3
+	    VT_SQ2Q2(sqs,y) = VT_SQ2Q2(sqs,y) + q2 * q2
+	    VT_SQ2Q3(sqs,y) = VT_SQ2Q3(sqs,y) + q2 * q3
+	    VT_SQ3Q3(sqs,y) = VT_SQ3Q3(sqs,y) + q3 * q3
+	    VT_NUMDATA(sqs,y) = VT_NUMDATA(sqs,y) + 1
+	}
+end
+	
+	
+# QRFUNCT -- Remove FUNCTion. Remove the calculated function from the data
+# from a particular diode.  Each data point is checked to see if it is on
+# disk.  If it is not then the input pixel is copied to the output array.
+# if it is on the disk, the function defined by a and c is subtracted from
+# the data point before it is copied to the output array.
+
+procedure qrfunct (in, out, npix, el, threshold, a, c, limbr, y)
+
+short	in[npix]		# inline without fit removed
+short	out[npix]		# inline with fit removed
+real	el[LEN_ELSTRUCT]	# ellipse parameter struct
+real	a, c			# fit coefficients
+real	limbr			# limb closeness coefficient
+int	y			# line of image
+int	npix			# number of pixels in this line
+int	threshold		# sqib threshold
+
+int	i
+short	fvalue
+short	data
+real	x, xfr, yfr, rsq, y4th, y6th
+short	correction
+short	k, kk
+
+short 	shifts()
+
+begin
+	k = -4
+	kk = 4
+
+	# If a and c have zeros, skip.
+	if (abs(a) < EPSILONR && abs(c) < EPSILONR) {
+	    do i = 1, npix {
+		out[i] = in[i]   # leave original data.
+	    }
+	    return
+	}
+
+	# First, calculate the y fractional radius.
+	yfr = (abs(real(y) - E_YCENTER[el]))**2 / (E_YSEMIDIAMETER[el]**2)
+
+	# Calculate the correction.
+	y4th = yfr*yfr
+	y6th = y4th*yfr
+	correction = short(FCORRECT*(6.0*yfr + 8.0*y4th + 16.0*y6th))
+
+	# Do this for all the pixels in the row.
+	do i = 1, npix {
+	    # Calculate the x fractional radius.
+	    x = real(npix/2 - i + 1)
+	    xfr = (abs(real(i) - E_XCENTER[el]))**2 / E_XSEMIDIAMETER[el]**2
+
+	    # If off the disk, skip.
+	    if (xfr > 1.0) {
+		out[i] = in[i]		# leave original data
+		next
+	    }
+
+	    # Check to see if the brightness of this data point is above the
+	    # threshold, if not, skip.
+
+	    if (and(int(in[i]),17B) < threshold) {
+		out[i] = in[i]		# leave original data
+		next
+	    }
+
+	    # Strip off the squibby brightness
+	    data = shifts(in[i], k)
+	    
+	    # Calculate the radius squared. (fractional)
+	    rsq = xfr + yfr
+
+	    # Check to see if the data point is on the disk.
+	    if (rsq > 1.0) {
+		out[i] = in[i]		# leave original data
+		next
+	    }
+
+	    # Calculate the function value.  Subtract it from the data value.
+	    fvalue = short(a * rsq**3 + c)   # a * r**6 + c
+	    data = data - fvalue + correction
+	    # data + squib bright
+	    out[i] = shifts(data, kk) + short(and(int(in[i]),17B))
+	}
+end
diff --git a/noao/imred/vtel/destreak5.cl b/noao/imred/vtel/destreak5.cl
new file mode 100644
index 00000000..40a3be55
--- /dev/null
+++ b/noao/imred/vtel/destreak5.cl
@@ -0,0 +1,91 @@
+#{ DESTREAK5 -- Destreak all five images from a vacuum telescope tape.  The
+# script accepts the general input image filename and the general output
+# image filename from the user (and now the scratch disk).  Destreak5
+# appends a digit [1-5] to the file name for each file read and each
+# corresponding file  written.
+
+# getinput,s,a,,,,General input filename for the 5 images
+# getoutput,s,a,,,,General output filename for the 5 images
+# inim,s,h
+# outim,s,h
+
+{
+
+	inim = getinput
+	outim = getoutput
+
+	if (access("vtelscr$"//inim//"001")) {
+	    readvt ("vtelscr$"//inim//"001", inim//"tmp1")
+	    quickfit (inim//"tmp1001",verbose=yes)
+	    delete ("vtelscr$"//inim//"001")
+	    getsqib (inim//"tmp1001", inim//"sqib1")
+	    destreak (inim//"tmp1001", inim//"temp1", inim//"tmpr1")
+	    imdelete (inim//"tmp1001")
+	    imdelete (inim//"tmpr1")
+	    putsqib (inim//"temp1", inim//"sqib1", outim//"1")
+	    imdelete (inim//"temp1")
+	    imdelete (inim//"sqib1")
+	} else {
+	    print ("vtelscr$"//inim//"001 not accessable")
+	}
+
+	if (access("vtelscr$"//inim//"002")) {
+	    readvt ("vtelscr$"//inim//"002", inim//"tmp2")
+	    quickfit (inim//"tmp2001",verbose=yes)
+	    delete ("vtelscr$"//inim//"002")
+	    getsqib (inim//"tmp2001", inim//"sqib2")
+	    destreak (inim//"tmp2001", inim//"temp2", inim//"tmpr2")
+	    imdelete (inim//"tmp2001")
+	    imdelete (inim//"tmpr2")
+	    putsqib (inim//"temp2", inim//"sqib2", outim//"2")
+	    imdelete (inim//"temp2")
+	    imdelete (inim//"sqib2")
+	} else {
+	    print ("vtelscr$"//inim//"002 not accessable")
+	}
+
+	if (access("vtelscr$"//inim//"003")) {
+	    readvt ("vtelscr$"//inim//"003", inim//"tmp3")
+	    quickfit (inim//"tmp3001",verbose=yes)
+	    delete ("vtelscr$"//inim//"003")
+	    getsqib (inim//"tmp3001", inim//"sqib3")
+	    destreak (inim//"tmp3001", inim//"temp3", inim//"tmpr3")
+	    imdelete (inim//"tmp3001")
+	    imdelete (inim//"tmpr3")
+	    putsqib (inim//"temp3", inim//"sqib3", outim//"3")
+	    imdelete (inim//"temp3")
+	    imdelete (inim//"sqib3")
+	} else {
+	    print ("vtelscr$"//inim//"003 not accessable")
+	}
+
+	if (access("vtelscr$"//inim//"004")) {
+	    readvt ("vtelscr$"//inim//"004", inim//"tmp4")
+	    quickfit (inim//"tmp4001",verbose=yes)
+	    delete ("vtelscr$"//inim//"004")
+	    getsqib (inim//"tmp4001", inim//"sqib4")
+	    destreak (inim//"tmp4001", inim//"temp4", inim//"tmpr4")
+	    imdelete (inim//"tmp4001")
+	    imdelete (inim//"tmpr4")
+	    putsqib (inim//"temp4", inim//"sqib4", outim//"4")
+	    imdelete (inim//"temp4")
+	    imdelete (inim//"sqib4")
+	} else {
+	    print ("vtelscr$"//inim//"004 not accessable")
+	}
+
+	if (access("vtelscr$"//inim//"005")) {
+	    readvt ("vtelscr$"//inim//"005", inim//"tmp5")
+	    quickfit (inim//"tmp5001",verbose=yes)
+	    delete ("vtelscr$"//inim//"005")
+	    getsqib (inim//"tmp5001", inim//"sqib5")
+	    destreak (inim//"tmp5001", inim//"temp5", inim//"tmpr5")
+	    imdelete (inim//"tmp5001")
+	    imdelete (inim//"tmpr5")
+	    putsqib (inim//"temp5", inim//"sqib5", outim//"5")
+	    imdelete (inim//"temp5")
+	    imdelete (inim//"sqib5")
+	} else {
+	    print ("vtelscr$"//inim//"004 not accessable")
+	}
+}
diff --git a/noao/imred/vtel/destreak5.par b/noao/imred/vtel/destreak5.par
new file mode 100644
index 00000000..41accc84
--- /dev/null
+++ b/noao/imred/vtel/destreak5.par
@@ -0,0 +1,4 @@
+getinput,s,a,,,,Root input filename for the 5 images 
+getoutput,s,a,,,,Root output filename for the 5 images 
+inim,s,h
+outim,s,h
diff --git a/noao/imred/vtel/dicoplot.h b/noao/imred/vtel/dicoplot.h
new file mode 100644
index 00000000..592fc8c8
--- /dev/null
+++ b/noao/imred/vtel/dicoplot.h
@@ -0,0 +1,35 @@
+# for the following it is assumed the scale of the coordinate system is zero
+# to one in both x and y. (0.0,0.0) to (1.0,1.0)
+# coordinates of first image (bottom-left-x, bottom-left-y, top-right-x, t-r-y)
+define IM1BL_X	.242
+define IM1BL_Y	.142
+define IM1TR_X	.452
+define IM1TR_Y	.822
+
+# coordinates of second image
+define IM2BL_X	.525
+define IM2BL_Y	.142
+define IM2TR_X	.735
+define IM2TR_Y	.822
+
+# coordinates of greyscale box
+define IMGBL_X	.229
+define IMGBL_Y	.867
+define IMGTR_X	.748
+define IMGTR_Y	.902
+
+# coordinates of outside boundary of entire plot
+define IMDBL_X	.210
+define IMDBL_Y	.076
+define IMDTR_X	.810
+define IMDTR_Y	.950
+
+# length of tics when labeling axes
+define TICLENGTH .002
+
+#image types
+define T10830	1
+define TFLUX	4
+define TWEIGHT	3
+define TABSFLX	2
+define TPLRTY	5
diff --git a/noao/imred/vtel/dicoplot.par b/noao/imred/vtel/dicoplot.par
new file mode 100644
index 00000000..e8348a76
--- /dev/null
+++ b/noao/imred/vtel/dicoplot.par
@@ -0,0 +1,4 @@
+image1,s,q,,,,Image1
+image2,s,q,,,,Image2
+rotnum,i,q,,,,carrington rotation number
+device,s,h,dicomed,,,plot device
diff --git a/noao/imred/vtel/dicoplot.x b/noao/imred/vtel/dicoplot.x
new file mode 100644
index 00000000..3754bb06
--- /dev/null
+++ b/noao/imred/vtel/dicoplot.x
@@ -0,0 +1,522 @@
+include <mach.h>
+include <imhdr.h>
+include <imset.h>
+include <math/curfit.h>
+include <gset.h>
+include "dicoplot.h"
+include "vt.h"
+
+# DICOPLOT -- Make dicomed (or other graphics device) plots of Carrington
+# rotation maps.  The output of this program is a metacode file called
+# "metacode" which can be plotted on whichever graphics device the user
+# chooses.  Before the program is run, STDGRAPH should be set to the target
+# device.
+
+procedure t_dicoplot()
+
+char	image1[SZ_FNAME]			# first image to draw
+char	image2[SZ_FNAME]			# second image to draw
+int	rotnum					# carrington rotation number
+char	device[SZ_FNAME]			# plot device
+
+int	type1, type2				# types of the two images
+pointer	imout1
+pointer	imout2
+int	count, obsdate
+int	i, longitude, latitude, month, day, year
+int	xresolution, yresolution
+real	delta_gray, delta_long, delta_gblock, x, y
+real	offset, longituder
+real	mapx1, mapx2, mapy1, mapy2
+char	ltext[SZ_LINE]
+char	system_id[SZ_LINE]
+
+bool	up, pastm
+int	dateyn
+
+short	gray[16]
+pointer	imgray1
+pointer	imgray2
+pointer	gp, p, sp
+pointer	im1, im2
+pointer	subras1, subras2
+
+pointer	imgs2r()
+pointer	immap()
+pointer	gopen()
+int	imaccf()
+int	ggeti()
+real	imgetr()
+int	clgeti(), imgeti()
+errchk	gopen, immap, imgs2r, sysid
+
+begin
+	call smark (sp)
+	call salloc (imout1, DIM_SQUAREIM*DIM_XCARMAP, TY_REAL)
+	call salloc (imout2, DIM_SQUAREIM*DIM_XCARMAP, TY_REAL)
+	call salloc (imgray1, DIM_SQUAREIM*DIM_XCARMAP, TY_SHORT)
+	call salloc (imgray2, DIM_SQUAREIM*DIM_XCARMAP, TY_SHORT)
+
+	# Get parameters from the cl.
+	call clgstr ("image1", image1, SZ_FNAME)
+	call clgstr ("image2", image2, SZ_FNAME)
+	rotnum = clgeti ("rotnum")
+	call clgstr ("device", device, SZ_FNAME)
+
+	# Open the output file.
+	gp = gopen (device, NEW_FILE, STDPLOT)
+
+	# Open the images
+	im1 = immap (image1, READ_ONLY, 0)
+	im2 = immap (image2, READ_ONLY, 0)
+
+	# Find out what kind of images we have.
+	call gimtype (im1, type1)
+	call gimtype (im2, type2)
+
+	# Draw boxes around the grayscale and the data images.
+	call box (gp, IM1BL_X, IM1BL_Y, IM1TR_X, IM1TR_Y)
+	call box (gp, IM2BL_X, IM2BL_Y, IM2TR_X, IM2TR_Y)
+
+	delta_gblock = (IMGTR_X - IMGBL_X)/16.
+	y = IMGBL_Y - .005
+	do i = 1, 16 {
+	    x = IMGBL_X + real(i-1) * delta_gblock + delta_gblock/2.
+	    call sprintf (ltext, SZ_LINE, "%d")
+		call pargi ((i-1)*int((254./15.)+0.5))
+	    call gtext (gp, x, y, ltext, "v=t;h=c;s=.20")
+	}
+
+
+	# Draw tic marks and labels on the image boxes.
+	# First the longitudes.
+
+	delta_long = (IM1TR_Y-IM1BL_Y)/36.
+	longitude = 0
+	do i = 1,37 {
+	    call sprintf (ltext, SZ_LINE, "%d")
+		call pargi (longitude)
+	    y = IM1TR_Y - real(i-1)*delta_long
+	    x = IM1TR_X
+	    call gline (gp, x,y,x+TICLENGTH,y)
+	    x = IM1BL_X
+	    call gline (gp, x,y,x-TICLENGTH,y)
+	    call gtext (gp, x-.005, y, ltext, "v=c;h=r;s=.25;u=0")
+	    x = IM2TR_X
+	    call gline (gp, x,y,x+TICLENGTH,y)
+	    x = IM2BL_X
+	    call gline (gp, x,y,x-TICLENGTH,y)
+	    call gtext (gp, x-.005, y, ltext, "v=c;h=r;s=.25;u=0")
+	    longitude = longitude + 10
+	}
+
+	# Now the latitudes.
+	# First draw the tics and labels at 0 degrees on both images
+
+	latitude = 0
+	call sprintf (ltext, SZ_LINE, "%d")
+	    call pargi (latitude)
+	x = (IM1BL_X + IM1TR_X)/2.
+	y = IM1TR_Y
+	call gline (gp, x, y, x, y+TICLENGTH)
+	call gtext (gp, x, y+.005, ltext, "v=b;h=c;s=.25;u=0")
+	y = IM1BL_Y
+	call gline (gp, x, y, x, y-TICLENGTH)
+	x = (IM2BL_X + IM2TR_X)/2.
+	y = IM2TR_Y
+	call gline (gp, x, y, x, y+TICLENGTH)
+	call gtext (gp, x, y+.005, ltext, "v=b;h=c;s=.25;u=0")
+	y = IM2BL_Y
+	call gline (gp, x, y, x, y-TICLENGTH)
+
+	# Now the north latitudes.
+	do i = 1,4 {
+	    switch (i) {
+	    case 1:
+		latitude = 20
+	    case 2:
+		latitude = 40
+	    case 3:
+		latitude = 60
+	    case 4:
+		latitude = 90
+	    }
+	    offset = ((IM1TR_X - IM1BL_X)/2.) * sin(real(latitude)*3.1415/180.)
+	    x = IM1BL_X + ((IM1TR_X - IM1BL_X)/2.) + offset
+	    y = IM1TR_Y
+	    call sprintf (ltext, SZ_LINE, "%s%d")
+		call pargstr ("N")
+	        call pargi (latitude)
+	    call gline (gp, x, y, x, y+TICLENGTH)
+	    call gtext (gp, x, y+.005, ltext, "v=b;h=c;s=.25;u=0")
+	    y = IM1BL_Y
+	    call gline (gp, x, y, x, y-TICLENGTH)
+	    x = x + IM2BL_X - IM1BL_X
+	    y = IM2TR_Y
+	    call gline (gp, x, y, x, y+TICLENGTH)
+	    call gtext (gp, x, y+.005, ltext, "v=b;h=c;s=.25;u=0")
+	    y = IM2BL_Y
+	    call gline (gp, x, y, x, y-TICLENGTH)
+	}
+
+	# Finally the south latitudes.
+	do i = 1,4 {
+	    switch (i) {
+	    case 1:
+		latitude = -20
+	    case 2:
+		latitude = -40
+	    case 3:
+		latitude = -60
+	    case 4:
+		latitude = -90
+	    }
+	    offset = ((IM2TR_X - IM2BL_X)/2.) * sin(real(latitude)*3.1415/180.)
+	    x = IM1BL_X + ((IM1TR_X - IM1BL_X)/2.) + offset
+	    y = IM1TR_Y
+	    call sprintf (ltext, SZ_LINE, "%s%d")
+		call pargstr ("S")
+	        call pargi (-latitude)
+	    call gline (gp, x, y, x, y+TICLENGTH)
+	    call gtext (gp, x, y+.005, ltext, "v=b;h=c;s=.25;u=0")
+	    y=IM1BL_Y
+	    call gline (gp, x, y, x, y-TICLENGTH)
+	    x = x + IM2BL_X - IM1BL_X
+	    y = IM2TR_Y
+	    call gline (gp, x, y, x, y+TICLENGTH)
+	    call gtext (gp, x, y+.005, ltext, "v=b;h=c;s=.25;u=0")
+	    y=IM2BL_Y
+	    call gline (gp, x, y, x, y-TICLENGTH)
+	}
+
+	# Put the titles on.
+	# We got the carrington rotation number from the cl.
+
+	call sprintf (ltext, SZ_LINE, "CARRINGTON ROTATION %d %s")
+	    call pargi (rotnum)
+	switch (type1) {
+	case T10830:
+	    call pargstr ("10830")
+	case TABSFLX:
+	    call pargstr ("ABS. FLUX")
+	case TWEIGHT:
+	    call pargstr ("WEIGHT")
+	case TFLUX:
+	    call pargstr ("FLUX")
+	case TPLRTY:
+	    call pargstr ("POLARITY")
+	}
+
+	x = IM1TR_X+.025
+	y = IM1BL_Y + (IM1TR_Y - IM1BL_Y) / 2.
+	call gtext (gp, x, y, ltext, "v=c;h=c;s=.5;u=0")
+	call sprintf (ltext, SZ_LINE, "CARRINGTON ROTATION %d %s")
+	    call pargi (rotnum)
+	switch (type2) {
+	case T10830:
+	    call pargstr ("10830")
+	case TABSFLX:
+	    call pargstr ("ABS. FLUX")
+	case TWEIGHT:
+	    call pargstr ("WEIGHT")
+	case TFLUX:
+	    call pargstr ("FLUX")
+	case TPLRTY:
+	    call pargstr ("POLARITY")
+	}
+
+	x = IM2TR_X+.025
+	y = IM2BL_Y + (IM2TR_Y - IM2BL_Y) / 2.
+	call gtext (gp, x, y, ltext, "v=c;h=c;s=.5;u=0")
+
+	# Put on the dates at the appropriate longitudes.
+	# Get the dates and longitudes from the image header.
+	# Read dates until we run out.
+	# This code alternates between long and short tics for the dates.
+	# For this to work it is assumed that the dates are in
+	# cronological order.
+
+	# Get the first date and longitude from the image header to check
+	# whether or not there are any dates.
+
+	count = 1
+	call sprintf (ltext, SZ_LINE, "DATE%04d")
+	    call pargi (count)
+	dateyn = imaccf (im1, ltext)
+	if (dateyn == NO)
+	    call error(0, "no dates in image header")
+	obsdate = imgeti (im1, ltext)
+	call sprintf (ltext, SZ_LINE, "LONG%04d")
+	    call pargi (count)
+	longituder = imgetr (im1, ltext)
+	longitude = int(longituder + .5)
+
+	# If we find some dates near the beginning of the list which have
+	# longitudes smaller than 180, they probably are some "extra" grams
+	# merged in to fill out the plot, don't plot these dates because they
+	# are really off the image and will come out in the wrong place if we
+	# allow them to be plotted.
+
+	while (longitude < 180) {
+	    count = count + 1
+	    call sprintf (ltext, SZ_LINE, "DATE%04d")
+	        call pargi (count)
+	    dateyn = imaccf (im1, ltext)
+	    if (dateyn == NO)
+		break
+	    obsdate = imgeti (im1, ltext)
+	    call sprintf (ltext, SZ_LINE, "LONG%04d")
+		call pargi (count)
+	    longituder = imgetr (im1, ltext)
+	    longitude = int(longituder + .5)
+	}
+
+	# Calculate the month/day/year.
+	month = obsdate/10000
+	day = obsdate/100 - 100 * (obsdate/10000)
+	year = obsdate - 100 * (obsdate/100)
+
+	up = FALSE
+	pastm = FALSE
+
+	while (dateyn == YES) {
+
+	    # We check to see whether or not we have gotten past 180 degrees
+	    # so that if we find some images near the end of the list with
+	    # longitudes greater than 180 degrees we will know not to plot 
+	    # them since they are off the image.  Longitudes of images in the
+	    # image merge list decrease as we go down the list.
+
+	    # Past the middle yet?
+	    if (longitude < 180)
+		pastm = true
+
+	    # Figure out where this longitude is in y on the image.
+	    y = real(IM1BL_Y) + ((360. - real(longitude))/360.) *
+	        real(IM1TR_Y - IM1BL_Y)
+	    x = real(IM1TR_X)
+
+	    # Draw the tic and the label.
+	    if (!up)
+	        call gline (gp, x, y, x+.005, y)
+	    else
+	        call gline (gp, x, y, x+.011, y)
+	    call sprintf(ltext, SZ_LINE, "%d/%d/%d")
+	        call pargi(month)
+	        call pargi(day)
+	        call pargi(year)
+	    if (!up)
+	        call gtext (gp, x+.006, y, ltext, "v=c;h=l;s=.20;u=0")
+	    else
+	        call gtext (gp, x+.012, y, ltext, "v=c;h=l;s=.20;u=0")
+
+	    # Do the other image.
+	    x = real(IM2TR_X)
+	    if (!up)
+	        call gline (gp, x, y, x+.005, y)
+	    else
+	        call gline (gp, x, y, x+.011, y)
+	    if (!up)
+	        call gtext (gp, x+.006, y, ltext, "v=c;h=l;s=.20;u=0")
+	    else
+	        call gtext (gp, x+.012, y, ltext, "v=c;h=l;s=.20;u=0")
+
+	    # Toggle up switch.
+	    up = !up
+
+	    count = count + 1
+	    call sprintf (ltext, SZ_LINE, "DATE%04d")
+	        call pargi (count)
+	    dateyn = imaccf (im1, ltext)
+
+	    if (dateyn == YES) {
+		# Calculate the month/day/year.
+	        obsdate = imgeti (im1, ltext)
+		month = obsdate/10000
+		day = obsdate/100 - 100 * (obsdate/10000)
+		year = obsdate - 100 * (obsdate/100)
+
+		# Read in the next longitude.
+	        call sprintf (ltext, SZ_LINE, "LONG%04d")
+	            call pargi (count)
+	        longituder = imgeti (im1, ltext)
+		longitude = int(longituder + .5)
+
+		# If we are past the middle and find a longitude in the list
+		# which is greater than 180 degrees, do not plot this date
+		# since it is off the image and will be plotted in the wrong
+		# place.
+
+		if (pastm && longitude > 180)
+		    dateyn = NO
+	    }
+	}	    # End of while loop on dates/longitudes.
+
+	# Fill in the gray scale.
+	delta_gray = 254./15.
+	do i = 1, 16 {
+	    gray[i] = 1.+real(i-1)*delta_gray+0.5
+	}
+	call gpcell (gp, gray, 16, 1, IMGBL_X, IMGBL_Y, IMGTR_X, IMGTR_Y)
+	
+	# Now map the input images from 360x180 to 180x360 and put them
+	# out to the image. We also map the data values into the appropriate
+	# gray scale.
+
+	# Get subrasters of the images.
+	subras1 = imgs2r (im1, 1, DIM_XCARMAP, 1, DIM_SQUAREIM)
+	subras2 = imgs2r (im2, 1, DIM_XCARMAP, 1, DIM_SQUAREIM)
+	
+	# Call the image maping routine on both images.
+	call remap (Memr[subras1], DIM_XCARMAP, DIM_SQUAREIM, Memr[imout1])
+	call remap (Memr[subras2], DIM_XCARMAP, DIM_SQUAREIM, Memr[imout2])
+
+	# Call the gray scale mapper.
+	call graymap (Memr[imout1], DIM_SQUAREIM, DIM_XCARMAP, Mems[imgray1],
+	    type1)
+	call graymap (Memr[imout2], DIM_SQUAREIM, DIM_XCARMAP, Mems[imgray2],
+	    type2)
+
+	# Put the images out to the final image.
+	xresolution = ggeti (gp, "xr")
+	yresolution = ggeti (gp, "yr")
+	mapx1 = IM1BL_X
+	mapx2 = IM1TR_X
+	mapy1 = IM1BL_Y
+	mapy2 = IM1TR_Y
+	call gpcell (gp, Mems[imgray1], DIM_SQUAREIM, DIM_XCARMAP, mapx1, mapy1,
+	    mapx2, mapy2)
+	mapx1 = IM2BL_X
+	mapx2 = IM2TR_X
+	mapy1 = IM2BL_Y
+	mapy2 = IM2TR_Y
+	call gpcell (gp, Mems[imgray2], DIM_SQUAREIM, DIM_XCARMAP, mapx1, mapy1,
+	    mapx2, mapy2)
+
+	# Put the system identification on the plot.
+	call sysid (system_id, SZ_LINE)
+	call gtext (gp, .51, .076, system_id, "h=c;s=0.45")
+
+	# Close the graphics pointer.
+	call gclose(gp)
+	call close(p)
+
+	call sfree (sp)
+end
+
+
+# BOX -- Draw a box around the square described by x1, y1 (bottom left corner)
+# and x2, y2 (top right corner).
+
+procedure box(gp, x1, y1, x2, y2)
+
+real	x1, y1		# bottom left corner position
+real	x2, y2		# top right corner position
+pointer	gp		# graphics pointer
+
+begin
+	call gline (gp, x1, y1, x1, y2)
+	call gline (gp, x1, y2, x2, y2)
+	call gline (gp, x2, y2, x2, y1)
+	call gline (gp, x2, y1, x1, y1)
+end
+
+
+# REMAP -- Reformat a 360x180 image into a 180x360 image by rotating the image
+# by 90 degrees clockwise.
+
+procedure remap (inim, x, y, outim)
+
+real	inim[x,y]		# input image
+real	outim[y,x]		# output image
+int	x, y			# size of images
+
+int	i, j	
+
+begin
+	do i = 1, x
+	    do j = 1, y
+		outim[j,x-i+1] = inim[i,j]
+end
+
+
+# GREYMAP -- Map an integer image into a short integer image using a specific
+# scaling algorithm to make the full scale 1 to 256.
+
+procedure graymap (inim, x, y, outim, type)
+
+real	inim[x,y]		# input image
+int	x, y			# size of images
+int	type			# type of image
+short	outim[x,y]		# output image
+
+real	zpp[5], zcc[5], zp, zc	# parameters for different image types
+int	i, j, index
+short	ztbl[512]		# grayscale map array, (in gryscl.inc)
+
+data	zpp /.25, .80, 0.2, 1.0, 100. /
+data	zcc /384., 80., 0., 128., 128. /
+include	"gryscl.inc"
+
+begin
+	# If the image is not a 10830 gram then just multiply each pixel
+	# by a constant and then add another constant. (different constants
+	# for flux, abs. flux, weight, and polarity)
+	# If it is a 10830 gram then multiply and add as above, then use
+	# the result as an index into a lookup table.  The table is enumerated
+	# above.
+
+	zp = zpp[type]
+	zc = zcc[type]
+	do i = 1, x {
+	    do j = 1, y {
+		outim[i,j] = inim[i,j] * zp + zc
+		if (type == 1) {                      # if this is a 10830 gram:
+		    if (outim[i,j] <= 0)	      # make it fit in the table
+			outim[i,j] = 1
+		    if (outim[i,j] > 512)
+			outim[i,j] = 512
+		    index = outim[i,j]
+		    outim[i,j] = ztbl[index] + 10     # look it up in the table.
+		}
+		if (outim[i,j] <= 0)                  # check boundaries
+		    outim[i,j] = 1
+		if (outim[i,j] >= 255)
+		    outim[i,j] = 254
+	    }
+	}
+end
+
+
+# GIMTYPE -- Get IMage TYPE.  Using information in the image header determine
+# what type of image it is. 1 = 10830, 2 = ABS. FLUX, 3 = WEIGHTS,
+# 4 = ABS. VALUE, 5 = POLARITY.
+
+procedure gimtype (im, type)
+
+pointer	im		# image pointer
+int	type		# type
+
+int	wavelength, imgeti()
+int	weightyn, absyn, polarityyn
+int	imaccf()
+
+begin
+	wavelength = imgeti (im, "WV_LNGTH")
+	weightyn = imaccf (im, "WEIGHTS")
+	absyn = imaccf (im, "ABS_VALU")
+	polarityyn = imaccf (im, "POLARITY")
+
+	if (weightyn == NO && absyn == NO && polarityyn == NO) {
+	    if (wavelength == 10830)
+		type = T10830
+	    if (wavelength == 8688)
+		type = TFLUX
+	}
+	if (weightyn == YES)
+	    type = TWEIGHT
+	if (absyn == YES)
+	    type = TABSFLX
+	if (polarityyn == YES)
+	    type = TPLRTY
+end
diff --git a/noao/imred/vtel/doc/destreak.hlp b/noao/imred/vtel/doc/destreak.hlp
new file mode 100644
index 00000000..ef05d905
--- /dev/null
+++ b/noao/imred/vtel/doc/destreak.hlp
@@ -0,0 +1,50 @@
+.help destreak Dec84 noao.imred.vtel
+.ih
+NAME
+destreak -- Remove streaks from Helium 10830 grams
+.ih
+USAGE
+destreak input_image output_image
+.ih
+PARAMETERS
+.ls input_image
+Image to be destreaked.
+.le
+.ls output_image
+Name to give destreaked output image (must be a separate image).
+.le
+.ls tempim
+Temporary image used for pixel storage between destreak passes.
+.le
+.ls verbose=no
+Flag to signal program that it should produce verbose output.
+.le
+.ls threshold = 4
+Squibby brightness threshold to use in determining limb points.
+.le
+.ih
+DESCRIPTION
+The helium 10830 grams as taken by the vacuum telescope have horizontal
+streaks caused by the detecting apparatus.  Destreak removes these streaks
+and the limb darkening
+using a two pass procedure.  First, for each diode, a function of the form
+'a + b*r**4', where r is the radius from disk center and a, b are parameters,
+is fit to the intensity distribution and is then subtracted from the data.
+Then a spatial filter is applied to the result and the final image is
+written to disk.  The full disk images are 2048 x 2048 and are taken using
+a 512 diode array which is scanned from west to east across the solar disk
+4 times.  Thus, data from a particular diode consists of four lines of the 
+image.
+.ih
+EXAMPLES
+1. To destreak "image1", put the output in "image2", put the temporary image in
+"temp2", and see verbose output, the command would be:
+
+.nf
+	vt> destreak image1 image2 temp2 v+
+.fi
+
+.ih
+SEE ALSO
+readvt, writevt, quickfit, getsqib, putsqib
+.endhelp
diff --git a/noao/imred/vtel/doc/destreak5.hlp b/noao/imred/vtel/doc/destreak5.hlp
new file mode 100644
index 00000000..8bf383fa
--- /dev/null
+++ b/noao/imred/vtel/doc/destreak5.hlp
@@ -0,0 +1,43 @@
+.help destreak5 Dec85 noao.imred.vtel
+.ih
+NAME
+destreak5 -- First pass of 10830 processing
+.ih
+USAGE
+destreak5 input_root output_root
+.ih
+PARAMETERS
+.ls input_root
+Root name for input files.
+.le
+.ls output_root
+Root name of output files.
+.le
+.ih
+DESCRIPTION
+Destreak5 takes as input the 5 files from a vacuum telescope 10830
+tape and produces 5 nearly identical files but with the streaks
+removed from the solar images and with the best fit ellipse parameters
+added to the image header.  The input files are expected to be in the
+directory 'imdir' and to have the extensions '001' thru '005'.  These
+input files are expected to be mag tape images produced by T2D.  The output
+files are stored in the current directory with the same extensions.
+Destreak5 calls 'readvt','quickfit', 'destreak', and various other utilities
+and is a cl script file.
+If an input image is not found, the processing for that image is skipped and
+a message is printed telling about the missing image.
+The next step in the 10830 reduction process is 'makehelium' which produces
+the projected daily grams.
+.ih
+EXAMPLES
+1. To destreak five files with root name m1585 and store the resulting images
+with root name M1585 the command would be:
+
+.nf
+	vt> destreak5 m1585 M1585
+.fi
+
+.ih
+SEE ALSO
+readvt, destreak, quickfit
+.endhelp
diff --git a/noao/imred/vtel/doc/dicoplot.hlp b/noao/imred/vtel/doc/dicoplot.hlp
new file mode 100644
index 00000000..5bb9f071
--- /dev/null
+++ b/noao/imred/vtel/doc/dicoplot.hlp
@@ -0,0 +1,36 @@
+.help dicoplot Dec84 noao.imred.vtel
+.ih
+NAME
+dicoplot -- Make plots of Carrington maps on the Dicomed
+.ih
+USAGE
+dicoplot input_image1 input_image2 rot_number
+.ih
+PARAMETERS
+.ls input_image1
+First image to plot on the output.
+.le
+.ls input_image2
+Second image to plot on the output.
+.le
+.ls rot_number
+Carrington rotation number.
+.le
+.ih
+DESCRIPTION
+Dicoplot produces plots on the Dicomed.
+.ih
+EXAMPLES
+1. To make a plot containing a 10830 gram and the associated weight gram where
+the carrington rotation number is 1841, the 10830 gram is "temp1",
+and the weight gram is "carweight" type:
+
+.nf
+	vt> dicoplot temp1 carweight 1841
+.fi
+
+The program gets information about the dates and longitudes from the image
+headers.
+.ih
+SEE ALSO
+.endhelp
diff --git a/noao/imred/vtel/doc/fitslogr.hlp b/noao/imred/vtel/doc/fitslogr.hlp
new file mode 100644
index 00000000..4a195e45
--- /dev/null
+++ b/noao/imred/vtel/doc/fitslogr.hlp
@@ -0,0 +1,58 @@
+.help fitslogr Dec85 noao.imred.vtel
+.ih
+NAME
+fitslogr -- Make a log of header information from a fits tape
+.ih
+USAGE
+fitslogr input_dev out_file startfnum endfnum
+.ih
+PARAMETERS
+.ls input_dev
+Tape drive, e.g. "mta1600" or just "mta"
+.le
+.ls out_file
+Name of output file to store information. Information is appended to this
+file to allow one to update a previously created file.
+.le
+.ls startfnum
+Tape file to start logging.
+.le
+.ls endfnum
+Tape file to stop logging.
+.le
+.ih
+DESCRIPTION
+Fitslogr reads FITS headers from successive tape files and compiles
+certain information into a single line of output for each file.
+Currently, the information output for each file includes:
+
+        Tape file number, IRAF image name, date, time, and the
+	Carrington longitude for each image.
+
+If all of these header parameters are not present, only the ones found
+will be printed out and garbage will come out for the empty parameters.
+The date is stored in a header parameter called OBS_DATE, the time is
+stored as 'seconds since midnight' in OBS_TIME and the Carrington
+longitude is stored in L_ZERO.
+To use this script, both the DATAIO package and the VTEL package must
+be loaded.
+.ih
+EXAMPLES
+1. To log all of the FITS images on a tape mounted on 'mta' and store the
+information in a file called 'CX052' the command would be:
+
+.nf
+	vt> fitslogr mta CX052 1 999
+.fi
+
+2. To log just the 40th through 60th files on mtb and see the output on
+your terminal, the command would be:
+
+.nf
+	vt> fitslogr mtb STDOUT 40 60
+.fi
+
+.ih
+SEE ALSO
+rfits
+.endhelp
diff --git a/noao/imred/vtel/doc/getsqib.hlp b/noao/imred/vtel/doc/getsqib.hlp
new file mode 100644
index 00000000..1bf24fb0
--- /dev/null
+++ b/noao/imred/vtel/doc/getsqib.hlp
@@ -0,0 +1,33 @@
+.help getsqib Jan85 noao.imred.vtel
+.ih
+NAME
+getsqib -- Extract a full disk squibby brightness image from a full disk image
+.ih
+USAGE
+getsqib inputimage outputimage
+.ih
+PARAMETERS
+.ls inputimage
+Name of image to get squibby brightness from.
+.le
+.ls outputimage
+Name of new output squibby brightness image.
+.le
+.ih
+DESCRIPTION
+Getsqib takes as input any full disk image and extracts the lower four bits
+from each pixel and stores this information in a new output image the same
+size as the input image.
+.ih
+EXAMPLES
+1. To extract the squibby brightness image from the image "test1" and store
+it in an image called "test1.sqib" the command would be:
+
+.nf
+	vt> getsqib test1 test1.sqib
+.fi
+
+.ih
+SEE ALSO
+putsqib
+.endhelp
diff --git a/noao/imred/vtel/doc/makehelium.hlp b/noao/imred/vtel/doc/makehelium.hlp
new file mode 100644
index 00000000..df27430c
--- /dev/null
+++ b/noao/imred/vtel/doc/makehelium.hlp
@@ -0,0 +1,38 @@
+.help makehelium Jan86 noao.imred.vtel
+.ih
+NAME
+makehelium -- Second pass of 10830 processing
+.ih
+USAGE
+makehelium input_root output_root
+.ih
+PARAMETERS
+.ls input_root
+Root name for input files.
+.le
+.ls output_root
+Root name of output files.
+.le
+.ih
+DESCRIPTION
+Makehelium takes the files output by 'destreak5' and projects them the
+small [180x180] maps.  The input files are expected to be in the current
+directory and have the extensions '1' thru '5'.  The output files are
+stored in the current directory with the extensions 'a1', 'a2', 'a3', 'b1', etc.
+This coding scheme is the same as that used in makeimages.  Note that the
+absolute value images for 10830 grams should be thrown out since they are
+garbage.
+Makehelium calls 'rmap' and 'imdelete' and is a cl script file.
+.ih
+EXAMPLES
+1. To run makehelium on five files with root name m1585 and store the resulting
+images with root name M1585 the command would be:
+
+.nf
+	vt> makehelium m1585 M1585
+.fi
+
+.ih
+SEE ALSO
+rmap
+.endhelp
diff --git a/noao/imred/vtel/doc/makeimages.hlp b/noao/imred/vtel/doc/makeimages.hlp
new file mode 100644
index 00000000..d5f5fe31
--- /dev/null
+++ b/noao/imred/vtel/doc/makeimages.hlp
@@ -0,0 +1,64 @@
+.help makeimages Jan86 noao.imred.vtel
+.ih
+NAME
+makeimages -- Magnetogram batch processing script
+.ih
+USAGE
+makeimages input_root output_root
+.ih
+PARAMETERS
+.ls input_root
+Root name for input files.
+.le
+.ls output_root
+Root name of output files.
+.le
+.ih
+DESCRIPTION
+Makeimages processes 5 magnetograms from raw data tape images into projected
+small [180x180] maps.  The input images are expected be output from T2D,
+be in the current imdir, and have the extensions '001' through '005'.
+The output files are stored in the current directory with the extensions
+'a1', 'a2', 'a3', 'b1', etc.  The output image coding scheme is the following:
+
+.nf
+	On the filename extensions the first character is a letter
+	corresponding to the tape file position.
+		a = first file on tape
+		b = second
+		    .
+		    .
+		e = fifth
+
+	The second character specifies which type of image this is.
+		1 = data
+		2 = absolute value
+		3 = weights
+.fi
+
+Note: A logical directory called "scratch" must be set up before this
+program is run.  This logical directory must point to the directory
+containing the input images.  This can be set up as in the following
+example:
+
+vt> set scratch = "scr1:[recely]"
+
+where this particular directory is a VAX/VMS type name.  If the image
+files are in the user's home directory then "scratch" can be set to
+"home".
+
+Makeimages calls 'readvt', 'quickfit', 'rmap',
+'delete', and 'imdelete' and is a cl script.
+.ih
+EXAMPLES
+1. To process five magnetograms with root name m1585 and produce output images
+with the root name M1585, the command would be.
+
+.nf
+	vt> makeimages m1585 M1585
+.fi
+
+.ih
+SEE ALSO
+readvt, quickfit, rmap, delete, imdelete
+.endhelp
diff --git a/noao/imred/vtel/doc/merge.hlp b/noao/imred/vtel/doc/merge.hlp
new file mode 100644
index 00000000..24dbb778
--- /dev/null
+++ b/noao/imred/vtel/doc/merge.hlp
@@ -0,0 +1,90 @@
+.help merge Dec84 noao.imred.vtel
+.ih
+NAME
+merge -- Merge together daily synoptic grams into a complete Carrington map
+.ih
+USAGE
+merge outimage outweight outabs outratio month day year
+.ih
+PARAMETERS
+.ls outimage
+Name of output image.
+.le
+.ls outweight
+Output image containing weights, number of pixels per pixel.
+.le
+.ls outabs
+Output image containing the sums of the absolute values of the flux.
+Not used when merging 10830 maps.
+.le
+.ls outratio
+Output image containing the ratio of outimage/outabs.
+Not used when merging 10830 maps.
+.le
+.ls month, day, year
+Date of the center of this Carrington rotation.
+.le
+.ls longout = 180
+Longitude of the center of this Carrington rotation.
+.le
+.ls mergelist = "mergelist"
+File containing list of files to be merged.
+.le
+.ih
+DESCRIPTION
+Merge adds up daily synoptic grams to produce a Carrington rotation map.
+the input images are 180x180 and the output images are 360x180.  The input
+images are read from the file mergelist.  Merge then weights the input
+image as cos**4 in x where the center of the image corresponds to zero angle
+and the left and right edges of the image correspond to -90 and +90 degrees
+respectively. The input image consists of an unweighted "data" image,
+a weight image, and an absolute value image.  The summing is done on the
+"data" image, on the weight image, and on the absolute value image
+separately to produce three output images.  Finally the "data" image is
+divided by the absolute value image to produce a 4th output image.
+If 10830 data is being merged there are only two(2) images per day, the
+"data" image and the "weight" image.  Also there are only two(2) output images,
+the "data" merged image and the "weights" merged image.
+A note about the mergelist file, the three grams for each day must be stored
+in the following sequence (data, absolute value, weight) for magnetograms
+and the two grams for each day must be stored as (data, weight) for 10830.
+The filenames must be one file name per line in the mergelist and files
+for different days must be grouped together, for example mergelist might look
+like:
+
+.nf
+	MAG01                                  MAG01
+	MAG01a                                 MAG01w
+	MAG01w     for magnetograms or         MAG02      for 10830 grams
+	MAG02                                  MAG02w
+	MAG02a
+	MAG02w
+.fi
+
+for merging only two days of data where the first day is MAG01 and the second
+is MAG02. The 'a' extension stands for absolute value and the 'w' for weights.
+.ih
+EXAMPLES
+1. To merge a number of images on disk into output images called "im",
+"imweight", "imabs", and "imratio", where the date corresponding to the
+center of the Carrington map is 3/20/84 the command would be (magnetograms):
+
+.nf
+	vt> merge im imweight imabs imratio 3 20 84
+.fi
+
+The same command used for 10830 grams would be:
+
+.nf
+	vt> merge im imweight 3 20 84
+.fi
+
+2. If you have the list of files to be merged listed in a file called "mlist"
+instead of "mergelist" the command would be modified to read:
+
+.nf
+	vt> merge im imweight 3 20 84 mergelist="mlist"
+.fi
+.ih
+SEE ALSO
+.endhelp
diff --git a/noao/imred/vtel/doc/mrotlogr.hlp b/noao/imred/vtel/doc/mrotlogr.hlp
new file mode 100644
index 00000000..f86dbc0e
--- /dev/null
+++ b/noao/imred/vtel/doc/mrotlogr.hlp
@@ -0,0 +1,63 @@
+.help mrotlogr Jul86 "noao.imred.vtel"
+.ih
+NAME
+mrotlogr -- Make a log of header information from a fits tape (Carrington maps).
+.ih
+USAGE
+mrotlogr input_dev out_file startfnum endfnum append
+.ih
+PARAMETERS
+.ls input_dev
+Tape drive, e.g. "mta1600" or just "mta"
+.le
+.ls out_file
+Name of output file to store information. Information is appended to this
+file to allow one to update a previously created file.
+.le
+.ls startfnum
+Tape file to start logging.
+.le
+.ls endfnum
+Tape file to stop logging.
+.le
+.ls append
+Flag to signal that we are appending to an existing file.
+.le
+.ih
+DESCRIPTION
+Mrotlogr reads FITS headers from successive tape files and compiles
+certain information into a single line of output for each file.
+Currently, the information output for each file includes:
+
+.nf
+        Tape file number, IRAF image name, date, time, and the
+	Carrington longitude for each image.
+.fi
+
+If all of these header parameters are not present, only the ones found
+will be printed out and garbage will come out for the empty parameters.
+The date is stored in a header parameter called OBS_DATE, the time is
+stored as 'seconds since midnight' in OBS_TIME and the Carrington
+longitude is stored in L_ZERO.
+To use this script, both the DATAIO package and the VTEL package must
+be loaded.
+.ih
+EXAMPLES
+1. To log all of the FITS images on a tape mounted on 'mta' and store the
+information in a file called 'CX052' the command would be:
+
+.nf
+	vt> mrotlogr mta CX052 1 999 no
+.fi
+
+2. To log just the 40th through 60th files on mtb and see the output on
+your terminal, the command would be:
+
+.nf
+	vt> mrotlogr mtb STDOUT 40 60 no
+.fi
+
+.ih
+SEE ALSO
+rfits
+.endhelp
diff --git a/noao/imred/vtel/doc/mscan.hlp b/noao/imred/vtel/doc/mscan.hlp
new file mode 100644
index 00000000..d6b7f46b
--- /dev/null
+++ b/noao/imred/vtel/doc/mscan.hlp
@@ -0,0 +1,86 @@
+.help mscan May88 noao.imred.vtel
+.ih
+NAME
+mscan -- Read sector scans from tape into IRAF images
+.ih
+USAGE
+mscan input
+.ih
+PARAMETERS
+.ls input
+File template or device, e.g. "junk" or "s*" or "mta1600[1]" or "mtb800"
+.le
+.ls files
+List of tape file numbers or ranges delimited by commas, e.g. "1-3,5-8".
+`Files' is requested only if no file number is given in `input' and the
+input is tape.
+Files will be read in ascending order, regardless of the order of the list.
+Reading will terminate if EOT is reached, thus a list such as "1-999"
+may be used to read all the files on the tape.
+.le
+.ls verbose = yes
+Flag to signal program that it should produce verbose output.  This means
+header information.
+.le
+.ls makeimage = yes
+Flag to signal the program that it should make images.  If this parameter
+is set to no, the header will be read and decoded but no data will be read
+and no image will be produced on disk.
+.le
+.ls brief = yes
+Flag to make mscan produce brief filenames for the output images.  These
+filenames have the form [svb]nnn e.g. s034 or b122.  The b is for a brightness
+image, the v is for a velocity image, and the s is for a select image.  The
+'nnn' is the tape sequence number or the filenumber in a template expansion.
+If this flag is set to false the long filenames described below in the 
+"Description" section will be produced.
+.le
+.ls select = yes
+Flag to tell the program to make a select image.
+.le
+.ls bright = yes
+Flag to tell the program to make a brightness image.
+.le
+.ls velocity = yes
+Flag to tell the program to make a velocity image.
+.le
+.ih
+DESCRIPTION
+Mscan reads all or selected area scans from a vacuum telescope tape
+and formats the data into multiple IRAF images.  Type 1, 2, and 3 area
+scans can produce 3 output images and type 4 produces one output image.
+The long image names are assembled in the following way:
+.nf
+
+     The first letter is one of [bsv] for brightness, select, or velocity.
+     The next two digits are the day of the month.
+     Underbar.
+     The next 4 digits are the hour and minute.
+     Underbar.
+     Finally there is a three digit tape sequence number.
+     ie.
+
+		 b13_1709_002
+.fi
+
+.ih
+EXAMPLES
+1. To read files 5-7 from mta at 1600 bpi, the command would be:
+
+.nf
+	vt> mscan mta1600 5-7
+.fi
+
+2. To see the header information only for file 6, one could use the command:
+
+.nf
+	vt> mscan mta1600[6] make-
+.fi
+
+3. To read file 4 from mta and only produce a velocity image:
+
+.nf
+	vt> mscan mta[4] bri- sel-
+.fi
+
+.endhelp
diff --git a/noao/imred/vtel/doc/pimtext.hlp b/noao/imred/vtel/doc/pimtext.hlp
new file mode 100644
index 00000000..e78fdc8d
--- /dev/null
+++ b/noao/imred/vtel/doc/pimtext.hlp
@@ -0,0 +1,110 @@
+.help pimtext May86 noao.imred.vtel
+.ih
+NAME
+pimtext -- Put image text. Use pixel font to write text into image.
+.ih
+USAGE
+pimtext iraf_files
+.ih
+PARAMETERS
+.ls iraf_files
+Image or images to be written into.  This entry may contain wild cards and
+will be expanded into however many files match the wild card.
+.le
+.ls refim
+Reference image to pull date and time parameters from in the event the "ref"
+flag is set.
+.le
+.ls ref
+Reference flag.  When set, causes the program to take information (date/time)
+from the reference image and write it into the image or images expanded from
+the template "iraf_images".
+.le
+.ls x = 10
+X position (column) in image to write text.
+.le
+.ls y = 10
+Y position (line) in image to write text.
+.le
+.ls xmag = 2
+Factor by which to magnify the text in the x direction.  This must be an
+integer.  The pixelfont is expanded by pixel replication.  The font width
+at xmag=1 is 6.
+.le
+.ls ymag = 2
+Factor by which to magnify the text in the y direction.  This must be an
+integer.  The pixelfont is expanded by pixel replication.  The font width
+at ymag=1 is 7.
+.le
+.ls val = -10000
+Value to put in text pixels.
+.le
+.ls setbgnd = yes
+Boolean parameter to signal the program to fill in the area behind the
+characters with pixels set to bgndval.
+.le
+.ls bgndval = 10000
+Pixel value to use to fill in background in text block.
+.le
+.ls date = yes
+Flag that instructs the program to look for the date in the 
+image header and write it into the image.  If the date and time
+flags are both set, both will be written into the image as a single
+string.
+.le
+.ls time = yes
+Flag that instructs the program to look for the time in the 
+image header and write it into the image.
+.le
+.ls text
+Text string to write into image.
+.le
+.ih
+DESCRIPTION
+Pimtext writes either the date and/or time or the indicated text string into
+the image or images specified.
+Pimtext, by default, writes the date and/or time into the image in the lower
+left corner.  If it cannot find the date or time pimtext will give a warning
+and read a text string from the users terminal.  If the date and time flags are
+set to 'no', pimtext will take the text string to be written from the user.
+The position of the text may be adjusted by setting
+the parameters 'x' and 'y' which set the lower left pixel of
+the text block.  The pixels in the text block behind the characters may
+be set to a particular value when the 'setbgnd' flag is set.  The pixel
+values used to write the text and the background can be set by adjusting
+the parameters 'val' and 'bgndval'.  If the text overlaps the image
+edge in the X direction it will be truncated.  If it overlaps in Y it will
+not be written.
+The user may magnify the text by adjusting the "xmag" and "ymag" parameters.
+The default (2,2) is a nice size for display in a 512 by 512 image.  Bigger
+images may need bigger text, smaller images may need smaller text.
+The "ref" flag is used to write information from one image into another
+image.
+
+.ih
+EXAMPLES
+1. To write the date and time into the three images s13_1709_001, v13_1709_001,
+and b13_1709_001 (assuming the directory contains only these three images)
+the command would be:
+
+.nf
+	vt> pimtext ?13*
+.fi
+
+2. To write the text string "hello world" into the image 'testim' the command
+would be
+
+.nf
+	vt> pimtext testim 'hello world' date=no time=no
+.fi
+
+3. To write the date and time into the images s1, s2, s3, s4 and position
+the text at pixel 30,30, and turn off the text background fill, the command
+would be:
+
+.nf
+	vt> pimtext s* x=30 y=30 setbgnd=no
+.fi
+.ih
+SEE ALSO
+.endhelp
diff --git a/noao/imred/vtel/doc/putsqib.hlp b/noao/imred/vtel/doc/putsqib.hlp
new file mode 100644
index 00000000..f6400cfe
--- /dev/null
+++ b/noao/imred/vtel/doc/putsqib.hlp
@@ -0,0 +1,38 @@
+.help putsqib Jan85 noao.imred.vtel
+.ih
+NAME
+putsqib -- Merge a full disk image with a squibby brightness image
+.ih
+USAGE
+putsqib inputimage sqibimage outputimage
+.ih
+PARAMETERS
+.ls inputimage
+Name of data image to merge with squibby brightness image.
+.le
+.ls sqibimage
+Name of squibby brightness image to merge with data image.
+.le
+.ls outputimage
+Name of new, merged, output image.
+.le
+.ih
+DESCRIPTION
+Putsqib accepts as input a data image and a squibby brightness image.  It
+multiplies each pixel in the input data image by 16 and adds the associated
+pixel from the squibby brightness input image.  The pixel is then written
+to the new, output image.
+.ih
+EXAMPLES
+1. To merge a data image called 'data' and a squibby brightness image called
+'sqib' and store the result in an image called 'complete', the command
+would be:
+
+.nf
+	vt> putsqib data sqib complete
+.fi
+
+.ih
+SEE ALSO
+getsqib
+.endhelp
diff --git a/noao/imred/vtel/doc/quickfit.hlp b/noao/imred/vtel/doc/quickfit.hlp
new file mode 100644
index 00000000..41621b6d
--- /dev/null
+++ b/noao/imred/vtel/doc/quickfit.hlp
@@ -0,0 +1,59 @@
+.help quickfit Dec84 noao.imred.vtel
+.ih
+NAME
+quickfit -- Fit an ellipse to the limb for a full disk scan
+.ih
+USAGE
+quickfit image
+.ih
+PARAMETERS
+.ls image
+Name of image to be fit.
+.le
+.ls threshold = 4
+Squibby brightness threshold to use in determining limb points.
+.le
+.ls xguess = 1024
+X coordinate of center of first guess circle.
+.le
+.ls yguess = 1024
+Y coordinate of center of first guess circle.
+.le
+.ls halfwidth = 50
+Halfwidth of window centered on previous limb point to search through
+for a limb point on the current line.
+.le
+.ls rowspace = 20
+Number of rows to skip between limbpoints near center in y.
+.le
+.ls rejectcoeff = .02
+Least squares rejection coefficient.  If radius of a limbpoint is more than
+this far from the limb, where limbradius = 1.0, it is not used in the fit.
+.le
+.ih
+DESCRIPTION
+Quickfit finds the least squares best fit ellipse to the limb in a full
+disk scan.  Quickfit returns the ellipse parameters (x,y coordinates of
+the ellipse center and the x and y semidiameters), the number of limbpoints
+found, the number of limbpoints rejected, and the fraction of limb
+points rejected by the least squares routine.  This 'fraction rejected'
+allows the user to determine to some extent the goodness of the data and
+allows him or her to rerun Quickfit with different parameters to take
+this goodness into account.  Quickfit also returns the sub-earth latitude
+and longitude when in verbose mode.  The ellipse and ephemeris parameters
+are stored in the image header for future reference.
+.ih
+EXAMPLES
+1. To find the best fit ellipse for the limb in an image called "image1" and to
+see verbose output, one would use the following command:
+
+.nf
+	vt> quickfit image1 v+
+.fi
+
+This will also use the default values of rowspace, halfwidth,
+and rejectcoeff.
+
+.ih
+SEE ALSO
+.endhelp
diff --git a/noao/imred/vtel/doc/readvt.hlp b/noao/imred/vtel/doc/readvt.hlp
new file mode 100644
index 00000000..b9d6abe7
--- /dev/null
+++ b/noao/imred/vtel/doc/readvt.hlp
@@ -0,0 +1,86 @@
+.help readvt May87 noao.imred.vtel
+.ih
+NAME
+readvt -- Read vacuum telescope full disk grams
+.ih
+USAGE
+readvt input_fd files output_image
+.ih
+PARAMETERS
+.ls input_fd
+File or device template, e.g. "mta1600[1]" or "mtb800" or "junk" or "s*"
+.le
+.ls files
+List of tape file numbers or ranges delimited by commas, e.g. "1-3,5-8".
+`Files' is requested only if no file number is given in `input'.
+Files will be read in ascending order, regardless of the order of the list.
+Reading will terminate if EOT is reached, thus a list such as "1-999"
+may be used to read all the files on the tape.
+.le
+.ls output_image template
+Name to give output image.  If the input file template is not a magtape
+specification then this can be an IRAF filename template to be
+expanded into a list of files.  If the number of files in the input
+template and in the output template do not match and if the output
+template expands to one filename then that filename is used as a
+root name to which filenumbers are appended for each input file.
+i.e. "junk" becomes "junk001", "junk002", etc.  If the input template
+is a magtape without a filenumber attached, i.e. "mta", the
+output name is used as a root name and the file number is appended
+for each file read.
+.le
+.ls verbose = no
+Flag to signal program that it should produce verbose output.  This includes
+header information and progress reports.
+.le
+.ls headeronly = no
+Flag to signal the program that it should only print out header information
+and quit without reading the data.  The 'verbose' flag must be set to yes
+to use this flag since otherwise the header information will not be printed.
+This flag is used to look at headers on the tape to check dates, times
+and observation types.
+.le
+.ls robust = no
+Flag to signal program that it should ignore a wrong observation type in the
+image header.
+.le
+.ih
+DESCRIPTION
+Readvt reads any one of the grams on a vacuum telescope tape and puts the
+data into an IRAF image.  The IRAF image is 2048x2048 short integers.
+.ih
+EXAMPLES
+1. To read the second image from mta at 1600 bpi, store the image into "image1"
+and see verbose output the command would be:
+
+.nf
+	vt> readvt mta1600[2] image1 v+
+.fi
+
+2. To look at the header information of the 4th file on a tape which is on
+mtb and which was written at 1600 bpi, the command would be:
+
+.nf
+	vt> readvt mtb1600[4] v+ h+
+.fi
+
+3. To read the disk files "s001", "s002", "s003", "s004" and put the output
+images into the files "s001i", "s002i", "s003i", "s004i" without
+verbose output (assuming no other file in the directory starts with "s")
+the command would be:
+
+.nf
+	vt> readvt s* s*//i
+.fi
+
+4. To read the first five files on mta and put the output images into files
+images with root name HHH the command would be:
+
+.nf
+	vt> readvt mta 1-5 HHH
+.fi
+
+.ih
+SEE ALSO
+writevt
+.endhelp
diff --git a/noao/imred/vtel/doc/rmap.hlp b/noao/imred/vtel/doc/rmap.hlp
new file mode 100644
index 00000000..e4b4a645
--- /dev/null
+++ b/noao/imred/vtel/doc/rmap.hlp
@@ -0,0 +1,47 @@
+.help rmap Dec84 noao.imred.vtel
+.ih
+NAME
+rmap -- Project a full disk gram into a 180x180 flat image
+.ih
+USAGE
+rmap inputimage outputimage outweight outabs
+.ih
+PARAMETERS
+.ls inputimage
+Name of image to be projected.
+.le
+.ls outputimage
+Name to give output data image.
+.le
+.ls outweight
+Name to give output weight image.
+.le
+.ls outabs
+Name to give output absolute value image.
+.le
+.ih
+DESCRIPTION
+Rmap accepts as input a full disk carrington gram in a 2048x2048 IRAF image
+and projects it into a 180x180 IRAF image such that the lines of longitude
+and latitude are straight lines.  The output is the data image, the weight
+image (which is the count of the number of pixels of the input image which
+were summed to produce the single output pixel), and the absolute value image
+which is the same as the data image except that the absolute value of each
+input pixel is taken before being summed into the output pixel.
+Rmap calculates the mean field, the mean of the absolute value of the field,
+and the number of pixels in the original gram used to make the projection.
+These three parameters are stored in the output "data" image header as
+MEAN_FLD, MEANAFLD, and NUMPIX respectively.
+.ih
+EXAMPLES
+1. To project an image called "im10830" and produce output images "im10830.d",
+"im10830.w", and "im10830.a", one would use the following command:
+
+.nf
+	vt> rmap im10830 im10830.d im10830.w im10830.a
+.fi
+
+.ih
+SEE ALSO
+readvt, quickfit, and merge.
+.endhelp
diff --git a/noao/imred/vtel/doc/syndico.hlp b/noao/imred/vtel/doc/syndico.hlp
new file mode 100644
index 00000000..25b4b0ee
--- /dev/null
+++ b/noao/imred/vtel/doc/syndico.hlp
@@ -0,0 +1,77 @@
+.help syndico May89 noao.imred.vtel
+.ih
+NAME
+syndico -- Make dicomed plots of full disk images (18 centimeters in diameter)
+.ih
+USAGE
+syndico image
+.ih
+PARAMETERS
+.ls image
+Image to plot on the dicomed.
+.le
+.ls logofile = iraf$noao/imred/vtel/nsolcrypt.dat
+File containing the text encoded NSO logo image.
+.le
+.ls device = dicomed
+Device on which to plot the image.
+.le
+.ls sbthresh = 2
+Squibby brightness threshold used to determine the limb for trimming.
+.le
+.ls plotlogo = yes
+Flag indicating whether or not to plot the logo.
+.le
+.ls verbose = yes
+Flag indicating to the program that it should give progress reports.
+.le
+.ls forcetype = no
+Flag to override the wavelength designation from the image header.
+.le
+.ls magnetic = yes
+If 'forcetype' = 'yes' then this flag designates that we should force
+to magnetic (8688).  If set to 'no' the type is forced to 10830.
+The effect of forcing the type is to choose which lookup table to
+use when scaling the image.
+.le
+.ls month
+Month the observation was taken (January = 1,,,December = 12).
+.le
+.ls day
+Day of the month the observation was taken.
+.le
+.ls year
+Year the observation was taken (two digits only, ie. 89 for 1989).
+.le
+.ls hour
+Hour of the day the observation was taken (universal time, 1-24).
+.le
+.ls minute
+Minute the observation was taken (0-59).
+.le
+.ls second
+Second the observation was taken (0-59).
+.le
+.ih
+DESCRIPTION
+Syndico produces full disk plots on the Dicomed.  The ephemeris data
+is used to estimate the radius of the image and the center of the
+disk is gotten from the image header.  Using this data, an image is
+made that is as close to 18 centimeters in diameter as possible.
+There are two greyscale lookup tables corresponding to the two types
+of image normally used, the magnetogram and the spectroheliogram.
+If the wavelength is something other than 8688 or 10830, a linear
+greyscale is used.
+
+The National Solar Observatory (tentative) logo is read from an encoded
+text file and put on the plot if requested (default).
+.ih
+EXAMPLES
+
+.nf
+	vt> syndico image1
+.fi
+
+.ih
+SEE ALSO
+.endhelp
diff --git a/noao/imred/vtel/doc/tcopy.hlp b/noao/imred/vtel/doc/tcopy.hlp
new file mode 100644
index 00000000..57a523cb
--- /dev/null
+++ b/noao/imred/vtel/doc/tcopy.hlp
@@ -0,0 +1,56 @@
+.help tcopy Oct85 noao.imred.vtel
+.ih
+NAME
+tcopy -- Tape to tape copy
+.ih
+USAGE
+tcopy input_fd output_fd
+.ih
+PARAMETERS
+.ls input_fd
+Tape file or device name for input, e.g. "mta1600[1]" or "mtb800"
+.le
+.ls files
+List of tape file numbers or ranges delimited by commas, e.g. "1-3,5-8".
+`Files' is requested only if no file number is given in `input_fd'.
+Files will be read in ascending order, reguardless of the order of the list.
+Reading will terminate if EOT is reached, thus a list such as "1-999"
+may be used to read all the files on the tape.
+.le
+.ls output_fd
+File or device name, e.g. "mta1600[1]" or "mtb800"  If a file number is not
+given the user will be asked whether or not this is a new tape.  If it is
+a new tape the file number "1" will be used.  If it is not a new tape, i.e. 
+it already has data on it, then file number "EOT" will be used.
+.le
+.ls new_tape = no
+New tape flag.  Usage is described above.
+.le
+.ls verbose = no
+Flag to signal program that it should print information about progress while
+running.
+.le
+.ih
+DESCRIPTION
+Tcopy copies files from one tape to another reporting read errors on the
+input tape as it goes.  Tcopy, when it encounters a read error, does its
+best to get as much data as possible by validating the input buffer after
+the error, guessing its length, and writing it out to the output tape.
+.ih
+EXAMPLES
+1. To copy all the files on mta to a new tape on mtb:
+
+.nf
+	vt> tcopy mta 1-999 mtb yes
+.fi
+
+2. To copy file 5 from mta and append it to the tape on mtb:
+
+.nf
+	vt> tcopy mta1600[5] mtb no
+.fi
+
+.ih
+SEE ALSO
+t2d
+.endhelp
diff --git a/noao/imred/vtel/doc/trim.hlp b/noao/imred/vtel/doc/trim.hlp
new file mode 100644
index 00000000..9962db80
--- /dev/null
+++ b/noao/imred/vtel/doc/trim.hlp
@@ -0,0 +1,33 @@
+.help trim Jan85 noao.imred.vtel
+.ih
+NAME
+trim -- Trim the limb. Zero all pixels off the limb in a full disk image
+.ih
+USAGE
+trim inputimage threshold
+.ih
+PARAMETERS
+.ls inputimage
+Name of data image to trim.
+.le
+.ls threshold
+Squibby brightness value to use as a threshold in determining the limb.
+.le
+.ih
+DESCRIPTION
+Trim scans all the pixels in an image and sets those pixels to zero that
+contain a squibby brightness smaller than the threshold value.  This is
+done in place, that is, the input image gets modified.
+.ih
+EXAMPLES
+1. To trim a data image called 'data' with a squibby brightness threshold
+of 4 (the standard value) the command would be:
+
+.nf
+	vt> trim data 4
+.fi
+
+.ih
+SEE ALSO
+getsqib, putsqib
+.endhelp
diff --git a/noao/imred/vtel/doc/unwrap.hlp b/noao/imred/vtel/doc/unwrap.hlp
new file mode 100644
index 00000000..67fad069
--- /dev/null
+++ b/noao/imred/vtel/doc/unwrap.hlp
@@ -0,0 +1,95 @@
+.help unwrap May87 noao.imred.vtel
+.ih
+NAME
+unwrap -- Filter an IRAF image; remove binary wrap-around.
+.ih
+USAGE
+unwrap listin listout
+.ih
+PARAMETERS
+.ls listin
+List of images to unwrap, this is an IRAF template.
+.le
+.ls listout
+List of output images, this is an IRAF template.  If the output list
+is the same as the input list, the unwrapping is done in-place.
+.le
+.ls threshold1 = 128
+Data jump threshold for first unwrap pass.
+.le
+.ls wrapval1 = 256
+Factor to multiply wrap value by for first unwrap pass.
+.le
+.ls threshold2 = 128
+Data jump threshold for second unwrap pass.
+.le
+.ls wrapval2 = 256
+Factor to multiply wrap value by for second unwrap pass.
+.le
+.ls cstart = 2
+Column of image to start unwrapping.  Columns are numbered from left to right.
+.le
+.ls step = 5
+Number of steps (1-5) to perform on image (unwrap1, difference, unwrap2,
+reconstruct, fixlines).
+.le
+.ls verbose = yes
+If set, program produces progress reports, etc.
+.le
+.ih
+DESCRIPTION
+Unwrap checks for binary wraparound in IRAF images.
+The algorithm consists of reading the image line by line, unwrapping
+each line, and writing the line out to another image.  The procedure
+for unwraping is a five step process.
+.ls Step one: unwrap1
+Unwrapping is accomplished by scanning the data line and looking for
+large jumps in the data values.  Large negative jumps are interpreted
+as data wrapping and large positive jumps are interpreted as data unwrapping.
+The program keeps track of the number of wraps, each data element in the
+array has wrapval1 * wrapnumber added.  This effectively unwraps an image
+in which the point to point variation in the data values is small compared
+to the variation caused by a binary wrap.
+.le
+.ls Step two: difference
+A difference image is produced from the above step one image by calculating
+the pixel to pixel difference between all of the pixels in the line.  The
+first column of the image is generally left intact so that the image can
+be reconstructed in a later step.  Step one often produces streaks in the
+image due to data variation large enough to mimic wrapping.  This step
+two difference image eliminates most of these streaks except for their
+point of origin, where the confusion occured.
+.le
+.ls Step three: unwrap2
+This is the second unwrapping step.  The image is unwrapped as in step
+one using the second set of unwrap values (threshold2, wrapval2).
+.le
+.ls Step four: reconstruct
+The original image is reconstructed from the step three image by
+adding pixel values successively to line pixels.
+.le
+.ls Step five: fixlines
+If bad lines (streaks) still can be found in the image, they are
+eliminated by replacing the line by the average of the lines above
+and below bad line.
+.le
+.ih
+EXAMPLES
+1. To unwrap an image called "continuum" and store the resulting image in
+"unwrapped", and use the default parameters, the command might be:
+
+.nf
+	vt> unwrap continuum unwrapped
+.fi
+
+2. To unwrap all the images in the directory starting with s1492 and store
+the unwrapped images in s1492*u, to start in column 31, to do four steps,
+and to see verbose output, the command might be:
+
+.nf
+	vt> unwrap s1494* s1492*//u cstart=31 step=4 v+
+.fi
+
+.ih
+SEE ALSO
+.endhelp
diff --git a/noao/imred/vtel/doc/vtblink.hlp b/noao/imred/vtel/doc/vtblink.hlp
new file mode 100644
index 00000000..0bb26779
--- /dev/null
+++ b/noao/imred/vtel/doc/vtblink.hlp
@@ -0,0 +1,53 @@
+.help vtblink Dec84 noao.imred.vtel
+.ih
+NAME
+vtblink -- Blink daily grams to check registration
+.ih
+USAGE
+vtblink 
+.ih
+PARAMETERS
+.ls imname1
+First image to be mapped.
+.le
+.ls imname2
+Subsequent images to be mapped
+.le
+.ls z1 = -3000.0
+Minimum grayscale intensity to be mapped during 'display'.
+.le
+.ls z2 = 3000.0
+Maximum grayscale intensity to be mapped during 'display'.
+.le
+.ih
+DESCRIPTION
+Vtblink allows the user to blink successive frames of data on the IIS.  The
+program calculates the offset between grams based on the
+longitudes for each image.  Vtblink will ask for each successive image 
+and will display it on the next (mod 4) IIS frame.
+After each image is displayed the user is put back out in the cl so that he/she
+can use any of the images$tv tasks to analyze the data.  The user returns to
+the blink program by typing 'bye' to the cl prompt.  To exit the program the
+user enters the "end" for the filename.  Images are displayed with the grayscale
+limits set by default to -3000.0 and 3000.0.  These values correspond to the
+parameters z1 and z2 which may be given on the command line.  If the user
+forgets which IIS frame contains which image, he/she can enter "stat" to the
+"next image" prompt and will get a list of which images are in which frames.
+.ih
+EXAMPLES
+1. To run vtblink with the default gray scale parameters just type:
+
+.nf
+	vt> vtblink
+.fi
+
+2. To run vtblink with gray scale parameters z1=-4000.0, z2=4000.0, the
+command would be:
+
+.nf
+	vt> vtblink z1=-4000.0 z2=4000.0
+.fi
+.ih
+SEE ALSO
+display, blink, lumatch
+.endhelp
diff --git a/noao/imred/vtel/doc/vtexamine.hlp b/noao/imred/vtel/doc/vtexamine.hlp
new file mode 100644
index 00000000..20bf13eb
--- /dev/null
+++ b/noao/imred/vtel/doc/vtexamine.hlp
@@ -0,0 +1,50 @@
+.help vtexamine Jan86 noao.imred.vtel
+.ih
+NAME
+vtexamine -- examine the headers and record structure of vacuum telescope files
+.ih
+USAGE
+mtexamine tape_file
+.ih
+PARAMETERS
+.ls tape_file
+Tape file, e.g. "mta1600[2]" or "mta1600".
+.le
+.ls files
+List of tape file numbers or
+ranges delimited by commas, e.g. "1-3,5-8".
+File_list is requested only if no file number is given in tape_file.
+Files will be read in ascending order, regardless of the order of the list.
+Reading
+will terminate if EOT is reached, thus a list such as "1-999"
+may be used to read all the files on the tape.
+.le
+.ls headers=yes
+Decode and print header information from each file examined.
+.le
+.ih
+DESCRIPTION
+By default, vtexamine decodes and prints header and record
+structure information for each file examined.  The header
+information can be turned off by setting headers=no.
+.ih
+EXAMPLES
+1. To see the header information and determine the record structure of all the
+files on a vacuum telescope tape and send the result to the file vtdump:
+
+.nf
+	vt> vtexamine mtb1600 1-999 > vtdump
+.fi
+
+2. To just get the record structure for the third file on a vacuum telescope
+tape the command would be:
+
+.nf
+	vt> vtexamine mtb1600[3] headers=no
+.fi
+.ih
+BUGS
+The IRAF magtape i/o routines do not permit data beyond a double EOF
+to be accessed. Therefore vtexamine cannot be used to examine tapes with
+embedded double EOFs.
+.endhelp
diff --git a/noao/imred/vtel/doc/writetape.hlp b/noao/imred/vtel/doc/writetape.hlp
new file mode 100644
index 00000000..6159c016
--- /dev/null
+++ b/noao/imred/vtel/doc/writetape.hlp
@@ -0,0 +1,35 @@
+.help writetape Jan86 noao.imred.vtel
+.ih
+NAME
+writetape -- Write 5 grams to tape in full disk format. (Used as
+intermediate step in 10830 processing.
+.ih
+USAGE
+writetape input_root tape_name
+.ih
+PARAMETERS
+.ls getname
+Root name for input files.
+.le
+.ls getmtape
+Tape file descriptor.
+.le
+.ih
+DESCRIPTION
+Writetape takes as input five(5) full disk grams in IRAF image format
+and writes them to tape in a format identical to the original full disk
+grams produced on the vacuum telescope.  The input image names are expected
+to be the "input_root" name concatenated with the numbers "1", "2", ... "5".
+Writetape calls 'writevt' and is a cl script file.
+.ih
+EXAMPLES
+1. To write five files with root name m1585 to tape mta, the command would be:
+
+.nf
+	vt> writetape m1585 mta
+.fi
+
+.ih
+SEE ALSO
+readvt, writevt
+.endhelp
diff --git a/noao/imred/vtel/doc/writevt.hlp b/noao/imred/vtel/doc/writevt.hlp
new file mode 100644
index 00000000..3475a5c4
--- /dev/null
+++ b/noao/imred/vtel/doc/writevt.hlp
@@ -0,0 +1,43 @@
+.help writevt Dec84 noao.imred.vtel
+.ih
+NAME
+writevt -- Write vacuum telescope full disk grams to tape
+.ih
+USAGE
+writevt input_image output_fd
+.ih
+PARAMETERS
+.ls input_image
+Name of input image.
+.le
+.ls output_fd
+File or device name, e.g. "mta1600[1]" or "mtb800"  If a file number is not
+given the user will be asked whether or not this is a new tape.  If it is
+a new tape the file number "1" will be used.  If it is not a new tape, i.e. 
+it already has data on it, then file number "EOT" will be used.
+.le
+.ls verbose = no
+Flag to signal program that it should produce verbose output.  This includes
+header information and progress reports.
+.le
+.ls new_tape = no
+New tape flag.  Usage is described above.
+.le
+.ih
+DESCRIPTION
+Writevt writes a full disk vacuum telescope gram in IRAF image format to tape.
+The IRAF image is 2048x2048 short integers.  The tape format is the same as
+that used to write original data tapes on the mountain.
+.ih
+EXAMPLES
+1. To write the image "image1" to mta at 1600 bpi at file number 3 and
+see verbose output the command would be:
+
+.nf
+	vt> writevt image1 mta1600[3] v+
+.fi
+
+.ih
+SEE ALSO
+readvt
+.endhelp
diff --git a/noao/imred/vtel/fitslogr.cl b/noao/imred/vtel/fitslogr.cl
new file mode 100644
index 00000000..42681118
--- /dev/null
+++ b/noao/imred/vtel/fitslogr.cl
@@ -0,0 +1,104 @@
+#{ FITSLOGR -- Read all the headers on a FITS tape and print out some
+# of the header information for each file.
+
+{
+    struct header, headline, tfile, irafname
+    struct obsdate, lzero, keyword
+    struct tape, outfile, zcm, meanafld, numpix, meanfld
+    struct *fp
+    int	sfnum, efnum, filenum, ssm
+    int	hours, minutes, seconds
+    bool append, mag
+
+    if (!deftask ("rfits")) {
+	print ("Task rfits not loaded. Load dataio and then try again.")
+	bye
+    }
+
+    # Get the tape name and the output file name.
+    tape = gettape
+    outfile = getout
+
+    # Get the starting and ending file numbers for the log.
+    sfnum = getsfnum
+    efnum = getefnum
+
+    # Get the append flag.
+    append = getapp
+
+    # Get the mag flag.
+    mag = getmag
+
+    if (!append) {
+	if (mag) {
+            print ("File      fname     date    time     L-zero   zcm      meanafld   numpix", >> outfile)
+	} else {
+            print ("File      fname     date    time     L-zero   meanfld  numpix", >> outfile)
+	}
+    }
+
+    filenum = sfnum
+    while (YES) {
+	
+	# Read the next fits header from the tape.
+        header = mktemp("temp")
+	fp = header
+	rfits (tape, filenum, make_image=no, long_header=yes, > header)
+
+	# Initialize the output variables.
+	tfile = "        "
+	irafname = "       "
+	obsdate = "        "
+	lzero = "            "
+	zcm = "     "
+	meanafld = "     "
+	numpix = "       "
+	hours = 0
+	minutes = 0
+	seconds = 0
+
+	# Now match keywords against this header to obtain needed output.
+tfile = filenum
+	while (fscan (fp, headline) != EOF) {
+	    keyword = substr(headline, 1, 8)
+	    if (keyword == "File: mt")
+		tfile = substr(headline, 7, 15)
+	    else if (keyword == "IRAFNAME")
+		irafname = substr(headline, 12, 18)
+	    else if (keyword == "OBS_DATE")
+		obsdate = substr(headline, 23, 30)
+	    else if (keyword == "OBS_TIME") {
+		ssm = int(substr(headline, 23, 30)) # Seconds Since Midnight.
+		hours = ssm/3600
+		minutes = (ssm - (hours*3600))/60
+		seconds = ssm - hours*3600 - minutes*60
+	    }
+	    else if (keyword == "L_ZERO  ")
+		lzero = substr(headline, 19, 26)
+	    else if (keyword == "ZCM     ")
+		zcm = substr(headline, 18, 26)
+	    else if (keyword == "MEANAFLD")
+		meanafld = substr(headline, 18, 26)
+	    else if (keyword == "MEAN_FLD")
+		meanfld = substr(headline, 18, 26)
+	    else if (keyword == "NUMPIX  ")
+		numpix = substr(headline, 19, 30)
+	    else if (keyword == "End of d") {
+		print (headline, >> outfile)
+		delete (header, verify-)
+		bye
+	    }
+	}
+	if (mag) {
+	    print (tfile, irafname, obsdate, "  ", hours, minutes, seconds,
+	        lzero, zcm, meanafld, numpix, >> outfile)
+	} else {
+	    print (tfile, irafname, obsdate, "  ", hours, minutes, seconds,
+	        lzero, meanfld, numpix, >> outfile)
+	}
+	filenum = filenum + 1
+        delete (header, verify-)
+	if (filenum > efnum)
+	    bye
+    }
+}
diff --git a/noao/imred/vtel/fitslogr.par b/noao/imred/vtel/fitslogr.par
new file mode 100644
index 00000000..f6d8c141
--- /dev/null
+++ b/noao/imred/vtel/fitslogr.par
@@ -0,0 +1,6 @@
+gettape,s,a,,,,Tape to read fits headers from (i.e. "mta")
+getout,s,a,,,,File to put output information in
+getsfnum,i,a,,,,File number on tape from which to start logging 
+getefnum,i,a,,,,File number on tape at which logging is to end
+getapp,b,a,,,,Append to existing file?
+getmag,b,a,,,,Is this data magnetic field? (yes = 8688  no = 10830)
diff --git a/noao/imred/vtel/gauss.x b/noao/imred/vtel/gauss.x
new file mode 100644
index 00000000..fc5f9211
--- /dev/null
+++ b/noao/imred/vtel/gauss.x
@@ -0,0 +1,16 @@
+procedure gauss (x, a, ymod, dyda, ma)
+
+real	x, a[ma], ymod, dyda[ma]
+int	ma
+
+real	arg, ex, fac
+
+begin
+	arg = (x - a(2))/a(3)
+	ex = exp(-arg**2)
+	fac = a(1)*ex*2.0*arg
+	ymod = a(1)*ex
+	dyda(1) = ex
+	dyda(2) = fac/a(3)
+	dyda(3) = fac*arg/a(3)
+end
diff --git a/noao/imred/vtel/getsqib.par b/noao/imred/vtel/getsqib.par
new file mode 100644
index 00000000..a148cafb
--- /dev/null
+++ b/noao/imred/vtel/getsqib.par
@@ -0,0 +1,2 @@
+image,s,q,,,,Image to get sqibimage from
+sqibimage,s,q,,,,New image to contain squibby brightness image
diff --git a/noao/imred/vtel/getsqib.x b/noao/imred/vtel/getsqib.x
new file mode 100644
index 00000000..76e7e44d
--- /dev/null
+++ b/noao/imred/vtel/getsqib.x
@@ -0,0 +1,55 @@
+include <mach.h>
+include <imhdr.h>
+include "vt.h"
+
+# GETSQIB -- Make a new image from a solar synoptic image containing just
+# the squibby brightness.
+
+procedure t_getsqib()
+
+char	image[SZ_FNAME]		# input image
+char	sqibimage[SZ_FNAME]	# output squibby brightness image
+
+int	i, numpix
+pointer	im, lgp, lpp, sqibim
+
+pointer	immap(), imgl2s(), impl2s()
+errchk	immap, imgl2s, impl2s
+
+begin
+	# Get parameters from the CL.
+	call clgstr ("image", image, SZ_FNAME)
+	call clgstr ("sqibimage", sqibimage, SZ_FNAME)
+
+	# Open image.
+	im = immap (image, READ_ONLY, 0)
+	sqibim = immap (sqibimage, NEW_COPY, im)
+
+	numpix = IM_LEN(im,1)
+	do i = 1, IM_LEN(im,2) {
+	    lgp = imgl2s (im, i)
+	    lpp = impl2s (sqibim, i)
+	    call sqibline (Mems[lgp], Mems[lpp], numpix)
+	}
+
+	# Unmap images.
+	call imunmap (im)
+	call imunmap (sqibim)
+end
+
+
+# SQIBLINE -- Unpack squibby brightness from line1 and put it into line2.
+
+procedure sqibline (line1, line2, numpix)
+
+short	line1[numpix]	# input image line
+short	line2[numpix]	# output image line
+int	numpix		# number of pixels in line
+
+int	i
+int	and()
+
+begin
+	do i = 1, numpix
+	    line2[i] = and(int(line1[i]),17B)
+end
diff --git a/noao/imred/vtel/gryscl.inc b/noao/imred/vtel/gryscl.inc
new file mode 100644
index 00000000..7198557a
--- /dev/null
+++ b/noao/imred/vtel/gryscl.inc
@@ -0,0 +1,52 @@
+data	(ztbl[i], i=1,10)  / 003, 003, 003, 003, 003, 003, 003, 003, 004, 005 /
+data	(ztbl[i], i=11,20) / 005, 005, 005, 005, 005, 005, 005, 005, 006, 006 /
+data	(ztbl[i], i=21,30) / 006, 006, 006, 006, 006, 006, 006, 006, 006, 007 /
+data	(ztbl[i], i=31,40) / 007, 007, 007, 007, 007, 007, 007, 007, 007, 008 /
+data	(ztbl[i], i=41,50) / 008, 008, 008, 008, 008, 008, 008, 008, 008, 009 /
+data	(ztbl[i], i=51,60) / 009, 009, 009, 009, 009, 009, 009, 009, 009, 010 /
+data	(ztbl[i], i=61,70) / 010, 010, 010, 010, 010, 010, 010, 010, 010, 010 /
+data	(ztbl[i], i=71,80) / 010, 011, 011, 011, 011, 011, 011, 011, 011, 012 /
+data	(ztbl[i], i=81,90) / 012, 012, 012, 012, 012, 012, 012, 013, 013, 013 /
+data	(ztbl[i], i=91,100) / 013, 013, 013, 014, 014, 014, 014, 014, 014, 015/
+data	(ztbl[i], i=101,110) /015, 015, 015, 015, 015, 015, 016, 016, 016, 016/
+data	(ztbl[i], i=111,120) /016, 016, 017, 017, 017, 017, 017, 017, 017, 018/
+data	(ztbl[i], i=121,130) /018, 018, 018, 018, 018, 018, 019, 019, 019, 019/
+data	(ztbl[i], i=131,140) /019, 019, 020, 020, 020, 020, 020, 020, 021, 021/
+data	(ztbl[i], i=141,150) /021, 021, 021, 021, 021, 022, 022, 022, 022, 022/
+data	(ztbl[i], i=151,160) /022, 022, 023, 023, 023, 023, 023, 023, 024, 024/
+data	(ztbl[i], i=161,170) /024, 024, 024, 024, 025, 025, 025, 025, 025, 026/
+data	(ztbl[i], i=171,180) /026, 026, 026, 026, 026, 027, 027, 027, 027, 027/
+data	(ztbl[i], i=181,190) /027, 028, 028, 028, 028, 028, 028, 029, 029, 029/
+data	(ztbl[i], i=191,200) /029, 029, 029, 029, 029, 030, 030, 030, 030, 030/
+data	(ztbl[i], i=201,210) /030, 030, 031, 031, 031, 031, 031, 031, 031, 031/
+data	(ztbl[i], i=211,220) /032, 032, 032, 032, 032, 032, 032, 033, 033, 033/
+data	(ztbl[i], i=221,230) /033, 033, 033, 034, 034, 034, 034, 034, 034, 035/
+data	(ztbl[i], i=231,240) /035, 035, 035, 035, 035, 036, 036, 036, 036, 036/
+data	(ztbl[i], i=241,250) /036, 037, 037, 037, 037, 037, 037, 038, 038, 038/
+data	(ztbl[i], i=251,260) /038, 038, 038, 039, 039, 039, 039, 039, 039, 040/
+data	(ztbl[i], i=261,270) /040, 040, 040, 040, 040, 041, 041, 041, 041, 041/
+data	(ztbl[i], i=271,280) /041, 042, 042, 042, 042, 042, 042, 042, 042, 043/
+data	(ztbl[i], i=281,290) /043, 043, 043, 044, 044, 044, 044, 045, 045, 045/
+data	(ztbl[i], i=291,300) /045, 046, 046, 047, 047, 048, 048, 049, 049, 050/
+data	(ztbl[i], i=301,310) /050, 051, 051, 052, 053, 054, 054, 055, 056, 057/
+data	(ztbl[i], i=311,320) /057, 057, 057, 058, 058, 059, 059, 060, 060, 060/
+data	(ztbl[i], i=321,330) /060, 061, 061, 063, 064, 065, 066, 067, 067, 068/
+data	(ztbl[i], i=331,340) /068, 069, 069, 070, 071, 072, 072, 073, 074, 075/
+data	(ztbl[i], i=341,350) /075, 076, 077, 078, 080, 082, 083, 084, 085, 086/
+data	(ztbl[i], i=351,360) /086, 086, 087, 087, 088, 089, 089, 090, 091, 093/
+data	(ztbl[i], i=361,370) /094, 095, 097, 099, 101, 102, 103, 105, 106, 108/
+data	(ztbl[i], i=371,380) /109, 111, 113, 114, 115, 118, 121, 125, 128, 130/
+data	(ztbl[i], i=381,390) /132, 135, 137, 140, 144, 148, 151, 154, 157, 162/
+data	(ztbl[i], i=391,400) /166, 172, 177, 180, 184, 192, 200, 207, 213, 219/
+data	(ztbl[i], i=401,410) /225, 231, 237, 240, 244, 246, 248, 250, 251, 252/
+data	(ztbl[i], i=411,420) /253, 253, 254, 254, 255, 255, 255, 255, 255, 255/
+data	(ztbl[i], i=421,430) /255, 255, 255, 255, 255, 255, 255, 255, 255, 255/
+data	(ztbl[i], i=431,440) /255, 255, 255, 255, 255, 255, 255, 255, 255, 255/
+data	(ztbl[i], i=441,450) /255, 255, 255, 255, 255, 255, 255, 255, 255, 255/
+data	(ztbl[i], i=451,460) /255, 255, 255, 255, 255, 255, 255, 255, 255, 255/
+data	(ztbl[i], i=461,470) /255, 255, 255, 255, 255, 255, 255, 255, 255, 255/
+data	(ztbl[i], i=471,480) /255, 255, 255, 255, 255, 255, 255, 255, 255, 255/
+data	(ztbl[i], i=481,490) /255, 255, 255, 255, 255, 255, 255, 255, 255, 255/
+data	(ztbl[i], i=491,500) /255, 255, 255, 255, 255, 255, 255, 255, 255, 255/
+data	(ztbl[i], i=501,510) /255, 255, 255, 255, 255, 255, 255, 255, 255, 255/
+data	(ztbl[i], i=511,512) /255, 255 /
diff --git a/noao/imred/vtel/imfglexr.x b/noao/imred/vtel/imfglexr.x
new file mode 100644
index 00000000..3c6d4649
--- /dev/null
+++ b/noao/imred/vtel/imfglexr.x
@@ -0,0 +1,76 @@
+include <mach.h>
+include <imhdr.h>
+include "vt.h"
+
+# IMFGLEXR -- IMFilt Get Line with EXtension Real.  Get a line from a
+# full disk solar image and extend the boundary appropriately for use
+# with acnvr.  All pixels outside the limb are set equal to the value
+# of the last pixel inside the limb.  The line is extended in size by
+# an amount given by 'extension' beyond the solar disk width.
+
+pointer procedure imfglexr (imptr, linenumber, el, extension)
+
+int	linenumber			# Line of input image to get
+int	extension			# Amount of boundary extension needed
+real	el[LEN_ELSTRUCT]		# limb ellipse structure
+pointer	imptr	   	 		# Input image pointer
+
+pointer	rlptr, sp, tmpptr
+real	p, n
+int	lpix1, lpix2
+int	linelength
+int	lexb, rexb, i
+short	k
+
+pointer	imgl2r()
+short	shifts()
+errchk	imgl2r
+
+begin
+	k = -4
+
+	# Calculate the left and right bounds of the extended data.
+	lexb = E_XCENTER[el] - E_XSEMIDIAMETER[el] - extension
+	rexb = E_XCENTER[el] + E_XSEMIDIAMETER[el] + extension
+
+	# Extend 10 extra pixels beyond the minimum.
+	lexb = lexb - 10
+	rexb = rexb + 10
+	linelength = IM_LEN(imptr,1)
+
+	# Make a temporary short buffer for stripping.
+	call smark (sp)
+	call salloc (tmpptr, linelength, TY_SHORT)
+
+	# Get a line in the normal way. Point the real pointer to it.
+	rlptr = imgl2r (imptr, linenumber)
+
+	# Copy the line into the short array for stripping.
+	do i = 1, linelength
+	    Mems[tmpptr+i-1] = short(Memr[rlptr+i-1])
+
+	# Strip off the squibby brightness. Put back into real array.
+	do i = 1, linelength
+	    Memr[rlptr+i-1] = real(shifts(Mems[tmpptr+i-1], k))
+
+	# If the whole line is off the limb, return NULL.
+	if (abs(linenumber - E_YCENTER[el]) >= E_YSEMIDIAMETER[el])
+	    return(NULL)
+
+	# Use ellipse parameters to determine where the limb intersections are.
+	p = (real(linenumber) - E_YCENTER[el])**2/E_YSEMIDIAMETER[el]**2
+	n = (1.0 - p) * E_XSEMIDIAMETER[el]**2
+
+	# The two limb points are:
+	lpix1 = int(-sqrt(abs(n)) + .5) + E_XCENTER[el]
+	lpix2 = int(sqrt(abs(n)) + .5) + E_XCENTER[el]
+
+	# Extend the boundary of the data  beyond the limb
+	# by duplicating the last inside_the_limb pixel.  This extension
+	# is done out to lexb on the left and rexb on the right.
+
+	call amovkr (Memr[rlptr+lpix1+1], Memr[rlptr+lexb], lpix1-1-lexb)
+	call amovkr (Memr[rlptr+lpix2-1], Memr[rlptr+lpix2+1], rexb-1-lpix2)
+	call sfree (sp)
+	return (rlptr)
+end
diff --git a/noao/imred/vtel/imfilt.x b/noao/imred/vtel/imfilt.x
new file mode 100644
index 00000000..1f25efcf
--- /dev/null
+++ b/noao/imred/vtel/imfilt.x
@@ -0,0 +1,170 @@
+include <mach.h>
+include <imhdr.h>
+include <imset.h>
+include "vt.h"
+
+# IMFILT -- Apply a spatial averageing filter to an image by convolving the
+# image with a filter kernel.  Return the resulting image in a separate
+# image file.
+
+procedure imfilt (inim, outim, kernel, kxdim, kydim, el)
+
+pointer	inim, outim		        # input and output images
+int	kxdim, kydim		        # dimensions of convolution kernel
+real	kernel[kxdim, kydim]	        # convolution kernel
+real	el[LEN_ELSTRUCT]		# limb ellipse structure
+
+int	nlines, linelength, startline
+int	linebuf, outline, i
+int	k, offset, x2semi
+int	extension, startpix, lastline
+real	p, n, lpix1, lpix2
+pointer	lines, tmpptr, outptr, inptr, sp
+
+pointer	impl2r(), imgl2r(), imfglexr()
+errchk	impl2r, imfglexr, imgl2r
+
+begin
+	# Set up the pointer array on the stack.
+	call smark (sp)
+	call salloc (lines, kydim, TY_POINTER)
+
+	# Calculate the extension.
+	extension = kxdim / 2
+	offset = E_XCENTER[el] - E_XSEMIDIAMETER[el]
+	x2semi = 2 * E_XSEMIDIAMETER[el]
+
+	# Startpix is the x-coordinate of the beginning of the 1-D array
+	# we pass to the convolution vector routine.  If wrong, return.
+
+	startpix = offset - extension
+	if (startpix <= 0) {
+	    call printf ("convolution kernel too wide for this image\n")
+	    return
+	}
+
+	# Get the dimensions of the image.
+	linelength = IM_LEN(inim, 1)
+	nlines = IM_LEN(inim, 2)
+
+	# Pointers to the input and the output images are passed to this
+	# subroutine by the user.
+	
+	# Use imseti to set up the appropriate number of input buffers.
+	call imseti (inim, IM_NBUFS, kydim+1)
+
+	# Read in the necessary number of input image lines to initially
+	# fill all but one of the input line buffers.
+	# First, skip over all lines that are off the limb.
+	# The size of the output image is defined prior to the call
+	# to this subroutine, the output image is the same size as the
+	# input image.
+
+	startline = 0
+	Memi[lines] = NULL
+
+	# Skip over empty lines.
+	while (Memi[lines] == NULL) {
+	    startline = startline + 1
+	    Memi[lines] = imfglexr (inim, startline, el, extension)
+	}
+
+	# Fill (almost) the line buffer.
+	do linebuf = 1, kydim-2
+	    Memi[lines+linebuf] = imfglexr (inim, linebuf+startline,
+		el, extension)
+
+	# Copy the first startline lines from the input image into the
+	# output image.
+	do outline = 1, startline + (kydim/2) {
+
+	    # Put next line to output image, get the corresponding line from
+	    # the input image.
+	    inptr = imgl2r (inim, outline)
+	    outptr = impl2r (outim, outline)
+
+	    # Copy the input line into the ouput line. Strip sqib.
+	    do i = 1, DIM_VTFD {
+	        Memr[outptr+i-1] = Memr[inptr+i-1]/16.
+	    }
+	}
+
+	# Do the convolution, output line by output line.
+	do outline = (kydim/2) + startline, nlines {
+
+	    # Use ellipse parameters to determine where the limb
+	    # intersections are.
+	    p = (real(outline) - E_YCENTER[el])**2/E_YSEMIDIAMETER[el]**2
+	    n = (1.0 - p) * E_XSEMIDIAMETER[el]**2
+
+	    # The two limb points are:
+	    lpix1 = int(-sqrt(abs(n)) + .5) + E_XCENTER[el]
+	    lpix2 = int(sqrt(abs(n)) + .5) + E_XCENTER[el]
+
+	    # Keep a copy of this input line around for filling outside
+	    # the limb.
+	    inptr = imgl2r (inim, outline)
+
+	    # Scroll the buffer pointer array.
+	    if (outline > ((kydim/2) + startline))
+	        do i = 0, kydim - 2
+		    Memi[lines+i] = Memi[lines+i+1]
+
+	    # Get next line from input image, if it is off the limb then we
+	    # are done.
+
+	    tmpptr = imfglexr (inim, outline+((kydim/2)+1), el, extension)
+	    if (tmpptr == NULL) {
+		lastline = outline
+		break
+	    }
+	    Memi[lines+kydim-1] = tmpptr
+
+	    # Put next line to output image.
+	    outptr = impl2r (outim, outline)
+
+	    # Zero the output line.
+	    call aclrr (Memr[outptr], DIM_VTFD)
+
+	    # Here is the actual convolution, this is a do loop over the lines
+	    # of the kernel, each call to acnvrs adds the convolution of a
+	    # kernel line with an input line to the output line.
+
+	    do k = 1, kydim
+	        call acnvr (Memr[Memi[lines+k-1]+startpix], Memr[outptr+offset],
+		    x2semi, kernel[1,k], kxdim)
+
+	    # Fill outside the limb with orig data.
+	    do i = 1, lpix1 {
+	        Memr[outptr+i-1] = Memr[inptr+i-1]/16.
+	    }
+	    do i = lpix2, DIM_VTFD {
+	        Memr[outptr+i-1] = Memr[inptr+i-1]/16.
+	    }
+
+	    # Roundoff adjustment.
+	    do i = startpix, startpix+x2semi {
+		if (Memr[outptr+i-1] < 0.0)
+		    Memr[outptr+i-1] = Memr[outptr+i-1] - .5
+		else
+		    Memr[outptr+i-1] = Memr[outptr+i-1] + .5
+	    }
+	            
+	}    # End of do loop on outline.
+
+	# Clear the rest of the image.
+	do outline = lastline, DIM_VTFD {
+
+	    # Put next line to output image, get the corresponding line from
+	    # the input image.
+	    inptr = imgl2r (inim, outline)
+	    outptr = impl2r (outim, outline)
+
+	    # Copy the input line into the ouput line. Strip sqib.
+	    do i = 1, DIM_VTFD {
+	        Memr[outptr+i-1] = Memr[inptr+i-1]/16.
+	    }
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/vtel/imratio.x b/noao/imred/vtel/imratio.x
new file mode 100644
index 00000000..5586d204
--- /dev/null
+++ b/noao/imred/vtel/imratio.x
@@ -0,0 +1,29 @@
+# IMRATIO -- Divide two images and return the result in a third image.
+
+procedure imratio (numerator, denominator, ratio, xdim, ydim)
+
+real	numerator[xdim, ydim]		# input numerator
+real	denominator[xdim, ydim]		# input denominator
+real	ratio[xdim, ydim]		# output ratio image
+int	xdim, ydim			# dimensions of the image
+
+int	i
+real	ezero()
+extern	ezero()
+
+begin
+	do i = 1, ydim {
+	    call arltr (denominator[1,i], xdim, 1E-10, 0.0)
+	    call advzr (numerator[1,i], denominator[1,i], ratio[1,i], xdim,
+		ezero)
+	}
+end
+
+
+real procedure ezero (input)
+
+real	input
+
+begin
+	return (0.0)
+end
diff --git a/noao/imred/vtel/lstsq.x b/noao/imred/vtel/lstsq.x
new file mode 100644
index 00000000..9091fb48
--- /dev/null
+++ b/noao/imred/vtel/lstsq.x
@@ -0,0 +1,85 @@
+include	<mach.h>
+
+# LSTSQ -- Do a least squares fit to the data contained in the zz array.
+# Algorithm is from Jack Harvey. (Yes, it's a black box...)
+
+procedure lstsq (zz, mz, fno)
+
+real	zz[mz, mz]
+int	mz
+real	fno
+
+int	n, m, m1, i, j, k, l, l1
+real	fn, pp
+
+begin
+	n = mz - 2
+	m = n + 1
+	m1 = m + 1
+	fn = n
+
+	do i = 1, m {
+	    l = i + 1
+	    do k = 1, i-1 {
+		zz[i,l] = zz[i,l] - zz[k,l]**2
+	    }
+
+	    if (i == m)
+		break
+	    if (zz[i,l] >= 0.0)
+	        zz[i,l] = zz[i,l]**.5
+	    else {
+		call eprintf ("square root of negitive number in lstsq\n")
+	        zz[i,l] = 0.0
+	    }
+	    l1 = l + 1
+
+	    do j = l1, m1 {
+		do k = 1, i-1 {
+		    zz[i,j] = zz[i,j] - zz[k,l] * zz[k,j]
+		}
+		if (zz[i,l] >= EPSILONR)
+		    zz[i,j] = zz[i,j] / zz[i,l]
+		else
+		    call eprintf ("divide by zero in lstsq\n")
+	    }
+
+	    if (zz[i,l] >= EPSILONR)
+	        zz[i,i] = 1. / zz[i,l]
+	    else
+		call eprintf ("divide by zero in lstsq\n")
+	    do j = 1, i-1 {
+		pp = 0.
+		l1 = i - 1
+		do k = j, l1 {
+		    pp = pp + zz[k,l] * zz[k,j]
+		}
+	        zz[i,j] = -zz[i,i] * pp
+	    }
+	}
+
+	if ((fno - fn) >= EPSILONR)
+	    if ((zz[m,m1] / (fno - fn)) >= 0.0)
+	        zz[m1,m1] = .6745 * (zz[m,m1] / (fno - fn))**.5
+	    else {
+		call eprintf ("square root of negitive number in lstsq\n")
+	        zz[m1,m1] = 0.0
+	    }
+	else
+	    call eprintf ("divide by zero in lstsq\n")
+
+	do i = 1, n {
+	    zz[m,i] = 0.
+	    pp = 0.
+	    do j = i, n {
+		zz[m,i] = zz[m,i] + zz[j,i] * zz[j,m1]
+		pp = pp + zz[j,i] * zz[j,i]
+	    }
+	    if (pp >= 0.0)
+	        zz[m1,i] = zz[m1,m1] * pp**.5
+	    else {
+		call eprintf ("square root of negitive number in lstsq\n")
+	        zz[m1,i] = 0.0
+	    }
+	}
+end
diff --git a/noao/imred/vtel/makehelium.cl b/noao/imred/vtel/makehelium.cl
new file mode 100644
index 00000000..5cab8696
--- /dev/null
+++ b/noao/imred/vtel/makehelium.cl
@@ -0,0 +1,51 @@
+#{ MAKEHELIUM --
+
+# getinroot,s,a,,,,Input root file name
+# getoutroot,s,a,,,,Root filename for output images
+# inroot,s,h
+# outroot,s,h
+
+{
+	inroot = getinroot
+	outroot = getoutroot
+
+	if (access(inroot//"1.imh")) {
+	    rmap (inroot//"1", outroot//"a1", outroot//"a3", outroot//"a2",
+		"H"//outroot//"a")
+	    imdelete (inroot//"1")
+	} else {
+	    print (inroot//"1 not accessable")
+	}
+
+	if (access(inroot//"2.imh")) {
+	    rmap (inroot//"2", outroot//"b1", outroot//"b3", outroot//"b2",
+		"H"//outroot//"b")
+	    imdelete (inroot//"2")
+	} else {
+	    print (inroot//"2 not accessable")
+	}
+
+	if (access(inroot//"3.imh")) {
+	    rmap (inroot//"3", outroot//"c1", outroot//"c3", outroot//"c2",
+		"H"//outroot//"c")
+	    imdelete (inroot//"3")
+	} else {
+	    print (inroot//"3 not accessable")
+	}
+
+	if (access(inroot//"4.imh")) {
+	    rmap (inroot//"4", outroot//"d1", outroot//"d3", outroot//"d2",
+		"H"//outroot//"d")
+	    imdelete (inroot//"4")
+	} else {
+	    print (inroot//"4 not accessable")
+	}
+
+	if (access(inroot//"5.imh")) {
+	    rmap (inroot//"5", outroot//"e1", outroot//"e3", outroot//"e2",
+		"H"//outroot//"e")
+	    imdelete (inroot//"5")
+	} else {
+	    print (inroot//"5 not accessable")
+	}
+}
diff --git a/noao/imred/vtel/makehelium.par b/noao/imred/vtel/makehelium.par
new file mode 100644
index 00000000..426eda03
--- /dev/null
+++ b/noao/imred/vtel/makehelium.par
@@ -0,0 +1,4 @@
+getinroot,s,a,,,,Input root file name
+getoutroot,s,a,,,,Root filename for output images
+inroot,s,h
+outroot,s,h
diff --git a/noao/imred/vtel/makeimages.cl b/noao/imred/vtel/makeimages.cl
new file mode 100644
index 00000000..1da6b832
--- /dev/null
+++ b/noao/imred/vtel/makeimages.cl
@@ -0,0 +1,66 @@
+#{ MAKEIMAGES --
+
+# getinroot,s,a,,,,Input root file name
+# getoutroot,s,a,,,,Root filename for output images
+# inroot,s,h
+# outroot,s,h
+
+{
+	inroot = getinroot
+	outroot = getoutroot
+
+	if (access("scratch$"//inroot//"001")) {
+	    readvt ("scratch$"//inroot//"001", inroot//"tmp1")
+	    quickfit (inroot//"tmp1001",verbose=yes)
+	    rmap (inroot//"tmp1001",outroot//"a1",outroot//"a3",
+		outroot//"a2","H"//outroot//"a")
+	    delete ("scratch$"//inroot//"001")
+	    imdelete (inroot//"tmp1001")
+	} else {
+	    print ("scratch$"//inroot//"001 not accessable")
+	}
+
+	if (access("scratch$"//inroot//"002")) {
+	    readvt ("scratch$"//inroot//"002", inroot//"tmp2")
+	    quickfit (inroot//"tmp2001",verbose=yes)
+	    rmap (inroot//"tmp2001",outroot//"b1",outroot//"b3",
+		outroot//"b2","H"//outroot//"b")
+	    delete ("scratch$"//inroot//"002")
+	    imdelete (inroot//"tmp2001")
+	} else {
+	    print ("scratch$"//inroot//"002 not accessable")
+	}
+
+	if (access("scratch$"//inroot//"003")) {
+	    readvt ("scratch$"//inroot//"003", inroot//"tmp3")
+	    quickfit (inroot//"tmp3001",verbose=yes)
+	    rmap (inroot//"tmp3001",outroot//"c1",outroot//"c3",
+		outroot//"c2","H"//outroot//"c")
+	    delete ("scratch$"//inroot//"003")
+	    imdelete (inroot//"tmp3001")
+	} else {
+	    print ("scratch$"//inroot//"003 not accessable")
+	}
+
+	if (access("scratch$"//inroot//"004")) {
+	    readvt ("scratch$"//inroot//"004", inroot//"tmp4")
+	    quickfit (inroot//"tmp4001",verbose=yes)
+	    rmap (inroot//"tmp4001",outroot//"d1",outroot//"d3",
+		outroot//"d2","H"//outroot//"d")
+	    delete ("scratch$"//inroot//"004")
+	    imdelete (inroot//"tmp4001")
+	} else {
+	    print ("scratch$"//inroot//"004 not accessable")
+	}
+
+	if (access("scratch$"//inroot//"005")) {
+	    readvt ("scratch$"//inroot//"005", inroot//"tmp5")
+	    quickfit (inroot//"tmp5001",verbose=yes)
+	    rmap (inroot//"tmp5001",outroot//"e1",outroot//"e3",
+		outroot//"e2","H"//outroot//"e")
+	    delete ("scratch$"//inroot//"005")
+	    imdelete (inroot//"tmp5001")
+	} else {
+	    print ("scratch$"//inroot//"005 not accessable")
+	}
+}
diff --git a/noao/imred/vtel/makeimages.par b/noao/imred/vtel/makeimages.par
new file mode 100644
index 00000000..426eda03
--- /dev/null
+++ b/noao/imred/vtel/makeimages.par
@@ -0,0 +1,4 @@
+getinroot,s,a,,,,Input root file name
+getoutroot,s,a,,,,Root filename for output images
+inroot,s,h
+outroot,s,h
diff --git a/noao/imred/vtel/merge.par b/noao/imred/vtel/merge.par
new file mode 100644
index 00000000..3a0b0768
--- /dev/null
+++ b/noao/imred/vtel/merge.par
@@ -0,0 +1,9 @@
+mergelist,s,h,"mergelist",,,List of files to merge
+outputimage,s,q,"carmap",,,Outputimage
+outweight,s,q,"carweight",,,Output image weights
+outabs,s,q,"carabs",,,Absolute value image
+outratio,s,q,"carratio",,,Ratio: outputimage over absolute value image
+longout,r,h,180.0,1.,360.,Longitude of center of this carrington rotation
+mapmonth,i,q,,1,12,Month of center of this carrington rotation
+mapday,i,q,,1,31,Day of center of this carrington rotation
+mapyear,i,q,,1,99,Year of center of this carrington rotation
diff --git a/noao/imred/vtel/merge.x b/noao/imred/vtel/merge.x
new file mode 100644
index 00000000..79aa23eb
--- /dev/null
+++ b/noao/imred/vtel/merge.x
@@ -0,0 +1,762 @@
+include <mach.h>
+include	<imhdr.h>
+include	"vt.h"
+
+# MERGE -- Put together all appropriate daily grams to produce a full
+# carrington rotation map.  This is done both for the average input images
+# and for the absolute value input images.  The output of the program is
+# 4 images, average image, absolute value image, weight image, ratio of
+# first image to second image.
+
+procedure t_merge()
+
+char	mergelist[SZ_FNAME]		# list of images to be merged
+
+int	wavelength, listfd
+char	inputimage[SZ_FNAME]
+pointer	inputim
+
+pointer	immap()
+int	imgeti(), open(), fscan()
+errchk	immap, open
+
+begin
+	# Get the image name file from the cl and open it.
+	call clgstr ("mergelist", mergelist, SZ_FNAME)
+	listfd = open (mergelist, READ_ONLY, TEXT_FILE)
+
+	# Get the wavelength from the first image in the mergelist.
+	if (fscan (listfd) != EOF) {
+	    call gargwrd (inputimage, SZ_FNAME)
+	    inputim = immap (inputimage, READ_ONLY, 0)
+	    wavelength = imgeti (inputim, "WV_LNGTH")
+	    call close (listfd)
+	} else {
+	    call error (0, "No images in 'mergelist'")
+	    call close (listfd)
+	    return
+	}
+
+	if (wavelength == 8688)
+	    call mergem (mergelist, wavelength)
+	else
+	    call mergeh (mergelist, wavelength)
+end
+
+
+# MERGEM -- MERGE Magnetograms.
+
+procedure mergem (mergelist, wavelength)
+
+char	mergelist[SZ_FNAME]		# list of images to be merged
+int	wavelength			# wavelength of images
+
+pointer	outputim, outw, outa, outr
+pointer outptr, outwptr, outaptr, outrptr
+char	outputimage[SZ_FNAME], outweight[SZ_FNAME]
+char	outabs[SZ_FNAME], outratio[SZ_FNAME]
+real	longout, weight_tbl[SZ_WTBL], bzeroave
+int	i, mapmonth, mapday, mapyear
+
+real	clgetr()
+int	clgeti()
+pointer	immap(), imps2r()
+errchk	immap, imps2r
+
+begin
+	# Get parameters from the cl.
+
+	# Output images.
+	call clgstr ("outputimage", outputimage, SZ_FNAME)
+	call clgstr ("outweight", outweight, SZ_FNAME)
+	call clgstr ("outabs", outabs, SZ_FNAME)
+	call clgstr ("outratio", outratio, SZ_FNAME)
+
+	# Longitude of center of output Carrington rotation map.
+	longout = clgetr ("longout")
+
+	# Month, day, and year of the center of the output map.
+	mapmonth = clgeti ("mapmonth")
+	mapday = clgeti ("mapday")
+	mapyear = clgeti ("mapyear")
+
+	# Open output image.
+	outputim = immap (outputimage, NEW_IMAGE, 0)
+
+	# Define some parameters for the output images.
+	IM_NDIM(outputim) = 2
+	IM_LEN(outputim, 1) = DIM_XCARMAP
+	IM_LEN(outputim, 2) = DIM_SQUAREIM
+	IM_PIXTYPE(outputim) = TY_REAL
+
+	# Open the rest of the output images.
+	outw = immap (outweight, NEW_COPY, outputim)
+	outa = immap (outabs, NEW_COPY, outputim)
+	outr = immap (outratio, NEW_COPY, outputim)
+
+	# Map the outputimages into memory.
+	outptr = imps2r (outputim, 1, DIM_XCARMAP, 1, DIM_SQUAREIM)
+	outwptr = imps2r (outw, 1, DIM_XCARMAP, 1, DIM_SQUAREIM)
+	outaptr = imps2r (outa, 1, DIM_XCARMAP, 1, DIM_SQUAREIM)
+	outrptr = imps2r (outr, 1, DIM_XCARMAP, 1, DIM_SQUAREIM)
+
+	# Create weight table.
+	do i = 1,SZ_WTBL
+	    weight_tbl[i] = (cos((real(i-91)+.5)*3.1415926/180.))**4
+
+	call mmall (mergelist, Memr[outptr], Memr[outwptr], Memr[outaptr],
+	    outputim, outw, outa, outr, wavelength, weight_tbl, longout,
+	    mapmonth, mapday, mapyear, bzeroave)
+
+	# Fill the ratio image.
+	call imratio (Memr[outptr],Memr[outaptr],Memr[outrptr],DIM_XCARMAP,
+	    DIM_SQUAREIM)
+
+	# Write some information out to the image headers.
+	call imaddr (outputim, "AV_BZERO", bzeroave)
+	call imaddi (outputim, "WV_LNGTH", wavelength)
+	call imaddr (outw, "AV_BZERO", bzeroave)
+	call imaddr (outw, "WV_LNGTH", wavelength)
+	call imaddb (outw, "WEIGHTS", TRUE)
+	call imaddr (outa, "AV_BZERO", bzeroave)
+	call imaddr (outr, "AV_BZERO", bzeroave)
+	call imaddr (outa, "WV_LNGTH", wavelength)
+	call imaddr (outr, "WV_LNGTH", wavelength)
+	call imaddb (outa, "ABS_VALU", TRUE)
+	call imaddb (outr, "POLARITY", TRUE)
+	
+	# Weight the data image and the abs image.
+	call imratio (Memr[outptr],Memr[outwptr],Memr[outptr],DIM_XCARMAP,
+	    DIM_SQUAREIM)
+	call imratio (Memr[outaptr],Memr[outwptr],Memr[outaptr],DIM_XCARMAP,
+	    DIM_SQUAREIM)
+
+	# Close images
+	call imunmap (outputim)
+	call imunmap (outw)
+	call imunmap (outa)
+	call imunmap (outr)
+end
+
+
+# MERGEH -- MERGE Helium 10830 grams.
+
+procedure mergeh (mergelist, wavelength)
+
+char	mergelist[SZ_FNAME]		# list of images to merge
+int	wavelength			# wavelength of observation
+
+pointer	outputim, outw
+pointer outptr, outwptr
+char	outputimage[SZ_FNAME], outweight[SZ_FNAME]
+real	longout, weight_tbl[SZ_WTBL], bzeroave
+int	i, mapmonth, mapday, mapyear
+
+real	clgetr()
+int	clgeti()
+pointer	immap(), imps2r()
+errchk	immap, imps2r
+
+begin
+	# Get parameters from the cl.
+
+	# Output images.
+	call clgstr ("outputimage", outputimage, SZ_FNAME)
+	call clgstr ("outweight", outweight, SZ_FNAME)
+
+	# Longitude of center of output Carrington rotation map.
+	longout = clgetr ("longout")
+
+	# Month, day, and year of the center of the output map.
+	mapmonth = clgeti ("mapmonth")
+	mapday = clgeti ("mapday")
+	mapyear = clgeti ("mapyear")
+
+	# Open output image.
+	outputim = immap (outputimage, NEW_IMAGE, 0)
+
+	# Define some parameters for the output images.
+	IM_NDIM(outputim) = 2
+	IM_LEN(outputim, 1) = DIM_XCARMAP
+	IM_LEN(outputim, 2) = DIM_SQUAREIM
+	IM_PIXTYPE(outputim) = TY_REAL
+
+	# Open the other output image.
+	outw = immap (outweight, NEW_COPY, outputim)
+
+	# Map the outputimages into memory.
+	outptr = imps2r (outputim, 1, DIM_XCARMAP, 1, DIM_SQUAREIM)
+	outwptr = imps2r (outw, 1, DIM_XCARMAP, 1, DIM_SQUAREIM)
+
+	# Create weight table.
+	do i = 1,SZ_WTBL
+	    weight_tbl[i] = (cos((real(i-91)+.5)*3.1415926/180.))**4
+
+	call mhall (mergelist, Memr[outptr], Memr[outwptr], outputim,
+	    outw, wavelength, weight_tbl, longout, mapmonth,
+	    mapday, mapyear, bzeroave)
+
+	# Write some information out to the image headers.
+	call imaddr (outputim, "AV_BZERO", bzeroave)
+	call imaddi (outputim, "WV_LNGTH", wavelength)
+	call imaddr (outw, "AV_BZERO", bzeroave)
+	call imaddr (outw, "WV_LNGTH", wavelength)
+	call imaddb (outw, "WEIGHTS", TRUE)
+	
+	# Weight the data image.
+	call imratio (Memr[outptr],Memr[outwptr],Memr[outptr],DIM_XCARMAP,
+	    DIM_SQUAREIM)
+
+	# Close images.
+	call imunmap (outputim)
+	call imunmap (outw)
+end
+
+
+# MMALL -- Merge Magnetograms ALL.
+# Map in each input image, weight it, figure out where it goes
+# and add it to the output image.
+
+procedure mmall (mergelist, outarray, outarrayw, outarraya, outputim,
+	outw, outa, outr, wavelength, weight_tbl, longout, mapmonth, mapday,
+	mapyear, bzeroave)
+
+char	mergelist[SZ_FNAME]			# list of images to be merged
+int	wavelength				# wavelength of observations
+real	outarray[DIM_XCARMAP, DIM_SQUAREIM]	# output data array
+real	outarrayw[DIM_XCARMAP, DIM_SQUAREIM]	# output weights array
+real	outarraya[DIM_XCARMAP, DIM_SQUAREIM]	# output absolute value array
+pointer	inputim					# pointer to input image
+pointer	outputim				# pointer to output image
+pointer	outw					# pointer to weight image
+pointer	outa					# pointer to abs value image
+pointer	outr					# pointer to ratio image
+int	mapmonth, mapday, mapyear		# date of output map
+real	weight_tbl[SZ_WTBL]			# weight table
+real	longout					# longitude of map center
+real	bzeroave				# average b-zero for map
+
+char	inputimage[SZ_FNAME], inweight[SZ_FNAME], inabs[SZ_FNAME]
+pointer	inw, ina, inptr, inwptr, inaptr
+int	listfd, month, day, year, count
+real	longin, bzero, bzerosum
+int	obsdate, temp, i, j
+char	ltext[SZ_LINE]
+
+int	open(), fscan(), imgeti()
+real	imgetr()
+pointer	immap(), imgs2i(), imgs2s()
+errchk	open, immap, imgs2i, imgs2s
+
+begin
+	count = 0
+	bzerosum = 0.0
+	listfd = open (mergelist, READ_ONLY, TEXT_FILE)
+
+	# Zero the output images.
+	do i = 1, DIM_XCARMAP {
+	    do j = 1, DIM_SQUAREIM {
+		outarray[i,j] = 0.0
+		outarrayw[i,j] = 0.0
+		outarraya[i,j] = 0.0
+	    }
+	}
+
+	# Get inputimages from the mergelist until they are all used up.
+	while (fscan (listfd) != EOF) {
+	    call gargwrd (inputimage, SZ_FNAME)
+
+	    # Get absolute value image.
+	    if(fscan (listfd) != EOF)
+	        call gargwrd (inabs, SZ_FNAME)
+	    else
+	        call error (0, "wrong number of file names in mergelist")
+
+	    # Get weight image.
+	    if(fscan (listfd) != EOF)
+	        call gargwrd (inweight, SZ_FNAME)
+	    else
+	        call error (0, "wrong number of file names in mergelist")
+
+	    # Open input image, its corresponding weight map, and its
+	    # corresponding absolute value map.
+
+	    inputim = immap (inputimage, READ_ONLY, 0)
+	    inw = immap (inweight, READ_ONLY, 0)
+	    ina = immap (inabs, READ_ONLY, 0)
+
+	    bzero = imgetr (inputim, "B_ZERO")
+	    bzerosum = bzerosum + bzero
+	    longin = imgetr (inputim, "L_ZERO")
+	    obsdate = imgeti (inputim, "OBS_DATE")
+
+	    # Check to see that the date is same on the three input images.
+	    temp = imgeti (inw, "OBS_DATE")
+ 	    if (temp != obsdate) {
+		call eprintf ("ERROR: date on weight image differs from that ")
+		call eprintf ("on data image!\n")
+		break
+	    }
+
+	    temp = imgeti (ina, "OBS_DATE")
+	    if (temp != obsdate) {
+		call eprintf ("ERROR: date on abs image differs from that ")
+	        call eprintf ("on data image!\n")
+	        break
+	    }
+
+	    # Decode month, day, year.
+	    month = obsdate/10000
+	    day = obsdate/100 - 100 * (obsdate/10000)
+	    year = obsdate - 100 * (obsdate/100)
+
+	    # Pack a name for this date and longitude and then put them out
+	    # into the outputimages' headers.
+
+	    count = count + 1
+	    call sprintf (ltext, SZ_LINE, "DATE%04d")
+		call pargi (count)
+	    call imaddi (outputim, ltext, obsdate)
+	    call imaddi (outw, ltext, obsdate)
+	    call imaddi (outa, ltext, obsdate)
+	    call imaddi (outr, ltext, obsdate)
+
+	    call sprintf (ltext, SZ_LINE, "LONG%04d")
+		call pargi (count)
+	    call imaddr (outputim, ltext, longin)
+	    call imaddr (outw, ltext, longin)
+	    call imaddr (outa, ltext, longin)
+	    call imaddr (outr, ltext, longin)
+	    
+	    # Map the inputimage, the weight map, and abs_image into memory.
+	    inptr = imgs2i (inputim, 1, DIM_SQUAREIM, 1, DIM_SQUAREIM)
+	    inwptr = imgs2s (inw, 1, DIM_SQUAREIM, 1, DIM_SQUAREIM)
+	    inaptr = imgs2i (ina, 1, DIM_SQUAREIM, 1, DIM_SQUAREIM)
+
+	    # Weight this image and add it to the output image.
+	    call addmweight (Memi[inptr],Mems[inwptr],Memi[inaptr],outarray,
+	        outarrayw, outarraya, weight_tbl, longin, longout,
+		month, day, year, mapmonth, mapday, mapyear)
+
+	    # Close this input image.
+	    call imunmap (inputim)
+	    call imunmap (inw)
+	    call imunmap (ina)
+
+	} # end of do loop on input images
+
+	bzeroave = bzerosum/real(count)
+	call close (listfd)
+end
+
+
+# MHALL -- Merge Heliumgrams ALL.
+# Map in each input image, weight it, figure out where it goes
+# and add it to the output image.
+
+procedure mhall (mergelist, outarray, outarrayw, outputim,
+	outw, wavelength, weight_tbl, longout, mapmonth, mapday,
+	mapyear, bzeroave)
+
+char	mergelist[SZ_FNAME]			# list of images to be merged
+int	wavelength				# wavelength of observations
+real	outarray[DIM_XCARMAP, DIM_SQUAREIM]	# output data array
+real	outarrayw[DIM_XCARMAP, DIM_SQUAREIM]	# output weights array
+pointer	inputim					# pointer to input image
+pointer	outputim				# pointer to output image
+pointer	outw					# pointer to weight image
+int	mapmonth, mapday, mapyear		# date of output map
+real	weight_tbl[SZ_WTBL]			# weight table
+real	longout					# longitude of map center
+real	bzeroave				# average b-zero for map
+
+char	inputimage[SZ_FNAME], inweight[SZ_FNAME]
+pointer	inw, inptr, inwptr
+int	listfd, month, day, year, count
+real	longin, bzero, bzerosum
+int	obsdate, temp, i, j
+char	ltext[SZ_LINE]
+
+real	imgetr()
+int	open(), fscan(), imgeti()
+pointer	immap(), imgs2i(), imgs2s()
+errchk	open, immap, imgs2i, imgs2s
+
+begin
+	count = 0
+	bzerosum = 0.0
+	listfd = open (mergelist, READ_ONLY, TEXT_FILE)
+
+	# Zero the output images.
+	do i = 1, DIM_XCARMAP {
+	    do j = 1, DIM_SQUAREIM {
+		outarray[i,j] = 0.0
+		outarrayw[i,j] = 0.0
+	    }
+	}
+
+	# Get inputimages from the mergelist until they are all used up.
+	while (fscan (listfd) != EOF) {
+	    call gargwrd (inputimage, SZ_FNAME)
+
+	    # Get weight image.
+	    if (fscan (listfd) != EOF)
+	        call gargwrd (inweight, SZ_FNAME)
+	    else
+	        call error (0, "wrong number of file names in mergelist")
+
+	    # Open input image, its corresponding weight map, and its
+	    # corresponding absolute value map.
+
+	    inputim = immap (inputimage, READ_ONLY, 0)
+	    inw = immap (inweight, READ_ONLY, 0)
+
+	    bzero = imgetr (inputim, "B_ZERO")
+	    bzerosum = bzerosum + bzero
+	    longin = imgetr (inputim, "L_ZERO")
+	    obsdate = imgeti (inputim, "OBS_DATE")
+
+	    # Check to see that the date is same on the three input images.
+	    temp = imgeti (inw, "OBS_DATE")
+ 	    if (temp != obsdate) {
+		call eprintf ("ERROR: date on weight image differs from that ")
+		call eprintf ("on data image!\n")
+		break
+	    }
+
+	    # Decode month, day, year.
+	    month = obsdate/10000
+	    day = obsdate/100 - 100 * (obsdate/10000)
+	    year = obsdate - 100 * (obsdate/100)
+
+	    # Pack a name for this date and longitude and then put them out
+	    # into the outputimages' headers.
+
+	    count = count + 1
+	    call sprintf (ltext, SZ_LINE, "DATE%04d")
+		call pargi (count)
+	    call imaddi (outputim, ltext, obsdate)
+	    call imaddi (outw, ltext, obsdate)
+
+	    call sprintf (ltext, SZ_LINE, "LONG%04d")
+		call pargi (count)
+	    call imaddr (outputim, ltext, longin)
+	    call imaddr (outw, ltext, longin)
+	    
+	    # Map the inputimage, the weight map, and abs_image into memory.
+	    inptr = imgs2i (inputim, 1, DIM_SQUAREIM, 1, DIM_SQUAREIM)
+	    inwptr = imgs2s (inw, 1, DIM_SQUAREIM, 1, DIM_SQUAREIM)
+
+	    # Weight this image and add it to the output image.
+	    call addhweight (Memi[inptr], Mems[inwptr], outarray, outarrayw,
+		weight_tbl, longin, longout, month, day, year, mapmonth,
+		mapday, mapyear)
+
+	    # Close this input image.
+	    call imunmap (inputim)
+	    call imunmap (inw)
+
+	} # end of do loop on input images
+
+	bzeroave = bzerosum/real(count)
+	call close (listfd)
+end
+
+
+# ADDMWEIGHT -- Weight input image by cos(longitude - (L-L0))**4, and add
+# it to the output image in the proper place.
+
+procedure addmweight (inim, inwim, inaim, outim, outwim, outaim,
+	weight_tbl, longin, longout, month, day, year, mapmonth, mapday,
+	mapyear)
+
+int	inim[DIM_SQUAREIM, DIM_SQUAREIM]	# input image
+short	inwim[DIM_SQUAREIM, DIM_SQUAREIM]	# input image weights
+int	inaim[DIM_SQUAREIM, DIM_SQUAREIM]	# input absolute image
+real	outim[DIM_XCARMAP, DIM_SQUAREIM]	# outputimage
+real	outwim[DIM_XCARMAP, DIM_SQUAREIM]	# output image weights
+real	outaim[DIM_XCARMAP, DIM_SQUAREIM]	# output absolute image
+int	month, day, year			# date of input image
+int	mapmonth, mapday, mapyear		# date of output image
+real	weight_tbl[DIM_SQUAREIM]		# weight table
+real	longin, longout				# longitudes of images
+
+int	p1offset, p2offset, firstpix, lastpix, column, row
+int	offset, datein, dateout, temp, temp2
+int	d1900()
+
+begin
+	# Translate the two dates into julian day numbers to make comparisons
+	# simpler.
+
+	datein = d1900 (month, day, year)
+	dateout = d1900 (mapmonth, mapday, mapyear)
+
+	# Figure out the pixel offset between the first pixel of the input
+	# image and the first pixel of ther output image.
+	# Actually, there may be two pixel offsets for a particular image
+	# corresponding to the correct position of the image and the 360
+	# degree offset position.
+
+	p1offset = mod(abs(int(longin - longout + .5)), 360)    # This is one.
+	p2offset = 360 - p1offset                         # This is the other.
+
+	# Determine which side of the output image center is each of these
+	# offsets.
+
+	if (datein > dateout) {
+	    if (longout > 180) {
+	        if (((longin >= longout) && (longin <= 360))  || 
+		    (longin <= mod((longout + 180.),360.))) {
+		    if (p1offset < 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+	        } else {
+		    if (p1offset >= 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+		}
+	    } else {
+	        if ((longin >= longout) && (longin <= (longout + 180))) {
+		    if (p1offset <= 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+	        } else {
+		    if (p1offset >= 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+		}
+	    }
+        } else {
+	    if (longout < 180) {
+	        if (((longin >= (180 + longout)) && (longin <= 360))  || 
+		    (longin <= longout)) {
+		    if (p1offset < 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+	        } else {
+		    if (p1offset >= 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+		}
+	    } else {
+	        if ((longin < longout) && (longin > (longout - 180))) {
+		    if (p1offset < 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+	        } else {
+		    if (p1offset >= 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+		}
+	    }
+	}
+
+        # Make sure the sign is right
+        if (datein > dateout)
+	    offset = -offset
+
+        # Check for the case that the two longitudes are equal.
+        if (longin == longout) {
+	    if (abs(datein - dateout) <= 1) {
+	        offset = 0
+	    } else {
+	        call eprintf ("input day too far from center of output map\n")
+	        return
+	    }
+        }
+	    
+        # Check for the case that the two dates are equal.
+        if (datein == dateout)
+	    offset = longin - longout
+
+        # If the offset is too large then do not use this image.
+        if (abs(offset) > 240) {
+	    call eprintf ("input day too far from center of output map\n")
+	    return
+        }
+
+        # Determine what part, if not all, of the input image will lie on the
+        # output image.
+
+        firstpix = 1
+        if (offset < -90)
+	    firstpix = abs(offset+90)
+        lastpix = DIM_SQUAREIM
+        if (offset > 90) 
+	    lastpix = 180 - (offset - 90)
+
+
+        # Do all 180 columns in the image.
+	if (offset <= 0)
+	    temp = 91
+	else
+	    temp = 90
+
+	do column = firstpix,lastpix {
+	    do row = 1, DIM_SQUAREIM {
+	        temp2 = column + temp + offset
+	        outim[temp2,row] = outim[temp2, row] +
+		    inim[column, row] * weight_tbl[column]
+	        outwim[temp2,row] = outwim[temp2, row] +
+		    inwim[column, row] * weight_tbl[column]
+	        outaim[temp2,row] = outaim[temp2, row] +
+		    inaim[column, row] * weight_tbl[column]
+	    }
+	}
+end
+
+
+# ADDHWEIGHT -- Weight input image by cos(longitude - (L-L0))**4, and add
+# it to the output image in the proper place. (For 10830 grams)
+
+procedure addhweight (inim, inwim, outim, outwim, weight_tbl, longin, longout,
+	month, day, year, mapmonth, mapday, mapyear)
+
+int	inim[DIM_SQUAREIM, DIM_SQUAREIM]	# input image
+short	inwim[DIM_SQUAREIM, DIM_SQUAREIM]	# input image weights
+real	outim[DIM_XCARMAP, DIM_SQUAREIM]	# outputimage
+real	outwim[DIM_XCARMAP, DIM_SQUAREIM]	# output image weights
+int	month, day, year			# date of input image
+int	mapmonth, mapday, mapyear		# date of output image
+real	weight_tbl[DIM_SQUAREIM]		# weight table
+real	longin, longout				# longitudes of images
+
+int	p1offset, p2offset, firstpix, lastpix, column, row
+int	offset, datein, dateout, temp, temp2
+int	d1900()
+
+begin
+	# Translate the two dates into julian day numbers to make comparisons
+	# simpler.
+
+	datein = d1900 (month, day, year)
+	dateout = d1900 (mapmonth, mapday, mapyear)
+
+	# Figure out the pixel offset between the first pixel of the input
+	# image and the first pixel of ther output image.
+	# Actually, there may be two pixel offsets for a particular image
+	# corresponding to the correct position of the image and the 360
+	# degree offset position.
+
+	p1offset = mod(abs(int(longin - longout + .5)), 360)    # this is one.
+	p2offset = 360 - p1offset                         # this is the other.
+
+	# Determine which side of the output image center is each of these
+	# offsets.
+
+	if (datein > dateout) {
+	    if (longout > 180) {
+	        if (((longin >= longout) && (longin <= 360))  || 
+		    (longin <= mod((longout + 180.),360.))) {
+		    if (p1offset < 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+	        } else {
+		    if (p1offset >= 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+		}
+	    } else {
+	        if ((longin >= longout) && (longin <= (longout + 180))) {
+		    if (p1offset <= 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+	        } else {
+		    if (p1offset >= 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+		}
+	    }
+        } else {
+	    if (longout < 180) {
+	        if (((longin >= (180 + longout)) && (longin <= 360))  || 
+		    (longin <= longout)) {
+		    if (p1offset < 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+	        } else {
+		    if (p1offset >= 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+		}
+	    } else {
+	        if ((longin < longout) && (longin > (longout - 180))) {
+		    if (p1offset < 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+	        } else {
+		    if (p1offset >= 180)
+		        offset = p2offset
+		    else
+		        offset = p1offset
+		}
+	    }
+	}
+
+        # Make sure the sign is right.
+        if (datein > dateout)
+	    offset = -offset
+
+        # Check for the case that the two longitudes are equal.
+        if (longin == longout) {
+	    if (abs(datein - dateout) <= 1) {
+	        offset = 0
+	    } else {
+	        call eprintf ("Input day too far from center of output map.\n")
+	        return
+	    }
+        }
+	    
+        # Check for the case that the two dates are equal.
+        if (datein == dateout)
+	    offset = longin - longout
+
+        # If the offset is too large then do not use this image.
+        if (abs(offset) > 240) {
+	    call eprintf ("input day too far from center of output map\n")
+	    return
+        }
+
+        # Determine what part, if not all, of the input image will lie on the
+        # output image.
+
+        firstpix = 1
+        if (offset < -90)
+	    firstpix = abs(offset+90)
+        lastpix = DIM_SQUAREIM
+        if (offset > 90) 
+	    lastpix = 180 - (offset - 90)
+
+
+        # Do all 180 columns in the image.
+	if (offset <= 0)
+	    temp = 91
+	else
+	    temp = 90
+
+	do column = firstpix, lastpix {
+	    do row = 1, DIM_SQUAREIM {
+	        temp2 = column + temp + offset
+	        outim[temp2,row] = outim[temp2, row] +
+		    inim[column, row] * weight_tbl[column]
+	        outwim[temp2,row] = outwim[temp2, row] +
+		    inwim[column, row] * weight_tbl[column]
+	    }
+	}
+end
diff --git a/noao/imred/vtel/mkpkg b/noao/imred/vtel/mkpkg
new file mode 100644
index 00000000..3da8ea5a
--- /dev/null
+++ b/noao/imred/vtel/mkpkg
@@ -0,0 +1,59 @@
+# Make the VTEL Package
+
+$call	relink
+$exit
+
+update:
+	$call	relink
+	$call	install
+	;
+
+relink:
+	$set	LIBS = "-lxtools"
+	$update	libpkg.a
+	$omake	x_vtel.x
+	$link	x_vtel.o libpkg.a $(LIBS)
+	;
+
+install:
+	$move	x_vtel.e noaobin$
+	;
+
+libpkg.a:
+	d1900.x	
+	decodeheader.x	"vt.h" <mach.h>
+	destreak.x	"vt.h" <imhdr.h> <imset.h> <mach.h>
+	dicoplot.x	"gryscl.inc" "dicoplot.h" "vt.h" <gset.h> <imhdr.h>\
+			<imset.h> <mach.h> <math/curfit.h>
+	dephem.x	
+	gauss.x
+	getsqib.x	"vt.h" <imhdr.h> <mach.h>
+	imfglexr.x	"vt.h" <imhdr.h> <mach.h>
+	imfilt.x	"vt.h" <imhdr.h> <imset.h> <mach.h>
+	imratio.x	
+	textim.x	 <imhdr.h> <mach.h>
+	lstsq.x	         <mach.h>
+	merge.x		"vt.h" <imhdr.h> <mach.h>
+	mrqmin.x
+	mscan.x		"vt.h" <error.h> <mach.h>
+	numeric.x	"vt.h" "numeric.h" <mach.h>
+	pimtext.x       "vt.h"
+	pixbit.x	"asciilook.inc" "pixelfont.inc"
+	putsqib.x	"vt.h" <imhdr.h> <mach.h>
+	quickfit.x	"vt.h" <imhdr.h> <mach.h>
+	readheader.x	"vt.h" <mach.h> <fset.h>
+	readss1.x	"vt.h" <imhdr.h> <mach.h> <fset.h>
+	readss2.x	"vt.h" <imhdr.h> <mach.h> <fset.h>
+	readss3.x	"vt.h" <imhdr.h> <mach.h> <fset.h>
+	readss4.x	"vt.h" <imhdr.h> <mach.h> <fset.h>
+	readsubswath.x	"vt.h" <mach.h> <fset.h>
+	readvt.x	"vt.h" <imhdr.h> <mach.h> <fset.h>
+	rmap.x		"vt.h" "numeric.h" <imhdr.h> <mach.h>
+	syndico.x	"vt.h" "trnsfrm.inc" "syndico.h" <mach.h> <imhdr.h>\
+			<imset.h> <gset.h>
+	tcopy.x		"vt.h" <error.h> <fset.h> <mach.h> <printf.h>
+	trim.x		"vt.h" <imhdr.h> <mach.h>
+	unwrap.x	<imhdr.h> <mach.h>
+	vtexamine.x	"vt.h" <error.h> <fset.h> <mach.h> <printf.h>
+	writevt.x	"vt.h" <error.h> <fset.h> <mach.h>
+	;
diff --git a/noao/imred/vtel/mrotlogr.cl b/noao/imred/vtel/mrotlogr.cl
new file mode 100644
index 00000000..1612d030
--- /dev/null
+++ b/noao/imred/vtel/mrotlogr.cl
@@ -0,0 +1,68 @@
+#{ MROTLOGR -- Read all the headers on a FITS tape and print out some
+# of the header information for each file. (for Carrington rotation maps)
+
+{
+    struct header, headline, tfile, irafname
+    struct avbzero, keyword
+    struct tape, outfile
+    struct *fp
+    int	sfnum, efnum, filenum
+    bool append
+
+    if (!deftask ("rfits")) {
+	print ("Task rfits not loaded. Load dataio and then try again.")
+	bye
+    }
+
+    # Get the tape name and the output file name.
+    tape = gettape
+    outfile = getout
+
+    # Get the starting and ending file numbers for the log.
+    sfnum = getsfnum
+    efnum = getefnum
+
+    # Get the append flag.
+    append = getapp
+
+    if (!append) {
+        print ("File      fname    avbzero", >> outfile)
+    }
+
+    filenum = sfnum
+    while (YES) {
+	
+	# Read the next fits header from the tape.
+        header = mktemp("temp")
+	fp = header
+	rfits (tape, filenum, make_image=no, long_header=yes, > header)
+
+	# Initialize the output variables.
+	tfile = "        "
+	irafname = "       "
+	avbzero = "     "
+
+	# Now match keywords against this header to obtain needed output.
+	while (fscan (fp, headline) != EOF) {
+	    keyword = substr(headline, 1, 8)
+	    if (keyword == "File: mt")
+		tfile = substr(headline, 7, 15)
+	    else if (keyword == "IRAFNAME")
+		irafname = substr(headline, 12, 20)
+	    else if (keyword == "AV_BZERO")
+		avbzero = substr(headline, 19, 27)
+	    else if (keyword == "L_ZERO  ")
+		lzero = substr(headline, 19, 26)
+	    else if (keyword == "End of d") {
+		print (headline, >> outfile)
+		delete (header, verify-)
+		bye
+	    }
+	}
+	print (tfile, irafname, avbzero, >> outfile)
+	filenum = filenum + 1
+        delete (header, verify-)
+	if (filenum > efnum)
+	    bye
+    }
+}
diff --git a/noao/imred/vtel/mrotlogr.par b/noao/imred/vtel/mrotlogr.par
new file mode 100644
index 00000000..a18b0f4b
--- /dev/null
+++ b/noao/imred/vtel/mrotlogr.par
@@ -0,0 +1,5 @@
+gettape,s,a,,,,Tape to read fits headers from (i.e. "mta")
+getout,s,a,,,,File to put output information in
+getsfnum,i,a,,,,File number on tape from which to start logging 
+getefnum,i,a,,,,File number on tape at which logging is to end
+getapp,b,a,,,,Append to existing file?
diff --git a/noao/imred/vtel/mrqmin.x b/noao/imred/vtel/mrqmin.x
new file mode 100644
index 00000000..197e7931
--- /dev/null
+++ b/noao/imred/vtel/mrqmin.x
@@ -0,0 +1,348 @@
+# MRQMIN -- Levenberg-Marquard nonlinear chi square minimization.
+# From NUMERICAL RECIPES by Press, Flannery, Teukolsky, and Vetterling, p526.
+#
+# Levenberg-Marquardt method, attempting to reduce the value of chi
+# square of a fit between a set of NDATA points X,Y with individual
+# standard deviations SIG, and a nonlinear function dependent on MA
+# coefficients A.  The array LISTA numbers the parameters A such that the
+# first MFIT elements correspond to values actually being adjusted; the
+# remaining MA-MFIT parameters are held fixed at their input value.  The
+# program returns the current best-fit values for the MA fit parameters
+# A, and chi square, CHISQ.  The arrays COVAR and ALPHA with physical
+# dimension NCA (>= MFIT) are used as working space during most
+# iterations.  Supply a subroutine FUNCS(X,A,YFIT,DYDA,MA) that evaluates
+# the fitting function YFIT, and its derivatives DYDA with respect to the
+# fitting parameters A at X.  On the first call provide an initial guess
+# for the parameters A, and set ALAMDA<0 for initialization (which then
+# sets ALAMDA=0.001).  If a step succeeds  CHISQ becomes smaller and
+# ALAMDA decreases by a factor of 10.  If a step fails ALAMDA grows by a
+# factor of 10.  You must call this routine repeatedly until convergence
+# is achieved.  Then make one final call with ALAMDA = 0, so that COVAR
+# returns the covariance matrix, and ALPHA the curvature matrix.
+#
+# This routine is cast in the IRAF SPP language but the variable names have
+# been maintained for reference to the original source.  Also the working
+# arrays ATRY, BETA, and DA are allocated dynamically to eliminate
+# limitations on the number of parameters fit.
+
+procedure mrqmin (x, y, sig, ndata, a, ma, lista, mfit, covar, alpha, nca,
+	chisq, funcs, alamda)
+
+real	x[ndata]		# X data array
+real	y[ndata]		# Y data array
+real	sig[ndata]		# Sigma array
+int	ndata			# Number of data points
+real	a[ma]			# Parameter array
+int	ma			# Number of parameters
+int	lista[ma]		# List array indexing parameters to fit
+int	mfit			# Number of parameters to fit
+real	covar[nca,nca]		# Covariance matrix
+real	alpha[nca,nca]		# Curvature matrix
+int	nca			# Matrix dimension (>= mfit)
+real	chisq			# Chi square of fit
+extern	funcs			# Function to compute derivatives
+real	alamda			# Initialization and convergence parameter
+
+int	j, k, kk, ihit
+real	ochisq
+pointer	atry, beta, da
+
+errchk	gaussj
+
+begin
+	# Initialize and check that LISTA contains a proper permutation.
+	if (alamda < 0.) {
+	    call mfree (atry, TY_REAL)
+	    call mfree (beta, TY_REAL)
+	    call mfree (da, TY_REAL)
+	    call malloc (atry, ma, TY_REAL)
+	    call malloc (beta, mfit, TY_REAL)
+	    call malloc (da, mfit, TY_REAL)
+
+	    kk = mfit + 1
+	    do j = 1, ma {
+		ihit = 0
+		do k = 1, mfit
+		    if (lista(k) == j)
+			ihit = ihit + 1
+		if (ihit == 0) {
+		    lista (kk) = j
+		    kk = kk + 1
+		} else if (ihit > 1)
+		    call error (0, "Improper permutation in LISTA")
+	    }
+	    if (kk != (ma + 1))
+		call error (0, "Improper permutation in LISTA")
+	    alamda = 0.001
+	    call mrqcof (x, y, sig, ndata, a, ma, lista, mfit, alpha,
+		Memr[beta], nca, chisq, funcs)
+	    ochisq = chisq
+	    do j = 1, ma
+		Memr[atry+j-1] = a[j]
+	}
+
+	# Alter linearized fitting matrix by augmenting diagonal elements.
+	do j = 1, mfit {
+	    do k = 1, mfit
+		covar[j,k] = alpha[j,k]
+	    covar[j,j] = alpha[j,j] * (1. + alamda)
+	    Memr[da+j-1] = Memr[beta+j-1]
+	}
+
+	# Matrix solution.
+	call gaussj (covar, mfit, nca, Memr[da], 1, 1)
+
+	# Once converged evaluate covariance matrix with ALAMDA = 0.
+	if (alamda == 0.) {
+	    call covsrt (covar, nca, ma, lista, mfit)
+	    call mfree (atry, TY_REAL)
+	    call mfree (beta, TY_REAL)
+	    call mfree (da, TY_REAL)
+	    return
+	}
+
+	# Did the trial succeed?
+	do j = 1, mfit
+	    Memr[atry+lista[j]-1] = a[lista[j]] + Memr[da+j-1]
+	call mrqcof (x, y, sig, ndata, Memr[atry], ma, lista, mfit, covar,
+	    Memr[da], nca, chisq, funcs)
+
+	# Success - accept the new solution, Failure - increase ALAMDA
+	if (chisq < ochisq) {
+	    alamda = 0.1 * alamda
+	    ochisq = chisq
+	    do j = 1, mfit {
+		do k = 1, mfit
+		    alpha[j,k] = covar[j,k]
+		Memr[beta+j-1] = Memr[da+j-1]
+		a[lista[j]] = Memr[atry+lista[j]-1]
+	    }
+	} else {
+	    alamda = 10. * alamda
+	    chisq = ochisq
+	}
+end
+
+
+# MRQCOF -- Evaluate linearized matrix coefficients.
+# From NUMERICAL RECIPES by Press, Flannery, Teukolsky, and Vetterling, p527.
+#
+# Used by MRQMIN to evaluate the linearized fitting matrix ALPHA and vector
+# BETA.
+#
+# This procedure has been recast in the IRAF/SPP language but the variable
+# names have been maintained.  Dynamic memory is used.
+
+procedure mrqcof (x, y, sig, ndata, a, ma, lista, mfit, alpha, beta, nalp,
+    chisq, funcs)
+
+real	x[ndata]		# X data array
+real	y[ndata]		# Y data array
+real	sig[ndata]		# Sigma array
+int	ndata			# Number of data points
+real	a[ma]			# Parameter array
+int	ma			# Number of parameters
+int	lista[ma]		# List array indexing parameters to fit
+int	mfit			# Number of parameters to fit
+real	alpha[nalp,nalp]	# Work matrix
+real	beta[ma]		# Work array
+int	nalp			# Matrix dimension (>= mfit)
+real	chisq			# Chi square of fit
+extern	funcs			# Function to compute derivatives
+
+int	i, j, k
+real	sig2i, ymod, dy, wt
+pointer	sp, dyda
+
+begin
+	call smark (sp)
+	call salloc (dyda, ma, TY_REAL)
+
+	do j = 1, mfit {
+	   do k = 1, j
+	       alpha[j,k] = 0.
+	    beta[j] = 0.
+	}
+
+	chisq = 0.
+	do i = 1, ndata {
+	    call funcs (x[i], a, ymod, Memr[dyda], ma)
+	    sig2i = 1. / (sig[i] * sig[i])
+	    dy = y[i] - ymod
+	    do j = 1, mfit {
+		wt = Memr[dyda+lista[j]-1] * sig2i
+		do k = 1, j
+		    alpha[j,k] = alpha[j,k] + wt * Memr[dyda+lista[k]-1]
+		beta[j] = beta[j] + dy * wt
+	    }
+	    chisq = chisq + dy * dy * sig2i
+	}
+
+	do j = 2, mfit
+	    do k = 1, j-1
+		alpha[k,j] = alpha[j,k]
+
+	call sfree (sp)
+end
+	    
+
+# GAUSSJ -- Linear equation solution by Gauss-Jordan elimination.
+# From NUMERICAL RECIPES by Press, Flannery, Teukolsky, and Vetterling, p28.
+#
+# Linear equation solution by Gauss-Jordan elimination.  A is an input matrix
+# of N by N elements, stored in an array of physical dimensions NP by
+# NP.  B is an input matrix of N by M containing the M right-hand side
+# vectors, stored in an array of physical dimensions NP by MP.  On
+# output, A is replaced by its matrix inverse, and B is replaced by the
+# corresponding set of solutionn vectors.
+#
+# This procedure has been recast in the IRAF/SPP language using dynamic
+# memory allocation and error return.  The variable names have been maintained.
+
+procedure gaussj (a, n, np, b, m, mp)
+
+real	a[np,np]		# Input matrix and returned inverse
+int	n			# Dimension of input matrix
+int	np			# Storage dimension of input matrix
+real	b[np,mp]		# Input RHS matrix and returned solution
+int	m			# Dimension of input matrix
+int	mp			# Storage dimension of input matrix
+
+int	i, j, k, l, ll, irow, icol, indxrl, indxcl
+real	big, pivinv, dum
+pointer	sp, ipiv, indxr, indxc
+
+begin
+	call smark (sp)
+	call salloc (ipiv,  n, TY_INT)
+	call salloc (indxr, n, TY_INT)
+	call salloc (indxc, n, TY_INT)
+
+	do j = 1, n
+	    Memi[ipiv+j-1] = 0
+
+	do i = 1, n {
+	    big = 0.
+	    do j = 1, n {
+		if (Memi[ipiv+j-1] != 1) {
+		    do k = 1, n {
+			if (Memi[ipiv+k-1] == 0) {
+			    if (abs (a[j,k]) >= big) {
+				big = abs (a[j,k])
+				irow = j
+				icol = k
+			    }
+			} else if (Memi[ipiv+k-1] > 1) {
+			    call sfree (sp)
+			    call error (0, "Singular matrix")
+			}
+		    }
+		}
+	    }
+
+	    Memi[ipiv+icol-1] = Memi[ipiv+icol-1] + 1
+
+	    if (irow != icol) {
+		do l = 1, n {
+		    dum = a[irow,l]
+		    a[irow,l] = a[icol,l]
+		    a[icol,l] = dum
+		}
+		do l = 1, m {
+		    dum = b[irow,l]
+		    b[irow,l] = b[icol,l]
+		    b[icol,l] = dum
+		}
+	    }
+	    Memi[indxr+i-1] = irow
+	    Memi[indxc+i-1] = icol
+	    if (a[icol,icol] == 0.) {
+		call sfree (sp)
+		call error (0, "Singular matrix")
+	    }
+	    pivinv = 1. / a[icol,icol]
+	    a[icol,icol] = 1
+	    do l = 1, n
+		a[icol,l] = a[icol,l] * pivinv
+	    do l = 1, m
+		b[icol,l] = b[icol,l] * pivinv
+	    do ll = 1, n {
+		if (ll != icol) {
+		    dum = a[ll,icol]
+		    do l = 1, n
+			a[ll,l] = a[ll,l] - a[icol,l] * dum
+		    do l = 1, m
+			b[ll,l] = b[ll,l] - b[icol,l] * dum
+		}
+	    }
+	}
+
+	do l = n, 1, -1 {
+	    indxrl = Memi[indxr+l-1]
+	    indxcl = Memi[indxr+l-1]
+	    if (indxrl != indxcl) {
+		do k = 1, n {
+		    dum = a[k,indxrl]
+		    a[k,indxrl] = a[k,indxcl]
+		    a[k,indxcl] = dum
+		}
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# COVSRT -- Sort covariance matrix.
+# From NUMERICAL RECIPES by Press, Flannery, Teukolsky, and Vetterling, p515.
+#
+# Given the covariance matrix COVAR of a fit for MFIT of MA total parameters,
+# and their ordering LISTA, repack the covariance matrix to the true order of
+# the parameters.  Elements associated with fixed parameters will be zero.
+# NCVM is the physical dimension of COVAR.
+#
+# This procedure has been recast into the IRAF/SPP language but the
+# original variable names are used.
+
+procedure covsrt (covar, ncvm, ma, lista, mfit)
+
+real	covar[ncvm,ncvm]	# Input and output array
+int	ncvm			# Physical dimension of array
+int	ma			# Number of parameters
+int	lista[mfit]		# Index of fitted parameters
+int	mfit			# Number of fitted parameters
+
+int	i, j
+real	swap
+
+begin
+	# Zero all elements below diagonal.
+	do j = 1, ma-1
+	    do i = j+1, ma
+		covar[i,j] = 0.
+
+	# Repack off-diag elements of fit into correct locations below diag.
+	do i = 1, mfit-1
+	    do j = i+1, mfit
+		if (lista[j] > lista[i])
+		    covar [lista[j],lista[i]] = covar[i,j]
+		else
+		    covar [lista[i],lista[j]] = covar[i,j]
+
+	# Temporarily store original diag elements in top row and zero diag.
+	swap = covar[1,1]
+	do j = 1, ma {
+	    covar[1,j] = covar[j,j]
+	    covar[j,j] = 0.
+	}
+	covar[lista[1],lista[1]] = swap
+
+	# Now sort elements into proper order on diagonal.
+	do j = 2, mfit
+	    covar[lista[j],lista[j]] = covar[1,j]
+
+	# Finally, fill in above diagonal by symmetry.
+	do j = 2, ma
+	    do i = 1, j-1
+		covar[i,j] = covar[j,i]
+end
diff --git a/noao/imred/vtel/mscan.par b/noao/imred/vtel/mscan.par
new file mode 100644
index 00000000..8c903220
--- /dev/null
+++ b/noao/imred/vtel/mscan.par
@@ -0,0 +1,8 @@
+input,s,a,,,,Input file descriptor
+verbose,b,h,yes,,,Print out header data 
+files,s,a,,,,List of files to be examined
+makeimage,b,h,yes,,,Make images?
+brief,b,h,y,,,short output image names
+select,b,h,y,,,make select image
+bright,b,h,y,,,make brightness image
+velocity,b,h,y,,,make velocity image
diff --git a/noao/imred/vtel/mscan.x b/noao/imred/vtel/mscan.x
new file mode 100644
index 00000000..9044b943
--- /dev/null
+++ b/noao/imred/vtel/mscan.x
@@ -0,0 +1,188 @@
+include <error.h>
+include <mach.h>
+include "vt.h"
+
+define	MAX_RANGES	100
+
+# MSCAN -- Read vacuum telescope area scans.
+
+procedure t_mscan()
+
+char	input[SZ_FNAME]		# input file template
+char	files[SZ_LINE]		# file list to process
+bool	verbose			# verbose flag
+bool	makeimage		# flag to make an image
+bool	bright			# flag to make a brightness image
+bool	velocity		# flag to make a velocity image
+bool	select			# flag to make a select image
+bool	brief			# flag to make brief file names
+
+char	tapename[SZ_FNAME]
+char	diskfile[SZ_LINE]
+int	filerange[2 * MAX_RANGES + 1]
+int	nfiles, filenumber, recsize, listin
+
+bool	clgetb()
+int	decode_ranges(), get_next_number(), mscan()
+int	fntopnb(), clgfil(), mtneedfileno()
+int	mtfile()
+errchk	mscan
+
+begin
+	# CLIO for parameters.
+	verbose = clgetb ("verbose")
+	makeimage = clgetb ("makeimage")
+	bright = clgetb ("bright")
+	velocity = clgetb ("velocity")
+	select = clgetb ("select")
+	brief = clgetb ("brief")
+
+	# If the user hasn't asked for ANY of the images, just return.
+	if (!bright && !velocity && !select)
+	    return
+
+        # Get input file(s).
+        call clgstr ("input", input, SZ_FNAME)
+        if (mtfile (input) == NO) {
+
+	    # This is not a tape file, expand as a list template.
+	    listin = fntopnb (input, 0)
+	    filenumber = 1
+
+	    while (clgfil (listin, diskfile, SZ_FNAME) != EOF) {
+		iferr (recsize =  mscan (diskfile, filenumber, brief,
+		    verbose, makeimage, select, bright, velocity)) {
+		    call eprintf ("Error reading file %s\n")
+		    	call pargstr (diskfile)
+	    	}
+	        if (recsize == EOF) {
+		    call printf ("Tape at EOT\n")
+		    break
+	        }
+		filenumber = filenumber + 1
+	    }
+	    call clpcls (listin)
+
+	} else if (mtneedfileno(input) == NO) {
+	    
+	    # This is a tape file and the user specified which file.
+	    iferr (recsize = mscan (input, 0, brief, verbose,
+	    	    makeimage, select, bright, velocity)) {
+		call eprintf ("Error reading file %s\n")
+		    call pargstr (input)
+	    }
+        } else {
+
+	    # This is a tape file or files and the user did not specify
+	    # which file.
+	    call clgstr ("files", files, SZ_LINE)
+
+            if (decode_ranges (files, filerange, MAX_RANGES, nfiles) == ERR)
+	        call error (0, "Illegal file number list.")
+
+	    if (verbose)
+	        call printf ("\n")
+
+            # Loop over files.
+	    filenumber = 0
+            while (get_next_number (filerange, filenumber) != EOF) {
+
+	        # Assemble the appropriate tape file name.
+		call mtfname (input, filenumber, tapename, SZ_FNAME)
+
+	        # Read this file.
+	        iferr {
+	            recsize = mscan (tapename, filenumber, brief,
+			verbose, makeimage, select, bright, velocity)
+	        } then {
+		    call eprintf ("Error reading file: %s\n")
+		        call pargstr (tapename)
+		    call erract (EA_WARN)
+		    next
+	        }
+	        if (recsize == EOF) {
+		    call printf ("Tape at EOT\n")
+		    break
+	        }
+
+            }  # End while.
+	}
+end
+
+
+# MSCAN -- Read in the next sector scan file from tape.  First read the file
+# header to determine what type scan it is and then call the appropriate
+# subroutime for that type of scan.
+
+int procedure mscan (input, filenumber, brief, verbose, makeimage, select, 
+		    bright, velocity)
+
+char	input[SZ_FNAME]		# input file name
+int	filenumber		# file number
+bool	brief			# brief disk file names?
+bool	verbose			# print header info?
+bool	makeimage		# make images?
+bool	select			# make select image?
+bool	bright			# make bright image?
+bool	velocity		# make velocity image?
+
+int	in
+int	lastrecsize
+int	recsize
+bool	selfbuf
+pointer	sp, hbuf, hs
+
+int	mtopen()
+int	readheader()
+define	nexit_ 10
+errchk	mtopen, close, readheader
+
+begin
+	call smark (sp)
+	call salloc (hbuf, SZ_VTHDR, TY_SHORT)
+	call salloc (hs, VT_LENHSTRUCT, TY_STRUCT)
+
+	in = mtopen (input, READ_ONLY, 0)
+
+	call printf ("File %s:  ")
+	    call pargstr (input)
+
+	lastrecsize = 0
+
+	# First, read the header file
+	selfbuf = FALSE
+	recsize = readheader (in, hbuf, selfbuf)
+	if (recsize == EOF)
+	    return (recsize)
+
+	# Decode the header and jump if '!makeimage'.
+	lastrecsize = recsize
+	call decodeheader (hbuf, hs, verbose)
+	if (verbose) {
+	    call printf ("\n")
+	    call flush (STDOUT)
+	}
+	if (!makeimage)
+	    goto nexit_
+
+	# Call the appropriate area scan reader.
+	switch (VT_HOBSTYPE(hs)) {
+	case 1:
+	    call readss1 (in, filenumber, brief, select, bright, velocity, hs)
+	case 2:
+	    call readss2 (in, filenumber, brief, select, bright, velocity, hs)
+	case 3:
+	    call readss3 (in, filenumber, brief, select, bright, velocity, hs)
+	case 4:
+	    call readss4 (in, filenumber, brief, select, bright, velocity, hs)
+	case 0:
+	    call printf ("Observation type zero encountered, image skipped.\n")
+	default:
+	    call error (0, "unknown observation type, image skipped")
+	} # End of switch case.
+
+nexit_
+	call sfree (sp)
+	call close (in)
+	return (recsize)
+end
diff --git a/noao/imred/vtel/nsolcrypt.dat b/noao/imred/vtel/nsolcrypt.dat
new file mode 100644
index 00000000..65c3b067
--- /dev/null
+++ b/noao/imred/vtel/nsolcrypt.dat
@@ -0,0 +1,555 @@
+                                                                               
+                                                                               
+    '                      
+                                                                               
+                #                                                              
+                     #     
+'                                                                              
+                                                           #                   
+                           
+                                                                               
+                                                                               
+                           
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+                                                                               
+                           
+                                                                               
+                                                                               
+                           
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+                                                                               
+                           
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+                                                                               
+                           
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+   6L      X}r   '[T     E_:                                                   
+                           
+                                                                             ' 
+  +}}#     y}}A  #v}:    v}2   TA                                              
+                           
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+   y}=    :}}}k   T}kEEEX}r   +}y                                              
+                           
+                                                                      +EXv+ I}_
+   _}T    [}[y}6  .}}}}}}}P   6}k                                              
+                           
+                                                                   #Lr}}}k. .}v
+   T}T    y}2T}g   g}_2I}}'   E}[     #EckcI#                                  
+                           
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+                           
+                                                             #2.   '}}#      _}
+}}}}}v6  _}P  [}[  #y}2r}A    g}E#  #n}r= '[}v'                                
+                           
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+yL.#[}c #y}.  2}y'  T}n}v     v}2   A}y.    _}P                                
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+                                +:# .y}E   X}}6 E}}#  :}}.                     
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+                                               =v}y[2.v}E  2y}vA T}T #y}}nL2   
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+                                        '      A}}2   [}A  L}v+  [}P  =I2      
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+                                                       .c}}n6}v                
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+                                                      'y}yL  }}                
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+                                     E}n      c}P  [g6                         
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+                                      g}g#   I}v#                              
+                                                             }}                
+                           
+        #                             2y}k=6X}}A                               
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+                                       6n}}}}r:                                
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+                                         :II6                              #   
+            :2 ''                                                              
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+                                                                               
+            }k kc                                                              
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+            }k rk                                                              
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+            }n nk                                                              
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+#          =EA.         =cXXXXXLXT+=}g                                         
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+                                        2A6'   6}y'                            
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+                                        Ay}_#    P}y'   Ig}}gI                 
+                                      =r}}}yP#  k}T                            
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+                                        #6y}c#  #y}T   _}}}}}}c                
+                                     A}}kEk}}_  :}}+                           
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+                                          #_y+  T}n#  P}yE  .k}T   +.          
+                                    .}}6   =}}E  g}[                           
+    #                      
+                                           +2# .v}E  'v}L#   6}v#  [k.         
+                            :PXT6   L}c     X}n  2}y.                          
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+                                               [}_   =}y#     k}: #}}'   6vk+  
+                          6n}}}}}I  k}E     2}}'  [}_                          
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+                                               =X'   E}k      k}E 6}n   6y}}26X
+A     .2  =PXPEPP        #v}k=2L}y' k}L      }}2  'yy#                         
+                           
+                                                     E}k     #v}= I}[  :}}}y A}
+r    #y}. }}}}}}}        :}y#   y}6 T}k     2}y#   :'                          
+                           
+                                                     +}}.    L}y# X}L E}}g}k  v
+}A2' T}g  }}A222.        A}X  '[}}2 6}}I    _}c                                
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+}}}}}}}6  }}+               .[}}}T   _}}T26_}y.                                
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+                                                      #g}}nv}}c#  }}g}}E X}=  :
+}}TXr}n   }}.              E}}}n= '  #_}}}}}r6                                 
+                           
+                                                        Agy}kI   2}}}y=  n}.   
+v}2 n}A   }}'             'y}c2 .yy    6TXX=                                   
+                           
+                                                                 A}}y6   }}    
+X}P6}v    k}'             2}}#  A}n                                            
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+                                  #                              E}y6   2}g    
+:}rg}I    r}2             'y}TAPy}I                                            
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+ v}}y'    n}.              A}}}}}P                                             
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+                        '                                               'A.  # 
+ P}}T     k}.               .LTE+                                              
+                           
+                        '                                                      
+ .kr'     [k#                                                                  
+                           
+                                                                               
+                #                                                              
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+                                                                               
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+                                                                              #
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+                                                                               
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+                    #      
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+                                                                               
+                                           $                                   
+                           
diff --git a/noao/imred/vtel/numeric.h b/noao/imred/vtel/numeric.h
new file mode 100644
index 00000000..765fac03
--- /dev/null
+++ b/noao/imred/vtel/numeric.h
@@ -0,0 +1,12 @@
+# Structure for argument list to subroutine 'numeric'.
+
+define	VT_LENNUMSTRUCT	8		# Length of VT num structure
+
+define	VT_DLODX	Memr[P2R($1)]	# deriv longitude wrt x
+define	VT_DLATDY	Memr[P2R($1+1)]	# deriv latitude wrt y
+define	VT_LATTOP	Memr[P2R($1+2)]	# latitude of top of output pixel
+define	VT_LATBOT	Memr[P2R($1+3)]	# latitude of bottom of output pixel
+define	VT_LOLEFT	Memr[P2R($1+4)]	# longitude of left side of out pixel
+define	VT_LORITE	Memr[P2R($1+5)]	# longitude of right side of out pixel
+define	VT_LATMID	Memr[P2R($1+6)]	# latitude of middle of output pixel
+define	VT_LOMID	Memr[P2R($1+7)]	# longitude of middle of output pixel
diff --git a/noao/imred/vtel/numeric.x b/noao/imred/vtel/numeric.x
new file mode 100644
index 00000000..640778c8
--- /dev/null
+++ b/noao/imred/vtel/numeric.x
@@ -0,0 +1,177 @@
+include <mach.h>
+include "vt.h"
+include "numeric.h"
+
+# NUMERIC -- calculate some of the necessary information, including
+# the partial derivitives of latitude and longitude with respect
+# to x and y, that we need to do the projection.
+
+procedure numeric (bzero, el, outputrow, pixel, xpixcenter, ypixcenter, num)
+
+real	bzero				# latitude of subearth point
+real	el[LEN_ELSTRUCT]		# ellipse parameters data structure
+int	outputrow			# which output row are we working on
+int	pixel				# which pixel in that output row
+real	xpixcenter, ypixcenter		# coordinates of center of pixel
+pointer	num				# numeric structure pointer
+
+real	dlatdy, dlongdx			# partial derivitives
+real	lat_top, lat_bot		# latitude of top and bottom of pix
+real	long_left, long_rite		# longitude of left and right of pix
+real	lat_mid, long_mid		# latitude and longitude of middle
+real	lat1, long1, lat3, long3, lat4, long4, lat5, long5
+real	x1, y1, x3, y3, x4, y4, x5, y5
+bool	skip
+
+begin
+	skip = false
+
+	# First calculate lats, longs for this pixel.
+	lat_top   = 180./3.1415926*asin(real(outputrow - 90)/90.)
+	lat_bot   = 180./3.1415926*asin(real(outputrow - 91)/90.)
+	long_left = real(pixel - 1) - 90.
+	long_rite = real(pixel) - 90.
+	lat_mid   = .5 * (lat_top + lat_bot)
+	long_mid  = .5 * (long_left + long_rite)
+
+	# Check the proximity of this pixel to the image boundary, if its
+	# too close, set that output pixel to zero.
+
+	if (abs(abs(lat_mid) - 90.0) < abs(bzero)) {
+	    if (abs(abs(lat_top) - 90.0) >= abs(bzero)) {
+		lat_bot = -90.0 + bzero
+		lat_mid = .5 * (lat_top + lat_bot)
+	    } else {
+		if (abs(abs(lat_bot) - 90.0) >= abs(bzero)) {
+		    lat_top = 90.0 + bzero
+		    lat_mid = .5 * (lat_top + lat_bot)
+		} else {
+	    	    # Nothing to map!
+		    # Flag to pixelmap marking zero pixel.
+		    VT_LATTOP(num) = 10000.
+	    	    return
+		}
+	    }
+	} else {
+	    if (abs(abs(lat_top) - 90.0) < abs(bzero))
+		lat_top = 90.0 + bzero
+	    else
+		if (abs(abs(lat_bot) - 90.0) < abs(bzero))
+		    lat_bot = -90.0 + bzero
+	}
+
+	# Now that we have the pixel we want defined, calculate the partial
+	# derivitives we need numerically.  First calculate the latitude and
+	# longitude of the centers of the 4 adjacent pixels.
+
+	lat1 = lat_mid
+	if (pixel == 1)
+	    long1 = long_mid
+	else
+	    long1 = long_mid - 1.0
+
+	lat3 = lat_mid
+	if (pixel == 180)
+	    long3 = long_mid
+	else
+	    long3 = long_mid + 1.0
+
+	long5 = long_mid
+	if (outputrow == 1)
+	    lat5 = lat_mid
+	else
+	    lat5 = 180./3.1415926*((asin(real(outputrow - 92)/90.) +
+		    asin(real(outputrow - 91)/90.))/2.)
+
+	long4 = long_mid
+	if (outputrow == 180)
+	    lat4 = lat_mid
+	else
+	    lat4 = 180./3.1415926*((asin(real(outputrow - 89)/90.) +
+	            asin(real(outputrow - 90)/90.))/2.)
+
+	# Given these latitudes and longitudes, find out where in xy coords
+	# they are. Get xpixcenter and ypixcenter then the x#s and y#s.
+
+	call getxy (lat_mid, long_mid, bzero, el, xpixcenter, ypixcenter, skip)
+	if (skip) {
+
+	    # Off the limb or behind the sun.
+	    # Flag to pixelmap marking zero pixel.
+	    VT_LATTOP(num) = 10000.
+	    return
+	}
+
+	call getxy (lat1, long1, bzero, el, x1, y1, skip)
+	call getxy (lat3, long3, bzero, el, x3, y3, skip)
+	call getxy (lat4, long4, bzero, el, x4, y4, skip)
+	call getxy (lat5, long5, bzero, el, x5, y5, skip)
+
+	# Calculate the partials.
+	if (x3 == x1)
+	    dlongdx = 9999.
+	else
+	    dlongdx = (long3 - long1) / (x3 - x1)
+
+	if (y4 == y5)
+	    dlatdy = 9999.
+	else
+	    dlatdy = (lat4 - lat5) / (y4 - y5)
+
+	VT_DLODX(num) = dlongdx 
+	VT_DLATDY(num) = dlatdy 
+	VT_LATTOP(num) = lat_top 
+	VT_LATBOT(num) = lat_bot 
+	VT_LOLEFT(num) = long_left 
+	VT_LORITE(num) = long_rite 
+	VT_LATMID(num) = lat_mid 
+	VT_LOMID(num) = long_mid 
+end
+
+
+# GETXY -- Given the latitude and longitude of a point and the image
+# parameters, return the x and y position of that point.
+
+procedure getxy (lat, lml0, b0, el, x, y, skip)
+
+real	lat			# latitude of point on image
+real	lml0			# distance in longitude from disk center
+real	b0			# latitude of sub earth point
+real	el[LEN_ELSTRUCT]	# ellipse parameters data structure
+real	x, y			# returned position
+bool	skip			# skip flag
+
+real	sinlat, coslat, sinbzero, cosbzero, sinlminusl0, coslminusl0
+real	cosrho, sinrho, sinpminustheta, cospminustheta 
+real	latitude, lminusl0, bzero
+
+begin
+	skip = false
+	lminusl0 = lml0*3.1415926/180.
+	bzero = b0*3.1415926/180.
+	latitude = lat*3.1415926/180.
+	sinlat = sin(latitude)
+	coslat = cos(latitude)
+	sinbzero = sin(bzero)
+	cosbzero = cos(bzero)
+	sinlminusl0 = sin(lminusl0)
+	coslminusl0 = cos(lminusl0)
+	cosrho = sinbzero * sinlat + cosbzero * coslat * coslminusl0
+
+	# If we are behind limb return skip = true.
+	if (cosrho <= 0.00) skip = true
+	sinrho = (1. - cosrho**2)**.5
+	if (sinrho >= EPSILONR) {
+	    sinpminustheta = (coslat/sinrho) * sinlminusl0
+	    cospminustheta = (coslat/sinrho) * (cosbzero * tan(latitude) -
+	        sinbzero * coslminusl0)
+	} else {
+	    sinpminustheta = 0.000001
+	    cospminustheta = 0.000001
+	}
+
+	x = E_XSEMIDIAMETER(el) * sinrho * sinpminustheta
+	y = E_YSEMIDIAMETER(el) * sinrho * cospminustheta
+	x = x + real(E_XCENTER(el))
+	y = y + real(E_YCENTER(el))
+end
diff --git a/noao/imred/vtel/pimtext.par b/noao/imred/vtel/pimtext.par
new file mode 100644
index 00000000..fa0494d9
--- /dev/null
+++ b/noao/imred/vtel/pimtext.par
@@ -0,0 +1,13 @@
+iraf_files,s,q,,,,Images to be written
+refim,s,q,,,,Reference image to get date and time from
+ref,b,h,no,,,Find the date and time in a reference image
+x,i,h,10,,,X position of text in image
+y,i,h,10,,,Y position of text in image
+xmag,i,h,2,,,Text magnification factor in x direction
+ymag,i,h,2,,,Text magnification factor in y direction
+val,i,h,-10000,,,Value to use to write text in images
+setbgnd,b,h,yes,,,Set the pixels in the image behind the text
+bgndval,i,h,10000,,,Value to use in background of text
+date,b,h,yes,,,Write the date into the images
+time,b,h,yes,,,Write the time into the images
+text,s,q,,,,Text string to write into image
diff --git a/noao/imred/vtel/pimtext.x b/noao/imred/vtel/pimtext.x
new file mode 100644
index 00000000..b39c12be
--- /dev/null
+++ b/noao/imred/vtel/pimtext.x
@@ -0,0 +1,131 @@
+include "vt.h"
+
+# PIMTEXT -- Put a text string directly into an image using a pixel font
+# and writing over the image pixels.
+
+procedure t_pimtext()
+
+char	im[SZ_FNAME]			# image to put text in
+char	refim[SZ_FNAME]			# reference image (get date/time)
+int	x, y				# position to put text
+int	xmag, ymag			# text magnification parameters
+int	val				# value to use for text pixels
+int	bgndval				# value to use for background pixels
+bool	setbgnd				# flag, should we set the background?
+bool	ref				# flag, are we using a ref image
+
+int	obstime, obsdate, hour, minute, second
+int	list, nfiles
+int	month, day, year
+char	dt[DTSTRING]
+bool	istime, isdate, date, time
+pointer	imp, rimp
+
+bool	clgetb(), imaccf()
+int	clgeti(), imgeti()
+int	clpopni(), clplen(), clgfil()
+pointer	immap()
+errchk	immap
+
+begin
+	# Get file name template from the CL.
+	list = clpopni ("iraf_files")
+	nfiles = clplen (list)
+
+	# Get some other parameters.
+	ref = clgetb ("ref")
+	if (ref)
+	    call clgstr ("refim", refim, SZ_FNAME)
+	x = clgeti ("x")
+	y = clgeti ("y")
+	xmag = clgeti ("xmag")
+	ymag = clgeti ("ymag")
+	val = clgeti ("val")
+	setbgnd = clgetb ("setbgnd")
+	bgndval = clgeti ("bgndval")
+	date = clgetb ("date")
+	time = clgetb ("time")
+
+	while (clgfil (list, im, SZ_FNAME) != EOF) {
+	    # Open the image(s).
+	    imp = immap (im, READ_WRITE, 0)
+	    if (ref)
+	        rimp = immap (refim, READ_ONLY, 0)
+
+	    if (date || time) {
+	        # Find out if the date and time exist in the image header.
+		if (ref) {
+	            istime = imaccf (rimp, "obs_time")
+	            isdate = imaccf (rimp, "obs_date")
+		} else {
+	            istime = imaccf (imp, "obs_time")
+	            isdate = imaccf (imp, "obs_date")
+		}
+
+		# Get the date and/or time.
+		if (date && isdate && !time) {
+		    if (ref)
+			obsdate = imgeti (rimp, "obs_date")
+		    else
+	                obsdate = imgeti (imp, "obs_date")
+
+	            month = obsdate / 10000
+	            day = obsdate/100 - 100 * (obsdate/10000)
+	            year = obsdate - 100 * (obsdate/100)
+	            call sprintf (dt, DTSTRING, "%02d/%02d/%02d")
+	                call pargi (month)
+	                call pargi (day)
+	                call pargi (year)
+
+		} else if (time && istime && !date) {
+		    if (ref)
+			obstime = imgeti (rimp, "obs_time")
+		    else
+	                obstime = imgeti (imp, "obs_time")
+
+	            hour = int(obstime/3600)
+	            minute = int((obstime - hour * 3600)/60)
+	            second = obstime - hour * 3600 - minute * 60
+	            call sprintf (dt, DTSTRING, "%02d:%02d:%02d")
+	                call pargi (hour)
+	                call pargi (minute)
+	                call pargi (second)
+
+		} else if (istime && isdate && time && date) {
+		    if (ref) {
+	                obstime = imgeti (rimp, "obs_time")
+	                obsdate = imgeti (rimp, "obs_date")
+		    } else {
+	                obstime = imgeti (imp, "obs_time")
+	                obsdate = imgeti (imp, "obs_date")
+		    }
+
+	            month = obsdate/10000
+	            day = obsdate/100 - 100 * (obsdate/10000)
+	            year = obsdate - 100 * (obsdate/100)
+	            hour = int(obstime/3600)
+	            minute = int((obstime - hour * 3600)/60)
+	            second = obstime - hour * 3600 - minute * 60
+	            call sprintf (dt, DTSTRING, "%02d:%02d:%02d %02d/%02d/%02d")
+	                call pargi (hour)
+	                call pargi (minute)
+	                call pargi (second)
+	                call pargi (month)
+	                call pargi (day)
+	                call pargi (year)
+	        } else {
+	            call printf ("Warning: cannot get date and/or time.\n")
+	            call printf ("Getting text string fron the CL.\n")
+	            call clgstr ("text", dt, DTSTRING)
+	        }
+	    } else
+	        call clgstr ("text", dt, DTSTRING)
+
+	    call textim (imp, dt, x, y, xmag, ymag, val, setbgnd, bgndval)
+	    call imunmap (imp)
+	    if (ref)
+		call imunmap (rimp)
+	} # end while
+
+	call clpcls (list)
+end
diff --git a/noao/imred/vtel/pixbit.x b/noao/imred/vtel/pixbit.x
new file mode 100644
index 00000000..a6db321a
--- /dev/null
+++ b/noao/imred/vtel/pixbit.x
@@ -0,0 +1,23 @@
+# PIXBIT -- Look up which bits should be set for this character on this line.
+
+procedure pixbit (code, line, bitarray)
+
+int	code		# character we are writing
+int	line		# line of the character we are writing
+int	bitarray[5]	# bit-array to receive data
+
+int	pix, i
+short	asciilook[128]
+short	font[455]
+int	bitupk()
+include	"pixelfont.inc"
+include	"asciilook.inc"
+
+begin
+	pix = font[asciilook[code+1]+line-1]
+	bitarray[5] = bitupk (pix, 1, 1)
+	bitarray[4] = bitupk (pix, 4, 1)
+	bitarray[3] = bitupk (pix, 7, 1)
+	bitarray[2] = bitupk (pix, 10, 1)
+	bitarray[1] = bitupk (pix, 13, 1)
+end
diff --git a/noao/imred/vtel/pixelfont.inc b/noao/imred/vtel/pixelfont.inc
new file mode 100644
index 00000000..92216e6d
--- /dev/null
+++ b/noao/imred/vtel/pixelfont.inc
@@ -0,0 +1,519 @@
+data	(font[i], i=1,7)      / 00000B,
+				00000B,
+				00000B,
+				00000B,
+				00000B,
+				00000B,
+				00000B /    # (space)
+
+data	(font[i], i=8,14)     / 00100B,
+				00100B,
+				00100B,
+				00100B,
+				00100B,
+				00000B,
+				00100B /    # !
+
+data	(font[i], i=15,21)    / 01010B,
+				01010B,
+				01010B,
+				00000B,
+				00000B,
+				00000B,
+				00000B /    # "
+
+data	(font[i], i=22,28)    / 01010B,
+				01010B,
+				11111B,
+				01010B,
+				11111B,
+				01010B,
+				01010B /    # #
+
+data	(font[i], i=29,35)    / 00100B,
+				01111B,
+				10100B,
+				01110B,
+				00101B,
+				11110B,
+				00100B /    # $
+
+data	(font[i], i=36,42)    / 11000B,
+				11001B,
+				00010B,
+				00100B,
+				01000B,
+				10011B,
+				00011B /    # %
+
+data	(font[i], i=43,49)    / 01000B,
+				10100B,
+				10100B,
+				01000B,
+				10101B,
+				10010B,
+				01101B /    # &
+
+data	(font[i], i=50,56)    / 00100B,
+				00100B,
+				00100B,
+				00000B,
+				00000B,
+				00000B,
+				00000B /    # '
+
+data	(font[i], i=57,63)    / 00100B,
+				01000B,
+				10000B,
+				10000B,
+				10000B,
+				01000B,
+				00100B /    # (
+
+data	(font[i], i=64,70)    / 00100B,
+				00010B,
+				00001B,
+				00001B,
+				00001B,
+				00010B,
+				00100B /    # )
+
+data	(font[i], i=71,77)    / 00100B,
+				10101B,
+				01110B,
+				00100B,
+				01110B,
+				10101B,
+				00100B /    # *
+
+data	(font[i], i=78,84)    / 00000B,
+				00100B,
+				00100B,
+				11111B,
+				00100B,
+				00100B,
+				00000B /    # +
+
+data	(font[i], i=85,91)    / 00000B,
+				00000B,
+				00000B,
+				00000B,
+				00100B,
+				00100B,
+				01000B /    # ,
+
+data	(font[i], i=92,98)    / 00000B,
+				00000B,
+				00000B,
+				11111B,
+				00000B,
+				00000B,
+				00000B /    # -
+
+data	(font[i], i=99,105)   / 00000B,
+				00000B,
+				00000B,
+				00000B,
+				00000B,
+				00000B,
+				00100B /    # .
+
+data	(font[i], i=106,112)  / 00000B,
+				00001B,
+				00010B,
+				00100B,
+				01000B,
+				10000B,
+				00000B /    # /
+
+data	(font[i], i=113,119)  / 01110B,
+				10001B,
+				10011B,
+				10101B,
+				11001B,
+				10001B,
+				01110B /    # 0
+
+data	(font[i], i=120,126)  / 00100B,
+				01100B,
+				00100B,
+				00100B,
+				00100B,
+				00100B,
+				01110B /    # 1
+
+data	(font[i], i=127,133)  / 01110B,
+				10001B,
+				00001B,
+				00110B,
+				01000B,
+				10000B,
+				11111B /    # 2
+
+data	(font[i], i=134,140)  / 11111B,
+				00001B,
+				00010B,
+				00110B,
+				00001B,
+				10001B,
+				11111B /    # 3
+
+data	(font[i], i=141,147)  / 00010B,
+				00110B,
+				01010B,
+				11111B,
+				00010B,
+				00010B,
+				00010B /    # 4
+
+data	(font[i], i=148,154)  / 11111B,
+				10000B,
+				11110B,
+				00001B,
+				00001B,
+				10001B,
+				01110B /    # 5
+
+data	(font[i], i=155,161)  / 00111B,
+				01000B,
+				10000B,
+				11110B,
+				10001B,
+				10001B,
+				01110B /    # 6
+
+data	(font[i], i=162,168)  / 11111B,
+				00001B,
+				00010B,
+				00100B,
+				01000B,
+				01000B,
+				01000B /    # 7
+
+data	(font[i], i=169,175)  / 01110B,
+				10001B,
+				10001B,
+				01110B,
+				10001B,
+				10001B,
+				01110B /    # 8
+
+data	(font[i], i=176,182)  / 01110B,
+				10001B,
+				10001B,
+				01111B,
+				00001B,
+				00010B,
+				11100B /    # 9
+
+data	(font[i], i=183,189)  / 00000B,
+				00000B,
+				00100B,
+				00000B,
+				00100B,
+				00000B,
+				00000B /    # :
+
+data	(font[i], i=190,196)  / 00000B,
+				00000B,
+				00100B,
+				00000B,
+				00100B,
+				00100B,
+				01000B /    # ;
+
+data	(font[i], i=197,203)  / 00010B,
+				00100B,
+				01000B,
+				10000B,
+				01000B,
+				00100B,
+				00010B /    # <
+
+data	(font[i], i=204,210)  / 00000B,
+				00000B,
+				11111B,
+				00000B,
+				11111B,
+				00000B,
+				00000B /    # =
+
+data	(font[i], i=211,217)  / 01000B,
+				00100B,
+				00010B,
+				00001B,
+				00010B,
+				00100B,
+				01000B /    # >
+
+data	(font[i], i=218,224)  / 01110B,
+				10001B,
+				00010B,
+				00100B,
+				00100B,
+				00000B,
+				00100B /    # ?
+
+data	(font[i], i=225,231)  / 01110B,
+				10001B,
+				10101B,
+				10111B,
+				10110B,
+				10000B,
+				01111B /    # @
+
+data	(font[i], i=232,238)  / 00100B,
+				01010B,
+				10001B,
+				10001B,
+				11111B,
+				10001B,
+				10001B /    # A
+
+data	(font[i], i=239,245)  / 11110B,
+				10001B,
+				10001B,
+				11110B,
+				10001B,
+				10001B,
+				11110B /    # B
+
+data	(font[i], i=246,252)  / 01110B,
+				10001B,
+				10000B,
+				10000B,
+				10000B,
+				10001B,
+				01110B /    # C
+
+data	(font[i], i=253,259)  / 11110B,
+				10001B,
+				10001B,
+				10001B,
+				10001B,
+				10001B,
+				11110B /    # D
+
+data	(font[i], i=260,266)  / 11111B,
+				10000B,
+				10000B,
+				11110B,
+				10000B,
+				10000B,
+				11111B /    # E
+
+data	(font[i], i=267,273)  / 11111B,
+				10000B,
+				10000B,
+				11110B,
+				10000B,
+				10000B,
+				10000B /    # F
+
+data	(font[i], i=274,280)  / 01111B,
+				10000B,
+				10000B,
+				10000B,
+				10011B,
+				10001B,
+				01111B /    # G
+
+data	(font[i], i=281,287)  / 10001B,
+				10001B,
+				10001B,
+				11111B,
+				10001B,
+				10001B,
+				10001B /    # H
+
+data	(font[i], i=288,294)  / 01110B,
+				00100B,
+				00100B,
+				00100B,
+				00100B,
+				00100B,
+				01110B /    # I
+
+data	(font[i], i=295,301)  / 00001B,
+				00001B,
+				00001B,
+				00001B,
+				00001B,
+				10001B,
+				01110B /    # J
+
+data	(font[i], i=302,308)  / 10001B,
+				10010B,
+				10100B,
+				11000B,
+				10100B,
+				10010B,
+				10001B /    # K
+
+data	(font[i], i=309,315)  / 10000B,
+				10000B,
+				10000B,
+				10000B,
+				10000B,
+				10000B,
+				11111B /    # L
+
+data	(font[i], i=316,322)  / 10001B,
+				11011B,
+				10101B,
+				10101B,
+				10001B,
+				10001B,
+				10001B /    # M
+
+data	(font[i], i=323,329)  / 10001B,
+				10001B,
+				11001B,
+				10101B,
+				10011B,
+				10001B,
+				10001B /    # N
+
+data	(font[i], i=330,336)  / 01110B,
+				10001B,
+				10001B,
+				10001B,
+				10001B,
+				10001B,
+				01110B /    # O
+
+data	(font[i], i=337,343)  / 11110B,
+				10001B,
+				10001B,
+				11110B,
+				10000B,
+				10000B,
+				10000B /    # P
+
+data	(font[i], i=344,350)  / 01110B,
+				10001B,
+				10001B,
+				10001B,
+				10101B,
+				10010B,
+				01101B /    # Q
+
+data	(font[i], i=351,357)  / 11110B,
+				10001B,
+				10001B,
+				11110B,
+				10100B,
+				10010B,
+				10001B /    # R
+
+data	(font[i], i=358,364)  / 01110B,
+				10001B,
+				10000B,
+				01110B,
+				00001B,
+				10001B,
+				01110B /    # S
+
+data	(font[i], i=365,371)  / 11111B,
+				00100B,
+				00100B,
+				00100B,
+				00100B,
+				00100B,
+				00100B /    # T
+
+data	(font[i], i=372,378)  / 10001B,
+				10001B,
+				10001B,
+				10001B,
+				10001B,
+				10001B,
+				01110B /    # U
+
+data	(font[i], i=379,385)  / 10001B,
+				10001B,
+				10001B,
+				10001B,
+				10001B,
+				01010B,
+				00100B /    # V
+
+data	(font[i], i=386,392)  / 10001B,
+				10001B,
+				10001B,
+				10101B,
+				10101B,
+				11011B,
+				10001B /    # W
+
+data	(font[i], i=393,399)  / 10001B,
+				10001B,
+				01010B,
+				00100B,
+				01010B,
+				10001B,
+				10001B /    # X
+
+data	(font[i], i=400,406)  / 10001B,
+				10001B,
+				01010B,
+				00100B,
+				00100B,
+				00100B,
+				00100B /    # Y
+
+data	(font[i], i=407,413)  / 11111B,
+				00001B,
+				00010B,
+				00100B,
+				01000B,
+				10000B,
+				11111B /    # Z
+
+data	(font[i], i=414,420)  / 11111B,
+				11000B,
+				11000B,
+				11000B,
+				11000B,
+				11000B,
+				11111B /    # [
+
+data	(font[i], i=421,427)  / 00000B,
+				10000B,
+				01000B,
+				00100B,
+				00010B,
+				00001B,
+				00000B /    # \
+
+data	(font[i], i=428,434)  / 11111B,
+				00011B,
+				00011B,
+				00011B,
+				00011B,
+				00011B,
+				11111B /    # ]
+
+data	(font[i], i=435,441)  / 00000B,
+				00000B,
+				00100B,
+				01010B,
+				10001B,
+				00000B,
+				00000B /    # ^
+
+data	(font[i], i=442,448)  / 00000B,
+				00000B,
+				00000B,
+				00000B,
+				00000B,
+				00000B,
+				11111B /    # _
+
+data	(font[i], i=449,455)  / 11111B,
+				10001B,
+				11011B,
+				10101B,
+				11011B,
+				10001B,
+				11111B /    # (unknown)
diff --git a/noao/imred/vtel/putsqib.par b/noao/imred/vtel/putsqib.par
new file mode 100644
index 00000000..635f540f
--- /dev/null
+++ b/noao/imred/vtel/putsqib.par
@@ -0,0 +1,3 @@
+image,s,q,,,,Data image to merge with squibby brightness image
+sqibimage,s,q,,,,Squibby brightness image
+merged,s,q,,,,New image to contain the merged image
diff --git a/noao/imred/vtel/putsqib.x b/noao/imred/vtel/putsqib.x
new file mode 100644
index 00000000..9299c4d4
--- /dev/null
+++ b/noao/imred/vtel/putsqib.x
@@ -0,0 +1,69 @@
+include <mach.h>
+include <imhdr.h>
+include "vt.h"
+
+# PUTSQIB -- Murge a solar synoptic 'data only' image with a
+# squibby brightness image.  Output image is separate image.
+
+procedure t_putsqib()
+
+char	image[SZ_FNAME]		# input image
+char	sqibimage[SZ_FNAME]	# squibby brightness image
+char	merged[SZ_FNAME]	# output merged image
+
+int	i, numpix
+pointer	im, ldatagp, lsqibgp, lpp,  sqibim, mim
+pointer	immap(), imgl2s(), impl2s()
+errchk	immap, imgl2s, impl2s
+
+begin
+	# Get parameters from the CL.
+	call clgstr ("image", image, SZ_FNAME)
+	call clgstr ("sqibimage", sqibimage, SZ_FNAME)
+	call clgstr ("merged", merged, SZ_FNAME)
+
+	# Open the two input images, see that they are the same size.
+	im = immap (image, READ_ONLY, 0)
+	sqibim = immap (sqibimage, READ_ONLY, 0)
+
+	# If not, error.
+	if (IM_LEN(im,2) != IM_LEN(sqibim,2))
+	    call error(0,"sizes of data image and sqib image must match")
+
+	if (IM_LEN(im,1) != IM_LEN(sqibim,1))
+	    call error(0,"sizes of data image and sqib image must match")
+
+	# Open the new image.
+	mim = immap (merged, NEW_COPY, im)
+
+	do i = 1, IM_LEN(im,2) {
+	    ldatagp = imgl2s (im, i)
+	    lsqibgp = imgl2s (sqibim, i)
+	    lpp = impl2s (mim, i)
+	    numpix = IM_LEN(im,1)
+	    call sqibput (Mems[ldatagp], Mems[lsqibgp], Mems[lpp], numpix)
+	}
+
+	# Unmap images.
+	call imunmap (im)
+	call imunmap (sqibim)
+	call imunmap (mim)
+end
+
+
+# SQIBPUT -- pack squibby brightness from line2 into line1 and put the
+# result into line3.
+
+procedure sqibput (line1, line2, line3, numpix)
+
+short	line1[numpix]		# data line
+short	line2[numpix]		# sqib line
+short	line3[numpix]		# out line
+int	numpix			# number of pixels
+
+int	i
+
+begin
+	do i = 1, numpix
+	    line3[i] = line1[i]*16 + line2[i]
+end
diff --git a/noao/imred/vtel/quickfit.par b/noao/imred/vtel/quickfit.par
new file mode 100644
index 00000000..6ce8e742
--- /dev/null
+++ b/noao/imred/vtel/quickfit.par
@@ -0,0 +1,8 @@
+image,s,q,,,,Image file descriptor
+threshold,i,h,4,,,Squibby brightness threshold 
+verbose,b,h,no,,,Print out in verbose mode?
+xguess,i,h,1024,,,X coordinate of center of guess circle
+yguess,i,h,1024,,,Y coordinate of center of guess circle
+halfwidth,i,h,50,,,Halfwidth of limbfinding window
+rowspace,i,h,20,,,# of rows to skip near center in limbfind
+rejectcoeff,r,h,.02,,,Least squares rejection coefficient
diff --git a/noao/imred/vtel/quickfit.x b/noao/imred/vtel/quickfit.x
new file mode 100644
index 00000000..40efb257
--- /dev/null
+++ b/noao/imred/vtel/quickfit.x
@@ -0,0 +1,499 @@
+include <mach.h>
+include <imhdr.h>
+include	"vt.h"
+
+define	SZ_VTPBUF	4096		# Size of limb point buffer.
+
+# QUICKFIT -- Given a fulldisk solar image, find the parameters of an ellipse
+# that best fits the limb.  First the points on the limb are determined using
+# the squibby brightness, then an initial guess for the limb parameters is
+# made, and finally a least squares fit is made by an iterative method.
+
+procedure t_quickfit()
+
+char	image[SZ_FNAME]				# image to find the limb on
+int	threshold				# squibby limb threshold
+bool	verbose					# verbose flag
+
+pointer	pb					# buffer for saving limb points
+int	npoints, rejects			# number of limb pts, rejects
+real	x, y, a, b				# x, y, a, b (a = z0)
+real	rguess, rpercent			# initial guess at r, % rejects
+errchk	limbfind, efit
+pointer	im, sp
+
+pointer	immap()
+int	clgeti()
+bool	clgetb()
+errchk	immap, limbfind
+
+begin
+	call smark (sp)
+	call salloc (pb, 2*SZ_VTPBUF, TY_INT)
+
+	# Get parameters from the cl.
+	call clgstr ("image", image, SZ_FNAME)
+	threshold = clgeti ("threshold")
+	verbose = clgetb ("verbose")
+
+	# Open image.
+	im = immap (image, READ_WRITE, 0)
+
+	# Get the point buffer and npoints.
+	iferr (call limbfind (im, Memi[pb], npoints, threshold, rguess,
+	    verbose))
+	    call eprintf("Error getting limbpoints.\n")
+	if (verbose) {
+	    call printf ("\nrguess = %g\n")
+	        call pargr (rguess)
+	        call flush (STDOUT)
+	}
+
+	# Fit the ellipse.
+	b = rguess
+	a = rguess
+	x = real(DIM_VTFD)/2.
+	y = real(DIM_VTFD)/2.
+	iferr (call efit (Memi[pb], npoints, x, y, a, b, rejects, verbose))
+	    call eprintf ("Error fitting elipse.\n")
+
+	rpercent = real(rejects)/real(npoints)
+	if (verbose) {
+	    call printf ("\nTotal number of limbpoints found was %d\n")
+	        call pargi (npoints)
+	    call printf ("Number of limbpoints rejected was %d\n")
+	        call pargi (rejects)
+	    call printf ("Fraction of limb points rejected = %g\n")
+	        call pargr (rpercent)
+	        call flush (STDOUT)
+	}
+
+	# Put ellipse parameters in image header.
+	call imaddr (im, "E_XCEN", x)
+	call imaddr (im, "E_YCEN", y)
+	call imaddr (im, "E_XSMD", a)
+	call imaddr (im, "E_YSMD", b)
+
+	# Close the image.
+	call imunmap (im)
+
+	call sfree (sp)
+end
+
+
+# LIMBFIND - Find all of the points on the image that determine the
+# limb.  This is done line by line.
+
+procedure limbfind (imageptr, pointbuf, npoints, threshold, rguess, verbose)
+
+pointer	imageptr		# pointer to image
+int	pointbuf[SZ_VTPBUF,2]	# buffer in which to store limb points
+int	npoints			# number of points
+int	threshold		# squibby threshold
+real	rguess			# first guess at radius
+bool	verbose			# verbose flag
+
+int	rowspace, halfwidth, leftsave, rightsave, y
+int	numpix, numrow, leftx, rightx, yesno
+int	month, day, year, hour, minute, second, obsdate, obstime
+real	b0, l0
+pointer	lpg
+
+pointer	imgl2s()
+int	clgeti(), imgeti()
+errchk	ephem, flocr, florr, imgl2s
+
+begin
+	# Get date and time from the header.
+	obsdate = imgeti (imageptr, "OBS_DATE")
+	obstime = imgeti (imageptr, "OBS_TIME")
+
+	# Calculate the month/day/year.
+	month = obsdate/10000
+	day = obsdate/100 - 100 * (obsdate/10000)
+	year = obsdate - 100 * (obsdate/100)
+
+	# Calculate the hour:minute:second.
+	hour = int(obstime/3600)
+	minute = int((obstime - hour * 3600)/60)
+	second = obstime - hour * 3600 - minute * 60
+	if (verbose) {
+	    call printf("date and time of this image = %d/%d/%d, %d:%d:%d\n")
+	        call pargi(month)
+	        call pargi(day)
+	        call pargi(year)
+	        call pargi(hour)
+	        call pargi(minute)
+	        call pargi(second)
+	    call flush (STDOUT)
+	}
+
+	# Get rowspace and halfwidth from the cl.
+	halfwidth = clgeti("halfwidth")
+	rowspace = clgeti("rowspace")
+
+	numpix = IM_LEN(imageptr, 1)
+	numrow = IM_LEN(imageptr, 2)
+	npoints = 0
+
+	# Get rguess from ephem.
+	iferr (call ephem (month, day, year, hour, minute, second, rguess,
+	    b0, l0, verbose))
+	    call eprintf ("Error getting ephemeris data.\n")
+
+	# Put b0 and l0 in the image header.
+	call imaddr (imageptr, "B_ZERO", b0)
+	call imaddr (imageptr, "L_ZERO", l0)
+
+	# Get central row to start with and find its limb points.
+	lpg = imgl2s (imageptr, numrow/2)
+	yesno = YES
+	iferr (call flocr (Mems[lpg], numpix, pointbuf, numrow, npoints, leftx,
+	    rightx, threshold, yesno))
+	    call eprintf ("Error in 'find limb on center row(flocr)'\n")
+	if (yesno == NO)
+	    call error (0,"Failure to find initial limb points, quickfit dies")
+
+	leftsave = leftx
+	rightsave = rightx
+
+	# Find the limb points for the lower half of the image.
+	yesno = YES
+	y = numrow/2-rowspace
+	while (y >= 1) {
+
+	    # Read this line in from the image.
+	    lpg = imgl2s (imageptr, y)
+
+	    # Find its limb points.
+	    iferr (call florr (Mems[lpg], numpix, pointbuf, npoints, numrow,
+	        y, leftx, rightx, threshold, yesno, rguess, halfwidth))
+		call eprintf ("Error in florr.\n")
+	    if (yesno == NO)
+		break
+	    if (abs(y-numrow/2) > rguess)
+		break
+	    if ((int(rowspace * (rguess**2 -
+		real(y-numrow/2)**2)**.5/rguess)) >= 1)
+	        y = y - int(rowspace * (rguess**2 -
+		    real(y-numrow/2)**2)**.5/rguess)
+	    else
+		y = y - 1
+	}
+
+	# Find the limb points for the upper half of the image.
+
+	# Restore the pointers to the limb at disk center.
+	leftx = leftsave
+	rightx = rightsave
+	yesno = NO
+	y = numrow/2+rowspace
+
+	while (y <= numrow) {
+	    # Read this line in from the image.
+	    lpg = imgl2s (imageptr, y)
+
+	    # Find its limb points.
+	    iferr (call florr (Mems[lpg], numpix, pointbuf, npoints, numrow,
+		y, leftx, rightx, threshold, yesno, rguess, halfwidth))
+		call eprintf ("Error in florr.\n")
+
+	    # If we couldn't find any limb points then it's time to go.
+	    if (yesno == NO)
+		break
+
+	    # If we are beyond the limb vertically then its time to go.
+	    if (abs(y-numrow/2) > rguess)
+		break
+
+	    # If the calculated rowspacing gets less than 1, just set it to 1.
+	    if ((int(rowspace * (rguess**2 -
+		real(y-numrow/2)**2)**.5/rguess)) >= 1) {
+	        y = y + int(rowspace * (rguess**2 -
+		    real(y-numrow/2)**2)**.5/rguess)
+	    } else
+		y = y + 1
+	}
+end
+
+
+# FLOCR -- Find Limbpoints On Center Row.  Since this is the first row
+# to be searched, we have no idea of approximately where the limb points
+# will be found in the row as we have in florr.  We search from the endpoints
+# of the row inward until the squibby brightness crosses the threshold.
+
+procedure flocr (array, numpix, pointbuf, npoints, numrow, leftx, rightx,
+		    threshold, yesno)
+
+short	array[numpix]		# line of image
+int	pointbuf[SZ_VTPBUF,2]	# limb point storage array
+int	numpix			# number of pixels in line
+int	npoints			# number of limb points
+int	numrow			# which row this is in image
+int	leftx			# return left boundary position here
+int	rightx			# return right boundary position here
+int	threshold		# squibby brightness limb threshold
+int	yesno			# return yes if we found the limb
+
+int	i, j, foundi, foundj
+
+begin
+	# Start at beginning and end of array and work in.
+	i = 1
+	j = numpix
+
+	# Flags that indicate when a limbpoint has been found.
+	foundi = 0
+	foundj = 0
+
+	while (i <= j) {
+	    if (foundi == 0) {
+		if (and(int(array[i]), 17B) >= threshold) {
+		    foundi = 1
+		    npoints = npoints + 1
+		    pointbuf[npoints,1] = i
+		    pointbuf[npoints,2] = numrow/2
+		    leftx = i
+		}
+		if (i == j) {
+		    yesno = NO
+		    return
+		}
+	    }
+
+	    if (foundj == 0) {
+		if (and(int(array[j]), 17B) >= threshold) {
+		    foundj = 1
+		    npoints = npoints + 1
+		    pointbuf[npoints,1] = j
+		    pointbuf[npoints,2] = numrow/2
+		    rightx = j
+		}
+	    }
+	    if ((foundi == 1) && (foundj == 1))
+		break
+	    i = i + 1
+	    j = j - 1
+	}
+end
+
+
+# FLORR -- Find Limbpoints On Random Row. Since we know the approximate
+# positions of the limbpoints based on their positions on the ajacent
+# row, we can restrict the range of x positions to be searched to those
+# within a certain distance of those positions.  These ranges we will
+# call windows.  Each window is checked for validity before it is
+# searched for the limbpoints, if invalid a correct window is found.
+
+procedure florr (array, numpix, pointbuf, npoints, numrow, y, leftx, rightx,
+	threshold, yesno, rguess, halfwidth)
+
+short	array[numpix]		# line of image
+int	pointbuf[SZ_VTPBUF,2]	# limb point storage array
+int	numpix			# number of pixels in line
+int	npoints			# number of limb points
+int	numrow			# which row this is in image
+int	leftx			# return left boundary position here
+int	rightx			# return right boundary position here
+int	threshold		# squibby brightness limb threshold
+int	yesno			# return yes if we found the limb
+int	halfwidth		# halfwidth of limb search window
+real	rguess			# radius for sun guess
+
+int	i, j, y
+
+begin
+	# Windows are leftx plus or minus halfwidth and rightx plus or
+	# minus halfwidth.  Before searching windows, check them for
+	# validity and call newwindow if necessary.
+
+	# Check for validity means the endpoint we expect to be outside
+	# the limb should have a squibby brightness less than the
+	# threshold and the inside the limb endpoint should have a
+	# squibby brightness greater than the threshold.
+
+	# if invalid...
+	if ((and(int(array[max(1,(leftx-halfwidth))]),17B) >= threshold) ||
+	    (and(int(array[leftx+halfwidth]),17B) < threshold)) {
+
+	    # if we are getting too far from the center (outside limb)
+	    # then return flag for no limbpoints.
+
+	    if (abs(y-numrow/2) > int(rguess)) {
+		yesno = NO
+		return
+	    }
+
+	    # Otherwise calculate a new leftx for this row.
+	    leftx = -((int(rguess**2) - (y-numrow/2)**2)**.5) + numrow/2
+	}
+
+	# If we now have a valid window...
+	if ((and(int(array[max(1,(leftx-halfwidth))]),17B) < threshold) &&
+	    (and(int(array[leftx+halfwidth]),17B) >= threshold)) {
+
+	    # Search window for limb point.
+	    do i = max(1,(leftx-halfwidth)), leftx+halfwidth {
+
+		# When we find it add it to the limbpoints array and
+		# break out of the do loop
+
+	        if (and(int(array[i]), 17B) >= threshold) {
+
+		    # Set the 'we found it' flag.
+		    yesno = YES
+
+		    npoints = npoints + 1
+		    pointbuf[npoints,1] = i
+		    pointbuf[npoints,2] = y
+		    leftx = i
+		    break
+	        }
+	    }
+	}
+
+	# Same stuff for the right hand window.
+	if ((and(int(array[min(numpix,(rightx+halfwidth))]),17B) >=
+	    threshold) || (and(int(array[rightx-halfwidth]),17B) < threshold)) {
+	    if (abs(y-numrow/2) > int(rguess)) {
+		yesno = NO
+		return
+	    }
+	    rightx = (int(rguess**2) - (y-numrow/2)**2)**.5 + numrow/2
+	}
+
+	if ((and(int(array[min(numpix,(rightx+halfwidth))]),17B) < threshold) &&
+	    (and(int(array[rightx-halfwidth]),17B) >= threshold)) {
+	    do j = min(numpix,(rightx+halfwidth)), rightx-halfwidth, -1 {
+	        if (and(int(array[j]), 17B) >= threshold) {
+		    yesno = YES
+		    npoints = npoints + 1
+		    pointbuf[npoints,1] = j
+		    pointbuf[npoints,2] = y
+		    rightx = j
+		    break
+	        }
+	    }
+	}
+end
+
+
+# EFIT - Find the best fitting ellipse to the limb points.  We iterate
+# 10 times, this seems to converge very well.
+# Algorithm due to Jack Harvey.
+
+procedure efit (pointbuf, npoints, xzero, yzero, azero, bzero, rejects,
+	verbose)
+
+int	pointbuf[SZ_VTPBUF,2]		# buffer containing limb points
+int	npoints 			# number of limb points
+real	xzero, yzero, azero, bzero	# return elipse parameters
+int	rejects				# number of points rejected
+bool	verbose				# verbose flag
+
+int	i, j, ij, n
+real	xcenter, ycenter, a, b, a2, b2, a3, b3
+real	z[6,6]
+real	x1, y1, x2, y2, q[5], fn, sq
+real	rejectcoeff
+
+real	clgetr()
+
+begin
+	# Get the least squares rejection coefficient.
+	rejectcoeff = clgetr("rejectcoeff")
+	xcenter = xzero
+	ycenter = yzero
+	a = azero
+	b = azero
+
+	do ij = 1, 10 {
+	    a2 = a**2
+	    a3 = a2 * a
+	    b2 = b**2
+	    b3 = b2 * b
+	    sq = 0.
+
+	    do i = 1, 6
+		do j = 1, 6
+		    z[i,j] = 0
+
+	    fn = 0.
+	    rejects = 0
+
+	    do n = 1, npoints {
+		x1 = real(pointbuf[n,1]) - xcenter
+		y1 = real(pointbuf[n,2]) - ycenter
+		x2 = x1**2
+		y2 = y1**2
+		q[1] = x1/a2
+		q[2] = y1/b2
+		q[3] = -x2/a3
+		q[4] = -y2/b3
+		q[5] = .5 * (1. - x2/a2 - y2/b2)
+
+		# Reject a point if it is too far from the approximate ellipse.
+		if (abs(q[5]) >= rejectcoeff) {
+		    rejects = rejects + 1
+		    next
+		}
+
+		sq = sq + q[5]
+
+		do i = 1, 5
+		    do j = i, 5
+			z[i,j+1] = z[i,j+1] + q[i] * q[j]
+
+		fn = fn + 1.
+	    }
+
+	    sq = sq/fn
+	    call flush(STDOUT)
+	    call lstsq (z, 6, fn)
+	    if (z(5,3) > 3.)
+		z(5,3) = 3.
+	    if (z(5,3) < -3.)
+		z(5,3) = -3.
+	    if (z(5,4) > 3.)
+		z(5,4) = 3.
+	    if (z(5,4) < -3.)
+		z(5,4) = -3.
+	    if (z(5,1) > 10.)
+		z(5,1) = 10.
+	    if (z(5,1) < -10.)
+		z(5,1) = -10.
+	    if (z(5,2) > 10.)
+		z(5,2) = 10.
+	    if (z(5,2) < -10.)
+		z(5,2) = -10.
+	    a = a + z[5,3]
+	    b = b + z[5,4]
+	    xcenter = xcenter - z[5,1]
+	    ycenter = ycenter - z[5,2]
+
+	    if (verbose) {
+		call printf ("x = %f, y = %f, a = %f, b = %f, sq = %13.10f\n")
+		    call pargr (xcenter)
+		    call pargr (ycenter)
+		    call pargr (a)
+		    call pargr (b)
+		    call pargr (sq)
+		call flush (STDOUT)
+	    }
+	}
+
+	if (verbose) {
+	    call printf ("\nCoordinates of center are x = %f, y = %f\n")
+	        call pargr(xcenter)
+	        call pargr(ycenter)
+	    call printf ("xsemidiameter = %f, ysemidiameter = %f\n")
+	        call pargr(a)
+	        call pargr(b)
+	    call flush (STDOUT)
+	}
+
+	xzero = xcenter
+	yzero = ycenter
+	azero = a
+	bzero = b
+end
diff --git a/noao/imred/vtel/readheader.x b/noao/imred/vtel/readheader.x
new file mode 100644
index 00000000..85fb6f66
--- /dev/null
+++ b/noao/imred/vtel/readheader.x
@@ -0,0 +1,59 @@
+include <mach.h>
+include <fset.h>
+include	"vt.h"
+
+# READHEADER -- Read header info from the input.
+
+int procedure readheader(inputfd, hbuf, selfbuf)
+
+int	inputfd		# input file discriptor
+pointer	hbuf		# header data input buffer pointer (short, SZ_VTHDR)
+bool	selfbuf		# flag to tell if we should do our own buffering
+
+int	numchars
+pointer	sp, tempbuf
+int	read()
+errchk	read
+
+begin
+	call smark (sp)
+	call salloc (tempbuf, 100, TY_SHORT)
+
+	# If we are reading from tape and buffering for ourselves then
+	# do a large read and see how many chars we get.  If too few or
+	# too many give an error.  Otherwise just read the correct number 
+	# of chars.
+
+	if (selfbuf) {
+	    iferr (numchars = read (inputfd, Mems[tempbuf],
+		10000*SZB_SHORT/SZB_CHAR)) {
+		call fseti (inputfd, F_VALIDATE, SZ_VTHDR*SZB_SHORT/SZB_CHAR)
+		call printf ("Error reading header.\n")
+		numchars = read (inputfd, Mems[tempbuf],
+		    SZ_VTHDR*SZB_SHORT/SZB_CHAR)
+	    }
+	    if (numchars < 10 || numchars >= 100) {
+	        call error (0, "error reading header")
+		return (numchars)
+	    }
+	    call amovs (Mems[tempbuf], Mems[hbuf], SZ_VTHDR*SZB_SHORT/SZB_CHAR)
+	} else {
+	    iferr (numchars = read (inputfd, Mems[hbuf],
+		SZ_VTHDR*SZB_SHORT/SZB_CHAR)) {
+		call fseti (inputfd, F_VALIDATE, SZ_VTHDR*SZB_SHORT/SZB_CHAR)
+		call printf ("Error reading header.\n")
+		numchars = read (inputfd, Mems[tempbuf],
+		    SZ_VTHDR*SZB_SHORT/SZB_CHAR)
+	    }
+	    if (numchars < SZ_VTHDR*SZB_SHORT/SZB_CHAR) {
+	        call error (0, "eof encountered when reading header")
+		return (0)
+	    }
+	}
+
+	if (BYTE_SWAP2 == YES)
+	    call bswap2 (Mems[hbuf], 1, Mems[hbuf], 1, SZ_VTHDR*SZB_SHORT)
+	call sfree (sp)
+
+	return (SZ_VTHDR*SZB_SHORT/SZB_CHAR)
+end
diff --git a/noao/imred/vtel/readss1.x b/noao/imred/vtel/readss1.x
new file mode 100644
index 00000000..2aea6d51
--- /dev/null
+++ b/noao/imred/vtel/readss1.x
@@ -0,0 +1,163 @@
+include <mach.h>
+include	<imhdr.h>
+include <fset.h>
+include	"vt.h"
+
+define	WDSBRSTR	50
+
+# READSS1 -- Read a type 1 sector scan from tape and format into 3 iraf images.
+# Type one sector scans consist of three images packed into 32 bits per
+# pixel.  The three images are 1. velocity (12 bits) 2. select (12 bits) and
+# 3. continuum intensity (8 bits).  The images are only 256 pixels high as
+# opposed to 512 pixels high for the other scans.
+
+procedure readss1 (inputfd, filenumber, brief, select, bright, velocity, hs)
+
+int	inputfd			# file descriptor for input (usually tape)
+int	filenumber		# file number on tape
+bool	brief			# short output file names
+bool	select			# flag to make select image
+bool	bright			# flag to make bright image
+bool	velocity		# flag to make velocity image
+int	hs			# header data structure pointer
+
+char	velimage[SZ_FNAME]	# Velocity image
+char	selimage[SZ_FNAME]	# Select image
+char	britimage[SZ_FNAME]	# Brightness image
+short	u[SWTH_HIGH], dat
+int	date, hour, minute, seconds, i, j, num, lrs
+pointer	velim, selim, britim, velsrp, selsrp, britsrp
+
+int	read()
+pointer	immap(), impl2s()
+errchk	immap, impl2s
+
+begin
+	# Calculate the time.  Assemble the output image names.
+	hour = int(VT_HTIME(hs)/3600)
+	minute = int((VT_HTIME(hs) - hour * 3600)/60)
+	seconds = int(VT_HTIME(hs) - hour * 3600 - minute * 60)
+	if (brief) {
+	    call sprintf (velimage[1], SZ_FNAME, "v%03d")
+	        call pargi (filenumber)
+	    call sprintf (selimage[1], SZ_FNAME, "s%03d")
+	        call pargi (filenumber)
+	    call sprintf (britimage[1], SZ_FNAME, "b%03d")
+	        call pargi (filenumber)
+	} else {
+	    call sprintf (velimage[1], SZ_FNAME, "v%02d_%02d%02d_%03d")
+	        call pargi (VT_HDAY(hs)) # day of month
+	        call pargi (hour)
+	        call pargi (minute)
+	        call pargi (filenumber)
+	    call sprintf (selimage[1], SZ_FNAME, "s%02d_%02d%02d_%03d")
+	        call pargi (VT_HDAY(hs)) # day of month
+	        call pargi (hour)
+	        call pargi (minute)
+	        call pargi (filenumber)
+	    call sprintf (britimage[1], SZ_FNAME, "b%02d_%02d%02d_%03d")
+	        call pargi (VT_HDAY(hs)) # day of month
+	        call pargi (hour)
+	        call pargi (minute)
+	        call pargi (filenumber)
+	}
+	if (select) {
+	    selim = immap (selimage, NEW_IMAGE, 0)
+	    IM_NDIM(selim) = 2
+	    IM_LEN(selim,1) = SWTH_HIGH/2
+	    IM_LEN(selim,2) = VT_HNUMCOLS(hs)
+	    IM_PIXTYPE(selim) = TY_SHORT
+	    call imaddi (selim, "obs_time", VT_HTIME(hs))
+	    date = VT_HMONTH(hs) * 10000 + VT_HDAY(hs) * 100 + VT_HYEAR(hs)
+	    call imaddi (selim, "obs_date", date )
+	    call imaddi (selim, "wv_lngth", VT_HWVLNGTH(hs))
+	    call imaddi (selim, "obs_type", VT_HOBSTYPE(hs))
+	    call imaddi (selim, "av_intns", VT_HAVINTENS(hs))
+	    call imaddi (selim, "num_cols", VT_HNUMCOLS(hs))
+	    call imaddi (selim, "intg/pix", VT_HINTGPIX(hs))
+	    call imaddi (selim, "rep_time", VT_HREPTIME(hs))
+	}
+	if (bright) {
+	    britim = immap (britimage, NEW_IMAGE, 0)
+	    IM_NDIM(britim) = 2
+	    IM_LEN(britim,1) = SWTH_HIGH/2
+	    IM_LEN(britim,2) = VT_HNUMCOLS(hs)
+	    IM_PIXTYPE(britim) = TY_SHORT
+	    call imaddi (britim, "obs_time", VT_HTIME(hs))
+	    date = VT_HMONTH(hs) * 10000 + VT_HDAY(hs) * 100 + VT_HYEAR(hs)
+	    call imaddi (britim, "obs_date", date )
+	    call imaddi (britim, "wv_lngth", VT_HWVLNGTH(hs))
+	    call imaddi (britim, "obs_type", VT_HOBSTYPE(hs))
+	    call imaddi (britim, "av_intns", VT_HAVINTENS(hs))
+	    call imaddi (britim, "num_cols", VT_HNUMCOLS(hs))
+	    call imaddi (britim, "intg/pix", VT_HINTGPIX(hs))
+	    call imaddi (britim, "rep_time", VT_HREPTIME(hs))
+	}
+	if (velocity) {
+	    velim = immap (velimage, NEW_IMAGE, 0)
+	    IM_NDIM(velim) = 2
+	    IM_LEN(velim,1) = SWTH_HIGH/2
+	    IM_LEN(velim,2) = VT_HNUMCOLS(hs)
+	    IM_PIXTYPE(velim) = TY_SHORT
+	    call imaddi (velim, "obs_time", VT_HTIME(hs))
+	    date = VT_HMONTH(hs) * 10000 + VT_HDAY(hs) * 100 + VT_HYEAR(hs)
+	    call imaddi (velim, "obs_date", date )
+	    call imaddi (velim, "wv_lngth", VT_HWVLNGTH(hs))
+	    call imaddi (velim, "obs_type", VT_HOBSTYPE(hs))
+	    call imaddi (velim, "av_intns", VT_HAVINTENS(hs))
+	    call imaddi (velim, "num_cols", VT_HNUMCOLS(hs))
+	    call imaddi (velim, "intg/pix", VT_HINTGPIX(hs))
+	    call imaddi (velim, "rep_time", VT_HREPTIME(hs))
+	}
+
+	do j = 1, VT_HNUMCOLS(hs) {
+	    if (select)
+	        selsrp = impl2s (selim, j)
+	    if (bright)
+	        britsrp = impl2s (britim, j)
+	    if (velocity)
+	        velsrp = impl2s (velim, j)
+
+	    iferr (num = read (inputfd, u, SWTH_HIGH*SZB_SHORT/SZB_CHAR)) {
+		call fseti (inputfd, F_VALIDATE, lrs*SZB_SHORT/SZB_CHAR)
+		call eprintf ("Error on tape read.\n")
+		num = read (inputfd, u, SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	    }
+	    lrs = num
+	    if (num < SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	        call error (0, "eof encountered when reading file")
+	    if (BYTE_SWAP2 == YES)
+	        call bswap2 (u, 1, u, 1, SWTH_HIGH * SZB_SHORT)
+
+	    # Unpack the data into the three arrays.
+	    do i = 257, 512 {
+		if (select) {
+		    dat = u[i]/16
+		    if (u[i] < 0)
+			dat = dat - 1
+		    Mems[selsrp+i-257] = dat
+		}
+		if (bright)
+		    Mems[britsrp+i-257] = and(int(u[i]),17B)*16
+	    }
+
+	    do i = 1, 256 {
+		if (velocity) {
+		    dat = u[i]/16
+		    if (u[i] < 0)
+			dat = dat - 1
+		    Mems[velsrp+i-1] = dat
+		}
+		if (bright)
+		    Mems[britsrp+i-1] = Mems[britsrp+i-1]+and(int(u[i]),17B)
+	    }
+	}
+
+	# Unmap images.
+	if (select)
+	    call imunmap (selim)
+	if (velocity)
+	    call imunmap (velim)
+	if (bright)
+	    call imunmap (britim)
+end
diff --git a/noao/imred/vtel/readss2.x b/noao/imred/vtel/readss2.x
new file mode 100644
index 00000000..71ae8758
--- /dev/null
+++ b/noao/imred/vtel/readss2.x
@@ -0,0 +1,174 @@
+include <mach.h>
+include	<imhdr.h>
+include <fset.h>
+include	"vt.h"
+
+define	WDSBRSTR	50
+
+# READSS2 -- Read a type 2 sector scan from tape and format into 3 iraf images.
+# Type two sector scans consist of three images with 16 bits per
+# pixel.  The three images are 1. velocity (16 bits) 2. select (16 bits) and
+# 3.  brightness (16 bits).  The images are 512 pixels high.
+
+procedure readss2 (inputfd, filenumber, brief, select, bright, velocity, hs)
+
+int	inputfd			# file descriptor for input (usually tape)
+int	filenumber		# file number on tape
+bool	brief			# short output file names
+bool	select			# flag to make select image
+bool	bright			# flag to make bright image
+bool	velocity		# flag to make velocity image
+int	hs			# header data structure pointer
+
+char	velimage[SZ_FNAME]	# velocity image
+char	selimage[SZ_FNAME]	# select image
+char	britimage[SZ_FNAME]	# brightness image
+short	u[SWTH_HIGH]
+int	date, hour, minute, seconds, i, j, num, lrs
+pointer	velim, selim, britim, velsrp, selsrp, britsrp
+
+int	read()
+pointer	immap(), impl2s()
+errchk	immap, impl2s
+
+begin
+	# Calculate the time.  Assemble the output image names.
+	hour = int(VT_HTIME(hs)/3600)
+	minute = int((VT_HTIME(hs) - hour * 3600)/60)
+	seconds = int(VT_HTIME(hs) - hour * 3600 - minute * 60)
+	if (brief) {
+	    call sprintf (velimage[1], SZ_FNAME, "v%03d")
+	        call pargi (filenumber)
+	    call sprintf (selimage[1], SZ_FNAME, "s%03d")
+	        call pargi (filenumber)
+	    call sprintf (britimage[1], SZ_FNAME, "b%03d")
+	        call pargi (filenumber)
+	} else {
+	    call sprintf (velimage[1], SZ_FNAME, "v%02d_%02d%02d_%03d")
+	        call pargi (VT_HDAY(hs)) # day of month
+	        call pargi (hour)
+	        call pargi (minute)
+	        call pargi (filenumber)
+	    call sprintf (selimage[1], SZ_FNAME, "s%02d_%02d%02d_%03d")
+	        call pargi (VT_HDAY(hs)) # day of month
+	        call pargi (hour)
+	        call pargi (minute)
+	        call pargi (filenumber)
+	    call sprintf (britimage[1], SZ_FNAME, "b%02d_%02d%02d_%03d")
+	        call pargi (VT_HDAY(hs)) # day of month
+	        call pargi (hour)
+	        call pargi (minute)
+	        call pargi (filenumber)
+	}
+
+	if (select) {
+	    selim = immap (selimage, NEW_IMAGE, 0)
+	    IM_NDIM(selim) = 2
+	    IM_LEN(selim,1) = SWTH_HIGH
+	    IM_LEN(selim,2) = VT_HNUMCOLS(hs)
+	    IM_PIXTYPE(selim) = TY_SHORT
+	    call imaddi (selim, "obs_time", VT_HTIME(hs))
+	    date = VT_HMONTH(hs) * 10000 + VT_HDAY(hs) * 100 + VT_HYEAR(hs)
+	    call imaddi (selim, "obs_date", date )
+	    call imaddi (selim, "wv_lngth", VT_HWVLNGTH(hs))
+	    call imaddi (selim, "obs_type", VT_HOBSTYPE(hs))
+	    call imaddi (selim, "av_intns", VT_HAVINTENS(hs))
+	    call imaddi (selim, "num_cols", VT_HNUMCOLS(hs))
+	    call imaddi (selim, "intg/pix", VT_HINTGPIX(hs))
+	    call imaddi (selim, "rep_time", VT_HREPTIME(hs))
+	}
+	if (bright) {
+	    britim = immap (britimage, NEW_IMAGE, 0)
+	    IM_NDIM(britim) = 2
+	    IM_LEN(britim,1) = SWTH_HIGH
+	    IM_LEN(britim,2) = VT_HNUMCOLS(hs)
+	    IM_PIXTYPE(britim) = TY_SHORT
+	    call imaddi (britim, "obs_time", VT_HTIME(hs))
+	    date = VT_HMONTH(hs) * 10000 + VT_HDAY(hs) * 100 + VT_HYEAR(hs)
+	    call imaddi (britim, "obs_date", date )
+	    call imaddi (britim, "wv_lngth", VT_HWVLNGTH(hs))
+	    call imaddi (britim, "obs_type", VT_HOBSTYPE(hs))
+	    call imaddi (britim, "av_intns", VT_HAVINTENS(hs))
+	    call imaddi (britim, "num_cols", VT_HNUMCOLS(hs))
+	    call imaddi (britim, "intg/pix", VT_HINTGPIX(hs))
+	    call imaddi (britim, "rep_time", VT_HREPTIME(hs))
+	}
+	if (velocity) {
+	    velim = immap (velimage, NEW_IMAGE, 0)
+	    IM_NDIM(velim) = 2
+	    IM_LEN(velim,1) = SWTH_HIGH
+	    IM_LEN(velim,2) = VT_HNUMCOLS(hs)
+	    IM_PIXTYPE(velim) = TY_SHORT
+	    call imaddi (velim, "obs_time", VT_HTIME(hs))
+	    date = VT_HMONTH(hs) * 10000 + VT_HDAY(hs) * 100 + VT_HYEAR(hs)
+	    call imaddi (velim, "obs_date", date )
+	    call imaddi (velim, "wv_lngth", VT_HWVLNGTH(hs))
+	    call imaddi (velim, "obs_type", VT_HOBSTYPE(hs))
+	    call imaddi (velim, "av_intns", VT_HAVINTENS(hs))
+	    call imaddi (velim, "num_cols", VT_HNUMCOLS(hs))
+	    call imaddi (velim, "intg/pix", VT_HINTGPIX(hs))
+	    call imaddi (velim, "rep_time", VT_HREPTIME(hs))
+	}
+
+	do j = 1, VT_HNUMCOLS(hs) {
+	    if (select)
+	        selsrp = impl2s (selim, j)
+	    if (bright)
+	        britsrp = impl2s (britim, j)
+	    if (velocity)
+	        velsrp = impl2s (velim, j)
+
+	    iferr (num = read (inputfd, u, SWTH_HIGH*SZB_SHORT/SZB_CHAR)) {
+		call fseti (inputfd, F_VALIDATE, lrs*SZB_SHORT/SZB_CHAR)
+		call eprintf ("Error on tape read.\n")
+		num = read (inputfd, u, SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	    }
+	    lrs = num
+	    if (num < SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	        call error (0, "eof encountered when reading file")
+	    if (BYTE_SWAP2 == YES)
+	        call bswap2 (u, 1, u, 1, SWTH_HIGH * SZB_SHORT)
+
+	    if (velocity)
+		do i = 1, 512
+		    Mems[velsrp+i-1] = u[i]
+
+	    iferr (num = read (inputfd, u, SWTH_HIGH*SZB_SHORT/SZB_CHAR)) {
+		call fseti (inputfd, F_VALIDATE, lrs*SZB_SHORT/SZB_CHAR)
+		call eprintf ("Error on tape read.\n")
+		num = read (inputfd, u, SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	    }
+	    lrs = num
+	    if (num < SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	        call error (0, "eof encountered when reading file")
+	    if (BYTE_SWAP2 == YES)
+	        call bswap2 (u, 1, u, 1, SWTH_HIGH * SZB_SHORT)
+
+	    if (select)
+		do i = 1, 512
+		    Mems[selsrp+i-1] = u[i]
+
+	    iferr (num = read (inputfd, u, SWTH_HIGH*SZB_SHORT/SZB_CHAR)) {
+		call fseti (inputfd, F_VALIDATE, lrs*SZB_SHORT/SZB_CHAR)
+		call eprintf ("Error on tape read.\n")
+		num = read (inputfd, u, SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	    }
+	    lrs = num
+	    if (num < SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	        call error (0, "eof encountered when reading file")
+	    if (BYTE_SWAP2 == YES)
+	        call bswap2 (u, 1, u, 1, SWTH_HIGH * SZB_SHORT)
+
+	    if (bright)
+		do i = 1, 512
+		    Mems[britsrp+i-1] = u[i]
+	}
+
+	# Unmap images.
+	if (select)
+	    call imunmap (selim)
+	if (velocity)
+	    call imunmap (velim)
+	if (bright)
+	    call imunmap (britim)
+end
diff --git a/noao/imred/vtel/readss3.x b/noao/imred/vtel/readss3.x
new file mode 100644
index 00000000..f8721ae0
--- /dev/null
+++ b/noao/imred/vtel/readss3.x
@@ -0,0 +1,171 @@
+include <mach.h>
+include	<imhdr.h>
+include <fset.h>
+include	"vt.h"
+
+define	WDSBRSTR	50
+
+# READSS3 -- Read a type 3 sector scan from tape and format into 3 iraf images.
+# Type three sector scans consist of three images packed into 32 bits per
+# pixel.  The three images are 1. velocity (12 bits) 2. select (12 bits) and
+# 3. continuum intensity (8 bits)
+
+procedure readss3 (inputfd, filenumber, brief, select, bright, velocity, hs)
+
+int	inputfd			# file descriptor for input (usually tape)
+int	filenumber		# file number on tape
+bool	brief			# short output file names
+bool	select			# flag to make select image
+bool	bright			# flag to make bright image
+bool	velocity		# flag to make velocity image
+int	hs			# header data structure pointer
+
+char	velimage[SZ_FNAME]	# Velocity image
+char	selimage[SZ_FNAME]	# Select image
+char	britimage[SZ_FNAME]	# Brightness image
+bool	zero
+short	t[SWTH_HIGH], u[SWTH_HIGH], k
+int	date, hour, minute, seconds, i, j, num, lrs
+pointer	velim, selim, britim, velsrp, selsrp, britsrp
+
+define	redo_	10
+
+int	read()
+short	shifts()
+pointer	immap(), impl2s()
+errchk	immap, impl2s
+
+begin
+	k = -4
+
+	# Calculate the time.  Assemble the output image names.
+	hour = int(VT_HTIME(hs)/3600)
+	minute = int((VT_HTIME(hs) - hour * 3600)/60)
+	seconds = int(VT_HTIME(hs) - hour * 3600 - minute * 60)
+	if (brief) {
+	    call sprintf (velimage[1], SZ_FNAME, "v%03d")
+	        call pargi (filenumber)
+	    call sprintf (selimage[1], SZ_FNAME, "s%03d")
+	        call pargi (filenumber)
+	    call sprintf (britimage[1], SZ_FNAME, "b%03d")
+	        call pargi (filenumber)
+	} else {
+	    call sprintf (velimage[1], SZ_FNAME, "v%02d_%02d%02d_%03d")
+	        call pargi (VT_HDAY(hs)) # day of month
+	        call pargi (hour)
+	        call pargi (minute)
+	        call pargi (filenumber)
+	    call sprintf (selimage[1], SZ_FNAME, "s%02d_%02d%02d_%03d")
+	        call pargi (VT_HDAY(hs)) # day of month
+	        call pargi (hour)
+	        call pargi (minute)
+	        call pargi (filenumber)
+	    call sprintf (britimage[1], SZ_FNAME, "b%02d_%02d%02d_%03d")
+	        call pargi (VT_HDAY(hs)) # day of month
+	        call pargi (hour)
+	        call pargi (minute)
+	        call pargi (filenumber)
+	}
+	if (select) {
+	    selim = immap (selimage, NEW_IMAGE, 0)
+	    IM_NDIM(selim) = 2
+	    IM_LEN(selim,1) = SWTH_HIGH
+	    IM_LEN(selim,2) = VT_HNUMCOLS(hs)
+	    IM_PIXTYPE(selim) = TY_SHORT
+	    call imaddi (selim, "obs_time", VT_HTIME(hs))
+	    date = VT_HMONTH(hs) * 10000 + VT_HDAY(hs) * 100 + VT_HYEAR(hs)
+	    call imaddi (selim, "obs_date", date )
+	    call imaddi (selim, "wv_lngth", VT_HWVLNGTH(hs))
+	    call imaddi (selim, "obs_type", VT_HOBSTYPE(hs))
+	    call imaddi (selim, "av_intns", VT_HAVINTENS(hs))
+	    call imaddi (selim, "num_cols", VT_HNUMCOLS(hs))
+	    call imaddi (selim, "intg/pix", VT_HINTGPIX(hs))
+	    call imaddi (selim, "rep_time", VT_HREPTIME(hs))
+	}
+	if (bright) {
+	    britim = immap (britimage, NEW_IMAGE, 0)
+	    IM_NDIM(britim) = 2
+	    IM_LEN(britim,1) = SWTH_HIGH
+	    IM_LEN(britim,2) = VT_HNUMCOLS(hs)
+	    IM_PIXTYPE(britim) = TY_SHORT
+	    call imaddi (britim, "obs_time", VT_HTIME(hs))
+	    date = VT_HMONTH(hs) * 10000 + VT_HDAY(hs) * 100 + VT_HYEAR(hs)
+	    call imaddi (britim, "obs_date", date )
+	    call imaddi (britim, "wv_lngth", VT_HWVLNGTH(hs))
+	    call imaddi (britim, "obs_type", VT_HOBSTYPE(hs))
+	    call imaddi (britim, "av_intns", VT_HAVINTENS(hs))
+	    call imaddi (britim, "num_cols", VT_HNUMCOLS(hs))
+	    call imaddi (britim, "intg/pix", VT_HINTGPIX(hs))
+	    call imaddi (britim, "rep_time", VT_HREPTIME(hs))
+	}
+	if (velocity) {
+	    velim = immap (velimage, NEW_IMAGE, 0)
+	    IM_NDIM(velim) = 2
+	    IM_LEN(velim,1) = SWTH_HIGH
+	    IM_LEN(velim,2) = VT_HNUMCOLS(hs)
+	    IM_PIXTYPE(velim) = TY_SHORT
+	    call imaddi (velim, "obs_time", VT_HTIME(hs))
+	    date = VT_HMONTH(hs) * 10000 + VT_HDAY(hs) * 100 + VT_HYEAR(hs)
+	    call imaddi (velim, "obs_date", date )
+	    call imaddi (velim, "wv_lngth", VT_HWVLNGTH(hs))
+	    call imaddi (velim, "obs_type", VT_HOBSTYPE(hs))
+	    call imaddi (velim, "av_intns", VT_HAVINTENS(hs))
+	    call imaddi (velim, "num_cols", VT_HNUMCOLS(hs))
+	    call imaddi (velim, "intg/pix", VT_HINTGPIX(hs))
+	    call imaddi (velim, "rep_time", VT_HREPTIME(hs))
+	}
+
+	do j = 1, VT_HNUMCOLS(hs) {
+redo_	    if (select)
+	        selsrp = impl2s (selim, j)
+	    if (bright)
+	        britsrp = impl2s (britim, j)
+	    if (velocity)
+	        velsrp = impl2s (velim, j)
+
+	    iferr (num = read (inputfd, u, SWTH_HIGH*SZB_SHORT/SZB_CHAR)) {
+		call fseti (inputfd, F_VALIDATE, lrs*SZB_SHORT/SZB_CHAR)
+		call eprintf ("Error on tape read.\n")
+		num = read (inputfd, u, SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	    }
+	    lrs = num
+	    if (num < SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	        call error (0, "eof encountered when reading file")
+	    if (BYTE_SWAP2 == YES)
+	        call bswap2 (u, 1, u, 1, SWTH_HIGH * SZB_SHORT)
+	    iferr (num = read (inputfd, t, SWTH_HIGH*SZB_SHORT/SZB_CHAR)) {
+		call fseti (inputfd, F_VALIDATE, lrs*SZB_SHORT/SZB_CHAR)
+		call eprintf ("Error on tape read.\n")
+		num = read (inputfd, t, SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	    }
+	    lrs = num
+	    if (num < SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	        call error (0, "eof encountered when reading file")
+	    if (BYTE_SWAP2 == YES)
+	        call bswap2 (t, 1, t, 1, SWTH_HIGH * SZB_SHORT)
+
+	    zero = true
+	    do i = 1, SWTH_HIGH {
+		if (select)
+	            Mems[selsrp+i-1] = shifts(t[i], k)
+		if (velocity)
+	            Mems[velsrp+i-1] = shifts(u[i], k)
+	        if (bright)
+		    Mems[britsrp+i-1] = and(int(t[i]),17B)*16+and(int(u[i]),17B)
+		if (t[i] != 0)
+		    zero = false
+	    }
+	    if (zero) {
+		call eprintf ("READSS3: found a zero line in image, skip.\n")
+		goto redo_
+	    }
+	}
+
+	# Unmap images.
+	if (select)
+	    call imunmap (selim)
+	if (velocity)
+	    call imunmap (velim)
+	if (bright)
+	    call imunmap (britim)
+end
diff --git a/noao/imred/vtel/readss4.x b/noao/imred/vtel/readss4.x
new file mode 100644
index 00000000..2ab3199d
--- /dev/null
+++ b/noao/imred/vtel/readss4.x
@@ -0,0 +1,85 @@
+include <mach.h>
+include	<imhdr.h>
+include <fset.h>
+include	"vt.h"
+
+define	WDSBRSTR	50
+
+# READSS4 -- Read data file from tape or disk and format the data into
+# an IRAF image.  This is for type 4 sector scans.
+
+procedure readss4 (inputfd, filenumber, brief, select, bright, velocity, hs)
+
+int	inputfd			# file descriptor for input (usually tape)
+int	filenumber		# file number on tape
+bool	brief			# short output file names
+bool	select			# flag to make select image
+bool	bright			# flag to make bright image
+bool	velocity		# flag to make velocity image
+int	hs			# header data structure pointer
+
+pointer	im, srp
+char	imagefile[SZ_FNAME]
+int	date, hour, minute, seconds, i, j, num, lrs
+short	u[SWTH_HIGH]
+
+int	read()
+pointer	immap(), impl2s()
+errchk	immap, impl2s
+
+begin
+	# Calculate the time.  Assemble the output image name.
+	hour = int(VT_HTIME(hs)/3600)
+	minute = int((VT_HTIME(hs) - hour * 3600)/60)
+	seconds = int(VT_HTIME(hs) - hour * 3600 - minute * 60)
+	if (brief) {
+	    call sprintf (imagefile[1], SZ_FNAME, "s%03d")
+	        call pargi (filenumber)
+	} else {
+	    call sprintf (imagefile[1], SZ_FNAME, "s%02d_%02d%02d_%03d")
+	        call pargi (VT_HDAY(hs)) # day of month
+	        call pargi (hour)
+	        call pargi (minute)
+	        call pargi (filenumber)
+	}
+
+	if (select) {
+	    im = immap (imagefile, NEW_IMAGE, 0)
+	    IM_NDIM(im) = 2
+	    IM_LEN(im,1) = SWTH_HIGH
+	    IM_LEN(im,2) = VT_HNUMCOLS(hs)
+	    IM_PIXTYPE(im) = TY_SHORT
+	    call imaddi (im, "obs_time", VT_HTIME(hs))
+	    date = VT_HMONTH(hs) * 10000 + VT_HDAY(hs) * 100 + VT_HYEAR(hs)
+	    call imaddi (im, "obs_date", date )
+	    call imaddi (im, "wv_lngth", VT_HWVLNGTH(hs))
+	    call imaddi (im, "obs_type", VT_HOBSTYPE(hs))
+	    call imaddi (im, "av_intns", VT_HAVINTENS(hs))
+	    call imaddi (im, "num_cols", VT_HNUMCOLS(hs))
+	    call imaddi (im, "intg/pix", VT_HINTGPIX(hs))
+	    call imaddi (im, "rep_time", VT_HREPTIME(hs))
+	}
+
+	do j = 1, VT_HNUMCOLS(hs) {
+	    if (select)
+	        srp = impl2s (im, j)
+
+	    iferr (num = read (inputfd, u, SWTH_HIGH*SZB_SHORT/SZB_CHAR)) {
+		call fseti (inputfd, F_VALIDATE, lrs*SZB_SHORT/SZB_CHAR)
+		call eprintf ("Error on tape read.\n")
+		num = read (inputfd, u, SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	    }
+	    lrs = num
+	    if (num < SWTH_HIGH*SZB_SHORT/SZB_CHAR)
+	        call error (0, "eof encountered when reading file")
+	    if (BYTE_SWAP2 == YES)
+	        call bswap2 (u, 1, u, 1, SWTH_HIGH * SZB_SHORT)
+
+	    if (select)
+	        do i = 1, 512
+		    Mems[srp+i-1] = u[i]
+	}
+
+	if (select)
+	    call imunmap (im)
+end
diff --git a/noao/imred/vtel/readsubswath.x b/noao/imred/vtel/readsubswath.x
new file mode 100644
index 00000000..9c15bb44
--- /dev/null
+++ b/noao/imred/vtel/readsubswath.x
@@ -0,0 +1,91 @@
+include <mach.h>
+include <fset.h>
+include	"vt.h"
+
+define	SZ_VTRECFD	5120		# length, in chars, of full disk recs
+
+# READSUBSWATH -- Read data from file whose logical unit is inputfd.
+# Swap the bytes in each data word.
+
+procedure readsubswath (inputfd, selfbuf, databuf, buflength, bp)
+
+int	inputfd			# input file discriptor
+int	buflength		# length of data buffer
+bool	selfbuf			# self buffering flag
+short	databuf[buflength]	# data buffer
+pointer	bp			# buffer pointer structure pointer
+
+int	num, bleft, last_recsize
+int	read()
+errchk	read
+
+begin
+	# If we are doing our own buffering, keep track of the number
+	# of records in each file, else let mtio do it.
+
+	last_recsize = 0
+	if (selfbuf) {		# do our own buffering
+
+	    # If there is enough data still in the buffer, just copy data
+	    # to the output buffer and move the pointer, otherwise, read
+	    # the next tape record.
+
+	    if ((VT_BUFBOT(bp) - VT_BP(bp)) >= buflength) {
+		# Copy the data into the data buffer, move the pointer.
+		call amovs (Mems[VT_BP(bp)], databuf, buflength)
+		VT_BP(bp) = VT_BP(bp) + buflength
+
+	    } else {
+		# Copy leftover data from the bottom of the input buffer
+		# into the top of the input buffer, reset the flags.
+
+		bleft = VT_BUFBOT(bp) - VT_BP(bp)
+		call amovs (Mems[VT_BP(bp)], Mems[VT_BUFP(bp)], bleft)
+		VT_BP(bp) = VT_BUFP(bp) + bleft
+
+		# Read in another tape record.
+		# Check the number of chars read.  If this number is EOF or
+		# too short, error.  If it is too long, truncate to correct
+		# length.  This is done because some data tapes are written
+		# in a weird way and have some noise chars tacked on the end
+		# of each tape record.
+
+	        iferr (num = read (inputfd, Mems[VT_BP(bp)],
+		    10000*SZB_SHORT/SZB_CHAR)) {
+		    call fseti (inputfd, F_VALIDATE,
+			SZ_VTRECFD*SZB_SHORT/SZB_CHAR)
+		    call printf ("Error reading subswath.\n")
+		    num = read (inputfd, Mems[VT_BP(bp)],
+		        SZ_VTRECFD*SZB_SHORT/SZB_CHAR)
+	        }
+		if (num == EOF)
+		    call error (0, "EOF encountered on tape read")
+	        else if (num < SZ_VTRECFD*SZB_SHORT/SZB_CHAR)
+	            call error (0, "error on tape read, record too short")
+		else if (num >= SZ_VTRECFD*SZB_SHORT/SZB_CHAR &&
+		    num < (SZ_VTRECFD+300)*SZB_SHORT/SZB_CHAR)
+		    num = SZ_VTRECFD*SZB_SHORT/SZB_CHAR 
+		else
+	            call error (0, "error on tape read, record too long")
+
+		# Update the pointers, move data into the data buffer.
+		VT_BUFBOT(bp) = VT_BP(bp) + num
+		call amovs (Mems[VT_BP(bp)], databuf, buflength)
+		VT_BP(bp) = VT_BP(bp) + buflength
+	    }
+	} else {		# Let the mtio do the buffering.
+	    iferr (num = read (inputfd, databuf,
+		buflength*SZB_SHORT/SZB_CHAR)) {
+		call fseti (inputfd, F_VALIDATE,
+		    last_recsize*SZB_SHORT/SZB_CHAR)
+		call printf ("Error on tape read.\n")
+		num = read (inputfd, databuf, buflength*SZB_SHORT/SZB_CHAR)
+	    }
+	    last_recsize = num
+	    if (num < buflength*SZB_SHORT/SZB_CHAR)
+	        call error (0, "eof encountered when reading subswath")
+	}
+
+	if (BYTE_SWAP2 == YES)
+	    call bswap2 (databuf, 1, databuf, 1, buflength * SZB_SHORT)
+end
diff --git a/noao/imred/vtel/readvt.par b/noao/imred/vtel/readvt.par
new file mode 100644
index 00000000..5986a8c0
--- /dev/null
+++ b/noao/imred/vtel/readvt.par
@@ -0,0 +1,6 @@
+infile,s,q,,,,Input file descriptor
+outfile,s,q,,,,Output image file descriptor
+files,s,q,,,,Tape files to read
+verbose,b,h,no,,,Print out header data and give progress reports
+headeronly,b,h,no,,,Print out the header data and quit
+robust,b,h,no,,,Ignore wrong observation type in header
diff --git a/noao/imred/vtel/readvt.x b/noao/imred/vtel/readvt.x
new file mode 100644
index 00000000..27e34be3
--- /dev/null
+++ b/noao/imred/vtel/readvt.x
@@ -0,0 +1,347 @@
+include <mach.h>
+include	<imhdr.h>
+include	<fset.h>
+include	"vt.h"
+
+define	MAX_RANGES	100
+define	VT_TBUF		15000
+
+# READVT -- Read data from tape or disk and format the data into an IRAF image.
+# Display header information to the user as a check if the 'verbose' flag is
+# set. 
+
+procedure t_readvt()
+
+pointer	infile			# pointer to input filename(s)
+pointer	outfile			# pointer to output filename(s)
+bool	verbose			# verbose flag
+bool	headeronly		# if set, just print the header
+bool	robust			# if set, ignore wrong observation type
+pointer	files			# file list for multiple tape files
+
+int	listin			# list of input images
+int	listout			# list of output images
+bool	selfbuf, rootflag
+int	nfiles, filenumber, stat
+pointer	bp, sp, tapename, dfilename, diskfile, root
+int	filerange[2 * MAX_RANGES + 1]
+
+bool	clgetb()
+int	get_next_number(), mtneedfileno()
+int	strlen(), decode_ranges()
+int	fntopnb(), imtopenp(), clgfil(), imtgetim(), clplen(), imtlen()
+int	mtfile()
+errchk	vt_rfd
+
+begin
+	call smark (sp)
+	call salloc (infile, SZ_LINE, TY_CHAR)
+	call salloc (outfile, SZ_LINE, TY_CHAR)
+	call salloc (tapename, 2*SZ_LINE, TY_CHAR)
+	call salloc (dfilename, 2*SZ_LINE, TY_CHAR)
+	call salloc (diskfile, SZ_LINE, TY_CHAR)
+	call salloc (root, SZ_LINE, TY_CHAR)
+	call salloc (files, SZ_LINE, TY_CHAR)
+
+	call fseti (STDOUT, F_FLUSHNL, YES)
+
+	# Get parameters from the CL.
+	verbose = clgetb ("verbose")
+	headeronly = clgetb ("headeronly")
+	robust = clgetb ("robust")
+
+        call clgstr ("infile", Memc[infile], SZ_FNAME)
+
+	# Set up the buffer structure, we may need it.
+	call salloc (bp, VT_LENBSTRUCT, TY_STRUCT)
+	call salloc (VT_BUFP(bp), VT_TBUF, TY_SHORT)
+	VT_BP(bp) = VT_BUFP(bp)
+	VT_BUFBOT(bp) = VT_BUFP(bp)
+
+        if (mtfile (Memc[infile]) == NO) {
+	    # This is not a tape file, expand as a list template.
+	    listin = fntopnb (Memc[infile], 0)
+	    rootflag = FALSE
+	    filenumber = 1
+	    if (!headeronly) {
+	        listout = imtopenp ("outfile")
+
+		# Compare the lengths of the two lists.  If equal, proceed,
+		# otherwise if the outlist is of length one, use it as a root
+		# name, otherwise error.
+		
+		if (imtlen (listout) == 1) {
+		    rootflag = TRUE
+		    stat = imtgetim (listout, Memc[root], SZ_FNAME)
+		} else if (clplen (listin) != imtlen (listout)) {
+		    call clpcls (listin)
+	    	    call imtclose (listout)
+	    	    call error (1, "Wrong number of elements in operand lists")
+		}
+	    }
+
+	    while (clgfil (listin, Memc[diskfile], SZ_FNAME) != EOF) {
+	        if (!headeronly) {
+		    if (!rootflag)
+	                stat = imtgetim (listout, Memc[dfilename], SZ_FNAME)
+		    else {
+			# Assemble an output filename from the root name.
+			call sprintf (Memc[dfilename], SZ_FNAME, "%s")
+			    call pargstr (Memc[root])
+	                call sprintf (Memc[dfilename+strlen(Memc[root])],
+		            SZ_FNAME, "%03d")
+		            call pargi (filenumber)
+			filenumber = filenumber + 1
+		    }
+		}
+
+		# Of course, if the user is reading from disk, we can't
+		# check record sizes.
+
+		selfbuf = false
+		iferr (call vt_rfd (diskfile, dfilename,
+			selfbuf, verbose, headeronly, robust, bp)) {
+		    call eprintf ("Error reading file %s\n")
+		    	call pargstr (Memc[infile])
+	    	}
+	    }
+	    call clpcls (listin)
+	    if (!headeronly)
+	        call imtclose (listout)
+
+	} else if (mtneedfileno(Memc[infile]) == NO) {
+
+	    # This is a tape file and the user specified which file.
+	    if (!headeronly)
+	        call clgstr ("outfile", Memc[outfile], SZ_FNAME)
+	    selfbuf = true
+	    iferr (call vt_rfd (infile, outfile, selfbuf, verbose,
+		headeronly, robust, bp)) {
+		call eprintf ("Error reading file %s\n")
+		    call pargstr (Memc[infile])
+	    }
+
+        } else {
+
+	    # This is a tape file and the user did not specify which file.
+	    call clgstr ("files", Memc[files], SZ_LINE)
+	    if (!headeronly)
+	        call clgstr ("outfile", Memc[outfile], SZ_FNAME)
+
+	    # Set up the file names, then do the read.
+            if (decode_ranges (Memc[files], filerange, MAX_RANGES,
+		nfiles) == ERR)
+	        call error (0, "Illegal file number list.")
+
+            while (get_next_number (filerange, filenumber) != EOF) {
+	        # Assemble the appropriate tape file name.
+		call mtfname (Memc[infile], filenumber, Memc[tapename],
+		    SZ_FNAME)
+
+	        # Assemble the appropriate disk file name.
+	        if (!headeronly) {
+	            call strcpy (Memc[outfile], Memc[dfilename], SZ_FNAME)
+	            call sprintf (Memc[dfilename+strlen(Memc[outfile])],
+		        SZ_FNAME, "%03d")
+		        call pargi (filenumber)
+		}
+
+	        selfbuf = TRUE
+	        iferr (call vt_rfd (tapename, dfilename, selfbuf,
+			verbose, headeronly, robust, bp)) {
+		    call eprintf ("Error reading file %s\n")
+		        call pargstr (Memc[infile])
+	        }
+	    }
+	}
+
+	call sfree (sp)
+end
+
+
+# VT_RFD -- Do the actual read of a full disk gram.
+
+procedure vt_rfd (in, out, selfbuf, verbose, headeronly, robust, bp)
+
+pointer	in		# input file
+pointer	out		# output file
+bool	selfbuf		# do input buffering and correct for bad record lengths
+bool	verbose		# verbose flag
+bool	headeronly	# if set, just print the header
+bool	robust		# if set, ignore wrong observation type
+
+short	one
+int	date, numchars
+int	subraster, x1, y1, inputfd
+pointer	table, bp, im, srp, hs, sp, hbuf
+pointer	immap(), imps2s()
+int	mtopen(), readheader()
+errchk	readheader, loadsubswath, immap, imps2s
+define	exit_	10
+
+begin
+	call smark (sp)
+	call salloc (hbuf, SZ_VTHDR, TY_SHORT)
+	call salloc (table, SZ_TABLE, TY_SHORT)
+	call salloc (hs, VT_LENHSTRUCT, TY_STRUCT)
+
+	if (verbose) {
+	    call printf ("\nfile %s  ")
+		call pargstr (Memc[in])
+	}
+
+	# Open input file.
+	inputfd = mtopen (Memc[in], READ_ONLY, 0)
+
+	# Read header.
+	iferr (numchars = readheader (inputfd, hbuf, selfbuf))
+	    call error (0, "Error reading header information.")
+	call decodeheader (hbuf, hs, verbose)
+	if (verbose)
+	    call printf ("\n")
+
+	# Check the observation type in the header.  If this value is not
+	# zero (full disk) then write an error message, if the robust flag
+	# is set go ahead and read the file.
+
+	if (!robust) {
+	    if (VT_HOBSTYPE[hs] != 0) {
+	        call printf ("file %s is not a type zero scan (full disk)\n")
+		    call pargstr (Memc[in])
+	        call printf ("Use 'mscan' to read this type %d area scan\n")
+		    call pargi (VT_HOBSTYPE[hs])
+	        goto exit_      # close input file and exit
+	    }
+	} else {
+	    if (VT_HOBSTYPE[hs] != 0) {
+		call printf ("The header for file %s contains 'observation ")
+		    call pargstr (Memc[in])
+		call printf ("type = %d'\n")
+		    call pargi (VT_HOBSTYPE[hs])
+		call printf ("READVT expects the observation type ")
+		call printf ("to be zero.\n")
+		call printf ("This error will be ignored since the 'robust'")
+		call printf (" flag is set\n")
+	    }
+	}
+
+	if (headeronly)
+	    goto exit_      # close input file and exit
+
+	if (verbose) {
+	    call printf ("\nwriting %s\n")
+		call pargstr (Memc[out])
+	}
+
+	# Open the output image. Set it up.
+	im  = immap (Memc[out], NEW_IMAGE, 0)
+	IM_NDIM(im) = 2
+	IM_LEN(im,1) = DIM_VTFD
+	IM_LEN(im,2) = DIM_VTFD
+	IM_PIXTYPE(im) = TY_SHORT
+
+	# Set up the 8 header fields we need and store the information we
+	# obtained from the raw data image header.
+
+	call imaddi (im, "obs_time", VT_HTIME[hs])
+	date = VT_HMONTH[hs] * 10000 + VT_HDAY[hs] * 100 + VT_HYEAR[hs]
+
+	call imaddi (im, "obs_date", date )
+	call imaddi (im, "wv_lngth", VT_HWVLNGTH[hs])
+	call imaddi (im, "obs_type", VT_HOBSTYPE[hs])
+	call imaddi (im, "av_intns", VT_HAVINTENS[hs])
+	call imaddi (im, "num_cols", VT_HNUMCOLS[hs])
+	call imaddi (im, "intg/pix", VT_HINTGPIX[hs])
+	call imaddi (im, "rep_time", VT_HREPTIME[hs])
+
+	# Set up lookuptable.
+	one = 1
+	call amovks (one, Mems[table], SZ_TABLE)
+	call aclrs (Mems[table], HALF_DIF)
+	call aclrs (Mems[table + SWTHWID_14 + HALF_DIF], HALF_DIF)
+	call aclrs (Mems[table + SWTHWID_23 * 3], HALF_DIF)
+	call aclrs (Mems[table + SZ_TABLE - HALF_DIF], HALF_DIF)
+
+	# Now, fill the image with data.
+	do subraster = 1, NUM_SRSTR {
+
+	    # Calculate position of bottom left corner of this subraster
+	    x1 = ((NUM_SRSTR_X - 1) - mod((subraster - 1), NUM_SRSTR_X)) *
+		SRSTR_WID + 1
+	    y1 = ((NUM_SRSTR_Y - 1) - ((subraster - mod((subraster - 1),
+		NUM_SRSTR_Y)) / NUM_SRSTR_Y)) * SWTH_HIGH + 1
+
+	    # Get subraster.
+	    srp = imps2s (im, x1, x1+(SRSTR_WID - 1), y1, y1+(SWTH_HIGH - 1))
+
+	    # Load the subraster with data.
+	    iferr (call loadsubraster (inputfd, Mems[srp], SRSTR_WID, SWTH_HIGH,
+		Mems[table], subraster, selfbuf, bp)) {
+		call eprintf ("Error in loadsubraster, subraster = %d\n")
+		    call pargi (subraster)
+		break
+	    }
+
+	    if (verbose) {
+		call printf("%d%% ")
+		    call pargi ((subraster*100)/NUM_SRSTR)
+		call flush (STDOUT)
+	    }
+	}
+
+	if (verbose)
+	    call printf ("\n")
+
+	# Unmap image and close input file.
+	call imunmap (im)
+exit_
+	call sfree (sp)
+	call close (inputfd)
+end
+
+
+# LOADSUBRASTER -- Get data from the input and load it into this
+# subraster, look in the table to see if each subswath should be
+# filled with data or zeros.
+
+procedure loadsubraster (inputfd, array, nx, ny, table, subraster, selfbuf, bp)
+
+int	inputfd			# input file we are reading from
+short	array[nx, ny]		# array to put the data in
+int	nx			# x length of the array
+int	ny			# y length of the array
+short	table[SZ_TABLE]		# lookup table for data
+int	subraster		# subraster number are we loading
+bool	selfbuf			# buffering and record length checking?
+pointer	bp			# pointer to buffer pointer structure
+
+pointer	sp, bufpointer
+int	i, subswath, tableindex
+errchk	readsubswath
+
+begin
+	call smark (sp)
+	call salloc (bufpointer, ny, TY_SHORT)
+
+	for (subswath = nx;  subswath >= 1;  subswath = subswath - 1) {
+	    tableindex = (subraster - 1) * nx + ((nx + 1) - subswath)
+
+	    if (table[tableindex] == IS_DATA) {
+		iferr (call readsubswath (inputfd, selfbuf, Mems[bufpointer],
+			ny, bp)) {
+
+		    call eprintf ("Error in readsubswath, subswath = %d\n")
+			call pargi (subswath)
+		}
+
+		do i = ny, 1, -1
+		    array[subswath,i] = Mems[bufpointer + ny - i]
+
+	    } else {
+		do i = 1, ny 
+		    array[subswath,i] = 0
+	    }
+	}
+
+	call sfree (sp)
+end
diff --git a/noao/imred/vtel/rmap.par b/noao/imred/vtel/rmap.par
new file mode 100644
index 00000000..b8c6efd0
--- /dev/null
+++ b/noao/imred/vtel/rmap.par
@@ -0,0 +1,5 @@
+inputimage,s,q,,,,Input image
+outputimage,s,q,,,,Output data image
+outweight,s,q,,,,Weights image
+outabs,s,q,,,,Absolute value image
+histoname,s,q,,,,Histogram name
diff --git a/noao/imred/vtel/rmap.x b/noao/imred/vtel/rmap.x
new file mode 100644
index 00000000..313b03db
--- /dev/null
+++ b/noao/imred/vtel/rmap.x
@@ -0,0 +1,563 @@
+include <mach.h>
+include	<imhdr.h>
+include	"vt.h"
+include "numeric.h"
+
+define	LEN_HISTO	1025
+define	SPACING		1
+
+# RMAP -- Project a full disk solar image [2048x2048] into a square
+# image [180x180] such that lines of latitude and longitude are
+# perpendicular straight lines.
+
+procedure t_rmap()
+
+char	inputimage[SZ_FNAME]	# input image
+char	outputimage[SZ_FNAME]	# output data image
+char	outweight[SZ_FNAME]	# output weight image
+char	outabs[SZ_FNAME]	# output absolute value image
+char	histoname[SZ_FNAME]	# output histogram name
+
+real	bzero			# latitude of sub-earth point
+real	el[LEN_ELSTRUCT]	# ellipse parameters data structure
+pointer	inputim, outputim, outw, outa, sp
+pointer inim_subras_ptr, outim_subras_ptr
+pointer	outwei_subras_ptr, outav_subras_ptr
+int	outputrow, wvlngth
+int	inim_subras_bottom
+double	meanf, meanaf, zcm, muzero
+int	numpix
+bool	skip, helium
+real	tempr
+
+real	imgetr()
+int	imgeti()
+pointer	immap()
+pointer imgs2s(), imps2s(), imps2i()
+double	rmap_mode()
+errchk	immap, imgs2s, imps2s, imps2i, checkimmem, rowmap
+
+begin
+	# Get parameters from the cl.
+
+	# Image names.
+	call clgstr ("inputimage", inputimage, SZ_FNAME)
+	call clgstr ("outputimage", outputimage, SZ_FNAME)
+	call clgstr ("outweight", outweight, SZ_FNAME)
+	call clgstr ("outabs", outabs, SZ_FNAME)
+	call clgstr ("histoname", histoname, SZ_FNAME)
+
+	# Open images.
+	inputim = immap (inputimage, READ_ONLY, 0)
+	wvlngth = imgeti (inputim, "wv_lngth")
+	helium = false
+	if (wvlngth == 10830)
+	    helium = true
+	outputim = immap (outputimage, NEW_COPY, inputim)
+	outw = immap (outweight, NEW_COPY, inputim)
+	if (!helium)
+	    outa = immap (outabs, NEW_COPY, inputim)
+
+	# Compute mode estimate from the input image.
+	muzero = rmap_mode (inputim, histoname, helium)
+
+	# Define some parameters for output images.
+	IM_LEN(outputim, 1) = DIM_SQUAREIM
+	IM_LEN(outputim, 2) = DIM_SQUAREIM
+	IM_PIXTYPE(outputim) = TY_INT
+
+	IM_LEN(outw, 1) = DIM_SQUAREIM
+	IM_LEN(outw, 2) = DIM_SQUAREIM
+
+	if (!helium) {
+	    IM_LEN(outa, 1) = DIM_SQUAREIM
+	    IM_LEN(outa, 2) = DIM_SQUAREIM
+	    IM_PIXTYPE(outa) = TY_INT
+	}
+
+	# Get latitude of sub-earth point from input image header.
+	bzero = imgetr (inputim, "B_ZERO")
+
+	# Ellipse parameters.
+	E_XCENTER(el) = imgetr (inputim, "E_XCEN")
+	E_YCENTER(el) = imgetr (inputim, "E_YCEN")
+	E_XSEMIDIAMETER(el) = imgetr (inputim, "E_XSMD")
+	E_YSEMIDIAMETER(el) = imgetr (inputim, "E_YSMD")
+
+	# Remove the elipse parameters from the header records of the
+	# output images
+
+	call imdelf (outputim, "E_XCEN")
+	call imdelf (outputim, "E_YCEN")
+	call imdelf (outputim, "E_XSMD")
+	call imdelf (outputim, "E_YSMD")
+
+	call imdelf (outw, "E_XCEN")
+	call imdelf (outw, "E_YCEN")
+	call imdelf (outw, "E_XSMD")
+	call imdelf (outw, "E_YSMD")
+	call imaddb (outw, "WEIGHTS", YES)
+
+	if (!helium) {
+	    call imdelf (outa, "E_XCEN")
+	    call imdelf (outa, "E_YCEN")
+	    call imdelf (outa, "E_XSMD")
+	    call imdelf (outa, "E_YSMD")
+	    call imaddb (outa, "ABS_VALU", YES)
+	}
+
+	# Set the variable that keeps track of where in the input image the
+	# bottom of the subraster is, map in the initial subraster.
+
+	inim_subras_bottom = 1
+	inim_subras_ptr = imgs2s (inputim, 1, DIM_VTFD, inim_subras_bottom,
+	    inim_subras_bottom+DIM_IN_RAS-1)
+
+	# Map the outputimages into memory.
+	outim_subras_ptr = imps2i (outputim, 1, DIM_SQUAREIM, 1, DIM_SQUAREIM)
+	outwei_subras_ptr = imps2s (outw, 1, DIM_SQUAREIM, 1, DIM_SQUAREIM)
+	if (!helium)
+	    outav_subras_ptr = imps2i (outa, 1, DIM_SQUAREIM, 1, DIM_SQUAREIM)
+	else {
+	    call smark (sp)
+	    call salloc (outav_subras_ptr, DIM_SQUAREIM*DIM_SQUAREIM, TY_INT)
+	}
+
+	# Initialize meanf, meanaf, numpix.
+	meanf = 0.0
+	meanaf = 0.0
+	numpix = 0
+
+	# Map the input image into the output image by output image rows.
+	do outputrow = 1, DIM_SQUAREIM {
+
+	    # Check the current input subraster to see if it covers
+	    # the next output row to be mapped and map in a new subraster
+	    # if necessary.
+
+	    call checkimmem (inim_subras_bottom, bzero, inputim, outputrow,
+	        inim_subras_ptr, el, skip)
+
+	    # If checkimmem returns skip = true then this row is not contained
+	    # in the input image so fill it with zeros and skip it.
+
+	    if (skip) {
+		# Fill the empty row with zeros.
+		call emptyrow (outputrow, Memi[outim_subras_ptr],
+		    Mems[outwei_subras_ptr], Memi[outav_subras_ptr])
+		next
+	    }
+
+	    # Map this pixel row.
+	    call rowmap (inim_subras_bottom, Mems[inim_subras_ptr], bzero,
+		outputrow, Memi[outim_subras_ptr], Mems[outwei_subras_ptr],
+		Memi[outav_subras_ptr], el, muzero, meanf, meanaf, numpix,
+		helium)
+	}
+
+	# Put the mean field, the number of pixels, the zero corrected mean
+	# absolute field, the mode estimate, the zero corrected mean field,
+	# and the standard deviation in the output image header.
+
+	meanaf = meanaf/double(numpix)
+	meanf = meanf/double(numpix)
+	zcm = meanf - muzero
+	tempr = real(meanf)
+	call imaddr (outputim, "MEAN_FLD", tempr)
+	call imaddi (outputim, "NUMPIX", numpix)
+	if (!helium) {
+	    tempr = real(meanaf)
+	    call imaddr (outputim, "MEANAFLD", tempr)
+	    tempr = real(muzero)
+	    call imaddr (outputim, "MUZERO", tempr)
+	    tempr = real(zcm)
+	    call imaddr (outputim, "ZCM", tempr)
+	}
+
+	# Close images.
+	call imunmap (inputim)
+	call imunmap (outputim)
+	call imunmap (outw)
+	if (!helium)
+	    call imunmap (outa)
+	if (helium)
+	    call sfree (sp)
+end
+
+
+# CHECKIMMEM -- Check this row to see if the input subraster in memory
+# covers it and if it doesn't, map in a new subraster.
+
+procedure checkimmem (inim_subras_bottom, bzero, inputim, outputrow,
+	inim_subras_ptr, el, skip)
+
+int	inim_subras_bottom	# current bottom of the loaded subraster
+real	bzero			# latitude of sub-earth point for this image
+pointer	inputim			# pointer to input image
+int	outputrow		# which output row to map
+pointer	inim_subras_ptr		# input image subraster pointer
+real	el[LEN_ELSTRUCT]	# ellipse parameters data structure
+bool	skip			# returned flag saying to skip this line
+
+real	x ,y
+int	ymax, ymin
+real	uplat, downlat, lminusl0, latitude
+pointer	imgs2s()
+errchk	imgs2s
+
+begin
+	skip = false
+
+	# Find values for the latitudes of the upper and lower edges of this
+	# pixel row.
+
+	uplat = 180./3.1415926*asin(float(outputrow - 90)/90.)
+	downlat = 180./3.1415926*asin(float(outputrow - 91)/90.)
+
+	# Check to see if this row is either completely off the image or
+	# partially off the image.  If it is off the image then return
+	# skip = true.  If it is partially off the image then truncate
+	# the appropriate boundary latitude at the image boundary.
+
+	if (bzero > 0) {
+	    if ( downlat < (-90 + bzero) && uplat < (-90 + bzero)) {
+
+		# This row is not on the image.
+		skip = true
+		return
+	    }
+	    if (downlat < (-90 + bzero))
+		downlat = -90 + bzero
+	} else {
+	    if ( downlat > (90 - bzero) && uplat > (90 - bzero)) {
+
+		# This row is not on the image.
+		skip = true
+		return
+	    }
+	    if (uplat > (90 - bzero))
+		uplat = 90 - bzero
+	}
+
+	# Calculate the minimum and maximum values of y in the input image that
+	# we will need to map this output row of pixels and check these
+	# values against the value of the current bottom of the subraster.
+
+	if (bzero > 0) {
+
+	    # Calculate y position in image.
+	    lminusl0 = 90.
+	    latitude = uplat
+	    call getxy (latitude, lminusl0, bzero, el, x, y, skip)
+	    ymax = int(y + .5)
+	    lminusl0 = -90.
+	    latitude = uplat
+	    call getxy (latitude, lminusl0, bzero, el, x, y, skip)
+	    if (int(y + .5) > ymax)
+		ymax = int(y + .5)
+
+	    # Calculate min y position.
+	    lminusl0 = 0.
+	    latitude = downlat
+	    call getxy (latitude, lminusl0, bzero, el, x, y, skip)
+	    ymin = int(y + .5)
+
+	} else {
+
+	    # Calculate y position in image.
+	    lminusl0 = 90.
+	    latitude = downlat
+	    call getxy (latitude, lminusl0, bzero, el, x, y, skip)
+	    ymin = int(y + .5)
+	    lminusl0 = -90.
+	    latitude = downlat
+	    call getxy (latitude, lminusl0, bzero, el, x, y, skip)
+	    if (int(y + .5) < ymin) ymin = int(y + .5)
+
+	    # Calculate max y position.
+	    lminusl0 = 0.
+	    latitude = uplat
+	    call getxy (latitude, lminusl0, bzero, el, x, y, skip)
+	    ymax = int(y + .5)
+	}
+
+	# If ymin or ymax is outside the current subraster, then map in
+	# an appropriate subraster.
+
+	if ((ymin < (inim_subras_bottom + 5)) ||
+	    (ymax > (inim_subras_bottom + 140))) {
+	    if ((ymax - ymin) > 150) {
+		call printf ("Subraster too small(ymax-ymin > 150), bye")
+	    }
+	    if ((ymin +  144) > 2048) {
+		ymin = 2048 - 144
+	    }
+	    if ((ymin - 5) < 1) {
+		skip = true
+		return
+	    }
+	    inim_subras_ptr = imgs2s (inputim, 1, DIM_VTFD, (ymin - 5),
+		(ymin + 144))
+	    inim_subras_bottom = ymin - 5
+	}
+end
+
+
+# ROWMAP -- Map this output row pixel by pixel.
+
+procedure rowmap (inim_subras_bottom, in_subraster, bzero, outputrow,
+	out_subraster, outw_subraster, outa_subraster, el, muzero, meanf,
+	meanaf, numpix helium)
+
+real	bzero						# lat of sub-earth
+real	el[LEN_ELSTRUCT]		# ellipse parameters data structure
+int	inim_subras_bottom				# bottom of current
+int	outputrow					# output row
+short	in_subraster[DIM_VTFD, DIM_IN_RAS]		# subraster
+int	out_subraster[DIM_SQUAREIM, DIM_SQUAREIM]	# output image
+short	outw_subraster[DIM_SQUAREIM, DIM_SQUAREIM]	# output weights
+int	outa_subraster[DIM_SQUAREIM, DIM_SQUAREIM]	# output abs. value
+double	muzero						# mode estimate
+double	meanf						# mean field
+double	meanaf						# mean absolute field
+int	numpix						# number of pixels
+bool	helium						# 10830 flag
+
+int	pixel
+
+errchk	pixelmap
+
+begin
+	# Do all 180 pixels in this output row.
+	do pixel = 1,180 {
+	    call pixelmap (pixel, in_subraster, inim_subras_bottom,
+		bzero, outputrow, out_subraster, outw_subraster, outa_subraster,
+		el, muzero, meanf, meanaf, numpix, helium)
+	}
+end
+
+
+# PIXELMAP -- Sum up and count the input pixels contained inside the
+# given output pixel.  The sum is carried out in the following way:
+#
+# Calculate, on the input image, the position of the center of the
+#    output pixel to be mapped.
+# Calculate the values of the partial derivitives of latitude and
+#    longitude with respect to x and y.
+# Calculate the boundaries of the pixel in the input image and
+#    sum and count all the pixels inside, assign the value
+#    to the output pixel = sum/count.
+
+procedure pixelmap (pixel, in_subraster, inim_subras_bottom,
+	bzero, outputrow, out_subraster, outw_subraster, outa_subraster,
+	el, muzero, meanf, meanaf, numpix, helium)
+
+int	pixel						# which pixel
+short	in_subraster[DIM_VTFD, DIM_IN_RAS]		# subraster
+int	inim_subras_bottom				# bottom of current
+real	bzero						# lat of sub-earth
+int	outputrow					# output row
+int	out_subraster[DIM_SQUAREIM, DIM_SQUAREIM]	# output image
+short	outw_subraster[DIM_SQUAREIM, DIM_SQUAREIM]	# output weights
+int	outa_subraster[DIM_SQUAREIM, DIM_SQUAREIM]	# output abs. value
+real	el[LEN_ELSTRUCT]		# ellipse parameters data structure
+double	muzero						# mode estimate
+double	meanf						# first moment accum.
+double	meanaf						# mean absolute field
+int	numpix						# number of pixels
+bool	helium						# helium flag
+
+real	lat_mid, long_mid, lat_bot, lat_top
+real	long_rite, long_left
+double	sum, sumabs
+int	count
+real	xpixcenter, ypixcenter
+real	dlongdx, dlatdy
+int	xleft,xright,ybottom,ytop,x,y
+int	num_pix_vert, num_pix_horz
+pointer	sp
+pointer	num					# numeric structure pointer
+real	dat
+
+begin
+	call smark (sp)
+	call salloc (num, VT_LENNUMSTRUCT, TY_STRUCT)
+
+	# First obtain the parameters necessary from numeric.
+	call numeric (bzero, el, outputrow, pixel, xpixcenter, ypixcenter, num)
+
+	dlongdx = VT_DLODX(num)
+	dlatdy = VT_DLATDY(num)
+	lat_top = VT_LATTOP(num)
+	lat_bot = VT_LATBOT(num)
+	long_left = VT_LOLEFT(num)
+	long_rite = VT_LORITE(num)
+	lat_mid = VT_LATMID(num)
+	long_mid = VT_LOMID(num)
+
+	if (lat_top == 10000.) {
+	    out_subraster[pixel,outputrow] = 0
+	    outw_subraster[pixel,outputrow] = 0
+	    outa_subraster[pixel,outputrow] = 0
+	    call sfree (sp)
+	    return
+	}
+
+	# Calculate the box of pixels we want.
+	num_pix_horz = int((1.0 / dlongdx) + .5)
+	xleft = xpixcenter - int((.5 / dlongdx) + .5)
+	xright = xleft + num_pix_horz - 1
+	num_pix_vert = int((abs(abs(lat_top) - abs(lat_bot)) / dlatdy) + .5)
+	ybottom = ypixcenter - int(((abs(abs(lat_mid) - abs(lat_bot))) /
+	    dlatdy) + .5) - (inim_subras_bottom - 1)
+	ytop = ybottom + num_pix_vert - 1
+	
+	# Sum up the pixels inside this box.
+	count = 0
+	sum = 0.0
+	sumabs = 0.0
+
+	do x = xleft, xright {
+	    do y = ybottom, ytop {
+		if (and(int(in_subraster[x,y]),17B) >= THRESHOLD+1) {
+		    count = count + 1
+
+		    # Divide by 16 to remove squibby brightness
+		    # Accumulate the various moment data.
+		    dat = real(in_subraster[x,y]/16)
+		    sum = sum + double(dat)
+		    sumabs = sumabs + double(abs(dat - muzero))
+		}
+	    }
+	}
+
+	outw_subraster[pixel,outputrow] = short(count)
+	out_subraster[pixel,outputrow] = int(sum - double(count*muzero) + .5)
+	if (!helium)
+	    outa_subraster[pixel,outputrow] = int(sumabs + .5)
+	meanf = meanf + sum
+	meanaf = meanaf + sumabs
+	numpix = numpix + count
+
+	call sfree (sp)
+end
+
+
+# EMPTYROW -- Set this row in the output image to zero.
+
+procedure emptyrow (outputrow, out_subraster, outw_subraster, outa_subraster)
+
+int	outputrow
+int	out_subraster[DIM_SQUAREIM, DIM_SQUAREIM]
+short	outw_subraster[DIM_SQUAREIM, DIM_SQUAREIM]
+int	outa_subraster[DIM_SQUAREIM, DIM_SQUAREIM]
+
+int	pixel
+
+begin
+	# Do all 180 pixels in this output row.
+	do pixel = 1,180 {
+	    out_subraster[pixel, outputrow] = 0
+	    outw_subraster[pixel, outputrow] = 0
+	    outa_subraster[pixel, outputrow] = 0
+	}
+end
+
+
+double procedure rmap_mode (inputim, histoname, helium)
+
+pointer	inputim			# Input image
+char	histoname[SZ_FNAME]	# Histogram name
+bool	helium
+
+int	count, i, j
+int	dati, hist_middle
+pointer	imline, histim, hiptr
+int	histo[LEN_HISTO]
+
+# Stuff for mrqmin.
+real    a[3], x[LEN_HISTO], y[LEN_HISTO], sig[LEN_HISTO]
+int     lista[3]
+real    alambda, chisq, covar[3,3], alpha[3,3]
+short	k
+
+pointer	imgl2s(), impl1i(), immap()
+short	shifts()
+
+extern	gauss
+
+begin
+	# Initialize.
+	count = 0
+	k = -4
+	do i = 1, LEN_HISTO
+	    histo[i] = 0
+
+	do i = 1, DIM_VTFD, SPACING{
+	    imline = imgl2s (inputim, i)
+	    do j = 1, DIM_VTFD, SPACING {
+		if (and(int(Mems[imline+j-1]),17B) >= THRESHOLD+1) {
+		    count = count + 1
+		    dati = shifts(Mems[imline+j-1], k)
+
+		    # Put the data into a histogram.
+		    hist_middle = (LEN_HISTO-1)/2 + 1
+		    if (abs(dati) <= hist_middle-1)
+			histo[dati+hist_middle] = histo[dati+hist_middle] + 1
+		}
+	    }
+	}
+
+	# Write this histogram out to an image.
+	histim = immap (histoname, NEW_COPY, inputim)
+	IM_NDIM(histim) = 1
+	IM_LEN(histim, 1) = LEN_HISTO
+	IM_PIXTYPE(histim) = TY_INT
+	hiptr = impl1i (histim)
+
+	# Put the histogram into this image.
+	do i = 1, LEN_HISTO
+	    Memi[hiptr+i-1] = histo[i]
+
+	if (!helium) {
+	    # Set up arrays, etc. for gaussian fit.
+	    a[2] = 1.0
+	    a[1] = real(histo[1])
+	    do i = 1, LEN_HISTO {
+	        x[i] = real(i)
+	        y[i] = real(histo[i])
+	        sig[i] = 1.0
+	        if (histo[i] > a[1]) {
+		    a[1] = real(histo[i])
+		    a[2] = real(i)
+	        }
+	    }
+	    a[3] = 15.0
+
+	    do i = 1, 3
+	        lista[i] = i
+
+	    # Fit the gaussian.
+	    alambda = -1.0
+	    call mrqmin (x, y, sig, LEN_HISTO, a, 3, lista, 3, covar, alpha, 3,
+	        chisq, gauss, alambda)
+	    do i = 1, 10 {
+	        call mrqmin (x, y, sig, LEN_HISTO, a, 3, lista, 3, covar,
+		    alpha, 3, chisq, gauss, alambda)
+	    }
+
+	    call imaddr (histim, "GSS_AMPL", a[1])
+	    call imaddr (histim, "GSS_CNTR", a[2])
+	    call imaddr (histim, "GSS_WDTH", a[3])
+
+	    # Put the mode estimate in the header.
+	    call imaddr (histim, "MUZERO", (a[2] - real(hist_middle)))
+	}
+
+	call imunmap (histim)
+
+	if (helium)
+	    return (0.0)
+	else
+	    return (double(a[2] - real(hist_middle)))
+end
diff --git a/noao/imred/vtel/syndico.h b/noao/imred/vtel/syndico.h
new file mode 100644
index 00000000..d7693057
--- /dev/null
+++ b/noao/imred/vtel/syndico.h
@@ -0,0 +1,13 @@
+# coordinates of center of picture.
+define DICO_XCENTER	.505
+define DICO_YCENTER	.500
+
+# The number of dicomed pixels it takes to make 18 centimeters on a 
+# standard dicomed plot.
+define DICO_18CM	2436.0
+
+# coordinates of greyscale box
+define IMGBL_X	.245
+define IMGBL_Y	.867
+define IMGTR_X	.765
+define IMGTR_Y	.902
diff --git a/noao/imred/vtel/syndico.par b/noao/imred/vtel/syndico.par
new file mode 100644
index 00000000..b36d0624
--- /dev/null
+++ b/noao/imred/vtel/syndico.par
@@ -0,0 +1,14 @@
+image,s,a,,,,input image
+logofile,s,h,iraf$noao/imred/vtel/nsolcrypt.dat,,,logo file
+device,s,h,dicomed,,,plot device
+sbthresh,i,h,2,,,squibby brightness threshold
+plotlogo,b,h,yes,,,plot the logo on the image?
+verbose,b,h,no,,,give progress reports?
+forcetype,b,h,no,,,force the data type?
+magnetic,b,h,yes,,,if forcing datatype is it magnetic else 10830
+month,i,q,,,,month the observation was made
+day,i,q,,,,day the observation was made
+year,i,q,,,,year the observation was made
+hour,i,q,,,,hour the observation was made
+minute,i,q,,,,minute the observation was made
+second,i,q,,,,second the observation was made
diff --git a/noao/imred/vtel/syndico.x b/noao/imred/vtel/syndico.x
new file mode 100644
index 00000000..64910679
--- /dev/null
+++ b/noao/imred/vtel/syndico.x
@@ -0,0 +1,416 @@
+include <mach.h>
+include <imhdr.h>
+include <imset.h>
+include <gset.h>
+include "syndico.h"
+include "vt.h"
+
+# SYNDICO -- Make Dicomed prints of synoptic images.  This program is tuned
+# to make the images 18 centimeters in diameter.
+
+procedure t_syndico()
+
+char	image[SZ_FNAME]				# image to plot
+char	logofile[SZ_FNAME]			# file containing logo
+char	device[SZ_FNAME]			# plot device
+int	sbthresh				# squibby brightness threshold
+bool	verbose					# verbose flag
+bool	plotlogo				# plotlogo flag
+bool	forcetype				# force image type flag
+bool	magnetic				# image type = magnetic flag
+
+int	obsdate, wavelength, obstime
+int	i, j, month, day, year, hour, minute, second, stat, bufptr
+real	delta_gblock, x, y
+real	excen, eycen, exsmd, eysmd, rguess
+real	b0, l0
+real	mapy1, mapy2, radius, scale, diskfrac
+char	ltext[SZ_LINE]
+char	system_id[SZ_LINE]
+
+short	grey[16]
+pointer	gp, sp, im, lf
+pointer	subrasp, subras1, buff
+int	trnsfrm[513]
+int	lkup10830[1091]
+int	gs10830[16]
+real	xstart, xend, ystart, yend, yinc
+real	xcenerr, ycenerr, ndc_xcerr, ndc_ycerr
+real	temp_xcenter, temp_ycenter
+
+pointer	immap(), gopen(), imgl2s()
+int	imgeti(), clgeti(), open(), read()
+real	imgetr()
+bool	clgetb(), imaccf()
+include	"trnsfrm.inc"
+errchk	gopen, immap, sysid, imgs2s, imgl2s
+
+# Grey scale points for 10830.
+data (gs10830[i], i = 1, 6) /-1000,-700,-500,-400,-300,-250/
+data (gs10830[i], i = 7, 10) /-200,-150,-100,-50/
+data (gs10830[i], i = 11, 16) /0,10,20,40,60,90/
+
+begin
+	call smark (sp)
+	call salloc (subrasp, DIM_VTFD, TY_SHORT)
+	call salloc (subras1, 185*185, TY_SHORT)
+	call salloc (buff, 185, TY_CHAR)
+
+	# Get parameters from the cl.
+	call clgstr ("image", image, SZ_FNAME)
+	call clgstr ("logofile", logofile, SZ_FNAME)
+	call clgstr ("device", device, SZ_FNAME)
+	sbthresh = clgeti ("sbthresh")
+	plotlogo = clgetb ("plotlogo")
+	verbose = clgetb ("verbose")
+	forcetype = clgetb ("forcetype")
+	magnetic = clgetb ("magnetic")
+
+	# Open the input image, open the logo image if requested.
+	im = immap (image, READ_ONLY, 0)
+	if (plotlogo)
+	    iferr {
+	        lf = open (logofile, READ_ONLY, TEXT_FILE)
+	    } then {
+		call eprintf ("Error opening the logo file, logo not made.\n")
+		plotlogo = false
+	    }
+
+	# Get/calculate some of the housekeeping data.
+	if (imaccf (im, "obs_date")) {
+	    obsdate = imgeti (im, "obs_date")
+	    obstime = imgeti (im, "obs_time")
+	    month = obsdate/10000
+	    day = obsdate/100 - 100 * (obsdate/10000)
+	    year = obsdate - 100 * (obsdate/100)
+	    hour = int(obstime/3600)
+	    minute = int((obstime - hour * 3600)/60)
+	    second = obstime - hour * 3600 - minute * 60
+	} else {
+	    # Use cl query parameters to get these values.
+	    call eprintf ("Date and Time not found in image header.\n")
+	    call eprintf ("Please enter them below.\n")
+	    month = clgeti ("month")
+	    day = clgeti ("day")
+	    year = clgeti ("year")
+	    hour = clgeti ("hour")
+	    minute = clgeti ("minute")
+	    second = clgeti ("second")
+	}
+
+	# Get the solar image center and radius from the image header,
+	# get the solar image radius from the ephemeris routine.  If 
+	# the two radii are similar, use the former one, if they are
+	# %10 percent or more different, use the ephemeris radius and
+	# assume the center is at (1024,1024).
+
+	# Get ellipse parameters from image header.
+	# If they are not there, warn the user that we are using ephemeris
+	# values.
+	if (imaccf (im, "E_XCEN")) {
+	    excen =  imgetr (im, "E_XCEN")
+	    eycen =  imgetr (im, "E_YCEN")
+	    exsmd =  imgetr (im, "E_XSMD")
+	    eysmd =  imgetr (im, "E_YSMD")
+
+	    # Get rguess from ephem.
+	    iferr (call ephem (month, day, year, hour, minute, second, rguess,
+	        b0, l0, false))
+	        call eprintf ("Error getting ephemeris data.\n")
+
+	    radius = (exsmd + eysmd) / 2.0
+	    if (abs(abs(radius-rguess)/rguess - 1.0) > 0.1) {
+	        radius = rguess
+	        excen = 1024.0
+	        eycen = 1024.0
+	    }
+
+	} else {
+	    call eprintf ("No ellipse parameters in image header.\n Using")
+	    call eprintf (" ephemeris value for radius and setting center to")
+	    call eprintf (" 1024, 1024\n")
+
+	    # Get rguess from ephem.
+	    iferr (call ephem (month, day, year, hour, minute, second, rguess,
+	        b0, l0, false))
+	        call eprintf ("Error getting ephemeris data.\n")
+
+	    radius = rguess
+	    excen = 1024.0
+	    eycen = 1024.0
+	}
+
+	# Error in center. (units of pixels)
+	xcenerr = excen - 1024.0
+	ycenerr = eycen - 1024.0
+
+	# Transform error to NDC.
+	ndc_xcerr = xcenerr * (1.0/4096.0)
+	ndc_ycerr = ycenerr * (1.0/4096.0)
+
+	# Next, knowing that the image diameter must be 18 centimeters,
+	# calculate the scaling factor we must use to expand the image.
+	# DICO_18CM is a MAGIC number = 18 centimeters on dicomed prints
+	# given the way the NOAO photo lab currently enlarges the images.
+	scale = DICO_18CM / real(radius*2)
+
+	# Open the output file.
+	gp = gopen (device, NEW_FILE, STDGRAPH)
+
+	# Put feducial(sp?) marks on plot.
+	diskfrac = radius/1024.0
+	temp_xcenter = DICO_XCENTER-ndc_xcerr
+	temp_ycenter = DICO_YCENTER-ndc_ycerr
+	call gline (gp, temp_xcenter, temp_ycenter+diskfrac*.25*scale+.01,
+	    temp_xcenter, temp_ycenter+diskfrac*.25*scale+.025)
+	call gline (gp, temp_xcenter, temp_ycenter-diskfrac*.25*scale-.01,
+	    temp_xcenter, temp_ycenter-diskfrac*.25*scale-.025)
+	
+	# Draw a little compass on the plot.
+	call gline (gp, .25, DICO_YCENTER+.25+.01,
+	    .25, DICO_YCENTER+.25+.035)
+	call gtext (gp, .25, DICO_YCENTER+.25+.037,
+	    "N", "v=b;h=c;s=.50")
+	call gmark (gp, .2565, DICO_YCENTER+.25+.037,
+	    GM_CIRCLE, .006, .006)
+	call gmark (gp, .2565, DICO_YCENTER+.25+.037,
+	    GM_CIRCLE, .001, .001)
+	call gline (gp, .25, DICO_YCENTER+.25+.01,
+	    .28, DICO_YCENTER+.25+.01)
+	call gtext (gp, .282, DICO_YCENTER+.25+.01,
+	    "W", "v=c;h=l;s=.50")
+	call gmark (gp, .290, DICO_YCENTER+.25+.01-.006,
+	    GM_CIRCLE, .006, .006)
+	call gmark (gp, .290, DICO_YCENTER+.25+.01-.006,
+	    GM_CIRCLE, .001, .001)
+
+	# Get the wavelength from the image header.  If the user wants
+	# to force the wavelength, do so.  (this is used if the header
+	# information about wavelength is wrong.)
+	wavelength = imgeti (im, "wv_lngth")
+	if (forcetype)
+	    if (magnetic)
+		wavelength = 8688
+	    else
+		wavelength = 10830
+
+	# Write the grey scale labels onto the plot.
+	delta_gblock = (IMGTR_X - IMGBL_X)/16.
+	y = IMGBL_Y - .005
+	do i = 1, 16 {
+	    x = IMGBL_X + real(i-1) * delta_gblock + delta_gblock/2.
+	    call sprintf (ltext, SZ_LINE, "%d")
+	    if (wavelength == 8688)
+		call pargi ((i-1)*(int((512./15.)+0.5))-256)
+	    else if (wavelength == 10830)
+		call pargi (gs10830(i))
+	    call gtext (gp, x, y, ltext, "v=t;h=c;s=.20")
+	}
+
+	# Label on grey scale.
+	call sprintf (ltext, SZ_LINE, "%s")
+	if (wavelength == 8688)
+	    call pargstr ("gauss")
+	else if (wavelength == 10830)
+	    call pargstr ("relative line strength")
+        call gtext (gp, DICO_XCENTER, (IMGBL_Y-.024), ltext, "v=c;h=c;s=.5")
+
+	# Put the title on.
+	call sprintf (ltext, SZ_LINE, "%s")
+	if (wavelength == 8688)
+	    call pargstr ("8688 MAGNETOGRAM")
+	else if (wavelength == 10830)
+	    call pargstr ("10830 SPECTROHELIOGRAM")
+	else
+	    call pargstr (" ")
+	call gtext (gp, DICO_XCENTER, .135, ltext, "v=c;h=c;s=.7")
+
+	# If we don't have a logo to plot, write the data origin on the plot.
+	if (!plotlogo) {
+
+	    call sprintf (ltext, SZ_LINE, "%s")
+	        call pargstr ("National")
+	    call gtext (gp, .24, .155, ltext, "v=c;h=c;s=.7")
+	    call sprintf (ltext, SZ_LINE, "%s")
+	        call pargstr ("Solar")
+	    call gtext (gp, .24, .135, ltext, "v=c;h=c;s=.7")
+	    call sprintf (ltext, SZ_LINE, "%s")
+	        call pargstr ("Observatory")
+	    call gtext (gp, .24, .115, ltext, "v=c;h=c;s=.7")
+	}
+
+	# Put month/day/year on plot.
+	call sprintf (ltext, SZ_LINE, "%02d/%02d/%02d")
+	    call pargi (month)
+	    call pargi (day)
+	    call pargi (year)
+	call gtext (gp, .70, .175, ltext, "v=c;h=l;s=.5")
+
+	# Put the hour:minute:second on plot.
+	call sprintf (ltext, SZ_LINE, "%02d:%02d:%02d UT")
+	    call pargi (hour)
+	    call pargi (minute)
+	    call pargi (second)
+	call gtext (gp, .70, .155, ltext, "v=c;h=l;s=.5")
+
+	# Fill in the grey scale.
+	if (wavelength == 8688) {
+	    do i = 1, 16
+	        grey[i] = (trnsfrm[(i-1)*(int((512./15.)+0.5))+1])
+	    call gpcell (gp, grey, 16, 1, IMGBL_X, IMGBL_Y, IMGTR_X, IMGTR_Y)
+	} else if (wavelength == 10830) {
+	    do i = 1, 16
+	        grey[i] = (lkup10830[gs10830(i)+1001])
+	    call gpcell (gp, grey, 16, 1, IMGBL_X, IMGBL_Y, IMGTR_X, IMGTR_Y)
+	}
+
+	# Prepare some constants for plotting.
+	xstart = temp_xcenter - .25 * scale
+	xend = temp_xcenter + .25 * scale
+	ystart = temp_ycenter - .25 * scale
+	yend = temp_ycenter + .5 * scale
+	mapy1 = ystart
+	mapy2 = ystart
+	yinc = (.5*scale)/real(DIM_VTFD)
+	
+	# Put the data on the plot. Line by line.
+	do i = 1, DIM_VTFD {
+
+	    if (verbose) {
+		call printf ("line = %d\n")
+		    call pargi (i)
+		call flush (STDOUT)
+	    }
+	
+	    subrasp = imgl2s (im, i)
+
+	    # Call the limb trimmer and data divider.
+	    call fixline (Mems[subrasp], DIM_VTFD, wavelength, sbthresh)
+
+	    # Update the top and bottom edges of this line.
+	    mapy1 = mapy2
+	    mapy2 = mapy2 + yinc
+
+	    # Put the line on the output plot.
+	    call gpcell (gp, Mems[subrasp], DIM_VTFD, 1, xstart,
+		mapy1, xend, mapy2)
+
+	} # End of do loop on image lines.
+
+	# Put the system identification on the plot.
+	call sysid (system_id, SZ_LINE)
+	call gtext (gp, DICO_XCENTER, .076, system_id, "h=c;s=0.45")
+
+	# Put the NSO logo on the plot.
+	if (plotlogo) {
+
+	    # Read in the image. (the image is encoded in a text file)
+	    do i = 1, 185 {
+	        bufptr = 0
+	        while (bufptr < 185-79) {
+	            stat = read (lf, Memc[buff+bufptr], 80)
+		    bufptr = bufptr + 79
+	        }
+	        stat = read (lf, Memc[buff+bufptr], 80)
+	        do j = 1, 185 {
+		    Mems[subras1+(i-1)*185+j-1] =
+			short((Memc[buff+j-1]-32.)*2.7027027)
+		}
+	    }
+
+	    # Put it on the plot.
+	    call gpcell (gp, Mems[subras1], 185, 185, .24, .13, .32, .21)
+	}
+
+	# Close the graphics pointer, unmap images, free stack.
+	call gclose (gp)
+	call imunmap (im)
+	if (plotlogo)
+	    call close (lf)
+	call sfree (sp)
+end
+
+
+# FIXLINE -- Clean up the line.  Set the value of pixels off the limb to
+# zero, remove the squibby brightness from each pixel, and apply a
+# nonlinear lookup table to the greyscale mapping.
+
+procedure fixline (ln, xlength, wavelength, sbthresh)
+
+int	xlength			# length of line buffer
+short	ln[xlength]		# line buffer
+int	wavelength		# wavelength of the observation
+int	sbthresh		# squibby brightness threshold
+
+int	trnsfrm[513]
+int	lkup10830[1091]
+bool	found
+int	i, left, right
+include	"trnsfrm.inc"
+
+begin
+	# Look in from the left end till squibby brightness goes above the
+	# threshold, remember where this limbpoint is.
+	found = false
+	do i = 1, xlength {		# Find left limbpoint.
+	    if (and(int(ln[i]),17B) > sbthresh) {
+		found = true
+		left = i
+		break
+	    }
+	}
+
+	if (found) {
+	    # Find the right limbpoint.
+	    do i = xlength, 1, -1 {
+	        if (and(int(ln[i]),17B) > sbthresh) {
+		    right = i
+		    break
+	        }
+	    }
+
+	    # Divide the image by 16, map the greyscale, and trim the limb.
+	    do i = left+1, right-1 {
+
+		# Remove squibby brightness.
+		ln[i] = ln[i]/16
+
+		if (wavelength == 8688) {
+		    # Magnetogram, nonlinear greyscale.
+		    # Make data fit in the table.
+		    if (ln[i] < -256)
+		        ln[i] = -256
+		    if (ln[i] > 256)
+		        ln[i] = 256
+
+		    # Look it up in the table.
+		    ln[i] = trnsfrm[ln[i]+257]
+		} else if (wavelength == 10830) {
+		    # 10830 spectroheliogram, nonlinear greyscale.
+		    # Make data fit in the table.
+		    if (ln[i] < -1000)
+		        ln[i] = -1000
+		    if (ln[i] > 90)
+		        ln[i] = 90
+		    # Look it up in the table.
+		    ln[i] = lkup10830[ln[i]+1001]
+		} else {
+		    # Unknown type, linear greyscale.
+		    if (ln[i] < 1)
+		        ln[i] = 1
+		    if (ln[i] > 255)
+		        ln[i] = 255
+		}
+	    }
+
+	    # Set stuff outside the limb to zero.
+	    do i = 1, left
+		ln[i] = 0
+	    do i = right, xlength
+		ln[i] = 0
+	} else {
+	    # This line is off the limb, set it to zero.
+	    do i = 1, xlength
+		ln[i] = 0
+        }
+end
diff --git a/noao/imred/vtel/tcopy.par b/noao/imred/vtel/tcopy.par
new file mode 100644
index 00000000..4facf827
--- /dev/null
+++ b/noao/imred/vtel/tcopy.par
@@ -0,0 +1,5 @@
+inputfile,s,q,,,,Input file descriptor
+files,s,q,,,,List of files to be examined
+outputfile,s,q,,,,Output file descriptor
+new_tape,b,q,,,,Are you using a new tape?
+verbose,b,h,no,,,Print out header data and give progress reports
diff --git a/noao/imred/vtel/tcopy.x b/noao/imred/vtel/tcopy.x
new file mode 100644
index 00000000..42709563
--- /dev/null
+++ b/noao/imred/vtel/tcopy.x
@@ -0,0 +1,190 @@
+include <error.h>
+include <fset.h>
+include <printf.h>
+include <mach.h>
+include	"vt.h"
+
+define	SZ_VTRECFD	5120		# length, in chars, of full disk recs
+define	YABUF		20000			# Yet Another BUFfer
+define	SWAP		{temp=$1;$1=$2;$2=temp}
+define	MAX_RANGES	100
+
+# TCOPY -- This is an asynchronous tape to tape copy routine.  It considers
+# the input and output to be streaming devices. 
+# The user specifies which files on tape s/he wants and a root name for the
+# output file names.
+
+procedure t_tcopy()
+
+char	inputfile[SZ_FNAME]
+char	files[SZ_LINE]
+char	outputfile[SZ_FNAME]
+
+char	tapename[SZ_FNAME]
+int	filerange[2 * MAX_RANGES + 1]
+int	nfiles, filenumber, numrecords, whichfile
+bool	verbose 
+
+int	decode_ranges(), mtfile()
+int	get_next_number(), tapecopy(), mtneedfileno()
+bool	clgetb()
+errchk	tapecopy
+
+begin
+	call fseti (STDOUT, F_FLUSHNL, YES)
+
+        # Get input file(s).
+        call clgstr ("inputfile", inputfile, SZ_FNAME)
+	if (mtfile (inputfile) == NO || mtneedfileno (inputfile) == NO) {
+	    call strcpy ("1", files, SZ_LINE)
+        } else {
+	    call clgstr ("files", files, SZ_LINE)
+	}
+
+        if (decode_ranges (files, filerange, MAX_RANGES, nfiles) == ERR)
+	    call error (0, "Illegal file number list.")
+
+	# Get the output file from the cl.
+	call clgstr ("outputfile", outputfile, SZ_FNAME)
+
+	# See if the output is mag tape, if not, error.
+	if (mtfile (outputfile) == NO)
+	    call error (1, "Outputfile should be magnetic tape.")
+
+	# If no tape file number is given, then ask whether the tape
+	# is blank or contains data.  If blank then start at [1], else
+	# start at [EOT].
+
+	if (mtneedfileno(outputfile) == YES)
+	    if (!clgetb ("new_tape"))
+		call mtfname (outputfile, EOT, outputfile, SZ_FNAME)
+	    else
+		call mtfname (outputfile, 1, outputfile, SZ_FNAME)
+
+	# Get verbose flag.
+	verbose = clgetb ("verbose")
+
+        # Loop over files
+	whichfile = 1
+	filenumber = 0
+        while (get_next_number (filerange, filenumber) != EOF) {
+
+	    # Assemble the appropriate tape file name.
+	    if (mtneedfileno (inputfile) == NO)
+		call strcpy (inputfile, tapename, SZ_FNAME)
+	    else
+		call mtfname (inputfile, filenumber, tapename, SZ_FNAME)
+
+	    if (whichfile > 1) {
+	        # Assemble the appropriate output file name.
+		call mtfname (outputfile, EOT, outputfile, SZ_FNAME)
+	    }
+
+	    if (verbose) {
+		call printf ("reading %s, writing %s\n")
+    		    call pargstr(tapename)
+    		    call pargstr(outputfile)
+	    }
+
+	    iferr {
+	        numrecords = tapecopy (tapename, outputfile)
+	    } then {
+		call eprintf ("Error copying file: %s\n")
+		    call pargstr (tapename)
+		call erract (EA_WARN)
+		next
+	    } else if (numrecords == 0) {
+	        call printf ("Tape at EOT\n")
+		break
+	    }
+	    whichfile = whichfile + 1
+
+        }  # End while.
+end
+
+
+# TAPECOPY -- This is the actual tape to tape copy routine.
+
+int procedure tapecopy (infile, outfile)
+
+char	infile[SZ_FNAME]
+char	outfile[SZ_FNAME]
+
+pointer	bufa, bufb, temp
+int	bufsz, numrecords
+int	nbytes, lastnbytes, in, out
+int	fstati(), mtopen(), awaitb()
+errchk	mtopen, areadb, awriteb, awaitb
+
+begin
+	# Open input file, see if it has anything in it.  If not, return.
+	in = mtopen (infile, READ_ONLY, 0)
+
+	bufsz = fstati (in, F_MAXBUFSIZE)	# Maximum output buffer size.
+	if (bufsz == 0)				# If no max, set a max.
+	    bufsz = YABUF
+
+	call malloc (bufa, bufsz, TY_CHAR) 	# Allocate output buffer.
+	call malloc (bufb, bufsz, TY_CHAR)	# Other output buffer
+
+	call areadb (in, Memc[bufa], bufsz, 0)
+	nbytes = awaitb (in)
+	if (nbytes == EOF) {
+	    call close (in)
+	    call mfree (bufa, TY_CHAR)
+	    call mfree (bufb, TY_CHAR)
+	    return (EOF)
+	}
+
+	# Open the output file.
+	out = mtopen (outfile, WRITE_ONLY, 0)
+
+	lastnbytes = 0				# Last record size memory.
+	numrecords = 0				# Number of records read.
+
+	if (nbytes > 0) {
+	    if (nbytes > SZ_VTRECFD*SZB_SHORT &&
+		nbytes < SZ_VTRECFD*SZB_SHORT+600)
+		nbytes = SZ_VTRECFD*SZB_SHORT
+	    call awriteb (out, Memc[bufa], nbytes, 0)
+	    call areadb (in, Memc[bufb], bufsz, 0)
+	    numrecords = numrecords + 1
+	}
+
+	SWAP (bufa, bufb)
+
+	# Main Loop.
+	repeat {
+	    if (awaitb (out) != nbytes) {
+		call printf ("Write error, record = %d.\n")
+		    call pargi (numrecords+1)
+	    }
+
+	    nbytes = awaitb (in)
+	    if (nbytes == ERR) {
+		call printf ("Read error, record = %d.\n")
+		    call pargi (numrecords+1)
+		nbytes = lastnbytes
+	    }
+	    lastnbytes = nbytes
+
+	    if (nbytes > 0) {
+		if (nbytes > SZ_VTRECFD*SZB_SHORT &&
+		    nbytes < SZ_VTRECFD*SZB_SHORT+600)
+		    nbytes = SZ_VTRECFD*SZB_SHORT
+	        call awriteb (out, Memc[bufa], nbytes, 0)
+	        call areadb (in, Memc[bufb], bufsz, 0)
+	        numrecords = numrecords + 1
+	    }
+
+	    SWAP (bufa, bufb)
+
+	} until (nbytes == 0)	# all done
+
+	call mfree (bufa, TY_CHAR)
+	call mfree (bufb, TY_CHAR)
+	call close (in)
+	call close (out)
+
+	return (numrecords)
+end
diff --git a/noao/imred/vtel/textim.x b/noao/imred/vtel/textim.x
new file mode 100644
index 00000000..4ca5a8c1
--- /dev/null
+++ b/noao/imred/vtel/textim.x
@@ -0,0 +1,114 @@
+include <mach.h>
+include <imhdr.h>
+
+define	FONTWIDE	6
+define	FONTHIGH	7
+define	MAXSTRING	100
+
+# TEXTIM -- Write a text string into an image using a pixel font for speed.
+# Characters are made twice as big as the font by doubling in both axes.
+
+procedure textim (im, s, x, y, xmag, ymag, value, zerobgnd, bgndvalu)
+
+pointer	im				# Image to put the text in.
+char	s[MAXSTRING]			# Text to put in the image.
+int	x, y				# x, y position in the image.
+int	xmag, ymag			# x, y magnification values.
+int	value				# Value to use in image for text.
+int	zerobgnd			# Flag to tell if we should zero bgnd.
+int	bgndvalu			# Background value to use.
+
+int	numrow, numcol, numchars
+int	fonthigh, fontwide
+int	i, l, ch
+int	nchar, line
+int	pixary[5]
+pointer	lineget, lineput
+
+short	tshort
+int	strlen()
+pointer	imgl2s(), impl2s()
+errchk	imgl2s, impl2s
+
+begin
+	# Find the length of the string (if there aren't any chars, return).
+	numchars = strlen (s)
+	if (numchars <= 0)
+	    return
+
+	# Calculate height and width of magnified font.
+	fonthigh = FONTHIGH * ymag
+	fontwide = FONTWIDE * xmag
+
+	# Check for row/col out of bounds.
+	numcol= IM_LEN(im,1)
+	numrow = IM_LEN(im,2)
+
+	if (x <= 0) {
+	    call printf ("Warning: Image text deleted, column <= 0.\n")
+	    return
+	}
+
+	if (x > numcol - fontwide*numchars) {
+	    call printf ("Warning: Image text truncated or deleted\n")
+	    numchars = int((numcol - x)/fontwide)
+	    if (numchars <= 0)
+	        return
+	}
+
+	if ((y <= 0) || (y > numrow - fonthigh)) {
+	    call printf ("Warning: Image text deleted, wrong row number.\n")
+	    return
+	}
+
+	# For each line of the text (backward).
+	for (i=7; i>=1; i=i-1) {
+	    line = y+(8-i)*ymag-1
+
+	    do l = 1, ymag {
+
+	        # Get and put the line of the image.
+	        lineget = imgl2s (im, line+(l-1))
+	        lineput = impl2s (im, line+(l-1))
+
+	        # Copy input array or the background value to output array.
+	        if (zerobgnd == 1) {
+		    tshort = bgndvalu
+	            call amovks (tshort, Mems[lineput+x-1],
+		        fontwide*numchars)
+	        } else
+	            call amovs (Mems[lineget], Mems[lineput], numcol)
+
+	        # Put the font.
+	        do ch = 1, numchars {
+	            nchar = int(s[ch])
+		    call pixbit (nchar, i, pixary)
+		    call putpix (pixary, Mems[lineput], numcol,
+			x+(ch-1)*fontwide, value, xmag)
+	        }
+	    }		# End of do on l.
+	}
+end
+
+
+# PUTPIX -- Put one line of one character into the data array.
+
+procedure putpix (pixary, array, size, position, value, xmag)
+
+int	pixary[5]		# array of pixels in character
+int	size, position		# size of data array
+short	array[size]		# data array in which to put character line
+int	value			# value to use for character pixels
+int	xmag			# x-magnification of text
+
+int	i, k, x
+
+begin
+	do i = 1, 5 {
+	    if (pixary[i] == 1) {
+		x = position + (i-1) * xmag
+		do k = 1, xmag
+		    array[x+(k-1)] = value
+	    }
+	}
+end
diff --git a/noao/imred/vtel/trim.par b/noao/imred/vtel/trim.par
new file mode 100644
index 00000000..49e6184e
--- /dev/null
+++ b/noao/imred/vtel/trim.par
@@ -0,0 +1,2 @@
+image,s,q,,,,Image name
+threshold,i,q,,0,15,Squibby brightness threshold for limb
diff --git a/noao/imred/vtel/trim.x b/noao/imred/vtel/trim.x
new file mode 100644
index 00000000..8e76489b
--- /dev/null
+++ b/noao/imred/vtel/trim.x
@@ -0,0 +1,75 @@
+include <mach.h>
+include <imhdr.h>
+include "vt.h"
+
+# TRIM -- Trim a full disk image using the squibby brightness template.
+# Leave all the squibby brightness information intact, set data outside the
+# limb to zero.
+
+procedure t_trim()
+
+char	image[SZ_FNAME]		# image to trim
+int	threshold		# squibby brightness threshold defining limb
+
+int	i, numpix
+pointer	im, lgp, lpp
+pointer	immap(), imgl2s(), impl2s()
+int	clgeti()
+errchk	immap, imgl2s, impl2s
+
+begin
+	# Get parameters from the CL.
+	call clgstr ("image", image, SZ_FNAME)
+	threshold = clgeti("threshold")
+
+	# Open image.
+	im = immap (image, READ_WRITE, 0)
+
+	do i = 1, IM_LEN(im,2) {
+	    lgp = imgl2s (im, i)
+	    lpp = impl2s (im, i)
+	    numpix = IM_LEN(im,1)
+	    call trimline (Mems[lgp], Mems[lpp], numpix, threshold)
+	}
+
+	# Unmap image.
+	call imunmap (im)
+end
+
+
+# TRIMLINE -- trim line1 and put it into line2.
+
+procedure trimline (line1, line2, numpix, threshold)
+
+short	line1[numpix]		# input line
+short	line2[numpix]		# output line
+int	numpix			# number of pixels in this line
+int	threshold		# squibby brightness threshold
+
+int	i, left, right
+
+begin
+	left = 0
+	right = 0
+
+	do i = 1, numpix {
+	    if (and(int(line1[i]),17B) >= threshold) {
+	        left = i
+	        break
+	    } else
+		line2[i] = and(int(line1[i]),17B)
+	}
+
+	if (left != 0)
+	    do i = numpix, 1, -1 {
+	        if(and(int(line1[i]),17B) >= threshold) {
+	            right = i
+	            break
+	        } else
+		    line2[i] = and(int(line1[i]),17B)
+	    }
+
+	if (left != 0 && right != 0 && left < right)
+	    do i = left, right
+		line2[i] = line1[i]
+end
diff --git a/noao/imred/vtel/trnsfrm.inc b/noao/imred/vtel/trnsfrm.inc
new file mode 100644
index 00000000..b916b126
--- /dev/null
+++ b/noao/imred/vtel/trnsfrm.inc
@@ -0,0 +1,163 @@
+data (trnsfrm[i], i = 1, 10) /56,56,56,56,57,57,57,57,58,58/
+data (trnsfrm[i], i = 11, 20) /58,58,59,59,59,59,60,60,60,60/
+data (trnsfrm[i], i = 21, 30) /61,61,61,61,62,62,62,63,63,63/
+data (trnsfrm[i], i = 31, 40) /63,64,64,64,64,65,65,65,65,66/
+data (trnsfrm[i], i = 41, 50) /66,66,67,67,67,67,68,68,68,68/
+data (trnsfrm[i], i = 51, 60) /69,69,69,70,70,70,70,71,71,71/
+data (trnsfrm[i], i = 61, 70) /71,72,72,72,73,73,73,73,74,74/
+data (trnsfrm[i], i = 71, 80) /74,75,75,75,75,76,76,76,77,77/
+data (trnsfrm[i], i = 81, 90) /77,77,78,78,78,79,79,79,79,80/
+data (trnsfrm[i], i = 91, 100) /80,80,81,81,81,82,82,82,82,83/
+data (trnsfrm[i], i = 101, 110) /83,83,84,84,84,85,85,85,85,86/
+data (trnsfrm[i], i = 111, 120) /86,86,87,87,87,88,88,88,89,89/
+data (trnsfrm[i], i = 121, 130) /89,90,90,90,90,91,91,91,92,92/
+data (trnsfrm[i], i = 131, 140) /92,93,93,93,94,94,94,95,95,95/
+data (trnsfrm[i], i = 141, 150) /96,96,96,97,97,97,98,98,98,99/
+data (trnsfrm[i], i = 151, 160) /99,99,100,100,101,101,101,102,102,102/
+data (trnsfrm[i], i = 161, 170) /103,103,103,104,104,104,105,105,106,106/
+data (trnsfrm[i], i = 171, 180) /106,107,107,107,108,108,109,109,109,110/
+data (trnsfrm[i], i = 181, 190) /110,110,111,111,112,112,112,113,113,114/
+data (trnsfrm[i], i = 191, 200) /114,114,115,115,116,116,117,117,117,118/
+data (trnsfrm[i], i = 201, 210) /118,119,119,120,120,120,121,121,122,122/
+data (trnsfrm[i], i = 211, 220) /123,123,124,124,125,125,126,126,127,127/
+data (trnsfrm[i], i = 221, 230) /128,128,129,129,130,130,131,131,132,132/
+data (trnsfrm[i], i = 231, 240) /133,133,134,135,135,136,136,137,138,138/
+data (trnsfrm[i], i = 241, 250) /139,140,140,141,142,143,143,144,145,146/
+data (trnsfrm[i], i = 251, 260) /147,148,149,150,151,153,156,158,160,161/
+data (trnsfrm[i], i = 261, 270) /162,163,164,165,166,167,168,168,169,170/
+data (trnsfrm[i], i = 271, 280) /171,171,172,173,173,174,175,175,176,176/
+data (trnsfrm[i], i = 281, 290) /177,178,178,179,179,180,180,181,181,182/
+data (trnsfrm[i], i = 291, 300) /182,183,183,184,184,185,185,186,186,187/
+data (trnsfrm[i], i = 301, 310) /187,188,188,189,189,190,190,191,191,191/
+data (trnsfrm[i], i = 311, 320) /192,192,193,193,194,194,194,195,195,196/
+data (trnsfrm[i], i = 321, 330) /196,197,197,197,198,198,199,199,199,200/
+data (trnsfrm[i], i = 331, 340) /200,201,201,201,202,202,202,203,203,204/
+data (trnsfrm[i], i = 341, 350) /204,204,205,205,205,206,206,207,207,207/
+data (trnsfrm[i], i = 351, 360) /208,208,208,209,209,209,210,210,210,211/
+data (trnsfrm[i], i = 361, 370) /211,212,212,212,213,213,213,214,214,214/
+data (trnsfrm[i], i = 371, 380) /215,215,215,216,216,216,217,217,217,218/
+data (trnsfrm[i], i = 381, 390) /218,218,219,219,219,220,220,220,221,221/
+data (trnsfrm[i], i = 391, 400) /221,221,222,222,222,223,223,223,224,224/
+data (trnsfrm[i], i = 401, 410) /224,225,225,225,226,226,226,226,227,227/
+data (trnsfrm[i], i = 411, 420) /227,228,228,228,229,229,229,229,230,230/
+data (trnsfrm[i], i = 421, 430) /230,231,231,231,232,232,232,232,233,233/
+data (trnsfrm[i], i = 431, 440) /233,234,234,234,234,235,235,235,236,236/
+data (trnsfrm[i], i = 441, 450) /236,236,237,237,237,238,238,238,238,239/
+data (trnsfrm[i], i = 451, 460) /239,239,240,240,240,240,241,241,241,241/
+data (trnsfrm[i], i = 461, 470) /242,242,242,243,243,243,243,244,244,244/
+data (trnsfrm[i], i = 471, 480) /244,245,245,245,246,246,246,246,247,247/
+data (trnsfrm[i], i = 481, 490) /247,247,248,248,248,248,249,249,249,250/
+data (trnsfrm[i], i = 491, 500) /250,250,250,251,251,251,251,252,252,252/
+data (trnsfrm[i], i = 501, 510) /252,253,253,253,253,254,254,254,254,255/
+data (trnsfrm[i], i = 511, 513) /255,255,255/
+
+data (lkup10830[i], i = 1, 10) /50,50,50,50,50,50,50,50,50,50/
+data (lkup10830[i], i = 11, 20) /50,50,50,50,50,50,50,50,50,50/
+data (lkup10830[i], i = 21, 30) /50,50,50,50,50,50,50,50,50,50/
+data (lkup10830[i], i = 31, 40) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 41, 50) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 51, 60) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 61, 70) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 71, 80) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 81, 90) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 91, 100) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 101, 110) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 111, 120) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 121, 130) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 131, 140) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 141, 150) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 151, 160) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 161, 170) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 171, 180) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 181, 190) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 191, 200) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 201, 210) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 211, 220) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 221, 230) /51,51,51,51,51,51,51,51,51,51/
+data (lkup10830[i], i = 231, 240) /51,51,52,52,52,52,52,52,52,52/
+data (lkup10830[i], i = 241, 250) /52,52,52,52,52,52,52,52,52,52/
+data (lkup10830[i], i = 251, 260) /52,52,52,52,52,52,52,52,52,52/
+data (lkup10830[i], i = 261, 270) /52,52,52,52,52,52,52,52,52,52/
+data (lkup10830[i], i = 271, 280) /52,52,52,52,52,52,52,52,52,52/
+data (lkup10830[i], i = 281, 290) /52,52,52,52,52,52,52,52,52,52/
+data (lkup10830[i], i = 291, 300) /52,52,52,52,52,52,52,52,52,52/
+data (lkup10830[i], i = 301, 310) /52,52,52,53,53,53,53,53,53,53/
+data (lkup10830[i], i = 311, 320) /53,53,53,53,53,53,53,53,53,53/
+data (lkup10830[i], i = 321, 330) /53,53,53,53,53,53,53,53,53,53/
+data (lkup10830[i], i = 331, 340) /53,53,53,53,53,53,53,53,53,54/
+data (lkup10830[i], i = 341, 350) /54,54,54,54,54,54,54,54,54,54/
+data (lkup10830[i], i = 351, 360) /54,54,54,54,54,54,54,54,54,54/
+data (lkup10830[i], i = 361, 370) /54,54,54,54,54,55,55,55,55,55/
+data (lkup10830[i], i = 371, 380) /55,55,55,55,55,55,55,55,55,55/
+data (lkup10830[i], i = 381, 390) /55,55,55,55,55,55,55,56,56,56/
+data (lkup10830[i], i = 391, 400) /56,56,56,56,56,56,56,56,56,56/
+data (lkup10830[i], i = 401, 410) /56,56,56,56,56,57,57,57,57,57/
+data (lkup10830[i], i = 411, 420) /57,57,57,57,57,57,57,57,57,57/
+data (lkup10830[i], i = 421, 430) /57,57,58,58,58,58,58,58,58,58/
+data (lkup10830[i], i = 431, 440) /58,58,58,58,58,58,58,59,59,59/
+data (lkup10830[i], i = 441, 450) /59,59,59,59,59,59,59,59,59,59/
+data (lkup10830[i], i = 451, 460) /59,60,60,60,60,60,60,60,60,60/
+data (lkup10830[i], i = 461, 470) /60,60,60,60,60,61,61,61,61,61/
+data (lkup10830[i], i = 471, 480) /61,61,61,61,61,61,61,62,62,62/
+data (lkup10830[i], i = 481, 490) /62,62,62,62,62,62,62,62,62,63/
+data (lkup10830[i], i = 491, 500) /63,63,63,63,63,63,63,63,63,63/
+data (lkup10830[i], i = 501, 510) /63,64,64,64,64,64,64,64,64,64/
+data (lkup10830[i], i = 511, 520) /64,64,65,65,65,65,65,65,65,65/
+data (lkup10830[i], i = 521, 530) /65,65,65,66,66,66,66,66,66,66/
+data (lkup10830[i], i = 531, 540) /66,66,66,67,67,67,67,67,67,67/
+data (lkup10830[i], i = 541, 550) /67,67,67,67,68,68,68,68,68,68/
+data (lkup10830[i], i = 551, 560) /68,68,68,68,69,69,69,69,69,69/
+data (lkup10830[i], i = 561, 570) /69,69,69,70,70,70,70,70,70,70/
+data (lkup10830[i], i = 571, 580) /70,70,70,71,71,71,71,71,71,71/
+data (lkup10830[i], i = 581, 590) /71,71,72,72,72,72,72,72,72,72/
+data (lkup10830[i], i = 591, 600) /72,73,73,73,73,73,73,73,73,73/
+data (lkup10830[i], i = 601, 610) /74,74,74,74,74,74,74,74,74,75/
+data (lkup10830[i], i = 611, 620) /75,75,75,75,75,75,75,75,76,76/
+data (lkup10830[i], i = 621, 630) /76,76,76,76,76,76,77,77,77,77/
+data (lkup10830[i], i = 631, 640) /77,77,77,77,78,78,78,78,78,78/
+data (lkup10830[i], i = 641, 650) /78,78,78,79,79,79,79,79,79,79/
+data (lkup10830[i], i = 651, 660) /79,80,80,80,80,80,80,80,80,81/
+data (lkup10830[i], i = 661, 670) /81,81,81,81,81,81,81,82,82,82/
+data (lkup10830[i], i = 671, 680) /82,82,82,82,82,83,83,83,83,83/
+data (lkup10830[i], i = 681, 690) /83,83,83,84,84,84,84,84,84,84/
+data (lkup10830[i], i = 691, 700) /85,85,85,85,85,85,85,85,86,86/
+data (lkup10830[i], i = 701, 710) /86,86,86,86,86,86,87,87,87,87/
+data (lkup10830[i], i = 711, 720) /87,87,87,88,88,88,88,88,88,88/
+data (lkup10830[i], i = 721, 730) /88,89,89,89,89,89,89,89,90,90/
+data (lkup10830[i], i = 731, 740) /90,90,90,90,90,91,91,91,91,91/
+data (lkup10830[i], i = 741, 750) /91,91,91,92,92,92,92,92,92,92/
+data (lkup10830[i], i = 751, 760) /93,93,93,93,93,93,93,94,94,94/
+data (lkup10830[i], i = 761, 770) /94,94,94,95,95,95,95,95,95,95/
+data (lkup10830[i], i = 771, 780) /96,96,96,96,96,96,97,97,97,97/
+data (lkup10830[i], i = 781, 790) /97,97,98,98,98,98,98,98,99,99/
+data (lkup10830[i], i = 791, 800) /99,99,99,99,100,100,100,100,100,101/
+data (lkup10830[i], i = 801, 810) /101,101,101,101,101,102,102,102,102,102/
+data (lkup10830[i], i = 811, 820) /103,103,103,103,103,104,104,104,104,104/
+data (lkup10830[i], i = 821, 830) /105,105,105,105,106,106,106,106,106,107/
+data (lkup10830[i], i = 831, 840) /107,107,107,108,108,108,108,108,109,109/
+data (lkup10830[i], i = 841, 850) /109,109,110,110,110,110,111,111,111,111/
+data (lkup10830[i], i = 851, 860) /112,112,112,113,113,113,113,114,114,114/
+data (lkup10830[i], i = 861, 870) /114,115,115,115,116,116,116,116,117,117/
+data (lkup10830[i], i = 871, 880) /117,118,118,118,118,119,119,119,120,120/
+data (lkup10830[i], i = 881, 890) /120,121,121,121,122,122,122,123,123,123/
+data (lkup10830[i], i = 891, 900) /124,124,124,125,125,125,126,126,126,127/
+data (lkup10830[i], i = 901, 910) /127,128,128,128,129,129,129,130,130,131/
+data (lkup10830[i], i = 911, 920) /131,131,132,132,132,133,133,134,134,135/
+data (lkup10830[i], i = 921, 930) /135,135,136,136,137,137,137,138,138,139/
+data (lkup10830[i], i = 931, 940) /139,140,140,141,141,141,142,142,143,143/
+data (lkup10830[i], i = 941, 950) /144,144,145,145,146,146,147,147,148,148/
+data (lkup10830[i], i = 951, 960) /149,149,150,150,151,151,152,152,153,153/
+data (lkup10830[i], i = 961, 970) /154,154,155,155,156,156,157,158,158,159/
+data (lkup10830[i], i = 971, 980) /159,160,160,161,162,162,163,163,164,164/
+data (lkup10830[i], i = 981, 990) /165,166,166,167,167,168,169,169,170,171/
+data (lkup10830[i], i = 991, 1000) /171,172,173,173,174,174,175,176,176,177/
+data (lkup10830[i], i = 1001, 1010) /178,178,179,180,180,181,182,183,183,184/
+data (lkup10830[i], i = 1011, 1020) /185,185,186,187,187,188,189,190,190,191/
+data (lkup10830[i], i = 1021, 1030) /192,193,193,194,195,196,196,197,198,199/
+data (lkup10830[i], i = 1031, 1040) /200,200,201,202,203,203,204,205,206,207/
+data (lkup10830[i], i = 1041, 1050) /208,208,209,210,211,212,213,213,214,215/
+data (lkup10830[i], i = 1051, 1060) /216,217,218,219,220,220,221,222,223,224/
+data (lkup10830[i], i = 1061, 1070) /225,226,227,228,229,230,230,231,232,233/
+data (lkup10830[i], i = 1071, 1080) /234,235,236,237,238,239,240,241,242,243/
+data (lkup10830[i], i = 1081, 1090) /244,245,246,247,248,249,250,251,252,253/
+data (lkup10830[i], i = 1091, 1091) /254/
diff --git a/noao/imred/vtel/unwrap.par b/noao/imred/vtel/unwrap.par
new file mode 100644
index 00000000..1a1d3504
--- /dev/null
+++ b/noao/imred/vtel/unwrap.par
@@ -0,0 +1,9 @@
+image,s,a,,,,image
+outimage,s,a,,,,outimage
+threshold1,i,h,128,,,threshold for first unwrap
+wrapval1,i,h,256,,,wrap displacement for first unwrap
+threshold2,i,h,128,,,threshold for second unwrap
+wrapval2,i,h,256,,,wrap displacement for second unwrap
+cstart,i,h,2,,,column start
+step,i,h,5,,,number of steps to take
+verbose,b,h,yes,,,verbose flag
diff --git a/noao/imred/vtel/unwrap.x b/noao/imred/vtel/unwrap.x
new file mode 100644
index 00000000..a753ddf4
--- /dev/null
+++ b/noao/imred/vtel/unwrap.x
@@ -0,0 +1,293 @@
+include <mach.h>
+include <imhdr.h>
+
+define	MAXBADLINES	20		# maximum number of bad lines
+define	BADTHRESH	1000		# threshold for bad lines
+define	FIXWIDTH	20		# Width of average for fixline
+
+# UNWRAP -- Filter an iraf image.  This filter checks for binary wraparound
+# in IRAF images.  The algorithm is described in detail in the help page.
+# The program accepts templates for both input and output image lists.
+
+procedure t_unwrap()
+
+char	image[SZ_FNAME]			# input image template
+char	outimage[SZ_FNAME]		# output image template
+int	threshold1			# threshold value for first unwrap
+int	threshold2			# threshold value for second unwrap
+int	wrapval1			# wrapvalue for first unwrap
+int	wrapval2			# wrapvalue for second unwrap
+int	cstart				# column to start on
+int	step				# number of steps to perform
+bool	verbose				# verbose flag
+
+int	i, j 
+int	listin, listout
+int	length, nlines
+int	badlines[MAXBADLINES]
+int	diff, nbad
+char	tempimage[SZ_FNAME]
+pointer	im, imout, lgp, lgp2, lpp, cck, sp
+
+bool	clgetb()
+int	imtopenp(), imtlen(), imtgetim(), clgeti()
+pointer	immap(), imgl2s(), impl2s()
+errchk	immap, imgl2s, impl2s
+
+begin
+	# Get parameters from the CL.
+	listin = imtopenp ("image")
+	listout = imtopenp ("outimage")
+	threshold1 = clgeti("threshold1")
+	wrapval1 = clgeti("wrapval1")
+	threshold2 = clgeti("threshold2")
+	wrapval2 = clgeti("wrapval2")
+	cstart = clgeti("cstart")
+	step = clgeti("step")
+	verbose = clgetb("verbose")
+
+	if (verbose) {
+	    call printf ("\n\nUNWRAP: ")
+	    call printf ("threshold1 = %d\n")
+	    call pargi (threshold1)
+	    call printf ("\twrapval1   = %d\n")
+	    call pargi (wrapval1)
+	    call printf ("\tthreshold2 = %d\n")
+	    call pargi (threshold2)
+	    call printf ("\twrapval2   = %d\n")
+	    call pargi (wrapval2)
+	    call printf ("\tcstart     = %d\n")
+	    call pargi (cstart)
+	    call printf ("\tstep       = %d\n\n")
+	    call pargi (step)
+	    call flush (STDOUT)
+	}
+
+	# Check the number of elements.
+	if (imtlen (listin) != imtlen (listout)) {
+	    call imtclose (listin)
+	    call imtclose (listout)
+	    call error (1, "Wrong number of elements in the operand lists")
+	}
+
+	# Get the next images from the lists.
+	while (imtgetim (listin, image, SZ_FNAME) != EOF) {
+	    if (imtgetim (listout, outimage, SZ_FNAME) != EOF) {
+
+	        if (verbose) {
+		    # Write out about the input file name and output file name.
+		    call printf ("\tUnwrapping %s into %s.  ")
+		        call pargstr (image)
+		        call pargstr (outimage)
+		    call flush (STDOUT)
+	        }
+
+	        # Open images.
+	        iferr {
+	            im = immap (image, READ_WRITE, 0)
+	        } then {
+		    call eprintf ("Cannot open image %s.\n")
+		        call pargstr (image)
+		    next
+	        }
+
+	        call xt_mkimtemp (image, outimage, tempimage, SZ_FNAME)
+
+	        iferr {
+	            imout = immap (outimage, NEW_COPY, im)
+	        } then {
+		    call eprintf ("Cannot open image %s, (already exists?).\n")
+		        call pargstr (outimage)
+		    next
+	        }
+
+	        length = IM_LEN(im,1)
+	        nlines = IM_LEN(im,2)
+
+	        # Set up the column check array, then unwrap line by line.
+	        call smark (sp)
+	        call salloc (cck, nlines, TY_INT)
+	        call amovks (0, Memi[cck], nlines)
+	        do i = 1, nlines {
+	            lgp = imgl2s (im, i)
+	            lpp = impl2s (imout, i)
+	            call unwrapline (Mems[lgp], Mems[lpp], cck, length,
+			threshold1, wrapval1, threshold2, wrapval2, cstart,
+			step, i)
+	        }
+
+	        # Step 5 is the final step. (fixline)
+	        if (step == 5) {
+	            # Analyze the column, check for wraps.
+	            nbad = 0
+	            do i = 2, nlines {
+	    	        diff = Memi[cck+i-1] - Memi[cck+i-2]
+	    	        if (abs(diff) > BADTHRESH) {
+	    	            # Mark this line bad.
+	    	            nbad = nbad + 1
+	    	            if (nbad > MAXBADLINES)
+	    		        break
+	    	            badlines[nbad] = i
+	    	        }
+	            }
+	        }
+
+	        # If number bad lines <= than MAXBADLINES, fix em, else, quit.
+	        if (nbad <= MAXBADLINES && nbad > 0) {
+	            do i = 1, nbad {
+
+	    	        # GET the lines above and below the bad line and PUT the
+	    	        # bad line.  Then average the above and below lines and
+			# save in the bad line.
+
+	    	        if (badlines[i] != 1 && badlines[i] != nlines) {
+	    	            if ((badlines[i+1] - badlines[i]) == 1) {
+	                        lgp = imgl2s (imout, badlines[i]-1)
+	                        lgp2 = imgl2s (imout, badlines[i]+1)
+	                        lpp = impl2s (imout, badlines[i])
+	    	                do j = 1, length {
+	    		            Mems[lpp+j-1] = int((real(Mems[lgp+j-1]) +
+	    		                real(Mems[lgp2+j-1]))/2. + .5)
+	    		        }
+	    	            } 
+	    	        }
+	            }
+	        }
+
+	        if (verbose) {
+	            call printf ("number of bad lines = %d\n")
+	                call pargi (nbad)
+	            do i = 1, nbad {
+	                call printf ("\tbadlines[%d] = %d\n")
+	    	        call pargi (i)
+	    	        call pargi (badlines[i])
+	            }
+		    call printf ("\n")
+	            call flush (STDOUT)
+	        }
+
+	        # Unmap images.
+	        call imunmap (im)
+	        call imunmap (imout)
+	        call xt_delimtemp (outimage, tempimage)
+	        call sfree (sp)
+
+	    } # End of if (not EOF)
+	}  # End of while loop on input images
+
+	call imtclose (listin)
+	call imtclose (listout)
+end
+
+
+# UNWRAPLINE -- Unwrap a line of the image.
+
+procedure unwrapline (line1, line2, cck, numpix, threshold1, wrapval1,
+	threshold2, wrapval2, cstart, step, whichline)
+
+short	line1[numpix]			# input line
+short	line2[numpix]			# output line
+pointer	cck				# pointer to array for column check
+int	numpix				# number of pixels per line
+int	threshold1			# unwrap threshold for first unwrap
+int	wrapval1			# unwrap value for first unwrap
+int	threshold2			# unwrap threshold for second unwrap
+int	wrapval2			# unwrap value for second unwrap
+int	cstart				# column to start on
+int	step				# steps to complete
+int	whichline			# which line this is we are unwrapping
+
+pointer	tl1, tl2, tl3			# pointers of temporary arrays
+pointer	sp				# stack pointer
+int	i, diff, sum
+short	wrap				# wrap number
+
+begin
+	# Mark the stack and allcoate the temporary arrays.
+	call smark (sp)
+	call salloc (tl1, numpix, TY_SHORT)
+	call salloc (tl2, numpix, TY_SHORT)
+	call salloc (tl3, numpix, TY_SHORT)
+
+	# Initialize wrap.
+	wrap = 0
+
+	# Copy the input line into the output line and the temporary arrays.
+	call amovs (line1, line2, numpix)
+	call amovs (line1, Mems[tl1], numpix)
+	call amovs (line1, Mems[tl2], numpix)
+	call amovs (line1, Mems[tl3], numpix)
+
+	# Check the image width, do various things if the image is too small.
+
+	# Too small for anything.
+	if (numpix <= 4) {
+	    call sfree (sp)
+	    return
+	}
+
+	# Too small for step 5 (fixline).
+	if (numpix <= FIXWIDTH && step == 5)
+	    step = 4
+
+	# Unwrap1 (step 1).
+	Mems[tl1+cstart-1] = line1[cstart]
+	do i = cstart+1, numpix {
+	    diff = line1[i] - line1[i-1]
+	    if (diff < -threshold1)
+		wrap = wrap + 1
+	    if (diff > threshold1)
+		wrap = wrap - 1
+
+	    Mems[tl1+i-1] = line1[i] + wrap * wrapval1
+	}
+	if (step == 1) {
+	    call amovs (Mems[tl1], line2, numpix)
+	    call sfree (sp)
+	    return
+	}
+
+	# If the user wants it, step 2 (dif).
+	do i = cstart, numpix
+	    Mems[tl2+i-1] = Mems[tl1+i-1] - Mems[tl1+i-2]
+
+	if (step == 2) {
+	    call amovs (Mems[tl2], line2, numpix)
+	    call sfree (sp)
+	    return
+	}
+
+	# If the user wants it, step 3 (unwrap2).
+	wrap = 0
+	line2[cstart] = Mems[tl2+cstart-1]
+	do i = cstart+1, numpix {
+	    diff = Mems[tl2+i-1] - Mems[tl2+i-2]
+	    if (diff < -threshold2)
+	        wrap = wrap + 1
+	    if (diff > threshold2)
+		wrap = wrap - 1
+
+	    line2[i] = Mems[tl2+i-1] + wrap * wrapval2
+	}
+	if (step == 3) {
+	    call sfree (sp)
+	    return
+	}
+
+	# If the user wants it, step 4 (reconstruct).
+	do i = cstart, numpix
+	    line2[i] = line2[i-1] + line2[i]
+	
+	if (step == 4) {
+	    call sfree (sp)
+	    return
+	}
+
+	# Again, if the user wants it, save data for step 5, (fixline).
+	sum = 0
+	do i = numpix-FIXWIDTH+1, numpix
+	    sum = sum + line2[i]
+	Memi[cck+whichline-1] = int(real(sum)/real(FIXWIDTH) + .5)
+
+	call sfree (sp)
+end
diff --git a/noao/imred/vtel/vt.h b/noao/imred/vtel/vt.h
new file mode 100644
index 00000000..73d9c22a
--- /dev/null
+++ b/noao/imred/vtel/vt.h
@@ -0,0 +1,73 @@
+# Vacuum_telescope analysis package header file.
+
+# General defines common to most of the programs in this package.
+define	DIM_VTFD	2048		  # full disk image = 2048 x 2048 array 
+define	SZB_SHORT	SZ_SHORT*SZB_CHAR # number of bytes per short integer
+define	SZB_REAL	SZ_REAL*SZB_CHAR  # number of bytes per real
+define	THRESHOLD	4		  # limb cutoff value, squib brightness
+
+# Defines related to the tape format.
+define 	SZ_VTHDR	20		# number of 16-bit words in vt header
+define	SZ_VTREC	5120		# number of 16-bit words in vt record
+define	NUM_VTREC	750		# number of records in full disk image
+
+# Ellipse structure defines.
+define	LEN_ELSTRUCT	4		# real el[LEN_ELSTRUCT]
+
+define	E_XCENTER	$1[1]		# x-coord of center of limb ellipse
+define	E_YCENTER	$1[2]		# y-coord of center of limb ellipse
+define	E_XSEMIDIAMETER	$1[3]		# length of x semiaxis of limb ellipse
+define	E_YSEMIDIAMETER	$1[4]		# length of y semiaxis of limb ellipse
+
+# Defines for readvt, etc.
+define	SWTH_HIGH	512		# height of each swath
+define	SWTHWID_14	1700		# width of swaths 1 and 4
+define	SWTHWID_23	2048		# width of swaths 2 and 3
+define	HALF_DIF	174		# one half of difference in swath widths
+define	SZ_TABLE	8192		# length of lookup table (16-bit words)
+define	NUM_SRSTR	16		# total # of subrasters in full disk
+define	LEN_HDRDAT	10		# length of header data
+define	NUM_SRSTR_X	4		# number of subrasters in x direction
+define	NUM_SRSTR_Y	4		# number of subrasters in y direction
+define	SRSTR_WID	512		# width of each subraster
+define	IS_DATA		1		# subswath data indicator
+define	DTSTRING	100		# length of date/time string
+
+# Defines for rmap, etc.
+define	DIM_IN_RAS	150		# y dimension for input image subraster
+define	DIM_SQUAREIM	180		# x or y dimension of daily projection
+
+# Defines for merge, etc.
+define	DIM_XCARMAP	360		# x dimension of carrington map
+define	SZ_WTBL		180		# size of weight table for merge
+
+# Mscan text (pixelfont) structure.
+define	LEN_TXSTRUCT	10
+
+define	TX_XPOS		Memi[$1]	# x position of start of text
+define	TX_YPOS		Memi[$1+1]	# y position of start of text
+define	TX_VALUE	Memi[$1+2]	# value to write text with
+define	PRINT_TEXT	Memi[$1+3]	# to text, or not to text  (1=yes,0=no)
+define	ZERO_BGND	Memi[$1+4]	# fill background w/ VALU? (1=yes,0=no)
+define	BGND_VALU	Memi[$1+5]	# background value to use
+
+# Vacuum telescope header struture.
+define	VT_LENHSTRUCT	10
+
+define	VT_HMONTH	Memi[$1]	# month of observation (1-12)
+define	VT_HDAY		Memi[$1+1]	# day of observation (1-31)
+define	VT_HYEAR	Memi[$1+2]	# year (two digits)
+define	VT_HTIME	Memi[$1+3]	# time (seconds since midnight)
+define	VT_HWVLNGTH	Memi[$1+4]	# wavelength (angstroms)
+define	VT_HOBSTYPE	Memi[$1+5]	# observation type (0,1,2,3,or 4)
+define	VT_HAVINTENS	Memi[$1+6]	# average intensity
+define	VT_HNUMCOLS	Memi[$1+7]	# number of columns
+define	VT_HINTGPIX	Memi[$1+8]	# integrations per pixel
+define	VT_HREPTIME	Memi[$1+9]	# repitition time
+
+# I/O buffer structure.
+define	VT_LENBSTRUCT	3
+
+define	VT_BUFP		Memi[$1]	# pointer, top of i/o buf
+define	VT_BP		Memi[$1+1]	# pointer, current position in i/o buf
+define	VT_BUFBOT	Memi[$1+2]	# pointer, current bottom of i/o buf
diff --git a/noao/imred/vtel/vtblink.cl b/noao/imred/vtel/vtblink.cl
new file mode 100644
index 00000000..d9e51a61
--- /dev/null
+++ b/noao/imred/vtel/vtblink.cl
@@ -0,0 +1,150 @@
+#{ VTBLINK -- Blink successive frames of daily grams to check registration.
+
+# imname1,s,a,,,,Name of first image
+# imname2,s,a,,,,Name of next image
+# z1,r,h,-3000.0,,,Minimum graylevel to be displayed.
+# z2,r,h,3000.0,,,Minimum graylevel to be displayed.
+
+{
+	real	zz1, zz2, offset, currentoffset
+	char	im1name, im2name, framelog[4]
+	int	im1long, im2long, currentframe, offscreenflag
+
+	# initialize
+	print ("  ")
+	print ("  ")
+	print ("vtblink vtblink vtblink vtblink vtblink vtblink vtblink")
+	print ("  ")
+	currentframe = 1
+	offscreenflag = 0
+	currentoffset = .72      # Start at the right side of the screen.
+	framelog[1] = "none"
+	framelog[2] = "none"
+	framelog[3] = "none"
+	framelog[4] = "none"
+
+	# Get the gray scale.
+	zz1 = z1
+	zz2 = z2
+
+	# Get the first frame from the user, display it, allow user to window.
+	im1name = imname1
+	if (im1name == "end") {
+	    bye
+	}
+	while (!access(im1name//".imh") && im1name != "end") {
+	    print (im1name, "not accessable, try again")
+	    im1name = imname1
+	    if (im1name == "end") {
+	        bye
+	    }
+	}
+	imgets (im1name, "L_ZERO")
+	im1long = real(imgets.value)
+	print ("Longitude of first image is ", im1long)
+	print ("Displaying frame.")
+	display (im1name, currentframe, xcenter=currentoffset, zrange=no,
+	    zscale=no, z1=zz1, z2=zz2)
+	framelog[currentframe] = im1name
+	frame (currentframe)
+	print ("Now, please window this frame for the desired color table.")
+	window
+
+	# Make all the color tables of the other 3 frames the same as this.
+	print ("Equalizing color tables of 4 frames, Please wait.")
+	lumatch (2, currentframe)
+	lumatch (3, currentframe)
+	lumatch (4, currentframe)
+
+	# Get the next frame from the user.
+	im2name = imname2
+	while (im2name == "stat") {
+	    print ("Frame 1 contains image ", framelog[1])
+	    print ("Frame 2 contains image ", framelog[2])
+	    print ("Frame 3 contains image ", framelog[3])
+	    print ("Frame 4 contains image ", framelog[4])
+	    im2name = imname2
+	}
+	if (im2name == "end") {
+	    bye
+	}
+	while (!access(im2name//".imh") && im2name != "end") {
+	    print (im2name, "not accessable, try again")
+	    im2name = imname2
+	    if (im2name == "end") {
+	        bye
+	    }
+	}
+	imgets (im2name, "L_ZERO")
+	im2long = real(imgets.value)
+	print ("Longitude of this image is ", im2long)
+
+	# While the user does not enter 'end' for the image name, keep going.
+	# also check the offscreenflag and exit it it becomes set.
+	while (im2name != 'end' && offscreenflag != 1) {
+	
+	    # Calculate offset. subsequent images in general have smaller
+	    # longitudes, that is, longitude decreases with time.
+	    # If the new image has a larger longitude then fix up offset.
+	    if (im1long < im2long) {
+	        offset = real((im2long - 360) - im1long)/512.
+	    } else {
+	        offset = real(im2long - im1long)/512.
+	    }
+
+	    # If we are getting too close to the left side, restart program.
+	    if ((currentoffset+offset) <= .18) {
+		print("*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*")
+		print("* The next image would overlap the edge of the      *")
+		print("* screen. Please restart the program with the last  *")
+		print("* image.                                            *")
+		print("*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*-*")
+		offscreenflag = 1
+	    }
+
+	    # Display the next image and blink it with the previously displayed
+	    # image.
+	    if (offscreenflag != 1) {
+	        print ("Displaying frame.")
+	        display (im2name, mod(currentframe,4)+1,
+		    xcenter=currentoffset+offset, zscale=no, zrange=no,
+		    z1=zz1, z2=zz2)
+		framelog[mod(currentframe,4)+1] = im2name
+
+	        # Return the user to the cl so s/he can do whatever s/he wants.
+	        print("  ")
+	        print("You are now in the cl, type 'bye' to return to vtlbink")
+	        cl()
+	        print("  ")
+
+	        # Update currentframe and print it out, update the offset.
+	        currentframe = mod(currentframe,4)+1
+		print ("The next frame to be used for display is frame ", 
+		    mod(currentframe,4)+1)
+	        currentoffset += offset
+
+	        # Move image2 to image1 and then get a new image2 and loop back.
+	        im1name = im2name
+	        im1long = im2long
+	        im2name = imname2
+		while (im2name == "stat") {
+	    	    print ("Frame 1 contains image ", framelog[1])
+	    	    print ("Frame 2 contains image ", framelog[2])
+	    	    print ("Frame 3 contains image ", framelog[3])
+	    	    print ("Frame 4 contains image ", framelog[4])
+	    	    im2name = imname2
+		}
+	        while (!access(im2name//".imh") && im2name != "end") {
+	            print (im2name, "not accessable, try again")
+	            im2name = imname2
+	            if (im2name == "end") {
+	                bye
+	            }
+	        }
+		if (im2name != "end") {
+		    imgets (im2name, "L_ZERO")
+		    im2long = real(imgets.value)
+		}
+	    }
+	}
+}
diff --git a/noao/imred/vtel/vtblink.par b/noao/imred/vtel/vtblink.par
new file mode 100644
index 00000000..def7c1eb
--- /dev/null
+++ b/noao/imred/vtel/vtblink.par
@@ -0,0 +1,4 @@
+imname1,s,a,,,,Name of first image
+imname2,s,a,,,,Name of next image
+z1,r,h,-3000.0,,,Minimum graylevel to be displayed.
+z2,r,h,3000.0,,,Minimum graylevel to be displayed.
diff --git a/noao/imred/vtel/vtel.cl b/noao/imred/vtel/vtel.cl
new file mode 100644
index 00000000..020a6455
--- /dev/null
+++ b/noao/imred/vtel/vtel.cl
@@ -0,0 +1,38 @@
+#{ VTEL -- Vacuum_telescope package.
+
+# load necessary packages
+images
+tv
+
+set	vtel		= "imred$vtel/"
+
+package vtel
+
+task	readvt,
+	writevt,
+	unwrap,
+	quickfit,
+	getsqib,
+	putsqib,
+	mscan,
+	rmap,
+	merge,
+	destreak,
+	trim,
+	vtexamine,
+	tcopy,
+	pimtext,
+	syndico,
+	dicoplot	= "vtel$x_vtel.e"
+
+# scripts
+
+task	vtblink		= "vtel$vtblink.cl"
+task	writetape	= "vtel$writetape.cl"
+task	destreak5	= "vtel$destreak5.cl"
+task	fitslogr	= "vtel$fitslogr.cl"
+task	mrotlogr	= "vtel$mrotlogr.cl"
+task	makeimages	= "vtel$makeimages.cl"
+task	makehelium	= "vtel$makehelium.cl"
+
+clbye()
diff --git a/noao/imred/vtel/vtel.hd b/noao/imred/vtel/vtel.hd
new file mode 100644
index 00000000..5a9871ab
--- /dev/null
+++ b/noao/imred/vtel/vtel.hd
@@ -0,0 +1,29 @@
+# Help directory for the VACUUM package.
+
+$doc	= "./doc/"
+
+vtel		men=vtel$vtel.men,		src=vtel$vtel.cl
+destreak	hlp=doc$destreak.hlp,		src=vtel$destreak.x
+destreak5	hlp=doc$destreak5.hlp,		src=vtel$destreak5.cl
+readvt		hlp=doc$readvt.hlp,		src=vtel$readvt.x
+writevt		hlp=doc$writevt.hlp,		src=vtel$writevt.x
+rmap		hlp=doc$rmap.hlp,		src=vtel$rmap.x
+vtblink		hlp=doc$vtblink.hlp,		src=vtel$vtblink.cl
+quickfit	hlp=doc$quickfit.hlp,		src=vtel$quickfit.x
+merge		hlp=doc$merge.hlp,		src=vtel$merge.x
+dicoplot	hlp=doc$dicoplot.hlp,		src=vtel$dicoplot.x
+unwrap		hlp=doc$unwrap.hlp,		src=vtel$unwrap.x
+getsqib		hlp=doc$getsqib.hlp,		src=vtel$getsqib.x
+putsqib		hlp=doc$putsqib.hlp,		src=vtel$putsqib.x
+trim		hlp=doc$trim.hlp,		src=vtel$trim.x
+mscan		hlp=doc$mscan.hlp,		src=vtel$mscan.x
+vtexamine	hlp=doc$vtexamine.hlp,		src=vtel$vtexamine.x
+tcopy		hlp=doc$tcopy.hlp,		src=vtel$tcopy.x
+pimtext		hlp=doc$pimtext.hlp,		src=vtel$pimtext.x
+fitslogr	hlp=doc$fitslogr.hlp,		src=vtel$fitslogr.cl
+mrotlogr	hlp=doc$mrotlogr.hlp,		src=vtel$mrotlogr.cl
+makeimages	hlp=doc$makeimages.hlp,		src=vtel$makeimages.cl
+makehelium	hlp=doc$makehelium.hlp,		src=vtel$makehelium.cl
+writetape	hlp=doc$writetape.hlp,		src=vtel$writetape.cl
+syndico		hlp=doc$syndico.hlp,		src=vtel$syndico.x
+revisions	sys=Revisions
diff --git a/noao/imred/vtel/vtel.men b/noao/imred/vtel/vtel.men
new file mode 100644
index 00000000..df98fc59
--- /dev/null
+++ b/noao/imred/vtel/vtel.men
@@ -0,0 +1,23 @@
+       destreak - Destreak He 10830 grams.
+      destreak5 - First pass processing CL script for 10830 grams.
+       dicoplot - Make dicomed plots of carrington maps.
+       fitslogr - Make a log of certain header parameters from a FITS tape.
+	getsqib - Extract the squibby brightness image from a full disk scan.
+     makehelium - Cl script for processing destreaked 10830 grams(second pass).
+     makeimages - Cl script for processing magnetograms into projected maps
+	  merge - Merge daily grams into a Carrington map.
+       mrotlogr - Log some header parameters from a FITS rotation map tape.
+	  mscan - Read all sector scans on a tape and put them into images.
+	pimtext - Put text directly into images using a pixel font.
+	putsqib - Merge a squibby brightness image into a full disk image.
+       quickfit - Fit an ellipse to the solar limb.
+	 readvt - Read a full disk tape and produce an IRAF image.
+	   rmap - Map a full disk image into a 180 by 180 flat image.
+	syndico - Make dicomed print of daily grams 18 cm across.
+	  tcopy - Tape to tape copy routine.
+	   trim - Set all pixels outside the limb to 0.0 (use sqib for limb).
+	 unwrap - Remove effects of data wraparound on continuum scans.
+	vtblink - Blink daily grams on the IIS to check for registration.
+      vtexamine - Examine a vacuum telescope tape, print headers and profile.
+      writetape - Cl script to write 5 full disk grams to tape.
+	writevt - Write an IRAF image to tape in vacuum telescope format.
diff --git a/noao/imred/vtel/vtel.par b/noao/imred/vtel/vtel.par
new file mode 100644
index 00000000..dde78dd5
--- /dev/null
+++ b/noao/imred/vtel/vtel.par
@@ -0,0 +1 @@
+version,s,h,"8Jun87"
diff --git a/noao/imred/vtel/vtexamine.par b/noao/imred/vtel/vtexamine.par
new file mode 100644
index 00000000..39283d0e
--- /dev/null
+++ b/noao/imred/vtel/vtexamine.par
@@ -0,0 +1,3 @@
+input,s,q,,,,Input file descriptor
+headers,b,h,yes,,,Print out header data 
+files,s,q,,,,List of files to be examined
diff --git a/noao/imred/vtel/vtexamine.x b/noao/imred/vtel/vtexamine.x
new file mode 100644
index 00000000..2b482bbe
--- /dev/null
+++ b/noao/imred/vtel/vtexamine.x
@@ -0,0 +1,195 @@
+include <error.h>
+include <fset.h>
+include <printf.h>
+include <mach.h>
+include "vt.h"
+
+define	MAX_RANGES	100
+
+# VTEXAMINE -- Examine a vacuum telescope tape.  Decode and print the
+# header and tell the user info about number and length of records
+# on the tape.
+
+procedure t_vtexamine()
+
+char	input[SZ_FNAME]		# input template
+char	files[SZ_LINE]		# which files to examine
+bool	headers			# print headers?
+
+char	tapename[SZ_FNAME]
+int	filerange[2 * MAX_RANGES + 1]
+int	nfiles, filenumber, nrecords
+
+bool	clgetb()
+int	decode_ranges(), get_next_number()
+int	vtexamine(), mtfile(), mtneedfileno()
+errchk	vtexamine
+
+begin
+	call fseti (STDOUT, F_FLUSHNL, YES)
+
+	# Find out if user wants to see header info.
+	headers = clgetb ("headers")
+	
+        # Get input file(s)
+        call clgstr ("input", input, SZ_FNAME)
+	if (mtfile (input) == NO || mtneedfileno (input) == NO)
+	    call strcpy ("1", files, SZ_LINE)
+        else
+	    call clgstr ("files", files, SZ_LINE)
+
+        if (decode_ranges (files, filerange, MAX_RANGES, nfiles) == ERR)
+	    call error (0, "Illegal file number list.")
+	call printf ("\n")
+
+        # Loop over files.
+	filenumber = 0
+        while (get_next_number (filerange, filenumber) != EOF) {
+
+	    # Assemble the appropriate tape file name.
+	    call strcpy (input, tapename, SZ_FNAME)
+	    if (mtfile(input) == YES && mtneedfileno (input) == YES)
+		call mtfname (input, filenumber, tapename, SZ_FNAME)
+
+	    iferr {
+	        nrecords = vtexamine (tapename, headers)
+	    } then {
+		call eprintf ("Error reading file: %s\n")
+		    call pargstr (tapename)
+		call erract (EA_WARN)
+		next
+	    } else if (nrecords == 0) {
+	        call printf ("Tape at EOT\n")
+		break
+	    }
+
+        }  # End while.
+end
+
+
+# VTEXAMINE -- examine a tape (or disk) file.  Report about size and
+# number of records and, if requested, decode and print the header
+# information.
+
+int procedure vtexamine (input, headers)
+
+char	input[ARB]		# input file name
+bool	headers
+
+int	in, bufsize, totrecords
+int	nrecords, totbytes, lastrecsize
+int	recsize
+bool	trufls
+pointer	hs, sp
+pointer	pchar, hpchar
+
+int	mtopen(), fstati(), get_next_record()
+errchk	mtopen, close, get_next_record
+
+begin
+	call smark (sp)
+	call salloc (hs, VT_LENHSTRUCT, TY_STRUCT)
+
+	in = mtopen (input, READ_ONLY, 0)
+	bufsize = fstati (in, F_BUFSIZE)
+
+	call malloc (pchar, bufsize, TY_CHAR)
+	call malloc (hpchar, bufsize, TY_SHORT)
+
+	call printf ("File %s:  ")
+	    call pargstr (input)
+
+	totrecords = 0
+	nrecords = 0
+	totbytes = 0
+	lastrecsize = 0
+
+
+	# First read the header file.
+	recsize = get_next_record (in, Memc[pchar], bufsize, recsize,
+	    SZ_VTHDR * SZB_SHORT/SZB_CHAR)
+	if (recsize == EOF)
+	    return (totrecords)
+	call amovs (Memc[pchar], Mems[hpchar], SZ_VTHDR * SZB_SHORT/SZB_CHAR)
+
+	nrecords = nrecords + 1
+	totrecords = totrecords + 1
+	totbytes = totbytes + recsize
+	lastrecsize = recsize
+	trufls = TRUE
+	if (headers)
+	    call decodeheader (hpchar, hs, trufls)
+	call printf ("\n")
+
+	# Loop through the rest of the records.
+	while (get_next_record (in, Memc[pchar], bufsize, recsize,
+	    lastrecsize) != EOF) {
+
+	    if (recsize == lastrecsize)
+		nrecords = nrecords + 1
+	    else {
+		call printf ("\t      %d %d-byte records\n")
+		    call pargi (nrecords)
+		    call pargi (lastrecsize)
+		nrecords = 1
+		lastrecsize = recsize
+	    }
+
+	    totrecords = totrecords + 1
+	    totbytes = totbytes + recsize
+
+	}  # End while.
+
+	if (nrecords > 0 ) {
+	    call printf ("\t      %d %d-byte records\n")
+		call pargi (nrecords)
+		call pargi (lastrecsize)
+	}
+
+	# Print total number of records and bytes.
+	call printf ("\t      Total %d records, %d bytes\n")
+	    call pargi (totrecords)
+	    call pargi (totbytes)
+
+	call mfree (pchar, TY_CHAR)
+	call mfree (hpchar, TY_SHORT)
+	call sfree (sp)
+	call close (in)
+
+	return (totrecords)
+end
+
+
+# GET_NEXT_RECORD -- Read the next record from tape (or disk) and,
+# if an error is found, patch up the data as best we can and use it.
+# Also, tell the user about the error.
+
+int procedure get_next_record(fd, buffer, bufsize, recsize, lastbufsize)
+
+int	bufsize
+char	buffer[bufsize]
+int	recsize, lastbufsize
+pointer	fd
+
+int	read(), fstati()
+bool	eofflag
+errchk	read
+
+begin
+	eofflag = false
+	iferr {
+	    if (read (fd, buffer, bufsize) == EOF)
+		eofflag = true
+	    recsize = fstati (fd, F_SZBBLK)
+	} then {
+	    call fseti (fd, F_VALIDATE, lastbufsize)
+	    recsize = read (fd, buffer, bufsize)
+	    recsize = fstati (fd, F_SZBBLK)
+	}
+	if (BYTE_SWAP2 == YES)
+	    call bswap2 (buffer, 1, buffer, 1, SZ_VTHDR*SZB_SHORT)
+	if (eofflag)
+	    return (EOF)
+	else
+	    return (recsize)
+end
diff --git a/noao/imred/vtel/writetape.cl b/noao/imred/vtel/writetape.cl
new file mode 100644
index 00000000..76bb23f2
--- /dev/null
+++ b/noao/imred/vtel/writetape.cl
@@ -0,0 +1,45 @@
+#{ WRITETAPE -- Write five images to a vacuum telescope tape.  The
+# script accepts the name of the mag tape device and the general input
+# image filename from the user.  Writetape appends a digit [1-5] to the
+# file name for each file to be written.
+
+# getmtape,s,a,,,,Mag tape device to write to
+# getname,s,a,,,,Root filename for the 5 images
+# magtape,s,h
+# imname,s,h
+
+{
+
+	imname = getname
+	magtape = getmtape
+
+	if (access(imname//"1.imh")) {
+	    writevt (imname//"1", magtape//"1600[1]")
+	} else {
+	    print (imname//"1 not accessable")
+	}
+
+	if (access(imname//"2.imh")) {
+	    writevt (imname//"2", magtape//"1600[2]")
+	} else {
+	    print (imname//"2 not accessable")
+	}
+
+	if (access(imname//"3.imh")) {
+	    writevt (imname//"3", magtape//"1600[3]")
+	} else {
+	    print (imname//"3 not accessable")
+	}
+
+	if (access(imname//"4.imh")) {
+	    writevt (imname//"4", magtape//"1600[4]")
+	} else {
+	    print (imname//"4 not accessable")
+	}
+
+	if (access(imname//"5.imh")) {
+	    writevt (imname//"5", magtape//"1600[5]")
+	} else {
+	    print (imname//"5 not accessable")
+	}
+}
diff --git a/noao/imred/vtel/writetape.par b/noao/imred/vtel/writetape.par
new file mode 100644
index 00000000..863a283d
--- /dev/null
+++ b/noao/imred/vtel/writetape.par
@@ -0,0 +1,5 @@
+
+getmtape,s,a,,,,Mag tape device to write to
+getname,s,a,,,,Root filename for the 5 images
+magtape,s,h
+imname,s,h
diff --git a/noao/imred/vtel/writevt.par b/noao/imred/vtel/writevt.par
new file mode 100644
index 00000000..de11cb13
--- /dev/null
+++ b/noao/imred/vtel/writevt.par
@@ -0,0 +1,4 @@
+imagefile,s,q,,,,Image file descriptor
+outputfile,s,q,,,,Output file descriptor
+verbose,b,h,no,,,Print out header data and give progress reports
+new_tape,b,q,,,,Are you using a new tape?
diff --git a/noao/imred/vtel/writevt.x b/noao/imred/vtel/writevt.x
new file mode 100644
index 00000000..390884b2
--- /dev/null
+++ b/noao/imred/vtel/writevt.x
@@ -0,0 +1,232 @@
+include <error.h>
+include <mach.h>
+include <fset.h>
+include "vt.h"
+
+define	SZ_TABLE	8192		# size of lookup table (data)
+
+# WRITEVT -- Write an IRAF image (vacuum telescope full disk image) out to
+# tape in a format identical to the format produced bye the vacuum telescope.
+
+procedure t_writevt()
+
+char	imagefile[SZ_FNAME]			# name of image to be written
+char	outputfile[SZ_FNAME]			# output file name (tape)
+bool	verbose					# verbose flag
+
+int	obsdate
+int	x1, y1, subraster, outfd
+int	one
+pointer	table
+pointer	srp, im, hs, sp
+
+int	imgeti(), mtopen()
+int	mtfile(), mtneedfileno()
+bool	clgetb()
+pointer	imgs2s(), immap()
+errchk	immap, imgs2s, mtopen
+
+begin
+	call smark (sp)
+	call salloc (table, SZ_TABLE, TY_SHORT)
+	call salloc (hs, VT_LENHSTRUCT, TY_STRUCT)
+
+	# Get the image name and the verbose flag from the cl.
+	call clgstr ("imagefile", imagefile, SZ_FNAME)
+	verbose = clgetb ("verbose")
+
+	# Get the output file from the cl.
+	call clgstr ("outputfile", outputfile, SZ_FNAME)
+
+	# See if the outputfile is mag tape, if not, error.
+        if (mtfile (outputfile) == NO)
+	    call error (1, "Outputfile should be magnetic tape.")
+
+	# If no tape file number is given, then ask whether the tape
+	# is blank or contains data.  If blank then start at [1], else
+	# start at [EOT].
+
+	if (mtneedfileno(outputfile) == YES)
+	    if (!clgetb ("new_tape"))
+		call mtfname (outputfile, EOT, outputfile, SZ_FNAME)
+	    else
+		call mtfname (outputfile, 1, outputfile, SZ_FNAME)
+
+	if (verbose) {
+	    call printf ("outputfile name = %s\n")
+		call pargstr (outputfile)
+	}
+
+	# Open the image file and the output file.
+	im = immap (imagefile, READ_ONLY, 0)
+	outfd = mtopen (outputfile, WRITE_ONLY, SZ_VTREC)
+
+	# Get date and time from the header.
+	obsdate = imgeti (im, "OBS_DATE")
+	VT_HMONTH(hs) = obsdate/10000
+	VT_HDAY(hs) = obsdate/100 - 100 * (obsdate/10000)
+	VT_HYEAR(hs) = obsdate - 100 * (obsdate/100)
+	VT_HTIME(hs) = imgeti (im, "OBS_TIME")
+	VT_HWVLNGTH(hs) = imgeti(im, "wv_lngth")
+	VT_HOBSTYPE(hs) = imgeti (im, "obs_type")
+	VT_HAVINTENS(hs) = imgeti (im, "av_intns")
+	VT_HNUMCOLS(hs) = imgeti (im, "num_cols")
+	VT_HINTGPIX(hs) = imgeti (im, "intg/pix")
+	VT_HREPTIME(hs) = imgeti (im, "rep_time")
+
+	# Write header data to tape.
+	call writeheader (outfd, hs, verbose)
+
+	# Set up lookuptable for data subswaths.
+	one = 1
+	call amovks (one, Mems[table], SZ_TABLE)
+	call aclrs (Mems[table], HALF_DIF)
+	call aclrs (Mems[table + SWTHWID_14 + HALF_DIF], HALF_DIF)
+	call aclrs (Mems[table + SWTHWID_23 * 3], HALF_DIF)
+	call aclrs (Mems[table + SZ_TABLE - HALF_DIF], HALF_DIF)
+
+	# Write the image data to tape.
+	do subraster = 1, NUM_SRSTR {
+
+	    # Calculate position of bottom left corner of this subraster.
+	    x1 = ((NUM_SRSTR_X - 1) - mod((subraster - 1), NUM_SRSTR_X)) *
+		SRSTR_WID + 1
+	    y1 = ((NUM_SRSTR_Y - 1) - ((subraster - mod((subraster - 1),
+		NUM_SRSTR_Y)) / NUM_SRSTR_Y)) * SWTH_HIGH + 1
+
+	    # Get subraster.
+	    srp = imgs2s (im, x1, x1+(SRSTR_WID - 1), y1, y1+(SWTH_HIGH - 1))
+	    iferr (call putsubraster (outfd, Mems[srp], SRSTR_WID,
+		SWTH_HIGH, Mems[table], subraster))
+		call eprintf ("Error in putsubraster, subraster = %d\n")
+		    call pargi (subraster)
+	    if (verbose) {
+		call printf("%d%% done\n")
+		    call pargi ((subraster*100)/NUM_SRSTR)
+		call flush (STDOUT)
+	    }
+	}
+
+	# Close output file and unmap image.
+	call close (outfd)
+	call imunmap (im)
+	call sfree (sp)
+end
+
+
+# WRITEHEADER -- Write header info to the output, pack date
+# and time, and, if 'verbose' flag is set, display some information
+# to the user.
+
+procedure writeheader(outfd, hs, verbose)
+
+int	outfd			# output file descriptor
+pointer	hs			# header data structure pointer
+bool	verbose			# verbose flag
+
+int	i
+short	hbuf[SZ_VTHDR]
+int	fstati()
+errchk	write
+
+begin
+	# Pack date, time.  The constants below are explained in the
+	# description of the image header and how it is packed.  If any
+	# changes are made the following code will have to be rewritten.
+
+	call bitpak (VT_HMONTH(hs)/10, hbuf[1], 13, 4)
+	call bitpak ((VT_HMONTH(hs)-(VT_HMONTH(hs)/10)*10), hbuf[1], 9, 4)
+	call bitpak (VT_HDAY(hs)/10, hbuf[1], 5, 4)
+	call bitpak ((VT_HDAY(hs)-(VT_HDAY(hs)/10)*10), hbuf[1], 1, 4)
+	call bitpak (VT_HYEAR(hs)/10, hbuf[2], 13, 4)
+	call bitpak ((VT_HYEAR(hs)-(VT_HYEAR(hs)/10)*10), hbuf[2], 9, 4)
+	call bitpak (VT_HTIME(hs)/2**15, hbuf[3], 1, 2)
+	call bitpak ((VT_HTIME(hs)-(VT_HTIME(hs)/2**15)*2**15), hbuf[4], 1, 15)
+
+	# Put other parameters in appropriate places.
+	hbuf[5] = VT_HWVLNGTH(hs)
+	hbuf[6] = VT_HOBSTYPE(hs)
+	hbuf[7] = VT_HAVINTENS(hs)
+	hbuf[8] = VT_HNUMCOLS(hs)
+	hbuf[9] = VT_HINTGPIX(hs)
+	hbuf[10] = VT_HREPTIME(hs)
+
+	# Store other header parameters.
+	for (i = 11 ; i <= SZ_VTHDR ; i = i + 1)
+	    hbuf[i] = 0
+
+	if (verbose) {
+	    call printf ("\nmonth/day/year = %d/%d/%d\n")
+		call pargi (VT_HMONTH(hs))
+		call pargi (VT_HDAY(hs))
+		call pargi (VT_HYEAR(hs))
+	    call printf ("time = %d seconds since midnight\n")
+		call pargi (VT_HTIME(hs))
+	    call printf ("wavelength = %d\nobservation type = %d\n")
+		call pargi (VT_HWVLNGTH(hs))
+		call pargi (VT_HOBSTYPE(hs))
+	    call flush (STDOUT)
+	}
+
+	if (BYTE_SWAP2 == YES)
+		call bswap2 (hbuf, 1, hbuf, 1, SZ_VTHDR*SZB_SHORT)
+	call write (outfd, hbuf, SZ_VTHDR*SZB_SHORT/SZB_CHAR)
+	if (fstati (outfd, F_NCHARS) !=  SZ_VTHDR*SZB_SHORT/SZB_CHAR)
+	    call error (0, "error when writing header")
+	call flush (outfd)
+end
+
+
+# PUTSUBRASTER -- Write data to the output from this subraster, look
+# in the table to see if each subswath should be filled with data or zeros.
+
+procedure putsubraster (outfd, array, nx, ny, table, subraster)
+
+int	outfd			# output file descriptor
+int	subraster		# subraster number
+int	nx			# size of the data array (x)
+int	ny			# size of the data array (y)
+short	array[nx, ny]		# data array
+short	table[SZ_TABLE]		# subswath lookup table
+
+int	i, subswath, tableindex
+pointer	sp, bufpointer
+errchk	writesubswath
+
+begin
+	call smark (sp)
+	call salloc (bufpointer, ny, TY_SHORT)
+
+	do subswath = nx, 1, -1 {
+	    tableindex = (subraster - 1) * nx + ((nx + 1) - subswath)
+	    if (table[tableindex] == IS_DATA) {
+		do i = ny, 1, -1
+		     Mems[bufpointer + ny - i] = array[subswath,i]
+		call writesubswath (outfd, Mems[bufpointer], ny)
+	    } else
+		next
+	}
+
+	call sfree(sp)
+end
+
+
+# WRITESUBSWATH -- Write data to file whose logical unit is outfd.
+# Swap the bytes in each data word.
+
+procedure writesubswath (outfd, buf, buflength)
+
+int	outfd			# output file descriptor
+int	buflength		# length of data buffer
+short	buf[buflength]		# data buffer
+
+int	fstati()
+errchk	write
+
+begin
+	if (BYTE_SWAP2 == YES)
+	    call bswap2 (buf, 1, buf, 1, buflength * SZB_SHORT)
+	call write (outfd, buf, buflength*SZB_SHORT/SZB_CHAR)
+	if (fstati (outfd, F_NCHARS) != buflength*SZB_SHORT/SZB_CHAR)
+	    call error (0, "eof encountered when reading subswath")
+end
diff --git a/noao/imred/vtel/x_vtel.x b/noao/imred/vtel/x_vtel.x
new file mode 100644
index 00000000..942afcf0
--- /dev/null
+++ b/noao/imred/vtel/x_vtel.x
@@ -0,0 +1,16 @@
+task	readvt		= t_readvt,
+	writevt		= t_writevt,
+	unwrap		= t_unwrap,
+	quickfit	= t_quickfit,
+	getsqib		= t_getsqib,
+	putsqib		= t_putsqib,
+	rmap		= t_rmap,
+	merge		= t_merge,
+	destreak	= t_destreak,
+	trim		= t_trim,
+	dicoplot	= t_dicoplot,
+	vtexamine	= t_vtexamine,
+	tcopy		= t_tcopy,
+	mscan		= t_mscan,
+	syndico		= t_syndico,
+	pimtext		= t_pimtext