path: root/noao/imred/quadred/src/quad/doc/quadman.hlp

.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