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

.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