\O=NOAO/IRAF V2.5 valdes@lyra Mon 15:42:35 12-Oct-87
\T=vt640
\G=vt640
clear\n\{%V-%!200\}
\n\{
			CCD REDUCTION DEMONSTRATION

    In this demonstration we are going to make some (artificial) CCD
    observations which we will reduce using the CCDRED package.  The
    dome is opening and we are ready to begin observing...\}
\n\{%V-\}
unlearn\sccdred;unlearn\sccdtest\n\{	# Initialize parameters and data...\}
imdelete\s%B%%*.??h\sv-\n\{%V-\}
imrename\sB*.??h\s%B%%*.??h\sv-\n\{%V-\}
delete\sDemo*\sv-\n\{%V-\}
\n\{%V-\}
setinstrument\sdemo\sreview-\n\{		# Set instrument parameters...\}
lpar\sartobs\n\{				# List observing parameters...\}
artobs\sZero\s0.\szero\n\{      		# Observe zero level images...\}
\n\{%V-\}
artobs.skyrate=0\n\{			# Observe a long dark count...\}
artobs\sDark\s1000.\sdark\n\{%V-\}
\n\{%V-\}
artobs.filter="V"\n\{			# Observe V flat fields...\}
artobs.skyrate=2000\n\{%V-\}
artobs\sFlatV\s1.\sflat\n\{%V-\}
\n\{%V-\}
artobs.filter="B"\n\{			# Observe B flat fields...\}
artobs.skyrate=1000\n\{%V-\}
artobs\sFlatB\s1.\sflat\n\{%V-\}
\n\{%V-\}
artobs.filter="V"\n\{			# Observe objects...\}
artobs.skyrate=100\n\{%V-\}
artobs\sobs001\s10.\sobject\simdata=dev$pix\n\{%V-\}
artobs.filter="B"\n\{%V-\}
artobs\sobs002\s30.\sobject\simdata=dev$pix\n\{%V-\}
dir\n\{					# Check directory of observations...\}
clear\n\{%5000				# Continue...\}
\n\{
			INSTRUMENT SETUP

    Because there are a variety of instruments, observatories, and data
    formats there are many parameters.  To set all of these conveniently
    there is a task which reads setup files prepared by the observing
    staff.  The setup task:
	1.  Defines an instrument header translation file which
	    translates the image header parameters to something
	    the CCDRED package understands.  This is an important
	    feature of the package.
	2.  It runs a setup script which sets parameters and performs
	    other functions desired by the observing staff.
	3.  The user is then given the opportunity to modify the
	    package and processing parameters...\}
\n\{%V-\}
setinstrument\smode=m\n\{		# Set demo instrument parameters...\}
demo\r
\{%1000\}^Z
\{%1000\}^Z
\{%1000\}\r
\r
\r
\r
\r
\r
\r
\r
\r
\r
\r
\r
\r
\r
\r
\r
\r
\r
Zero\r
Dark\r
Flat*.??h\r
^Z
clear\n\{%5000				# Continue...\}
\n\{
			PROCESS OBSERVATIONS

    We are now ready to process our observations.  The processing steps we
    have selected are to replace bad pixels by interpolation, fit and
    subtract a readout bias given by an overscan strip, subtract the zero
    level calibration image, scale and subtract a dark count calibration,
    divide by a flat field, trim the image of the overscan strip and border
    columns and lines.  The task which does this is "ccdproc".  The task is
    expert at reducing CCD observations easily and efficiently.  It checks
    the image types, applies the proper filter flat field, applies the
    proper part of the calibration images to subsection readouts, does only
    the processing steps selected if not done previously, and automatically
    processes the calibration images as needed.  As before we simply specify
    all the images and the task selects the appropriate images to process.
    Watch the log messages to see what the task is doing...\}
\n\{%V-\}
ccdproc\sobs*.??h\n\{			# Process object images...\}
\n\{%V-\}
\{%V-\}q0,+,\r
NO\n\{%V-\}
\n\{
    That's it!  We're done.  Now lets check the results.  The "ccdlist"
    listing will show the processing status and the images are now smaller
    and of pixel datatype real.  The CCDSEC parameter identifies the relation
    of the image to the actual CCD pixels of the detector...\}
\n\{%V-\}
ccdlist\sobs*.??h\sccdtype=object\n\{		# List short CCD status...\}
ccdlist\sobs001\sl+\n\{     			# List long CCD status...\}
imhead\sobs001\sl+\n\{     			# List object image header...\}
dir\n\{     				# Check the data directory...\}
\n\{%V-
    We specified that the original images be saved by using the prefix B.
    We are also left with a text log file, a metacode file containing the
    fits to the overscan regions, and a file which maps the filter subset
    strings to short identifiers used in CCDLIST and when creating the
    combined images "FlatV" and "FlatB".  You may look through these files,
    or use GKIMOSAIC to examine the metacode file, now if you want.
\}