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.help flatcombine Aug91 noao.imred.ccdred
.ih
NAME
flatcombine -- Combine and process flat field images
.ih
USAGE
flatcombine input
.ih
PARAMETERS
.ls input
List of flat field images to combine. The \fIccdtype\fR parameter
may be used to select the flat field images from a list containing all
types of data.
.le
.ls output = "Flat"
Output flat field root image name. The subset ID is appended.
.le
.ls combine = "average" (average|median)
Type of combining operation performed on the final set of pixels (after
rejection). The choices are
"average" or "median". The median uses the average of the two central
values when the number of pixels is even.
.le
.ls reject = "avsigclip" (none|minmax|ccdclip|crreject|sigclip|avsigclip|pclip)
Type of rejection operation. See \fBcombine\fR for details.
.le
.ls ccdtype = "flat"
CCD image type to combine. If no image type is given then all input images
are combined.
.le
.ls process = yes
Process the input images before combining?
.le
.ls subsets = yes
Combine images by subset parameter? If yes then the input images are
grouped by subset parameter and each group combined into a separate output
image. The subset identifier is appended to the output and sigma image
names. See \fBsubsets\fR for more on the subset parameter. This is generally
used with flat field images.
.le
.ls delete = no
Delete input images after combining? Only those images combined are deleted.
.le
.ls clobber = no
Clobber existing output images?
.le
.ls scale = "mode" (none|mode|median|mean|exposure)
Multiplicative image scaling to be applied. The choices are none, scale
by the mode, median, or mean of the specified statistics section, or scale
by the exposure time given in the image header.
.le
.ls statsec = ""
Section of images to use in computing image statistics for scaling.
If no section is given then the entire region of the image is
sampled (for efficiency the images are sampled if they are big enough).
.le
.ce
Algorithm Parameters
.ls nlow = 1, nhigh = 1 (minmax)
The number of low and high pixels to be rejected by the "minmax" algorithm.
.le
.ls nkeep = 1
The minimum number of pixels to retain or the maximum number to reject
when using the clipping algorithms (ccdclip, crreject, sigclip,
avsigclip, or pclip). When given as a positive value this is the minimum
number to keep. When given as a negative value the absolute value is
the maximum number to reject. This is actually converted to a number
to keep by adding it to the number of images.
.le
.ls mclip = yes (ccdclip, crreject, sigclip, avsigcliip)
Use the median as the estimate for the true intensity rather than the
average with high and low values excluded in the "ccdclip", "crreject",
"sigclip", and "avsigclip" algorithms? The median is a better estimator
in the presence of data which one wants to reject than the average.
However, computing the median is slower than the average.
.le
.ls lsigma = 3., hsigma = 3. (ccdclip, crreject, sigclip, avsigclip, pclip)
Low and high sigma clipping factors for the "ccdclip", "crreject", "sigclip",
"avsigclip", and "pclip" algorithms. They multiply a "sigma" factor
produced by the algorithm to select a point below and above the average or
median value for rejecting pixels. The lower sigma is ignored for the
"crreject" algorithm.
.le
.ls rdnoise = "0.", gain = "1.", snoise = "0." (ccdclip, crreject)
CCD readout noise in electrons, gain in electrons/DN, and sensitivity noise
as a fraction. These parameters are used with the "ccdclip" and "crreject"
algorithms. The values may be either numeric or an image header keyword
which contains the value.
.le
.ls pclip = -0.5 (pclip)
Percentile clipping algorithm parameter. If greater than
one in absolute value then it specifies a number of pixels above or
below the median to use for computing the clipping sigma. If less
than one in absolute value then it specifies the fraction of the pixels
above or below the median to use. A positive value selects a point
above the median and a negative value selects a point below the median.
The default of -0.5 selects approximately the quartile point.
See \fBcombine\fR for further details.
.le
.ls blank = 1.
Output value to be used when there are no pixels.
.le
.ih
DESCRIPTION
The flat field images in the input image list are combined. If there
is more than one subset (such as a filter or grating) then the input
flat field images are grouped by subset and an combined separately.
The input images may be processed first if desired. However if all
zero level bias effects are linear then this is not necessary and some
processing time may be saved. The original images may be deleted
automatically if desired. The output pixel datatype will be real.
This task is a script which applies \fBccdproc\fR and \fBcombine\fR. The
parameters and combining algorithms are described in detail in the help for
\fBcombine\fR. This script has default parameters specifically set for
flat field images and simplifies the combining parameters. There are other
combining options not included in this task. For these additional
features, such as thresholding, offseting, masking, and projecting, use
\fBcombine\fR.
.ih
EXAMPLES
1. The image data contains four flat field images for three filters.
To automatically select them and combine them as a background job
using the default combining algorithm:
cl> flatcombine ccd*.imh&
The final images are "FlatV", "FlatB", and "FlatR".
.ih
SEE ALSO
ccdproc, combine, subsets
.endhelp
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