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pedsub stsdas.hst_calib.nicmos


NAME · USAGE · DESCRIPTION · PARAMETERS · EXAMPLES · REVISIONS
BUGS · REFERENCES · SEE_ALSO

NAME

pedsub -- subtract pedestal signal from a NICMOS image

USAGE

pedsub input output

DESCRIPTION

The pedsub task measures and removes an estimate of the quadrant-dependent residual bias (or "pedestal") in a NICMOS image. The input image to the task must be fully calibrated, including zero-read subtraction, dark subtraction, linearization, and flatfielding. Unlike the pedsky task, which only works well on images containing few sources and large regions of blank sky, this task can be used effectively on most any NICMOS image, regardless of source content. However, some experimentation with parameter settings may be necessary in order to achieve optimum results for different types of fields. Best use of the various settings are briefly described below.

Pedsub runs on a single science image (i.e. not on all the separate readouts of a NICMOS MULTIACCUM file). It operates only on the [SCI,1] extension, which is appropriate when the task is run on, e.g., the _cal type images that are the final product of the "calnica" calibration pipeline.

The task takes as input a calibrated NICMOS image and the image that was used to apply the flatfield correction during the calibration process. It then estimates, for each quadrant of the image, the size of any constant bias signal that may be present in the data, but was not subtracted before flatfielding was applied. An output image is created that has the best-fitting constant pedestal subtracted. An algorithm that attempts to remove any remaining DC offsets between image quadrants is also included.

The task assumes that the calibrated signal in each pixel (C) is composed of the intrinsic signal from sky and sources (I), plus the pedestal (P) times the flatfield value for the pixel (F):

  C = I + P*F

The task tries to determine the pedestal value, P, by exploiting the fact that the additional term P*F in the calibrated image introduces a spread in the pixel values in the image. The task loops over a range of trial pedestal values, T, and for each value it generates a trial image I_T = C - T*F, and then measures the spread in pixel values in the trial image I_T. The trial value that produces the minimum spread in pixel values is taken as the best guess for the pedestal value. This process is performed independently for each image quadrant.

A filtering operation can optionally be applied to each trial image in order to remove unwanted features or spatial frequencies that might bias the calculation of the pixel value spread. The task provides various choices for the filtering operation, which is set via the task parameter "filter":

filter = "none"
No filtering is applied to the trial image, which implies that all Fourier frequencies in the trial image are used to compute the spread. This approach is likely to work well only if the image is almost completely free of sources.
filter = "median"
A ring-median filter is applied to the trial image (i.e. every pixel is replaced by the median value in a ring of pixels around it). This implies that all pixel-to-pixel variations are removed, and only the low Fourier frequencies in the trial image are used. This approach may work well for a field that contains only small sources (stars or faint, small galaxies). The inner and outer radii of the median filter annulus are set by the parameters "minbox" and "maxbox".
filter = "mask"
This option produces an unsharp mask version of the trial image, by first applying a ring-median filter (as in the previous option) and then subtracting the median-filtered image from the unfiltered trial image. This implies that low frequency structure is removed and only pixel-to-pixel variations remain. Thus only high frequency information in the trial image is used. This approach may work well for any field, even if it contains stars or galaxies, or even if it contains a galaxy that fills the whole image.

The spread in pixel values in a trial image is taken to be the Gaussian dispersion of the pixel value histogram. The pixel values are sorted into ascending order, binned into a histogram, and a Gaussian is then fitted to the histogram. This approach helps minimize sensitivity to bad pixels and outliers, because the Gaussian fit is sensitive primarily to only the core of the pixel histogram, and not to its wings.

Known bad pixels and/or pixels containing source signal can also be explicitly rejected from the pixel spread computations through the use of the pixel masking feature (parameter "dqon=yes"), which rejects pixels based on their Data Quality bit settings in the input image. Furthermore, the "statregions" pset can be used to specify limits to the regions of each quadrant used in the pixel spread computation. This is useful, for example, to exclude the vignetted regions in the lower quadrants (1 and 2) of NICMOS camera 2 and 3 images.

The search for the optimal pedestal value in each image quadrant is performed in two phases. First, a "quick and dirty" estimate of the pedestal value is determined by using the Brent minimization algorithm to search for the minimum in the function pixel spread vs. pedestal value. This "quick'n'dirty" result should be interpreted with some care, since numerical errors may make the function jagged near its minimum, and the pedestal value arrived at may be due to a local minimum. A second phase is then applied to refine the initial pedestal estimate. The second phase consists of computing the pixel spread in a set of trial images using a range of pedestal values centered on the initial estimate. The number of pedestal values and their spacing are set by the parameters "nrefine" and "refstep", respectively. A smooth polynomial of order "reforder" is fitted to these trial values, and the minimum of this polynomial is determined and adopted as the best guess for the pedestal value. If "dorefine=no", this second phase in the pedestal estimation is skipped.

After the best-fitting pedestal value has been determined and subtracted from each image quadrant, differences in the DC levels between the quadrants may still exist. The task includes an algorithm for removing these differences and is performed if "doquadeq=yes". Offsets between the quadrants are determined by sampling the pixel values in each row or column near the borders of adjoining quadrants. If "eqorder>=0", the algorithm fits a polynomial of order "eqorder" to pixels in the range "eqpix1" through "eqpix2" on each side of a quadrant boundary, extrapolates the fit to the border position, and then computes the difference between the extrapolated values from either side of the border. If "eqorder=-1" or "eqorder=-2", the median or the mode, respectively, of the sampled pixel values will be computed, rather than fitting a polynomial, and the difference in these values across the border is computed. This is done for every row or column along each border.

The polynomial fit option tends to work best for images that have bright sources on or near the quadrant boundaries, where either the source itself (e.g. a large galaxy) or the wings of the PSF (e.g. stars) result in large signal gradients near the boundaries. The median and mode methods, on the other hand, often produce better results for images that are sparsely populated, due to the fact that the polynomial fits can be easily biased by background noise in the image.

The differences between the quadrants are minimized by attempting to minimize the high-frequency Fourier power along the quadrant borders. The Fourier power is proportional to the squared differences in intensity extracted (as outlined above) at each side of a border. The algorithm uses the "amoeba" (downhill simplex) minimization method to search for the set of DC offsets that minimize the power estimator. The offsets that simultaneously minimize the power between all four quadrants are added to each image quadrant.

If "eqflat=no", only the constant offset values are added to each quadrant. If "eqflat=yes", the constant multiplied by the flatfield is added. When using this option, the fit to the offsets is iterated 3 times, to take into account the fact that the flatfield may not be normalized exactly to unity in the region around the quadrant boundaries. The best setting of this option for particular images often requires some experimentation.

The pedestal values determined by the task are stored in the output image header in the keywords "PEDQUAD1" through "PEDQUAD4". The DC quadrant offsets, if computed, are stored in the output image header in the keywords "DCQUAD1" through "DCQUAD4". The quadrant numbering scheme is as follows:

---------
| 3 | 4 |
---------
| 1 | 2 |
---------

The pedsub task complements and supplements the pedstal removal techniques available in the pedsky task. While pedsky will only work well for images which are relatively blank, the image filtering techniques employed in this task should make it relatively insensitive to sources. The "filter=none" mode of operation utilizes techniques roughly equivalent to those in pedsky and yields comparable results when applied to images that have few sources. The "filter=mask" mode can be applied to any image, regardless of source content, but is particularly useful for images of crowded stellar fields and large, extended sources.

PARAMETERS

input [file]
Input image name(s). This will normally be a single IMSET file (_cal type) that has been processed through "calnica". The full file name must be given.
output [file]
Output image name(s). Must be a full file name specification and the numbers of input and output images must be equal.
(filter = "mask") [string, allowed values: |none|median|mask]
Filter type for trial images. "None" = no filtering, "median" = ring-median filter, "mask" = unsharp mask (image minus median-filtered image).
(minbox = INDEF) [integer]
Inner box radius, in pixels, for median filter. Only used if "filter" is not equal to "none". If INDEF, default value is 6 for "filter=median" and 1 for "filter=mask".
(maxbox = INDEF) [integer]
Outer box radius, in pixels, for median filter. Only used if "filter" is not equal to "none". If INDEF, default value is 8 for "filter=median" and 2 for "filter=mask".
(dorefine = yes) [boolean]
Compute refined pedestal estimate after initial "quick'n'dirty" estimate?
(nrefine = 41) [integer, min=3]
Number of trial pedestal values to use in refinement phase. Only used if "dorefine=yes". Should be an odd number.
(refstep = INDEF) [real]
Step size between trial pedestal values in refinement phase. Only used if "dorefine=yes". If INDEF, the maximum of either 3% of the initial pedestal value or 0.5 DN will be used.
(reforder = 5) [integer, min=0, max=10]
Order of the polynomial fit used in the refinement phase. Only used if "dorefine=yes".
(doquadeq = yes) [boolean]
Equalize quadrant DC levels after subtracting pedestal values?
(eqorder = 1) [integer, min=-2, max=7]
Order of polynomial fit used in quadrant equalization. If "eqorder=-1" the median pixel value is computed; if "eqorder=-2" the mode is computed. Only used if "doquadeq=yes".
(eqpix= 2) [integer, min=1, max=128]
First pixel to use in each row/column for quadrant equalization. Pixels are counted outwards from quadrant boundary, starting with 1. Only used if "doquadeq=yes".
(eqpix= 10) [integer, min=1, max=128]
Last pixel to use in each row/column for quadrant equalization. Pixels are counted outwards from quadrant boundary, starting with 1. Only used if "doquadeq=yes".
(eqflat = yes) [boolean]
Apply flatfield to quadrant equalization offset values? Only used if "doquadeq=yes".
(flatfield = "") [file]
Name of the flatfield file to use for pedestal subtraction. If left blank, the task will read the name of the flatfield file from the FLATFILE keyword in the input image header.
(statregions = "") [pset]
Pset containing image section specifications for computing statistics. The "quad1" through "quad4" parameters specify the boundaries to use for each quadrant when computing the pixel spread in trial images. The "statsec" parameter is not used at this time. See the description section above for the quadrant numbering scheme.
(dqon = yes) [boolean]
Turn on pixel masking by data quality bits? If yes, then pixels with DQ bits corresponding to those listed in the dqpar pset (see below) will not be used in any statistical computations.
(dqpar = "") [pset]
Data quality bits parameter set. Pixels with DQ bits corresponding to those bits turned on in this pset will be rejected from statistical computations if "dqon=yes".
(logfile = "") [file]
Processing log file name. If not null, a text file is created containing a log of information generated during processing.
(verbose = yes) [boolean]
Verbose output during task execution?

EXAMPLES

1. Estimate and subtract pedestal from the calibrated image n3z302g7m_cal.fits, storing the resulting image in the file n3z302g7m_ped.fits. The flatfield image named in the input image header is used, unsharp masking is applied to the trial images, and the inter-quadrant DC levels are equalized by adding a constant multiplied by the flatfield:

ni> pedsub n3z302g7m_cal.fits n3z302g7m_ped.fits

2. Correct the same image, but use the median value of border pixels to determine the quadrant equalization:

ni> pedsub n3z302g7m_cal.fits n3z302g7m_ped.fits eqorder=-1

3. Correct the image n4ls01i1q_cal.fits without applying any filtering to the trial images and also do not multiply the quadrant equalization constants by the flatfield:

ni> pedsub n4ls01i1q_cal.fits n4ls01i1q_ped.fits filter=none eqflat-

4. Process the images listed in the file "cal.lis", using all default parameter settings. The corresponding list of output file names is contained in the file "ped.lis":

ni> pedsub @cal.lis @ped.lis

REVISIONS

Version 23-Jun-(STSDAS v2.2)
First release of the task.

BUGS

REFERENCES

Original core algorithms based on the "unpedestal" program, which was written by Roeland van der Marel and David Zurek (STScI). Ported to the C language and the IRAF environment, with further algorithm refinements, by Howard Bushouse (STScI).

SEE ALSO

pedsky, biaseq


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