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simnoise stsdas.hst_calib.synphot.simulators


NAME · USAGE · DESCRIPTION · PARAMETERS · EXAMPLES_ · REFERENCES
SEE_ALSO

NAME

simnoise -- Two-dimensional HST noise simulator

USAGE

simnoise obsmode output

DESCRIPTION

This task computes a simulated noise image for HST instruments with two-dimensional formats (FOC, WFPC, WFPC2, and NICMOS) for a given observing mode. The output image has the same dimensions as the detector specified by the mode.

The instrument noise is calculated from expression given by the task parameter noise, or if this is set to none, the NOISE parameter stored in the throughput table headers. The noise parameter contains an expression which is used to compute the mean of a Poisson random process. The distribution is sampled and the random noise minus its mean is added to each pixel. If more than one throughput table contains a NOISE parameter, the strings will be concatenated with the & operator (explained later). The noise expression can contain constants and the three variables t, n, and x. These represent the exposure time, the number of reads, and the pixel flux. Since there is no input image, the flux and thus the value of x, is always zero for this task. So, the mean will always be constant over the image. The noise expression may contain the following operators and functions:

+	addition
-	subtraction or negation
*	multiplication 
/	division
**	exponentiation
&	magnitude (e.g., 3 & 4 = sqrt(3 ** 2 + 4 ** 2) = 5)
log()	natural logarithm
sqrt()	square root

Operator precedence and associativity are the same as in Fortran, though these can be changed by grouping with parentheses. The magnitude operator has lower precedence than any of the other operators.

PARAMETERS

obsmode [string]
Telescope observation mode. The observation mode is a comma- or space-separated list of keywords that specifies a valid light path through the telescope. The observation mode is used to compute the instrument throughput, and select the detector dimensions.
output [string]
Output image name. The result of running this task is a single group image whose dimensions are set according to the detector that is to be simulated.
(input = none) [string]
The name of the optional input file. If this file is present, the noise will be added to the input. If there is no file name or the name is set to "none", the noise will be added to zero.
(noise = none) [string]
If this task parameter is present, the noise expression will be taken from it instead of being read from the noise keyword in the throughput table header. If it is blank or set to none, the noise expression will be read from the throughput tables. The syntax of the throughput tables is explained above.
(exptime = 1.0) [real] [min = 0.0] [max = INDEF]
Observation exposure time in seconds.
(nread = 1) [int] [min = 1, max = INDEF]
Number of detector reads to obtain the final image. Most of the HST instruments offer the capability of taking more than one exposure on a target in order to reduce the detector read noise and/or detect cosmic rays. This parameter will be used in conjuction with the expression for detector noise to determine the final noise level for the output image.
(wavetab = "none") [string]
Wavelength table An appropriate table can be generated by using the `genwave' task. If a binary table is used, the wavelength column name must be WAVELENGTH. If a text table is used the first column is taken to be the wavelength column. The subdirectory synphot$data has text wavelength tables useful for specific HST passbands.

If no wavelength table is specified, a default wavelength set is used. The default wavelength table covers the wavelength range where the telescope and magnitude passbands are non-zero. Wavelengths are spaced logarithmically over this range.

(simbackp = "") [pset]
The parameter file containing the noise and background parameters. These parameter used by this task is:
(seed = 42) [int]
The seed for the random number generator used by the noise model.
(simcatp = "") [pset]
The parameter set containing the file and catalog parameters. The parameter used by this task is:
(detcat = "simulators$data/detectors.dat") [string]
Catalog of detector dimensions. The catalog is a table containing four columns: the observation mode, the pixel scale, the number of pixels in the X dimension, and the number of pixels in the Y dimension. If the catalog is a binary table, the columns are named OBSMODE, SCALE, NX and NY. If it is a text table, they are the first through fourth columns. The row in the catalog is selected if the input observation mode is a superset of the catalog observation mode. If the table is a binary table, the units of the detector scale are read from the SCALE column units. If the table is a text table, the units are assumed to be arcseconds.
(refdata = "") [pset]
The parameter set for reference data used in calculations. This pset contains the following parameters:
(area = 45238.93416) [real]
HST telescope area in cm**2.
(grtbl = "mtab$*.tmg") [string]
HST graph table. By default, this uses the most recent version.
(cmptbl = "mtab$*.tmc") [string]
Instrument component table. By default, this uses the most recent version.

EXAMPLES

1. Simulate the noise seen by detector 2 of the WFPC-2 camera, using the F555W filter:

    cl> simnoise wfpc2,f555w,2 output.hhh

REFERENCES

Written by Bernie Simon.

SEE ALSO

simimg, simbackgd, obsmode


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