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countrate stsdas.hst_calib.synphot


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

NAME

countrate -- Evaluate the count rate for a target and observing mode.

USAGE

countrate instrument

DESCRIPTION

This task computes the predicted flux for a specified source spectrum and telescope observing mode. At the user's option, it can also create an output spectrum containing the flux as a function of wavelength. The observing mode of the HST is specified in several task parameters. These are instrument, detector, spec_elem, and aperture. The instrument must always be specified, but the other three parameters may be blank, depending on which instrument and instrument configuration is used. If you set the instrument to "hrs" or "stis", you should also specify cenwave, the central wavelength of the spectrum. This parameter has no effect on any of the other instruments. More than one observing mode keyword may be specified in a task parameter by separating the keywords with a comma. The obsmode task has more information on the legal observing mode keywords.

The target spectrum is specified in the spectrum' parameter. The crcalspec$ and crgrid$ directories contain some tables which can be used as source spectra. The spectrum may also be one of several functions. The functions have the form of a function name followed by one or more arguments in parentheses. Here are a few of the supported functions. More are described in the help for calcspec.

bb(temp)		A black body at the specified temperature
hi(temp,colden)		Emission spectrum of an LTE slab of hydrogen at 
			the specified temperature and column density
pl(refval,exp,units)	Powerlaw spectrum of the form 
			(wavelength/refval)**exp

The magnitude parameter is used to normalize the spectrum to a chosen absolute flux level by specifying an integrated broadband magnitude for the spectrum. This parameter has two words. The first is the integrated magnitude, in units of magform. The second is the passband over which the magnitude is integrated. This may be fully specified in the usual syntax (eg, "johnson,V" or "sdss,g") or abbreviated by specifying a single letter. If no system name is given for any of the UBVRIJHK bands, the defaults are Johnson UBV, Cousins RI, and Bessell JHK.

The output table is specified by the parameter output. If this parameter is set to "none" (the default) or left blank, no output table will be created. Otherwise, the task will create a table of wavelength versus flux.

PARAMETERS

spectrum [string]
A file name or function string specifying the spectrum to be evaluated. If this parameter is a file name, it must be a table containing two columns, WAVELENGTH and FLUX. The WAVELENGTH column must have units of Angstroms and must be in ascending or descending order. If it is a function string, the first word in the string gives the functional form of the spectrum and the remaining words are a parentehsized list of arguments to the function. The following functions are a few of the supported functions:

bb(temp)		A black body at the specified temperature
hi(temp,colden)		Emission spectrum of an LTE slab of hydrogen at 
			the specified temperature and column density
pl(refval,exp,unit)	Powerlaw spectrum of the form 
			(wavelength/refval)**exp
magnitude [string]
The integrated magnitude of the spectrum. The first word gives the magnitude in units of VEGAMAG and the second word specifies the desired passband. The passband is generally abbreviated with a single letter, although it may be fully specified in the usual syntax (eg, "johnson,V" or "sdss,g"). If no system name is given for any of the UBVRIJHK bands, the defaults are Johnson UBV, Cousins RI, and Bessell JHK. If this parameter is left blank or set to "none", the spectrum will not be renormalized.
instrument [string]
The name of the telescope instrument used in the observation.
(detector = " ") [string]
The name of the instrument detector, if there is more than one available for the instrument being used.
(spec_elem = " ") [string]
The name of the spectral elements, such as filters or gratings, used in the observation.
(aperture = " ") [string]
The name of the instrument aperture, if there is more than one available for the instrument being used.
(cenwave = INDEF) [real] [min = 1.0, max = 200000.]
The central wavelength of the observation, in Angstroms. The output spectrum will be centered on this wavelength. If this parameter is set to INDEF, the output spectrum will contain the entire wavelength range that the observation mode covers. This parameter only effects the HRS and STIS, because they are the only instrument where the detector cannot cover the entire wavelength range of the observation.
(exptime = 1.0) [real] [min = 0.0, max = INDEF]
The exposure time in seconds.
(reddening = 0.0) [real]
The E(B-V) extinction to be applied to the input spectrum. Either the user spectrum or a synthetic spectrum may be modified by this parameter.
(redlaw = "gal1") [string, allowed values: gal1|gal2|gal3|smc|lmc|xgal]
The type of reddening law used to compute the extinction. The task supports three galactic reddening laws (gal1 to gal3) and one law each for the Small Magellanic Cloud (smc), Large Magellanic Cloud (lmc), and extra-galactic objects (xgal). The laws are derived from the following papers.
gal1	Seaton (1979) MNRAS, vol 187, p. 75 
gal2	Savage & Mathis (1979) ARA&A, vol. 17, p. 73-111
gal3	Cardelli, Clayton & Mathis (1989) ApJ vol. 345, p. 245-256
smc	Prevot et al. (1984) A&A, vol. 132, p. 389-392
lmc	Howarth (1983) MNRAS, vol. 203, p. 301
xgal	Calzetti, Kinney and Storchi-Bergmann, (1994) ApJ, vol. 429, p.582
(output = "none") [string]
The name of the output spectrum produced by this task. If this parameter is set to "none" (the default) or a blank string, no output table will be created. Otherwise, it will create an STSDAS table with two columns, WAVELENGTH and FLUX. The WAVELENGTH column will contain wavelengths in Angstroms. The FLUX column will contain the flux at the corresponding wavelengths. The table will also contain the header parameters GRFTABLE, CMPTABLE, OBSMODE, SPECTRUM, and EXPTIME. These will contain the name of the graph table, the component lookup table, the observation mode and spectral expression constructed from the task parameters, and the exposure time.
(form = "counts") [string]
Desired output form for the calculation. The following forms are recognized:

	FNU		ergs / s / cm^2 / Hz
	FLAM		ergs / s / cm^2 / A
	PHOTNU		photons / s / cm^2 / Hz
	PHOTLAM		photons / s / cm^2 / A
	COUNTS		photons / s 
	ABMAG		-2.5 log_10 (FNU)  - 48.60
	STMAG		-2.5 log_10 (FLAM) - 21.10
	OBMAG		-2.5 log_10 (COUNTS)
	VEGAMAG		-2.5 log_10 (F/F_vega)
	JY		10^-23 ergs / s / cm^2 / Hz
 	MJY		10^-26 ergs / s / cm^2 / Hz
Note that if form = counts or obmag, the result will be integrated over the passband and normalized to the collecting area of the HST.

A standard magnitude system is VEGAMAG, for which Vega by definition has magnitude 0 at all wavelengths. The AB and ST magnitude systems are based on constant flux per unit frequency and per unit wavelength, respectively. The zero points for these two systems are set for convenience so that Vega has magnitude 0 in both systems for the Johnson V passband.

(magform = "vegamag") [string]
Form of the magnitude units. The definition of the units is the same as those given above for parameter form.
(wavecat = "crmodewave$wavecat.dat") [string]
The name of the wavelength catalog. The catalog is a table with two columns. The first column contains an observation mode string and the second contains a wavelength table name. This task reads the wavelength catalog and searches for the observation mode that best matches the input observation mode (constructed from task parameters) it then uses the wavelength table to resample the spectrum on the wavelength grid of the detector. If the wavelength catalog is an STSDAS table, the observation mode column must be named OBSMODE and the wavelength table column must be named FILE. If the wavelength catalog is a text table, the observation mode column and the wavelength table columns are the first and second columns, respectively.
(refwave = INDEF) [real] [min = 1.0, max = 200000.]
The reference wavelength in the spectrum. If this parameter is not INDEF, the output will contain the flux at this wavelength.
(verbose = yes) [boolean]
Write calculated quantities to STDOUT?
(flux_tot = INDEF) [real]
The integrated flux combination of observation mode and passband. This is an output parameter, the user should not supply a value.
(flux_ref = INDEF) [real]
The flux at the reference wavelenth. This parameter will be set to INDEF if refwave is set to INDEF. This is an output parameter, the user should not supply a value.
(refdata = " ") [pset name]
A parameter set containing the HST telescope area, the name of the HST graph table, and the name of the component lookup table. These parameters have been placed in a pset because they are common to most of the tasks in this package.

EXAMPLES

1. Compute the results of a 100 second observation of a 17th magnitude G0V star using the HRS with the large science aperture (lsa) and the G270M grating. Store the result in table hrsobs.fits:

  sy> countrate.spectrum = "crgrid$bpgs/bpgs_36.fits"
  sy> countrate.magnitude = "17 v"
  sy> countrate.instrument = "hrs"
  sy> countrate.spec_elem = "g270m"
  sy> countrate.aperture = "lsa"
  sy> countrate.cenwave = 2700.
  sy> countrate.exptime = 100.
  sy> countrate.output = "hrsobs.fits"
  sy> countrate mode=h

REFERENCES

Written by B.Simon based on XCAL code written by Keith Horne

SEE ALSO

calcphot, calcspec


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