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plratio stsdas.hst_calib.synphot



plratio -- Plot the ratio of observed to predicted spectrophotometry and photometry.


plratio obsmode spectrum form spfile


This task will calculate and plot the ratio of observed spectrophotometric data to a synthetic HST spectrum. It also optionally plots the ratios of photometric observations to the synthetic photometry computed from the synthetic HST spectrum. This task produces plots similar to those produced by plspec, except that it plots ratios of the observed data (the spectrophotometric and photometric tables) to the predicted data (the combination of obsmode and spectrum) instead of plotting the data themeselves. The task also plots chi quared error of the fit, and the bias and root mean squared errors in magnitudes.

Spectrophotometric ratios are plotted as histograms if the form is counts or obmag and as continuous curves if the form is not. Photometric ratios are plotted as horizontal lines whose midpoints are marked by a circle. The horizontal line has its x value set to the pivot wavelength of the observation mode passband and its y value set to the ratio of the effective stimulus taken from the photometric table to the effective stimulus calculated from the spectrum and obsmode. The length of the line is set to the full width half maximum of the equivalent gaussian of the observation mode passband. The observation mode passbands are overplotted at the base of the plot.

Which plots are produced are controlled by the task parameters spfile and pfile. If spectophotometric ratios are not desired, spfile should be set to "none" or left blank. If photometric ratios are not desired, pfile should be set to "none" or left blank. Spectrophotometric ratios are computed for every combination of synthetic spectra and spectrophotometric files. Synthetic spectra are matched to rows in the photometic table by matching the obsmode and spectrum parameters to the OBSMODE and TARGETID columns in the photometric table. The strings must be exactly the same in order to make the match.

The obsmode string may be set to "none". In this case, the task uses an observation mode that is one over the wavelength set of the spectrum. If photometric errors are being computed, however, the form must be set to counts or obmag, because otherwise the task cannot compute the effective stimulus of the synthetic spectrum.


obsmode [string]
This is a sequence of commands that creates the synthetic passband. The name of a command file can be passed to obsmode by preceding the file name with a "@" character, for example, "@filename".

Each command may either be a simple bandpass, which is represented by a comma separated string of keywords uniquely specifying an observing mode of the telescope or a more complex command, described in the help file for calcband. The keywords which make up the observing mode are explained further in the obsmode task. If this parameter is left blank or set to "none", a default observation mode that is everywhere one will be used.

spectrum [string]
This is a sequence of commands that create the synthetic spectrum. The commands can be placed in a file, whose name is passed to this parameter, preceded by a "@" character, e.g., @filename. Each line in this command file is treated as a separate set of commands. If this parameter is left blank or set to none, no spectra will be plotted.

The commands that can be passed to this parameter are described in detail in the help file for the calcspec task.

form [string]
Desired output form. The following forms are recognized:

	FNU		erg / s / cm^2 / Hz
	FLAM		erg / 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
	VEGAMAG		-2.5 log_10 (F/F_vega)
	OBMAG		-2.5 log_10 (COUNTS)
	JY		10^-23 erg / s / cm^2 / Hz
 	MJY		10^-26 erg / s / cm^2 / Hz

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.
(vzero = " ") [string]
A list of values to substitute for variable zero. Each value in the list is substituted in turn for the string $0 wherever it occurs in the input spectrum. The values must be real numbers. Using vzero is the equivalent of placing the input spectrum several times in a file, with each spectrum containing one of the values in the list. The list may contain single values or ranges. The endpoints of the ranges are separated by a dash. An optional step size follows the range, preceded by the letter x. If the step size is not present, the step size defaults to 1 or -1, depending on the order of the endpoints. The following table gives several examples of valid lists

	.1,.2,.3,.4	A list of single values
	.1-.4x.1	The same list expressed as a range
	-1 - -4 	A range with an implicit step size of -1
	1-9,10-20x2	A list of more than one range
spfile [file name]
A table or ascii file containing spectrophotometry data; a list of one or more files can be specified using the "@filename" syntax. If the value of this parameter is set to "none" or blank, the ratio of the spectrophotometric data to the theoretical spectra will not be plotted. In this case, the pfile parameter should have a value other than "none". The spectrophotometric table can have the columns WAVELENGTH, FLUX, STATERROR, and FWHM. The STATERROR and FWHM columns can be missing or all INDEF. The WAVENGTH and FLUX columns contain the wavelength and values of flux at that wavelength, respectively. The STATERROR and FWHM collumns contain the respective errors of the FLUX and WAVELENGTH columns. If the spectrophotometry file is an ascii file, the first through fourth columns are the wavelength, flux, staterror, and flux and the third and fourth columns are optional.
(pfile = "none") [string]
A file containing photometric data, generated by the calcphot task. A list of files can be passed as "@filename". If the value of this parameter is "none" or blank, the ratio of the photometric data to the photometric data generated from the synthtic spectra will not be plotted. A table generated by calcphot will have column names DATUM, FORM, OBSMODE and TARGETID. These columns contain the effective stimulus, its form, the observation mode, and spectrum passed to calcphot. If the photometric file is an ascii file, the file will have four columns in the order specified above. This task matches the photometic data to the data generated from the spectra by the strings in the OBSMODE and TARGETID columns.
(left = INDEF) [real]
Minimum wavelength to plot. If set to INDEF, the task will set it to the minimum wavelength in the wavelength set.
(right = INDEF) [real]
Maximum wavelength to plot. If set to INDEF, the task will set it to the maximum wavelength in the wavelength set.
(bottom = INDEF) [real]
Minimum flux value to plot. If set to INDEF, the task will set it to the minimum value of the ratios.
(top = INDEF) [real]
Maximum flux value to plot. If set to INDEF, the task will set it to the maximum value of the ratios.
(append = no) [boolean]
Append results to an existing plot?
(ltype = "solid") [string]
The line type to be used for plotting the mode1 passband. The allowed values are: clear, solid, dashed, dotted, and dotdash.
(device = "stdgraph") [string]
Send output to the designated device.
(wavetab = "") [file name]
Name of an optional wavelength table or file. An appropriate table can be generated by using the genwave task. If a table is used, the wavelength column name must be "WAVELENGTH". If an ASCII file is used the first column is taken to be the wavelength column. The subdirectory 'synphot$data has ASCII wavelength tables useful for specific HST passbands.

If no wavelength table is specified, the task generates a wavelength set which covers the range between the left and right plot limits. If there is no wavelength table, and plot limits are not specified, a default wavelength set is used. The default wavelength set covers the wavelength range where the spectrum is non-zero. Wavelengths are spaced logarithmically over this range. If more than one spectrum is plotted, the range is computed based on the first spectrum. If the wavelength range of the spectra differ significantly, a wavelength table should be specified explicitly or plot limits should be set.

(refdata = " ") [pset name]
Parameter set for reference data used in calculations. The following parameters are stored in this set.

     area = 45238.93416:  HST telescope area in cm**2.

     grtbl = "mtab$*.tmg":  HST graph table.  Uses the
	       most recent version by default.

     cmptbl = "mtab$*.tmc":  Instrument component table.  
                The most recent version is used by default.

(device = "stdgraph") [real]
Send output to the designated device. "stdgraph" plots to the screen, "stdplot" sends output to your default laser printer.


1. Calculate the ratio of a 15000 K blackbody spectrum to that of Vega. We first renormalize the blackbody spectrum to have magnitude 0 in the V passband (to match the absolute flux level of Vega). The ratio is plotted in units of flam.

sy> plratio none "rn(bb(15000),band(v),0,vegamag)" flam \
>>> crcalspec$alpha_lyr_stis_002.fits


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



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