From 40e5a5811c6ffce9b0974e93cdd927cbcf60c157 Mon Sep 17 00:00:00 2001
From: Joe Hunkeler <jhunkeler@gmail.com>
Date: Tue, 11 Aug 2015 16:51:37 -0400
Subject: Repatch (from linux) of OSX IRAF

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+.help datapars May00 noao.digiphot.apphot
+.ih
+NAME
+datapars -- edit the data dependent parameters
+.ih
+USAGE
+datapars
+.ih
+PARAMETERS
+.ls scale = 1.0
+The scale of the image in user units, e.g arcseconds per pixel.
+All APPHOT distance dependent parameters are assumed to be in units of scale.
+If scale = 1.0 these parameters are assumed to be in units of pixels.
+Most APPHOT users should leave scale set to 1.0 unless they intend to
+compare their aperture photometry results directly with data 
+in the literature.
+.le
+.ls fwhmpsf = 2.5 (scale units)
+The full-width at half-maximum of the point spread function in scale units.
+The DAOFIND, FITPSF and WPHOT tasks and the "gauss" and "ofilter" centering
+algorithms depend on the value of fwhmpsf. APPHOT users can either determine
+a value for fwhmpsf using an external task such as IMEXAMINE, or make use of
+the interactive capabilities of the APPHOT tasks to set and store it.
+.le
+.ls emission = yes
+The features to be measured are above sky. By default the APPHOT package
+considers all features to be emission features. However all the package tasks
+measure absorption features if emission is set to no.
+.le
+.ls sigma = INDEF
+The standard deviation of the sky pixels. The DAOFIND task and the "constant"
+sky fitting algorithm error estimate depend on the value of sigma. APPHOT
+users should set sigma to a value which is representative of the noise
+in the sky background.
+.le
+.ls datamin = INDEF
+The minimum good pixel value. Datamin defaults to -MAX_REAL, the minimum
+floating point number supported by the host computer.  APPHOT users should
+set this parameter if they wish to remove bad data from the sky pixel
+distribution before the sky is fit or if they wish to flag stars with
+bad data in the centering and / or photometry apertures.
+.le
+.ls datamax = INDEF
+The maximum good pixel value. Datamax defaults to MAX_REAL the maximum
+floating point number supported by the host computer.
+APPHOT users should set this parameter if they wish to flag
+saturated stars or stars with bad data in the centering and / or
+photometry apertures.
+.le
+.ls noise = "poisson"
+The noise model used to estimate the uncertainties in the computed APPHOT
+magnitudes. The options are the following:
+.ls poisson
+Poisson statistics in the object and the sky background are used to estimate
+the error in the object measurement.  There are two components to the sky 
+noise measurement the sky noise in the object aperture and the mean error
+in the estimated sky value.
+.le
+.ls constant
+The standard deviation of the sky background is used to estimate the
+error in the object measurement.  There are two components to the error
+estimate the sky noise in the object aperture and the mean error in the
+estimated sky value.
+.le
+
+Most APPHOT users should use the Poisson model appropriate for CCD detectors.
+APPHOT users should also be aware that one or other of the parameters
+gain or epadu must be set correctly in order to compute the magnitude
+errors correctly.
+.le
+.ls ccdread = ""
+The image header keyword defining the readout noise parameter whose units are
+assumed to be electrons.
+.le
+.ls gain = ""
+The image header keyword defining the gain parameter whose units are assumed
+to be electrons per adu.
+.le
+.ls readnoise = 0.0
+The readout noise of the image in electrons.  APPHOT users should set this
+parameter or the ccdread parameter to its correct value before running any
+of the APPHOT tasks.
+.le
+.ls epadu = 1.0
+The gain in electrons per adu.  APPHOT users should set epadu or ain to its
+correct value before running any of the APPHOT tasks in order to insure that
+the magnitude error estimates are correct.
+.le
+.ls exposure = ""
+The image header exposure time keyword. The time units are arbitrary but
+must be consistent for any list of images whose magnitudes are to be compared.
+The computed magnitudes are normalized to 1 timeunit.  Setting the exposure
+parameter will greatly simplify  future reduction steps. The value of exposure
+is recorded in the APPHOT output file.
+.le
+.ls airmass = ""
+The image header airmass keyword.  The airmass parameter is not used
+directly by APPHOT but the airmass value is stored in the output file
+and its presence there will simplify future calibration steps.
+.le
+.ls filter = ""
+The image header filter id keyword.  The filter parameter is not used
+directly by APPHOT but the filter id is stored in the output file
+and its presence there will simplify future calibration steps.
+.le
+.ls obstime = ""
+The image header time of observation keyword. The obstime parameter is not used
+directly by APPHOT but the obstime value is stored in the output file
+and its presence there will simplify future calibration steps.
+.le
+.ls itime = 1.0
+The exposure time for the image in arbitrary units. The APPHOT magnitudes are
+normalized to 1 timeunit  using the value of exposure in the image header
+if exposure is defined or the value of itime.
+.le
+.ls xairmass = INDEF
+The airmass value.  The airmass is read from the image header if airmass
+is defined  or from xairmass. The airmass value is stored in the APPHOT
+output files.
+.le
+.ls ifilter = "INDEF"
+The filter id string. The filter id is read from the image header if filter
+is defined otherwise from ifilter. The filter id is stored in the APPHOT
+output files.
+.le
+.ls otime = "INDEF"
+The value of the time of observation. The time of observation is read from
+the image header if obstime is defined otherwise from otime. The time of
+observation is stored in the APPHOT output files.
+.le
+.ih
+DESCRIPTION
+\fIDatapars\fR sets the image data dependent parameters. These parameters are
+functions, of the instrument optics, the noise characteristics and range of
+linearity of the detector, and the observing conditions. Many of the
+centering, sky fitting, and photometry algorithm parameters in the CENTERPARS,
+FITSKYPARS and PHOTPARS  parameter sets scale with the data dependent
+parameters.
+
+The parameter \fIscale\fR sets the scale of the apertures used by the
+centering, sky fitting and photometry algorithms.  Scale converts radial
+distance measurements in pixel units to radial distance measurements in
+scale units. The APPHOT parameters, cbox, maxshift, rclean and rclip
+in the CENTERPARS parameter set; annulus, dannulus, and rgrow in
+the FITSKYPARS parameter set; and apertures in the PHOTPARS
+parameter set are expressed in units of the scale. The scale parameter is
+useful in cases where the observations are to be compared to published
+aperture photometry measurements in the literature.
+
+The parameter \fIfwhmpsf\fR defines the full-width at half-maximum of the
+stellar point spread function.  Most APPHOT tasks and algorithms do not 
+require this parameter. The exceptions are the DAOFIND task, the centering
+algorithms "gauss" and "ofilter", the FITPSF task, and the WPHOT task.
+
+By setting the \fIscale\fR and \fIfwhmpsf\fR appropriately the aperture
+sizes and radial distances may be  expressed in terms of the half-width
+at half-maximum of the stellar point spread function.  The way to do this
+is to define the scale parameter in units of the number of half-width at
+half-maximum per pixel, set the fwhmpsf parameter to 2.0, and then
+set the remaining scale dependent centering, sky fitting and photometry
+algorithm parameters in CENTERPARS, FITSKYPARS and PHOTPARS to
+appropriate values in units of the half-width at half-maximum of the
+point-spread function. Once an optimum set of algorithm parameters is
+chosen, the user need only alter the DATAPARS scale parameter before
+executing an APPHOT task on a new image.
+
+If  \fIemission\fR is "yes", the features to be measured are assumed to be
+above sky. By default the APPHOT package considers all measurements to
+be measurements of emission features. In most cases APPHOT users should
+leave emission set to "yes".
+
+The parameter \fIsigma\fR estimates the standard deviation of the sky
+background pixels. The star finding algorithm in DAOFIND uses sigma
+and the \fIfindpars.threshold\fR parameter to define the stellar
+detection threshold in adu. The centering algorithms uses sigma,
+1) with the \fIcenterpars.kclean\fR parameter to define deviant pixels
+if \fIcenterpars.clean\fR is enabled; 2) to estimate the signal to
+noise ratio in the centering box; 3) and with the \fIcenterpars.cthreshold\fR
+parameter to define the lower intensity limit for the pixels to be used
+for centering.  If sigma is undefined or <= 0.0 1) no cleaning is performed
+regardless of the value of centerpars.clean; 2) the background
+noise in the centering box is assumed to be 0; and 3) default cutoff
+intensity intensity is used for centering. 
+
+The \fIdatamin\fR and \fIdatamax\fR parameters define the  good data range.
+If datamin or datamax are defined bad data is removed from the sky pixel
+distribution before the sky is fit, data containing bad pixels in the 
+photometry apertures is flagged, and the corresponding aperture photometry
+magnitudes are set to INDEF. APPHOT users should set datamin and datamax
+to appropriate values before running the APPHOT tasks.
+
+Two noise models are available "constant" and "poisson". If \fInoise\fR =
+constant, the total noise is assumed to be due to noise in the sky background
+alone. If \fInoise\fR = poisson, the total noise includes Poisson noise from
+the object and the sky noise. 
+
+The parameters \fIgain\fR and \fIepadu\fR define the image gain.
+The gain parameter specifies which keyword in the image header contains
+the gain value. If gain is undefined or not present in the image header
+the value of epadu is used.  Epadu must be in units of electrons per adu.
+APPHOT users should set either gain or epadu before running any 
+APPHOT tasks to insure the magnitude error computations are correct.
+
+The two parameters \fIccdread\fR and \fIreadnoise\fR define the image
+readout noise.  The ccdread parameter specifies which keyword in the
+image header contains the readout noise value. If ccdread is undefined or
+not present in the image header the value of readnoise is used.
+Readnoise is assumed to be in units of electrons.
+APPHOT users should set either ccdread or readnoise before running any 
+APPHOT tasks to insure the magnitude error computations are correct.
+
+The magnitudes are normalized to an exposure time of 1 timeunit using
+the value of the exposure time in the image header parameter \fIexposure\fR
+or \fIitime\fR. If exposure is undefined or not present in the image header
+the value of itime is used. Itime can be in arbitrary units.
+Setting either exposure or itime will simplify future analysis steps.
+
+The parameters \fIairmass\fR and \fIxairmass\fR define the airmass
+of the observation. The airmass parameter specifies which keyword in the
+image header contains the airmass value. If airmass is undefined or
+not present in the image header the value of xairmass is used.
+The airmass values are not used in any APPHOT computations, however their
+presence in the APPHOT output files will simplify future reduction steps. 
+
+The parameters \fIfilter\fR and \fIifilter\fR define the filter
+of the observation. The filter parameter specifies which keyword in the
+image header contains the filter id. If filter is undefined or not present
+in the image header the value of ifilter is used. The filter id values are
+not used in any APPHOT computations, however their presence in the APPHOT
+output files can will simplify future reduction steps. 
+
+The parameters \fIobstime\fR and \fIotime\fR define the time 
+of the observation (e.g. UT). The obstime parameter specifies which keyword
+in the image header contains the time stamp of the observation. If obstime is
+undefined or not present in the image header the value of otime is used.
+The time of observations values are not used in any APPHOT 
+computations, however their presence in the APPHOT output files can
+greatly simplify future reduction steps. 
+
+.ih
+EXAMPLES
+
+1. List the data dependent parameters.
+
+.nf
+	ap> lpar datapars
+.fi
+
+2. Edit the data dependent parameters.
+
+.nf
+	ap> datapars
+.fi
+
+3. Edit the DATAPARS parameters from within the PHOT task.
+
+.nf
+    da> epar phot
+
+	... edit a few parameters
+
+	... move to the datapars parameter and type :e
+
+	... edit the datapars parameters and type :wq
+
+	... finish editing the phot parameters and type :wq
+.fi
+
+4. Save the current DATAPARS parameter set in a text file datnite1.par.
+This can also be done from inside a higher level task as in the
+previous example.
+
+.nf
+    da> datapars
+
+	... edit a few parameters
+
+	... type ":w datnite1.par"  from within epar
+.fi
+
+.ih
+TIME REQUIREMENTS
+
+.ih
+BUGS
+
+.ih
+SEE ALSO
+epar,lpar,daofind,center,fitsky,phot,wphot,polyphot,radprof,fitpsf
+.endhelp
-- 
cgit 

