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

---
 noao/twodspec/longslit/doc/extinction.hlp | 87 +++++++++++++++++++++++++++++++
 1 file changed, 87 insertions(+)
 create mode 100644 noao/twodspec/longslit/doc/extinction.hlp

(limited to 'noao/twodspec/longslit/doc/extinction.hlp')

diff --git a/noao/twodspec/longslit/doc/extinction.hlp b/noao/twodspec/longslit/doc/extinction.hlp
new file mode 100644
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--- /dev/null
+++ b/noao/twodspec/longslit/doc/extinction.hlp
@@ -0,0 +1,87 @@
+.help extinction May87 noao.twodspec.longslit
+.ih
+NAME
+extinction -- Apply atmospheric extinction corrections
+.ih
+USAGE
+extinction images
+.ih
+PARAMETERS
+.ls input
+List of input images to be extinction corrected.
+.le
+.ls output
+List of output extinction corrected images.  Output images may be the
+same as the input images.
+.le
+.ls extinction = "onedstds$kpnoextinct.dat"
+Extinction file to be used.  The standard extinction files:
+
+.nf
+	onedstds$kpnoextinct.dat - KPNO standard extinction
+	onedstds$ctioextinct.dat - CTIO standard extinction
+.fi
+.le
+.ih
+DESCRIPTION
+The specified images are corrected for atmospheric extinction according
+to the formula
+
+    correction factor = 10 ** (0.4 * airmass * extinction)
+
+where the extinction is a tabulated function of the wavelength.  The
+extinction file contains lines of wavelength and extinction at that
+wavelength.  The units of the wavelength must be the same as those of
+the dispersion corrected images; i.e. Angstroms.   If the image is
+dispersion corrected in logarithmic wavelength intervals (DC-FLAG = 1)
+the task will convert to wavelength and so the extinction file must
+still be wavelength.  The table values are interpolated
+to the wavelengths of the image pixels and the correction applied to
+the pixel values.  Note that the image pixel values are modifed.
+
+The airmass is sought in the image header under the name AIRMASS.  If the
+airmass is not found then it is computed from the zenith distance (ZD in hours)
+using the approximation formula from Allen's "Astrophysical Quantities", 1973,
+page125 and page 133
+
+	AIRMASS = sqrt (cos (ZD) ** 2 + 2 * scale + 1)
+
+where the atmospheric scale height is set to be 750.  If the parameter ZD
+is not found then it must be computed from the hour angle (HA in hours),
+the declination (DEC in degrees), and the observation latitude (LATITUDE
+in degress).   The hour angle may be computed from the right ascension
+(RA in hours) and siderial time (ST in hours).  Computed quantities are
+recorded in the image header.  Flags indicating extinction correction are
+also set in the image header.
+
+The image header keyword DISPAXIS must be present with a value of 1 for
+dispersion parallel to the lines (varying with the column coordinate) or 2
+for dispersion parallel to the columns (varying with line coordinate).
+This parameter may be added using \fBhedit\fR.  Note that if the image has
+been transposed (\fBimtranspose\fR) the dispersion axis should still refer
+to the original dispersion axis unless the physical world coordinate system
+is first reset (see \fBwcsreset\R).  This is done in order to allow images
+which have DISPAXIS defined prior to transposing to still work correctly
+without requiring this keyword to be changed.
+.ih
+EXAMPLES
+1. A set of dispersion corrected images is extinction corrected in-place as
+follows:
+
+.nf
+	cl> extinction img* img*
+.fi
+
+2. To keep the uncorrected image:
+
+.nf
+	cl> extinction nite1.004 nite1ext.004
+.fi
+
+3.  If the DISPAXIS keyword is missing and the dispersion is running
+vertically (varying with the image lines):
+
+.nf
+	cl> hedit *.imh dispaxis 2 add+
+.fi
+.endhelp
-- 
cgit 

