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  • Committer: Package Import Robot
  • Author(s): Ole Streicher
  • Date: 2014-04-22 14:44:58 UTC
  • Revision ID: package-import@ubuntu.com-20140422144458-okiwi1assxkkiz39
Tags: upstream-13.09pl1.2+dfsg
Import upstream version 13.09pl1.2+dfsg

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stdred/long/help/rebin_long.hlq
 
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% @(#)rebin_long.hlq    19.1 (ESO-IPG) 02/25/03 14:24:06
 
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%++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
 
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%.COPYRIGHT  (c)  1993 European Southern Observatory
 
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%.IDENT      rebin_long.hlq
 
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%.AUTHOR     01-APR-93, IPG/ESO
 
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%.KEYWORDS   MIDAS, help files, 
 
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%.PURPOSE    On-line help file for the command: REBIN/LONG
 
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%.VERSION    1.0  PB : Creation, 01-APR-93
 
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%----------------------------------------------------------------
 
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\se
 
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SECTION./LONG
 
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\es\co
 
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REBIN/LONG                                         PB   30-OCT-95
 
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\oc\su
 
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REBIN/LONG  in  out   [start,end,step]  [mtd]  [table]
 
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        Rebin a long-slit spectrum using the row-by-row method
 
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\us\pu
 
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Purpose:    
 
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            Non linear rebinning of 2D long-slit spectra using the
 
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            row-by-row method.
 
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\up\sy
 
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Syntax:     
 
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            REBIN/LONG  in  out  [start,end,step]  [mtd]  [table]
 
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\ys\pa
 
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            in             = Input image.
 
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\ap\pa
 
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            out            = Output spectrum.
 
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\ap\pa
 
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            start,end,step = Starting, final and bin wavelength, in 
 
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                             wavelength units. \\
 
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                             Session keywords: REBSTRT, REBEND, REBSTP \\
 
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                             Values initialised by CALIBRATE/LONG.
 
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\ap\pa      
 
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            mtd            = Rebinning method. (LINEAR, QUADRATIC, SPLINE). \\
 
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                             Session keyword: REBMTD; default: LINEAR
 
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\ap\pa      
 
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            table          = coefficients table. \\
 
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                             Session keyword: COERBR; default: coerbr.tbl
 
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\ap\sa
 
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See also: 
 
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            CALIBRATE/LONG, RECTIFY/LONG
 
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\as\no
 
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Note:       
 
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            1) Very strong variations of flux, like in bright emission lines
 
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            or cosmics can yield to negative interpolated values with 
 
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            methods QUADRATIC or SPLINE.
 
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            2) The command CALIBRATE/LONG initializes the values of
 
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            start, end and step wavelength. The step wavelength is set
 
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            by default to the average dispersion per pixel. It must be
 
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            noted that in order to respect the Nyquist criterion, step value
 
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            should be half of the average dispersion per pixel, the rebinned
 
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            spectra becoming about twice as large as the original
 
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            spectrum.
 
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\on\exs
 
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Examples:
 
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\ex
 
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            REBIN/LONG  ccd0023  reb23
 
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\xe \sxe
 
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