% @(#)apply_disp.hlq 17.1.1.1 (ESO-IPG) 01/25/02 17:53:22 %++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++ %.COPYRIGHT (c) 1993 European Southern Observatory %.IDENT apply_disp.hlq %.AUTHOR 23-MAR-93, IPG/ESO %.KEYWORDS MIDAS, help files, %.PURPOSE On-line help file for the command: APPLY/DISPERSION %.VERSION 1.0 PB : Creation, 23-MAR-93 %---------------------------------------------------------------- \se SECTION./DISPERSION \es\co APPLY/DISPERSION PB 23-MAR-93 \oc\su APPLY/DISPERSION in out [y] [coef] Apply the dispersion relation to a 1D spectrum and generates a table \us\pu Purpose: The dispersion relation is taken from the coefficients table (keyword COERBR, default: coerbr.tbl) and applied to a 1D spectrum or a given row of a long-slit spectrum. The output spectrum is presented as a table in order to avoid interpolations. \up\sy Syntax: APPLY/DISPERSION in out [y] [coef] \ys\pa in = Name of the input image \ap\pa out = Name of the output table \ap\pa y = Spectrum position. The position can be provided in pixels (if preceded by an @ sign) or in world coordinates. If the input image is a 1D spectrum, the dispersion relation will be read at position y in the coefficients table. Default : @{YSTART} \ap\pa coef = Name of the coefficients table.\\ Session keyword : COERBR\\ Default : coerbr.tbl \ap\sa See also: CALIBRATE/LONG, REBIN/LONG, RECTIFY/LONG, PLOT/SPECTRUM \as\no Note: 1) Command CALIBRATE/LONG must have been executed previously to generate the coefficients table. \\ 2) Command PLOT/SPECTRUM can be used to visualize the output table \on\exs Examples: \ex APPLY/DISPERSION ccd0001 sptab @300 \xe\ex PLOT/SPECTRUM sptab \xe \sxe