%++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
%.COPYRIGHT  (c)  1990 European Southern Observatory
%.IDENT      apply_mos.hlq
%.AUTHOR     JDP, IPG/ESO
%.KEYWORDS   MIDAS, help files, APPLY/MOS
%.PURPOSE    On-line help file for the command: APPLY/MOS
%.VERSION    1.0  18-DEC-1986 : Creation, JDP
%----------------------------------------------------------------
\se
SECTION./MOS
\es\co
APPLY/MOS					4-JAN-1994 OS
\oc\su
APPLY/MOS extracted linfit output_table
	apply dispersion relation to extracted data
\us\pu
Purpose:   
	  Apply dispersion relation to extracted MOS data
\up\sy
Syntax:
	  APPLY/MOS [extobjec] [linfit] [calobjec]
\ys\pa

	  extobjec = image with extracted data (line by line)
              Session keyword: EXTOBJEC
              Default: none
	  linfit = table with dispersion coefficients
              Session keyword: LINFIT
              Default: coerbr
	  calobjec = root name for output tables (number is appended)
              Session keyword: CALOBJEC
              Default: none
\ap/sa
See also: 
          REBIN/MOS, REB1D/MOS
\as\no
Note:       
	  This command applies the dispersion relation from table
	  LINFIT to the extracted spectra in image EXTOBJEC.
	  The table with dispersion coefficients is typically created 
	  with the commands SEARCH/MOS and CALIBRATE/MOS.
	  The spectra should be extracted with EXTRACT/MOS.
	  The output of this command is one table for each spectrum
          with the columns
          :LAMBDA (wavelength), 
          :BIN (wavelength/pixel), 
          :FLUX (flux), and
          :FLUX_ERROR (flux error)
	  No rebinning is done with this command.
\on\exs
Examples:
\ex
	  APPLY/MOS extobj coerbr ext
          Takes the extracted spectra stored in extobj.bdf and the dispersion
          coefficients stored in coerbr.tbl. For each spectrum the wavelength
          position of each pixel as well as the wavelength bin corresponding
          to each pixel are computed and stored in the table ext####.tbl 
          (where #### is the running number of the spectrum, 0001, 0002, 
          etc.). Also the flux and the error of the flux per pixel are stored. 
          :LAMBDA. 
\xe \sxe

