% @(#)flux_irsp.hlq	19.1 (ESO-IPG) 02/25/03 14:23:16 
% @(#)
%++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++
%.COPYRIGHT  (c)  1992 European Southern Observatory
%.IDENT      flux_irsp.hlq
%.AUTHOR     E.Oliva, Arcetri (Florence)
%.KEYWORDS   MIDAS, help files, FLUX/IRSPEC
%.PURPOSE    On-line help file for the command: FLUX/IRSPEC
%.VERSION    1.0  24-SEP-1992 : Creation, E.Oliva
%----------------------------------------------------------------
\se
SECTION./IRSPEC
\es\co
FLUX/IRSPEC                                          24-SEP-1992 EO
\oc\su
FLUX/IRSPEC in_ima response_ima out_ima [smooth=s1,s2] [shift=sh]
            [norm=normalize_option] [rect=rectify_option]
        Flux calibrate a spectrum (either 2D or 1D) using a response frame
        created using RESPONSE/IRSPEC
\us\pu
Purpose:    To flux calibrate a spectrum which could either be a 2D
            long-slit image or a 1D spectrum. You must have previously
            created a "response frame" using RESPONSE/IRSPEC.
\up\sy
Syntax:     FLUX/IRSPEC in_ima response_ima out_ima [smooth=s1,s2] 
                        [shift=sh] [norm=normalize_option]
\ys\pa
            in_ima  =  input image. Could be either 2D (a long-slit frame)
                       or 1D (a spectrum) and must be wavelength calibrated
                       (see CALIBRATE/IRSPEC). It must not be normalized 
                       unless you use the normalize_option (see below).
                       In case of 2D long-slit spectrum the command also
                       rectifies the image if you have forgotten it.
                       N.B. the input frame is untouched on exit.
\ap\pa
            response_ima =
                       input (1D) response image previously created with
                       RESPONSE/IRSPEC. It must obviously refer to standard
                       star data taken at the same grating position.
\ap\pa
            out_ima =  name of the output, flux calibrated spectrum. It
                       will have the same size and limits as the input frame,
                       i.e. it will be a 2D flux calibrated spectrum in case
                       the input was a long-slit frame.\\
\\
            Additional parameters and options:
\ap\pa 
            smooth  =  If you want to smooth along X (the dispersion 
                       direction) the object image and/or the response
                       frame use      smooth=s1,s2     (or just sm=s1,s2) 
                       where s1,s2 are the amount - in pixels - by which 
                       you want to smooth the object and the response
                       frame, respectively. The smoothing may help in the
                       reduction of spectra at wavelengths where the
                       atmospheric transmission is very bad. Be however
                       careful not to abuse it because you may easily
                       "invent" good data from bad spectra.
\ap\pa
            shift    = This parameter allows you to shift the star (response)
                       spectrum by a given fraction of a pixel before flux
                       calibrating; it may be of some use for data at 
                       wavelengths with very bad atmospheric transmission.
                       Use e.g.  shift=0.2  (or just sh=0.2) to apply a shift
                       of 0.2 pixels. The default value is obviously sh=0.
\ap\pa
            normalize_option =\\ 0,1;  default=1.
                       The command automatically takes into account, and
                       corrects for, the on-chip integration time of the
                       object frame. Use norm=0 (or just n=0) to force 
                       the command to skip the automatic, normalization 
                       procedure.
\ap\pa
            rectify_option = \\ 0,1  default=1.
                       In case the input object frame is  2D, the command
                       checks if the image was rectified - using 
                       RECTIFY/IRSPEC - and performs this operation in case 
                       this was not previously done.
                       Use rect=0 (or just r=0) to skip this control.
\ap\no
Note:       The command checks if the response frame is a "proper" response
            frame by looking at a descriptor in the response image. If you
            get strange messages it may be that your response frame is the
            result of of a series of non standard operations in which
            the descriptor got lost. Use
                COPY/DD original_response_ima *,3 your_image
            to recover it (original_response_ima is the output of the 
            RESPONSE/IRSPEC command).
            A similar argument applies to the normalization and to the
            "rectify-control" (see also the help of RESP/IRSPEC).
\on\exs
Examples:
\ex
            FLUX/IRS objh8 resph8 fluxh8
\xe\ex
            FLUX/IRS objk01 respk01 fluxk01 smooth=1,1 shift=-0.15
\xe\sxe






