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NAME

       vmmosobsstare - Reduce a MOS science exposure.

SYNOPSIS

       esorex vmmosobsstare [OPTIONS] FILE.sof

DESCRIPTION

       This  recipe  is  used to apply basic reduction steps to one exposure made in MOS mode, to
       locate objects, and to optimally extract their spectra.

       Input files:

         DO category:             Type:       Explanation:         Required:
         MOS_SCIENCE              Raw         Science exposure        Y
         MASTER_BIAS              Calib       Master bias             Y
         MASTER_DARK              Calib       Master dark             .

         MOS_MASTER_SCREEN_FLAT   Calib       Normalised flat field   .

         EXTRACT_TABLE            Calib       Extraction table        .

         GRISM_TABLE              Calib       Grism table             Y
         EXTINCT_TABLE            Calib       Atmospheric extinction  .

         MOS_SPECPHOT_TABLE       Calib       Response curve          .

         CCD_TABLE                Calib       Bad pixel table         .

       Output files:

         DO category:             Data type:  Explanation:
         MOS_SCIENCE_REDUCED      FITS image  Extracted objects spectra
         MOS_SCIENCE_FLUX_REDUCED FITS image  Flux calibrated objects spectra
         MOS_SCIENCE_EXTRACTED    FITS image  Sky subtracted slit spectra
         MOS_SCIENCE_SKY          FITS image  Sky spectra
         MOS_SKY_REDUCED          FITS image  Extracted sky spectra
         OBJECT_TABLE             FITS table  Objects spectra identification
         WINDOW_TABLE             FITS table  Objects positions in slit

       A flat field correction is applied only if a normalised master flat field (produced by the
       recipe vmspflat) is specified.

       The  extraction table is the product of the local spectral distortions modelling performed
       by the recipe vmspcaldisp. If an extraction  table  is  not  specified,  then  the  global
       distortion models read from the science frame header are used.

       The  grism  table contains necessary information to control the way spectra are extracted,
       starting from the reference wavelength (header entry PRO WLEN CEN), on a specific range of
       pixels  above  and below its position on the CCD (header entries PRO SPECT LLEN LO and PRO
       SPECT LLEN HI). Other parameters, used in the extraction of the science slit spectra,  are
       the  start  and  the  end  wavelength  of  the image of the extracted slit spectra (header
       entries PRO WLEN START and PRO  WLEN  END),  and  the  step  of  the  sampling  along  the
       dispersion  direction  (header  entry  PRO  WLEN INC). Finally, the wavelengths of the sky
       lines used in the alignment of the spectral distortion  models,  necessary  to  keep  into
       account  the  possible  coordinates  shifts  introduced  by  a variation of the instrument
       flexures between the science and the calibration  exposures,  are  listed  in  the  header
       keywords  PRO  SKY WLENi, with i ranging from 1 to the number specified in the keyword PRO
       SKY NO.

       A CCD table must be specified in input only if a bad pixel cleaning is requested.

       The slit spectra are remapped with the instrument  distortions  removed  and  at  a  fixed
       wavelength step. A sky value is estimated for each wavelength and then subtracted from the
       data.  The  result  is  stored  in  the  MOS_SCIENCE_EXTRACTED  image,  while  the   image
       MOS_SCIENCE_SKY  contains the subtracted sky model. The 1D extracted spectra are stored in
       the MOS_SCIENCE_REDUCED image, while the corresponding sky spectra extracted with the same
       method are stored in the MOS_SKY_REDUCED image.

       The  positions  of  the  extracted  slit spectra and of the detected objects that they may
       contain are listed in the window table.

       If a spectro-photometric  table  (produced  by  the  recipe  vmmosstandard)  is  specified
       together with an atmospheric extinction table, and a flux calibration is requested, then a
       MOS_SCIENCE_FLUX_REDUCED  image  is  also  created.  This  image  is  identical   to   the
       MOS_SCIENCE_REDUCED,  but  the  spectra  it contains are flux calibrated, and expressed in
       units of erg/cm/cm/s/Angstrom.

       For more details, please refer to the VIMOS Pipeline User´s Guide.

OPTIONS

       --BiasMethod <str>
              Bias removal method. (str; default: ´Zmaster´). The full name of  this  option  for
              the  EsoRex  configuration file is vimos.Parameters.bias.removing.method [default =
              Zmaster].

       --SkyMethod <str>
              Sky level determination method. (str; default: ´Median´). The  full  name  of  this
              option  for the EsoRex configuration file is vimos.Parameters.sky.method [default =
              Median].

       --PolyOrder <long>
              Degree of polynomial used when the SkyMethod is set to Fit. (long; default: 0). The
              full    name    of   this   option   for   the   EsoRex   configuration   file   is
              vimos.Parameters.sky.order [default = 0].

       --SkyKSigmaLow <float>
              Low threshold for K-sigma rejection in sky fitting. (float; default: 1.0). The full
              name    of    this    option    for    the    EsoRex    configuration    file    is
              vimos.Parameters.sky.ksigma.low [default = 1.0].

       --SkyKSigmaHigh <float>
              High threshold for K-sigma rejection in sky fitting.  (float;  default:  1.0).  The
              full    name    of   this   option   for   the   EsoRex   configuration   file   is
              vimos.Parameters.sky.ksigma.high [default = 1.0].

       --Fuzz <long>
              Extra pixels from  expected  position  of  spectrum  edge  in  extraction.   (long;
              default:  5).  The  full  name  of this option for the EsoRex configuration file is
              vimos.Parameters.extraction.fuzz [default = 5].

       --SlitMargin <long>
              Number of  excluded  pixels  at  slit  ends  in  object  search  or  in  sky  level
              determination.  (long;  default:  2).  The  full name of this option for the EsoRex
              configuration file is vimos.Parameters.detection.exclude [default = 2].

       --LineWidth <long>
              Size of spectrum to extract around any skyline. (long; default: 16). The full  name
              of  this option for the EsoRex configuration file is vimos.Parameters.sky.linewidth
              [default = 16].

       --DetectionLevel <float>
              Object detection level in units of sigma. (float; default: 2.0). The full  name  of
              this  option  for the EsoRex configuration file is vimos.Parameters.detection.sigma
              [default = 2.0].

       --WatershedLevels <long>
              Number of levels in the watershed method in object detection. (long; default:  32).
              The   full   name   of   this   option   for   the  EsoRex  configuration  file  is
              vimos.Parameters.detection.levels [default = 32].

       --WatershedFraction <float>
              Flux fraction to use in watershed. (float; default: 0.01). The full  name  of  this
              option  for  the  EsoRex  configuration file is vimos.Parameters.detection.fraction
              [default = 0.01].

       --MinObjectSize <long>
              Minimal size for an object candidate to be considered an object.   (long;  default:
              2).   The   full  name  of  this  option  for  the  EsoRex  configuration  file  is
              vimos.Parameters.detection.minsize [default = 2].

       --MaxObjectSize <long>
              Maximal size for an object candidate for not  trying  deblend  into  sub-  objects.
              (long;  default: 7). The full name of this option for the EsoRex configuration file
              is vimos.Parameters.detection.maxsize [default = 7].

       --CleanBadPixel <bool>
              Bad pixel correction on MOS science exposure. (bool; default: False). The full name
              of this option for the EsoRex configuration file is vimos.Parameters.badpixel.clean
              [default = False].

       --CalibrateFlux <bool>
              Extracted spectra are flux calibrated. (bool; default: False).  The  full  name  of
              this  option for the EsoRex configuration file is vimos.Parameters.flux.calibration
              [default = False].

       --HorneExtraction <bool>
              Use 1D Horne extraction. (bool; default: False). The full name of this  option  for
              the  EsoRex  configuration  file  is vimos.Parameters.extraction.optimal [default =
              False].

       --ModelSlit <bool>
              Model wavelength solution within each slit. (bool; default: True). The full name of
              this  option  for  the  EsoRex  configuration  file  is vimos.Parameters.slit.model
              [default = True].

       --ModelSlitOrder <long>
              Order of polynomial for wavelength solution  modeling  within  each  slit.   (long;
              default:  0).  The  full  name  of this option for the EsoRex configuration file is
              vimos.Parameters.slit.order [default = 0].

       --UseSkylines <bool>
              Use sky lines to refine the wavelength calibration (bool; default: True). The  full
              name of this option for the EsoRex configuration file is vimos.Parameters.sky.align
              [default = True].

       Note that it is possible to create a configuration file containing  these  options,  along
       with  suitable default values. Please refer to the details provided by the 'esorex --help'
       command.

SEE ALSO

       The full documentation for the vimos pipeline can be downloaded as a PDF  file  using  the
       following URL:

              ftp://ftp.eso.org/pub/dfs/pipelines/vimos/vimos-pipeline-manual-6.9.pdf

       An   overview   over   the   existing   ESO  pipelines  can  be  found  on  the  web  page
       http://www.eso.org/sci/software/pipelines/.

       Basic documentation about the EsoRex program can be found at the esorex (1) man page.

       It is possible to call the pipelines  from  python  using  the  python-cpl  package.   See
       http://packages.python.org/python-cpl/index.html for further information.

       The   other   recipes  of  the  vimos  pipeline  are  vmifucombinecube(7),  vmifucalib(7),
       vmimflatsky(7),   vmspflat(7),   vmimflatscreen(7),   vmimpreimaging(7),   vmimcalphot(7),
       vmmoscombine(7),  vmimstandard(7),  vmmosobsjitter(7),  vmimobsstare(7), vmimobsjitter(7),
       vmspphot(7),     vmdet(7),     vmmosscience(7),     vmmosstandard(7),      vmspcaldisp(7),
       vmifustandard(7), vmbias(7), vmmoscalib(7), vmifucombine(7), vmdark(7), vmifuscience(7)

VERSION

       vmmosobsstare 2.9.9

AUTHOR

       ESO VIMOS Pipeline Team and VIMOS Consortium <usd-help@eso.org>

BUG REPORTS

       Please  report  any  problems to usd-help@eso.org. Alternatively, you may send a report to
       the ESO User Support Department <usd-help@eso.org>.

LICENSE

       This file is part of the  VIMOS  Instrument  Pipeline  Copyright  (C)  2002-2005  European
       Southern Observatory

       This program is free software; you can redistribute it and/or modify it under the terms of
       the GNU General Public License as  published  by  the  Free  Software  Foundation;  either
       version 2 of the License, or (at your option) any later version.

       This  program is distributed in the hope that it will be useful, but WITHOUT ANY WARRANTY;
       without even the implied warranty of MERCHANTABILITY or FITNESS FOR A PARTICULAR  PURPOSE.
       See the GNU General Public License for more details.

       You should have received a copy of the GNU General Public License along with this program;
       if not, write to the Free Software Foundation, Inc., 51 Franklin St, Fifth Floor,  Boston,
       MA  02110-1301 USA