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NAME

       muse_standard - Create a flux response curve from a standard star exposure.

SYNOPSIS

       esorex muse_standard [OPTIONS] FILE.sof

DESCRIPTION

       Merge pixel tables from all IFUs and correct for differential atmospheric refraction, when
       necessary. To derive the flux response curve, integrate the flux of all  objects  detected
       within  the  field of view using the given profile. Select one object as the standard star
       (either the brightest or the one nearest one,  depending  on  --select)  and  compare  its
       measured fluxes to tabulated fluxes to derive the sensitivity over wavelength. Postprocess
       this sensitivity  curve  to  mark  wavelength  ranges  affected  by  telluric  absorption.
       Interpolate  over the telluric regions and derive a telluric correction spectrum for them.
       The final response curve is then  linearly  extrapolated  to  the  largest  possible  MUSE
       wavelength  range  and smoothed (with the method given by --smooth). The derivation of the
       telluric correction spectrum assumes that the  star  has  a  smooth  spectrum  within  the
       telluric  regions.  If  there  are  more  than  one  exposure given in the input data, the
       derivation of the flux response and telluric corrections  are  done  separately  for  each
       exposure.  For  each  exposure,  an image containing the extracted stellar spectra and the
       datacube used for flux integration are saved, together  with  collapsed  images  for  each
       given  filter.  In  MUSE´s  WFM  data  (both  AO and non-AO), the Moffat profile is a good
       approximation of the actual PSF. Using the smoothed profile ("smoffat") helps to  increase
       the  S/N  and  in  most  cases  removes  systematics.  In  NFM,  however, the profile is a
       combination of a wide PSF plus the central AO-corrected peak, which cannot be fit well  by
       an  analytical  profile. In this case the circular aperture is the best way to extract the
       flux. Using --profile="auto" (the default) selects these options to  give  the  best  flux
       extraction for most cases.

OPTIONS

       --profile <str>
              Type of flux integration to use. "gaussian", "moffat", and "smoffat" use 2D profile
              fitting, "circle" and "square" are non-optimal aperture flux integrators. "smoffat"
              uses  smoothing  of the Moffat parameters from an initial fit, to derive physically
              meaningful wavelength- dependent  behavior.  "auto"  selects  the  smoothed  Moffat
              profile for WFM data and circular flux integration for NFM. (str; default: ´auto´).
              The  full  name  of  this   option   for   the   EsoRex   configuration   file   is
              muse.muse_standard.profile [default = auto].

       --select <str>
              How  to select the star for flux integration, "flux" uses the brightest star in the
              field, "distance" uses the detection nearest to the approximate coordinates of  the
              reference  source. (str; default: ´distance´). The full name of this option for the
              EsoRex configuration file is muse.muse_standard.select [default = distance].

       --smooth <str>
              How to smooth the response curve before writing it to disk. "none" does not do  any
              kind  of  smoothing  (such a response curve is only useful, if smoothed externally;
              "median" does a median-filter of 15 Angstrom  half-width;  "ppoly"  fits  piecewise
              cubic polynomials (each one across 2x150 Angstrom width) postprocessed by a sliding
              average filter of 15 Angstrom half-width. (str; default: ´ppoly´). The full name of
              this option for the EsoRex configuration file is muse.muse_standard.smooth [default
              = ppoly].

       --lambdamin <float>
              Cut off the data below this wavelength after loading the  pixel  table(s).  (float;
              default: 4000.0). The full name of this option for the EsoRex configuration file is
              muse.muse_standard.lambdamin [default = 4000.0].

       --lambdamax <float>
              Cut off the data above this wavelength after loading the  pixel  table(s).  (float;
              default:  10000.0).  The full name of this option for the EsoRex configuration file
              is muse.muse_standard.lambdamax [default = 10000.0].

       --lambdaref <float>
              Reference wavelength used for correction of  differential  atmospheric  refraction.
              The  R-band  (peak  wavelength ~7000 Angstrom) that is usually used for guiding, is
              close to the central wavelength of MUSE, so a value of 7000.0  Angstrom  should  be
              used if nothing else is known.  A value less than zero switches DAR correction off.
              (float; default: 7000.0). The full name of this option for the EsoRex configuration
              file is muse.muse_standard.lambdaref [default = 7000.0].

       --darcheck <str>
              Carry  out  a  check of the theoretical DAR correction using source centroiding. If
              "correct" it will also apply an empirical correction.  (str; default: ´none´).  The
              full    name    of   this   option   for   the   EsoRex   configuration   file   is
              muse.muse_standard.darcheck [default = none].

       --filter <str>
              The filter name(s) to be used for the output field-of-view image. Each name has  to
              correspond to an EXTNAME in an extension of the FILTER_LIST file. If an unsupported
              filter name is given, creation of the respective  image  is  omitted.  If  multiple
              filter  names  are  given,  they  have  to  be comma separated. If the zeropoint QC
              parameters are wanted, make  sure  to  add  "Johnson_V,Cousins_R,Cousins_I".  (str;
              default:  ´white´).  The full name of this option for the EsoRex configuration file
              is muse.muse_standard.filter [default = white].

       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 muse pipeline can be downloaded as a  PDF  file  using  the
       following URL:

              ftp://ftp.eso.org/pub/dfs/pipelines/muse/muse-pipeline-cookbook-2.8.5.pdf

       An   overview   over   the   existing   ESO  pipelines  can  be  found  on  the  web  page
       https://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
       https://packages.python.org/python-cpl/index.html for further information.

       The other recipes of the muse pipeline are muse_ampl(7), muse_astrometry(7), muse_bias(7),
       muse_create_sky(7), muse_dark(7),  muse_exp_align(7),  muse_exp_combine(7),  muse_flat(7),
       muse_geometry(7),    muse_illum(7),    muse_lingain(7),    muse_lsf(7),   muse_qi_mask(7),
       muse_scibasic(7),            muse_scipost(7),            muse_scipost_apply_astrometry(7),
       muse_scipost_calibrate_flux(7),                         muse_scipost_combine_pixtables(7),
       muse_scipost_correct_dar(7),    muse_scipost_correct_rv(7),     muse_scipost_make_cube(7),
       muse_scipost_raman(7),  muse_scipost_subtract_sky(7), muse_scipost_subtract_sky_simple(7),
       muse_twilight(7), muse_wavecal(7)

VERSION

       muse_standard 2.8.5

AUTHOR

       Peter Weilbacher <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  MUSE  Instrument Pipeline Copyright (C) 2005, 2019 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  02111-1307  USA