Provided by: cpl-plugin-muse-doc_2.8.7+dfsg-3build1_all 
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-2.8.7.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 2.8.7
AUTHOR
Peter Weilbacher <https://support.eso.org>
BUG REPORTS
Please report any problems to https://support.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