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