muse_standard - Create a flux response curve from a standard star exposure.
Merge pixel tables from all IFUs and correct for differential atmospheric
refraction. 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 cuve 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,
the datacube used for flux integration is saved, together with collapsed
images for each given filter.
- --profile <str>
- Type of flux integration to use. "gaussian" and
"moffat" use 2D profile fitting, circle and square are
non-optimal flux integrators. (str; default: ´moffat´). The
full name of this option for the EsoRex configuration file is
muse.muse_standard.profile [default = moffat].
- --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 =
- --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 =
- --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 =
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.
The full documentation for the muse pipeline can be downloaded as a PDF file
using the following URL:
An overview over the existing ESO pipelines can be found on the web page
Basic documentation about the EsoRex program can be found at the esorex (1) man
It is possible to call the pipelines from python using the python-cpl package.
The other recipes of the muse pipeline are muse_ampl
Peter Weilbacher <firstname.lastname@example.org>
Please report any problems to email@example.com. Alternatively, you may send a
report to the ESO User Support Department <firstname.lastname@example.org>.
This file is part of the MUSE Instrument Pipeline Copyright (C) 2005, 2017
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
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