SYNOPSIS

esorex muse_scipost [OPTIONS] FILE.sof

DESCRIPTION

Sort input pixel tables into lists of files per exposure, merge pixel tables from all IFUs of each exposure. Correct each exposure for differential atmopheric refraction (unless --lambdaraf is far outside the MUSE wavelength range). Then the flux calibration is carried out, if a respnse curve was given in the input; it includes a correction of telluric absorption, if a telluric absorption correction file was given. Then the sky subtraction is carried out (unless --skymethod=&none&), either directly subtracting an input sky continuum and an input sky emission lines (for --skymethod=&subtract-model&), or (--skymethod=&model&) create a sky spectrum from the darkest fraction (--skymodel_fraction, after ignoring the lowest --skymodel_ignore as artifacts) of the field of view, then fitting and subtracting sky emission lines using an initial estimate of the input sky lines; then the continuum (residuals after subtracting the sky lines from the sky spectrum) is subtracted as well. If --save contains &skymodel&, all sky-related products are saved for each exposure. Afterwards the data is corrected for the radial velocity of the observer (--rvcorr), before the input (or a default) astrometric solution is applied. Now each individual exposure is fully reduced; the pixel tables at this stage can be saved by setting &individual& in --save. If multiple exposures were given, they are then combined. If --save contains &combined&, this final merged pixel table is saved. Finally (if --save contains &cube&), the data is resampled into a datacube, using all parameters given to the recipe. The extent and orientation of the cube is normally computed from the data itself, but this can be overridden by passing a file with the output world coordinate system (OUTPUT_WCS), for example a MUSE cube. This can also be used to sample the wavelength axis logorithmically (in that file set &CTYPE3='AWAV-LOG'&). As a last step, the computed cube is integrated over all filter functions given (--filter) that are also present in the input filter list table.

OPTIONS

--save <str>

Select output product(s) to save. Can contain one or more of "cube", "skymodel", "individual", "positioned", "combined", and "stacked". If several options are given, they have to be comma-separated. ("cube": output cube and associated images, if this is not given, no final resampling is done at all -- "skymodel": up to four additional output products about the effectively used sky that was subtracted with the "model" method -- "individual": fully reduced pixel table for each individual exposure -- "positioned": fully reduced and positioned pixel table for each individual exposure, the difference to "individual" is that here, the output pixel tables have coordinates in RA and DEC; this is only useful, if both the relative exposure weighting and the final resampling are to be done externally -- "combined": fully reduced and combined pixel table for the full set of exposures, the difference to "positioned" is that all pixel tables are combined into one, with an added weight column; this is useful, if only the final resampling step is to be done separately -- "stacked": an additional output file in form of a 2D column-stacked image, i.e. x direction is pseudo-spatial, y direction is wavelength.) (str; default: 'cube,skymodel'). The full name of this option for the EsoRex configuration file is muse.muse_scipost.save [default = cube,skymodel].

--resample <str>

The resampling technique to use for the final output cube. (str; default: 'drizzle'). The full name of this option for the EsoRex configuration file is muse.muse_scipost.resample [default = drizzle].

--dx <float>

Horizontal step size for resampling (in arcsec or pixel). The following defaults are taken when this value is set to 0.0: 0.2'' for WFM, 0.075'' for NFM, 1.0 if data is in pixel units. (float; default: 0.0). The full name of this option for the EsoRex configuration file is muse.muse_scipost.dx [default = 0.0].

--dy <float>

Vertical step size for resampling (in arcsec or pixel). The following defaults are taken when this value is set to 0.0: 0.2'' for WFM, 0.075'' for NFM, 1.0 if data is in pixel units. (float; default: 0.0). The full name of this option for the EsoRex configuration file is muse.muse_scipost.dy [default = 0.0].

--dlambda <float>

Wavelength step size (in Angstrom). Natural instrument sampling is used, if this is 0.0 (float; default: 0.0). The full name of this option for the EsoRex configuration file is muse.muse_scipost.dlambda [default = 0.0].

--crtype <str>

Type of statistics used for detection of cosmic rays during final resampling. "iraf" uses the variance information, "mean" uses standard (mean/stdev) statistics, "median" uses median and the median median of the absolute median deviation. (str; default: 'median'). The full name of this option for the EsoRex configuration file is muse.muse_scipost.crtype [default = median].

--crsigma <float>

Sigma rejection factor to use for cosmic ray rejection during final resampling. A zero or negative value switches cosmic ray rejection off. (float; default: 15.0). The full name of this option for the EsoRex configuration file is muse.muse_scipost.crsigma [default = 15.0].

--rc <float>

Critical radius for the "renka" resampling method. (float; default: 1.25). The full name of this option for the EsoRex configuration file is muse.muse_scipost.rc [default = 1.25].

--pixfrac <float>

Pixel down-scaling factor for the "drizzle" resampling method. (float; default: 0.8). The full name of this option for the EsoRex configuration file is muse.muse_scipost.pixfrac [default = 0.8].

--ld <long>

Number of adjacent pixels to take into account during resampling in all three directions (loop distance); this affects all resampling methods except "nearest". (long; default: 1). The full name of this option for the EsoRex configuration file is muse.muse_scipost.ld [default = 1].

--format <str>

Type of output file format, "Cube" is a standard FITS cube with NAXIS=3 and multiple extensions (for data and variance). The extended "x" formats include the reconstructed image(s) in FITS image extensions within the same file. (str; default: 'Cube'). The full name of this option for the EsoRex configuration file is muse.muse_scipost.format [default = Cube].

--weight <str>

Type of weighting scheme to use when combining multiple exposures. "exptime" just uses the exposure time to weight the exposures, "fwhm" uses the best available seeing information from the headers as well, "none" preserves an existing weight column in the input pixel tables without changes. (str; default: 'exptime'). The full name of this option for the EsoRex configuration file is muse.muse_scipost.weight [default = exptime].

--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. (str; default: 'white'). The full name of this option for the EsoRex configuration file is muse.muse_scipost.filter [default = white].

--skymethod <str>

The method used to subtract the sky background. "model" should work in all cases, it uses a global sky spectrum model with a local LSF. If "model" is selected, calibration frames for SKY_LINES and LSF_PROFILE must be set; SKY_CONTINUUM and SKY_MASK are optional. If "subtract- model" is selected, precalculated sky lines and continuum are subtracted if specified by SKY_LINES and SKY_CONTINUUM. An LSF_PROFILE is necessary for the two model-based methods. "simple" directly subtracts a sky spectrum created from the data, without regard to LSF variations; it also works on data taht was not flux calibrated. (str; default: 'model'). The full name of this option for the EsoRex configuration file is muse.muse_scipost.skymethod [default = model].

--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_scipost.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_scipost.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_scipost.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_scipost.darcheck [default = none].

--skymodel_fraction <float>

Fraction of the image (without the ignored part) to be considered as sky. If an input sky mask is provided, the fraction is applied to the regions within the mask. If the whole sky mask should be used, set this parameter to 1. (float; default: 0.1). The full name of this option for the EsoRex configuration file is muse.muse_scipost.skymodel_fraction [default = 0.1].

--skymodel_ignore <float>

Fraction of the image to be ignored. If an input sky mask is provided, the fraction is applied to the regions within the mask. If the whole sky mask should be used, set this parameter to 0. (float; default: 0.05). The full name of this option for the EsoRex configuration file is muse.muse_scipost.skymodel_ignore [default = 0.05].

--skymodel_sampling <float>

Spectral sampling of the sky spectrum [Angstrom]. (float; default: 0.3125). The full name of this option for the EsoRex configuration file is muse.muse_scipost.skymodel_sampling [default = 0.3125].

--skymodel_csampling <float>

Spectral sampling of the continuum spectrum [Angstrom]. (float; default: 0.3125). The full name of this option for the EsoRex configuration file is muse.muse_scipost.skymodel_csampling [default = 0.3125].

--sky_crsigma <str>

Sigma level clipping for cube-based and spectrum-based CR rejection when creating the sky spectrum. This has to be a string of two comma- separated floating-point numbers. The first value gives the sigma- level rejection for cube-based CR rejection (using "median"), the second value the sigma-level for spectrum-based CR cleaning. Both can be switched off, by passing zero or a negative value; by default, the spectrum-based rejection is switched off. (str; default: '15.,15.'). The full name of this option for the EsoRex configuration file is muse.muse_scipost.sky_crsigma [default = 15.,15.].

--rvcorr <str>

Correct the radial velocity of the telescope with reference to either the barycenter of the Solar System (bary), the center of the Sun (helio), or to the center of the Earth (geo). (str; default: 'bary'). The full name of this option for the EsoRex configuration file is muse.muse_scipost.rvcorr [default = bary].

--astrometry <bool>

If false, skip any astrometric calibration, even if one was passed in the input set of files. This causes creation of an output cube with a linear WCS and may result in errors. If you want to use a sensible default, leave this true but do not pass an ASTROMETRY_WCS. (bool; default: True). The full name of this option for the EsoRex configuration file is muse.muse_scipost.astrometry [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.

VERSION

muse_scipost 1.6.2

AUTHOR

Peter Weilbacher <[email protected]>

LICENSE

This file is part of the MUSE Instrument Pipeline Copyright (C) 2005, 2015 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