Prepare reduced and combined science products.
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 absorptin 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) 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.
Create an object for the recipe muse_scipost.
import cpl
muse_scipost = cpl.Recipe("muse_scipost")
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’) [default=”cube,skymodel”].
The resampling technique to use for the final output cube. (str; default: ‘drizzle’) [default=”drizzle”].
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) [default=0.0].
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) [default=0.0].
Wavelength step size (in Angstrom). Natural instrument sampling is used, if this is 0.0 (float; default: 0.0) [default=0.0].
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’) [default=”median”].
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) [default=15.0].
Critical radius for the “renka” resampling method. (float; default: 1.25) [default=1.25].
Pixel down-scaling factor for the “drizzle” resampling method. (float; default: 0.8) [default=0.8].
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) [default=1].
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’) [default=”Cube”].
Type of weighting scheme to use when combining multiple exposures. “exptime” just uses the exposure time to weight the exposures, “fwhm” uses the DIMM information in the header as well, “none” preserves an existing weight column in the input pixel tables without changes. (str; default: ‘exptime’) [default=”exptime”].
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’) [default=”white”].
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. (str; default: ‘model’) [default=”model”].
Cut off the data below this wavelength after loading the pixel table(s). (float; default: 4000.0) [default=4000.0].
Cut off the data above this wavelength after loading the pixel table(s). (float; default: 10000.0) [default=10000.0].
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) [default=7000.0].
Carry out a check of the theoretical DAR correction using source centroiding. If “correct” it will also apply an empirical correction. (str; default: ‘none’) [default=”none”].
Fraction of the image 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: 0.05) [default=0.05].
Spectral sampling of the sky spectrum [Angstrom]. (float; default: 1.25) [default=1.25].
Spectral sampling of the continuum spectrum [Angstrom]. (float; default: 1.25) [default=1.25].
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’) [default=”bary”].
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) [default=True].
The following code snippet shows the default settings for the available parameters.
import cpl
muse_scipost = cpl.Recipe("muse_scipost")
muse_scipost.param.save = "cube,skymodel"
muse_scipost.param.resample = "drizzle"
muse_scipost.param.dx = 0.0
muse_scipost.param.dy = 0.0
muse_scipost.param.dlambda = 0.0
muse_scipost.param.crtype = "median"
muse_scipost.param.crsigma = 15.0
muse_scipost.param.rc = 1.25
muse_scipost.param.pixfrac = 0.8
muse_scipost.param.ld = 1
muse_scipost.param.format = "Cube"
muse_scipost.param.weight = "exptime"
muse_scipost.param.filter = "white"
muse_scipost.param.skymethod = "model"
muse_scipost.param.lambdamin = 4000.0
muse_scipost.param.lambdamax = 10000.0
muse_scipost.param.lambdaref = 7000.0
muse_scipost.param.darcheck = "none"
muse_scipost.param.skymodel_fraction = 0.05
muse_scipost.param.skymodel_sampling = 1.25
muse_scipost.param.skymodel_csampling = 1.25
muse_scipost.param.rvcorr = "bary"
muse_scipost.param.astrometry = True
You may also set or overwrite some or all parameters by the recipe parameter param, as shown in the following example:
import cpl
muse_scipost = cpl.Recipe("muse_scipost")
[...]
res = muse_scipost( ..., param = {"save":"cube,skymodel", "resample":"drizzle"})
See also
cpl.Recipe for more information about the recipe object.
Please report any problems to Peter Weilbacher. Alternatively, you may send a report to the ESO User Support Department.
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
Code author: Peter Weilbacher <usd-help@eso.org>