SYNOPSIS

esorex muse_twilight [OPTIONS] FILE.sof

DESCRIPTION

Processing first handles each raw input image separately: it trims the raw data and records the overscan statistics, subtracts the bias (taking account of the overscan, if --overscan is not &none&), converts the images from adu to count, subtracts the dark, divides by the flat-field and combines all the exposures using input parameters. The input calibrations geometry table, trace table, and wavelength calibration table are used to assign 3D coordinates to each CCD-based pixel, thereby creating a pixel table from the master sky-flat. These pixel tables are then cut in wavelength using the --lambdamin and --lambdamax parameters. The integrated flux in each IFU is computed as the sum of the data in the pixel table, and saved in the header, to be used later as estimate for the relative throughput of each IFU. If an ILLUM exposure was given as input, it is then used to correct the relative illumination between all slices of one IFU. For this, the data of each slice within the pixel table of each IFU is multiplied by the normalized median flux of that slice in the ILLUM exposure. The pixel tables of all IFUs are then merged, using the integrated fluxes as inverse scaling factors, and a cube is reconstructed from the merged dataset, using given parameters. A white-light image is created from the cube. This skyflat cube is then saved to disk, with the white-light image as one extension. To construct a smooth 3D illumination correction, the cube is post-processed in the following way: the white-light image is used to create a mask of the illuminated area. From this area, the optional vignetting mask is removed. The smoothing is then computed for each plane of the cube: the illuminated area is smoothed (by a 5x7 median filter), normalized, fit with a 2D polynomial (of given polynomial orders), and normalized again. A smooth white image is then created by collapsing the smooth cube. If a vignetting mask was given, the corner area given by the mask is used to compute a 2D correction for the vignetted area: the original unsmoothed white-light image is corrected for large scale gradients by dividing it with the smooth white image. The residuals in the corner area then smoothed using input parameters. This smoothed vignetting correction is the multiplied onto each plane of the smooth cube, normalizing each plane again. This twilight cube is then saved to disk.

OPTIONS

--overscan <str>

If this is "none", stop when detecting discrepant overscan levels (see ovscsigma), for "offset" it assumes that the mean overscan level represents the real offset in the bias levels of the exposures involved, and adjusts the data accordingly; for "vpoly", a polynomial is fit to the vertical overscan and subtracted from the whole quadrant. (str; default: 'vpoly'). The full name of this option for the EsoRex configuration file is muse.muse_twilight.overscan [default = vpoly].

--ovscreject <str>

This influences how values are rejected when computing overscan statistics. Either no rejection at all ("none"), rejection using the DCR algorithm ("dcr"), or rejection using an iterative constant fit ("fit"). (str; default: 'dcr'). The full name of this option for the EsoRex configuration file is muse.muse_twilight.ovscreject [default = dcr].

--ovscsigma <float>

If the deviation of mean overscan levels between a raw input image and the reference image is higher than |ovscsigma x stdev|, stop the processing. If overscan="vpoly", this is used as sigma rejection level for the iterative polynomial fit (the level comparison is then done afterwards with |100 x stdev| to guard against incompatible settings). Has no effect for overscan="offset". (float; default: 30.0). The full name of this option for the EsoRex configuration file is muse.muse_twilight.ovscsigma [default = 30.0].

--ovscignore <long>

The number of pixels of the overscan adjacent to the data region of the CCD that are ignored when computing statistics or fits. (long; default: 3). The full name of this option for the EsoRex configuration file is muse.muse_twilight.ovscignore [default = 3].

--combine <str>

Type of combination to use (str; default: 'sigclip'). The full name of this option for the EsoRex configuration file is muse.muse_twilight.combine [default = sigclip].

--nlow <long>

Number of minimum pixels to reject with minmax (long; default: 1). The full name of this option for the EsoRex configuration file is muse.muse_twilight.nlow [default = 1].

--nhigh <long>

Number of maximum pixels to reject with minmax (long; default: 1). The full name of this option for the EsoRex configuration file is muse.muse_twilight.nhigh [default = 1].

--nkeep <long>

Number of pixels to keep with minmax (long; default: 1). The full name of this option for the EsoRex configuration file is muse.muse_twilight.nkeep [default = 1].

--lsigma <float>

Low sigma for pixel rejection with sigclip (float; default: 3.0). The full name of this option for the EsoRex configuration file is muse.muse_twilight.lsigma [default = 3.0].

--hsigma <float>

High sigma for pixel rejection with sigclip (float; default: 3.0). The full name of this option for the EsoRex configuration file is muse.muse_twilight.hsigma [default = 3.0].

--scale <bool>

Scale the individual images to a common exposure time before combining them. (bool; default: False). The full name of this option for the EsoRex configuration file is muse.muse_twilight.scale [default = False].

--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_twilight.resample [default = drizzle].

--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_twilight.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: 50.0). The full name of this option for the EsoRex configuration file is muse.muse_twilight.crsigma [default = 50.0].

--lambdamin <float>

Minimum wavelength for twilight reconstruction. (float; default: 5000.0). The full name of this option for the EsoRex configuration file is muse.muse_twilight.lambdamin [default = 5000.0].

--lambdamax <float>

Maximum wavelength for twilight reconstruction. (float; default: 9000.0). The full name of this option for the EsoRex configuration file is muse.muse_twilight.lambdamax [default = 9000.0].

--dlambda <float>

Sampling for twilight reconstruction, this should result in planes of equal wavelength coverage. (float; default: 250.0). The full name of this option for the EsoRex configuration file is muse.muse_twilight.dlambda [default = 250.0].

--xorder <long>

Polynomial order to use in x direction to fit the full field of view. (long; default: 2). The full name of this option for the EsoRex configuration file is muse.muse_twilight.xorder [default = 2].

--yorder <long>

Polynomial order to use in y direction to fit the full field of view. (long; default: 2). The full name of this option for the EsoRex configuration file is muse.muse_twilight.yorder [default = 2].

--vignmaskedges <float>

Pixels on edges stronger than this fraction in the normalized image are excluded from the fit to the vignetted area. Set to non-positive number to include them in the fit. (float; default: 0.02). The full name of this option for the EsoRex configuration file is muse.muse_twilight.vignmaskedges [default = 0.02].

--vignsmooth <str>

Type of smoothing to use for the vignetted region given by the VIGNETTING_MASK; gaussian uses (vignxpar + vignypar)/2 as FWHM. (str; default: 'polyfit'). The full name of this option for the EsoRex configuration file is muse.muse_twilight.vignsmooth [default = polyfit].

--vignxpar <long>

Parameter used by the vignetting smoothing: x order for polyfit (default, recommended 4), parameter that influences the FWHM for the gaussian (recommended: 10), or x dimension of median filter (recommended 5). (long; default: 4). The full name of this option for the EsoRex configuration file is muse.muse_twilight.vignxpar [default = 4].

--vignypar <long>

Parameter used by the vignetting smoothing: y order for polyfit (default, recommended 4), parameter that influences the FWHM for the gaussian (recommended: 10), or y dimension of median filter (recommended 5). (long; default: 4). The full name of this option for the EsoRex configuration file is muse.muse_twilight.vignypar [default = 4].

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_twilight 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