SYNOPSIS

esorex vmmosobsstare [OPTIONS] FILE.sof

DESCRIPTION

This recipe is used to apply basic reduction steps to one exposure made in MOS mode, to locate objects, and to optimally extract their spectra.

Input files:

  DO category:             Type:       Explanation:         Required:
  MOS_SCIENCE              Raw         Science exposure        Y
  MASTER_BIAS              Calib       Master bias             Y
  MASTER_DARK              Calib       Master dark             .

  MOS_MASTER_SCREEN_FLAT   Calib       Normalised flat field   .

  EXTRACT_TABLE            Calib       Extraction table        .

  GRISM_TABLE              Calib       Grism table             Y
  EXTINCT_TABLE            Calib       Atmospheric extinction  .

  MOS_SPECPHOT_TABLE       Calib       Response curve          .

  CCD_TABLE                Calib       Bad pixel table         .

Output files:

  DO category:             Data type:  Explanation:
  MOS_SCIENCE_REDUCED      FITS image  Extracted objects spectra
  MOS_SCIENCE_FLUX_REDUCED FITS image  Flux calibrated objects spectra
  MOS_SCIENCE_EXTRACTED    FITS image  Sky subtracted slit spectra
  MOS_SCIENCE_SKY          FITS image  Sky spectra
  MOS_SKY_REDUCED          FITS image  Extracted sky spectra
  OBJECT_TABLE             FITS table  Objects spectra identification
  WINDOW_TABLE             FITS table  Objects positions in slit

A flat field correction is applied only if a normalised master flat field (produced by the recipe vmspflat) is specified.

The extraction table is the product of the local spectral distortions modelling performed by the recipe vmspcaldisp. If an extraction table is not specified, then the global distortion models read from the science frame header are used.

The grism table contains necessary information to control the way spectra are extracted, starting from the reference wavelength (header entry PRO WLEN CEN), on a specific range of pixels above and below its position on the CCD (header entries PRO SPECT LLEN LO and PRO SPECT LLEN HI). Other parameters, used in the extraction of the science slit spectra, are the start and the end wavelength of the image of the extracted slit spectra (header entries PRO WLEN START and PRO WLEN END), and the step of the sampling along the dispersion direction (header entry PRO WLEN INC). Finally, the wavelengths of the sky lines used in the alignment of the spectral distortion models, necessary to keep into account the possible coordinates shifts introduced by a variation of the instrument flexures between the science and the calibration exposures, are listed in the header keywords PRO SKY WLENi, with i ranging from 1 to the number specified in the keyword PRO SKY NO.

A CCD table must be specified in input only if a bad pixel cleaning is requested.

The slit spectra are remapped with the instrument distortions removed and at a fixed wavelength step. A sky value is estimated for each wavelength and then subtracted from the data. The result is stored in the MOS_SCIENCE_EXTRACTED image, while the image MOS_SCIENCE_SKY contains the subtracted sky model. The 1D extracted spectra are stored in the MOS_SCIENCE_REDUCED image, while the corresponding sky spectra extracted with the same method are stored in the MOS_SKY_REDUCED image.

The positions of the extracted slit spectra and of the detected objects that they may contain are listed in the window table.

If a spectro-photometric table (produced by the recipe vmmosstandard) is specified together with an atmospheric extinction table, and a flux calibration is requested, then a MOS_SCIENCE_FLUX_REDUCED image is also created. This image is identical to the MOS_SCIENCE_REDUCED, but the spectra it contains are flux calibrated, and expressed in units of erg/cm/cm/s/Angstrom.

For more details, please refer to the VIMOS Pipeline User's Guide.

OPTIONS

--BiasMethod <str>

Bias removal method. (str; default: 'Zmaster'). The full name of this option for the EsoRex configuration file is vimos.Parameters.bias.removing.method [default = Zmaster].

--SkyMethod <str>

Sky level determination method. (str; default: 'Median'). The full name of this option for the EsoRex configuration file is vimos.Parameters.sky.method [default = Median].

--PolyOrder <long>

Degree of polynomial used when the SkyMethod is set to Fit. (long; default: 0). The full name of this option for the EsoRex configuration file is vimos.Parameters.sky.order [default = 0].

--SkyKSigmaLow <float>

Low threshold for K-sigma rejection in sky fitting. (float; default: 1.0). The full name of this option for the EsoRex configuration file is vimos.Parameters.sky.ksigma.low [default = 1.0].

--SkyKSigmaHigh <float>

High threshold for K-sigma rejection in sky fitting. (float; default: 1.0). The full name of this option for the EsoRex configuration file is vimos.Parameters.sky.ksigma.high [default = 1.0].

--Fuzz <long>

Extra pixels from expected position of spectrum edge in extraction. (long; default: 5). The full name of this option for the EsoRex configuration file is vimos.Parameters.extraction.fuzz [default = 5].

--SlitMargin <long>

Number of excluded pixels at slit ends in object search or in sky level determination. (long; default: 2). The full name of this option for the EsoRex configuration file is vimos.Parameters.detection.exclude [default = 2].

--LineWidth <long>

Size of spectrum to extract around any skyline. (long; default: 16). The full name of this option for the EsoRex configuration file is vimos.Parameters.sky.linewidth [default = 16].

--DetectionLevel <float>

Object detection level in units of sigma. (float; default: 2.0). The full name of this option for the EsoRex configuration file is vimos.Parameters.detection.sigma [default = 2.0].

--WatershedLevels <long>

Number of levels in the watershed method in object detection. (long; default: 32). The full name of this option for the EsoRex configuration file is vimos.Parameters.detection.levels [default = 32].

--WatershedFraction <float>

Flux fraction to use in watershed. (float; default: 0.01). The full name of this option for the EsoRex configuration file is vimos.Parameters.detection.fraction [default = 0.01].

--MinObjectSize <long>

Minimal size for an object candidate to be considered an object. (long; default: 2). The full name of this option for the EsoRex configuration file is vimos.Parameters.detection.minsize [default = 2].

--MaxObjectSize <long>

Maximal size for an object candidate for not trying deblend into sub- objects. (long; default: 7). The full name of this option for the EsoRex configuration file is vimos.Parameters.detection.maxsize [default = 7].

--CleanBadPixel <bool>

Bad pixel correction on MOS science exposure. (bool; default: False). The full name of this option for the EsoRex configuration file is vimos.Parameters.badpixel.clean [default = False].

--CalibrateFlux <bool>

Extracted spectra are flux calibrated. (bool; default: False). The full name of this option for the EsoRex configuration file is vimos.Parameters.flux.calibration [default = False].

--HorneExtraction <bool>

Use 1D Horne extraction. (bool; default: False). The full name of this option for the EsoRex configuration file is vimos.Parameters.extraction.optimal [default = False].

--ModelSlit <bool>

Model wavelength solution within each slit. (bool; default: True). The full name of this option for the EsoRex configuration file is vimos.Parameters.slit.model [default = True].

--ModelSlitOrder <long>

Order of polynomial for wavelength solution modeling within each slit. (long; default: 0). The full name of this option for the EsoRex configuration file is vimos.Parameters.slit.order [default = 0].

--UseSkylines <bool>

Use sky lines to refine the wavelength calibration (bool; default: True). The full name of this option for the EsoRex configuration file is vimos.Parameters.sky.align [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

vmmosobsstare 3.1.6

AUTHOR

ESO VIMOS Pipeline Team and VIMOS Consortium <[email protected]>

LICENSE

This file is part of the VIMOS Instrument Pipeline Copyright (C) 2002-2005 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 02110-1301 USA