vmmosobsstare(7)
NAME
vmmosobsstare - Reduce a MOS science exposure.
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 Users 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.
SEE ALSO
The full documentation for the vimos pipeline can be downloaded as a
PDF file using the following URL:
ftp://ftp.eso.org/pub/dfs/pipelines/vimos/vimos-pipeline-manual-6.9.pdf
An overview over the existing ESO pipelines can be found on the web
page http://www.eso.org/sci/software/pipelines/.
Basic documentation about the EsoRex program can be found at the esorex
(1) man page.
It is possible to call the pipelines from python using the python-cpl
package. See http://packages.python.org/python-cpl/index.html for
further information.
The other recipes of the vimos pipeline are vmbias(7), vmdark(7),
vmdet(7), vmifucalib(7), vmifucombine(7), vmifucombinecube(7),
vmifuscience(7), vmifustandard(7), vmimcalphot(7), vmimflatscreen(7),
vmimflatsky(7), vmimobsjitter(7), vmimobsstare(7), vmimpreimaging(7),
vmimstandard(7), vmmoscalib(7), vmmoscombine(7), vmmosobsjitter(7),
vmmosscience(7), vmmosstandard(7), vmspcaldisp(7), vmspflat(7),
vmspphot(7)
VERSION
vmmosobsstare 3.1.7
AUTHOR
ESO VIMOS Pipeline Team and VIMOS Consortium <usd-help@eso.org>
BUG REPORTS
Please report any problems to usd-help@eso.org. Alternatively, you may send a report to the ESO User Support Department <usd-help@eso.org>.
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
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