Reduce a mos science exposure.
esorex vmmosobsstare [OPTIONS] FILE.sof
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.
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 .
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.
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].
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].
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].
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].
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].
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].
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].
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].
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].
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].
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].
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].
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].
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].
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].
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].
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].
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].
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.
The full documentation for the vimos pipeline can be downloaded as a PDF file using the following URL:
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 vmifucombinecube(7), vmifucalib(7), vmimflatsky(7), vmspflat(7), vmimflatscreen(7), vmimpreimaging(7), vmimcalphot(7), vmmoscombine(7), vmimstandard(7), vmmosobsjitter(7), vmifucombine(7), vmimobsjitter(7), vmspphot(7), vmdet(7), vmmosscience(7), vmmosstandard(7), vmspcaldisp(7), vmifustandard(7), vmbias(7), vmmoscalib(7), vmimobsstare(7), vmdark(7), vmifuscience(7)
ESO VIMOS Pipeline Team and VIMOS Consortium <[email protected]>
This file is part of the VIMOS Instrument Pipeline Copyright (C) 2002-2005 European Southern Observatory
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