Detect mos/mxu spectra on ccd
esorex fors_detect_spectra [OPTIONS] FILE.sof
This recipe is used to detect and locate MOS/MXU slit spectra on the CCD, applying a pattern-matching algorithm. The input spectral exposure must contain spectra with the dispersion direction approximately horizontal, with blue on the left and red on the right. Use recipe fors_wave_calib_lss for LSS data, or for MOS/MXU data where all slits have the same offset.
The rows of the input spectral exposure are processed separately, one by one. First, the background continuum is removed. Second, a list of positions of reference lines candidates is created. Only peaks above a given threshold (specified by the parameter --peakdetection) are selected.
Third, the pattern-matching task selects from the found peaks the ones corresponding to the reference lines, listed in the input line catalog, associating them to the appropriate wavelengths. The ensuing polynomial fit is used to locate the central wavelength of the applied grism along each image row. The contributions from all rows form an image of the location of all spectra, that can be used as a starting point for the proper modeling of the optical and spectral distortions. For more details on this reduction strategy please refer to the FORS Pipeline User\'s Manual.
Note that specifying an input GRISM_TABLE will set some of the recipe configuration parameters to default values valid for a particular grism.
Again, see the pipeline manual for more details.
In the table below the MXU acronym can be alternatively read as MOS.
DO category: Type: Explanation: Required: LAMP_UNBIAS_MXU Calib Bias subtracted arc Y MASTER_LINECAT Calib Line catalog Y GRISM_TABLE Calib Grism table .
DO category: Data type: Explanation: SLIT_MAP_MXU FITS image Map of central wavelength on CCD SLIT_LOCATION_DETECT_MXU FITS table Slits positions on CCD SPECTRA_DETECTION_MXU FITS image Check of preliminary detection
Expected spectral dispersion (Angstrom/pixel) (float; default: 0.0). The full name of this option for the EsoRex configuration file is fors.fors_detect_spectra.dispersion [default = 0.0].
Initial peak detection threshold (ADU) (float; default: 0.0). The full name of this option for the EsoRex configuration file is fors.fors_detect_spectra.peakdetection [default = 0.0].
Degree of wavelength calibration polynomial (long; default: 0). The full name of this option for the EsoRex configuration file is fors.fors_detect_spectra.wdegree [default = 0].
Search radius if iterating pattern-matching with first-guess method (long; default: 4). The full name of this option for the EsoRex configuration file is fors.fors_detect_spectra.wradius [default = 4].
Rejection threshold in dispersion relation fit (pixel) (float; default: 0.7). The full name of this option for the EsoRex configuration file is fors.fors_detect_spectra.wreject [default = 0.7].
Name of line catalog table column with wavelengths (str; default: \'WLEN\'). The full name of this option for the EsoRex configuration file is fors.fors_detect_spectra.wcolumn [default = WLEN].
Start wavelength in spectral extraction (float; default: 0.0). The full name of this option for the EsoRex configuration file is fors.fors_detect_spectra.startwavelength [default = 0.0].
End wavelength in spectral extraction (float; default: 0.0). The full name of this option for the EsoRex configuration file is fors.fors_detect_spectra.endwavelength [default = 0.0].
Attempt slit identification for MOS or MXU (bool; default: True). The full name of this option for the EsoRex configuration file is fors.fors_detect_spectra.slit_ident [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 fors 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 fors pipeline are fors_wave_calib_lss(7), fors_img_sky_flat(7), fors_resample(7), fors_config(7), fors_extract_objects(7), fors_calib(7), fors_wave_calib(7), fors_detect_objects(7), fors_pmos_science(7), fors_extract_slits(7), test_hough(7), fors_img_screen_flat(7), fors_extract(7), fors_remove_bias(7), fors_subtract_sky(7), fors_normalise_flat(7), montecarlo(7), fors_photometry(7), fors_zeropoint(7), fors_dark(7), fors_subtract_sky_lss(7), fors_trace_flat(7), fors_flatfield(7), fors_img_science(7), fors_sumflux(7), fors_pmos_extract(7), fors_align_sky_lss(7), fors_bias(7), fors_align_sky(7), fors_pmos_calib(7), fors_spec_mflat(7), fors_science(7)
Carlo Izzo <[email protected]>
This file is currently part of the FORS Instrument Pipeline Copyright (C) 2002-2010 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.
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