Create the telluric correction frame.
esorex kmo_std_star [OPTIONS] FILE.sof
This recipe creates a telluric calibration frame and a PSF frame. It must be called after the kmo_illumination-recipe.
Since there won’t be enough standard stars to observe for all IFUs in one ex- posure, one has to do several exposures in a way that there is at least one standard star and one sky exposure in each IFU. A internal data organiser will analyse the provided exposures and select the appropriate frames as follows: 1. For each IFU the first standard star in the list of provided exposures is
taken. All subsequent standard star exposures for this IFU will be ignored
2. A corresponding sky exposure will be chosen which will be as close in time
to the standard star exposure as possible.
3. For any IFUs not containing a standard star and a sky exposure an empty
frame will be returned.
NOISE_SPEC contains in any case the shot noise [sqrt(counts*gain)/gain]. If the exposures have been taken with template KMOS_spec_cal_stdstarscipatt, then an additional noise component is added in: All existing sky exposures for an IFU are subtracted pairwise, spectra are extracted and the std deviation is calculated.
--startype If this parameter is specified, the stored star types of the observed obejcts in the FITS headers are overridden. This value applies to all objects exa- mined in the input frames. Examples would be “A3I”, “G3IV” or “K0I”. The first letter defines the star type, the second letter the spectral class and the last letters the luminosity class.
--magnitude If this parameter is specified, the stored magnitudes in the FITS headers are overridden. For HK two magnitudes for each H and K have to be specified. All other gratings just use a single magnitude. If two values are provided, they have to be separated with a comma.
--fmethod The type of function that should be fitted spatially to the collapsed image.
This fit is used to create a mask to extract the spectrum of the object. Valid values are “gauss” and “moffat”.
--imethod The interpolation method used for reconstruction. As default \'CS\' is selected.
Note that no error spectra will be generated for this interpolation method.
Select a nearest neighbour method otherwise
--range The spectral range [um] to combine when collapsing the reconstructed cubes.
--save_cubes Set to TRUE if the intermediate reconstructed cubes (eventually divided by illumination correction) should be saved as well. Default is FALSE.
--no_noise Applies only for data taken with template KMOS_spec_cal_stdstarscipatt: Skip lengthy calculation of noise-spectra on all sky exposures (no NOISE_SPEC will be produced).
--flux Specify if flux conservation should be applied.
--neighborhoodRange Defines the range to search for neighbors during reconstruction
--b_samples The number of samples in spectral direction for the reconstructed cube.
Ideally this number should be greater than 2048, the detector size.
--b_start --b_end Used to define manually the start and end wavelength for the reconstructed cube. By default the internally defined values are used.
--cmethod Following methods of frame combination are available:
* \'ksigma\' (Default)
An iterative sigma clipping. For each position all pixels in the spectrum
are examined. If they deviate significantly, they will be rejected according
to the conditions:
val > mean + stdev * cpos_rej
and
val < mean - stdev * cneg_rej
where --cpos_rej, --cneg_rej and --citer are the corresponding configuration
parameters. In the first iteration median and percentile level are used.
* \'median\' At each pixel position the median is calculated.
* \'average\' At each pixel position the average is calculated.
* \'sum\' At each pixel position the sum is calculated.
* \'min_max\' The specified number of minimum and maximum pixel values will be rejected.
--cmax and --cmin apply to this method.
--cpos_rej --cneg_rej --citer see --cmethod=\'ksigma\'
--cmax --cmin see --cmethod=\'min_max\'
--xcal_interpolation If true interpolate the pixel position in the slitlet (xcal) using the two closest rotator angles in the calibration file. Otherwise take the values of the closest rotator angle
--suppress_extension If set to TRUE, the arbitrary filename extensions are supressed. If multiple products with the same category are produced, they will be numered consecutively starting from 0.
Input files:
DO KMOS
category Type Explanation Required #Frames
-------- ----- ----------- -------- -------
STD RAW Std. star & sky exposures Y >=1
XCAL F2D x calibration frame Y 1
YCAL F2D y calibration frame Y 1
LCAL F2D Wavelength calib. frame Y 1
MASTER_FLAT F2D Master flat frame Y 1
WAVE_BAND F2L Table with start-/end-wavelengths Y 1
ILLUM_CORR F2I Illumination correction N 0,1
SOLAR_SPEC F1S Solar spectrum N 0,1
(only for G stars)
ATMOS_MODEL F1S Model atmospheric transmisson N 0,1
(only for OBAF stars in K band)
SPEC_TYPE_LOOKUP F2L LUT eff. stellar temperature N 0,1
Output files:
DO KMOS
category Type Explanation
-------- ----- -----------
TELLURIC F1I The normalised telluric spectrum
(including errors)
STAR_SPEC F1I The extracted star spectrum
(including errors)
STD_IMAGE F2I The standard star PSF images
STD_MASK F2I The generated mask used to extract the star
spectrum
NOISE_SPEC F1I The extracted noise spectrum
--startype <str>
The spectral type of the star (O, B, A, F, G) Format: G4V etc. (str; default: \'\'). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.startype [default = ].
--imethod <str>
Method to use for interpolation. ["NN" (nearest neighbour), "lwNN" (linear weighted nearest neighbor), "swNN" (square weighted nearest neighbor), "MS" (Modified Shepard\'s method), "CS" (Cubic spline)] (str; default: \'CS\'). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.imethod [default = CS].
--fmethod <str>
Either fit a \'gauss\' or \'moffat\' profile. (str; default: \'gauss\'). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.fmethod [default = gauss].
--neighborhoodRange <float>
Defines the range to search for neighbors in pixels (float; default: 1.001). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.neighborhoodRange [default = 1.001].
--magnitude <str>
The magnitude of the std star. For HK two values have to provided (eg. 12.1,13.2) (str; default: \'\'). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.magnitude [default = ].
--flux <bool>
TRUE: Apply flux conservation. FALSE: otherwise (bool; default: True). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.flux [default = True].
--save_cubes <bool>
TRUE: Save reconstructed cubes, FALSE: otherwise (bool; default: False). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.save_cubes [default = False].
--no_noise <bool>
Applies only for data taken with template KMOS_spec_cal_stdstarscipatt: FALSE: Calculate noise-spectra on all sky exposures. TRUE: skip this step (bool; default: False). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.no_noise [default = False].
--xcal_interpolation <bool>
TRUE: Interpolate xcal between rotator angles. FALSE: otherwise (bool; default: True). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.xcal_interpolation [default = True].
--suppress_extension <bool>
Suppress arbitrary filename extension.(TRUE (apply) or FALSE (don\'t apply) (bool; default: False). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.suppress_extension [default = False].
--b_samples <long>
The number of samples in wavelength for the reconstructed cube (long; default: 2048). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.b_samples [default = 2048].
--b_start <float>
The lowest wavelength [um] to use when reconstructing. Derived by default, depending on the band (float; default: -1.0). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.b_start [default = -1.0].
--b_end <float>
The highest wavelength [um] to use when reconstructing. Derived by default, depending on the band (float; default: -1.0). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.b_end [default = -1.0].
--cmethod <str>
Apply "average", "median", "sum", "min_max." or "ksigma". (str; default: \'ksigma\'). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.cmethod [default = ksigma].
--cpos_rej <float>
The positive rejection threshold for kappa-sigma-clipping (sigma). (float; default: 3.0). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.cpos_rej [default = 3.0].
--cneg_rej <float>
The negative rejection threshold for kappa-sigma-clipping (sigma). (float; default: 3.0). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.cneg_rej [default = 3.0].
--citer <long>
The number of iterations for kappa-sigma-clipping. (long; default: 3). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.citer [default = 3].
--cmax <long>
The number of maximum pixel values to clip with min/max-clipping. (long; default: 1). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.cmax [default = 1].
--cmin <long>
The number of minimum pixel values to clip with min/max-clipping. (long; default: 1). The full name of this option for the EsoRex configuration file is kmos.kmo_std_star.cmin [default = 1].
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 kmos pipeline can be downloaded as a PDF file using the following URL:
ftp://ftp.eso.org/pub/dfs/pipelines/kmos/kmos-pipeline-manual-2.9.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 kmos pipeline are kmo_copy(7), kmo_fits_check(7), kmo_sci_red(7), kmo_fits_stack(7), kmo_noise_map(7), kmo_rotate(7), kmo_extract_spec(7), kmo_multi_reconstruct(7), kmo_sky_tweak(7), kmo_shift(7), kmos_gen_reflines(7), kmo_stats(7), kmo_arithmetic(7), kmos_dark(7), kmo_fits_strip(7), kmo_combine(7), kmo_illumination_flat(7), kmo_make_image(7), kmos_flat(7), kmo_fit_profile(7), kmo_sky_mask(7), kmos_illumination(7), kmos_wave_cal(7), kmo_reconstruct(7)
kmo_std_star 1.3.5
Alex Agudo Berbel <[email protected]>
Please report any problems to [email protected]. Alternatively, you may send a report to the ESO User Support Department <[email protected]>.
This file is part of the CRIRES Instrument Pipeline Copyright (C) 2002,2003 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., 59 Temple Place, Suite 330, Boston, MA 02111-1307 USA