Create the telluric correction frame.
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
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.
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
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
Create an object for the recipe kmo_std_star.
import cpl
kmo_std_star = cpl.Recipe("kmo_std_star")
The spectral type of the star (O, B, A, F, G) Format: G4V etc. (str; default: ‘’) [default=”“].
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’) [default=”CS”].
Either fit a ‘gauss’ or ‘moffat’ profile. (str; default: ‘gauss’) [default=”gauss”].
Defines the range to search for neighbors in pixels (float; default: 1.001) [default=1.001].
The magnitude of the std star. For HK two values have to provided (eg. 12.1,13.2) (str; default: ‘’) [default=”“].
TRUE: Apply flux conservation. FALSE: otherwise (bool; default: True) [default=True].
TRUE: Save reconstructed cubes, FALSE: otherwise (bool; default: False) [default=False].
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) [default=False].
TRUE: Interpolate xcal between rotator angles. FALSE: otherwise (bool; default: True) [default=True].
Suppress arbitrary filename extension.(TRUE (apply) or FALSE (don’t apply) (bool; default: False) [default=False].
The number of samples in wavelength for the reconstructed cube (long; default: 2048) [default=2048].
The lowest wavelength [um] to use when reconstructing. Derived by default, depending on the band (float; default: -1.0) [default=-1.0].
The highest wavelength [um] to use when reconstructing. Derived by default, depending on the band (float; default: -1.0) [default=-1.0].
Apply “average”, “median”, “sum”, “min_max.” or “ksigma”. (str; default: ‘ksigma’) [default=”ksigma”].
The positive rejection threshold for kappa-sigma-clipping (sigma). (float; default: 3.0) [default=3.0].
The negative rejection threshold for kappa-sigma-clipping (sigma). (float; default: 3.0) [default=3.0].
The number of iterations for kappa-sigma-clipping. (long; default: 3) [default=3].
The number of maximum pixel values to clip with min/max-clipping. (long; default: 1) [default=1].
The number of minimum pixel values to clip with min/max-clipping. (long; default: 1) [default=1].
The following code snippet shows the default settings for the available parameters.
import cpl
kmo_std_star = cpl.Recipe("kmo_std_star")
kmo_std_star.param.startype = ""
kmo_std_star.param.imethod = "CS"
kmo_std_star.param.fmethod = "gauss"
kmo_std_star.param.neighborhoodRange = 1.001
kmo_std_star.param.magnitude = ""
kmo_std_star.param.flux = True
kmo_std_star.param.save_cubes = False
kmo_std_star.param.no_noise = False
kmo_std_star.param.xcal_interpolation = True
kmo_std_star.param.suppress_extension = False
kmo_std_star.param.b_samples = 2048
kmo_std_star.param.b_start = -1.0
kmo_std_star.param.b_end = -1.0
kmo_std_star.param.cmethod = "ksigma"
kmo_std_star.param.cpos_rej = 3.0
kmo_std_star.param.cneg_rej = 3.0
kmo_std_star.param.citer = 3
kmo_std_star.param.cmax = 1
kmo_std_star.param.cmin = 1
You may also set or overwrite some or all parameters by the recipe parameter param, as shown in the following example:
import cpl
kmo_std_star = cpl.Recipe("kmo_std_star")
[...]
res = kmo_std_star( ..., param = {"startype":"", "imethod":"CS"})
See also
cpl.Recipe for more information about the recipe object.
Please report any problems to Alex Agudo Berbel. Alternatively, you may send a report to the ESO User Support Department.
This file is part of the KMOS 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, 51 Franklin Street, Suite 500, Boston, MA 02110-1335 USA
Code author: Alex Agudo Berbel <usd-help@eso.org>