Compute the response function in SLIT and on/off mode
This recipe reduces science exposure in SLIT configuration and on/off mode Input Frames :
- A set of n Science frames ( n even ), Tag = STD_FLUX_SLIT_OFFSET_arm, SKY_SLIT_arm
- Spectral format table (Tag = SPECTRAL_FORMAT_TAB_arm)
- A master flat frame (Tag = MASTER_FLAT_SLIT_arm)
- An order table frame(Tag = ORDER_TABLE_EDGES_SLIT_arm)
- A wavelength calibration solution frame(Tag = WAVE_TAB_2D_arm)
- [OPTIONAL] Table with dispersion coefficients (Tag = DISP_TAB_arm)
- [OPTIONAL] A telluric model catalog (Tag = TELL_MOD_CAT_arm arm=VIS,NIR)
- A standard star fluxes catalog (Tag = FLUX_STD_CATALOG_arm Type = FLX)
- A table to set response sampling points (Tag = RESP_FIT_POINTS_CAT_arm)
- An atmospheric extinction table (Tag = ATMOS_EXT_arm)
- [OPTIONAL] An master response curve table (Tag = MRESPONSE_MERGE1D_SLIT_arm) if provided this is the one used to flux calibrate the spectra
Products : Products :
- [If STD is in catal] The response ord-by-ord function (Tag = RESPONSE_ORDER1D_SLIT_arm)
- [If STD is in catal] The response merged function (Tag = RESPONSE_MERGE1D_SLIT_arm)
- PREFIX_ORDER2D_arm extracted spectrum, order-by-order, 2D
- PREFIX_ORDER1D_arm extracted spectrum, order-by-order, 1D
- PREFIX_MERGE2D_arm merged spectrum, 2D
- PREFIX_MERGE1D_arm merged spectrum, 1D
- [If STD is in catal] Flux calibrated order-by-order 2D spectrum (Tag = PREFIX_FLUX_ORDER2D_arm)
- [If STD is in catal] Flux calibrated order-by-order 1D spectrum (Tag = PREFIX_FLUX_ORDER1D_arm)
- [If STD is in catal] Flux calibrated merged 2D spectrum (Tag = PREFIX_FLUX_MERGE2D_arm)
- [If STD is in catal] Flux calibrated merged 1D spectrum (Tag = PREFIX_FLUX_MERGE1D_arm)
- PREFIX_SKY_arm, 2D sky frame
- SKY_SLIT_ORDER2D_arm, 2D sky image (order-by-order)
- SKY_SLIT_MERGE2D_arm, 2D sky image (merged)
- [If STD is in catal] The efficiency (Tag = EFFICIENCY_arm)
- PREFIX_WAVE_MAP_arm, wave map image
- PREFIX_SLIT_MAP_arm, slit map image
- where PREFIX is SCI, FLUX, TELL if input raw DPR.TYPE contains OBJECT or FLUX or TELLURIC
Create an object for the recipe xsh_respon_slit_offset.
import cpl
xsh_respon_slit_offset = cpl.Recipe("xsh_respon_slit_offset")
If ‘no’, temporary files are deleted. (str; default: ‘no’) [default=”no”].
Additional xshooter debug level. One of ‘none’, ‘low’, ‘medium’, ‘high’ (str; default: ‘none’) [default=”none”].
Add timestamp to product file name. (bool; default: False) [default=False].
Integer representation of the bits to be considered bad when decoding the bad pixel mask pixel values. Most frequent codes relevant for the user: 0: good pixel, 8: pick-up noise, 16: cosmic-ray removed, 32: cosmic-ray unremoved, 128: calibration file defect, 256: hot pixel, 512: dark pixel, 4096: A/D converted saturation, 32768: non linear pixel, 1048576: extrapolated flux in NIR, 4194304: Interpolated flux during extraction. (long; default: 2144337919) [default=2144337919].
pre-overscan correction.0: no correction1: mean overscan correction2: mean prescan correction3: (mean pre+mean overscan)/2 correction (long; default: 1) [default=1].
Poisson fluctuation threshold to flag CRHs (see van Dokkum, PASP,113,2001,p1420-27) (float; default: 20.0) [default=20.0].
Minimum contrast between the Laplacian image and the fine structure image that a point must have to be flagged as CRH. (see van Dokkum, PASP,113,2001,p1420-27) (float; default: 2.0) [default=2.0].
Max number of iterations (long; default: 4) [default=4].
Name of the Interpolation Kernel Used. Possible values are: tanh, sinc, sinc2, lanczos, hamming, hann. (str; default: ‘tanh’) [default=”tanh”].
Rectify Interpolation radius [bin units]. (float; default: 2.0) [default=2.0].
Wavelength step in the output spectrum [nm] (float; default: -1.0) [default=-1.0].
Spatial step along the slit in the output spectrum [arcsec] (float; default: -1.0) [default=-1.0].
Localization method (MANUAL, MAXIMUM, GAUSSIAN) used to detect the object centroid and height on the slit (str; default: ‘MANUAL’) [default=”MANUAL”].
Number of chunks in the full spectrum to localize the object (long; default: 10) [default=10].
Threshold relative to the peak intensity below which the edges of the object are detected for MAXIMUM localization (float; default: 0.1) [default=0.1].
Degree in lambda in the localization polynomial expression slit=f(lambda), used only for MAXIMUM and GAUSSIAN (long; default: 0) [default=0].
Object position on the slit for MANUAL localization [arcsec] (float; default: 0.0) [default=0.0].
Object half height on the slit for MANUAL localization [arcsec] (float; default: 2.0) [default=2.0].
Kappa value for sigma clipping in the localization polynomial fit (float; default: 3.0) [default=3.0].
Number of iterations for sigma clipping in the localization polynomial fit (long; default: 3) [default=3].
TRUE if we want to mask sky lines using SKY_LINE_LIST file. (bool; default: False) [default=False].
Half size of mask used to define object cross order profile (long; default: 30) [default=30].
Combination method for nodded frames (MEDIAN, MEAN) (str; default: ‘MEAN’) [default=”MEAN”].
if TRUE a 2D sky frame, a 2D rectified, a 2D merged sky are generated (bool; default: True) [default=True].
TRUE if during response computation we apply telluric correction (bool; default: True) [default=True].
The following code snippet shows the default settings for the available parameters.
import cpl
xsh_respon_slit_offset = cpl.Recipe("xsh_respon_slit_offset")
xsh_respon_slit_offset.param.keep_temp = "no"
xsh_respon_slit_offset.param.debug_level = "none"
xsh_respon_slit_offset.param.time_stamp = False
xsh_respon_slit_offset.param.decode_bp = 2144337919
xsh_respon_slit_offset.param.pre_overscan_corr = 1
xsh_respon_slit_offset.param.removecrhsingle_sigmalim = 20.0
xsh_respon_slit_offset.param.removecrhsingle_flim = 2.0
xsh_respon_slit_offset.param.removecrhsingle_niter = 4
xsh_respon_slit_offset.param.rectify_kernel = "tanh"
xsh_respon_slit_offset.param.rectify_radius = 2.0
xsh_respon_slit_offset.param.rectify_bin_lambda = -1.0
xsh_respon_slit_offset.param.rectify_bin_slit = -1.0
xsh_respon_slit_offset.param.localize_method = "MANUAL"
xsh_respon_slit_offset.param.localize_chunk_nb = 10
xsh_respon_slit_offset.param.localize_thresh = 0.1
xsh_respon_slit_offset.param.localize_deg_lambda = 0
xsh_respon_slit_offset.param.localize_slit_position = 0.0
xsh_respon_slit_offset.param.localize_slit_hheight = 2.0
xsh_respon_slit_offset.param.localize_kappa = 3.0
xsh_respon_slit_offset.param.localize_niter = 3
xsh_respon_slit_offset.param.localize_use_skymask = False
xsh_respon_slit_offset.param.stdextract_interp_hsize = 30
xsh_respon_slit_offset.param.combinenod_method = "MEAN"
xsh_respon_slit_offset.param.gen_sky = True
xsh_respon_slit_offset.param.correct_tellurics = True
You may also set or overwrite some or all parameters by the recipe parameter param, as shown in the following example:
import cpl
xsh_respon_slit_offset = cpl.Recipe("xsh_respon_slit_offset")
[...]
res = xsh_respon_slit_offset( ..., param = {"keep_temp":"no", "debug_level":"none"})
See also
cpl.Recipe for more information about the recipe object.
Please report any problems to D. Bramich, A.Modigliani. Alternatively, you may send a report to the ESO User Support Department.
This file is part of the X-shooter Instrument Pipeline Copyright (C) 2006 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
Code author: D. Bramich, A.Modigliani <amodigli@eso.org>