The xsh_respon_slit_nod recipe

xsh_respon_slit_nod

Synopsis

Reduce STD star frames in SLIT configuration and nod mode

Description

This recipe reduces science exposure in SLIT configuration and NOD mode Input Frames :

  • A set of n Science frames ( n even ), Tag = OBJECT_SLIT_NOD_arm

  • Spectral format table (Tag = SPECTRAL_FORMAT_TAB_arm)

  • [UVB,VIS] A master bias frame (Tag = MASTER_BIAS_arm)

  • A master flat frame (Tag = MASTER_FLAT_SLIT_arm)

  • An order table frame(Tag = ORDER_TABLE_EDGES_SLIT_arm)

  • [poly mode] A wave solution frame(Tag = WAVE_TAB_2D_arm)

  • [poly mode] A wave map frame(Tag = WAVE_MAP_arm)

  • [poly mode] A disp table frame(Tag = DISP_TAB_arm)

  • [physical model mode]A model cfg table (Format = TABLE, Tag = XSH_MOD_CFG_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)

  • [OPTIONAL] An atmospheric extinction table (Tag = ATMOS_EXT_arm) if provided this is the one used to flux calibrate the spectra

Products :

  • [If STD is in catal] The response function (Tag = PREFIX_RESPONSE_ORDER1D_SLIT_arm)

  • [If STD is in catal] The response function (Tag = PREFIX_RESPONSE_MERGE1D_SLIT_arm)

  • PREFIX_ORDER2D_arm (2 dimension)

  • PREFIX_ORDER1D_arm (1 dimension)

  • PREFIX_MERGE2D_arm (2 dimension)

  • PREFIX_MERGE1D_arm (1 dimension)

  • PREFIX_WAVE_MAP_arm, wave map image

  • PREFIX_SLIT_MAP_arm, slit map image

  • [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)

  • [If STD is in catal] The efficiency (Tag = EFFICIENCY_SLIT_arm)

  • where PREFIX is SCI, FLUX, TELL if input raw DPR.TYPE contains OBJECT or FLUX or TELLURIC

Constructor

cpl.Recipe("xsh_respon_slit_nod")

Create an object for the recipe xsh_respon_slit_nod.

import cpl
xsh_respon_slit_nod = cpl.Recipe("xsh_respon_slit_nod")

Parameters

xsh_respon_slit_nod.param.keep_temp

If ‘no’, temporary files are deleted. (str; default: ‘no’) [default=”no”].

xsh_respon_slit_nod.param.debug_level

Additional xshooter debug level. One of ‘none’, ‘low’, ‘medium’, ‘high’ (str; default: ‘none’) [default=”none”].

xsh_respon_slit_nod.param.time_stamp

Add timestamp to product file name. (bool; default: False) [default=False].

xsh_respon_slit_nod.param.decode_bp

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. (int; default: 1875902463) [default=1875902463].

xsh_respon_slit_nod.param.pre_overscan_corr

pre-overscan correction. 0: no correction 1: mean overscan correction 2: mean prescan correction 3: (mean pre+mean overscan)/2 correction (int; default: 1) [default=1].

xsh_respon_slit_nod.param.stack_method

Method used to build master frame. (str; default: ‘median’) [default=”median”].

xsh_respon_slit_nod.param.klow

Kappa used to clip low level values, when method is set to ‘mean’ (float; default: 5.0) [default=5.0].

xsh_respon_slit_nod.param.khigh

Kappa used to clip high level values, when method is set to ‘mean’ (float; default: 5.0) [default=5.0].

xsh_respon_slit_nod.param.removecrhsingle_sigmalim

Poisson fluctuation threshold to flag CRHs (see van Dokkum, PASP,113,2001,p1420-27) (float; default: 20.0) [default=20.0].

xsh_respon_slit_nod.param.removecrhsingle_flim

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].

xsh_respon_slit_nod.param.removecrhsingle_niter

Max number of iterations (int; default: 4) [default=4].

xsh_respon_slit_nod.param.rectify_kernel

Name of the Interpolation Kernel Used. Possible values are: tanh, sinc, sinc2, lanczos, hamming, hann. (str; default: ‘tanh’) [default=”tanh”].

xsh_respon_slit_nod.param.rectify_radius

Rectify Interpolation radius [bin units]. (float; default: 2.0) [default=2.0].

xsh_respon_slit_nod.param.rectify_bin_lambda

Wavelength step in the output spectrum [nm] (float; default: -1.0) [default=-1.0].

xsh_respon_slit_nod.param.rectify_bin_slit

Spatial step along the slit in the output spectrum [arcsec] (float; default: -1.0) [default=-1.0].

xsh_respon_slit_nod.param.rectify_fast

Fast if TRUE (Rect[B-A] = -Rect[A-B]), in that case only entire pixel shifts are applied. (bool; default: True) [default=True].

xsh_respon_slit_nod.param.localize_method

Localization method (MANUAL, MAXIMUM, GAUSSIAN) used to detect the object centroid and height on the slit (str; default: ‘MANUAL’) [default=”MANUAL”].

xsh_respon_slit_nod.param.localize_chunk_nb

Number of chunks in the full spectrum to localize the object (int; default: 10) [default=10].

xsh_respon_slit_nod.param.localize_thresh

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].

xsh_respon_slit_nod.param.localize_deg_lambda

Degree in lambda in the localization polynomial expression slit=f(lambda), used only for MAXIMUM and GAUSSIAN (int; default: 0) [default=0].

xsh_respon_slit_nod.param.localize_slit_position

Object position on the slit for MANUAL localization [arcsec] (float; default: 0.0) [default=0.0].

xsh_respon_slit_nod.param.localize_slit_hheight

Object half height on the slit for MANUAL localization [arcsec] (float; default: 2.0) [default=2.0].

xsh_respon_slit_nod.param.localize_kappa

Kappa value for sigma clipping in the localization polynomial fit (float; default: 3.0) [default=3.0].

xsh_respon_slit_nod.param.localize_niter

Number of iterations for sigma clipping in the localization polynomial fit (int; default: 3) [default=3].

xsh_respon_slit_nod.param.localize_use_skymask

TRUE if we want to mask sky lines using SKY_LINE_LIST file. (bool; default: False) [default=False].

xsh_respon_slit_nod.param.localize_nod_throw

Step (arcsec) between A and B images in nodding mode. (float; default: 0.0) [default=0.0].

xsh_respon_slit_nod.param.extract_method

Method used for extraction (LOCALIZATION, NOD) (str; default: ‘NOD’) [default=”NOD”].

xsh_respon_slit_nod.param.stdextract_interp_hsize

Half size of mask used to define object cross order profile (int; default: 30) [default=30].

xsh_respon_slit_nod.param.combinenod_throwlist

Name of ascii file containing the list of throw shifts with respect to the first exposure (str; default: ‘throwlist.asc’) [default=”throwlist.asc”].

xsh_respon_slit_nod.param.combinenod_method

Combination method for nodded frames (MEDIAN, MEAN) (str; default: ‘MEAN’) [default=”MEAN”].

xsh_respon_slit_nod.param.max_slit

Lower Slit Limit (localize and extract (float; default: 5.7) [default=5.7].

xsh_respon_slit_nod.param.min_slit

Upper Slit Limit (localize and extract (float; default: -5.3) [default=-5.3].

xsh_respon_slit_nod.param.correct_tellurics

TRUE if during response computation we apply telluric correction (bool; default: True) [default=True].

xsh_respon_slit_nod.param.correct_sky_by_median

TRUE if the resampled spectrum at each wavelength is median subtracted to remove sky lines (bool; default: True) [default=True].

xsh_respon_slit_nod.param.scale_combine_nod_method

frame scaling when nod frames are combined: 0 (no-scaling); 1 (scaling) (int; default: 1) [default=1].

The following code snippet shows the default settings for the available parameters.

import cpl
xsh_respon_slit_nod = cpl.Recipe("xsh_respon_slit_nod")

xsh_respon_slit_nod.param.keep_temp = "no"
xsh_respon_slit_nod.param.debug_level = "none"
xsh_respon_slit_nod.param.time_stamp = False
xsh_respon_slit_nod.param.decode_bp = 1875902463
xsh_respon_slit_nod.param.pre_overscan_corr = 1
xsh_respon_slit_nod.param.stack_method = "median"
xsh_respon_slit_nod.param.klow = 5.0
xsh_respon_slit_nod.param.khigh = 5.0
xsh_respon_slit_nod.param.removecrhsingle_sigmalim = 20.0
xsh_respon_slit_nod.param.removecrhsingle_flim = 2.0
xsh_respon_slit_nod.param.removecrhsingle_niter = 4
xsh_respon_slit_nod.param.rectify_kernel = "tanh"
xsh_respon_slit_nod.param.rectify_radius = 2.0
xsh_respon_slit_nod.param.rectify_bin_lambda = -1.0
xsh_respon_slit_nod.param.rectify_bin_slit = -1.0
xsh_respon_slit_nod.param.rectify_fast = True
xsh_respon_slit_nod.param.localize_method = "MANUAL"
xsh_respon_slit_nod.param.localize_chunk_nb = 10
xsh_respon_slit_nod.param.localize_thresh = 0.1
xsh_respon_slit_nod.param.localize_deg_lambda = 0
xsh_respon_slit_nod.param.localize_slit_position = 0.0
xsh_respon_slit_nod.param.localize_slit_hheight = 2.0
xsh_respon_slit_nod.param.localize_kappa = 3.0
xsh_respon_slit_nod.param.localize_niter = 3
xsh_respon_slit_nod.param.localize_use_skymask = False
xsh_respon_slit_nod.param.localize_nod_throw = 0.0
xsh_respon_slit_nod.param.extract_method = "NOD"
xsh_respon_slit_nod.param.stdextract_interp_hsize = 30
xsh_respon_slit_nod.param.combinenod_throwlist = "throwlist.asc"
xsh_respon_slit_nod.param.combinenod_method = "MEAN"
xsh_respon_slit_nod.param.max_slit = 5.7
xsh_respon_slit_nod.param.min_slit = -5.3
xsh_respon_slit_nod.param.correct_tellurics = True
xsh_respon_slit_nod.param.correct_sky_by_median = True
xsh_respon_slit_nod.param.scale_combine_nod_method = 1

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_nod = cpl.Recipe("xsh_respon_slit_nod")
[...]
res = xsh_respon_slit_nod( ..., param = {"keep_temp":"no", "debug_level":"none"})

See also

cpl.Recipe for more information about the recipe object.

Bug reports

Please report any problems to P.Goldoni, L.Guglielmi, R. Haigron, F. Royer, D. Bramich A. Modigliani. Alternatively, you may send a report to the ESO User Support Department.