QC documentation system: QC procedure xshooter_std_slit_nodoff.py for XSHOOTER

This documentation is intended both for QC scientists and SciOps astronomers (who may want to ignore the technical information displayed in grey).   HOME   CRIRES FORS1 FORS2 KMOS NACO   GIRAFFE UVES XSHOOTER   ISAAC SPHERE VIMOS VISIR   HAWKI MUSE SINFONI   AMBER GRAVITY MIDI PIONIER   ESPRESSO   OMEGACAM VIRCAM [best viewing with style sheets and javascript enabled] xshooter_bias.py xshooter_dark.py xshooter_dark_nir.py xshooter_detlin.py xshooter_fmtchk.py xshooter_orderdef.py xshooter_wave.py xshooter_flexure.py xshooter_flat_slit.py xshooter_arc_slit.py xshooter_flat_ifu.py xshooter_arc_ifu.py xshooter_std_slit_stare.py xshooter_std_slit_nodoff.py xshooter_sci_slit_stare.py xshooter_sci_slit_nodoff.py xshooter_sci_ifu.py   bottom  plots   |   contact NAME xshooter_std_slit_nodoff.py VERSION 1.0 -- September 2009 1.1 -- 2017-01-01 new plots included 1.2 -- 2017-10-01 docu updated SYNTAX PYTHON CALL processQC from $DFS_PRODUCT/STD_TELL_SLIT_NOD_<arm>/$DATE /home/python/xshooter_sci_slit_nod.py -i -a $AB INSTRUMENT XSHOOTER RAWTYPE STD_TELL_SLIT_STARE_NIR | STD_TELL_SLIT_STARE_VIS STD_TELL_SLIT_NOD_NIR | STD_TELL_SLIT_NOD_VIS STD_TELL_SLIT_OFF_NIR | STD_TELL_SLIT_OFF_VIS STD_FLUX_SLIT_STARE_NIR | STD_FLUX_SLIT_STARE_VIS | STD_FLUX_SLIT_STARE_UVB STD_FLUX_SLIT_NOD_NIR | STD_FLUX_SLIT_NOD_VIS | STD_FLUX_SLIT_NOD_UVB STD_FLUX_SLIT_OFF_NIR | STD_FLUX_SLIT_OFF_VIS | STD_FLUX_SLIT_OFF_UVB PURPOSE QC check of processed standard star exposures, extracted spectra, and other products PROCINPUT raw and product standard star and science frames QC1TABLE trending | table(s) in QC1 database: xshooter_telluric | xshooter_flux TRENDPLOT trending | HealthCheck plot associated to this procedure: none QC1PAGE trending | associated documentation: standard_qc1.html QC1PLOTS top std_flux_slit_nod_UVB_X00.png extracted merged 1D spectrum std_flux_slit_nod_UVB_X04.png Moffat function fit to line spread function to monitor spectrum curvature std_flux_slit_nod_UVB_0005.png response function, with master response, D2 lamp std_flux_slit_nod_UVB_0006.png response function, with master response, QTH lamp std_flux_slit_nod_UVB_0007.png response function, with reference response, D2 lamp std_flux_slit_nod_UVB_0008.png response function, with reference response, QTH lamp std_flux_slit_nod_UVB_A02.png full display of merged 2D SCI_SLIT_NOD_UVB frame, broken in four parts std_flux_slit_nod_UVB_A03.png full display of merged 2D SCI_SLIT_NOD_UVB frame std_flux_slit_nod_VIS_X00.png extracted merged 1D spectrum std_flux_slit_nod_VIS_X04.png Moffat function fit to line spread function to monitor spectrum curvature std_flux_slit_nod_VIS_0005.png response function, with master response std_flux_slit_nod_VIS_0007.png response function, with reference response std_flux_slit_nod_VIS_A02.png full display of merged 2D oCI_SLIT_NOD_VIS, broken in four parts std_flux_slit_nod_VIS_A03.png full display of merged 2D SCI_SLIT_NOD_VIS frame std_flux_slit_nod_NIR_X00.png extracted merged 1D spectrum std_flux_slit_nod_NIR_X04.png Moffat function fit to line spread function to monitor spectrum curvature std_flux_slit_nod_NIR_0005.png response function, with master response std_flux_slit_nod_NIR_0007.png response function, with reference response std_flux_slit_nod_NIR_A02.png full display of merged 2D SCI_SLIT_NOD_NIR frame, broken in two parts full display of merged 2D SCI_SLIT_NOD_NIR frame std_flux_slit_nod_NIR_A02.png full display of merged 2D SCI_SLIT_NOD_NIR frame, broken in two parts full display of merged 2D SCI_SLIT_NOD_NIR frame std_tell_slit_nod_VIS_A02.png full display of merged 2D frame, broken in four parts std_tell_slit_nod_VIS_A03.png full display of merged 2D frame std_tell_slit_nod_VIS_X00.png 1D spectrum, orders highlighted by shifts std_tell_slit_nod_VIS_X04.png Moffat function fit to line spread function to monitor spectrum curvature std_tell_slit_nod_VIS_X14.png molecfit best fit to wavelength fitting regions std_tell_slit_nod_VIS_X10.png calctrans corrected spectrum part1 (very blue) std_tell_slit_nod_VIS_X11.png calctrans corrected spectrum part2 (blue) std_tell_slit_nod_VIS_X12.png calctrans corrected spectrum part3 (red) std_tell_slit_nod_VIS_X13.png calctrans corrected spectrum part4 (very red) std_tell_slit_nod_NIR_A02.png full display of merged 2D frame, broken in four parts std_tell_slit_nod_NIR_A03.png full display of merged 2D frame std_tell_slit_nod_NIR_X00.png 1D spectrum, orders highlighted by shifts std_tell_slit_nod_NIR_X04.png Moffat function fit to line spread function to monitor spectrum curvature std_tell_slit_nod_NIR_X14.png molecfit best fit to wavelength fitting regions std_tell_slit_nod_NIR_X10.png calctrans corrected spectrum part1 (very blue) std_tell_slit_nod_NIR_X11.png calctrans corrected spectrum part2 (blue) std_tell_slit_nod_NIR_X12.png calctrans corrected spectrum part3 (red) std_tell_slit_nod_NIR_X13.png calctrans corrected spectrum part4 (very red) QC1PARAM QC1 parameters written in QC1 database: # QC1db names: flux<i> (i=1...3) | err<i> (i=1...3) | sn<i> (i=1...3) | npix_sat | fpix_sat FITS key names: QC.FLUXi.VAL (i=1...3) | QC.FLUXi.ERR (i=1...3) | QC.FLUXi.SN (i=1...3) | QC.NPIXSAT | QC.FPIXSAT QC1db names: peak_eff_<i> (i=1...16) | med_eff_<i> (i=1...16) | npix_sat | npix_high FITS key names: QC.EFF.PEAK.ORD.i (i=1...16) | QC.EFF.MED.ORD.i (i=1...16) | QC.NPIXSAT | num_sat npix_sat (in this script) = npix_high (in QC1 DB) is the number of pixel above 60000|60000|42000 ADU in a raw frame; the highest among any raw frame ALGORITHM CERTIF Reasons for rejection: saturation or flux below 1000 ADU in extracted 1D spectrum (TELL) saturation or bad sky correction (FLUX) COMMENTS top [2020-11-18T14:49:14]         created by qcDocu v1.1.2, a tqs tool