QC documentation system: QC procedure qc_SCI_SPEC for ISAAC

This documentation is intended both for QC scientists and SciOps astronomers (who may want to ignore the technical information displayed in grey).   HOME   CRIRES FORS2   FORS1 GIRAFFE UVES XSHOOTER   ISAAC VIMOS VISIR   HAWKI NACO SINFONI   AMBER MIDI   OMEGACAM VIRCAM [best viewing with style sheets and javascript enabled] qc_DARK qc_CHECK_FLAT qc_IMG_FLAT qc_SP_FLAT qc_ZPOINT qc_TELLURIC qc_SP_ARC qc_STARTRACE qc_SLIT qc_ILLU qc_LINE qc_SCI_IMG qc_SCI_SPEC   bottom  plots   |   contact NAME qc_SCI_SPEC.sh VERSION 1.0 -- 2006-07-25 fill template by handbook 1.1 -- 2008-01-10 migrate to trendPlotter, new QC reports SYNTAX SHELL CALL called by processQC as qc_SCI_SPEC -d $DATE -f $primfile INSTRUMENT ISAAC RAWTYPE SCI_SPEC PURPOSE a) calculates post-pipeline FPN and OES QC1 parameters b) generates QC report c) writes QC1 parameters into local list The script reads the the OCS.SELECT-ARM SW_N_SCI_SPEC, SW_G_SCI_SPEC, LW_N_SCI_SPEC, LW_C_SCI_SPEC, LW_G_SCI_SPEC, SW_SP_FLUX PROCINPUT a) $DATE in yyyy-mm-dd, b) $primfile is the PRO.CATG=COADD_STD product with the _0000.fits extension. c) raw frames are implicitely read from the AB. QC1TABLE trending | table(s) in QC1 database: isaac_sci_spec TRENDPLOT trending | HealthCheck plot(s) associated to this procedure: trend_report_SCI_SPEC_SLK_HC.html | trend_report_SCI_SPEC_SMK_HC.html QC1PAGE trending | associated documentation: qc_IS_SCI_SPEC.html QC1PLOTS top sci_spec0.png display STD on RealTimeDisplay sci_spec1.png plot of the brighest extracted spectrum sci_spec2.png plot of the brighest extracted specrtum (red), one of the telluric standard stars scaled in intensity (blue) and the ratio spectrum in pixel coords sci_spec3.png UL: median sky derived from raw frames UR: relative offset within the nodding sequence LL: raw spectrum instensity relative to the one of the first frame LR: cumuative offset within the nodding sequence sci_spec4.png RED: median collapsed image of first raw frame (sky spectrum) GREEN: median collapsed image of last raw frame (sky spectrum) BLUE: OH line atlas with fluxes, to check wavelngth calibration sci_spec5.png upper: PSF derived from median collapsed product frame upper: Gaussian fit with sigma anf Moffat fit with R (~width) and beta (~ wing) lower: PSF derived from raw frame at x=400 (red) and x=600 (green) lower: The x=400 raw frame PSF is fit by a Gaussian and a Moffat QC1PARAM QC1 parameters written into QC1 table: FITSNAME, DBNAME , typical value, description: wavelength solution parameters of sky/physical model wavelength solution parameters of of day-time arcs wavelength offset between both solutions up to 2006 In case the MAG and MK-type of the telluric is found in the catalog NONE , A linear fit of F = A + B * lambda to response function in interval NONE , B linear fit of F = A + B * lambda to response function in interval ALGORITHM Description of algorithms: wavelength : is just to monitor the difference between night time and day-time spectroscopic setting (mostly the few pixdel offset). response : Only for SW LR setting a linear function is fit to the response function. The intervals are given by: SZ: [10000:11000] J: [11700:13300] SH: [15000:17500] SK: [21000:24500] and are choosen to avoid impact of broad-band telluric features. CERTIF Quality diminishing features (not under control, but tolerated) : - tilted telluric features, see extra internal document - 50Hz noise (does not impact spectrum at these count rates) Reasons for rejection: - saturation - photon noise much less than that of science object - no signal COMMENTS From P78 on (Oct 2006) is is planned to implement an extra SW_SP_FLUX RAW_TYPE for reasons of technical throughput measurements in slitles spectroscopy top [2012-06-20T10:57:42]         created by qcDocu v1.1.2, a tqs tool