| This documentation is intended both for QC scientists and SciOps astronomers (who may want to ignore the technical information displayed in grey). | ||||||||||||||||||||||||
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| bottom plots | contact | ||||||||||||||||||||||||
| NAME | qc_TELLURIC.sh | |||||||||||||||||||||||
| VERSION |
1.0 -- 2006-07-25 fill template by handbook 1.1 -- 2006-07-26 verified and completed 1.2 -- 2007-07-13 functionality extended 1.3 -- 2008-01-09 trending plots migrated 1.4 -- 2008-04-25 writeQC | |||||||||||||||||||||||
| SYNTAX | SHELL | |||||||||||||||||||||||
| CALL |
called by processQC as qc_TELLURIC -d $DATE -f $primfile | |||||||||||||||||||||||
| INSTRUMENT | ISAAC | |||||||||||||||||||||||
| RAWTYPE | TELLURIC SW_SP_FLUX | |||||||||||||||||||||||
| PURPOSE |
a) generates QC report b) writes QC1 parameters into local list The script reads the the OCS.SELECT-ARM SW_N_TELLURIC, SW_G_TELLURIC, LW_N_TELLURIC, LW_C_TELLURIC, LW_G_TELLURIC, SW_SP_FLUX The script is called for telluric standard stars and for monthly flux standard stars. The first part of the script is applied for both TELL and FLUX. The second part is applied to flux standards alone. The telluric standard star is taken close in time (~1h) close in air mass (+-0.05) to the science spectrum using the same setup. The flux standard star is taken without slit using the four SW-LR settings. | |||||||||||||||||||||||
| PROCINPUT |
a) $DATE in yyyy-mm-dd, b) $primfile is the PRO.CATG=COADDED_STD product with the _0000.fits extension. c) raw frames are implicitely read from the AB. | |||||||||||||||||||||||
| QC1TABLE |
trending | table(s) in QC1 database: isaac_telluric | isaac_flux | |||||||||||||||||||||||
| TRENDPLOT |
trending | HealthCheck plot(s) associated to this procedure: trend_report_SP_TELL_SZ_HC.html | trend_report_SP_FLUX_SZ_HC.html | |||||||||||||||||||||||
| QC1PAGE |
trending | associated documentation: qc_IS_std.html | qc_IS_flux.html | |||||||||||||||||||||||
| QC1PLOTS top |
tellu0.png display the telluric standard star product image spectrum on RealTimeDisplay There should be one bright spectrum in the center and two negative spectra with half intensity. tellu1.png plot of the telluric standard star (red) together with some previous telluric standard stars with the same of similar setting. tellu2.png plot of the telluric standard star (black) together with some previous telluric standard stars with the same or similar setting, all normalized to the same scale. tellu3.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 tellu4.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 tellu5.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 sp_flux2.png extracted flux standard star spectrum in counts sp_flux3.png normalized spectrum and a recent one sp_flux4.png conversion factor derived from the flux standard sp_flux5.png efficiency and linear fit (blue) to a clean sepctral region (red bars) sp_flux6.png as tellu3.png sp_flux7.png This plot is generated for reasons of operational symmetry. It is the same as tellu4.png. There appear no sky lines in slitless spectroscopy. | |||||||||||||||||||||||
| 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 | [2012-06-20T10:57:21] created by qcDocu v1.1.2, a tqs tool | |||||||||||||||||||||||
