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SINFONI:
Quality Control Parameters and Trending

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Instrument Properties Trended

SINFONI calibration data are pipeline-processed to create calibration products. The technical performance of the instrument is measured by QC1 parameters which are obtained by either pipeline procedures or QC-intrinsic python routines. All measured QC1 parameters are stored in the QC1 database. Their evolution with time is evaluated by the trending process. SINFONI QC1 parameters are routinely measured for all calibration and science products measured in SINFONI pipeline supported modes.

The plots shown here are trending plots. They show the evolution of the last 90, 180, or 365 days up to the date for which data have been processed by the pipeline in Garching. The latest date in the trending plots is usually 10 or more days behind the observing night due to the hard disk delivery times between South America and Europe. QC1 parameters of data still on their way to Europe are monitored via Health Check Plots. They are based on ftp transfer of data and are assessed within minutes.

The following properties of the SINFONI detector and instrument are trended:

 

  • DARKS (for DITS: 60, 120, 300, 600, and 900 seconds)
    • median level
    • sigma of median level
    • read-out noise
    • fixed-patttern noise
    • number of hot pixels
    • and ratio of odd/even column stripes

     

  • HCAO (only obtained for the K-band at the 25 mas pixel scale)
    • median strehl ratio
    • median encircled energy
    • standard deviation of the strehl ratio
    • mean flux of the extracted fibre spectrum

     

  • FLATS (all gratings: J, H, K, and H+K; and pixel scales: 25, 100, and 250 mas)
    • lamp efficiency
    • number of bad pixels
    • lamp-off flux
    • fixed-patttern noise (as measured in two different regions)
    • vignetting check

     

  • WAVE (all gratings: J, H, K, and H+K; and pixel scales: 25, 100, and 250 mas)
    • nominal wavelength
    • resolving power
    • nominal position of slitlet #17
    • FWHM of identified spectral lines
    • number of identified spectral lines
    • quality of image re-sampling

     

  • GAIN & LINEARITY (all gratings: J, H, K, and H+K)
    • detector gain
    • number of non-linear pixels
    • linearity coefficients: C0, C1, and C2

     

  • PUPIL
    • absolute centroid position
    • offset relative to nominal image center

     

  • DISTORTION (all gratings: J, H, K, and H+K)
    • average of 32 slitlet distances
    • distortion measure in five quadrants of detector
    • distortion coeficients: C00, C01, C10, C11, C20, C02, C21, and C12

     

  • STD (all gratings: J, H, K, and H+K; and pixel scales: 25, 100, and 250 mas)
    • mean flux per pixel within a 3 sigma aperture
    • median strehl ratio (i.e. the median over all wavelengths in cube)
    • persistence (over-flux) detection and number of pixels affected by persistence
    • image quality: SINFONI fwhm is compared to DIMM seeing (which has been corrected for airmass difference and converted to the infrared)

     

  • PSF (all gratings: J, H, K, and H+K; and pixel scales: 25, 100, and 250 mas)
    • mean flux per pixel within a 3 sigma aperture
    • median strehl ratio (i.e. the median over all wavelengths in cube)
    • persistence (over-flux) detection and number of pixels affected by persistence
    • image quality: SINFONI fwhm is compared to DIMM seeing (which has been corrected for airmass difference and converted to the infrared)

     

  • SCIENCE (trended data is combined for all gratings: J, H, K, and H+K; and pixel scales: 25, 100, and 250 mas)
    • persistence (over-flux) detection and number of pixels affected by persistence
    • difference in time and airmass to the nearest telluric standard star
    • difference in detector and grating temperature to the nearest wavelength calibration frame

     

     

     

     

     


 
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