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VIMOS Quality Control:
image quality

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Trending & QC1
   image qual
Data Package
Data Management
QC links:
IQ vs. seeing
QC1 database (advanced users): browse | plot
Click on HISTORY to see the historical evolution of the trending.

Image quality is calculated from each science frame taken in imaging mode. SExtractor (Bertin and Arnouts 1996, A&A 117, 393) is run on the reduced images to detect objects, compute their FWHM and ellipticity, and select stars. If the number of stars (i.e. objects with stellarity index > 0.5) found is at least 10, the image quality is assumed to be the median of the FWHM of the stars. Outliers (3 sigma) are iteratively excluded for the final value (up to 4 iterations).

The expected image quality is derived from the DIMM seeing measurements that are stored in the header of the science frames when the DIMM seeing monitor is operational. The keywords "TEL AMBI FWHM START" and "TEL AMBI FWHM END" store DIMM seeing measurements at start and at the end of the exposure, respectively. The average is computed and assumed as the DIMM seeing value of the exposure. Because DIMM measurements are done at zenith and at 0.5 micron, the DIMM values are reduced to the zenith angles and wavelengths of the science observation, in addition a first order outer scale correction appropriate for a 8m telescope is applied. The formula used to obtain the expected image quality is given by M. Sarazin.

Processing of science observations was discontinued as of 3 October 2011. Access to QC1 parameters and trending is available for historical data.
top Image quality

QC1 parameters

parameter QC1 database: table, name procedure
image quality vimos_sci_img, fwhm_median median of FWHM of detected stars
seeing vimos_sci_img, dimm_seeing expected image quality, corrected DIMM seeing


Trending shows the image quality of each science frame vs. the expected image quality.