OMEGA ground calibration results: implications for the science return

Details OMEGA ground calibration results: implications for the science return OMEGA ground calibration results: implications for the science return

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....9373b&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #9373

Computer Science

Performance

Scientific paper

An extensive ground calibration campaign has been performed for the OMEGA imaging spectrometer on board Mars Express, so as to evaluate its performances in terms of photometric response, spectral resolution and pointing offsets between spectral channels. OMEGA is constituted of two units: a pushbroom visible spectrometer (128 pixels, 96 or 144 spectels from 0.36 to 1.1 μm) and a whiskbroom IR spectrometer with a single slit and two channels (128 spectels each) covering a spectral range of 0.93 to 2.73 μm and 2.55 to 5.11 μm respectively. The whiskbroom IR unit uses a flat scanning mirror in front of the primary. This means that to first order the photometric response, spectral positions and relative looking directions of the 256 spectels do not depend on the position of the scanning mirror. On the contrary, as the visible pushbroom spectrometer projects its slit on a 2-D detector, the phometric response, spectral positions and relative looking directions depend on the selected pixel. Spectra in representative Mars observation conditions have been derived from the results of the ground calibration. The consequences of the photometric response and the offsets between spectels on the scientific return of the OMEGA instrument will be presented.

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