OMEGA/Mars Express Observations of the Martian Dust

Details OMEGA/Mars Express Observations of the Martian Dust OMEGA/Mars Express Observations of the Martian Dust

Nov 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004dps....36.3107f&link_type=abstract

American Astronomical Society, DPS meeting #36, #31.07; Bulletin of the American Astronomical Society, Vol. 36, p.1137

Astronomy and Astrophysics

Astronomy

Scientific paper

The OMEGA spectro-imaging system aboard the Mars Express (MEx) mission covers the 0.35-5.1 μ m wavelength range at a resolving power of 200. Since MEx orbit insertion in late 2003, OMEGA observations have covered a wide variety of latitudes, longitudes, and a third of a martian year. We present here the dust content of the martian atmosphere as inferred from the OMEGA dataset. Three different and complementary techniques were used : (i) analysis of limb observations to retrieve the dust vertical profile at selected locations, (ii) analysis of observations relative to the same spot at different emission and phase angles, allowing us to disentangle dust spectral characteristics from surface features, (iii) analysis of the reflected light in the 2.7-μ m CO2 band to map the dust opacity above 20 km independently of the surface albedo.

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