Mathematics – Logic
Scientific paper
Oct 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000p%26ss...48.1393l&link_type=abstract
Planetary and Space Science, Volume 48, Issue 12-14, p. 1393-1405.
Mathematics
Logic
50
Scientific paper
The spectrum of Mars at 2.4-45μm has been observed on July 31, 1997 (Ls=157°) by the short-wavelength spectrometer of the Infrared Space Observatory. The data consist of a high signal to noise, complete grating spectrum (resolving power /R~1500-2500) and portions of the 20-40μm spectrum observed in Fabry-Perot mode /(R~31000). The data show the infrared bands of known martian atmospheric species (CO2,H2O, and CO) with an unprecedented amount of details. The vertical distribution of H2O is determined, showing saturation near 10 km. Evidence for scattering in the saturated CO2 band at 2.7μm and for fluorescence emission in the CO24.3μm band is obtained. No detection of new atmospheric species is achieved, but upper limits are obtained for CH4 and H2CO. In the solar reflected part of the spectrum, which dominates at λ<=4.2μm, the surface reflectance clearly shows the hydration band with maximum absorption at 2.9μm, from which a 2.0-2.7% (by weight) water content in the martian uppermost layer is estimated. A decrease of reflectance from 3.8 to 5μm is also seen. This behaviour is consistent with basalts and palagonite, but not hematite. In the thermal part, mineralogic signatures at 5-12μm are globally consistent with a basaltic composition. Specific minima are also detected at 5.7, 6.3 (tentative), 7.2 and 11.1μm. Reexamination of earlier datasets indicates that the latter two have been observed before, although generally not discussed. The presence of additional absorptions at 26.5, 31 and 43.5μm is also indirectly suggested. Carbonate minerals are tentatively detected from this ensemble of features, though no single carbonate species can be unambiguously identified.
Burgdorf Martin
Crovisier Jacques
de Graauw Th.
Encrenaz Th.
Erard Stephane
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