Thermal Emission Spectrometer (TES) Observations of the Martian Atmosphere During the MGS Mission

Details Thermal Emission Spectrometer (TES) Observations of the Martian Atmosphere During the MGS Mission Thermal Emission Spectrometer (TES) Observations of the Martian Atmosphere During the MGS Mission

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.0323p&link_type=abstract

American Astronomical Society, DPS meeting #28, #03.23; Bulletin of the American Astronomical Society, Vol. 28, p.1069

Astronomy and Astrophysics

Astronomy

Scientific paper

The TES experiment on the Mars Global Surveyor mission is well suited to make atmospheric observations of Mars. Its spectral range is 200-1650 cm-1 (6-50 microns), with selectable resolutions of 5 and 10 cm-1. In addition, it has two broadband channels covering the visible (0.3-2.7 microns), and thermal (5.5-100 microns) regions of the spectrum. Each of the spectral, visible and thermal channels is provided with a 2x3 detector array; all of the arrays are boresighted. The instrument also has a single-axis rotating pointing mirror that provides unobstructed viewing over a range of nearly 180 degrees; during mapping operations, this will enable scanning from the nadir to well above the limb, both ahead of and behind the spacecraft. From the mapping altitude, the projected size of the individual pixels will be 3 km at nadir, and 13 km on the limb. Included in the spectral range of TES are the 15 micron band of CO2, the 10 and 20 micron features of silicate dust, the 45 and 12 micron water ice signatures, and rotational water vapor lines below 50 microns. This will allow determination of such quantities as atmospheric thermal structure, dust and ice aerosol abundances and properties, and water vapor abundance. Different observational constraints exist during aerobraking, when large portions of the disk will be mapped (179

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