Martian Surface Compositions and Spectral Unit Mapping From the Thermal Emission Imaging System

Details Martian Surface Compositions and Spectral Unit Mapping From the Thermal Emission Imaging System Martian Surface Compositions and Spectral Unit Mapping From the Thermal Emission Imaging System

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufm.p21c0157b&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #P21C-0157

Mathematics

Logic

5464 Remote Sensing, 5470 Surface Materials And Properties, 5480 Volcanism (6063, 8148, 8450), 5494 Instruments And Techniques, 6225 Mars

Scientific paper

The Thermal Emission Imaging System (THEMIS) on board the Mars Odyssey spacecraft observes Mars at nine spectral intervals between 6 and 15 microns and at 100 meter spatial sampling. This spectral and spatial resolution allows for mapping of local spectral units and coarse compositional determination of a variety of rock-forming materials such as carbonates, sulfates, and silicates. A number of data processing and atmospheric correction techniques have been developed to ease and speed the interpretation of multispectral THEMIS infrared images. These products and techniques are in the process of being made publicly available via the THEMIS website and were used to produce the results presented here. Spectral variability at kilometer scales in THEMIS data is more common in the southern highlands than in the northern lowlands. Many of the spectral units are associated with a mobile surface layer such as dune fields and mantled dust. However, a number of spectral units appear to be directly tied to the local geologic rock units. These spectral units are commonly associated with crater walls, floors, and ejecta blankets. Other surface compositions are correlated with layered volcanic materials and knobby remnant terrains. Most of the spectral variability observed to date appears to be tied to a variation in silicate mineralogy. Olivine rich units that have been previously reported in Nili Fossae, Ares Valles, and the Valles Marineris region appear to be sparse but common in a number of regions in the southern highlands. Variations in silica content consistent with previously reported global surface units also appear to be present in THEMIS images, allowing for an examination of their local geologic context. Previously reported quartz and feldspar rich exposures in northern Syrtis Major appear more extensive in the region than previously reported. A coherent global and local picture of the mineralogy of the Martian surface is emerging from THEMIS measurements along with other orbital thermal and near infrared spectroscopy measurements from the Mars Express and Mars Global Surveyor spacecraft.

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