Bright soil units on Mars determined from ISM imaging spectrometer data

Details Bright soil units on Mars determined from ISM imaging spectrometer data Bright soil units on Mars determined from ISM imaging spectrometer data

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993lpi....24.1027m&link_type=abstract

In its Twenty-Fourth Lunar and Planetary Science Conference. Part 2: G-M p 1027-1028 (SEE N94-16173 03-91)

Mathematics

Logic

1

Absorption Spectra, Lithology, Mars Surface, Mineralogy, Moisture Content, Planetary Geology, Soil Moisture, Soils, Equatorial Regions, Imaging Spectrometers, Near Infrared Radiation, Optical Properties, Spatial Resolution, Temperature Distribution, Viking Mars Program

Scientific paper

The lithology of bright Martian soil provides evidence for chemical and physical processes that have modified the planet's surface. Data from the ISM imaging spectrometer, which observed much of the equatorial region at a spatial resolution of approximately 22 km, cover the NIR wavelength range critical to ascertaining the presence and abundance of Fe-containing phases, hydroxylated silicates, and H2O in the bright soil. ISM data previously have revealed spatial variations in depth of the 3.0-microns H2O absorption suggesting differences in water content, a weak absorption at 2.2 microns indicative of metal-OH in phyllosilicate, and variations in the 1-micron Fe absorption indicative of differences in Fe mineralogy. This paper summarizes first results of a systematic investigation of spectral heterogeneity in bright soils observed by ISM. At least seven 'units' with distinctive properties were discriminated. Comparison of their spatial distributions with Viking data shows that they generally correspond with previously recognized morphologic, color, and thermal features. These correspondences and the units' spectral attributes provide evidence for lithologic differences between the soils in different geologic settings.

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