Automatic definition of spectral units in the equatorial regions of Mars

Details Automatic definition of spectral units in the equatorial regions of Mars Automatic definition of spectral units in the equatorial regions of Mars

Mar 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993lpi....24..443e&link_type=abstract

In Lunar and Planetary Inst., Twenty-fourth Lunar and Planetary Science Conference. Part 1: A-F p 443-444 (SEE N94-12015 01-91)

Computer Science

2

Equatorial Regions, Image Analysis, Imaging Spectrometers, Infrared Spectra, Infrared Spectrometers, Mars Surface, Planetary Composition, Planetary Geology, Remote Sensing, Absorption Spectra, Dust, Hydration, Mars Atmosphere, Mars Volcanoes, Mineralogy, Pixels, Spectral Bands, Spectral Reflectance

Scientific paper

ISM was the first instrument that acquired spectra of small areas (25x25 sq km) on a planetary surface. The data set consists mainly in images made up of about 3000 such pixels, each one corresponding to a near-infrared spectrum (0.76 to 3.15 microns in 128 spectral channels) with high signal-to-noise ratio. These data were used to define spectral units and to constrain the mineralogy of surface materials in the equatorial regions of the planet. Future spaceborne imaging spectrometers (e.g. OMEGA on board the Mars-94 Russian spacecraft) are expected to provide several hundred times as much data as ISM, so there's a strong need for fast and reliable processing methods. The present work is an attempt to define spectral units in the region of Syrtis Major-Isidis Planitia by means of G-mode analysis. The method allows to cluster the spectra according to their similarities; different levels of classification can be achieved by tuning a threshold of confidence.

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