DPS 35th Meeting, 1-6 September 2003
Session 19. Mars Surface II
Poster, Highlighted on, Wednesday, September 3, 2003, 3:00-5:30pm, Sierra Ballroom I-II

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[19.10] Revised Modified Gaussian Model Analyses of Martian Meteorite Spectra

M. Parente (Stanford University), J. Bishop (SETI Institute/NASA-ARC)

Modified Gaussian Model (MGM) analyses have been performed on visible/near-infrared (VNIR) reflectance spectra of several Martian meteorites. Revisions have been made to the code initially presented by Sunshine et al. (1990). This revised code is being tested for use in mineral abundance detection for mixtures. Preliminary analyses on spectra of chips and powders of meteorite ALH 84001 resulted in bands near 0.92 and 1.9 m due to low-Ca pyroxene, as well as bands near 1.0, 1.2 and 2.2 m due to a small amount of high-Ca pyroxene (mineral bands are shown in blue, ALH 84001 split 271 spectrum shown in orange). Spectra of meteorites EETA 79001 (lithologies A, B), Los Angeles, DaG 670, and NWA 1068 are also under study and include bands due to high- and low-Ca pyroxene, olivine, and Fe-bearing glass. Our goal is to create tools for mineral searches on Mars using the Omega and Crism datasets.


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Bulletin of the American Astronomical Society, 35 #4
2003. The American Astronomical Society.