HR: 0800h
AN: P11A-0958    [Abstracts]
TI: Mineral Classification of the Martian Surface Using THEMIS Multi-Spectral Infrared Imagery
AU: * Osterloo, M M
EM: osterloo@lanl.gov
AF: Los Alamos National Laboratory, ISR-1,P.O. Box 1663, MS D466, Los Alamos, NM 87545
AU: Brumby, S P
EM: brumby@lanl.gov
AF: Los Alamos National Laboratory, ISR-1,P.O. Box 1663, MS D466, Los Alamos, NM 87545
AU: Funsten, H O
EM: hfunsten@lanl.gov
AF: Los Alamos National Laboratory, ISR-1,P.O. Box 1663, MS D466, Los Alamos, NM 87545
AU: Feldman, W C
EM: wfeldman@lanl.gov
AF: Los Alamos National Laboratory, ISR-1,P.O. Box 1663, MS D466, Los Alamos, NM 87545
AB: Recent advancements in multi-spectral imaging and image analysis techniques have greatly enhanced our ability to do planetary research. Much has been discovered about Mars through recent missions such as Mars Global Surveyor, 2001 Mars Odyssey, and the Mars Exploration Rovers. The Thermal Emission Spectrometer on board the Mars Global Surveyor has allowed the mapping of surface mineralogies on Mars at several kilometers scale through hyperspectral imaging [1]. Here, we use the high resolution multi-spectral imagery of THEMIS (THermal Emission Imaging System) on board the 2001 Mars Odyssey to identify different mineral classes at spatial scales of hundreds of meters. THEMIS contains two independent multi-spectral imaging systems: a 10-band thermal infrared imager (IR) with a resolution of 100m/pixel, and a 5-band visible imager with a resolution of 10m/pixel. Here we will use the IR data. The 9 IR bands are centered from 6.8 microns to 14 .9 microns [2]. Using Arizona State University's online spectral library[3], we have been investigating the extent to which we can differentiate between different mineral classes. By identifying certain mineral classes we can better understand the geologic processes which created them and detect areas of interest for further study. Linear mixing of minerals and dust is investigated to estimate ratios of minerals and their resulting spectra. We then compare these spectra to observations of several regions on Mars. We compare these results with TES data and previous mineralogical maps. [1] Christensen et al, (2001) JGR 106, E10; [2] Christensen et al, (2002) Space Science Reviews 110, 1; [3] Christensen et al, (2000) JGR 105, E4
DE: 5464 Remote sensing
DE: 5470 Surface materials and properties
SC: Planetary Sciences [P]
MN: 2004 AGU Fall Meeting