Linear spectral unmixing of near-infrared hyperspectral data from Juventae Chasma, Mars

Details Linear spectral unmixing of near-infrared hyperspectral data from Juventae Chasma, Mars Linear spectral unmixing of near-infrared hyperspectral data from Juventae Chasma, Mars

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spie.7477e..19w&link_type=abstract

Image and Signal Processing for Remote Sensing XV. Edited by Bruzzone, Lorenzo; Notarnicola, Claudia; Posa, Francesco. Proceedi

Mathematics

Logic

Scientific paper

Juventae Chasma is a depression north of Valles Marineris on Mars, approximately 185 km wide and 270 km long. It contains several mounds of light-toned, layered deposits several tens of kilometers of maximum extension and up to 3300 m in elevation. Near infrared spectral data from the Observatoire pour l'Eau, des Glaces et l'Activité onboard ESA's Mars Express indicated mono- and polyhydrated sulfates as main constituents of these deposits, including gypsum in one of the mounds (Gendrin et al., 2005, Science). We analyze the light-toned outcrops based on data from NASA's Compact Reconnaissance Imaging Spectrometer for Mars (CRISM), featuring an increased spatial resolution of up to 18m/pixel and increased spectral resolution of 7 nm. We perform Spectral Mixture Analysis (SMA) in order to introduce physical modeling and to enhance some surface units. We use one type of SMA, the Multiple-Endmember Linear Unmixing Model MELSUM (Combe et al., 2008, PSS), which guarantees positive mixing coefficients and allows us to limit the number of spectral components used at a time. We use linear unmixing both as a similarity measure using spectra from the image itself as endmembers to assess the internal variability of the data, and to detect mineral spectra within the observations. We successfully confirm the presence of the monohydrated sulfate szomolnokite (previously detected by Kuzmin et al., 2008, and Rossi et al., 2008) in all of the four light-toned deposits observed. Based on our analysis, we reject the presence of gypsum on mound B (previously detected by Gendrin et al., 2005). A possible match for the polyhydrated sulfate present here could be rozenite, but other sulfate minerals also have to be considered. The implications of the possible presence of iron bearing polyhydrated sulfates such as rozenite and the absence of calcium - bearing gypsum for the geological history of the outcrops are not yet fully understood. Our next step is the geochemical modeling of the weathering of Martian basaltic rocks, dominated by iron and magnesium silicates, to iron bearing sulfates, under acidic conditions.

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