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[1] The NASA Discovery Moon Mineralogy Mapper imaging spectrometer was selected to pursue a wide range of science objectives requiring measurement of composition at fine spatial scales over the full lunar surface. To pursue these objectives, a broad spectral range imaging spectrometer with high uniformity and high signal‐to‐noise ratio capable of measuring(More)
[1] High‐resolution compositional data from Moon Mineralogy Mapper (M 3) for the Moscoviense region on the lunar farside reveal three unusual, but distinctive, rock types along the inner basin ring. These are designated " OOS " since they are dominated by high concentrations of orthopyroxene, olivine, and Mg‐rich spinel, respectively. The OOS occur as small(More)
Absorption features on Phobos and Deimos in the visible/near infrared wavelength region (0.4–3.9 lm) are mapped using observations from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM). Fe 2+ electronic absorptions diagnostic of olivine and pyroxene are not detected. A broad absorption centered around 0.65 lm within the red spectral units of(More)
[1] Analysis of two absorption features near 3 mm in the lunar reflectance spectrum, observed by the orbiting M 3 spectrometer and interpreted as being due to OH and H 2 O, is presented, and the results are used to discuss the processes producing these molecules. This analysis focuses on the dependence of the absorptions on lunar physical properties,(More)
Introduction: Almost all lunar multi-ringed impact basins have been eroded by impacts or filled by mare volcanism. One multi-ringed basin, Orientale, remains largely unfilled by mare volcanism and offers substantial clues to the nature of basin forming events and their early evolution. The Orientale basin (~930 km in diameter) (Fig. 1), the youngest (~3.82(More)
Introduction: The VIMS imaging spectrometer onboard CASSINI provides hyperspectral images of Titan in 352 spectral channels from 0.3 to 5.1 µm [1]. A giant cloud system covering the north pole of Titan was observed in December 2006 using infrared wavelengths. We report here on the processing and analysis of the corresponding VIMS data. (T22 flyby), VIMS(More)
Introduction: Gale Crater is a ~150 km diameter impact crater located at 5.3°S, 137.7°E that contains a thick (>5 km) sequence of strata interpreted as sedi-mentary rocks [1]. Gale is one of four final candidate landing sites for the 2011 Mars Science Laboratory (MSL) rover. Recent data acquired by the Compact Reconnaissance Imaging Spectrometer for Mars(More)