LE MOUELIC, S.; PAILLOU, Philippe; RODRIGUEZ, S.; CRAPEAU, M.; SOTIN, C.; HIRTZIG, M.; BROWN, R. H.; SODERBLOM, L.; CLARK, R.; BURATTI, B.

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PAILLOU, Philippe
Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux [L3AB]
Observatoire aquitain des sciences de l'univers [OASU]
Laboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]

RODRIGUEZ, S.

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Communication dans un congrès

Ce document a été publié dans

European Planetary Science Congress 2006. Berlin, Germany, 18 - 22 September 2006., p.491, 2006, Berlin. 2006

Résumé en anglais

Only few impact craters have been observed so far on Titan by the CASSINI imaging instruments. A 80 km diameter crater named Sinlap has been observed by the ISS, radar and VIMS instruments, with a resolution up to 14 km/pixel for VIMS. Observations at infrared and radar wavelengths provide complementary information on the composition, topography and surface roughness of the surface materials. Despite scattering by haze particles and strong absorption of light by methane contained in the atmosphere, there are several infrared windows that allow the observations of the surface of Titan with VIMS, enabling first order analysis of surface heterogeneities thanks to the use of band ratios. Several distinct units appear in these band ratios, with a possible enrichment in water ice around the main bright ejecta blanket. We report here on the cross comparison between VIMS band ratios and the radar T3 observations, in order to investigate the compositional and physical characteristics of the materials excavated by the impact.< Réduire

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Laboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804