Spectral properties of the Saturnian satellite Tethys as derived from Cassini-VIMS data

Kurzfassung

Since 2004 the Cassini spacecraft performed numerous targeted and non-targeted flybys at the major Saturnian satellites. During these flybys the Visual and Infrared Mapping Spectrometer (VIMS) onboard the Cassini spacecraft [1] detects the spectral properties of the satellites’ surfaces in the wavelength range from 0.35 to 5.1 μm with a spectral resolution that allows the mapping of the distribution of major surface compounds like H2O ice as well as discov-ery/identification of minor and/or trace compounds like CO2 as shown for several Saturnian satellites [2-6]. Mapping of these compounds revealed a distinct distribution of most of these surface compounds either related to geological surface features/processes or to weathering of the uppermost surface layer. In order to further our understanding of the Satutnian system we now performed an analysis of the spectral surface properties of Tethys in context of the surface geology as well as topography based on simultaneously ac-quired Cassini ISS images.