Studies of Titan's 5-Micron-Bright Regions Using Combined VIMS and ISS Observations

Details Studies of Titan's 5-Micron-Bright Regions Using Combined VIMS and ISS Observations Studies of Titan's 5-Micron-Bright Regions Using Combined VIMS and ISS Observations

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p11a..04b&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P11A-04

Physics

5470 Surface Materials And Properties, 5480 Volcanism (6063, 8148, 8450)

Scientific paper

Coanalysis of the datasets obtained by Cassini VIMS (Visual and Infrared Mapping Spectrometer), ISS (Imaging Science Subsystem), RADAR, and the Huygens probe is driving our understanding of Titan's haze- shrouded surface. We find that high spatial resolution imaging of Titan at 0.938um from ISS provides a useful complement to VIMS' spectral image mapping of Titan at 352 wavelengths but lower spatial resolution. We used ISS images from Tb and VIMS cubes from Tb, T5, and T12 to study in detail those areas identified by VIMS to have unusually high surface reflectivities at 5 microns, Tui Regio and Hotei Regio. VIMS' 5-micron- bright Hotei Regio corresponds to a distinctive bright arc in the ISS data. Correlation of high-resolution and color information from western Tui Regio shows flow-like features, possibly of extrusive, cryovolcanic origin. A small-grained water-ice unit surrounding Tui Regio best explains the area's brightness in short-wavelength ISS data relative to VIMS. We will discuss these findings as well as prospects for future VIMS/ISS collaborations.

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