Mapping Titan's Surface Features within the Visible Spectrum

Details Mapping Titan's Surface Features within the Visible Spectrum Mapping Titan's Surface Features within the Visible Spectrum

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.3605v&link_type=abstract

American Astronomical Society, DPS meeting #41, #36.05

Astronomy and Astrophysics

Astronomy

Scientific paper

Titan shows its surface through many methane windows in the IR wavelengths; however, windows at shorter wavelengths also exist. At visible wavelengths, the surface of Titan has been observed by Voyager I, the Hubble Space Telescope, and ground-based telescopes. We present here global surface mapping of Titan using the visible wavelength channels from the Visual and Infrared Mapping Spectrometer (VIMS). We show global maps in each of the VIMS-V channels extending from 0.35-1.05 microns. Using the methane windows at 0.754 µm, 0.827 µm, and 0.937 µm, we apply an RGB color scheme to search for surface albedo variations. Maps of this genre have already been made and published using the infrared channels of VIMS. These are the first global maps of Titan shortward of 0.938 microns. We compare the older IR maps to the new VIMS-V maps to constrain surface composition. For instance Tui Regio and Hotei Regio, referred to as 5-micron bright spots in previous papers, do not distinguish themselves at all at visible wavelengths. However, the distinction between the dune areas and the bright albedo spots, such as the difference between Xanadu and Senkyo, are still distinct. Further discoveries will develop from ongoing work as the Cassini Equinox Mission progresses in the coming years. The work done here is made possible by the NASA, ESA, and the VIMS team.

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