Development of Titan Atmospheric Removal Models for Cassini VIMS Data

Details Development of Titan Atmospheric Removal Models for Cassini VIMS Data Development of Titan Atmospheric Removal Models for Cassini VIMS Data

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.5603p&link_type=abstract

American Astronomical Society, DPS meeting #39, #56.03; Bulletin of the American Astronomical Society, Vol. 39, p.529

Astronomy and Astrophysics

Astronomy

Scientific paper

I/F spectra of Titan's surface acquired by Cassini's Visual & Infrared Mapping Spectrometer (VIMS) include signal contributions from both Titan's surface and atmosphere; the strength and wavelength coverage of the atmospheric absorptions leaves on the order of 10 data points with which spectral identification of surface ices and hydrocarbons can be reasonably attempted. Plane parallel radiative transfer (RT) correction methods offer some utility for modeling and subtracting out the atmospheric component in VIMS observations of Titan that are away from the limb and where angle of emergence e≤30° and angle of incidence i≤120-130°. To accomplish this, we use a DISORT-based radiative transfer correction code, extended from the version used successfully in surface-atmospheric separation retrievals for Mars to include a vertically varying CH4 to N2 ratio, multiple non-Lambertian options for defining the bidirectional reflectance function (BDRF) of the surface layer, and vertically varying haze aerosol properties. In a previous work, we reported our progress on replacing Voyager with Cassini-Huygens model inputs, e.g., pressure-temperature as a function of altitude profile from Huygens ASI and methane mixing ratio combined from Huygens GCMS. In this work, we incorporate new density data from Cassini INMS and haze scattering properties provided by the Huygens DISR team to generate model I/F for Titan's atmosphere up to 1400 km altitude above a non-Lambertian surface. Examples of surface-atmospheric separation of VIMS I/F data extracted from 64 x 64 pixel scenes and planned work to extend this protocol to global VIMS mosaics using 3D spherical shell radiative transfer models will be discussed.
Work performed under contract to NASA and under appointment to the NASA Postdoctoral Program (ORAU).

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