HR: 1340h
AN: P23B-1357    [Abstracts]
TI: Surface-Atmospheric Separation Models for Titan: Plane Parallel vs. Spherical Shell Radiative Transfer Solutions for Cassini VIMS Data
AU: * Pitman, K M
EM: Karly.M.Pitman@jpl.nasa.gov
AF: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Buratti, B J
AF: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Baines, K H
AF: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: West, R A
AF: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Dumont, P
AF: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Wolff, M J
AF: Space Science Institute, 4750 Walnut Street Suite 205, Boulder, CO 80301, United States
AU: Brown, R H
AF: Lunar & Planetary Lab, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721- 0092, United States
AU: Bellucci, G
AF: Institute di Fisica dello Spazio Interplanetario, Via del Fosso del Cavaliere, 100, Rome, 00133, Italy
AU: Bibring, J
AF: Institute of Planetary Exploration, DLR, Rutherfordstrasse 2, Berlin, D-12489, Germany
AU: Capaccioni, F
AF: Institute di Fisica dello Spazio Interplanetario, Via del Fosso del Cavaliere, 100, Rome, 00133, Italy
AU: Cerroni, P
AF: Institute di Fisica dello Spazio Interplanetario, Via del Fosso del Cavaliere, 100, Rome, 00133, Italy
AU: Clark, R N
AF: U. S. Geological Survey, Mail Stop 964, Box 25046 Federal Center, Denver, CO 80225, United States
AU: Combes, M
AF: Observatoire de Paris-Meudon, Département de Recherche Spatial, 5 Place Jules Jannsen, Meudon Cedex, 92195, France
AU: Coradini, A
AF: Institute di Fisica dello Spazio Interplanetario, Via del Fosso del Cavaliere, 100, Rome, 00133, Italy
AU: Cruikshank, D P
AF: NASA Ames Research Center, Astrophysics Branch, Moffett Field, CA 94035-1000, United States
AU: Drossart, P
AF: Observatoire de Paris-Meudon, Département de Recherche Spatial, 5 Place Jules Jannsen, Meudon Cedex, 92195, France
AU: Formisano, V
AF: Institute di Fisica dello Spazio Interplanetario, Via del Fosso del Cavaliere, 100, Rome, 00133, Italy
AU: Jaumann, R
AF: Institute of Planetary Exploration, DLR, Rutherfordstrasse 2, Berlin, D-12489, Germany
AU: Langevin, Y
AF: Institut d'Astrophysique Spatiale, Universite de Paris Sud-Orsay, Batiment 120, Orsay Cedex, 91405, France
AU: Matson, D L
AF: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: McCord, T B
AF: Space Science Institute, 4750 Walnut Street Suite 205, Boulder, CO 80301, United States
AU: Mennella, V
AF: Institute di Fisica dello Spazio Interplanetario, Via del Fosso del Cavaliere, 100, Rome, 00133, Italy
AU: Nelson, R M
AF: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: Nicholson, P D
AF: Dept. of Astronomy, Cornell University, 418 Space Sciences Building, Ithaca, NY 14853, United States
AU: Sicardy, B
AF: Observatoire de Paris-Meudon, Département de Recherche Spatial, 5 Place Jules Jannsen, Meudon Cedex, 92195, France
AU: Sotin, C
AF: Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, United States
AU: VIMS Team, C
AB: The Cassini orbiter's Visual & Infrared Mapping Spectrometer (VIMS) observes Titan's surface intensity at wavelengths where its methane-rich atmosphere is heavily absorbing and light is strongly scattering. Therefore, most analyses of Titan's surface that require use of the VIMS dataset (e.g., photoclinometry, geologic interpretation, spectral identification of surface materials, photometry) are impeded until a method to separate the atmospheric from the surface spectral signature of Titan is fully developed. In a previous work (Pitman et al. 2007,AAS-DPS meeting #39), we presented a fully-functional plane-parallel radiative transfer (RT) correction method with core components extended from Mars surface-atmospheric separation models that can be used for modeling and removing Titan's atmosphere for VIMS observations which are far from the limb. This "Mars/Titan" hybrid plane-parallel RT correction model includes inputs from Cassini-Huygens c. 2007, allows for vertical variation of major atmospheric properties, and incorporates newly released methane absorption coefficients and haze scattering properties derived from in situ measurements by the Huygens DISR team. In this work, we attempt to resolve the issue of atmospheric variation as a function of Titan's geographic coordinates by utilizing a spherical-shell radiative transfer model, originally used by Cassini engineers to model radiation flow through Titan's atmosphere and used by other Cassini teams for atmospheric correction as well. Trade-offs on when and where to use which type of model will be discussed. Work performed under contract to NASA and under appointment to the NASA Postdoctoral Program (ORAU).
DE: 5405 Atmospheres (0343, 1060)
DE: 5464 Remote sensing
DE: 5470 Surface materials and properties
DE: 6281 Titan
SC: Planetary Sciences [P]
MN: 2007 Fall Meeting