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High-resolution CASSINI-VIMS mosaics of Titan and the icy Saturnian satellites |
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| Authors: | R. Jaumann K. Stephan B.J. Buratti T.B. McCord F. Capaccioni P. Cerroni G. Bellucci M. Combes P. Drossart Y. Langevin R.M. Nelson B. Sicardy L.A. Soderbloom K.-D. Matz F. Scholten |
| Affiliation: | a DLR, Institute of Planetary Research, Rutherfordstrasse 2, D-12489 Berlin, Germany b Department Planetary Science and LPL, University of AZ, Tucson, AZ 85721-0092, USA c Jet Propulsion Laboratory, Pasadena, CA 91109, USA d USGS, Mail Stop 964, Box 25046, Denver Federal Center, Denver, CO, USA e Planetary Science Institute, 22 Fiddler's Rd., Winthrop, WA 98862-0667, USA f Istituto Fisica Spazio Interplanetario, CNR, Via Fosso del Cavaliere, Roma, Italy g Instituto di Astrofisica Spaziale, Via Fosso del Cavaliere, Roma, Italy h Universite de Paris Sud-Orsay, IAS, 91405 Orsay Cedex, France i Observatoire de Paris-Meudon, 5 Place Jules Jannsen, 92195 Meudon Cedex, France j NASA Ames Research Center, Astrophysics Branch, Moffett Field, CA 94035-1000, USA k Cornell University, 418 Space Science Bldg, Ithaca, NY 14853, USA l University of Nantes, B.P. 92208, 2 rue de la Houssinière, 44072 Nantes Cedex 3, France m US Geological Survey, Flagstaff, AZ 86011, USA n Lunar and Planetary Laboratory and Stewart Observatory, University of Arizona, Tucson, AZ, USA o Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA |
| Abstract: | The Visual Infrared Mapping Spectrometer (VIMS) onboard the CASSINI spacecraft obtained new spectral data of the icy satellites of Saturn after its arrival at Saturn in June 2004. VIMS operates in a spectral range from 0.35 to 5.2 μm, generating image cubes in which each pixel represents a spectrum consisting of 352 contiguous wavebands.As an imaging spectrometer VIMS combines the characteristics of both a spectrometer and an imaging instrument. This makes it possible to analyze the spectrum of each pixel separately and to map the spectral characteristics spatially, which is important to study the relationships between spectral information and geological and geomorphologic surface features.The spatial analysis of the spectral data requires the determination of the exact geographic position of each pixel on the specific surface and that all 352 spectral elements of each pixel show the same region of the target. We developed a method to reproject each pixel geometrically and to convert the spectral data into map projected image cubes. This method can also be applied to mosaic different VIMS observations. Based on these mosaics, maps of the spectral properties for each Saturnian satellite can be derived and attributed to geographic positions as well as to geological and geomorphologic surface features. These map-projected mosaics are the basis for all further investigations. |
| Keywords: | Cassini VIMS Imaging spectroscopy Saturnian satellites Map projection Mosaics |
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