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T. B. McCord (Univ. of HI and Planet. Sci. Inst.), J. B. Adams (Univ. of Wash.), R. Jaumann (DLR Inst. fur Planet.), G. B. Hansen (Planet. Sci. Inst.), H. Hoffmann (DLR Inst. fur Planet.), F. Poulet (Inst. d'Astrop. Spatial U. of Paris), G. Bellucci (CNR Inst. di Fisica Spaz.), P. Pinet (CNRS Toulouse), G. Neukum (Freie Univ. Berlin), Mars Express HRSC Team
The High Resolution Stereo Camera (HRSC) on the Mars Express Mission is a push broom instrument that scans the Martian surface in 9 channels or linear arrays of CCD detectors. Four of these channels are equipped with color filters in the wave-length ranges blue (440 ± 45 nm), green (530 ± 45 nm), red (750 ± 20 nm) and infra-red (970 ± 45 nm). The remaining channels are equipped with a 675 ± 90 nm filter. According to the push broom technique, all color channels are expose simultane-ously but for different look angles and different areas of Mars (associated with the separation of the arrays in the focal plane) as the image of the surface sweeps across the focal plane and the lines of detectors. The HRSC color channels can be operated at highest spatial resolution of about 10 m. However the basic color mode of the camera is with 2x2 pixel binning, resulting in about 20 m spatial resolution. The issue of calibration is central to this work. We have explored the color channel calibration and the effects of the atmosphere in an attempt to obtain accurate reflec-tances for surface materials. Further, we have analyzed selected scenes to detect and describe the fundamental compositional units present and to associate these with geologic features and specific materials. So far, we find only a limited number of compositionally different materials but the color analysis nevertheless yields distinct and unique geological information in most scenes. Examples will be presented.
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Bulletin of the American Astronomical Society, 36 #4
© 2004. The American Astronomical Soceity.