Compact reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO)

被引:806
|
作者
Murchie, S.
Arvidson, R.
Bedini, P.
Beisser, K.
Bibring, J.-P.
Bishop, J.
Boldt, J.
Cavender, P.
Choo, T.
Clancy, R. T.
Darlington, E. H.
Marais, D. Des
Espiritu, R.
Fort, D.
Green, R.
Guinness, E.
Hayes, J.
Hash, C.
Heffernan, K.
Hemmler, J.
Heyler, G.
Humm, D.
Hutcheson, J.
Izenberg, N.
Lee, R.
Lees, J.
Lohr, D.
Malaret, E.
Martin, T.
McGovern, J. A.
McGuire, P.
Morris, R.
Mustard, J.
Pelkey, S.
Rhodes, E.
Robinson, M.
Roush, T.
Schaefer, E.
Seagrave, G.
Seelos, F.
Silverglate, P.
Slavney, S.
Smith, M.
Shyong, W.-J.
Strohbehn, K.
Taylor, H.
Thompson, P.
Tossman, B.
Wirzburger, M.
Wolff, M.
机构
[1] Appl Phys Lab, Laurel, MD 20723 USA
[2] Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA
[3] Inst Astrophys Spatiale, F-91405 Orsay, France
[4] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA
[5] Space Sci Inst, Boulder, CO 80301 USA
[6] Appl Coherent Technol, Herndon, VA USA
[7] NASA, Jet Propuls Lab, Pasadena, CA 91109 USA
[8] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA
[9] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA
[10] Northwestern Univ, Ctr Planetary Sci, Evanston, IL 60208 USA
[11] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
关键词
D O I
10.1029/2006JE002682
中图分类号
P3 [地球物理学]; P59 [地球化学];
学科分类号
0708 ; 070902 ;
摘要
The Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) is a hyperspectral imager on the Mars Reconnaissance Orbiter (MRO) spacecraft. CRISM consists of three subassemblies, a gimbaled Optical Sensor Unit (OSU), a Data Processing Unit (DPU), and the Gimbal Motor Electronics (GME). CRISM's objectives are (1) to map the entire surface using a subset of bands to characterize crustal mineralogy, (2) to map the mineralogy of key areas at high spectral and spatial resolution, and (3) to measure spatial and seasonal variations in the atmosphere. These objectives are addressed using three major types of observations. In multispectral mapping mode, with the OSU pointed at planet nadir, data are collected at a subset of 72 wavelengths covering key mineralogic absorptions and binned to pixel footprints of 100 or 200 m/pixel. Nearly the entire planet can be mapped in this fashion. In targeted mode the OSU is scanned to remove most along-track motion, and a region of interest is mapped at full spatial and spectral resolution (15-19 m/pixel, 362-3920 nm at 6.55 nm/channel). Ten additional abbreviated, spatially binned images are taken before and after the main image, providing an emission phase function (EPF) of the site for atmospheric study and correction of surface spectra for atmospheric effects. In atmospheric mode, only the EPF is acquired. Global grids of the resulting lower data volume observations are taken repeatedly throughout the Martian year to measure seasonal variations in atmospheric properties. Raw, calibrated, and map-projected data are delivered to the community with a spectral library to aid in interpretation.
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