The Hyperspectral Stereo Camera Project

Details The Hyperspectral Stereo Camera Project The Hyperspectral Stereo Camera Project

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p51c1204g&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P51C-1204

Other

5210 Planetary Atmospheres, Clouds, And Hazes (0343), 5220 Hydrothermal Systems And Weathering On Other Planets, 5405 Atmospheres (0343, 1060), 5410 Composition (1060, 3672), 6225 Mars

Scientific paper

The MSSL Hyperspectral Stereo Camera (HSC) is developed from Beagle2 stereo camera heritage. Replaceing filter wheels with liquid crystal tuneable filters (LCTF) turns each eye into a compact hyperspectral imager. Hyperspectral imaging is defined here as acquiring 10s-100s of images in 10-20 nm spectral bands. Combined together these bands form an image `cube' (with wavelength as the third dimension) allowing a detailed spectrum to be extracted at any pixel position. A LCTF is conceptually similar to the Fabry-Perot tuneable filter design but instead of physical separation, the variable refractive index of the liquid crystal etalons is used to define the wavelength of interest. For 10 nm bandwidths, LCTFs are available covering the 400-720 nm and 650-1100 nm ranges. The resulting benefits include reduced imager mechanical complexity, no limitation on the number of filter wavelengths available and the ability to change the wavelengths of interest in response to new findings as the mission proceeds. LCTFs are currently commercially available from two US companies - Scientific Solutions Inc. and Cambridge Research Inc. (CRI). CRI distribute the `Varispec' LCTFs used in the HSC. Currently, in Earth orbit hyperspectral imagers can prospect for minerals, detect camouflaged military equipment and determine the species and state of health of crops. Therefore, we believe this instrument shows great promise for a wide range of investigations in the planetary science domain (below). MSSL will integrate and test at representative Martian temperatures the HSC development model (to determine power requirements to prevent the liquid crystals freezing). Additionally, a full radiometric calibration is required to determine the HSC sensitivity. The second phase of the project is to demonstrate (in a ground based lab) the benefit of much higher spectral resolution to the following Martian scientific investigations: - Determination of the mineralogy of rocks and soil - Detection of water vapour due to its absorption of sun light at 935 nm - The measurement of the dust optical density as a function of wavelength - Determination of the solar spectrum at the surface as a function of time of day - The search for putative biological pigments (i.e. chlorophyll and carotenoids) The detector for this proposal is a commercial low noise CCD imaging chip providing sufficient SNR to detect the 10s of ppm of water vapour present in the Martian atmosphere.

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