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Spectral reflectance properties of carbonates from terrestrial analogue environments: Implications for Mars |
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| Authors: | Edward A Cloutis Stephen E Grasby Barbara L Sherriff |
| Institution: | a Department of Geography, University of Winnipeg, 515 Portage Avenue, Winnipeg, MB, Canada R3B 2E9 b Geological Survey of Canada—Calgary, Natural Resources Canada, 3303 33rd St. N.W., Calgary, Alberta, Canada T2L-2A7 c Department of Geological Sciences, University of Manitoba, Winnipeg, MB, Canada R3T 2N2 d Canadian Space Agency, 6767, route de l’Aéroport, Saint-Hubert, QC, Canada J3Y 8Y9 e Department of Earth Sciences, University of Western Ontario, 1151 Richmond Street, London, ON, Canada N6A 5B7 f Department of Physics & Astronomy, University of Western Ontario, 1151 Richmond Street, London, ON, Canada N6A 5B7 |
| Abstract: | Spectroscopic analysis of carbonate-bearing samples from a variety of terrestrial environments provides important insights into spectroscopy-based investigations of Mars designed to detect the presence of carbonate minerals. In order to better address the spectral detectability of carbonates on Mars, we examined the spectral reflectance properties of carbonates and carbonate-bearing lithologies from a variety of terrestrial environments, including impact structures (Haughton, St. Martin, Eagle Butte), landslides (Frank), quarrying operations (Hecla), carbonates affected by weathering (Haughton, East German Creek), and sulfide-sulfate-carbonate assemblages (Central Manitoba). The goal is to identify processes and environments that can affect spectroscopy-based carbonate detection, for more detailed follow-on studies. Common carbonates appear to be stable, from a spectroscopic perspective, to various tectonic processes. Iron oxides/hydroxides do not appear to significantly affect spectral detectability of carbonates, as the spectrum-altering effects of these phases are largely restricted to the region below ∼1 μm, while useful carbonate absorption bands occur longward of ∼1.8 μm. Carbonate detection and characterization in the 0.35-2.5-μm region is largely restricted to a single absorption feature in the 2.3-μm region, which can be problematic for robust carbonate identification. While tectonic processes and iron oxide/hydroxide staining do not appear to significantly impair carbonate detection based on the 2.3-μm region absorption band, a number of other factors can affect carbonate detection. These include the fact that this absorption band is weak compared to many other minerals, a number of other minerals also exhibit absorption bands in this wavelength region (leading to possible misidentifications), and that even small abundances of minerals that absorb strongly in this region will reduce the strength of the carbonate absorption band. Identifying the nature of accessory minerals associated with carbonates can be used to constrain possible formation environments. Ongoing research at carbonate-bearing terrestrial analogue sites will continue to provide new insights into the occurrence and detection of carbonates on Mars. |
| Keywords: | Mars Analogue research Carbonates Impact cratering Spectroscopy |
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