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Spectroscopic Identification of Carbonate Minerals in the Martian Dust
Joshua L. Bandfield,*Timothy D. Glotch,Philip R. Christensen
Thermal infrared spectra of the martian surface indicate thepresence of small concentrations (2 to 5 weight %) of carbonates,specifically dominated by magnesite (MgCO3). The carbonatesare widely distributed in the martian dust, and there is noindication of a concentrated source. The presence of small concentrationsof carbonate minerals in the surface dust and in martian meteoritescan sequester several bars of atmospheric carbon dioxide andmay have been an important sink for a thicker carbon dioxideatmosphere in the martian past.
Department of Geological Sciences, Arizona State University, Tempe, AZ 85287–6305, USA.
* To whom correspondence should be addressed. E-mail: joshband{at}asu.edu
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2 to 5 weight %) of carbonates, specifically dominated by magnesite (MgCO3). The carbonates are widely distributed in the martian dust, and there is no indication of a concentrated source. The presence of small concentrations of carbonate minerals in the surface dust and in martian meteorites can sequester several bars of atmospheric carbon dioxide and may have been an important sink for a thicker carbon dioxide atmosphere in the martian past. 
