Global mineral distributions on Mars
Article first published online: 27 JUN 2002
Copyright 2002 by the American Geophysical Union.
Journal of Geophysical Research: Planets (1991–2012)
Volume 107, Issue E6, pages 9-1–9-20, June 2002
How to Cite
Global mineral distributions on Mars, J. Geophys. Res., 107(E6), doi:10.1029/2001JE001510, 2002.,
- Issue published online: 27 JUN 2002
- Article first published online: 27 JUN 2002
- Manuscript Accepted: 26 MAR 2002
- Manuscript Revised: 29 JAN 2002
- Manuscript Received: 27 APR 2001
- infrared spectroscopy;
- surface mineralogy;
- remote sensing
 Determining the mineralogy of Mars is an essential part of revealing the conditions of the surface and subsurface. A deconvolution method was used to remove atmospheric components and determine surface mineralogy from Thermal Emission Spectrometer data at 1 pixel per degree (ppd). Minerals are grouped into categories on the basis of compositional and spectral similarity, and global concentration maps are produced. All binned pixels are fit well with RMS errors of ≤0.005 in emissivity. Higher RMS errors are attributed to short wavelength particle size effects on dust-covered surfaces. Significant concentrations (>0.10) of plagioclase, high-Ca pyroxene, sheet silicates/high-Si glass, and hematite are detected and display distributions consistent with previous studies. Elevated concentrations of plagioclase and high-Ca pyroxene are consistent with basaltic surfaces and are located in low-albedo highlands regions north of ∼45°S. Significant concentrations of plagioclase and sheet silicates/high-Si glass and low concentrations of high-Ca pyroxenes are consistent with andesitic surfaces and are concentrated in both southern and northern high-latitude, low-albedo regions. Andesitic surfaces in the southern hemisphere have a lower spectral contrast than northern surfaces. An isolated surface located in Solis Planum is spectrally distinct but compositionally similar to other surfaces interpreted to be andesitic in composition. Concentrations of olivine below the detection limit correctly identify its presence in two of three locations. Potassium feldspar, low-Ca pyroxene, basaltic glass, olivine, sulfate, carbonate, quartz, and amphibole are not detected with confidence at 1 ppd. The results presented here indicate a predominance of volcanic compositions within Martian dust-free surfaces.