Syrtis Major is an old, low relief volcanic plateau near the equatorial regions of Mars. It is a peristent low-albedo feature on the planet and is thought to contain a high abundance of exposed bedrock and/or locally derived surface material and debris. Spatially resolved variations in surface spectral properties, and therefore composition, are investigated with data from the Imaging Spectrometer for Mars (ISM) instrument. ISM obtained 128 wavelength channel spectra from 0.76 to 3.16 μm for contiguous pixels approximately 22¿22 km in size across much of the plateau. The value and spatial distribution of four primary spectral variables (albedo, continuum slope, wavelength of the ferric-ferrous band minimum, area of the ferric-ferrous absorption) are mapped and coregistered to Viking digital photomosaics. Analysis of these maps shows that although there is a high degree of overall spectral variability on the plateau, the key indicators of mafic mineralogy are relatively homogeneous.

Detailed examination of reflectance spectra from representative areas across the plateau indicate the volcanic surface is dominated by augite-bearing basalts and the pyroxene composition in the basalts is estimated to be 0.275¿0.075 Ca/(Ca+Fe+Mg) and 0.3¿0.1 Fe/(Fe+Ca+Mg). Additional mineral components may include olivine, feldspar, and glass. Most of the spectral variability on the plateau is interpreted to result from mixing of volcanic bedrock and/or locally derived surface material and debris with highly altered dust and soil. In western Syrtis Major the altered material is a transient component on the surface or occurs in large spatially coherent patches (e.g., crater rims). In eastern Syrtis Major it is apparent that the dust components are firmly fixed to the basaltic substrate as a stable oxide rind or coating. ¿American Geophysical Union 1993