Abstract
Reflectance spectra of Mars obtained by the imaging infrared spectrometer ISM in the wavelength range from 0.76 to 3.16 μm have been analyzed and previous studies have been reviewed. A new method of error calculation has been developed that enables improved interpretation of the Martian surface composition from the infrared spectroscopic data. Based on this calculation criteria are defined to evaluate the spatial variation of weak surface absorption bands. Spectral variables have been calculated taking into account the viewing geometry and atmospheric absorptions. Variations in the spectral properties of Mars are shown in spectral maps of characteristic target areas, including the Ascraeus Mons volcano and Lunae Planum. Spatial variation in the intensity of a weak feature at 2.2 μm has been studied for these areas. Spectral subunits have been defined and are discussed in relation to the surface composition of Mars.
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