Spectroscopy of Mars form 2.04 to 2.44 micron during the 1993 opposition: Absolute calibration and atmospheric VS mineralogic origin of narrow absorption features

Details Spectroscopy of Mars form 2.04 to 2.44 micron during the 1993 opposition: Absolute calibration and atmospheric VS mineralogic origin of narrow absorption features Spectroscopy of Mars form 2.04 to 2.44 micron during the 1993 opposition: Absolute calibration and atmospheric VS mineralogic origin of narrow absorption features

Sep 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994icar..111..106b&link_type=abstract

Icarus (ISSN 0019-1035), vol. 111, no. 1, p. 106-123

Mathematics

Logic

25

Absorption Spectra, Atmospheric Composition, Carbon Dioxide, Carbon Monoxide, Infrared Spectra, Mars (Planet), Mars Atmosphere, Near Infrared Radiation, Spectral Reflectance, Spectrum Analysis, Astronomical Spectroscopy, Bandwidth, Infrared Spectrometers, Infrared Spectroscopy, Mineralogy, Signal To Noise Ratios, Silicates, Telescopes

Scientific paper

We present moderate-resolution (lambda/delta lambda = 300 to 370) reflectance spectral of Mars from 2.04 to 2.44 microns that were obtained at United Kingdom Infrared Telescope (UKIRT) during the 1993 opposition. Seven narrow absorption features were detected and found to have a Mars origin. By comparison with solar and Mars atmospheric spectra, five of these features were attributed all or in part to Mars atmospheric CO2 or CO (2.052 +/- 0.003, 2.114 +/- 0.002, 2.150 +/- 0.003, 2.331 +/- 0.001, and 2.357 +/- 0.002 microns). Two of the bands (2.331 +/- 0.001 and 2.357 +/- 0.002 micron) appear to have widths and depths that are consistent with additional, nonatmospheric absorptions, although a solar contribution cannot be entirely ruled out. Two other weak bands centered at 2.278 +/- 0.002 and 2.296 +/- 0.002 microns may be at least partially mineralogic in origin. The data provide no conclusive identification of the mineralogy responsible for these absorption features. However, examination of terrestrial spectral libraries and previous mineralogy responsible for these absorption features. However, examination of terrestrial spectral libraires and previous moderate spectral resolution mineral studies indicates that the most likely origin of these features is either (bi)carbonate or (bi)sulfate anions in framework silicates of (Fe, Mg)-OH bonds in sheet silicates. If the bands are caused by phyllosilicate minerals, then an explanation must be found for the extremely narrow widths of the cation-OH features in the Mars spectra as compared to terrestrial minerals.

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