High-resolution spectroscopy of Mars at 3.7 and 8 μm: A sensitive search of <formula>H2O2, <formula>H2CO, HCl, and <formula>CH4, and detection of HDO

Details High-resolution spectroscopy of Mars at 3.7 and 8 μm: A sensitive search of <formula>H2O2, <formula>H2CO, HCl, and <formula>CH4, and detection of HDO High-resolution spectroscopy of Mars at 3.7 and 8 μm: A sensitive search of <formula>H2O2, <formula>H2CO, HCl, and <formula>CH4, and detection of HDO

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997jgr...102.6525k&link_type=abstract

Journal of Geophysical Research, Volume 102, Issue E3, p. 6525-6534

Physics

57

Planetology: Solid Surface Planets: Atmospheres-Composition And Chemistry, Planetology: Solid Surface Planets: Composition, Planetology: Solid Surface Planets: Remote Sensing

Scientific paper

We report the first sensitive upper limits for H2O2, H2CO, and HCl, a sensitive upper limit for CH4, and a measured column abundance for HDO. A combination of the Kitt Peak National Observatory (KPNO) 4-m telescope and Fourier transform spectrometer with the Goddard Space Flight Center (GSFC) postdisperser was used to observe low-latitude regions of Mars in spectral ranges of 2650-2800cm-1 and 1229-1237cm-1 with resolving power ν/δν=2.7×105 and 1.2×105, respectively. The main spectral features are lines of isotopic CO2 and HDO. A radiation transfer code has been developed which divides the atmosphere into 30 layers and the Voigt profile of each line in each layer into 60 intervals. This code couples the reflected solar and thermal radiations. A search for H2O2 at 1229-1237cm-1 results in a 2-σ upper limit of 30 ppb, close to the predictions of recent photochemical models. Our 2-σ upper limit for HCl (<2ppb) precludes any significant chlorine chemistry in the atmosphere. Our value for methane (70+/-50ppb) is consistent with, but does not improve upon, earlier results from Mariner 9 infrared interferometer spectrometer (IRIS). Our 2-σ upper limit for H2CO (3 ppb) is much smaller than recently claimed abundances. The observed HDO lines result in an abundance of (6.06+/-0.5)×1016cm-2, which, when compared with that of H2O measured by the Viking orbiters at the same season and latitudes, yields an enrichment in the D/H ratio of a factor of 5.5+/-2 relative to Earth. The given uncertainty is mainly caused by possible variations of Mars' atmospheric water abundance.

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