Implications of Laboratory Infrared Reflectance Spectra for Finding H2S on Io

Details Implications of Laboratory Infrared Reflectance Spectra for Finding H2S on Io Implications of Laboratory Infrared Reflectance Spectra for Finding H2S on Io

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27..109b&link_type=abstract

Lunar and Planetary Science, volume 27, page 109

Computer Science

Hydrogen Sulfide, Infrared, Io, Spectroscopy

Scientific paper

Does H2S exist on Io's surface? We believe this is an open question with significant implications for Io's volcanic and surface processes. Current evidence for its presence depends most upon infrared bands detected from Earth that overlap not only with H2S fundamentals, but also with bands seen in SO2 ice. Thus, to better prepare for Galileo observations of IO, and as part of a broader look at H2S infrared spectra and Io, we present H2S spectra in the range 2.3-5.2 micrometers and compare them with the known Io surface constituent, SO2. In particular, we combined our lab H2S spectra and SO2 spectra with the approximate Galileo-NIMS spectral bandpasses and channel separations to create simulated NIMS spectra of H2S and SO2 frost surfaces. The 2.7 micrometers H2S band (vl + v2 and/or V3 + v2) is the most significant and unique band for distinguishing H2S from SO2 in this spectral range, but the shape and size of the extremely strong 3.9 micrometers band (vl and V3 stretching fundamentals) will be useful in determining the thickness of H2S deposits. Thin (0.1 to 1 mm) H2S frosts create deep bands relative to much thicker SO2, so on IO, NIMS should be able to distinguish very thin deposits of H2S from thicker or intermingled SO2 deposits.

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