CH3D Absorption Bands Between 2.86 And 3.10 Microns In The High-resolution Spectra Of Titan

Details CH3D Absorption Bands Between 2.86 And 3.10 Microns In The High-resolution Spectra Of Titan CH3D Absorption Bands Between 2.86 And 3.10 Microns In The High-resolution Spectra Of Titan

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.2717k&link_type=abstract

American Astronomical Society, DPS meeting #38, #27.17; Bulletin of the American Astronomical Society, Vol. 38, p.530

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The ν2 + ν3 band of CH3D near 2.86 microns (Kim et al. 2005) has been detected in absorption in the high-resolution spectra of Titan observed with NIRSPEC at Keck II (Geballe et al. 2003). Between 2.92 and 3.10 microns in the same spectra other weak CH3D band lines have been identified based on a recent line list compiled by one of us. These CH3D lines are useful to investigate stratospheric and tropospheric haze opacities in this wavelength range, because: 1) CH4 mixing ratios during the descendent of Huygens at the landing site are now determined from the in situ measurements of the Gas Chromatograph and Mass Spectrometer (GCMS) (e.g., Niemann et al. 2005); 2) the CH3D/CH4 mixing ratio is believed to be uniform from surface to high-altitude atmosphere, and, therefore, altitude-dependent CH3D mixing ratios should also be derived; and 3) the 2.96 - 3.20 micron range is relatively free from strong absorptions of other molecular bands. We will present preliminary results on the derived optical property of haze layers between 2.86 and 3.10 microns; and we will also test a possibility of the global supersaturation of CH4 in the troposphere of Titan utilizing the CH3D lines.
References
Geballe, T.R., Kim,S.J., Noll, K.S., and Griffith, C.A. 2003. Ap. J. 583, L39-L42.
Kim, S.J., Geballe, T.R., Noll, K.S., and Courtin, R. 2005. Icarus, 173, 522-532.Niemann, H.B., and 17 coauthors. 2005. Nature. 438, 779-784.

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