DPS 35th Meeting, 1-6 September 2003
Session 16. Laboratory Research II
Poster, Highlighted on, Wednesday, September 3, 2003, 3:00-5:30pm, Sierra Ballroom I-II

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[16.04] Line parameters of methanol (CH3OH) at 10 microns

R.M. Lees, L.-H. Xu, P. Wang (University of New Brunswick, Saint John, N.B. Canada E2L 4L5), L.R. Brown (Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109), I. Kleiner (Laboratire de Physique Moleculaire et Applications, Universite Paris Sud, Batimenet 350, 91405 Orsay Cedex, France), J.W.C. Johns (Steacie Institute for Molecular Sciences, National Research Council of Canada, 100 Sussex Drive, Ottawa, ON K1A 0R6, Canada)

Laboratory spectra of methanol have been measured at high resolution and analyzed to provide spectroscopic information required for astrophysics and solar system studies. Line positions and quantum assignments have been obtained using spectra recorded at 0.002 cm-1 resolution using a modified Bomem DA3,002 spectrometer. Line intensities have been retrieved using laboratory scans from the McMath-Pierce Fourier-transform spectrometer located at the National Solar Observatory. The 10 micron region methanol absorption arises mainly from the fundamental CO-stretch mode (nu8) at 1033 cm-1, along with occasional transitions perturbed in the region by several nearby interacting states of the methyl rock (nu7), methyl bends (nu5, nu10, nu4) and the OH-bending (nu6) in combination with the torsion (nu12). Overall, the nu8 CO-stretch mode follows the traditional torsion-rotational pattern. We modeled the line positions and intensities for the CO-stretch mode with the one-dimensional torsional Hamiltonian and produced a HITRAN line list for cometary studies.

The research described in this paper was carried out by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. RML and LHXu wish to acknowledge financial support from the Natural Sciences and Engineering Research Council of Canada. IK would like to thank the French Programme National de Planétologie (PNP) for funding this research.

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