LINE BY LINE SPECTRAL PARAMETERS IN THE 4

LINE BY LINE SPECTRAL PARAMETERS IN THE 4 nu 3 SPECTRAL REGION OF METHANE D. CHRIS BENNER, V. MALATHY DEVI, College of William and Mary J. J. O’BRIEN, S. SHAJI, University of Missouri - St. Louis P. T. SPICKLER, C. P. HOUCK, J. A. COAKLEY, J. DOLPH and K. RANKIN, Bridgewater College

Planetary History of the Visible and Near IR Methane bands H. C. Vogel, Ap J 1, 273 (1895). Photography of the bands V. M. Slipher, Lowell Obs Bull 13 (1904). Gas lighter than H 2 suggested for Neptune V. M. Slipher, Ap J 26, 59 (1907). Bands absent in rings of Saturn. V. M. Slipher, Lowell Obs Bull 42 (1909). Spectroscopy extended to 700 nm. Adel and Slipher, Phys Rev. 46, 902 (1934). Absorber might be methane. Herzberg, 1940 s. Identifies the absorber as methane via lab spectra. Kuiper, late 1940 s. Discovers methane in atmosphere of Titan. Benner and Fink, Icarus (1980). Clearly showed the 890 nm band on Pluto.

Adel and Slipher, Phys Rev. 46, 902 (1934).

Benner, Dissertation (1979).

Spectrum Details Spectral Range: 10925 to 11500 cm-1 Resolution: 0. 01 cm-1 HWHM Temperatures: 99, 131 and 161 K Doppler Widths: ~0. 01 cm-1 HWHM Pressures: 0. 12 -7. 13 Torr Path Length: 3. 14 -5. 65 km Number of lines measured: 11 200+

Summary Positions, intensities and E” measured for 11200+ lines of methane at 890 nm Lorentz widths for N 2, air, H, He and self broadening are provided Pressure shifts for N 2, air, H, He and self broadening are provided Simulations of this region are possible at outer solar system temperatures Non homogeneous atmospheres can be simulated (not band models) Scattering models can now be calculated (could not be done with band models) Higher resolution increases detectability of the band dramatically Pluto’s 890 nm feature is almost entirely due to ice, not gas