title: Infrared spectroscopy of Triton and Pluto ice analogs:  the case for saturated hydrocarbons.
abstract: The infrared transmission spectra and photochemical behavior of various organic compounds isolated in solid N2 ices, appropriate for applications to Triton and Pluto, are presented. It is shown that excess absorption in the surface spectra of Triton and Pluto, i.e., absorption not explained by present models incorporating molecules already identified on these bodies (N2, CH4, CO, and CO2), that starts near 4450 cm-1 (2.25 micrometers) and extends to lower frequencies, may be due to alkanes (C(n)H2n+2) and related molecules frozen in the nitrogen. Branched and linear alkanes may be responsible. Experiments in which the photochemistry of N2:CH4 and N(2):CH4:CO ices was explored demonstrate that the surface ices of Triton and Pluto may contain a wide variety of additional species containing H, C, O, and N. Of these, the reactive molecule diazomethane, CH2N2, is particularly important since it may be largely responsible for the synthesis of larger alkanes from CH4 and other small alkanes. Diazomethane would also be expected to drive chemical reactions involving organics in the surface ices of Triton and Pluto toward saturation, i.e., to reduce multiple CC bonds.  The positions and intrinsic strengths (A values) of many of the infrared absorption bands of N2 matrix-isolated molecules of relevance to Triton and Pluto have also been determined. These can be used to aid in their search and to place constraints on their abundances. For example, using these A values the abundance ratios CH4/N2 approximately 1.3 x 10(-3), C2H4/N2 < or = 9.5 x 10(-7) and H2CO/N2 < or = 7.8 x 10(-7) are deduced for Triton and CH4/N2 approximately 3.1 x 10(-3), C2H4/N2 < or = 4.1 x 10(-6), and H2CO/N2 < or = 5.2 x 10(-6) deduced for Pluto. The small amounts of C2H4 and H2CO in the surface ices of these bodies are in disagreement with the large abundances expected from many theoretical models.
authors.affiliation: NASA-Ames Research Center, Moffett Field, California 94035, USA.
authors.forename: R B
authors.initials: RB
authors.lastname: Bohn
authors.forename: S A
authors.initials: SA
authors.lastname: Sandford
authors.forename: L J
authors.initials: LJ
authors.lastname: Allamandola
authors.forename: D P
authors.initials: DP
authors.lastname: Cruikshank
mesh_terms: D000473:Alkanes / Q000032:analysis* / Q000737:chemistry; D055580:Astronomical Phenomena; D001256:Astronomy; D002245:Carbon Dioxide / Q000032:analysis / Q000737:chemistry; D002248:Carbon Monoxide / Q000032:analysis / Q000737:chemistry; D005118:Extraterrestrial Environment; D006838:Hydrocarbons / Q000032:analysis / Q000737:chemistry; D007053:Ice / Q000032:analysis*; D008697:Methane / Q000032:analysis / Q000737:chemistry; D008956:Models, Chemical; D018541:Neptune; D009584:Nitrogen / Q000032:analysis / Q000737:chemistry; D010777:Photochemistry; D018542:Pluto; D013055:Spectrophotometry, Infrared; D014466:Ultraviolet Rays
chemical_list: D000473:Alkanes; D006838:Hydrocarbons; D007053:Ice; D002245:Carbon Dioxide; D002248:Carbon Monoxide; D009584:Nitrogen; D008697:Methane