IR spectroscopy and real and imaginary indicies of ice mixtures of relevance to the outer Solar System

Details IR spectroscopy and real and imaginary indicies of ice mixtures of relevance to the outer Solar System IR spectroscopy and real and imaginary indicies of ice mixtures of relevance to the outer Solar System

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusm.p23a..07b&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #P23A-07

Other

3934 Optical, Infrared, And Raman Spectroscopy, 6020 Ices, 6218 Jovian Satellites, 6224 Kuiper Belt Objects, 6280 Saturnian Satellites

Scientific paper

Much of the outer Solar System is covered by ice; mostly, as on the icy Galilean and Saturnian satellites and KBOs, H2O ice containing other molecules such as carbon dioxide (CO2), methane (CH4), ammonia (NH3), and other more complex compounds such as nitriles (-CN). Often, much what we know of these icy objects is from Infrared (IR) reflectance spectra. The IR absorptions of molecules in ice depend strongly on the conditions; this is an advantage because it's a probe, but a complication because appropriate lab data is needed to correctly interpret observational data. Outer Solar System IR spectra have been in the near-IR (i.e., below 3 micron, or 5 micron at most) where reflected sunlight is greatest. Very few laboratory spectra of relevant ices have been available in the near-IR, and almost no indices of refraction (n's and k's) for incorporation into scattering models. As a result planetary scientists trying to fit spectra of complex surfaces composed of mixtures have been limited n's and k's of pure materials, often at the wrong temperature. We shall present near IR spectra of ice mixtures of relevance to icy outer Solar System bodies and show that they still hold surprises, such as the Cheshire cat-like CO2 (2v3) overtone near 2.134 micron (4685 cm-1) that is absent from spectra of pure CO2 but present in H2O-CO2 mixtures, see http://www.astrochem.org/CO2H2O.html for spectra. We shall also present near IR spectra for other binary mixtures such as H2O/CH4 (see http://www.astrochem.org/H2OCH4.html) and H2O/HCN and H2O/NH3 mixtures, and also present n's and k's for ices and mixtures in the near-IR.

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