H, C, N, and O Isotopic Substitution Studies of the 2165 Wavenumber (4.62 Micron) ``XCN'' Feature Produced by Ultraviolet Photolysis of Mixed Molecular Ices

Details H, C, N, and O Isotopic Substitution Studies of the 2165 Wavenumber (4.62 Micron) ``XCN'' Feature Produced by Ultraviolet Photolysis of Mixed Molecular Ices H, C, N, and O Isotopic Substitution Studies of the 2165 Wavenumber (4.62 Micron) ``XCN'' Feature Produced by Ultraviolet Photolysis of Mixed Molecular Ices

Oct 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...542..894b&link_type=abstract

The Astrophysical Journal, Volume 542, Issue 2, pp. 894-897.

Astronomy and Astrophysics

Astronomy

27

Infrared: Ism: Lines And Bands, Ism: Lines And Bands, Ism: Molecules, Methods: Laboratory

Scientific paper

To better understand the chemical species that gives rise to the 2165 cm-1 (4.62 μm) ``XCN'' absorption feature seen toward embedded protostars such as W33A, we have performed laboratory studies using deuterium (2H) isotopic labeling. We report the observation of a small but significant deuterium isotope shift for the ``XCN'' peak which demonstrates that the atomic motion(s) causing the ``XCN'' band in the laboratory samples must involve hydrogen. We also report the results of 13C, 15N, and 18O labeling experiments that are consistent with previously reported values.

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