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Title:
Identification of the interstellar cyanomethyl radical (CH2CN) in the molecular clouds TMC-1 and Sagittarius B2
Authors:
Irvine, W. M.; Friberg, P.; Hjalmarson, A.; Ishikawa, S.; Kaifu, N.; Kawaguchi, K.; Madden, S. C.; Matthews, H. E.; Ohishi, M.; Saito, S.; Suzuki, H.; Thaddeus, P.; Turner, B. E.; Yamamoto, S.; Ziurys, L. M.
Affiliation:
AA(Five College Radio Astronomy Observatory, Amherst, MA), AB(Onsala Rymdobservatorium, Sweden), AC(Onsala Rymdobservatorium, Sweden), AD(Nobeyama Radio Observatory, Minamimaki, Japan), AE(Nobeyama Radio Observatory, Minamimaki, Japan), AF(Institute for Molecular Science), AG(Five College Radio Astronomy Observatory, Amherst, MA), AH(Herzberg Institute of Astrophysics, National Research Council of Canada), AI(Toyama University), AJ(Department of Astrophysics, Nagoya University), AK(Nobeyama Radio Observatory, Minamimaki, Japan), AL(Harvard-Smithsonian Center for Astrophysics), AM(National Radio Astronomy Observatory), AN(Department of Astrophysics, Nagoya University), AO(Five College Radio Astronomy Observatory, Amherst, MA)
Publication:
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 334, Nov. 15, 1988, p. L107-L111. Research supported by the U.S.-Sweden Cooperative Science Program and Inoue Foundation for Science. (ApJL Homepage)
Publication Date:
11/1988
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Cyano Compounds, Interstellar Matter, Molecular Clouds, Abundance, Free Radicals, Hyperfine Structure, Methyl Compounds, Milky Way Galaxy
DOI:
10.1086/185323
Bibliographic Code:
1988ApJ...334L.107I

Abstract

The authors report the astronomical identification of the cyanomethyl radical, CH2CN, the heaviest nonlinear molecular radical to be identified in interstellar clouds. The complex fine and hyperfine structures of the lowest rotational transitions at about 20.12 and 40.24 GHz are resolved in TMC-1, where the abundance appears to be about 5×10-9 relative to that of H2. In Sgr B2 the hyperfine structure is blended in the higher frequency transitions at 40, 80, and 100 GHz, although the spin-rotation doubling is clearly evident. Preliminary searches in other sources indicate that the distribution of CH2CN is similar to that for such carbon chain species as HC3N or C4H.

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