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The HCO(+)/HOC(+) abundance ratio in molecular clouds
Woods, R. C.; Gudeman, C. S.; Dickman, R. L.; Goldsmith, P. F.; Huguenin, G. R.; Irvine, W. M.; Hjalmarson, A.; Nyman, L.-A.; Olofsson, H.
AA(Wisconsin, University, Madison, WI), AB(Wisconsin, University, Madison, WI), AC(Five College Radio Astronomy Observatory, Amherst, MA), AD(Five College Radio Astronomy Observatory, Amherst, MA), AE(Five College Radio Astronomy Observatory, Amherst, MA), AF(Five College Radio Astronomy Observatory, Amherst, MA), AG(Onsala Rymdobservatorium, Onsala, Sweden), AH(Onsala Rymdobservatorium, Onsala, Sweden), AI(Onsala Rymdobservatorium, Onsala, Sweden)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 270, July 15, 1983, p. 583-588. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Abundance, Interstellar Matter, Molecular Clouds, Positive Ions, Brightness Temperature, Interstellar Chemistry, Molecular Ions
Bibliographic Code:


Using the recently determined rest frequency of its first rotational transition, a sensitive search has been made for the J = 1 yields 0 transition of HOC(+) in 14 interstellar sources. A line having a frequency and shape consistent with optically thin emission due to this species was detected toward Sgr B2; this spectral feature is provisionally identified as being due to HOC(+). Comparison with the 1 yields 0 transition of H(C-18)O(+) in this source yields an isomeric abundance ratio HCO(+)/HOC(+) of about 330, if the detected line is in fact due to HOC(+). Independent of, and consistent with, this conclusion, comparisons with isotopically substituted HCO(+) in the other clouds searched show that HCO(+) is at least two orders of magnitude more abundant than HOC(+). This large ratio places interesting constraints on the fractional abundance of related species.

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