Interstellar HOC(+) Revisited

Details Interstellar HOC(+) Revisited Interstellar HOC(+) Revisited

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aas...185.8111a&link_type=abstract

American Astronomical Society, 185th AAS Meeting, #81.11; Bulletin of the American Astronomical Society, Vol. 26, p.1451

Astronomy and Astrophysics

Astronomy

Scientific paper

One abundance ratio of importance for astrochemistry is [HCO(+) ] / [HOC(+) ]. HOC(+) is the metastable isomer of HCO(+) and lies about 17,000 K higher in energy. Both theory and experiment suggest that this ratio should be > 10(4) in interstellar gas. A tentative detection of the J=1-0 transition of HOC(+) towards SgrB2(OH) by Woods et al.(Ap.J.370, 538), however, indicates that [HCO(+) ]/[HOC(+) ] ~ 330. We report here on new observations to confirm the identification of interstellar HOC(+) and establish the true [HCO(+) ]/[HOC(+) ] ratio. We have detected spectral lines at the frequency of the J=1-0 transition of HOC(+) at 89 GHz towards several new sources, including Orion-KL, W51, and DR21(OH), using the NRAO 12 m telescope. In addition, we have observed lines at the J=3-2 frequency of this molecular ion at 268 GHz in SgrB2(OH) and Orion-KL. These measurements suggest that the [HCO(+) ]/[HOC(+) ] ratio established by Woods et al. may be correct, and that HOC(+) is more abundant than chemical models predict.

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