Observations of interstellar HOCO+: abundance enhancements toward the galactic center.

Y. C. Minh, W. M. Irvine, Lucy M Ziurys

Research output: Contribution to journalArticle

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Abstract

A survey of the 4(04)-3(03) and 1(01)-0(00) transitions of HOCO+ has been made toward several molecular clouds. The HOCO+ molecule was not observed in any sources except Sgr B2 and Sgr A. The 5(05)-4(04) and 4(14)-3(13) transitions were also detected toward Sgr B2. The results indicate that gas phase CO2 is not a major carbon reservoir in typical molecular clouds. In Sgr B2, the HOCO+ antenna temperature exhibits a peak approximately 2' north of the Sgr B2 central position (Sgr B2[M]) and the 4(04)-3(03) line emission is extended over a approximately 10' x 10' region. The column density of HOCO+ at the northern peak in Sgr B2 is approximately 3 x 10(14) cm-2, and the fractional abundance relative to H2 > or = 3 x 10(-10), which is about 2 orders of magnitude greater than recent predictions of quiescent cloud ion-molecule chemistry.

Original languageEnglish (US)
Pages (from-to)175-181
Number of pages7
JournalAstrophysical Journal
Volume334
Issue number1
StatePublished - Nov 1 1988
Externally publishedYes

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molecular clouds
antenna
relative abundance
ion
augmentation
carbon
prediction
gas
molecules
antennas
temperature
chemistry
vapor phases
predictions
ions

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Observations of interstellar HOCO+ : abundance enhancements toward the galactic center. / Minh, Y. C.; Irvine, W. M.; Ziurys, Lucy M.

In: Astrophysical Journal, Vol. 334, No. 1, 01.11.1988, p. 175-181.

Research output: Contribution to journalArticle

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N2 - A survey of the 4(04)-3(03) and 1(01)-0(00) transitions of HOCO+ has been made toward several molecular clouds. The HOCO+ molecule was not observed in any sources except Sgr B2 and Sgr A. The 5(05)-4(04) and 4(14)-3(13) transitions were also detected toward Sgr B2. The results indicate that gas phase CO2 is not a major carbon reservoir in typical molecular clouds. In Sgr B2, the HOCO+ antenna temperature exhibits a peak approximately 2' north of the Sgr B2 central position (Sgr B2[M]) and the 4(04)-3(03) line emission is extended over a approximately 10' x 10' region. The column density of HOCO+ at the northern peak in Sgr B2 is approximately 3 x 10(14) cm-2, and the fractional abundance relative to H2 > or = 3 x 10(-10), which is about 2 orders of magnitude greater than recent predictions of quiescent cloud ion-molecule chemistry.

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