The molecular core in G34.3 + 0.2 - Millimeter interferometric observations of HCO(+), H(C-13)N, H(C-15)N, and SO

Details The molecular core in G34.3 + 0.2 - Millimeter interferometric observations of HCO(+), H(C-13)N, H(C-15)N, and SO The molecular core in G34.3 + 0.2 - Millimeter interferometric observations of HCO(+), H(C-13)N, H(C-15)N, and SO

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...385..244c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 385, Jan. 20, 1992, p. 244-254. Research supported by Universidad Nacional

Astronomy and Astrophysics

Astrophysics

43

Carbon Isotopes, Formyl Ions, Hydrocyanic Acid, Microwave Interferometers, Molecular Gases, Star Formation, Sulfur Oxides, H Ii Regions, High Resolution, Interstellar Matter, Nitrogen Isotopes

Scientific paper

This study presents high-resolution observations of the molecular core in the star-forming region G34.3 + 0.2. Maps at 6-arcsec resolution of emission and absorption of the J = 1 - 0 transitions of HCO(+), H (C-13)N, H(C-15)N, and of the 2(2) - 1(1) transition of SO were obtained in addition to a map of the 3.4-mm continuum emission from the compact H II component. The HCL(+) emission toward G34.3 + 0.2 traces a warm molecular core about 0.9 pc in size. Emission from H (C-13)N is detected over about 0.3 pc. The cometary H II region lies near the edge of the molecular core. The blueshift of the radio recombination lines with respect to the molecular emission suggests that gas from the H II region is accelerated in a champagne flow caused by a steep gradient in the ambient gas density.

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