On the Nature of the Molecular Condensation Downstream from HH 80 North

Details On the Nature of the Molecular Condensation Downstream from HH 80 North On the Nature of the Molecular Condensation Downstream from HH 80 North

Mar 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998apj...495l..59g&link_type=abstract

Astrophysical Journal Letters v.495, p.L59

Astronomy and Astrophysics

Astronomy

21

Ism: Individual Alphanumeric: Hh 80 North, Ism: Jets And Outflows, Ism: Molecules, Radio Lines: Ism, Stars: Formation

Scientific paper

We present HCO+ ( J=3-->2 ), H13CO+ ( J=3-->2 ), CS ( J=5-->4 ), and 13CO ( J=2-->1 ) Caltech Submillimeter Observatory observations toward the dense quiescent clump downstream from HH 80 North. This condensation is one in a class of sources that show anomalous molecular abundances, probably produced by UV radiation from a nearby shock. The HCO+ emission properties--location, size, center velocity, line widths, and excitation temperature--are similar to those of the ammonia emission, suggesting that it arises from the same region. The H13CO+ ( J=3-->2 ) and CS ( J=5-->4 ) lines are marginally detected. Comparison between NH3, HCO+, and CS implies an ammonia enhancement relative to CS of at least 1 order of magnitude, whereas HCO+ shows only a weak enhancement relative to CS. These results are compatible with the radiative shock-induced chemistry models (Taylor & Williams; Wolfire & Konigl) when we take into account the extinction. Our results suggest that the dense clump detected in NH3 and HCO+ is illuminated by HH 80 North, making this region a good laboratory for studying the chemical processes in a quiescent clump radiatively excited by shocks.

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