A Survey of Molecular Lines Toward Massive Clumps in Early Evolutionary Stages of High-mass Star Formation

Details A Survey of Molecular Lines Toward Massive Clumps in Early Evolutionary Stages of High-mass Star Formation A Survey of Molecular Lines Toward Massive Clumps in Early Evolutionary Stages of High-mass Star Formation

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010apj...714.1658s&link_type=abstract

The Astrophysical Journal, Volume 714, Issue 2, pp. 1658-1671 (2010).

Astronomy and Astrophysics

Astronomy

8

Ism: Clouds, Ism: Molecules, Stars: Formation

Scientific paper

We have observed the CH3OH J = 2-1, SiO J = 2-1, C34S J = 2-1, H13CO+ J = 1-0, HN13C J = 1-0, CCH N = 1-0, OCS J = 8-7, and SO JN = 22-11 lines toward 20 massive clumps, including Midcourse Space Experiment (MSX) 8 μm dark sources (infrared dark clouds) and MSX 8 μm sources, by using the Nobeyama Radio Observatory 45 m telescope. We have found that the velocity widths of the CH3OH and C34S lines are broader than those of the H13CO+ line in the MSX dark sources. On the other hand, they are comparable to the velocity width of the H13CO+ line in the MSX sources. In addition, the [SiO]/[H13CO+] abundance ratio is found to be enhanced in the MSX dark sources in comparison with the MSX sources. These results suggest that shocks caused by interaction between an outflow and an ambient dense gas would have substantial impact on the chemical composition of the MSX dark sources. The velocity widths of the CH3OH and C34S lines relative to that of the H13CO+ line as well as the [SiO]/[H13CO+] abundance ratio could be used as good tools for investigating evolutionary stages of massive clumps. On the basis of the results, we discuss the chemical and physical evolution of massive clumps.

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