The energetics of molecular clouds. V - The S37 molecular cloud

Details The energetics of molecular clouds. V - The S37 molecular cloud The energetics of molecular clouds. V - The S37 molecular cloud

Feb 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...253..115e&link_type=abstract

Astrophysical Journal, Part 1, vol. 253, Feb. 1, 1982, p. 115-130. Research supported by Research Corp. No. AST-79-20966;

Astronomy and Astrophysics

Astronomy

4

Infrared Astronomy, Molecular Clouds, Molecular Spectra, Carbon Monoxide, Cosmic Dust, Formaldehyde, Infrared Spectra

Scientific paper

The molecular clouds of S37, which coincides with a region of visual obscuration, is observed at several molecular transition frequencies and at IR wavelengths in the 2-125 micron range. It is found that the temperature and the column density peak near the reflection nebulae vdB 118 and 119, with line splitting and possible self-absorption being observed near the latter. Although many 2-micron sources are observed in the direction of the cloud, no bright, 10-micron sources are seen, and far-IR emission is found over an extensive region in the cloud. An energetics analysis leads to the prediction of a dust cooling rate consistent with the far-IR observations, which indicate not less than 15,000-35,000 solar luminosities, and more detailed energetics examinations show that the conditions necessary for collision heating of the gas by warm dust exist.

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