The energetics of molecular clouds. IV - The S88 molecular cloud

Details The energetics of molecular clouds. IV - The S88 molecular cloud The energetics of molecular clouds. IV - The S88 molecular cloud

Nov 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...250..200e&link_type=abstract

Astrophysical Journal, Part 1, vol. 250, Nov. 1, 1981, p. 200-212. Research supported by the Research Corp.

Astronomy and Astrophysics

Astronomy

24

Emission Spectra, Infrared Astronomy, Interstellar Gas, Molecular Clouds, Molecular Spectra, Carbon Monoxide, H Ii Regions, Line Spectra, Luminosity, Radio Sources (Astronomy), Spectrum Analysis

Scientific paper

The S88 molecular cloud has been observed in several molecular lines and at infrared wavelengths from 1 to 100 microns. The CO emission has a single, sharp peak which is near the H-alpha emission region S88 B and centered on a compact H II region observed in the radio continuum. The infrared observations indicate that the principal luminosity source is located near the radio continuum peak and is hidden behind substantial extinction, presumably from the molecular cloud. The molecular cloud has a size of about 6.5 pc and a mass of about 5,000 solar masses at an assumed distance of 2 kpc. Regions of very high density (more than 10,000/cu cm) do not seem to be present. Analysis of the energetics leads to a predicted dust cooling rate in good agreement with the infrared observations, which indicate L = 180,000 solar luminosities. A more detailed examination of the energetics indicates that densities may be insufficient for collisions of molecules with warm dust grains to heat the gas to the observed kinetic temperature.

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