Observations of interstellar carbon monosulfide - Evidence for turbulent cores in giant molecular clouds

Details Observations of interstellar carbon monosulfide - Evidence for turbulent cores in giant molecular clouds Observations of interstellar carbon monosulfide - Evidence for turbulent cores in giant molecular clouds

Jan 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...235..437l&link_type=abstract

Astrophysical Journal, Part 1, vol. 235, Jan. 15, 1980, p. 437-451.

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158

Astronomical Models, Carbon Compounds, Interstellar Gas, Nebulae, Sulfides, Abundance, Gas Density, Hydrogen, Radiative Transfer, Temperature Distribution

Scientific paper

Lines of CS(J = 1 to 0) and CS(J = 2 to 1) have been observed with nearly equal beam sizes and high velocity resolution in 32 sources including both giant molecular clouds and dark clouds; with a few exceptions, these two transitions show nearly equal intensities and line widths. Hydrogen densities and CS fractional abundances derived from the data using a velocity gradient radiative transfer (RT) model are in good agreement with the same quantities obtained from the microturbulent model of Liszt and Leung. In addition, values for the (J = 2 to 1) optical depths obtained from RT modeling and other independent arguments fall in the range 0.3 to 3.0, indicating that mold saturation effects can be expected for some CS lines.

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