CN line emission from the molecular clouds associated with S106 and and NGC 7538

Details CN line emission from the molecular clouds associated with S106 and and NGC 7538 CN line emission from the molecular clouds associated with S106 and and NGC 7538

Jul 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...258..515c&link_type=abstract

Astrophysical Journal, Part 1, vol. 258, July 15, 1982, p. 515-532.

Astronomy and Astrophysics

Astrophysics

36

Cyanogen, Emission Spectra, Interstellar Gas, Line Spectra, Molecular Clouds, Stellar Evolution, Abundance, Astronomical Maps, Electron Transitions, Gas Temperature, Hydrogen Clouds

Scientific paper

The molecular clouds associated with S106 and NGC 7538 are studied to determine the line intensity distributions of the N=1-0 transition of CN. In the case of S106, CN line emission is proportional to CN column density and, despite the complexity and direct influence of the galaxy's temperature and density structure, CN column density and line intensity vary together. In NGC 7538, CN column density is constant over the entire region mapped, and CN line intensities vary with excitation temperature. CN emission toward NGC 7538 therefore outlines a region of enhanced H2 density, or kinetic temperature, or both. Of three regions of successive star formation apparent toward NGC 7538, the most recent star formation seems to be taking place in the region of maximum CN emission. The similarity of relative molecular abundances of the two objects studied suggests that the same chemical processes occur in their clouds, and that the chemical time scale is probably short relative to the ages of the clouds.

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