Atomic carbon near the molecular cloud/H II region interface in S 140

Details Atomic carbon near the molecular cloud/H II region interface in S 140 Atomic carbon near the molecular cloud/H II region interface in S 140

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992a%26a...259l..77h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 259, no. 2, p. L77-L80.

Astronomy and Astrophysics

Astrophysics

12

Atomic Spectra, Carbon, Fine Structure, H Ii Regions, Molecular Clouds, Spectral Line Width, Abundance, Interstellar Matter, Neutral Atoms, Recombination Reactions

Scientific paper

We have observed the (CI) 3P1 - 3P0 fine structure line of atomic carbon at 492 GHz in the edge-on interface between the molecular cloud L 1204 and the S 140 H II region with the KOSMA telescope on Gornergrat, Switzerland. We find that the (CI)-emission near the interface consists of a narrow velocity component with position and line width similar to that of the ambient molecular cloud material, superimposed on a wider component (FWHM is approximately equal to 15 km/s) exhibiting a line profile similar to that of the higher velocity material visible in CO and carrying most of the CI column density. The velocity integrated (CI) emission peaks near the edge of the cloud facing the exciting star. This finding is in contrast to earlier results by Keene et al. (1985) who missed the wide velocity component in their observations. The relative CI/CO abundance is strongly enhanced in the high velocity material (100 percent) relative to the ambient cloud material (11 percent).

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