The correlation of C II 158 micron and CO (J = 1 - 0) line emission

Details The correlation of C II 158 micron and CO (J = 1 - 0) line emission The correlation of C II 158 micron and CO (J = 1 - 0) line emission

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...344..770w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 344, Sept. 15, 1989, p. 770-778.

Astronomy and Astrophysics

Astrophysics

86

Carbon, Galactic Nuclei, H Ii Regions, Line Spectra, Spectral Correlation, Carbon Monoxide, Emission Spectra, Photodissociation, Planetary Nebulae, Reflection Nebulae

Scientific paper

The good correlation observed between the C II 158 micron and CO (J = 1 - 0) line emission from a large sample of Galactic H II regions, reflection nebulae, PN, and extragalactic nuclei is explained here by postulating a common origin to these two lines: photodissociation regions produced by the illumination of molecular clouds by FUV flux which are more than 100 times the average local interstellar field. Part of the correlation is due to a similar density dependence of I(C II) and I(CO) at high incident flux and part is due to beam dilution of Galactic and extragalactic sources. A method is presented for estimating a low limit to the beam filling factor of emitting gas and the incident UV radiation field.

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