Far-infrared spectroscopy of galaxies - The 158 micron C(+) line and the energy balance of molecular clouds

Details Far-infrared spectroscopy of galaxies - The 158 micron C(+) line and the energy balance of molecular clouds Far-infrared spectroscopy of galaxies - The 158 micron C(+) line and the energy balance of molecular clouds

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...291..755c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 291, April 15, 1985, p. 755-771.

Astronomy and Astrophysics

Astrophysics

198

Abundance, Galactic Nuclei, Infrared Spectroscopy, Interstellar Matter, Line Spectra, Molecular Clouds, Carbon, Carbon Monoxide, Emission Spectra, Energy Budgets, Far Infrared Radiation, Hydrogen Clouds, Ionized Gases, Radiant Flux Density, Ultraviolet Radiation

Scientific paper

Observations of the 158 microns fine-structure line of C(+) toward the nuclei of six gas-rich galaxies are presented. The observations are compared with observations of the CO J = 1-0 and H I 21 cm lines, observations of far-IR continuum emission, and observations of forbidden C II emission with the Galaxy. The forbidden C II line comes from dense, warm gas in UV-illuminated photodissociation regions at the surfaces of molecular clouds. This line is probably optically thin in all but the brightest of galactic sources. The variation of forbidden C II brightness from source to source and its ratio to the integrated infrared continuum intensity agree well with the theoretical prediction that UV absorption by dust controls the C(+) column density. The forbidden C II line is a tracer of molecular clouds, especially those near intense sources of UV radiation.

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