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Title:
Far-infrared spectroscopy of galaxies - The 158 micron C(+) line and the energy balance of molecular clouds
Authors:
Crawford, M. K.; Genzel, R.; Townes, C. H.; Watson, D. M.
Affiliation:
AA(California, University, Berkeley, CA), AB(California, University, Berkeley, CA), AC(California, University, Berkeley, CA), AD(California Institute of Technology, Pasadena, CA)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 291, April 15, 1985, p. 755-771. (ApJ Homepage)
Publication Date:
04/1985
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
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
DOI:
10.1086/163113
Bibliographic Code:
1985ApJ...291..755C

Abstract

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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