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2000ApJ...537..644G - Astrophys. J., 537, 644-653 (2000/July-2)
Atomic carbon in galaxies.
GERIN M. and PHILLIPS T.G.
Abstract (from CDS):
Atomic carbon can contribute significantly to the thermal budget of interstellar gas. The cooling due to C and CO are of the same order of magnitude for most galaxies. However, CO is generally a more important coolant in starburst galaxies. Cooling due to C and CO amounts typically to 2x10–5 of the far-IR (FIR) continuum, or 5% of the C II line. However, C and CO cooling reaches ∼30% of the gas total in ultraluminous infrared galaxies such as Arp 220, where C II is abnormally faint.
Together with C II/FIR, the emissivity ratio C I (1-0)/FIR can be used as a measure of the nonionizing UV radiation field in galaxies. The plots of C II/C I or C II/FIR versus C I/FIR show good correlations, in agreement with photodissociation region (PDR) models, except for two remarkable galaxies, Arp 220 and Mrk 231, where high opacities of the C II line and possibly the dust thermal emission may be factors reducing the C II strength below the predictions of the current PDR models.
Abstract Copyright: ∼
Journal keyword(s): Galaxies: ISM - ISM: Lines and Bands - Radio Lines: Galaxies - Submillimeter
Simbad objects: 22
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