Cosmic evolution of extragalactic C 1, C 2, and CO luminosity

Details Cosmic evolution of extragalactic C 1, C 2, and CO luminosity Cosmic evolution of extragalactic C 1, C 2, and CO luminosity

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993egte.conf..345b&link_type=abstract

In NASA. Ames Research Center, The Evolution of Galaxies and Their Environment p 345-346 (SEE N93-26706 10-90)

Physics

1

Carbon, Carbon Monoxide, Cosmic Dust, Galactic Evolution, Interstellar Matter, Luminosity, Milky Way Galaxy, Molecular Clouds, Abundance, Emission Spectra, Hydrogen, Red Shift, Time Dependence, Vapor Phases

Scientific paper

Carbon is the fourth most abundant element in the Galaxy with an abundance of approximately 4 x 10(exp -4) relative to hydrogen. Of all abundant metals it is the easiest to observe in the interstellar medium (ISM). Carbon can be found in four dominant forms: dust grains, C 2, C 1, and CO. The latter is the most abundant molecule (next to H2) in molecular clouds. All three gas-phase forms produce strong sub-mm wavelength emission lines and are the principal tracers of the warm and dense neutral phases of the ISM. We calculate the gas-phase abundances of neutral carbon (C 1), ionized carbon (C 2), and carbon monoxide (CO) as a function of cosmic time or redshift z in an idealized scenario of galactic evolution.

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