Submillimeter CI and CO Lines in Galaxies
- Creators
- Gerin, Maryvonne
- Phillips, Thomas G.
Abstract
Together with C^+ and CO, C is an important reservoir of carbon in the interstellar medium. We present recent results on the ground state transition of atomic carbon at 492 GHz, and on submillimeter CO lines in nearby galaxies. We show that atomic carbon is a good tracer of molecular gas in spiral galaxy disks. It has also a contribution to the molecular gas cooling: the cooling due to C and CO are of the same order of magnitude, and amounts typically to 4 × 10^(−5) of the FIR continuum. C and CO cooling becomes significant in ULIRG galaxies like Arp220. It is possible to use CI measurements to diagnose the physical conditions in galaxies. Together with CII/CI, the emissivity ratio CI/FIR can be used as a measure of the non-ionizing UV radiation field in galaxies.
Additional Information
© Springer Science+Business Media Dordrecht 2001. We are grateful to F. Boulanger and G. Lagache for helping us using the COBE/FIRAS data, and J. Le Bourlot, G. Pineau des Forêts and E. Roueff for the use of their PDR model. CSO is funded by NSF contract AST96-15025. M.G. acknowledges grants from INSU/CNRS, and NATO.Additional details
- Eprint ID
- 98233
- Resolver ID
- CaltechAUTHORS:20190826-124739498
- AST 96-15025
- NSF
- Institut national des sciences de l'Univers (INSU)
- Centre National de la Recherche Scientifique (CNRS)
- North Atlantic Treaty Organization (NATO)
- Created
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2019-08-26Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field