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The [CII] and [OI] emission lines in NGC6946 and NGC1313

Contursi, A. and Brauher, J. and Helou, G. (2001) The [CII] and [OI] emission lines in NGC6946 and NGC1313. Astrophysics and Space Science, 277 (S1). pp. 59-62. ISSN 0004-640X. https://resolver.caltech.edu/CaltechAUTHORS:20191018-094103570

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Abstract

The [CII (158 μm)] fine structure line, which is the principal cooling line of the atomic gas, in two nearby galaxies observed with LWS on board ISO is compared to dust and HI gas emission and heating intensity. The relation between photoelectric effect on different grains populations, dust and gas heating found for a sample of 60 normal galaxies for which global [CII] measurements are available, still holds on scale of ∼1.5 kpc. We also succeed in detecting cooling from a low density diffuse atomic gas associated with the diffuse optical disk in both galaxies, accounting typically for ∼ 30–40% of the total [CII] emission.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1023/a:1012771409683DOIArticle
https://rdcu.be/bUIOOPublisherFree ReadCube access
ORCID:
AuthorORCID
Helou, G.0000-0003-3367-3415
Additional Information:© 2001 Kluwer Academic Publishers.
Group:Infrared Processing and Analysis Center (IPAC)
Subject Keywords:ISO, Far infrared structure lines, galaxies, galaxies, ISMdust, gas, ISM, heating, cooling
Issue or Number:S1
Record Number:CaltechAUTHORS:20191018-094103570
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20191018-094103570
Official Citation:Contursi, A., Brauher, J. & Helou, G. Astrophysics and Space Science (2001) 277(Suppl 1): 59. https://doi.org/10.1023/A:1012771409683
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:99355
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:22 Oct 2019 22:40
Last Modified:22 Oct 2019 22:40

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