Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 742786.0, MPI für Astronomie / Publikationen_mpia
The origins of [C II] emission in local star-forming galaxies
Authors:Croxall, K. V.; Smith, J. D.; Pellegrini, E.; Groves, B.; Bolatto, A.; Herrera-Camus, R.; Sandstrom, K. M.; Draine, B.; Wolfire, M. G.; Armus, L.; Boquien, M.; Brandl, B.; Dale, D.; Galametz, M.; Hunt, L.; Kennicutt, R.; Kreckel, K.; Rigopoulou, D.; van der Werf, P.; Wilson, C.
Date of Publication (YYYY-MM-DD):2017
Title of Journal:The Astrophysical Journal
Volume:845
Issue / Number:2
Start Page:id. 96 (7 pp)
Audience:Not Specified
Abstract / Description:The [C ii] 158 μm fine-structure line is the brightest emission line observed in local star-forming galaxies. As a major coolant of the gas-phase interstellar medium, [C ii] balances the heating, including that due to far-ultraviolet photons, which heat the gas via the photoelectric effect. However, the origin of [C ii] emission remains unclear because C+ can be found in multiple phases of the interstellar medium. Here we measure the fractions of [C ii] emission originating in the ionized and neutral gas phases of a sample of nearby galaxies. We use the [N ii] 205 μm fine-structure line to trace the ionized medium, thereby eliminating the strong density dependence that exists in the ratio of [C ii]/[N ii] 122 μm. Using the FIR [C ii] and [N ii] emission detected by the KINGFISH (Key Insights on Nearby Galaxies: a Far- Infrared Survey with Herschel) and Beyond the Peak Herschel programs, we show that 60%-80% of [C ii] emission originates from neutral gas. We find that the fraction of [C ii] originating in the neutral medium has a weak dependence on dust temperature and the surface density of star formation, and has a stronger dependence on the gas-phase metallicity. In metal-rich environments, the relatively cooler ionized gas makes substantially larger contributions to total [C ii] emission than at low abundance, contrary to prior expectations. Approximate calibrations of this metallicity trend are provided.
Free Keywords:galaxies: ISM; ISM: lines and bands
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-637X
URL:http://adsabs.harvard.edu/abs/2017ApJ...845...96C
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.