Please note that eDoc will be permanently shut down in the first quarter of 2021!      Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 730209.0, MPI für Astronomie / Publikationen_mpia
[C II] 158 μm emission as a star formation tracer
Authors:Herrera-Camus, R.; Bolatto, A. D.; Wolfire, M. G.; Smith, J. D.; Croxall, K. V.; Kennicutt, R. C.; Calzetti, D.; Helou, G.; Walter, F.; Leroy, A. K.; Draine, B.; Brandl, B. R.; Armus, L.; Sandstrom, K. M.; Dale, D. A.; Aniano, G.; Meidt, S. E.; Boquien, M.; Hunt, L. K.; Galametz, M.; Tabatabaei, F. S.; Murphy, E. J.; Appleton, P.; Roussel, H.; Engelbracht, C.; Beirao, P.
Date of Publication (YYYY-MM-DD):2015
Title of Journal:The Astrophysical Journal
Issue / Number:1
Start Page:id. 1 (22 pp)
Audience:Not Specified
Abstract / Description:The [C II] 157.74 μm transition is the dominant coolant of the neutral interstellar gas, and has great potential as a star formation rate (SFR) tracer. Using the Herschel KINGFISH sample of 46 nearby galaxies, we investigate the relation of [C II] surface brightness and luminosity with SFR. We conclude that [C II] can be used for measurements of SFR on both global and kiloparsec scales in normal star-forming galaxies in the absence of strong active galactic nuclei (AGNs). The uncertainty of the Σ[C II] - ΣSFR calibration is ±0.21 dex. The main source of scatter in the correlation is associated with regions that exhibit warm IR colors, and we provide an adjustment based on IR color that reduces the scatter. We show that the color-adjusted Σ[C II] - ΣSFR correlation is valid over almost five orders of magnitude in ΣSFR, holding for both normal star-forming galaxies and non-AGN luminous infrared galaxies. Using [C II] luminosity instead of surface brightness to estimate SFR suffers from worse systematics, frequently underpredicting SFR in luminous infrared galaxies even after IR color adjustment (although this depends on the SFR measure employed). We suspect that surface brightness relations are better behaved than the luminosity relations because the former are more closely related to the local far-UV field strength, most likely the main parameter controlling the efficiency of the conversion of far-UV radiation into gas heating. A simple model based on Starburst99 population-synthesis code to connect SFR to [C II] finds that heating efficiencies are 1%-3% in normal galaxies.
Free Keywords:galaxies: ISM; galaxies: star formation; infrared: galaxies; ISM: structure
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
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.