158 μm emission as a star formation tracer

R. Herrera-Camus, A. D. Bolatto, M. G. Wolfire, J. D. Smith, K. V. Croxall, R. C. Kennicutt, D. Calzetti, G. Helou, F. Walter, A. K. Leroy, B. Draine, B. R. Brandl, L. Armus, K. M. Sandstrom, D. A. Dale, G. Aniano, S. E. Meidt, M. Boquien, L. K. Hunt, M. GalametzF. S. Tabatabaei, E. J. Murphy, P. Appleton, H. Roussel, C. Engelbracht, P. Beirao

Research output: Contribution to journalArticle

73 Scopus citations

Abstract

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]SFR 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]SFR 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.

Original languageEnglish (US)
Article number1
JournalAstrophysical Journal Letters
Volume800
Issue number1
DOIs
StatePublished - Feb 10 2015

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • ISM: structure
  • galaxies: ISM
  • galaxies: star formation
  • infrared: galaxies

Fingerprint Dive into the research topics of '158 μm emission as a star formation tracer'. Together they form a unique fingerprint.

  • Cite this

    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., ... Beirao, P. (2015). 158 μm emission as a star formation tracer. Astrophysical Journal Letters, 800(1), [1]. https://doi.org/10.1088/0004-637X/800/1/1