Star formation rates from [C II] 158 μm and mid-infrared emission lines for starbursts and active galactic nuclei

Journal Article · Sun Jul 20 04:00:00 EDT 2014 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/790/1/15· OSTI ID:22365619

Sargsyan, L.; Lebouteiller, V.; Weedman, D.; Barry, D.; Spoon, H. ^[1]; Samsonyan, A. ^[2]; Bernard-Salas, J. ^[3]

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1. Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853 (United States)
2. Byurakan Astrophysical Observatory, Byurakan 0213 (Armenia)
3. Department of Physical Sciences, Open University, Milton Keynes MK7 6AA (United Kingdom)

A summary is presented for 130 galaxies observed with the Herschel Photodetector Array Camera and Spectrometer instrument to measure fluxes for the [C II] 158 μm emission line. Sources cover a wide range of active galactic nucleus to starburst classifications, as derived from polycyclic aromatic hydrocarbon strength measured with the Spitzer Infrared Spectrograph. Redshifts from [C II] and line to continuum strengths (equivalent width (EW) of [C II]) are given for the full sample, which includes 18 new [C II] flux measures. Calibration of L([C II)]) as a star formation rate (SFR) indicator is determined by comparing [C II] luminosities with mid-infrared [Ne II] and [Ne III] emission line luminosities; this gives the same result as determining SFR using bolometric luminosities of reradiating dust from starbursts: log SFR = log L([C II)]) – 7.0, for SFR in M{sub ☉} yr{sup –1} and L([C II]) in L{sub ☉}. We conclude that L([C II]) can be used to measure SFR in any source to a precision of ∼50%, even if total source luminosities are dominated by an active galactic nucleus (AGN) component. The line to continuum ratio at 158 μm, EW([C II]), is not significantly greater for starbursts (median EW([C II]) = 1.0 μm) compared to composites and AGNs (median EW([C II]) = 0.7 μm), showing that the far-infrared continuum at 158 μm scales with [C II] regardless of classification. This indicates that the continuum at 158 μm also arises primarily from the starburst component within any source, giving log SFR = log νL{sub ν}(158 μm) – 42.8 for SFR in M{sub ☉} yr{sup –1} and νL{sub ν}(158 μm) in erg s{sup –1}.

• OSTI ID: 22365619
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 790; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
ACCURACY
BOLOMETERS
CALIBRATION
CLASSIFICATION
COMPARATIVE EVALUATIONS
DUSTS
EMISSION
GALAXIES
GALAXY NUCLEI
LUMINOSITY
POLYCYCLIC AROMATIC HYDROCARBONS
RED SHIFT
SPECTROMETERS
STARS