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arXiv · 1405.5759

Star Formation Rates from [CII] 158 um and Mid Infrared Emission Lines for Starbursts and AGN

Lusine Sargsyan·Anahit Samsonyan·Vianney Lebouteiller·Daniel Weedman·Donald Barry·Jeronimo Bernard-Salas·James Houck·Henrik Spoon
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Abstract

A summary is presented for 130 galaxies observed with the Herschel PACS instrument to measure fluxes for the [CII] 158 um emission line. Sources cover a wide range of active galactic nucleus to starburst classifications, as derived from polycyclic aromatic hydrocarbon (PAH) strength measured with the Spitzer Infrared Spectrograph. Redshifts from [CII] and line to continuum strengths (equivalent width of [CII]) are given for the full sample, which includes 18 new [CII] flux measures. Calibration of L([CII)]) as a star formation rate (SFR) indicator is determined by comparing [CII] luminosities with mid-infrared [NeII] and [NeIII] emission line luminosities; this gives the same result as determining SFR using bolometric luminosities of reradiating dust from starbursts: log SFR = log L([CII)]) - 7.0, for SFR in solar masses per year and L([CII]) in solar luminosities. We conclude that L([CII]) can be used to measure SFR in any source to a precision of ~ 50%, even if total source luminosities are dominated by an AGN component. The line to continuum ratio at 158 um, EW([CII]), is not significantly greater for starbursts (median EW([CII]) = 1.0 um) compared to composites and AGN (median EW([CII]) = 0.7 um), showing that the far infrared continuum at 158 um scales with [CII] regardless of classification. This indicates that the continuum at 158 um also arises primarily from the starburst component within any source, giving log SFR = log vLv(158 um) - 42.8 for SFR in solar masses per year and vLv(158 um) in erg per sec.

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Lusine Sargsyan, Anahit Samsonyan, Vianney Lebouteiller, Daniel Weedman, Donald Barry, Jeronimo Bernard-Salas, James Houck, Henrik Spoon. 2014-05-22. Star Formation Rates from [CII] 158 um and Mid Infrared Emission Lines for Starbursts and AGN. https://doi.org/10.1088/0004-637x%2F790%2F1%2F15

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