Astrophys. J., 714, 1256-1279 (2010/May-2)
The calibration of monochromatic far-infrared star formation rate indicators.
CALZETTI D., WU S.-Y., HONG S., KENNICUTT R.C., LEE J.C., DALE D.A., ENGELBRACHT C.W., VAN ZEE L., DRAINE B.T., HAO C.-N., GORDON K.D., MOUSTAKAS J., MURPHY E.J., REGAN M., BEGUM A., BLOCK M., DALCANTON J., FUNES J., GIL DE PAZ A., JOHNSON B., SAKAI S., SKILLMAN E., WALTER F., WEISZ D., WILLIAMS B. and WU Y.
Abstract (from CDS):
Spitzer data at 24, 70, and 160 µm and ground-based Hα images are analyzed for a sample of 189 nearby star-forming and starburst galaxies to investigate whether reliable star formation rate (SFR) indicators can be defined using the monochromatic infrared dust emission centered at 70 and 160 µm. We compare recently published recipes for SFR measures using combinations of the 24 µm and observed Hα luminosities with those using 24 µm luminosity alone. From these comparisons, we derive a reference SFR indicator for use in our analysis. Linear correlations between SFR and the 70 µm and 160 µm luminosity are found for L(70) ≳ 1.4x1042 erg/s and L(160) ≳ 2x1042 erg/s, corresponding to SFR ≳ 0.1-0.3 M☉/yr, and calibrations of SFRs based on L(70) and L(160) are proposed. Below those two luminosity limits, the relation between SFR and 70 µm (160 µm) luminosity is nonlinear and SFR calibrations become problematic. A more important limitation is the dispersion of the data around the mean trend, which increases for increasing wavelength. The scatter of the 70 µm (160 µm) data around the mean is about 25% (factor ∼2) larger than the scatter of the 24 µm data. We interpret this increasing dispersion as an effect of the increasing contribution to the infrared emission of dust heated by stellar populations not associated with the current star formation. Thus, the 70 (160) µm luminosity can be reliably used to trace SFRs in large galaxy samples, but will be of limited utility for individual objects, with the exception of infrared-dominated galaxies. The nonlinear relation between SFR and the 70 and 160 µm emission at faint galaxy luminosities suggests a variety of mechanisms affecting the infrared emission for decreasing luminosity, such as increasing transparency of the interstellar medium, decreasing effective dust temperature, and decreasing filling factor of star-forming regions across the galaxy. In all cases, the calibrations hold for galaxies with oxygen abundance higher than roughly 12 +log(O/H) ∼ 8.1. At lower metallicity, the infrared luminosity no longer reliably traces the SFR because galaxies are less dusty and more transparent.
galaxies: interactions - galaxies: ISM - galaxies: starburst - infrared: galaxies - ISM: structure - stars: formation
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<Available at CDS (J/ApJ/714/1256): table1.dat refs.dat>
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