Spitzer 70~$μ$m Emission as a SFR Indicator for Sub--Galactic Regions

We use Spitzer 24 $μ$m, 70 $μ$m and ground based H$α$ data for a sample of 40 SINGS galaxies to establish a star formation rate (SFR) indicator using 70 $μ$m emission for sub--galactic ($\sim0.05-2\ \rm{kpc}$) line-emitting regions and to investigate limits in application. A linear correlation between 70 $μ$m and SFR is found and a star formation indicator SFR(70) is proposed for line-emitting sub-galactic regions as $\rm Σ(SFR)\ ({M_{\odot}\cdot yr^{-1}\cdot kpc^{-2}})=9.4\times10^{-44}\ Σ(70)\ \rm{(ergs\cdot s^{-1}\cdot kpc^{-2})}$, for regions with $12+\rm{log(O/H)}\gtrsim8.4$ and $\rm Σ(SFR)\gtrsim10^{-3}\ (M_{\odot}\cdot yr^{-1}\cdot kpc^{-2})$, with a 1-$σ$ dispersion around the calibration of $\sim0.16$ dex. We also discuss the influence of metallicity on the scatter of the data. Comparing with the SFR indicator at 70 $μ$m for integrated light from galaxies, we find that there is $\sim40$ excess 70 $μ$m emission in galaxies, which can be attributed to stellar populations not involved in the current star formation activity.

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