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

TL;DR

This study establishes a linear relation between 70 μm emission and star formation rate for sub-galactic regions, providing a new SFR indicator and analyzing its limitations and dependence on metallicity.

Contribution

The paper introduces a calibrated SFR indicator based on 70 μm emission for sub-galactic regions, accounting for metallicity effects and differences from galaxy-wide measurements.

Findings

A linear correlation between 70 μm emission and SFR for sub-galactic regions.

Proposed SFR(70) indicator with specific calibration parameters.

Approximately 40% excess 70 μm emission in entire galaxies due to older stellar populations.

Abstract

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