Calibrating Photometric Mid-Infrared Star Formation Rates for JWST

TL;DR

This study calibrates mid-infrared photometry from JWST as a reliable star formation rate indicator across a wide luminosity range, accounting for dust effects and galaxy mass.

Contribution

It introduces broken power-law and composite relations for MIRI photometry to accurately estimate SFR, improving previous IR-based methods.

Findings

Rest-frame 6-8um luminosity correlates superlinearly with SFR below 8 solar masses per year.

A UV+IR composite relation reduces scatter to ~0.15 dex, enhancing SFR estimates.

MIRI photometry effectively traces SFR for galaxies with stellar mass above 10^9 solar masses up to z~3.

Abstract

The mid-infrared (IR) spectrum of galaxies has a long history as a valuable proxy for the dust-obscured star formation rate (SFR) in massive galaxies. Now, with JWST, we can explore the mid-IR's full potential as a SFR tracer over four orders of magnitude in total infrared luminosity (9<~log LIR/Lo<~13). First, combining the SMILES and FRESCO surveys, we evaluate MIRI photometry against the Pa-alpha emission line - a gold standard SFR indicator - in Main Sequence (MS) galaxies at cosmic noon. We find the rest-frame 6-8um luminosity has a steeply superlinear relation with SFR(Pa-alpha) below ~8 Mo/yr, in contrast with the unity slope seen in coeval massive galaxies. We derive broken power-law SFR indicators from single-band MIRI photometry plus a representative dust template, with a scatter typical of IR SFRs (~0.2-0.3 dex). Despite the break in the mid-IR behavior and our simplifying assumption of a single dust SED, we next successfully formulate a UV+IR composite relation (scatter ~0.15 dex) under the usual assumption of energy balance. This implies that the rest-frame 6-8um primarily tracks the global dust-obscuration fraction - which decreases rapidly at log M*/Mo<~10 - rather than reflecting a deficit in PAH abundances at low mass. Our results thus support MIRI photometry as a robust SFR proxy at log M*/Mo>~9 up to z~3. Finally, extending to local and z>~1 ultraluminous infrared galaxies not represented in SMILES, we examine when Pa-alpha and the IR reliably track SFR in the bright regime.