Continuous Mid-Infrared Star Formation Rate Indicators: Diagnostics for 0<z<3 Star Forming Galaxies

TL;DR

This paper develops continuous, monochromatic star formation rate indicators across 6-70 microns, calibrated with local galaxy data, and applicable to galaxies up to redshift 3, aiding galaxy evolution studies.

Contribution

It introduces a new set of continuous mid-infrared SFR indicators calibrated with multi-wavelength data, extending applicability to higher redshifts and providing publicly accessible tools.

Findings

Indicators are consistent with local calibrations.

Achieve dispersion of 30% or less in SFR estimates.

Applicable to galaxies up to z~3 with JWST.

Abstract

We present continuous, monochromatic star formation rate (SFR) indicators over the mid-infrared wavelength range of 6-70 micron. We use a sample of 58 star forming galaxies (SFGs) in the Spitzer-SDSS-GALEX Spectroscopic Survey (SSGSS) at z<0.2, for which there is a rich suite of multi-wavelength photometry and spectroscopy from the ultraviolet through to the infrared. The data from the Spitzer infrared spectrograph (IRS) of these galaxies, which spans 5-40 micron, is anchored to their photometric counterparts. The spectral region between 40-70 micron is interpolated using dust model fits to the IRS spectrum and Spitzer 70 and 160 micron photometry. Since there are no sharp spectral features in this region, we expect these interpolations to be robust. This spectral range is calibrated as a SFR diagnostic using several reference SFR indicators to mitigate potential bias. Our band-specific continuous SFR indicators are found to be consistent with monochromatic calibrations in the local universe, as derived from Spitzer, WISE, and Herschel photometry. Our local composite template and continuous SFR diagnostics are made available for public use through the NASA/IPAC Infrared Science Archive (IRSA) and have typical dispersions of 30% or less. We discuss the validity and range of applicability for our SFR indicators in the context of unveiling the formation and evolution of galaxies. Additionally, in the era of the James Webb Space Telescope this will become a flexible tool, applicable to any SFG up to z~3.