The infrared-radio correlation of star-forming galaxies is strongly M${}_{\star }$-dependent but nearly redshift-invariant since z$\sim$4

Abstract

Several works in the past decade have used the ratio between total (rest 8-1000$\mu$m) infrared and radio (rest 1.4~GHz) luminosity in star-forming galaxies (q${}_{IR}$), often referred to as the "infrared-radio correlation" (IRRC), to calibrate radio emission as a star formation rate (SFR) indicator. Previous studies constrained the evolution of q${}_{IR}$ with redshift, finding a mild but significant decline, that is yet to be understood. For the first time, we calibrate q${}_{IR}$ as a function of \textit{both} stellar mass (M${}_{\star }$) and redshift, starting from an M${}_{\star }$-selected sample of $>$400,000 star-forming galaxies in the COSMOS field, identified via (NUV-r)/(r-J) colours, at redshifts 0.1$<$z$<$4.5. Within each (M${}_{\star }$,z) bin, we stack the deepest available infrared/sub-mm and radio images. We fit the stacked IR spectral energy distributions with typical star-forming galaxy and IR-AGN templates, and carefully remove radio AGN candidates via a recursive approach. We find that the IRRC evolves primarily with M${}_{\star }$, with more massive galaxies displaying systematically lower q${}_{IR}$. A secondary, weaker dependence on redshift is also observed. The best-fit analytical expression is the following: q${}_{IR}$(M${}_{\star }$,z)=(2.646$\pm$0.024)$\times$(1+z)${}^{(-0.023\pm 0.008)}$-(0.148$\pm$0.013)$\times$($\log M_{\star }$/M${}_{\odot }$-10). The lower IR/radio ratios seen in more massive galaxies are well described by their higher observed SFR surface densities. Our findings highlight that using radio-synchrotron emission as a proxy for SFR requires novel M${}_{\star }$-dependent recipes, that will enable us to convert detections from future ultra deep radio surveys into accurate SFR measurements down to low-SFR, low-M${}_{\star }$ galaxies.

Accepted for publication in A&A. 22 pages + Appendices. 24 figures, 4 tables

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