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Several works in the past decade have used the ratio between total (rest8-1000$\mu$m) infrared and radio (rest 1.4~GHz) luminosity in star-forminggalaxies (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 amild 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 $>$400,000star-forming galaxies in the COSMOS field, identified via (NUV-r)/(r-J)colours, at redshifts 0.1$<$z$<$4.5. Within each (M$_{\star}$,z) bin, we stackthe deepest available infrared/sub-mm and radio images. We fit the stacked IRspectral energy distributions with typical star-forming galaxy and IR-AGNtemplates, and carefully remove radio AGN candidates via a recursive approach.We find that the IRRC evolves primarily with M$_{\star}$, with more massivegalaxies displaying systematically lower q$_{IR}$. A secondary, weakerdependence on redshift is also observed. The best-fit analytical expression isthe following:q$_{IR}$(M$_{\star}$,z)=(2.646$\pm$0.024)$\times$(1+z)$^{(-0.023\pm0.008)}$-(0.148$\pm$0.013)$\times$($\log~M_{\star}$/M$_{\odot}$-10).The lower IR/radio ratios seen in more massive galaxies are well described bytheir higher observed SFR surface densities. Our findings highlight that usingradio-synchrotron emission as a proxy for SFR requires novelM$_{\star}$-dependent recipes, that will enable us to convert detections fromfuture ultra deep radio surveys into accurate SFR measurements down to low-SFR,low-M$_{\star}$ galaxies.

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