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The infrared-radio correlation (IRRC) of star-forming galaxies can be used toestimate their star formation rate (SFR) based on the radio continuumluminosity at MHz-GHz frequencies. For its application in future deep radiosurveys, it is crucial to know whether the IRRC persists at high redshift z.Previous works have reported that the 1.4 GHz IRRC correlation of star-forminggalaxies is nearly z-invariant up to z=4, but depends strongly on stellar massM. This should be taken into account for SFR calibrations based on radioluminosity. To understand the physical cause behind the M dependence of theIRRC and its properties at higher z, we constructed a phenomenological modelfor galactic radio emission. Our model is based on a dynamo-generated magneticfield and a steady-state cosmic ray population. It includes a number of freeparameters as well as observed scaling relations. We find that the resultingspread of the infrared-to-radio luminosity ratio, q(z, M), with respect to M ismostly determined by the scaling of the galactic radius with M, while theabsolute value of the q(z, M) curves decreases with more efficient conversionof supernova energy to magnetic fields and cosmic rays. Decreasing the slope ofthe cosmic ray injection spectrum, aCR, results in higher radio luminosity,decreasing the absolute values of the q(z, M) curves. Our model reproduces theobserved dependence of the IRRC on M and z when the efficiency ofsupernova-driven turbulence is 5%, 10% of the kinetic energy is converted intomagnetic energy, and aCR = 3. For galaxies with intermediate to high M(10^9.5-10^11 M_sun), our model results in an IRRC that is nearly independentof z. For galaxies with lower M (M=10^8.5 M_sun), we find that the IR-to-radioflux ratio increases with increasing redshift. This matches the observationaldata in that mass bin which currently, however, only extends to z~1.5.

A model for the infrared-radio correlation of main-sequence galaxies at GHz frequencies and its variation on redshift and stellar mass