Galaxy populations and redshift dependence of the correlation between infrared and radio luminosity

¹ INAF, Osservatorio Astronomico di Padova, Vicolo Osservatorio 5, 35122 Padova, Italy
² INAF, Istituto di Radioastronomia – Italian ARC, Via Piero Gobetti 101, 40129 Bologna, Italy
³ INAF, Istituto di Radioastronomia, Via Piero Gobetti 101, 40129 Bologna, Italy
⁴ SISSA, Via Bonomea 265, 34136 Trieste, Italy
⁵ School of Physics and Astronomy, Cardiff University, The Parade CF24 3AA, UK
⁶ Hiroshima Astrophysical Science Center, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan
⁷ National Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, Tokyo, Japan
⁸ Department of Astronomy, University of Cape Town, 7701 Rondebosch, Cape Town, South Africa

Received: 22 January 2024
Accepted: 26 June 2024

Abstract

We argue that the difference in infrared-to-radio luminosity ratio between local and high-redshift star-forming galaxies reflects the alternative physical conditions –including magnetic field configurations– of the dominant population of star-forming galaxies in different redshift ranges. We define three galactic types, based on our reference model, with reference to ages of stellar populations. “Normal” late-type galaxies dominate the star formation in the nearby Universe; “starburst” galaxies take over at higher redshifts, up to z ∼ 1.5; while “protospheroidal” galaxies dominate at high redshift. A reanalysis of data from the COSMOS field combined with literature results shows that, for each population, the data are consistent with an almost redshift-independent mean value of the parameter q_IR, which quantifies the infrared–radio correlation. However, we find a hint of an upturn of the mean q_IR at z ≳ 3.5 consistent with the predicted dimming of synchrotron emission due to cooling of relativistic electrons by inverse Compton scattering off the cosmic microwave background. The typical stellar masses increase from normal, to starburst, and to protospheroidal galaxies, accounting for the reported dependence of the mean q_IR on stellar mass. Higher values of q_IR found for high-z strongly lensed dusty galaxies selected at 500 μm might be explained by differential magnification.