Cosmic evolution of radio-excess active galactic nuclei in quiescent and star-forming galaxies across 0 < z < 4

ontext.Radio-excess active galactic nuclei (radio-AGNs) are essential to our understanding of both the physics of black hole (BH)accretion and the interaction between BHs and host galaxies. Recent deep and wide radio continuum surveys have made it possibleto study radio-AGNs down to lower luminosities and up to higher redshifts than previous studies, and are providing new insights intothe abundance and physical origin of radio-AGNs.Aims.Here we focus on the cosmic evolution, physical properties, and AGN-host galaxy connections of radio-AGNs selected from atotal sample of similar to 400 000 galaxies at 0<z<4 in the GOODS-N and COSMOS fields.Methods.Combining the deep radio continuum data with multi-band, de-blended far-infrared, and submillimeter data, we were ableto identify 983 radio-AGNs out of the entire galaxy sample through radio excess relative to the far-infrared-radio relation.Results.We studied the cosmic evolution of 1.4 GHz radio luminosity functions (RLFs) for both star-forming galaxies (SFGs) andradio-AGNs, which can be well described by a pure luminosity evolution of L proportional to(1+z)-0.34xz+3.57and a pure density evolution of Phi?proportional to(1+z)-0.77xz+2.69, respectively. We derived the turnover luminosity, above which the number density of radio-AGNs surpasses that of SFGs. We show that this crossover luminosity increases with increasing redshifts, from 1022.9W Hz-1atz similar to 0 to 1025.2W Hz-1atz similar to 4. At the full redshift range of 0<z<4, we further derive the probability (pradio) of SFGs and quiescent galaxies (QGs) hosting a radio-AGN, as a function of stellar mass (M?), radio luminosity (LR), and redshift (z), which yields p radio proportional to(1+z)3.08M1.06?L-0.77Rfor SFGs, and pradio proportional to(1+z)2.47M1.41?L-0.60Rfor QGs, respectively. Conclusions. The quantitative relation for the probabilities of galaxies hosting a radio-AGN indicates that radio-AGNs in QGs preferto reside in more massive galaxies with higherL R than those in SFGs. The fraction of radio-AGN increases toward higher redshift in both SFGs and QGs, with a more rapid increase in SFGs.