The evolution of the low-frequency radio AGN population to z ≃ 1.5 in the ELAIS N1 field

We study the cosmic evolution of radio sources out to z similar or equal to 1.5 using a GMRT 610 MHz survey covering similar to 1.86 deg(2) of the ELAIS N1 field with a minimum/median rms noise 7.1/19.5 mu Jy beam(-1) and an angular resolution of 6 arcsec. We classify sources as star forming galaxies (SFGs), radio-quiet (RQ) and radio-loud (RL) Active Galactic Nuclei (AGNs) using a combination of multiwavelength diagnostics and find evidence in support of the radio emission in SFGs and RQ AGN arising from star formation, rather than AGN-related processes. At high luminosities, however, both SFGs and RQ AGN display a radio excess when comparing radio and infrared star formation rates. The vast majority of our sample lie along the SFR - M-* 'main sequence' at all redshifts when using infrared star formation rates. We derive the 610 MHz radio luminosity function for the total AGN population, constraining its evolution via continuous models of pure density and pure luminosity evolution with Phi* proportional to ( 1 + z)((2.25 +/- 0.38)-(0.63 +/- 0.35)z) and L-610MHz proportional to (1 + 2)((3.45 +/- 0.53)-(0.55 +/- 0.29)z), respectively. For our RQ and RL AGN, we find a fairly mild evolution with redshift best fitted by pure luminosity evolution with L-610MHz proportional to (1 + z)((2.81 +/- 0.43)-(0.57 +/- 0.30)z) for RQ AGN and L-610 MHz proportional to (1+z)((3.5810.54)-(0.5610.29)z) RL AGN. The 610 MHz radio AGN population thus comprises two differently evolving populations whose radio emission is mostly SF-driven or AGN-driven, respectively.

Automated summary

We studied the cosmic evolution of radio sources out to z similar to 1.5 using GMRT 610 MHz survey data, finding that radio emission in SFGs and RQ AGN arises from star formation rather than AGN-related processes. Both SFGs and RQ AGN display a radio excess at high luminosities, and the majority of samples lie along the SFR - M-* 'main sequence' when using infrared star formation rates.