The radio-loud AGN population atz≳ 1 in the COSMOS field

Abstract

We select a sample of radio galaxies at high redshifts (z>~1) in the COSMOS field, by cross-matching optical/infrared images with the FIRST radio data. The aim of this study is to explore the high-z radio-loud (RL) AGN population at much lower luminosities than the classical samples of distant radio sources and similar to those of the local population of radio galaxies. The wide multiwavelength coverage provided by the COSMOS survey allows us to derive their Spectral Energy Distributions (SEDs). The SED modeling with stellar and dust components (with our code 2SPD) returns several important quantities associated with the AGN and host properties. The final sample consists of 74 RL AGN, which extends the sample previously selected by Chiaberge et al. (2009) and studied by Baldi et al. (2013). The resulting photometric redshifts range from z~0.7 to 3. The sample mostly includes compact radio sources, but also 21 FRIIs; the radio power distribution of the sample at 1.4 GHz covers ~10^(31.5)-10^(34.3) \erg\s\Hz. The stellar mass of the hosts ranges ~10^(10)-10^(11.5) M_{sun}. The SEDs are dominated by the contribution from an old stellar population for most of the sources. UV and mid-IR (MIR) excesses are observed for half of the sample. The dust luminosities are in the range L_(dust) ~10^(43)-10^(45.5) erg/s (T ~350-1200 K). UV luminosities at 2000 A ranges ~10^(41.5)-10^(45.5) erg/s. UV emission is significantly correlated with both IR and radio luminosities, the former being the stronger link. However, the origin of UV and dust emission, whether it is produced by the AGN of by star formation, is still unclear. Our results show that this RL AGN population at high redshifts displays a wide variety of properties from possible quasars at the highest luminosities, to low-luminosity old galaxies, similarly to the local FRI-FRII dichotomy.