Radio galaxies in galaxy groups: kinematics, scaling relations, and AGN feedback

We investigate the kinematic properties of a large (N=998) sample COSMOS spectroscopic galaxy members distributed among 79 groups. identify Brightest Group Galaxies (BGGs) and cross-match our data with VLA-COSMOS Deep survey at 1.4 GHz, classifying parent into radio/non-radio BGGs satellites. The radio luminosity distribution spans from $L_R\sim2\times10^{21}$ W Hz$^{-1}$ to $L_R\sim3\times$10$^{25}$ Hz$^{-1}$. A phase-space analysis, performed by comparing velocity ratio (line-of-sight divided group dispersion) galaxy-group centre offset, reveals that (radio non-radio) are mostly ($\sim$80\%) ancient infallers. Furthermore, strongest ($L_R>10^{23}$ Hz$^{-1}$) galaxies always found within 0.2$R_{\rm vir}$ centre. Comparing samples HORIZON-AGN, we find velocities offsets simulated more similar than non-radio BGGs, albeit statistical tests still highlight significant differences between real objects. likely be hosted in high-mass Finally, observe correlations powers BGG X-ray temperatures, $T_{\rm x}$, luminosities, $L_{\rm host This supports existence link intragroup medium central source. occurrence powerful centres can explained Chaotic Cold Accretion, as AGN feed both galactic condensation, leading observed positive R}-T_{\rm x}$ correlation.