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

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Pasini , T , Finoguenov , A , Brueggen , M , Gaspari , M , de Gasperin , F & Gozaliasl , G 2021 , ' Radio galaxies in galaxy groups : kinematics, scaling relations, and AGN feedback ' , Monthly Notices of the Royal Astronomical Society , vol. 505 , no. 2 , pp. 2628-2637 . https://doi.org/10.1093/mnras/stab1451

Title: Radio galaxies in galaxy groups : kinematics, scaling relations, and AGN feedback
Author: Pasini, T.; Finoguenov, A.; Brueggen, M.; Gaspari, M.; de Gasperin, F.; Gozaliasl, G.
Other contributor: University of Helsinki, Department of Physics
University of Helsinki, Department of Physics



Date: 2021-08
Language: eng
Number of pages: 10
Belongs to series: Monthly Notices of the Royal Astronomical Society
ISSN: 0035-8711
DOI: https://doi.org/10.1093/mnras/stab1451
URI: http://hdl.handle.net/10138/336504
Abstract: We investigate the kinematic properties of a large (N = 998) sample of COSMOS spectroscopic galaxy members distributed among 79 groups. We identify the Brightest Group Galaxies (BGGs) and cross-match our data with the VLA-COSMOS Deep survey at 1.4 GHz, classifying our parent sample into radio/non-radio BGGs and radio/non-radio satellites. The radio luminosity distribution spans from L-R similar to 2 x 10(21) WHz-1 to LR similar to 3 x 10(25) WHz(-1). A phase-space analysis, performed by comparing the velocity ratio (line-of-sight velocity divided by the group velocity dispersion) with the galaxy-group centre offset, reveals that BGGs (radio and non-radio) are mostly (similar to 80 per cent) ancient infallers. Furthermore, the strongest (L-R > 10(23) W Hz(-1)) radio galaxies are always found within 0.2R(vir) from the group centre. Comparing our samples with HORIZON-AGN, we find that the velocities and offsets of simulated galaxies aremore similar to radio BGGs than to non-radio BGGs, albeit statistical tests still highlight significant differences between simulated and real objects. We find that radio BGGs are more likely to be hosted in high-mass groups. Finally, we observe correlations between the powers of BGG radio galaxies and the X-ray temperatures, T-x, and X-ray luminosities, L-x, of the host groups. This supports the existence of a link between the intragroup medium and the central radio source. The occurrence of powerful radio galaxies at group centres can be explained by Chaotic Cold Accretion, as the AGN can feed from both the galactic and intragroup condensation, leading to the observed positive L-R - T-x correlation.
Subject: 114 Physical sciences
galaxies: clusters: general
galaxies: clusters: intracluster medium
galaxies: groups: general
radio continuum: galaxies
X-rays: galaxies: clusters
BRIGHTEST CLUSTER GALAXIES
ACTIVE GALACTIC NUCLEI
SUPERMASSIVE BLACK-HOLES
X-RAY
STAR-FORMATION
OBSERVATIONAL EVIDENCE
REDSHIFT SURVEY
COLD ACCRETION
MOLECULAR GAS
STELLAR MASS
115 Astronomy, Space science
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