J/A+A/699/A66ivo://CDS.VizieR/J/A+A/699/A66CDSvan der Jagt S.Osinga E.van Weeren R.J.Miley G.K.Roberts I.D.,Botteon A.Ignesti A.2026-05-06T12:45:55Z2025-06-27T08:17:28ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxy-clustersradio-galaxiesactive-galactic-nucleiredshiftedThe radio jets of radio galaxies in galaxy clusters are often bent due to the ram pressure of the intracluster medium. Most studies of bent radio tails initially identified tailed sources and then attempted to characterise their environments. In this paper we take an alternative approach, by starting with a well-defined sample of galaxy clusters and subsequently identifying tailed radio sources in these known environments. Our sample consists of 81 galaxy clusters from the Planck ESZ cluster sample. We present a catalogue of 127 extended cluster radio sources, including brightest cluster galaxies, obtained by visually inspecting Karl G. Jansky Very Large Array (1-2 GHz) observations. We have determined the bending angle of 109 well-structured sources, and classified them accordingly: 84 narrow-angle tailed sources (NATs), 16 wide-angle tailed sources (WATs), and 9 non-bent radio sources (i.e. with bending angles of less than 15{deg}). We find a negative correlation between the bending angle and the distance to the cluster centre (impact radius), and we observe that NATs generally have smaller impact radii than the regular galaxy population and WATs. We present a phase-space diagram of tailed radio galaxy velocities and impact radii and find that NATs have a significant excess in the high-velocity and low-impact radius region of phase space, indicating they undergo the largest amount of ram pressure bending. We compared the results from our sample with those for jellyfish galaxies, and suggest that the mechanism responsible for bending the radio tails is similar to the stripping of gas in jellyfish galaxies, although tailed radio galaxies are more concentrated in the centre of the phase space. Finally, we find that NATs and WATs have the same occurrence ratio in merging and relaxed clusters. However, their distribution in the phase-space is significantly different. We report an excess of NATs in the high-velocity and low-impact-radius phase-space region in merging clusters, and an excess of NATs in relaxed clusters in the low-velocity and low-impact-radius region.2025A&A...699A..66Vhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/699/A66CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/699/A66https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/699/A66http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/699/A66https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/699/A66https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/699/A66http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/699/A66GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/699/A66/tablea1 (Extended radio source catalogue)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/699/A66/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/699/A66/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/699/A66/tablea1?GETtext/xml+votable180.050000true357.9846-26.0640.0055555555555555566/97 2488 4965 4976 5099 5597 6011 6017 6019 6088 6873 7513 9050 9168 9476 9593 9997 10527 10664 11042 11063 11080 11253 11467 11626 11901 12255 12642 12664 15192 15286 15351 16032-16033 16609 16702 17457 18800 19089 19101 19451 19935 20874 22607 22786 24822 25188 25391 25542 26189 27136 27660-27661 28429-28430 28622 31537 31851 32500 36017 44802-44803 44817 45044 48735 48966https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/699/A66?format=asciiRadiodefaultJ/A+A/699/A66/tablea1Extended radio source cataloguerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Source right ascension (J2000)degpos.eq.ra;meta.mainSimbadNameSimbad column added by the CDSmeta.idcharnullablezGalaxy redshiftsrc.redshiftfloatDEJ2000Source declination (J2000)degpos.eq.dec;meta.mainBA? Bending angle extended radio sourcedegsrc.morph.paramfloatnullabler/r500Distance to the cluster centerphys.size.radius;arith.ratiofloattheta? Orientation angle towards the cluster centerdegpos.posAngfloatnullablePLCKESZPlanck-ESZ cluster namemeta.id.parentcharBCG[yes no] Brightest Cluster Galaxy source indicatormeta.codecharv/sigma? Ofsett Galaxy velocity to the cluster velocity normalised by the cluster dispersionphys.veloc;arith.difffloatnullable