2025A&A...699A..66V

Query : 2025A&A...699A..66V

2025A&A...699A..66V - Astronomy and Astrophysics, volume 699A66 (2025/7-1)

The phase-space of tailed radio galaxies in massive clusters.

VAN DER JAGT S., OSINGA E., VAN WEEREN R.J., MILEY G.K., ROBERTS I.D., BOTTEON A. and IGNESTI A.

Abstract (from CDS):

The 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°). 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.

Abstract Copyright: © The Authors 2025

Journal keyword(s): galaxies: clusters: general - galaxies: jets - galaxies: kinematics and dynamics

VizieR on-line data: <Available at CDS (J/A+A/699/A66): tablea1.dat>

Simbad objects: 51

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Number of rows : 51
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 ACO 2813 ClG 00 43 22.8 -20 37 21           ~ 111 0
2 ACO 115 ClG 00 55 59 +26 23.2           ~ 295 1
3 ACO 209 ClG 01 31 52.9 -13 36 53           ~ 326 0
4 PLCKESZ G171.9-40.7 ClG 03 12 55 +08 22.8           ~ 58 0
5 ACO 426 ClG 03 19 47.6 +41 30 54           ~ 2508 1
6 3C 129 rG 04 49 09.064 +45 00 39.40   19       ~ 273 2
7 MCXC J0616.3-2156 ClG 06 16 21.5 -21 56 30           ~ 27 0
8 ZwCl 0634+4750 ClG 06 38 07.5 +47 47 27           ~ 48 0
9 ACO 697 ClG 08 42 57.6 +36 21 45           ~ 277 0
10 ACO 781 ClG 09 20 25.4 +30 30 07           ~ 167 0
11 ACO 868 ClG 09 45 28.1 -08 38 51           ~ 67 0
12 ACO 980 ClG 10 22 30.6 +50 06 06           ~ 70 0
13 ACO 1132 ClG 10 58 32.05 +56 47 14.2           ~ 145 1
14 ACO 1300 ClG 11 32 00.7 -19 53 34           ~ 168 0
15 ACO 1351 ClG 11 42 24.7795 +58 32 05.558           ~ 90 0
16 ACO 1391 ClG 11 49 47.2581 -12 17 47.653           ~ 41 0
17 ACO 1413 ClG 11 55 12.87 +23 23 46.9           ~ 456 0
18 ACO 1423 ClG 11 57 17.3206 +33 36 39.364           ~ 181 0
19 ACO 1430 ClG 11 59 17.5 +49 47 46           ~ 59 0
20 ACO 1437 ClG 12 00 24.5 +03 19 52           ~ 93 0
21 ACO 1443 ClG 12 01 12.1 +23 05 57           ~ 53 0
22 ACO 1576 ClG 12 36 59.5 +63 11 18           ~ 116 0
23 ACO 1656 ClG 12 59 44.40 +27 54 44.9           ~ 5141 2
24 ACO 1689 ClG 13 11 29.5 -01 20 28           ~ 1178 0
25 ACO 1703 ClG 13 15 05.2 +51 49 02           ~ 157 0
26 MCXC J1332.7+5032 ClG 13 32 44.8 +50 32 24           ~ 134 0
27 ACO 1763 ClG 13 35 20.1 +41 00 04           ~ 335 0
28 ACO 1895 ClG 14 14 07.9735 +71 16 56.256           ~ 47 0
29 ACO 1914 ClG 14 25 57.4 +37 49 54           ~ 338 0
30 ACO 1995 ClG 14 52 55.0 +58 02 59           ~ 140 0
31 ACO S 780 ClG 14 59 29.1 -18 10 45           ~ 93 0
32 ACO 2034 ClG 15 10 03.9 +33 30 57           ~ 248 1
33 2MASX J15150305-1521537 ClG 15 14.9 -15 23           ~ 57 0
34 ACO 2069 ClG 15 24 02.92 +29 53 20.3           ~ 165 0
35 ACO 2204 ClG 16 32 47.7 +05 34 18           ~ 457 0
36 ACO 2218 ClG 16 35 54.0 +66 13 00           ~ 827 1
37 ACO 2219 ClG 16 40 22.1 +46 42 20           ~ 381 0
38 ClG J1720+2638 ClG 17 20 09.6 +26 37 35           ~ 284 0
39 ACO 2261 ClG 17 22 26.9 +32 07 58           ~ 370 0
40 ACO 2294 ClG 17 24 10.1 +85 53 09           ~ 69 0
41 ZwCl 1745+4513 ClG 17 47 12.0 +45 12 37           ~ 46 0
42 CIZA J1804.4+1002 ClG 18 04 31.0476 +10 03 19.069           ~ 28 0
43 ACO 2302 ClG 18 19 57.6 +57 09 58           ~ 37 0
44 ClG 1821+64 ClG 18 21 56.7276 +64 20 55.841           ~ 511 1
45 CIZA J1938.3+5409 ClG 19 38 18.6 +54 09 33           ~ 42 0
46 ACO 2345 ClG 21 27 05.391 -12 09 07.41           ~ 151 0
47 ClG J2135-0102 ClG 21 35 12.00 -01 03 00.1           ~ 70 0
48 ACO 2355 ClG 21 35 18.70 +01 25 27.0           ~ 75 0
49 ACO 2390 ClG 21 53 37.4 +17 41 46           ~ 732 2
50 ACO 2409 ClG 22 00 52.7 +20 58 27           ~ 101 0
51 ACO 2443 ClG 22 26 14.09 +17 25 13.5           ~ 126 0

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