J/A+A/699/A66 Extended cluster radio sources catalog (van der Jagt+, 2025)
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., Ignesti A.
<Astron. Astrophys. 699, A66 (2025)>
=2025A&A...699A..66V 2025A&A...699A..66V (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, radio ; Active gal. nuclei ;
Redshifts
Keywords: galaxies: clusters - galaxies: jets -
galaxies: kinematics and dynamics
Abstract:
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.
Description:
In this paper, we investigate tailed radio galaxies in 81 massive
clusters of galaxies at z<0.35 observed with the Karl G. Jansky Very
Large Array.
We present a catalogue of 127 extended cluster radio sources, obtained
by visually inspecting Karl G. Jansky Very Large Array (1-2GHz)
observations. We determined the bending angle, as well as the Galaxy
velocity compared to the cluster and the distance to the cluster
center.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 65 127 Extended radio source catalogue
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 F8.4 deg RAdeg Source right ascension (J2000)
10- 17 F8.4 deg DEdeg Source declination (J2000)
19- 23 F5.2 --- z Galaxy redshift
25- 30 F6.2 deg BA ?=- Bending angle extended radio source
32- 35 F4.2 --- r/r500 Distance to the cluster center
37- 42 F6.2 deg theta ?=- Orientation angle towards the cluster center
44- 56 A13 --- PLCKESZ Planck-ESZ cluster name
58- 60 A3 --- BCG [yes no] Brightest Cluster Galaxy source
indicator
62- 65 F4.2 --- v/sigma ?=- Ofsett Galaxy velocity to the cluster
velocity normalised by the cluster dispersion
--------------------------------------------------------------------------------
Acknowledgements:
Stefan van der Jagt, s_vdjagt(at)hotmail.com
(End) Patricia Vannier [CDS] 22-May-2025