2022A&A...666A...8S


Query : 2022A&A...666A...8S

2022A&A...666A...8S - Astronomy and Astrophysics, volume 666A, 8 (2022/10-1)

Using the polarization properties of double radio relics to probe the turbulent compression scenario.

STUARDI C., BONAFEDE A., RAJPUROHIT K., BRUGGEN M., DE GASPERIN F., HOANG D., VAN WEEREN R.J. and VAZZA F.

Abstract (from CDS):


Context. Radio relics are megaparsec-sized synchrotron sources located in the outskirts of some merging galaxy clusters. Binary-merging systems with a favorable orientation may host two almost symmetric relics, named double radio relics.

Aims. Double radio relics are seen preferentially edge-on and, thus, constitute a privileged sample for statistical studies. Their polarization and Faraday rotation properties give direct access to the relics' origin and magnetic fields.
Methods. In this paper, we present a polarization and rotation measure (RM) synthesis study of four clusters hosting double radio relics, namely 8C 0212+703, Abell 3365, and PLCK G287.0+32.9; previously missing polarization studies; and ZwCl 2341+0000, for which conflicting results have been reported. We used 1-2 GHz Karl G. Jansky Very Large Array observations. We also provide an updated compilation of known double radio relics with important observed quantities. We studied their polarization and Faraday rotation properties at 1.4 GHz and we searched for correlations between fractional polarization and physical resolution, the distance from the cluster center, and the shock Mach number.
Results. The weak correlations found between these quantities are well reproduced by state-of-the-art magneto-hydrodynamical simulations of radio relics, confirming that merger shock waves propagate in a turbulent medium with tangled magnetic fields. Both external and internal Faraday depolarization should play a fundamental role in determining the polarization properties of radio relics at 1.4 GHz. Although the number of double radio relics with RM information is still low, their Faraday rotation properties (i.e., rest-frame RM and RM dispersion below 40 rad m–2 and non-Gaussian RM distribution) can be explained in the scenario in which shock waves with Mach numbers larger than 2.5 propagate along the plane of the sky and compress the turbulent intra-cluster medium.

Abstract Copyright: © C. Stuardi et al. 2022

Journal keyword(s): galaxies: clusters: individual: 8C 0212+703 - galaxies: clusters: individual: Abell 3365 - magnetic fields - galaxies: clusters: individual: PLCK G287.0+32.9 - galaxies: clusters: individual: ZwCl 2341+0000 - galaxies: clusters: intracluster medium

VizieR on-line data: <Available at CDS (J/A+A/666/A8): list.dat fits/*>

Simbad objects: 32

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Number of rows : 32
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 ZwCl 0008+5215 ClG 00 11 37.197 +52 32 31.68           ~ 52 0
2 MCS J0025.4-1222 ClG 00 25 29.381 -12 22 37.06           ~ 138 0
3 ACT-CL J0102-4915 ClG 01 02 52.50 -49 14 58.0           ~ 230 0
4 ZwCl 0104+5350 ClG 01 07 47.8 +54 08 31           ~ 29 0
5 ClG 0217+70 ClG 02 17 00.0 +70 36 00           ~ 32 0
6 GB3 0212+703 Rad 02 17 03.4 +70 35 33           ~ 4 0
7 ACT-CL J0232.2-4421 ClG 02 32 18.69 -44 20 41.5           ~ 110 0
8 ACO S 295 ClG 02 45 35.80 -53 02 16.8           ~ 71 0
9 ACO 3186 ClG 03 52 20.6 -74 00 11           ~ 49 0
10 ACT-CL J0417.5-1154 ClG 04 17 34.6 -11 54 32           ~ 87 0
11 PLCKESZ G200.9-28.2 ClG 04 50 20.90 -02 56 57.6           ~ 11 0
12 ACO 521 ClG 04 54 08.6 -10 14 39           ~ 250 0
13 ACO S 520 ClG 05 16 37.40 -54 30 01.5           ~ 95 0
14 ACO 3365 ClG 05 48 12 -21 56.1           ~ 36 0
15 ACO 3376 ClG 06 01 25.000 -39 59 51.00           ~ 306 0
16 ACT-CL J0935.2+0048 ClG 09 35 15.2 +00 47 46           ~ 10 0
17 ACO 1240 ClG 11 23 37.7 +43 03 28           ~ 99 0
18 PLCKESZ G287.0+32.9 ClG 11 50 49.20 -28 04 36.5           ~ 73 0
19 BAX 199.3086-25.5133 ClG 13 14 25.4 -25 15 44           ~ 102 0
20 ZwCl 1447+2619 ClG 14 49 28.2 +26 07 57           ~ 50 0
21 ACO 2146 ClG 15 56 04.7 +66 20 24           ~ 178 0
22 MCS J1752.0+4440 ClG 17 52 02.2 +44 40 38           ~ 59 0
23 ZwCl 1856+6616 ClG 18 56 38.4 +66 23 10           ~ 36 0
24 ACO 3667 ClG 20 12 33.68 -56 50 26.3           ~ 629 1
25 ACO 3685 ClG 20 32 19.2 -56 27 21           ~ 33 0
26 ACO 2345 ClG 21 27 05.391 -12 09 07.41           ~ 131 0
27 NVSS J212709-120958 Rad 21 27 09.5 -12 09 58           ~ 132 1
28 NAME Sausage Cluster ClG 22 42 53.0 +53 01 05           ~ 206 0
29 PSZ1 G108.18-11.53 ClG 23 22 28.2499 +48 44 29.172           ~ 29 0
30 NAME Saraswati supercluster SCG 23 37 40.7 +00 16 35           ~ 11 0
31 ZwCl 2341+0000 ClG 23 43 40.566 +00 18 18.94           ~ 71 0
32 RXC J2351.0-1934 ClG 23 51.0 -19 34           ~ 1 0

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