2016A&A...593A..81C


C.D.S. - SIMBAD4 rel 1.7 - 2020.05.27CEST08:37:47

2016A&A...593A..81C - Astronomy and Astrophysics, volume 593A, 81-81 (2016/9-1)

Can giant radio halos probe the merging rate of galaxy clusters?

CASSANO R., BRUNETTI G., GIOCOLI C. and ETTORI S.

Abstract (from CDS):

Observations of galaxy clusters both in the radio and X-ray bands probe a direct link between cluster mergers and giant radio halos, suggesting that these sources can be used as probes of the cluster merging rate with cosmic time. While all giant radio halos are found in merging clusters, not every merging cluster hosts a giant radio halo. In this paper we carry out an explorative study that combines the observed fractions of merging clusters and radio halos with the merging rate predicted by cosmological simulations, and we attempt to infer constraints on merger properties of clusters that appear disturbed in X-rays and clusters that host radio halos. We used classical morphological parameters to identify merging systems and analysed the largest current (mass-selected M500≥6x1014M and 0.2≥z≥0.33) sample of galaxy clusters with radio and X-ray data; we extracted this sample from the Planck Sunyaev-Zeldovich cluster catalogue. We found that the fraction of merging clusters in this sample is f_m∼62-67%, while that of clusters with radio halos is fRH∼44-51%. We assume that the morphological disturbance measured in the X-rays is driven by the merger with the largest mass ratio, ξ (ξ=Mi/M1<1, where Mi and M1 are the progenitor masses), which is still ongoing in the cluster at the epoch of observation.
Result. from theoretical studies allow us to derive the fraction of mergers with mass ratio above a minimum threshold (those with ξ≳ξmin) in our sample, under the assumption of a timescale τm for the duration of merger-induced disturbance. The comparison of the theoretical merger fraction with the observed merger fraction allows us to constrain a region in the (ξmin, τm) plane. We find that under the assumption of τm∼2-3Gy, as constrained by simulations, the observed merger fraction matches the theoretical value for ξmin∼0.1-0.18. This is consistent with optical and near-infrared (IR) observations of galaxy clusters in the sample that constrain ξmin~=0.14-0.16 through weak lensing analysis or study of the velocity distribution of galaxies in the clusters. The fact that radio halos are only found in a fraction of merging galaxy clusters may suggest that merger events generating radio halos are characterized by larger mass ratios; this seems to be supported by optical/near-IR observations of radio halo clusters in the sample that indeed allow us to constrain ξmin∼0.2-0.25. Alternatively, radio halos may be generated in all mergers but their lifetime is shorter (by ∼fRH/fm) than the timescale of the merger-induced disturbance. We stress that this is an explorative study, however it suggests that follow-up studies using the forthcoming radio surveys and adequate numerical simulations have the potential to derive quantitative constraints on the link between cluster merging rate and radio halos at different cosmic epochs and for different cluster masses.

Abstract Copyright: © ESO, 2016

Journal keyword(s): galaxies: clusters: intracluster medium - cosmology: theory - radio continuum: general - X-rays: galaxies: clusters

Status at CDS:  

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 - 2020
#notes
1 ACO 2697 ClG 00 03 11.5 -06 05 30           ~ 35 0
2 ACO 2744 ClG 00 14 20.03 -30 23 17.8           ~ 565 0
3 ACO 56 ClG 00 33 53.1 -07 52 10           ~ 15 0
4 ACO 68 ClG 00 37 06.2 +09 09 33           ~ 156 0
5 ACO 2813 ClG 00 43 27.8821 -20 37 01.282           ~ 70 0
6 ACO 2895 ClG 01 18 04.48 -27 00 13.4           ~ 32 0
7 ACO 209 ClG 01 31 57.5 -13 34 35           ~ 247 0
8 ACO 220 ClG 01 37 22.0270 +07 52 31.390           ~ 13 0
9 ClG J0142+2131 ClG 01 42 03.1 +21 30 39           ~ 48 1
10 ACO 3041 ClG 02 41 23.03 -28 38 48.9           ~ 18 0
11 PSZ1 G205.07-62.94 ClG 02 46 22 -20 31.6           ~ 11 0
12 ACO 384 ClG 02 48 08.3 -02 16 37           ~ 16 0
13 ACO 402 ClG 02 57 41.33 -22 09 14.4           ~ 35 0
14 ACO 3088 ClG 03 07 02.12 -28 39 57.3           ~ 60 0
15 PSZ1 G171.96-40.64 ClG 03 12 55 +08 22.8           ~ 29 0
16 ACO 521 ClG 04 54 08.6 -10 14 39           ~ 213 0
17 ACO 520 ClG 04 54 19.0 +02 56 49           ~ 379 0
18 [DBG99] 46 ClG 05 10 43.85 -08 01 13.0           ~ 20 0
19 ACO 697 ClG 08 42 57.6 +36 21 45           ~ 213 0
20 ACO 773 ClG 09 17 51.3 +51 43 20           ~ 260 0
21 ACO 781 ClG 09 20 25.4 +30 30 07           ~ 129 0
22 ACO 3444 ClG 10 23 53.1540 -27 15 07.840           ~ 63 0
23 ACO 1300 ClG 11 32 00.7 -19 53 34           ~ 132 0
24 ACO 1351 ClG 11 42 30.8 +58 32 20           ~ 66 0
25 ACO 1423 ClG 11 57 47.34 +33 42 43.5           ~ 140 0
26 ACO 1443 ClG 12 01 12.1 +23 05 57           ~ 30 0
27 ZwCl 1231+1007 ClG 12 34 21.9 +09 47 02           ~ 57 0
28 ACO 1576 ClG 12 36 59.5 +63 11 18           ~ 88 0
29 ACO 1682 ClG 13 06 49.7 +46 32 59           ~ 117 1
30 2MASX J13142209-2515456 ClG 13 14 31.5049 -25 15 56.602           ~ 86 0
31 1RXS J132249.6+313844 ClG 13 22 52.3 +31 38 45           ~ 14 0
32 ACO 1733 ClG 13 26 08.78 +02 12 25.7           ~ 6 0
33 ACO 1763 ClG 13 35 20.1 +41 00 04           ~ 259 0
34 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 620 1
35 ACO S 780 ClG 14 59 29.1 -18 10 45           ~ 62 0
36 ClG J1504-0248 ClG 15 04 07.4 -02 48 15           ~ 149 0
37 2MASX J15150305-1521537 ClG 15 14.9 -15 23           ~ 31 0
38 ACO 2163 ClG 16 15 34.1 -06 07 26           ~ 519 0
39 PSZ1 G019.12+31.23 ClG 16 36 29.80 +03 08 37.5           ~ 8 0
40 ACO 2219 ClG 16 40 22.1 +46 42 20           ~ 316 0
41 ACO 2261 ClG 17 22 28.3 +32 09 13           ~ 281 0
42 RXC J2003.5-2323 ClG 20 03 32.3 -23 23 30           ~ 53 0
43 ACT-CL J2051.1+0215 ClG 20 51 12.20 +02 15 58.3           ~ 16 0
44 ClG J2135-0102 ClG 21 35 12.1 -01 02 57           ~ 36 0
45 ACO 2355 ClG 21 35 18.70 +01 25 27.0           ~ 50 0
46 ACO 2390 ClG 21 53 34.6 +17 40 11           ~ 624 2
47 ACO 2472 ClG 22 41 58.0 +17 33 03           ~ 18 0
48 ACO 2537 ClG 23 08 22.3 -02 11 29           ~ 106 0
49 ACO 2552 ClG 23 11 33.1 +03 38 37           ~ 61 0
50 ACO 2631 ClG 23 37 40.7 +00 16 35           ~ 138 0
51 ACO 2667 ClG 23 51 39.37 -26 05 02.7           ~ 148 0

    Equat.    Gal    SGal    Ecl

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2020.05.27-08:37:47

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