2012A&A...548A..59C


Query : 2012A&A...548A..59C

2012A&A...548A..59C - Astronomy and Astrophysics, volume 548A, 59-59 (2012/12-1)

Statistics and implications of substructure detected in a representative sample of X-ray clusters.

CHON G., BOEHRINGER H. and SMITH G.P.

Abstract (from CDS):

We present a morphological study of 35 X-ray luminous galaxy clusters at 0.15<z<0.3, selected in a similar manner to the Local Cluster Substructure Survey (LoCuSS), for which deep XMM-Newton observations are available. We characterise the structure of the X-ray surface brightness distribution of each cluster by measuring both their power ratios and centroid shift, and thus rank the clusters by the degree of substructure. These complementary probes give a consistent description of the cluster morphologies with some well understood exceptions. We find a remarkably tight correlation of regular morphology with the occurrence of cool cores in clusters. We also compare our measurements of X-ray morphology with measurements of the luminosity gap statistics and ellipticity of the brightest cluster galaxy (BCG), to examine recent suggestions that these quantities may be efficient probes of the assembly history of and observer's viewing angle through cluster-scale mass distributions. Our X-ray analysis confirms that cluster with large luminosity gaps form a relatively homogeneous population that appears more regular with the implication that such systems did not suffer from recent merger activity. Similarly, we find a clear correlation between the ellipticity of the BCGs and the shape of the cluster. In particular nearly circular BCGs (epsilon<0.2) are found in undisturbed systems with regular X-ray morphologies. For these systems it has been suggested that they are intrinsically prolate and viewed along the line of sight close to the major axis. Finally, we check how our new X-ray morphological analysis maps onto cluster scaling relations, finding that (i) clusters with relatively undisturbed X-ray morphologies are on average more luminous at fixed X-ray temperature than those with disturbed morphologies, and (ii) disturbed clusters have larger X-ray masses than regular clusters for a given temperature in the MX-T relation. We also show that the scatter in the ratio of X-ray and weak lensing based cluster mass measurements is larger for disturbed clusters than for those of more regular morphology. Overall, our results demonstrate the feasibility of assembling a self-consistent picture of the physical structure of clusters from X-ray and optical data, and the potential to apply this in the measurement of cosmological cluster scaling relations.

Abstract Copyright:

Journal keyword(s): X-rays: galaxies: clusters - galaxies: clusters: general - cosmology: observations

Simbad objects: 39

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Number of rows : 39
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 ACO 68 ClG 00 37 06.2 +09 09 33           ~ 177 0
2 ACO 2813 ClG 00 43 27.8821 -20 37 01.282           ~ 84 0
3 ACO 115 ClG 00 55 59.5 +26 19 14           ~ 253 1
4 ACO 209 ClG 01 31 57.5 -13 34 35           ~ 278 0
5 ACO 267 ClG 01 52 42.10 +01 00 29.4           ~ 217 0
6 2MAXI J0231-440 ClG 02 32 18.69 -44 20 41.5           ~ 93 0
7 ACO 383 ClG 02 48 03.30 -03 31 43.4           ~ 337 0
8 ACO 3088 ClG 03 07 02.12 -28 39 57.3           ~ 65 0
9 ACO S 520 ClG 05 16 37.40 -54 30 01.5           ~ 84 0
10 ACT-CL J0528.8-3927 ClG 05 28 56.2 -39 27 49           ~ 58 0
11 MCXC J0532.9-3701 ClG 05 32 56.4 -37 01 34           ~ 40 0
12 ACO 3364 ClG 05 47 36.1753 -31 52 22.695           ~ 66 0
13 ACO 3404 ClG 06 45 29.50 -54 13 37.0           ~ 85 0
14 ClG 0657-56 ClG 06 58 29.6 -55 56 39           ~ 889 1
15 ACO 773 ClG 09 17 51.3 +51 43 20           ~ 279 0
16 ACO 781 ClG 09 20 25.4 +30 30 07           ~ 137 0
17 ACO 868 ClG 09 45 28.1 -08 38 51           ~ 56 0
18 ACO 901 ClG 09 55 56.9256 -10 01 46.519           ~ 106 1
19 ACO 902 ClG 09 56 33.600 -10 09 13.10           ~ 60 1
20 ACO 907 ClG 09 58 21.84 -11 03 47.5           ~ 123 0
21 ACO 963 ClG 10 17 09.6 +39 01 00           ~ 375 0
22 ACO 1413 ClG 11 55 18.0 +23 24 19           ~ 406 0
23 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4571 2
24 ACO 1689 ClG 13 11 29.5 -01 20 28           ~ 1083 0
25 ACO 1758 ClG 13 32 32.1 +50 30 37           ~ 241 2
26 ACO 1763 ClG 13 35 20.1 +41 00 04           ~ 291 0
27 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 662 1
28 ACO 1914 ClG 14 26 01.3 +37 49 36           ~ 295 0
29 ZwCl 1455+2232 ClG 14 57 15.2 +22 20 30     18.62 20.04   ~ 278 0
30 ACO 2204 ClG 16 32 45.7 +05 34 43           ~ 418 0
31 ACO 2218 ClG 16 35 54.0 +66 13 00           ~ 793 1
32 ACO 2261 ClG 17 22 28.3 +32 09 13           ~ 324 0
33 ClG J2129+0005 ClG 21 29 40.5 +00 05 47           ~ 245 0
34 ACO 2390 ClG 21 53 34.6 +17 40 11           ~ 659 2
35 ACO 3856 ClG 22 18 45.2 -38 53 57           ~ 73 2
36 ACO 3888 ClG 22 34 23.0 -37 43 29           ~ 131 1
37 ACO 2537 ClG 23 08 22.3 -02 11 29           ~ 126 0
38 ACO 2631 ClG 23 37 40.7 +00 16 35           ~ 156 0
39 ACO 2667 ClG 23 51 39.37 -26 05 02.7           ~ 164 0

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2022.11.28-13:12:21

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