2016A&A...590A.126A

Query : 2016A&A...590A.126A

2016A&A...590A.126A - Astronomy and Astrophysics, volume 590A, 126-126 (2016/6-1)

The relation between mass and concentration in X-ray galaxy clusters at high redshift.

AMODEO S., ETTORI S., CAPASSO R. and SERENO M.

Abstract (from CDS):

Context. Galaxy clusters are the most recent, gravitationally bound products of the hierarchical mass accretion over cosmological scales. How the mass is concentrated is predicted to correlate with the total mass in the halo of the cluster, wherein systems at higher mass are less concentrated at given redshift and, for any given mass, systems with lower concentration are found at higher redshifts.
Aims. Through a spatial and spectral X-ray analysis, we reconstruct the total mass profile of 47 galaxy clusters observed with Chandra in the redshift range 0.4<z<1.2, which we selected to exclude major mergers, to investigate the relation between the mass and dark matter concentration and the evolution of this relation with redshift. This sample is the largest investigated so far at z>0.4, and is well suited to providing the first constraint on the concentration-mass relation at z>0.7 from X-ray analysis.
Methods. Under the assumption that the distribution of the X-ray emitting gas is spherically symmetric and in the hydrostatic equilibrium with the underlined gravitational potential, we combine the deprojected gas density and spectral temperature profiles through the hydrostatic equilibrium equation to recover the parameters that describe a Navarro-Frenk-White total mass distribution. The comparison with results from weak-lensing analysis reveals a very good agreement both for masses and concentrations. The uncertainties are however too large to make any robust conclusion about the hydrostatic bias of these systems.
Results. The distribution of concentrations is well approximated by a log-normal function in all the mass and redshift ranges investigated. The relation is well described by the form c∝MB(1+z)C with B=-0.50±0.20, C=0.12±0.61 (at 68.3% confidence). This relation is slightly steeper than that predicted by numerical simulations (B~-0.1) and does not show any evident redshift evolution. We obtain the first constraints on the properties of the concentration-mass relation at z>0.7 from X-ray data, showing a reasonable good agreement with recent numerical predictions.

Abstract Copyright: © ESO, 2016

Journal keyword(s): galaxies: clusters: general - intergalactic medium - X-rays: galaxies - cosmology: observations - dark matter

Simbad objects: 47

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Number of rows : 47
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 PSZSPT J0000-5748 ClG 00 01 00 -57 48.5           ~ 51 0
2 ClG 0016+16 ClG 00 18 33.3 +16 26 36           ~ 502 0
3 ACT-CL J0159.8-0849 ClG 01 59 49.4 -08 50 00           ~ 84 0
4 ACT-CL J0257.1-2325 ClG 02 57 09.151 -23 26 05.83           ~ 70 0
5 ClG J0329-0212 ClG 03 29 41.6 -02 11 47           ~ 142 0
6 ClG 0451-03 ClG 04 54 10.9 -03 01 07     20.0     ~ 352 0
7 ClG J0522-3624 ClG 05 22 13.8 -36 24 49           ~ 38 0
8 ClG J0542-4100 ClG 05 42 49.9 -40 59 58           ~ 62 0
9 ACT-CL J0546-5346 ClG 05 46 35.0 -53 46 04           ~ 86 0
10 ClG J0647+7015 ClG 06 47 50.0 +70 14 55           ~ 153 0
11 ClG J0717+3745 ClG 07 17 36.50 +37 45 23.0           ~ 462 0
12 ClG J0744+3927 ClG 07 44 52.5 +39 27 30           ~ 181 0
13 ClG J0848+4453 ClG 08 48 34.800 +44 53 41.90           ~ 123 1
14 ACT-CL J0911.1+1746 ClG 09 11 11.277 +17 46 31.94           ~ 72 0
15 ClG 1054-03 ClG 10 57 00.2 -03 37 27     22     ~ 454 0
16 ClG J1113-2615 ClG 11 13 05.7 -26 15 36           ~ 35 0
17 ClG J1117+1744 ClG 11 17 30.2 +17 44 44           ~ 30 0
18 ClG J1120+4318 ClG 11 20 07.6 +43 18 07           ~ 60 0
19 ClG 1137+66 ClG 11 40 23.0 +66 08 16     21.0     ~ 138 0
20 MCS J1149.5+2223 ClG 11 49 35.8 +22 23 55           ~ 458 0
21 MCS J1206.2-0847 ClG 12 06 12.2 -08 48 02           ~ 246 0
22 ClG J1221+4918 ClG 12 21 25.0 +49 18 07           ~ 58 0
23 ClG J1226+3332 ClG 12 26 57.7 +33 32 50           ~ 215 0
24 XMMXCS J123017.1+133903.8 ClG 12 30 17.100 +13 39 03.80           ~ 4 0
25 ClG J1252-2927 ClG 12 52 54.4 -29 27 17           ~ 156 0
26 ClG J1311-0311 ClG 13 11 01.7 -03 10 38           ~ 109 0
27 ClG J1347-1145 ClG 13 47 30.5 -11 45 07           ~ 547 0
28 ClG J1350+6007 ClG 13 50 48.55 +60 07 06.7           ~ 44 0
29 ClG J1415+3611 ClG 14 15 11.1 +36 12 03           ~ 78 1
30 LCDCS 0954 ClG 14 20 29.7 -11 34 04           ~ 5 0
31 ClG J1423+2404 ClG 14 23 47.7 +24 04 40           ~ 208 0
32 ClG J1524+0957 ClG 15 24 40.3 +09 57 35           ~ 60 0
33 ClG J1621+3810 ClG 16 21 25.5 +38 09 43           ~ 79 0
34 ClG 1621+26 ClG 16 23 35.7 +26 33 50           ~ 142 0
35 ClG J1701+6414 ClG 17 01 22.6 +64 14 09           ~ 72 0
36 ClG J1716+6708 ClG 17 16 49.6 +67 08 30           ~ 134 0
37 SPT-CL J2043-5035 ClG 20 43 17.60 -50 35 32.0           ~ 40 0
38 ClG 2053-04 ClG 20 56 21.2 -04 37 46   21.0       ~ 165 0
39 ACT-CL J2106.0-5844 ClG 21 06 04.3 -58 44 32           ~ 90 0
40 ClG J2129-0741 ClG 21 29 26.0 -07 41 28           ~ 171 0
41 ACT-CL J2214.9-1359 ClG 22 14 57.3 -14 00 12           ~ 88 0
42 BAX 337.1433+20.6131 ClG 22 28 32.6 +20 37 08           ~ 117 0
43 ClG J2243-0935 ClG 22 43 21.1 -09 35 43           ~ 78 0
44 ClG J2302+0844 ClG 23 02 48.1 +08 43 50           ~ 41 0
45 CDGS 50 ClG 23 18 30.670 +00 34 03.03           ~ 17 0
46 ACT-CL J2327.4-0204 ClG 23 27 27.60 -02 04 37.4           ~ 39 0
47 ACT-CL J2337.4-5942 ClG 23 37 24.2 -59 42 17           ~ 45 0

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