2008A&A...482..451Z


Query : 2008A&A...482..451Z

2008A&A...482..451Z - Astronomy and Astrophysics, volume 482, 451-472 (2008/5-1)

LoCuSS: comparison of observed X-ray and lensing galaxy cluster scaling relations with simulations.

ZHANG Y.-Y., FINOGUENOV A., BOEHRINGER H., KNEIB J.-P., SMITH G.P., KNEISSL R., OKABE N. and DAHLE H.

Abstract (from CDS):

The Local Cluster Substructure Survey (LoCuSS, Smith et al., in prep.) is a systematic multi-wavelength survey of more than 100 X-ray luminous galaxy clusters in the redshift range 0.14-0.3 selected from the ROSAT All Sky Survey. We used data on 37 LoCuSS clusters from the XMM-Newton archive to investigate the global scaling relations of galaxy clusters. The scaling relations based solely on the X-ray data (S-T, S-YX, P-YX, M-T, M-YX, M-Mgas, Mgas-T, L-T, L-YX, and L-M) obey empirical self-similarity and reveal no additional evolution beyond the large-scale structure growth. They also reveal up to 17 per cent segregation between all 37 clusters and non-cool core clusters. Weak lensing mass measurements are also available in the literature for 19 of the clusters with XMM-Newton data. The average of the weak lensing mass to X-ray based mass ratio is 1.09±0.08, setting the limit of the non-thermal pressure support to 9 ±8 per cent. The mean of the weak lensing mass to X-ray based mass ratio of these clusters is ∼1, indicating good agreement between X-ray and weak lensing masses for most clusters, although with 31-51 per cent scatter. The scatter in the mass-observable relations (M-YX, M-Mgas, and M-T) is smaller using X-ray based masses than using weak lensing masses by a factor of 2. With the scaled radius defined by the YX profile - r500^ YX,X^, r500^Y_ X_,wl^, and r500YX_,si^, we obtain lower scatter in the weak lensing mass based mass-observable relations, which means the origin of the scatter is Mwl and M^ X^ instead of YX. The normalization of the M-Y_ X_ relation using X-ray mass estimates is lower than the one from simulations by up to 18-24 per cent at 3σ significance. This agrees with the M-YX relation based on weak lensing masses, the normalization of the latter being ∼20 per cent lower than the one from simulations at ∼2σ significance. This difference between observations and simulations is also indicated in the M-Mgas and M-T relations. Despite the large scatter in the comparison of X-ray to lensing, the agreement between these two completely independent observational methods is an important step towards controlling astrophysical and measurement systematics in cosmological scaling relations.

Abstract Copyright:

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

Errata: + corrigendum vol. 527, C3 (2011)

CDS comments: Tables in Appendix: RXC J0645.4-5413 is probably 1RXS J064529.1-541338 in Simbad, RXC J0958.3-1103 is 1RXS J095821.8-110344.

Simbad objects: 37

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Number of rows : 37
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 ACO 68 ClG 00 37 06.2 +09 09 33           ~ 172 0
2 ACO 2813 ClG 00 43 27.8821 -20 37 01.282           ~ 81 0
3 ACO 115 ClG 00 55 59.5 +26 19 14           ~ 249 1
4 ACO 209 ClG 01 31 57.5 -13 34 35           ~ 271 0
5 ACO 267 ClG 01 52 41 +01 00.4           ~ 213 0
6 2MAXI J0231-440 ClG 02 32 18.69 -44 20 41.5           ~ 89 0
7 ACO 383 ClG 02 48 06.9 -03 29 32           ~ 323 0
8 ACO 3088 ClG 03 07 02.12 -28 39 57.3           ~ 64 0
9 ACO S 520 ClG 05 16 37.40 -54 30 01.5           ~ 81 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           ~ 39 0
12 ACO 3364 ClG 05 47 36.1753 -31 52 22.695           ~ 65 0
13 ACO 3404 ClG 06 45 29.50 -54 13 37.0           ~ 82 0
14 ClG 0657-56 ClG 06 58 29.6 -55 56 39           ~ 867 1
15 ACO 773 ClG 09 17 51.3 +51 43 20           ~ 272 0
16 ACO 781 ClG 09 20 25.4 +30 30 07           ~ 134 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           ~ 105 1
19 ACO 907 ClG 09 58 21.84 -11 03 47.5           ~ 122 0
20 ACO 963 ClG 10 17 09.6 +39 01 00           ~ 370 0
21 ACO 1413 ClG 11 55 18.0 +23 24 19           ~ 399 0
22 ACO 1689 ClG 13 11 29.5 -01 20 28           ~ 1067 0
23 ACO 1758 ClG 13 32 32.1 +50 30 37           ~ 233 2
24 ACO 1763 ClG 13 35 20.1 +41 00 04           ~ 282 0
25 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 655 1
26 ACO 1914 ClG 14 26 01.3 +37 49 36           ~ 288 0
27 ZwCl 1455+2232 ClG 14 57 15.2 +22 20 30     18.62     ~ 274 0
28 ACO 2204 ClG 16 32 45.7 +05 34 43           ~ 414 0
29 ACO 2218 ClG 16 35 54.0 +66 13 00           ~ 789 1
30 ACO 2261 ClG 17 22 28.3 +32 09 13           ~ 311 0
31 ClG J2129+0005 ClG 21 29 40.5 +00 05 47           ~ 237 0
32 ACO 2390 ClG 21 53 34.6 +17 40 11           ~ 651 2
33 ACO 3856 ClG 22 18 45.2 -38 53 57           ~ 72 2
34 ACO 3888 ClG 22 34 23.0 -37 43 29           ~ 130 1
35 ACO 2537 ClG 23 08 22.3 -02 11 29           ~ 121 0
36 ACO 2631 ClG 23 37 40.7 +00 16 35           ~ 150 0
37 ACO 2667 ClG 23 51 39.37 -26 05 02.7           ~ 161 0

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2022.05.22-03:09:39

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