2010A&A...524A..68E


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.05CET18:39:11

2010A&A...524A..68E - Astronomy and Astrophysics, volume 524, A68-68 (2010/12-1)

Mass profiles and c-MDM relation in X-ray luminous galaxy clusters.

ETTORI S., GASTALDELLO F., LECCARDI A., MOLENDI S., ROSSETTI M., BUOTE D. and MENEGHETTI M.

Abstract (from CDS):

Galaxy clusters represent valuable cosmological probes using tests that mainly rely on measurements of cluster masses and baryon fractions. X-ray observations represent one of the main tools for uncovering these quantities. We aim to constrain the cosmological parameters Ωm and σ8 using the observed distribution of the both values of the concentrations and dark mass within R200 and of the gas mass fraction within R500. We applied two different techniques to recover the profiles the gas and dark mass, described according to the Navarro, Frenk & White (1997ApJ...490..493N) functional form, of a sample of 44 X-ray luminous galaxy clusters observed with XMM-Newton in the redshift range 0.1-0.3. We made use of the spatially resolved spectroscopic data and of the PSF-deconvolved surface brightness and assumed that hydrostatic equilibrium holds between the intracluster medium and the gravitational potential. We evaluated several systematic uncertainties that affect our reconstruction of the X-ray masses. We measured the concentration c200, the dark mass M200 and the gas mass fraction in all the objects of our sample, providing the largest dataset of mass parameters for galaxy clusters in the redshift range 0.1-0.3. We confirm that a tight correlation between c200 and M200 is present and in good agreement with the predictions from numerical simulations and previous observations. When we consider a subsample of relaxed clusters that host a low entropy core, we measure a flatter c-M relation with a total scatter that is lower by 40 per cent. We conclude, however, that the slope of the c-M relation cannot be reliably determined from the fitting over a narrow mass range as the one considered in the present work. From the distribution of the estimates of c200 and M200, with associated statistical (15-25%) and systematic (5-15%) errors, we used the predicted values from semi-analytic prescriptions calibrated through N-body numerical runs and obtain σ8m0.60±0.03=0.45±0.01 (at 2 σ level, statistical only) for the subsample of the clusters where the mass reconstruction has been obtained more robustly and σ8m0.56±0.04=0.39±0.02 for the subsample of the 11 more relaxed LEC objects. With the further constraint from the gas mass fraction distribution in our sample, we break the degeneracy in the σ8m plane and obtain the best-fit values σ8≃1.0±0.2 (0.83±0.1 when the subsample of the more relaxed objects is considered) and Ωm=0.26±0.02. Analysis of the distribution of the c200-M200-fgas values represents a mature and competitive technique in the present era of precision cosmology, even though it needs more detailed analysis of the output of larger sets of cosmological numerical simulations to provide definitive and robust results.

Abstract Copyright:

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

Errata: corrigendum vol. 526, p. C1 (2011)

Simbad objects: 44

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Number of rows : 44

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 ACO 2700 ClG 00 03 49.7 +02 03 59           ~ 80 0
2 ACO 22 ClG 00 20 34.8 -25 41 51           ~ 96 0
3 ACO 68 ClG 00 37 06.2 +09 09 33           ~ 164 0
4 ACO 2813 ClG 00 43 27.8821 -20 37 01.282           ~ 72 0
5 ACO S 84 ClG 00 49 23.2 -29 31 33           ~ 78 0
6 ACO 209 ClG 01 31 57.5 -13 34 35           ~ 254 0
7 2MAXI J0231-440 ClG 02 32 18.69 -44 20 41.5           ~ 83 0
8 ACO 383 ClG 02 48 06.9 -03 29 32           ~ 309 0
9 RXC J0303.8-7752 ClG 03 03 00.0 -77 52 00           ~ 10 0
10 ACO 3088 ClG 03 07 02.12 -28 39 57.3           ~ 60 0
11 ACO S 520 ClG 05 16 37.40 -54 30 01.5           ~ 78 0
12 RXC J0532.9-3701 ClG 05 32 56.4 -37 01 34           ~ 38 0
13 ACO 3364 ClG 05 47 36.1753 -31 52 22.695           ~ 64 0
14 ACO 3378 ClG 06 05 52.6923 -35 18 32.801           ~ 73 1
15 ACO 3404 ClG 06 45 29.50 -54 13 37.0           ~ 78 0
16 ACO 773 ClG 09 17 51.3 +51 43 20           ~ 263 0
17 ACO 907 ClG 09 58 21.84 -11 03 47.5           ~ 117 0
18 ACO 963 ClG 10 17 09.6 +39 01 00           ~ 358 0
19 ZwCl 1021+0426 ClG 10 23 39.0 +04 11 14   15.6       ~ 258 0
20 ACO 1068 ClG 10 40 47.1 +39 57 19           ~ 190 0
21 ACO 1084 ClG 10 44 37.1 -07 04 47           ~ 69 0
22 ACO 1300 ClG 11 32 00.7 -19 53 34           ~ 133 0
23 ACO 1348 ClG 11 41 24.0 -12 16 00           ~ 61 0
24 ACO 1413 ClG 11 55 18.0 +23 24 19           ~ 387 0
25 ACO 1689 ClG 13 11 29.5 -01 20 28           ~ 1037 0
26 ACO 1763 ClG 13 35 20.1 +41 00 04           ~ 265 0
27 ACO 1835 ClG 14 01 02.07 +02 52 43.2           ~ 636 1
28 ZwCl 1455+2232 ClG 14 57 15.2 +22 20 30     18.62     ~ 272 0
29 ACO 2034 ClG 15 10 10.80 +33 30 21.6           ~ 179 1
30 ACO 2050 ClG 15 16 21.6 +00 05 59           ~ 91 0
31 ACO 2051 ClG 15 16 53.8 -01 05 06           ~ 47 0
32 ACO 2204 ClG 16 32 45.7 +05 34 43           ~ 404 0
33 ACO 2218 ClG 16 35 54.0 +66 13 00           ~ 782 1
34 2MAXI J2014-244 ClG 20 14 49.7 -24 30 30           ~ 59 0
35 ACO 2328 ClG 20 48 13.9 -17 48 53           ~ 67 0
36 ClG J2129+0005 ClG 21 29 40.5 +00 05 47           ~ 224 0
37 ACO 3814 ClG 21 49 07.24 -30 42 06.4           ~ 51 0
38 ACO 2390 ClG 21 53 34.6 +17 40 11           ~ 633 2
39 ACO 3827 ClG 22 01 49.1 -59 57 15           ~ 139 0
40 ACO 3856 ClG 22 18 45.2 -38 53 57           ~ 71 2
41 ACO 3888 ClG 22 34 23.0 -37 43 29           ~ 127 1
42 ACO 3911 ClG 22 46 10.9 -52 41 21           ~ 56 0
43 ACO 2631 ClG 23 37 40.7 +00 16 35           ~ 140 0
44 ACO 2667 ClG 23 51 39.37 -26 05 02.7           ~ 153 0

    Equat.    Gal    SGal    Ecl

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2021.03.05-18:39:12

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