2000A&A...362..809B


Query : 2000A&A...362..809B

2000A&A...362..809B - Astronomy and Astrophysics, volume 362, 809-824 (2000/10-3)

A new local temperature distribution function for X-ray clusters: cosmological applications.

BLANCHARD A., SADAT R., BARTLETT J.G. and LE DOUR M.

Abstract (from CDS):

We present a new determination of the local temperature function of X-ray clusters using a sample of X-ray clusters with fluxes above 2.2x10–11erg/s/cm2 in the [0.1-2.4] keV band, most of these clusters come from the Abell XBAC's sample to which a handful of known non-Abell clusters has been added. We estimate this sample to be 85% complete, and should therefore provide a useful estimation of the present-day number density of clusters. Comprising fifty clusters for which the temperature information is available, it is the largest complete sample of this kind. It is therefore expected to significantly improve the estimation of the temperature distribution function of clusters. We find that the resulting temperature function is higher than previous estimations, but it agrees with the temperature distribution function inferred from the BCS and RASS luminosity function (Ebeling et al., 1997ApJ...479L.101E; De Grandi et al., 1999ApJ...513L..17D). We have used this sample to constrain the amplitude of the matter fluctuations σc on cluster's scale of 8sqrt([3])Ω0–1h–1Mpc, assuming a mass-temperature relation based on recent numerical simulations. We find σc∼0.6±0.02 for an Ω0=1 model (for which σc8). Our sample provides a useful reference at z∼0 to use in the application of the cosmological test based on the evolution of X-ray clusters abundance (Oukbir & Blanchard, 1992A&A...262L..21O, 1997A&A...317....1O). We have therefore estimated the temperature distribution function at z=0.33 using Henry's sample of high-z X-ray clusters (Henry, 1997ApJ...489L...1H; hereafter H97) and performed a preliminary estimate of Ω0. We find that the abundance of clusters at z=0.33 is significantly smaller, by a factor larger than 2, which shows that the EMSS sample provides strong evidence for evolution of the cluster abundance. A likelihood analysis leads to a rather high value of the mean density parameter of the universe: Ω0=0.92+0.255–0.215 (1σ) for open universes and Ω0=0.865+0.35–0.245 for flat universes, which is consistent with a previous independent estimation based on the full EMSS sample by Sadat et al. (1998A&A...329...21S). Some systematic uncertainties which could alter this result are briefly discussed.

Abstract Copyright:

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

CDS comments: p. 812: RX J0419 incomplete format, not identified

Simbad objects: 54

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Number of rows : 54
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 85 ClG 00 41 37.8 -09 20 33           ~ 841 0
2 ACO 119 ClG 00 56 16.8 -01 15 00           ~ 535 2
3 ACO 133 ClG 01 02 39.0 -21 57 15           ~ 350 1
4 ACO 262 ClG 01 52 50.4 +36 08 46           ~ 677 1
5 ACO 399 ClG 02 57 56.4 +13 00 59           ~ 369 0
6 ACO 401 ClG 02 58 56.9 +13 34 56           ~ 538 0
7 ACO 3112 ClG 03 17 52.4 -44 14 35           ~ 297 1
8 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 357 1
9 ACO 3158 ClG 03 42 39.6 -53 37 50           ~ 280 0
10 ACO 478 ClG 04 13 20.7 +10 28 35           ~ 482 0
11 NGC 1550 BiC 04 19 37.9450450152 +02 24 35.918168940   14.0       ~ 165 1
12 RBS 533 GrG 04 19 38.2 +02 25 12           ~ 40 1
13 ClG 0422-09 ClG 04 25 51.02 -08 33 38.5           ~ 89 0
14 ACO 3266 ClG 04 31 11.9 -61 24 23           ~ 383 0
15 ACO 496 ClG 04 33 30.3838 -13 14 21.584           ~ 670 2
16 ACO 3376 ClG 06 01 25.000 -39 59 51.00           ~ 284 0
17 ACO 3391 ClG 06 26 15.4 -53 40 52           ~ 182 1
18 ACO 3395 ClG 06 27 31.1 -54 23 58           ~ 190 0
19 ACO 576 ClG 07 21 24.1 +55 44 20           ~ 287 1
20 ACO 754 ClG 09 08 50.1 -09 38 12           ~ 643 1
21 ACO 780 ClG 09 18 30 -12 15.7           ~ 443 0
22 NAME Hydra I Cluster ClG 10 36 36.0 -27 31 04           ~ 805 1
23 ACO 1367 ClG 11 44 44.6 +19 41 59           ~ 1038 1
24 [YSS2008] 13 ClG 12 17 41.13 +03 39 20.9           ~ 18 0
25 NAME Virgo Cluster ClG 12 26 32.1 +12 43 24           ~ 6265 0
26 ACO 3526 ClG 12 48 51.8 -41 18 21           ~ 1018 2
27 ACO 1644 ClG 12 57 11.6 -17 24 34           ~ 343 1
28 ACO 1650 ClG 12 58 36.76 -01 43 34.2           ~ 279 0
29 ACO 1651 ClG 12 59 22.43 -04 11 47.1           ~ 277 0
30 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4514 2
31 ACO 1736 ClG 13 26 52.1 -27 06 33           ~ 239 2
32 ACO 3558 ClG 13 27 54.8 -31 29 32           ~ 419 2
33 ACO 3562 ClG 13 33 31.8 -31 40 23           ~ 294 1
34 ACO 3571 ClG 13 47 28.9 -32 51 57           ~ 269 2
35 ACO 1795 ClG 13 49 00.5 +26 35 07           ~ 1202 0
36 ACO 3581 ClG 14 07 29.8 -27 01 04           ~ 174 3
37 ACO 2029 ClG 15 10 58.7 +05 45 42           ~ 892 0
38 ACO 2052 ClG 15 16 45.5 +07 00 01           ~ 702 1
39 NAME NGC 5920 Group ClG 15 21 50.7 +07 42 18     15.13     ~ 295 0
40 ACO 2065 ClG 15 22 42.6 +27 43 21           ~ 352 0
41 ACO 2063 ClG 15 23 01.8 +08 38 22           ~ 379 2
42 ACO 2142 ClG 15 58 20.00 +27 14 00.3           ~ 713 0
43 ACO 2147 ClG 16 02 17.2 +15 53 43           ~ 388 0
44 ACO 2199 ClG 16 28 37.0 +39 31 28           ~ 1129 1
45 ACO 2244 ClG 17 02 34.01 +34 04 41.1           ~ 256 0
46 ACO 2256 ClG 17 03 43.5 +78 43 03           ~ 854 1
47 ACO 3667 ClG 20 12 33.68 -56 50 26.3           ~ 590 1
48 ZW II 108 BiC 21 13 55.918 +02 33 55.39   15.1       ~ 53 1
49 ACO 2589 ClG 23 24 00.5 +16 49 29           ~ 304 1
50 ACO 2597 ClG 23 25 19.70 -12 07 27.7           ~ 517 0
51 ACO 2634 ClG 23 38 18.4 +27 01 37           ~ 491 2
52 ACO 2657 ClG 23 44 51.0 +09 08 40           ~ 264 3
53 ACO 4038 ClG 23 47 31.1 -28 12 10           ~ 326 3
54 ACO 4059 ClG 23 56 40.7 -34 40 18           ~ 367 1

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2022.06.25-01:27:43

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