2004ApJ...609..603H

Query : 2004ApJ...609..603H

2004ApJ...609..603H - Astrophys. J., 609, 603-616 (2004/July-2)

X-ray temperatures for the extended medium-sensitivity survey high-redshift cluster sample: constraints on cosmology and the dark energy equation of state.

HENRY J.P.

Abstract (from CDS):

We measure the X-ray temperature (and luminosity) with ASCA of all but one cluster in the Einstein Extended Medium-Sensitivity Survey (EMSS) high-redshift (z≥0.3) sample. We compare these data to a complete sample of low-redshift clusters that also has temperature measurements, thereby providing cosmological constraints. Improvements over our previous work include (1) an enlarged high-redshift sample; (2) temperatures for the low-redshift comparison sample that come from the same instrument as the high-redshift sample; (3) the elimination of three EMSS clusters with the same redshift as the target (i.e., not truly serendipitous) and a fourth with an ASCA flux well below the completeness limit; (4) using a theoretical cluster mass function that more closely matches N-body simulations (the Sheth-Torman function); (5) using a cold dark matter power spectrum instead of a power law; (6) using a general cosmology with arbitrary matter density and cosmological constant; (7) using a cosmology that generalizes the cosmological constant to quintessence; (8) including the effects of temperature measurement errors and scatter in the cluster luminosity-temperature relation; and (9) marginalizing over the poorly known normalization of the mass-temperature relation. We find an allowed band in the Ωm0-ΩΛ0plane of different orientation to the band of constraints provided by the supernovae Ia Hubble diagram and the cosmic microwave background fluctuations. All three bands intersect at the same place: Ωm0~0.3, ΩΛ0~0.7. We measure the quintessence equation-of-state parameter to be w=-(0.42±0.21) (68% confidence for one interesting parameter), consistent with previously determined upper limits. We measure the normalization of the mass fluctuation power spectrum to be σ8=0.66±0.16 (68% confidence for three interesting parameters). Systematic errors are larger than the statistical errors only for σ8with our sample; thus the errors for it depend on the details of the marginalization over the temperature-mass normalization.

Abstract Copyright: ∼

Journal keyword(s): Cosmology: Cosmological Parameters - Cosmology: Observations - Galaxies: Clusters: General - Cosmology: Large-Scale Structure of Universe - X-Rays: Galaxies

Errata: erratum vol. 732, art. 130 (2011)

Simbad objects: 53

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Number of rows : 53
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 ClG 0014+15 ClG 00 14 41 +15 37.3           ~ 2 0
2 ClG 0016+16 ClG 00 18 33.3 +16 26 36           ~ 502 0
3 ACO 85 ClG 00 41 36.21 -09 19 30.4           ~ 909 0
4 ACO 119 ClG 00 56 08.57 -01 12 00.8           ~ 555 2
5 ClG 0147.8-3941 ClG 01 50 00.9 -39 27 00     19.2     ~ 11 0
6 ACO 399 ClG 02 57 56.4 +13 00 59           ~ 396 0
7 ACO 401 ClG 02 58 56.9 +13 34 56           ~ 566 0
8 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 7066 0
9 ClG 0302+17 ClG 03 05 19.0 +17 28 38     21.00     ~ 56 0
10 ClG 0303+1658 ClG 03 05 31.6 +17 10 02     20.13     ~ 90 0
11 ClG 0303+17 ClG 03 06 19.0 +17 18 50           ~ 49 0
12 ZwCl 0335+0956 ClG 03 38 35.3 +09 57 54           ~ 383 1
13 ACO S 400 ClG 03 55 33.29 -36 34 18.5           ~ 38 0
14 ACO 478 ClG 04 13 20.7 +10 28 35           ~ 502 0
15 ClG 0418.3-3844 ClG 04 20 06.2 -38 37 34     18.3     ~ 18 0
16 ACO 3266 ClG 04 31 11.9 -61 24 23           ~ 410 0
17 ACO 496 ClG 04 33 38.8 -13 15 59           ~ 694 2
18 ClG 0451-03 ClG 04 54 10.9 -03 01 07     20.0     ~ 352 0
19 ClG 0811+63 ClG 08 16 04.0 +62 52 19     18.5     ~ 23 0
20 ClG 0821+03 ClG 08 24 05.0 +03 26 18     19.0     ~ 15 0
21 ACO 754 ClG 09 09 08.4 -09 39 58           ~ 666 1
22 ClG 1008-12 ClG 10 10 34.1 -12 39 48     18.0     ~ 152 0
23 NAME Hydra I Cluster ClG 10 36 36.0 -27 31 04           ~ 840 1
24 ClG 1054-03 ClG 10 57 00.2 -03 37 27     22     ~ 454 0
25 ClG 1137+66 ClG 11 40 23.0 +66 08 16     21.0     ~ 138 0
26 ACO 1367 ClG 11 44 44.6 +19 41 59           ~ 1076 1
27 ClG 1147.3+1103 ClG 11 49 52.6 +10 46 37     19.0     ~ 28 0
28 ClG 1208+39 ClG 12 11 16.0 +39 11 41     19.8     ~ 37 0
29 SDSS J121134.20+390053.5 BLL 12 11 34.20672 +39 00 53.5644     20.0 20.4   ~ 34 0
30 NAME Virgo Cluster ClG 12 26 32.1 +12 43 24           ~ 6645 0
31 ClG 1224+20 ClG 12 27 14.9 +19 51 06   19.0       ~ 95 0
32 ClG 1241+17 ClG 12 44 02.6 +16 54 11     19.0     ~ 40 0
33 ACO 3526 ClG 12 48 51.8 -41 18 21           ~ 1068 2
34 ACO 1651 ClG 12 59 22.43 -04 11 47.1           ~ 290 0
35 ACO 1656 ClG 12 59 44.40 +27 54 44.9           ~ 4803 2
36 ACO 3558 ClG 13 27 54.8 -31 29 32           ~ 442 2
37 ACO 3562 ClG 13 33 31.8 -31 40 23           ~ 314 1
38 2E 3105 ClG 13 35 48.7 +17 09 53     19.9     ~ 20 0
39 ACO 3571 ClG 13 47 28.9 -32 51 57           ~ 284 2
40 ACO 1795 ClG 13 48 50.48 +26 35 07.4           ~ 1267 0
41 ZwCl 1358+6245 ClG 13 59 54.3 +62 30 36     18.5     ~ 361 0
42 ClG 1426.4+0158 ClG 14 28 58.9 +01 43 59     19.0     ~ 32 0
43 ACO 2029 ClG 15 10 56.2 +05 44 42           ~ 943 0
44 ClG J1514+3636 ClG 15 14 22.0 +36 36 22     19.0     ~ 136 0
45 ClG 1532+01 ClG 15 35 02.7 +01 20 58     19.0     ~ 17 0
46 ACO 2142 ClG 15 58 14.38 +27 12 57.8           ~ 768 0
47 ACO 2147 ClG 16 02 11.96 +15 55 11.5           ~ 403 0
48 ClG 1621+26 ClG 16 23 35.7 +26 33 50           ~ 142 0
49 ACO 2199 ClG 16 28 43.31 +39 34 07.6           ~ 1171 1
50 ACO 2256 ClG 17 03 09.4 +78 39 36           ~ 885 1
51 ACO 3667 ClG 20 12 33.68 -56 50 26.3           ~ 627 1
52 ClG 2053-04 ClG 20 56 21.2 -04 37 46   21.0       ~ 165 0
53 ClG 2137-2353 ClG 21 40 12.8 -23 39 27     18.5     ~ 378 0

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