2009A&A...498..361P


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.07CET20:24:19

2009A&A...498..361P - Astronomy and Astrophysics, volume 498, 361-378 (2009/5-1)

Galaxy cluster X-ray luminosity scaling relations from a representative local sample (REXCESS).

PRATT G.W., CROSTON J.H., ARNAUD M. and BOEHRINGER H.

Abstract (from CDS):

We examine the X-ray luminosity scaling relations of 31 nearby galaxy clusters from the Representative XMM-Newton Cluster Structure Survey (REXCESS). The objects are selected only in X-ray luminosity, optimally sampling the cluster luminosity function. Temperatures range from 2 to 9keV, and there is no bias toward any particular morphological type. To reduce measurement scatter we extract pertinent values in an aperture corresponding to R500, estimated using the tight correlation between YX (the product of gas mass and temperature) and total mass. The data exhibit power law relations between bolometric X-ray luminosity and temperature, YX and total mass, all with slopes that are significantly steeper than self-similar expectations. We examine the possible causes for the steepening, finding that structural variations have little effect and that the primary driver appears to be a systematic variation of the gas content with mass. Scatter about the relations is dominated in all cases by the presence of cool cores. The natural logarithmic scatter about the raw X-ray luminosity-temperature relation is about 70 per cent, and about the X-ray luminosity-YX relation it is 40 percent. Systems with more morphological substructure show similar scatter about scaling relations than clusters with less substructure, due to the preponderance of cool core systems in the regular cluster subsample. Cool core and morphologically disturbed systems occupy distinct regions in the residual space with respect to the best fitting mean relation, the former lying systematically at the high luminosity side, the latter lying systematically at the low luminosity side. Simple exclusion of the central regions serves to reduce the scatter about the scaling relations by more than a factor of two. The scatter reduces by a similar amount with the use of the central gas density as a third parameter. Using YX as a total mass proxy, we derive a Malmquist bias-corrected local luminosity-mass relation and compare with other recent determinations. Our results indicate that luminosity can be a reliable mass proxy with controllable scatter, which has important implications for upcoming all-sky cluster surveys, such as those to be undertaken with Planck and eROSITA, and ultimately for the use of the cluster population for cosmological purposes.

Abstract Copyright:

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

Simbad objects: 32

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Number of rows : 32

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 2721 ClG 00 06 14.5 -34 42 51           ~ 86 0
3 ACO 22 ClG 00 20 34.8 -25 41 51           ~ 96 0
4 ACO S 84 ClG 00 49 23.2 -29 31 33           ~ 78 0
5 SPT-CL J0145-5301 CGG 01 45 03.60 -53 01 23.4           ~ 43 0
6 ACO 2984 ClG 02 11 27 -40 16.9           ~ 47 0
7 BAX 036.2925-29.4731 ClG 02 25 08.6 -29 28 34           ~ 30 0
8 ACO S 384 ClG 03 45 45.0 -41 10 42           ~ 33 0
9 ACO 3364 ClG 05 47 36.1753 -31 52 22.695           ~ 64 0
10 ACO 3378 ClG 06 05 52.6923 -35 18 32.801           ~ 73 1
11 RXC J0616.8-4748 ClG 06 16 56.8320 -47 47 26.473           ~ 27 0
12 ACO 3404 ClG 06 45 29.50 -54 13 37.0           ~ 78 0
13 ACO 653 ClG 08 21 50.6 +01 11 49           ~ 34 0
14 NAME ACO 901-902 Supercluster SCG 09 56 -10.0           ~ 118 1
15 ACO 907 ClG 09 58 21.84 -11 03 47.5           ~ 117 0
16 ACO 1084 ClG 10 44 37.1 -07 04 47           ~ 69 0
17 ACO 1348 ClG 11 41 24.0 -12 16 00           ~ 61 0
18 ACO S 700 ClG 12 36 40 -33 54.5           ~ 28 0
19 ACO 1663 ClG 13 02 52.55 -02 31 04.0           ~ 91 0
20 ACO 1689 ClG 13 11 29.5 -01 20 28           ~ 1037 0
21 ACO 2050 ClG 15 16 21.6 +00 05 59           ~ 91 0
22 ACO 2051 ClG 15 16 53.8 -01 05 06           ~ 47 0
23 2MAXI J2014-244 ClG 20 14 49.7 -24 30 30           ~ 59 0
24 ACO S 868 ClG 20 23 00 -20 56.3           ~ 30 1
25 ACO 2328 ClG 20 48 13.9 -17 48 53           ~ 67 0
26 ACO 3771 ClG 21 29 47.7233 -50 46 37.428           ~ 40 0
27 ACO 3814 ClG 21 49 07.24 -30 42 06.4           ~ 51 0
28 ACO 2399 ClG 21 57 27.64 -07 48 12.9           ~ 167 0
29 ACO 3854 ClG 22 17 45.72 -35 43 31.4           ~ 59 0
30 ACO 3856 ClG 22 18 45.2 -38 53 57           ~ 71 2
31 ACO 3888 ClG 22 34 23.0 -37 43 29           ~ 127 1
32 ACO 3992 ClG 23 19 41.8 -73 13 51           ~ 31 0

    Equat.    Gal    SGal    Ecl

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2021.03.07-20:24:19

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