2004A&A...417...13E


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.17CET17:42:41

2004A&A...417...13E - Astronomy and Astrophysics, volume 417, 13-27 (2004/4-1)

Scaling laws in X-ray galaxy clusters at redshift between 0.4 and 1.3.

ETTORI S., TOZZI P., BORGANI S. and ROSATI P.

Abstract (from CDS):

We present a study of the integrated physical properties of a sample of 28 X-ray galaxy clusters observed with Chandra at a redshift between 0.4 and 1.3. In particular, we have twelve objects in the redshift range 0.4-0.6, five between 0.6 and 0.8, seven between 0.8 and 1 and four at z>1.0, compounding the largest sample available for such a study. We focus particularly on the properties and evolution of the X-ray scaling laws. We fit both a single and a double β-model with the former which provides a good representation of the observed surface brightness profiles, indicating that these clusters do not show any significant excess in their central brightness. By using the best-fit parameters of the β-model together with the measured emission-weighted temperature (in the range 3-11keV), we recover gas luminosity, gas mass and total gravitating mass out to R500. We observe scaling relations steeper than expected from the self-similar model by a significant (>3σ) amount in the L-T and Mgas-T relations and by a marginal value in the M_ tot_-T and L-Mtot relations. The degree of evolution of the Mtot-T relation is found to be consistent with the expectation based on the hydrostatic equilibrium for gas within virialized dark matter halos. We detect hints of negative evolution in the L-T, Mgas-T and L-Mtot relations, thus suggesting that systems at higher redshift have lower X-ray luminosity and gas mass for fixed temperature. In particular, when the 16 clusters at z>0.6 are considered, the evolution becomes more evident and its power-law modelization is a statistically good description of the data. In this subsample, we also find significant evidence for positive evolution, such as (1+z)0.3, in the Ez4/3S-T relation, where the entropy S is defined as T/ngas2/3 and is measured at 0.1R200. Such results point toward a scenario in which a relatively lower gas density is present in high-redshift objects, thus implying a suppressed X-ray emission, a smaller amount of gas mass and a higher entropy level. This represents a non-trivial constraint for models aiming at explaining the thermal history of the intra-cluster medium out to the highest redshift reached so far.

Abstract Copyright:

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

Simbad objects: 27

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Number of rows : 27

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 ClG 0016+16 ClG 00 18 33.3 +16 26 36           ~ 468 0
2 ClG J0152-1358 ClG 01 52 41.3 -13 58 13           ~ 238 3
3 ClG 0303+1658 ClG 03 05 31.6 +17 10 02     20.13     ~ 89 0
4 ClG 0451-03 ClG 04 54 10.9 -03 01 07     20.0     ~ 324 0
5 ClG J0542-4100 ClG 05 42 49.9 -40 59 58           ~ 51 0
6 ClG J0848+4453 ClG 08 48 34.800 +44 53 41.90           ~ 121 1
7 ClG J0848+4456 ClG 08 48 46.9 +44 56 22           ~ 56 1
8 ClG J0849+4452 ClG 08 48 56.3 +44 52 16           ~ 101 1
9 ClG J0910+5422 ClG 09 10 44.9 +54 22 09           ~ 84 0
10 ClG 1054-03 ClG 10 57 00.2 -03 37 27     22     ~ 448 0
11 ClG J1113-2615 ClG 11 13 05.7 -26 15 36           ~ 33 0
12 ClG J1120+2326 ClG 11 20 57.9 +23 26 41           ~ 39 0
13 ClG 1137+66 ClG 11 40 23.3 +66 09 01     21.0     ~ 134 0
14 ClG J1221+4918 ClG 12 21 25.0 +49 18 07           ~ 54 0
15 ClG J1226+3332 ClG 12 26 57.7 +33 32 50           ~ 190 0
16 ClG J1252-2927 ClG 12 52 54.4 -29 27 17           ~ 150 0
17 ClG J1317+2911 ClG 13 17 21.70 +29 11 18.1           ~ 30 0
18 ClG J1347-1145 ClG 13 47 33.5 -11 45 42           ~ 453 0
19 ClG J1350+6007 ClG 13 50 48.55 +60 07 06.7           ~ 40 0
20 ClG J1411+5211 ClG 14 11 24.4 +52 12 38     20.11     ~ 112 3
21 ClG J1416+4446 ClG 14 16 28.1 +44 46 38           ~ 41 0
22 ClG J1524+0957 ClG 15 24 40.3 +09 57 35           ~ 55 0
23 ClG 1621+26 ClG 16 23 35.7 +26 33 50           G0V 132 0
24 ClG J1701+6421 ClG 17 01 48.77 +64 21 03.0           ~ 14 0
25 ClG J1716+6708 ClG 17 16 49.6 +67 08 30           ~ 112 0
26 ClG 2053-04 ClG 20 56 21.2 -04 37 46   21.0       ~ 160 0
27 ClG J2302+0844 ClG 23 02 48.1 +08 43 50           ~ 39 0

    Equat.    Gal    SGal    Ecl

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2019.11.17-17:42:41

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