2003ApJ...587..589M


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.28CET15:05:22

2003ApJ...587..589M - Astrophys. J., 587, 589-604 (2003/April-3)

Chandra X-ray analysis of the massive high-redshift galaxy clusters Cl J1113.1-2615 and Cl J0152.7-1357.

MAUGHAN B.J., JONES L.R., EBELING H., PERLMAN E., ROSATI P., FRYE C. and MULLIS C.R.

Abstract (from CDS):

We present an analysis of Chandra observations of two high-redshift clusters of galaxies, Cl J1113.1-2615 at z=0.725 and Cl J0152.7-1357 at z=0.833. We find Cl J1113.1-2615 to be morphologically relaxed with a temperature of kT=4.3+0.5–0.4keV and a mass (within the virial radius) of 4.3+0.8–0.7x1014 M. Cl J0152.7-1357, by contrast, is resolved into a northern and southern subcluster, each massive and X-ray-luminous, in the process of merging. The temperatures of the subclusters are found to be 5.5+0.9–0.8and 5.2+1.1–0.9 keV, respectively, and we estimate their respective masses to be 6.1+1.7–1.5x1014 and 5.2+1.8–1.4x1014 Mwithin the virial radii. A dynamical analysis of the system shows that the subclusters are likely to be gravitationally bound. If the subclusters merge, they will form a system with a mass similar to that of the Coma Cluster. Two-dimensional modeling of the X-ray surface brightness reveals excess emission between the subclusters, suggestive, but not conclusive, evidence of a shock front. We make a first attempt at measuring the cluster M-T relation at z~0.8 and find no evolution in its normalization, supporting the previous assumption of an unevolving M-T relation when constraining cosmological parameters from cluster evolution studies. A comparison of the cluster properties with those of nearby systems also finds little or no evolution in the L-T relation, the gas fraction-T relation, the β-T relation, or the metallicity. These results suggest that, in at least some massive clusters, the hot gas was in place, and containing its metals, at z~0.8 and thus that the clusters were assembled at redshifts significantly higher than z=0.8, as predicted in low-ΩMmodels. We also highlight the need to correct for the degradation of the Chandra ACIS low-energy quantum efficiency in high-redshift cluster studies when the low-energy absorption is often assumed to be the Galactic value, rather than measured.

Abstract Copyright:

Journal keyword(s): Cosmology: Observations - Galaxies: Clusters: General - Galaxies: Clusters: Individual: Alphanumeric: Cl J0152.7-1357 - Galaxies: Clusters: Individual: Alphanumeric: Cl J1113.1-2615 - Galaxies: High-Redshift - Galaxies: Intergalactic Medium - X-Rays: Galaxies: Clusters

Nomenclature: Text: [MJE2003] JHHMMSS.ss+DDMMSS.ss N=3.

CDS comments: Table 2: North and South subclusters are later designated as [MEJ2006] ClG J0152-1357 C and [MEJ2006] ClG J0152-1357 E respectively.

Simbad objects: 6

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Number of rows : 6

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 [MJE2003] J015239.89-135827.48 GrG 01 52 39.590 -13 58 27.48           ~ 7 1
2 ClG J0152-1358 ClG 01 52 41.3 -13 58 13           ~ 239 3
3 [MJE2003] J015244.18-135715.84 GrG 01 52 44.180 -13 57 15.84           ~ 7 1
4 [MJE2003] J015252.42-135805.52 X 01 52 52.420 -13 58 05.52           ~ 2 0
5 ClG J1113-2615 ClG 11 13 05.7 -26 15 36           ~ 33 0
6 ACO 1656 ClG 12 59 48.7 +27 58 50           ~ 4134 2

    Equat.    Gal    SGal    Ecl

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2020.01.28-15:05:22

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