An<i>XMM-Newton</i>observation of the massive, relaxed galaxy cluster ClJ1226.9+3332 at<i>z</i>= 0.89

Maughan, Ben; Jones, Laura; Ebeling, H.; Scharf, Caleb

doi:10.1111/j.1365-2966.2004.07860.x

Cited by 53 publications

(77 citation statements)

References 41 publications

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“…We find L X (r < 1:43 Mpc) ¼ 4:57 AE 0:11 ergs s À1 and L X (r < 1) ¼ 5:12 AE 0:12 ergs s À1 , including uncertainties on the temperature and metal abundance in those on the luminosity. These luminosities are consistent with those found by Maughan et al (2006b) based on a shorter XMMNewton observation of Cl J1226.9+3332.…”

Section: The Global Properties Of CL J12269+3332 and The Scaling Relsupporting

confidence: 81%

“…Cl J1226.9+3332 was detected in the Wide Angle ROSAT Pointed Survey (WARPS; Scharf et al 1997;Ebeling et al 2001), and an analysis of a 15 ks AO1 XMMNewton observation confirmed its temperature at 11:5 keV with a bolometric luminosity of 5 ; 10 45 ergs s À1 and a relaxed morphology ( Maughan et al 2004a). An early, short Chandra observation of Cl J1226.9+3332 was presented by Cagnoni et al (2001), who also pointed out that the VLA 3 FIRST catalog shows a faint pointlike radio source at the cluster center, consistent with a lowluminosity radio-loud active galactic nucleus (AGN).…”

Section: Introductionmentioning

confidence: 99%

“…The scaling relations between cluster properties at high redshifts are then of key importance, and their uncertainty is a dominant contributor to the error budget of derived cosmological parameters (Henry 2004). Furthermore, studies of the evolution of the cluster scaling relations can be used to probe cluster formation and the history of nongravitational heating (e.g., Ettori et al 2003;Maughan et al 2006b). …”

Section: Introductionmentioning

confidence: 99%

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DeepXMM‐NewtonandChandraObservations of Cl J1226.9+3332: A Detailed X‐Ray Mass Analysis of az= 0.89 Galaxy Cluster

Maughan¹,

Jones²,

Jones³

et al. 2007

ApJ

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107

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Deep XMM-Newton and Chandra observations of Cl J1226.9+3332 at z ¼ 0:89 have enabled the most detailed X-ray mass analysis of any such high-redshift galaxy cluster. The XMM-Newton temperature profile of the system shows no sign of central cooling, with a hot core and a radially declining profile. A temperature map shows asymmetry with a hot region that appears to be associated with a subclump of galaxies at the cluster redshift but is not visible in the X-ray surface brightness. This is likely to be the result of a merger event in the cluster but does not appear to significantly affect the overall temperature profile. The XMM-Newton temperature profile and combined Chandra and XMM-Newton emissivity profile allowed precise measurements of the global properties of Cl J1226.9+3332. Within an overdensity radius of 500 times the critical density at z ¼ 0:89 (R 500 ), we find kT ¼ 10:4 AE 0:6 keV, Z ¼ 0:16 AE 0:05 Z , and M ¼ 5:2 þ1:0 À0:8 ; 10 14 M . We obtain profiles of the metallicity, entropy, cooling time, and gas fraction and find a high concentration parameter for the total density profile of the system. The global properties are compared with the local L-T and M-T relations, and we are able to make the first observational test of the predicted evolution of the Y X -M 500 relation. We find that departures from these scaling relations are most likely caused by an underestimate of the total mass by $30% in the X-ray hydrostatic mass analysis due to the apparent recent or ongoing merger activity.

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Section: The Global Properties Of CL J12269+3332 and The Scaling Relsupporting

confidence: 81%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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DeepXMM‐NewtonandChandraObservations of Cl J1226.9+3332: A Detailed X‐Ray Mass Analysis of az= 0.89 Galaxy Cluster

Maughan¹,

Jones²,

Jones³

et al. 2007

ApJ

Self Cite

107

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“…They are suitable laboratories in which to study galaxy populations, providing clues to better understand the effects of the local environment on galaxy properties and galaxy evolution. Cluster X-ray luminosity and temperature indicate the existence of massive systems (M > 10 14 M ) already when the universe was half its present age (Jeltema et al 2001;Maughan et al 2003Maughan et al , 2004Rosati et al 2004;Mullis et al 2005). While some of these clusters have a relaxed X-ray morphology by z $ 0:8 (Maughan et al 2004), others show clear signatures of being still in a formation stage, as indicated by their filamentary morphology and the presence of substructure (Gioia et al 1999(Gioia et al , 2004Demarco et al 2005;Girardi et al 2005;Tanaka et al 2006).…”

Section: Introductionmentioning

confidence: 99%

VLT and ACS Observations of RDCS J1252.9−2927: Dynamical Structure and Galaxy Populations in a Massive Cluster atz= 1.237

Demarco

Rosati

Lidman

et al. 2007

ApJ

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We present results from an extensive spectroscopic survey, carried out with VLT FORS, and from an extensive multiwavelength imaging data set from the HST Advanced Camera for Surveys and ground-based facilities, of the cluster of galaxies RDCS J1252.9À2927. We have spectroscopically confirmed 38 cluster members in the redshift range 1:22 < z < 1:25. A cluster median redshift of z ¼ 1:237 and a rest-frame velocity dispersion of 747 þ74 À84 km s À1 are obtained. Using the 38 confirmed redshifts, we were able to resolve, for the first time at z > 1, kinematic structure. The velocity distribution, which is not Gaussian at the 95% confidence level, is consistent with two groups that are also responsible for the projected east-west elongation of the cluster. The groups are composed of 26 and 12 galaxies with velocity dispersions of 486 þ47 À85 and 426 þ57 À105 km s À1 , respectively. The elongation is also seen in the intracluster gas and the dark matter distribution. This leads us to conclude that RDCS J1252. 9À2927 has not yet reached a final virial state. We extend the analysis of the color-magnitude diagram of spectroscopic members to more than 1 Mpc from the cluster center. The scatter and slope of non-[O ii]-emitting cluster members in the near-IR red sequence is similar to that seen in clusters at lower redshift. Furthermore, most of the galaxies with luminosities greater than $K Ã s þ 1:5 do not show any [O ii], indicating that these more luminous, redder galaxies have stopped forming stars earlier than the fainter, bluer galaxies. Our observations provide detailed dynamical and spectrophotometric information on galaxies in this exceptional high-redshift cluster, delivering an in-depth view of structure formation at this epoch only 5 Gyr after the big bang.

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“…The X-ray selected samples at z ≥ 1 probe the most massive and dynamically relaxed systems (e.g., Maughan et al 2004;Stanford et al 2006;Bremer et al 2006;Lidman et al 2008). Large-area multicolour surveys, such as the red-sequence survey (e.g.…”

Section: Introductionmentioning

confidence: 99%

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

Salimbeni

Castellano

Pentericci

et al. 2009

A&A

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Aims. The aim of the present paper is to identify and study the properties and galactic content of groups and clusters in the GOODSSouth field up to z ∼ 2.5, and to analyse the physical properties of galaxies as a continuous function of environmental density up to high redshift. Methods. We used the deep (z 850 ∼ 26), multi-wavelength GOODS-MUSIC catalogue, which has a 15% of spectroscopic redshifts and accurate photometric redshifts for the remaining fraction. On these data, we applied a (2+1)D algorithm, previously developed by our group, that provides an adaptive estimate of the 3D density field. We supported our analysis with simulations to evaluate the purity and the completeness of the cluster catalogue produced by our algorithm. Results. We find several high-density peaks embedded in larger structures in the redshift range 0.4-2.5. From the analysis of their physical properties (mass profile, M 200 , σ v , L X , U − B vs. B diagram), we find that most of them are groups of galaxies, while two are poor clusters with masses a few times 10 14 M . For these two clusters we find from the Chandra 2Ms data an X-ray emission significantly lower than expected from their optical properties, suggesting that the two clusters are either not virialised or are gas poor. We find that the slope of the colour magnitude relation, for these groups and clusters, is constant at least up to z ∼ 1. We also analyse the dependence on environment of galaxy colours, luminosities, stellar masses, ages, and star formations. We find that galaxies in high-density regions are, on average, more luminous and massive than field galaxies up to z ∼ 2. The fraction of red galaxies increases with luminosity and with density up to z ∼ 1.2. At higher z this dependence on density disappears. The variation of galaxy properties as a function of redshift and density suggests that a significant change occurs at z ∼ 1.5-2.

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AnXMM-Newtonobservation of the massive, relaxed galaxy cluster ClJ1226.9+3332 atz= 0.89

Cited by 53 publications

References 41 publications

DeepXMM‐NewtonandChandraObservations of Cl J1226.9+3332: A Detailed X‐Ray Mass Analysis of az= 0.89 Galaxy Cluster

DeepXMM‐NewtonandChandraObservations of Cl J1226.9+3332: A Detailed X‐Ray Mass Analysis of az= 0.89 Galaxy Cluster

VLT and ACS Observations of RDCS J1252.9−2927: Dynamical Structure and Galaxy Populations in a Massive Cluster atz= 1.237

A comprehensive study of large-scale structures in the GOODS-SOUTH field up to ${\mathsf z} \sim $ 2.5

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