The
                    <i>XMM</i>
                    Cluster Survey: A Massive Galaxy Cluster at
                    <i>z</i>
                    = 1.45

Stanford, S. A.; Romer, A. K.; Sabirli, Kivanc; Davidson, M.; Hilton, Matthew; Viana, P. T. P.; Collins, Chris; Kay, Scott T.; Liddle, Andrew R.; Mann, Robert; Miller, Christopher J.; Nichol, R. C.; West, Michael J.; Conselice, Christopher J.; Spinrad, Hyron; Stern, Daniel; Bundy, Kevin

doi:10.1086/506449

Cited by 171 publications

(213 citation statements)

References 19 publications

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“…If cluster masses have grown by a factor 2 or 3 since z ≃ 1, as some authors suggest 33 In order to compare our data with simulations we use the bolometric X-ray luminosity of each system (L X ) 11,12,34,35 as this can be used to determine cluster mass from power-law scaling relations 36,37 . For J2235 we use the published X-ray luminosity 15 …”

Section: Cluster Massesmentioning

confidence: 99%

“…Properties of our BCGs and their host clusters are listed in Table 1. All five clusters were discovered serendipitously in X-rays and they are the most distant clusters discovered in their respective X-ray surveys 11-15 .The cluster J2215 was discovered as part of the XMM Cluster Survey (XCS 16,17 ) and has the highest redshift of any spectroscopically confirmed cluster 12,18 . …”

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confidence: 95%

“…The cluster J2215 was discovered as part of the XMM Cluster Survey (XCS 16,17 ) and has the highest redshift of any spectroscopically confirmed cluster 12,18 .…”

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confidence: 99%

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Early assembly of the most massive galaxies

Collins

Stott

Hilton

et al. 2009

Nature

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The current consensus is that galaxies begin as small density fluctuations in the early Universe and grow by in situ star formation and hierarchical merging 1 . Stars begin to form relatively quickly in sub-galactic sized building blocks called haloes which are subsequently assembled into galaxies. However, exactly when this assembly takes place is a matter of some debate 2, 3 . Here we report that the stellar masses of brightest cluster galaxies, which are the most luminous objects emitting stellar light, some 9 billion years ago are not significantly different from their stellar masses today. Brightest cluster galaxies are almost fully assembled 4 − 5 Gyrs after the Big Bang, having 2 grown to more than 90% of their final stellar mass by this time. Our data conflict with the most recent galaxy formation models 4, 5 based on the largest simulations of dark matter halo development 1 . These models predict protracted formation of brightest cluster galaxies over a Hubble time, with only 22% of the stellar mass assembled at the epoch probed by our sample. Our findings suggest a new picture in which brightest cluster galaxies experience an early period of rapid growth rather than prolonged hierarchical assembly.Brightest cluster galaxies (BCGs) are located at the centres of galaxy clusters. They constitute a separate population from bright elliptical galaxies 6 and both their homogeneity and extreme luminosity have motivated their use as standard candles for cosmology 7-9 .Our investigation focuses on BCGs in the most distant X-ray emitting galaxy clusters at redshifts z = 1.2 −1.5, where (1 + z) is the expansion factor of the Universe relative to the present. It has been shown that X-ray cluster selection is currently the optimum strategy for an unbiased investigation of BCG evolution 10 . Properties of our BCGs and their host clusters are listed in Table 1. All five clusters were discovered serendipitously in X-rays and they are the most distant clusters discovered in their respective X-ray surveys 11-15 .The cluster J2215 was discovered as part of the XMM Cluster Survey (XCS 16,17 ) and has the highest redshift of any spectroscopically confirmed cluster 12,18 . 3The stellar mass of a BCG depends upon the hierarchical build up of its host dark matter halo and its stellar evolution history, along with the baryonic physics of the galaxy.We base our study of BCGs on photometry in the infrared wavebands J (1.26 µm) and K s (2.14 µm). Infrared imaging is essential at these large redshifts to compensate for the redshifting of the early-type galaxy spectra. Also, these wavebands are less sensitive than optical light to the presence of young stars and are a more accurate tracer of the underlying old stellar population and, hence, of the stellar mass of the systems. Fig. 1 shows an infrared image of the cluster J2235 from our sample (see also Supplementary Fig. 1).We start by examining the ages of the stars themselves in these galaxies using the run of J − K s colour evolution with redshift as shown in Fig. 2. For BCGs at ...

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Section: Cluster Massesmentioning

confidence: 99%

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confidence: 95%

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Early assembly of the most massive galaxies

Collins

Stott

Hilton

et al. 2009

Nature

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175

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“…On the X-ray side, new identifications of X-ray luminous clusters are currently largely driven by XMM-Newton serendipitous surveys (e.g. Mullis et al 2005;Stanford et al 2006;Fassbender et al 2008;Santos et al 2009;Schwope et al 2010) and smaller dedicated surveys of a A&A 527, A78 (2011) few square degrees (e.g. Andreon et al 2005;Bremer et al 2006;Pierre et al 2006;Finoguenov et al 2007Finoguenov et al , 2010Tanaka et al 2010).…”

Section: Introductionmentioning

confidence: 99%

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

Fassbender

Böhringer

Santos

et al. 2011

A&A

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Context. Observations of the formation and evolution of massive galaxy clusters and their matter components provide crucial constraints on cosmic structure formation, the thermal history of the intracluster medium (ICM), galaxy evolution, transformation processes, and gravitational and hydrodynamic interaction physics of the subcomponents. Aims. We characterize the global multi-wavelength properties of the X-ray selected galaxy cluster XMMU J1230.3+1339 at z = 0.975, a new system discovered within the XMM-Newton Distant Cluster Project (XDCP). We measure and compare various widely used mass proxies and identify multiple cluster-associated components from the inner core region out to the large-scale structure environment.Methods. We present a comprehensive galaxy cluster study based on a joint analysis of X-ray data, optical imaging and spectroscopy observations, weak lensing results, and radio properties for achieving a detailed multi-component view on a system at z ∼ 1. Results. We find an optically very rich and massive system with M 200 (4.2 ± 0.8) × 10 14 M , T X,2500 5.3 +0.7 −0.6 keV, and L bol X,500 (6.5 ± 0.7) × 10 44 erg s −1 . We have identified a central fly-through group close to core passage and find marginally extended 1.4 GHz radio emission possibly associated with the turbulent wake region of the merging event. On the cluster outskirts we see evidence for an on-axis infalling group with a second brightest cluster galaxy (BCG) and indications for an additional off-axis group accretion event. We trace two galaxy filaments beyond the nominal cluster radius and provide a tentative reconstruction of the 3D-accretion geometry of the system. Conclusions. In terms of total mass, ICM structure, optical richness, and the presence of two dominant BCG-type galaxies, the newly confirmed cluster XMMU J1230.3+1339 is likely the progenitor of a system very similar to the local Coma cluster, differing by 7.6 Gyr of structure evolution. This new system is an ideally suited astrophysical model laboratory for in-depth follow-up studies on the aggregation of baryons in the cold and hot phases.

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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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The XMM Cluster Survey: A Massive Galaxy Cluster at z = 1.45

Cited by 171 publications

References 19 publications

Early assembly of the most massive galaxies

Early assembly of the most massive galaxies

A pan-chromatic view of the galaxy cluster XMMU J1230.3+1339 atz= 0.975

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

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