The Distribution of Rich Clusters of Galaxies.

Abell, G. O.

doi:10.1086/190036

Cited by 1,293 publications

(1,120 citation statements)

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“…As starting point, we determine the classical optical richness measure, the Abell richness R rich (Abell 1958), defined as the number of cluster galaxies within the projected Abell radius R A 2.14 h −1 70 Mpc and with apparent magnitudes in the interval [m 3 , m 3 + 2], where m 3 is the third brightest cluster galaxy. We use the LBT/LBC z -band as the reddest optical wide-field imaging filter, providing the highest clusterto-foreground/background contrast and allowing background estimations in the same field.…”

Section: Richness Measuresmentioning

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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Section: Richness Measuresmentioning

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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“…We take into account the fact that all compact systems transform to extended objects after smoothing. In our previous analysis (E03a and E03b) we used Gaussian smoothing with rms scale 10 h −1 Mpc, and the limiting radius of the smallest system to be considered as a supercluster is 5.04 h −1 Mpc; this radius corresponds to a system of volume 535 (h −1 Mpc) 3 . When using an Epanechnikov kernel with radius ≈8 h −1 Mpc we can use a smaller limiting radius.…”

Section: Preliminary Study Of 2dfgrs Superclusters: Choice Of Selectimentioning

confidence: 99%

“…Additionally we searched for galaxies and groups around the central peak within relative distance limits ±8 h −1 Mpc from the central peak. The smoothed density field integrates luminosities of galaxies inside the whole sphere of radius equal to the smoothing radius, the volume of the sphere is 4πr 3 0 /3 = 2145 (h −1 Mpc) 3 . This sphere contains in nearby regions 200. .…”

Section: Df-clusters and Supercluster Richnessmentioning

confidence: 99%

“…These studies were based on observational data about galaxies, as well as on data about nearby groups and clusters of galaxies. Classical, relatively deep all-sky supercluster catalogues were constructed using the Abell (1958) and Abell et al (1989) cluster catalogues by Zucca et al (1993), Einasto et al (1994Einasto et al ( , 1997Einasto et al ( , 2001, hereafter E94, E97, E01) and Kalinkov & Kuneva (1995).…”

Section: Introductionmentioning

confidence: 99%

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Superclusters of galaxies from the 2dF redshift survey

Einasto¹,

Einasto²,

Tago³

et al. 2006

A&A

120

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Aims. We use the 2dF Galaxy Redshift Survey data to compile catalogues of superclusters for the Northern and Southern regions of the 2dFGRS, altogether 543 superclusters at redshifts 0.009 ≤ z ≤ 0.2. Methods. We analyse methods of compiling supercluster catalogues and use results of the Millennium Simulation to investigate possible selection effects and errors. We find that the most effective method is the density field method using smoothing with an Epanechnikov kernel of radius 8 h −1 Mpc. Results. We derive positions of the highest luminosity density peaks and find the most luminous cluster in the vicinity of the peak, this cluster is considered as the main cluster and its brightest galaxy the main galaxy of the supercluster. In catalogues we give equatorial coordinates and distances of superclusters as determined by positions of their main clusters. We also calculate the expected total luminosities of the superclusters.

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“…The simplest approach is to identify a cluster as an overdensity in the projected distribution of galaxies in an optical image. The first catalog was indeed a compilation of galaxy concentrations found by eye in optical images (Abell 1958). Today, the quality of optical images, especially that from the Hubble Space Telescope, are such that bright (or, in terms of galaxies, rich) clusters of galaxies are among the most spectacular objects of the extragalactic sky.…”

Section: What Is a Cluster Of Galaxiesmentioning

confidence: 99%

Cosmological Parameters from Galaxy Clusters: An Introduction

Tozzi¹

2007

Lecture Notes in Physics

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This lecture is an introduction to cosmological tests with clusters of galaxies. Here I do not intend to provide a complete review of the subject, but rather to describe the basic procedures to set up the fitting machinery to constrain cosmological parameters from clusters, and to show how to handle data with a critical insight. I will focus mainly on the properties of X-ray clusters of galaxies, showing their success as cosmological tools, to end up discussing the complex thermodynamics of the diffuse intracluster medium and its impact on the cosmological tests.

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The Distribution of Rich Clusters of Galaxies.

Cited by 1,293 publications

References 0 publications

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

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

Superclusters of galaxies from the 2dF redshift survey

Cosmological Parameters from Galaxy Clusters: An Introduction

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