Multiple Merging Events in the Double Cluster A3128/A3125

Rose, James A.; Gaba, Alejandro E.; Christiansen, W. A.; Davis, David; Caldwell, Nelson; Hunstead, R. W.; Johnston‐Hollitt, M.

doi:10.1086/339183

Cited by 40 publications

(79 citation statements)

References 56 publications

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“…Rich superclusters contain high-density cores (Einasto et al 2007c). The fraction of rich clusters and X-ray clusters in rich superclusters is larger than in poor superclusters (Einasto et al 2001;Luparello et al 2011), and the core regions of the richest superclusters may contain merging X-ray clusters (Bardelli et al 2000;Rose et al 2002). However, we still lack a detailed analysis of whether the differences between the properties of the galaxy and group content of rich and poor superclusters are related also to the differences in morphology of superclusters.…”

Section: Comparison With Other Studiesmentioning

confidence: 97%

SDSS DR7 superclusters

Einasto

Liivamägi

Tago

et al. 2011

A&A

122

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Aims. We study the morphology of a set of superclusters drawn from the SDSS DR7. Methods. We calculate the luminosity density field to determine superclusters from a flux-limited sample of galaxies from SDSS DR7 and select superclusters with 300 and more galaxies for our study. We characterise the morphology of superclusters using the fourth Minkowski functional V 3 , the morphological signature (the curve in the shapefinder's K 1 -K 2 plane) and the shape parameter (the ratio of the shapefinders K 1 /K 2 ). We investigate the supercluster sample using multidimensional normal mixture modelling. We use Abell clusters to identify our superclusters with known superclusters and to study the large-scale distribution of superclusters. Results. The superclusters in our sample form three chains of superclusters; one of them is the Sloan Great Wall. Most superclusters have filament-like overall shapes. Superclusters can be divided into two sets; more elongated superclusters are more luminous, richer, have larger diameters and a more complex fine structure than less elongated superclusters. The fine structure of superclusters can be divided into four main morphological types: spiders, multispiders, filaments, and multibranching filaments. We present the 2D and 3D distribution of galaxies and rich groups, the fourth Minkowski functional, and the morphological signature for all superclusters. Conclusions. Widely different morphologies of superclusters show that their evolution has been dissimilar. A study of a larger sample of superclusters from observations and simulations is needed to understand the morphological variety of superclusters and the possible connection between the morphology of superclusters and their large-scale environment.

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Section: Comparison With Other Studiesmentioning

confidence: 97%

SDSS DR7 superclusters

Einasto

Liivamägi

Tago

et al. 2011

A&A

122

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“…Until Werner et al (2007), using XMM-Newton data, revealed a more distant (z = 0.440) and more massive cluster superposed on the northeastern component of A3128, it was believed to be part of the Horologium-Reticulum supercluster at z = 0.06, although its X-ray morphology is clearly double peaked with the two components separated on the sky by some 12 (Rose et al 2002). Hincks et al (2009) confirmed the Werner et al (2007) results that A3128 (NE) is indeed a separate higher redshift cluster, and a case of finding a cluster behind a cluster.…”

Section: Act-cl J0330−5227 (A3128 North-east)mentioning

confidence: 99%

The Atacama Cosmology Telescope: Physical Properties and Purity of a Galaxy Cluster Sample Selected via the Sunyaev-Zel'dovich Effect

Menanteau

González

Juin

et al. 2010

ApJ

113

145

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We present optical and X-ray properties for the first confirmed galaxy cluster sample selected by the Sunyaev-Zel'dovich effect (SZE) from 148 GHz maps over 455 deg 2 of sky made with the Atacama Cosmology Telescope (ACT). These maps, coupled with multi-band imaging on 4 m class optical telescopes, have yielded a sample of 23 galaxy clusters with redshifts between 0.118 and 1.066. Of these 23 clusters, 10 are newly discovered. The selection of this sample is approximately mass limited and essentially independent of redshift. We provide optical positions, images, redshifts, and X-ray fluxes and luminosities for the full sample, and X-ray temperatures of an important subset. The mass limit of the full sample is around 8.0×1014 M , with a number distribution that peaks around a redshift of 0.4. For the 10 highest significance SZE-selected cluster candidates, all of which are optically confirmed, the mass threshold is 1 × 10 15 M and the redshift range is 0.167-1.066. Archival observations from Chandra, XMM-Newton, and ROSAT provide X-ray luminosities and temperatures that are broadly consistent with this mass threshold. Our optical follow-up procedure also allowed us to assess the purity of the ACT cluster sample. Eighty (one hundred) percent of the 148 GHz candidates with signal-to-noise ratios greater than 5.1 (5.7) are confirmed as massive clusters. The reported sample represents one of the largest SZE-selected sample of massive clusters over all redshifts within a cosmologically significant survey volume, which will enable cosmological studies as well as future studies on the evolution, morphology, and stellar populations in the most massive clusters in the universe.

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“…The supercluster environment affects the properties of groups and clusters located there (Plionis 2004). The fraction of X-ray clusters in rich superclusters is larger than in poor superclusters (Einasto et al 2001), and the core regions of the richest superclusters may contain merging X-ray clusters (Rose et al 2002;Bardelli et al 2000).…”

Section: Introductionmentioning

confidence: 99%

The richest superclusters

Einasto¹,

Saar²,

Liivamägi³

et al. 2007

A&A

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Context. Superclusters are the largest systems in the Universe to give us information about the formation and evolution of structures in the very early Universe. Our present series of papers is devoted to the study of the morphology and internal structure of superclusters of galaxies. Aims. We study the morphology of the richest superclusters from the catalogs of superclusters of galaxies in the 2dF Galaxy Redshift Survey and compare the morphology of real superclusters with model superclusters in the Millennium Simulation. Methods. We use Minkowski functionals and shapefinders to quantify the morphology of superclusters: their sizes, shapes, and clumpiness. We generate empirical models of simple geometry to understand which morphologies correspond to the supercluster shapefinders (Appendix A). Results. Rich superclusters have elongated, filamentary shapes with high-density clumps in their core regions. The clumpiness of superclusters is determined using the fourth Minkowski functional V 3 . In the K 1 -K 2 shapefinder plane the morphology of superclusters is described by a curve which is characteristic of multi-branching filaments as shown by our empirical models. We found several differences between observed and model superclusters. The curves of the fourth Minkowski functional V 3 for observed and model superclusters have different shapes indicating that their structure is different. The values of V 3 for the supercluster SCL126 (the Sloan Great Wall) show that this supercluster has a very high density core which is absent in other superclusters. The values of the shapefinders H 1 -H 3 and K 1 and K 2 for observed superclusters have much larger scatter than for model superclusters. The differences between the fourth Minkowski functional V 3 for the bright and faint galaxies in observed superclusters are larger than in simulated superclusters. Conclusions. Our results show how the Minkowski functionals and shapefinders can be used to describe the morphology of superclusters: their shapes, sizes and clumpiness. The shapes of observed superclusters are more diverse than the shapes of simulated superclusters. The larger scatter of the fourth Minkowski functional V 3 for the bright and faint galaxies for observed superclusters compared to simulated superclusters is an indication that the clumpiness of bright and faint galaxies in models does not reflect well the clumpiness of different galaxies in observed superclusters. Our results suggest also that the volume covered by the Millennium Simulations may be too small to properly describe the large morphological variety of superclusters.

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Multiple Merging Events in the Double Cluster A3128/A3125

Cited by 40 publications

References 56 publications

SDSS DR7 superclusters

SDSS DR7 superclusters

The Atacama Cosmology Telescope: Physical Properties and Purity of a Galaxy Cluster Sample Selected via the Sunyaev-Zel'dovich Effect

The richest superclusters

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