The Norris Survey of the Corona Borealis Supercluster. III. Structure and Mass of the Supercluster

Small, Todd; Ma, Chung‐Pei; Sargent, W. L. W.; Hamilton, D.

doi:10.1086/305037

Cited by 88 publications

(118 citation statements)

References 65 publications

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“…The results quoted in Table 1 are for A2067 only as determined from our separation ; 200 velocities from Small, Sargeant, & Hamilton (1997) have been included in this analysis of the clusters A2067 and A2061. Small et al (1998) discuss the structure and dynamics of the larger supercluster.…”

Section: A1749mentioning

confidence: 99%

Dynamics of [CLC]c[/CLC]D Clusters of Galaxies. IV. Conclusion of a Survey of 25 Abell Clusters

Oegerle

Hill

2001

The Astronomical Journal

149

152

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We present the Ðnal results of a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of cD galaxies with peculiar velocities. Redshifts measured with the MX Spectrometer have been combined with those obtained from the literature to obtain typically 50È150 observed velocities in each of 25 galaxy clusters containing a central cD galaxy. We present a dynamical analysis of the Ðnal 11 clusters to be observed in this sample. All 25 clusters are analyzed in a uniform manner to test for the presence of substructure and to determine peculiar velocities and their statistical signiÐcance for the central cD galaxy. These peculiar velocities were used to determine whether or not the central cD galaxy is at rest in the cluster potential well. We Ðnd that 30%È50% of the clusters in our sample possess signiÐcant subclustering (depending on the cluster radius used in the analysis), which is in agreement with other studies of non-cD clusters. Hence, the dynamical state of cD clusters is not di †erent than that of other present-day clusters. After careful study, four of the clusters appear to have a cD galaxy with a signiÐcant peculiar velocity. Dressler-Shectman tests indicate that three of these four clusters have statistically signiÐcant substructure within 1.5Mpc of the cluster center. The dispersion of the cD h 75 1 peculiar velocities is km s~1 around the mean cluster velocity. This represents a signiÐcant detec-164~3 4 41 tion of peculiar cD velocities but at a level that is far below the mean velocity dispersion for this sample of clusters. The picture that emerges is one in which cD galaxies are nearly at rest with respect to the cluster potential well but have small residual velocities due to subcluster mergers.

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Section: A1749mentioning

confidence: 99%

Dynamics of [CLC]c[/CLC]D Clusters of Galaxies. IV. Conclusion of a Survey of 25 Abell Clusters

Oegerle

Hill

2001

The Astronomical Journal

149

152

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“…Morphologically SCl 094 is a multispider with a number of clusters connected by low density filaments, with an overall very elongated shape that resembles a horse-shoe, with the merging X-ray cluster A2065 at the top (Chatzikos et al 2006). SCl 094 has been studied by Small et al (1998), who found that the core of this system probably has started to collapse. Numerical simulations show that such collapsing cores in superclusters are rare (Gramann & Suhhonenko 2002).…”

Section: Notes On Individual Superclustersmentioning

confidence: 99%

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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“…The structure of the superclusters is formed during a hierarchical evolution where the high-density cores of superclusters are older and dynamically more evolved than outskirts regions. While full rich superclusters are not bound systems, their high-density cores may collapse at present or in the course of the future evolution (Small et al 1998;Reisenegger et al 2000;Rines et al 2002;Nagamine & Loeb 2003;Proust et al 2006;Dünner et al 2006;Luparello et al 2011;Pearson et al 2014;Chon et al 2015;O'Mill et al 2015;Einasto et al 2015;Gramann et al 2015). This makes galaxy superclusters unique objects to study their properties and the properties and evolution of the galaxy systems (groups, clusters, and filaments) inside the dynamically evolving environment of superclusters.…”

Section: Introductionmentioning

confidence: 99%

Sloan Great Wall as a complex of superclusters with collapsing cores

Einasto

Lietzen

Gramann

et al. 2016

A&A

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Context. The formation and evolution of the cosmic web is governed by the gravitational attraction of dark matter and antigravity of dark energy (cosmological constant). In the cosmic web, galaxy superclusters or their high-density cores are the largest objects that may collapse at present or during the future evolution. Aims. We study the dynamical state and possible future evolution of galaxy superclusters from the Sloan Great Wall (SGW), the richest galaxy system in the nearby Universe. Methods. We calculated supercluster masses using dynamical masses of galaxy groups and stellar masses of galaxies. We employed normal mixture modelling to study the structure of rich SGW superclusters and search for components (cores) in superclusters. We analysed the radial mass distribution in the high-density cores of superclusters centred approximately at rich clusters and used the spherical collapse model to study their dynamical state. Results. The lower limit of the total mass of the SGW is approximately M = 2.5 × 10 16 h −1 M . Different mass estimators of superclusters agree well, the main uncertainties in masses of superclusters come from missing groups and clusters. We detected three high-density cores in the richest SGW supercluster (SCl 027) and two in the second richest supercluster (SCl 019). They have masses of 1.2−5.9 × 10 15 h −1 M and sizes of up to ≈60 h −1 Mpc. The high-density cores of superclusters are very elongated, flattened perpendicularly to the line of sight. The comparison of the radial mass distribution in the high-density cores with the predictions of spherical collapse model suggests that their central regions with radii smaller than 8 h −1 Mpc and masses of up to M = 2 × 10 15 h −1 M may be collapsing. Conclusions. The rich SGW superclusters with their high-density cores represent dynamically evolving environments for studies of the properties of galaxies and galaxy systems.

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The Norris Survey of the Corona Borealis Supercluster. III. Structure and Mass of the Supercluster

Cited by 88 publications

References 65 publications

Dynamics of [CLC]c[/CLC]D Clusters of Galaxies. IV. Conclusion of a Survey of 25 Abell Clusters

Dynamics of [CLC]c[/CLC]D Clusters of Galaxies. IV. Conclusion of a Survey of 25 Abell Clusters

SDSS DR7 superclusters

Sloan Great Wall as a complex of superclusters with collapsing cores

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