Sloan Great Wall as a complex of superclusters with collapsing cores

Einasto, M.; Lietzen, H.; Gramann, Mirt; Tempel, Elmo; Saar, E.; Liivamägi, L. J.; Heinämäki, P.; Nurmi, P.; Einasto, J.

doi:10.1051/0004-6361/201628567

Cited by 34 publications

(62 citation statements)

References 96 publications

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“…This suggests that we have no strong biases in the mass calculations. The same was concluded in Einasto et al (2016) in which several mass estimates of the core regions of superclusters from the Sloan Great Wall were compared. At clustercentric distances up to approximately 3 h −1 Mpc the mass of the supercluster core is determined by the mass of the cluster A2142 and its infalling subclusters, including group Gr5 at clustercentric distance of 2.4 h −1 Mpc.…”

Section: Discussionmentioning

confidence: 56%

“…7 are calculated using group mass errors, which depend on the group richness (shaded regions in the figure). Einasto et al (2016) estimate that, on average, supercluster mass errors due to group dynamical mass errors are of about 0.3 dex. For the core region of SCl A2142 such errors were probably overestimated.…”

Section: Discussionmentioning

confidence: 96%

“…where (M * /M halo ) 0 = 0.02817 is the normalisation of the stellar to halo mass relation, the halo mass M halo is the virial mass of haloes, M 1 = 7.925 × 10 11 M ⊙ is a characteristic mass, and β = 1.068 and γ = 0.611 are the slopes of the lowand high-mass ends of the relation, respectively. This method was used by Einasto et al (2016) to find the mass of the Sloan Great Wall (SGW) superclusters, and by Lietzen et al (2016) and Einasto et al (2017) to estimate the mass of the BOSS Great Wall superclusters. The total mass was obtained summing the masses of groups and by adding 10% of the mass as the mass of gas in the supercluster.…”

Section: Discussionmentioning

confidence: 99%

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Supercluster A2142 and collapse in action: infalling and merging groups and galaxy transformations

Einasto

Gramann

Park

et al. 2018

A&A

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Context. Superclusters with collapsing cores represent dynamically evolving environments for galaxies, galaxy groups, and clusters. Aims. We study the dynamical state and properties of galaxies and groups in the supercluster SCl A2142 that has a collapsing core, to understand its possible formation and evolution. Methods. We find the substructure of galaxy groups using normal mixture modelling. We have used the projected phase space (PPS) diagram, spherical collapse model, clustercentric distances, and magnitude gap between the brightest galaxies in groups to study the dynamical state of groups and to analyse group and galaxy properties. We compared the alignments of groups and their brightest galaxies with the supercluster axis. Results. The supercluster core has a radius of about 8 h −1 Mpc and total mass M tot ≈ 2.3 × 10 15 h −1 M ⊙ and is collapsing. Galaxies in groups on the supercluster axis have older stellar populations than off-axis groups, with median stellar ages 4 − 6 and < 4 Gyr, correspondingly. The cluster A2142 and the group Gr8 both host galaxies with the oldest stellar populations among groups in SCl A2142 having the median stellar age t > 8 Gyr. Recently quenched galaxies and active galactic nuclei (AGNs) are mostly located at virial radii or in merging regions of groups, and at clustercentric distances D c ≈ 6 h −1 Mpc. The most elongated groups lie along the supercluster axis and are aligned with it. Magnitude gaps between the brightest galaxies of groups are less than one magnitude, suggesting that groups in SCl A2142 are dynamically young. Conclusions. The collapsing core of the supercluster, infall of galaxies and groups, and possible merging groups, which affect galaxy properties and may trigger the activity of AGNs, show how the whole supercluster is evolving.

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Section: Discussionmentioning

confidence: 56%

Section: Discussionmentioning

confidence: 96%

Section: Discussionmentioning

confidence: 99%

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Supercluster A2142 and collapse in action: infalling and merging groups and galaxy transformations

Einasto

Gramann

Park

et al. 2018

A&A

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“…Arguments based on geometrical and fitness diameter functions suggest that very large over-density regions, such as the Sloan Great Wall and the BOSS Great Wall, are actually complexes of superclusters, as studied by Liivamägi et al (2012); Einasto et al (2016Einasto et al ( , 2017. Similarly the Laniakea Supercluster, introduced by Tully et al (2014), is a complex of several previously known superclusters: the Local Supercluster, the Great Attractor, and some smaller cluster filaments and clouds.…”

Section: Evolution Of the Ensemble Of Superclustersmentioning

confidence: 99%

Evolution of superclusters in the cosmic web

Einasto

Suhhonenko

Liivamägi

et al. 2019

A&A

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Aims. We investigate how properties of the ensemble of superclusters in the cosmic web evolve with time. Methods. We perform numerical simulations of the evolution of the cosmic web using the ΛCDM model in box sizes L 0 = 1024, 512, 256 h −1 Mpc. We find supercluster ensembles of models for four evolutionary stages, corresponding to the present epoch z = 0, and to redshifts z = 1, z = 3, and z = 10. We calculate fitness diameters of superclusters defined from volumes of superclusters divided to filling factors of over-density regions. Geometrical and fitness diameters of largest superclusters, and the number of superclusters as functions of the threshold density are used as percolation functions to describe geometrical properties of the ensemble of superclusters in the cosmic web. We calculate distributions of geometrical and fitness diameters and luminosities of superclusters, and follow time evolution of percolation functions and supercluster distributions. We compare percolation functions and supercluster distributions of models and samples of galaxies of the Sloan Digital Sky Survey (SDSS). Results. Our analysis shows that fitness diameters of superclusters have a minimum at certain threshold density. Fitness diameters around minima almost do not change with time in co-moving coordinates. Numbers of superclusters have maxima which are approximately constant for all evolutionary epochs. Geometrical diameters of superclusters decrease during the evolution of the cosmic web; luminosities of superclusters increase during the evolution. Conclusions. Our study suggests that evolutionary changes occur inside dynamical volumes of superclusters. The stability of fitness diameters and numbers of superclusters during the evolution is an important property of the cosmic web.

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“…Thus, in order to challenge a dark energy model using the maximum size versus mass criterion, it is most effective to look into structures which lie above that transitional mass scale. We refer our reader to [11] for a discussion of the future evolution of the cosmic webs of such large masses and to [12][13][14] for a discussion of the possible violation of the maximum turn around bound by looking into the peculiar velocity profiles of members of a given structure. We further refer the reader to e.g.…”

Section: Introduction and Overviewmentioning

confidence: 99%

Cosmic structure sizes in generic dark energy models

Bhattacharya

Tomaras

2017

Eur. Phys. J. C

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The maximum allowable size of a spherical cosmic structure as a function of its mass is determined by the maximum turn around radius R TA,max , the distance from its center where the attraction on a radial test particle due to the spherical mass is balanced with the repulsion due to the ambient dark energy. In this work, we extend the existing results in several directions. (a) We first show that, for w = −1, the expression for R TA,max found earlier, using the cosmological perturbation theory, can be derived using a static geometry as well. (b) In the generic dark energy model with arbitrary time dependent state parameter w(t), taking into account the effect of inhomogeneities upon the dark energy as well, it is shown that the data constrain w(t = today) > −2.3. (c) We address the quintessence and the generalized Chaplygin gas models, both of which are shown to predict structure sizes consistent with observations.

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Sloan Great Wall as a complex of superclusters with collapsing cores

Cited by 34 publications

References 96 publications

Supercluster A2142 and collapse in action: infalling and merging groups and galaxy transformations

Supercluster A2142 and collapse in action: infalling and merging groups and galaxy transformations

Evolution of superclusters in the cosmic web

Cosmic structure sizes in generic dark energy models

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