The Corona Borealis supercluster: connectivity, collapse, and evolution

Einasto, M.; Kipper, Rain; Tenjes, P.; Lietzen, H.; Tempel, Elmo; Liivamägi, L. J.; Einasto, J.; Tamm, A.; Heinämäki, P.; Nurmi, P.

doi:10.1051/0004-6361/202040200

Cited by 18 publications

(34 citation statements)

References 148 publications

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“…We can look at the HDCs of superclusters as future rich clusters that are presently still forming. In the local superclusters, such HDCs with several rich clusters that may merge in the future have been found, for example, in the Corona Borealis supercluster (Einasto et al 2021b), and in the Shapley supercluster (de Filippis et al 2005). The cores of the BGW superclusters may represent such systems.…”

Section: Evolution Of Superclusters In the Cosmic Webmentioning

confidence: 98%

“…The density contrast at the borders of the spheres of influence is ∆ρ ≈ 30. Einasto et al (2020) and Einasto et al (2021b) found that the spheres of influence passed the turnaround and started to collapse at redshifts z ≈ 0.4, approximately at the redshift of the BGW. We may assume that the HDCs of the BGW superclusters may be considered the progenitors of the spheres of influence around clusters in the HDCs of local superclusters.…”

Section: Comparison With Local Superclustersmentioning

confidence: 99%

“…To compare the masses and radii of the HDCs in the BGW (at redshift z = 0.5) and local superclusters (at redshift z = 0) in Fig. 10, we used data regarding the two richest superclusters in the SGW (Einasto et al 2016), the Corona Borealis (CorBor) supercluster (Einasto et al 2021b), and the supercluster SCl A2142 (Einasto et al 2018). The SGW is a complex of two rich and three poor superclusters.…”

Section: Comparison With Local Superclustersmentioning

confidence: 99%

“…We can use another estimate based on the spheres of influence around rich clusters in superclusters. Einasto et al (2020) and Einasto et al (2021b) showed that rich clusters in the HDCs of supercluster SCl A2142 and the Corona Borealis are surrounded by a sphere of influence, where all galaxies and A&A proofs: manuscript no. AA42938 groups of galaxies are infalling towards clusters.…”

Section: Comparison With Local Superclustersmentioning

confidence: 99%

“…The positions of highdensity peaks and voids do not change much during the cosmic evolution, only the amplitude of over-and under-densities grows with time (Bond et al 1996;van de Weygaert & Schaap 2009;Suhhonenko et al 2011;Einasto et al 2019, 2021a, and Send offprint requests to: Einasto, M. references therein). Superclusters or their HDCs are the largest systems in the cosmic web that may eventually collapse (de Vaucouleurs 1956;Jõeveer et al 1978;Einasto et al 2015;Chon et al 2015;Lietzen et al 2016;Einasto et al 2016Einasto et al , 2018Einasto et al , 2021b.…”

Section: Introductionmentioning

confidence: 99%

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The evolution of high-density cores of the BOSS Great Wall superclusters

Einasto,

Tenjes,

Gramann

et al. 2022

Preprint

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Context. High-density cores (HDCs) of galaxy superclusters that embed rich clusters and groups of galaxies are the earliest large objects to form in the cosmic web, and the largest objects that may collapse in the present or future. Aims. We aim to study the dynamical state and possible evolution of the HDCs in the BOSS Great Wall (BGW) superclusters at redshift z ≈ 0.5 from the CMASS (constant mass) galaxy sample, based on the Baryon Oscillation Spectroscopic Survey (BOSS) in order to understand the growth and evolution of structures in the Universe. Methods. We analysed the luminosity density distribution in the BGW superclusters to determine the HDCs in them. We derived the density contrast values for the spherical collapse model in a wide range of redshifts and used these values to study the dynamical state and possible evolution of the HDCs of the BGW superclusters. The masses of the HDCs were calculated using stellar masses of galaxies in them. We found the masses and radii of the turnaround and future collapse regions in the HDCs of the BGW superclusters and compared them with those of local superclusters. Results. We determined eight HDCs in the BGW superclusters. The masses of their turnaround regions are in the range of M T ≈ 0.4 − 3.3 × 10 15 h −1 M ⊙ , and radii are in the range of R T ≈ 3.5 − 7 h −1 Mpc. The radii of their future collapse regions are in the range of R FC ≈ 4 − 8 h −1 Mpc. Distances between individual cores in superclusters are much larger: of the order of 25 − 35 h −1 Mpc. The richness and sizes of the HDCs are comparable with those of the HDCs of the richest superclusters in the local Universe. Conclusions. The BGW superclusters will probably evolve to several poorer superclusters with masses similar to those of the local superclusters. This may weaken the tension with the ΛCDM model, which does not predict a large number of very rich and large superclusters in our local cosmic neighbourhood, and explains why there are no superclusters as elongated as those in the BGW in the local Universe.

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Section: Evolution Of Superclusters In the Cosmic Webmentioning

confidence: 98%

Section: Comparison With Local Superclustersmentioning

confidence: 99%

Section: Comparison With Local Superclustersmentioning

confidence: 99%

Section: Comparison With Local Superclustersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The evolution of high-density cores of the BOSS Great Wall superclusters

Einasto,

Tenjes,

Gramann

et al. 2022

Preprint

Self Cite

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The evolution of high-density cores of the BOSS Great Wall superclusters

Einasto

Tenjes

Gramann

et al. 2022

A&A

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Context. High-density cores (HDCs) of galaxy superclusters that embed rich clusters and groups of galaxies are the earliest large objects to form in the cosmic web, and the largest objects that may collapse in the present or future. Aims. We aim to study the dynamical state and possible evolution of the HDCs in the BOSS Great Wall (BGW) superclusters at redshift z ≈ 0.5 from the CMASS (constant mass) galaxy sample, based on the Baryon Oscillation Spectroscopic Survey (BOSS) in order to understand the growth and evolution of structures in the Universe. Methods. We analysed the luminosity density distribution in the BGW superclusters to determine the HDCs in them. We derived the density contrast values for the spherical collapse model in a wide range of redshifts and used these values to study the dynamical state and possible evolution of the HDCs of the BGW superclusters. The masses of the HDCs were calculated using stellar masses of galaxies in them. We found the masses and radii of the turnaround and future collapse regions in the HDCs of the BGW superclusters and compared them with those of local superclusters. Results. We determined eight HDCs in the BGW superclusters. The masses of their turnaround regions are in the range of MT ≈ 0.4–3.3 × 1015 h−1 M⊙, and radii are in the range of RT ≈ 3.5–7 h−1 Mpc. The radii of their future collapse regions are in the range of RFC ≈ 4–8 h−1 Mpc. Distances between individual cores in superclusters are much larger: of the order of 25–35 h−1 Mpc. The richness and sizes of the HDCs are comparable with those of the HDCs of the richest superclusters in the local Universe. Conclusions. The BGW superclusters will probably evolve to several poorer superclusters with masses similar to those of the local superclusters. This may weaken the tension with the ΛCDM model, which does not predict a large number of very rich and large superclusters in our local cosmic neighbourhood, and explains why there are no superclusters as elongated as those in the BGW in the local Universe.

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Quasi-spherical superclusters

Heinämäki

Teerikorpi

Douspis

et al. 2022

A&A

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Context. Superclusters are systems with varied properties and varied fractional overdensities. Their dynamical state evolves under the influence of two components: dark energy and gravitational force. The dominant component at any spatial location and cosmic epoch is determined by the total mass and the local overdensity of the system. However, generally the dynamical state of superclusters is poorly known. Aims. We study properties of superclusters and select a sample of quasi-spherical superclusters, the dynamics of which can be studied using the Λ significance diagram. Methods. We extracted our supercluster sample with an adaptive local threshold density method from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) data and estimated their masses using the dynamical masses for member galaxies and groups. We used topological analysis based on Minkowski functionals and the positions of galaxies and galaxy groups in superclusters. Finally, we highlight the dynamical state of a few exceptional types of superclusters found in this study using the Λ significance diagram. Results. Our final sample contains 65 superclusters in the distance range of 130 to 450 Mpc. Supercluster masses range between 1.1 × 10 15 M and 1.4 × 10 16 M and sizes between 25 Mpc and 87 Mpc. We find that pancake-type superclusters form the lowluminosity, small, poor and low-mass end of superclusters. We find four superclusters of unusual types, exhibiting exceptionally spherical shapes. These so-called quasi-spherical systems contain a high-density core surrounded by a relatively spherical density and galaxy distribution. The mass-to-light ratio of these quasi-sphericals is higher than those of the other superclusters, suggesting a relatively high dark matter content. Using the Λ significance diagram for oblate and prolate spheroids, we find that three quasispherical superclusters are gravitationally bound at the present epoch. Conclusions. Quasi-spherical superclusters are among the largest gravitationally bound systems found to date, and form a special class of giant systems that, dynamically, are in between large gravitationally unbound superclusters and clusters of galaxies in an equilibrium configuration.

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The Corona Borealis supercluster: connectivity, collapse, and evolution

Cited by 18 publications

References 148 publications

The evolution of high-density cores of the BOSS Great Wall superclusters

The evolution of high-density cores of the BOSS Great Wall superclusters

The evolution of high-density cores of the BOSS Great Wall superclusters

Quasi-spherical superclusters

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