Multiscale cosmic web detachments, connectivity, and preprocessing in the supercluster SCl A2142 cocoon

Einasto, M.; Deshev, Boris; Tenjes, P.; Heinämäki, P.; Tempel, Elmo; Liivamägi, L. J.; Einasto, J.; Lietzen, H.; Tuvikene, T.; Chon, G.

doi:10.1051/0004-6361/202037982

Cited by 35 publications

(95 citation statements)

References 172 publications

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“…We note that the term pre-processing is commonly used in the literature to refer to all environmental effects that could affect galaxies prior to their accretion into clusters (eg. Boselli et al 2005;Wetzel et al 2012;De Lucia et al 2012;Einasto et al 2020). This is, regardless of whether the result is the cease of their star formation or not.…”

Section: Quenching Of the Star Formationmentioning

confidence: 94%

Too dense to go through: the role of low-mass clusters in the pre-processing of satellite galaxies

Pallero

Gómez

Padilla

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We study the evolution of satellite galaxies in clusters of the C-EAGLE simulations, a suite of 30 high-resolution cosmological hydrodynamical zoom-in simulations based on the EAGLE code. We find that the majority of galaxies that are quenched at z = 0 (≳ 80${{\ \rm per\ cent}}$) reached this state in a dense environment (log10M200[M⊙] ≥13.5). At low redshift, regardless of the final cluster mass, galaxies appear to reach their quenching state in low mass clusters. Moreover, galaxies quenched inside the cluster that they reside in at z = 0 are the dominant population in low-mass clusters, while galaxies quenched in a different halo dominate in the most massive clusters. When looking at clusters at z > 0.5, their in-situ quenched population dominates at all cluster masses. This suggests that galaxies are quenched inside the first cluster they fall into. After galaxies cross the cluster’s r200 they rapidly become quenched (≲ 1Gyr). Just a small fraction of galaxies ($\lesssim 15{{\ \rm per\ cent}}$) is capable of retaining their gas for a longer period of time, but after 4Gyr, almost all galaxies are quenched. This phenomenon is related to ram pressure stripping and is produced when the density of the intracluster medium reaches a threshold of ρICM ∼ 3 × 10−5 nH (cm−3). These results suggest that galaxies start a rapid-quenching phase shortly after their first infall inside r200 and that, by the time they reach r500, most of them are already quenched.

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Section: Quenching Of the Star Formationmentioning

confidence: 94%

Too dense to go through: the role of low-mass clusters in the pre-processing of satellite galaxies

Pallero

Gómez

Padilla

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…The ID numbers of the richest clusters in the high-density cores of the supercluster are shown (Abell clusters A2065, A2061, and A2089, and cluster Gr2064 that does not belong to Abell). used by Einasto et al (2018aEinasto et al ( , 2020 in the analysis of supercluster SCl A2142.…”

Section: Supercluster Group and Filament Datamentioning

confidence: 99%

“…As candidates for the centres of attraction in the high-density cores of the supercluster, we chose the richest clusters above the global luminosity density level D8 ≥ 8. This threshold density level for high-density cores of CB was chosen on the basis of earlier studies of superclusters, which showed that rich superclusters contain high-density cores, while such cores are absent in poor superclusters (Einasto et al 2007b(Einasto et al ,a, 2015(Einasto et al , 2020. We searched for rich clusters from the group catalogue with D8 ≥ 8, and selected the richest of them as possible centres of attraction in the supercluster.…”

Section: Supercluster Group and Filament Datamentioning

confidence: 99%

“…Studies of superclusters have shown that rich superclusters have high-density cores that may contain one or several rich clusters (Einasto et al 2007a(Einasto et al ,c, 2015(Einasto et al , 2016b(Einasto et al , 2020. Rich clusters in supercluster cores may be merging or be in pre-merger state, for example, in the Shapley supercluster, in the Corona Borealis supercluster, or in the Sloan Great Wall superclusters (Hanami et al 1999;de Filippis et al 2005;Belsole et al 2005;Farnsworth et al 2013;Einasto et al 2016b).…”

Section: Introductionmentioning

confidence: 99%

“…One aim of this paper is to compare the properties of the richest clusters in the CB with the properties of cluster A2142, which is the richest cluster in the supercluster SCl A2142 (Einasto et al 2015(Einasto et al , 2020. Munari et al (2016) found that cluster A2142 has a very high number of luminous galaxies that are not reproduced in simulations.…”

Section: Introductionmentioning

confidence: 99%

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The Corona Borealis supercluster: connectivity, collapse, and evolution

Einasto,

Kipper,

Tenjes

et al. 2021

Preprint

Self Cite

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Context. Rich superclusters of galaxies represent dynamically active environments in which galaxies and their systems form and evolve.Aims. We study the dynamical properties and connectivity of the richest galaxy clusters in the Corona Borealis (CB) supercluster and in the whole supercluster, and analyse star formation of galaxies in them with the aim to understand the evolution of the supercluster and the galaxies within it. We compare it with the supercluster SCl A2142. Methods. We used the luminosity-density field to determine the high-density cores of the CB. We identified the richest galaxy clusters in them and studied the dynamical state of the clusters, analysed their substructure, and studied the star formation properties of galaxies in them using normal mixture modelling and the projected phase space diagram. We determined filaments in the supercluster to analyse the connectivity of clusters. To understand the possible future evolution of the CB, we compared the mass distribution in it with predictions from the spherical collapse model and analysed the gravitational acceleration field in the CB. Results. The richest clusters in the high-density cores of the CB are the Abell clusters A2065, A2061 (together with A2067), A2089, and Gr2064. At a radius R 30 around each cluster (corresponding to the density contrast ∆ρ ≈ 30), the galaxy distribution shows a minimum. The R 30 values for individual clusters lie in the range of 3 − 6 h −1 Mpc. The radii of the clusters (splashback radii) lie in the range of R cl ≈ 2 − 3 R vir . The projected phase space diagrams and the comparison with the spherical collapse model suggest that R 30 regions have passed turnaround and are collapsing, forming infall regions around each cluster. Galaxies in the richest cluster of the CB, A2065, and in its infall region have on average younger stellar populations than other clusters and their environment. The cluster A2061 has the highest fraction of galaxies with very old stellar populations, similar to those in A2142. The number of long filaments that begin near clusters vary from one near A2089 to five near A2061. The total connectivity of these clusters (the number of infalling groups and filaments) varies from two to nine. Conclusions. During the future evolution, the clusters in the main part of the CB may merge and form one of the largest bound systems in the nearby Universe. Another part, with the cluster Gr2064, will form a separate system. Our study suggests that structures with a current characteristic density contrast ∆ρ ≈ 30 have passed turnaround and started to collapse at redshifts z ≈ 0.3 − 0.4. The comparison of the number and properties of the most massive collapsing supercluster cores from observations and simulations may serve as a test for cosmological models.

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Evolution of superclusters and supercluster cocoons in various cosmologies

Einasto

Hütsi

Suhhonenko

et al. 2021

A&A

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Aims. We investigate the evolution of superclusters and supercluster cocoons (basins of attraction), and the effect of cosmological parameters on the evolution. Methods. We performed numerical simulations of the evolution of the cosmic web for different cosmological models: the Λ cold dark matter (LCDM) model with a conventional value of the dark energy (DE) density, the open model OCDM with no DE, the standard SCDM model with no DE, and the hyper-DE HCDM model with an enhanced DE density value. We find ensembles of superclusters of these models for five evolutionary stages, corresponding to the present epoch z = 0, and to redshifts z = 1, 3, 10, and 30. We used the diameters of the largest superclusters and the number of superclusters as percolation functions to describe the properties of the ensemble of superclusters in the cosmic web. We analysed the size and mass distribution of superclusters in models and in real samples based on the Sloan Digital Sky Survey. Results. In all models, the numbers and volumes of supercluster cocoons are independent of the cosmological epochs. The supercluster masses increase with time and the geometrical sizes in comoving coordinates decrease with time for all models. The LCDM, OCDM, and HCDM models have almost similar percolation parameters. This suggests that the essential parameter, which defines the evolution of superclusters, is the matter density. The DE density affects the growth of the amplitude of density perturbations and the growth of masses of superclusters, but significantly weaker. The HCDM model has the highest speed of the growth of the density fluctuation amplitude and the largest growth of supercluster masses during the evolution. The geometrical diameters and the numbers of HCDM superclusters at high threshold densities are larger than for the LCDM and OCDM superclusters. The SCDM model has about twice as many superclusters as other models, and the SCDM superclusters have smaller diameters and lower masses. Conclusions. We find that supercluster embryos form at very early cosmological epochs and that the evolution of superclusters occurs mainly inside their cocoons. The evolution of superclusters and their cocoons as derived from density fields agress well with the evolution found from velocity fields.

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Multiscale cosmic web detachments, connectivity, and preprocessing in the supercluster SCl A2142 cocoon

Cited by 35 publications

References 172 publications

Too dense to go through: the role of low-mass clusters in the pre-processing of satellite galaxies

Too dense to go through: the role of low-mass clusters in the pre-processing of satellite galaxies

The Corona Borealis supercluster: connectivity, collapse, and evolution

Evolution of superclusters and supercluster cocoons in various cosmologies

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