The cosmic web for density perturbations of various scales

Suhhonenko, I.; Einasto, J.; Liivamägi, L. J.; Saar, E.; Einasto, M.; Hütsi, Gert; Müller, V.; Starobinsky, Alexei A.; Tago, E.; Tempel, Elmo

doi:10.1051/0004-6361/201016394

Cited by 36 publications

(38 citation statements)

References 79 publications

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“…During the structure formation in the Universe, halo sizes in the supercluster core regions increase, while in void regions halo sizes remain unchanged (Tempel et al 2009). Thus, during the evolution of structure the overall density in superclusters increases, which enhances the evolution of the small-scale protohalos in them (Suhhonenko et al 2011). This may lead to the differences in the properties of galaxy groups and galaxies in them in superclusters and in the field.…”

Section: Discussionmentioning

confidence: 99%

SDSS superclusters: morphology and galaxy content

Einasto

Lietzen

Tempel

et al. 2014

A&A

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Context. Understanding the formation, evolution and present-day properties of the cosmic web and objects forming it is an important task in cosmology. Aims. We compare the galaxy populations in superclusters of different morphology in the nearby Universe (180 h −1 Mpc ≤ d ≤ 270 h −1 Mpc) to see whether the inner structure and overall morphology of superclusters are important in shaping galaxy properties in superclusters. Methods. We find supercluster morphology with Minkowski functionals and analyse the probability density distributions of colours, morphological types, stellar masses, star formation rate (SFR) of galaxies, and the peculiar velocities of the main galaxies in groups in superclusters of filament and spider types, and in the field. We test the statistical significance of the results with the KS test. Results. The fraction of red, early-type, low SFR galaxies in filament-type superclusters is higher than in spider-type superclusters; in low-density global environments their fraction is lower than in superclusters. In all environments the fraction of red, high stellar mass, and low SFR galaxies in rich groups is higher than in poor groups. In superclusters of spider morphology red, high SFR galaxies have higher stellar masses than in filament-type superclusters. Groups of equal richness host galaxies with larger stellar masses, a larger fraction of early-type and red galaxies, and a higher fraction of low SFR galaxies, if they are located in superclusters of filament morphology. The peculiar velocities of the main galaxies in groups from superclusters of filament morphology are higher than in those of spider morphology. Groups with higher peculiar velocities of their main galaxies in filament-type superclusters are located in higher density environment than those with low peculiar velocities. There are significant differences between galaxy populations of the individual richest superclusters. Conclusions. Both local (group) and global (supercluster) environments and even supercluster morphology play an important role in the formation and evolution of galaxies. Differences in the inner structure of superclusters of filament and spider morphology and the dynamical state of galaxy groups in them may lead to the differences found in our study.

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Section: Discussionmentioning

confidence: 99%

SDSS superclusters: morphology and galaxy content

Einasto

Lietzen

Tempel

et al. 2014

A&A

Self Cite

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“…It is generally assumed that the maximal size of these structures is 100−150 Mpc (Frisch et al 1995;Einasto et al 1997;Suhhonenko et al 2011;Aragon-Calvo & Szalay 2013). Quite recently Tully et al (2014) discovered the local supercluster (the "Laniakea") having a diameter of 320 Mpc.…”

Section: Formation Of the Ringmentioning

confidence: 99%

“…Some concern may arise, however, concerning the interpretation of the ring as a true physical structure, and of the causal relationship between the GRBs displaying it. Suhhonenko et al (2011) has pointed out that cosmic structures greater than 140 Mpc in co-moving coordinates did not communicate with one another during the late stage of universal expansion preceding Recombination. The skeleton of the web was created during the inflationary period (Kofman & Shandarin 1988) and evolved slowly following this epoch.…”

Section: Spatial Distribution Of Grbs and Large Scale Structure Of Thmentioning

confidence: 99%

A giant ring-like structure at 0.78 < z < 0.86 displayed by GRBs

Balázs

Bagoly

Hakkila

et al. 2015

Mon. Not. R. Astron. Soc.

127

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According to the cosmological principle, Universal large-scale structure is homogeneous and isotropic. The observable Universe, however, shows complex structures even on very large scales. The recent discoveries of structures significantly exceeding the transition scale of 370 Mpc pose a challenge to the cosmological principle.We report here the discovery of the largest regular formation in the observable Universe; a ring with a diameter of 1720 Mpc, displayed by 9 gamma ray bursts (GRBs), exceeding by a factor of five the transition scale to the homogeneous and isotropic distribution. The ring has a major diameter of 43 o and a minor diameter of 30 o at a distance of 2770 Mpc in the 0.78 < z < 0.86 redshift range, with a probability of 2 × 10 −6 of being the result of a random fluctuation in the GRB count rate.Evidence suggests that this feature is the projection of a shell onto the plane of the sky. Voids and string-like formations are common outcomes of large-scale structure. However, these structures have maximum sizes of 150 Mpc, which are an order of magnitude smaller than the observed GRB ring diameter. Evidence in support of the shell interpretation requires that temporal information of the transient GRBs be included in the analysis.This ring-shaped feature is large enough to contradict the cosmological principle. The physical mechanism responsible for causing it is unknown.

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“…In a forthcoming paper we will search for characteristic scales in the distribution of galaxy groups and clusters in more detail. Einasto et al (2011a,b) and Suhhonenko et al (2011) showed how the density waves of different scales affect the richness of galaxy systems. Rich galaxy clusters and high-density cores of superclusters form in regions of high environmental density, where positive sections of medium-and large-scale density perturbations combine.…”

Section: The Shape Of Superclusters As a Test For Cosmological Modelsmentioning

confidence: 99%

Unusual A2142 supercluster with a collapsing core: distribution of light and mass

Einasto

Gramann

Saar

et al. 2015

A&A

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Context. Superclusters of galaxies can be used to test cosmological models of the formation and evolution of the largest structures in the cosmic web, and of galaxy and cluster evolution in superclusters. Aims. We study the distribution, masses, and dynamical properties of galaxy groups in the A2142 supercluster. Methods. We analyse the global luminosity density distribution in the supercluster and divide the supercluster into the high-density core and the low-density outskirts regions. We find galaxy groups and filaments in these regions, calculate their masses and mass-tolight ratios and analyse their dynamical state with 1D and 3D statistics. We use the spherical collapse model to study the dynamical state of the supercluster. Results. In the A2142 supercluster rich groups and clusters lie along an almost straight line forming the 50 h −1 Mpc long main body of the supercluster. The A2142 supercluster has a very high density core surrounded by lower-density outskirts. The total estimated mass of the supercluster is M est = 6.2 × 10 15 M . More than a half of groups with at least ten member galaxies in the supercluster lie in the high-density core of the supercluster, centred at the X-ray cluster A2142. Most of the groups in the core region are multimodal. In the outskirts of the supercluster, the number of groups is larger than in the core, and groups are poorer. The orientation of the axis of the cluster A2142 follows the orientations of its X-ray substructures and radio halo, and is aligned along the supercluster axis. The high-density core of the supercluster with the global density D8 ≥ 17 and perhaps with D8 ≥ 13 may have started to collapse. Conclusions. A2142 supercluster with collapsing core and straight body, is an unusual object among superclusters. In the course of the future evolution, the supercluster may split into several systems.

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The cosmic web for density perturbations of various scales

Cited by 36 publications

References 79 publications

SDSS superclusters: morphology and galaxy content

SDSS superclusters: morphology and galaxy content

A giant ring-like structure at 0.78 < z < 0.86 displayed by GRBs

Unusual A2142 supercluster with a collapsing core: distribution of light and mass

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