Observations and Morphology of the Cosmic Web

Weygaert, Rien van de; Bond, J. R.

doi:10.1007/978-1-4020-6941-3_11

Cited by 28 publications

(25 citation statements)

References 162 publications

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“…They form at the interception of filaments and/or walls, where the galaxy density is larger and where infall is strongest (eg., van de Weygaert & Bond 2008, Kravtsov & Borgani 2012. They contain from a few tens to a few thousands of galaxies.…”

Section: Introductionmentioning

confidence: 99%

Galaxy cluster's rotation

Manolopoulou

Plionis

2016

Mon. Not. R. Astron. Soc.

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We study the possible rotation of cluster galaxies, developing, testing and applying a novel algorithm which identifies rotation, if such does exist, as well as its rotational centre, its axis orientation, rotational velocity amplitude and, finally, the clockwise or counterclockwise direction of rotation on the plane of the sky. To validate our algorithms we construct realistic Monte Carlo mock rotating clusters and confirm that our method provides robust indications of rotation. We then apply our methodology on a sample of Abell clusters with z 0.1 with member galaxies selected from the Sloan Digital Sky Survey (SDSS) DR10 spectroscopic data base. After excluding a number of substructured clusters, which could provide erroneous indications of rotation, and taking into account the expected fraction of misidentified coherent substructure velocities for rotation, provided by our Monte-Carlo simulation analysis, we find that ∼ 23% of our clusters are rotating under a set of strict criteria. Loosening the strictness of the criteria, on the expense of introducing spurious rotation indications, we find this fraction increasing to ∼ 28%. We correlate our rotation indicators with the cluster dynamical state, provided either by their Bautz-Morgan type or by their Xray isophotal shape and find for those clusters showing rotation within 1.5 h −1 70 Mpc that the significance of their rotation is related to the dynamically younger phases of cluster formation but after the initial anisotropic accretion and merging has been completed. Finally, finding rotational modes in galaxy clusters could lead to the necessity of correcting the dynamical cluster mass calculations.

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Section: Introductionmentioning

confidence: 99%

Galaxy cluster's rotation

Manolopoulou

Plionis

2016

Mon. Not. R. Astron. Soc.

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“…Thus, in essence, the outcome of these processes is that gravitational collapse naturally produces a filamentary topology, which accounts for the overall topology of the cosmic web on the largest scales, revealed both by numerical simulations and observations (e.g. Klypin & Shandarin, 1983;Van de Weygaert & Bond, 2008;Klar & Mücket, 2010;Eckert et al, 2015;Gheller et al, 2015). Note that sheets and filaments of matter appear in many other Astrophysical contexts too.…”

Section: Global Cosmological Model: Some Elementsmentioning

confidence: 99%

Baryonic Processes in the Large-Scale Structuring of the Universe

Durrive

2017

Springer Theses

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“…For furthering our understanding of the Cosmic Web, and to 2 Because of the expansion of the Universe, any observed cosmic object will have its light shifted redward: its redshift z. According to Hubble's law, the redshift z is directly proportional to the distance r of the object, for z 1: cz = Hr (with c the velocity of light, and H ≈ 71km/s/M pc the Hubble constant).…”

Section: Topology Of the Cosmic Density Fieldmentioning

confidence: 99%

“…Galaxies and mass exist in a wispy weblike spatial arrangement consisting of dense compact clusters, elongated filaments, and sheetlike walls, amidst large near-empty void regions, with similar patterns existing at earlier epochs, albeit over smaller scales. The hierarchical nature of this mass distribution, marked by substructure over a wide range of scales and densities, has been clearly demonstrated [2]. Its appearance has been most dramatically illustrated by the recently produced maps of the nearby cosmos, the 2dFGRS, 1 The main measure of length in astronomy is the parsec.…”

Section: Introduction: the Cosmic Webmentioning

confidence: 97%

Alpha Shape Topology of the Cosmic Web

Weygaert

Platen

Vegter

et al. 2010

2010 International Symposium on Voronoi Diagrams in Science and Engineering

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We study the topology of the Megaparsec Cosmic Web on the basis of the Alpha Shapes of the galaxy distribution. The simplicial complexes of the alpha shapes are used to determine the set of Betti numbers (β k , k = 1, . . . , D), which represent a complete characterization of the topology of a manifold. This forms a useful extension of the geometry and topology of the galaxy distribution by Minkowski functionals, of which three specify the geometrical structure of surfaces and one, the Euler characteristic, represents merely a summary of its topology. In order to develop an intuitive understanding for the relation between Betti numbers and the running α parameter of the alpha shapes, and thus in how far they may discriminate between different topologies, we study them within the context of simple heuristic Voronoi clustering models. These may be tuned to consist of a few or even only one specific morphological element of the Cosmic Web, ie. clusters, filaments or sheets.

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Observations and Morphology of the Cosmic Web

Cited by 28 publications

References 162 publications

Galaxy cluster's rotation

Galaxy cluster's rotation

Baryonic Processes in the Large-Scale Structuring of the Universe

Alpha Shape Topology of the Cosmic Web

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