Open AccessSuperlarge‐scale structure in N ‐body simulations
Author(s) -
Doroshkevich A. G.,
Müller V.,
Retzlaff J.,
Turchaninov V.
Publication year - 1999
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.1999.02531.x
Subject(s) - physics , omega , astrophysics , spectral density , spectral line , anisotropy , galaxy cluster , structure formation , dark matter , statistical physics , mass distribution , galaxy , statistics , quantum mechanics , mathematics
The simulated matter distribution on large scales is studied using core‐sampling, cluster analysis, inertia tensor analysis and minimal spanning tree techniques. Seven simulations in large boxes for five cosmological models with COBE ‐normalized CDM‐like power spectra are studied. A wall‐like superlarge‐scale structure with parameters similar to the observed one is found for the OCDM and ΛCDM models with Ο m h = 0.2−0.3. In these simulations, the rich structure elements with a typical value for the largest extension of ∼(30 − 50) h −1 Mpc incorporate ∼40 per cent of matter with overdensity of about 10 above the mean. These rich elements are formed by the anisotropic non‐linear compression of sheets with an original size of ∼(15−25) h −1 Mpc. They surround low‐density regions with a typical diameter ∼(50−70) h −1 Mpc. The statistical characteristics of these structures are found to be approximately consistent with observations and theoretical expectations. The cosmological models with higher matter density Ω m =1 in CDM with Harrison–Zeldovich or tilted power spectra cannot reproduce the characteristics of the observed galaxy distribution because of the very strong disruption of the rich structure elements. Another model with a broken scale‐invariant initial power spectrum (BCDM) does not show enough matter concentration in the rich structure elements.