NASA Logo

NTRS

NTRS - NASA Technical Reports Server

Back to Results
percolation technique for galaxy clusteringWe study percolation in mass and galaxy distributions obtained in 3D simulations of the CDM, C + HDM, and the power law (n = -1) models in the Omega = 1 universe. Percolation statistics is used here as a quantitative measure of the degree to which a mass or galaxy distribution is of a filamentary or cellular type. The very fast code used calculates the statistics of clusters along with the direct detection of percolation. We found that the two parameters mu(infinity), characterizing the size of the largest cluster, and mu-squared, characterizing the weighted mean size of all clusters excluding the largest one, are extremely useful for evaluating the percolation threshold. An advantage of using these parameters is their low sensitivity to boundary effects. We show that both the CDM and the C + HDM models are extremely filamentary both in mass and galaxy distribution. The percolation thresholds for the mass distributions are determined.
Document ID
19930068034
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Klypin, Anatoly
(NASA Headquarters Washington, DC United States)
Shandarin, Sergei F.
(Kansas Univ. Lawrence, United States)
Date Acquired
August 16, 2013
Publication Date
August 10, 1993
Publication Information
Publication: Astrophysical Journal, Part 1
Volume: 413
Issue: 1
ISSN: 0004-637X
Subject Category
ASTROPHYSICS
Funding Number(s)
CONTRACT_GRANT: NAGW-2923
CONTRACT_GRANT: NSF AST-90-21414
Distribution Limits
Public
Copyright
Other