Open AccessLinking cluster formation to large‐scale structure
Author(s) -
Colberg J. M.,
White S. D. M.,
Jenkins A.,
Pearce F. R.
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.1365-8711.1999.02400.x
Subject(s) - physics , cluster (spacecraft) , astrophysics , mass distribution , structure formation , galaxy cluster , cold dark matter , universe , dark matter , homogeneous , galaxy , scale (ratio) , cluster analysis , statistical physics , quantum mechanics , computer science , programming language , machine learning
We use two high‐resolution cold dark matter (CDM) simulations to investigate how the formation of clusters of galaxies is related to the distribution of the surrounding mass. It is well known that in CDM universes objects grow in a hierarchical fashion. This process cannot be completely independent of its environment. We show that when clusters form the infall pattern is not random, but shows clear features, which are correlated in time. In addition, this infall pattern correlates with the large‐scale structure (LSS) surrounding the cluster. Thus LSS not only exerts a tidal field on clustering but also specifies preferred directions from which clusters are built up. We extend this point of view and study the distribution of mass outside the clusters. We find that LSS shows a mix of both filaments and sheets, which can be clearly identified using the representation chosen for this study. Filaments and sheets appear to be clumpy rather than homogeneous. Having identified filaments we obtain mass estimates for them. We show that the mass fraction in filaments is slightly larger in a low‐density universe.