The Ellipticity and Orientation of Clusters of Galaxies from N-Body Experiments

Details The Ellipticity and Orientation of Clusters of Galaxies from N-Body Experiments The Ellipticity and Orientation of Clusters of Galaxies from N-Body Experiments

1996-07-28

arxiv.org/abs/astro-ph/9607144v2

Astrophys.J.479:632-641,1997

Astronomy and Astrophysics

Astrophysics

22 pages, requires aaspp4.sty, flushrt.sty, and epsf.sty Revised manuscript, accepted for publication in ApJ

Scientific paper

10.1086/303896

In this study we use simulations of 128$^3$ particles to study the ellipticity and orientation of clusters of galaxies in N-body simulations of differing power-law initial spectra (P(k) \propto k^n ,n = +1, 0, -1, -2$), and density parameters ($\Omega_0 = 0.2$ to 1.0). Furthermore, unlike most theoretical studies we mimic most observers by removing all particles which lie at distances greater than 2 1/h Mpc from the cluster center of mass. We computed the axial ratio and the principal axes using the inertia tensor of each cluster. The mean ellipticity of clusters increases strongly with increasing $n$. We also find that clusters tend to become more spherical at smaller radii. We compared the orientation of a cluster to the orientation of neighboring clusters as a function of distance (correlation). In addition, we considered whether a cluster's major axis tends to lie along the line connecting it to a neighboring cluster, as a function of distance (alignment). Both alignments and correlations were computed in three dimensions and in projection to mimic observational surveys. Our results show that significant alignments exist for all spectra at small separations ($D < 15 h^{-1}$ Mpc) but drops off at larger distance in a strongly $n-$dependent way.

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