1993/11/17 by August E. Evrard, Evrard, August E.
Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9311042
14 pages, compressed uuencoded postscript (with four figures), UM-AC-93-17 (review presented at the 1st UNAM/CRAY Workshop ``Modelling the Dynamics of the Universe'', Mexico City, July 1993)
arxiv created 1993/11/17 · arxiv updated 2009/12/01
The abundance and internal characteristics of rich clusters of galaxies can provide useful constraints on models of large--scale structure formation. This article will review some recent three dimensional, multi--fluid simulations of cluster dynamics and discuss their impact on issues raised from optical and X-ray observations of clusters. In `bottom--up' formation scenarios (such as the ubiquitous cold dark matter model), galaxies form before rich clusters; hence, cluster formation is intimately linked to galaxy formation which, in turn, is tied to star formation. I will examine two issues which appear relatively insensitive to galaxy/star formation --- the baryon fraction in clusters and the connection between X--ray morphology and Ωo --- and end with a topic that is intimately linked to it --- dynamical biases in the cluster galaxy population.