The structure of galaxy clusters in various cosmologies
P. ThomasAstronomy Centre , University of Sussex , Falmer , Brighton BN1 9QHJ. M. ColbergMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85740, Garching bei München, GermanyHugh CouchmanDepartment of Physics & Astronomy , University of Western Ontario , London , Ontario , N6A 3K7 , CanadaG. EfstathiouDepartment of Astrophysics , Nuclear & Astrophysics Laboratory , Keble Road , Oxford OX1 3RHCarlos S. FrenkDepartment of Physics , South Road , Durham DH1 3LEAdrian JenkinsDepartment of Physics , South Road , Durham DH1 3LEA. H. NelsonDept of Physics, College of Cardiff, PO Box 913, Cardiff CF4 3THR. HutchingsAstronomy Centre , University of Sussex , Falmer , Brighton BN1 9QHJ. A. PeacockRoyal Observatory Edinburgh , Blackford Hill , Edinburgh EH9 3HJF. R. PearceDepartment of Physics , South Road , Durham DH1 3LESimon D. M. WhiteMax-Planck-Institut fu ¨r Astrophysik , Karl-Schwarzschild-Strasse 1 , 85740 , Garching bei Mu ¨nchen , Germany
1998en
ABI
Abstract
We investigate the internal structure of clusters of galaxies in high-resolution N-body simulations of four different cosmologies. There is a higher proportion of disordered clusters in critical-density than in low-density universes, although the structure of relaxed clusters is very similar in each case. Crude measures of substructure, such as the shift in the position of the centre-of-mass as the density threshold is varied, can distinguish the two in a sample of just 20 or so clusters; it is harder to differentiate between clusters in open and flat models with the same density parameter. Most clusters are in a quasi-steady state within the virial radius and are well-described by the density profile of Navarro, Frenk & White.
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