Numerical simulations of merging galaxy clusters

Details Numerical simulations of merging galaxy clusters Numerical simulations of merging galaxy clusters

Feb 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apl%26c..33..213p&link_type=abstract

Astrophysical Letters and Communications, 1996, vol. 33, pp. 213-216

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Scientific paper

There are observational hints that galaxy clusters may lie close to a Fundamental Plane (FP) in the space of their basic observables, total luminosity, effective radius and velocity dispersion, just as elliptical galaxies do. Seemingly, a transformation of coordinates into the (k1,k2,k3) coordinate system is possible: for fixed k1, there appears to be a small dispersion of k3 (i.e. of M/L). On the other hand merging of clusters results on temporary departures from virial equilibrium, and therefore tends to increase the dispersion about the FP. By means of N-body simulations and with a set of different initial distributions, we study the evolution of clusters in the k-space during merging processes, thus setting an upper limit for the recent merging rate from the observed FP thickness.

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