Assessing the Limits of N-body Simulations of Clusters of Galaxies

Details Assessing the Limits of N-body Simulations of Clusters of Galaxies Assessing the Limits of N-body Simulations of Clusters of Galaxies

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999dda....31.0604l&link_type=abstract

American Astronomical Society, DDA meeting #31, #06.04

Mathematics

Logic

Scientific paper

I will report collisionless N-body simulations of galaxies and clusters that are formed from Cold Dark Matter Initial conditions. Among the results from these simulations are: 1) Clusters of galaxies form with roughly the right distribution of lumps, there is no overmerging problem. 2) Galaxies appear as scaled versions of clusters. They fail to overmerge and form smooth systems. Since an L* galaxy in a cluster scales to roughly an LMC within a galaxy halo, there are dozens of LMCs and thousands of dwarfs in a simulated galaxy. 3) Reports of universal profiles and ``cores" in simulations owed to poor resolution. Increasing the resolution produces profiles without cores that may well be a poor match to cosmological structure. The issue of ``cores" within N-body simulations is very interesting. Of course, a core implies a maximum phase density or a lack of information. One way to miss information is to simulate fewer particles. Just how is the maximum phase density achievable in a simulation related to the number of simulated particles? What physical mechanisms might generate the cores that (we think) we see in real systems? I will reject some of the easy answers to these questions and appeal for your collective wisdom to be brought to bear on the problem.

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