Other
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.7904b&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #79.04; Bulletin of the American Astronomical Society, Vol. 24, p.1248
Other
Scientific paper
We present results of a new high resolution N-body simulation in which we follow the growth of a massive dark galaxy halo in a region of low mass density. A standard cold dark matter universe (Omega = 1, Lambda = 0, H_0 = 100 h(-1) Mpc, h = 1/2) is assumed. We use J. V. Villumsen's Hierarchical Particle Mesh (HPM) code in which large dynamic ranges in mass and length are obtained by nesting one or more ``subgrids'' inside the main simulation volume (the ``top grid''). The HPM code thus achieves a ``power zoom'' effect with which one can look at smaller and smaller regions of the simulation at higher and higher resolution. We use a three-level calculation (a top grid with one subgrid nested inside another subgrid) to examine in detail the growth of a large density fluctuation. The top grid is 40 h(-1) Mpc on a side, the first subgrid is 6.67 h(-1) Mpc on a side, and the second subgrid is 1.11 h(-1) Mpc on a side. In all cases 128(3) grid cells are used and, thus, the smallest length scale we can resolve is that of one grid cell in the second subgrid: 8.68 h(-1) kpc. In the top grid 64(3) particles of mass m_p = 1.36 times 10(11) Msun are used, and in the subgrids ~ 10(5) particles of mass m_p = 6.28 times 10(8) Msun (subgrid 1) and ~ 10(6) particles of mass m_p = 2.91 times 10(6) Msun (subgrid 2) are used. Subgrid 1 is located in a low density region of the top grid (mass density ~ 0.3 times the mean density of the simulation at the end of the simulation). Subgrid 2 follows the growth of the largest density fluctuation in subgrid 1 (mass density ~ 4 times the mean density of the simulation at the end of the simulation). In subgrid 2 a dark ``halo'' is located using a friends-of-friends algorithm with a linking parameter of 0.2. At an epoch corresponding to 1/sigma_8 = 2.5 , the halo consists of ~ 5.1 times 10(5) particles (M_halo ~ 1.5 times 10(12) Msun) and significant substructure is visible. By 1/sigma_8 = 1.5 the halo consists of ~ 7.4 times 10(5) particles (M_halo ~ 2.1 times 10(12) Msun) and much less substructure is apparent. The halo grows both by infall of mass and by ``cannibalism'' of smaller halos in its vicinity.
Brainerd Tereasa G.
Villumsen Jens V.
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