Higher resolution simulations in smaller boxes

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Introduction: Formation and Evolution of Large Scale Stucture

Pic.1 This picture shows projected dark-matter distribution in four different model universes. It also shows the time evolution along horizontal sequence in each row. The cosmological parameters are the same as in the Virgo simulations for each model and the number of particles is also 2563, but the box size is smaller. Thus these simulations have higher mass resolution.
Credit: Kauffmann, Colberg, Diaferio, and White, ref.1

Simulation parameters

ModelOmega0lambda hGammaSigma8Npar L (Mpc/h) mp (M_sun/h) l_soft (Kpc/h)
SCDM1.00.0 0.50.500.62563 84.5 1.0 x 1010 36
tCDM1.00.0 0.50.210.62563 84.5 1.0 x 1010 36
LCDM0.30.7 0.70.210.902563 141.3 1.4 x 1010 20
OCDM0.30.0 0.70.210.852563 141.3 1.4 x 1010 30

Formation of Galaxy Clusters

Pic.2 This picture shows the same cluster from the tCDM (left panel) and LCDM (right panel) model for redshifts of 2 (top), 1 (middle), and 0 (bottom). The simulations were run with the same phases of the intial density field but the sizes of the regions are different: 21x21x8 (Mpc/h)3 and 35x35x13 (Mpc/h)3 for tCDM and LCDM, respectively.


Credit: Kauffmann, Colberg, Diaferio, and White, ref.1

Reference
  1. Clustering of Galaxies in a Hierarchical Universe: I. Methods and Results at z=0, G. Kauffmann, J.M. Colberg, A. Diaferio, S.D.M. White, 1999, MNRAS, 303, 188-206, (Preprint astro-ph/9805283)
    2. Back to     MPA/ NumCos

    Last modified: Thu Jan 13 13:10:50 MET 2000 by Virgo Administrator