Understanding the PSCz Galaxy Power Spectrum with N-body Simulations

Abstract

By comparing the PSCz galaxy power spectrum with the results of nested pure dark matter N-body simulations, we try to understand how infrared-selected galaxies populate dark-matter haloes, paying special attention to the method of halo identification in the simulations. We thus test the hypothesis that baryonic physics negligibly affects the distribution of galaxies down to the smallest scales yet observed. We are successful in reproducing the PSCz power spectrum on scales < ~40 h/Mpc, near our resolution limit, by imposing a central density cut-off on simulated haloes, which gives a rough minimum mass and circular velocity of haloes in which PSCz galaxies formed.

12 pages, 16 figures (one added), conforms to version in MNRAS

References in corpus (3)

• Halo Models of Large Scale Structure
• The Halo Occupation Distribution and the Physics of Galaxy Formation
• Substructure and the halo model of large-scale structure

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