Small Scale Structure in Dark Matter Models and Consequences for Galaxy Formation

Details Small Scale Structure in Dark Matter Models and Consequences for Galaxy Formation Small Scale Structure in Dark Matter Models and Consequences for Galaxy Formation

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dmap.conf..327p&link_type=abstract

DARK MATTER IN ASTROPARTICLE AND PARTICLE PHYSICS. Proceedings of the 6th International Heidelberg Conference. Held 24-28 Septem

Physics

Cosmology, Dark Matter, N-Body Simulations, Galaxy Formation

Scientific paper

A defining prediction of the Cold Dark Matter (CDM) model of cosmological structure formation is that the number density of low-mass dark matter haloes - or small scale structure - is large and increasing with decreasing mass. Using cosmological N-body simulations, we have studied truncated dark matter models in which low-mass halo formation is suppressed below a mass cut-off scale Mcut, which we vary between 5 × 109h-1M&sun; and 1011h-1M&sun;. We assess the impact of the mass cut-off on dark matter halo clustering, mass assembly and angular momentum growth on galaxy and group-mass scales compared to a fiducial ΛCDM model. As we would expect, the number density of haloes with masses M ≥ Mcut in truncated dark matter models is suppressed relative to the ΛCDM model. This leads to a reduction in the number density of low-mass haloes around galaxy- and group-mass haloes, and consequently a reduction in the frequency of minor mergers experienced by these systems. However, we find no significant differences between the angular momenta of galaxy- and group-mass haloes in truncated models when compared with those in the ΛCDM model. We consider the implications of this for our understanding of the growth of halo angular momentum and as a potential tests of the CDM paradigm.

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