The Evolution of Dark Matter Halo Properties in Clusters, Filaments, Sheets and Voids

Details The Evolution of Dark Matter Halo Properties in Clusters, Filaments, Sheets and Voids The Evolution of Dark Matter Halo Properties in Clusters, Filaments, Sheets and Voids

2007-04-19

arxiv.org/abs/0704.2595v2

Astronomy and Astrophysics

Astrophysics

12 pages, 12 figures. Version accepted for publication in MNRAS. Version with high-resolution figures available at http://ww

Scientific paper

10.1111/j.1365-2966.2007.12249.x

We use a series of N-body simulations of the LCDM cosmology to investigate the redshift evolution since z=1 of the properties and alignment with the large-scale structure of haloes in clusters, filaments, sheets and voids. We find that: (i) Once a rescaling of the halo mass with M*, the mass scale collapsing at redshift z, is performed, there is no further significant redshift dependence in the halo properties; (ii) The environment influences halo shape and formation time at all investigated redshifts for haloes with masses MM* in filaments spin more rapidly than similar mass haloes in clusters; haloes in voids have the lowest median spin parameters; c) Haloes with MM* perpendicular to it. For masses M>M*, the major axis of haloes in filaments and sheets is strongly aligned with the filament or the sheet. Such halo-LSS alignments may be of importance in weak lensing analyses of cosmic shear. A question that is opened by our study is why, in the 0 < z < 1 redshift regime that we have investigated, the mass scale M* sets roughly the threshold below which the LSS-environment either begins to affect, or reverses, the properties of dark matter haloes.

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