Properties of Dark Matter Haloes in Clusters, Filaments, Sheets and Voids

Simple item page
dc.creatorHahn, Oliver
dc.creatorPorciani, Cristiano
dc.creatorCarollo, C. Marcella
dc.creatorDekel, Avishai
dc.date2006-10-10
dc.date2006-11-23
dc.date.accessioned2026-07-07T10:23:51Z
dc.date.available2026-07-07T10:23:51Z
dc.descriptionUsing a series of high-resolution N-body simulations of the concordance cosmology we investigate how the formation histories, shapes and angular momenta of dark-matter haloes depend on environment. We first present a classification scheme that allows to distinguish between haloes in clusters, filaments, sheets and voids in the large-scale distribution of matter. This method is based on a local-stability criterion for the orbits of test particles and closely relates to the Zel'dovich approximation. Applying this scheme to our simulations we then find that: i) Mass assembly histories and formation redshifts strongly depend on environment for haloes of mass M<M* (haloes of a given mass tend to be older in clusters and younger in voids) and are independent of it for larger masses; ii) Low-mass haloes in clusters are generally less spherical and more oblate than in other regions; iii) Low-mass haloes in clusters have a higher median spin than in filaments and present a more prominent fraction of rapidly spinning objects; we identify recent major mergers as a likely source of this effect. For all these relations, we provide accurate functional fits as a function of halo mass and environment. We also look for correlations between halo-spin directions and the large-scale structures: the strongest effect is seen in sheets where halo spins tend to lie within the plane of symmetry of the mass distribution. Finally, we measure the spatial auto-correlation of spin directions and the cross-correlation between the directions of intrinsic and orbital angular momenta of neighbouring haloes. While the first quantity is always very small, we find that spin-orbit correlations are rather strong especially for low-mass haloes in clusters and high-mass haloes in filaments.
dc.description13 pages, 13 figures. Version accepted for publication in MNRAS (references added). Version with high-resolution figures available at http://www.exp-astro.phys.ethz.ch/hahn/pub/HPCD06.pdf
dc.identifierhttps://arxiv.org/abs/astro-ph/0610280
dc.identifierhttp://arxiv.org/abs/astro-ph/0610280
dc.identifierMon.Not.Roy.Astron.Soc.375:489-499,2007
dc.identifierdoi:10.1111/j.1365-2966.2006.11318.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175981
dc.subjectAstrophysics
dc.titleProperties of Dark Matter Haloes in Clusters, Filaments, Sheets and Voids
dc.typetext

Files

Collections

arXiv