Universal Substructure Distributions in LCDM halos: Can we find a Fossil Group?

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dc.creatorD'Onghia, E.
dc.creatorMaccio', A. V.
dc.creatorLake, G.
dc.creatorStadel, J.
dc.creatorMoore, B.
dc.date2007-04-19
dc.date.accessioned2026-07-07T07:57:32Z
dc.date.available2026-07-07T07:57:32Z
dc.descriptionWe use large cosmological N-body simulations to study the subhalo population in galaxy group sized halos. In particular, we look for fossil group candidates with typical masses ~10-25% of Virgo cluster but with an order of magnitude less substructure. We examine recent claims that the earliest systems to form are deficient enough in substructure to explain the luminosity function found in fossil groups. Although our simulations show a correlation between the halo formation time and the number of subhalos, the maximum suppression of subhalos is a factor of 2-2.5, whereas a factor of 6 is required to match fossil groups and galaxies. While the number of subhalos depends weakly on the formation time, the slope of the halo substructure velocity function does not. The satellite population within Cold Dark Matter (CDM) halos is self-similar at scales between galaxies and galaxy clusters regardless of mass, whereas current observations show a break in self-similarity at a mass scale corresponding to group of galaxies.
dc.descriptionSubmitted for publication in MNRAS, 8 pages, 8 figures
dc.identifierhttps://arxiv.org/abs/0704.2604
dc.identifierhttp://arxiv.org/abs/0704.2604
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/127682
dc.subjectAstrophysics
dc.titleUniversal Substructure Distributions in LCDM halos: Can we find a Fossil Group?
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