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The Copernicus Complexio: statistical properties of warm dark matter haloes

Artykuł
Czasopismo : MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY   Tom: 455, Strony: 318-333
Sownak Bose [1] , Wojciech Hellwing [2] , Carlos S. Frenk [1] , Adrian Jenkins [1] , Mark R. Lovell [3] , [4] , John C. Helly [1] , Baojiu Li [1]
  • [1]
    Institiute for Computational cosmology, Durham University, UK
  • [2]
  • [3]
    GRAPPA Institiute, Universiteit van Amsterdam, The Netherlands
  • [4]
    Instituut-Lorentz for theoretical Physics, The Netherlands
2015 angielski
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The recent detection of a 3.5 keV X-ray line from the centres of galaxies and clusters by Bulbul et al. (2014a) and Boyarsky et al. (2014a) has been interpreted as emission from the decay of 7 keV sterile neutrinos which could make up the (warm) dark matter (WDM). As part of the COpernicus COmplexio (COCO) programme, we investigate the properties of dark matter haloes formed in a high-resolution cosmological N-body simulation from initial conditions similar to those expected in a universe in which the dark matter consists of 7 keV sterile neutrinos. This simulation and its cold dark matter (CDM) counterpart have ∼13.4bn particles, each of mass ∼105h−1M⊙, providing detailed information about halo structure and evolution down to dwarf galaxy mass scales. Non-linear structure formation on small scales (M200≤2×109h−1M⊙) begins slightly later in COCO-Warm than in COCO-Cold. The halo mass function at the present day in the WDM model begins to drop below its CDM counterpart at a mass ∼2×109h−1M⊙ and declines very rapidly towards lower masses so that there are five times fewer haloes of mass M200=108h−1M⊙ in COCO-Warm than in COCO-Cold. Halo concentrations on dwarf galaxy scales are correspondingly smaller in COCO-Warm, and we provide a simple functional form that describes its evolution with redshift. The shapes of haloes are similar in the two cases, but the smallest haloes in COCO-Warm rotate slightly more slowly than their CDM counterparts.
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