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The mass–concentration–redshift relation of cold and warm dark matter haloes

Artykuł
Czasopismo : MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY   Tom: 460, Zeszyt: 2, Strony: 1214-1232
Aaron D. Ludlow [1] , Sownak Bose [1] , Raúl E. Angulo [2] , Lan Wang [3] , Wojciech Hellwing [1] , [4] , [5] , Julio F. Navarro [6] , Shaun Cole [1] , Carlos S. Frenk [1]
  • [1]
    Institute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK
  • [2]
    Centro de Estudios de Física del Cosmos de Aragón, Plaza San Juan 1, Planta-2, E-44001 Teruel, Spain
  • [3]
    Key Laboratory of Computational Astrophysics, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012, China
  • [4]
    Institute of Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Portsmouth P01 3FX, UK
  • [5]
  • [6]
    Department of Physics and Astronomy, University of Victoria, PO Box 1700 STN CSC, Victoria, BC V8W 2Y2, Canada
2016 angielski
Liczba arkuszy: 1
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  • Oryginalny artykuł naukowy
  • Zrecenzowana naukowo
Dyscypliny naukowe
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Astronomia
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Abstrakty ( angielski )
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We use a suite of cosmological simulations to study the mass–concentration–redshift relation, c(M, z), of dark matter haloes. Our simulations include standard Λ-cold dark matter (CDM) models, and additional runs with truncated power spectra, consistent with a thermal warm dark matter (WDM) scenario. We find that the mass profiles of CDM and WDM haloes are self-similar and well approximated by the Einasto profile. The c(M, z) relation of CDM haloes is monotonic: concentrations decrease with increasing virial mass at fixed redshift, and decrease with increasing redshift at fixed mass. The mass accretion histories (MAHs) of CDM haloes are also scale-free, and can be used to infer concentrations directly. These results do not apply to WDM haloes: their MAHs are not scale-free because of the characteristic scale imposed by the power spectrum suppression. Further, the WDM c(M, z) relation is non-monotonic: concentrations peak at a mass scale dictated by the truncation scale, and decrease at higher and lower masses. We show that the assembly history of a halo can still be used to infer its concentration, provided that the total mass of its progenitors is considered (the ‘collapsed mass history’; CMH), rather than just that of its main ancestor. This exploits the scale-free nature of CMHs to derive a simple scaling that reproduces the mass–concentration–redshift relation of both CDM and WDM haloes over a vast range of halo masses and redshifts. Our model therefore provides a robust account of the mass, redshift, cosmology and power spectrum dependence of dark matter halo concentrations.
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