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Cusps in cold dark matter haloes

Diemand, Jürg ; Zemp, Marcel ; Moore, Ben ; Stadel, Joachim ; Carollo, Marcella

In: Monthly Notices of the Royal Astronomical Society, 2005, vol. 364, no. 2, p. 665-673

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    Titre
    • Cusps in cold dark matter haloes
    Auteur
    • Diemand, Jürg. Institute for Theoretical Physics, University of Zürich, Winterthurerstrasse 190, CH-8057 Zürich, Switzerland
    • Zemp, Marcel. Institute for Theoretical Physics, University of Zürich, Winterthurerstrasse 190, CH-8057 Zürich, Switzerland
    • Moore, Ben. Institute for Theoretical Physics, University of Zürich, Winterthurerstrasse 190, CH-8057 Zürich, Switzerland
    • Stadel, Joachim. Institute for Theoretical Physics, University of Zürich, Winterthurerstrasse 190, CH-8057 Zürich, Switzerland
    • Carollo, Marcella. Institute of Astronomy, ETH Zürich, ETH Hönggerberg HPF D6, CH-8093 Zürich, Switzerland
    Type de document
    • Postprint
    Langue
    • Inglese
    Publié dans
    • Monthly Notices of the Royal Astronomical Society, 2005, vol. 364, no. 2, p. 665-673. Blackwell Science Ltd
    Autre version électronique
    Identifiant OAI-PMH
    • oai:doc.rero.ch:296116
    Summary
    We resolve the inner region of a massive cluster forming in a cosmological Λ cold dark matter (CDM) simulation with a mass resolution of 2 × 106 M⊙ and before z= 4.4 even 3 × 105 M⊙. This is a billion times less than the cluster's final virial mass and a substantial increase over current ΛCDM simulations. We achieve this resolution using a new multimass refinement procedure and are now able to probe a dark matter halo density profile down to 0.1 per cent of the virial radius. The inner density profile of this cluster halo is well fitted by a power law ρ∝r−γ down to the smallest resolved scale. An inner region with roughly constant logarithmic slope is now resolved, which suggests that cuspy profiles describe the inner profile better than recently proposed profiles with a core. The cluster studied here is one out of a sample of six high-resolution cluster simulations, and its inner slope of about γ= 1.2 lies close to the sample average