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Cores in warm dark matter haloes: a Catch 22 problem

Macciò, Andrea V. ; Paduroiu, Sinziana ; Anderhalden, Donnino ; Schneider, Aurel ; Moore, Ben

In: Monthly Notices of the Royal Astronomical Society, 2012, vol. 424, no. 2, p. 1105-1112

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    Title
    • Cores in warm dark matter haloes: a Catch 22 problem
    Author
    • Macciò, Andrea V.. Max-Planck-Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany
    • Paduroiu, Sinziana. Geneva Observatory, University of Geneva, CH-1290 Sauverny, Switzerland
    • Anderhalden, Donnino. Institute for Theoretical Physics, University of Zürich, CH-8057 Zürich, Switzerland
    • Schneider, Aurel. Institute for Theoretical Physics, University of Zürich, CH-8057 Zürich, Switzerland
    • Moore, Ben. Institute for Theoretical Physics, University of Zürich, CH-8057 Zürich, Switzerland
    Document Type
    • Postprint
    OAI-PMH Identifier
    • oai:doc.rero.ch:294909
    Summary
    The free streaming of warm dark matter particles dampens the fluctuation spectrum, flattens the mass function of haloes and sets a fine-grained phase density limit for dark matter structures. The phase-space density limit is expected to imprint a constant-density core at the halo centre in contrast to what happens for cold dark matter. We explore these effects using high-resolution simulations of structure formation in different warm dark matter scenarios. We find that the size of the core we obtain in simulated haloes is in good agreement with theoretical expectations based on Liouville's theorem. However, our simulations show that in order to create a significant core (rc ∼ kpc) in a dwarf galaxy (M∼ 1010 M⊙), a thermal candidate with mass as low as 0.1 keV is required. This would fully prevent the formation of the dwarf galaxy in the first place. For candidates satisfying large-scale structure constraints (mν larger than ≈1-2 keV), the expected size of the core is of the order of 10 (20) pc for a dark matter halo with a mass of 1010 (108) M⊙. We conclude that ‘standard' warm dark matter is not a viable solution for explaining the presence of cored density profiles in low-mass galaxies