Lovell, M.R. and Eke, V. and Frenk, C.S. and Gao, L. and Jenkins, A. R. and Theuns, Tom and Wang, J. and White, S.D.M. and Boyarsky, A. and Ruchayskiy, O. (2012) 'The haloes of bright satellite galaxies in a warm dark matter universe.', Monthly notices of the Royal Astronomical Society., 420 (3). pp. 2318-2324.
High-resolution N-body simulations of galactic cold dark matter haloes indicate that we should expect to find a few satellite galaxies around the Milky Way whose haloes have a maximum circular velocity in excess of 40 km s−1. Yet, with the exception of the Magellanic Clouds and the Sagittarius dwarf, which likely reside in subhaloes with significantly larger velocities than this, the bright satellites of the Milky Way all appear to reside in subhaloes with maximum circular velocities below 40 km s−1. As recently highlighted by Boylan-Kolchin et al., this discrepancy implies that the majority of the most massive subhaloes within a cold dark matter galactic halo are too concentrated to be consistent with the kinematic data for the bright Milky Way satellites. Here we show that no such discrepancy exists if haloes are made of warm rather than cold dark matter because these haloes are less concentrated on account of their typically later formation epochs. Warm dark matter is one of several possible explanations for the observed kinematics of the satellites.
|Keywords:||Galaxies: dwarf, Dark matter.|
|Full text:||(VoR) Version of Record|
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|Publisher Web site:||http://dx.doi.org/10.1111/j.1365-2966.2011.20200.x|
|Publisher statement:||This article has been accepted for publication in Monthly notices of the Royal Astronomical Society © 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS Published by Oxford University Press on behalf of Royal Astronomical Society. All rights reserved.|
|Date accepted:||No date available|
|Date deposited:||22 August 2014|
|Date of first online publication:||March 2012|
|Date first made open access:||No date available|
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