Bose, S. and Hellwing, W.A. and Frenk, C.S. and Jenkins, A. and Lovell, M.R. and Helly, J.C. and Li, B. and Gonzalez-Perez, V. and Gao, L. (2017) 'Substructure and galaxy formation in the Copernicus Complexio warm dark matter simulations.', Monthly notices of the Royal Astronomical Society., 464 (4). pp. 4520-4533.
We use the Copernicus Complexio (coco) high-resolution N-body simulations to investigate differences in the properties of small-scale structures in the standard cold dark matter (CDM) model and in a model with a cutoff in the initial power spectrum of density fluctuations consistent with both a thermally produced warm dark matter (WDM) particle with a rest mass of 3.3 keV and a sterile neutrino with mass 7 keV and leptogenesis parameter L6 = 8.7. The latter corresponds to the ‘coldest’ model with this sterile neutrino mass compatible with the identification of the recently detected 3.5 keV X-ray line as resulting from particle decay. CDM and WDM predict very different number densities of subhaloes with mass ≲ 109 h−1 M⊙ although they predict similar, nearly universal, normalized subhalo radial density distributions. Haloes and subhaloes in both models have cuspy Navarro-Frenk-White profiles, but WDM subhaloes below the cut-off scale in the power spectrum (corresponding to maximum circular velocities Vmaxz = 0 ≤ 50 kms− 1) are less concentrated than their CDM counterparts. We make predictions for observable properties using the galform semi-analytic model of Galaxy formation. Both models predict Milky Way satellite luminosity functions consistent with observations, although the WDM model predicts fewer very faint satellites. This model, however, predicts slightly more UV bright galaxies at redshift z > 7 than CDM, but both are consistent with observations. Gravitational lensing offers the best prospect of distinguishing between the models.
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|Publisher Web site:||https://doi.org/10.1093/mnras/stw2686|
|Publisher statement:||This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.|
|Date accepted:||17 October 2016|
|Date deposited:||02 March 2017|
|Date of first online publication:||19 October 2016|
|Date first made open access:||02 March 2017|
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