Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 415, Issue 4, Pages 3177-3188Publisher
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2011.18930.x
Keywords
galaxies: haloes; cosmology: theory; dark matter
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Funding
- DOE
- Chinese academy of science (CAS)
- National basic research programme of China (programme 973) [2009CB24901]
- NSFC [10973018]
- STFC
- hospitality of the Institute for Computational Cosmology in Durham, UK
- STFC [ST/F010176/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/F010176/1] Funding Source: researchfish
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We explore the cosmological halo-to-halo scatter of the distribution of mass within dark matter haloes utilizing a well-resolved statistical sample of clusters from the cosmological Millennium Simulation. We find that at any radius, the spherically averaged dark matter density of a halo (corresponding to the 'smooth component') and its logarithmic slope are well described by a Gaussian probability distribution. At small radii (within the scale radius), the density distribution is fully determined by the measured Gaussian distribution in halo concentrations. The variance in the radial distribution of mass in dark matter haloes is important for the interpretation of direct and indirect dark matter detection efforts. The scatter in mass profiles imparts approximately a 25 per cent cosmological uncertainty in the dark matter density at the Solar neighbourhood and a factor of similar to 3 uncertainty in the expected Galactic dark matter annihilation flux. The aggregate effect of halo-to-halo profile scatter leads to a small (few per cent) enhancement in dark matter annihilation background if the Gaussian concentration distribution holds for all halo masses versus a 10 per cent enhancement under the assumption of a lognormal concentration distribution. The Gaussian nature of the cluster profile scatter implies that the technique of 'stacking' haloes to improve signal-to-noise ratio should not suffer from bias.
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