Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 455, Issue 1, Pages 318-333Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv2294
Keywords
methods: numerical; dark matter
Categories
Funding
- STFC [ST/K501979/1, ST/H008519/1]
- ERC Advanced Investigator grant COSMIWAY [GA 267291]
- Science and Technology Facilities Council [ST/F001166/1, ST/I00162X/1]
- Polish National Science Center [DEC-2011/01/D/ST9/01960]
- Royal Astronomical Society
- Durham University
- BIS National E-infrastructure capital grant [ST/K00042X/1]
- STFC DiRAC Operations grant [ST/K003267/1]
- HPC Infrastructure for Grand Challenges of Science and Engineering Project
- European Regional Development Fund under the Innovative Economy Operational Programme
- Dutch Ministry of Education, Culture and Science (OCW)
- Science and Technology Facilities Council [ST/H008519/1, ST/K00042X/1, ST/M007006/1, ST/K501979/1] Funding Source: researchfish
- STFC [ST/M007006/1, ST/K00042X/1, ST/I00162X/1] Funding Source: UKRI
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The recent detection of a 3.5 keV X-ray line from the centres of galaxies and clusters by Bulbul et al. and Boyarsky et al. has been interpreted as emission from the decay of 7 keV sterile neutrinos which could make up the (warm) dark matter (WDM). As part of the Copernicus Complexio (COCO) programme, we investigate the properties of dark matter haloes formed in a high-resolution cosmological N-body simulation from initial conditions similar to those expected in a universe in which the dark matter consists of 7 keV sterile neutrinos. This simulation and its cold dark matter (CDM) counterpart have similar to 13.4 bn particles, each of mass similar to 10(5) h(-1) M-circle dot, providing detailed information about halo structure and evolution down to dwarf galaxy mass scales. Non-linear structure formation on small scales (M-200 <= 2 x 10(9) h(-1) M-circle dot) begins slightly later in COCO-WARM than in COCO-COLD. The halo mass function at the present day in the WDM model begins to drop below its CDM counterpart at a mass similar to 2 x 10(9) h(-1) M-circle dot and declines very rapidly towards lower masses so that there are five times fewer haloes of mass M-200 = 10(8) h(-1) M-circle dot in COCO-WARM than in COCO-COLD. Halo concentrations on dwarf galaxy scales are correspondingly smaller in COCO-WARM, and we provide a simple functional form that describes its evolution with redshift. The shapes of haloes are similar in the two cases, but the smallest haloes in COCO-WARM rotate slightly more slowly than their CDM counterparts.
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