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The Copernicus Complexio: statistical properties of warm dark matter haloes.
- Source :
-
Monthly Notices of the Royal Astronomical Society . 1/1/2016, Vol. 455 Issue 1, p318-333. 16p. - Publication Year :
- 2016
-
Abstract
- 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 ~13.4 bn particles, each of mass ~105 h-1M☉, providing detailed information about halo structure and evolution down to dwarf galaxy mass scales. Non-linear structure formation on small scales (M200 ≲2 × 109 h-1M☉) 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 ~2 × 109 h-1M☉ and declines very rapidly towards lower masses so that there are five times fewer haloes of mass M200 = 108 h-1M☉ 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. [ABSTRACT FROM AUTHOR]
- Subjects :
- *DARK matter
*EMISSION control
*DWARF galaxies
*SIMULATION methods & models
Subjects
Details
- Language :
- English
- ISSN :
- 00358711
- Volume :
- 455
- Issue :
- 1
- Database :
- Academic Search Index
- Journal :
- Monthly Notices of the Royal Astronomical Society
- Publication Type :
- Academic Journal
- Accession number :
- 111331145
- Full Text :
- https://doi.org/10.1093/mnras/stv2294