The Copernicus Complexio: statistical properties of warm dark matter haloes
The Copernicus Complexio: statistical properties of warm dark matter haloes
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DOI：
10.1093/mnras/stv2294
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发表时间：
2015-07
影响因子：
4.8
通讯作者：
S. Bose;W. Hellwing;C. Frenk;A. Jenkins;M. Lovell;J. Helly;Baojiu Li
中科院分区：
文献类型：
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作者：
S. Bose;W. Hellwing;C. Frenk;A. Jenkins;M. Lovell;J. Helly;Baojiu Li
Bulbul等人（2014 a）和Boyarsky等人（2014 a）最近从星系和星系团中心探测到3.5 keV X射线线，这被解释为7 keV无菌中微子衰变的发射，这些中微子可以构成（暖）暗物质（WDM）。作为哥白尼COmplexio（COCO）计划的一部分，我们调查的性质形成的暗物质晕的高分辨率宇宙学N体模拟从初始条件类似于在宇宙中的暗物质由7千电子伏的不育中微子的预期。这个模拟和它的冷暗物质（CDM）对应有13：40亿粒子，每个质量10 5 h 1 M，提供详细的信息晕结构和演化到矮星系质量尺度。COCO-WARM中小尺度（M200 <2 × 10 - 9 h-1 M）非线性结构的形成比COCO-COLD中稍晚。光环质量功能在目前的WDM模型开始下降到低于其CDM对应的质量2 - 10 - 9小时1 M，并下降非常迅速地向较低的质量，使有5倍少的质量M200 = 10 - 8小时1 M的晕COCO-WARM比COCO-COLD。在COCO-WARM中，矮星系尺度上的晕浓度相应较小，我们提供了一个简单的函数形式来描述其随红移的演化。在这两种情况下，光环的形状是相似的，但COCO-WARM中最小的光环比CDM中的光环旋转得稍微慢一些。
The recent detection of a 3.5 keV X-ray line from the centres of galaxies and clusters by Bulbul et al. (2014a) and Boyarsky et al. (2014a) 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 13:4bn particles, each of mass 10 5 h 1 M , providing detailed information about halo structure and evolution down to dwarf galaxy mass scales. Non-linear structure formation on small scales (M200 <2 10 9 h 1 M ) 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 10 9 h 1 M and declines very rapidly towards lower masses so that there are five times fewer haloes of mass M200 = 10 8 h 1 M 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.