团、丝、片和空洞中暗物质晕性质的演化
The Evolution of Dark Matter Halo Properties in Clusters, Filaments, Sheets and Voids
摘要：
我们使用一系列的N体模拟的LCDM宇宙学研究红移的演变，因为z=1的性质和对齐的大尺度结构的晕在集群，细丝，片和空隙。我们发现：（i）一旦用M* 重新标度晕质量，质量标度在红移z处坍缩，在晕属性中没有进一步的显著红移依赖性;（ii）环境影响晕的形状和形成时间，在所有研究的红移中，质量M<M* 的晕;和（iii）有一个显着的自旋和形状的晕与细丝和薄片对齐。详细地说，在z=1之前的所有红移中：a）M<M* 的晕在星团中比在其他环境中更倾向于扁长;这种趋势在更高的质量上是相反的：在大约M* 以上，星团中的晕通常比类似的大质量晕在片、丝和空隙中更扁长。b）细丝中M>M* 的晕比团簇中类似质量的晕旋转得更快;空洞中的晕具有最低的中值自旋参数; c）空洞中M<M* 的晕倾向于更年轻，而团簇中更老; d）在片中，晕自旋矢量倾向于位于片平面内，与质量无关;相反，在细丝中，M<M* 的晕倾向于平行于细丝旋转，而M>M* 的晕垂直于细丝旋转。对于质量M>M*，细丝和片材中的晕的主轴与细丝或片材强烈对齐。这样的晕-LSS排列可能在宇宙剪切的弱透镜分析中具有重要意义。我们的研究提出的一个问题是，为什么在我们所研究的0 < z < 1的红移区域中，质量尺度M* 大致设定了一个阈值，低于该阈值，LSS环境开始影响或逆转暗物质晕的性质。
英文摘要：
We use a series of N-body simulations of the LCDM cosmology to investigate the redshift evolution since z=1 of the properties and alignment with the large-scale structure of haloes in clusters, filaments, sheets and voids. We find that: (i) Once a rescaling of the halo mass with M*, the mass scale collapsing at redshift z, is performed, there is no further significant redshift dependence in the halo properties; (ii) The environment influences halo shape and formation time at all investigated redshifts for haloes with masses M<M*; and (iii) There is a significant alignment of both spin and shape of haloes with filaments and sheets. In detail, at all redshifts up to z=1: a) Haloes with M<M* tend to be more oblate when located in clusters than in the other environments; this trend is reversed at higher masses: above about M*, halos in clusters are typically more prolate than similar massive haloes in sheets, filaments and voids. b) Haloes with M>M* in filaments spin more rapidly than similar mass haloes in clusters; haloes in voids have the lowest median spin parameters; c) Haloes with M<M* tend to be younger in voids and older in clusters; d) In sheets, halo spin vectors tend to lie within the sheet plane independent of mass; in filaments, instead, haloes with M<M* tend to spin parallel to the filament and haloes with M>M* perpendicular to it. For masses M>M*, the major axis of haloes in filaments and sheets is strongly aligned with the filament or the sheet. Such halo-LSS alignments may be of importance in weak lensing analyses of cosmic shear. A question that is opened by our study is why, in the 0 < z < 1 redshift regime that we have investigated, the mass scale M* sets roughly the threshold below which the LSS-environment either begins to affect, or reverses, the properties of dark matter haloes.
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