The evolution of dark matter halo properties in clusters, filaments, sheets and voids
The evolution of dark matter halo properties in clusters, filaments, sheets and voids
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DOI：
10.1111/j.1365-2966.2007.12249.x
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发表时间：
2007-04
影响因子：
4.8
通讯作者：
O. Hahn;C. Carollo;C. Porciani;A. Z. E. Zurich;HU Jerusalem
中科院分区：
文献类型：
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作者：
O. Hahn;C. Carollo;C. Porciani;A. Z. E. Zurich;HU Jerusalem
我们使用一系列高分辨率的N体模拟的和谐宇宙学研究红移的演变，因为z = 1的性质和对准的大尺度结构（LSS）的晕在集群，细丝，片和空隙。我们发现：（i）一旦用M *（z）重新标度晕质量，即在红移z处坍缩的典型质量标度，晕性质不再有显著的红移依赖性;（ii）对于质量为M ≤ M * 的晕，环境影响晕的形状和形成时间晕圈的自旋和形状与细丝和薄片都有显著的对齐。详细地说，在z = 1之前的所有红移中：（a）质量低于100 M * 的晕在星系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下是相反的：在大约M * 以上，星系团中的晕通常比类似的大质量的片、丝和空洞中的晕更扁长。(b)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)M ≤ M * 的晕在空洞中往往更年轻，而在星团中则更古老。(d)在片层中，晕圈自旋矢量倾向于优先位于片层平面内，与晕圈质量无关;相反，在细丝中，M ≤ M * 的晕圈倾向于平行于细丝旋转，而更高质量的晕圈则垂直于它。对于晕圈质量M ≥ M *，细丝和片中晕圈的长轴分别与宿主细丝或片层平面强烈对齐。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。我们的研究提出了一个问题，为什么在我们研究的0 < z < 1红移区域中，引力坍缩的质量尺度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基本性质。
We use a series of high-resolution N-body simulations of the concordance cosmology to investigate the redshift evolution since z = 1 of the properties and alignment with the large-scale structure (LSS) of haloes in clusters, filaments, sheets and voids. We find that (i) once a rescal-ing of the halo mass with M * (z), the typical mass scale collapsing at redshift z, is performed, there is no further significant redshift dependence in the halo properties; (ii) the environment influences the 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 masses below ∼ 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 * , haloes in clusters are typically more prolate than similar massive haloes in sheets, filaments and voids. (b) The 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 preferentially within the sheet plane independent of halo mass; in filaments, instead, haloes with M ≤ M * tend to spin parallel to the filament and higher mass haloes perpendicular to it. For halo masses M ≥ M * , the major axis of haloes in filaments and sheets is strongly aligned with the host filament or the sheet plane, respectively. 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 for gravitational collapse, M * , sets roughly the threshold below which the LSS environment either begins to affect, or reverses, fundamental properties of dark matter haloes.