暗物质晕的聚类与次晕各向异性及平面性的依赖关系
The Dependence of Halo Clustering on Subhalo Anisotropy and Planarity
AI总结：
研究通过宇宙N体模拟揭示次晕的各向异性和平面性影响暗物质晕聚类，发现环境因素显著改变次晕分布特征，为理解卫星晕的各向异性提供新视角。
摘要：
我们证明宿主冷暗物质（CDM）晕的聚类方式取决于其次晕的各向异性和平面性，表明环境因素影响次晕的各向异性和平面性。卫星星系相对于中心星系以及次晕相对于宿主晕的空间分布已备受关注二十年。重要问题包括卫星相对于宿主的分布是否各向异性或表现出平面性，以及这种各向异性是否依赖于系统的环境。我们研究了宇宙N体模拟中次晕的空间分布。我们发现CDM次晕的分布方式高度各向异性且平面，与先前工作一致，但以新方式呈现。更新的结果是各向异性具有环境依赖性。具有较少（更多）各向异性、较少（更多）平面性、远离（靠近）宿主中心的系统聚类更强烈（更弱）。此外，这些聚类效应并非主要由次晕各向异性和平面性与另一个已知影响聚类的单一晕属性（如浓度）的相关性导致。这是新的独特效应。我们讨论了这一结果对CDM预测的卫星各向异性的影响、其可检验性以及其可能与本地群大星系观察到的各向异性关系。在附录中，我们澄清了我们椭球体模拟晕目录的构建方法。
英文摘要：
We show that host cold dark matter (CDM) haloes cluster in a manner that depends upon the anisotropy and planarity of their subhaloes, indicating an environmental dependence to subhalo anisotropy and planarity. The spatial distributions of both satellite galaxies about central galaxies and subhaloes about host haloes have been subjects of interest for two decades. Important questions include the degree to which satellites are distributed anisotropically about their hosts or exhibit planarity as well as the degree to which this anisotropy depends on the environment of the system. We study the spatial distributions of subhaloes in a cosmological N-body simulation. We find that CDM subhaloes are distributed in a manner that is strongly anisotropic and planar, in agreement with prior work, though w e present this in a new way. The more novel result is that anisotropy has an environmental dependence. Systems with subhaloes that exhibit $\textit{less}$ ($\textit{more}$) anisotropy, $\textit{less}$ ($\textit{more}$) planarity, and reside $\textit{further}$ from ($\textit{closer}$ to) their host centres cluster more $\textit{strongly}$ ($\textit{weakly}$). Moreover, these clustering effects are not primarily the result of the correlation between subhalo anisotropy and/or planarity and another $\textit{single}$ halo property upon which clustering is already known to depend (e.g. concentration). This is a new and distinct effect. We discuss the impact of this result on the anisotropies of satellites as predict ed by CDM, its testability, and its possible relation to the anisotropies observed about the large galaxies of the Local Group. In an appendix, we clarify our construction of ellipsoidal mock halo catalogues.
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