论文标题
本地宇宙约束对光晕丰度和聚类的影响
The effect of local universe constraints on halo abundance and clustering
论文作者
论文摘要
宇宙$ n $ - 宇宙暗物质组成部分的模拟通常使用固定功率谱和密度场的随机阶段的初始条件，从而导致结构仅在统计意义上与星系的局部分布一致。但是，可以推断出导致我们周围看到的星系和簇的配置的初始阶段。我们分析了101个模拟的CSiborg套件，该套件是通过将密度字段在155 mpc $/h $内约束，暗物质粒子质量$ 4.38 \ times10^9 m_ \ odot $，以量化对在2.65 mpc $/h $量表上对2.65 mpc $/h $量表的约束的程度降低了量质量质量和量表功能的变化。这是通过将CSiborg与无约束Quijote模拟的子集进行对比的，并且对$λ$ CDM平均值的期望。使用FOF，PHEW和HOP HALOFINDERS，我们表明CSIBORG Suite在较大的质量尺度（$ \ gtrsim 10^{14} M _ {\ odot}/H $）上击败了宇宙差异，这些差异最初是由最初的条件限制的，并显示出重要的halo-halo交叉交叉交叉交叉$/$ $ $ $ $ $ $ $ \ \ $ \ \ $ c。此外，约束的效果将渗透到较低的质量对象和低于其施加的物体以下的尺度。最后，我们在实现之间开发了一种算法来“双”光环，并表明质量大于$ 10^{15} m _ {\ odot}/h $的光环中约有50％可以在CSIBORG Suite的所有实现中识别。我们使CSIBORG HALO目录公开用于未来的应用程序，需要了解本地Halo字段。
Cosmological $N$-body simulations of the dark matter component of the universe typically use initial conditions with a fixed power spectrum and random phases of the density field, leading to structure consistent with the local distribution of galaxies only in a statistical sense. It is, however, possible to infer the initial phases which lead to the configuration of galaxies and clusters that we see around us. We analyse the CSiBORG suite of 101 simulations, formed by constraining the density field within 155 Mpc$/h$ with dark matter particle mass $4.38\times10^9 M_\odot$, to quantify the degree to which constraints imposed on 2.65 Mpc$/h$ scales reduce variance in the halo mass function and halo-halo cross-correlation function on a range of scales. This is achieved by contrasting CSiBORG with a subset of the unconstrained Quijote simulations and expectations for the $Λ$CDM average. Using the FOF, PHEW and HOP halofinders, we show that the CSiBORG suite beats cosmic variance at large mass scales ($\gtrsim 10^{14}M_{\odot}/h$), which are most strongly constrained by the initial conditions, and exhibits a significant halo-halo cross-correlation out to $\sim30$ Mpc$/h$. Moreover, the effect of the constraints percolates down to lower mass objects and to scales below those on which they are imposed. Finally, we develop an algorithm to "twin" halos between realisations and show that approximately 50% of halos with mass greater than $10^{15}M_{\odot}/h$ can be identified in all realisations of the CSiBORG suite. We make the CSiBORG halo catalogues publicly available for future applications requiring knowledge of the local halo field.
