Marked correlation functions in perturbation theory
Marked correlation functions in perturbation theory
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DOI：
10.1088/1475-7516/2020/01/006
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发表时间：
2019-11
影响因子：
6.4
通讯作者：
A. Aviles;K. Koyama;J. Cervantes-Cota;H. Winther;Baojiu Li
中科院分区：
文献类型：
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作者：
A. Aviles;K. Koyama;J. Cervantes-Cota;H. Winther;Baojiu Li
我们开发了微扰理论方法来对为增加宇宙低密度区域的权重而构建的标记相关函数进行建模，这可能有助于将修改后的重力模型与基于广义相对论的标准宇宙学模型区分开来。在卷积拉格朗日扰动理论中，我们得到加权相关函数可以表示为双卷积积分，我们使用欧拉和拉格朗日方案的组合来近似。我们发现不同的方法在准非线性尺度上的一致性在 1% 以内。与N体模拟相比，微扰理论可以对低至30 Mpc/h的暗物质场、暗物质晕以及晕占据分布星系的显着相关函数提供准确的预测。这些分析方法有助于理解标记和星系偏差之间的简并性，并找到一种方法来最大化各种宇宙学模型之间的差异。
We develop perturbation theory approaches to model the marked correlation function constructed to up-weight low density regions of the Universe, which might help distinguish modified gravity models from the standard cosmology model based on general relativity. Working within Convolution Lagrangian Perturbation Theory, we obtain that weighted correlation functions are expressible as double convolution integrals that we approximate using a combination of Eulerian and Lagrangian schemes. We find that different approaches agree within 1% on quasi non-linear scales. Compared with N-body simulations, the perturbation theory is found to provide accurate predictions for the marked correlation function of dark matter fields, dark matter halos as well as Halo Occupation Distribution galaxies down to 30 Mpc/h. These analytic approaches help to understand the degeneracy between the mark and the galaxy bias and find a way to maximize the differences among various cosmological models.