跨宇宙学的密度概率分布函数的近似
Approximating Density Probability Distribution Functions Across Cosmologies
摘要：
使用一套自相似的宇宙学模拟，我们测量的概率分布函数（PDF）的实空间密度，红移空间密度，和它们的几何平均值。我们发现，实空间密度PDF是很好地描述了两个参数的函数：$n_s$，频谱斜率，和$σ_L$，线性均方根密度波动。对于红移空间密度以及实空间密度和红移空间密度的几何平均，我们引入了第三个参数，$s_L={\sqrt{\langle(dv^L_{\rm pec}/dr)^2\rangle}}/{H}$。我们发现，密度PDF的LCDM宇宙学也很好的参数化这三个参数。因此，我们能够使用一套自相似宇宙学模拟来近似一系列宇宙学的密度PDF。我们公开了密度PDF，并为它们提供了一个分析拟合公式。
英文摘要：
Using a suite of self-similar cosmological simulations, we measure the probability distribution functions (PDFs) of real-space density, redshift-space density, and their geometric mean. We find that the real-space density PDF is well-described by a function of two parameters: $n_s$, the spectral slope, and $σ_L$, the linear rms density fluctuation. For redshift-space density and the geometric mean of real- and redshift-space densities, we introduce a third parameter, $s_L={\sqrt{\langle(dv^L_{\rm pec}/dr)^2\rangle}}/{H}$. We find that density PDFs for the LCDM cosmology is also well-parameterized by these three parameters. As a result, we are able to use a suite of self-similar cosmological simulations to approximate density PDFs for a range of cosmologies. We make the density PDFs publicly available and provide an analytical fitting formula for them.
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