CODEX簇的聚类
Clustering of CODEX clusters
摘要：
目的。我们分析了星系团的一个大的连续样本的自相关函数，约束暗能量与X射线（CODEX）的样本，其中我们特别照顾集群的定义。这些星团是使用RASS巡天的X射线选择的，然后使用SDSS测光运行的代码redMapper确定为星系团。我们开发的方法，精确占样本选择的聚类效果，并证明其鲁棒性，使用数值模拟。方法.使用干净的CODEX样本，这是通过应用红移相关的丰富度选择，我们计算了两点自相关函数的星系团的$0.1<z<0.3$和$0.3<z<0.5$红移箱。我们比较了偏差在测量的相关函数与数值模拟中获得的值，使用类似的集群质量范围。结果通过拟合幂律，我们测量了全红移范围内的关联函数的关联长度$r_0=18.7 \pm 1.1$和斜率$γ=1.98 \pm 0.14$。通过将其他宇宙学参数固定到它们的WMAP 9值，我们再现了在以下宇宙学条件下观测到的相关函数的形状：$Ω_{m_0}=0.22^{+0.04}_{-0.03}$和$S_8=σ_8 (Ω_{m_0} /0.3)^{0.5}=0.85^{+0.10}_{-0.08}$，并估计了$σ_{Ω_{m_0}} = 0.02$和$σ_{S_8} = 0.20$的额外系统误差。我们说明了聚类约束的互补性，结合它们与CODEX宇宙学约束的基础上的X射线光度函数，推导出$Ω_{m_0} = 0.25 \pm 0.01$和$σ_8 = 0.81^{+0.01}_{-0.02}$与估计的额外系统误差的$σ_{Ω_{m_0}} = 0.07$和$σ_{σ_8} = 0.04$。质量示踪剂的质量校准和统计质量是不确定性的主要来源。
英文摘要：
Aims. We analyze the autocorrelation function of a large contiguous sample of galaxy clusters, the Constrain Dark Energy with X-ray (CODEX) sample, in which we take particular care of cluster definition. These clusters were X-ray selected using the RASS survey and then identified as galaxy clusters using the code redMaPPer run on the photometry of the SDSS. We develop methods for precisely accounting for the sample selection effects on the clustering and demonstrate their robustness using numerical simulations. Methods. Using the clean CODEX sample, which was obtained by applying a redshift-dependent richness selection, we computed the two-point autocorrelation function of galaxy clusters in the $0.1<z<0.3$ and $0.3<z<0.5$ redshift bins. We compared the bias in the measured correlation function with values obtained in numerical simulations using a similar cluster mass range. Results. By fitting a power law, we measured a correlation length $r_0=18.7 \pm 1.1$ and slope $γ=1.98 \pm 0.14$ for the correlation function in the full redshift range. By fixing the other cosmological parameters to their WMAP9 values, we reproduced the observed shape of the correlation function under the following cosmological conditions: $Ω_{m_0}=0.22^{+0.04}_{-0.03}$ and $S_8=σ_8 (Ω_{m_0} /0.3)^{0.5}=0.85^{+0.10}_{-0.08}$ with estimated additional systematic errors of $σ_{Ω_{m_0}} = 0.02$ and $σ_{S_8} = 0.20$. We illustrate the complementarity of clustering constraints by combining them with CODEX cosmological constraints based on the X-ray luminosity function, deriving $Ω_{m_0} = 0.25 \pm 0.01$ and $σ_8 = 0.81^{+0.01}_{-0.02}$ with an estimated additional systematic error of $σ_{Ω_{m_0}} = 0.07$ and $σ_{σ_8} = 0.04$. The mass calibration and statistical quality of the mass tracers are the dominant source of uncertainty.
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