标题： 关于星系团层析聚类作为宇宙学探针的研究 显示英文标题

标题： On the tomographic cluster clustering as a cosmological probe

摘要： 星系团的空间分布是推断基本宇宙学参数的有价值探针。 我们测量了来自\textsc{匹诺曹}模拟的暗物质晕在红移范围$0.2 < z < 1.0$内且具有晕星系团样本预期质量选择的晕的聚类性质，其晕质量为$M_\mathrm{vir} > 10^{14} M_\odot \, h^{-1}$。 我们分析的过去光锥具有60度的角大小，这大约对应于四分之一的天空。 我们采用了一个线性功率谱模型，考虑了重子声波振荡尺度上的非线性修正，以进行三维和二维层析聚类的比较研究。 为此，我们建模了三维两点相关函数的多极矩$\xi(r)$、角相关函数$w(\theta)$和角功率谱$C_\ell$。 我们考虑了观测效应，例如由追踪物的peculiar速度产生的红移空间畸变以及红移误差。 我们发现，与二维聚类相比，光电红移误差对三维聚类有更严重的影响，因为它们只影响晕之间的径向分离而非角分离，并对三维多极矩产生显著影响。 使用贝叶斯分析，我们在$\Omega_m-\sigma_8$平面上，以不同的断层扫描策略探索了所考虑探针的后验分布，并重点关注了总结参数$S_8\equiv \sigma_8\sqrt{\Omega_m/0.3}$。 我们的结果显示，在存在较大的测光误差的情况下，二维聚类可以相对于完整的三维聚类统计提供具有竞争力的宇宙学限制，并且可以成功应用于分析来自正在进行和即将进行的阶段 III 和阶段 IV 测光红移巡天的星系团目录。 显示英文摘要

摘要： The spatial distribution of galaxy clusters is a valuable probe for inferring fundamental cosmological parameters. We measured the clustering properties of dark matter haloes from the \textsc{Pinocchio} simulations, in the redshift range $0.2 < z < 1.0$ and with virial masses $M_\mathrm{vir} > 10^{14} M_\odot \, h^{-1}$, which reproduce the expected mass selection of galaxy cluster samples. The past-light cones we analysed have an angular size of 60 degrees, which approximately corresponds to a quarter of the sky. We adopted a linear power spectrum model, accounting for nonlinear corrections at the baryon acoustic oscillations scale, to perform a comparative study between 3D and 2D tomographic clustering. For this purpose, we modelled the multipoles of the 3D two-point correlation function, $\xi(r)$, the angular correlation function, $w(\theta)$, and the angular power spectrum, $C_\ell$. We considered observational effects such as redshift-space distortions, produced by the peculiar velocities of tracers, and redshift errors. We found that photometric redshift errors have a more severe consequence on the 3D than on the 2D clustering, as they affect only the radial separation between haloes and not the angular one, with a relevant impact on the 3D multipoles. Using a Bayesian analysis, we explored the posterior distributions of the considered probes with different tomographic strategies, in the $\Omega_m-\sigma_8$ plane, focusing on the summary parameter $S_8\equiv \sigma_8\sqrt{\Omega_m/0.3}$. Our results show that in the presence of large photometric errors the 2D clustering can provide competitive cosmological constraints with respect to the full 3D clustering statistics, and can be successfully applied to analyse the galaxy cluster catalogues from the ongoing and forthcoming Stage-III and Stage-IV photometric redshift surveys.