标题： 星系团宇宙学 显示英文标题

标题： Cosmology with Galaxy Clusters

摘要： 我们回顾了宇宙学中关于星系团的最新进展。星系团是宇宙中质量最大的天体。因此，作为函数的星系团数密度与星系团质量（即星系团丰度）对宇宙学参数非常敏感，特别是宇宙物质密度 $\Omega_{\rm m}$ 和物质密度涨落的振幅 $\sigma_8$。在这篇综述中，我们描述了通过光学近红外（O-NIR）、X射线和CMB观测来探测星系团的方法，并概述了通过不同波长探测星系团的优点和缺点。我们描述了测量星系团质量的方法，重点介绍了弱透镜（WL）测量的校准方法。然后，我们讨论了如何通过星系团选择函数和MOR模型化不同波长可观测量与星系团丰度之间的联系，并量化了边际化无用参数对宇宙学约束的影响。最后，我们还介绍了基于O-NIR、X射线和CMB观测的星系团丰度的近期宇宙学约束结果。 显示英文摘要

摘要： We review recent advancements in cosmology with galaxy clusters. Galaxy clusters are the most massive objects in the Universe. Consequently the cluster number density as a function of cluster mass, or cluster abundance, is sensitive to cosmological parameters, particularly the matter density of the Universe $\Omega_{\rm m}$ and the amplitude of matter density fluctuation $\sigma_8$. In this review, we describe the methods used to detect galaxy clusters through optical near-infrared (O-NIR), X-ray, and CMB observations, outlining the advantages and disadvantages of cluster detection through different wavelengths. We describe methods for measuring cluster mass, with a particular focus on calibration by WL measurements. We then discuss how the connection between observables in different wavelengths and cluster abundance can be modeled through a cluster selection function and MOR, and quantify the impact of marginalization of nuisance parameters on cosmological constraints. Finally, we also walk through the recent results of cosmological constraints by cluster abundance with the O-NIR, X-ray, and CMB observations.