LOcal Clusters And supercLuster In sZ: Adding Thermal, kInetic and relativistic cOrrectioNs

星系团为检验宇宙模型提供了独特的机会。这依赖于通过比较模拟和观测对其特性进行统计评估。为了克服统计方法的局限性，理想情况下，人们需要对宇宙进行真实的再现。有限的模拟现在允许在600Mpc直径范围内建立宇宙本地大尺度结构（LSS）的高保真克隆，有效到集群尺度。本地化将产生并使用本地星系团和超星系团的模拟克隆，以充分了解这些宇宙实验室的建立。我们将通过宇宙流、x射线和Sunyaev-Zeldovich信号研究它们的物理和动力学特性，并在大尺度宇宙背景下推导出局部LSS的宇宙学特征。定位将为精确宇宙学从平均统计走向精确理解宇宙结构增长铺平道路。的确，ΛCDM模型是一个巨大的成功，然而精确宇宙学的出现揭示了理论预期和观测之间无法解释的差异。其中，CMB测量的物质功率谱线性演化幅度与星系团的差异，即σ8张力，以及CMB大尺度异常特征。通过重新审视这两个有争议的宇宙学问题，LOCALIZATION首次为这两个问题寻求一个共同的解决方案。为了应对这一挑战，将基于局部宇宙高达z<0.07的流体动力学数值克隆，对局部星系团和LSS及其对CMB的影响进行全面分析。将对普朗克观测数据与数值局部星团、超星团和全LSS克隆进行无偏比较。多亏了本地化的集群克隆，我们将首次推导出集群质量和它们观察到的代理之间的确切关系。我们将解决普朗克数据中的CMB异常，重点关注来自本地超星系团和星系团的CMB信号源在最大角度尺度上的贡献。此外，由于最先进的约束模拟，我们将在大角度尺度上对所有可能的次级CMB各向异性的贡献进行首次详尽估计。通过本地化，我们将回答以下问题：能否通过缩放关系精确地、忠实地校准σ8张力，这要归功于本地化模拟中的本地集群克隆？以及有多少低多极CMB异常可以用局地星系外环境来解释，局地LSS克隆完全复制了局地LSS ？

Galaxy clusters offer unique opportunities to test the cosmological model. This relies on the use of statistical assessments of their properties from comparison of simulations and observations. To overcome the limitation of statistical approaches, one would ideally need an actual reproduction of the Universe. Constrained simulations now permit building high fidelity clones of the local Large Scale Structure (LSS) of the Universe within 600Mpc diameter valid down to cluster scales. LOCALIZATION will produce and use simulated clones of local clusters and superclusters to fully understand the building up of these cosmic laboratories. We will study their physical and dynamical properties via cosmic flows, X-rays and Sunyaev-Zeldovich signals and we will derive the cosmological signatures of the local LSS on the cosmic background at large scales. LOCALIZATION will pave the way from precision cosmology from averaged statistics towards accurate understanding of the cosmological growth of structures.Indeed, the ΛCDM model is a great success, still the advent of precision cosmology revealed yet unexplained discrepancies between theoretical expectations and observations. Among these the difference between the linearly evolved amplitude of the matter power spectrum measured with the CMB and galaxy clusters, i.e. σ8 tension, as well as CMB large-scale anomalous features. By revisiting these two debated cosmological issues, LOCALIZATION seeks, for the first time, a common solution to both of them. To address this challenge, a comprehensive analysis of the local galaxy clusters and LSS and of their impact on the CMB will be performed based on the hydrodynamical numerical clones of the local Universe up to z<0.07. An unbiased comparison between observational data from Planck and numerical local cluster, supercluster and full LSS clones will be performed.Thanks to LOCALIZATION’s cluster clones, we will derive for the first time the exact relation between cluster masses and their observed proxies. We will address the CMB anomalies in Planck data focusing on sources of CMB signal that contribute at the largest angular scales from the local supercluster and clusters. In addition thanks to the state-of-the-art constrained simulations, we will perform the first exhaustive estimate of the contribution from all possible secondary CMB anisotropies at large angular scales.With LOCALIZATION we will thus answer the following questions: Can the σ8 tension be solved or reduced with a scaling relation exactly and faithfully calibrated thanks to local cluster clones from LOCALIZATION simulations? and How much of the low-multipole CMB anomalies can be explained by the local extragalactic environment fully reproduced by the local LSS clone built within LOCALIZATION?