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

星系团为检验宇宙学模型提供了独特的机会。这依赖于对其特性的统计评估的使用，这些评估来自模拟和观测的比较。为了克服统计方法的局限性，理想情况下，人们需要一个真实的宇宙复制。受约束的模拟现在允许在600Mpc直径范围内建立宇宙局部大尺度结构(LSS)的高保真克隆，其有效范围可精确到星系团尺度。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性质，并在大尺度上推导出宇宙背景下局部LSS的宇宙学特征。本地化将为精确宇宙学从平均统计到准确理解结构的宇宙学增长铺平道路。事实上，Λ清洁发展机制模型是一个巨大的成功，但精密宇宙学的出现揭示了理论预期和观测之间尚未解释的差异。其中，用CMB和星系团测得的物质功率谱的线性演化幅度之间的差异，即σ8张力，以及CMB的大尺度异常特征。通过重新讨论这两个有争议的宇宙学问题，地方化第一次寻求了这两个问题的共同解决方案。为了应对这一挑战，将根据直到z&lt；0.07的本地宇宙的流体动力学数值克隆，对本地星系团和LSS及其对CMB的影响进行全面分析。我们将把普朗克的观测数据与数值局域星系团、超星系团和全LSS克隆的观测数据进行无偏见的比较。由于局部化的星系团克隆，我们将首次推导出星系团质量与它们的观测指标之间的精确关系。我们将解决普朗克数据中的CMB反常现象，重点是局域超星系团和星系团在最大角度尺度上贡献CMB信号的来源。此外，由于最先进的约束模拟，我们将第一次详尽地估计所有可能的次生天体各向异性在大角度尺度上的贡献。在局部化的情况下，我们将回答以下问题：由于局部化模拟的局部星团克隆，σ8张力能否用标度关系精确而忠实地校准？而CMB的低多极异常有多少可以用局域内建立的LSS克隆完全复制的局域河外环境来解释？

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?