在LambdaCDM宇宙学中星系团的丰度、质量和弱透镜质量分布作为丰度和光度的函数
Abundances, masses, and weak-lensing mass profiles of galaxy clusters as a function of richness and luminosity in LambdaCDM cosmologies
摘要：
我们测试的一致性LCDM宇宙学比较预测的平均性能的星系团的观测。我们使用高分辨率的N体模拟宇宙结构的形成和星系形成的半解析模型来计算的丰度，平均密度分布，和质量的星系团的丰富度和光度的函数，我们比较这些预测的观察斯隆数字巡天（SDSS）maxBCG目录中的集群。讨论了质量丰度关系中的散射、由质量丰度关系重建星系团质量函数以及对弱透镜星系团质量分布的拟合。宇宙学参数的预测的影响进行了研究，通过比较结果从银河系模型的基础上千年模拟（MS）和另一个WMAP 1模拟从WMAP 3模拟。我们发现模拟的弱透镜质量分布和观测到的SDSS maxBCG团簇的分布在形状和振幅上吻合得很好。模拟中的质量-丰度关系与观测关系接近，相差不超过30%。MS和WMAP 1模拟产生的星团丰度与观察到的相似，而WMAP 3模拟中的丰度要低2-3倍。模拟和观测之间的星系团丰度、质量和密度振幅的差异可以归因于基础宇宙学参数的差异，特别是功率谱归一化σ_8。预测和观测之间的更好的一致性应该通过归一化$0.722<sigma_8<0.9$（可能更接近上限值）来实现，即在两个模拟集的基础值之间。
英文摘要：
We test the concordance LCDM cosmology by comparing predictions for the mean properties of galaxy clusters to observations. We use high-resolution N-body simulations of cosmic structure formation and semi-analytic models of galaxy formation to compute the abundance, mean density profile, and mass of galaxy clusters as a function of richness and luminosity, and we compare these predictions to observations of clusters in the Sloan Digital Sky Survey (SDSS) maxBCG catalogue. We discuss the scatter in the mass-richness relation, the reconstruction of the cluster mass function from the mass-richness relation, and fits to the weak-lensing cluster mass profiles. The impact of cosmological parameters on the predictions is investigated by comparing results from galaxy models based on the Millennium Simulation (MS) and another WMAP1 simulation to those from a WMAP3 simulation. We find that the simulated weak-lensing mass profiles and the observed profiles of the SDSS maxBCG clusters agree well in shape and amplitude. The mass-richness relations in the simulations are close to the observed relation, with differences lesssim 30%. The MS and WMAP1 simulations yield cluster abundances similar to those observed, whereas abundances in the WMAP3 simulation are 2-3 times lower. The differences in cluster abundance, mass, and density amplitude between the simulations and the observations can be attributed to differences in the underlying cosmological parameters, in particular the power spectrum normalisation sigma_8. Better agreement between predictions and observations should be reached with a normalisation $0.722<sigma_8<0.9$ (probably closer to the upper value), i.e. between the values underlying the two simulation sets.
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