Abundances, masses and weak-lensing mass profiles of galaxy clusters as a function of richness and luminosity in ΛCDM cosmologies
Abundances, masses and weak-lensing mass profiles of galaxy clusters as a function of richness and luminosity in ΛCDM cosmologies
复制标题
DOI：
10.1111/j.1365-2966.2010.16310.x
复制
发表时间：
2009-07
影响因子：
4.8
通讯作者：
S. Hilbert;S. White
中科院分区：
文献类型：
--
作者：
S. Hilbert;S. White
我们通过比较星系团平均性质的预测与观测结果来测试和谐冷暗物质（CDM）宇宙学。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星系团的丰度，平均密度分布和质量作为丰富度和光度的函数，我们比较这些预测在斯隆数字巡天（SDSS）maxBCG目录中的星系团的观测。讨论了质量丰度关系的离散性、由质量丰度关系重构的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，通过比较银河系模型的千禧年模拟（MS）和WMAP1模拟从WMAP3模拟的结果。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。在模拟的质量丰富度关系接近观察到的关系，差异30%.MS和WMAP1模拟产生集群的丰度类似于观察到的，而在WMAP3模拟的丰度低两到三倍。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。预测值和观测值之间应达到更好的一致性，归一化为0.722
We test the concordancecold dark matter (� CDM) cosmology by comparing predictions for the mean properties of galaxy clusters to observations. We use high-resolution N-body simula- tions 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 the WMAP1 simulation to those from the 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 30 per cent. The MS and WMAP1 simulations yield cluster abundances similar to those observed, whereas abundances in the WMAP3 simulation are two to three 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 normalization σ 8. Better agreement between predictions and observations should be reached with a normalization 0.722