Redshift-space clustering distortions provide one of the most powerful probes to test the gravity theory on the largest cosmological scales. We perform a systematic validation study of the state-of-the-art statistical methods currently used to constrain the linear growth rate from redshift-space distortions in the galaxy two-point correlation function. The numerical pipelines are tested on mock halo catalogues extracted from large N-body simulations of the standard cosmological framework. We consider both the monopole and quadrupole multipole moments of the redshift-space two-point correlation function, as well as the radial and transverse clustering wedges, in the comoving scale range $10<r[$\Mpch$]<55$. Moreover, we investigate the impact of redshift measurement errors on the growth rate and linear bias measurements due to the assumptions in the redshift-space distortion model. Considering both the dispersion model and two widely-used models based on perturbation theory, we find that the linear growth rate is underestimated by about $5-10\%$ at $z<1$, while limiting the analysis at larger scales, $r>30$ \Mpch, the discrepancy is reduced below $5\%$. At higher redshifts, we find instead an overall good agreement between measurements and model predictions. Though this accuracy is good enough for clustering analyses in current redshift surveys, the models have to be further improved not to introduce significant systematics in RSD constraints from next generation galaxy surveys. The effect of redshift errors is degenerate with the one of small-scale random motions, and can be marginalised over in the statistical analysis, not introducing any statistically significant bias in the linear growth constraints, especially at $z\geq1$.
Challenges of standard halo models in constraining galaxy properties from CIB anisotropies
Institutes of Computer Science and Astrophysics, Foundation for Research and Technology Hellas (FORTH)（计算机科学与天体物理研究所，希腊研究与技术基金会）；Aix Marseille Univ, CNRS, CNES, LAM（艾克斯马赛大学）；Université de Strasbourg, CNRS, Observatoire astronomique de Strasbourg, UMR 7550（斯特拉斯堡大学）；Kavli Institute for Particle Astrophysics and Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理学与宇宙学研究所）；SLAC National Accelerator Laboratory（SLAC国家加速器实验室）
How I stop worrying about non-universality and $b_ϕ$: Constraining local $f_{\rm NL}$ with $b_ϕ$ priors from HOD posteriors
Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学）；Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo（东京大学）；Institute For Interdisciplinary Research in Science and Education, ICISE（理科教育跨学科研究所）
Cosmological constraints from galaxy clustering in the presence of massive neutrinos
聚类比定义为平滑后的过密度场的关联函数与方差之比。在不考虑大质量中微子的LCDM宇宙学中，它已经被证明在一系列线性尺度上与偏压和红移空间扭曲无关。因此，它允许直接比较测量（来自红移空间中的星系）和预测（对于真实空间中的物质）。在本文中，我们首先扩展的适用性，包括大规模中微子的宇宙学，通过对模拟数据进行测试的聚类比等属性。然后，我们调查的约束权力的集群比宇宙学参数，如总中微子质量和状态方程的暗能量是自由的。我们分析的联合后验分布的参数，必须满足，在同一时间，在SDSS DR 12中的星系聚类比的测量，和角功率谱的温度和偏振各向异性的CMB测量的普朗克卫星。我们发现，集群比是非常敏感的CDM密度参数，但不是很大，所以总中微子质量。最后，我们预测的约束力的聚类比将实现与即将到来的调查，预测其误差的幅度在欧几里德星系调查。在这种情况下，我们发现，预计将改善约束在95%的水平上的CDM密度的40%和总中微子质量的14%。
