The power spectrum is the most commonly applied summary statistics to extract cosmological information from the observed three-dimensional distribution of galaxies in spectroscopic surveys. We present CLASS-OneLoop, a new numerical tool, fully integrated into the Boltzmann code CLASS, enabling the calculation of the one-loop power spectrum of biased tracers in spectroscopic surveys. Built upon the Eulerian moment expansion framework for redshift-space distortions, the implemented model incorporates a complete set of nonlinear biases, counterterms, and stochastic contributions, and includes the infrared resummation and the Alcock-Paczynski effect. The code features an evaluation of the loops by either direct numerical integration or Fast Fourier Transform, and employs a fast-slow parameter decomposition, which is essential for accelerating MCMC runs. After presenting performance and validation tests, as an illustration of the capabilities of the code, we apply it to fit the measured redshift-space halo power spectrum wedges on a $Λ$CDM subset of the AbacusSummit simulation suite and considering scales up to $k_{\rm max} = 0.3\,h/$Mpc. We find that the one-loop model adeptly recovers the fiducial cosmology of the simulation, while a simplified model commonly used in the literature for sensitivity forecasts yields significantly biased results. Furthermore, we conduct Monte Carlo Markov Chain (MCMC) forecasts for a DESI-like survey, considering a model with a dynamical dark energy component. Our results demonstrate the ability to independently constrain cosmological and nuisance parameters, even in the presence of a large parameter space with twenty-nine variables.
An ALMA survey of submillimetre galaxies in the Extended Chandra Deep Field South: an unbiased study of SMG environments measured with narrowband imaging
Evolution of The Velocity-Dispersion Function of Luminous Red Galaxies: A Hierarchical Bayesian Measurement
本文给出了斯隆数字巡天III（SDSS-III）重子振荡光谱巡天（BOSS）在相对低的光谱信噪比（SNR ~3-5/69 km s^（-1））下观测到的大约430，000个大质量发光红星系（LRGs）的速度色散函数的分级贝叶斯确定。我们边缘化的光谱红移误差，并使用完整的速度色散似然函数为每个星系的速度色散分布参数作为一个函数的绝对星等和红移的自我一致的确定，以及校正宽带的大小误差对我们的合并的影响。参数化的分布在每一个点的亮度红移平面与对数正态形式，我们检测到显着的演变，在更高的红移的分布的宽度向更高的内在散射。使用一个子集的深重新观测的BOSS星系，我们证明了我们的分布参数估计是无偏的，无论光谱信噪比。我们还通过模拟表明，我们的方法没有引入系统参数的红移偏置。我们强调的优势，层次贝叶斯方法的频谱频率论的“堆叠”，并说明我们测得的分布参数可以通过作为信息先验的速度分散测量从个别嘈杂的光谱。
The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: measurement of the growth rate of structure from the small-scale clustering of the luminous red galaxy sample
Growth rate measurements from a joint analysis of the large-scale galaxy clustering in Fourier and configuration space
Aix Marseille Univ, CNRS/IN2P3, CPPM（艾克斯马赛大学）；IRFU, CEA, Université Paris-Saclay（法国原子能和替代能源委员会IRFU、巴黎萨克雷大学）；Departament de Física Quàntica i Astrofísica, Universitat de Barcelona（巴塞罗那大学量子物理与天体物理学系）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究所）；Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB)（巴塞罗那宇宙科学研究所）
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological implications of the configuration-space clustering wedges
The Impact of Spectroscopic Redshift Errors on Cosmological Measurements
École Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院）；The University of Tokyo（东京大学）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study (UTIAS)（东京大学宇宙物理数学研究所（ Kavli 研究所））；Universitat de Barcelona (UB)（巴塞罗那大学）；Tsinghua University（清华大学）；CEA, Université Paris-Saclay（巴黎萨克雷大学）；University of Cambridge（剑桥大学）
The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Pairwise-Inverse-Probability and Angular Correction for Fibre Collisions in Clustering Measurements
完成的eBOSS星表包含344080个红移超过0.8<z<2.2的类星体，覆盖4808度$^2$，174816个0.6<z<1.0的LRG，覆盖4242 deg $^2$，173736个0.6<z<1.1覆盖1170度的$^2$，以便通过集群测量来约束宇宙的膨胀历史和结构的增长率。斯隆望远镜上的光纤光谱仪的机械限制阻止了两条光纤放置在62”（光纤碰撞尺度）以下，在仪器在天空中的单次通过中。这些“纤维碰撞”与目标的固有群集密切相关，并可能使两点关联函数的测量产生偏差，导致宇宙学参数推断值出现系统误差。我们结合成对逆概率加权和角向上加权的新技术来校正纤维碰撞效应的聚类测量。使用模拟目录，我们表明，我们的校正提供无偏的测量，在数据精度范围内，投影相关函数$w_p$和多极$ξ^l$的红移空间关联函数下降到0.1Mpc/h，无论示踪剂类型。我们将更正应用于eBOSS DR 16目录。我们发现，在大于s~ 20 Mpc/h的$ξ^l$的尺度上，用于进行BAO和大规模RSD测量，考虑到数据的统计误差，近似方法如最近邻上加权是足够准确的。使用PIP方法，第一次为斯隆数字巡天的光谱程序，我们能够成功地访问1-晕项的三维聚类测量下降到~0.1Mpc/h的规模。因此，我们的研究结果将允许使用小规模的集群测量，以加强对宇宙学参数和晕占据分布模型的约束。
Lens Modeling and Cosmological Inference from an Impure Sample of Galaxy-Galaxy Strong Lenses
University of Portsmouth（朴茨茅斯大学）；University of Oxford（牛津大学）；Stanford University（斯坦福大学）；SLAC National Accelerator Laboratory（SLAC国家加速器实验室）；University of Illinois Urbana-Champagin（伊利诺伊大学厄巴纳-香槟分校）；Stony Brook University（石溪大学）
