The 6dF Galaxy Survey: Peculiar Velocity Field and Cosmography
Christopher M. Springob, Christina Magoulas, Matthew Colless, Jeremy Mould, Pirin Erdogdu, D. Heath Jones, John R. Lucey, Lachlan Campbell, Christopher J. Fluke
备注：
22 pages, 14 figures, accepted for publication in MNRAS. Table 1 is available in its entirety as an ancillary file. Fully interactive 3D versions of Figures 11 and 12 are also available as ancillary files. A version of this paper with the 3D versions of Figs. 11 and 12 embedded within the pdf can also be accessed from http://www.6dfgs.net/vfield/veldata.pdf
We derive peculiar velocities for the 6dF Galaxy Survey (6dFGS) and describe the velocity field of the nearby ($z<0.055$) southern hemisphere. The survey comprises 8885 galaxies for which we have previously reported Fundamental Plane data. We obtain peculiar velocity probability distributions for the redshift space positions of each of these galaxies using a Bayesian approach. Accounting for selection bias, we find that the logarithmic distance uncertainty is 0.11 dex, corresponding to $26\%$ in linear distance. We use adaptive kernel smoothing to map the observed 6dFGS velocity field out to $cz \sim 16,000$ \kms, and compare this to the predicted velocity fields from the PSCz Survey and the 2MASS Redshift Survey. We find a better fit to the PSCz prediction, although the reduced $χ^2$ for the whole sample is approximately unity for both comparisons. This means that, within the observational uncertainties due to redshift independent distance errors, observed galaxy velocities and those predicted by the linear approximation from the density field agree. However, we find peculiar velocities that are systematically more positive than model predictions in the direction of the Shapley and Vela superclusters, and systematically more negative than model predictions in the direction of the Pisces-Cetus Supercluster, suggesting contributions from volumes not covered by the models.
TDCOSMO XXIV. First spatially resolved kinematics of the lens galaxy obtained using JWST-NIRSpec to improve time-delay cosmography
Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；Center for Astronomy, Space Science and Astrophysics, Independent University, Bangladesh（孟加拉独立大学天文学、空间科学与天体物理中心）；Department of Physics and Astronomy, University of California, Los Angeles（加州大学洛杉矶分校物理与天文系）；Technical University of Munich, TUM School of Natural Sciences, Physics Department（慕尼黑工业大学自然科学院物理系）；Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；Sub-Department of Astrophysics, Department of Physics, University of Oxford（牛津大学物理系天体物理子部门）
Effects of a central dark matter core on time-delay cosmography with galaxy clusters
Institute of Astronomy and Physics, Inner Mongolia University（内蒙古大学天文与物理学院）；School of Physical Science and Technology, Inner Mongolia University（内蒙古大学物理科学与技术学院）；Center for Frontier Science, Chiba University（千叶大学前沿科学中心）；Department of Physics, Graduate School of Science, Chiba University（千叶大学理学研究科物理学系）
TDCOSMO XIX. Measuring stellar velocity dispersion with sub-percent accuracy for cosmography
University of California, Los Angeles（加州大学洛杉矶分校）；University of Chicago（芝加哥大学）；Independent University, Bangladesh（孟加拉国独立大学）；University of Oxford（牛津大学）；Stony Brook University（石溪大学）
Constraining Primordial Power Asymmetry from Galaxy Clustering and Peculiar Velocity Information
Kyoto University（京都大学）；Yukawa Institute for Theoretical Physics, Kyoto University（京都大学汤川理论物理研究所）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo（东京大学前沿科学高等研究院宇宙物理数学卡弗里研究所（WPI））；Korea Institute for Advanced Study（韩国高等科学研究院）；Academia Sinica Institute of Astronomy and Astrophysics (ASIAA)（中央研究院天文及天文物理学研究所）；Onomichi City University（尾道市立大学）
An accurate method to determine the systematics due to the peculiar velocities of galaxies in measuring the Hubble constant from gravitational wave standard sirens
Cosmography of the Sloan Basin of Attraction and Neighborhood
Institut de Recherche sur les Lois Fondamentales de l’Univers, CEA, Université Paris-Saclay（基础物理规律研究所，法国原子能委员会，巴黎萨克雷大学）；Institute for Astronomy, University of Hawaii（天体物理研究所，夏威夷大学）；Aix Marseille Université, CNRS/IN2P3, CPPM（艾克斯-马赛大学，法国国家科学研究中心/欧洲核子与粒子物理研究所，粒子物理中心）；Leibniz Institut für Astrophysik Potsdam (AIP)（波茨坦阿基米德天体物理研究所）；Racah Institute of Physics, Hebrew University（拉卡物理学系，希伯来大学）
利用哈密顿蒙特卡洛前向重建方法，在ΛCDM框架下基于Cosmicflows-4数据重建速度场，识别并描述了斯隆吸引盆（Sloan Basin of Attraction）的结构特征及其与Ho`oleilana重子声学振荡特征的关系。
Effective Theories of Redshift-Space Galaxy Peculiar Velocities
School of Natural Sciences, Institute for Advanced Study（自然科技学院，高等研究院）；Physics Department, Columbia University（哥伦比亚大学物理系）；School of Mathematics and Physics, The University of Queensland（昆士兰大学数学与物理学院）；Aix-Marseille University, CNRS/IN2P3, CPPM（艾克斯-马赛大学，法国国家科学研究中心/欧洲核子研究组织粒子与物理研究所，粒子与宇宙学中心）
TDCOSMO IV: Hierarchical time-delay cosmography -- joint inference of the Hubble constant and galaxy density profiles
H 0 LiCOW合作推断通过引力透镜时间延迟哈勃常数$H_0=73.3^{+1.7}_{-1.8}$公里秒$^{-1}{\rm Mpc}^{-1}$，描述偏转器质量密度分布的幂律或恒星加上标准的暗物质晕。保持透镜观测量不变的质量片变换（MST）被认为是$H_0$中剩余不确定性的主要来源。我们量化任何潜在的影响MST与灵活的质量模型，最大限度地退化与H 0。我们的计算是基于一个新的层次的方法，其中MST只受恒星运动学。该方法在流体动力学模拟透镜上进行了验证。我们将该方法应用于7个镜片的TDCOSMO样品（6个来自H 0 LiCOW）并测量了$H_0=74.5^{+5.6}_{-6.1}$ km s $^{-1}{\rm Mpc}^{-1}$。为了进一步限制偏转器质量分布，我们然后添加了来自SLACS样本的33个强引力透镜的成像和光谱学。对于9个SLAC透镜，我们使用解析的运动学来约束恒星的各向异性。从TDCOSMO+SLACS样本的联合分析，我们测量$H_0=67.4^{+4.1}_{-3.2}$ km s $^{-1}{\rm Mpc}^{-1}$，假设TDCOSMO和SLACS星系是从相同的母体人口。盲态H 0 LiCOW、仅TDCOSMO和TDCOSMO+SLACS分析在统计学上相互一致。TDCOSMO+SLACS分析比H 0 LiCOW或仅TDCOSMO更倾向于略微浅的质量…
Correlated residuals in Tully-Fisher and Fundamental Plane relations and their impact on peculiar velocity measurements
Aix Marseille Univ, CNRS/IN2P3, CPPM（艾克斯-马赛大学，法国国家科学研究中心/法国国家核与粒子物理研究所，普罗旺斯宇宙粒子物理中心）；Universitat Autònoma de Barcelona, IFAE（巴塞罗那自治大学，高能物理研究所）；Donostia International Physics Center（圣塞巴斯蒂安国际物理中心）；IKERBASQUE, Basque Foundation for Science（伊克尔巴斯基克，巴斯克科学基金会）；LadHyX UMR CNRS 7646, École Polytechnique, Institut Polytechnique de Paris（拉迪克斯实验室（CNRS联合研究单位7646），巴黎综合理工学院，巴黎理工学院）；Institute for Computational Cosmology, Department of Physics, Durham University（达勒姆大学物理系计算宇宙学研究所）；Harvard-Smithsonian Center for Astrophysics（哈佛-史密森尼天体物理中心）
Cosmography with DESI-DR1 Cosmic Chronometers: Direct H(z) measurements from Luminous Red Galaxy ages
Scuola Internazionale Superiore di Studi Avanzati (SISSA)（国际高等研究院）；Facultad de Ciencias, Universidad de Oviedo（奥维耶多大学理学院）；Institute for Fundamental Physics of the Universe (IFPU)（宇宙基础物理研究所）；Dipartimento di Fisica e Astronomia “Augusto Righi”–Università di Bologna（博洛尼塔大学物理与天文学系）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（博洛尼亚天文物理与空间科学国家研究所）；IRA-INAF（意大利国家天体物理研究所）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；Universitat Heidelberg, Zentrum fur Astronomie, Institut fur theoretische Astrophysik（海德堡大学天文学中心理论天体物理研究所）
Probing the environment around GW170817 with DESI: insights on galaxy group peculiar velocities for standard siren measurements
Carnegie Mellon University（卡内基梅隆大学）；University of Rochester（罗切斯特大学）；University of Queensland（昆士兰大学）；SLAC National Accelerator Laboratory（斯坦福直线加速器中心）；Siena University（锡耶纳大学）；Stanford University（斯坦福大学）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Boston University（波士顿大学）；University College London（伦敦大学学院）；Korea Astronomy and Space Science Institute（韩国天文与空间科学研究所）；NSF NOIRLab（美国国家光学-红外天文研究实验室）；University of Toronto（多伦多大学）；University of Pittsburgh（匹兹堡大学）；The Barcelona Institute of Science and Technology（巴塞罗那科学技术研究院）；University of Portsmouth（朴茨茅斯大学）；ICE-CSIC（宇宙学与统计物理研究所）；University of Virginia（弗吉尼亚大学）；Fermi National Accelerator Laboratory（费米国家加速器实验室）；The Ohio State University（俄亥俄州立大学）；The University of Texas at Dallas（德克萨斯大学达拉斯分校）；Southern Methodist University（南方卫理公会大学）
