Observations of gravitational waves from binary black hole (BBH) mergers have measured the redshift evolution of the BBH merger rate. The number density of galaxies in the Universe evolves differently with redshift based on their physical properties, such as their stellar masses and star formation rates. In this work we show that the measured population-level redshift distribution of BBHs sheds light on the properties of their probable host-galaxies. We first assume that the hosts of BBHs can be described by a mixture model of galaxies weighted by stellar mass or star formation rate, and find that we can place upper limits on the fraction of mergers coming from a stellar mass weighted sample of galaxies. We then constrain parameters of a physically motivated power-law delay-time distribution using GWTC-3 data, and self-consistently track galaxies in the \textsc{UniverseMachine} simulations with this delay-time model to infer the probable host-galaxies of BBHs over a range of redshifts. We find that the inferred host-galaxy distribution at redshift $z=0.21$ has a median star formation rate $\sim 0.9\,M_\odot\mathrm{yr}^{-1}$ and a median stellar mass of $\sim 1.9 \times 10^{10}\,M_\odot$. We also provide distributions for the mean stellar age, halo mass, halo radius, peculiar velocity, and large scale bias associated with the host-galaxies, as well as their absolute magnitudes in the B- and ${ \rm K_s}$-bands. Our results can be used to design optimal electromagnetic follow-up strategies for BBHs, and also to aid the measurement of cosmological parameters using the statistical dark siren method.
Searching for gravitational waves from compact binary mergers powering long gamma-ray bursts during LIGO-Virgo-KAGRA's O3 run
Monash University（莫纳什大学）；OzGrav: The ARC Centre of Excellence for Gravitational Wave Discovery（引力波发现ARC卓越中心）；Princeton University（普林斯顿大学）；University of Cambridge（剑桥大学）
The Proper Motion of Strongly Lensed Binary Neutron Star Mergers in LIGO/Virgo/Kagra can be Constrained by Measuring Doppler Induced Gravitational Wave Dephasing
Search for continuous gravitational waves from neutron stars in five globular clusters in the first part of the fourth LIGO-Virgo-KAGRA observing run
University of Michigan（密歇根大学）；Universitat de les Illes Balears（巴利阿里群岛大学）；LIGO Livingston Observatory（LIGO利文斯顿天文台）；Instituto Nacional de Pesquisas Espaciais（国家空间研究所）；University of British Columbia（不列颠哥伦比亚大学）；University of Melbourne（墨尔本大学）
Scalar fields around black hole binaries in LIGO-Virgo-KAGRA
Université Catholique de Louvain（天主教鲁汶大学）；Royal Observatory of Belgium（比利时皇家天文台）；University of Amsterdam（阿姆斯特丹大学）；Massachusetts Institute of Technology（麻省理工学院）；Queen Mary University of London（伦敦玛丽女王大学）；University of Oxford（牛津大学）
Application of the third RIT binary black hole simulations catalog to parameter estimation of gravitational waves signals from the LIGO-Virgo O1/O2 observational runs
Searches for inspiral gravitational waves associated with short gamma-ray bursts in LIGO's fifth and Virgo's first science run
两个致密物体的合并，比如两颗中子星或一颗中子星和一个黑洞，很可能是短伽马射线暴的起源。这些事件也是有希望的引力波来源，目前正在激发国际引力波探测器网络的相关搜索。在这里，我们描述了一个搜索的引力波从螺旋阶段的两个合并紧凑的对象，在巧合的短伽玛射线暴发生在LIGO的第五次科学运行和处女座的第一次科学运行。这次搜索包括22个GRB，这些GRB的数据来自LIGO/Virgo网络中的多个探测器。没有发现统计上显著的引力波候选者，参数检验表明在我们的伽玛暴样本中没有多余的弱引力波信号。90%~ C. L.在中子星-黑洞祖先模型假设下，我们的样本中伽玛暴的中位排斥距离为6.7 Mpc。
How do the LIGO-Virgo-KAGRA's Heavy Black Holes Form? No evidence for core-collapse Intermediate-mass black holes in GWTC-4
Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台暗物质与空间天文重点实验室）；Institute for Theoretical Physics and Cosmology, Zhejiang University of Technology（浙江工业大学理论物理与宇宙学研究所）；Department of Physics, Anhui Normal University（安徽师范大学物理系）
Archival Search for IceCube Sub-TeV Neutrino Counterparts to Sub-Threshold Gravitational Wave Events from the Third Observing Run of the LIGO-Virgo-KAGRA
Search for gravitational waves associated with high-energy neutrinos detected by IceCube during the third observing run of LIGO-Virgo
Universiteit Gent（根特大学）；STAR Institute, Université de Liège（列日大学STAR研究所）；Johns Hopkins University（约翰斯·霍普金斯大学）；University of Catania（卡塔尼亚大学）；Cardiff University（卡迪夫大学）
Constraints on the Population of Common Sources of Gravitational Waves and High-Energy Neutrinos with IceCube During the Third Observing Run of the LIGO and Virgo Detectors
Orta Doğu Teknik Üniversitesi（中东技术大学）；Columbia University in the City of New York（纽约市哥伦比亚大学）
Constraints on primordial black holes from the first part of LIGO-Virgo-KAGRA fourth observing run
LIGO Laboratory, Massachusetts Institute of Technology（麻省理工学院）；Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院）；Institut de Física d’Altes Energies (IFAE), Barcelona Institute of Science and Technology（巴塞罗那科学技术大学）；New York University Abu Dhabi（纽约大学阿布扎比分校）；Keemilise ja Bioloogilise Füüsika Instituut（塔尔图大学化学与生物物理研究所）；Dipartimento di Fisica e Astronomia, Università degli Studi di Padova（帕多瓦大学）；Istituto Nazionale di Fisica Nucleare, Sezione di Padova（意大利国家核物理研究所）；Catalan Institution for Research and Advanced Studies (ICREA)（加泰罗尼亚研究高级学院）
Detecting electromagnetic counterparts to LIGO/Virgo/KAGRA gravitational wave events with DECam: Neutron Star Mergers
Carnegie Mellon University（卡内基梅隆大学）；University of Chicago（芝加哥大学）；University of Ferrara（费拉拉大学）；INFN, Sezione di Ferrara（意大利国家核物理研究所费拉拉分部）；INAF, Osservatorio Astronomico d’Abruzzo（意大利国家天体物理研究所阿布鲁佐天文台）；Universität Potsdam（波茨坦大学）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理学研究所（爱因斯坦研究所））；Utrecht University（乌得勒支大学）；Nikhef（荷兰国家核物理与粒子物理研究所）；California Institute of Technology（加州理工学院）；University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校）
Implications of recoil kicks for black hole mergers from LIGO/Virgo catalogs
LIGO/Virgo合作的第一和第二个引力波瞬态目录包括$50$确认的合并事件，来自第一，第二和第三次观测运行的前半部分。我们计算反冲踢的分布赋予合并残余物和估计其保留概率在各种天体物理环境中的最大祖自旋（$χ_{\rm max}$）的函数，假设LIGO/处女座二进制黑洞（BBH）合并催化的动态组装在一个致密的星团。我们发现，对于$0.1$，$0.3$，$0.5$，$0.8$的最大祖自旋，平均反冲分布分别在$150$ km s $^{-1}$，$250$ km s $^{-1}$，$350$ km s $^{-1}$，$600$ km s $^{-1}$附近达到峰值.只有逃逸速度为$\gtrsim 100$ km s $^{-1}$的环境，如在银河系核星团以及最大质量的球状星团和超级星团中发现的那样，才能有效地保留LIGO/室女座BBH人口的合并残余，即使是低祖先自旋（$χ_{\rm max}=0.1$）。在高祖先自旋（$χ_{\rm max}\gtrsim 0.5$）的情况下，只有质量最大的核星团才能保留合并产物。我们还发现，如果GW 170729，GW 190412，GW 190519和GW 190620的祖先是中等自旋（$χ_{\rm max}\gtrsim 0.3$），而GW 190517的祖先是快速自旋（$χ_{\rm max}\gtrsim 0.8$），则可以再现有效自…
