Next-generation ground-based gravitational-wave detectors, such as Cosmic Explorer (CE), are expected to be sensitive to gravitational-wave signals with frequencies as low as 5 Hz, allowing signals to spend a significant amount of time in the detector frequency band. As a result, the effects caused by the rotation of the Earth become increasingly important for such signals. Additionally, the length of the arms of these detectors can be comparable to the wavelength of detectable gravitational waves, which introduces frequency-dependent effects that are not significant in current-generation detectors. These effects are expected to improve the ability to localize compact binary coalescences in the sky even when using only one detector. This study aims to understand how much these effects can help in localization. We present the first comprehensive Bayesian parameter estimation framework that accounts for all these effects using \textsc{Bilby}, a commonly used Bayesian parameter estimation tool. We focus on sky localization constraints for binary neutron star events with an optimal signal-to-noise ratio of 1000 with one detector at the projected CE sensitivity. We find that these effects help localize sources using one detector with sky areas as low as 10 square degrees. Moreover, we explore and discuss how ignoring these effects in the parameter estimation can lead to biases in the inference.
Inferring the role of binary neutron star mergers in r-process nucleosynthesis with multi-messenger observations using Cosmic Explorer and Einstein Telescope
Institute of Physics, University of Greifswald（格赖夫斯瓦尔德大学物理研究所）；Department of Astronomy & Astrophysics, Tata Institute of Fundamental Research（塔塔基础研究院天文学与天体物理学系）
Improved early-warning estimates of luminosity distance and orbital inclination of compact binary mergers using higher modes of gravitational radiation
Precision constraints on the neutron star equation of state with third-generation gravitational-wave observatories
International Centre for Radio Astronomy Research, University of Western Australia（西澳大利亚大学国际射电天文研究中心）；OzGrav: The ARC Centre of Excellence for Gravitational Wave Discovery（ARC引力波发现卓越中心）；School of Physics and Astronomy, Monash University（蒙纳士大学物理与天文学院）；Swinburne University of Technology（斯威本科技大学）
Fast targeted gravitational-wave followup search for compact binary mergers using GSTLAL pipeline
University of Nevada, Las Vegas（内华达大学拉斯维加斯分校）；Georgia Institute of Technology（佐治亚理工学院）；The Pennsylvania State University（宾夕法尼亚州立大学）；University of California, Berkeley（加州大学伯克利分校）
Detectability of QCD phase transitions in binary neutron star mergers: Bayesian inference with the next generation gravitational wave detectors
The Pennsylvania State University（宾夕法尼亚州立大学）；Friedrich-Schiller-Universität Jena（耶拿弗里德里希·席勒大学）；Scuola Internazionale Superiore di Studi Avanzati (SISSA)（高级国际研究学院）；Istituto Nazionale di Fisica Nucleare (INFN)（意大利国家核物理研究所）
Distinguishing the Origin of Eccentric Black Hole Mergers with Gravitational-wave Spin Measurements
Max Planck Institute for Astrophysics（马克斯·普朗克天体物理研究所）；Dipartimento di Fisica “G. Occhialini”, Università degli Studi di Milano-Bicocca（米兰比可卡大学 G. Occhialini 物理系）；INFN, Sezione di Milano-Bicocca（意大利国家核物理学会米兰比可卡分部）；Department of Applied Mathematics and Theoretical Physics, Cambridge（剑桥大学应用数学与理论物理系）；Kavli Institute for Cosmology Cambridge（剑桥卡弗里宇宙学研究所）；Shanghai Astronomical Observatory（上海天文台）；Niels Bohr International Academy, The Niels Bohr Institute（尼尔斯·玻尔国际学院，尼尔斯·玻尔研究所）
Measuring the delay time distribution of binary neutron stars. II. Using the redshift distribution from third-generation gravitational wave detectors network
Black holes in the low mass gap: Implications for gravitational wave observations
Pennsylvania State University（宾夕法尼亚州立大学）；University of Birmingham（伯明翰大学）；Chennai Mathematical Institute（金奈数学研究所）；Johns Hopkins University（约翰斯·霍普金斯大学）；Cardiff University（卡迪夫大学）；Flatiron Institute（平顿研究所）；Stony Brook University（石溪大学）；The University of Mississippi（密西西比大学）
Distinguishing cosmology, astrophysics and systematics: the Bayesian search for a primordial gravitational-wave background in next-generation observatories
Princeton University（普林斯顿大学）；University of Nevada, Las Vegas（内华达大学拉斯维加斯分校）
Pre-localization of Massive Black Hole Binaries in the Millihertz Band
Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（阿尔伯特·爱因斯坦研究所））；TianQin Research Center for Gravitational Physics, Sun Yat-sen University（中山大学天琴引力物理研究中心）；School of Physics and Astronomy, Sun Yat-sen University（中山大学物理学院）；School of Physics and Astronomy, University of Glasgow（格拉斯哥大学物理与天文学院）；Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Artemis（蔚蓝海岸大学、蔚蓝海岸天文台、法国国家科学研究中心阿耳忒弥斯实验室）
A case study of GW190425 for classifying binary neutron star versus binary black hole mergers and constraining asymmetric dark matter with gravitational wave detectors
Detection, sky localization and early warning for binary neutron star mergers by detectors located in China of different configurations in third generation detector network
本文评估了在中国部署不同构型第三代探测器对 ET-CE 网络探测双中子星并合的提升，发现中国探测器可提高探测率、显著改善天区定位并增强预警能力，其中 20 km 高频探测器在远距离探测上贡献突出。
Real-Time Multi-Mode Post-Merger Gravitational Wave Detection using Convolutional Neural Networks: Methodology Development for Third-Generation Detectors
Department of Astronomy & Astrophysics, The Pennsylvania State University（天文学与天体物理系，宾夕法尼亚州立大学）
Too small to fail: characterizing sub-solar mass black hole mergers with gravitational waves
LIGO Laboratory, Massachusetts Institute of Technology（麻省理工学院）；Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology（麻省理工学院）
