The Einstein Telescope (ET) is a proposed third-generation, wide-band gravitational wave (GW) detector. Given its improved detection sensitivity in comparison to the second-generation detectors, it will be capable of exploring the Universe with GWs up to very high redshifts. In this paper, we present a population-independent method to infer the functional form of star formation rate density (SFR) for different populations of compact binaries originating in stars from Population (Pop) I+II and Pop III using ET as a single instrument. We use an algorithm to answer three major questions regarding the SFR of different populations of compact binaries. Specifically, these questions refer to the termination redshift of the formation of Pop III stars, the redshift at peak SFR, and the functional form of SFR at high redshift, all of which remain to be elucidated. We show that the reconstruction of SFR as a function of redshift for the different populations of compact binaries is independent of the time-delay distributions up to $z \sim 14,$ and that the accuracy of the reconstruction only strongly depends on this distribution at higher redshifts of $z\gtrsim 14$. We define the termination redshift for Pop III stars as the redshift where the SFR drops to 1\% of its peak value. In this analysis, we constrain the peak of the SFR as a function of redshift and show that ET as a single instrument can distinguish the termination redshifts of different SFRs for Pop III stars, which have a true separation of at least $Δz \sim 2$. The accurate estimation of the termination redshift depends on correctly modelling the tail of the time-delay distribution, which constitutes delay times of $\gtrsim 8$ Gyr.
Determining the equation of state of neutron stars with Einstein Telescope using tidal effects and r-mode excitations from a population of binary inspirals
Pre-merger alert to detect the very-high-energy prompt emission from binary neutron-star mergers: Einstein Telescope and Cherenkov Telescope Array synergy
Core-Collapse Supernova detections from Einstein Telescope within the Milky Way
INAF, Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Gran Sasso Science Institute (GSSI)（格兰萨索科学研究所）；INFN, Laboratori Nazionali del Gran Sasso（意大利国家核物理研究所格兰萨索国家实验室）；INAF, Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；DARK, Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所暗物质中心）
Calibration database design for the wide-field X-ray telescope on board the Einstein Probe
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文学院）
Radio sirens: inferring $H_0$ with binary black holes and neutral hydrogen in the era of the Einstein Telescope and the SKA Observatory
Marietta Blau Institute - Austrian Academy of Sciences（玛丽亚·布劳研究所 - 奥地利科学院）；INFN, Sezione di Roma（罗马国家核物理研究所）；Observatoire de la Côte d’Azur, Laboratoire Lagrange（蔚蓝海岸天文台，拉格朗日实验室）；Department of Physics & Astronomy, University of the Western Cape（西开普大学物理与天文学系）；INAF - Institute of Radioastronomy (IRA)（意大利国家天体物理研究所射电天文研究所）；Gran Sasso Science Institute (GSSI)（格兰萨索科学研究所）；INFN - Laboratori Nazionali del Gran Sasso (LNGS)（意大利国家核物理研究所格兰萨索国家实验室）；Dipartimento di Fisica, Università degli Studi di Cagliari（卡利亚里大学物理系）；INFN, Sezione di Cagliari（卡利亚里国家核物理研究所）；INAF - Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）
Tests of General Relativity with Einstein Telescope
Università degli Studi di Padova（帕多瓦大学）；INFN, Sezione di Padova（意大利国家核物理研究所帕多瓦分部）；Università di Pisa（比萨大学）；INFN, Sezione di Pisa（意大利国家核物理研究所比萨分部）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理学研究所（阿尔伯特·爱因斯坦研究所））
Constraining Wormhole Geometries using the Orbit of S2 Star and the Event Horizon Telescope
在本文中，我们研究的可能性，有一个虫洞（WH）作为一个候选人的Sgr A $^\star$中心对象和测试这个想法，通过限制他们的几何形状使用的运动S2星和重建的阴影图像。特别地，我们考虑三个WH模型，包括爱因斯坦理论中的WH，膜世界引力和Einstein-Dirac-Maxwell理论。为此，我们约束WH喉使用的运动S2星，并表明耀斑的条件是满足的。我们还考虑了下落气体的吸积模型，研究了吸积率、电磁辐射强度和阴影像。
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）
Fast and accurate parameter estimation of high-redshift sources with the Einstein Telescope
Gran Sasso Science Institute (GSSI)（格兰萨索科学研究所）；INFN, Laboratori Nazionali del Gran Sasso（意大利国家核物理研究所，格兰萨索国家实验室）；Institute of High Energy Physics - Austrian Academy of Sciences（奥地利科学院高能物理研究所）；ETH Zurich（苏黎世联邦理工学院）；ELLIS Institute Tübingen（蒂宾根欧洲语言学习研究所）；Max Planck Institute for Intelligent Systems（马克斯·普朗克智能系统研究所）；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））；University of Nottingham（诺丁汉大学）；University of Maryland, College Park（马里兰大学帕克分校）；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（卡弗里宇宙学剑桥研究所）；H.H. Wills Physics Laboratory（H.H.威尔斯物理实验室）；Johns Hopkins University（约翰斯·霍普金斯大学）
Natural Supercooling and Reheating along Supersymmetric Flat Directions and Observable Gravitational Waves at the Einstein Telescope and the Cosmic Explorer
Multi-messenger observations in the Einstein Telescope era: binary neutron star and black hole - neutron star mergers
INAF – Osservatorio Astronomico di Brera（意大利国家天体物理研究所比拉天文台）；INFN – Sezione di Milano-Bicocca（意大利国家核物理研究所米兰-比科卡分校）；Département de Physique Théorique, Université de Genève（日内瓦大学理论物理系）；Gravitational Wave Science Center (GWSC), Université de Genève（日内瓦大学引力波科学中心）；William H. Miller III Department of Physics and Astronomy, Johns Hopkins University（约翰斯·霍普金斯大学威廉·H·米勒三世物理与天文学系）；Aix-Marseille Université, Université de Toulon, CNRS, CPT, Marseille（艾克斯-马赛大学、土伦大学、法国国家科学研究中心、CPT）
