The Einstein Telescope (ET), a wide-band, future third generation gravitational wave detector, is expected to have detection rates of $\sim 10^5 - 10^6$ binary black hole (BBH) detections and $\sim 7 \times 10^4$ binary neutron star (BNS) detections in one year. The coalescence of compact binaries with a total mass of 20 - 100 $M_{\odot}$, typical of BH-BH or BH-NS binaries, will be visible up to redshift $z\approx 20$ and even higher, thus facilitating the understanding of the dark era of the Universe preceding the birth of the first stars. The ET will therefore be a crucial instrument for population studies. We analysed the compact binaries originating in stars from (i) Population (Pop) I+II, (ii) Pop III, and (iii) globular clusters (GCs), with the single ET instrument, using the ET-D design sensitivity for the analysis. We estimated the constraints on the chirp mass, redshift, and merger rate as function of redshift for these classes of compact object binaries. We conclude that the ET as a single instrument is capable of detecting and distinguishing different compact binary populations separated in chirp mass - redshift space. While compact binaries originating in stars from Pop III are clearly distinguishable, owing to the separation in chirp mass - redshift space, the other two populations, Pop I+II, and GCs, can be distinguished with just 500 detections, corresponding to an observation time of $\sim 1$ hr. The mass distribution characteristics of such different compact binary populations can also be estimated with the single ET instrument.
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）
Determining the equation of state of neutron stars with Einstein Telescope using tidal effects and r-mode excitations from a population of binary inspirals
Exploring sub-GeV Dark Matter Physics with Cosmic Ray and Future Telescopes
Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences（暗物质与空间天文重点实验室，紫金山天文台，中国科学院）；School of Astronomy and Space Science, University of Science and Technology of China（天文与空间科学学院，中国科学技术大学）；National Centre for Nuclear Research（国家核研究中心）
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。
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）
