Gravitational-wave physics with Cosmic Explorer: limits to low-frequency sensitivity
Evan D. Hall, Kevin Kuns, Joshua R. Smith, Yuntao Bai, Christopher Wipf, Sebastien Biscans, Rana X Adhikari, Koji Arai, Stefan Ballmer, Lisa Barsotti, Yanbei Ch… 展开作者
Evan D. Hall, Kevin Kuns, Joshua R. Smith, Yuntao Bai, Christopher Wipf, Sebastien Biscans, Rana X Adhikari, Koji Arai, Stefan Ballmer, Lisa Barsotti, Yanbei Chen, Matthew Evans, Peter Fritschel, Jan Harms, Brittany Kamai, Jameson Graef Rollins, David Shoemaker, Bram Slagmolen, Rainer Weiss, Hiro Yamamoto
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24 pages, 19 figures; expanded discussion of residual gas and quantum noises, and updated scattered light estimates
Cosmic Explorer (CE) is a next-generation ground-based gravitational-wave observatory concept, envisioned to begin operation in the 2030s, and expected to be capable of observing binary neutron star and black hole mergers back to the time of the first stars. Cosmic Explorer's sensitive band will extend below 10 Hz, where the design is predominantly limited by geophysical, thermal, and quantum noises. In this work, thermal, seismic, gravity-gradient, quantum, residual gas, scattered-light, and servo-control noises are analyzed in order to motivate facility and vacuum system design requirements, potential test mass suspensions, Newtonian noise reduction strategies, improved inertial sensors, and cryogenic control requirements. Our analysis shows that with improved technologies, Cosmic Explorer can deliver a strain sensitivity better than $10^{-23}/\mathrm{Hz}^{1/2}$ down to 5 Hz. Our work refines and extends previous analysis of the Cosmic Explorer concept and outlines the key research areas needed to make this observatory a reality.
Overlap reduction functions for a polarized stochastic gravitational-wave background in the Einstein Telescope-Cosmic Explorer and the LISA-Taiji networks
本文将基于球谐展开的重叠减少函数计算方法推广到第三代地基 Einstein Telescope-Cosmic Explorer 网络及 LISA-Taiji 空间联合任务，以分析极化随机引力波背景。
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）
Comments on the 2001 run of the EXPLORER/NAUTILUS gravitational wave experiment
最近发表的关于2001年EXPLORER和NAUTILUS引力波探测器之间的巧合的分析（Astone et al. 2002）引起了一些批评（Finn 2003）。我们不同意这些反对意见，即使我们同意不能用我们的数据提出索赔。我们发表的这篇论文报告了前所未有的高质量数据，并为符合搜索设定了一个新的程序，我们和其他小组可以再次重复该程序，以搜索可能信号的特征。关于报告的重合过剩，我们注意到，它注定不会长期保持一个有趣的观察：它将很快被干涉仪和以预期灵敏度运行的棒所证实或否认。
Exploring the sky localization and early warning capabilities of third generation gravitational wave detectors in three-detector network configurations
这项工作描述了第三代引力波探测器网络的天空定位和预警性能，这些探测器网络由在北美、欧洲和澳大利亚的站点中具有爱因斯坦望远镜或宇宙探测器配置的探测器的不同组合组成。使用Fisher矩阵方法，其中包括地球自转的影响，我们估计的天空定位不确定性的$1.4\text{M}\odot$ - $1.4\text{M}\odot$二进制中子星合并的距离$40\text{Mpc}$，$200\text{Mpc}$，$400\text{Mpc}$，$800\text{Mpc}$，$1600\text{Mpc}$，和一个假设的天体物理人口的红移为2，以表征其性能的二进制中子星观测。我们发现，在$200\text{Mpc}$和一个网络组成的爱因斯坦望远镜，宇宙探测器和一个额外的爱因斯坦望远镜在澳大利亚（2 ET 1CE），最好的本地化90%的信号的90%可信区域的大小的上限是$0.25\text{deg}^2$的中子星合并。对于模拟的天体物理分布，这个上限是$91.79\text{deg}^2$。如果将澳大利亚的类爱因斯坦望远镜探测器替换为类宇宙探测器（1 ET 2CE），对于$200\text{Mpc}$情况，上限为$0.18\text{deg}^2$，而对于天体物理分布，上限为$56.77\text{deg}^2$。我们注意到，1 ET 2CE网络可以比2 ET 1CE网络多检测7.2%的模拟天体物…
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）
Next-generation global gravitational-wave detector network: Impact of detector orientation on compact binary coalescence and stochastic gravitational-wave background searches
