发表机构
Sapienza Università di Roma; INFN, Sezione di Roma; Scuola Normale Superiore; INFN, Sezione di Pisa; Università degli Studi di Milano-Bicocca; INFN, Sezione di Milano-Bicocca; INFN, Sezione di Cagliari; Università degli Studi di Sassari; Istituto Nazionale di Geofisica e Vulcanologia, Sezione di Pisa; Istituto Nazionale di Geofisica e Vulcanologia, Sezione di Bologna; Deutsches Zentrum für Astrophysik (DZA)（罗马第一大学; 罗马国家核物理研究所; 比萨高等师范学院; 比萨国家核物理研究所; 米兰比可卡大学; 米兰比可卡国家核物理研究所; 卡利亚里国家核物理研究所; 萨萨里大学; 比萨国家地球物理与火山学研究所; 博洛尼亚国家地球物理与火山学研究所; 德国天体物理学中心）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究分析台站依赖噪声对爱因斯坦望远镜低频科学性能的影响，对比不同构型，发现提升低频灵敏度可增强其科学表现，台站选择与噪声抑制对发挥其10Hz以下频段潜力至关重要。
AI 中文摘要
本研究探讨台站依赖的牛顿噪声配置如何影响第三代引力波探测器爱因斯坦望远镜（Einstein Telescope, ET）的科学性能。我们对比基线三角形构型与2L探测器构型，二者臂长分别为10km和15km，对应三种基于默兹-莱茵-欧雷吉奥地区、劳西茨及撒丁岛测量数据构建的台站依赖噪声场景。所采用的灵敏度差异主要集中在10Hz以下，因此对依赖轻天体早期旋进的科学案例，或特征频率处于低频段的大质量系统的科学案例影响最大。我们针对ET的四项科学案例量化这些影响：（1）中等质量黑洞双星的探测与参数估计；（2）基于早期旋进的广义相对论后牛顿检验；（3）大质量残余体的黑洞振铃光谱学；（4）双中子星并合的早期预警与天区定位能力。通过贝叶斯参数估计，我们发现提升低频灵敏度可显著增强ET在所有四项案例中的科学性能。在本文考虑的构型中，2L网络（其两个L形干涉仪中至少一个达到撒丁岛台站假设的噪声水平）通常比三角形构型提供更好的性能；反之，10Hz以下灵敏度的严重劣化会大幅降低，在某些情况下还会抵消将臂长从10km增至15km所预期的科学增益。这些结果凸显了台站选择与低频噪声抑制，以及网络构型，对于充分发挥ET在10Hz以下这一尚未充分探索的频段科学潜力的重要性。
英文摘要
We investigate how site-dependent Newtonian noise configurations affect the scientific performance of the Einstein Telescope (ET), a third-generation gravitational-wave observatory. We compare the baseline triangular and 2L detector geometries, with arm lengths of 10km and 15km, respectively, under three site-dependent noise scenarios constructed from measurements in the Euregio Meuse-Rhine region, Lausitz, and Sardinia. The differences among the adopted sensitivities are concentrated mainly below 10Hz and thus have the greatest impact on science cases that rely on the early inspiral of light objects, or on massive systems whose characteristic frequencies lie in the low-frequency band. We quantify these effects for four ET science cases: (1) detection and parameter estimation of intermediate-mass black-hole binaries; (2) post-Newtonian tests of General Relativity based on the early inspiral; (3) black-hole ringdown spectroscopy with massive remnants; and (4) early-warning and sky-localization capabilities for binary neutron-star mergers. Using Bayesian parameter estimation, we find that improved low-frequency sensitivity can significantly enhance ET's scientific performance across all four cases. Within the configurations considered here, a 2L network in which at least one of the two L-shaped interferometers attains a noise level comparable to that assumed for the Sardinian site generally provides better performance than the triangular configurations. Conversely, strong degradation of the sensitivity below 10Hz can substantially reduce, and in some regimes offset, the scientific gains expected from increasing the arm length from 10km to 15km. These results highlight the importance of site selection and low-frequency noise mitigation, alongside network geometry, for fully realizing ET's scientific potential in the largely unexplored frequency band below 10Hz.
