AI 中文总结
本研究构建参考框架，量化爱因斯坦望远镜（ET）各频段灵敏度对不同引力波源科学目标的影响，为第三代引力波观测站设计提供仪器要求与科学目标的关联基准。
AI 中文摘要
本研究探讨第三代（3G）引力波（GW）观测站爱因斯坦望远镜（ET）的仪器要求与科学性能之间的关系。不同技术设计选择会产生不同的噪声预算，最终决定探测器的科学能力。为系统评估和比较其影响，我们定义了一套涵盖致密双星并合（CBC）探测与参数估计，以及随机引力波背景、孤立自旋中子星、核心坍缩超新星（CCSNe）等其他源的综合性能指标。我们构建了一个比较参考框架，将特定噪声贡献和频段的退化与科学能力的损失关联起来。我们考虑了一系列代表性技术参数，如涂层和悬挂温度、低频仪器的滤波腔长度、高频仪器的光束尺寸。我们评估特定频段的灵敏度变化如何影响不同科学目标，量化了30Hz以下的灵敏度对大质量和/或高红移源的可探测性、长时CBC信号重建，以及双中子星（BNSs）的早期预警和天空定位的影响；30-450Hz范围的灵敏度主导大部分CBC参数估计指标；450Hz以上的高频灵敏度主要影响BNS并合后研究和CCSNe可探测性，对探测率影响较小。即使考虑最严重的退化，ET的科学案例总体仍保持稳健。我们的结果提供了将科学目标与仪器要求关联的综合基准，这对3G观测站的最终设计和基础设施确定至关重要。
英文摘要
We investigate the relationship between instrumental requirements and the scientific performance of the Einstein Telescope (ET), a third-generation (3G) gravitational-wave (GW) observatory. Different technical design choices result in distinct noise budgets, ultimately shaping the detector's scientific capabilities. To systematically assess and compare their impact, we define a comprehensive set of performance metrics spanning compact binary coalescence (CBC) detection and parameter estimation, as well as other sources, including stochastic GW backgrounds, isolated spinning neutron stars, and core-collapse supernovae (CCSNe). We build a comparative reference framework that links degradations in specific noise contributions and frequency bands to losses in scientific capabilities. We consider a representative selection of technical parameters, such as coating and suspension temperatures, the filter cavity length in the low-frequency instrument, and the beam size in the high-frequency instrument. We evaluate how sensitivity variations across specific frequency bands affect different scientific objectives. We quantify how the sensitivity below 30 Hz impacts the detectability of massive and/or high-redshift sources and the reconstruction of long-duration CBC signals, affecting early warning and sky localization for binary neutron stars (BNSs). Sensitivity in the 30-450 Hz range governs most CBC parameter-estimation metrics, while high-frequency sensitivity above ~450 Hz predominantly impacts BNS post-merger studies and CCSN detectability, with modest effects on detection rates. Even with the most significant degradations considered, the ET science case remains robust overall. Our results provide a comprehensive benchmark linking scientific objectives to instrumental requirements, particularly important as the final design and infrastructure of 3G observatories are being defined.
Comments27 figures, 17 tables, 46+26 pages
