AI 中文总结
该研究通过贝叶斯模型比较在LVK观测的致密双星并合事件中搜索引力闪光，未找到相关证据，估计了闪光概率上限以约束微扰体性质，且对第四次观测运行能探测到闪光持乐观态度。
AI 中文摘要
激光干涉引力波天文台（LIGO）-处女座（Virgo）-神冈引力波探测器（KAGRA）合作对致密双星并合（CBC）的观测在最初三次观测运行中产生了90个事件。通过进行贝叶斯模型比较，我们在这些探测中最响亮的事件附近搜索所谓的“引力闪光”。引力闪光是由信号与时空微扰体相互作用引起的引力波尾，理论上表现为原始信号的回声。我们在信噪比至少为12的双黑洞或中等质量黑洞双星事件中未找到引力闪光的令人信服证据。我们还发现，使用不包含引力闪光的模板库进行标准匹配滤波CBC搜索可能不会错过包含引力闪光的信号。因此，我们估计了闪光概率上限作为其相对幅度的函数，并利用这些估计来约束宇宙中微扰体的性质。随着第四次观测运行灵敏度的提高，可探测事件的数量和信噪比将增加，我们仍然乐观地认为很快就能探测到闪光。
英文摘要
Observations of compact binary coalescences (CBCs) by the LIGO-Virgo-KAGRA collaboration resulted in 90 events in the first three observing runs. We search the data near the loudest of these detections for so-called "gravitational glints," by performing Bayesian model comparison. Gravitational glints are gravitational-wave tails caused by interactions between a signal and a spacetime perturber and are theorized to present as echoes of the primary signal. We do not find convincing evidence of gravitational glints in binary black hole or intermediate-mass black hole binary events with a signal-to-noise ratio (SNR) of at least 12. We also found that standard matched-filter CBC searches with template banks that do not contain gravitational glints would likely not have missed signals containing a gravitational glint. We therefore estimate upper limits on the probability of a glint as a function of its relative amplitude and use these estimates to constrain the properties of perturbers in the Universe. With increased sensitivity in the fourth observing run, which will increase the number and SNR of detectable events, we remain optimistic that glints will soon be detectable.
