使用边界细化的引力波干扰瞬态（glitch）自动识别与扣除
Automated identification and subtraction of gravitational-wave glitches using boundary refinement
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中文总结 AI 辅助
该研究针对引力波干扰瞬态无法自动识别边界的问题，提出三种边界识别方法与三种扣除技术，经实验验证其能高效、准确恢复注入信号的高比例信噪比，为引力波数据处理提供了关键技术。
中文摘要 AI 辅助
引力波应变数据中的瞬态噪声伪影（即干扰瞬态，glitch）会提高天体物理搜索的虚警率，且在与信号重叠时会降低参数估计的精度。此前没有任何方法能识别干扰瞬态的时间边界：现有的检测与分类工具仅标记和标注干扰瞬态，却无法确定其范围，这使得扣除操作必须在带填充的窗口上运行，既耗时又会擦除干扰瞬态之外的信号。我们提出了三种边界识别方法，分别是AMPS（基于振幅的多干扰瞬态脉冲分段器）、FLARE（基于拟合度的定位与细化提取器）和CRISP（通过频谱图功率的连通区域识别），并搭配三种扣除技术：自适应样条拟合、小波收缩及其组合，实验使用了来自GravitySpy数据库的5个干扰瞬态，涵盖高级LIGO的前三次观测运行。AMPS通过稳健振幅阈值确定边界，FLARE通过分段样条拟合的最佳拟合度确定边界，CRISP通过频谱图功率确定边界。在四个宽带干扰瞬态上注入啁啾信号后，组合技术可恢复注入信噪比的95%至97%，而单独使用小波收缩仅能恢复约64%。CRISP在不同干扰瞬态间的边界宽度最均匀；AMPS和CRISP均能在几分之一秒内识别边界，比FLARE快两到三个数量级。对于与GW170817重叠的干扰瞬态，在默认边界下会存在低频残留，这是为避免去除信号功率而刻意做出的权衡。散射光干扰瞬态尚未经过测试，是未来工作的主要方向。
英文摘要
Transient noise artifacts, or glitches, in gravitational wave strain data elevate the false alarm rate of astrophysical searches and degrade parameter estimation when overlapping a signal. No method previously identified a glitch's time boundary: existing detection and classification tools flag and label glitches without resolving their extent, forcing subtraction to run over padded windows that cost time and erase signal beyond the glitch itself. We present three boundary identification methods, AMPS (Amplitude-based Multi-glitch Pulse Segmenter), FLARE (Fitness-based Localization And Refinement Extractor), and CRISP (connected-region identification via spectrogram power), paired with three subtraction techniques, adaptive spline fitting, wavelet shrinkage, and their combination, across five glitches from the GravitySpy database spanning Advanced LIGO's first three observing runs. AMPS sets a boundary from a robust amplitude threshold, FLARE from the best fitness of a segmented spline fit, and CRISP from spectrogram power. Injecting a chirp signal on four broadband glitches, the combined technique recovers 95 to 97 percent of the injected signal-to-noise ratio, against roughly 64 percent for wavelet shrinkage alone. CRISP gives the most uniform boundary width across glitches; AMPS and CRISP both identify a boundary in a fraction of a second, two to three orders of magnitude faster than FLARE. For the glitch overlapping GW170817, a low-frequency residual persists under the default boundary, a deliberate tradeoff against removing signal power. Scattered light glitches remain untested and are the primary direction for future work.
发表机构
- Rensselaer Polytechnic Institute（伦斯勒理工学院）
- Department of Physics and Astronomy, The University of Texas Rio Grande Valley（德克萨斯大学里奥格兰德河谷分校物理与天文系）
机构由 AI 辅助整理，请以论文原文为准。
