AI 中文总结
研究利用微透镜化的引力波信号，通过贝叶斯参数估计量化广义相对论测试偏差，引入新统计量比较测试，发现微透镜会致波形畸变产生与广义相对论的错误偏差，凸显波动光学引力透镜是重要系统偏差及建模必要性。
AI 中文摘要
引力波对致密双星合并的观测能够在强场区域对广义相对论进行精确测试，但其可靠性依赖于精确的波形建模。未建模的物理效应会引发系统偏差，模拟出与广义相对论的偏差。本文利用质量在\(10 - 10^{5}M_\odot\)范围内的孤立点质量物体透镜化的类似GW150914的模拟信号，研究引力波微透镜对标准LIGO - Virgo - KAGRA广义相对论测试的影响。通过无透镜波形模板进行贝叶斯参数估计，量化参数化测试、修正色散关系测试、合并 - 旋降一致性测试（IMRCT）和元IMRCT框架中的偏差。引入基于广义相对论分位数的统一广义相对论偏差显著性统计量进行比较。发现微透镜引起的波形畸变会产生显著的与广义相对论的错误偏差，在一维测试中达到约\(4\sigma\)，二维一致性测试中达到约\(4.5\sigma\)。这些错误偏差主要出现在波动光学区域，长波长和几何光学区域的信号与广义相对论基本一致。还发现这些明显偏差的显著性与贝叶斯因子衡量的微透镜可探测性相关性不强。结果表明波动光学引力透镜是当前和未来广义相对论精确测试的重要天体物理系统偏差，强调了在下一代引力波分析中对传播效应建模的必要性。
英文摘要
Gravitational-wave (GW) observations of compact binary mergers enable precision tests of general relativity (GR) in the strong-field regime, but their reliability depends on accurate waveform modeling. Unmodeled physical effects can induce systematic biases that mimic deviations from GR. Here we study the impact of GW microlensing on standard LIGO-Virgo-KAGRA tests of GR using GW150914-like simulated signals lensed by isolated point-mass objects with masses in the range $10-10^{5}M_\odot$. We perform Bayesian parameter estimation with unlensed waveform templates and quantify biases in parameterized tests, modified dispersion relation tests, the inspiral-merger-ringdown consistency test (IMRCT) and the meta-IMRCT framework. To compare these tests with a common discriminator, we introduce a unified GR-deviation significance statistic based on the GR quantile, applicable to both one- and multi-dimensional deviation parameters. We find that microlensing-induced waveform distortions can produce significant false deviations from GR, reaching $\sim4σ$ in one-dimensional tests and $\sim4.5σ$ in two-dimensional consistency tests, despite the injected signals being fully GR-compatible. These false deviations arise mainly in the wave-optics regime, where diffraction induces frequency-dependent amplitude and phase modulations, while signals in the long-wavelength and geometric-optics regimes remain largely consistent with GR. We also find that the significance of these apparent deviations does not correlate strongly with microlensing detectability as measured by Bayes factors, showing that GR tests probe waveform projections not captured by global lensing diagnostics. Our results establish wave-optics gravitational lensing as an important astrophysical systematic for present and future precision tests of GR and highlight the need to model propagation effects in next-generation GW analyses.
