利用强引力透镜双黑洞并合探测暗物质：近期前景
Probing Dark Matter with Strongly Lensed Binary Black Hole Mergers: Prospects in the Near Future
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- International Centre for Theoretical Sciences, Tata Institute of Fundamental Research（国际理论科学中心，塔塔基础研究所）
- Department of Physics, The Chinese University of Hong Kong（香港中文大学物理系）
- Department of Physics, University of California at Santa Barbara（加州大学圣塔芭芭拉分校物理系）
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中文总结 AI 辅助
本文利用升级后的LIGO-Virgo-KAGRA网络观测，研究用强引力透镜双黑洞并合约束温暗物质粒子质量的前景，O6可获与现有相当的约束，后续运行将大幅收紧，为暗物质探测提供新手段。
中文摘要 AI 辅助
经中间星系和星系团强引力透镜的引力波（GW）瞬变事件，预计占地基探测器可探测事件的一小部分（约0.1-0.5%）。强引力透镜双黑洞（BBH）并合会产生多个GW信号副本，这些信号到达探测器的时间不同。这些透镜事件的丰度和时间延迟分布对透镜群体的质量、密度剖面和红移分布敏感，进而与暗物质的本质相关。Jana等人（见https://doi.org/10.1093/mnras/stae1140，《 MNRAS》135卷，2025年，第11期，111402页）近期提出了一种方法，利用下一代GW探测器可探测的强引力透镜事件来约束温暗物质（WDM）粒子的质量。本研究中，我们利用升级后的LIGO-Virgo-KAGRA网络的即将到来的观测，研究约束WDM粒子质量的前景，这需要仔细建模探测器的选择效应。预计即将到来的第五次观测运行（O5）只会产生适度的约束，因为在早期阶段预计只有少数透镜对。到第六次观测运行（O6），我们预测WDM粒子质量的约束为$m_{\rm wdm}^{-1} \not\thicksim 0.1-0.2\text{keV}^{-1}$（即$m_{\rm wdm} \not\thicksim 5-10\text{keV}$），这与现有的最严格天体物理约束相当。O6之后的观测运行将把约束收紧约一个数量级。因此，强引力透镜GW提供了一种互补、有竞争力且独立的暗物质探测手段。
英文摘要
Gravitational-wave~(GW) transients, strongly lensed by intervening galaxies and clusters, are expected to constitute a small fraction ($\sim 0.1$-$0.5\%$) of the events detectable by ground-based detectors. A strongly lensed binary black hole (BBH) merger will produce multiple copies of the GW signal arriving at different times at the detector. The abundance and time-delay distribution of these lensed events are sensitive to the mass, density profile, and redshift distribution of the lens population, and in turn, to the underlying nature of dark matter. Jana et al. (Phys.Rev.Lett. 135 (2025) 11, 111402) recently proposed a method to constrain the masses of warm dark matter (WDM) particles making use of the strongly lensed events detectable by next-generation GW detectors. In this work, we investigate the prospects of constraining the mass of the WDM particle using upcoming observations of the upgraded LIGO-Virgo-KAGRA network. This requires a careful modeling of the detector selection effects. The upcoming fifth observing run (O5) is expected to yield only a modest bound, since only a few lensed pairs are expected at that early stage. By the sixth observing run (O6), we forecast a bound on the WDM particle mass, $m_{\rm wdm}^{-1} \lesssim 0.1$-$0.2\text{keV}^{-1}$ ($m_{\rm wdm} \gtrsim 5$-$10\text{keV}$), which is comparable to the tightest existing astrophysical constraints. Runs beyond O6 will tighten the constraint by roughly an order of magnitude. Strongly lensed GWs therefore offer a complementary, competitive, and independent probe of dark matter.
