arXiv 2205.054092022-05-11astro-ph.GAastro-ph.CO

引力波的引力透镜：星系尺度透镜群中微透镜的概率

Gravitational Lensing of Gravitational Waves: Probability of Microlensing in Galaxy-Scale Lens Population

Ashish Kumar Meena, Anuj Mishra, Anupreeta More, Sukanta Bose, Jasjeet Singh Bagla

备注：: 12 pages, 9 figures; Comments welcome
DOI：: 10.1093/mnras/stac2721

摘要：

随着观测到的引力波信号数量的增加，探测星系强引力波已成为可能。透镜星系也包含微透镜（例如，恒星和黑洞），在LIGO频率范围内的强透镜GW信号中引入进一步的频率依赖调制。给定透镜系统中的多个透镜化信号具有不同的基础宏观放大率（$|μ|$），并且位于不同的微透镜密度（$Σ_\bullet$）中，导致不同水平的微透镜化失真。这项工作量化的分数强透镜系统的影响，使用现实的模拟观测微透镜。我们研究了50个四重成像系统（四边形），通过为每个透镜信号生成50个实现。然而，我们的结论是同样有效的双成像系统（双打）的透镜信号。这里研究的透镜信号有$|μ|\sim[0.5, 10]$和$Σ_\bullet\sim[10, 10^3]~{\rm M}_\odot/{\rm pc^2}$。我们发现，微透镜效应是更敏感的宏观放大率比底层的微透镜密度，即使后者超过$10^3~{\rm M}_\odot/{\rm pc^2}$。对于总质量范围内的几乎所有双黑洞源[10 M $_\odot$，200 M $_\odot$ ]，透镜和非透镜GW信号之间的失配很少超过$1\%$。这意味着微透镜预计不会影响这种信号的检测或参数估计，并且当宏观放大率为${\leq}10$时，不会对识别不同的透镜对应物提出任何进一步的挑战。在LIGO-Virgo探测器网络的第四次观测运行中，四个探测器对中的${\sim}50\%$和两个探测器对中的${\sim}90\%$预计将满足这样的放大率切割。

英文摘要：

With the increase in the number of observed gravitational wave (GW) signals, detecting strongly lensed GWs by galaxies has become a real possibility. Lens galaxies also contain microlenses (e.g., stars and black holes), introducing further frequency-dependent modulations in the strongly lensed GW signal within the LIGO frequency range. The multiple lensed signals in a given lens system have different underlying macro-magnifications ($|μ|$) and are located in varied microlens densities ($Σ_\bullet$), leading to different levels of microlensing distortions. This work quantifies the fraction of strong lens systems affected by microlensing using realistic mock observations. We study 50 quadruply imaged systems (quads) by generating 50 realizations for each lensed signal. However, our conclusions are equally valid for lensed signals in doubly imaged systems (doubles). The lensed signals studied here have $|μ|\sim[0.5, 10]$ and $Σ_\bullet\sim[10, 10^3]~{\rm M}_\odot/{\rm pc^2}$. We find that the microlensing effects are more sensitive to the macro-magnification than the underlying microlens density, even if the latter exceeds $10^3~{\rm M}_\odot/{\rm pc^2}$. The mismatch between lensed and unlensed GW signals rarely exceeds $1\%$ for nearly all binary black hole sources in the total mass range [10 M$_\odot$, 200 M$_\odot$]. This implies that microlensing is not expected to affect the detection or the parameter estimation of such signals and does not pose any further challenges in identifying the different lensed counterparts when macro-magnification is ${\leq}10$. Such a magnification cut is expected to be satisfied by ${\sim}50\%$ of the detectable pairs in quads and ${\sim}90\%$ of the doubles in the fourth observing run of the LIGO-Virgo detector network.

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英文摘要：

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