arXiv 2103.130152021-03-25astro-ph.GAgr-qc

用视差微透镜寻找引力波黑洞

Finding gravitational-wave black holes with parallax microlensing

Satoshi Toki, Masahiro Takada

备注：: 18 pages, 14 figures, 1 table

摘要：

LIGO-Virgo引力波（GW）观测揭示了新的黑洞（BH）群体，它们似乎具有扩展的质量谱，高达$70M_\odot$左右，比以前认为的质量范围（$\sim 8M_\odot$）重得多。在本文中，我们研究的能力，在银河系（MW）隆起区的恒星微透镜观测，以确定银河系质量尺度的黑洞，考虑到微透镜视差的特征参数$π_{\rm E}\propto M^{-1/2}$（$M$是透镜的质量），这是一个无量纲的量定义的比率的天文单位投影爱因斯坦半径。首先，假设BH遵循相同的空间和速度分布的恒星预测的标准MW模型，我们表明，微透镜事件与长的光变曲线的时间尺度，$t_{\rm E}\gtrsim 100~{\rm days}$，和小视差效应，$π_{\rm E}\sim 10^{-2}$，主要由BH透镜相比，恒星质量透镜。其次，使用马尔可夫链蒙特卡罗分析的模拟光变曲线，我们表明，BH透镜候选人是安全地确定在个人的基础上，如果视差效应被检测到或以及约束到一个百分比水平的精度在$π_{\rm E}$。我们还讨论了一个微透镜事件的一个中等质量的BH的$\sim 1000M_\odot$，如果它发生，可以识别出一个区别于恒星质量的BH。

英文摘要：

The LIGO-Virgo gravitational-wave (GW) observation unveiled the new population of black holes (BHs) that appears to have an extended mass spectrum up to around $70M_\odot$, much heavier than the previously-believed mass range ($\sim 8M_\odot$). In this paper, we study the capability of a microlensing observation of stars in the Milky Way (MW) bulge region to identify BHs of GW mass scales, taking into account the microlensing parallax characterized by the parameter $π_{\rm E}\propto M^{-1/2}$ ($M$ is the mass of a lens), which is a dimension-less quantity defined by the ratio of the astronomical unit to the projected Einstein radius. First, assuming that BHs follow the same spatial and velocity distributions of stars as predicted by the standard MW model, we show that microlensing events with long light curve timescales, $t_{\rm E}\gtrsim 100~{\rm days}$, and small parallax effects, $π_{\rm E}\sim 10^{-2}$, are dominated by BH lenses compared to stellar-mass lenses. Second, using a Markov chain Monte Carlo analysis of the simulated light curve, we show that BH lens candidates are securely identified on individual basis, if the parallax effect is detected or well constrained to the precision of a percent level in $π_{\rm E}$. We also discuss that a microlensing event of an intermediate-mass BH of $\sim 1000M_\odot$, if it occurs, can be identified in a distinguishable way from stellar-mass BHs.

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