Observing Intermediate-mass Black Holes and the Upper Stellar-mass gap with LIGO and Virgo
Observing Intermediate-mass Black Holes and the Upper Stellar-mass gap with LIGO and Virgo
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DOI：
10.3847/1538-4357/ac3130
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发表时间：
2021-05
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影响因子：
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通讯作者：
A. Mehta;A. Buonanno;J. Gair;M. Miller;E. Farag;R. deBoer;M. Wiescher;F. Timmes
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作者：
A. Mehta;A. Buonanno;J. Gair;M. Miller;E. Farag;R. deBoer;M. Wiescher;F. Timmes
利用地面引力波探测器，我们探测了中等质量黑洞（IMBHs）的质量函数，其中我们还包括了在~ 60-130 M⊙的高质量间隙中的BHs。利用即将到来的LIGO和Virgo第四次观测（O4）的预测灵敏度，我们对总质量为50-500 M⊙、质量比为1.25、4和10、无量纲自旋高达0.95的准圆非处理、自旋IMBHBs （IMBHBs）进行了贝叶斯分析，并估计了源帧参数测量的精度。我们发现，在2σ时，在信噪比为20的情况下，IMBHBs的较重组分的质量可以被不确定性约束在10%-40%之间。针对12C(α, γ)16O反应速率及其不确定度的恒星质量缺口，我们利用MESA对大质量氦核恒星进行了演化，建立了质量缺口的下边缘和上边缘分别为：59−13+34 M⊙和139−14+30 M⊙，其中误差条给出了12C(α, γ)16O核反应速率的±3σ不确定度的质量范围。我们发现，高分辨率的反应速率表和精细的时间分辨率是确定黑洞质谱峰的必要条件。然后，我们研究了具有位于质量间隙中的组件的IMBHBs，并表明O4运行将能够鲁棒地识别大多数此类系统。最后，我们用最先进的对准自旋波形模型重新分析了GW190521，发现主质量位于质量间隙，可信度为90%。
Using ground-based gravitational-wave detectors, we probe the mass function of intermediate-mass black holes (IMBHs) wherein we also include BHs in the upper mass gap at ∼60–130 M ⊙. Employing the projected sensitivity of the upcoming LIGO and Virgo fourth observing run (O4), we perform Bayesian analysis on quasi-circular nonprecessing, spinning IMBH binaries (IMBHBs) with total masses 50–500 M ⊙, mass ratios 1.25, 4, and 10, and dimensionless spins up to 0.95, and estimate the precision with which the source-frame parameters can be measured. We find that, at 2σ, the mass of the heavier component of IMBHBs can be constrained with an uncertainty of ∼10%–40% at a signal-to-noise ratio of 20. Focusing on the stellar-mass gap with new tabulations of the 12C(α, γ)16O reaction rate and its uncertainties, we evolve massive helium core stars using MESA to establish the lower and upper edges of the mass gap as ≃ 59−13+34 M ⊙ and ≃ 139−14+30 M ⊙ respectively, where the error bars give the mass range that follows from the ±3σ uncertainty in the 12C(α, γ)16O nuclear reaction rate. We find that high resolution of the tabulated reaction rate and fine temporal resolution are necessary to resolve the peak of the BH mass spectrum. We then study IMBHBs with components lying in the mass gap and show that the O4 run will be able to robustly identify most such systems. Finally, we reanalyze GW190521 with a state-of-the-art aligned-spin waveform model, finding that the primary mass lies in the mass gap with 90% credibility.