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arXiv 2201.11088astro-ph.GA
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TNG50-3模拟的大质量黑洞双星：I.聚结和LISA检测率

Massive Black Hole Binaries from the TNG50-3 Simulation: I. Coalescence and LISA Detection Rates

Kunyang Li, Tamara Bogdanović, David R. Ballantyne, Matteo Bonetti

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Accepted to ApJ, 20 pages, 10 figures
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摘要：

我们评估了大质量黑洞（MBH）双星的宇宙学合并和探测率的引力波天文台激光干涉仪空间天线（LISA）的目标。我们的计算开始与人口的引力未绑定的MBH对，从TNG 50 -3宇宙学模拟，并遵循其轨道演化从kpc尺度一直到合并使用半解析模型在我们以前的工作。我们发现，大多数MBH对合并在哈勃时间内的动力学摩擦是最重要的机制，决定他们的合并率。我们的模型预测MBH聚结率< 0.45/年，LISA检测率< 0.34/年。大多数激光干涉仪的探测应该来自于红移为1.6 < z < 2.4的富气星系中10^6 - 10^6.8太阳质量的星系，并且具有特征性的信噪比SNR ~ 100。然而，我们发现一个显着减少的合并和检测率，以及平均信噪比，如果考虑到吸积MBHs的辐射反馈的影响。在这种情况下，MBH聚结率降低了78%（至< 0.1/年），LISA检测率降低了94%（至0.02/年），而平均SNR为~ 10。我们强调，我们的模型提供了LISA检测率的下限，与文献中的其他作品一致，从宇宙学模拟中绘制他们的MBH对。

英文摘要：

We evaluate the cosmological coalescence and detection rates for massive black hole (MBH) binaries targeted by the gravitational wave observatory Laser Interferometer Space Antenna (LISA). Our calculation starts with a population of gravitationally unbound MBH pairs, drawn from the TNG50-3 cosmological simulation, and follows their orbital evolution from kpc scales all the way to coalescence using a semi-analytic model developed in our previous work. We find that for a majority of MBH pairs that coalesce within a Hubble time dynamical friction is the most important mechanism that determines their coalescence rate. Our model predicts a MBH coalescence rate < 0.45/ yr and a LISA detection rate < 0.34/ yr. Most LISA detections should originate from 10^6 - 10^6.8 solar masses MBHs in gas-rich galaxies at redshifts 1.6 < z < 2.4, and have a characteristic signal to noise ratio SNR ~ 100. We however find a dramatic reduction in the coalescence and detection rates, as well as the average SNR, if the effects of radiative feedback from accreting MBHs are taken into account. In this case, the MBH coalescence rate is reduced by 78% (to < 0.1/ yr), and the LISA detection rate is reduced by 94% (to 0.02/ yr), whereas the average SNR is ~ 10. We emphasize that our model provides a lower limit on the LISA detection rate, consistent with other works in the literature that draw their MBH pairs from cosmological simulations.

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