On the properties of the massive binary black hole merger GW170729
On the properties of the massive binary black hole merger GW170729
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DOI：
10.1103/physrevd.100.104015
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发表时间：
2019-03
影响因子：
5
通讯作者：
K. Chatziioannou;R. Cotesta;S. Ghonge;J. Lange;K. Ng;J. C. Bustillo;J. Clark;C. Haster;Sebastian Khan;Michael Puerrer;V. Raymond;S. Vitale;Nousha Afshari;S. Babak;K. Barkett;J. Blackman;A. Bohé;M. Boyle;A. Buonanno;M. Campanelli;Gregorio Carullo;T. Chu;E. Flynn;H. Fong;Alyssa Garcia;M. Giesler;M. Haney;M. Hannam;I. Harry;J. Healy;D. Hemberger;I. Hinder;K. Jani;Bhavesh Khamersa;Lawrence E. Kidder;Prayush Kumar;P. Laguna;C. Lousto;G. Lovelace;T. Littenberg;L. London;M. Millhouse;L. Nuttall;F. Ohme;R. O’Shaughnessy;S. Ossokine;F. Pannarale;P. Schmidt;H. Pfeiffer;M. Scheel;L. Shao;D. Shoemaker;B. Szilágyi;A. Taracchini;S. Teukolsky;Y. Zlochower
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文献类型：
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作者：
K. Chatziioannou;R. Cotesta;S. Ghonge;J. Lange;K. Ng;J. C. Bustillo;J. Clark;C. Haster;Sebastian Khan;Michael Puerrer;V. Raymond;S. Vitale;Nousha Afshari;S. Babak;K. Barkett;J. Blackman;A. Bohé;M. Boyle;A. Buonanno;M. Campanelli;Gregorio Carullo;T. Chu;E. Flynn;H. Fong;Alyssa Garcia;M. Giesler;M. Haney;M. Hannam;I. Harry;J. Healy;D. Hemberger;I. Hinder;K. Jani;Bhavesh Khamersa;Lawrence E. Kidder;Prayush Kumar;P. Laguna;C. Lousto;G. Lovelace;T. Littenberg;L. London;M. Millhouse;L. Nuttall;F. Ohme;R. O’Shaughnessy;S. Ossokine;F. Pannarale;P. Schmidt;H. Pfeiffer;M. Scheel;L. Shao;D. Shoemaker;B. Szilágyi;A. Taracchini;S. Teukolsky;Y. Zlochower
我们对GW 170729的性质进行了详细的研究，GW 170729是迄今为止确认的最大质量和最远源的引力波。我们采用了广泛的一组波形模型，包括新的改进模型，将高阶波形模式的效果，这是特别重要的大规模系统。我们没有发现自旋进动的迹象，但在模型中包含高阶模式的结果在90%的可信水平上的质量比$（0.3-0.8）$的改进估计。我们更新的测量排除了该水平上的相等质量。我们还发现，高阶模式的模型导致的数据是更一致的一个较小的有效自旋，与有效自旋大于零的概率从99\%$减少到94\%$。有效自旋参数的90%可信区间现在为$（-0.01-0.50）$。此外，恢复的信噪比增加了$\sim0.3$单位相比，没有高阶模式的分析。我们研究了常见的自旋先验对自旋和质量测量的影响，并观察到自旋的微小变化，而质量不受影响。我们认为，我们的结论是强大的对系统误差的波形模型。我们还比较了上述基于波形的分析，其采用紧凑的二进制波形模型，以更灵活的基于小波和线性调频波的分析。我们发现两者之间的一致性，重叠的$\sim 0.9$，典型的是从模拟类似于GW 170729的信号，确认数据是很好地描述了现有的波形模型。最后，我们研究了GW 170729的主要成分是过去两个黑洞合并的残余物的可能性，并发现这种情况下是无法区分的标准形成的情况。
We present a detailed investigation into the properties of GW170729, the gravitational wave with the most massive and distant source confirmed to date. We employ an extensive set of waveform models, including new improved models that incorporate the effect of higher-order waveform modes which are particularly important for massive systems. We find no indication of spin-precession, but the inclusion of higher-order modes in the models results in an improved estimate for the mass ratio of $(0.3-0.8)$ at the 90\% credible level. Our updated measurement excludes equal masses at that level. We also find that models with higher-order modes lead to the data being more consistent with a smaller effective spin, with the probability that the effective spin is greater than zero being reduced from $99\%$ to $94\%$. The 90\% credible interval for the effective spin parameter is now $(-0.01-0.50)$. Additionally, the recovered signal-to-noise ratio increases by $\sim0.3$ units compared to analyses without higher-order modes. We study the effect of common spin priors on the derived spin and mass measurements, and observe small shifts in the spins, while the masses remain unaffected. We argue that our conclusions are robust against systematic errors in the waveform models. We also compare the above waveform-based analysis which employs compact-binary waveform models to a more flexible wavelet- and chirplet-based analysis. We find consistency between the two, with overlaps of $\sim 0.9$, typical of what is expected from simulations of signals similar to GW170729, confirming that the data are well-described by the existing waveform models. Finally, we study the possibility that the primary component of GW170729 was the remnant of a past merger of two black holes and find this scenario to be indistinguishable from the standard formation scenario.