GW190521: A binary black hole merger inside an active galactic nucleus?

GW190521: A binary black hole merger inside an active galactic nucleus?
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DOI:
10.1103/physrevd.108.123039
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发表时间:
2023-10
期刊:
影响因子:
5
通讯作者:
Sophia Morton;Stefano Rinaldi;Alejandro Torres-Orjuela;Andrea Derdzinski;M. P. Vaccaro;W. D. Pozzo
Sophia Morton;Stefano Rinaldi;Alejandro Torres-Orjuela;Andrea Derdzinski;M. P. Vaccaro;W. D. Pozzo
中科院分区:
物理与天体物理2区
文献类型:
--
作者:
Sophia Morton;Stefano Rinaldi;Alejandro Torres-Orjuela;Andrea Derdzinski;M. P. Vaccaro;W. D. Pozzo

文献摘要

相似文献

GW190521 是 LIGO-Virgo-KAGRA 合作可靠探测到的最大质量双黑洞合并,是对中等质量黑洞的首次引力波观测。大约 34 天后,ZTF19abanrhr 信号跟随耀斑 ZTF19abanrhr,由 Zwicky 瞬态设施在 78% 空间轮廓处在 AGN J124942.3+344929 中检测到,用于 GW190521 的天空定位。使用 GWTC-2.1 数据发布,我们发现 GW190521 和耀斑 ZTF19abanrhr 作为其电磁对应物之间的关联优于两个瞬变的随机重合,对数贝叶斯因子为 8.6,对应于相同先验赔率的 $\sim$ 5400 比 1 的赔率比,假设天体物理先验赔率为 1/13,则 $\sim$ 400 比 1。考虑到这种关联,多信使信号可以估计哈勃常数,在单独分析 GW190521 和 $79.2^{+17.6}_{-9.6}\mathrm{\ km \ s^{-1} \ 时发现 $H_0 = 102^{+27}_{-25}\mathrm{\ km \ s^{-1} \ Mpc^{-1}}$ Mpc^{-1}}$假设先验信息来自双中子星并合GW170817,两者与现有文献一致。
GW190521, the most massive binary black hole merger confidently detected by the LIGO-Virgo-KAGRA collaboration, is the first gravitational-wave observation of an intermediate-mass black hole. The signal was followed approximately 34 days later by flare ZTF19abanrhr, detected in AGN J124942.3+344929 by the Zwicky Transient Facility at the 78% spatial contour for GW190521s sky localization. Using the GWTC-2.1 data release, we find that the association between GW190521 and flare ZTF19abanrhr as its electromagnetic counterpart is preferred over a random coincidence of the two transients with a log Bayes factor of 8.6, corresponding to an odds ratio of $\sim$ 5400 to 1 for equal prior odds and $\sim$ 400 to 1 assuming an astrophysical prior odds of 1/13. Given the association, the multi-messenger signal allows for an estimation of the Hubble constant, finding $H_0 = 102^{+27}_{-25}\mathrm{\ km \ s^{-1} \ Mpc^{-1}}$ when solely analyzing GW190521 and $79.2^{+17.6}_{-9.6}\mathrm{\ km \ s^{-1} \ Mpc^{-1}}$ assuming prior information from the binary neutron star merger GW170817, both consistent with the existing literature.