本文对Bernard F. 1986年，Shutz仅使用引力波从GW 190814中推断出哈勃常数（$\text{H}_0$），GW 190814是激光干涉仪引力波天文台（LIGO）和室女座干涉仪探测到的第一个高概率中子星-黑洞（NS-BH）合并候选者。我们应用这种方法的基线测试的双星（BNS）合并GW 170817和发现$\text{H}_0 = 70^{+35.0}_{-18.0}$ km s $^{-1}$ Mpc $^{-1}$（最大{ \it后验}和68.3%的最高密度后验间隔）的星系$B$带光度阈值$L_B \geq 0.001 L_B^*$与目录不完整的校正。重复GW 190814的计算，我们分别得到$L_B \geq 0.001 L_B^*$和$L_B \geq 0.626 L_B^*$的$\text{H}_0 = 67^{+41.0}_{-26.0}$ km s $^{-1}$ Mpc $^{-1}$和$\text{H}_0 = 71^{+34.0}_{-30.0}$ km s $^{-1}$ Mpc $^{-1}$。结合后验的两个事件产生$\text{H}_0 = 70^{+29.0}_{-18.0}$ km s $^{-1}$ Mpc $^{-1}$，证明了改进的约束时，使用多个引力波事件。我们还证实了采用这种方法的其他作品的结果，表明增加$L_B$阈值增强了后验结构，并将分布的峰值略微移动到更高的$\text{H}_0$值。我们分别使用低自旋PhenomPNRT（Abbott等人，2019 a）和GW 170817和GW 190814的新可用组合（SEOBNRv 4PHM + IMRPhenomPv 3 HM; Abbott等人，2020）后验样本重复联合推断，实现了$\text{H}_0 = 69^{+29.0}_{-14.0}$ km s PDMATHAMO Mpc PDMATHAMO的更严格约束。
英文摘要：
We present a test of the statistical method introduced by Bernard F. Shutz in 1986 using only gravitational waves to infer the Hubble constant ($\text{H}_0$) from GW190814, the first high-probability neutron-star--black-hole (NS-BH) merger candidate detected by the Laser Interferometer Gravitational-wave Observatory (LIGO) and the Virgo interferometer. We apply a baseline test of this method to the binary neutron star (BNS) merger GW170817 and find $\text{H}_0 = 70^{+35.0}_{-18.0}$km s$^{-1}$ Mpc$^{-1}$ (maximum {\it a posteriori} and 68.3\% highest density posterior interval) for a galaxy $B$-band luminosity threshold of $L_B \geq 0.001 L_B^*$ with a correction for catalog incompleteness. Repeating the calculation for GW190814, we obtain $\text{H}_0 = 67^{+41.0}_{-26.0}$ km s$^{-1}$ Mpc$^{-1}$ and $\text{H}_0 = 71^{+34.0}_{-30.0}$ km s$^{-1}$ Mpc$^{-1}$ for $L_B \geq 0.001 L_B^*$ and $L_B \geq 0.626 L_B^*$, respectively. Combining the posteriors for both events yields $\text{H}_0 = 70^{+29.0}_{-18.0}$ km s$^{-1}$ Mpc$^{-1}$, demonstrating the improvement on constraints when using multiple gravitational-wave events. We also confirm the results of other works that adopt this method, showing that increasing the $L_B$ threshold enhances the posterior structure and slightly shifts the distribution's peak to higher $\text{H}_0$ values. We repeat the joint inference using the low-spin PhenomPNRT (Abbott et al. 2019a) and the newly available combined (SEOBNRv4PHM + IMRPhenomPv3HM; Abbott et al. 2020) posterior samples for GW170817 and GW190814, respectively, achieving a tighter constraint of $\text{H}_0 = 69^{+29.0}_{-14.0}$ km s$^{-1}$ Mpc$^{-1}$.
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