A Measurement of the Hubble Constant using Gravitational Waves from the Binary Merger GW190814

Abstract

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 ${\text{H}}_0=70_{-18.0}^{+35.0}$km s${}^{-1}$ Mpc${}^{-1}$ (maximum {\it a posteriori} and 68.3\% highest density posterior interval) for a galaxy $B$-band luminosity threshold of $L_B\ge 0.001L_B^{\ast }$ with a correction for catalog incompleteness. Repeating the calculation for GW190814, we obtain ${\text{H}}_0=67_{-26.0}^{+41.0}$ km s${}^{-1}$ Mpc${}^{-1}$ and ${\text{H}}_0=71_{-30.0}^{+34.0}$ km s${}^{-1}$ Mpc${}^{-1}$ for $L_B\ge 0.001L_B^{\ast }$ and $L_B\ge 0.626L_B^{\ast }$, respectively. Combining the posteriors for both events yields ${\text{H}}_0=70_{-18.0}^{+29.0}$ 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 ${\text{H}}_0=69_{-14.0}^{+29.0}$ km s${}^{-1}$ Mpc${}^{-1}$.

(Received: 04/28/2020, Accepted: 09/06/2020)

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