First measurement of the Hubble parameter from bright binary black hole GW190521

Creators: Mukherjee, Suvodip; Ghosh, Archisman; Graham, Matthew J.; Karathanasis, Christos; Kasliwal, Mansi M.; Magaña Hernandez, Ignacio; Nissanke, Samaya M.; Silvestri, Alessandra; Wandelt, Benjamin D.

Abstract

The Zwicky Transient Facility (ZTF) reported the event "ZTF19abanrhr" as a candidate electromagnetic (EM) counterpart at a redshift z=0.438 to the gravitational wave (GW) emission from the binary black hole merger GW190521. Assuming that ZTF19abanrhr is the bona fide EM counterpart to GW190521, and using the GW luminosity distance estimate from three different waveforms NRSur7dq4, SEOBNRv4PHM, and IMRPhenomPv3HM, we report a measurement of the Hubble constant H₀ = 50.4^(+28.1)_(−19.5) km/s/Mpc, 62.2^(+29.5)_(−19.7) km/s/Mpc, and 43.1^(+24.6)_(−11.4) km/s/Mpc (median along with 68% credible interval) respectively after marginalizing over matter density Ωm (or dark energy equation of state w0) assuming the flat LCDM (or wCDM) model. Combining our results with the binary neutron star event GW170817 with its redshift measurement alone, as well as with its inclination angle inferred from Very Large Baseline Interferometry (VLBI), we find H₀ = 67.6^(+4.3)_(−4.2) km/s/Mpc, Ω_m = 0.47^(+0.34)_(−0.27), and w₀ = −1.17^(+0.68)_(−0.57) (median along with 68% credible interval) providing the most stringent measurement on H0 and the first estimation on Ω_m and w₀ from bright standard siren. In the future, 1.3% measurement of H₀ = 68 km/s/Mpc and 28% measurement of w₀ = −1 is possible from about 200 GW190521-like sources.

Additional Information

We thank Simone Mastrogiovanni for carefully reviewing the manuscript and providing useful suggestions. SM acknowledges useful discussions with Will M. Farr and Rachel Gray. This analysis was carried out at the Horizon cluster hosted by IAP. We thank Stephane Rouberol for smoothly running the Horizon cluster. SM and SMN are supported by the research program Innovational Research Incentives Scheme (Vernieuwingsimpuls), which is financed by the Netherlands Organization for Scientific Research through the NWO VIDI Grant No. 2016/ENW/639.042.612. AG is grateful for funding from the D-ITP. This work was supported by the GROWTH project funded by the National Science Foundation under Grant No 1545949. This work was partially supported by the Spanish MINECO under the grants SEV-2016-0588 and PGC2018-101858-B-I00, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. IMH is supported by the NSF Graduate Research Fellowship Program under grant DGE-17247915. AS acknowledges support from the NWO and the Dutch Ministry of Education, Culture and Science (OCW) (through NWO VIDI Grant No. 2019/ENW/00678104 and from the D-ITP consortium). BDW and part of the computational work are supported by the Labex ILP (reference ANR-10-LABX-63) part of the Idex SUPER, received financial state aid managed by the Agence Nationale de la Recherche, as part of the programme Investissements d'avenir under the reference ANR-11-IDEX-0004-02. BDW acknowledges financial support from the ANR BIG4 project, under reference ANR-16-CE23-0002. The Center for Computational Astrophysics is supported by the Simons Foundation. In this analysis, following packages are used: Corner (Foreman-Mackey 2016), emcee: The MCMC Hammer (Foreman-Mackey et al. 2013), IPython (Pérez & Granger 2007), Matplotlib (Hunter 2007), NumPy (van der Walt et al. 2011), and SciPy (Jones et al. 01 ). AVAILABILITY OF DATA. The datasets were derived from sources in the public domain: https://dcc.ligo.org/LIGO-P2000158/public.

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