Measuring the Hubble constant with a sample of kilonovae

Michael W. Coughlin (), Sarah Antier, Tim Dietrich, Ryan J. Foley, Jack Heinzel, Mattia Bulla, Nelson Christensen, David A. Coulter, Lina Issa and Nandita Khetan
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Michael W. Coughlin: University of Minnesota
Sarah Antier: APC, UMR 7164, 10 rue Alice Domon et Léonie Duquet
Tim Dietrich: Universität Potsdam
Ryan J. Foley: University of California
Jack Heinzel: Artemis, Université Côte d’Azur, Observatoire Côte d’Azur, CNRS, CS 34229
Mattia Bulla: Nordita, KTH Royal Institute of Technology and Stockholm University
Nelson Christensen: Artemis, Université Côte d’Azur, Observatoire Côte d’Azur, CNRS, CS 34229
David A. Coulter: University of California
Lina Issa: Nordita, KTH Royal Institute of Technology and Stockholm University
Nandita Khetan: Gran Sasso Science Institute (GSSI)

Nature Communications, 2020, vol. 11, issue 1, 1-9

Abstract: Abstract Kilonovae produced by the coalescence of compact binaries with at least one neutron star are promising standard sirens for an independent measurement of the Hubble constant (H0). Through their detection via follow-up of gravitational-wave (GW), short gamma-ray bursts (sGRBs) or optical surveys, a large sample of kilonovae (even without GW data) can be used for H0 contraints. Here, we show measurement of H0 using light curves associated with four sGRBs, assuming these are attributable to kilonovae, combined with GW170817. Including a systematic uncertainty on the models that is as large as the statistical ones, we find $${H}_{0}=73.{8}_{-5.8}^{+6.3}\ {\rm{km}}\ {{\rm{s}}}^{-1}\ {{\rm{Mpc}}}^{-1}$$ H 0 = 73 . 8 − 5.8 + 6.3 km s − 1 Mpc − 1 and $${H}_{0}=71.{2}_{-3.1}^{+3.2}\ {\rm{km}}\ {{\rm{s}}}^{-1}\ {{\rm{Mpc}}}^{-1}$$ H 0 = 71 . 2 − 3.1 + 3.2 km s − 1 Mpc − 1 for two different kilonova models that are consistent with the local and inverse-distance ladder measurements. For a given model, this measurement is about a factor of 2-3 more precise than the standard-siren measurement for GW170817 using only GWs.

Date: 2020
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DOI: 10.1038/s41467-020-17998-5

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