Measuring the Hubble Constant with a sample of kilonovae

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 ($H_0$). 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 $H_0$ contraints. Here, we show measurement of $H_0$ 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 $H_0=73.8_{-5.8}^{+6.3}$\,$\mathrm{km}$ ${\mathrm{s}}^{-1}$ ${\mathrm{Mpc}}^{-1}$ and $H_0=71.2_{-3.1}^{+3.2}$\,$\mathrm{km}$ ${\mathrm{s}}^{-1}$ ${\mathrm{Mpc}}^{-1}$ 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.

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