Measuring the Hubble Constant with a sample of kilonovae. (arXiv:2008.07420v2 [astro-ph.HE] UPDATED)

Measuring the Hubble Constant with a sample of kilonovae. (arXiv:2008.07420v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Coughlin_M/0/1/0/all/0/1">Michael W. Coughlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antier_S/0/1/0/all/0/1">Sarah Antier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dietrich_T/0/1/0/all/0/1">Tim Dietrich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Foley_R/0/1/0/all/0/1">Ryan J. Foley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Heinzel_J/0/1/0/all/0/1">Jack Heinzel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bulla_M/0/1/0/all/0/1">Mattia Bulla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Christensen_N/0/1/0/all/0/1">Nelson Christensen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coulter_D/0/1/0/all/0/1">David A. Coulter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Issa_L/0/1/0/all/0/1">Lina Issa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khetan_N/0/1/0/all/0/1">Nandita Khetan</a>

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 $H_0 = 73.8^{+6.3}_{-5.8}$,$mathrm{km}$
$mathrm{s}^{-1}$ $mathrm{Mpc}^{-1}$ and $H_0 =
71.2^{+3.2}_{-3.1}$,$mathrm{km}$ $mathrm{s}^{-1}$ $mathrm{Mpc}^{-1}$ 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.

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 $H_0 = 73.8^{+6.3}_{-5.8}$,$mathrm{km}$
$mathrm{s}^{-1}$ $mathrm{Mpc}^{-1}$ and $H_0 =
71.2^{+3.2}_{-3.1}$,$mathrm{km}$ $mathrm{s}^{-1}$ $mathrm{Mpc}^{-1}$ 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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