A gravitational-wave measurement of the Hubble constant following the second observing run of Advanced LIGO and Virgo. (arXiv:1908.06060v4 [astro-ph.CO] UPDATED)

A gravitational-wave measurement of the Hubble constant following the second observing run of Advanced LIGO and Virgo. (arXiv:1908.06060v4 [astro-ph.CO] UPDATED)
The <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_LIGO_Scientific/0/1/0/all/0/1">LIGO Scientific Collaboration</a>, the <a href="http://arxiv.org/find/astro-ph/1/au:+Collaboration_Virgo/0/1/0/all/0/1">Virgo Collaboration</a>: <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_B/0/1/0/all/0/1">B. P. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_R/0/1/0/all/0/1">R. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_T/0/1/0/all/0/1">T. D. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abraham_S/0/1/0/all/0/1">S. Abraham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Acernese_F/0/1/0/all/0/1">F. Acernese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ackley_K/0/1/0/all/0/1">K. Ackley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adams_C/0/1/0/all/0/1">C. Adams</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adhikari_R/0/1/0/all/0/1">R. X. Adhikari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Adya_V/0/1/0/all/0/1">V. B. Adya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Affeldt_C/0/1/0/all/0/1">C. Affeldt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agathos_M/0/1/0/all/0/1">M. Agathos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agatsuma_K/0/1/0/all/0/1">K. Agatsuma</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aggarwal_N/0/1/0/all/0/1">N. Aggarwal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguiar_O/0/1/0/all/0/1">O. D. Aguiar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aiello_L/0/1/0/all/0/1">L. Aiello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ain_A/0/1/0/all/0/1">A. Ain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ajith_P/0/1/0/all/0/1">P. Ajith</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_G/0/1/0/all/0/1">G. Allen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allocca_A/0/1/0/all/0/1">A. Allocca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aloy_M/0/1/0/all/0/1">M. A. Aloy</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Altin_P/0/1/0/all/0/1">P. A. Altin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amato_A/0/1/0/all/0/1">A. Amato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anand_S/0/1/0/all/0/1">S. Anand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ananyeva_A/0/1/0/all/0/1">A. Ananyeva</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_S/0/1/0/all/0/1">S. B. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anderson_W/0/1/0/all/0/1">W. G. Anderson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Angelova_S/0/1/0/all/0/1">S. V. Angelova</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antier_S/0/1/0/all/0/1">S. Antier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Appert_S/0/1/0/all/0/1">S. Appert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arai_K/0/1/0/all/0/1">K. Arai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Araya_M/0/1/0/all/0/1">M. C. Araya</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Areeda_J/0/1/0/all/0/1">J. S. Areeda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arene_M/0/1/0/all/0/1">M. Arène</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnaud_N/0/1/0/all/0/1">N. Arnaud</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aronson_S/0/1/0/all/0/1">S. M. Aronson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arun_K/0/1/0/all/0/1">K. G. Arun</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ascenzi_S/0/1/0/all/0/1">S. Ascenzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ashton_G/0/1/0/all/0/1">G. Ashton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aston_S/0/1/0/all/0/1">S. M. Aston</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Astone_P/0/1/0/all/0/1">P. Astone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aubin_F/0/1/0/all/0/1">F. Aubin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aufmuth_P/0/1/0/all/0/1">P. Aufmuth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+AultONeal_K/0/1/0/all/0/1">K. AultONeal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Austin_C/0/1/0/all/0/1">C. Austin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avendano_V/0/1/0/all/0/1">V. Avendano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_Alvarez_A/0/1/0/all/0/1">A. Avila-Alvarez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Babak_S/0/1/0/all/0/1">S. Babak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bacon_P/0/1/0/all/0/1">P. Bacon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Badaracco_F/0/1/0/all/0/1">F. Badaracco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bader_M/0/1/0/all/0/1">M. K. M. Bader</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bae_S/0/1/0/all/0/1">S. Bae</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Baird_J/0/1/0/all/0/1">J. 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This paper presents the gravitational-wave measurement of the Hubble constant
($H_0$) using the detections from the first and second observing runs of the
Advanced LIGO and Virgo detector network. The presence of the transient
electromagnetic counterpart of the binary neutron star GW170817 led to the
first standard-siren measurement of $H_0$. Here we additionally use binary
black hole detections in conjunction with galaxy catalogs and report a joint
measurement. Our updated measurement is $H_0 = 69^{+16}_{-8}$ km/s/Mpc (68.3%
of the highest density posterior interval with a flat-in-log prior) which is an
improvement by a factor of 1.04 (about 4%) over the GW170817-only value of
$69^{+17}_{-8}$ km/s/Mpc. A significant additional contribution currently comes
from GW170814, a loud and well-localized detection from a part of the sky
thoroughly covered by the Dark Energy Survey. With numerous detections
anticipated over the upcoming years, an exhaustive understanding of other
systematic effects are also going to become increasingly important. These
results establish the path to cosmology using gravitational-wave observations
with and without transient electromagnetic counterparts.

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