Abstract
On 17 August 2017, the Advanced LIGO1 and Virgo2 detectors observed the gravitational-wave event GW170817—a strong signal from the merger of a binary neutron-star system3. Less than two seconds after the merger, a γ-ray burst (GRB 170817A) was detected within a region of the sky consistent with the LIGO–Virgo-derived location of the gravitational-wave source4,5,6. This sky region was subsequently observed by optical astronomy facilities7, resulting in the identification8,9,10,11,12,13 of an optical transient signal within about ten arcseconds of the galaxy NGC 4993. This detection of GW170817 in both gravitational waves and electromagnetic waves represents the first ‘multi-messenger’ astronomical observation. Such observations enable GW170817 to be used as a ‘standard siren’14,15,16,17,18 (meaning that the absolute distance to the source can be determined directly from the gravitational-wave measurements) to measure the Hubble constant. This quantity represents the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Here we report a measurement of the Hubble constant that combines the distance to the source inferred purely from the gravitational-wave signal with the recession velocity inferred from measurements of the redshift using the electromagnetic data. In contrast to previous measurements, ours does not require the use of a cosmic ‘distance ladder’19: the gravitational-wave analysis can be used to estimate the luminosity distance out to cosmological scales directly, without the use of intermediate astronomical distance measurements. We determine the Hubble constant to be about 70 kilometres per second per megaparsec. This value is consistent with existing measurements20,21, while being completely independent of them. Additional standard siren measurements from future gravitational-wave sources will enable the Hubble constant to be constrained to high precision.
This is a preview of subscription content, access via your institution
Access options
Access Nature and 54 other Nature Portfolio journals
Get Nature+, our best-value online-access subscription
$29.99 / 30 days
cancel any time
Subscribe to this journal
Receive 51 print issues and online access
$199.00 per year
only $3.90 per issue
Rent or buy this article
Prices vary by article type
from$1.95
to$39.95
Prices may be subject to local taxes which are calculated during checkout



References
The LIGO Scientific Collaboration. Advanced LIGO. Class. Quantum Gravity 32, 074001 (2015)
Acernese, F. et al. Advanced Virgo: a second-generation interferometric gravitational wave detector. Class. Quantum Gravity 32, 024001 (2015)
Abbott, B. P. et al. GW170817: observation of gravitational waves from a binary neutron star inspiral. Phys. Rev. Lett. 119, 161101 (2017)
Abbott, B. P. et al. Gravitational waves and gamma-rays from a binary neutron star merger: GW170817 and GRB 170817A. Astrophys. J. 848, https://doi.org/10.3847/2041-8213/aa920c (2017)
Goldstein, A. et al. An ordinary short gamma-ray burst with extraordinary implications: Fermi-GBM detection of GRB 170817A. Astrophys. J. 848, https://doi.org/10.3847/2041-8213/aa8f41 (2017)
Savchenko, V. et al. INTEGRAL detection of the first prompt gamma-ray signal coincident with the gravitational event GW170817. Astrophys. J. 848, https://doi.org/10.3847/2041-8213/aa8f94 (2017)
Abbott, B. P. et al. Multi-messenger observations of a binary neutron star merger. Astrophys. J. 848, https://doi.org/10.3847/2041-8213/aa91c9 (2017)
Coulter, D. A. et al. Swope Supernova Survey 2017a (SSS17a), the optical counterpart to a gravitational wave source. Science http://doi.org/10.1126/science.aap9811 (2017)
Soares-Santos, M. et al. The electromagnetic counterpart of the binary neutron star merger LIGO/VIRGO GW170817. I. Discovery of the optical counterpart using the dark energy camera. Astrophys. J. 848, https://doi.org/10.3847/2041-8213/aa9059 (2017)
Valenti, S. et al. The discovery of the electromagnetic counterpart of GW170817: kilonova AT 2017gfo/DLT17ck. Astrophys. J. 848, https://doi.org/10.3847/2041-8213/aa8edf (2017)
Arcavi, I. et al. Optical emission from a kilonova following a gravitational-wave-detected neutron-star merger. Nature http://doi.org/10.1038/nature24291 (2017)
Tanvir, N. et al. The emergence of a lanthanide-rich kilonova following the merger of two neutron stars. Astrophys. J. 848, https://doi.org/10.3847/2041-8213/aa90b6 (2017)
Lipunov, V. et al. MASTER optical detection of the first LIGO/Virgo NSs merging GW170817/ G298048. Astrophys. J. (in the press)
Schutz, B. F. Determining the Hubble constant from gravitational wave observations. Nature 323, 310–311 (1986)
Holz, D. E. & Hughes, S. A. Using gravitational-wave standard sirens. Astrophys. J. 629, 15–22 (2005)
Dalal, N., Holz, D. E., Hughes, S. A. & Jain, B. Short GRB and binary black hole standard sirens as a probe of dark energy. Phys. Rev. D 74, 063006 (2006)
Nissanke, S., Holz, D. E., Hughes, S. A., Dalal, N. & Sievers, J. L. Exploring short gamma-ray bursts as gravitational-wave standard sirens. Astrophys. J. 725, 496–514 (2010)
Nissanke, S. et al. Determining the Hubble constant from gravitational wave observations of merging compact binaries. Preprint at https://arxiv.org/abs/1307.2638 (2013)
Freedman, W. L. et al. Final results from the Hubble Space Telescope key project to measure the Hubble constant. Astrophys. J. 553, 47–72 (2001)
Planck Collaboration. Planck 2015 results. XIII. Cosmological parameters. Astron. Astrophys. 594, A13 (2016)
Riess, A. G. et al. A 2.4% determination of the local value of the Hubble constant. Astrophys. J. 826, 56 (2016)
Del Pozzo, W. Inference of the cosmological parameters from gravitational waves: application to second generation interferometers. Phys. Rev. D 86, 043011 (2012)
Abbott, B. P. et al. Binary black hole mergers in the first Advanced LIGO observing run. Phys. Rev. X 6, 041015 (2016)
Messenger, C. & Veitch, J. Avoiding selection bias in gravitational wave astronomy. New J. Phys. 15, 053027 (2013)
Sakai, S. et al. The Hubble Space Telescope key project on the extragalactic distance scale. XXIV. The calibration of Tully-Fisher relations and the value of the Hubble constant. Astrophys. J. 529, 698–722 (2000)
Hinshaw, G. et al. Five-year Wilkinson microwave anisotropy probe observations: data processing, sky maps, and basic results. Astrophys. J. Suppl. Ser. 180, 225–245 (2009)
Crook, A. C. et al. Groups of galaxies in the Two Micron All Sky Redshift Survey. Astrophys. J. 655, 790–813 (2007); erratum 685, 1320–1323 (2008)
Springob, C. M. et al. The 6dF Galaxy Survey: peculiar velocity field and cosmography. Mon. Not. R. Astron. Soc. 445, 2677–2697 (2014)
Carrick, J., Turnbull, S. J., Lavaux, G. & Hudson, M. J. Cosmological parameters from the comparison of peculiar velocities with predictions from the 2M++ density field. Mon. Not. R. Astron. Soc. 450, 317–332 (2015)
Aubourg, É. et al. Cosmological implications of baryon acoustic oscillation measurements. Phys. Rev. D 92, 123516 (2015)
Bonvin, V. et al. H0LiCOW – V. New COSMOGRAIL time delays of HE 0435−1223: H0 to 3.8 per cent precision from strong lensing in a flat ΛCDM model. Mon. Not. R. Astron. Soc. 465, 4914–4930 (2017)
Henning, J. W. et al. Measurements of the temperature and E-mode polarization of the CMB from 500 square degrees of SPTpol data. Preprint at https://arxiv.org/abs/1707.09353 (2017)
Huang, J.-S., Cowie, L. L. & Luppino, G. A. Morphological classification of the local I- and K-band galaxy sample. Astrophys. J. 496, 31–38 (1998)
Bloom, J. S., Kulkarni, S. R. & Djorgovski, S. G. The observed offset distribution of gamma-ray bursts from their host galaxies: a robust clue to the nature of the progenitors. Astron. J. 123, 1111–1148 (2002)
Skrutskie, M. F. et al. The Two Micron All Sky Survey (2MASS). Astron. J. 131, 1163–1183 (2006)
Jones, D. H. et al. The 6dF Galaxy Survey: final redshift release (DR3) and southern large-scale structures. Mon. Not. R. Astron. Soc. 399, 683–698 (2009)
Huchra, J. P. et al. The 2MASS Redshift Survey—description and data release. Astrophys. J. Supp. Ser. 199, 26 (2012)
Veitch, J. et al. Parameter estimation for compact binaries with ground-based gravitational-wave observations using the LALInference software library. Phys. Rev. D 91, 042003 (2015)
Hannam, M. et al. Simple model of complete precessing black-hole-binary gravitational waveforms. Phys. Rev. Lett. 113, 151101 (2014)
Cornish, N. J. & Littenberg, T. B. Bayeswave: Bayesian inference for gravitational wave bursts and instrument glitches. Class. Quantum Gravity 32, 135012 (2015)
Buonanno, A. & Damour, T. Effective one-body approach to general relativistic two-body dynamics. Phys. Rev. D 59, 084006 (1999)
Blanchet, L. Gravitational radiation from post-Newtonian sources and inspiralling compact binaries. Living Rev. Relativ. 17, 2 (2014)
Hinderer, T. & Flanagan, É. É. Two-timescale analysis of extreme mass ratio inspirals in Kerr spacetime: orbital motion. Phys. Rev. D 78, 064028 (2008)
Vines, J., Flanagan, É. É. & Hinderer, T. Post-1-Newtonian tidal effects in the gravitational waveform from binary inspirals. Phys. Rev. D 83, 084051 (2011)
Loredo, T. J. Accounting for source uncertainties in analyses of astronomical survey data. AIP Conf. Proc. 735, 195–206 (2004)
Mandel, I., Farr, W. M. & Gair, J. Extracting Distribution Parameters From Multiple Uncertain Observations With Selection Biases. Report No. P1600187-v1, https://dcc.ligo.org/LIGO-P1600187/public (LIGO, 2016)
Metzger, B. D. & Berger, E. What is the most promising electromagnetic counterpart of a neutron star binary merger? Astrophys. J. 746, 48 (2012)
Abbott, B. P. et al. Supplement: “The rate of binary black hole mergers inferred from Advanced LIGO observations surrounding GW150914” (2016, ApJL, 833, L1). Astrophys. J. Suppl. Ser. 227, 14 (2016)
Dalya, G., Frei, Z., Galgoczi, G., Raffai, P. & de Souza, R. S. GLADE catalog (Dalya+, 2016). VizieR Online Data Catalog http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=VII/275 (2016)
Strauss, M. A. & Willick, J. A. The density and peculiar velocity fields of nearby galaxies. Phys. Rep. 261, 271–431 (1995)
Acknowledgements
We acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. We acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. We acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science and Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación, the Vicepresidència i Conselleria d’Innovació, Recerca i Turisme and the Conselleria d’Educació i Universitat del Govern de les Illes Balears, the Conselleria d’Educació, Investigació, Cultura i Esport de la Generalitat Valenciana, the National Science Centre of Poland, the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National Research, Development and Innovation Office Hungary (NKFI), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, the Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, Innovations, and Communications, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. We acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and the State of Niedersachsen/Germany for provision of computational resources. This paper has been assigned the document number LIGO-P1700296. We thank the University of Copenhagen, DARK Cosmology Centre, and the Niels Bohr International Academy for hosting D.A.C., R.J.F., A.M.B., E. Ramirez-Ruiz and M.R.S. during the discovery of GW170817/SSS17a. R.J.F., A.M.B., E. Ramirez-Ruiz and D.E.H. were participating in the Kavli Summer Program in Astrophysics, ‘Astrophysics with gravitational wave detections’. This program was supported by the the Kavli Foundation, Danish National Research Foundation, the Niels Bohr International Academy, and the DARK Cosmology Centre. The UCSC group is supported in part by NSF grant AST–1518052, the Gordon & Betty Moore Foundation, the Heising-Simons Foundation, generous donations from many individuals through a UCSC Giving Day grant, and from fellowships from the Alfred P. Sloan Foundation (R.J.F.), the David and Lucile Packard Foundation (R.J.F. and E. Ramirez-Ruiz) and the Niels Bohr Professorship from the DNRF (E. Ramirez-Ruiz). A.M.B. acknowledges support from a UCMEXUS-CONACYT Doctoral Fellowship. Support for this work was provided by NASA through Hubble Fellowship grants HST–HF–51348.001 and HST–HF–51373.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5–26555. The Berger Time-Domain Group at Harvard is supported in part by the NSF through grants AST-1411763 and AST-1714498, and by NASA through grants NNX15AE50G and NNX16AC22G. Funding for the DES Projects has been provided by the DOE and NSF (USA), MEC/MICINN/MINECO (Spain), STFC (UK), HEFCE (UK). NCSA (UIUC), KICP (U. Chicago), CCAPP (Ohio State), MIFPA (Texas A&M), CNPQ, FAPERJ, FINEP (Brazil), DFG (Germany) and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne Lab, UC Santa Cruz, University of Cambridge, CIEMAT-Madrid, University of Chicago, University College London, DES-Brazil Consortium, University of Edinburgh, ETH Zürich, Fermilab, University of Illinois, ICE (IEEC-CSIC), IFAE Barcelona, Lawrence Berkeley Lab, LMU München and the associated Excellence Cluster Universe, University of Michigan, NOAO, University of Nottingham, Ohio State University, University of Pennsylvania, University of Portsmouth, SLAC National Lab, Stanford University, University of Sussex, Texas A&M University and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES Data Management System is supported by the NSF under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015-71825, ESP2015-88861, FPA2015-68048, and Centro de Excelencia SEV-2012-0234, SEV-2016-0597 and MDM-2015-0509. Research leading to these results has received funding from the ERC under the European Union’s Seventh Framework Programme including grants ERC 240672, 291329 and 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. This manuscript has been authored by Fermi Research Alliance, LLC under contract number DE-AC02-07CH11359 with the US Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. D.J.S. acknowledges support for the DLT40 programme from NSF grant AST-1517649. Support for I. Arcavi was provided by NASA through the Einstein Fellowship Program, grant PF6-170148. G. Hosseinzadeh, D.A.H. and C. McCully are supported by NSF grant AST-1313484. D. Poznanski acknowledges support by Israel Science Foundation grant 541/17. VINROUGE is an European Southern Observatory Large Survey (id: 0198.D-2010). MASTER acknowledges the Lomonosov MSU Development Programme and the Russian Federation Ministry of Education and Science. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.
Author information
Authors and Affiliations
Consortia
Contributions
All authors contributed to the work presented in this paper.
Ethics declarations
Competing interests
The author declare no competing financial interests.
Additional information
Reviewer Information Nature thanks N. Suntzeff and the other anonymous reviewer(s) for their contribution to the peer review of this work.
Publisher's note: Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.
Extended data figures and tables
Extended Data Figure 1 Graphical model illustrating the statistical relationships between the data and parameters.
Open circles indicate parameters that require a prior; filled circles describe measured data, which are conditioned on in the analysis. Here we assume that we have measurements of the gravitational-wave data xGW, a recessional velocity (that is, redshift) vr, and the mean peculiar velocity in the neighborhood of NGC 4993 〈vp〉. Arrows flowing into a node indicate that the conditional probability density for the node depends on the source parameters; for example, the conditional distribution for the observed gravitational-wave data p(xGW | d, cosι) depends on the distance and inclination of the source (and additional parameters, here marginalized out).
Extended Data Figure 2 Using different assumptions compared to our canonical analysis.
The posterior distribution on H0 discussed in the main text is shown in black, the alternative flat prior on z (discussed in Methods) gives the distribution shown in blue, and the increased uncertainty (250 km s−1) applied to our peculiar velocity measurement (also discussed in Methods) is shown in pink. Minimal 68.3% (1σ) credible intervals are shown by dashed lines.
Rights and permissions
About this article
Cite this article
The LIGO Scientific Collaboration and The Virgo Collaboration., The 1M2H Collaboration., The Dark Energy Camera GW-EM Collaboration and the DES Collaboration. et al. A gravitational-wave standard siren measurement of the Hubble constant. Nature 551, 85–88 (2017). https://doi.org/10.1038/nature24471
Received:
Accepted:
Published:
Issue Date:
DOI: https://doi.org/10.1038/nature24471
This article is cited by
-
Spherical symmetry in the kilonova AT2017gfo/GW170817
Nature (2023)
-
Cosmology with fast radio bursts in the era of SKA
Science China Physics, Mechanics & Astronomy (2023)
-
Primordial black hole archaeology with gravitational waves from cosmic strings
Journal of High Energy Physics (2023)
-
Primordial gravity waves in a rainbow background
General Relativity and Gravitation (2023)
-
Neutrino transport in general relativistic neutron star merger simulations
Living Reviews in Computational Astrophysics (2023)
Comments
By submitting a comment you agree to abide by our Terms and Community Guidelines. If you find something abusive or that does not comply with our terms or guidelines please flag it as inappropriate.