4.6 Article

First Measurement of the Hubble Constant from a Dark Standard Siren using the Dark Energy Survey Galaxies and the LIGO/Virgo Binary-Black-hole Merger GW170814

Journal

ASTROPHYSICAL JOURNAL LETTERS
Volume 876, Issue 1, Pages -

Publisher

IOP Publishing Ltd
DOI: 10.3847/2041-8213/ab14f1

Keywords

catalogs; cosmology: observations; gravitational waves; surveys

Funding

  1. DOE (USA)
  2. NSF (USA)
  3. MEC/MICINN/MINECO (Spain)
  4. STFC (UK)
  5. HEFCE (UK)
  6. NCSA (UIUC)
  7. KICP (University of Chicago)
  8. CCAPP (Ohio State)
  9. MIFPA (Texas AM)
  10. CNPQ (Brazil)
  11. FAPERJ (Brazil)
  12. FINEP (Brazil)
  13. DFG (Germany)
  14. Argonne Lab
  15. UC Santa Cruz
  16. University of Cambridge
  17. CIEMAT-Madrid
  18. University of Chicago
  19. University College London
  20. DES-Brazil Consortium
  21. University of Edinburgh
  22. ETH Zurich
  23. Fermilab
  24. University of Illinois
  25. ICE (IEEC-CSIC)
  26. IFAE Barcelona
  27. Lawrence Berkeley Lab
  28. LMU Munchen
  29. University of Michigan
  30. NOAO
  31. University of Nottingham
  32. Ohio State University
  33. University of Pennsylvania
  34. University of Portsmouth
  35. SLAC National Lab
  36. Stanford University
  37. University of Sussex
  38. Texas AM University
  39. OzDES Membership Consortium
  40. NSF [AST-1138766, AST-1536171]
  41. MINECO [AYA2015-71825, ESP2015-88861, FPA2015-68048]
  42. Centro de Excelencia [SEV-2016-0588, SEV-2016-0597, MDM-2015-0509]
  43. ERC under the EU's 7thFramework Programme [ERC 240672, 291329, 306478]
  44. Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]
  45. U.S. Department of Energy, Office of Science, Office of High Energy Physics [DE-AC02-07CH11359]
  46. Science and Technology Facilities Council (STFC) of the United Kingdom
  47. Max-Planck-Society (MPS)
  48. State of Niedersachsen/Germany
  49. Australian Research Council
  50. Department of Science and Technology, India
  51. Spanish Agencia Estatal de Investigacion
  52. Vicepresidencia i Conselleria d'Innovacio Recerca i Turisme
  53. Conselleria d'Educacio i Universitat del Govern de les Illes Balears
  54. Conselleria d'Educacio Investigacio Cultura i Esport de la Generalitat Valenciana
  55. National Science Centre of Poland
  56. Swiss National Science Foundation (SNSF)
  57. Russian Foundation for Basic Research
  58. Russian Science Foundation
  59. European Commission
  60. European Regional Development Funds (ERDF)
  61. Royal Society
  62. Scottish Funding Council
  63. Scottish Universities Physics Alliance
  64. Hungarian Scientific Research Fund (OTKA)
  65. Lyon Institute of Origins (LIO)
  66. Paris Ile-de-France Region
  67. National Research, Development and Innovation Office Hungary (NKFIH)
  68. National Research Foundation of Korea
  69. Province of Ontario through the Ministry of Economic Development and Innovation
  70. Natural Science and Engineering Research Council Canada
  71. Canadian Institute for Advanced Research
  72. Brazilian Ministry of Science, Technology, Innovations, and Communications
  73. International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR)
  74. Research Grants Council of Hong Kong
  75. National Natural Science Foundation of China (NSFC)
  76. Leverhulme Trust
  77. Ministry of Science and Technology (MOST), Taiwan
  78. Kavli Foundation
  79. United States National Science Foundation (NSF)
  80. Netherlands Organisation for Scientific Research
  81. EGO consortium
  82. Council of Scientific and Industrial Research of India
  83. Science AMP
  84. Engineering Research Board (SERB), India
  85. Ministry of Human Resource Development, India
  86. National Research Council of Science & Technology (NST), Republic of Korea [2019187500] Funding Source: Korea Institute of Science & Technology Information (KISTI), National Science & Technology Information Service (NTIS)
  87. National Research Foundation of Korea [2018R1D1A1B07048599, 2016R1C1B2010064, 21A20151213022, 2016R1A5A1013277] Funding Source: Korea Institute of Science & Technology Information (KISTI), National Science & Technology Information Service (NTIS)
  88. EPSRC [2161515] Funding Source: UKRI
  89. STFC [1802888, 1938553, ST/N000633/1, ST/I006269/1, 1653089, 1654298, ST/L000652/1, ST/K000845/1, ST/N005422/1, 2142081, 1947165, ST/S000305/1, ST/H002006/1, ST/M005844/1, ST/N00003X/1, ST/M003574/1, 2039699, ST/J00166X/1, 1947199, ST/N000072/1, ST/K005014/1, Gravitational Waves, PPA/G/S/2002/00652, 1802894, 1945971, ST/V001396/1, ST/K005014/2, ST/N001087/1, ST/P000525/1] Funding Source: UKRI

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We present a multi-messenger measurement of the Hubble constant H-0 using the binary-black-hole merger GW170814 as a standard siren, combined with a photometric redshift catalog from the Dark Energy Survey (DES). The luminosity distance is obtained from the gravitational wave signal detected by the Laser Interferometer Gravitational-Wave Observatory (LIGO)/Virgo Collaboration (LVC) on 2017 August 14, and the redshift information is provided by the DES Year 3 data. Black hole mergers such as GW170814 are expected to lack bright electromagnetic emission to uniquely identify their host galaxies and build an object-by-object Hubble diagram. However, they are suitable for a statistical measurement, provided that a galaxy catalog of adequate depth and redshift completion is available. Here we present the first Hubble parameter measurement using a black hole merger. Our analysis results in H-0 = 75(-32)(+40) km s(-1) Mpc(-1) , which is consistent with both SN Ia and cosmic microwave background measurements of the Hubble constant. The quoted 68% credible region comprises 60% of the uniform prior range [20, 140] km s(-1) Mpc(-1) , and it depends on the assumed prior range. If we take a broader prior of [10, 220] km s(-1) Mpc(-1) , we find H-0 = 78(-24)(+96) km s(-1) Mpc(-1) (57% of the prior range). Although a weak constraint on the Hubble constant from a single event is expected using the dark siren method, a multifold increase in the LVC event rate is anticipated in the coming years and combinations of many sirens will lead to improved constraints on H-0.

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