Abbott, B. P. and Abbott, R. and Adams, C. and Adhikari, R. X. and Ananyeva, A. and Anderson, S. B. and Appert, S. and Arai, K. and Araya, M. C. and Aston, S. M. and Barayoga, J. C. and Barish, B. C. and Billingsley, G. and Blackburn, J. K. and Bork, R. and Brooks, A. F. and Brunett, S. and Cahillane, C. and Cepeda, C. B. and Callister, T. A. and Corban, P. and Couvares, P. and Coyne, D. C. and Cripe, J. and Drever, R. W. P. and Ehrens, P. and Eichholz, J. and Etzel, T. and Feicht, J. and Fries, E. M. and Frolov, V. V. and Fyffe, M. and Giaime, J. A. and Giardina, K. D. and Gossan, S. E. and Gushwa, K. E. and Gustafson, E. K. and Hall, E. D. and Hanson, J. and Heintze, M. C. and Heptonstall, A. W. and Huynh-Dinh, T. and Isi, M. and Kanner, J. B. and Katzman, W. and Kondrashov, V. and Korth, W. Z. and Kozak, D. B. and Lazzarini, A. and Maros, E. and Marx, J. N. and Massinger, T. J. and McCormick, S. and McIntyre, G. and McIver, J. and Meshkov, S. and Nelson, T. J. N. and Nolting, D. and Oram, Richard J. and O'Reilly, B. and Overmier, H. and Parker, W. and Pedraza, M. and Pele, A. and Quintero, E. A. and Reitze, D. H. and Robertson, N. A. and Rollins, J. G. and Romie, J. H. and Sachdev, S. and Sanchez, E. J. and Schmidt, P. and Sellers, D. and Singer, A. and Smith, B. and Smith, R. J. E. and Stuver, A. L. and Taylor, R. and Thomas, M. and Thorne, K. A. and Torrie, C. I. and Traylor, G. and Tso, R. and Urban, A. L. and Vajente, G. and Vass, S. and Venugopalan, G. and Wade, A. R. and Wallace, L. and Weinstein, A. J. and Williams, R. D. and Wipf, C. C. and Wu, G. and Yamamoto, H. and Zhang, L. and Zweizig, J. and Chatziioannou, K. (2017) GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2. Physical Review Letters, 118 (22). Art. No. 221101. ISSN 0031-9007. doi:10.1103/PhysRevLett.118.221101. https://resolver.caltech.edu/CaltechAUTHORS:20170601-101514708
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Abstract
We describe the observation of GW170104, a gravitational-wave signal produced by the coalescence of a pair of stellar-mass black holes. The signal was measured on January 4, 2017 at 10∶11:58.6 UTC by the twin advanced detectors of the Laser Interferometer Gravitational-Wave Observatory during their second observing run, with a network signal-to-noise ratio of 13 and a false alarm rate less than 1 in 70 000 years. The inferred component black hole masses are 31.2^(8.4) _(−6.0)M_⊙ and 19.4^(5.3)_( −5.9)M_⊙ (at the 90% credible level). The black hole spins are best constrained through measurement of the effective inspiral spin parameter, a mass-weighted combination of the spin components perpendicular to the orbital plane, χ_(eff) = −0.12^(0.21)_( −0.30). This result implies that spin configurations with both component spins positively aligned with the orbital angular momentum are disfavored. The source luminosity distance is 880^(450)_(−390) Mpc corresponding to a redshift of z = 0.18^(0.08)_( −0.07) . We constrain the magnitude of modifications to the gravitational-wave dispersion relation and perform null tests of general relativity. Assuming that gravitons are dispersed in vacuum like massive particles, we bound the graviton mass to m_g ≤ 7.7 × 10^(−23) eV/c^2. In all cases, we find that GW170104 is consistent with general relativity.
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| Additional Information: | Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI. Received May 9 2017. Published June 1 2017. The authors gratefully 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 GEO 600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully 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. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, Department of Science and Technology, India, Science & Engineering Research Board (SERB), India, Ministry of Human Resource Development, India, the Spanish Ministerio de Economía y Competitividad, the Vicepresidència i Conselleria d’Innovació, Recerca i Turisme and the Conselleria d’Educació i Universitat del Govern de les Illes Balears, the National Science Centre of Poland, the European Commission, 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 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, Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, and Innovation, International Center for Theoretical Physics South American Institute for Fundamental Research (ICTP-SAIFR), Russian Foundation for Basic Research, the Leverhulme Trust, the Research Corporation, Ministry of Science and Technology (MOST), Taiwan, and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS, and the State of Niedersachsen/Germany for provision of computational resources. This article has been assigned the document number LIGO-P170104. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| Issue or Number: | 22 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.1103/PhysRevLett.118.221101 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20170601-101514708 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20170601-101514708 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| ID Code: | 77888 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| Deposited By: | Joy Painter | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 01 Jun 2017 21:36 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 15 Nov 2021 17:34 |
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