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Gravitational Waves and Gamma-Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A

B. P. AbbottLIGO, California Institute of Technology, Pasadena, CA 91125, USAR. AbbottLIGO, California Institute of Technology, Pasadena, CA 91125, USAT. D. AbbottLouisiana State University, Baton Rouge, LA 70803, USAF. AcerneseINFN, Sezione di Napoli, Complesso Universitario di Monte S.Angelo, I-80126 Napoli, ItalyK. AckleyUniversity of Florida, Gainesville, FL 32611, USAC. AdamsLIGO Livingston Observatory, Livingston, LA 70754, USAT. AdamsInstitut National de Physique Nucléaire et de Physique des ParticulesP. AddessoIstituto Nazionale di Fisica Nucleare, Sezione di NapoliR. X. AdhikariLIGO, California Institute of Technology, Pasadena, CA 91125, USAV. B. AdyaMax Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, GermanyC. AffeldtMax Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, GermanyM. AfroughThe University of Mississippi, University, MS 38677, USAB. AgarwalNCSA, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USAM. AgathosUniversity of Cambridge, Cambridge CB2 1TN, UKK. AgatsumaNikhef, Science Park, 1098 XG Amsterdam, The NetherlandsN. AggarwalLIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USAO. D. AguiarInstituto Nacional de Pesquisas Espaciais, 12227-010 São José dos Campos, São Paulo, BrazilL. AielloINFN, Laboratori Nazionali del Gran Sasso, I-67100 Assergi, ItalyA. AinInter-University Centre for Astronomy and Astrophysics, Pune 411007, IndiaP. AjithInternational Centre for Theoretical SciencesB. AllenUniversity of Wisconsin-Milwaukee, Milwaukee, WI 53201, USAA. AlloccaINFN, Sezione di Pisa, I-56127 Pisa, ItalyM. Á. AloyDepartamento de Astronomía y Astrofísica, Universitat de València, E-46100 Burjassot, València, SpainP. A. AltinOzGrav, Australian National University, Canberra, ACT 0200, AustraliaA. AmatoLaboratoire des Matériaux AvancésA. AnanyevaLIGO, California Institute of Technology, Pasadena, CA 91125, USAS. B. AndersonLIGO, California Institute of Technology, Pasadena, CA 91125, USAW. G. AndersonUniversity of Wisconsin-Milwaukee, Milwaukee, WI 53201, USAS. V. AngelovaSUPA, University of the West of Scotland, Paisley PA1 2BE, UKS. AntierInstitut National de Physique Nucléaire et de Physique des ParticulesS. AppertLIGO, California Institute of Technology, Pasadena, CA 91125, USAK. AraiLIGO, California Institute of Technology, Pasadena, CA 91125, USAM. C. ArayaLIGO, California Institute of Technology, Pasadena, CA 91125, USAJ. S. AreedaCalifornia State University Fullerton, Fullerton, CA 92831, USAN. ArnaudLAL, Univ. Paris-Sud, CNRS/IN2P3, Université Paris-Saclay, F-91898 Orsay, FranceK. G. ArunChennai Mathematical Institute, Chennai 603103, IndiaS. AscenziUniversità di Roma Tor Vergata, I-00133 Roma, ItalyG. AshtonMax Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, GermanyM. AstUniversität Hamburg, D-22761 Hamburg, GermanyS. M. AstonLIGO Livingston Observatory, Livingston, LA 70754, USAP. AstoneINFN, Sezione di Roma, I-00185 Roma, ItalyD. V. AtallahCardiff University, Cardiff CF24 3AA, UKP. AufmuthLeibniz Universität Hannover, D-30167 Hannover, GermanyC. AulbertMax Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, GermanyK. AultONealEmbry-Riddle Aeronautical University, Prescott, AZ 86301, USAC. AustinLouisiana State University, Baton Rouge, LA 70803, USAA. Avila-AlvarezCalifornia State University Fullerton, Fullerton, CA 92831, USAS. BabakMax Planck Institute for Gravitational Physics (Albert Einstein Institute), D-14476 Potsdam-Golm, GermanyP. BaconUniversité Paris CitéM. K. M. BaderNikhef, Science Park, 1098 XG Amsterdam, The NetherlandsS. BaeKorea Institute of Science and Technology Information, Daejeon 34141, KoreaP. T. BakerWest Virginia University, Morgantown, WV 26506, USAF. BaldacciniINFN, Sezione di Perugia, I-06123 Perugia, ItalyG. BallardinEuropean Gravitational Observatory (EGO), I-56021 Cascina, Pisa, ItalyS. W. BallmerSyracuse University, Syracuse, NY 13244, USAS. BanagiriUniversity of Minnesota, Minneapolis, MN 55455, USAJ. C. BarayogaLIGO, California Institute of Technology, Pasadena, CA 91125, USAS. E. BarclaySUPA, University of Glasgow, Glasgow G12 8QQ, UKB. C. BarishLIGO, California Institute of Technology, Pasadena, CA 91125, USAD. BarkerK. BarkettCaltech CaRT, Pasadena, CA 91125, USAF. BaroneUniversità di Salerno, Fisciano, I-84084 Salerno, ItalyB. BarrSUPA, University of Glasgow, Glasgow G12 8QQ, UKL. BarsottiLIGO, Massachusetts Institute of Technology, Cambridge, MA 02139, USAM. BarsugliaSorbonne Paris CitéD. BartaWigner RCP, RMKI, H-1121 Budapest, Konkoly Thege Miklós út 29-33, HungaryJ. BartlettI. BartosColumbia University, New York, NY 10027, USAR. BassiriStanford University, Stanford, CA 94305, USAA. BastiINFN, Sezione di Pisa, I-56127 Pisa, ItalyJ. C. BatchM. BawajUniversità di Camerino, Dipartimento di Fisica, I-62032 Camerino, ItalyJ. C. BayleySUPA, University of Glasgow, Glasgow G12 8QQ, UKM. BazzanINFN, Sezione di Padova, I-35131 Padova, ItalyB. BécsyInstitute of Physics, Eötvös University, Pázmány P. s. 1/A, Budapest 1117, HungaryC. BeerMax Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, GermanyM. BejgerPolish Academy of SciencesI. BelahceneUniversité Paris-SaclayA. S. BellSUPA, University of Glasgow, Glasgow G12 8QQ, UKB. K. BergerLIGO, California Institute of Technology, Pasadena, CA 91125, USAG. BergmannMax Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, GermanyJ. J. BeroRochester Institute of Technology, Rochester, NY 14623, USAC. P. L. BerryUniversity of Birmingham, Birmingham B15 2TT, UKD. BersanettiINFN, Sezione di Genova, I-16146 Genova, ItalyA. BertoliniNikhef, Science Park, 1098 XG Amsterdam, The NetherlandsJ. BetzwieserLIGO Livingston Observatory, Livingston, LA 70754, USAS. BhagwatSyracuse University, Syracuse, NY 13244, USAR. BhandareRRCAT, Indore MP 452013, IndiaI. A. BilenkoFaculty of Physics, Lomonosov Moscow State University, Moscow 119991, RussiaG. BillingsleyLIGO, California Institute of Technology, Pasadena, CA 91125, USAC. R. BillmanUniversity of Florida, Gainesville, FL 32611, USAJ. BirchLIGO Livingston Observatory, Livingston, LA 70754, USAR. BirneySUPA, University of Strathclyde, Glasgow G1 1XQ, UKO. BirnholtzMax Planck Institute for Gravitational Physics (Albert Einstein Institute), D-30167 Hannover, GermanyS. BiscansLIGO, California Institute of Technology, Pasadena, CA 91125, USAS. BiscoveanuMonash UniversityA. BishtLeibniz Universität Hannover, D-30167 Hannover, GermanyM. BitossiINFN, Sezione di Pisa, I-56127 Pisa, ItalyC. BiwerSyracuse University, Syracuse, NY 13244, USA

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Abstract On 2017 August 17, the gravitational-wave event GW170817 was observed by the Advanced LIGO and Virgo detectors, and the gamma-ray burst (GRB) GRB 170817A was observed independently by the Fermi Gamma-ray Burst Monitor, and the Anti-Coincidence Shield for the Spectrometer for the International Gamma-Ray Astrophysics Laboratory . The probability of the near-simultaneous temporal and spatial observation of GRB 170817A and GW170817 occurring by chance is <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mn>5.0</mml:mn> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>8</mml:mn> </mml:mrow> </mml:msup> </mml:math> . We therefore confirm binary neutron star mergers as a progenitor of short GRBs. The association of GW170817 and GRB 170817A provides new insight into fundamental physics and the origin of short GRBs. We use the observed time delay of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo stretchy="false">(</mml:mo> <mml:mo>+</mml:mo> <mml:mn>1.74</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.05</mml:mn> <mml:mo stretchy="false">)</mml:mo> <mml:mspace width="0.25em"/> <mml:mi mathvariant="normal">s</mml:mi> </mml:math> between GRB 170817A and GW170817 to: (i) constrain the difference between the speed of gravity and the speed of light to be between <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>−</mml:mo> <mml:mn>3</mml:mn> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>15</mml:mn> </mml:mrow> </mml:msup> </mml:math> and <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>+</mml:mo> <mml:mn>7</mml:mn> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>16</mml:mn> </mml:mrow> </mml:msup> </mml:math> times the speed of light, (ii) place new bounds on the violation of Lorentz invariance, (iii) present a new test of the equivalence principle by constraining the Shapiro delay between gravitational and electromagnetic radiation. We also use the time delay to constrain the size and bulk Lorentz factor of the region emitting the gamma-rays. GRB 170817A is the closest short GRB with a known distance, but is between 2 and 6 orders of magnitude less energetic than other bursts with measured redshift. A new generation of gamma-ray detectors, and subthreshold searches in existing detectors, will be essential to detect similar short bursts at greater distances. Finally, we predict a joint detection rate for the Fermi Gamma-ray Burst Monitor and the Advanced LIGO and Virgo detectors of 0.1–1.4 per year during the 2018–2019 observing run and 0.3–1.7 per year at design sensitivity.

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DOI: 10.3847/2041-8213/aa920c

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