Статья

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. AcerneseUniversità di Salerno, Fisciano, I-84084 Salerno, ItalyK. AckleyOzGrav, School of Physics & Astronomy, Monash University, Clayton, VIC 3800, AustraliaC. AdamsLIGO Livingston Observatory, Livingston, LA 70754, USAT. AdamsLaboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université Savoie Mont Blanc, CNRS/IN2P3, F-74941 Annecy, FranceP. AddessoUniversity of Sannio at Benevento, I-82100 Benevento, Italy and INFN, Sezione di Napoli, I-80100 Napoli, ItalyR. 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. AielloGran Sasso Science Institute (GSSI), I-67100 L'Aquila, ItalyA. AinInter-University Centre for Astronomy and Astrophysics, Pune 411007, IndiaP. AjithInternational Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Bengaluru 560089, IndiaB. AllenLeibniz Universität Hannover, D-30167 Hannover, GermanyA. 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 Avancés (LMA), CNRS/IN2P3, F-69622 Villeurbanne, FranceA. 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. AntierLAL, Univ. Paris-Sud, CNRS/IN2P3, Université Paris-Saclay, F-91898 Orsay, FranceS. 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. ArnaudEuropean Gravitational Observatory (EGO), I-56021 Cascina, Pisa, ItalyK. G. ArunChennai Mathematical Institute, Chennai 603103, IndiaS. AscenziINFN, Sezione 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. BaconAPC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, F-75205 Paris Cedex 13, FranceM. 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. BarsugliaAPC, AstroParticule et Cosmologie, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cité, F-75205 Paris Cedex 13, FranceD. BartaWigner RCP, RMKI, H-1121 Budapest, Konkoly Thege Miklós út 29-33, HungaryJ. BartlettI. BartosUniversity of Florida, Gainesville, FL 32611, 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. BazzanUniversità di Padova, Dipartimento di Fisica e Astronomia, 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. BejgerNicolaus Copernicus Astronomical Center, Polish Academy of Sciences, 00-716, Warsaw, PolandI. BelahceneLAL, Univ. Paris-Sud, CNRS/IN2P3, Université Paris-Saclay, F-91898 Orsay, FranceA. 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. BiscoveanuOzGrav, School of Physics & Astronomy, Monash University, Clayton, VIC 3800, AustraliaA. BishtLeibniz Universität Hannover, D-30167 Hannover, GermanyM. BitossiEuropean Gravitational Observatory (EGO), I-56021 Cascina, Pisa, ItalyC. BiwerSyracuse University, Syracuse, NY 13244, USA

2017en

ABI

Аннотация

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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Идентификаторы

DOI: 10.3847/2041-8213/aa920c

Цитирования и источники

Цитирований: 9Использованных источников: 0

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