Compact radio emission indicates a structured jet was produced by a binary neutron star merger
G. GhirlandaDipartimento di Fisica G. Occhialini, Università di Milano-Bicocca, Piazza della Scienza 3, IT-20126 Milano, ItalyO. S. SalafiaDipartimento di Fisica G. Occhialini, Università di Milano-Bicocca, Piazza della Scienza 3, IT-20126 Milano, ItalyZ. ParagiJoint Institute for Very Long Baseline Interferometry (VLBI) European Research Infrastructure Consortium (ERIC), Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, NetherlandsM. GirolettiIstituto Nazionale di Astrofisica–Istituto di Radioastronomia, via Gobetti 101, I40129, Bologna, ItaliaJ. YangChalmers University of Technology, Onsala Space Observatory, SE-439 92, SwedenB. MarcoteJoint Institute for Very Long Baseline Interferometry (VLBI) European Research Infrastructure Consortium (ERIC), Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, NetherlandsJ. BlanchardJoint Institute for Very Long Baseline Interferometry (VLBI) European Research Infrastructure Consortium (ERIC), Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, NetherlandsI. AgudoInstituto de Astrofísica de Andalucía–Consejo Superior de Investigaciones Científicas (CSIC), Glorieta de la Astronomía s/n, E-18008, Granada, SpainT. AnShanghai Astronomical Observatory, Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, 200030 Shanghai, ChinaM. G. BernardiniLaboratoire Univers et Particules de Montpellier, Universitè de Montpellier, Centre National de la Recherche Scientifique/Institute National de Physique Nucleaire et Physique des Particules (CNRS/IN2P3), place Eugéne Bataillon, F–34085 Montpellier, FranceR. BeswickElectronic Multi-Element Radio Linked Interferometer Network/Very Long Baseline Interferometry (e-MERLIN/VLBI) National Facility, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester, UKM. BranchesiGran Sasso Science Institute, Viale F. Crispi 7, I-67100, L’Aquila, ItalyS. CampanaIstituto Nazionale di Astrofisica–Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate, ItalyC. CasadioMax Planck Institute fur Radioastronomie, Auf dem Huegel 69, Bonn D-53121, GermanyE. Chassande-MottinAstroParticule et Cosmologie (APC), Université Paris Diderot, CNRS/IN2P3, Commissariat à l’Énergie Atomique et aux Énergies Alternatives/ Institute for Research on the Fundamental Laws of the Universe (CEA/IRFU), Observatoire de Paris, Sorbonne Paris Cité, F-75205 Paris Cedex 13, FranceM. ColpiDipartimento di Fisica G. Occhialini, Università di Milano-Bicocca, Piazza della Scienza 3, IT-20126 Milano, ItalyS. CovinoIstituto Nazionale di Astrofisica–Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate, ItalyP. D’AvanzoIstituto Nazionale di Astrofisica–Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate, ItalyV. D’EliaSpace Science Data Center, Agenzia Spaziale Italiana (ASI), Via del Politecnico, 00133, Roma, ItalyS. FreyKonkoly Observatory, Magyar Tudományos Akadémia (MTA) Research Centre for Astronomy and Earth Sciences, Konkoly Thege Miklós út 15-17, H-1121 Budapest, HungaryM. GawronskiCentre for Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziadzka 5, 87-100 Torun, PolandG. GhiselliniIstituto Nazionale di Astrofisica–Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate, ItalyL. I. GurvitsDepartment of Astrodynamics and Space Missions, Delft University of Technology, Kluyverweg 1, 2629 HS Delft, NetherlandsP. G. JonkerDepartment of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University, Post Office Box 9010, 6500 GL Nijmegen, NetherlandsH. J. van LangeveldeJoint Institute for Very Long Baseline Interferometry (VLBI) European Research Infrastructure Consortium (ERIC), Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, NetherlandsA. MelandriIstituto Nazionale di Astrofisica–Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate, ItalyJ. MoldonElectronic Multi-Element Radio Linked Interferometer Network/Very Long Baseline Interferometry (e-MERLIN/VLBI) National Facility, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester, UKL. NavaIstituto Nazionale di Astrofisica–Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate, ItalyA. PeregoSezione di Milano Bicocca, Istituto Nazionale Fisica Nucleare (INFN), Piazza della Scienza 3, 20126 Milano, ItalyM. A. Perez-TorresDepartamento de Física Teórica, Facultad de Ciencias, Universidad de Zaragoza, E-50019, SpainC. ReynoldsCommonwealth Scientific and Industrial Research Organization (CSIRO) Astronomy and Space Science, PO Box 1130, Bentley WA 6102, AustraliaR. SalvaterraIstituto Nazionale di Astrofisica, Istituto di Astrofisica Spaziale e Fisica cosmica (IASF), via E. Bassini 15, 20133 Milano, ItalyG. TagliaferriIstituto Nazionale di Astrofisica–Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate, ItalyT. VenturiIstituto Nazionale di Astrofisica–Istituto di Radioastronomia, via Gobetti 101, I40129, Bologna, ItaliaS. D. VerganiGalaxies, Etoiles, Physique et Instrumentation (GEPI) Observatoire de Paris, CNRS UMR 8111, Meudon, FranceM. ZhangKey Laboratory for Radio Astronomy, Chinese Academy of Sciences, 2 West Beijing Road, Nanjing 210008, China
2019en
ABI
Аннотация
The binary neutron star merger event GW170817 was detected through both electromagnetic radiation and gravitational waves. Its afterglow emission may have been produced by either a narrow relativistic jet or an isotropic outflow. High-spatial-resolution measurements of the source size and displacement can discriminate between these scenarios. We present very-long-baseline interferometry observations, performed 207.4 days after the merger by using a global network of 32 radio telescopes. The apparent source size is constrained to be smaller than 2.5 milli-arc seconds at the 90% confidence level. This excludes the isotropic outflow scenario, which would have produced a larger apparent size, indicating that GW170817 produced a structured relativistic jet. Our rate calculations show that at least 10% of neutron star mergers produce such a jet.
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