| Compact radio emission indicates a structured jet was produced by a binary neutron star merger | |
Ghirlanda, G.1,2,3; Salafia, O. S.1,2,3; Paragi, Z.4; Giroletti, M.5; Yang J(杨军)6,7 ; Marcote, B.4; Blanchard, J.4; Agudo, I.8; An, T.9; Bernardini, M. G.10,29; Beswick, R.11; Branchesi, M.12,13; Campana, S.1; Casadio, C.14; Chassande-Mottin, E.15; Colpi, M.2,3; Covino, S.1; D'Avanzo, P.1; D'Elia, V.16; Frey, S.17; Gawronski, M.18; Ghisellini, G.1; Gurvits, L. I.4,19; Jonker, P. G.20,21; van Langevelde, H. J.4,22; Melandri, A.1; Moldon, J.11; Nava, L.1; Perego, A.3,30; Perez-Torres, M. A.8,23; Reynolds, C.24; Salvaterra, R.25; Tagliaferri, G.1; Venturi, T.5; Vergani, S. D.26; Zhang, M.27,28
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| 发表期刊 | SCIENCE
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| 2019-03-01 | |
| 卷号 | 363期号:6430页码:968-+ |
| DOI | 10.1126/science.aau8815 |
| 产权排序 | 第7完成单位 |
| 收录类别 | SCI |
| 摘要 | 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. |
| 资助项目 | National Institute of Astrophysics[1.05.01.88.06] ; Italian Ministry for University and Research (MIUR)[1.05.06.13] ; ASI[I/004/11/3] ; European Commission Horizon 2020 Research and Innovation Programme[730562] ; Spanish Ministerio de Economa y Competitividad (MINECO) of ICCUB (Unidad de Excelencia Mara de Maeztu)[AYA201676012-C3-1-P] ; Spanish Ministerio de Economa y Competitividad (MINECO) of ICCUB (Unidad de Excelencia "Mara de Maeztu")[FPA2015-69210-C6-2-R] ; Spanish Ministerio de Economa y Competitividad (MINECO) of ICCUB (Unidad de Excelencia "Mara de Maeztu")[MDM-2014-0369] ; Spanish MINECO[AYA2012-38491-C02-02] ; Spanish MINECO[AYA2015-63939-C2-1-P] ; National Key R&D Programme of China[2018YFA0404603] ; European Union's Horizon 2020 research and innovation program[653477] ; Hungarian National Research, Development and Innovation Office[OTKA NN110333] ; Australian Government |
| 项目资助者 | National Institute of Astrophysics[1.05.01.88.06] ; Italian Ministry for University and Research (MIUR)[1.05.06.13] ; ASI[I/004/11/3] ; European Commission Horizon 2020 Research and Innovation Programme[730562] ; Spanish Ministerio de Economa y Competitividad (MINECO) of ICCUB (Unidad de Excelencia Mara de Maeztu)[AYA201676012-C3-1-P, FPA2015-69210-C6-2-R, MDM-2014-0369] ; Spanish MINECO[AYA2012-38491-C02-02, AYA2015-63939-C2-1-P] ; National Key R&D Programme of China[2018YFA0404603] ; European Union's Horizon 2020 research and innovation program[653477] ; Hungarian National Research, Development and Innovation Office[OTKA NN110333] ; Australian Government |
| 语种 | 英语 |
| 学科领域 | 天文学 ; 射电天文学 ; 恒星与银河系 |
| 文章类型 | Article |
| 出版者 | AMER ASSOC ADVANCEMENT SCIENCE |
| 出版地 | 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA |
| ISSN | 0036-8075 |
| URL | 查看原文 |
| WOS记录号 | WOS:000460194200043 |
| WOS研究方向 | Science & Technology - Other Topics |
| WOS类目 | Multidisciplinary Sciences |
| 关键词[WOS] | AFTERGLOW LIGHT CURVES ; ELECTROMAGNETIC COUNTERPART ; LUMINOSITY FUNCTION ; GRB JETS ; RAY ; GW170817 |
| 引用统计 | |
| 文献类型 | 期刊论文 |
| 条目标识符 | http://ir.ynao.ac.cn/handle/114a53/19520 |
| 专题 | 射电天文研究组 |
| 通讯作者 | Ghirlanda, G.; Salafia, O. S. |
| 作者单位 | 1.Istituto Nazionale di Astrofisica–Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate, Italy 2.Dipartimento di Fisica G. Occhialini, Università di Milano-Bicocca, Piazza della Scienza 3, IT-20126 Milano, Italy 3.Sezione di Milano Bicocca, Istituto Nazionale Fisica Nucleare (INFN), Piazza della Scienza 3, 20126 Milano, Italy 4.Joint Institute for Very Long Baseline Interferometry (VLBI) European Research Infrastructure Consortium (ERIC), Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, Netherlands 5.Istituto Nazionale di Astrofisica–Istituto di Radioastronomia, via Gobetti 101, I40129, Bologna, Italia 6.Chalmers University of Technology, Onsala Space Observatory, SE-439 92, Sweden 7.Yunnan Observatories, Chinese Academy of Sciences, 650216 Kunming, Yunnan, China 8.Instituto de Astrofísica de Andalucía–Consejo Superior de Investigaciones Científicas (CSIC), Glorieta de la Astronomía s/n, E-18008, Granada, Spain 9.Shanghai Astronomical Observatory, Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, 200030 Shanghai, China 10.Laboratoire 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, France 11.Electronic 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, UK 12.Gran Sasso Science Institute, Viale F. Crispi 7, I-67100, L’Aquila, Italy 13.Laboratori Nazionali del Gran Sasso, INFN, I-67100 L’Aquila, Italy 14.Max Planck Institute fur Radioastronomie, Auf dem Huegel 69, Bonn D-53121, Germany 15.AstroParticule 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, 16.Space Science Data Center, Agenzia Spaziale Italiana (ASI), Via del Politecnico, 00133, Roma, Italy 17.Konkoly Observatory, Magyar Tudományos Akadémia (MTA) Research Centre for Astronomy and Earth Sciences, Konkoly Thege Miklós út 15-17, H-1121 Budapest, Hungary 18.Centre for Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziadzka 5, 87-100 Torun, Poland 19.Department of Astrodynamics and Space Missions, Delft University of Technology, Kluyverweg 1, 2629 HS Delft, Netherlands 20.Space Research Organisation of the Netherlands (SRON), Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, Netherland 21.Department of Astrophysics, Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University, Post Office Box 9010, 6500 GL Nijmegen, Netherlands 22.Leiden Univ, Sterrewacht Leiden, POB 9513, NL-2300 RA Leiden, Netherlands 23.Departamento de Física Teórica, Facultad de Ciencias, Universidad de Zaragoza, E-50019, Spain 24.Commonwealth Scientific and Industrial Research Organization (CSIRO) Astronomy and Space Science, PO Box 1130, Bentley WA 6102, Australia 25.Istituto Nazionale di Astrofisica, Istituto di Astrofisica Spaziale e Fisica cosmica (IASF), via E. Bassini 15, 20133 Milano, Italy 26.Galaxies, Etoiles, Physique et Instrumentation (GEPI) Observatoire de Paris, CNRS UMR 8111, Meudon, France 27.Xinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science 1-Street, Urumqi 831001, China 28.Key Laboratory for Radio Astronomy, Chinese Academy of Sciences, 2 West Beijing Road, Nanjing 210008, China 29.Osservatorio Astronomico di Brera, INAF, Milan, Italy 30.Department of Physics, University of Trento, via Sommarive 14, I-38123 Trento, Italy |
| 推荐引用方式 GB/T 7714 | Ghirlanda, G.,Salafia, O. S.,Paragi, Z.,et al. Compact radio emission indicates a structured jet was produced by a binary neutron star merger[J]. SCIENCE,2019,363(6430):968-+. |
| APA | Ghirlanda, G..,Salafia, O. S..,Paragi, Z..,Giroletti, M..,Yang J.,...&Zhang, M..(2019).Compact radio emission indicates a structured jet was produced by a binary neutron star merger.SCIENCE,363(6430),968-+. |
| MLA | Ghirlanda, G.,et al."Compact radio emission indicates a structured jet was produced by a binary neutron star merger".SCIENCE 363.6430(2019):968-+. |
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