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.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
Source PublicationSCIENCE
Contribution Rank27
AbstractThe 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.
Indexed BySCI
Funding ProjectAustralian Government ; National Institute of Astrophysics[] ; Italian Ministry for University and Research (MIUR)[] ; 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]
WOS Research AreaScience & Technology - Other Topics
WOS SubjectMultidisciplinary Sciences
WOS IDWOS:000460194200043
Citation statistics
Cited Times:90[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Corresponding AuthorGhirlanda, G.; Salafia, O. S.
Affiliation1.Osserv Astron Brera, Ist Nazl Astrofis, Via E Bianchi 46, I-23807 Merate, Italy
2.Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, IT-20126 Milan, Italy
3.Ist Nazl Fis Nucl, Sez Milano Bicocca, Piazza Sci 3, I-20126 Milan, Italy
4.Joint Inst Very Long Baseline Interferometry VLBI, Oude Hoogeveensedijk 4, NL-7991 PD Dwingeloo, Netherlands
5.Ist Nazl Astrofis, Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy
6.Chalmers Univ Technol, Onsala Space Observ, S-43992 Gothenburg, Sweden
7.Chinese Acad Sci, Yunnan Observ, Kunming 650216, Yunnan, Peoples R China
8.CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain
9.Chinese Acad Sci, Shanghai Astron Observ, Key Lab Radio Astron, Shanghai 200030, Peoples R China
10.Univ Montpellier, Lab Univers & Particules Montpellier, Inst Natl Phys Nucl & Phys Particules, CNRS,IN2P3, Pl Eugene Bataillon, F-34085 Montpellier, France
11.Univ Manchester, Elect Multielement Radio Linked Interferomer Netw, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester, Lancs, England
12.Gran Sasso Sci Inst, Viale F Crispi 7, I-67100 Laquila, Italy
13.INFN, Lab Nazl Gran Sasso, I-67100 Laquila, Italy
14.Max Planck Inst Radioastron, Huegel 69, D-53121 Bonn, Germany
15.Univ Paris Diderot, Commissariat Energie Atom & Energies Alternat, Inst Res Fundamental Laws Universe CEA IRFU,Sorbo, AstroParticule & Cosmol APC,CNRS,IN2P3,Observ Par, F-75205 Paris 13, France
16.ASI, Space Sci Data Ctr, Via Politecn, I-00133 Rome, Italy
17.Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary
18.Nicolaus Copernicus Univ, Ctr Astron, Fac Phys Astron & Informat, Grudziadzka 5, PL-87100 Torun, Poland
19.Delft Univ Technol, Dept Astrodynam & Space Mission, Kluyverweg 1, NL-2629 HS Delft, Netherlands
20.SRON Netherlands Inst Space Res, SRON, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands
21.Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands
22.Leiden Univ, Sterrewacht Leiden, POB 9513, NL-2300 RA Leiden, Netherlands
23.Univ Zaragoza, Dept Fis Teor, Fac Ciencias, E-50019 Zaragoza, Spain
24.Commonwealth Sci & Ind Res Org CSIRO Astron & Spa, POB 1130, Bentley, WA 6102, Australia
25.Ist Nazl Astrofis, Ist Astrofis Spaziale & Fis Cosm IASF, Via E Bassini 15, I-20133 Milan, Italy
26.Galaxies Etoiles Phys & Instrumentat GEPI Obsev P, CNRS, UMR 8111, Meudon, France
27.Chinese Acad Sci, Xinjiang Astron Observ, 150 Sci 1 St, Urumqi 831001, Peoples R China
28.Chinese Acad Sci, Key Lab Radio Astron, 2 West Beijing Rd, Nanjing 210008, Jiangsu, Peoples R China
29.INAF, Osservatorio Astronom Brera, Milan, Italy
30.Univ Trento, Dept Phys, Via Sommar 14, I-38123 Trento, Italy
Recommended Citation
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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