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Ghirlanda, G; Salafia, O S; Paragi, Z; Giroletti, M; Yang, J; Marcote, B; Blanchard, J; Agudo, I; An, T; Bernardini, M G; Beswick, R; Branchesi, M; Campana, S; Casadio, C; Chassande-Mottin, E; Colpi, M; Covino, S; D'Avanzo, P; D'Elia, V; Frey, S; Gawronski, M; Ghisellini, G; Gurvits, L I; Jonker, P G; van Langevelde, H J; Melandri, A; Moldon, J; Nava, L; Perego, A; Perez-Torres, M A; Reynolds, C; Salvaterra, R; Tagliaferri, G; Venturi, T; Vergani, S D; Zhang, M
Science (American Association for the Advancement of Science), 03/2019, Volume: 363, Issue: 6430Journal Article
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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