A radio counterpart to a neutron star merger
G. HallinanDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAA. CorsiDepartment of Physics and Astronomy, Texas Tech University, Lubbock, TX 79409, USAK. P. MooleyAstrophysics, Department of Physics, University of Oxford, Oxford OX1 3RH, UKKenta HotokezakaCenter for Computational Astrophysics, Flatiron Institute, 162 5th Avenue, New York, NY 10010, USAEhud NakarRaymond and Beverly Sackler School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, IsraelM. M. KasliwalDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAD. L. KaplanDepartment of Physics, University of Wisconsin, Milwaukee, WI 53201, USAD. A. FrailNational Radio Astronomy Observatory, Socorro, NM 87801, USAS. T. MyersNational Radio Astronomy Observatory, Socorro, NM 87801, USAT. MurphyAustralian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)Kishalay DeDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAD. DobieAustralia Telescope National Facility, Commonwealth Scientific and Industrial Research Organisation, Astronomy and Space Science, Epping, NSW 1710, AustraliaJ. R. AllisonAustralian Research Council Centre of Excellence for All-sky Astrophysics in 3 Dimensions (ASTRO 3D)K. W. BannisterAustralia Telescope National Facility, Commonwealth Scientific and Industrial Research Organisation, Astronomy and Space Science, Epping, NSW 1710, AustraliaV. BhaleraoDepartment of Physics, Indian Institute of Technology Bombay, Mumbai 400076, IndiaP. ChandraNational Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune University Campus, Ganeshkhind Pune 411007, IndiaT. E. ClarkeRemote Sensing Division, Naval Research Laboratory, Washington, DC 20375, USAS. GiacintucciRemote Sensing Division, Naval Research Laboratory, Washington, DC 20375, USAA. Y. Q. HoDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAA. HoreshRacah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, IsraelN. E. KassimRemote Sensing Division, Naval Research Laboratory, Washington, DC 20375, USAS. R. KulkarniDivision of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA 91125, USAE. LencAustralian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)Felix J. LockmanC. LynchAustralian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)D. NicholsInstitute of Mathematics, Astrophysics and Particle Physics, Radboud University, 6525 AJ Nijmegen, NetherlandsS. NissankeInstitute of Mathematics, Astrophysics and Particle Physics, Radboud University, 6525 AJ Nijmegen, NetherlandsN. PalliyaguruDepartment of Physics and Astronomy, Texas Tech University, Lubbock, TX 79409, USAWendy PetersRemote Sensing Division, Naval Research Laboratory, Washington, DC 20375, USATsvi PiranRacah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, IsraelJ. RanaInter University Centre for Astronomy and Astrophysics, Pune University Campus, Pune, Maharashtra 411007, IndiaE. M. SadlerAustralian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO)L. P. SingerAstroparticle Physics Laboratory, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA
2017en
ABI
Аннотация
Gravitational waves have been detected from a binary neutron star merger event, GW170817. The detection of electromagnetic radiation from the same source has shown that the merger occurred in the outskirts of the galaxy NGC 4993, at a distance of 40 megaparsecs from Earth. We report the detection of a counterpart radio source that appears 16 days after the event, allowing us to diagnose the energetics and environment of the merger. The observed radio emission can be explained by either a collimated ultrarelativistic jet, viewed off-axis, or a cocoon of mildly relativistic ejecta. Within 100 days of the merger, the radio light curves will enable observers to distinguish between these models, and the angular velocity and geometry of the debris will be directly measurable by very long baseline interferometry.
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