Статья

The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VI. Radio Constraints on a Relativistic Jet and Predictions for Late-time Emission from the Kilonova Ejecta

K. D. AlexanderHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAE. BergerHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAWen‐fai FongCenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USAPeter K. G. WilliamsHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAC. GuidorziDepartment of Physics and Earth Science, University of Ferrara, via Saragat 1, I-44122, Ferrara, ItalyR. MarguttiCenter for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL 60208, USAB. D. MetzgerDepartment of Physics and Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USAJ. AnnisFermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USAP. K. BlanchardHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAD. BroutDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAD. A. BrownDepartment of Physics, Syracuse University, Syracuse NY 13224, USAH.-Y. ChenKavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USAR. ChornockAstrophysical Institute, Department of Physics and Astronomy, 251B Clippinger Lab, Ohio University, Athens, OH 45701, USAP. S. CowperthwaiteHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAM. DroutCarnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USAT. EftekhariHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAJ. FriemanFermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USAD. E. HolzEnrico Fermi Institute, Department of Physics, Department of Astronomy and Astrophysics, 5640 South Ellis Avenue, Chicago, IL 60637, USAM. NichollHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USAA. RestDepartment of Physics and Astronomy, The Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218, USAM. SakoDepartment of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104, USAM. Soares-SantosFermi National Accelerator Laboratory, P.O. Box 500, Batavia, IL 60510, USAV. A. VillarHarvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA

2017en

ABI

Аннотация

Abstract We present Very Large Array (VLA) and Atacama Large Millimeter/submillimeter Array (ALMA) radio observations of GW170817, the first Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo gravitational wave (GW) event from a binary neutron star merger and the first GW event with an electromagnetic (EM) counterpart. Our data include the first observations following the discovery of the optical transient at both the centimeter (13.7 hr post-merger) and millimeter (2.41 days post-merger) bands. We detect faint emission at 6 GHz at 19.47 and 39.23 days after the merger, but not in an earlier observation at 2.46 days. We do not detect cm/mm emission at the position of the optical counterpart at frequencies of 10–97.5 GHz at times ranging from 0.6 to 30 days post-merger, ruling out an on-axis short gamma-ray burst (SGRB) for energies <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>≳</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>48</mml:mn> </mml:mrow> </mml:msup> </mml:math> erg. For fiducial SGRB parameters, our limits require an observer viewer angle of ≳20°. The radio and X-ray data can be jointly explained as the afterglow emission from an SGRB with a jet energy of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mo>∼</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>49</mml:mn> </mml:mrow> </mml:msup> <mml:mo>–</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>50</mml:mn> </mml:mrow> </mml:msup> </mml:math> erg that exploded in a uniform density environment with <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>n</mml:mi> <mml:mo>∼</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>4</mml:mn> </mml:mrow> </mml:msup> <mml:mo>–</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>2</mml:mn> </mml:mrow> </mml:msup> </mml:math> cm −3 , viewed at an angle of ∼20°–40° from the jet axis. Using the results of our light curve and spectral modeling, in conjunction with the inference of the circumbinary density, we predict the emergence of late-time radio emission from the deceleration of the kilonova (KN) ejecta on a timescale of ∼5–10 years that will remain detectable for decades with next-generation radio facilities, making GW170817 a compelling target for long-term radio monitoring.

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Идентификаторы

DOI: 10.3847/2041-8213/aa905d

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Цитирований: 3Использованных источников: 0

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