Compact radio emission indicates a structured jet was produced by a binary neutron star merger
Journal article, 2019

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.

Author

G. Ghirlanda

University of Milano-Bicocca

Osservatorio Astronomico di Brera

National Institute for Nuclear Physics

O. S. Salafia

Osservatorio Astronomico di Brera

University of Milano-Bicocca

National Institute for Nuclear Physics

Z. Paragi

Joint Institute for VLBI in Europe (JIVE)

M. Giroletti

Istituto nazionale di astrofisica (INAF)

Jun Yang

Chinese Academy of Sciences

Chalmers, Space, Earth and Environment, Onsala Space Observatory, Observation Support

B. Marcote

Joint Institute for VLBI in Europe (JIVE)

J. Blanchard

Joint Institute for VLBI in Europe (JIVE)

I. Agudo

Institute of Astrophysics of Andalusia (IAA)

T. An

Shanghai Astronomical Observatory

M. G. Bernardini

Laboratoire Univers et Particules de Montpellier

R. J. Beswick

University of Manchester

M. Branchesi

Gran Sasso Science Institute (GSSI)

National Institute for Nuclear Physics

S. Campana

Osservatorio Astronomico di Brera

C. Casadio

Max Planck Society

E. Chassande-Mottin

Paris Diderot University

M. Colpi

National Institute for Nuclear Physics

University of Milano-Bicocca

S. Covino

Osservatorio Astronomico di Brera

P. D'Avanzo

Osservatorio Astronomico di Brera

V. D'Elia

Agenzia Spaziale Italiana

S. Frey

Hungarian Academy of Sciences

M. P. Gawroński

Nicolaus Copernicus University

G. Ghisellini

Osservatorio Astronomico di Brera

L. I. Gurvits

Joint Institute for VLBI in Europe (JIVE)

Delft University of Technology

P. G. Jonker

Netherlands Institute for Space Research (SRON)

Radboud University

H. J. van Langevelde

Joint Institute for VLBI in Europe (JIVE)

Leiden University

A. Melandri

Osservatorio Astronomico di Brera

J. Moldon

University of Manchester

L. Nava

Osservatorio Astronomico di Brera

A. Perego

National Institute for Nuclear Physics

M.A. Pérez-Torres

Institute of Astrophysics of Andalusia (IAA)

University of Zaragoza

C. Reynolds

Commonwealth Scientific and Industrial Research Organisation (CSIRO)

R. Salvaterra

Istituto nazionale di astrofisica (INAF)

G. Tagliaferri

Osservatorio Astronomico di Brera

T. Venturi

Istituto nazionale di astrofisica (INAF)

S. D. Vergani

Observatoire de Paris-Meudon

M. Zhang

Chinese Academy of Sciences

Science (New York, N.Y.)

1095-9203 (eISSN)

Vol. 363 6430 968-971

Subject Categories

Accelerator Physics and Instrumentation

Subatomic Physics

Astronomy, Astrophysics and Cosmology

DOI

10.1126/science.aau8815

PubMed

30792360

More information

Latest update

11/12/2021