The environment of the binary neutron star merger GW170817

Research output: Contribution to journalArticlepeer-review


  • A. J. Levan
  • J. D. Lyman
  • N. R. Tanvir
  • J. Hjorth
  • E. R. Stanway
  • D. Steeghs
  • A. S. Fruchter
  • E. Troja
  • S. L Schrøder
  • K. Wiersema
  • S. H. Bruun
  • Z. Cano
  • S. B. Cenko
  • A de Ugarte Postigo
  • P. Evans
  • S. Fairhurst
  • O. D. Fox
  • J. P. U. Fynbo
  • B. Gompertz
  • J. Greiner
  • M. Im
  • L. Izzo
  • P. Jakobsson
  • T. Kangas
  • H. G. Khandrika
  • A. Y. Lien
  • D. Malesani
  • P. O'Brien
  • J. P. Osborne
  • E. Plazzi
  • E. Pian
  • D. A. Perley
  • S. Rosswog
  • R. E. Ryan
  • S. Schulze
  • P. Sutton
  • C. C. Thöne
  • D. J. Watson
  • R. A. M. J. Wijers

Colleges, School and Institutes


We present Hubble Space Telescope and Chandra imaging, combined with Very Large Telescope MUSE integral field spectroscopy of the counterpart and host galaxy of the first binary neutron star merger detected via gravitational wave emission by LIGO & Virgo, GW170817. The host galaxy, NGC 4993, is an S0 galaxy at z=0.009783. There is evidence for large, face-on spiral shells in continuum imaging, and edge-on spiral features visible in nebular emission lines. This suggests that NGC 4993 has undergone a relatively recent (

Bibliographic note

ApJL in press, 13 pages


Original languageEnglish
Article numberL28
JournalAstrophysical Journal Letters
Issue number2
Publication statusPublished - 16 Oct 2017


  • astro-ph.HE