Search for post-merger gravitational waves from the remnant of the binary neutron star merger GW170817

Research output: Contribution to journalArticlepeer-review

Authors

  • LIGO Scientific Collaboration
  • Virgo Collaboration

External organisations

  • California Institute of Technology
  • Louisiana State University
  • University of Salerno
  • Complesso Universitario di Monte S.Angelo
  • University of Florida
  • Monash University
  • LIGO Livingston Observatory
  • IN2P3
  • University of Sannio at Benevento
  • Albert-Einstein-Institut, Max-Planck-Institut für, Gravitationsphysik
  • University of Mississippi
  • University of Illinois
  • University of Cambridge
  • Institution Nikhef National Institute for Subatomic Physics
  • Massachusetts Institute of Technology
  • Instituto Nacional de Pesquisas Espaciais
  • Facebook
  • Laboratori Nazionali del Gran Sasso
  • Inter-University Centre for Astronomy and Astrophysics India
  • Tata Institute of Fundamental Research
  • University of Wisconsin-Milwaukee
  • Università di Pisa
  • Sezione INFN di Pisa
  • Australian National University
  • Domaine Scientifique de la Doua
  • University of the West of Scotland

Abstract

The first observation of a binary neutron star (NS) coalescence by the Advanced LIGO and Advanced Virgo gravitational-wave (GW) detectors offers an unprecedented opportunity to study matter under the most extreme conditions. After such a merger, a compact remnant is left over whose nature depends primarily on the masses of the inspiraling objects and on the equation of state of nuclear matter. This could be either a black hole (BH) or an NS, with the latter being either long-lived or too massive for stability implying delayed collapse to a BH. Here, we present a search for GWs from the remnant of the binary NS merger GW170817 using data from Advanced LIGO and Advanced Virgo. We search for short- (≲1 s) and intermediate-duration (≲500 s) signals, which include GW emission from a hypermassive NS or supramassive NS, respectively. We find no signal from the post-merger remnant. Our derived strain upper limits are more than an order of magnitude larger than those predicted by most models. For short signals, our best upper limit on the root sum square of the GW strain emitted from 1-4 kHz is at 50% detection efficiency. For intermediate-duration signals, our best upper limit at 50% detection efficiency is for a millisecond magnetar model, and for a bar-mode model. These results indicate that post-merger emission from a similar event may be detectable when advanced detectors reach design sensitivity or with next-generation detectors.

Details

Original languageEnglish
Article numberL16
JournalAstrophysical Journal Letters
Volume851
Issue number1
Publication statusPublished - 7 Dec 2017