Search for Post-merger Gravitational Waves from the Remnant of the Binary Neutron Star Merger GW170817
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Abbott_2017_ApJL_851_L16.pdf
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Author(s)
LIGO Scientific Collaboration
Virgo Collaboration
Aggarwal, Nancy
Barsotti, Lisa
Biscans, Sebastien
Buikema, Aaron
Demos, Nicholas
Donovan, Frederick J
Eisenstein, Robert Alan
Essick, Reed Clasey
Date Issued
December 2017
Journal
Astrophysical Journal. Letters
Publisher
American Astronomical Society
Citation
Abbott, B. P. et al. “Search for Post-Merger Gravitational Waves from the Remnant of the Binary Neutron Star Merger GW170817.” The Astrophysical Journal 851, 1 (December 2017): L16 © 2017 The American Astronomical Society
Version
Final published version
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.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
LIGO (Observatory : Massachusetts Institute of Technology)
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DOI of Published Version
https://doi.org/10.3847/2041-8213/AA9A35
