Properties of the binary neutron star merger GW170817

B. P. Abbott, Svetoslava Angelova, Nicholas Lockerbie, Stuart Reid, Kirill Tokmakov, LIGO Scientific Collaboration, Virgo Collaboration

Research output: Contribution to journalArticle

128 Citations (Scopus)

Abstract

On August 17, 2017, the Advanced LIGO and Advanced Virgo gravitational-wave detectors observed a low-mass compact binary inspiral. The initial sky localization of the source of the gravitational-wave signal, GW170817, allowed electromagnetic observatories to identify NGC 4993 as the host galaxy. In this work, we improve initial estimates of the binary's properties, including component masses, spins, and tidal parameters, using the known source location, improved modeling, and recalibrated Virgo data. We extend the range of gravitational-wave frequencies considered down to 23 Hz, compared to 30 Hz in the initial analysis. We also compare results inferred using several signal models, which are more accurate and incorporate additional physical effects as compared to the initial analysis. We improve the localization of the gravitational-wave source to a 90% credible region of 16 deg2. We find tighter constraints on the masses, spins, and tidal parameters, and continue to find no evidence for nonzero component spins. The component masses are inferred to lie between 1.00 and 1.89 M when allowing for large component spins, and to lie between 1.16 and 1.60 M (with a total mass 2.73-0.01+0.04 M) when the spins are restricted to be within the range observed in Galactic binary neutron stars. Using a precessing model and allowing for large component spins, we constrain the dimensionless spins of the components to be less than 0.50 for the primary and 0.61 for the secondary. Under minimal assumptions about the nature of the compact objects, our constraints for the tidal deformability parameter Λ are (0,630) when we allow for large component spins, and 300-230+420 (using a 90% highest posterior density interval) when restricting the magnitude of the component spins, ruling out several equation-of-state models at the 90% credible level. Finally, with LIGO and GEO600 data, we use a Bayesian analysis to place upper limits on the amplitude and spectral energy density of a possible postmerger signal.

Original languageEnglish
Article number011001
Number of pages32
JournalPhysical Review X
Volume9
Issue number1
DOIs
Publication statusPublished - 2 Jan 2019

Fingerprint

binary stars
merger
neutron stars
gravitational waves
LIGO (observatory)
Bayesian analysis
equation of state
observatory
sky
observatories
modeling
equations of state
energy
parameter
flux density
electromagnetism
galaxies
intervals
detectors
analysis

Keywords

  • LIGO-Virgo
  • gravitational waves
  • binary neutron star merger

Cite this

Abbott, B. P., Angelova, S., Lockerbie, N., Reid, S., Tokmakov, K., LIGO Scientific Collaboration, & Virgo Collaboration (2019). Properties of the binary neutron star merger GW170817. Physical Review X, 9(1), [011001]. https://doi.org/10.1103/PhysRevX.9.011001
Abbott, B. P. ; Angelova, Svetoslava ; Lockerbie, Nicholas ; Reid, Stuart ; Tokmakov, Kirill ; LIGO Scientific Collaboration ; Virgo Collaboration. / Properties of the binary neutron star merger GW170817. In: Physical Review X. 2019 ; Vol. 9, No. 1.
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Abbott, BP, Angelova, S, Lockerbie, N, Reid, S, Tokmakov, K, LIGO Scientific Collaboration & Virgo Collaboration 2019, 'Properties of the binary neutron star merger GW170817', Physical Review X, vol. 9, no. 1, 011001. https://doi.org/10.1103/PhysRevX.9.011001

Properties of the binary neutron star merger GW170817. / Abbott, B. P.; Angelova, Svetoslava; Lockerbie, Nicholas; Reid, Stuart; Tokmakov, Kirill; LIGO Scientific Collaboration; Virgo Collaboration.

In: Physical Review X, Vol. 9, No. 1, 011001, 02.01.2019.

Research output: Contribution to journalArticle

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T1 - Properties of the binary neutron star merger GW170817

AU - Abbott, B. P.

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AU - Lockerbie, Nicholas

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AB - On August 17, 2017, the Advanced LIGO and Advanced Virgo gravitational-wave detectors observed a low-mass compact binary inspiral. The initial sky localization of the source of the gravitational-wave signal, GW170817, allowed electromagnetic observatories to identify NGC 4993 as the host galaxy. In this work, we improve initial estimates of the binary's properties, including component masses, spins, and tidal parameters, using the known source location, improved modeling, and recalibrated Virgo data. We extend the range of gravitational-wave frequencies considered down to 23 Hz, compared to 30 Hz in the initial analysis. We also compare results inferred using several signal models, which are more accurate and incorporate additional physical effects as compared to the initial analysis. We improve the localization of the gravitational-wave source to a 90% credible region of 16 deg2. We find tighter constraints on the masses, spins, and tidal parameters, and continue to find no evidence for nonzero component spins. The component masses are inferred to lie between 1.00 and 1.89 M when allowing for large component spins, and to lie between 1.16 and 1.60 M (with a total mass 2.73-0.01+0.04 M) when the spins are restricted to be within the range observed in Galactic binary neutron stars. Using a precessing model and allowing for large component spins, we constrain the dimensionless spins of the components to be less than 0.50 for the primary and 0.61 for the secondary. Under minimal assumptions about the nature of the compact objects, our constraints for the tidal deformability parameter Λ are (0,630) when we allow for large component spins, and 300-230+420 (using a 90% highest posterior density interval) when restricting the magnitude of the component spins, ruling out several equation-of-state models at the 90% credible level. Finally, with LIGO and GEO600 data, we use a Bayesian analysis to place upper limits on the amplitude and spectral energy density of a possible postmerger signal.

KW - LIGO-Virgo

KW - gravitational waves

KW - binary neutron star merger

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M3 - Article

VL - 9

JO - Physical Review X

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