Properties of the Binary Neutron Star Merger GW170817

LIGO Scientific Collaboration and Virgo Collaboration

Research output: Contribution to JournalArticleAcademicpeer-review

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
Pages (from-to)1-32
Number of pages32
JournalPhysical Review X
Volume9
Issue number1
DOIs
Publication statusPublished - 2 Jan 2019

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binary stars
neutron stars
gravitational waves
LIGO (observatory)
sky
observatories
equations of state
flux density
electromagnetism
galaxies
intervals
detectors
estimates

Cite this

LIGO Scientific Collaboration and Virgo Collaboration (2019). Properties of the Binary Neutron Star Merger GW170817. Physical Review X, 9(1), 1-32. [011001]. https://doi.org/10.1103/PhysRevX.9.011001
LIGO Scientific Collaboration and Virgo Collaboration. / Properties of the Binary Neutron Star Merger GW170817. In: Physical Review X. 2019 ; Vol. 9, No. 1. pp. 1-32.
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title = "Properties of the Binary Neutron Star Merger GW170817",
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.",
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Taracchini and Tasson, {J. D.} and Taylor, {J. A.} and R. Taylor and Tewari, {S. V.} and T. Theeg and F. Thies and Thomas, {E. G.} and M. Thomas and P. Thomas and Thorne, {K. A.} and E. Thrane and S. Tiwari and V. Tiwari and Tokmakov, {K. V.} and K. Toland and M. Tonelli and Z. Tornasi and A. Torres-Forn{\'e} and Torrie, {C. I.} and D. T{\"o}yr{\"a} and F. Travasso and G. Traylor and J. Trinastic and Tringali, {M. C.} and L. Trozzo and Tsang, {K. W.} and M. Tse and R. Tso and D. Tsuna and L. Tsukada and D. Tuyenbayev and K. Ueno and D. Ugolini and Urban, {A. L.} and Usman, {S. A.} and H. Vahlbruch and G. Vajente and G. Valdes and {Van Bakel}, N. and {Van Beuzekom}, M. and {Van Den Brand}, {J. F.J.} and {Van Den Broeck}, C. and Vander-Hyde, {D. C.} and {Van Der Schaaf}, L. and {Van Heijningen}, {J. V.} and {Van Veggel}, {A. A.} and M. Vardaro and V. Varma and S. Vass and M. Vas{\'u}th and A. Vecchio and G. Vedovato and J. Veitch and Veitch, {P. J.} and K. Venkateswara and G. Venugopalan and D. Verkindt and F. Vetrano and A. Vicer{\'e} and Viets, {A. D.} and S. Vinciguerra and Vine, {D. J.} and Vinet, {J. Y.} and S. Vitale and T. Vo and H. Vocca and C. Vorvick and Vyatchanin, {S. P.} and Wade, {A. R.} and Wade, {L. E.} and M. Wade and R. Walet and M. Walker and L. Wallace and S. Walsh and G. Wang and H. Wang and Wang, {J. Z.} and Wang, {W. H.} and Wang, {Y. F.} and Ward, {R. L.} and J. Warner and M. Was and J. Watchi and B. Weaver and Wei, {L. W.} and M. Weinert and Weinstein, {A. J.} and R. Weiss and F. Wellmann and L. Wen and Wessel, {E. K.} and P. We{\ss}els and J. Westerweck and K. Wette and Whelan, {J. T.} and Whiting, {B. F.} and C. Whittle and D. Wilken and D. Williams and Williams, {R. D.} and Williamson, {A. R.} and Willis, {J. L.} and B. Willke and Wimmer, {M. H.} and W. Winkler and Wipf, {C. C.} and H. Wittel and G. Woan and J. Woehler and Wofford, {J. K.} and Wong, {W. K.} and J. Worden and Wright, {J. L.} and Wu, {D. S.} and Wysocki, {D. M.} and S. Xiao and W. Yam and H. Yamamoto and Yancey, {C. C.} and L. Yang and Yap, {M. J.} and M. Yazback and Hang Yu and Haocun Yu and M. Yvert and A. Zadrożny and M. Zanolin and T. Zelenova and Zendri, {J. P.} and M. Zevin and J. Zhang and L. Zhang and M. Zhang and T. Zhang and Zhang, {Y. H.} and C. Zhao and M. Zhou and Z. Zhou and Zhu, {S. J.} and Zhu, {X. J.} and Zimmerman, {A. B.} and Y. Zlochower and Zucker, {M. E.} and J. Zweizig and {LIGO Scientific Collaboration and Virgo Collaboration}",
year = "2019",
month = "1",
day = "2",
doi = "10.1103/PhysRevX.9.011001",
language = "English",
volume = "9",
pages = "1--32",
journal = "Physical Review X",
issn = "2160-3308",
publisher = "American Physical Society",
number = "1",

}

LIGO Scientific Collaboration and Virgo Collaboration 2019, 'Properties of the Binary Neutron Star Merger GW170817' Physical Review X, vol. 9, no. 1, 011001, pp. 1-32. https://doi.org/10.1103/PhysRevX.9.011001

Properties of the Binary Neutron Star Merger GW170817. / LIGO Scientific Collaboration and Virgo Collaboration.

In: Physical Review X, Vol. 9, No. 1, 011001, 02.01.2019, p. 1-32.

Research output: Contribution to JournalArticleAcademicpeer-review

TY - JOUR

T1 - Properties of the Binary Neutron Star Merger GW170817

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AU - LIGO Scientific Collaboration and Virgo Collaboration

PY - 2019/1/2

Y1 - 2019/1/2

N2 - 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.

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.

UR - http://www.scopus.com/inward/record.url?scp=85061618892&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85061618892&partnerID=8YFLogxK

U2 - 10.1103/PhysRevX.9.011001

DO - 10.1103/PhysRevX.9.011001

M3 - Article

VL - 9

SP - 1

EP - 32

JO - Physical Review X

JF - Physical Review X

SN - 2160-3308

IS - 1

M1 - 011001

ER -

LIGO Scientific Collaboration and Virgo Collaboration. Properties of the Binary Neutron Star Merger GW170817. Physical Review X. 2019 Jan 2;9(1):1-32. 011001. https://doi.org/10.1103/PhysRevX.9.011001