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Properties of the Binary Neutron Star Merger GW170817

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Properties of the Binary Neutron Star Merger GW170817

dc.contributor.author	LIGO Scientific Collaboration
dc.contributor.author	Virgo Collaboration
dc.contributor.author	Abbott, B. P.
dc.contributor.author	Aloy Toras, Miguel Angel
dc.contributor.author	Cerdá Durán, Pablo
dc.contributor.author	Cordero Carrión, Isabel
dc.contributor.author	Font Roda, José Antonio
dc.contributor.author	Marquina Vila, Antonio
dc.contributor.author	Obergaulinger, M.
dc.contributor.author	Sanchis Gual, Nicolas
dc.contributor.author	Torres Forné, Alejandro
dc.date.accessioned	2020-01-09T15:27:37Z
dc.date.available	2020-01-09T15:27:37Z
dc.date.issued	2019
dc.identifier.citation	LIGO Scientific Collaboration Virgo Collaboration Abbott, B. P. Aloy Toras, Miguel Angel Cerdá Durán, Pablo Cordero Carrión, Isabel Font Roda, José Antonio Marquina Vila, Antonio Obergaulinger, M. Sanchis Gual, Nicolas Torres Forné, Alejandro 2019 Properties of the Binary Neutron Star Merger GW170817 Physical Review X 9 1 011001-1 011001-32
dc.identifier.uri	https://hdl.handle.net/10550/72540
dc.description.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.
dc.language.iso	eng
dc.relation.ispartof	Physical Review X, 2019, vol. 9, num. 1, p. 011001-1-011001-32
dc.subject	Gravitació
dc.subject	Astrofísica
dc.title	Properties of the Binary Neutron Star Merger GW170817
dc.type	journal article	es_ES
dc.date.updated	2020-01-09T15:27:38Z
dc.identifier.doi	10.1103/PhysRevX.9.011001
dc.identifier.idgrec	135619
dc.rights.accessRights	open access	es_ES