Properties of the binary black hole merger GW150914

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dc.contributor.authorAbbott, B. P.
dc.contributor.authorDavies, G. S.
dc.contributor.authorLIGO Scientific Collaboration and Virgo Collaboration
dc.date.accessioned2017-04-05T13:24:47Z
dc.date.available2017-04-05T13:24:47Z
dc.date.issued2016-06
dc.description.abstractOn September 14, 2015, the Laser Interferometer Gravitational-Wave Observatory (LIGO) detected a gravitational-wave transient (GW150914); we characterize the properties of the source and its parameters. The data around the time of the event were analyzed coherently across the LIGO network using a suite of accurate waveform models that describe gravitational waves from a compact binary system in general relativity. GW150914 was produced by a nearly equal mass binary black hole of masses 36þ5 −4M⊙ and 29þ4 −4M⊙; for each parameter we report the median value and the range of the 90% credible interval. The dimensionless spin magnitude of the more massive black hole is bound to be < 0.7 (at 90% probability). The luminosity distance to the source is 410þ160 −180 Mpc, corresponding to a redshift 0.09þ0.03 −0.04 assuming standard cosmology. The source location is constrained to an annulus section of 610 deg2, primarily in the southern hemisphere. The binary merges into a black hole of mass 62þ4 −4M⊙ and spin 0.67þ0.05 −0.07 . This black hole is significantly more massive than any other inferred from electromagnetic observations in the stellar-mass regime.en_UK
dc.identifier.citationAbbott, BP., et al., (LIGO Scientific Collaboration and Virgo Collaboration). Properties of the binary black hole merger GW150914. Physical Review Letters, 116(24) 241102 (2016)en_UK
dc.identifier.urihttps://doi.org/10.1103/PhysRevLett.116.241102
dc.identifier.urihttp://dspace.lib.cranfield.ac.uk/handle/1826/11719
dc.publisherAmerican Physical Societyen_UK
dc.rightsAttribution 3.0
dc.rights.urihttp://creativecommons.org/licenses/by/3.0/
dc.titleProperties of the binary black hole merger GW150914en_UK
dc.typeArticleen_UK

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