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Properties of the binary black hole merger GW150914

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dc.contributor.authorAbbott, B.P.
dc.contributor.authorLIGO Scientific Collaboration,
dc.contributor.authorVirgo Collaboration,
dc.contributor.authorAbbott, R.
dc.contributor.authorAbbott, T.D.
dc.contributor.authorAbernathy, M.R.
dc.contributor.authorAcernese, F.
dc.contributor.authorAckley, K.
dc.contributor.authorAdams, C.
dc.contributor.authorAdams, T.
dc.contributor.authorAddesso, P.
dc.contributor.authorAdhikari, R.X.
dc.contributor.authorAdya, V.B.
dc.contributor.authorAffeldt, C.
dc.contributor.authorAgathos, M.
dc.contributor.authorAgatsuma, K.
dc.contributor.authorAggarwal, N.
dc.contributor.authorAguiar, O.D.
dc.contributor.authorAiello, L.
dc.contributor.authorAin, A.
dc.contributor.authoret al.
dc.date.issued2016
dc.descriptionPublished 14 June 2016
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 36_{-4}^{+5}M_{⊙} and 29_{-4}^{+4}M_{⊙}; 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 410_{-180}^{+160}  Mpc, corresponding to a redshift 0.09_{-0.04}^{+0.03} assuming standard cosmology. The source location is constrained to an annulus section of 610  deg^{2}, primarily in the southern hemisphere. The binary merges into a black hole of mass 62_{-4}^{+4}M_{⊙} and spin 0.67_{-0.07}^{+0.05}. This black hole is significantly more massive than any other inferred from electromagnetic observations in the stellar-mass regime.
dc.description.statementofresponsibilityB. P. Abbott ... S. E. Hollitt ... D. J. Hosken ... E. J. King ... J. Munch ... D. J. Ottaway ... P. J. Veitch ... et al. (The LIGO Scientific Collaboration and the Virgo Collaboration)
dc.identifier.citationPhysical Review Letters, 2016; 116(24):241102-1-241102-19
dc.identifier.doi10.1103/PhysRevLett.116.241102
dc.identifier.issn0031-9007
dc.identifier.issn1079-7114
dc.identifier.urihttp://hdl.handle.net/2440/101198
dc.language.isoen
dc.publisherAmerican Physical Society
dc.relation.grantARC
dc.rightsThis article is available under the terms of the Creative Commons Attribution 3.0 License. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI.
dc.source.urihttps://doi.org/10.1103/physrevlett.116.241102
dc.subjectLIGO Scientific Collaboration and Virgo Collaboration
dc.titleProperties of the binary black hole merger GW150914
dc.typeJournal article
pubs.publication-statusPublished

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