Properties of the Binary Black Hole Merger GW150914

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dc.identifier.uri http://dx.doi.org/10.15488/2109
dc.identifier.uri http://www.repo.uni-hannover.de/handle/123456789/2134
dc.contributor.author Abbott, B.P.
dc.contributor.author Abbott, R.
dc.contributor.author Abbott, T.D.
dc.contributor.author Abernathy, M.R.
dc.contributor.author Acernese, F.
dc.contributor.author et al.
dc.contributor.author LIGO Scientific Collaboration
dc.contributor.author Virgo Collaboration
dc.date.accessioned 2017-10-24T08:25:15Z
dc.date.available 2017-10-24T08:25:15Z
dc.date.issued 2016
dc.identifier.citation Abbott, B.P.; Abbott, R.; Abbott, T.D.; Abernathy, M.R.; Acernese, F.; et, al. (LIGO Scientific Collaboration and Virgo Collaboration): Properties of the Binary Black Hole Merger GW150914. In: Physical Review Letters 116 (2016), Nr. 24, 241102. DOI: https://doi.org/10.1103/PhysRevLett.116.241102
dc.description.abstract On 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+5M and 29-4+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 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 deg2, primarily in the southern hemisphere. The binary merges into a black hole of mass 62-4+4M 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. © 2016 authors. Published by the American Physical Society. eng
dc.language.iso eng
dc.publisher College Park, MD : American Physical Society
dc.relation.ispartofseries Physical Review Letters 116 (2016), Nr. 24
dc.rights CC BY 3.0 Unported
dc.rights.uri https://creativecommons.org/licenses/by/3.0/
dc.subject Bins eng
dc.subject Gravitation eng
dc.subject Gravitational effects eng
dc.subject Gravity waves eng
dc.subject Interferometers eng
dc.subject Laser interferometry eng
dc.subject Relativity eng
dc.subject Credible interval eng
dc.subject Electromagnetic observations eng
dc.subject General Relativity eng
dc.subject Laser interferometer gravitational-wave observatories eng
dc.subject Massive black holes eng
dc.subject Source location eng
dc.subject Southern Hemisphere eng
dc.subject Waveform models eng
dc.subject Stars eng
dc.subject Gravitationswelle ger
dc.subject.ddc 530 | Physik ger
dc.title Properties of the Binary Black Hole Merger GW150914
dc.type article
dc.type Text
dc.relation.issn 0031-9007
dc.relation.doi https://doi.org/10.1103/PhysRevLett.116.241102
dc.bibliographicCitation.issue 24
dc.bibliographicCitation.volume 116
dc.bibliographicCitation.firstPage 241102
dc.description.version publishedVersion
tib.accessRights frei zug�nglich


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