Properties of the binary black hole merger GW150914
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(Published version)
Date
2016
Authors
Abbott, B.P.
LIGO Scientific Collaboration,
Virgo Collaboration,
Abbott, R.
Abbott, T.D.
Abernathy, M.R.
Acernese, F.
Ackley, K.
Adams, C.
Adams, T.
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Advisors
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Journal article
Citation
Physical Review Letters, 2016; 116(24):241102-1-241102-19
Statement of Responsibility
B. 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)
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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}^{+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.
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Dissertation Note
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Published 14 June 2016
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This 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.