Properties of the Binary Black Hole Merger GW150914

(LIGO Scientific Collaboration and Virgo Collaboration)

doi:10.1103/PhysRevLett.116.241102

Properties of the Binary Black Hole Merger GW150914

(LIGO Scientific Collaboration and Virgo Collaboration)

Research output: Contribution to journal › Article › peer-review

852 Scopus citations

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.

Original language	English
Article number	241102
Journal	Physical Review Letters
Volume	116
Issue number	24
DOIs	https://doi.org/10.1103/PhysRevLett.116.241102
State	Published - 14 Jun 2016
Externally published	Yes

Bibliographical note

Publisher Copyright:
© 2016 authors. Published by the American Physical Society.

Funding

Funders	Funder number
???publication-publication-funding-organisation-not-added???	ST/I006285/1, ST/N000064/1, ST/N005430/1
National Science Foundation	0955825, 1104371, 1404395, 1429873, 1207010, 1306702, 1333129, 1505629, 1505308, 1505824, 1205512, 1550461, 1506497, 1305730, 1506254, 1306125, 1404139, 1125897, 1242090, 1307429, 1205882, 1516150, 1505779, 1307020, 1450006, 1541396, 1307401, 1307489, 1404569, 1506360, 1028087
Horizon 2020 Framework Programme	647839
Science and Technology Facilities Council	ST/N005716/1, PPA/G/S/2002/00652, ST/K005014/1, ST/M004090/1, ST/N00003X/1, ST/N005406/1, ST/J000019/1, Gravitational Waves, ST/K000845/1, ST/H002006/1, ST/L000954/1, ST/L003465/1, ST/I006242/1, ST/I006269/1, ST/N000080/1, ST/L000946/1, ST/N000633/1, ST/N000072/1, ST/J00166X/1

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10.1103/PhysRevLett.116.241102

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@article{44a615ce33e14137b4d4e6227ba86498,

title = "Properties of the Binary Black Hole Merger GW150914",

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.",

author = "\{(LIGO Scientific Collaboration and Virgo Collaboration)\} and Abbott, \{B. P.\} and R. Abbott and Abbott, \{T. D.\} and Abernathy, \{M. R.\} and F. Acernese and K. Ackley and C. Adams and T. Adams and P. Addesso and Adhikari, \{R. X.\} and Adya, \{V. B.\} and C. Affeldt and M. Agathos and K. Agatsuma and N. Aggarwal and Aguiar, \{O. D.\} and L. Aiello and A. Ain and P. Ajith and B. Allen and A. Allocca and Altin, \{P. A.\} and Anderson, \{S. B.\} and Anderson, \{W. G.\} and K. Arai and Araya, \{M. C.\} and Arceneaux, \{C. C.\} and Areeda, \{J. S.\} and N. Arnaud and Arun, \{K. G.\} and S. Ascenzi and G. Ashton and M. Ast and Aston, \{S. M.\} and P. Astone and P. Aufmuth and C. Aulbert and S. Babak and P. Bacon and Bader, \{M. K.M.\} and Baker, \{P. T.\} and F. Baldaccini and G. Ballardin and Ballmer, \{S. W.\} and Barayoga, \{J. C.\} and Barclay, \{S. E.\} and Barish, \{B. C.\} and D. Barker and O. Birnholtz and H. Dereli",

note = "Publisher Copyright: {\textcopyright} 2016 authors. Published by the American Physical Society.",

year = "2016",

month = jun,

day = "14",

doi = "10.1103/PhysRevLett.116.241102",

language = "אנגלית",

volume = "116",

journal = "Physical Review Letters",

issn = "0031-9007",

publisher = "American Physical Society",

number = "24",

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TY - JOUR

T1 - Properties of the Binary Black Hole Merger GW150914

AU - (LIGO Scientific Collaboration and Virgo Collaboration)

AU - Abbott, B. P.

AU - Abbott, R.

AU - Abbott, T. D.

AU - Abernathy, M. R.

AU - Acernese, F.

AU - Ackley, K.

AU - Adams, C.

AU - Adams, T.

AU - Addesso, P.

AU - Adhikari, R. X.

AU - Adya, V. B.

AU - Affeldt, C.

AU - Agathos, M.

AU - Agatsuma, K.

AU - Aggarwal, N.

AU - Aguiar, O. D.

AU - Aiello, L.

AU - Ain, A.

AU - Ajith, P.

AU - Allen, B.

AU - Allocca, A.

AU - Altin, P. A.

AU - Anderson, S. B.

AU - Anderson, W. G.

AU - Arai, K.

AU - Araya, M. C.

AU - Arceneaux, C. C.

AU - Areeda, J. S.

AU - Arnaud, N.

AU - Arun, K. G.

AU - Ascenzi, S.

AU - Ashton, G.

AU - Ast, M.

AU - Aston, S. M.

AU - Astone, P.

AU - Aufmuth, P.

AU - Aulbert, C.

AU - Babak, S.

AU - Bacon, P.

AU - Bader, M. K.M.

AU - Baker, P. T.

AU - Baldaccini, F.

AU - Ballardin, G.

AU - Ballmer, S. W.

AU - Barayoga, J. C.

AU - Barclay, S. E.

AU - Barish, B. C.

AU - Barker, D.

AU - Birnholtz, O.

AU - Dereli, H.

PY - 2016/6/14

Y1 - 2016/6/14

N2 - 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.

AB - 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.

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U2 - 10.1103/PhysRevLett.116.241102

DO - 10.1103/PhysRevLett.116.241102

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C2 - 27367378

AN - SCOPUS:84975451312

SN - 0031-9007

VL - 116

JO - Physical Review Letters

JF - Physical Review Letters

IS - 24

M1 - 241102

ER -

Properties of the Binary Black Hole Merger GW150914

Abstract

Bibliographical note

Funding

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