Properties of the Binary Black Hole Merger GW150914

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 su...

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Vydáno v:Physical review letters Ročník 116; číslo 24; s. 241102
Hlavní autoři: Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Camp, J. B.
Médium: Journal Article
Jazyk:angličtina
Vydáno: Goddard Space Flight Center APS Physics 17.06.2016
American Physical Society
Témata:
Astrophysics
Cosmology
Engineering, computing & technology
General Relativity and Quantum Cosmology
Gravitational waves
High Energy Astrophysical Phenomena
Ingénierie mécanique
Ingénierie, informatique & technologie
Interferometers
Lasers
Mathematical models
Mechanical engineering
Physics
Texts
Waveforms
ISSN:0031-9007, 1079-7114, 1079-7114
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Popis
Shrnutí: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(+5/-4) solar mass and 29(+4/-4) solar mass; 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 less than 0.7 (at 90% probability). The luminosity distance to the source is 410(+160/-180) Mpc, corresponding to a redshift 0.09(+0.03/−0.04) assuming standard cosmology. The source location is constrained to an annulus section of 610 sq deg, primarily in the southern hemisphere. The binary merges into a black hole of mass 62(+4/−4) solar mass and spin 0.67(+0.05/−0.07). This black hole is significantly more massive than any other inferred from electromagnetic observations in the stellar-mass regime.
Bibliografie:ISSN: 0031-9007
Report Number: GSFC-E-DAA-TN41674
GSFC-E-DAA-TN41674
E-ISSN: 1079-7114
GSFC
Report Number: GSFC-E-DAA-TN41647
Goddard Space Flight Center
GSFC-E-DAA-TN41647
ObjectType-Article-1
SourceType-Scholarly Journals-1
ObjectType-Feature-2
content type line 23
scopus-id:2-s2.0-84975451312
ISSN:0031-9007
1079-7114
1079-7114
DOI:10.1103/PhysRevLett.116.241102