dc.identifier.uri |
http://dx.doi.org/10.15488/2101 |
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dc.identifier.uri |
http://www.repo.uni-hannover.de/handle/123456789/2126 |
|
dc.contributor.author |
Abbott, B.P.
|
|
dc.contributor.author |
Abbott, R.
|
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dc.contributor.author |
Abbott, T.D.
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|
dc.contributor.author |
Acernese, F.
|
|
dc.contributor.author |
Ackley, K.
|
|
dc.contributor.author |
et al.
|
|
dc.contributor.author |
LIGO Scientific Collaboration
|
|
dc.contributor.author |
Virgo Collaboration
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dc.date.accessioned |
2017-10-24T08:01:11Z |
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dc.date.available |
2017-10-24T08:01:11Z |
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dc.date.issued |
2017 |
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dc.identifier.citation |
Abbott, B.P.; Abbott, R.; Abbott, T.D.; Acernese, F.; Ackley, K.; et, al. (LIGO Scientific Collaboration and Virgo Collaboration): GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2. In: Physical Review Letters 118 (2017), Nr. 22, 221101. DOI: https://doi.org/10.1103/PhysRevLett.118.221101 |
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dc.description.abstract |
We describe the observation of GW170104, a gravitational-wave signal produced by the coalescence of a pair of stellar-mass black holes. The signal was measured on January 4, 2017 at 10 11:58.6 UTC by the twin advanced detectors of the Laser Interferometer Gravitational-Wave Observatory during their second observing run, with a network signal-to-noise ratio of 13 and a false alarm rate less than 1 in 70 000 years. The inferred component black hole masses are 31.2-6.0+8.4M' and 19.4-5.9+5.3M (at the 90% credible level). The black hole spins are best constrained through measurement of the effective inspiral spin parameter, a mass-weighted combination of the spin components perpendicular to the orbital plane, χeff=-0.12-0.30+0.21. This result implies that spin configurations with both component spins positively aligned with the orbital angular momentum are disfavored. The source luminosity distance is 880-390+450 Mpc corresponding to a redshift of z=0.18-0.07+0.08. We constrain the magnitude of modifications to the gravitational-wave dispersion relation and perform null tests of general relativity. Assuming that gravitons are dispersed in vacuum like massive particles, we bound the graviton mass to mg≤7.7×10-23 eV/c2. In all cases, we find that GW170104 is consistent with general relativity. © 2017 American Physical Society. |
eng |
dc.language.iso |
eng |
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dc.publisher |
College Park, MD : American Physical Society |
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dc.relation.ispartofseries |
Physical Review Letters 118 (2017), Nr. 22 |
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dc.rights |
CC BY 4.0 Unported |
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dc.rights.uri |
https://creativecommons.org/licenses/by/4.0/ |
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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 |
Signal to noise ratio |
eng |
dc.subject |
Stars |
eng |
dc.subject |
Testing |
eng |
dc.subject |
Advanced detector |
eng |
dc.subject |
General Relativity |
eng |
dc.subject |
Gravitational-wave signals |
eng |
dc.subject |
Laser interferometer gravitational-wave observatories |
eng |
dc.subject |
Massive particles |
eng |
dc.subject |
Orbital angular momentum |
eng |
dc.subject |
Spin configurations |
eng |
dc.subject |
Stellar-mass black holes |
eng |
dc.subject |
Gravitation |
eng |
dc.subject |
Gravitationswelle |
ger |
dc.subject.ddc |
530 | Physik
|
ger |
dc.title |
GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2 |
|
dc.type |
Article |
|
dc.type |
Text |
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dc.relation.issn |
0031-9007 |
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dc.relation.doi |
https://doi.org/10.1103/PhysRevLett.118.221101 |
|
dc.bibliographicCitation.issue |
22 |
|
dc.bibliographicCitation.volume |
118 |
|
dc.bibliographicCitation.firstPage |
221101 |
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dc.description.version |
publishedVersion |
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tib.accessRights |
frei zug�nglich |
|