GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence - IN2P3 - Institut national de physique nucléaire et de physique des particules
Article Dans Une Revue Physical Review Letters Année : 2016

GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence

B.P. Abbott
  • Fonction : Auteur
M. Was
J. Degallaix
N. Arnaud
J. Casanueva Diaz
  • Fonction : Auteur
N. Leroy
François Bondu

Résumé

We report the observation of a gravitational-wave signal produced by the coalescence of two stellar-mass black holes. The signal, GW151226, was observed by the twin detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO) on December 26, 2015 at 03:38:53 UTC. The signal was initially identified within 70 s by an online matched-filter search targeting binary coalescences. Subsequent off-line analyses recovered GW151226 with a network signal-to-noise ratio of 13 and a significance greater than 5 σ. The signal persisted in the LIGO frequency band for approximately 1 s, increasing in frequency and amplitude over about 55 cycles from 35 to 450 Hz, and reached a peak gravitational strain of 3.4+0.7−0.9×10−22. The inferred source-frame initial black hole masses are 14.2+8.3−3.7M⊙ and 7.5+2.3−2.3M⊙ and the final black hole mass is 20.8+6.1−1.7M⊙. We find that at least one of the component black holes has spin greater than 0.2. This source is located at a luminosity distance of 440+180−190 Mpc corresponding to a redshift 0.09+0.03−0.04. All uncertainties define a 90 % credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.
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Dates et versions

in2p3-01332514 , version 1 (10-01-2024)

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B.P. Abbott, T. Adams, R. Bonnand, D. Buskulic, M. Ducrot, et al.. GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence. Physical Review Letters, 2016, 116 (24), pp.241103. ⟨10.1103/PhysRevLett.116.241103⟩. ⟨in2p3-01332514⟩
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