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 5σ. 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 3.4-0.9+0.7 x 10-22. The inferred source-frame initial black hole masses are 14.2-3.7+8.3M⊙ and 7.5+2.3-2.3M⊙, and the final black hole mass is 20.8z+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 of 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.
B. P. Abbott et al., "GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence," Physical Review Letters, vol. 116, no. 24, American Physical Society (APS), Jun 2016.
The definitive version is available at https://doi.org/10.1103/PhysRevLett.116.241103
Keywords and Phrases
Bins; Frequency bands; Gravitational effects; Gravity waves; Interferometers; Laser interferometry; Matched filters; Relativity; Signal to noise ratio; Stars; Black hole mass; Credible interval; General Relativity; Gravitational-wave signals; Laser interferometer gravitational-wave observatories; Off-line analysis; Stellar populations; Stellar-mass black holes; Gravitation
International Standard Serial Number (ISSN)
Article - Journal
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