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 − 3.7 M ⊙ and 7. 5 + 2.3 − 2.3 M ⊙ , and the final black hole mass is 20.8 + 6.1 − 1.7 M ⊙ . 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 44 0 + 180 − 190     Mpc corresponding to a redshift of 0.0 9 + 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.

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

Branchesi M;Coccia E;Drago M;Harms J;
2016

Abstract

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 − 3.7 M ⊙ and 7. 5 + 2.3 − 2.3 M ⊙ , and the final black hole mass is 20.8 + 6.1 − 1.7 M ⊙ . 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 44 0 + 180 − 190     Mpc corresponding to a redshift of 0.0 9 + 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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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/20.500.12571/1295
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