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 sigma. 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)(+8.3) M-circle dot and 7.5(-2.3)(+2.3) M-circle dot, and the final black hole mass is 20.8(-1.7)(+6.1) M-circle dot. 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(-190)(+180) Mpc corresponding to a redshift of 0.09(-0.04)(+0.03). All uncertainties define a 90% credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.

Abbott, B., Abbott, R., Abbott, T., Abernathy, M., Acernese, F., Ackley, K., et al. (2016). GW151226: observation of gravitational waves from a 22-solar-mass binary black hole coalescence. PHYSICAL REVIEW LETTERS, 116(24) [10.1103/PhysRevLett.116.241103].

GW151226: observation of gravitational waves from a 22-solar-mass binary black hole coalescence

FAFONE, VIVIANA;Lorenzini, M;
2016-01-01

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 sigma. 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)(+8.3) M-circle dot and 7.5(-2.3)(+2.3) M-circle dot, and the final black hole mass is 20.8(-1.7)(+6.1) M-circle dot. 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(-190)(+180) Mpc corresponding to a redshift of 0.09(-0.04)(+0.03). All uncertainties define a 90% credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.
2016
Pubblicato
Rilevanza internazionale
Articolo
Esperti anonimi
Settore FIS/01 - FISICA SPERIMENTALE
English
Abbott, B., Abbott, R., Abbott, T., Abernathy, M., Acernese, F., Ackley, K., et al. (2016). GW151226: observation of gravitational waves from a 22-solar-mass binary black hole coalescence. PHYSICAL REVIEW LETTERS, 116(24) [10.1103/PhysRevLett.116.241103].
Abbott, B; Abbott, R; Abbott, T; Abernathy, M; Acernese, F; Ackley, K; Adams, C; Adams, T; Addesso, P; Adhikari, R; Adya, V; Affeldt, C; Agathos, M; A...espandi
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2108/176633
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