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 +8.4 −6.0 M⊙ and 19.4 + 5.3 −5.9 M⊙ (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, χ_eff = −0.12 +0.21 −0.30. 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 +450 −390 Mpc corresponding to a redshift of z = 0.18 +0.08 −0.07. 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 m_g ≤ 7.7 ×10−23 eV/c^2. In all cases, we find that GW170104 is consistent with general relativity.

GW170104: Observation of a 50-Solar-Mass Binary Black Hole Coalescence at Redshift 0.2

BRANCHESI, MARICA;CERBONI BAIARDI, LORENZO;GRECO, GIUSEPPE;GUIDI, GIANLUCA MARIA;HARMS, JAN;MARTELLI, FILIPPO;MONTANI, MATTEO;PIERGIOVANNI, FRANCESCO;STRATTA, MARIA GIULIANA;VETRANO, FLAVIO;VICERE', ANDREA;
2017-01-01

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 +8.4 −6.0 M⊙ and 19.4 + 5.3 −5.9 M⊙ (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, χ_eff = −0.12 +0.21 −0.30. 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 +450 −390 Mpc corresponding to a redshift of z = 0.18 +0.08 −0.07. 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 m_g ≤ 7.7 ×10−23 eV/c^2. In all cases, we find that GW170104 is consistent with general relativity.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11576/2646301
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