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Papers

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

https://doi.org/10.1103/PhysRevLett.118.221101

  • Research Fields산업수학기반연구부
  • AuthorB.?P. Abbott et al.(J.J.Oh, S.H.Oh, E.J.Son, W.S.Kim)
  • JournalPhysical Review Letters 118 (2017
  • Link https://doi.org/10.1103/PhysRevLett.118.221101
  • Classification of papersSCI

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+8.46.0M and 19.4+5.35.9M (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, χeff=0.12+0.210.30. 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+450390Mpc corresponding to a redshift of z=0.18+0.080.07. 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 mg7.7×1023eV/c2. In all cases, we find that GW170104 is consistent with general relativity.

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+8.46.0M and 19.4+5.35.9M (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, χeff=0.12+0.210.30. 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+450390Mpc corresponding to a redshift of z=0.18+0.080.07. 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 mg7.7×1023eV/c2. In all cases, we find that GW170104 is consistent with general relativity.