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

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<SUB>-6.0</SUB><SUP>+8.4</SUP>M<SUB>☉</SUB> and 19. 4<SUB>-5.9</SUB><SUP>+5.3</SUP> M<SUB>☉</SUB> (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<SUB>eff</SUB>=-0.1 2<SUB>-0.30</SUB><SUP>+0.21</SUP> . This result implies that spin configurations with both component spins positively aligned with the orbital angular momentum are disfavored. The source luminosity distance is 88 0<SUB>-390</SUB><SUP>+450</SUP> Mpc corresponding to a redshift of z =0.1 8<SUB>-0.07</SUB><SUP>+0.08</SUP> . 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<SUB>g</SUB>≤7.7 ×10<SUP>-23</SUP> eV /c<SUP>2</SUP> . In all cases, we find that GW170104 is consistent with general relativity.