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

Date

2017

Authors

Abbott, B P
Abbott, R
Abbott, T D
Acernese, F
Ackley, K
Adams, C
Adams, T
Addesso, T
Adhikari, Rana X
Affeldt, C

Journal Title

Journal ISSN

Volume Title

Publisher

American Physical Society

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 31.2-6.0+8.4M' and 19.4-5.9+5.3M (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=-0.12-0.30+0.21. This result implies that spin configurations with both component spins positively aligned with the orbital angular momentum are disfavored. The source luminosity distance is 880-390+450 Mpc corresponding to a redshift of z=0.18-0.07+0.08. 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 mg≤7.7×10-23 eV/c2. In all cases, we find that GW170104 is consistent with general relativity. Assuming that gravitons are dispersed in vacuum like massive particles, we bound the graviton mass to mg≤7.7×10-23 eV/c2. In all cases, we find that GW170104 is consistent with general relativity. © 2017 American Physical Society.

Description

Keywords

Gravitation, Cosmology, Astrophysics

Citation

Source

Physical Review Letters

Type

Journal article

Book Title

Entity type

Access Statement

Open Access

License Rights

DOI

10.1103/PhysRevLett.118.221101

Restricted until