Properties of the Binary Black Hole Merger GW150914

[en] On September 14, 2015, the Laser Interferometer Gravitational-Wave Observatory (LIGO) detected a gravitational-wave transient (GW150914); we characterize the properties of the source and its parameters. The data around the time of the event were analyzed coherently across the LIGO network using a suite of accurate waveform models that describe gravitational waves from a compact binary system in general relativity. GW150914 was produced by a nearly equal mass binary black hole of masses 36-4+5M and 29-4+4M; for each parameter we report the median value and the range of the 90 credible interval. The dimensionless spin magnitude of the more massive black hole is bound to be <0.7 (at 90 probability). The luminosity distance to the source is 410-180+160 Mpc, corresponding to a redshift 0.09-0.04+0.03 assuming standard cosmology. The source location is constrained to an annulus section of 610 deg2, primarily in the southern hemisphere. The binary merges into a black hole of mass 62-4+4M and spin 0.67-0.07+0.05. This black hole is significantly more massive than any other inferred from electromagnetic observations in the stellar-mass regime.

Disciplines :

Mechanical engineering

Author, co-author :

Abbott, B. P.

Collette, Christophe ; Université de Liège - ULiège > Département d'aérospatiale et mécanique > Active aerospace struct. and adv. mecha. systems

Fays, Maxime ; Cardiff University

Language :

English

Title :

Properties of the Binary Black Hole Merger GW150914

Publication date :

2016

Journal title :

Physical Review Letters

ISSN :

0031-9007

eISSN :

1079-7114

Publisher :

American Physical Society, Ridge, United States - New York

Volume :

116

Issue :

Peer reviewed :

Peer Reviewed verified by ORBi

Additional URL :

http://hdl.handle.net/2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/262502
https://dipot.ulb.ac.be/dspace/bitstream/2013/262502/3/PhysRevLett.116.241102.pdf

Commentary :

Language of publication: en DOI: 10.1103/PhysRevLett.116.241102

Available on ORBi :

since 19 October 2020

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