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Properties of the binary black hole merger GW150914

Dooley, Katherine, Fairhurst, Stephen, Grote, Hartmut, Hannam, Mark, Hopkins, Paul, Ohme, Frank, Pannarale Greco, Francesco, Predoi, Valeriu, Sathyaprakash, Bangalore, Schutz, Bernard, Sutton, Patrick, Tiwari, Vaibhav, LIGO Scientific Collaboration, and Virgo Collaboration, 2016. Properties of the binary black hole merger GW150914. Physical Review Letters 116 , 241102. 10.1103/PhysRevLett.116.241102

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Abstract

On September 14, 2015, the Laser Interferometer Gravitational-wave Observatory (LIGO) detected a gravitational-wave transient (GW150914); we characterise the properties of the source and its parameters. The data around the time of the event were analysed 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 36+5−4M⊙ 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+160−180 Mpc, corresponding to a redshift 0.09+0.03−0.04 assuming standard cosmology. The source location is constrained to an annulus section of 590 deg2, primarily in the southern hemisphere. The binary merges into a black hole of 62+4−4M⊙ and spin 0.67+0.05−0.07. This black hole is significantly more massive than any other known in the stellar-mass regime.

Item Type: Article
Date Type: Publication
Status: Published
Schools: Physics and Astronomy
Subjects: Q Science > QB Astronomy
Publisher: American Physical Society
ISSN: 0031-9007
Related URLs:
Date of First Compliant Deposit: 30 June 2016
Date of Acceptance: 19 April 2016
Last Modified: 12 Jun 2019 02:48
URI: http://orca.cf.ac.uk/id/eprint/89619

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