Properties of the binary black hole merger GW150914

Document #:

LIGO-P1500218-v14

Document type:

P - Publications

Abstract:

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 36(+5/−4) and 29(+4/−4) solar masses; 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 610 square degrees, primarily in the southern hemisphere. The binary merges into a black hole of 62(+4/−4) solar masses and spin 0.67(+0.05/−0.07). This black hole is significantly more massive than any other inferred from electromagnetic observations in the stellar-mass regime.

Files in Document:

• PhysRevLett.116.241102.pdf (1.2 MB)

Topics:

• Data Analysis
• Compact Binaries

Author Groups:

• LVC

Keywords:

GW150914 BBH parameter estimation

Notes and Changes:

published version

Related Documents:

• LIGO-P1500213: Tests of general relativity with GW150914
• LIGO-P1500217: The Rate of Binary Black Hole Mergers Inferred from Advanced LIGO Observations Surrounding GW150914
• LIGO-P1500262: Astrophysical Implications of the Binary Black-Hole Merger GW150914

Referenced by:

• LIGO-P150914-v14: Observation of Gravitational Waves from a Binary Black Hole Merger
• LIGO-T1600018-v4: Phenomenological fit of the peak luminosity from non-precessing binary-black-hole coalescences

Journal References:

Published in Phys Rev Letters vol. 116 pg. 241102.

Publication Information:

http://dx.doi.org/10.1103/PhysRevLett.116.241102