Papers › Observation of Gravitational Waves from a Binary Black Hole Merger
Observation of Gravitational Waves from a Binary Black Hole Merger
The LIGO Scientific Collaboration, the Virgo Collaboration
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On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0 ×10⁻²¹. It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203 000 years, equivalent to a significance greater than 5.1 {\sigma}. The source lies at a luminosity distance of 410⁺¹⁶⁰₋₁₈₀ Mpc corresponding to a redshift z = 0.09^(+0.03)_(-0.04). In the source frame, the initial black hole masses are 36⁺⁵₋₄ M_⊙ and 29⁺⁴₋₄ M_⊙, and the final black hole mass is 62⁺⁴₋₄ M_⊙, with 3.0^(+0.5)_(-0.5) M_⊙ c² radiated in gravitational waves. All uncertainties define 90% credible intervals.These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.
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