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Preprint

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 \(1.0 \times
10^{-21}\). 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 \(36^{+5}_{-4} M_\odot\) and \(29^{+4}_{-4}
M_\odot\), and the final black hole mass is \(62^{+4}_{-4} M_\odot\), with
\(3.0^{+0.5}_{-0.5} M_\odot c^2\) 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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Roy Kerr (1963)

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P Marronetti, M. Campanelli, C. O. Lousto … (2005)

http://creativecommons.org/licenses/by/4.0/