9 − 0.4 + 0.5 ms later at H1 for a visual comparison, the H1 data are also shown, shifted in time by this amount and inverted (to account for the detectors’ relative orientations). For visualization, all time series are filtered with a 35–350 Hz bandpass filter to suppress large fluctuations outside the detectors’ most sensitive frequency band, and band-reject filters to remove the strong instrumental spectral lines seen in the Fig. Times are shown relative to Septemat 09:50:45 UTC. The gravitational-wave event GW150914 observed by the LIGO Hanford (H1, left column panels) and Livingston (L1, right column panels) detectors. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger. These observations demonstrate the existence of binary stellar-mass black hole systems. All uncertainties define 90% credible intervals. 0 − 0.5 + 0.5 M ⊙ c 2 radiated in gravitational waves. In the source frame, the initial black hole masses are 3 6 − 4 + 5 M ⊙ and 2 9 − 4 + 4 M ⊙, and the final black hole mass is 6 2 − 4 + 4 M ⊙, with 3. The source lies at a luminosity distance of 41 0 − 180 + 160 Mpc corresponding to a redshift z = 0.0 9 − 0.04 + 0.03. 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 σ. 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 sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of 1.0 × 10 − 21. On Septemat 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal.
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