%0 Generic %1 collaboration2016observation %A Collaboration, The LIGO Scientific %A the Virgo Collaboration, %D 2016 %K detection gravitational waves %R 10.1103/PhysRevLett.116.061102 %T Observation of Gravitational Waves from a Binary Black Hole Merger %U http://arxiv.org/abs/1602.03837 %X 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 $36^+5_-4 M_ødot$ and $29^+4_-4 M_ødot$, and the final black hole mass is $62^+4_-4 M_ødot$, with $3.0^+0.5_-0.5 M_c^2$ 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.

@misc{collaboration2016observation, abstract = {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.}, added-at = {2016-02-12T10:26:31.000+0100}, author = {Collaboration, The LIGO Scientific and the Virgo Collaboration}, biburl = {https://www.bibsonomy.org/bibtex/21eace313ad2687f446042445a43c17b2/miki}, description = {[1602.03837] Observation of Gravitational Waves from a Binary Black Hole Merger}, doi = {10.1103/PhysRevLett.116.061102}, interhash = {3e924702e42df4b7b0b1d00501b98a04}, intrahash = {1eace313ad2687f446042445a43c17b2}, keywords = {detection gravitational waves}, note = {cite arxiv:1602.03837Comment: 16 pages, 4 figures}, timestamp = {2016-02-12T10:26:31.000+0100}, title = {Observation of Gravitational Waves from a Binary Black Hole Merger}, url = {http://arxiv.org/abs/1602.03837}, year = 2016 }