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# SEARCHING THE GAMMA-RAY SKY FOR COUNTERPARTS TO GRAVITATIONAL WAVE SOURCES:FERMIGAMMA-RAY BURST MONITORAND LARGE AREA TELESCOPE OBSERVATIONS OF LVT151012 AND GW151226

The Astrophysical Journal

American Astronomical Society

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### Most cited references51

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### Observation of Gravitational Waves from a Binary Black Hole Merger

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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### Nucleosynthesis, neutrino bursts and γ-rays from coalescing neutron stars

(1989)
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### GW151226: Observation of Gravitational Waves from a 22-Solar-Mass Binary Black Hole Coalescence

We report the observation of a gravitational-wave signal produced by the coalescence of two stellar-mass black holes. The signal, GW151226, was observed by the twin detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO) on December 26, 2015 at 03:38:53 UTC. The signal was initially identified within 70 s by an online matched-filter search targeting binary coalescences. Subsequent off-line analyses recovered GW151226 with a network signal-to-noise ratio of 13 and a significance greater than 5 $$\sigma$$. The signal persisted in the LIGO frequency band for approximately 1 s, increasing in frequency and amplitude over about 55 cycles from 35 to 450 Hz, and reached a peak gravitational strain of $$3.4_{-0.9}^{+0.7} \times 10^{-22}$$. The inferred source-frame initial black hole masses are $$14.2_{-3.7}^{+8.3} M_{\odot}$$ and $$7.5_{-2.3}^{+2.3} M_{\odot}$$ and the final black hole mass is $$20.8_{-1.7}^{+6.1} M_{\odot}$$. We find that at least one of the component black holes has spin greater than 0.2. This source is located at a luminosity distance of $$440_{-190}^{+180}$$ Mpc corresponding to a redshift $$0.09_{-0.04}^{+0.03}$$. All uncertainties define a 90 % credible interval. This second gravitational-wave observation provides improved constraints on stellar populations and on deviations from general relativity.
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### Author and article information

###### Journal
The Astrophysical Journal
ApJ
American Astronomical Society
1538-4357
January 20 2017
January 19 2017
: 835
: 1
: 82
###### Affiliations
[1 ]Fermi LAT Collaboration
###### Article
10.3847/1538-4357/835/1/82