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      Localization accuracy of compact binary coalescences detected by the third-generation gravitational-wave detectors and implication for cosmology

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      Physical Review D
      American Physical Society (APS)

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          Most cited references127

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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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            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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              Accelerating Universes with Scaling Dark Matter

              Friedmann-Robertson-Walker universes with a presently large fraction of the energy density stored in an \(X\)-component with \(w_X<-1/3\), are considered. We find all the critical points of the system for constant equations of state in that range. We consider further several background quantities that can distinguish the models with different \(w_X\) values. Using a simple toy model with a varying equation of state, we show that even a large variation of \(w_X\) at small redshifts is very difficult to observe with \(d_L(z)\) measurements up to \(z\sim 1\). Therefore, it will require accurate measurements in the range \(1
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                Author and article information

                Journal
                PRVDAQ
                Physical Review D
                Phys. Rev. D
                American Physical Society (APS)
                2470-0010
                2470-0029
                March 2018
                March 26 2018
                : 97
                : 6
                Article
                10.1103/PhysRevD.97.064031
                bf343ee1-6a8b-453d-9a8e-16365afe2172
                © 2018

                https://link.aps.org/licenses/aps-default-license

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