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      Estimating parameters of binary black holes from gravitational-wave observations of their inspiral, merger and ringdown

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          Abstract

          We characterize the expected statistical errors with which the parameters of black-hole binaries can be measured from gravitational-wave (GW) observations of their inspiral, merger and ringdown by a network of second-generation ground-based GW observatories. We simulate a population of black-hole binaries with uniform distribution of component masses in the interval \((3,80)~M_\odot\), distributed uniformly in comoving volume, with isotropic orientations. From signals producing signal-to-noise ratio \(\geq 5\) in at least two detectors, we estimate the posterior distributions of the binary parameters using the Bayesian parameter estimation code LALInference. The GW signals will be redshifted due to the cosmological expansion and we measure only the "redshifted" masses. By assuming a cosmology, it is possible to estimate the gravitational masses by inferring the redshift from the measured posterior of the luminosity distance. We find that the measurement of the gravitational masses will be in general dominated by the error in measuring the luminosity distance. In spite of this, the component masses of more than \(50\%\) of the population can be measured with accuracy better than \(\sim 25\%\) using the Advanced LIGO-Virgo network. Additionally, the mass of the final black hole can be measured with median accuracy \(\sim 18\%\). Spin of the final black hole can be measured with median accuracy \(\sim 5\% ~(17\%)\) for binaries with non-spinning (aligned-spin) black holes. Additional detectors in Japan and India significantly improve the accuracy of sky localization, and moderately improve the estimation of luminosity distance, and hence, that of all mass parameters. We discuss the implication of these results on the observational evidence of intermediate-mass black holes and the estimation of cosmological parameters using GW observations.

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          Detector configuration of KAGRA - the Japanese cryogenic gravitational-wave detector

          Construction of the Japanese second-generation gravitational-wave detector KAGRA has been started. In the next 6 \sim 7 years, we will be able to observe the space-time ripple from faraway galaxies. KAGRA is equipped with the latest advanced technologies. The entire 3-km long detector is located in the underground to be isolated from the seismic motion, the core optics are cooled down to 20 K to reduce thermal fluctuations, and quantum non-demolition techniques are used to decrease quantum noise. In this paper, we introduce the detector configuration of KAGRA; its design, strategy, and downselection of parameters.
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