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      Gravitational Waves from Mergin Compact Binaries: How Accurately Can One Extract the Binary's Parameters from the Inspiral Waveform?

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          Abstract

          The most promising source of gravitational waves for the planned detectors LIGO and VIRGO are merging compact binaries, i.e., neutron star/neutron star (NS/NS), neutron star/black hole (NS/BH), and black hole/black-hole (BH/BH) binaries. We investigate how accurately the distance to the source and the masses and spins of the two bodies will be measured from the gravitational wave signals by the three detector LIGO/VIRGO network using ``advanced detectors'' (those present a few years after initial operation). The combination \({\cal M} \equiv (M_1 M_2)^{3/5}(M_1 +M_2)^{-1/5}\) of the masses of the two bodies is measurable with an accuracy \(\approx 0.1\%-1\%\). The reduced mass is measurable to \(\sim 10\%-15\%\) for NS/NS and NS/BH binaries, and \(\sim 50\%\) for BH/BH binaries (assuming \(10M_\odot\) BH's). Measurements of the masses and spins are strongly correlated; there is a combination of \(\mu\) and the spin angular momenta that is measured to within \(\sim 1\%\). We also estimate that distance measurement accuracies will be \(\le 15\%\) for \(\sim 8\%\) of the detected signals, and \(\le 30\%\) for \(\sim 60\%\) of the signals, for the LIGO/VIRGO 3-detector network.

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          Most cited references29

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          The rate of neutron star binary mergers in the universe - Minimal predictions for gravity wave detectors

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            Tidal interactions of inspiraling compact binaries

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              The VIRGO Project: A wide band antenna for gravitational wave detection

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                Author and article information

                Journal
                04 February 1994
                Article
                10.1103/PhysRevD.49.2658
                gr-qc/9402014
                d994837a-9914-48ea-96cb-bfbf19c05bac
                History
                Custom metadata
                Phys.Rev.D49:2658-2697,1994
                103 pages, 20 figures, submitted to Phys Rev D, uses revtex macros, Caltech preprint GRP-369
                gr-qc astro-ph

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