Binary black hole detection rates in inspiral gravitational wave searches

Abstract

The signal-to-noise ratios (SNRs) for quasi-circular binary black hole inspirals computed from restricted post-Newtonian waveforms are compared with those attained by more complete post-Newtonian signals, which are superpositions of amplitude-corrected harmonics of the orbital phase. It is shown that if one were to use the best available amplitude-corrected waveforms for detection templates, one should expect SNRs in actual searches to be significantly lower than those suggested by simulations based purely on restricted waveforms.

9 pages, 1 figure

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• Using Full Information When Computing Modes of Post-Newtonian Waveforms From Inspiralling Compact Binaries in Circular Orbit
• Higher signal harmonics, LISA's angular resolution, and dark energy
• Matched Filtering of Numerical Relativity Templates of Spinning Binary Black Holes
• Black-hole binary simulations: the mass ratio 10:1
• Binary black hole spectroscopy
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• Bounding the mass of the graviton with gravitational waves: Effect of higher harmonics in gravitational waveform templates
• Higher harmonics increase LISA's mass reach for supermassive black holes
• Comparison of post-Newtonian mode amplitudes with numerical relativity simulations of binary black holes
• Interpreting the results of searches for gravitational waves from coalescing binaries
• Parameter estimation of coalescing supermassive black hole binaries with LISA
• Parameter estimation of neutron star-black hole binaries using an advanced gravitational-wave detector network: Effects of the full post-Newtonian waveform
• Parametrized multipolar gravitational waveforms for testing general relativity: Amplitude corrections up to 2PN order