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A data-analysis driven comparison of analytic and numerical coalescing binary waveforms: nonspinning case

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Buonanno,  Alessandra
Department of Physics, University of Maryland;
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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0704.1964.pdf
(Preprint), 901KB

PhysRevD.77_024014.pdf
(Any fulltext), 876KB

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Citation

Pan, Y., Buonanno, A., Baker, J. G., Centrella, J., Kelly, B. J., McWilliams, S. T., et al. (2008). A data-analysis driven comparison of analytic and numerical coalescing binary waveforms: nonspinning case. Physical Review D, 77: 024014. doi:10.1103/PhysRevD.77.024014.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0018-D148-C
Abstract
We compare waveforms obtained by numerically evolving nonspinning binary black holes to post-Newtonian (PN) template families currently used in the search for gravitational waves by ground-based detectors. We find that the time-domain 3.5PN template family, which includes the inspiral phase, has fitting factors (FFs) >= 0.96 for binary systems with total mass M = 10 ~ 20 Msun. The time-domain 3.5PN effective-one-body template family, which includes the inspiral, merger and ring-down phases, gives satisfactory signal-matching performance with FFs >= 0.96 for binary systems with total mass M = 10 ~ 120 Msun. If we introduce a cutoff frequency properly adjusted to the final black-hole ring-down frequency, we find that the frequency-domain stationary-phase-approximated template family at 3.5PN order has FFs >= 0.96 for binary systems with total mass M = 10 ~ 20 Msun. However, to obtain high matching performances for larger binary masses, we need to either extend this family to unphysical regions of the parameter space or introduce a 4PN order coefficient in the frequency-domain GW phase. Finally, we find that the phenomenological Buonanno-Chen-Vallisneri family has FFs >= 0.97 with total mass M=10 ~ 120Msun. The main analyses use the noise spectral-density of LIGO, but several tests are extended to VIRGO and advanced LIGO noise-spectral densities.