Comparing Effective-One-Body gravitational waveforms to accurate numerical data

Details Comparing Effective-One-Body gravitational waveforms to accurate numerical data Comparing Effective-One-Body gravitational waveforms to accurate numerical data

2007-11-16

arxiv.org/abs/0711.2628v2

Phys.Rev.D77:024043,2008

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

15 pages, 7 figures, submitted to Phys. Rev. D. Revised version. Figs. 2-7 improved. Slight changes in a few numbers. One refe

Scientific paper

10.1103/PhysRevD.77.024043

We continue the program of constructing, within the Effective-One-Body (EOB) approach, high accuracy, faithful analytic waveforms describing the gravitational wave signal emitted by inspiralling and coalescing binary black holes (BHs). We present the comparable-mass version of a new, resummed 3PN-accurate EOB quadrupolar waveform recently introduced in the small-mass-ratio limit. We compare the phase and the amplitude of this waveform to the recently published results of a high-accuracy numerical relativity (NR) simulation of 15 orbits of an inspiralling equal-mass binary BHs system performed by the Caltech-Cornell group. We find a remarkable agreement, both in phase and in amplitude, between the new EOB waveform and the published numerical data. More precisely: (i) in the gravitational wave (GW) frequency domain $M\omega <0.08$ where the phase of one of the non-resummed ``Taylor approximant'' (T4) waveform matches well with the numerical relativity one, we find that the EOB phase fares as well, while (ii) for higher GW frequencies, $0.08

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