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We continue the program of constructing, within the Effective-One-Body (EOB)approach, high accuracy, faithful analytic waveforms describing thegravitational wave signal emitted by inspiralling and coalescing binary blackholes (BHs). We present the comparable-mass version of a new, resummed3PN-accurate EOB quadrupolar waveform recently introduced in thesmall-mass-ratio limit. We compare the phase and the amplitude of this waveformto the recently published results of a high-accuracy numerical relativity (NR)simulation of 15 orbits of an inspiralling equal-mass binary BHs systemperformed by the Caltech-Cornell group. We find a remarkable agreement, both inphase and in amplitude, between the new EOB waveform and the publishednumerical data. More precisely: (i) in the gravitational wave (GW) frequencydomain $M\omega <0.08$ where the phase of one of the non-resummed ``Taylorapproximant'' (T4) waveform matches well with the numerical relativity one, wefind that the EOB phase fares as well, while (ii) for higher GW frequencies,$0.08<M\omega\lesssim 0.14$, where the TaylorT4 approximant starts tosignificantly diverge from the NR phase, we show that the EOB phase continuesto match well the NR one. We further propose various methods of tuning the twoinspiral flexibility parameters, $a_5$ and $v_{\rm pole}$, of the EOB waveformso as to ``best fit'' EOB predictions to numerical data. We find that themaximal dephasing between EOB and NR can then be reduced below $10^{-3}$ GWcycles over the entire span (30 GW cycles) of the simulation. Our resummed EOBamplitude agrees much better with the NR one than any of the previouslyconsidered non-resummed, post-Newtonian one.

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