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We calibrate the effective-one-body (EOB) model to an accurate numericalsimulation of an equal-mass, non-spinning binary black-hole coalescenceproduced by the Caltech-Cornell collaboration. Aligning the EOB and numericalwaveforms at low frequency over a time interval of ~1000M, and taking intoaccount the uncertainties in the numerical simulation, we investigate thesignificance and degeneracy of the EOB adjustable parameters during inspiral,plunge and merger, and determine the minimum number of EOB adjustableparameters that achieves phase and amplitude agreements on the order of thenumerical error. We find that phase and fractional amplitude differencesbetween the numerical and EOB values of the dominant gravitational wave modeh_{22} can be reduced to 0.02 radians and 2%, respectively, until a time 26 Mbefore merger, and to 0.1 radians and 10%, at a time 16M after merger (duringringdown), respectively. Using LIGO, Enhanced LIGO and Advanced LIGO noisecurves, we find that the overlap between the EOB and the numerical h_{22},maximized only over the initial phase and time of arrival, is larger than 0.999for equal-mass binary black holes with total mass 30-150 Msun. In addition tothe leading gravitational mode (2,2), we compare the dominant subleading modes(4,4) and (3,2) and find phase and amplitude differences on the order of thenumerical error. We also determine the mass-ratio dependence of one of the EOBadjustable parameters by fitting to numerical {\it inspiral} waveforms forblack-hole binaries with mass ratios 2:1 and 3:1. These results improve andextend recent successful attempts aimed at providing gravitational-wave dataanalysts the best analytical EOB model capable of interpolating accuratenumerical simulations.

Effective-one-body waveforms calibrated to numerical relativity simulations: coalescence of non-spinning, equal-mass black holes