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We improve the effective-one-body (EOB) description of nonspinning coalescingblack hole binaries by incorporating several recent analytical advances,notably: (i) logarithmic contributions to the conservative dynamics; (ii)resummed horizon-absorption contribution to the orbital angular momentum loss;and (iii) a specific radial component of the radiation reaction force impliedby consistency with the azimuthal one. We then complete this analyticallyimproved EOB model by comparing it to accurate numerical relativity (NR)simulations performed by the Caltech-Cornell-CITA group for mass ratios$q=(1,2,3,4,6)$. In particular, the comparison to NR data allows us todetermine with high-accuracy ($\sim 10^{-4}$) the value of the main EOB radialpotential: $A(u;\,\nu)$, where $u=GM/(R c^2)$ is the inter-body gravitationalpotential and $\nu=q/(q+1)^2$ is the symmetric mass ratio. We introduce a newtechnique for extracting from NR data an intrinsic measure of the phaseevolution, ($Q_\omega(\omega)$ diagnostics). Aligning the NR-completed EOBquadrupolar waveform and the NR one at low frequencies, we find that they keepagreeing (in phase and amplitude) within the NR uncertainties throughout theevolution for all mass ratios considered. We also find good agreement forseveral subdominant multipoles without having to introduce and tune any extraparameters.

Improved effective-one-body description of coalescing nonspinning black-hole binaries and its numerical-relativity completion