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We calibrate an effective-one-body (EOB) model to numerical-relativitysimulations of mass ratios 1, 2, 3, 4, and 6, by maximizing phase and amplitudeagreement of the leading (2,2) mode and of the subleading modes (2,1), (3,3),(4,4) and (5,5). Aligning the calibrated EOB waveforms and the numericalwaveforms at low frequency, the phase difference of the (2,2) mode betweenmodel and numerical simulation remains below 0.1 rad throughout the evolutionfor all mass ratios considered. The fractional amplitude difference at peakamplitude of the (2,2) mode is 2% and grows to 12% during the ringdown. Usingthe Advanced LIGO noise curve we study the effectualness and measurementaccuracy of the EOB model, and stress the relevance of modeling thehigher-order modes for parameter estimation. We find that the effectualness,measured by the mismatch, between the EOB and numerical-relativitypolarizations which include only the (2,2) mode is smaller than 0.2% forbinaries with total mass 20-200 Msun and mass ratios 1, 2, 3, 4, and 6. Whennumerical-relativity polarizations contain the strongest seven modes, andstellar-mass black holes with masses less than 50Msun are considered, themismatch for mass ratio 6 (1) can be as high as 5% (0.2%) when only the EOB(2,2) mode is included, and an upper bound of the mismatch is 0.5% (0.07%) whenall the four subleading EOB modes calibrated in this paper are taken intoaccount. For binaries with intermediate-mass black holes with masses greaterthan 50Msun the mismatches are larger. We also determine for whichsignal-to-noise ratios the EOB model developed here can be used to measurebinary parameters with systematic biases smaller than statistical errors due todetector noise.

Inspiral-merger-ringdown multipolar waveforms of nonspinning black-hole binaries using the effective-one-body formalism