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We present a new frequency-domain phenomenological model of thegravitational-wave signal from the inspiral, merger and ringdown ofnon-precessing (aligned-spin) black-hole binaries. The model is calibrated to19 hybrid effective-one-body--numerical-relativity waveforms up to mass ratiosof 1:18 and black-hole spins of $|a/m| \sim 0.85$ ($0.98$ for equal-masssystems). The inspiral part of the model consists of an extension offrequency-domain post-Newtonian expressions, using higher-order terms fit tothe hybrids. The merger-ringdown is based on a phenomenological ansatz that hasbeen significantly improved over previous models. The model exhibits mismatchesof typically less than 1\% against all 19 calibration hybrids, and anadditional 29 verification hybrids, which provide strong evidence that, overthe calibration region, the model is sufficiently accurate for all relevantgravitational-wave astronomy applications with the Advanced LIGO and Virgodetectors. Beyond the calibration region the model produces physicallyreasonable results, although we recommend caution in assuming that \emph{any}merger-ringdown waveform model is accurate outside its calibration region. Asan example, we note that an alternative non-precessing model, SEOBNRv2(calibrated up to spins of only 0.5 for unequal-mass systems), exhibitsmismatch errors of up to 10\% for high spins outside its calibration region. Weconclude that waveform models would benefit most from a larger number ofnumerical-relativity simulations of high-aligned-spin unequal-mass binaries.

Frequency-domain gravitational waves from non-precessing black-hole binaries. II. A phenomenological model for the advanced detector era