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We compare results from numerical simulations of spinning binaries in the"orbital hangup" case, where the binary completes at least nine orbits beforemerger, with post-Newtonian results using the approximants TaylorT1, T4 and Et.We find that, over the ten cycles before the gravitational-wave frequencyreaches $M\omega = 0.1$, the accumulated phase disagreement between NR and2.5PN results is less than three radians, and is less than 2.5 radians whenusing 3.5PN results. The amplitude disagreement between NR and restricted PNresults increases with the black holes' spin, from about 6% in the equal-masscase to 12% when the black holes' spins are $S_i/M_i^2 = 0.85$. Finally, ourresults suggest that the merger waveform will play an important role inestimating the spin from such inspiral waveforms.

Comparison between numerical-relativity and post-Newtonian waveforms from spinning binaries: the orbital hang-up case