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We present the first surrogate model for gravitational waveforms from thecoalescence of precessing binary black holes. We call this surrogate modelNRSur4d2s. Our methodology significantly extends recently introducedreduced-order and surrogate modeling techniques, and is capable of directlymodeling numerical relativity waveforms without introducing phenomenologicalassumptions or approximations to general relativity. Motivated by GW150914,LIGO's first detection of gravitational waves from merging black holes, themodel is built from a set of $276$ numerical relativity (NR) simulations withmass ratios $q \leq 2$, dimensionless spin magnitudes up to $0.8$, and therestriction that the initial spin of the smaller black hole lies along the axisof orbital angular momentum. It produces waveforms which begin $\sim 30$gravitational wave cycles before merger and continue through ringdown, andwhich contain the effects of precession as well as all $\ell \in \{2, 3\}$spin-weighted spherical-harmonic modes. We perform cross-validation studies tocompare the model to NR waveforms \emph{not} used to build the model, and finda better agreement within the parameter range of the model than other,state-of-the-art precessing waveform models, with typical mismatches of$10^{-3}$. We also construct a frequency domain surrogate model (calledNRSur4d2s_FDROM) which can be evaluated in $50\, \mathrm{ms}$ and is suitablefor performing parameter estimation studies on gravitational wave detectionssimilar to GW150914.

A Surrogate Model of Gravitational Waveforms from Numerical Relativity Simulations of Precessing Binary Black Hole Mergers