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We develop new strategies to build numerical relativity surrogate models foreccentric binary black hole systems, which are expected to play an increasinglyimportant role in current and future gravitational-wave detectors. We introducea new surrogate waveform model, \texttt{NRSur2dq1Ecc}, using 47 nonspinning,equal-mass waveforms with eccentricities up to $0.2$ when measured at areference time of $5500M$ before merger. This is the first waveform model thatis directly trained on eccentric numerical relativity simulations and does notrequire that the binary circularizes before merger. The model includes the$(2,2)$, $(3,2)$, and $(4,4)$ spin-weighted spherical harmonic modes. We alsobuild a final black hole model, \texttt{NRSur2dq1EccRemnant}, which models themass, and spin of the remnant black hole. We show that our waveform model canaccurately predict numerical relativity waveforms with mismatches $\approx10^{-3}$, while the remnant model can recover the final mass and dimensionlessspin with absolute errors smaller than $\approx 5 \times 10^{-4}M$ and $\approx2 \times10^{-3}$ respectively. We demonstrate that the waveform model can alsorecover subtle effects like mode-mixing in the ringdown signal without anyspecial ad-hoc modeling steps. Finally, we show that despite being trained onlyon equal-mass binaries, \texttt{NRSur2dq1Ecc} can be reasonably extended up tomass ratio $q\approx3$ with mismatches $\simeq 10^{-2}$ for eccentricitiessmaller than $\sim 0.05$ as measured at a reference time of $2000M$ beforemerger. The methods developed here should prove useful in the building offuture eccentric surrogate models over larger regions of the parameter space.

Eccentric binary black hole surrogate models for the gravitational waveform and remnant properties: comparable mass, nonspinning case