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

Understand

We develop new strategies to build numerical relativity surrogate models for eccentric binary black hole systems, which are expected to play an increasingly important role in current and future gravitational-wave detectors.

• We introduce a new surrogate waveform model, \texttt{NRSur2dq1Ecc}, using 47 nonspinning, equal-mass waveforms with eccentricities up to $0.2$ when measured at a reference time of $5500M$ before merger.
• This is the first waveform model that is directly trained on eccentric numerical relativity simulations and does not require that the binary circularizes before merger.
• The model includes the $(2,2)$, $(3,2)$, and $(4,4)$ spin-weighted spherical harmonic modes.