Surrogate remnant model for non-spinning eccentric binary black hole mergers

The properties of the final remnant (mass, dimensionless spin, and kick velocity) formed at the end of a binary black hole (BBH) coalescence are crucial for fundamental tests of general relativity as well as for astrophysical modeling, including the occurrence of hierarchical mergers. While remnant models for quasi-circular BBH mergers are well-developed, no reliable remnant model is available for eccentric BBH mergers. We perform 109 numerical relativity (NR) simulations featuring non-spinning eccentric BBHs, encompassing mass ratios from 1:1 to 1:4, and eccentricities below 0.4, as measured at a reference time of roughly 20 orbits before merger. These simulations are utilized to construct a data-driven surrogate model for the remnant black hole properties, including final mass, dimensionless spin, and kick velocity. We demonstrate that the remnant model can accurately predict the remnant properties. By leveraging both NR data and the remnant surrogate, we also explore the correlation between the initial eccentricity of the binary and the remnant properties.