Validating the effective-one-body numerical-relativity waveform models for spin-aligned binary black holes along eccentric orbits

Effective-one-body (EOB) numerical-relativity (NR) waveform models for spin-aligned binary black holes (BBHs), known as the SEOBNR waveform models, are based on the EOB theoretical framework and NR simulations. SEOBNR models have played an important role in the LIGO Scientific Collaboration (LSC) gravitational wave (GW) data analysis for both signal search and parameter estimation. SEOBNR models for quasicircular orbits have evolved through version 1 to version 4 by extending their validity domain and including more NR results. Along another direction, we recently extended the SEOBNRv1 model to the SEOBNRE model which is valid for spin-aligned BBH coalescence along eccentric orbits. In this paper we validate this theoretical waveform model by comparing them against the NR simulation bank, simulating extreme spacetimes (SXS) catalog. In total, 278 NR waveforms are investigated which include binaries with large eccentricity; large spin and large mass ratio. Our SEOBNRE can model the NR waveforms quite well. The fitting factor for most of the 278 waveforms is larger than 99%. It indicates that the SEOBNRE model could be used as template waveforms for eccentric spin-aligned BBH coalescence. Moreover, we investigate the limitation in using circular BBH waveform templates in the Advanced LIGO and Einstein Telescope era.