Comparing eccentric waveform models based on post-Newtonian and effective-one-body approaches, over an observationally relevant parameter space

We used two numerical models, namely the CBwaves and SEOBNRE algorithms, based on the post-Newtonian and effective-one-body approaches for binary black holes evolving on eccentric orbits. We performed 20.000 new simulations for non-spinning and 240.000 simulations for aligned-spin configurations on a common grid of parameter values over the parameter space spanned by the mass ratio q≡ m₁/m₂∈[0.1,\,1], the gravitational mass mᵢ ∈ [10M_,\, 100M_] of each component labeled by i, the corresponding spin magnitude Sᵢ ∈ [0,\,0.6] and a constant initial orbital eccentricity e₀. A detailed investigation was conducted to ascertain whether there was a discrepancy in the waveforms generated by the two codes. This involved an in-depth analysis of the mismatch. Furthermore, an extensive comparison was carried out on the outlier points between the two codes.