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 \texttt{CBwaves} and \texttt{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 $q\equiv m_1/m_2\in[0.1,\,1]$, the gravitational mass $m_i \in [10M_\odot,\, 100M_\odot]$ of each component labeled by $i$, the corresponding spin magnitude $S_i \in [0,\,0.6]$ and a constant initial orbital eccentricity $e_{0}$. 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.