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 $\mathtt{\text{CBwaves}}$ and $\mathtt{\text{SEOBNRE}}$ 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 $q\equiv m_1\mathrm{/}{m}_2\in [0.1,1]$, 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.