Comparing eccentric waveform models based on post-Newtonian and effective-one-body approaches

In the present study, two numerical models were compared to each other, namely the CBWaves and SEOBNRE algorithms, developed using the post-Newtonian and effective-one-body approaches, respectively, for the study of binary black holes evolving on eccentric orbits. To map the mismatch between the two models 260 000 simulations were conducted - 20 000 for non-spinning configurations and 240 000 for spinning ones-on a common grid of parameter values over the parameter space. This space is defined by the mass ratio q equivalent to m1/m2 is an element of[0.1,1], the gravitational mass mi is an element of[10M circle dot,100M circle dot] of each component labeled by i, the corresponding spin magnitude Si is an element of[0,0.6] and a constant initial orbital eccentricity e0. A comprehensive investigation was conducted to determine whether there was a discrepancy in the waveforms generated by the two codes. This entailed an in-depth analysis of the mismatch, and an extensive comparison was carried out on the outlier points between the two codes.