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

Balázs Kacskovics; Dániel Barta

doi:10.1088/1361-6382/ad72cb

paper

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

arXiv:2405.15087 · doi:10.1088/1361-6382/ad72cb

Abstract

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 $m_{i} \in [10 M_{⊙}, 100 M_{⊙}]$ 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.

25 pages, 8 figures

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

Abstract

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