Study of eccentric binary black hole mergers using numerical relativity and an inspiral-merger-ringdown model

We study the phenomenology of non-spinning eccentric binary black hole (BBH) mergers using numerical relativity (NR) waveforms and $\mathtt{\text{EccentricIMR}}$ waveform model, as presented in Ref. \cite{Hinder:2017sxy} (Hinder, Kidder, and Pfeiffer, arXiv:1709.02007). This model is formulated by combining an eccentric inspiral, derived from a post-Newtonian (PN) approximation including 3PN conservative and 2PN reactive contributions to the BBH dynamics, with a circular merger model. A distinctive feature of $\mathtt{\text{EccentricIMR}}$ is its two-parameter treatment, utilizing eccentricity and mean anomaly, to characterize eccentric waveforms. We implement the $\mathtt{\text{EccentricIMR}}$ model in $\mathtt{\text{Python}}$ to facilitate routine use. We then validate the model against 35 eccentric NR waveforms obtained from both the SXS and RIT NR catalogs. We find that $\mathtt{\text{EccentricIMR}}$ model reasonably match NR data for eccentricities up to $0.16$, specified at a dimensionless reference frequency of $x=0.07$, and mass ratios up to $q=4$. Additionally, we use this model as a tool for cross-comparing eccentric NR data obtained from the SXS and RIT catalogs. Furthermore, we explore the validity of a circular merger model often used in eccentric BBH merger modelling using both the NR data and $\mathtt{\text{EccentricIMR}}$ model. Finally, we use this model to explore the effect of mean anomaly in eccentric BBH mergers.