Characterization of numerical relativity waveforms of eccentric binary black hole mergers

Abstract

We introduce a method to quantify the initial eccentricity, gravitational wave frequency, and mean anomaly of numerical relativity simulations that describe non-spinning black holes on moderately eccentric orbits. We demonstrate that this method provides a robust characterization of eccentric binary black hole mergers with mass-ratios $q\le 10$ and eccentricities $e_0\le 0.2$ fifteen cycles before merger. We quantify the circularization rate of a variety of eccentric numerical relativity waveforms introduced in [1] by computing overlaps with their quasi-circular counterparts, finding that $50M$ before merger they attain overlaps $\mathcal{O}\ge 0.99$, furnishing evidence for the circularization of moderately eccentric binary black hole mergers with mass-ratios $q\le 10$. We also quantify the importance of including higher-order waveform modes for the characterization of eccentric binary black hole mergers. Using two types of numerical waveforms, one that includes $(\ell ,|m|)=\{(2,2),(2,1),(3,3),(3,2),(3,1),(4,4),(4,3),(4,2),(4,1)\}$ and one that only includes the $\ell =|m|=2$ mode, we find that the overlap between these two classes of waveforms is as low as $\mathcal{O}=0.89$ for $q=10$ eccentric binary black hole mergers, underscoring the need to include higher-order waveform modes for the description of these gravitational wave sources. We discuss the implications of these findings for future source modeling and gravitational wave detection efforts.

arXiv comment12 pages, 5 figures, 1 table; v2: one figure added. Accepted to Phys. Rev. D

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