Numerical relativity higher order gravitational waveforms of eccentric, spinning, non-precessing binary black hole mergers

Abstract

We use the open source, community-driven, numerical relativity software, the Einstein Toolkit to study the physics of eccentric, spinning, nonprecessing binary black hole mergers with mass-ratios $q=\{2,4,6\}$, individual dimensionless spin parameters ${\chi }_{1z}=\pm 0.6$, ${\chi }_{2z}=\pm 0.3$, that include higher order gravitational wave modes $\ell \le 4$, except for memory modes. Assuming stellar mass binary black hole mergers that may be detectable by the advanced LIGO detectors, we find that including modes up to $\ell =4$ increases the signal-to-noise of compact binaries between $3.5\%$ to $35\%$, compared to signals that only include the $\ell =|m|=2$ mode. We use two waveform models, TEOBResumS and SEOBNRE, which incorporate spin and eccentricity corrections in the waveform dynamics, to quantify the orbital eccentricity of our numerical relativity catalog in a gauge-invariant manner through fitting factor calculations. Our findings indicate that the inclusion of higher order wave modes has a measurable effect in the recovery of moderately and highly eccentric black hole mergers, and thus it is essential to develop waveform models and signal processing tools that accurately describe the physics of these astrophysical sources.

13 pages, 5 figures, updated manuscript with added waveform comparisons to TEOBResumS. accepted in Phys. Rev. D

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• The Science of the Einstein Telescope
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• Faithful effective-one-body waveform of small-mass-ratio coalescing black hole binaries: the eccentric, nonspinning, case
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• Comparing eccentric waveform models based on post-Newtonian and effective-one-body approaches, over an observationally relevant parameter space