http://arxiv.org/abs/2204.02377
Spherical harmonic modes of gravitational waveforms for inspiraling compact binaries in eccentric orbits from post-Newtonian (PN) theory accurate to third post-Newtonian order, and those extracted from Numerical Relativity (NR) simulations for binary black holes (BBHs) are compared. We combine results from the two approaches (PN and NR) to construct time-domain hybrid waveforms that describe the complete evolution of BBH mergers through inspiral(I), merger(M) and the ringdown(R) stages. These hybrids are then used in constructing a fully analytical dominant mode (l=2, |m|=2) eccentric IMR model. Overlaps with quasi-circular IMR waveform models including the effect of higher modes, maximized over a time- and phase-shift, hint at the importance (mismatches > 1%) of including eccentricity in gravitational waveforms when analysing BBHs lighter than ~ 80 M_sun, irrespective of the binary’s eccentricity (as it enters the LIGO bands), or mass-ratio. Combined impact of eccentricity and higher modes seems to become more apparent through smaller overlaps with increasing inclination angles and mass ratios. Finally, we show that the state-of-the-art quasi-circular models including the effect of higher modes will not be adequate in extracting source properties for signals with initial eccentricities e0 >= 0.1.
A. Chattaraj, T. RoyChowdhury, D. Divyajyoti, et. al.
Wed, 6 Apr 22
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