Papers › An eccentric binary black hole inspiral-merger-ringdown gravitational waveform model...
An eccentric binary black hole inspiral-merger-ringdown gravitational waveform model from numerical relativity and post-Newtonian theory
Ian Hinder, Lawrence E. Kidder, Harald P. Pfeiffer
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We present a prescription for computing gravitational waveforms for the inspiral, merger and ringdown of non-spinning eccentric binary black hole systems. The inspiral waveform is computed using the post-Newtonian expansion and the merger waveform is computed by interpolating a small number of quasi-circular NR waveforms. The use of circular merger waveforms is possible because eccentric binaries circularize in the last few cycles before the merger, which we demonstrate up to mass ratio q = m₁/m₂ = 3. The complete model is calibrated to 23 numerical relativity (NR) simulations starting ~20 cycles before the merger with eccentricities e_(ref) ≤0.08 and mass ratios q ≤3, where e_(ref) is the eccentricity ~7 cycles before the merger. The NR waveforms are long enough that they start above 30 Hz (10 Hz) for BBH systems with total mass M ≥80 M_⊙ (230 M_⊙). We find that, for the sensitivity of advanced LIGO at the time of its first observing run, the eccentric model has a faithfulness with NR of over 97% for systems with total mass M ≥85 M_⊙ across the parameter space (e_(ref) ≤0.08, q ≤3). For systems with total mass M ≥70 M_⊙, the faithfulness is over 97% for e_(ref) ≲0.05 and q ≤3. The NR waveforms and the Mathematica code for the model are publicly available.
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