Effective-one-body waveform model for non-circularized, planar, coalescing black hole binaries: the importance of radiation reaction

We present an updated version of the TEOBResumS-Dali effective-one-body (EOB) waveform model for spin aligned binaries on non-circularized orbits. Recently computed 4PN (nonspinning) terms are incorporated in the waveform and radiation reaction. The model is informed by a restricted sample (~60) of spin-aligned, quasi-circular, Numerical Relativity (NR) simulations. In the quasi-circular limit, the model displays EOB/NR unfaithfulness F̄ᵐᵃˣEOBNR 10⁻² (with median~ 1.06× 10⁻³) (with Advanced LIGO noise and in the total mass range 10-200M_) for the dominant =m=2 mode all over the 534 spin-aligned configurations available through the Simulating eXtreme Spacetime catalog of NR waveforms. Similar figures are also obtained with the 28 public eccentric SXS simulations and good compatibility between EOB and NR scattering angles is found. The quasi-circular limit of TEOBResumS-Dali is also found to be highly consistent with the TEOBResumS-GIOTTO quasi-circular model. We then systematically explore the importance of NR-tuning { also} the radiation reaction of the system. When this is done, the median of the distribution of quasi-circular F̄ᵐᵃˣEOBNR is lowered to 3.92× 10⁻⁴, though balanced by a tail up to ~ 0.1 for large, positive spins. The same is true for the eccentric-inspiral datasets. We conclude that an improvement of the analytical description of the spin-dependent flux (and its interplay with the conservative part) is likely to be the cornerstone to lower the EOB/NR unfaithfulness below the 10⁻⁴ level all over the parameter space, thus grazing the current NR uncertainties as well as the expected needs for next generation of GW detector like Einstein Telescope.