Effective-one-body waveform model for noncircularized, planar, coalescing black hole binaries: The importance of radiation reaction

We present an updated version of the teobresums-dal & iacute; effective one body (EOB) waveform model for spin-aligned binaries on noncircularized orbits. Recently computed 4 Post Newtonian (PN) (nonspinning) terms are incorporated in the waveform and radiation reaction. The model is informed by a restricted sample (similar to 60) of spin-aligned, quasicircular, numerical relativity (NR) simulations. In the quasicircular limit, the model displays EOB/NR maximal unfaithfulness (F) over bar (max)(EOBNR)less than or similar to 10(-2) (with median 1.06x10(-3)) (with Advanced LIGO noise and in the total mass range 10-200M(circle dot)) for the dominant l=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 simulating extreme spacetime simulations as well as good compatibility between EOB and NR scattering angles. The quasicircular limit of teobresums-dal & iacute; is highly consistent with the teobresums-giotto quasicircular 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 quasicircular (F) over bar (max)(EOBNR) is lowered to 3.92x10(-4), though balanced by a tail up to similar 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 gravitational wave detector like the Einstein Telescope.