Abstract

The effective-one-body (EOB) approach to the general relativistic two body dynamics is a powerful analytic method to improve the behavior of perturbative series (typically, post-Newtonian results) and make them reliable and predictive in the strong-field, fast velocity regime, up to merger. The analytical construction is finally informed by Numerical Relativity (NR) simulations to obtain a highly faithful representation of the merger and ringdown regime. Faithful waveform models are essential for analyzing data of current and future gravitational wave detectors. EOB [NR]-based waveform models for coalescing relativistic binaries (either black holes and neutron stars) have nowadays reached a high level of maturity. I will summarize the state-of-the-art, in particular focusing on the TEOB ResumS waveform model that is the only one currently able of dealing with any binary configuration, from quasi-circular (precessing) orbits, to eccentric ones up to dynamical captures. As a concrete example, I will mention the special case of GW190521 , that is more likely interpretable within the scenario of the dynamical capture of two black holes than as a, more standard, quasi-circular, precessing, binary. Perspective for 3G detectors, like Einstein Telescope, and for LISA will also be discussed.