Toward a gravitational self-force-informed effective-one-body waveform model for nonprecessing, eccentric, large-mass-ratio inspirals

International audienceBuilding upon several recent advances in the developmentof effective-one-body (EOB) models for spin-aligned eccentric binaries with individual masses (m1,m2), we introduce a new EOB waveform model that aims at describing inspiraling binaries in the large mass-ratio regime, m1≫m2. The model exploits the current state-of-the-art TEOBResumS-DALI model for eccentric binaries, but the standard EOB potentials (A,D¯,Q), informed by numerical relativity (NR) simulations, are replaced with the corresponding functions that are linear in the symmetric mass ratio ν≡m1m2/(m1+m2)2 taken at 8.5PN (Post-Newtonian) accuracy. To improve their strong-field behavior, these functions are (i) suitably factorized and resummed using Padé approximants and (ii) additionally effectively informed to state-of-the-art numerical results obtained by gravitational self-force theory (GSF). For simplicity, the spin sector of the model is taken to be the one of TEOBResumS-DALI, though removing the NR-informed spin-orbit effective corrections. We propose the current GSF-informed EOB framework as a conceptually complete analytical tool to generate waveforms for eccentric extreme (and intermediate) mass ratio inspirals for future gravitational wave detectors