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

Building 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, m₁m₂. 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 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 Pad\'e 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.