We present the first systematic comparison between gravitational waveforms emitted by inspiralling, quasi-circular and nonspinning black hole binaries computed with three different approaches: second-order self-force (2GSF) theory, as implemented in 1PAT1 model; numerical relativity (NR), SXS collaboration; effective one body (EOB) formalism, TEOBResumS waveform model. To compare models we use both a standard, time-domain alignment gauge-invariant analysis based on dimensionless function...

The success of analytic waveform modeling within the effective-one-body (EOB) approach relies on precise understanding physical importance each technical element included in model. urgency constructing progressively more sophisticated and complete models (e.g. including spin precession eccentricity) partly defocused research from a careful comprehension building block Hamiltonian, radiation reaction, ringdown attachment). Here we go back to spirit first EOB works. We focus nonspinning,...

We present a first complete implementation of an effective-one-body (EOB) model for extreme-mass-ratio inspirals (EMRIs) that incorporates aligned spins (on both the primary and secondary) as well orbital eccentricity. The extends TEOBResumS-Dal\'{\i} these binaries by (i) recasting conservative first-order gravitational self-force (1GSF) information in resummed EOB potentials, (ii) employing post-Newtonian (PN) ${3}^{+19}\mathrm{PN}$-accurate (3PN comparable-mass terms hybridized with...

The use of effective-one-body (EOB) waveforms for black hole binaries analysis in gravitational-wave astronomy requires faithful models and fast generation times. A key aspect to achieve faithfulness is the inclusion numerical-relativity (NR) informed next-to-quasicircular corrections (NQC), dependent on radial momentum, waveform radiation reaction. robust method speed up postadiabatic iteration approximate solution EOB Hamiltonian equations. In this work, we assess performances a NQC...

We compare recently computed waveforms from second-order gravitational self-force (GSF) theory to those generated by a new, GSF-informed, effective one body (EOB) waveform model for (spin-aligned, eccentric) inspiralling black hole binaries with large mass ratios. focus on quasicircular, nonspinning, configurations and perform detailed GSF/EOB phasing comparisons, either in the time domain or via gauge-invariant dimensionless function...

We present the first comparison of waveforms evaluated using effective-one-body (EOB) approach and gravitational self-force (GSF) theory for inspiralling black hole binaries with a nonspinning primary spinning secondary. This paper belongs to series papers comparing EOB model teobresums GSF results, where latter are used benchmark analytical choices in large-mass-ratio regime. In this work, we explore performance two gauge gyro-gravitomagnetic functions ${G}_{S}$, ${G}_{{S}_{*}}$ entering...

One of the open problems in developing binary black hole (BBH) waveforms for gravitational wave astronomy is to model intermediate mass ratio regime and connect it extreme regime. A natural approach employ effective one body (EOB) two-body dynamics that, by design, can cover entire range naturally incorporates limit. Here we use recently obtained numerical relativity (NR) data with ratios $m_1/m_2=(7,15,\,32,\,64,\,128)$ test accuracy state-of-the-art EOB TEOBResumS We generally find an...

We consider a spinning test particle around rotating black hole and compare the Mathisson-Papapetrou-Dixon (MPD) formalism under Tulczyjew-Dixon spin supplementary condition to test-mass limit of effective-one-body (EOB) Hamiltonian [Phys. Rev. D.90, 044018(2014)], with enhanced spin-orbit sector. focus on circular equatorial orbits: we first constants motion at their linear in secondary approximation then compute gravitational-wave (GW) fluxes using frequency domain Teukolsky equation...

We present a comprehensive comparison between the numerical relativity (NR) angular momentum flux at infinity and corresponding quantity entering radiation reaction in teobresums, an effective one body (EOB) waveform model for nonprecessing coalescing black hole binaries on quasicircular orbits. This prompted us to implement two changes model: (i) including next-to-quasi-circular corrections $\ensuremath{\ell}=m$, $\ensuremath{\ell}\ensuremath{\le}5$ multipoles (ii) consequently updating...

We present a first complete implementation of an effective-one-body (EOB) model for extreme-mass-ratio inspirals (EMRIs) that incorporates aligned spins (on both the primary and secondary) as well orbital eccentricity. The extends TEOBResumS-Dal\'i these binaries by (i) recasting conservative first-order gravitational self-force (1GSF) information in resummed EOB potentials; (ii) employing post-Newtonian (PN) $3^{+19}$PN-accurate (3PN comparable-mass terms hybridized with test-particle up to...

The success of analytic waveform modeling within the effective-one-body (EOB) approach relies on precise understanding physical importance each technical element included in model. urgency constructing progressively more sophisticated and complete models (e.g. including spin precession eccentricity) partly defocused research from a careful comprehension building block Hamiltonian, radiation reaction, ringdown attachment). Here we go back to spirit first EOB works. We focus nonspinning,...

We compare recently computed waveforms from second-order gravitational self-force (GSF) theory to those generated by a new, GSF-informed, effective one body (EOB) waveform model for (spin-aligned, eccentric) inspiralling black hole binaries with large mass ratios. focus on quasi-circular, nonspinning, configurations and perform detailed GSF/EOB phasing comparisons, either in the time domain or via gauge-invariant dimensionless function $Q_ω\equiv ω^2/\dotω$, where $ω$ is wave frequency. The...