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. We focus on quasi-circular, nonspinning,
    configurations and perform detailed GSF/EOB waveform phasing comparisons,
    either in the time domain or via the gauge-invariant dimensionless function
    $Q_\omega\equiv \omega^2/\dot{\omega}$, where $\omega$ is the gravitational
    wave frequency. The inclusion of high-PN test-mass terms within the EOB
    radiation reaction (notably, up to 22PN) is crucial to achieve an EOB/GSF
    phasing agreement below 1~rad up to the end of the inspiral for mass ratios up
    to 500. For larger mass ratios, up to $5\times 10^4$, the contribution of
    horizon absorption becomes more and more important and needs to be accurately
    modeled. Our results indicate that our GSF-informed EOB waveform model is a
    promising tool to describe waveforms generated by either intermediate or
    extreme mass ratio inspirals for future gravitational wave detectors

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