  Effective-one-body (EOB) waveforms employed by the LIGO-Virgo-KAGRA
Collaboration have primarily been developed by resumming the post-Newtonian
expansion of the relativistic two-body problem. Given the recent significant
advancements in post-Minkowskian (PM) theory and gravitational self-force
formalism, there is considerable interest in creating waveform models that
integrate information from various perturbative methods in innovative ways.
This becomes particularly crucial when tackling the accuracy challenge posed by
upcoming ground-based detectors (such as the Einstein Telescope and Cosmic
Explorer) and space-based detectors (such as LISA, TianQin or Taiji) expected
to operate in the next decade. In this context, we present the derivation of
the first spinning EOB Hamiltonian that incorporates PM results up to
three-loop order: the SEOB-PM model. The model accounts for the complete
hyperbolic motion, encompassing nonlocal-in-time tails. To evaluate its
accuracy, we compare its predictions for the conservative scattering angle,
augmented with dissipative contributions, against numerical-relativity data of
non-spinning and spinning equal-mass black holes. We observe very good
agreement, comparable, and in some cases slightly better to the recently
proposed $w_{\rm EOB}$-potential model, of which the SEOB-PM model is a
resummation around the probe limit. Indeed, in the probe limit, the SEOB-PM
Hamiltonian and scattering angles reduce to the one of a test mass in Kerr
spacetime. Once complemented with nonlocal-in-time contributions for bound
orbits, the SEOB-PM Hamiltonian can be utilized to generate waveform models for
spinning black holes on quasi-circular orbits.
