  The past three years have seen two significant advances in models of
gravitational waveforms emitted by quasicircular compact binaries in two
regimes: the weak-field, post-Newtonian regime, in which the gravitational wave
energy flux has now been calculated to fourth-and-a-half post-Newtonian order
(4.5PN) [Phys. Rev. Lett. 131, 121402 (2023)]; and the small-mass-ratio,
gravitational self-force regime, in which the flux has now been calculated to
second perturbative order in the mass ratio (2SF) [Phys. Rev. Lett. 127, 151102
(2021)]. We compare these results and find excellent agreement for the total
flux, showing consistency between the two calculations at all available PN and
SF orders. However, although the total fluxes agree, we find disagreements in
the fluxes due to individual spherical-harmonic modes of the waveform, strongly
suggesting the two waveforms might be in different asymptotic frames.
