We analyze the spherical harmonic mode amplitudes of quasicircular, nonprecessing binary black hole mergers using 275 numerical relativity simulations from the SXS, RIT, and MAYA catalogs. We construct fits using the leading-order post-Newtonian (PN) dependence on intrinsic parameters, replacing the PN velocity with fit coefficients. We compare these to polynomial fits in symmetric mass ratio and spin. We analyze $(\ell ,m)$ modes with $\ell \le 4$ from late inspiral [$t=-500M$ relative to the (2, 2) peak] to postmerger ($t=40M$). For nonspinning systems, the (2, 2), (2, 1), and (3, 3) modes retain the leading-order PN dependence on mass ratio throughout the merger. Higher-order modes deviate from the PN dependence only near and after the merger, where polynomial fits of degree $N\le 3$ can capture the amplitude behavior up to $40M$. For aligned-spin systems at fixed mass ratio, the (2, 1) mode retains its PN spin dependence, while the (3, 2) and (4, 3) modes exhibit a quadratic spin dependence near merger. The PN-inspired fits lose accuracy with increasing mass ratio, particularly near merger. Results broadly agree across catalogs, though discrepancies appear in the (3, 1), (4, 2), and (4, 1) modes, likely from resolution differences. Our results clarify the extent to which PN structure persists in mode amplitudes. Although the fits cannot be fully interpreted within the PN formalism near merger, low-degree polynomial corrections to the PN amplitude Ansätze can capture strong-field behavior, enabling closed-form and efficient modeling of waveform amplitudes in this regime.

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• Classical black holes
• General relativity
• Gravitational wave sources
• Gravitational waves
• Numerical simulations in gravitation & astrophysics