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Gravitational wave signals from asymmetric binary black hole systems have been shown to exhibit additional chirps beyond the primary merger chirp in the post-merger region of the time–frequency domain. These secondary post-merger chirps correlate to the evolving geometry of the common horizon that forms as the binary merges and were previously studied through numerical relativity simulation in a zero-spin regime. In this work, we investigate the post-merger time–frequency structure in systems with both aligned and precessing spin using widely available waveform models. We find that the inclusion of strong aligned spin (ξ=0.75) induces further post-merger time–frequency peaks. Additionally we show that even a mildly precessing spin (χp=0.25) strongly affects the distribution of post-merger radiative power across the celestial sky of the final black hole. Our results support the theory of a correlation between the post-merger signal and horizon geometry.
