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Gravitational waves from coalescing binary black holes encode the evolutionof their spins prior to merger. In the post-Newtonian regime and on theprecession timescale, this evolution has one of three morphologies, with thespins either librating around one of two fixed points ("resonances") orcirculating freely. In this work we perform full parameter estimation onresonant binaries with fixed masses and spin magnitudes, changing threeparameters: a conserved "projected effective spin" $\xi$ and resonant family$\Delta\Phi=0,\pi$ (which uniquely label the source), the inclination$\theta_{JN}$ of the binary's total angular momentum with respect to the lineof sight (which determines the strength of precessional effects in thewaveform), and the signal amplitude. We demonstrate that resonances can bedistinguished for a wide range of binaries, except for highly symmetricconfigurations where precessional effects are suppressed. Motivated by newinsight into double-spin evolution, we introduce new variables to characterizeprecessing black hole binaries which naturally reflects the timescaleseparation of the system and therefore better encode the dynamical informationcarried by gravitational waves.

Distinguishing black-hole spin-orbit resonances by their gravitational wave signatures. II: Full parameter estimation