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Measurements of black-hole spins from gravitational-wave observations ofblack-hole binaries with ground-based detectors are expected to be hampered bypartial degeneracies in the gravitational-wave phasing: between the twocomponent spins, and between the spins and the binary's mass ratio, at leastfor signals that are dominated by the binary's inspiral. Through the merger andringdown, however, a different set of degeneracies apply. This suggests thepossibility that, if the inspiral, merger and ringdown are all within thesensitive frequency band of a detector, we may be able to break thesedegeneracies and more accurately measure both spins. In this work weinvestigate our ability to measure individual spins for non-precessingbinaries, for a range of configurations and signal strengths, and conclude thatin general the spin of the larger black hole will be measurable (at best) withobservations from Advanced LIGO and Virgo. This implies that in manyapplications waveform models parameterized by only one \emph{effective spin}will be sufficient. Our work does not consider precessing binaries orsub-dominant harmonics, although we provide some arguments why we expect thatthese will not qualitatively change our conclusions.

Can we measure individual black-hole spins from gravitational-wave observations?