  Barycentric corrections made to the timing of Kepler observations,
necessitated by variations in light arrival time at the satellite, break the
regular time-sampling of the data -- the time stamps are periodically
modulated. A consequence is that Nyquist aliases are split into multiplets that
can be identified by their shape. Real pulsation frequencies are
distinguishable from these aliases and their frequencies are completely
recoverable, even in the super-Nyquist regime, that is, when the sampling
interval is longer than half the pulsation period. We provide an analytical
derivation of the phenomenon, alongside demonstrations with simulated and real
Kepler data for \delta Sct, roAp, and sdBV stars. For Kepler data sets spanning
more than one Kepler orbital period (372.5 d), there are no Nyquist ambiguities
on the determination of pulsation frequencies, which are the fundamental data
of asteroseismology.
