  We investigate the observational requirements for the detection of
sound-wave-like features in galaxy cluster cores. We calculate the effect of
projection on the observed wave amplitude, and find that the projection factor
depends only weakly on the underlying cluster properties but strongly on the
wavelength of the sound waves, with the observed amplitude being reduced by a
factor ~5 for 5 kpc waves but only by a factor ~ 2 for 25 kpc waves. We go on
to estimate the time needed to detect ripples similar to those previously
detected in the Perseus cluster in other clusters. We find that the detection
time scales most strongly with the flux of the cluster and the amplitude of the
ripples. By connecting the ripple amplitude to the heating power in the system,
we estimate detection times for a selection of local clusters and find that
several may have ripples detected with ~1Ms Chandra time.
