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 of ∼5 for 5 kpc waves but only by a factor of ∼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...

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 of ∼5 for 5 kpc waves but only by a factor of ∼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 ∼1-Ms Chandra time.