  Deep Chandra observations of the core of the Perseus cluster show a plethora
of complex structure. It has been found that when the observed density
fluctuations in the intracluster medium are converted into constraints on AGN
induced turbulence, the resulting turbulent heating rates are sufficient to
balance cooling locally throughout the central 220kpc. However while the
signatures of AGN feedback (inflated bubbles) dominate the central 60kpc in
X-ray images, beyond this radius the intracluster medium is increasingly shaped
by the effects of gas sloshing, which can also produce subtle variations in
X-ray surface brightness. We use mock Chandra observations of gas sloshing
simulations to investigate what fraction of the observed density fluctuations
in the core of the Perseus galaxy cluster may originate from sloshing rather
than AGN induced feedback. Outside 60kpc, we find that the observed level of
the density fluctuations is broadly consistent with being produced by sloshing
alone. If this is the case, AGN-generated turbulence is likely to be
insufficient in combating cooling outside 60kpc.
