  Using a deep Chandra observation of the Perseus cluster of galaxies, we find
a high-abundance shell 250 arcsec (93 kpc) from the central nucleus. This ridge
lies at the edge of the Perseus radio mini-halo. In addition we identify two
Halpha filaments pointing towards this shell. We hypothesise that this ridge is
the edge of a fossil radio bubble, formed by entrained enriched material lifted
from the core of the cluster. There is a temperature jump outside the shell,
but the pressure is continuous indicating a cold front. A non-thermal component
is mapped over the core of the cluster with a morphology similar to the
mini-halo. Its total luminosity is 4.8x10^43 erg/s, extending in radius to ~75
kpc. Assuming the non-thermal emission is the result of inverse Compton
scattering of the CMB and infrared emission from NGC 1275, we map the magnetic
field over the core of the cluster.
