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 H \alpha 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 4.8 \times 10 ^ { 43 } \hbox { $ \thinspace erg \thinspace s ^ { -1 } $ } , extending in radius to \sim 75 \thinspace 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 .