Non-thermal X-rays, a high abundance ridge and fossil bubbles in the   core of the Perseus cluster of galaxies
  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. 
J.S. Sanders, A.C. Fabian, R.J.H. Dunn