We present temperature and metallicity maps of the Perseus cluster core obtained with the Chandra X-ray Observatory .
We find an overall temperature rise from \sim 3.0 keV in the core to \sim 5.5 keV at 120 kpc and a metallicity profile that rises slowly from \sim 0.5 solar to \sim 0.6 solar inside 60 kpc , but drops to \sim 0.4 solar at 120 kpc .
Spatially resolved spectroscopy in small cells shows that the temperature distribution in the Perseus cluster is not symmetrical .
There is a wealth of structure in the temperature map on scales of \sim 10 arcsec ( 5.2 kpc ) showing swirliness and a temperature rise that coincides with a sudden surface brightness drop in the X-ray image .
We obtain a metallicity map of the Perseus cluster core and find that the spectra extracted from the two central X-ray holes as well as the western X-ray hole are best-fit by gas with higher temperature and higher metallicity than is found in the surroundings of the holes .
A spectral deprojection analysis suggests , however , that this is due to a projection effect ; for the northern X-ray hole we find tight limits on the presence of an isothermal component in the X-ray hole , ruling out volume-filling X-ray gas with temperatures below 11 keV at 3 \sigma .