  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 ~3.0 keV in the core to ~5.5 keV at 120 kpc and a metallicity profile
that rises slowly from ~0.5 solar to ~0.6 solar inside 60 kpc, but drops to
\~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 ~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.
