We report on a Chandra observation of the massive , medium redshift ( z = 0.1386 ) cooling flow cluster Abell 1068 .
We detect a clear temperature gradient in the X–ray emitting gas from kT \sim 5 keV in the outer part of the cluster down to roughly 2 keV in the core , and a striking increase in the metallicity of the gas toward the cluster center .
The total spectrum from the cluster can be fit by a cooling flow model with a total mass deposition rate of \sim 150 { { M } _ { \odot } } { yr } ^ { -1 } .
Within the core ( r < 30 kpc ) , the mass depositon rate of \sim 40 { { M } _ { \odot } } { yr } ^ { -1 } is comparable to estimates for the star formation rate from optical data .
We find an apparent correlation between the cD galaxy ’ s optical isophotes and enhanced metallicity isocontours in the central \sim 100 kpc of the cluster .
We show that the approximate doubling of the metallicity associated with the cD can be plausibly explained by supernova explosions associated with the cD ’ s ambient stellar population and the recent starburst .
Finally , we calculate the amount of heating due to thermal conduction and show that this process is unlikely to offset cooling in Abell 1068 .