  Metals in the hot gaseous halos of galaxies encode the history of star
formation as well as the feedback processes that eject metals from the
galaxies. X-ray observations suggest that massive galaxies have extended
distributions of metals in their gas halos. We present predictions for the
metal properties of massive galaxies and their gaseous halos from recent high
resolution zoom-in simulations that include mechanical and radiation driven
feedback from Active Galactic Nuclei (AGN). In these simulations, AGN launch
high-velocity outflows, mimicking observed broad absorption line winds. By
comparing two sets of simulations with and without AGN feedback, we show that
our prescription for AGN feedback is capable of driving winds and enriching
halo gas `inside-out' by spreading centrally enriched metals to the outskirts
of galaxies, into the halo and beyond. The metal (iron) profiles of halos
simulated with AGN feedback have a flatter slope than those without AGN
feedback, consistent with recent X-ray observations. The predicted gas iron
abundance of group scale galaxies simulated with AGN feedback is $Z_{\rm Fe} =
0.23$ $Z_{\rm Fe,\odot}$ at $0.5 r_{500}$, which is 2.5 times higher than that
in simulations without AGN feedback. In these simulations, AGN winds are also
important for the metal enrichment of the intergalactic medium, as the vast
majority of metals ejected from the galaxy by AGN-driven winds end up beyond
the halo virial radius.
