  We present an analysis of the flow of metals through the circumgalactic
medium (CGM) in the Feedback in Realistic Environments (FIRE) simulations of
galaxy formation, ranging from isolated dwarfs to $L*$ galaxies. We find that
nearly all metals produced in high-redshift galaxies are carried out in winds
that reach $0.25 R_{\rm vir}$. When measured at $0.25 R_{\rm vir}$ the
metallicity of outflows is slightly higher than the interstellar medium (ISM)
metallicity. Many metals thus reside in the CGM. Cooling and recycling from
this reservoir determine the metal budget in the ISM. The outflowing metal flux
decreases by a factor of $\sim2-5$ between $0.25 R_{\rm vir}$ and $R_{\rm
vir}$. Furthermore, outflow metallicity is typically lower at $R_{\rm vir}$
owing to dilution of the remaining outflow by metal-poor material swept up from
the CGM. The inflow metallicity at $R_{\rm vir}$ is generally low, but outflow
and inflow metallicities are similar in the inner halo. At low redshift,
massive galaxies no longer generate outflows that reach the CGM, causing a
divergence in CGM and ISM metallicity. Dwarf galaxies continue to generate
outflows, although they preferentially retain metal ejecta. In all but the
least massive galaxy considered, a majority of the metals are within the halo
at $z=0$. We measure the fraction of metals in CGM, ISM and stars, and quantify
the thermal state of CGM metals in each halo. The total amount of metals in the
low-redshift CGM of two simulated $L*$ galaxies is consistent with estimates
from the COS halos survey, while for the other two it appears to be lower.
