  We use cosmological hydrodynamic simulations including galactic feedback
based on observations of local starbursts to find a self-consistent
evolutionary model capable of fitting the observations of the intergalactic
metallicity history as traced by C IV between z=6.0->1.5. Our main finding is
that despite the relative invariance in the measurement of Omega(C IV) as well
as the column density and linewidth distributions over this range, continual
feedback from star formation-driven winds are able to reproduce the
observations, while an early enrichment scenario where a majority of the metals
are injected into the IGM at z>6 is disfavored. The constancy of the C IV
observations results from a rising IGM metallicity content balanced by a
declining C IV ionization fraction due to a 1) decreasing physical densities,
2) increasing ionization background strength, and 3) metals becoming more
shock-heated at lower redshift. Our models predict that ~20x more metals are
injected into the IGM between z=6->2 than at z>6. We show that the median C IV
absorber at z=2 traces metals injected 1 Gyr earlier indicating that the
typical metals traced by C IV are neither from very early times nor from very
recent feedback.
