  Using Gadget-2 cosmological hydrodynamic simulations including an
observationally-constrained model for galactic outflows, we investigate how
feedback from star formation distributes mass, metals, and energy on cosmic
scales from z=6->0. We include instantaneous enrichment from Type II SNe,
delayed enrichment from Type Ia SNe and stellar (AGB) mass loss, and we
individually track C, O, Si, and Fe. Following on the successes of the
momentum-driven wind scalings, we improve our implementation with an on-the-fly
galaxy finder to derive wind properties based on host galaxy masses. By
tracking wind particles in a suite of simulations, we find: (1) Wind material
reaccretes onto a galaxy on a recycling timescale that varies inversely with
galaxy mass. Hence metals driven into the IGM by galactic superwinds cannot be
assumed to leave their galaxy forever. Wind material is typically recycled
several times; the median number of ejections for a given wind particle is 3,
so by z=0 the total mass ejected in winds exceeds 0.5\Omega_b. (2) The physical
distance winds travel is fairly independent of redshift and galaxy mass (60-100
physical kpc). For sizable galaxies at later epochs, winds typically do not
escape the galaxy halo, and rain back down in a halo fountain. High-z galaxies
enrich a significantly larger comoving volume of the IGM, with metals migrating
back into galaxies to lower z. (3) The energy imparted into winds scales with
M_{gal}^{1/3}, and energy from another source besides SNe (such as photons from
young stars) may be required to distributed cosmic metals as observed. (4) The
production of all 4 metals tracked is globally dominated by Type II SNe at all
epochs. However, intracluster gas iron content triples as a result of non-Type
II sources, and the low-z IGM carbon content is boosted by AGB feedback.
