  We use gas dynamic simulations to explore the effects of galactic winds on
galaxy clusters. Two ensembles of 18 realizations, spanning a decade in
temperature, are evolved with and without winds in an underlying biased CDM
cosmology. Galaxies are identified as peaks in the initial density field, and
are assumed to lose half their initial mass over a Hubble time in winds with an
effective temperature of 8 keV. The energy input through winds boosts the
entropy of the ICM above that generated by infall, resulting in a more extended
density profile. The magnitude of this effect increases with decreasing mass or
temperature, consistent with observations. The extended nature of the ICM with
winds can lead to underestimates of the global baryon fraction, with
low-temperature clusters particularly deficient. We calibrate the amplitude of
this effect at density contrasts of 170 and 500. On the other hand, the final
temperature of the gas is relatively unaffected; a similar mass-temperature
relation exists with or without winds. The input wind energy is effectively
consumed as work to lift the gas in the dark matter dominated potential. While
the dark matter profile exhibits a self-similar form seen in other studies, the
galaxy distribution is more centrally concentrated than either the dark matter
or gas, and evidences a mild velocity bias. The gradient of galaxies with
respect to primordial gas produces strong, negative radial gradients in
metallicity within the ICM.
