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We employ high-resolution cosmological zoom-in simulations focusing on ahigh-sigma peak and an average cosmological field at $z\sim 6-12$, in order toinvestigate the influence of environment and baryonic feedback on galaxyevolution in the reionization epoch. Strong feedback, e.g., galactic winds,caused by elevated star formation rates (SFRs) is expected to play an importantrole in this evolution. We compare different outflow prescriptions: (i)constant wind velocity (CW), (ii) variable wind scaling with galaxy properties(VW), and (iii) no outflows (NW). The overdensity leads to acceleratedevolution of dark matter and baryonic structures, absent in the "normal"region, and to shallow galaxy stellar mass functions at the low-mass end.Although CW shows little dependence on both environments, the more physicallymotivated VW model does exhibit this effect. In addition, VW can reproduce theobserved specific SFR (sSFR) and the sSFR-stellar mass relation, which CW andNW fail to satisfy simultaneously. Winds also differ substantially in affectingthe state of the intergalactic medium (IGM). The difference lies involume-filling factor of hot, high-metallicity gas which is near unity for CW,while it remains confined in massive filaments for VW, and locked up ingalaxies for NW. Such gas is nearly absent in the normal region. Although allwind models suffer from deficiencies, the VW model seems to be promising incorrelating the outflow properties to those of host galaxies. Furtherconstraints on the state of the IGM at high-$z$ are needed to separatedifferent wind models.

The Baryon Cycle at High Redshifts: Effects of Galactic Winds on Galaxy Evolution in Overdense and Average Regions