Recent observations have revealed that abundance differences exist between low metallicity stars in the Milky Way stellar halo and those in the ultrafaint dwarf galaxies. We take a first look at what role the early environment for pre-galactic star formation might have played in shaping these stellar populations. In particular, we consider whether differences in cross-pollution between the progenitors of the stellar halo and the ultra- faints could help to explain the differences in abundance patterns. Using an N-body simulation, we find that the progenitor halos of the main halo are primarily clustered together at z = 10 while the progenitors of the dwarf galaxies remain on the outskirts of this cluster. Next, we analytically model supernova-driven winds and find that main halo progenitors cross-pollute each other more effectively while dwarf galaxy progenitors remain more isolated. Thus, inhomogeneous cross-pollution as a result of different high-z spatial locations of the object progenitors can help to explain observed differences in abundance patterns today. Conversely, these differences are a signature of the inhomogeneity of metal enrichment at early times.