Top: simulated stellar chemical abundances (shown as lines) for different stellar rotation velocities in a GCE OMEGA model using AGB wind yields from S. Cristallo et al. (2015) and Population II CCSN and massive-star wind yields from M. Limongi & A. Chieffi (2018). Observations of metal-poor stars in the Milky Way are shown in orange. Bottom: results after boosting the Mg yields from LC18 by a factor of 2.2 to match observations.