Galactic Chemical Evolution of the Iron Peak Elements in the Lowest Metallicity Regimes

We use the nucleosynthetic yields of Chieffi & Limongi (2004) in conjunction with a Salpeter initial mass function (IMF) to determine the evolution of iron peak element abundances (Z = 21–28) as a function of metallicity. Since we will focus on the extremely metal poor region below [Fe/H] = −1.5, we will consider input from core collapse supernovae (SNe) only, as chemical enrichment from Type Ia SNe is minimal at low metallicities (e. g. Kobayashi & Nomoto (2009) and references therein). For the Fe‐peak elements, we will evaluate the relative agreement between theoretical yield calculations and recently‐acquired observational data. We will determine the yield dependence on metallicity and compare our results to those of Kobayashi et al.. (2006). It is our eventual goal to employ alternate IMF’s in order to examine the resulting effects on the iron group abundance ratios.