Searching for Local Evidence of Supernova Enrichment in the Scorpius Centaurus OB Association

Can we detect and model enrichment within a star-forming complex with a well-constrained star-formation history, kinematics and membership? The proximity of the Scorpius-Centaurus OB Association (hereafter Sco-Cen) makes it an ideal target for answering this question. Using a Salpeter IMF and a total inferred mass for Sco-Cen subgroups, approximately one dozen supernovae are expected to have occurred within the two oldest subgroups (UCL and LCC), potentially enriching the slightly younger Upper Sco subgroup. In this work we present updated abundances of intermediate mass elements (O, Na, Mg, Si, S, Al, Ca and Ti) in relation to Fe-peak elements to quantify core collapse supernova enrichment between the subgroups. The results are derived based on high-resolution ( 60000), high S/N (S/ 200-400) spectra from the Magellan MIKE spectrograph. In addition to discussing the implications of these results on our understanding of small-scale supernova chemical evolution we briefly explore the presence of NLTE overionization/overexcitation effects in our stellar sample.