Institution(s): 1. University of Rochester
The Scorpius-Centaurus region is the nearest large-scale star-forming complex to the Sun, spanning the southern skies from the Southern Cross to the Oph/Sco region. The complex consists of three classic subgroups defined by Blaauw with mean ages spanning ~11-16 Myr (Upper Sco, Upper Cen-Lup, Lower Cen-Cru), some smaller <10 Myr-old peripheral associations (e.g. Eta Cha, Epsilon Cha, TW Hya groups, etc.), and on-going star-formation in several molecular clouds (e.g. Cha, Lup, CrA, Oph regions). I will show that the properties of the 3 main Sco-Cen subgroups shows that the common picture of monolithic, expanding, singular "bursts" of star-formation among OB subgroups is overly simplistic. I will discuss recent results regarding the membership of the Sco-Cen groups, the chemical composition of its solar-type members, evidence for additional substructures, and summarize what Sco-Cen appears to be revealing regarding the formation and evolution of GMC complexes and dissolution of young clusters.