[Fe/H] distribution for: SFRs within 500 pc from the Sun (dashed histogram), young nearby loose associations (dot-dashed line), and open clusters younger than 150 Myr and within 500 pc from the Sun (solid line). Sources of [Fe/H] values for the young open clusters are the following: α Persei (Boesgaard & Friel 1990), NGC 2516 (Terndrup et al. 2002), NGC 2451A/B (Hünsch et al. 2004), Blanco 1 (Ford et al. 2005), IC 4665 (Shen et al. 2005), IC 2602 and IC 2391 (D’Orazi & Randich 2009), and Pleiades (Soderblom et al. 2009).