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Fig. 6

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Abundance ratios [X/Fe] versus [Fe/H]. Red squares: cluster giants of NGC 3114; blue crosses: field giants of Luck & Heiter (2007); black crosses: clump giants of Mishenina et al. (2006); yellow crosses: clump giants of Tautvaišienė et al. (2010); green filled squares: mean abundances of other open clusters (with ages higher than 1.0 Gyr); green open squares: clusters with ages less than 1.0 Gyr. Data from young clusters were taken from Smiljanic et al. (2009; IC 4756, NGC 3532, NGC 2447, NGC 2360, NGC 6281, NGC 6633); Pancino et al. (2010; NGC 2099); Jacobson et al. (2011; NGC 1245 and NGC 1817); Carrera & Pancino (2011; Hyades and Praesepe); Začs et al. (2011; NGC 1545 and Tr 2); Villanova et al. (2009; NGC 6475); Brown et al. (1996; Mellote 71). Data from old clusters were taken from Pacino et al. (2010; NGC 2420, NGC 7789, Cr 100, M 67); Carrera & Pancino (2011; Berkeley 32 and NGC 752); Jacobson et al. (2011; NGC 2158); Jacobson et al. (2008; NGC 7142); Friel et al. (2010; NGC 188 and Berkeley 39); Carretta et al. (2005; Cr 261); Gratton & Contarini (1994; Mellote 66 and NGC 2243); Friel et al. (2005; Berkeley 17); Young et al. (2005; Berkeley 20 and Berkeley 29).

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