Top-left panel: age-metallicity relation of the Carina dSph as obtained from individual stars on the upper RGB. Low-resolution Ca ii triplet spectroscopy from Starkenburg et al. (2010) is shown in red, high-resolution spectroscopy from (Shetrone et al. 2003; Koch et al. 2008; Lemasle et al. 2012; Venn et al. 2012) is shown as blue points. The [Mg/Fe] b), [Ca/Fe] c) and [Ba/Fe] d) abundances for the high-resolution spectroscopic samples of RGB stars are also shown (Shetrone et al. 2003; Koch et al. 2008; Lemasle et al. 2012; Venn et al. 2012). Triangles indicate stars without a statistical age estimate. For these stars only a rough age is given, based on the closest distance from evolutionary features in the SFH. The colours represent the age estimate of individual stars in Gyr, as derived from the SFH. Stars in the Milky Way are shown for comparison (small grey points).