Assumed nucleosynthetic over- or underabundances (red solid curves), in units of [Zn/Fe]. The values of α_X,0 (at [Zn/Fe] = 0) are adopted from the observed intercepts of the sequences of relative abundances (α_O,0 = 0.38 ± 0.10, α_P,0 = 0.00 ± 0.06, α_S,0 = 0.25 ± 0.03, α_Si,0 = 0.26 ± 0.03, α_Mg,0 = 0.30 ± 0.04, and α_Mn,0 = −0.39 ± 0.03). The shape of the curves are adopted from Galactic observations in the literature, from Lambert (1987) and McWilliam (1997) for α elements (dashed black curves), from Wheeler et al. (1989), Mishenina et al. (2015), and Battistini & Bensby (2015) for Mn, and from Caffau et al. (2016) and Roederer et al. (2014) for P. These are presented in units of stellar metallicity [M/H], where the scaling to ISM [Zn/Fe] units assumes a linear relation of the data shown in Fig. 6. This is only a scale conversion that allows us to use the nucleosynthetic over- or underabundances in the literature, and should not be used as a one-to-one conversion between [Zn/Fe] and [M/H]. The shaded region corresponds to the α-element enhancement measured by Becker et al. (2012) for metal-poor DLAs (within 1σ of the mean), while the small dots are derived from Jonsell et al. (2005) for metal-poor stars (see Appendix C).