Abundance ratios in the diluted ISM with varying dilution factor, f = 1 − 1000. Top row: log(N/O) vs log(O/H) + 12. Bottom row: log(C/O) vs log(O/H) + 12. Left column: Scenarios where the stars eject everything above the remnant mass. Right column: Scenarios where the stars eject everything above the CO core. In each panel, we show the results for three of the six metallicities: Z = 0 (Pop III, cyan), Z = 10⁻⁵ (EMP, green), and Z = 0.014 (solar, grey). Solid lines represent populations sampled from a Salpeter IMF and dashed lines from a top-heavy IMF. The markers on these lines represent specific values for f = 1 − 500. The other markers (as indicated in the top right panel), pink dashed lines and pink-shaded regions show results and lower bounds from observations, taken from Marques-Chaves et al. (2024). These results, as well as those for the remaining three metallicities not shown on this figure, can be found in tabular form in Tables 2 and 3.