Mean iron abundance, ⟨[Fe/H]⟩, as a function of total V-band magnitude, M_V, for all simulations presented in this work, divided into four groups (see Table 1) for easier comparison. Top left: exploring the role of stochasticity by fixing the subgrid model to be NUGRID (delay) with t_Ia = 38 Myr (red) or LC18 with t_Ia = 100 Myr (blue) varying only the random number seed. This panel also includes the simulations from Andersson et al. (2025) in black. Top right: exploring the rotation models from LC18 (teal, green, and blue for 0, 150, and 300 km s⁻¹, respectively), including one example with the rotation distribution from Prantzos et al. (2018, purple). All these models use t_Ia = 38 Myr. Lower left: testing different SNIa models, including 38 (green) and 100 Myr (blue) for t_Ia, one example without SNIa (purple), and one with metallicity-dependent SNIa yields (teal). All models use yields from LC18 for massive stars. Bottom right: comparing the NUGRID models with the delay (red) and rapid (blue) explosion triggers for CCSN, both with t_Ia = 38 Myr. These simulations use a model identical to NUGRID (delay), t_Ia = 38 Myr, but from different initial conditions. The error bars on the vertical axis indicate the dispersion in [Fe/H], calculated by taking the standard deviation of all stars in each galaxy. Gray error bars show values from dwarf galaxies in the Local Group Volume, taken from the database by Pace (2025). For these points, M_V has error bars indicating upper and lower errors, while error bars on [Fe/H] indicate the dispersion. The dashed gray line shows the dwarf galaxy luminosity-[Fe/H] fit from Kirby et al. (2013).