Predicted MZR relation for different sets of minimal models with 10⁹ M_⊙ ≤ M_dm ≤ 10¹³ M_⊙ halos at z = 6. In the upper left panel, we report the “base models” with ϵ_SN and t_d = 20 Myr (see Sect. 3.2). In the upper right panel, we modify the base model by reducing the efficiency of the feedback (ϵ_SN = 1/4 in Eq. (2a)). In the lower left panel, we consider both weak feedback and a cosmic accretion that is modulated on a timescale of 100 Myr (A₁₀₀ = 1/3 in Eq. (4)). In the lower left panel, we show the effect of turning off the SN-delay for the weak feedback models with modulated cosmic accretion. In each panel, pastel lines are the individual tracks sampled every 2 Myr; their median and 16 − 84% dispersion are plotted with dashed and solid violet lines, respectively; the dashed black line is the control case with no-SN-delay (t_d = 0) and no modulated accretion (A₁₀₀ = 0). For each model, we report the value values of the SFR flickering (σ_SFR) and the MZR dispersion (σ_Z, see Fig. 5). As in Fig. 1, we show JWST data and fits (Nakajima et al. 2023; Curti et al. 2024; Chemerynska et al. 2024b).