The interpolated model grids from A. W. Shafter & K. Hornoch (2026a) for our key input parameters, the bolometric luminosity at the peak of the eruption, L₄ (top panel), and the mass-loss timescale, t_ml (bottom panel), as functions of ﹩\mathrm{log}\dot{M}﹩ (M_⊙ yr⁻¹) and M_WD (M_⊙). The interpolations were performed by fitting second-order polynomials to the nova models of O. Yaron et al. (2005) as described in Section 5.1.