Fit of the radioactive decay of ⁵⁶Ni to the first maximum of the bolometric light curve of SN 2022jli, using the Arnett (1982) analytic approximation. The parameters of the best-fit model are τ_rise = 14 days, M_ej ∼ 1.5 M_⊙, M_Ni ∼ 0.12 M_⊙, v_ej = 8500 km s⁻¹ and κ = 0.07 cm² gr⁻¹. This model illustrates that the first maximum of SN 2022jli is consistent with the typical rise time, ⁵⁶Ni and ejecta mass of a normal SN Ic. The estimated MJD of the explosion is 59695.4 days. The secondary maximum is modelled as the sum of the radioactive decay of ⁵⁶Ni and the spin-down energy from a magnetar (dotted cyan line; see Cartier et al. 2022, for details about the magnetar model). To model the secondary maximum the magnetar birth is delayed 37 days relative to the assumed time of the SN explosion and the magnetar parameters are B ∼ 8.5 × 10¹⁴ G and P ∼ 48 ms. The dotted purple line shows the magnetar contribution to the bolometric light curve. The optical and NIR luminosity at +383 days are shown using green and red pentagons, respectively. The pseudo-bolometric (UVOIR) light curve of the well-observed SE SN 2011dh (IIb) is shown for comparison (M_Ni = 0.075 M_⊙; Ergon et al. 2015).