Comparison of the properties of SN 2026gzf derived from our analysis (black stars; Section 4) with GRB (magenta), FXT (orange; including Type Ib SN 2008D, which is shown in green), and optically discovered Type Ic-BL SNe (blue). In the top left panel we plot the SN expansion velocities (Section 4.2; K. Iwamoto et al. 1998; P. A. Mazzali et al. 2000, 2002, 2003, 2006; E. Pian et al. 2006; D. N. Sauer et al. 2006; P. A. Mazzali et al. 2008; M. Modjaz et al. 2009; F. Taddia et al. 2019; A. Corsi et al. 2023; S. Anand et al. 2024; G. P. Srinivasaragavan et al. 2024, 2025b). In the right top and bottom panels, we compare SN 2026gzf’s M_ej, M_Ni, and E_K inferred from our CSM + ⁵⁶Ni model (Section 4.4.5). In the bottom left panel, we plot the time from explosion to peak (τ_rise) against the diffusion timescale (τ_m), highlighting that SN 2026gzf’s diffusion timescale is relatively fast compared to other events (J. D. Lyman et al. 2016; G. P. Srinivasaragavan et al. 2024). Overall, SN 2026gzf’s properties are most consistent with optically discovered Type Ic-BL SNe.