Radio light curve of SN 2024abup at frequencies shown in Table C1, shown alongside other well-studied SN Ic-bl for comparison: 1998bw (S. R. Kulkarni et al. 1998); 2002ap (E. Berger et al. 2002); 2003jd (A. M. Soderberg et al. 2006); 2007bg (P. Salas et al. 2013); 2009bb (A. M. Soderberg et al. 2010); detections and upper limits of several other SNe are from A. Soderberg (2007), A. Corsi et al. (2023), and G. Schroeder et al. (2025). The solid and dashed curves show the expected 6 GHz light curves generated using VegasAfterglow (Y. Wang et al. 2026) for a typical relativistic jet with energy E_iso = 10⁵¹ erg, initial Lorentz factor Γ₀ = 10², jet opening angle θ_j = 0.2, electron power-law index p = 2.3, and microphysical parameters ϵ_e = 0.1 and ϵ_B = 0.01. The solid curve assumes an ISM-like CSM with density n = 0.1 cm⁻³, while the dashed curve assumes a wind-like medium with A_* = 0.1, both for a maximally off-axis viewing angle of θ_obs = 90^∘. Our nondetections rule out these typical GRB-like jet models for any viewing angle more on-axis than θ_obs = 90^∘, implying that any relativistic jet in SN 2024abup if present, must be either less energetic than standard GRB jets or propagating through a significantly lower-density environment.