Qualitative placement of GRB 250702B (shaded rectangle) in (K, q) space, where K ≡ r/r_ISCO(a_*) and q ≡ M_T/M_BH is the torus-to-BH mass ratio (M. H. P. M. van Putten et al. 2024). For the observed period P ≃ 2825 s and a fiducial M_BH = 6 M_⊙, GRB 250702B occupies K ≃ 59–130 for BH spins a_* = 0.5–0.9 and q ∼ 10⁻⁴ (shaded band). The adopted q value places the event between canonical long GRBs (q ∼ 10⁻²) and SLSNe (q ∼ 10⁻⁷). The rectangular boxes show representative (K, q) regions for GW170817B (the post-merger BH spindown signal associated with GW170817 with estimated K ∼ 3–4 and q ∼ 10⁻³–10⁻²; M. H. P. M. van Putten et al. 2024) and M87 with minimal torus fraction q ∼ 10⁻⁷–10⁻⁸ (jet launching and collimation occur on scales of a few r_ISCO, inferred from VLBI constraints and jet kinematics—e.g., S. S. Doeleman et al. 2012; F. Mertens et al. 2016; J. Y. Kim et al. 2018; and further supported by the detection of jet precession—e.g., Y. Cui et al. 2023). Both GW170817B and M87 therefore anchor the “few–r_ISCO” end of the diagram, whereas GRB 250702B requires a much larger K, where the precession is set by the outer working annulus of a thick inner flow.