Figure adapted from M. MacLeod et al. (2025) and compiled using PWMorphology. Colored circles represent confirmed exoplanets with radii >1.6 R_⊕ from the sunset catalog shown as a function of gravitational potential and the ratio of the Hill to planet radius. Survey targets as well as HAT-P-32 b, HAT-P-67 b, KELT-9 b, WASP-33 b, WASP-94 A b, and WASP-121 b are indicated with circles outlined in black and labeled appropriately. The different colors represent the predicted hill sphere Rossby number ﹩\mathrm{ln}({R}_{o,H})﹩, where ﹩\mathrm{ln}({R}_{o,H})\gt 0﹩ indicates a bubble-like outflow geometry, and ﹩\mathrm{ln}({R}_{o,H})\lt 0﹩ indicates a stream or tail-like outflow geometry. We note that values of ﹩\mathrm{ln}({R}_{o,H})﹩ for HAT-P-32 b, HAT-P-67 b, KELT-9 b, WASP-33 b, WASP-94 A b, and WASP-121 b are calculated using the sunset photoevaporative outflow models for these planets. The dashed gray line indicates photoevaporative outflows with sound speeds of 10 km s⁻¹ and R_o,H = 1.