The optical diagnostic BPT diagrams plotted [O III] λ5007/Hβ vs. [N II] λ6584/Hα (left) and [O III] λ5007/Hβ vs. [S II] λ λ6717, 6731/Hα (right panels) for the fully radiation-bounded models with mass-loss rates ﹩\mathrm{log}{\dot{M}}_{\mathrm{sc}}=-4﹩, −3, −2, and −1 M _⊙ yr^–1 (from top to bottom), ambient densities n _amb = 1, 10, 10², and 10³ cm⁻³ (labeled on plots), metallicities ﹩\hat{Z}\equiv Z/﹩ Z_⊙ = 1 (blue), 0.5 (red), 0.25 (green), and 0.125 (yellow color), and wind terminal velocities V _∞ = 250 (dashed), 500 (dashed–dotted), and 1000 km s⁻¹ (dotted lines). For the subsolar models, we use the solar model parameters scaled as ﹩{\dot{M}}_{\mathrm{sc}}\propto {Z}^{0.72}﹩ and V _∞ ∝ Z ^0.13. The optically thin and thick models are plotted by filled and open circles, respectively. Line emissivities for optically thick models are somewhat uncertain. The wind catastrophic cooling (CC) and catastrophic cooling with the bubble (CB) modes are labeled by the plus signs and crosses, respectively. The solid (red color) and dashed (blue color) lines show the upper and lower boundaries to star-forming galaxies from Kewley et al. (2001) and Kauffmann et al. (2003), respectively, whereas those above the solid red line are classed as AGNs. The plotted observations are from Richard et al. (2011), Masters et al. (2014), Berg et al. (2016), and Senchyna et al. (2017).