The 1D V_rms vs. JAM predictions of mass models with varying BH masses. The red solid lines show our best-fit JAMs. The long-dashed and short-dashed lines indicate the upper and lower range of BH masses within 3σ (see Figure 6 and Table 6), while the black lines show the best-fit JAMs without a BH. All models are fixed to the corresponding best-fit inclination angles of galaxies (column 9, Table 6) but varying for anisotropy, mass scaling ratio, and BH mass, which will be written in the form of (β_z, γ, ﹩{M}_{\mathrm{BH}}﹩, i). The specific zero-mass and best-fit BH models plotted have (0.10, 1.20, 0 M_⊙, 70°) and (−0.2, 1.08, 2.5 × 10⁶ M_⊙, 70°) for M32, (0.27, 1.12, 0 M_⊙, 63°) and (0.27, 1.10, 7.0 × 10⁴ M_⊙, 55°) for NGC 205, (0.26, 1.19, 0 M_⊙, 71.°5) and (0.15, 1.15, 8.8 × 10⁵ M_⊙, 71.°5) for NGC 5102, and (0.30, 1.16, 0 M_⊙, 44.°5) and (0.25, 1.06, 4.7 × 10⁵ M_⊙, 45.°5) for NGC 5206. Both the V_rms profiles of spectroscopic data and their corresponding JAM predictions are binned radially in the same manner for all galaxies as presented in the right panels of Figure 5. The error bars are 1σ deviations of the kinematic measurements of the Voronoi bins in the same annuli.