Comparison of the 1D V_rms profiles from the best-fit JAM model with radially varying M/L profiles and M_BH = 1.6 × 10⁷ M_⊙ (using the F814W stellar-mass model; solid red line, $R_{\mathrm{SOI}}\approx 0\stackrel{″}{.}276$) or M_BH = 1.3 × 10⁷ M_⊙ (using the F160W stellar-mass model; solid blue line, $R_{\mathrm{SOI}}\approx 0\stackrel{″}{.}226$) and an alternative model with M_BH = 5 × 10⁶ M_⊙ (solid green line) against the JAM model with M_BH = 0 M_⊙ (solid black line) within a radial extent of 3″. Despite the small SOI of the SMBH ($R_{\mathrm{SOI}}\approx 0\stackrel{″}{.}226-0\stackrel{″}{.}276$), our best-fit M_BH model exhibits a kinematic imprint extending across the NIRSpec FoV ($\approx 1\stackrel{″}{.}5$) compared to the JAM model without a black hole (which accounts only for the stellar mass component). This results in a systematic increase in V_rms by approximately ΔV_rms ≈ 2 km s⁻¹, with the shift becoming more pronounced for higher M_BH values, as shown in Figs. 2 and D2. For reference, an SMBH at the lowest mass limit detectable by NIRSpec high-spectral-resolution observations using stellar dynamical techniques (M_BH, min = 5 × 10⁶ M_⊙ claimed in this work; Sect. 4) does not produce a visible kinematic effect beyond $\approx 0\stackrel{″}{.}8$.