(a) X-Ray spectra of 3C 120 obtained by the XRISM/Resolve microcalorimeter (black) and Xtend CCD (red). Data are shown as ratios to a power-law continuum with a photon index of Γ = 1.8. (b) High-resolution GMVA 86 GHz image of the relativistic jet base in 3C 120. (c) Schematic illustration of the inferred accretion flow and jet structure near the black hole in 3C 120. The cold, geometrically thin disk (brown) is truncated at approximately 20R_g. Within this radius, the flow transitions to a hot, geometrically thick accretion flow (yellow), which inwardly transports large-scale strong magnetic fields to power and collimate the relativistic jet (cyan) efficiently. The jet is launched from within 10R_g and is subsequently collimated into a parabolic profile.