Kinematic moment maps of Hβ around J0313-1806 and bandwidth-matched continuum. Gaussian spatial smoothing over a 2.5 pixel kernel was applied (at 0$\stackrel{″}{.}$05/pix scale). First panel: Flux map of 3σ detected Hβ (57 spaxels). These are highlighted by the red contour. We define this distribution as Hβ shell. Adjunct spaxels in eight-connectivity to these detection spaxels with at least S/N_Hβ > 1.5 are also shown. The flux in the line peaks close to the quasar location, consistent with a central ionizing source. Second panel: Velocity offset map as traced by the the v₅₀ parameter. A clear velocity gradient is observed along the shell, indicating expansion or rotation of the structure. Spaxels with extreme velocities (∣v₅₀ ∣ > 400 km s⁻¹) are marked with green contours. Third panel: Velocity dispersion, σ. Patches of large dispersions (> 600 km/s) are observed at the edges and to the south-east of the structure, potentially indicating highly turbulent gas motion. Fourth panel: Continuum map constructed by integrating the fitted continuum model over a line-free spectral window with bandwidth matched to that of Hβ. While elevated continuum emission overlaps spatially with the Hβ shell, the absence of brightened nuclear morphology in the map following the Hβ flux confirms that the observed Hβ structure is not driven by background variations or continuum residuals. The continuum map shows a clear flux peak offset to the north from the quasar position. This component does not trace the shell-like Hβ morphology and lacks any associated kinematic structure. We therefore interpret it as an artifact from imperfect fitting in imperfectly PSF-subtracted spaxels, rather than extended stellar or nebular continuum emission.