Projected maps of line flux, velocity, and velocity dispersion. Top and middle row: flux (left), velocity (middle), and velocity dispersion corrected for instrumental resolution (right) as measured from the narrow [O III] component (top) and the narrow Hα component (middle) tracing the host galaxy kinematics. Bottom: flux (left), V10, the velocity at the 10th percentile of the emission-line profile (middle), and V90, the velocity at the 90th percentile (right), from the outflow [O III] component. North is up and East is to the left. The spaxel size is 0.1″. A bar in the first column indicates 1″, corresponding to roughly 6 kpc at the source redshift. The highest projected velocities are found in the East-South-East region in both the narrow Hα and [O III] velocity maps, and are possibly related to an ongoing interaction with a faint companion (see Appendix A). Apart from this region, a velocity gradient of Δv ∼ 70 km s⁻¹ along the North-North-West to South-South-East direction is visible in both the narrow [O III] and Hα, possibly indicative of rotation. There is a small offset between the integrated [O III] and Hα line centroids of about 8 km s⁻¹. We find elevated velocity dispersions in the galaxy centre, as expected for observations of a rotating disc affected by beam smearing. The outflow is visible in the nuclear region, with positive and negative velocities respectively the systemic velocity of |600–700| km s⁻¹.