Left panels: narrowband images of the Fe ii* emission optimally extracted from the MUSE cube shown with a 1′′-wide slit oriented −20° (top) and +70° (bottom). The +70° slit orientation in the bottom panels follows the Fe ii* major kinematic axis. The white crosses indicate the galaxy major and minor axes from the Contini et al. (2016) kinematic analysis of [O ii]. Right panels: position-velocity diagrams of the Fe ii* emission from a slit oriented −20° (top) and +70° (bottom). Zero velocity is relative to the galaxy systemic redshift, z =1.29018 ± 0.00006, measured from the [O ii] emission. Solid black contours trace Fe ii* flux levels at 1.2, 3.6, 6, 8.4, and 11 × 10^-20 erg s^-1 cm^-2. Dashed black contours show the negative flux levels at –1.2 and –2.4 × 10^-20 erg s^-1 cm^-2. Green contours represent the ISM component estimated from [O ii] (see text). The red gradient indicates the continuum intensity. The right side panel of each p−v diagram compares the spatial profile of the Fe ii* emission (black) with that of the stellar continuum (red) and the ISM component (green). The bottom sub-panel of each p−v diagram shows the total 1D flux spectrum integrated across the spatial region between −1″ and + 1″ in the p−v diagram with the Feii* emission in black and the [O ii] emission in green. In the bottom p−v diagram, the white solid line follows the velocity gradient. This panel also reveals a “C”-shape pattern in the blue wing of the Fe ii* emission extending to –400 km s^-1. The blue wing of the Fe ii* emission is more pronounced along the slit orientation corresponding to the minor-axis (PA = + 70°), whereas the red wing appears for both slit orientations.