Right: 20″ × 20″ difference image between the NTT/EMMI/[O III]/0 and NTT/EMMI/[O III]/6000 images. The blue circle has the same meaning as in Fig. 5. The flux scaling is linear. To highlight the [O III] glow, red contours are inserted for intensities up to 23% of the peak surface intensity of the PWN. Filament F1 has been marked. North is up and east to the left. Middle two top panels: [O III] λ5007 as viewed by VIMOS/IFU Sandin et al. (2013). The left of the two middle panels shows the central part, where blue is for approaching ejecta, and red for receding. A possible jet axis is highlighted for the pulsar jet. The right of the two panels brings out fainter halo emission. Middle two bottom panels: same as the two top panels, but in velocity space. A symmetry axis (also shown in the top panel) is marked that goes through rings of [O III] emitting ejecta, and the possible jet axis is highlighted for the pulsar jet (guided by Fig. 4 of Sandin et al. 2013). For the lower right panel, likely contamination from LMC H II region He Iλ5016 is marked, as is also a region with emission on the approaching side (≤ − 750 km s⁻¹) named the blue “Wall” (also seen for [O III] λ5007 in Fig. 10). Left: Wavelet filtered HST/WFPC2/F502N map and contours of a wavelet filtered HST/WFPC2/F457M map (Lundqvist et al. 2011). Areas where the F502N fails to detect [O III] emission are highlighted. To guide the eye, a 1″ slit with PA = 90° has been drawn across all top panels. A green line in the rightmost panel marks how far west the VIMOS field reaches. All images are to scale.