Fig. 6.
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The 2011 outburst ejecta observed with MUSE-NFM. Left panel: the [O III] gas distribution observed with the MUSE-NFM (7.5″ × 7.5″). White contours correspond to iso-surface brightness contours derived from the HST/WFC3 F657N image. Right panel: two 2″ × 2″ zoom-ins of the region covering the central WD and the bright pole ejecta. After registering the MUSE [O III] map for the HST astrometry, we measured a shift of 0.71 arcsec between the centroid positions of the ejecta observed in 2014 (with HST – green cross) and in 2021 (with MUSE – red cross).
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