Fig. D.6
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Time variation of Hβ and Hα of AzV 362. Both lines seem to show a prominent blueshifted emission in 2001 and 2020. The Hα in the recent X-Shooter observation even appears as a completely inverted P Cygni profile, which is also shown in Fig 2. Higher-order Balmer lines do not show significant variability. The C II lines are shown for alignment purposes.
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