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Fig. 6.


[FeIII] and Brγ line distribution in the Galactic center around Sgr A*. In every image, north is up and east to the left. The scaling of the figures is either mentioned or match the marked squares. Panel a: we adapt the Brγ detection presented in Lutz et al. (1993) in the GC around Sgr A*. The green box marks the size of the SINFONI FOV. The red circle with the open side towards the west indicates the position of the Sgr A* bubble that is described in detail in Yusef-Zadeh et al. (2012). Panel b: zoomed-in figure of (a). Sgr A* is marked with a red cross. Panel c: Brγ line map at around 2.1661 μm extracted from our SINFONI data-cube in 2015. The bright north-south Brγ-bar can be detected in every data-cube and is approximately at the position of the open side of the Sgr A* bubble. Panel d: [FeIII] distribution around Sgr A*. The [FeIII] line-map emission of the dusty sources around Sgr A* is shown in Fig. B.1. Panel e: zoomed-in cutout of (d). The edge of the [FeIII] distribution coincides with the position of the detected Brγ-bar shown in (c). From (a) and (b) we can conclude that the [FeIII] emission is significantly decreased inside the Sgr A* bubble. The related velocities, uncertainties, and widths of the [FeIII] line emission are given in Table 6. The phenomena described here are in line with Yusef-Zadeh et al. (2012) (see also Fig. 5 in the mentioned publication and Fig. E.1).

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