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Fig. 1.

image

[FeIII] distribution, K-band continuum, and Doppler-shifted line maps of the GC. North is up, east is to the left in every image. In the upper left corner, a [FeIII] line map adapted from Lutz et al. (1993) is presented. It shows the V-shaped [FeIII] distribution that results in the detection of a bow shock like feature. Also, IRS7, IRS13, and IRS16 are indicated. It is 200 × 150 overview where we mark the S-cluster with a green box. Next to the [FeIII] map, a K-band continuum image from the data cube of 2015 is presented. The size of the image matches the green square in the [FeIII] distribution figure next to it and provides a 10 × 10 zoom into that region. In this SINFONI K-band continuum image, the contour lines of the, in this work investigated, dusty sources are at 55% of their intensity peak. The white contour lines represent the sources that show no Doppler-shifted [FeIII] emission lines. The blue and red contour lines can be associated with objects that do show Doppler-shifted [FeIII] emission lines. The red and blue color also indicates the Doppler-shift direction. The line maps (a–d) show the dusty sources in 2008 and 2015. Due to the limited FOV of the SINFONI cubes, not all sources are visible in all years. Therefore in (a) we show the 2008 line map to highlight 4 sources. In (b) to (d), we show 2015 line maps to highlight the remaining sources. They are based on the related Doppler shifted Brγ line extracted from the SINFONI data cubes. The green contour lines are based on the upper right presented K-band continuum image at 10%, 20%, 30%, 40%, 50%, and 100% of the peak intensity. The related line map velocities, widths, errors, and emission source sizes are listed in Table 1.

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