All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{hd281_fig1.eps} \end{figure}$ Figure 1: Astrometric/photometric errors and their standard deviations. Crosses are for Night1, stars for Night2, diamonds for Night3, triangles for Night4, and squares for Night5. Errors are estimated for each magnitude bin of the luminosity function computed by StarFinder. The translation to get the absolute photometry can be done with the zero-point of each night ( $\approx$ 4.5). To avoid confusion, the different symbols are horizontally shifted with respect to the bin centers.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=17.8cm,height=20.2cm,clip]{hd281_fig2.eps} \end{figure}$ Figure 2: Upper line: Sgr A*/ $L^\prime$ (continuous line/crosses) and S2 (dash line/filled circles) light curves. Second line: distance in mas between Sgr A*/L $^\prime$ and DC. Third line: opposite of the Sgr A*/ $L^\prime$ polar angle with respect to DC. The curves of the different nights are separated by a vertical line. All curves have been smoothed with a boxcar average of 2. Bottom line: 1.4 $^{\prime \prime }$ $\times$ 1.4 $^{\prime \prime }$ Night 3 images of the central stellar cluster during Sgr A*/ $L^\prime$ flare (couple of images on the left) and quiescent (couple of images on the right) states. Each couple of images is made of a 105 s integration time reduced image and the deconvolved corresponding one, obtained with 40 iterations of the maximum likelihood deconvolution IDL procedure. The deconvolved images are presented here only to highlight the sources position/extension and have not been used elsewhere for any quantitative analysis.
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In the text

$\begin{figure} \par\includegraphics[width=17.8cm,clip]{hd281_fig3.eps} \end{figure}$ Figure 3: Left: distance of Sgr A*/ $L^\prime$ from DC in mas as a function of the Sgr A*/ $L^\prime$ magnitude. Crosses, stars, diamonds, triangles, squares and filled circles are Night1, 2, 3/part1, 3/part2, 4, 5 data points respectively. Right: Sgr A*/ $L^\prime$ positions with respect to DC. Crosses represent positions for $12.2\leq L^\prime$ (Sgr A*/ $L^\prime$ ) < 12.6, diamonds for $12.6\leq L^\prime$ (Sgr A*/ $L^\prime$ ) < 13.0, stars for $13.0\leq L^\prime$ (Sgr A*/ $L^\prime$ ) < 13.4, triangles for $13.4\leq L^\prime$ (Sgr A*/ $L^\prime$ ) < 13.8.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{hd281_fig4.eps} \end{figure}$ Figure 4: Encircled H II components positions on a 2.4 $^{\prime \prime }$ $\times$ 2.4 $^{\prime \prime }$ $L^\prime$ NACO image. From left to right: H II 5D, H II 5C, source $\epsilon$ , source $\xi$ (Yusef-Zadeh et al. 1998; Zhao & Goss 1999). The circle diameter is the 0.1 $^{\prime \prime }$ radio resolution. ID18 is the bright extended source just south to the H II 5D circle.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{hd281_fig4.eps} \end{figure}$	Figure 4: Encircled H II components positions on a 2.4 $^{\prime \prime }$ $\times$ 2.4 $^{\prime \prime }$ $L^\prime$ NACO image. From left to right: H II 5D, H II 5C, source $\epsilon$ , source $\xi$ (Yusef-Zadeh et al. 1998; Zhao & Goss 1999). The circle diameter is the 0.1 $^{\prime \prime }$ radio resolution. ID18 is the bright extended source just south to the H II 5D circle.
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