All Figures

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{1748fig1.eps} \end{figure}$ Figure 1: ISAAC M-band final image of the Galactic Center. The field of view is 72.6 $^{\prime \prime }$ $\times$ 72.6 $^{\prime \prime }$ .
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{1748fig2.eps} \end{figure}$ Figure 2: Part of the ISAAC L-band final image of the Galactic Center showing most of the named sources.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{1748fig3.eps} \end{figure}$ Figure 3: H-, K- and M-band view of IRS 3 (encircled in the H-band view). The bright source to the northeast ( upper left) is the supergiant IRS 7. A histogram equalization color scale is used, while the contour lines follow a logarithmic scale in order to show the IRS 3 source structure as clearly as possible.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1748fig4.eps} \end{figure}$ Figure 4: L-band view of IRS 3 with NAOS/CONICA (Eckart 2004). The circular structures surrounding the bright sources are due to the adaptive optics. Note the asymmetry in the lower contour lines producing a bow-shock-like effect at the southern edge of the extended emission.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{1748fig5.eps} \end{figure}$ Figure 5: Two-color diagram showing $(K-L)_{{\rm obs}}$ versus $(H-K)_{{\rm obs}}$ . The triangles represent sources from the inner 18 $^{\prime \prime }$ $\times$ 18 $^{\prime \prime }$ , the squares represent brighter sources (m_L<9.5) and the diamonds a selection of fainter sources from outside this inner region.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{1748fig6.eps} \end{figure}$ Figure 6: Two-color diagram showing $(L-M)_{{\rm obs}}$ versus $(K-L)_{{\rm obs}}$ . The triangles represent sources from the inner 18 $^{\prime \prime }$ $\times$ 18 $^{\prime \prime }$ , the squares represent brighter sources (m_L<9.5) and the diamonds a selection of fainter sources from outside this inner region. The marked areas fully contain the spectroscopically identified He stars and red giants / AGB stars from Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1748fig7.eps} \end{figure}$ Figure 7: Extinction towards Sgr A* according to Lutz et al. (1996). The data points are derived from SWS H recombination line data, while the solid curve is the extinction law of Draine (1989) for standard graphite-silicate mixes. The data point marked by an arrow is our new M-band result.
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{1748fig1.eps} \end{figure}$	Figure 1: ISAAC M-band final image of the Galactic Center. The field of view is 72.6 $^{\prime \prime }$ $\times$ 72.6 $^{\prime \prime }$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{1748fig2.eps} \end{figure}$	Figure 2: Part of the ISAAC L-band final image of the Galactic Center showing most of the named sources.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{1748fig3.eps} \end{figure}$	Figure 3: H-, K- and M-band view of IRS 3 (encircled in the H-band view). The bright source to the northeast ( upper left) is the supergiant IRS 7. A histogram equalization color scale is used, while the contour lines follow a logarithmic scale in order to show the IRS 3 source structure as clearly as possible.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1748fig4.eps} \end{figure}$	Figure 4: L-band view of IRS 3 with NAOS/CONICA (Eckart 2004). The circular structures surrounding the bright sources are due to the adaptive optics. Note the asymmetry in the lower contour lines producing a bow-shock-like effect at the southern edge of the extended emission.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{1748fig5.eps} \end{figure}$	Figure 5: Two-color diagram showing $(K-L)_{{\rm obs}}$ versus $(H-K)_{{\rm obs}}$ . The triangles represent sources from the inner 18 $^{\prime \prime }$ $\times$ 18 $^{\prime \prime }$ , the squares represent brighter sources (m_L<9.5) and the diamonds a selection of fainter sources from outside this inner region.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{1748fig7.eps} \end{figure}$	Figure 7: Extinction towards Sgr A* according to Lutz et al. (1996). The data points are derived from SWS H recombination line data, while the solid curve is the extinction law of Draine (1989) for standard graphite-silicate mixes. The data point marked by an arrow is our new M-band result.
Open with DEXTER