All Figures

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{ms3995f1_revised.eps} \end{figure}$ Figure 1: The SMC N81 region and its surrounding field as seen through the J filter. The image, taken with VLT/ISAAC, results from the coaddition of 10 basic exposures. The field size is 2' $\times$ 2' corresponding to 38 pc $\times$ 38 pc. The arrows indicate the candidate background galaxies (Sect. 3.2). North is up and east to the left.
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In the text

$\begin{figure} \par\hspace*{2.1cm}% \resizebox{10.2cm}{!}{\includegraphics{ms399... ...\resizebox{12.5cm}{!}{\includegraphics{ms3995f2b_revised.eps}}\par \end{figure}$ Figure 2: The SMC H II region N81 and its immediate field. a) Composite JHKs color image, b) as in a) with stars identified.
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In the text

$\begin{figure} \par\includegraphics[width=15.5cm,clip]{ms3992f3.eps} \end{figure}$ Figure 3: Color-magnitude, Ks versus H - Ks, diagram for the observed stars towards SMC N81. The solid curves show isochrones predicted by the Geneva group (Lejeune & Schaerer 2001). The left curve represents an age of 0.1 Gyr and the right one 1 Gyr. Two mass boundaries are marked on each isochrone, 4 and 4.73 $M_{\odot }$ on the left isochrone and 1.9 and 2 $M_{\odot }$ on the right one. The dashed curves are evolutionary tracks for masses 1.5, 2, and 3 $M_{\odot }$ . The reddening track is plotted with a dotted line and extends to A_V = 10 mag. Note that an A_V = 10 mag, much too high for the area of SMC N81 (see text) would be needed for interstellar reddening to create the different color properties of the third stellar population we identified. The numbers refer to the stellar identifications presented in Fig. 1 and Table 1, and triangles represent stars that are also identified in Paper I.
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In the text

$\begin{figure} \par\includegraphics[width=15.6cm,clip]{ms3992f4.eps} \end{figure}$ Figure 4: Color-color, J-H versus H-Ks, diagram for the observed SMC N81 stars. See the Fig. 3 caption for explanations regarding the model fits. Note that here the 0.1 Gyr isochrone is indicated as a solid line and the 1 Gyr curve as a dashed one. Triangles represent stars that are also identified in Paper I.
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In the text

$\begin{figure} \par\includegraphics[width=12.4cm,clip]{ms3992f5.eps} \end{figure}$ Figure 5: Variation of color index H-Ks as a function of the angular distance from the center of N81.
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In the text

$\begin{figure} \par\includegraphics[width=16.8cm,clip]{ms3995f1_revised.eps} \end{figure}$	Figure 1: The SMC N81 region and its surrounding field as seen through the J filter. The image, taken with VLT/ISAAC, results from the coaddition of 10 basic exposures. The field size is 2' $\times$ 2' corresponding to 38 pc $\times$ 38 pc. The arrows indicate the candidate background galaxies (Sect. 3.2). North is up and east to the left.
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$\begin{figure} \par\hspace*{2.1cm}% \resizebox{10.2cm}{!}{\includegraphics{ms399... ...\resizebox{12.5cm}{!}{\includegraphics{ms3995f2b_revised.eps}}\par \end{figure}$	Figure 2: The SMC H II region N81 and its immediate field. a) Composite JHKs color image, b) as in a) with stars identified.
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$\begin{figure} \par\includegraphics[width=15.6cm,clip]{ms3992f4.eps} \end{figure}$	Figure 4: Color-color, J-H versus H-Ks, diagram for the observed SMC N81 stars. See the Fig. 3 caption for explanations regarding the model fits. Note that here the 0.1 Gyr isochrone is indicated as a solid line and the 1 Gyr curve as a dashed one. Triangles represent stars that are also identified in Paper I.
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$\begin{figure} \par\includegraphics[width=12.4cm,clip]{ms3992f5.eps} \end{figure}$	Figure 5: Variation of color index H-Ks as a function of the angular distance from the center of N81.
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