All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4203_1.ps} \end{figure}$ Figure 1: $K_{\rm s}$ band 2MASS image of vdB-RN 92. Open circle indicates the object central part. Crosses indicate instrumental artifacts.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4203_2.ps} \end{figure}$ Figure 2: Same as Fig. 1 for Gy 3-7.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4203_3.ps} \end{figure}$ Figure 3: R image of vdB-RN 92 from the Digitized Sky Survey.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4203_4.ps} \end{figure}$ Figure 4: Same as Fig. 3 for Gy 3-7.
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In the text

$\begin{figure} \par\includegraphics[width=6cm,clip]{H4203_5.ps} \end{figure}$ Figure 5: IRAS 12 $\mu$ m image of CMaR1. Open circles encompass vdB-RN 92 (right) and Gy 3-7 (left).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4203_6.ps} \end{figure}$ Figure 6: vdB-RN 92: J,(J-H) CMD of the cluster region (filled circles) and comparison fields (open diamonds). Field 1 corresponds to the left panel and field 3 to the right one. All extractions have radius 1 $^\prime$ . No cutoff was used.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4203_7.ps} \end{figure}$ Figure 7: vdB-RN 92: ( $(J-H),(H-K_{\rm s})$ ) diagram for the cluster (filled circles) and comparison field 1 (open diamonds). Triangles are the four more luminous stars in the object. Reddening vector and reddening lines for M5 giant (dashed-pointed line) and O3 stars (dashed line) are shown. The continuous curve is the intrinsic distribution of spectral types. A cutoff at $K_{\rm s} = 14.5$ was used.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4203_8.ps} \end{figure}$ Figure 8: vdB-RN 92: J,(J-H) CMD of the cluster (filled circles) with PMS isochrones of 1 Myr (dashed line) and 7 Myr (dotted line). The ZAMS is represented by continuous line (Siess et al. 2000) and dashed-dotted line (Bertelli et al. 1994). Left panel presents the fit for the most massive star. Right panel presents the fit with A_J=1.21. Colour and magnitude errors are indicated.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4203_9.ps} \end{figure}$ Figure 9: Gy 3-7: J,(J-H) CMD of the cluster region (filled circles) and comparison star fields (open diamonds). Field 5 corresponds to the left panel and field 6 to the right one. All extractions have radius 1 $^\prime$ . No magnitude cutoff was used.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4203_10.ps} \end{figure}$ Figure 10: Gy 3-7: ( $(J-H),(H-K_{\rm s})$ ) diagram for the cluster (filled circles) and comparison field 5 (open diamonds). Triangle is the most luminous star in the object. Reference lines as in Fig. 7. A cutoff at $K_{\rm s} = 14.5$ was applied to minimize errors.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4203_11.ps} \end{figure}$ Figure 11: Gy 3-7: J,(J-H) CMD of the cluster (filled circles) with PMS isochrones of 1 Myr (dashed line) and 7 Myr (pointed line). The ZAMS is represented by continuous line (Siess et al. 2000) and dashed-dotted line (Bertelli et al. 1994). Left panel presents the fit for the distance found by Wouterloot & Brand (1989). Right panel presents the fit with A_J=1.74. Colour and magnitude errors are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4203_1.ps} \end{figure}$	Figure 1: $K_{\rm s}$ band 2MASS image of vdB-RN 92. Open circle indicates the object central part. Crosses indicate instrumental artifacts.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4203_2.ps} \end{figure}$	Figure 2: Same as Fig. 1 for Gy 3-7.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4203_3.ps} \end{figure}$	Figure 3: R image of vdB-RN 92 from the Digitized Sky Survey.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{H4203_4.ps} \end{figure}$	Figure 4: Same as Fig. 3 for Gy 3-7.
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$\begin{figure} \par\includegraphics[width=6cm,clip]{H4203_5.ps} \end{figure}$	Figure 5: IRAS 12 $\mu$ m image of CMaR1. Open circles encompass vdB-RN 92 (right) and Gy 3-7 (left).
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4203_6.ps} \end{figure}$	Figure 6: vdB-RN 92: J,(J-H) CMD of the cluster region (filled circles) and comparison fields (open diamonds). Field 1 corresponds to the left panel and field 3 to the right one. All extractions have radius 1 $^\prime$ . No cutoff was used.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4203_8.ps} \end{figure}$	Figure 8: vdB-RN 92: J,(J-H) CMD of the cluster (filled circles) with PMS isochrones of 1 Myr (dashed line) and 7 Myr (dotted line). The ZAMS is represented by continuous line (Siess et al. 2000) and dashed-dotted line (Bertelli et al. 1994). Left panel presents the fit for the most massive star. Right panel presents the fit with A_J=1.21. Colour and magnitude errors are indicated.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4203_9.ps} \end{figure}$	Figure 9: Gy 3-7: J,(J-H) CMD of the cluster region (filled circles) and comparison star fields (open diamonds). Field 5 corresponds to the left panel and field 6 to the right one. All extractions have radius 1 $^\prime$ . No magnitude cutoff was used.
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$\begin{figure} \par\includegraphics[angle=270,width=8.8cm,clip]{H4203_10.ps} \end{figure}$	Figure 10: Gy 3-7: ( $(J-H),(H-K_{\rm s})$ ) diagram for the cluster (filled circles) and comparison field 5 (open diamonds). Triangle is the most luminous star in the object. Reference lines as in Fig. 7. A cutoff at $K_{\rm s} = 14.5$ was applied to minimize errors.
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