All Figures

$\begin{figure} \resizebox{8.4cm}{!}{\includegraphics[clip]{2337fig1.ps}}\end{figure}$ Figure 1: Near infrared images of CC 04, CC 08, CC 13, and CC 14 ( top left, top right, bottom left, and bottom right, respectively). For images with multiband observations the J, H, and $K_{\rm S}$ are mapped onto blue, green and red, respectively. The individual images are 1.55 arcmin on the side. North is up, and East is to the left.
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{2337fig2.eps}}\end{figure}$ Figure 2: CC 04. Color-color diagram J-H versus $H-K_{\rm S}$ from the UFTI data. The size of the dots is proportional to the apparent brightness of the stars. The cross in the upper left corner demonstrates the typical measurement errors. The solid line shows the intrinsic colors of the main sequence stars from Frogel et al. (1978), extended to A0 spectral class, assuming zero magnitude colors for the A0 star. The dashed line indicates the colors of unreddened T Tau stars from Meyer et al. (1997). The reddening vectors for $A_{\rm V}=10$ mag are also plotted. The interval between ticks correspond to $\Delta A_{\rm V} =2$ mag.
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{2337fig3.eps}}\end{figure}$ Figure 3: CC 04: UFTI $M_{K_{\rm S}}$ versus $(J-K_{\rm S})_0$ color-magnitude diagrams of all stars in the cluster field (top left), the stars remaining in the cluster field after the decontamination (top center), and all stars in the sky field (top right). The zero-age main sequence from Schmidt-Kaler (1982) is plotted, and the stellar spectral types are indicated on the left. The reddening vectors for $A_{\rm V}=10$ mag are shown, with crosses spacing every 2 mag. The corresponding M_J-band luminosity functions are also given (bottom row). The theoretical luminosity functions from Storm et al. (1993) for 1, 3, and 10 Myr are plotted (dashed and solid lines, bottom center; bottom right) for comparison. A distance modulus of (m-M)₀=13.2 mag and reddening of $A_{\rm V}=0.6$ mag were adopted for all stars in both the cluster and the sky fields (see Sect. 3 for details).
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{2337fig4.eps}}\end{figure}$ Figure 4: CC 08. Color-color diagram J-H versus $H-K_{\rm S}$ from the UFTI data. The sequence of red supergiants from Bessell & Brett (1988) is shown with star symbols. See Fig. 2 for further explanations.
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{2337fig5.eps}}\end{figure}$ Figure 5: CC 08: UFTI $M_{K_{\rm S}}$ versus $(J-K_{\rm S})_0$ color-magnitude diagrams. The details are identical to Fig. 3, except for the omitted theoretical luminosity functions. A distance modulus of (m-M)₀=13.0 mag and reddening of $A_{\rm V}=3.0$ mag were adopted for all stars in both the cluster and the sky fields (see Sect. 4).
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{2337fig6.eps}}\end{figure}$ Figure 6: CC 13. Luminosity functions of the field of the cluster candidate (solid line) and a nearby sky field (dotted line).
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{2337fig7.eps}}\end{figure}$ Figure 7: CC 14. Color-color diagram J-H versus $H-K_{\rm S}$ from the UFTI data. See Fig. 2 for further explanations. The ticks on the reddening vectors here span 5 mag intervals.
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In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{2337fig8.eps}}\end{figure}$ Figure 8: CC 14: UFTI $M_{K_{\rm S}}$ versus $(J-K_{\rm S})_0$ color-magnitude diagrams. The details are identical to Fig. 3, except for the omitted theoretical luminosity functions. Distance modulus of (m-M)₀=15.8 mag and reddening of $A_{\rm V}=15.0$ mag were adopted for the stars on the decontaminated diagram. The stars in the other two panels were de-reddened with $A_{\rm V}=8.0$ mag (see Sect. 4).
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In the text

$\begin{figure} \resizebox{8.4cm}{!}{\includegraphics[clip]{2337fig1.ps}}\end{figure}$	Figure 1: Near infrared images of CC 04, CC 08, CC 13, and CC 14 ( top left, top right, bottom left, and bottom right, respectively). For images with multiband observations the J, H, and $K_{\rm S}$ are mapped onto blue, green and red, respectively. The individual images are 1.55 arcmin on the side. North is up, and East is to the left.
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$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{2337fig4.eps}}\end{figure}$	Figure 4: CC 08. Color-color diagram J-H versus $H-K_{\rm S}$ from the UFTI data. The sequence of red supergiants from Bessell & Brett (1988) is shown with star symbols. See Fig. 2 for further explanations.
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$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{2337fig5.eps}}\end{figure}$	Figure 5: CC 08: UFTI $M_{K_{\rm S}}$ versus $(J-K_{\rm S})_0$ color-magnitude diagrams. The details are identical to Fig. 3, except for the omitted theoretical luminosity functions. A distance modulus of (m-M)₀=13.0 mag and reddening of $A_{\rm V}=3.0$ mag were adopted for all stars in both the cluster and the sky fields (see Sect. 4).
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$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{2337fig6.eps}}\end{figure}$	Figure 6: CC 13. Luminosity functions of the field of the cluster candidate (solid line) and a nearby sky field (dotted line).
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$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{2337fig7.eps}}\end{figure}$	Figure 7: CC 14. Color-color diagram J-H versus $H-K_{\rm S}$ from the UFTI data. See Fig. 2 for further explanations. The ticks on the reddening vectors here span 5 mag intervals.
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