All Figures

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{7210fig01.eps} \end{figure}$ Figure 1: Colour composite of the long-exposure observed field of view in J (blue), H (green) and $K_{\rm s}$ (red). North is up and east is to the left.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig02.eps}} \end{figure}$ Figure 2: NACO H band image of the central area of Tr14. The intensity scale is logarithmic. North is up and east is to the left.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig03.eps}} \end{figure}$ Figure 3: $K_{\rm s}$ -band contour plot of the stellar density distribution from the SOFI and NACO data. The highest and lowest density contours correspond to 2330 and 330 sources/arcmin², respectively.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig04.eps}} \end{figure}$ Figure 4: $K_{\rm s}$ -band radial stellar density distribution from the SOFI and NACO data. The solid line is our best fit to a King (1962) profile.
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In the text

$\begin{figure} \par\includegraphics[width=17cm]{7210fig05.eps} \end{figure}$ Figure 5: Left panel: (J-H) vs. $(H-K_{\rm s})$ colour-colour diagram for the SOFI data. The brightest objects have larger symbols and the dashed lines define the reddening band of Rieke & Lebofsky (1985). Middle panel: $K_{\rm s}$ vs. $(H-K_{\rm s})$ colour-magnitude diagram for the SOFI data. Right panel: $K_{\rm s}$ vs. $(J-K_{\rm s})$ colour-magnitude diagram for the SOFI data.
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In the text

$\begin{figure} \par\includegraphics[width=17cm]{7210fig06.eps} \end{figure}$ Figure 6: Same as Fig. 5 but with the main sequence of Bessell & Brett (1988) ( left panel) and of Lejeune & Schaerer (2001) ( middle and right panels) reddened by $A_{\rm v}=0.5$ , 1.4, and 2.6 mag.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig07.eps}} \end{figure}$ Figure 7: Spatial distribution of the sources in the blue and red sequences ( blue circles and red circles, see text). The light contours are the same as in Fig. 3 (surface density contour distribution).
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In the text

$\begin{figure} \par\includegraphics[width=17cm]{7210fig08.eps} \end{figure}$ Figure 8: Left panel: 2MASS stellar density map in the area containing and surrounding Tr14. The darkest areas correspond to the highest densities. The locations of Tr14 and Tr16 (namely $\eta$ Car) are indicated with a star and the appropriate indication. Right panel: radial density profile for the same 2MASS data. The bins are $12\hbox {$^{\prime \prime }$ }$ wide.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{7210fig09.eps} \end{figure}$ Figure 9: Left panel: (J-H) vs. $(H-K_{\rm s})$ colour-colour diagram for the cluster, highlighting the sources used to build the extinction map as black filled circles. Right panel: background extinction map for the central area of our field. The darker contours are for higher extinctions, and the star symbol represents the position of the O2.
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In the text

$\begin{figure} \par\includegraphics[width=17cm]{7210fig10.eps} \end{figure}$ Figure 10: Left panel: (J-H) - ( $H-K_{\rm s}$ ) colour-colour diagram for the SOFI data. The solid line on the data represents the main-sequence of Bessell & Brett (1988) reddened by $A_{\rm v}=2.6$ mag. Right panel: (J-H) - ( $K_{\rm s}-L'$ ) colour-colour diagram for the NACO data.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig11.eps}} \end{figure}$ Figure 11: Left panel: $K_{\rm s}$ vs. $(J-K_{\rm s})$ colour-magnitude diagram for the NACO data ( black stars) superposed on the SOFI data ( gray plus signs). Right panel: location of the sources from ANCHORS detected in X-rays ( black stars) superposed on the SOFI data ( gray plus signs) on the $K_{\rm s}$ vs. $(J-K_{\rm s})$ colour-magnitude diagram.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig12.eps}} \end{figure}$ Figure 12: Spatial distribution of the sources detected with Chandra (ANCHORS database). The light contours are the same as in Fig. 3 (surface density contour distribution).
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In the text

$\begin{figure} \par\includegraphics[width=17cm]{7210fig13.eps} \end{figure}$ Figure 13: $K_{\rm s}$ vs. $(J-K_{\rm s})$ colour-magnitude diagram for the SOFI data without( left panel) and with ( right panel) the PMS isochrones of Palla & Stahler (1993): 0.0-0.3 Myr ( blue), 1.4-2.5 Myr ( orange), and 3.2-5.0 Myr ( red).
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In the text

$\begin{figure} \par\includegraphics[width=17cm]{7210fig14.eps} \end{figure}$ Figure 14: Left panel: $K_{\rm s}$ -luminosity function for the SOFI data. The light and dark lines represent the function before and after the control field subtraction, respectively. Right panel: $K_{\rm s}$ -luminosity function for the NACO data. No control field subtraction was applied.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig15.eps}} \end{figure}$ Figure 15: Location of the proplyd candidates identified by Smith et al. (2003) in our SOFI images. From left to right, using their nomenclature: (e) (104339.1-593257 and 104339.8-593247), (f) (104402.8-593209, 104402.3-593214, and 104402.5-593218), (g) (104411.2-593325) and (i) (104359.6-593238). In the colour images blue is J, green is H, and red is $K_{\rm s}$ . The leftmost image is black and white because it is only present in our $K_{\rm s}$ -band image.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig16.eps}} \end{figure}$ Figure 16: Left: compact nebula around a B star located at $10^{\rm h}44^{\rm m}05\hbox{$.\!\!^{\rm s}$ }1$ , $-59^\circ 33\hbox {$^\prime $ }41\hbox {$^{\prime \prime }$ }$ in the surveyed field. Blue is J, green is H, and red is $K_{\rm s}$ . Right: extended feature ( $10^{\rm h}43^{\rm m}57\hbox{$.\!\!^{\rm s}$ }3$ , $-59^\circ32'57\hbox{$.\!\!^{\prime\prime}$ }59$ ) detected in the $L^{\prime }$ -band. North is up and east is to the left in both images.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{7210fig01.eps} \end{figure}$	Figure 1: Colour composite of the long-exposure observed field of view in J (blue), H (green) and $K_{\rm s}$ (red). North is up and east is to the left.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig02.eps}} \end{figure}$	Figure 2: NACO H band image of the central area of Tr14. The intensity scale is logarithmic. North is up and east is to the left.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig03.eps}} \end{figure}$	Figure 3: $K_{\rm s}$ -band contour plot of the stellar density distribution from the SOFI and NACO data. The highest and lowest density contours correspond to 2330 and 330 sources/arcmin², respectively.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig04.eps}} \end{figure}$	Figure 4: $K_{\rm s}$ -band radial stellar density distribution from the SOFI and NACO data. The solid line is our best fit to a King (1962) profile.
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$\begin{figure} \par\includegraphics[width=17cm]{7210fig05.eps} \end{figure}$	Figure 5: Left panel: (J-H) vs. $(H-K_{\rm s})$ colour-colour diagram for the SOFI data. The brightest objects have larger symbols and the dashed lines define the reddening band of Rieke & Lebofsky (1985). Middle panel: $K_{\rm s}$ vs. $(H-K_{\rm s})$ colour-magnitude diagram for the SOFI data. Right panel: $K_{\rm s}$ vs. $(J-K_{\rm s})$ colour-magnitude diagram for the SOFI data.
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$\begin{figure} \par\includegraphics[width=17cm]{7210fig06.eps} \end{figure}$	Figure 6: Same as Fig. 5 but with the main sequence of Bessell & Brett (1988) ( left panel) and of Lejeune & Schaerer (2001) ( middle and right panels) reddened by $A_{\rm v}=0.5$ , 1.4, and 2.6 mag.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig07.eps}} \end{figure}$	Figure 7: Spatial distribution of the sources in the blue and red sequences ( blue circles and red circles, see text). The light contours are the same as in Fig. 3 (surface density contour distribution).
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$\begin{figure} \par\includegraphics[width=17cm]{7210fig08.eps} \end{figure}$	Figure 8: Left panel: 2MASS stellar density map in the area containing and surrounding Tr14. The darkest areas correspond to the highest densities. The locations of Tr14 and Tr16 (namely $\eta$ Car) are indicated with a star and the appropriate indication. Right panel: radial density profile for the same 2MASS data. The bins are $12\hbox {$^{\prime \prime }$ }$ wide.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{7210fig09.eps} \end{figure}$	Figure 9: Left panel: (J-H) vs. $(H-K_{\rm s})$ colour-colour diagram for the cluster, highlighting the sources used to build the extinction map as black filled circles. Right panel: background extinction map for the central area of our field. The darker contours are for higher extinctions, and the star symbol represents the position of the O2.
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$\begin{figure} \par\includegraphics[width=17cm]{7210fig10.eps} \end{figure}$	Figure 10: Left panel: (J-H) - ( $H-K_{\rm s}$ ) colour-colour diagram for the SOFI data. The solid line on the data represents the main-sequence of Bessell & Brett (1988) reddened by $A_{\rm v}=2.6$ mag. Right panel: (J-H) - ( $K_{\rm s}-L'$ ) colour-colour diagram for the NACO data.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig11.eps}} \end{figure}$	Figure 11: Left panel: $K_{\rm s}$ vs. $(J-K_{\rm s})$ colour-magnitude diagram for the NACO data ( black stars) superposed on the SOFI data ( gray plus signs). Right panel: location of the sources from ANCHORS detected in X-rays ( black stars) superposed on the SOFI data ( gray plus signs) on the $K_{\rm s}$ vs. $(J-K_{\rm s})$ colour-magnitude diagram.
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$\begin{figure} \par\resizebox{8.8cm}{!}{\includegraphics{7210fig12.eps}} \end{figure}$	Figure 12: Spatial distribution of the sources detected with Chandra (ANCHORS database). The light contours are the same as in Fig. 3 (surface density contour distribution).
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$\begin{figure} \par\includegraphics[width=17cm]{7210fig13.eps} \end{figure}$	Figure 13: $K_{\rm s}$ vs. $(J-K_{\rm s})$ colour-magnitude diagram for the SOFI data without( left panel) and with ( right panel) the PMS isochrones of Palla & Stahler (1993): 0.0-0.3 Myr ( blue), 1.4-2.5 Myr ( orange), and 3.2-5.0 Myr ( red).
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$\begin{figure} \par\includegraphics[width=17cm]{7210fig14.eps} \end{figure}$	Figure 14: Left panel: $K_{\rm s}$ -luminosity function for the SOFI data. The light and dark lines represent the function before and after the control field subtraction, respectively. Right panel: $K_{\rm s}$ -luminosity function for the NACO data. No control field subtraction was applied.
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