Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=6.3cm,height=5.4cm]{1429f1a.ps}\hspace... ...space*{1.7cm} \includegraphics[width=6.3cm,height=5.4cm]{1429f1d.ps}\end{figure}$ Figure 1: The spatial distribution of the 2MASS sources toward the RMC as a function of the H-Ks colour: a) sources with $H-K{\rm s}<0.2$ , b) $0.2<H-K{\rm s}<0.5$ , c) $H-K{\rm s}>0.5$ , d) $H-K{\rm s}>1.0$ mag. Contours of the IRAS 100 $\mu$ m emission are overplotted to elucidate the spatial distribution of the embedded clusters with respect to the highly clumped cloud structure. Well defined regions of clustered star formation are marked as A, B, C and D with the extent of stellar groups further delineated by dotted circles or rectangles according to their individual appearance. The dashed circle drawn at the upper right of all plots indicates the location of the young open cluster NGC 2444 and, consequently, the H II region.
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In the text

$\begin{figure} \par\includegraphics[width=8.cm]{1429f2a.ps}\vspace*{0.5cm} {\hspace*{1cm}\includegraphics[width=6.1cm]{1429f2b.ps}\hspace*{1cm}} \end{figure}$ Figure 2: Spatial distribution of the sources in Regions A ( upper panel) and B ( lower panel). Subcluster members are overplotted on the distribution of optical depth at 100 $\mu$ m of the corresponding fields, which clearly illustrate the well-confined shell structures. The samples with $H-K{\rm s}>0.5$ are displayed.
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In the text

$\begin{figure} \par\includegraphics[width=6.2cm]{1429f3a.eps}\vspace*{0.4cm} \includegraphics[width=6.2cm]{1429f3b.eps}\end{figure}$ Figure 3: The two-point correlation functions for the clusters embedded in Regions A ( top panel) and B ( lower panel). The full, dotted and dashed lines correspond to samples with $H-K{\rm s} >0.7$ , >0.5 and >0.2, respectively. The inset panels display the spatial distributions for $H-K{\rm s} >0.7$ . The error bars correspond to $\surd$ N statistics.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm]{1429f4a.ps}\hspace*{0.5cm} \inc... ...ce*{4.5cm}\includegraphics[width=7.7cm]{1429f4c.ps}\hspace*{4.5cm}} \end{figure}$ Figure 4: Colour-colour diagrams of a) the reference field with a diameter of 40 $^\prime$ and the clusters in b) Region A and c) Region B. The source with the highest H-Ks colour excess in each cluster is overplotted with a bold type diamond. Solid lines represent the loci of the main-sequence dwarves and giant stars (Bessell & Brett 1988). The arrow in the upper left of the plot shows a reddening vector of $A_{\rm V}=5$ mag (Rieke et al. 1985). The dot-dashed line indicates the locus of dereddened T Tauri stars (Meyer et al. 1997). The dashed lines define the reddening band for the normal stars and T Tauri stars, drawn parallel to the reddening vector. Crosses are overplotted at intervals corresponding to 5 mag of visual extinction.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1429f5a.ps}\par\vspace*{0.4cm} \par\includegraphics[width=8.6cm,clip]{1429f5b.ps}\end{figure}$ Figure 5: Colour-Magnitude Diagrams of the clusters in Regions A and B. The source with the highest H-Ks colour excess in each diagram is overplotted with a bold diamond, and criteria missed candidate young stars are presented as pluses. The main sequence for stars with masses between 0.8 and 120 $M_\odot$ is plotted as a solid line (Lejeune & Schaerer 2001). The slanted line with an arrow at the tip denotes a reddening of $A_{\rm V} = 20$ mag of a A0 type dwarf.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1429f6.ps}\end{figure}$ Figure 6: The Ks Luminosity Function of the clusters in Regions A and B. The KLF of the Region A cluster is plotted as a solid line, and of the Region B cluster as a dotted line. It is evident that the clusters have a very similar slope of >0.3 in the range $11.0 < K{\rm s}<14.5$ , signifying that they have ages of around 1 Myr and are still in their early stages of evolution.
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In the text

$\begin{figure} \par\includegraphics[width=8.cm]{1429f2a.ps}\vspace{0.5cm} {\hspace{1cm}\includegraphics[width=6.1cm]{1429f2b.ps}\hspace*{1cm}} \end{figure}$	Figure 2: Spatial distribution of the sources in Regions A ( upper panel) and B ( lower panel). Subcluster members are overplotted on the distribution of optical depth at 100 $\mu$ m of the corresponding fields, which clearly illustrate the well-confined shell structures. The samples with $H-K{\rm s}>0.5$ are displayed.
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$\begin{figure} \par\includegraphics[width=6.2cm]{1429f3a.eps}\vspace*{0.4cm} \includegraphics[width=6.2cm]{1429f3b.eps}\end{figure}$	Figure 3: The two-point correlation functions for the clusters embedded in Regions A ( top panel) and B ( lower panel). The full, dotted and dashed lines correspond to samples with $H-K{\rm s} >0.7$ , >0.5 and >0.2, respectively. The inset panels display the spatial distributions for $H-K{\rm s} >0.7$ . The error bars correspond to $\surd$ N statistics.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1429f6.ps}\end{figure}$	Figure 6: The Ks Luminosity Function of the clusters in Regions A and B. The KLF of the Region A cluster is plotted as a solid line, and of the Region B cluster as a dotted line. It is evident that the clusters have a very similar slope of >0.3 in the range $11.0 < K{\rm s}<14.5$ , signifying that they have ages of around 1 Myr and are still in their early stages of evolution.
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