All Figures

$\begin{figure} \par\includegraphics[width=10.6cm,clip]{3593fig1.eps} \end{figure}$ Figure 1: IRAS 100 $\mu$ m emission map of the Chamaeleon cloud complex. Chamaeleon I and III-B are marked with rectangles, and positions of the reference fields used in the extinction calculation are marked with circles.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{3593fig2.eps}\hspace*{5mm} \includegraphics[width=7.25cm,clip]{3593fig3.eps} \end{figure}$ Figure 2: Left: integrated C¹⁸O intensity map of Chamaeleon I. The map is smoothed to correspond the 2.0' FWHM resolution of the extinction map (Fig. 4). The contour levels start from 0.5 K km s^-1 and the step is 0.2 K km s^-1. The numbers give the positions of some CO clumps identified by H05. Right: the same for Cha III-B. The contour levels start from 0.4 K km s^-1 and the step is 0.1 K km s^-1. The letters mark the most intense clumps identified by Gahm et al. (2002).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{3593fig4.eps}\hspace*{4mm} \includegraphics[width=6.6cm,clip]{3593fig5.eps} \end{figure}$ Figure 3: Left: color-color diagram of 2MASS stars with S/N > 10 in Cha I. Diamonds mark the previously identified YSOs from the list of Carpenter (2002). The solid curves are the intrinsic colors of unreddened stars (after Bessell & Brett 1988), and dashed lines tangenting these curves define the reddening sector. Right: the same for Cha III-B. Plus signs in the upper left corner of diagrams are the typical errors of colors.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3593fig6.eps} \end{figure}$ Figure 4: Visual extinction map of Chamaeleon I derived using the NICER color excess method (Lombardi & Alves 2001) and JHK photometry of 2MASS survey. The FWHM resolution of the map is 2.0'. The white pixels result from not having a single star within the FWHM range from the pixel centre, which means that the extinction in these pixels is higher than can be determined. The contour levels start from $A_V = 5^{\rm m}$ and the step is $2^{\rm m}$ . The letters mark the position of CO cores investigated in Fig. 7. White circles indicate the C¹⁸O cores of Mizuno et al. (1999) and the plus signs the very cold cores detected in the ISOPHOT Serendipity survey by Tóth et al. (2000).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3593fig7.eps} \end{figure}$ Figure 5: Visual extinction map of Chamaeleon III-B derived using the NICER color excess method (Lombardi & Alves 2001) and JHK photometry of 2MASS survey. The FWHM resolution of the map is 1.5'. The contour levels start from $A_V = 4^{\rm m}$ and the step is $1^{\rm m}$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{3593fig8.eps}\hspace*{8mm} \includegraphics[width=6.6cm,clip]{3593fig9.eps} \end{figure}$ Figure 6: Left: the average standard deviation of extinction as a function of star density in Cha I. The x-axis gives the number of stars within the FWHM range from the pixel center. Right: the same for Cha III-B.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=5.6cm,clip]{3593fi10.eps}\hspace*{1cm}... ...cm}\includegraphics[width=5.6cm,clip]{3593fi18.eps}\hspace*{3.2cm}} \end{figure}$ Figure 7: The correlations of N(C¹⁸O) and $A{_{\rm V}}$ in Cha I a), Cha III-B b), and in selected clumps of Cha I. The clump locations following Haikala et al. (2005): c) clumps 1 and 2, d) clump 8, e) clumps 4 and 7, f) clump 6, g) clump 12, h) (RA, Dec) = (11:05:19, -77:58:02), i) clump 21. The locations of the clumps are shown in Fig. 2.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3593fi19.eps} \end{figure}$ Figure 8: A tentative dust temperature map of Cha I derived from the ISO 100, 150 and 200 $\mu$ m observations (Lehtinen et al. in prep.). The numbers refer to some of the C¹⁸O clumps identified by H05. The temperature minimum coincides with the region of the clumps 4 and 7, revealing a prominent cold, heavily depleted core.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=10.6cm,clip]{3593fig1.eps} \end{figure}$	Figure 1: IRAS 100 $\mu$ m emission map of the Chamaeleon cloud complex. Chamaeleon I and III-B are marked with rectangles, and positions of the reference fields used in the extinction calculation are marked with circles.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3593fig7.eps} \end{figure}$	Figure 5: Visual extinction map of Chamaeleon III-B derived using the NICER color excess method (Lombardi & Alves 2001) and JHK photometry of 2MASS survey. The FWHM resolution of the map is 1.5'. The contour levels start from $A_V = 4^{\rm m}$ and the step is $1^{\rm m}$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{3593fig8.eps}\hspace*{8mm} \includegraphics[width=6.6cm,clip]{3593fig9.eps} \end{figure}$	Figure 6: Left: the average standard deviation of extinction as a function of star density in Cha I. The x-axis gives the number of stars within the FWHM range from the pixel center. Right: the same for Cha III-B.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=5.6cm,clip]{3593fi10.eps}\hspace{1cm}... ...cm}\includegraphics[width=5.6cm,clip]{3593fi18.eps}\hspace{3.2cm}} \end{figure}$	Figure 7: The correlations of N(C¹⁸O) and $A{_{\rm V}}$ in Cha I a), Cha III-B b), and in selected clumps of Cha I. The clump locations following Haikala et al. (2005): c) clumps 1 and 2, d) clump 8, e) clumps 4 and 7, f) clump 6, g) clump 12, h) (RA, Dec) = (11:05:19, -77:58:02), i) clump 21. The locations of the clumps are shown in Fig. 2.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3593fi19.eps} \end{figure}$	Figure 8: A tentative dust temperature map of Cha I derived from the ISO 100, 150 and 200 $\mu$ m observations (Lehtinen et al. in prep.). The numbers refer to some of the C¹⁸O clumps identified by H05. The temperature minimum coincides with the region of the clumps 4 and 7, revealing a prominent cold, heavily depleted core.
Open with DEXTER