All Figures

$\begin{figure} \par\includegraphics[width=5cm,height=8.25cm,angle=-90,clip]{2397... ...degraphics[width=5cm,height=8.3cm,angle=-90,clip]{2397fg1c.eps} \par\end{figure}$ Figure 1: SEDs of T Cha, Sz 68 and RU Lup. The photometry has been corrected for extinction using the corresponding optical extinction $A_{\rm {V}}$ given in Table 3. In this figure, photometric points from the literature and the 2MASS survey are given as filled squares, ISO points as filled diamonds and IRAS points as black x's. A typical star plus flat reprocessing disk fit to the spectra is shown in the case of Sz 68 as a dashed line. The presumed spectral type is also listed. Stars with their name underlined are known CTTS. Other symbols used are explained in the notes for the individual objects.
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In the text

$\begin{figure} \par {\includegraphics[width=5.0cm,height=8.3cm,angle=-90,clip]{2... ...,height=8.3cm,angle=-90,clip]{2397fg2c.eps} } \vspace{3mm} \par\par\end{figure}$ Figure 2: SEDs (cont.) of EX Lup, Sz 124 and ROX 2, as in Fig. 1.
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In the text

$\begin{figure} \par\vspace{-0.2mm} {\includegraphics[width=5cm,height=8.3cm,angl... ...,height=8.3cm,angle=-90,clip]{2397fg3c.eps} } \vspace{3mm} \par\par\end{figure}$ Figure 3: SEDs (cont.) of DoAr 24, DoAr 24E and SR 12, as in Fig. 1.
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In the text

$\begin{figure} \par {\includegraphics[width=5.0cm,height=8.3cm,angle=-90,clip]{2... ...,height=8.3cm,angle=-90,clip]{2397fg4c.eps} } \vspace{3mm} \par\par\end{figure}$ Figure 4: SEDs (cont.) of ROX 31, Wa Oph/4 and Wa Oph/6, as in Fig. 1.
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In the text

$\begin{figure} \par {\includegraphics[width=5.0cm,height=8.3cm,angle=-90,clip]{2... ...,height=8.3cm,angle=-90,clip]{2397fg5c.eps} } \vspace{3mm} \par\par\end{figure}$ Figure 5: SEDs (cont.) of IX Oph, V1725 Oph and CoKu Ser G1, as in Fig. 1.
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In the text

$\begin{figure} \par {\includegraphics[width=5.0cm,height=8.3cm,angle=-90,clip]{2... ...,height=8.3cm,angle=-90,clip]{2397fg6c.eps} } \vspace{3mm} \par\par\end{figure}$ Figure 6: SEDs (cont.) of CoKu Ser G7, V536 Aql and MacC H3, as in Fig. 1.
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In the text

$\begin{figure} \par {\includegraphics[scale=0.85,angle=-90,clip]{2397fg7.eps} } \par\par\end{figure}$ Figure 7: SED of Sz 68 A+B. Sz 68-A is represented by a black body of 4955 K fitted to R (continuous line). The squares are U to L band measurements of Sz 68-A, corrected for an $A_{\rm {V}}$ of 1.09. Sz 68-B is represented by a black body of 4000 K fitted to R (discontinuous line) with $A_{\rm {V}}$ = 0.75. The filled circles are the corresponding photometric measurements of Sz 68-B. The diamonds correspond to the fluxes obtained by ISO. The x's correspond to the fluxes obtained by IRAS. References for the photometry of Sz 68-A are given in Table 2. The photometry of the companion is from Hughes et al. (1994) for the R and I bands, and Geoffray & Monin (2001) for J, H, K and L.
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In the text

$\begin{figure} \par {\includegraphics[scale=0.85,angle=-90,clip]{2397fg8.eps} } \par\par\end{figure}$ Figure 8: SED of Sz 124 + Sz 124SE. The black body curve of 3917 K belongs to Sz 124, with the filled squares representing the star's photometry corrected for an $A_{\rm {V}}$ of 0.22. Full diamonds are ISO observations and x's IRAS. The filled circles correspond to the JHK photometry given by Hughes et al. (1994) for Sz 124SE, not corrected for extinction.
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In the text

$\begin{figure} \par {\includegraphics[scale=0.85,angle=-90,clip]{2397fg9.eps} } \par\par\end{figure}$ Figure 9: SED of the system DoAr 24E A+B. The continuous line is the photosphere of DoAr 24E-A: a black body of 5236 K fitted to R; the filled squares represent the corrected photometry of the star. The filled circles are the photometry given by Chelli et al. (1988), except for J from Ageorges et al. (1997), for the companion, not corrected for extinction. Full diamonds are ISO measurements. Crosses are IRAS measurements. Empty triangles are photometry at 10 and 20 $\mu$ m, from Chelli et al. (1988).
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In the text

$\begin{figure} \par {\includegraphics[scale=0.83,angle=-90,clip]{2397fg10.eps} } \par \par\par\end{figure}$ Figure 10: SED of the system SR 12 A+B. A is the photosphere of SR 12-A with the empty triangles representing the corrected photometry of the star. B is the photosphere of SR 12-B with the filled circles being the apparent JHKL photometry of the companion. The empty squares are the photometry observed for the whole system. The discontinuous line corresponds to the sum of the blackbody fits for the two stars. The diamonds correspond to the fluxes obtained with ISO. References for the photometry are given in Table 2, except for SR12-B and the whole system which are from Simon et al. (1987).
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In the text

$\begin{figure} \par {\includegraphics[scale=0.83,angle=-90,clip]{2397fg11.eps} } \par\par\end{figure}$ Figure 11: SED of Wa Oph/4 A and B. The continuous line is the photosphere of Wa Oph/4-A: a K4 black body (4500 K) fitted to V; the filled squares represent the corrected photometry for Wa Oph/4-A. The filled circles are the uncorrected photometry of the companion, Wa Oph/4-B. The diamonds correspond to the fluxes obtained by ISO. The x's correspond to the fluxes obtained by IRAS for Wa Oph/4. References for the photometry of the primary are given in Table 2. The photometry of the companion is from DENIS (I-band) and 2MASS (J, H and K bands).
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In the text

$\begin{figure} \par {\includegraphics[scale=0.83,angle=-90,clip]{2397fg12.eps} } \par\par\end{figure}$ Figure 12: SED of V1725 Oph (H $\alpha$ 3) and B62-H $\alpha$ 2 (H $\alpha$ 2). The continuous line is the photosphere of V1725 Oph: a black body of 3802 K (M0.5) fitted to V; the filled squares represent the corrected photometry of the star. The discontinuous line is the photosphere of B62-H $\alpha$ 2: a black body of 3500 K fitted to J, with the filled circles being the uncorrected photometry of this second star. The diamonds correspond to the fluxes obtained by ISO. The x's correspond to the fluxes obtained by IRAS for B62-H $\alpha$ 2. These fluxes could also come from V1725 Oph (Weaver & Jones 1992). References for the photometry of V1725 Oph are given in Table 2. The photometry of the nearby star is from Reipurth & Gee (1986).
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In the text

$\begin{figure} \par {\includegraphics[scale=0.83,angle=-90,clip]{2397fg13.eps} } \par\par\end{figure}$ Figure 13: SED of the system CoKu Ser G1 (HBC 667) and HBC 666. The black body curve belongs to CoKu Ser G1, with the filled squares representing the star's photometry (see references in Table 2) corrected for an $A_{\rm {V}}$ of 3.48. Full diamonds are ISO observations and x's IRAS. The filled circles correspond to the photometry of the companion HBC 666, not corrected for extinction, with V (20.4 mag), R (19.3 mag) and I (17.4 mag) from the observations taken in La Palma for this paper and J, H and K from 2MASS.
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In the text

$\begin{figure} \par {\includegraphics[scale=0.83,angle=-90,clip]{2397fg14.eps} } \par\par\end{figure}$ Figure 14: SED of the system V536 Aql A+B. A is the photosphere of V536 Aql-A: the squares represent the corrected photometry and the continuous line is a black body of 4000 K fitted to V. The filled circles are the uncorrected JHKL photometry of V536 Aql-B. The diamonds correspond to the fluxes obtained by ISO. The x's correspond to the fluxes obtained by IRAS. References for the photometry of V536 Aql-A are given in Table 2. The photometry of the companion is from Geoffray & Monin (2001).
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In the text

$\begin{figure} \par {\includegraphics[scale=0.60,angle=-90,clip]{2397fg15.eps} } \par \par\par\end{figure}$ Figure 15: H-R diagram with evolutionary tracks to estimate the masses and ages of the stars observed. Stars with their names underlined are CTTS. The others are WTTS. The ZAMS (thick continuous line) is from VandenBerg & Bridges (1984). The evolutionary tracks (thin continuous lines), isochrones (thin discontinuous lines) and birthline (thick discontinuous line) are from Palla & Stahler (1999).
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In the text

$\begin{figure} \par {\includegraphics[scale=0.65,angle=-90,clip]{2397fg16.eps} } \par \par\end{figure}$ Figure 16: In a), b) and c), $L_{\rm H\alpha }$ is in units of $L_{\odot }$ . In d), EW(H $\alpha$ ) is in Å. In the four figures: filled diamonds are the WTTS from our sample with possible circumstellar disks, filled circles are the WTTS from Cabrit et al. (1990), empty diamonds are the CTTS from our sample and empty circles are the CTTS from Cabrit et al. (1990). The Pearson product-moment correlation coefficients found between the different magnitudes are: a) 0.85, b) 0.85, c) 0.72, d) 0.53.
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In the text

$\begin{figure} \par {\includegraphics[width=5.0cm,height=8.3cm,angle=-90,clip]{2... ...,height=8.3cm,angle=-90,clip]{2397fg2c.eps} } \vspace{3mm} \par\par\end{figure}$	Figure 2: SEDs (cont.) of EX Lup, Sz 124 and ROX 2, as in Fig. 1.
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$\begin{figure} \par\vspace{-0.2mm} {\includegraphics[width=5cm,height=8.3cm,angl... ...,height=8.3cm,angle=-90,clip]{2397fg3c.eps} } \vspace{3mm} \par\par\end{figure}$	Figure 3: SEDs (cont.) of DoAr 24, DoAr 24E and SR 12, as in Fig. 1.
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$\begin{figure} \par {\includegraphics[width=5.0cm,height=8.3cm,angle=-90,clip]{2... ...,height=8.3cm,angle=-90,clip]{2397fg4c.eps} } \vspace{3mm} \par\par\end{figure}$	Figure 4: SEDs (cont.) of ROX 31, Wa Oph/4 and Wa Oph/6, as in Fig. 1.
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$\begin{figure} \par {\includegraphics[width=5.0cm,height=8.3cm,angle=-90,clip]{2... ...,height=8.3cm,angle=-90,clip]{2397fg5c.eps} } \vspace{3mm} \par\par\end{figure}$	Figure 5: SEDs (cont.) of IX Oph, V1725 Oph and CoKu Ser G1, as in Fig. 1.
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$\begin{figure} \par {\includegraphics[width=5.0cm,height=8.3cm,angle=-90,clip]{2... ...,height=8.3cm,angle=-90,clip]{2397fg6c.eps} } \vspace{3mm} \par\par\end{figure}$	Figure 6: SEDs (cont.) of CoKu Ser G7, V536 Aql and MacC H3, as in Fig. 1.
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$\begin{figure} \par {\includegraphics[scale=0.85,angle=-90,clip]{2397fg8.eps} } \par\par\end{figure}$	Figure 8: SED of Sz 124 + Sz 124SE. The black body curve of 3917 K belongs to Sz 124, with the filled squares representing the star's photometry corrected for an $A_{\rm {V}}$ of 0.22. Full diamonds are ISO observations and x's IRAS. The filled circles correspond to the JHK photometry given by Hughes et al. (1994) for Sz 124SE, not corrected for extinction.
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