All Figures

$\begin{figure} \par\includegraphics[angle=90,width=7.7cm,clip]{aah4315-fig1.ps} \end{figure}$ Figure 1: A comparison of the MARCS ("M''), Kurucz ("K'') and Allard & Hauschildt ("A&H'') model atmospheres. Calculated line profiles of the Ca I 6122.2 Å line are shown in the upper panel for the three models. From top to bottom these are the "M'', "K'' and "A&H'' models. In the lower panel we show the ratio of the calculated line profiles. The continuous line is ("M'' / "K'') and the dashed line ("A&H'' / "K''). Units for the horizontal axis are Å.
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In the text

$\begin{figure} \par\includegraphics[width=115mm, height=14cm]{aah4315-fig2.ps} \end{figure}$ Figure 2: A selection of representative spectral regions that were used to determine the veiling factor in the Sun. We plot the observations (thin line), the veiled synthetic spectrum (thick line) and the contribution of the veiling continuum (dashed line). The residual of the observations and the veiled synthetic spectrum is also shown (thin line near the horizontal axis). The dark grey areas were used to establish the continuum level of the observations and the white areas were excluded when determining the veiling factor. Units for the horizontal axis are Å.
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In the text

$\begin{figure}\par\includegraphics[width=115mm, height=14cm]{aah4315-fig3.ps} \end{figure}$ Figure 3: Same as Fig. 2, but for 61 Cyg A. Note that for this star the selection of wavelength regions is slightly different (see Sect. 3.5).
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In the text

$\begin{figure}\par\includegraphics[width=115mm, height=14cm]{aah4315-fig4.ps}\end{figure}$ Figure 4: Same as Fig. 2, but for CT Cha.
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In the text

$\begin{figure}\par\includegraphics[width=115mm, height=14cm]{aah4315-fig5.ps} \end{figure}$ Figure 5: Same as Fig. 2, but for CV Cha.
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In the text

$\begin{figure}\par\includegraphics[width=115mm, height=14cm]{aah4315-fig6.ps}\end{figure}$ Figure 6: Same as Fig. 2, but for RU Lup.
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In the text

$\begin{figure}\par\includegraphics[width=115mm, height=14cm]{aah4315-fig7.ps}\end{figure}$ Figure 7: Same as Fig. 2, but for RY Lup.
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In the text

$\begin{figure} \par\includegraphics[width=10.2cm,height=12cm,clip]{aah4315-fig8.ps} \end{figure}$ Figure 8: Same as Fig. 2, but for Sz 68.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=90,width=8cm]{aah4315-fig9-1.ps}... ...7.ps} } \par\includegraphics[angle=90,width=8cm]{aah4315-fig9-6.ps} \end{figure}$ Figure 9: Spectra of the veiling factor (upper panel in each plot) and the veiling flux (lower panel). Units for the veiling flux are ergs s^-1 cm^-2, and units for the horizontal axis are Å. The veiling flux is obtained by multiplying the recovered values of the veiling factor with the model atmosphere continuum flux, which is shown for comparison in the lower panel (full line). For CV Cha, CT Cha and RU Lup several spectra are plotted in the same figure.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=16cm,clip]{aah4315-fig10.ps} \end{figure}$ Figure 10: This plot shows in detail the quality of the obtained solutions for the level of veiling in RU Lup. These panels show the regions in the spectrum of RU Lup that were not included in Fig. 6. The high values of veiling recovered in the region 5000-5500 (see Fig. 9) are not due to misinterpretation of strong line emission. Large regions without strong line emission are present in all panels. A high value for the veiling factor is also recovered for the region 5600-5650 which is void of emission lines.
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In the text

$\begin{figure}\par\includegraphics[width=8.4cm]{aah4315-fig11.ps} \end{figure}$ Figure 11: This figure shows the distribution of the line depth versus wavelength of Fe lines that are present in the VALD database. The line depths were calculated for $T_{\rm eff}$ 4000 K and $\log g=4$ . Within the observerd wavelength range, the ratio of strong and weak lines changes very slowly. Therefore, we do not expect emission from an ensemble of weak lines to be able to cause excess veiling values in the range 5500-5700 Å where no strong line emission is seen.
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In the text

$\begin{figure}\par\includegraphics[width=115mm, height=14cm]{aah4315-fig3.ps} \end{figure}$	Figure 3: Same as Fig. 2, but for 61 Cyg A. Note that for this star the selection of wavelength regions is slightly different (see Sect. 3.5).
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$\begin{figure}\par\includegraphics[width=115mm, height=14cm]{aah4315-fig4.ps}\end{figure}$	Figure 4: Same as Fig. 2, but for CT Cha.
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$\begin{figure}\par\includegraphics[width=115mm, height=14cm]{aah4315-fig5.ps} \end{figure}$	Figure 5: Same as Fig. 2, but for CV Cha.
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$\begin{figure}\par\includegraphics[width=115mm, height=14cm]{aah4315-fig6.ps}\end{figure}$	Figure 6: Same as Fig. 2, but for RU Lup.
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$\begin{figure}\par\includegraphics[width=115mm, height=14cm]{aah4315-fig7.ps}\end{figure}$	Figure 7: Same as Fig. 2, but for RY Lup.
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$\begin{figure} \par\includegraphics[width=10.2cm,height=12cm,clip]{aah4315-fig8.ps} \end{figure}$	Figure 8: Same as Fig. 2, but for Sz 68.
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