$\begin{figure} \par\includegraphics[height=22.7cm,width=17cm,clip]{1673fig1.eps} \end{figure}$ Figure 1: The ratio between the actual flux (F) and that computed using Eq. (5) (F'). Sloan filters, ATLAS models, log g= 4.5, solar abundance, microturbulet velocity = 2 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=4.8cm,clip]{1673fig2.eps} \end{figure}$ Figure 2: The linear coefficient u for ultraviolet bands. Continuous lines represent Strömgren u and asterisks denote Sloan u'. ATLAS models. log g= 4.5, solar abundance, microturbulet velocity = 2 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[height=13.8cm,width=16.2cm,clip]{1673fig3.eps} \end{figure}$ Figure 3: The linear coefficient u for u' g' r' i' z' following PHOENIX models (asterisks) and ATLAS (continuous line). log g= 4.5, solar abundance, microturbulet velocity = 2 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=4.8cm,clip]{1673fig4.eps} \end{figure}$ Figure 4: The profiles of the specific intensities following a non-linear law (Eq. (5)) for a model with $T_{\rm eff} = 5000$ K. PHOENIX models (dashed line) and ATLAS (continuous line). log g = 4.5, solar abundance, microturbulet velocity = 2 km s^-1.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=22.7cm,width=17cm,clip]{1673fig1.eps} \end{figure}$	Figure 1: The ratio between the actual flux (F) and that computed using Eq. (5) (F'). Sloan filters, ATLAS models, log g= 4.5, solar abundance, microturbulet velocity = 2 km s^-1.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=4.8cm,clip]{1673fig2.eps} \end{figure}$	Figure 2: The linear coefficient u for ultraviolet bands. Continuous lines represent Strömgren u and asterisks denote Sloan u'. ATLAS models. log g= 4.5, solar abundance, microturbulet velocity = 2 km s^-1.
Open with DEXTER

$\begin{figure} \par\includegraphics[height=13.8cm,width=16.2cm,clip]{1673fig3.eps} \end{figure}$	Figure 3: The linear coefficient u for u' g' r' i' z' following PHOENIX models (asterisks) and ATLAS (continuous line). log g= 4.5, solar abundance, microturbulet velocity = 2 km s^-1.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=4.8cm,clip]{1673fig4.eps} \end{figure}$	Figure 4: The profiles of the specific intensities following a non-linear law (Eq. (5)) for a model with $T_{\rm eff} = 5000$ K. PHOENIX models (dashed line) and ATLAS (continuous line). log g = 4.5, solar abundance, microturbulet velocity = 2 km s^-1.
Open with DEXTER