All Figures

$\begin{figure} \par\includegraphics[width=7.29cm,clip]{1416fig1.eps}\vspace*{5mm} \includegraphics[width=7.29cm,clip]{1416fig2.eps}\end{figure}$ Figure 1: Linear fit of F_V(V-K) (upper part) and the corresponding residuals (lower part). The fitted coefficients are given in Table 4.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{aa1416f2.eps}\end{figure}$ Figure 2: Surface brightness F_V relations as a function of color. The error bars have been omitted for clarity, and the fitted models are represented alternatively as solid and dashed lines. From left to right, using the colors: (V-B), (V-I), (V-J), (V-H) and (V-K). The zero-axis intersection does not happen at the same point for all relations.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{1416fig4.eps}\end{figure}$ Figure 3: Specific F_V(V-K) relation fits for $\eta$ Aql, $\zeta$ Gem and $\ell$ Car. The error bars have been omitted for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{1416fig5.eps}\vspace*{5mm} \includegraphics[width=7.65cm,clip]{1416fig6.eps}\end{figure}$ Figure 4: Comparison of the positions of the Cepheids (solid dots) and dwarfs (open squares) in the F_V(B-V) diagram. The lower part of the figure shows an enlargement of the Cepheid color range.The error bars have been omitted for clarity.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{1416fig7.eps}\vspace*{5mm} \includegraphics[width=7.65cm,clip]{1416fig8.eps}\end{figure}$ Figure 5: Comparison of the positions of the Cepheids (solid dots) and dwarfs (open squares) in the F_V(V-K) diagram. The dashed line represents the best fit SB-color relation for dwarf stars and the solid line for Cepheids. The lower part of the figure is an enlargement of the Cepheid color range.
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In the text

$\begin{figure} \par\includegraphics[width=7.29cm,clip]{1416fig1.eps}\vspace*{5mm} \includegraphics[width=7.29cm,clip]{1416fig2.eps}\end{figure}$	Figure 1: Linear fit of F_V(V-K) (upper part) and the corresponding residuals (lower part). The fitted coefficients are given in Table 4.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{aa1416f2.eps}\end{figure}$	Figure 2: Surface brightness F_V relations as a function of color. The error bars have been omitted for clarity, and the fitted models are represented alternatively as solid and dashed lines. From left to right, using the colors: (V-B), (V-I), (V-J), (V-H) and (V-K). The zero-axis intersection does not happen at the same point for all relations.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{1416fig4.eps}\end{figure}$	Figure 3: Specific F_V(V-K) relation fits for $\eta$ Aql, $\zeta$ Gem and $\ell$ Car. The error bars have been omitted for clarity.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{1416fig5.eps}\vspace*{5mm} \includegraphics[width=7.65cm,clip]{1416fig6.eps}\end{figure}$	Figure 4: Comparison of the positions of the Cepheids (solid dots) and dwarfs (open squares) in the F_V(B-V) diagram. The lower part of the figure shows an enlargement of the Cepheid color range.The error bars have been omitted for clarity.
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$\begin{figure} \par\includegraphics[width=7.65cm,clip]{1416fig7.eps}\vspace*{5mm} \includegraphics[width=7.65cm,clip]{1416fig8.eps}\end{figure}$	Figure 5: Comparison of the positions of the Cepheids (solid dots) and dwarfs (open squares) in the F_V(V-K) diagram. The dashed line represents the best fit SB-color relation for dwarf stars and the solid line for Cepheids. The lower part of the figure is an enlargement of the Cepheid color range.
Open with DEXTER