All Figures

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{6541fig1.ps}\end{figure}$ Figure 1: Selected evolutionary tracks with Z = 0.0001 and [ $\alpha$ /Fe] = 0.4 in comparison with the predicted FOBE, FBE and FRE. At luminosity levels brighter than the intersection between FOBE and FBE, we found only fundamental models.
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In the text

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{6541fig2.ps}\end{figure}$ Figure 2: Period-magnitude diagrams of fundamental pulsators with $l/H_{\rm p}$ = 1.5, Z = 0.0001 and [ $\alpha$ /Fe] = 0.4.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{6541fig3.ps}\end{figure}$ Figure 3: Selected period-Wesenheit diagrams of fundamental pulsators with $l/H_{\rm p}$ = 1.5, Z = 0.0001 and [ $\alpha$ /Fe] = 0.4.
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In the text

$\begin{figure} \par\includegraphics[width=6.85cm,clip]{6541fig4.ps}\end{figure}$ Figure 4: $\it WBV$ function versus period of selected fundamental pulsators with $l/H_{\rm p}$ = 1.5. The solid and dashed lines are the linear and quadratic fits, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{6541fig5.ps}\end{figure}$ Figure 5: $\it PM$ and $\it PW$ distributions of observed P2Cs under two different assumptions on the absolute magnitude of RR Lyrae stars. The numbers in parentheses are the slopes of the relations, as derived by a linear regression to the data. The arrow indicates V7 in NGC 6341. The infrared magnitudes are taken from Matsunaga et al. (2006).
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{6541fig6.ps}\end{figure}$ Figure 6: $\it PM$ and $\it PW$ distributions of observed P2Cs under two different assumptions on the absolute magnitude of RR Lyrae stars. The outliers are V24 and V28 in NGC 4372, V12 and V32 in NGC 6205 and V3 in NGC 6254. The optical magnitudes are taken from Pritzl et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{6541fig1.ps}\end{figure}$	Figure 1: Selected evolutionary tracks with Z = 0.0001 and [ $\alpha$ /Fe] = 0.4 in comparison with the predicted FOBE, FBE and FRE. At luminosity levels brighter than the intersection between FOBE and FBE, we found only fundamental models.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.15cm,clip]{6541fig2.ps}\end{figure}$	Figure 2: Period-magnitude diagrams of fundamental pulsators with $l/H_{\rm p}$ = 1.5, Z = 0.0001 and [ $\alpha$ /Fe] = 0.4.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{6541fig3.ps}\end{figure}$	Figure 3: Selected period-Wesenheit diagrams of fundamental pulsators with $l/H_{\rm p}$ = 1.5, Z = 0.0001 and [ $\alpha$ /Fe] = 0.4.
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$\begin{figure} \par\includegraphics[width=6.85cm,clip]{6541fig4.ps}\end{figure}$	Figure 4: $\it WBV$ function versus period of selected fundamental pulsators with $l/H_{\rm p}$ = 1.5. The solid and dashed lines are the linear and quadratic fits, respectively.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{6541fig5.ps}\end{figure}$	Figure 5: $\it PM$ and $\it PW$ distributions of observed P2Cs under two different assumptions on the absolute magnitude of RR Lyrae stars. The numbers in parentheses are the slopes of the relations, as derived by a linear regression to the data. The arrow indicates V7 in NGC 6341. The infrared magnitudes are taken from Matsunaga et al. (2006).
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{6541fig6.ps}\end{figure}$	Figure 6: $\it PM$ and $\it PW$ distributions of observed P2Cs under two different assumptions on the absolute magnitude of RR Lyrae stars. The outliers are V24 and V28 in NGC 4372, V12 and V32 in NGC 6205 and V3 in NGC 6254. The optical magnitudes are taken from Pritzl et al. (2003).
Open with DEXTER