All Figures

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{8206f1.ps} \end{figure}$ Figure 1: From bottom to top: the average mass M(RR) in solar units, the absolute visual magnitude M_V(RR), and the evolutionary parameter $k(1.5)_{\rm ev}$ as a function of the HB type. Current predictions rely on a set of SHB simulations discussed in Paper IV.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f2.ps} \end{figure}$ Figure 2: The HB type versus the metal content [Fe/H]_K for Oosterhoff type II (OoII, filled circles) and Oosterhoff type I (OoI, open circles) Galactic globular clusters. The error bars have been estimated by assuming $\epsilon {\rm (HB)}=\pm 0.1$ and $\epsilon [{\rm Fe/H}]_K=\pm 0.1$ For $\omega$ Cen (asterisk), we plot the average value [Fe/H] $_R=-1.62\pm 0.27$ derived by Rey et al. (2000).
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{8206f3.ps} \end{figure}$ Figure 3: Visual amplitude versus period for RR_ab stars in Oosterhoff type II (OoII, top panel) and Oosterhoff type I (OoI, bottom panel) globular clusters. The solid line shows the ridge line of variables in OoII clusters and is based on the predicted slope $\delta\log P_F/\delta A_V=-$ 0.189.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f4.ps} \end{figure}$ Figure 4: The average $\langle k(1.5)_{\rm puls}\rangle$ ( bottom panel) and $\langle k(2.0)_{\rm puls}\rangle$ ( top panel) values for RR_ab stars in Oosterhoff type I (OoI, open circles) and Oosterhoff type II (OoII, filled circles) globular clusters plotted as a function of the cluster HB type.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f5.ps} \end{figure}$ Figure 5: The average $\langle k(1.5)_{\rm puls}\rangle$ ( bottom panel) and $\langle k(2.0)_{\rm puls}\rangle$ ( top panel) values for RR_ab stars in Oosterhoff type I (OoI, open circles) and Oosterhoff type II (OoII) globular clusters as a function of metal abundance. The filled circles mark OoII clusters with HB type ranging from red to moderately blue, while the filled squares refer to those with very blue HB type. The dashed and the dotted lines in the bottom panel display two different choices in the selection of the calibrating clusters. See text for more details.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f6.ps} \end{figure}$ Figure 6: Same as in Fig. 3, but for RR_ab stars in the two peculiar clusters NGC 6441 (triangles) and $\omega$ Cen (asterisks).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f7.ps} \end{figure}$ Figure 7: The $k(1.5)_{\rm puls}$ ( bottom panel) and the $k(2.0)_{\rm puls}$ ( top panel) parameter for RR_ab stars in $\omega$ Cen (asterisks) as a function of the metal abundance. Open circles, filled circles, and filled squares display Galactic globular clusters and have the same meaning as in Fig. 5.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f8.ps} \end{figure}$ Figure 8: Distribution of the $k(1.5)_{\rm puls}$ parameter for RR_ab stars in $\omega$ Cen ( bottom panel) together with OoI and OoII Galactic globular clusters.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f9.ps} \end{figure}$ Figure 9: RR_ab stars in the solar neighborhood with measured [Fe/H] abundances ( top panel; Layden 2007, private communication) and visual amplitudes ( bottom panel; Nikolov et al. 1984). The arrows mark the shortest period observed in OoI and OoII Galactic globular clusters. The solid line shows the predicted ridge line for cluster OoII variables (see Fig. 3).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f10.ps} \end{figure}$ Figure 10: Difference between the observed and the calculated [Fe/H] versus period for all the stars in Fig. 9.
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In the text

$\begin{figure} \par\includegraphics[width=5.5cm,clip]{8206f11.ps} \end{figure}$ Figure 11: Residuals to Eq. (3) for all the fundamental models from Z=0.0001 to Z=0.02.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f12.ps} \end{figure}$ Figure 12: Pulsational parameter $k(1.5)_{\rm puls}$ as a function of metal abundance [Fe/H]_L for all the field RR_ab stars plotted in Fig. 9. The average values for Galactic globular clusters (symbols as in Fig. 5) and NGC 6441 (triangle) are also shown.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f13.ps} \end{figure}$ Figure 13: Left panel: mean absolute magnitude of RR_ab stars in Galactic globular clusters versus $\langle k_{\rm puls}\rangle$ for $l/H_{\rm p}=1.5$ and by adopting scaled-solar chemical compositions and the solar ratio $(Z/X)_{\odot }=0.0245$ . The symbols are the same as in Fig. 5. The solid line is Eq. (5), while the dashed lines have a brighter zero-point (0.05 mag). Right panel: same as in the left panel, but with $l/H_{\rm p}=2.0$ . The solid line is Eq. (6).
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f14.ps} \end{figure}$ Figure 14: Mean absolute visual magnitudes $\langle M_V^{k(1.5)}\rangle$ ( bottom panel) and $\langle M_V^{k(2.0}\rangle$ ( top panel) of RR_ab stars in Galactic globular clusters versus [Fe/H]_K, according to scaled-solar chemical compositions and a solar ratio $(Z/X)_{\odot }=0.0245$ . The symbols are the same as in Fig. 5. The solid line shows the linear regression through the entire sample and has a slope of 0.20 mag dex^-1, while the dashed lines show the 1 $\sigma$ uncertainty. See text for more details.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f15.ps} \end{figure}$ Figure 15: Absolute visual magnitudes M_V^k(1.5) versus [Fe/H]_L for field RR_ab stars more metal-rich than [Fe/H]_L=-1.0 in comparison with Galactic globular cluster variables. Symbols and lines are the same as in the bottom panel of Fig. 14.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f16.ps} \end{figure}$ Figure 16: Same as Fig. 14, but with cluster and field data fitted with a quadratic relation.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{8206f17.ps} \end{figure}$ Figure 17: Unreddened visual magnitude V₀ of RR_ab stars in $\omega$ Cen plotted versus $k(1.5)_{\rm puls}$ and $k(2.0)_{\rm puls}$ . The solid line plotted in the left panel refers to Eq. (5) and accounts for an intrinsic distance modulus $\mu _0=13.68$ mag. The solid line plotted in the right panel refers to Eq. (6) and accounts for $\mu _0=13.80$ mag.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8206f18.ps} \end{figure}$ Figure 18: Comparison between the apparent distance moduli of RR_cvariables based on the FOBE method and the RR_ab distance moduli based on the PA_V relation for the two adopted values of the mixing-length parameter. The data refer to scaled-solar chemical compositions and to the solar ratio $(Z/X)_{\odot }=0.0245$ .
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{8206f1.ps} \end{figure}$	Figure 1: From bottom to top: the average mass M(RR) in solar units, the absolute visual magnitude M_V(RR), and the evolutionary parameter $k(1.5)_{\rm ev}$ as a function of the HB type. Current predictions rely on a set of SHB simulations discussed in Paper IV.
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$\begin{figure} \par\includegraphics[width=8cm]{8206f3.ps} \end{figure}$	Figure 3: Visual amplitude versus period for RR_ab stars in Oosterhoff type II (OoII, top panel) and Oosterhoff type I (OoI, bottom panel) globular clusters. The solid line shows the ridge line of variables in OoII clusters and is based on the predicted slope $\delta\log P_F/\delta A_V=-$ 0.189.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f4.ps} \end{figure}$	Figure 4: The average $\langle k(1.5)_{\rm puls}\rangle$ ( bottom panel) and $\langle k(2.0)_{\rm puls}\rangle$ ( top panel) values for RR_ab stars in Oosterhoff type I (OoI, open circles) and Oosterhoff type II (OoII, filled circles) globular clusters plotted as a function of the cluster HB type.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f6.ps} \end{figure}$	Figure 6: Same as in Fig. 3, but for RR_ab stars in the two peculiar clusters NGC 6441 (triangles) and $\omega$ Cen (asterisks).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f7.ps} \end{figure}$	Figure 7: The $k(1.5)_{\rm puls}$ ( bottom panel) and the $k(2.0)_{\rm puls}$ ( top panel) parameter for RR_ab stars in $\omega$ Cen (asterisks) as a function of the metal abundance. Open circles, filled circles, and filled squares display Galactic globular clusters and have the same meaning as in Fig. 5.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f8.ps} \end{figure}$	Figure 8: Distribution of the $k(1.5)_{\rm puls}$ parameter for RR_ab stars in $\omega$ Cen ( bottom panel) together with OoI and OoII Galactic globular clusters.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f9.ps} \end{figure}$	Figure 9: RR_ab stars in the solar neighborhood with measured [Fe/H] abundances ( top panel; Layden 2007, private communication) and visual amplitudes ( bottom panel; Nikolov et al. 1984). The arrows mark the shortest period observed in OoI and OoII Galactic globular clusters. The solid line shows the predicted ridge line for cluster OoII variables (see Fig. 3).
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$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f10.ps} \end{figure}$	Figure 10: Difference between the observed and the calculated [Fe/H] versus period for all the stars in Fig. 9.
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$\begin{figure} \par\includegraphics[width=5.5cm,clip]{8206f11.ps} \end{figure}$	Figure 11: Residuals to Eq. (3) for all the fundamental models from Z=0.0001 to Z=0.02.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f12.ps} \end{figure}$	Figure 12: Pulsational parameter $k(1.5)_{\rm puls}$ as a function of metal abundance [Fe/H]_L for all the field RR_ab stars plotted in Fig. 9. The average values for Galactic globular clusters (symbols as in Fig. 5) and NGC 6441 (triangle) are also shown.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f15.ps} \end{figure}$	Figure 15: Absolute visual magnitudes M_V^k(1.5) versus [Fe/H]_L for field RR_ab stars more metal-rich than [Fe/H]_L=-1.0 in comparison with Galactic globular cluster variables. Symbols and lines are the same as in the bottom panel of Fig. 14.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{8206f16.ps} \end{figure}$	Figure 16: Same as Fig. 14, but with cluster and field data fitted with a quadratic relation.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{8206f17.ps} \end{figure}$	Figure 17: Unreddened visual magnitude V₀ of RR_ab stars in $\omega$ Cen plotted versus $k(1.5)_{\rm puls}$ and $k(2.0)_{\rm puls}$ . The solid line plotted in the left panel refers to Eq. (5) and accounts for an intrinsic distance modulus $\mu _0=13.68$ mag. The solid line plotted in the right panel refers to Eq. (6) and accounts for $\mu _0=13.80$ mag.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{8206f18.ps} \end{figure}$	Figure 18: Comparison between the apparent distance moduli of RR_cvariables based on the FOBE method and the RR_ab distance moduli based on the PA_V relation for the two adopted values of the mixing-length parameter. The data refer to scaled-solar chemical compositions and to the solar ratio $(Z/X)_{\odot }=0.0245$ .
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