Astronomy & Astrophysics

Table 1: Selected results of synthetic HB simulations at Y= 0.23. Each row gives the metallicity, the mean HB mass, the HB type, the number of RR Lyrae stars together with their mean mass, mean visual magnitude and mean fundamentalised period, the AGB ratio $R^{{\rm AGB}}=$ N(AGB)/N(HB) and the predicted number ratio of HB to RGB stars more luminous than i) the ZAHB bolometric magnitude at the RR Lyrae gap ( $R^{\rm I}$ ); ii) the absolute visual magnitude of the faintest RR Lyrae pulsator ( $R^{{\rm II}}$ ); and iii) the mean $\langle M_V^{{\rm RR}}\rangle$ magnitude of the pulsators. Masses are in solar units. Absolute visual magnitudes of the ZAHB at log $T_{\rm e}=$ 3.83 are given in parentheses below the corresponding metallicity values.
Table 2: The comparison between observed and predicted mean periods for the sample of RR Lyrae rich Galactic globulars (see Paper I). Metal abundances and HB type (HB) are from Harris.
Table 3: Slope and zero point (in magnitudes) of predicted PL_Kand PW relations for various metallicity and HB type with significant numbers of RR Lyrae pulsators ( $\ge$ 5% the total number of HB stars), except the HB types in italics.