All Tables

Table 1: Chemical composition of stellar models with total metallicity Z, initial helium Y₀, hydrogen abundance X₀, iron abundance with respect to hydrogen (in spectroscopic notation [Fe/H]) and total metallicity with respect to hydrogen [M/H].
Table 2: Combinations of age indicators. The weight w_i in Eq. (3) is given for each indicator.
Table 3: Indicator value, age $t_{\rm min}$ , minimum value $M(t_{\rm min})$ , and fit quality Q for all age indicators applied to NGC 6934.
Table 4: Comparison of bump properties for stellar models of $1~M_\odot$ and Z=0.001. The references are: Girardi et al. (2000, Padova), Cariulo et al. (2004, Pisa), Pietrinferni et al. (2004, BASTI), and Kim et al. (2002, Y²).
Table 5: Ages (in Gyr) for galactic globular clusters from Case A (Col. 4), from Case S (Col. 5) and quoted from Salaris & Weiss (2002, Col., "SW02''). The age range is that for which M(t) has Q > 0.32 ( $1\sigma$ -range). If only one age is given, it is $M_{\rm min}$ , with $Q(M_{\rm min}) < 0.32$ . Columns 7 and 8 contain the result when using the BASTI isochrones (Pietrinferni et al. 2004) for Case A, and for case BC (see Table 2), which includes the bump brightness. Case S is not shown as it is not better than for our own isochrones.
Table 6: Data of the critical points of all Globular Cluster Colour-Magnitude Diagrams in our sample as determined by us (see Sect. 3); part I: the turn-off region and colours of turn-off, lower RGB, and bump.
Table 7: As Table 6, but displaying horizontal branch, RGB bump, and tip brightness as well as the cluster distances inferred from $V_{\rm ZAHB}$ and $V_{\rm tip}$ . $(B-V)_{\rm ZAHB}$ is the colour of the point on the ZAHB closest to the TO colour.
Table 8: Polynomial relations for points along our isochrones used as age indicators. The relations are all of the form f(t)=a₀+a₁t+a₂t²+a₃t³, where t is in Gyr. Part I: V-magnitudes.
Table 9: As Table 8. Part II: Colours.