Table 1: Comparison of the ZAHB levels, He core masses (in solar mass units), HB evolutionary times (in Myr) and RGB evolutionary times at brighter magnitudes than the ZAHB (in Myr) between the models used in Zoccali et al. (2000), in Paper I, and the models by Cassisi et al. (1998), for two selected metallicities (see text for details).
Zoccali et al. (2000) $M_V\rm (ZAHB)$ $M_{\rm c}\rm (He)$ $t_{\rm HB}$ $t_{\rm RGB}$

Z=0.001 0.54 0.499 102 63

Z=0.006 0.72 0.493 112 55

Cassisi et al. (1998)

Z=0.001 0.49 0.500 85 58

Z=0.006 0.68 0.493 94 47

Paper I

Z=0.001 0.58 0.495 88 65

Z=0.006 0.74 0.489 93 56

**Table 1:** Comparison of the ZAHB levels, He core masses (in solar mass units), HB evolutionary times (in Myr) and RGB evolutionary times at brighter magnitudes than the ZAHB (in Myr) between the models used in Zoccali et al. (2000), in Paper I, and the models by Cassisi et al. (1998), for two selected metallicities (see text for details).
Zoccali et al. (2000)	$M_V\rm (ZAHB)$	$M_{\rm c}\rm (He)$	$t_{\rm HB}$	$t_{\rm RGB}$
Z=0.001	0.54	0.499	102	63
Z=0.006	0.72	0.493	112	55
Cassisi et al. (1998)
Z=0.001	0.49	0.500	85	58
Z=0.006	0.68	0.493	94	47
Paper I
Z=0.001	0.58	0.495	88	65
Z=0.006	0.74	0.489	93	56

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