Theoretical tracks from Pietrinferni et al. (2006) for different masses (from 1.1 to ﹩1.5\,M_{\odot }﹩; solid lines) are overplotted to the ACS CMD of 47 Tuc. The theoretical tracks, with α‐enhancement ([α/Fe] = 0.4) and [Fe/H] = −0.66 (﹩Z=0.008﹩), have been transformed in the ACS filters following Bedin et al. (2005). Distance modulus ﹩( m-M) _{0}=13.33﹩ and reddening ﹩E( B-V) =0.04﹩ have been adopted (Ferraro et al. 1999). The RGB phase for such massive stars turns out to occupy the same region of the CMD where "normal" low‐mass AGB stars are observed. The post‐RGB evolutionary track for a ﹩1.5\,M_{\odot }﹩ star is also shown (dashed line). Note that the ZAHB level for such a massive star lies in the bright extension of the observed HB where the bHB sample has been defined. The evolutionary time needed by a ﹩1.3\,M_{\odot }﹩ star to cover the RGB portion between the two horizontal lines is also reported.