Theoretical Hertzsprung-Russell diagrams. Top panel: our candidate MS stars over-plotted on the evolutionary tracks of Ekström et al. (2012) for rotating stars. The masses of each model are plotted in correspondence of the zero-age MS. The luminosities were derived by adopting the spectrophotometric distances. Bottom panel: our candidate BHB stars over-plotted on the horizontal branch that is represented by a gray-shaded area and the evolutionary tracks for post-horizontal branch stars of given masses (Dorman 1992; Dorman et al. 1993). We note that three stars are classified both as MS and BHB candidates, hence they are featured in both panels with the appropriate parameters.