5 Conclusion

Second overtone mode Cepheids could be discriminated from fundamental and first overtone mode Cepheids by taking into account their period, luminosity, low amplitude and Fourier parameters (Antonello & Kanbur 1997; Alcock et al. 1997). However, none of the stars analyzed in the present study, and which are characterized by low amplitude, can be discriminated from the other known Cepheid types on the basis of the light curve shape. Only HV 1779 is relatively bright for its period, but this is not a sufficient criterium, since the relatively large luminosity could be explained by other reasons (e.g. a companion or a background star). We conclude that the three suspected second overtone candidates are fundamental (HV 1353) and first overtone (HV 1777, HV 1779) mode pulsators. HV 1763, whose nature was previously unknown, resulted to be a short-period Cepheid pulsating in the first overtone mode.