Stellar pulsations in main-sequence B-type stars are driven by the \kappa -mechanism due to the Fe-group opacity bump .
The current models do not predict the presence of instability strips in the B spectral domain at very low metallicities .
As the metallicity of the Magellanic Clouds ( MC ) has been measured to be around Z = 0.002 for the Small Magellanic Cloud ( SMC ) and Z = 0.007 for the Large Magellanic Cloud ( LMC ) , they constitute a very suitable objects to test these predictions . The aim of this work is to investigate the existence of B-type pulsators at low metallicities , searching for short-term periodic variability in a large sample of B and Be stars from the MC with accurately determined fundamental astrophysical parameters .