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According to recent theoretical studies, the progenitors of Long Gamma RayBursts should be very fast rotating stars, massive enough but not so forcollapsing into a black hole. In addition, recent observations seem to showthat stars of about 20 solar masses could be at the origin of LGRBs. At lowmetallicity B-type stars rotate faster than at higher metallicity. We foundwith the ESO-WFI an occurrence of Be/Oe stars, that are quasi criticalrotators, 3 to 5 times larger in the SMC than in the Galaxy. According to ourresults, and using observational clues on the SMC WR stars, as well as thetheoretical predictions of the characteristics must have the LGRB progenitors,we have identified the low metallicity massive Be/Oe stars as potential LGRBprogenitors. To support this identification, the expected rates and the numbersof LGRB were then calculated and compared to the observed ones: 3 to 6 LGRBswere found in the local universe in 11 years while 8 were actually observed.

Massive Be and Oe stars at low metallicity and long gamma ray bursts