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The 30 Doradus (30\,Dor) region in the Large Magellanic Cloud (also known asthe Tarantula Nebula) is the nearest massive starburst region, containing therichest sample of massive stars in the Local Group. It is the best possiblelaboratory to investigate aspects of the formation and evolution of massivestars. Here, we focus on rotation which is a key parameter in the evolution ofthese objects. We establish the projected rotational velocity, $v_{e}\sin i$,distribution of an unprecedented sample of 216 radial velocity constant($\rm{\Delta RV\, \leq\, 20 \,km s^{-1}}$) O-type stars in 30\,Dor observed inthe framework of the VLT-FLAMES Tarantula Survey (VFTS). The distribution of$v_{e}\sin i$ shows a two-component structure: a peak around 80 $\rm{kms^{-1}}$ and a high-velocity tail extending up to $\sim$600 $\rm{km s^{-1}}$.Around 75% of the sample has 0 $\leq\, v_{e}\sin i \leq$ 200 $\rm{km s^{-1}}$with the other 25% distributed in the high-velocity tail. The presence of thelow-velocity peak is consistent with that found in other studies of late-O andearly-B stars. The high-velocity tail is compatible with expectations frombinary interaction synthesis models and may be predominantly populated bypost-binary interaction, spun-up, objects and mergers. This may have importantimplications for the nature of progenitors of long-duration gamma ray bursts.

Rotational properties of the O-type star population in the Tarantula region