  The 30 Doradus (30\,Dor) region in the Large Magellanic Cloud (also known as
the Tarantula Nebula) is the nearest massive starburst region, containing the
richest sample of massive stars in the Local Group. It is the best possible
laboratory to investigate aspects of the formation and evolution of massive
stars. Here, we focus on rotation which is a key parameter in the evolution of
these 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 in
the framework of the VLT-FLAMES Tarantula Survey (VFTS). The distribution of
$v_{e}\sin i$ shows a two-component structure: a peak around 80 $\rm{km
s^{-1}}$ 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 the
low-velocity peak is consistent with that found in other studies of late-O and
early-B stars. The high-velocity tail is compatible with expectations from
binary interaction synthesis models and may be predominantly populated by
post-binary interaction, spun-up, objects and mergers. This may have important
implications for the nature of progenitors of long-duration gamma ray bursts.
