  The canonical picture of star formation involves disk-mediated accretion,
with Keplerian accretion disks and associated bipolar jets primarily observed
in nearby, low-mass young stellar objects (YSOs). Recently, rotating gaseous
structures and Keplerian disks have been detected around a number of massive (M
> 8 solar masses) YSOs (MYSOs) including several disk-jet systems. All of the
known MYSO systems are located in the Milky Way, and all are embedded in their
natal material. Here we report the detection of a rotating gaseous structure
around an extragalactic MYSO in the Large Magellanic Cloud. The gas motions
show radial flow of material falling from larger scales onto a central
disk-like structure, the latter exhibiting signs of Keplerian rotation, i.e., a
rotating toroid feeding an accretion disk and thus the growth of the central
star. The system is in almost all aspects comparable to Milky Way high-mass
young stellar objects accreting gas via a Keplerian disk. The key difference
between this source and its Galactic counterparts is that it is optically
revealed, rather than being deeply embedded in its natal material as is
expected of such a young massive star. We suggest that this is the consequence
of the star having formed in a low-metallicity and low-dust content
environment, thus providing important constraints for models of the formation
and evolution of massive stars and their circumstellar disks.
