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

A probable Keplerian disk feeding an optically revealed massive young star