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It is well established that Solar-mass stars gain mass via disk accretion,until the mass reservoir of the disk is exhausted and dispersed, or condensesinto planetesimals. Accretion disks are intimately coupled with mass ejectionvia polar cavities, in the form of jets and less collimated winds, which allowmass accretion through the disk by removing a substantial fraction of itsangular momentum. Whether disk accretion is the mechanism leading to theformation of stars with much higher masses is still unclear. Here, we are ableto build a comprehensive picture for the formation of an O-type star, bydirectly imaging a molecular disk which rotates and undergoes infall around thecentral star, and drives a molecular jet which arises from the inner diskregions. The accretion disk is truncated between 2000-3000au, it has a mass ofabout a tenth of the central star mass, and is infalling towards the centralstar at a high rate (6x10^-4 Msun/yr), as to build up a very massive object.These findings, obtained with the Atacama Large Millimeter/submillimeter Arrayat 700au resolution, provide observational proof that young massive stars canform via disk accretion much like Solar-mass stars.

Discovery of a sub-Keplerian disk with jet around a 20Msun young star. ALMA observations of G023.01-00.41