SANNA, ALBERTOALBERTOSANNAMOSCADELLI, LucaLucaMOSCADELLICESARONI, RiccardoRiccardoCESARONICARATTI O GARATTI, AlessioAlessioCARATTI O GARATTIMenten, K. M.K. M.MentenKölligan, A.A.KölliganKuiper, R.R.Kuiper2022-12-192022-12-1920170037-8720http://hdl.handle.net/20.500.12386/32773We want to understand whether or not young stars, with masses of tens of Solar masses, can form in the disk accretion scenario. This challenge requires to resolve the spatial morphology of gas and dust within a few 1000 au of a massive young stellar object, and to measure the gas kinematics with respect to the star. Also, because the gas kinematics near the young star can be a mixture of rotating, expanding, and infalling motions all together, to separate each velocity component it is necessary to map the emission of various gas tracers, as well as to image the circumstellar gas at different distances from the star. With this in mind, we made use of the Atacama Large Millimeter Array (ALMA) at wavelengths near 1 mm, with the aim to image the dense molecular gas in the vicinity of a well-known O-type young star. We previously observed this source with the Submillimeter Array (SMA), at scales of about 0.1 pc, with the Karl G. Jansky Very Large Array (VLA), at scales of the order of 1000 au, and with the Very Long Baseline Array (VLBA) and European VLBI Network (EVN), at scales of a few au.ELETTRONICOenConference paperhttp://sait.oat.ts.astro.it/MSAIt880417/index.html2017MmSAI..88..814SFIS/05 - ASTRONOMIA E ASTROFISICA