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(Abridged) METHODS: We performed SMA observations at 1.3 mm with both themost extended and compact array configurations, providing sub-arcsecond andhigh sensitivity maps of various molecular lines, including both hot-core andoutflow tracers. We also reconstruct the spectral energy distribution of theregion from millimeter to near infrared wavelengths, using the Herschel/Hi-GALmaps, as well as archival data. RESULTS: From the spectral energy distribution,we derive a bolometric luminosity of about 4x10^4 Lsun. Our interferometricobservations reveal that the distribution of dense gas and dust in the HMC issignificantly flattened and extends up to a radius of 8000 AU from the centerof radio continuum and maser emission in the region. The equatorial plane ofthis HMC is strictly perpendicular to the elongation of the collimated bipolaroutflow, as imaged on scales of about 0.1-0.5 pc in the main CO isotopomers aswell as in the SiO(5-4) line. In the innermost HMC regions (ca. 1000 AU), thevelocity field traced by the CH3CN(12_K-11_K) line emission shows thatmolecular gas is both expanding along the outflow direction following aHubble-law, and rotating about the outflow axis, in agreement with the (3-D)velocity field traced by methanol masers. The velocity field associated withrotation indicates a dynamical mass of 19 Msun at the center of the core. Thelatter is likely to be concentrated in a single O9.5 ZAMS star, consistent withthe estimated bolometric luminosity of G023.01-00.41. The physical propertiesof the CO(2-1) outflow emission, such as its momentum rate 6x10^-3 Msun km/s/yr and its outflow rate 2x10^-4 Msun/yr, support our estimates of theluminosity (and mass) of the embedded young stellar object.

A sub-arcsecond study of the hot molecular core in G023.01-00.41