THE SLOW IONIZED WIND AND ROTATING DISKLIKE SYSTEM THAT ARE ASSOCIATED WITH THE HIGH-MASS YOUNG STELLAR OBJECT G345.4938+01.4677

We report the detection, made using ALMA, of the 92 GHz continuum and hydrogen recombination lines (HRLs) H40 alpha , H42 alpha , and H50 beta emission toward the ionized wind associated with the high-mass young stellar object G345.4938+01.4677. This is the luminous central dominating source located in the massive and dense molecular clump associated with IRAS 16562-3959. The HRLs exhibit Voigt profiles, which is a strong signature of Stark broadening. We successfully reproduce the observed continuum and HRLs simultaneously using a simple model of a slow ionized wind in local thermodynamic equilibrium, with no need for a high-velocity component. The Lorentzian line wings imply electron densities of 5 x 10 super(7) cm super(-3) on average. In addition, we detect SO and SO sub(2) emission arising from a compact (~3000 AU) molecular core associated with the central young star. The molecular core exhibits a velocity gradient that is perpendicular to the jet-axis, which we interpret as evidence of rotation. The set of observations toward G345.4938 +01.4677 are consistent with it being a young high-mass star associated with a slow photo-ionized wind.