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We report the detection, made using ALMA, of the 92 GHz continuum andhydrogen recombination lines (HRLs) H40$\alpha$, H42$\alpha$, and H50$\beta$emission toward the ionized wind associated with the high-mass young stellarobject G345.4938+01.4677. This is the luminous central dominating sourcelocated in the massive and dense molecular clump associated with IRAS16562$-$3959. The HRLs exhibit Voigt profiles, a strong signature of Starkbroadening. We successfully reproduce the observed continuum and HRLssimultaneously using a simple model of a slow ionized wind in localthermodynamic equilibrium, with no need a high-velocity component. TheLorentzian line wings imply electron densities of $5\times10^7$ cm$^{-3}$ onaverage. In addition, we detect SO and SO$_2$ emission arising from a compact($\sim3000$ AU) molecular core associated with the central young star. Themolecular core exhibits a velocity gradient perpendicular to the jet-axis,which we interpret as evidence of rotation. The set of observations towardG345.4938+01.4677 are consistent with it being a young high-mass starassociated with a slow photo-ionized wind.

Slow ionized wind and rotating disklike system associated with the high-mass young stellar object G345.4938+01.4677