We report the detection, made using ALMA, of the 92 GHz continuum and hydrogen recombination lines (HRLs) H40α, H42α, and H50β 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, 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 a high-velocity component. The Lorentzian line wings imply electron densities of 5×107 cm−3 on average. In addition, we detect SO and SO2 emission arising from a compact (∼3000 AU) molecular core associated with the central young star. The molecular core exhibits a velocity gradient 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.
@article{arxiv.1410.0233,
title = {Slow ionized wind and rotating disklike system associated with the high-mass young stellar object G345.4938+01.4677},
author = {Andrés E. Guzmán and Guido Garay and Luis F. Rodríguez and James Moran and Kate J. Brooks and Leonardo Bronfman and Lars-Åke Nyman and Patricio Sanhueza and Diego Mardones},
journal= {arXiv preprint arXiv:1410.0233},
year = {2015}
}