Slow ionized wind and rotating disklike system associated with the high-mass young stellar object G345.4938+01.4677 (doi:10.7910/DVN/24060)

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

doi:10.7910/DVN/24060

Harvard Dataverse

2014-05-07

3

Guzman, Andres E.; Garay, Guido; Rodriguez, Luis F.; Moran, James; Brooks, Kate J.; Bronfman, Leonardo; Nyman, Lars-Ake; Sanhueza, Patricio; Mardones, Diego, 2014, "Slow ionized wind and rotating disklike system associated with the high-mass young stellar object G345.4938+01.4677", https://doi.org/10.7910/DVN/24060, Harvard Dataverse, V3

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

doi:10.7910/DVN/24060

Guzman, Andres E. (DAs-UChile / CfA)

Garay, Guido (DAs-UChile)

Rodriguez, Luis F. (CRyA-UNAM)

Moran, James (CfA)

Brooks, Kate J. (CASS)

Bronfman, Leonardo (DAs-UChile)

Nyman, Lars-Ake (JAO)

Sanhueza, Patricio (BU)

Mardones, Diego (DAs-UChile)

NNX12AI55G

NNX10AD68G

Harvard Dataverse

2013-12-20

https://doi.org/10.7910/DVN/24060

Astronomy and Astrophysics, ISM: jets and outflows --- radio continuum: stars --- stars: formation --- IRAS 16562$-$3959 --- 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, 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 $5\times10^7$~cm$^{-3}$ on average. In addition, we detect SO and SO$_2$ emission arising from a compact ($\sim3000$~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.

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