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

Journal Article · Mon Dec 01 00:00:00 EST 2014 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/796/2/117· OSTI ID:22370132

Guzmán, Andrés E.; Garay, Guido; Bronfman, Leonardo; Mardones, Diego ^[1]; Rodríguez, Luis F. ^[2]; Moran, James ^[3]; Brooks, Kate J. ^[4]; Nyman, Lars-Åke ^[5]; Sanhueza, Patricio ^[6]

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1. Departamento de Astronomía, Universidad de Chile, Camino el Observatorio 1515, Las Condes, Santiago (Chile)
2. Centro de Radioastronomía y Astrofísica (UNAM), Morelia 58089 (Mexico)
3. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA (United States)
4. CSIRO Astronomy and Space Science, P.O. Box 76, Epping, 1710 NSW (Australia)
5. Joint ALMA Observatory (JAO), Alonso de Córdova 3107, Vitacura, Santiago (Chile)
6. Institute for Astrophysical Research, Boston University, Boston, MA 02215 (United States)

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, 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 × 10{sup 7} cm{sup –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.

• OSTI ID: 22370132
• Journal Information: Astrophysical Journal, Vol. 796, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
DETECTION
ELECTRON DENSITY
EMISSION
GHZ RANGE
HYDROGEN
MASS
RECOMBINATION
ROTATION
STARS
STELLAR WINDS
VELOCITY