SMA observations towards the compact, short-lived bipolar water maser outflow in the LkHα234 region
We present Submillimeter Array (SMA) 1.35 mm subarcsecond angular resolution observations towards the LkHα234 intermediate-mass star-forming region. The dust emission arises from a filamentary structure of ∼5 arcsec (∼4500 au) enclosing VLA 1-3 and MM 1, perpendicular to the different outflows detec...
| Autores: | , , , , , , , , , , |
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| Formato: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2016 |
| País: | España |
| Recursos: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/383286 |
| Acesso em linha: | http://hdl.handle.net/10261/383286 |
| Access Level: | acceso abierto |
| Palavra-chave: | Masers Stars: formation ISM: individual objects: LkHα234-VLA 2 ISM: jets and outflows ISM: molecules |
| Resumo: | We present Submillimeter Array (SMA) 1.35 mm subarcsecond angular resolution observations towards the LkHα234 intermediate-mass star-forming region. The dust emission arises from a filamentary structure of ∼5 arcsec (∼4500 au) enclosing VLA 1-3 and MM 1, perpendicular to the different outflows detected in the region. The most evolved objects are located at the southeastern edge of the dust filamentary structure and the youngest ones at the northeastern edge. The circumstellar structures around VLA 1, VLA 3, and MM 1 have radii between∼200 and∼375 au and masses in the∼0.08-0.3M⊙ range. The 1.35mmemission of VLA 2 arises from an unresolved (r ≲ 135 au) circumstellar disc with a mass of ∼0.02 M⊙. This source is powering a compact (∼4000 au), low radial velocity (∼7 km s) SiO bipolar outflow, close to the plane of the sky. We conclude that this outflow is the 'large-scale' counterpart of the short-lived, episodic, bipolar outflow observed through HO masers at much smaller scales (∼180 au), and that has been created by the accumulation of the ejection of several episodic collimated events of material. The circumstellar gas around VLA 2 and VLA 3 is hot (∼130 K) and exhibits velocity gradients that could trace rotation. There is a bridge of warm and dense molecular gas connecting VLA 2 and VLA 3. We discuss the possibility that this bridge could trace a stream of gas between VLA 3 and VLA 2, increasing the accretion rate on to VLA 2 to explain why this source has an important outflow activity. © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. |
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