Volume 564, April 2014
|Number of page(s)||7|
|Section||Stellar structure and evolution|
|Published online||01 April 2014|
Department of PhysicsHCM International University-VNU,
Block 6, Linh Trung Ward, Thu Duc
Ho Chi Minh City,
2 Institute of Astronomy and Astrophysics, Academia Sinica, PO Box 23-141, 106 Taipei, Taiwan
3 Centro de Astrobiologia (CAB-CSIC), Ctra. Ajalvir km 4, 28850 Torrejón de Ardoz, Madrid, Spain
4 Harvard-Smithsonian Center for Astrophysics, Cambridge MA 02/138, USA
Accepted: 27 February 2014
Context. The previously identified source SSTB213 J041757 is a proto brown dwarf candidate in Taurus, which has two possible components A and B. It was found that component B is probably a class 0/I proto brown dwarf associated with an extended envelope.
Aims. Studying molecular outflows from young brown dwarfs provides important insight into brown dwarf formation mechanisms, particularly brown dwarfs at the earliest stages such as class 0, I. We therefore conducted a search for molecular outflows from SSTB213 J041757.
Methods. We observed SSTB213 J041757 with the Submillimeter Array to search for CO molecular outflow emission from the source.
Results. Our CO maps do not show any outflow emission from the proto brown dwarf candidate.
Conclusions. The non-detection implies that the molecular outflows from the source are weak; deeper observations are therefore needed to probe the outflows from the source.
Key words: ISM: jets and outflows / brown dwarfs / techniques: interferometric / stars: formation
Appendix A is available in electronic form at http://www.aanda.org
SMA data cutes (FITS format) are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/564/A32
© ESO, 2014
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