Disentangling the jet emission from protostellar systems. The ALMA view of VLA1623
Journal
Date Issued
2015
Author(s)
Santangelo, G.
•
Murillo, N. M.
•
•
•
Bruderer, S.
•
Lai, S. -P.
•
van Dishoeck, E. F.
Description
This paper made use of the following ALMA data: ADS/JAO.ALMA 2011.0.00902.S and 2013.1.01004.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The 2011.0.00902.S data were obtained by N.M.M. while she was a Masters student at National Tsing Hua University, Taiwan, under the supervision of S.P.L. The work was partly supported by the ASI–INAF project 01/005/11/0 and the PRIN INAF 2012 – Jets, disks, and the dawn of planets (JEDI).
Abstract
Context. High-resolution studies of class 0 protostars represent the key to constraining protostar formation models. VLA16234-2417 represents the prototype of class 0 protostars, and it has been recently identified as a triple non-coeval system. Aims: We aim at deriving the physical properties of the jets in VLA16234-2417 using tracers of shocked gas. Methods: ALMA Cycle 0 Early Science observations of CO(2-1) in the extended configuration are presented in comparison with previous SMA CO(3-2) and Herschel-PACS [Oi] 63 μm observations. Gas morphology and kinematics were analysed to constrain the physical structure and origin of the protostellar outflows. Results: We reveal a collimated jet component associated with the [Oi] 63 μm emission at about 8'' (~960 AU) from source B. This newly detected jet component is inversely oriented with respect to the large-scale outflow driven by source A, and it is aligned with compact and fast jet emission very close to source B (about 0''̣3) rather than with the direction perpendicular to the A disk. We also detect a cavity-like structure at low projected velocities, which surrounds the [Oi] 63 μm emission and is possibly associated with the outflow driven by source A. Finally, no compact outflow emission is associated with source W. Conclusions: Our high-resolution ALMA observations seem to suggest there is a fast and collimated jet component associated with source B. This scenario would confirm that source B is younger than A, that it is in a very early stage of evolution, and that it drives a faster, more collimated, and more compact jet with respect to the large-scale slower outflow driven by A. However, a different scenario of a precessing jet driven by A cannot be firmly excluded from the present observations. Appendix A is available in electronic form at "http://www.aanda.org/10.1051/0004-6361/201526428/olm"
Volume
581
Start page
A91
Issn Identifier
0004-6361
Ads BibCode
2015A&A...581A..91S
Rights
open.access
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