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Context: High-resolution studies of class 0 protostars represent the key toconstraining protostar formation models. VLA16234-2417 represents the prototypeof class 0 protostars, and it has been recently identified as a triplenon-coeval system. Aim: We aim at deriving the physical properties of the jetsin VLA16234-2417 using tracers of shocked gas. Methods: ALMA Cycle 0 EarlyScience observations of CO(2-1) in the extended configuration are presented incomparison with previous SMA CO(3-2) and Herschel-PACS [OI}] 63 micronobservations. Gas morphology and kinematics were analysed to constrain thephysical structure and origin of the protostellar outflows. Results: We reveala collimated jet component associated with the [OI] 63 micron emission at about8'' (about 960 AU) from source B. This newly detected jet component isinversely 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. Wealso detect a cavity-like structure at low projected velocities, whichsurrounds the [OI] 63 micron emission and is possibly associated with theoutflow driven by source A. Finally, no compact outflow emission is associatedwith source W. Conclusions: Our high-resolution ALMA observations seem tosuggest 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 avery 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 byA. However, a different scenario of a precessing jet driven by A cannot befirmly excluded from the present observations.

Disentangling the jet emission from protostellar systems. The ALMA view of VLA1623