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Context: IRAS 04166+2706 in Taurus is one of the most nearby young stellarobjects whose molecular outflow contains a highly collimated fast component.  Methods: We have observed the IRAS 04166+2706 outflow with the IRAM Plateaude Bure interferometer in CO(J=2-1) and SiO(J=2-1) achieving angularresolutions between 2'' and 4''. To improve the quality of the CO(2-1) images,we have added single dish data to the interferometer visibilities.  Results: The outflow consists of two distinct components. At velocities <10km/s, the gas forms two opposed, approximately conical shells that have the YSOat their vertex. These shells coincide with the walls of evacuated cavities andseem to result from the acceleration of the ambient gas by a wide-angle wind.At velocities >30 km/s, the gas forms two opposed jets that travel along thecenter of the cavities and whose emission is dominated by a symmetriccollection of at least 7 pairs of peaks. The velocity field of this componentpresents a sawtooth pattern with the gas in the tail of each peak moving fasterthan the gas in the head. This pattern, together with a systematic widening ofthe peaks with distance to the central source, is consistent with the emissionarising from internal working surfaces traveling along the jet and resultingfrom variations in the velocity field of ejection. We interpret this componentas the true protostellar wind, and we find its composition consistent with achemical model of such type of wind.  Conclusions: Our results support outflow wind models that have simultaneouslywide-angle and narrow components, and suggest that the EHV peaks seen in anumber of outflows consist of internally-shocked wind material.

Shells, jets, and internal working surfaces in the molecular outflow from IRAS 04166+2706