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The high-velocity molecular jet driven by Class 0 protostar IRAS 04166+2706exhibits a unique saw-tooth velocity pattern. It consists of a series ofwell-aligned symmetric knots with similar averaged speeds, whose speeds atpeaks of emission decreases roughly linearly away from the origin. Recent ALMAobservations of knots R6 and B6 reveal kinematic behavior with expansionvelocity increasing linearly from the axis to the edge. This pattern can beformed by a spherically expanding wind with axial density concentration. Inthis picture, the diverging velocity profile naturally possesses an increasingexpansion velocity away from the axis, resulting in a tooth-like feature on theposition-velocity diagram through projection. Such geometric picture predicts acorrespondence between the slopes of the teeth and the outflow inclinationangles, and the same inclination angle of 52$^\circ$ of the IRAS 04166+2706 cangenerally explain the whole pattern. Aided by numerical simulations in theframework of unified wind model by Shang et al. (2006), the observed velocitypattern can indeed be generated. A proper geometrical distribution of the jetand wind material is essential to the reconstruction the ejection history ofthe system.

Ejection History of the IRAS 04166+2706 Molecular Jet