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We present molecular line observations of the protostellar outflow associatedwith HH270mms1 in the Orion B molecular cloud with ALMA. The 12CO(J = 3 - 2)emissions show that the outflow velocity structure consists of four distinctcomponents of low ($\gtrsim$ 10 km s-1), intermediate (~ 10 - 25 km s-1) andhigh ($\gtrsim$ 40 km s-1) velocities in addition to the entrained gas velocity(~ 25 - 40 km s-1). The high- and intermediate-velocity flows havewell-collimated structures surrounded by the low-velocity flow. The chain ofknots is embedded in the high-velocity flow or jet, which is the evidence ofepisodic mass ejections induced by time-variable mass accretion. We coulddetect the velocity gradients perpendicular to the outflow axis in both thelow- and intermediate-velocity flows. We confirmed the rotation of the envelopeand disk in the 13CO and C17O emission and found that their velocity gradientsare the same as those of the outflow. Thus, we concluded that the velocitygradients in the low- and intermediate-velocity flows are due to the outflowrotation. Using observational outflow properties, we estimated the outflowlaunching radii to be 67.1 - 77.1 au for the low-velocity flow and 13.3 - 20.8au for the intermediate-velocity flow. Although we could not detect therotation in the jets due to the limited spatial resolution, we estimated thejet launching radii to be (2.36 - 3.14) x 10^-2 au using the observed velocityof each knots. Thus, the jet is driven from the inner disk region. We couldidentify the launching radii of distinct velocity components within a singleoutflow with all the prototypical characteristics expected from recenttheoretical works.

Revealing multiple nested molecular outflows with rotating signatures in HH270mms1-A with ALMA