tokens: not correspond to the velocity expected from the kinematical model presented in this work. We thus conclude that the clumps of the EHVO seen in Fig. 7 correspond to material that was swept up by a different outflow, which is faster and likely older than the HVO. Additionally, there seems to be traces of entrained material of the EHVO outflow that appear as “horns” of the HVO and confined within the region traced by the CO( J = 1 → 0) emission. Therefore, it is likely that the extension of the region traced by the CO( J = 1 → 0) emission determines the radius of CO photo-dissociation by interstellar UV radiation. 4.3 Kinetic energy and scalar momentum of molecular outflow Since our model is fundamentally different from the one presented by Sahai et al. (2017) , here we re-calculate the scalar momentum and kinematic energy of the molecular outflow. To obtain the kinetic energy and scalar momentum, in principle, it is possible to use the mass spectrum shown in Fig. 6 . However, the velocity offset in this plot is simply the component of the expansion velocity on the line-of-sight. The 3D expansion velocity is necessary for the calculations. To circumvent this problem, one can take advantage of the morphology adopted for the emitting region, which has an elongated, narrow shape. In such a case, it is possible to de-project the velocity vectors by multiplying the velocity offsets by a factor of 1/sin θ inc , with θ inc = 45°. This is not strictly true for all the velocity vectors, since the gas is not really moving along one single line. Particularly, for the gas located close to the central source, which might be expanding along the line-of-sight, the expansion velocity will be overestimated by a factor of 1/sin θ inc . For such gas, this leads to an overestimation of the scalar momentum by a factor of and for the kinetic energy by a factor of 2. In addition, there is an uncertainty due to the optical depth of the CO( J = 3 → 2) emission since it was assumed to be optically thin to obtain the mass spectrum of Fig. 6 . If the emission is optically thick the estimated value of the mass simply represents a lower limit. Having this in mind, we proceeded to calculate the kinetic energy and scalar momentum in the manner introduced by Bujarrabal et al. (2001) and described inthe following. Firstly, we multiplied the mass in each channel by the square of the corresponding velocity to obtain the kinetic energy per channel. By adding the kinetic energy of all the channels we obtain K LVC = 8 × 10 44 erg and K HVC = 1 × 10 45 erg for the LVC and HVC, respectively. Similarly, the derived scalar momentum is 1.6 × 10 38 gm cm s −1 and 6 × 10 37 gm cm s −1 for the LVC and HVC, respectively. The total kinetic energy and scalar momentum in the outflow are of the same order of magnitude as the values calculated by Sahai et al. (2017) . Subsequently, the scalar momentum in the molecular outflow transferred by the jet, Δ P , is obtained by subtracting the scalar
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