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tokens: also shows a U-shaped cavity wall encompassing the E1 and E2 lobes, extending to ∼17 from the source. The emission is from the swept-up material in the dense core, which has a radius of 1500 au (∼17). Unlike the observation, however, no emission is seen extending over ∼17 from the source to ∼4′′ to the northeast. In our model, that region is within the AGB halo. Thus, in order to produce detectable emission there, the AGB halo could be denser than currently assumed in our model. Figure 6 shows the comparison of HV CO J = 3–2 emissions between the observation and the model. Both panels are also plotted over the HST images of CRL 618. In the observation (Figure 6 (a)), HV (−183.2 to −114.1 km s −1 ) emission is observed at the tips of lobes E1, E3, E4, and E5, but not observed at the tip of lobe E2. In the model, HV emission, with a similar velocity range to that in the observation, is predicted to be seen at the tips of all the lobes. The velocity of the emission increases with distance, similar to that seen in the observation. Notice that the emission intensity in our model is about half of that observed, and thus more bullet mass may be needed to produce more HV CO emission. The reason for no HV emission being detected at the tip of and along the southern edge of lobe E2 is unknown. Figure 6. (a) Observed HV CO J = 3–2 emission (contours) plotted on the H α image of CRL 618 (from Figure 2 of Lee et al. 2013a ). The velocity ranges of the contours are −183.2 to −160.6 km s −1 (blue), −157.8 to −132.5 km s −1 (cyan), and −132.5 to −114.1 km s −1 (green). The contours start at 1 Jy beam −1 km s −1 , with a step of 2 Jy beam −1 km s −1 . The synthesized beam is ∼053 × 035 at a position angle of ∼83°. (b) Simulated HV CO J = 3–2 emission (contours) in Model 2, with similar velocity ranges to those in (a). HV CO emissions are seen at the tips of the E1 to E5 lobes. The contours start at 0.5 Jy beam −1 km s −1 , with a step of 1 Jy beam −1 km s −1 . The synthesized beam is the same as that in (a). Figures 7 (a) and (b) show the PV diagrams of the observed outflows in CO, cut along the axis of lobes E1 and E2. Figures 7 (c) and (d) show the same PV diagrams but calculated from the model. In these diagrams, lobes E4 and E5 can also been seen. In Figures 7 (c) and (d), the bullets are seen at the tips of the outflows and thus are traced by the fast molecular outflows. The diagrams also show that the velocities of the molecular outflows decrease linearly with the distance to the central source, as seen in the observations. The slope of the PV structure is roughly equal to , where p is the projected distance from the center and t is the time after ejection. Therefore, different slopes are seen for the outflows in different ejection episodes. Notice that since no molecular emission is detected for lobe E2, no PV structure is detected for lobe E2 in the observation, as shown in Figure 7 (b). Figure 7. (a and b) PV diagrams of CO J = 3–2 emission of CRL