Molecular abundances with respect to CO scaled by 10⁴ for Ser-emb 8 (N). The distance from the protostar is on the x-axis. Panels from left to right are for the slow wing, the fast wing, and the EHV component. The abundances measured for three different regions along the outflow are shown for blueshifted and redshifted parts of the outflow separately. Abundances are measured in the same manner as in Fig. 6. The HCN emission is likely optically thick and therefore the abundance should be treated as a lower limit.