(+5 [kms$^{-1}$]{} LSR) reported by Zhang et al. (2000) is significantly different from the spectrum reported here and is likely at least partly interstellar.

011.9+04.2 (M 1-32) Tentative 3-$\sigma$ detection. $V_{\rm o}$ consistent with $V_{\rm opt}$ ($-90.6\pm7.6$ [kms$^{-1}$]{}).

016.0$-$04.3 (M 1-54) $V_{\rm o}$ of the CO peak is offset by $\sim 15$ [kms$^{-1}$]{} from $V_{\rm opt}$ ($-47.4\pm4.2$ [kms$^{-1}$]{}), so the tentative, second CO feature at $V = -87$ [kms$^{-1}$]{} may be part of a broad, double-peaked profile.

019.9+00.9 (M 3-53) Probably a flat-topped profile, but strong IS (spike/dip) contamination of the blue wing. $V_{\rm o}$ consistent with uncertain $V_{\rm opt}$ ($+20.6\pm14.0$ [kms$^{-1}$]{}).

021.1$-$05.9 (M 1-63) Double-peaked profile. $V_{\rm o}$ consistent with $V_{\rm opt}$ ($+8.5\pm10.3$ [kms$^{-1}$]{}).

021.7$-$00.6 (M 3-55) Strong, parabolic profile, with severe IS (spike/dip) contamination; emission at $V \ga 40$ [kms$^{-1}$]{} is probably all IS. The broad wing to the blue appears to belong to the PN. $V_{\rm o}$ consistent with uncertain $V_{\rm opt}$ ($+9.7\pm15.0$ [kms$^{-1}$]{}).

021.8$-$00.4 (M 3-28) Strong, double peaked profile with IS (spike) contamination on red wing and at higher velocities. A CO spectrum obtained with the SEST 15 m telescope was previously reported by Gomez, Rodriguez, & Garay (1992). $V_{\rm o}$ consistent with uncertain $V_{\rm 