the profiles, and compare with available optical radial velocities ($V_{\rm opt}$). These are taken from the compilation by Durand, Acker, & Zijlstra (1998), except where explicitly cited. Previous CO observations at other telescopes are also noted.

002.6+04.2 (Th 3-27) Tentative 6-$\sigma$ detection. $V_{\rm o}$ consistent with $V_{\rm opt}$ ($-135.3\pm10.1$ [kms$^{-1}$]{}). The narrow CO spike at $V =
    -13$ [kms$^{-1}$]{} is IS.

003.8+05.3 (H 2-15) Tentative 5-$\sigma$ detection. $V_{\rm o}$ consistent with $V_{\rm opt}$ ($-63.2\pm3.7$ [kms$^{-1}$]{}).

008.3$-$01.1 (M 1-40) Roughly flat-topped profile with severe IS contamination; the emission at $V \ga 0$ [kms$^{-1}$]{} is probably all IS. $V_{\rm o}$ consistent with $V_{\rm opt}$ ($-34.4\pm2.0$ [kms$^{-1}$]{}).

008.6$-$07.0 (He 2-406) Double-peaked profile. $V_{\rm o}$ consistent with $V_{\rm opt}$ ($+28.2\pm5.2$ [kms$^{-1}$]{}).

010.1+00.7 (NGC 6537) Strong, triangular profile, with IS contamination on the red wing. $V_{\rm o}$ of peak differs from $V_{\rm opt}$ ($-16.9\pm1.9$ [kms$^{-1}$]{}) by 13 [kms$^{-1}$]{}, suggesting some structural asymmetry. In deep images the nebula is much more extended than the $10\arcsec$ listed in the Strasbourg-ESO catalog, but CO is seen only in the central pixel, and likely arises in the dense inner torus whose diameter in HST images is $\sim 5\arcsec$ (Huggins & Manley 2005). A broad CO(1–0) feature at $-$8 [kms$^{-1}$]{} 