H I spectra averaged towards Cha I, Cha II, Cha III, the eastern region of the Chamaeleon cloud and Musca. The dashed vertical lines give the ¹²CO velocities of the dense regions Cha I, Cha II, Cha III and Musca (Mizuno et al. 2001). This shows that the dense gas traced by ¹²CO for all regions is redshifted compared to their H I emission, identical to what is found for the filament crest of Musca when comparing ¹²CO and C¹⁸O.