The study of molecular clouds in dwarf galaxies was, until recently, an arduous task and provided detections in only a handful of sources (see Thronson and Bally 1986; Wiklind et al. 1986; Tacconi and Young 1987; Arnoult et al. 1988). Line strengths observed in CO were small (<100mK) and measurements were confined to one position per source, thus inhibiting any detailed work. However, dwarf galaxies appear to be much more abundant than either spirals or large ellipticals and play an important role in our understanding of star and galaxy formation (see e.g. Gerola et al. 1980; Gallagher and Hunter 1984; Silk et al. 1987). With small rotational velocities (typically 50-lOOkms-1), the absence of density waves, and low metallicities, they provide, by "local" standards, an interstellar environment with even more extreme conditions than the outer Galaxy. Detailed molecular studies are hence important.