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Star-formation in dwarf starburst galaxies can be quite intense for their sizes, especially in the very young ones characterized by Wolf-Rayet emission features. Since stars form out of molecular gas (H2), it is important to investigate in detail, where the molecular gas is relative to the star formation in such young starbursts. The molecular gas may also indicate what might have triggered the starburst. The ISM in dwarfs can be quite warm, is the molecular gas also warm? In an attempt to investigate the properties of molecular gas in WR galaxies we have obtained high resolution images of the J = 2–1 transitions of CO for two dwarf starbursts, NGC5253 and He2–10. Both galaxies are nearby dwarf starbursts with WR emission features (e.g., Conti 1991). NGC 5253 may be one of the youngest starbursts known (e.g., Rieke, Lebofsky & Walker 1988).