  We present the results from a search for HI emission from a sample of newly
discovered dwarf galaxies in the M81 group. HI is detected in three galaxies,
all of which are classified as BCDs. The HI masses of these galaxies are ~ 10^6
M_sun, making these some of the lowest mass BCDs known. For these three
galaxies FUV images (from GALEX) and H-alpha images (from the Russian 6m BTA
telescope) are available.The H-alpha emission is very faint, and, in principle
could be produced by a single O star. Further, in all cases we find offsets
between the peak of the FUV emission and that of the H-alpha emission. Offsets
between the most recent sites of star formation (i.e. those traced by H-alpha)
and the older sites (i.e. those traced by FUV) would be natural if the star
formation is stochastic. In spite of the expectation that the effects of
mechanical feedback from star formation would be most directly seen in the
smallest galaxies with low gravitational potentials, we only see tentative
evidence of outflowing HI gas associated with the star forming region in one of
the galaxies.
