  We present a comprehensive multi-wavelength study of the nearby interacting
dwarf galaxy NGC3077 (member of the M81 triplet). High resolution VLA HI
observations show that most of the atomic gas (~90%) around NGC3077 is situated
in a prominent tidal arm with a complex velocity structure. Little HI (~5 x
10^7 M_sun) is associated with NGC3077 itself. High resolution OVRO
observations of the molecular component (CO) reveal the presence of 16
molecular complexes near the center of NGC3077 (total mass: ~1.6 x 10^6 M_sun).
A virial mass analysis of the individual complexes yields a lower CO-to-H_2
conversion factor in NGC3077 than the Galactic value - a surprising result for
a dwarf galaxy. The total (atomic and molecular) gas content in the centre of
NGC3077 is displaced from the stellar component of NGC3077 -- this implies that
not only the gas at large galactocentric radii is affected by the interaction
within the triplet but also the center. We speculate that the starburst
activity of NGC3077 was triggered by this redistribution of gas in the center.
Some of these supershells are surrounded by neutral hydrogen. In a few cases,
the rims of the ionized supershells are associated with dust absorption. The
most prominent star forming region in NGC3077 as probed by Pa-alpha
observations is hidden behind a dust cloud which is traced by the molecular
complexes. Correcting for extinction we derive a star forming rate of 0.05
M_sun year^-1, i.e. given the reservoir in atomic and molecular gas in NGC3077,
star formation may proceed at a similar rate for a few 10^8 years. The
efficiency to form stars out of molecular gas in NGC3077 is similar to that in
M82.
