Molecular gas and star formation in NGC 3077

We present high-resolution (similar to2."5) CO(1-0) and CO(2-1) images of t he central 1 kpc of NGC 3077 made with the Owens Valley Millimeter Array. C O emission is distributed in three major complexes, which resolve into at l east seven giant molecular clouds (GMCs). Two complexes are associated with the central starburst. A third, more distant complex is not associated wit h strong star formation. The GMCs are similar to 70 pc in size and contain similar to 10(6) M-circle dot of molecular gas. The Galactic conversion fac tor appears applicable to NGC 3077, consistent with its solar metallicity. Galactic rotation in NGC 3077 is detected for the first time in the molecul ar gas. The molecular gas counterrotates with respect to the large-scale H I tidal bridge. The molecular clouds closest to the starburst have supervir ial line widths, possibly related to the turbulence generated by the starbu rst. The 2.6 mm radio continuum flux indicates that thermal bremsstrahlung dominates the emission from the starburst region below 5 cm and that the N (Lyc) similar or equal to 3.7 amount of molecular gas can sustain star form ation for only similar to 10 Myr; thus, NGC 3077 is a true starburst galaxy . The derived age of the starburst is consistent with the inferred ages of the superbubbles, which suggests that the burst is much younger than the ag e of the M81-M82-NGC 3077 interaction. We suggest that it is caused by gas that was pulled out of NGC 3077 during the interaction with M81, raining ba ck down onto the galaxy.