Atomic and Molecular Gas near NGC 3077 : The Making of a New Dwarf Galaxy ? Fabian

Using the IRAM 30m radio telescope we have mapped the tidal arm feature south–east of NGC3077 where we recently detected molecular gas in the CO (J=1→0) and (2→1) transitions. We find that the molecular gas is much more extended than previously thought (several kpc). The CO emission can be separated into at least 3 distinct complexes with equivalent radii between 250 pc and 700 pc – the newly detected complexes therefore range among the largest molecular complexes in the local universe. Mass estimates based on virialization and employing an XCO factor yield a total mass for the complexes of order 4× 10 M⊙, i.e. more than the estimated molecular mass within NGC3077 itself. This implies that interactions between galaxies can efficiently remove heavy elements and molecules from a galaxy and enrich the intergalactic medium. A comparison of the distribution of HI and CO shows no clear correlation. However, CO is only found in regions where the HI column density exceeds 1.1 × 10 cm. HI masses for the molecular complexes mapped are of the same order as the corresponding molecular masses. Since the complexes have all the ingredients to form stars in the future, we are thus presumably witnessing the birth of a dwarf galaxy. This process may have dominated the creation of dwarf galaxies at larger look–back times.