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With the ATNF Mopra telescope we are performing a survey in the 12CO(1-0)line to map the molecular gas in the Large Magellanic Cloud (LMC). For someregions we also obtained interferometric maps of the high density gas tracersHCO+ and HCN with the Australia Telescope Compact Array (ATCA). Here we discussthe properties of the elongated molecular complex that stretches about 2 kpcsouthward from 30 Doradus. Our data suggests that the complex, which we referto as the ``molecular ridge,'' is not a coherent feature but consists of manysmaller clumps that share the same formation history. Likely molecular cloudformation triggers are shocks and shearing forces that are present in thesurrounding south-eastern HI overdensity region, a region influenced by strongram pressure and tidal forces. The molecular ridge is at the western edge ofthe the overdensity region where a bifurcated velocity structure transitionsinto a single disk velocity component. We find that the 12CO(1-0) and HIemission peaks in the molecular ridge are typically near each other but nevercoincide. A likely explanation is the conversion of warmer, low-opacity HI tocolder, high-opacity HI from which H2 subsequently forms. On smaller scales, wefind that very dense molecular gas, as traced by interferometric HCO+ and HCNmaps, is associated with star formation along shocked filaments and with rimsof expanding shell-like structures, both created by feedback from massivestars.

The Molecular Ridge Close to 30 Doradus in the Large Magellanic Cloud