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We investigate the effects of Supergiant Shells (SGSs) and their interactionon dense molecular clumps by observing the Large Magellanic Cloud (LMC) starforming regions N48 and N49, which are located between two SGSs, LMC 4 and LMC5. $^{12}$CO ($J$=3-2, 1-0) and $^{13}$CO ($J$=1-0) observations with the ASTEand Mopra telescopes have been carried out towards these regions. A clumpydistribution of dense molecular clumps is revealed with 7 pc spatialresolution. Large velocity gradient analysis shows that the molecular hydrogendensities ($n({\rm H}_2)$) of the clumps are distributed from low to highdensity ($10^3$-$10^5$ cm$^{-3}$) and their kinetic temperatures ($T_{\rmkin}$) are typically high (greater than $50$ K). These clumps seem to be in theearly stages of star formation, as also indicated from the distribution ofH$\alpha$, young stellar object candidates, and IR emission. We found that theN48 region is located in the high column density HI envelope at the interfaceof the two SGSs and the star formation is relatively evolved, whereas the N49region is associated with LMC 5 alone and the star formation is quiet. Theclumps in the N48 region typically show high $n({\rm H}_2)$ and $T_{\rm kin}$,which are as dense and warm as the clumps in LMC massive cluster-forming areas(30 Dor, N159). These results suggest that the large-scale structure of theSGSs, especially the interaction of two SGSs, works efficiently on theformation of dense molecular clumps and stars.

Dense Molecular Clumps associated with the LMC Supergiant Shells LMC 4 \& LMC 5