Submillimeter Observations of Giant Molecular Clouds in the Large Magellanic Cloud: Temperature and Density as Determined from J = 3-2 and J = 1-0 Transitions of CO

We have carried out submillimeter super(12)CO(J = 3 2) observations of six giant molecular clouds (GMCs) in the Large Magellanic Cloud (LMC) with the ASTE 10 m submillimeter telescope at a spatial resolution of 5 pc and very high sensitivity. We have identified 32 molecular clumps in the GMCs and revealed significant details of the warm and dense molecular gas with n(H sub(2)) similar to 10 super(3)-10 super(5) cm super(-3) and T sub(ki) [unk] similar to G0 k. These data are combined with super(12)CO(J = 1 0) and super(13)CO(J =1 0) results and compared with LVG calculations. The results indicate that clumps that we detected are distributed continuously from cool ( similar to 10-30 K) to warm ( [unk]30-200 K), and warm clumps are distributed from less dense ( similar to 10 super(3) cm super(-3)) to dense ( similar to 10 super(3.5)-10 super(5) cm super(-3)). We found that the ratio of super(12)CO(j = 3 2) to super(12)CO(J = 1 0) emission is sensitive to and is well correlated with the local Ho flux. We infer that differences of clump properties represent an evolutionary sequence of GMCs in terms of density increase leading to star formation. Type I and II GMCs (starless GMCs and GMCs with H II regions only, respectively) are at the young phase of star formation where density does not yet become high enough to show active star formation, and Type III GMCs (GMCs with H II regions and young star clusters) represent the later phase where the average density is increased and the GMCs are forming massive stars. The high kinetic temperature correlated with Ho flux suggests that FUV heating is dominant in the molecular gas of the LMC.