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We compare the CO J =(1-0) and HI emission in the Large Magellanic Cloud(LMC) in three dimensions, i.e. including a velocity axis in addition to thetwo spatial axes, with the aim of elucidating the physical connection betweengiant molecular clouds (GMCs) and their surrounding HI gas. The CO J =1-0dataset is from the second NANTEN CO survey and the HI dataset is from themerged Australia Telescope Compact Array (ATCA) and Parkes Telescope surveys.The major findings of our analysis are: 1) GMCs are associated with an envelopeof HI emission, 2) in GMCs [average CO intensity] is proportional to [averageHI intensity]^[1.1+-0.1] and 3) the HI intensity tends to increase with thestar formation activity within GMCs, from Type I to Type III. An analysis ofthe HI envelopes associated with GMCs shows that their average linewidth is 14km s-1 and the mean density in the envelope is 10 cm-3. We argue that the HIenvelopes are gravitationally bound by GMCs. These findings are consistent witha continual increase in the mass of GMCs via HI accretion at an accretion rateof 0.05 Msun/yr over a time scale of 10 Myr. The growth of GMCs is terminatedvia dissipative ionization and/or stellar-wind disruption in the final stage ofGMC evolution.

Molecular and Atomic Gas in the Large Magellanic Cloud II. Three-dimensional Correlation between CO and HI