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Paper: Physical Properties of Molecular Couds in the Magellanic Clouds Revealed by Observations in Multi-transition CO Molecular Lines
Volume: 476, New Trends in Radio Astronomy in the ALMA Era
Page: 73
Authors: Kawamura, A.; Minamidani, T.; Onishi, T.; Mizuno, T.; Kizawa, J.; Mizuno, N.; Fukui, Y.
Abstract: The Magellanic Clouds offer an ideal laboratory to study how the interstellar medium evolves and how stars are formed throughout a galaxy at an unrivaled closeness to us. It is known that young populous clusters like R136 are still being formed, making it possible to study cluster formation and its effects to the surrounding medium. We have established a catalog of the molecular clouds through the 12CO J = 1–0 observations by NANTEN. We have been extending our observations to higher transition lines of CO in submm by ASTE and NANTEN2. More detailed structure and properties of the GMCs are obtained by the Mopra observations. These datasets are combined and compared with LVG calculations to derive the density and temperature of clumps. The derived density and temperature are distributed in wide ranges. We suggest that these differences of clump properties represent an evolutionary sequence of GMCs in terms of density increase leading to star formation.
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