Asymmetric distribution of gas in the Large Magellanic Cloud and dynamical condition for globular cluster formation.

Details Asymmetric distribution of gas in the Large Magellanic Cloud and dynamical condition for globular cluster formation. Asymmetric distribution of gas in the Large Magellanic Cloud and dynamical condition for globular cluster formation.

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pgrp.work...75f&link_type=abstract

Japan-France Seminar on Primeval Galaxies and Related Problems, p. 75 - 86

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Highly asymmetric distributions of H I and CO gases in LMC (Large Magellanic Cloud) are reproduced by taking account of hydrodynamical collision between LMC and SMC (Small Magellanic Cloud) about 0.2 Gyr ago. Two valued rotation curves in H I gas in LMC are due, respectively, to the gas clouds accelerated by the collision and those escaped therefrom. A comparison is made between dynamical features of gas of the Magellanic Clouds and of the Galaxy, concluding that a large-scale unorganized motion of gas with eddy size of more than a few hundred parsecs and random velocity of 50 to 100 km s-1 is a necessary condition for the globular cluster formation. It is also suggested that the chemical abundance of heavy elements is of secondary importance to the globular cluster formation, at least, in the range of -2.0 ≤ [Fe/H] ≤ 0 normalized to the sun, although it could regulate the mass of protoglobular clusters. Applications of this condition is made to the interpretation of some characteristics of old as well as young globular clusters in the Galaxy, M31, M82, M87 and other nearby galaxies.

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