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Abstract: We have analyzed the HI aperture synthesis image of the Large MagellanicCloud LMC, using an objective and quantitative measure of topology tounderstand the HI distribution hosting a number of holes and clumps of varioussizes in the medium. The HI distribution shows different topology at fourdifferent chosen scales. At the smallest scales explored 19-29 pc, the HImass is distributed in such a way that numerous clumps are embedded on top of alow density background. At the larger scales from 73 to 194 pc, it shows ageneric hole topology. These holes might have been formed mainly by stellarwinds from hot stars. At the scales from 240 to 340 pc, slightly above the diskscale-height of the gaseous disk, major clumps in the HI map change thedistribution to have a slight clump topology. These clumps include the giantcloud associations in the spiral arms and the thick filaments surroundingsuperholes. At the largest scales studied 390-485 pc, the hole topology ispresent again. Responsible to the hole topology at this scale are a fewsuperholes which seem mainly associated with supernova explosions in the outerdisk. The gaps between the bar and spiral arms have a minor effect on thetopology at this scale.

Autor: S. Kim, C. Park


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