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Revealing the Large-Scale Structures of Interstellar Gas Associated with the Magellanic SNR N132D

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arxiv 1503.04390 v1 pith:6UVF2GSD submitted 2015-03-15 astro-ph.GA astro-ph.HE

H. Sano , Y. Fukui , S. Yoshiike , T. Fukuda , K. Tachihara , S. Inutsuka , A. Kawamura , K. Fujii
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N. Mizuno T. Inoue T. Onishi F. Acero J. Vink
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keywords large-scalemagellanicmopran132dstructurestowardalmaalong
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abstract

We report preliminary results of large-scale distribution toward the Magellanic supernova remnant N132D using Mopra and Chandra archival datasets. We identified a cavity-like CO structure along the X-ray shell toward the southern half of it. The total mass of associating molecular gas is $\sim10^4 M_\odot$, which is smaller than the previous study by an order of magnitude. Further observations using ALMA, ASTE, and Mopra will reveal the detailed spatial structures and its physical conditions.

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