DENSE MOLECULAR CLUMPS ASSOCIATED WITH THE LARGE MAGELLANIC CLOUD SUPERGIANT SHELLS LMC 4 AND LMC 5
DENSE MOLECULAR CLUMPS ASSOCIATED WITH THE LARGE MAGELLANIC CLOUD SUPERGIANT SHELLS LMC 4 AND LMC 5
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DOI：
10.1088/0004-637x/796/2/123
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发表时间：
2014-11
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通讯作者：
K. Fujii;T. Minamidani;N. Mizuno;T. Onishi;A. Kawamura;E. Muller;J. Dawson;K. Tatematsu;T. Hasegawa;T. Tosaki;R. Miura;K. Muraoka;T. Sakai;T. Tsukagoshi;Kunihiko Tanaka;H. Ezawa;Y. Fukui
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作者：
K. Fujii;T. Minamidani;N. Mizuno;T. Onishi;A. Kawamura;E. Muller;J. Dawson;K. Tatematsu;T. Hasegawa;T. Tosaki;R. Miura;K. Muraoka;T. Sakai;T. Tsukagoshi;Kunihiko Tanaka;H. Ezawa;Y. Fukui
通过观测位于两个超巨星壳层LMC 4和LMC 5之间的大麦哲伦云（LMC）恒星形成区N48和N49，研究了超巨星壳层及其相互作用对致密分子团的影响.用ASTE和Mopra望远镜对这些地区进行了~（12）CO（J = 3-2，1-0）和~（13）CO（J = 1-0）的观测。一个密集的分子团簇的集群分布显示与7 pc的空间分辨率。大速度梯度分析表明，团块的分子氢密度（n（H2））从低密度到高密度（103-105 cm-3）分布，并且它们的动力学温度（Tkin）通常很高（大于50 K）。这些团块似乎处于星星形成的早期阶段，Hα的分布、年轻恒星候选者和红外辐射也表明了这一点。结果表明，N48区位于两个星系交界处的高密度H i包层中，星星形成相对演化，而N49区仅与LMC 5有关，星星形成相对平静. N48区域的团块通常表现出高n（H2）和Tkin，它们与LMC大质量星团形成区（30 Dor，N159）的团块一样密集和温暖。这些结果表明，星系的大尺度结构，特别是两个星系之间的相互作用，有效地形成了致密的分子团和恒星。
We investigate the effects of supergiant shells (SGSs) and their interaction on dense molecular clumps by observing the Large Magellanic Cloud (LMC) star-forming regions N48 and N49, which are located between two SGSs, LMC 4 and LMC 5. 12CO (J = 3–2, 1–0) and 13CO(J = 1–0) observations with the ASTE and Mopra telescopes have been carried out toward these regions. A clumpy distribution of dense molecular clumps is revealed with 7 pc spatial resolution. Large velocity gradient analysis shows that the molecular hydrogen densities (n(H2)) of the clumps are distributed from low to high density (103–105 cm−3) and their kinetic temperatures (Tkin) are typically high (greater than 50 K). These clumps seem to be in the early stages of star formation, as also indicated from the distribution of Hα, young stellar object candidates, and IR emission. We found that the N48 region is located in the high column density H i envelope at the interface of the two SGSs and the star formation is relatively evolved, whereas the N49 region is associated with LMC 5 alone and the star formation is quiet. The clumps in the N48 region typically show high n(H2) and Tkin, which are as dense and warm as the clumps in LMC massive cluster-forming areas (30 Dor, N159). These results suggest that the large-scale structure of the SGSs, especially the interaction of two SGSs, works efficiently on the formation of dense molecular clumps and stars.