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arXiv 1604.06010astro-ph.GA
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大麦云星云N159东侧大质量星YSO周围分子气体的运动学结构

Kinematic Structure of Molecular Gas around High-mass Star YSO, Papillon Nebula, in N159 East in the Large Magellanic Cloud

Kazuya Saigo, Toshikazu Onishi, Omnarayani Nayak, Margaret Meixner, Kazuki Tokuda, Ryohei Harada, Yuuki Morioka, Marta Sewilo, Remy Indebetouw, Kazufumi Torii, … 展开作者

Kazuya Saigo, Toshikazu Onishi, Omnarayani Nayak, Margaret Meixner, Kazuki Tokuda, Ryohei Harada, Yuuki Morioka, Marta Sewilo, Remy Indebetouw, Kazufumi Torii, Akiko Kawamura, Akio Ohama, Yusuke Hattori, Hiroaki Yamamoto, Kengo Tachihara, Tetsuhiro Minamidani, Tsuyoshi Inoue, Suzanne Madden, Maud Galametz, Vianney Lebouteiller, C. -H. Rosie Chen, Norikazu Mizuno, Yasuo Fukui

备注：
28 pages, 7 figures. Submitted to ApJ
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摘要：

本文给出了大麦云（LMC）中N159东巨分子云（N159 E）的ALMA波段3和波段6的~（12）CO（2 - 1）、~（13）CO（2-1）、~（30）Halpha复合线、~（98）GHz附近的自由-自由辐射和~（230）GHz附近的尘埃热辐射结果。大麦哲伦星系是距离地球最近的活动大质量恒星形成星系，距离地球约50千秒差距，是研究大质量恒星形成的最佳目标。ALMA观测表明，N159 E是一个宽约1 pc、长约5 pc - 10 pc的对流云复合体。根据13 CO（2-1）的强度，总分子量为0.92 x 10^5 Msun。N159 E拥有著名的Papillon星云，一个紧凑的高激发HII区域。我们发现与蝶形星云有关的YSO质量为35 Msun，位于三个对流云的交汇处。结果表明，高质量YSO的形成是由对流云碰撞引起的。Fukui等人在2015年报告了N159西部区域的YSO的类似运动学结构，这是这两个区域中质量大于35 Msun的另一个YSO。这表明，对流云的碰撞是大质量恒星形成的主要机制。我们在蝶形星云的YSO周围发现了一个亚pc尺度的小分子洞。它由自由-自由和H30 α发射填充。空穴周围的分子气体温度达到~ 80 K。这表明，这颗YSO刚刚开始破坏母体分子云。

英文摘要：

We present the ALMA Band 3 and Band 6 results of 12CO(2-1), 13$CO(2-1), H30alpha recombination line, free-free emission around 98 GHz, and the dust thermal emission around 230 GHz toward the N159 East Giant Molecular Cloud (N159E) in the Large Magellanic Cloud (LMC). LMC is the nearest active high-mass star forming face-on galaxy at a distance of 50 kpc and is the best target for studing high-mass star formation. ALMA observations show that N159E is the complex of filamentary clouds with the width and length of ~1 pc and 5 pc - 10 pc, respectively. The total molecular mass is 0.92 x 10^5 Msun from the 13CO(2-1) intensity. N159E harbors the well-known Papillon Nebula, a compact high-excitation HII region. We found that a YSO associated with the Papillon Nebula has the mass of 35 Msun and is located at the intersection of three filamentary clouds. It indicates that the formation of the high-mass YSO was induced by the collision of filamentary clouds. Fukui et al. 2015 reported a similar kinematic structure toward a YSO in the N159 West region which is another YSO that has the mass larger than 35 Msun in these two regions. This suggests that the collision of filamentary clouds is a primary mechanism of high-mass star formation. We found a small molecular hole around the YSO in Papillon Nebula with sub-pc scale. It is filled by free-free and H30alpha emission. Temperature of the molecular gas around the hole reaches ~ 80 K. It indicates that this YSO has just started the distruction of parental molecular cloud.

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