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Massive star formation in the Carina nebula complex and Gum 31. I. the Carina nebula complex
Publications of the Astronomical Society of Japan ( IF 2.2 ) Pub Date : 2020-08-19 , DOI: 10.1093/pasj/psaa078
Shinji Fujita 1, 2 , Hidetoshi Sano 1, 3 , Rei Enokiya 1 , Katsuhiro Hayashi 1, 4 , Mikito Kohno 1, 5 , Kisetsu Tsuge 1 , Kengo Tachihara 1 , Atsushi Nishimura 2 , Akio Ohama 1 , Yumiko Yamane 1 , Takahiro OHNO 1 , Rin Yamada 1 , Yasuo Fukui 1
Affiliation  

Herein, we present results from observations of the 12CO (J=1-0), 13CO (J=1-0), and 12CO (J=2-1) emission lines toward the Carina nebula complex (CNC) obtained with the Mopra and NANTEN2 telescopes. We focused on massive-star-forming regions associated with the CNC including the three star clusters Tr14, Tr15, and Tr16, and the isolated WR-star HD92740. We found that the molecular clouds in the CNC are separated into mainly four clouds at velocities -27, -20, -14, and -8 km/s. Their masses are 0.7x10^4Msun, 5.0x10^4 Msun, 1.6x10^4 Msun, and 0.7x10^4 Msun, respectively. Most are likely associated with the star clusters, because of their high 12CO (J=2-1)/12CO (J=1-0) intensity ratios and their correspondence to the Spitzer 8 micron distributions. In addition, these clouds show the observational signatures of cloud--cloud collisions. In particular, there is a V-shaped structure in the position--velocity diagram and a complementary spatial distribution between the -20 km/s cloud and the -14 km/s cloud. Based on these observational signatures, we propose a scenario wherein the formation of massive stars in the clusters was triggered by a collision between the two clouds. By using the path length of the collision and the assumed velocity separation, we estimate the timescale of the collision to be ~1 Myr. This is comparable to the ages of the clusters estimated in previous studies.

中文翻译:

船底座星云复合体和 Gum 31 中的大量恒星形成。 I. 船底座星云复合体

在本文中,我们展示了使用 Mopra 获得的对船底座星云复合体 (CNC) 的 12CO (J=1-0)、13CO (J=1-0) 和 12CO (J=2-1) 发射线的观测结果和 NANTEN2 望远镜。我们专注于与 CNC 相关的大质量恒星形成区域,包括三个星团 Tr14、Tr15 和 Tr16,以及孤立的 WR 星 HD92740。我们发现 CNC 中的分子云主要以 -27、-20、-14 和 -8 km/s 的速度分成四个云。它们的质量分别为 0.7x10^4Msun、5.0x10^4 Msun、1.6x10^4 Msun 和 0.7x10^4 Msun。大多数可能与星团有关,因为它们的 12CO (J=2-1)/12CO (J=1-0) 强度比很高,并且与斯皮策 8 微米分布相对应。此外,这些云显示了云的观测特征——云碰撞。特别是,-20 km/s 云和-14 km/s 云在位置-速度图中存在V 形结构和互补的空间分布。基于这些观测特征,我们提出了一个场景,其中星团中大质量恒星的形成是由两个云之间的碰撞触发的。通过使用碰撞的路径长度和假定的速度间隔,我们估计碰撞的时间尺度为 ~1 Myr。这与先前研究中估计的集群年龄相当。我们提出了一个场景,其中星团中大质量恒星的形成是由两个云之间的碰撞触发的。通过使用碰撞的路径长度和假定的速度间隔,我们估计碰撞的时间尺度为 ~1 Myr。这与先前研究中估计的集群年龄相当。我们提出了一个场景,其中星团中大质量恒星的形成是由两个云之间的碰撞触发的。通过使用碰撞的路径长度和假定的速度间隔,我们估计碰撞的时间尺度为 ~1 Myr。这与先前研究中估计的集群年龄相当。
更新日期:2020-08-19
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