Large-scale CO J=1-0 observations of the giant molecular cloud associated with the infrared ring N35 with the Nobeyama 45-m telescope-猫眼课题宝

DOI：

10.1093/pasj/psy019

发表时间：

2017-10

期刊：

arXiv: Astrophysics of Galaxies

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

K. Torii;S. Fujita;M. Matsuo;A. Nishimura;M. Kohno;M. Kuriki;Y. Tsuda;T. Minamidani;T. Umemoto;N. Kuno;Y. Hattori;S. Yoshiike;A. Ohama;K. Tachihara;K. Shima;A. Habe;Y. Fukui

我们报道了对与银河系红外环状结构N35及其附近的两个HII区G024.392+00.072(HII区A)和G024.510-00.060(HII区B)有关的巨型分子云的观测研究，该观测数据是作为Nobeama 45-m望远镜森林无偏星系平面成像调查的一部分获得的，空间分辨率为21“。CO数据表明，GMC的总分子质量为2.1×10~(-6)Mo，在~10-15公里/S范围内有两个速度分量，在~110-114公里/S范围内，分子气主要由低速分量组成，而在~118-126公里/S范围内的较高速度分量则由位于三个HII区附近的三个较小的分子云组成。LVC和HVC沿视线呈空间互补分布，尽管速度相差约5-15公里/S，并由中等强度的CO排放在速度上联系在一起。通过将观测结果与模拟结果进行比较，我们讨论了这样一种情形，即三个HVC与LVC以大约10-15公里/S的速度相撞时，可以解释这两个观测信号。LVC和HVC之间的中间速度特征可以理解为宽桥特征，它指示了气体在碰撞界面上的湍流运动，而空间互补分布表示HVC通过碰撞在LVC中产生的空洞。我们的模型表明，这三个HII区是在碰撞开始后形成的，因此我们认为GMC中高质量恒星的形成是由碰撞触发的。

We report an observational study of the giant molecular cloud (GMC) associated with the Galactic infrared ring-like structure N35 and two nearby HII regions G024.392+00.072 (HII region A) and G024.510-00.060 (HII region B), using the new CO J=1-0 data obtained as a part of the FOREST Unbiased Galactic Plane Imaging survey with the Nobeyama 45-m telescope (FUGIN) project at a spatial resolution of 21". Our CO data revealed that the GMC, with a total molecular mass of 2.1x10^6Mo, has two velocity components over ~10-15km/s. The majority of molecular gas in the GMC is included in the lower-velocity component (LVC) at ~110-114km/s, while the higher-velocity components (HVCs) at ~118-126km/s consist of three smaller molecular clouds which are located near the three HII regions. The LVC and HVCs show spatially complementary distributions along the line-of-sight, despite large velocity separations of ~5-15km/s, and are connected in velocity by the CO emission with intermediate intensities. By comparing the observations with simulations, we discuss a scenario where collisions of the three HVCs with LVC at velocities of ~10-15km/s can provide an interpretation of these two observational signatures. The intermediate velocity features between the LVC and HVCs can be understood as broad bridge features, which indicate the turbulent motion of the gas at the collision interfaces, while the spatially complementary distributions represent the cavities created in the LVC by the HVCs through the collisions. Our model indicates that the three HII regions were formed after the onset of the collisions, and it is therefore suggested that the high-mass star formation in the GMC was triggered by the collisions.

Large-scale CO J=1-0 observations of the giant molecular cloud associated with the infrared ring N35 with the Nobeyama 45-m telescope

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