Gas kinematics and star formation in the filamentary molecular cloud G47.06+0.26
Gas kinematics and star formation in the filamentary molecular cloud G47.06+0.26
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DOI：
10.1051/0004-6361/201629189
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发表时间：
2017-08
期刊：
影响因子：
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通讯作者：
Jin-Long Xu;Ye Xu;Chuan-peng Zhang;Xiao-Lan Liu;N. Yu;C. Ning;B. Ju
中科院分区：
文献类型：
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作者：
Jin-Long Xu;Ye Xu;Chuan-peng Zhang;Xiao-Lan Liu;N. Yu;C. Ning;B. Ju
为了研究气体运动学和星星的形成，我们对对流云G47.06+0.26进行了多波长研究。利用紫金山天文台（PMO）13.7 m射电望远镜对G47.06+0.26的12 CO（J = 1 - 0）、13 CO（J=1-0）和C18 O（J=1-0）观测资料，详细研究了暗条的运动学. G47.06+0.26的~（12）CO（J = 1 -0）和~（13）CO（J=1-0）的发射光谱显示出一种晶体结构。灯丝沿东西方向延伸约45弧分（58.1 pc）沿着。平均宽度约为6.8pc，由13 CO（J=1-0）排放跟踪。G47.06+0.26具有约361.5Msun/pc的线性质量密度。外部压力（由于相邻的气泡和H II区域）可以帮助防止长丝在湍流的影响下分散。从速度场图中，我们可以看出垂直于G47.06+0.26的速度梯度。从Bolocam银道巡天（BGPS）星表中，我们发现了G47.06+0.26中的9个BGPS源，这些源似乎有足够的质量形成大质量恒星。实验结果表明，纤维中的团簇形成效率约为18%。发现四个红外气泡位于G47.06+0.26中并与其相邻。特别是，红外气泡N98显示出彗星结构。邻近N98的CO分子气体也显示出非常强的发射。与红外气泡相关的H II区域可以将能量注入周围气体。我们计算了G47.06+0.26中两个H II区的动能、电离能和热能。从GLIMPSE I星表中，我们选择了一些年龄约为10万年的I类源，它们沿着暗条聚集。来自H II区的反馈可能导致暗条G47.06+0.26中新一代恒星的形成。
We performed a multi-wavelength study toward the filamentary cloud G47.06+0.26 to investigate the gas kinematics and star formation. We present the 12CO (J=1-0), 13CO (J=1-0) and C18O (J=1-0) observations of G47.06+0.26 obtained with the Purple Mountain Observation (PMO) 13.7 m radio telescope to investigate the detailed kinematics of the filament. The 12CO (J=1-0) and 13CO (J=1-0) emission of G47.06+0.26 appear to show a filamentary structure. The filament extends about 45 arcmin (58.1 pc) along the east-west direction. The mean width is about 6.8 pc, as traced by the 13CO (J=1-0) emission. G47.06+0.26 has a linear mass density of about 361.5 Msun/pc. The external pressure (due to neighboring bubbles and H II regions) may help preventing the filament from dispersing under the effects of turbulence. From the velocity-field map, we discern a velocity gradient perpendicular to G47.06+0.26. From the Bolocam Galactic Plane Survey (BGPS) catalog, we found nine BGPS sources in G47.06+0.26, that appear to these sources have sufficient mass to form massive stars. We obtained that the clump formation efficiency (CFE) is about 18% in the filament. Four infrared bubbles were found to be located in, and adjacent to, G47.06+0.26. Particularly, infrared bubble N98 shows a cometary structure. CO molecular gas adjacent to N98 also shows a very intense emission. H II regions associated with infrared bubbles can inject the energy to surrounding gas. We calculated the kinetic energy, ionization energy, and thermal energy of two H II regions in G47.06+0.26. From the GLIMPSE I catalog, we selected some Class I sources with an age of about 100000 yr, which are clustered along the filament. The feedback from the H II regions may cause the formation of a new generation of stars in filament G47.06+0.26.