论文标题
丝状红外云的Artémis成像G1.75-0.08和G11.36+0.80：云及其团块的基于灰尘的物理特性
ArTéMiS imaging of the filamentary infrared dark clouds G1.75-0.08 and G11.36+0.80: Dust-based physical properties of the clouds and their clumps
论文作者
论文摘要
我们使用Artémisbolometer对红色的红云（IRDC）G1.75-0.08和G11.36+0.80+0.80+0.80。这些数据与我们以前的870美元$ $ M $ M的观察结果一起使用，该数据与大顶点重计摄像头（Laboca）一起使用。在n $ _2 $ _2 $ h $^+（1-0）$中，g11.36+0.80中的团块也观察到了IRAM 30米望远镜的过渡。发现G1.75-0.08被发现由两个感冒（$ \ sim14.5 $ k）组成，大量（几个$ \ sim10^3 $ m $ _ {\ odot} $）由$ \ sim3.7 $ PC投射分开。这两个团块都是70美元的黑暗，但它们似乎并没有受到自我重度的界限。发现G1.75-0.08细丝相对于其临界线质量而言是$ \ sim14 $的因数。发现G11.36+0.80是超临界的中等（以$ \ sim2 $为倍），由四个团组成。团块的灰尘温度为$ \ sim13-15 $ k，其质量在$ \ sim 232-633 $ m $ _ {\ odot} $中。所有的团块都在重力上。预计的平均分离是$ \ sim1 $ PC。在G1.75-0.08中观察到的配置，即细丝末端的两个团块，可能是引力聚焦沿云作用的结果。这两个团块满足了高质量星形组的Mass-Radius阈值。由于G1.75-0.08在银河中心附近的位置（$ \ sim270 $ PC），环境效果（例如高湍流，潮汐力和剪切运动）可能会影响云动力学。 G11.36+0.80中观察到的团块分离可以通过香肠不稳定性来理解。 G11.36+0.80团块不位于高质量恒星形成的质量拉迪乌斯阈值之上。在G11.36+0.80中的一个团块中观察到的子结构表明，IRDC已以层次结构的方式分散。这符合银河恒星形成的丝状范例。
We imaged the infrared dark clouds (IRDCs) G1.75-0.08 and G11.36+0.80 at 350 $μ$m and 450 $μ$m using the ArTéMiS bolometer. These data were used in conjunction with our previous 870 $μ$m observations with the Large APEX BOlometer CAmera (LABOCA). The clumps in G11.36+0.80 were also observed in the N$_2$H$^+(1-0)$ transition with the IRAM 30-metre telescope. G1.75-0.08 was found to be composed of two cold ($\sim14.5$ K), massive (several $\sim10^3$ M$_{\odot}$) clumps that are projectively separated by $\sim3.7$ pc. Both clumps are 70 $μ$m dark, but they do not appear to be bounded by self-gravity. The G1.75-0.08 filament was found to be subcritical by a factor of $\sim14$ with respect to its critical line mass. G11.36+0.80 was found to be moderately (by a factor of $\sim2$) supercritical and composed of four clumps. The dust temperatures of the clumps are $\sim13-15$ K, and their masses are in the range $\sim 232-633$ M$_{\odot}$. All the clumps are gravitationally bound. The projected, average separation of the clumps is $\sim1$ pc. A configuration that is observed in G1.75-0.08, namely two clumps at the ends of the filament, could be the result of gravitational focussing acting along the cloud. The two clumps fulfil the mass-radius threshold for high-mass star formation. Owing to the location of G1.75-0.08 near the Galactic centre ($\sim270$ pc), environmental effects such as a high level of turbulence, tidal forces, and shearing motions could affect the cloud dynamics. The observed clump separation in G11.36+0.80 can be understood in terms of a sausage instability. The G11.36+0.80 clumps do not lie above the mass-radius threshold for high-mass star formation. The substructure observed in one of the clumps in G11.36+0.80 suggests that the IRDC has fragmented in a hierarchical fashion. This conforms to the filamentary paradigm for Galactic star formation.
