论文标题
Carina辐射的西墙的Alma数据单元和连续图
ALMA Datacubes and Continuum Maps of the Irradiated Western Wall in Carina
论文作者
论文摘要
我们介绍了$^{12} $ co的连续和线排放的观察结果，$^{13} $ CO，C $^{18} $ O和[C I]在Carina Star-Forming Complect的G287.38-0.62（CAR 1-E）地区的一部分中。新数据记录了分子云在经受强大的辐射界面时如何在子弧度尺度上做出反应，并提供有关包含最庞大的年轻恒星的区域内恒星形成的整体过程的见解。地图显示了视线上的几种分子云超级斑点，包括西墙的一部分，这是一个高度辐射的云，位于年轻的星团群框架附近。与理论一致，从荧光的h $ _2 $，[c i]到c $^{18} $ o，从荧光的h $ _2 $，to pdr pdr pdr pdr。从光学厚的$^{12} $ CO发出的排放遍布整个区域，而$^{13} $ CO，[C I]，尤其是C $^{18} $ O更薄，并集中于靠近PDR接口的团块和细丝。在西墙云本身中，我们在C $^{18} $ O的数据存储中识别254个不同的核心大小团块。这些对象的质量分布与恒星IMF的质量分布相似。除了大规模的速度梯度外，团块径向速度还缺乏任何空间相干大小。没有直接的证据表明在西墙触发恒星形成，表明其c $^{18} $ o团块和连续岩心似乎没有明星，没有支柱。但是，云的最密集的部分位于最接近PDR，并且沿辐射前线扁平的C $^{18} $ O发射。
We present ALMA observations of the continuum and line emission of $^{12}$CO, $^{13}$CO, C$^{18}$O, and [C I] for a portion of the G287.38-0.62 (Car 1-E) region in the Carina star-forming complex. The new data record how a molecular cloud responds on subarcsecond scales when subjected to a powerful radiation front, and provide insights into the overall process of star formation within regions that contain the most massive young stars. The maps show several molecular clouds superpose upon the line of sight, including a portion of the Western Wall, a highly-irradiated cloud situated near the young star cluster Trumpler 14. In agreement with theory, there is a clear progression from fluoresced H$_2$, to [C I], to C$^{18}$O with distance into the PDR front. Emission from optically thick $^{12}$CO extends across the region, while $^{13}$CO, [C I] and especially C$^{18}$O are more optically thin, and concentrate into clumps and filaments closer to the PDR interface. Within the Western Wall cloud itself we identify 254 distinct core-sized clumps in our datacube of C$^{18}$O. The mass distribution of these objects is similar to that of the stellar IMF. Aside from a large-scale velocity gradient, the clump radial velocities lack any spatial coherence size. There is no direct evidence for triggering of star formation in the Western Wall in that its C$^{18}$O clumps and continuum cores appear starless, with no pillars present. However, the densest portion of the cloud lies closest to the PDR, and the C$^{18}$O emission is flattened along the radiation front.
