GV Tau N中关键益生元分子的气体运动学揭示了ALMA、PdBI和Herschel协同作用
Gas kinematics of key prebiotic molecules in GV Tau N revealed with an ALMA, PdBI, and Herschel synergy
摘要：
利用空间和地面近红外设施，人们已经作出了很大的努力来探测星周盘行星形成区的暖气体。GV Tau N是GV Tau系统中最模糊的组分，是一个突出的来源，是HCN中检测到的第一个靶标之一，也是迄今为止在CH $_4$中检测到的唯一一个靶标。虽然近红外观测揭示了它的化学成分，但星周物质的物理结构和运动学仍然未知。我们使用干涉图像的HCN 3-2和$^{13}$ CO 3-2线，和远红外观测的$^{13}$ CO，HCN，CN和H $_2$ O转换辨别的形态，运动学和化学的致密气体接近恒星。这些观察结果构成了对GV Tau N的H $_2$ O的首次检测。此外，ALMA高空间分辨率（~ 7 au）图像的连续在1.1毫米和HCN 3-2线解决不同的气体成分对GV Tau N，一个气体盘与R~25 au，电离射流，和一个（或两个）分子流出。气盘的不对称形态表明它已被射流侵蚀。所有的观测结果都可以解释，如果GV Tau N是双星，并且其主要组成部分相对于环双星盘有一个高度倾斜的独立盘。我们讨论了水和其他分子的排放根据这种情况下的起源。特别是，我们建议，水的排放将来自中断的气体盘和分子外流。
英文摘要：
A large effort has been made to detect warm gas in the planet formation zone of circumstellar discs using space and ground-based near infrared facilities. GV Tau N, the most obscured component of the GV Tau system, is an outstanding source, being one of the first targets detected in HCN and the only one detected in CH$_4$ so far. Although near infrared observations have shed light on its chemical content, the physical structure and kinematics of the circumstellar matter remained unknown. We use interferometric images of the HCN 3-2 and $^{13}$CO 3-2 lines, and far-IR observations of $^{13}$CO, HCN, CN and H$_2$O transitions to discern the morphology, kinematics, and chemistry of the dense gas close to the star. These observations constitute the first detection of H$_2$O towards GV Tau N. Moreover, ALMA high spatial resolution (~ 7 au) images of the continuum at 1.1 mm and the HCN 3-2 line resolve different gas components towards GV Tau N, a gaseous disc with R~25 au, an ionized jet, and one (or two) molecular outflows. The asymmetric morphology of the gaseous disc shows that it has been eroded by the jet. All observations can be explained if GV Tau N is binary, and the primary component has a highly inclined individual disc relative to the circumbinary disc. We discuss the origin of the water and the other molecules emission according to this scenario. In particular, we propose that the water emission would come from the disrupted gaseous disc and the molecular outflows.
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