来自UWISH2的银河平面中的YSO喷流：III -仙后座和御夫座中的喷流和外流
YSO jets in the Galactic Plane from UWISH2: III - Jets and Outflows in Cassiopeia and Auriga
摘要：
我们分析了来自英国对仙后座和御夫座的H2宽视场红外巡天（UWISH 2）的H2 1- 0 S（1）线中35.5平方度的图像。我们已经确定了98个由年轻恒星驱动的分子氢发射线天体，其中60%是双极流出，都是新发现的。我们估计，UWISH 2扩展的排放对象目录包含少于%的假阳性，并在95%的水平上完成了比UWISH 2检测限更亮的喷流和流出物。我们为四分之三的检测到的外流确定了可靠的驱动源候选者，其中40%与恒星群和星团有关。驱动源候选者是20%的原恒星，其余的是CTTS。我们还确定了15个新的星团候选人附近的MHO的调查区域。我们发现，在样本中识别出的典型流出具有以下特征：位置角随机取向，双极流出在几度范围内是直的，两个叶的长度和亮度略有不对称，叶的长度和亮度不相关，典型的时间间隔之间的主要喷射的材料是1- 3 kyr，因此FU-Ori或EX-Ori喷发是最有可能的原因，这些，但我们建议MNors作为一个可能的来源。此外，我们发现，流出叶长度分布是统计上的差异，从广泛使用的总长度分布。有一个比预期的更大数量的明亮的流出，表明通量分布不遵循幂律。
英文摘要：
We present the analysis of 35.5 square degrees of images in the 1-0S(1) line of H2 from the UK Widefield Infrared Survey for H2 (UWISH2) towards Cassiopeia and Auriga. We have identified 98 Molecular Hydrogen emission-line Objects (MHOs) driven by Young Stellar Objects, 60% of which are bipolar outflows and all are new discoveries. We estimate that the UWISH2 extended emission object catalogue contains fewer than % false positives and is complete at the 95% level for jets and outflows brighter than the UWISH2 detection limit. We identified reliable driving source candidates for three quarters of the detected outflows, 40% of which are associated with groups and clusters of stars. The driving source candidates are 20% protostars, the remainder are CTTSs. We also identified 15 new star cluster candidates near MHOs in the survey area. We find that the typical outflow identified in the sample has the following characteristics: the position angles are randomly orientated; bipolar outflows are straight within a few degrees; the two lobes are slightly asymmetrical in length and brightness; the length and brightness of the lobes are not correlated; typical time gaps between major ejections of material are 1-3kyr, hence FU-Ori or EX-Ori eruptions are most likely not the cause of these, but we suggest MNors as a possible source. Furthermore, we find that outflow lobe length distributions are statistically different from the widely used total length distributions. There are a larger than expected number of bright outflows indicating that the flux distribution does not follow a power law.
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