Th ~（28）喷流的MUSE光谱成像研究：喷流内部的进动
A MUSE Spectro-imaging Study of the Th 28 Jet: Precession in the Inner Jet
摘要：
背景：Th 28是一颗位于狼疮3星云中的经典金牛座T星，它驱动着一个扩展的双极喷流。以前的研究内喷流确定签名的旋转周围的流出轴，一个关键的结果，理论的喷射发射。因此，这是一个重要的来源，其中调查知之甚少的喷气发动机的机制。我们调查的Th 28微射流的形态和运动学，其目的是表征其结构和流出活动，使用VLT/MUSE获得的光学积分场光谱观测。我们使用光谱成像和位置-速度图来研究喷流的运动学和形态特征，并获得可见喷流的发射线目录。Lucy-Richardson反卷积程序用于区分内部微射流区域的结构。垂直于射流轴线提取的空间轮廓进行拟合，以研究射流宽度，开度角和射流轴线的演变。我们确认以前确定的结HHW $_{2}$内的红移喷流，并确定三个额外的结在每个叶的第一次。我们还发现[O III] $λ$ 5007发射的蓝移微喷流，包括结最接近的恒星。自行车的最里面的结在每一边的估计，我们表明，新的结喷射的近似时间尺度为10-15年。喷流轴的质心在两个微喷流的内部显示出点对称的摆动，这表明进动。我们用喷流的形状来测量8年的岁差周期，半张角< 0.6 $^{\circ}$。这可能为先前报告的旋转签名提供另一种解释。我们发现喷流的形状是兼容的岁差由于一个棕矮星同伴轨道分离$\leq$ 0.3 AU。
英文摘要：
Context: Th 28 is a Classical T Tauri star in the Lupus 3 cloud which drives an extended bipolar jet. Previous studies of the inner jet identified signatures of rotation around the outflow axis, a key result for theories of jet launching. Thus this is an important source in which to investigate the poorly understood jet launching mechanism. We investigate the morphology and kinematics of the Th 28 micro-jets with the aim of characterizing their structure and outflow activity, using optical integral-field spectroscopy observations obtained with VLT/MUSE. We use spectro-imaging and position-velocity maps to investigate the kinematic and morphological features of the jet, and obtain a catalogue of emission lines in which the jet is visible. A Lucy-Richardson deconvolution procedure is used to differentiate the structure of the inner micro-jet region. Spatial profiles extracted perpendicular to the jet axis are fitted to investigate the jet width, opening angle and the evolution of the jet axis. We confirm the previously identified knot HHW$_{2}$ within the red-shifted jet and identify three additional knots in each lobe for the first time. We also find [O III]$λ$5007 emission from the blue-shifted micro-jet including the knot closest to the star. Proper motions for the innermost knots on each side are estimated and we show that new knots are ejected on an approximate timescale of 10-15 years. The jet axis centroids show a point-symmetric wiggle within the inner portion of both micro-jets indicating precession. We use the jet shape to measure a precession period of 8 years, with a half-opening angle < 0.6$^{\circ}$. This may provide an alternative explanation for the rotation signatures previously reported. We find the jet shape to be compatible with precession due to a brown dwarf companion orbiting at a separation $\leq$ 0.3 au.
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