高角分辨率圆盘子结构计划（DSHARP）：X.金牛座T星周围有多个环、一个未对准的内盘和一个明亮的弧形HD 143006
The Disk Substructures at High Angular Resolution Project (DSHARP): X. Multiple rings, a misaligned inner disk, and a bright arc in the disk around the T Tauri star HD 143006
摘要：
我们提出了一个详细的分析新的ALMA观测的磁盘周围的T-Tauri星HD 143006，在46质量（7.6金）的分辨率揭示了新的子结构在1.25毫米连续发射。圆盘分解成一系列同心环和间隙，环外部有一个明亮的弧形，类似于漩涡的流体动力学模拟，以及连接两个最里面的环的桥状特征。虽然我们的$^{12}$ CO观测在类似的空间分辨率没有显示出明显的子结构，他们揭示了一个内盘耗尽的CO排放。从连续辐射和CO速度场我们发现，最内环比最外环和弧有更大的倾角。这是内外盘之间小（$\sim8^{\circ}$）或中等（$\sim41^{\circ}$）未对准的证据，这取决于内外盘近/远侧的特定方向。我们比较了ALMA观测中观察到的子结构与最近的散射光数据从VLT/SPHERE这个对象。特别是，SPHERE图像中狭窄阴影线的位置与压力标度高度估计相结合，有利于大约$41^{\circ}$的大失准。我们讨论了我们的研究结果的背景下，尘埃捕获的漩涡，行星雕刻的差距，和错位的内盘由于存在一个倾斜的同伴HD 143006。
英文摘要：
We present a detailed analysis of new ALMA observations of the disk around the T-Tauri star HD 143006, which at 46 mas (7.6 au) resolution reveal new substructures in the 1.25 mm continuum emission. The disk resolves into a series of concentric rings and gaps together with a bright arc exterior to the rings that resembles hydrodynamics simulations of a vortex, and a bridge-like feature connecting the two innermost rings. Although our $^{12}$CO observations at similar spatial resolution do not show obvious substructure, they reveal an inner disk depleted of CO emission. From the continuum emission and the CO velocity field we find that the innermost ring has a higher inclination than the outermost rings and the arc. This is evidence for either a small ($\sim8^{\circ}$) or moderate ($\sim41^{\circ}$) misalignment between the inner and outer disk, depending on the specific orientation of the near/far sides of the inner/outer disk. We compare the observed substructures in the ALMA observations with recent scattered light data from VLT/SPHERE of this object. In particular, the location of narrow shadow lanes in the SPHERE image combined with pressure scale height estimates, favor a large misalignment of about $41^{\circ}$. We discuss our findings in the context of a dust-trapping vortex, planet-carved gaps, and a misaligned inner disk due to the presence of an inclined companion to HD 143006.
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