发表机构
Universidad Nacional Autónoma de México. Instituto de Astronomía; Mullard Space Science Laboratory, University College London; Department of Astronomy, University of Florida; Kavli Institute for Astronomy and Astrophysics, Peking University; Max-Planck Institute for Astronomy (MPIA); Departamento de Astronomía, Universidad de Chile; Department of Astronomy, University of Michigan; Departamento de Física, Universidad Técnica Federico Santa María; Joint ALMA Observatory（墨西哥国立自治大学天文研究所; 伦敦大学学院穆拉德空间科学实验室; 佛罗里达大学天文学系; 北京大学柯夫利天体物理与天文研究所; 马克斯·普朗克天文学研究所; 智利大学天文学系; 密歇根大学天文学系; 弗雷德里科·圣玛丽亚理工大学物理系; ALMA联合天文台）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过ALMA观测发现J16120原行星盘的尘埃亚结构与气体运动学特征，为盘间隙内正在进行的行星形成提供了新的有力证据。
AI 中文摘要
此前，从2MASS J16120668-301027的原行星盘间隙中，已通过毫米连续谱、红外和H-alpha观测独立报道了行星形成的迹象。本研究利用阿塔卡马大型毫米/亚毫米波阵列（ALMA）7波段观测，为正在进行的行星形成提供了新证据，探测到0.87毫米尘埃连续谱发射，以及12CO（J=3-2）和13CO（J=3-2）谱线发射。对连续谱数据的可见度建模显示，存在一个内盘和两个峰值分别位于23天文单位和75天文单位的尘埃环；相较于轴对称盘，偏心盘模型（偏心率约为0.1）能更好地重现连续谱形态。我们进一步通过对12CO通道图的建模研究气体运动学，残差线宽图显示，在先前报道的候选原行星盘（去投影半径约为32天文单位，方位角约为170度）位置及其轨道上，速度色散出现局域性增加。该信号在空间上与扭结状特征以及亚开普勒速度向超开普勒速度的转变重合。此外，速度残差图显示出从候选行星向外延伸的弧状结构，尽管存在较大不确定性，气体运动学仍与流向候选行星轨道半径的流入过程一致。观测到的速度色散增加与行星-盘相互作用模拟的预测相符，这些模拟在行星位置及其轨道路径上产生增强的湍流。综上，连续谱形态和气体运动学特征为盘间隙内正在进行的行星形成提供了有力的新证据。
英文摘要
Hints of planet formation have been independently reported within the gap of the disc around 2MASS J16120668-301027 from millimetre continuum, infrared, and H-alpha observations. In this work, we present new evidence for ongoing planet formation based on Atacama Large Millimeter/submillimeter Array (ALMA) Band 7 observations, detecting 0.87 mm dust continuum emission together with 12CO (J=3-2) and 13CO (J=3-2) line emission. Visibility modelling of the continuum data reveals an inner disc and two dust rings peaking at 23 and 75 au. The continuum morphology is better reproduced by an eccentric disc model (e approximately 0.1) than by an axisymmetric disc. We further investigate the gas kinematics through modelling of the 12CO channel maps. The residual line-width map shows a localised increase in velocity dispersion at the position of a previously reported circumplanetary disc candidate (deprojected radius approximately 32 au, position angle approximately 170 degrees) and along its orbit. This signal is spatially coincident with kink-like features and a transition from sub-Keplerian to super-Keplerian velocities. In addition, the velocity residual map exhibits an arc-like structure extending outward from the planet candidate, while the gas kinematics, despite substantial uncertainties, is consistent with inflow towards the candidate's orbital radius. The observed increase in velocity dispersion agrees with predictions from planet-disc interaction simulations, which produce enhanced turbulence both at the planet location and along its orbital path. Taken together, the continuum morphology and gas kinematic signatures provide compelling new evidence for ongoing planet formation within the disc gap.
