标题： CQ Tau和MWC 758周围动态扰动的原行星盘中的SO发射 显示英文标题

标题： SO emission in the dynamically perturbed protoplanetary disks around CQ Tau and MWC 758

摘要： 我们报告在档案中的阿塔卡马大型毫米波/亚毫米波阵列(ALMA)观测中意外检测到围绕CQ Tau的螺旋状原行星盘（具有$\approx4.9\sigma$显著性）和MWC 758（具有$\approx3.4\sigma$显著性）中的SO$J_N=6_5-5_4$（219.949 GHz）旋转跃迁。 在前者中，SO辐射呈环状，来源于连续谱空腔的边缘，并在目前可用的光谱分辨率下定性上与开普勒旋转一致。 而在后者中，虽然SO辐射主要来自连续谱空腔内部，但也延伸到连续谱环，其形态和动力学不太清晰。 我们将这些源置于其他已报道SO检测的原行星盘的背景下，并讨论SO可能的起源，即（热）解吸或气相中的形成。 我们认为这些过程可能由未被观测到的嵌入式大质量伴星、阴影或晚期吸积引起的动态扰动所促进，从而暗示了扰动的动力学与（这些）原行星盘中SO辐射之间可能存在联系。 如果得到证实，我们的解释将意味着这些系统中的化学演化时间尺度可能比通常假设的要短得多，表明动态扰动可能通过改变其形成环境的挥发物组成来影响新生（原）行星的成分。 显示英文摘要

摘要： We report the serendipitous detection of the SO $J_N=6_5-5_4$ (219.949 GHz) rotational transition in archival Atacama Large Millimeter/submillimeter Array (ALMA) observations of the spiral hosting protoplanetary disks around CQ Tau (with $\approx4.9\sigma$ significance) and MWC 758 (with $\approx3.4\sigma$ significance). In the former, the SO emission comes in the shape of a ring, arises from the edge of the continuum cavity, and is qualitatively consistent, at the currently available spectral resolution, with being in Keplerian rotation. In the latter, instead, while arising primarily from inside the continuum cavity, the SO emission also extends to the continuum ring(s), and its morphology and kinematics are less clear. We put these sources in the context of the other protoplanetary disks where SO detections have been previously reported in the literature and discuss the possible origins of SO in terms of (thermal) desorption or formation in the gas phase. We argue that these processes might be fostered by dynamical perturbations caused by unseen embedded massive companions, shadows, or late-time infall, thus suggesting a possible link between perturbed dynamics and SO emission in (these) protoplanetary disks. If confirmed, our interpretation would imply that chemical evolution timescales could be significantly shorter in these systems than is commonly assumed, indicating that dynamical perturbations might influence the composition of newborn (proto-)planets by altering the volatile makeup of their formation environment.