标题： 解开围绕膨胀银河红外泡的反馈调节恒星形成活动 [HKS2019] E71 显示英文标题

标题： Unraveling the Feedback-Regulated Star Formation Activities around the Expanding Galactic MIR Bubble [HKS2019] E71

摘要： 我们通过多波长方法探索银河系中红外 (MIR) 泡泡 [HKS2019] E71（以下简称 E71）的物理环境。E71 位于丝状结构的边缘，如赫歇尔图像（250-500$\mu$m）、赫歇尔柱密度图以及速度范围 [-20,-14] km/s 内的分子图所示。它包含一个恒星团（半径~1.26 pc，距离~1.81+/-0.15 kpc），与射电连续谱辐射有关，包括一个中心定位的 B1.5 型大质量恒星（以下简称 'm2'），以及演化的低质量恒星和年轻恒星物体的增强种群。MIR 图像和分子线图显示 'm2' 周围存在一个 PDR，沿 E71 边缘呈现出弧形结构。在此结构上识别出规则间隔的分子和尘埃凝聚体。12CO 发射的位移-速度图表明分子气体在 E71 边缘集中并正在膨胀。近红外光谱观测使用 TANSPEC 确认了靠近气泡边缘的大质量年轻恒星物体（MYSO）中的吸积过程的存在。高分辨率 uGMRT 射电连续谱图揭示了电离辐射中的子结构，分别朝向 MYSO 和 E71 的中心。这些发现支持 'm2' 通过其反馈过程形成了弧形形态。'm2' 所施加的压力以及 12/13CO(1-0) 发射的速度结构表明，恒星反馈可能已经驱散了分子物质，导致了膨胀的 E71 气泡的形成。我们的整体调查推断，"收集和坍缩" 过程可能是描述 E71 气泡周围正在进行的恒星形成活动的一种可能机制。 显示英文摘要

摘要： We explore the physical environment of the Galactic mid-infrared (MIR) bubble [HKS2019] E71 (hereafter E71) through a multi-wavelength approach. E71 is located at the edge of a filamentary structure, as traced in Herschel images (250-500 $\mu$m), Herschel column density map, and molecular maps in the velocity range [-20,-14] km/s. It hosts a stellar cluster (radius~1.26 pc, distance~1.81+/-0.15 kpc) associated with radio continuum emission, including a centrally positioned B1.5-type massive star (hereafter 'm2'), along with an enhanced population of evolved low-mass stars and young stellar objects. MIR images and molecular line maps reveal a PDR surrounding 'm2', exhibiting an arc-like structure along the edges of E71. Regularly spaced molecular and dust condensations are identified along this structure. The position-velocity map of 12CO emission suggests an expansion of molecular gas concentrated at the periphery of E71. Near-infrared spectroscopic observations with TANSPEC confirm the presence of the accretion process in a massive young stellar object (MYSO) located near the edge of the bubble. High-resolution uGMRT radio continuum maps uncover substructures in the ionized emission, both toward the MYSO and the center of E71. These findings support that 'm2' has shaped an arc-like morphology through its feedback processes. The pressure exerted by 'm2' and the velocity structure of the 12/13CO(1-0) emission suggest that the stellar feedback has likely driven out molecular material, leading to the formation of the expanding E71 bubble. Our overall investigation infers that the "collect and collapse" process might be a possible mechanism that can describe the ongoing star formation activities around the E71 bubble.