揭示银河系中红外气泡 [HKS2019] E71 周围由反馈调控的恒星形成活动
Unraveling the Feedback-Regulated Star Formation Activities around the Expanding Galactic MIR Bubble [HKS2019] E71
AI总结：
本文通过多波段观测研究银河系中红外气泡 E71，发现中心大质量恒星的反馈驱动分子气体膨胀并形成弧形结构，支持“收集与坍缩”机制解释其周围的恒星形成活动。
摘要：
我们通过多波段方法探索银河系中红外（MIR）气泡 [HKS2019] E71（以下简称 E71）的物理环境。E71 位于一个纤维状结构的边缘，该结构由 Herschel 图像（250-500 μm）、Herschel 柱密度图以及速度范围在 [-20,-14] km/s 的分子图所追踪。它包含一个恒星团（半径约 1.26 pc，距离约 1.81±0.15 kpc），该恒星团与射电连续谱辐射相关联，其中包括一颗位于中心位置的 B1.5 型大质量恒星（以下简称“m2”），以及增多的演化晚型小质量恒星和年轻恒星天体。MIR 图像和分子谱线图揭示了围绕“m2”的光致离解区（PDR），该区域沿 E71 边缘呈现出弧形结构。沿此结构识别出规则间隔的分子和尘埃凝聚体。12CO 发射的位置-速度图表明分子气体在 E71 外围集中膨胀。利用 TANSPEC 进行的近红外光谱观测证实了位于气泡边缘附近的一个大质量年轻恒星天体（MYSO）中存在吸积过程。高分辨率 uGMRT 射电连续谱图揭示了朝向 MYSO 和 E71 中心的电离发射中的亚结构。这些发现支持“m2”通过其反馈过程塑造了弧形形态。“m2”施加的压力以及 12/13CO(1-0) 发射的速度结构表明，恒星反馈很可能驱动了分子物质外流，从而导致膨胀的 E71 气泡的形成。我们的整体研究推断，“收集与坍缩”过程可能是一种能够描述 E71 气泡周围正在进行的恒星形成活动的机制。
英文摘要：
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 $μ$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.
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