发表机构
Aryabhatta Research Institute of Observational Sciences (ARIES); Department of Applied Physics, Mahatma Jyotiba Phule Rohilkhand University; Astronomy & Astrophysics Division, Physical Research Laboratory; Department of Applied Physics/Physics, Bareilly College（阿里亚哈塔观测科学研究所以; 马哈拉贾约提巴普尔罗希勒坎德大学应用物理系; 物理研究实验室天体物理学与天文学部; 贝莱利学院应用物理/物理系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究通过多波段观测揭示LDN 1204-Sh2 145-Sh2 140复合体中恒星反馈驱动的壳膨胀与相互作用压缩交界面气体，促进纤维形成和恒星形成。
AI 中文摘要
我们对一个包含LDN 1204、Sh2 145和Sh2 140区域的扩展分子云进行了多波段研究，以探究恒星反馈、云动力学和恒星形成之间的相互作用。红外图像揭示了两个与已知大质量O型星相关的半弧形/壳状结构（尺度14-18 pc）。Herschel温度和柱密度图在LDN 1204A和LDN 1204B两个子区域中识别出一个候选的枢纽-纤维系统（HFS），其峰值柱密度分别为3.1 x 10^23和1.3 x 10^23 cm^-2。这两个子区域位于Sh2-145 H ii区的边缘。分子谱线数据揭示了一个大型弧形/壳状云，可分解为两个运动学上不同的成分，速度范围分别为-15至-9.5 km s^-1和-9至-3 km s^-1。每个成分均呈现弧形/壳状形态，以其中一颗大质量恒星为中心，并显示出倒C形的位置-速度结构，表明其由相关的H ii区驱动膨胀。两个LDN子区域均位于两个膨胀云成分的投影交界面处。年轻恒星天体（YSO），尤其是Class I型YSO，集中分布于这些子区域，而矩2图显示出增强的速度弥散，表明交界面处的湍流运动增强。总体而言，LDN 1204子区域中致密纤维、候选枢纽-纤维系统以及活跃恒星形成的存在表明，反馈驱动的壳膨胀和相互作用在交界面处压缩了气体，为纤维形成和持续的恒星形成创造了必要条件。这些结果凸显了反馈驱动的云相互作用在调控分子云中致密结构形成和恒星形成方面的重要作用。
英文摘要
We present a multi-wavelength study of an extended molecular cloud hosting the LDN 1204, Sh2 145, and Sh2 140 regions to investigate the interplay between stellar feedback, cloud dynamics, and star formation. Infrared images reveal two semi-arc/shell-like structures (extent 14-18 pc) associated with known massive O-type stars. Herschel temperature and column density maps identify one hub-filament system (HFS) candidate toward both LDN 1204A and LDN 1204B sub-regions, with peak column densities of 3.1 x 10^23 and 1.3 x 10^23 cm^-2, respectively. These sub-regions are located at the periphery of the Sh2-145 H ii region. Molecular line data reveal a large arc-/shell-like cloud resolved into two kinematically distinct components spanning -15 to -9.5 km s^-1 and -9 to -3 km s^-1. Each component exhibits an arc-/shell-like morphology, is centered on one of the massive stars, and displays an inverted C-shaped position-velocity structure, indicating expansion driven by its associated H ii region. Both LDN sub-regions are located at the projected interface of the two expanding cloud components. Young stellar objects (YSOs), particularly Class I YSOs, are concentrated toward these sub-regions, while moment 2 maps reveal enhanced velocity dispersion, suggesting increased turbulent motions at the interface. Altogether, the presence of dense filaments, candidate hub-filament systems, and active star formation in LDN 1204 sub-regions demonstrates that feedback driven shell expansion and interaction compressed the gas at the interface, establishing the necessary conditions for filaments and ongoing star formation. These results highlight the important role of feedback-driven cloud interactions in regulating dense structure formation and star formation in molecular clouds.
Comments24 pages, 10 figures. Accepted for publication in ApJ
