SPYGLASS. VI. Circinus复合体中的反馈驱动星形成
SPYGLASS. VI. Feedback-Driven Star Formation in the Circinus Complex
AI总结：
本研究首次全面分析了Circinus复合体，发现其恒星年龄结构和动力学特征符合两阶段星形成模型，提出了一种依赖单个中心星团反馈而非传统多世代的顺序星形成新观点。
摘要：
年轻星协提供了追踪星形成过程的记录，而最年轻的星群将前身气体的动力学与最终形成的恒星星群联系起来。因此，我们对Circinus复合体进行了首次全面概述，这是一个研究不足且质量巨大（约1500 M$_{\odot}$）的区域，包含大约3100颗新形成的恒星以及Circinus分子云（CMC）。我们在连续的中心区域（CirCe）发现了一个清晰的年龄模式，即越年轻的恒星距离大质量中心星团越远，且其速度与均匀膨胀一致。通过将这种结构与类似的STARFORGE模拟进行比较，我们发现该星协的年龄结构和动力学与两阶段星形成一致：母云的全球坍缩构建了500 M$_{\odot}$的中心星团ASCC 79，随后在第一批大质量恒星形成后扫起的壳层中发生触发星形成。我们还发现，距离中心星团不同距离的丝状体由于反馈强度和暴露程度的差异，可以自然产生多代年龄序列。外围星群的速度与独立于CirCe区域形成的速度一致，但其速度足够相似，以至于在它们膨胀的后期可能难以区分。因此，我们提供了一种关于顺序星形成的新替代观点，该观点依赖于单个中心星团的反馈，而不是传统上引用的多个连续世代，同时也为较老星群的星形成历史提供了见解。
英文摘要：
Young associations provide a record that traces the star formation process, and the youngest populations connect progenitor gas dynamics to the resulting stellar populations. We therefore conduct the first comprehensive overview of the Circinus Complex, an under-studied and massive ($\sim$1500 M$_{\odot}$) region consisting of approximately 3100 recently formed stars alongside the Circinus Molecular Cloud (CMC). We find a clear age pattern in the contiguous central region (CirCe), where younger stars are found further from the massive central cluster, and where the velocities are consistent with uniform expansion. By comparing this structure to an analogous STARFORGE simulation, we find that the age structure and dynamics of the association are consistent with star formation in two stages: the global collapse of the parent cloud that builds the $500 M_{\odot}$ central cluster ASCC 79, followed by triggered star formation in a shell swept up after the first massive stars form. We also find that filaments with a range of distances from the central cluster can naturally produce multi-generational age sequences due to differences in feedback strength and exposure. Outlying populations show velocities consistent with formation independent from the CirCe region, but with similar enough velocities that they may be difficult to distinguish from one another later in their expansion. We therefore provide a new alternative view of sequential star formation that relies on feedback from a single central cluster rather than the multiple sequential generations that are traditionally invoked, while also providing insight into the star formation history of older populations.
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