寻找年轻疏散星团的扩散兄弟。使用Gaia DR3的动力学回溯模拟
Finding the dispersing siblings of young open clusters. Dynamical traceback simulations using Gaia DR3
AI总结：
提出一种基于Gaia DR3径向速度子样本的动力学回溯新方法，通过计算概率估计识别近邻年轻星团的逃逸成员，成功应用于十个星团并发现逃逸恒星形成的细长结构，为研究星团瓦解与恒星动力学提供有效手段。
摘要：
背景。恒星倾向于成团形成，但许多恒星很早就逃离了它们的诞生星团。识别星团的逃逸成员可以为我们提供关于星团瓦解的信息，也可以让我们了解银河系中的恒星动力学。需要能够从许多星团中寻找逃逸恒星的方法，以充分利用Gaia时代的大量数据。目标。我们提出了一种识别近邻星团逃逸成员的新方法，并将其应用于十个年轻星团。方法。我们假设逃逸恒星在过去靠近星团，并基于Gaia DR3径向速度子样本进行了回溯计算。对于每颗单独的恒星，我们的方法会生成其作为星团逃逸成员的概率估计，而对于每个星团，它也会估计所识别逃逸者的场星污染率。结果。我们的方法能够找到在过去几千万年内逃离其星团的逃逸者。在许多情况下，逃逸者形成了一个覆盖大体积的细长结构。结论。这里展示的结果表明，使用Gaia DR3数据进行回溯计算可以识别最近逃离其星团的恒星。当应用于包含更多径向速度测量的未来Gaia数据发布时，我们的方法将更加有用。
英文摘要：
Context. Stars tend to form in clusters, but many escape their birth clusters very early. Identifying the escaped members of clusters can inform us about the dissolution of star clusters, but also about the stellar dynamics in the galaxy. Methods capable of finding escaped stars from many clusters are required to fully exploit the large amounts of data in the Gaia era. Aims. We present a new method of identifying escaped members of nearby clusters and apply it to ten young clusters. Methods. We assumed the escaped stars were close to the cluster in the past and performed traceback computations based on the Gaia DR3 radial velocity subsample. For each individual star, our method produces a probability estimate that it is an escaped member of a cluster, and for each cluster it also estimates the field star contamination rate of the identified fugitives. Results. Our method is capable of finding fugitives that have escaped from their cluster in the last few ten million years. In many cases the fugitives form an elongated structure that covers a large volume. Conclusions. The results presented here show that traceback computations using Gaia DR3 data can identify stars that have recently escaped their cluster. Our method will be even more useful when applied to future Gaia data releases that contain more radial velocity measurements.
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