发表机构
Universitäts-Sternwarte München, Ludwig-Maximilians-Universität; Excellence Cluster ORIGINS（慕尼黑大学天文台; ORIGINS卓越集群）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究通过Gaia DR3回溯分析，揭示了船底座OB1星协中八个大质量星团的形成历史，提出超新星爆炸驱动的气泡触发了年轻星团的顺序形成，但星协整体膨胀源于初始运动学。
AI 中文摘要
船底座OB1星协在其中心附近拥有著名的船底座星云，是我们银河系中质量最大、研究最充分的OB星协。它包含几个年龄不同的巨大恒星团，展现出复杂的时空结构。我们探索了Car OB1中八个最大恒星团的形成历史和运动学演化。我们确定了这些星团的年龄、恒星种群、初始大质量恒星含量，以及自每个星团形成以来发生的超新星爆炸次数。利用Gaia DR3天体测量数据，我们确定了该星协的三维结构，并对过去13百万年内的星团位置进行了回溯分析。回溯分析将最古老（13百万年）的星团NGC 3293的诞生位置置于船底座旋臂中。大约四百万年后，一系列11次超新星爆炸在NGC 3293中开始。我们构建了一个可能的情景，其中由这些超新星爆炸驱动的膨胀气泡与原始云复合体的南部相互作用，导致了中央船底座星云中较年轻星团的顺序形成。我们的情景表明，在过去10百万年内，该星协中16±4次超新星爆炸的序列在创造Car OB1中的大质量星团方面发挥了重要作用。然而，超新星反馈并不主导该星协的大尺度膨胀；整体膨胀似乎更反映了原始未束缚云复合体的初始运动学。
英文摘要
The Carina OB1 association, harboring the famous Carina Nebula near its center, is the most massive, well-studied OB association in our Galaxy. Containing several massive star clusters with different ages, it shows a complex spatio-temporal structure. We explore the formation history and kinematic evolution of the eight most massive clusters in Car OB1. We determine the cluster ages, stellar populations, the initial massive star content, and the number of supernova explosions since the time of each cluster's formation. Using Gaia DR3 astrometry, we determine the 3D configuration of the association and perform a traceback analysis of the cluster positions over the last 13 Myr. The traceback analysis places the birth location of the oldest (13 Myr) cluster, NGC 3293, in the Carina spiral arm. Approximately four Myr later, a series of 11 supernova explosions started in NGC 3293. We construct a possible scenario in which the expanding bubble driven by these supernova explosions interacted with the southern part of the original cloud complex and led to the sequential formation of the younger clusters in the central Carina Nebula. Our scenario suggests that the sequence of 16+/-4 supernova explosions in the association during the last 10 Myr played an important role in creating the massive clusters in Car OB1. However, the supernova feedback does not dominate the large-scale expansion of the association; the general expansion rather seems to reflect the initial kinematics of the original unbound cloud complex.
Comments16 pages, 10 figures, accepted for publication in Astronomy & Astrophysics
