行星状星云中心星作为银河系中行星状星云-星团关联的示踪体
Planetary Nebula Central Stars as Tracers of Planetary Nebula-Star Cluster Associations in the Galaxy
- Observatório do Valongo, Universidade Federal do Rio de Janeiro（瓦隆戈天文台，里约热内卢联邦大学）
- Instituto de Astrofísica, Depto. de. Física y Astronomía, Facultad de Ciencias Exactas, Universidad Andrés Bello（安德烈斯·贝略大学精确科学学院物理与天文学系天体物理研究所）
- Vatican Observatory（梵蒂冈天文台）
- Instituto de Física, Universidade Federal do Rio de Janeiro（里约热内卢联邦大学物理研究所）
机构由 AI 辅助整理，请以论文原文为准。
AI总结：
本研究利用中心星与星团星表及Gaia DR3数据，系统搜寻银河系中行星状星云-星团关联，识别出38个候选配对，其中8个具有一致性消光，为恒星演化及IFMR提供新约束。
AI中文摘要：
与星团在物理上相关联的行星状星云（PNe）虽然罕见，但对恒星演化研究至关重要，因为它们使得能够独立确定恒星的初始和最终性质，从而有助于约束初始-最终质量关系（IFMR），该关系追踪恒星质量损失。尽管识别此类配对至关重要，但大多数已报道的案例是偶然发现的，而非通过系统性搜索。在此，我们尝试利用文献中的行星状星云中心星（CSs）和星团星表，在我们的银河系中发现新的此类关联。通过探索天空中的相关角位置和Gaia DR3运动学数据，我们识别出38个候选的CS-星团配对。其中8个配对的分量具有一致的星际消光，且其中心星性质与恒星演化模型相容。这些候选配对中有两个已在文献中被报道为真实关联。我们利用文献中的行星状星云观测数据，对剩余的六个配对进行了单独评估，评估了每个配对成为真实关联的可能性。我们最佳候选者的初始和最终质量大多与最新的IFMR预测及已确认的星团-PNe数据点一致。另有46个CS-星团配对的分量具有相容的角位置，但缺乏运动学中心星数据，因此被单独列出。需要对大多数候选者的物理参数进行精确估计并确认这些关联，这需要更多数据，将在未来的研究中加以解决。
英文摘要：
Planetary nebulae (PNe) that are physically associated with star clusters are rare but crucial for stellar evolution studies because they allow their initial and final stellar properties to be determined independently, contributing to constraints on the initial-to-final-mass relation (IFMR), which traces stellar mass loss. Although the identification of such pairs is essential, most reported cases have been identified incidentally rather than through systematic searches. Here, we attempt to uncover new such associations in our Galaxy employing literature PN central stars (CSs) and star cluster catalogues. Exploring relevant angular positions on the sky and kinematic Gaia DR3 data, we identify 38 candidate CS-cluster pairs. The components of eight of these pairs present consistent interstellar extinctions, and their CS properties are compatible with stellar evolution models. Two of these candidate pairs are already reported in the literature as true associations. We evaluate separately the remaining six pairs using literature PN observational data, assessing the likelihood of each pair being a true association. The initial and final masses of our best candidates are mostly consistent with the latest IFMR predictions and confirmed cluster-PNe points. An additional 46 CS-cluster pairs have components with compatible angular positions but lack kinematic CS data and are thus presented separately. More data are needed for a precise estimation of the physical parameters of most of our candidates and to confirm these associations, which will be addressed in future studies.
