AI 中文总结
研究利用盖亚数据等，编制OC-WD对样本，结合多种手段分析其性质，识别出多个相关对，发现污染严重，尾中尤甚，还识别出候选双星起源WD和IFMR候选者，为星团探测及相关模拟提供限制，解决WD短缺需多方面改进。
AI 中文摘要
最近的盖亚研究识别出了众多疏散星团（OCs）和潮汐尾目录，使得能够系统地搜寻与星团及其延展结构相关的白矮星（WDs）。我们编制了一个基于文献的OC-WD对样本，以验证WD在星团核心和尾中的成员身份，研究初始-最终质量关系（IFMR），识别通过非规范演化形成的WD，并使用N体模拟网格解释观测到的WD群体。我们将盖亚DR3星团和尾目录与紫外-红外测光相结合来分析OC-WD对。利用颜色-星等图和光谱能量分布估算WD的质量、冷却年龄、半径、温度和光度。这些观测结果在N体模拟的背景下进行解释。我们在80个星团中识别出235个OC-WD对（99个在尾中）。超过28%的对可能是虚假的，尾中的污染（>48%）比星团核心（>13%）高得多，表明当前基于盖亚的目录中存在显著的场星污染。昴宿星团的尾也显示出被老年WD严重污染。模拟预测核心WD的比例随星团年龄增加，达到>10%，而观测到的比例系统地更低，与WD短缺问题一致。尽管污染率很高，但大多数尾中的WD（约83%）与在潮汐半径内诞生一致。我们还识别出63个候选双星起源的WD和47个新的IFMR候选者。WD对白矮星群体提供了一个强大的污染探测手段，并对星团探测方法和N体模拟施加了重要限制。解决WD短缺问题并改善成员身份验证将需要改进观测、成员身份方法、WD物理学和光谱后续观测，以便对动态星团演化和WD IFMR施加更强的限制。
英文摘要
Recent Gaia studies have identified numerous open clusters (OCs) & tidal tail catalogues, enabling systematic searches for white dwarfs (WDs) associated with clusters & their extended structures. We compile a literature-based sample of OC-WD pairs to validate WD membership in cluster cores & tails, investigate the initial-final mass relation (IFMR), identify WDs formed through non-canonical evolution, and interpret the observed WD populations using a grid of N-body simulations. We combine Gaia DR3 cluster & tail catalogues with UV-IR photometry to analyse the OC-WD pairs. WD masses, cooling ages, radii, temperatures & luminosities are estimated using colour-magnitude diagrams & spectral energy distributions. These observations are interpreted in the context of N-body simulations. We identify 235 OC-WD pairs (99 in tails) in 80 clusters. More than 28% of the pairs are likely spurious, with contamination substantially higher in the tails (>48%) than in the cluster cores (>13%), indicating significant field-star contamination in current Gaia-based catalogues. The Pleiade tails also show severe contamination by old WDs. Simulations predict that the fraction of core WDs increases with cluster age, reaching >10%, whereas the observed fractions remain systematically lower, consistent with the WD deficit problem. Despite the high contamination rate, most tail WDs (~83%) are consistent with having been born inside the tidal radius. We also identify 63 candidate binary-origin WDs & 47 new IFMR candidates. WDs provide a powerful probe of contamination in cluster and tail catalogues and place important constraints on cluster detection methods & N-body simulations. Resolving the WD deficit and improving membership validation will require improved observations, membership methods, WD physics, and spectroscopic follow-up, enabling stronger constraints on dynamical cluster evolution & the WD IFMR.
Comments12 pages main text, 48 pages appendix. Appendix C is only available on arXiv. Tables B1 and B2 will be available on CDS. Accepted in A&A
DOI：10.1051/0004-6361/202661206
