arXiv 2307.013372023-07-03astro-ph.SR

利用Gaia DR3揭示新的白矮星-疏散星团关联

Uncovering new white dwarf - open cluster associations using Gaia DR3

M. Prišegen, N. Faltová

备注：: 17 pages, 3 figures, accepted in A&A
发表信息：: A&A 678, A20 (2023)
DOI：: 10.1051/0004-6361/202245706

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AI总结：

本研究利用Gaia DR3数据和HDBSCAN算法，在太阳附近疏散星团中发现36个新的白矮星候选成员，为约束初始-终态质量关系提供了新观测样本。

摘要：

研究背景：疏散星团（OCs）提供了具有已知距离、消光和总年龄的白矮星（WDs）同质样本。Gaia前所未有的天体测量精度使我们能够识别许多新的OC-WD对。在母疏散星团的背景下研究白矮星，使得确定白矮星前身星的性质以及研究初始-终态质量关系（IFMR）成为可能。研究目的：我们旨在寻找太阳附近疏散星团潜在的新白矮星成员。通过分析疏散星团成员的视差，我们可以高精度确定疏散星团的距离，进而计算白矮星的质量和冷却年龄，并约束初始-终态质量关系。研究方法：我们使用基于密度的机器学习聚类算法HDBSCAN（带噪声的基于密度的空间聚类应用层次），在附近的疏散星团中寻找新的潜在白矮星成员。聚类分析在五个天体测量维度——天球位置、自行和视差——中开展，同时也在不考虑位置信息的三个维度中进行了聚类分析。识别出的候选疏散星团白矮星进一步通过测光标准以及其假定宿主疏散星团的性质进行筛选。我们利用所有可用的Gaia、Pan-STARRS、SDSS和GALEX测光数据，通过测光方法计算了白矮星的质量和冷却年龄。白矮星前身星的质量则通过其宿主疏散星团的年龄和金属丰度确定。研究结果：总共发现了63个疏散星团白矮星候选体，其中27个已在文献中报道。我们对36个具有显著疏散星团成员概率的新发现白矮星进行了表征。其中6个位于初始-终态质量关系中约束相对较弱的区域，该关系在这些区域似乎表现出非线性行为。我们未能识别出任何源自大质量前身星的白矮星，这些前身星的质量甚至远未达到被广泛认可的白矮星前身星质量上限。（有删节）

英文摘要：

Context: Open clusters (OCs) provide homogeneous samples of white dwarfs (WDs) with known distances, extinctions, and total ages. The unprecedented astrometric precision of \textit{\textit{Gaia}} allows us to identify many novel OC--WD pairs. Studying WDs in the context of their parent OCs makes it possible to determine the properties of WD progenitors and study the initial-final mass relation (IFMR). Aims: We seek to find potential new WD members of OCs in the solar vicinity. The analysis of OC members' parallaxes allows us to determine the OC distances to a high precision, which in turn enables us to calculate WD masses and cooling ages and to constrain the IFMR. Methods: We searched for new potential WD members of nearby OCs using the density-based machine learning clustering algorithm \texttt{HDBSCAN}. The clustering analysis was applied in five astrometric dimensions -- positions in the sky, proper motions and parallaxes -- and in three dimensions where the positional information was not considered in the clustering analysis. The identified candidate OC WDs were further filtered using the photometric criteria and properties of their putative host OCs. The masses and cooling ages of the WDs were calculated via a photometric method using all available \textit{\textit{Gaia}}, Pan-STARRS, SDSS, and GALEX photometry. The WD progenitor masses were determined using the ages and metallicities of their host OCs. Results: Altogether, 63 OC WD candidates were recovered, 27 of which are already known in the literature. We provide characterization for 36 novel WDs that have significant OC membership probabilities. Six of them fall into relatively unconstrained sections of the IFMR where the relation seems to exhibit nonlinear behavior. We were not able to identify any WDs originating from massive progenitors that would even remotely approach the widely adopted WD progenitor mass limit. (abridged)

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英文摘要：

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