发表机构
University of Sheffield; Universita’ degli Studi di Trieste; University of Warwick; Hamburger Sternwarte, University of Hamburg; Universidad Técnica Federico Santa María; Universitat Politècnica de Catalunya; Institut d’Estudis Espacials de Catalunya (IEEC); National Astronomical Observatories, Chinese Academy of Sciences（谢菲尔德大学; 的里雅斯特大学; 华威大学; 汉堡天文台，汉堡大学; 费德里科·圣塔玛利亚技术大学; 加泰罗尼亚理工大学; 加泰罗尼亚空间研究所; 中国科学院国家天文台）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
利用 Gaia DR3 和 GALEX 紫外超，构建 350 pc 内 2597 个 WD+FGK 候选双星样本，估计白矮星参数与系统年龄，污染率 10-35%，为研究双星演化提供宝贵资源。
AI 中文摘要
具有 F、G 或 K 型双星伴星的白矮星（WD）是一系列奇异现象的最近共同祖先。找到此类系统的干净样本很困难，因为这类双星中的白矮星在光学波段通常被其非简并伴星的光芒所掩盖。拥有此类双星的样本是有用的——它们可以被研究以探究双星演化，因为它们可能经历过先前的质量转移阶段。利用 Gaia 数据发布 3 和 GALEX，我们编制了 350 pc 内 2597 个候选 WD + FGK 系统的样本。这些系统是通过其相对于 MESA 等时线与恒星轨迹（MIST）模型预测的紫外超来识别的，这些预测与其非简并伴星的 Gaia 参数一致。我们通过将多余的紫外通量拟合到模型，或在仅有单一紫外波段可用时通过插值，来估计白矮星的质量、表面重力和有效温度。我们还尽可能通过比较高阶恒星系统中的宽距白矮星伴星，或检查系统是否为星团成员，来估计系统的年龄。与 Simbad 比较后，我们估计样本中的污染水平在 10% 至 35% 之间。这是研究 WD + FGK 双星，特别是那些包含较热白矮星（Teff,WD >~ 25 kK）和具有主序后伴星的系统的宝贵样本。
英文摘要
White dwarfs (WDs) with F, G or K type binary companions are the last common ancestor to a zoo of exotic phenomena. Finding a clean sample of such systems is difficult, as WDs in such binaries are usually outshone at optical wavelengths by their non-degenerate companion. It is useful to have a sample of such binaries - they can be studied to investigate binary evolution, as they may have undergone a previous phase of mass transfer. Using Gaia data release 3 and GALEX, we compile a sample of 2597 candidate WD + FGK systems within 350 pc. These were identified via their ultraviolet excesses relative to MESA Isochrones and Stellar Tracks (MIST) model predictions consistent with the Gaia parameters of their non-degenerate companions. We estimate the mass, surface gravity and effective temperature of the WDs by fitting the excess ultraviolet flux to models, or through interpolation where only one ultraviolet band was available. We also estimate the age of the system where possible, by comparing against any wide WD companions in higher-order stellar systems, or by checking if the system is a member of a cluster. On comparing against Simbad, we estimate the level of contamination within our sample to be between 10-35 per cent. This is a valuable sample for investigating WD + FGK binaries, particularly those containing hotter WDs (Teff,WD >~ 25 kK), and systems with post-main sequence companions.
