两个恒星时钟，一段历史：基于盖亚颜色-星等图重建的太阳邻域恒星形成历史与白矮星的对比检验
Two stellar clocks, one history: a Gaia colour-magnitude-diagram reconstruction of the solar-neighbourhood star-formation history tested against white dwarfs
AI总结：
研究通过盖亚DR3 CMD重建太阳邻域恒星形成历史，用SFERA代码拟合非简并恒星，采用多种白矮星冷却模型生成合成白矮星种群与观测比较。两种基于CMD的解在SFH主要特征上一致，不同模型的WDLF与观测有差异，Montreal最佳，且微弱尾部不支持老白矮星大量贡献。
AI中文摘要：
太阳邻域恒星形成历史（SFH）可通过非简并恒星的颜色-星等图（CMD）来约束，并能用白矮星光度函数（WDLF）独立检验。这两种示踪剂采样互补的演化阶段，可对恢复的SFH和采用的白矮星冷却模型进行一致性检查。我们从盖亚DR3 CMD重建本地SFH，并测试所得历史是否能再现观测到的40 pc WDLF。使用SFERA合成种群代码对半径200 pc、垂直范围±40 pc的圆柱体内的非简并恒星进行拟合，采用PISA和PARSEC恒星库。然后用每个基于CMD的解生成合成白矮星种群，与40 pc WDLF进行比较，采用相同的初始-最终质量关系和四组白矮星冷却模型：BaSTI、MIST、La Plata和Montreal。两种基于CMD的解在本地SFH的主要特征上一致，但预测的WDLFs在WDLF最大值附近和沿微弱尾部与观测分布有显著差异。Montreal提供了最佳的整体折衷。在这个冷却尺度上，逐步去除最古老的合成白矮星表明，微弱尾部不支持总年龄超过约11 Gyr的白矮星有大量贡献。
英文摘要：
The solar-neighbourhood star-formation history (SFH) can be constrained from the colour-magnitude diagram (CMD) of non-degenerate stars and tested independently with the white-dwarf luminosity function (WDLF). These two tracers sample complementary evolutionary phases and provide a consistency check on both the recovered SFH and the adopted WD cooling models. We reconstruct the local SFH from the Gaia DR3 CMD and test whether the resulting history reproduces the observed 40 pc WDLF. We fit non-degenerate stars in a cylinder of radius 200 pc and vertical extent $\pm40$ pc using the SFERA synthetic-population code. The fit is performed with the PISA and PARSEC stellar libraries. Each CMD-derived solution is then used to generate a synthetic WD population for comparison with the 40 pc WDLF, adopting the same initial-final mass relation and four WD cooling model sets: BaSTI, MIST, La Plata, and Montreal. The two CMD-based solutions agree on the main features of the local SFH: low activity at the oldest ages, an early episode around 9-11 Gyr ago, reduced activity between about 4 and 9 Gyr, and enhanced star formation over the last few Gyr. The predicted WDLFs reproduce the bright and intermediate part of the observed distribution for all cooling grids, but differ substantially around the WDLF maximum and along the faint tail. MIST and BaSTI shift too much weight to magnitudes fainter than the observed maximum, whereas La Plata gives the closest match to the faint tail but leaves larger residuals around the maximum. Montreal provides the best overall compromise. On this cooling scale, progressively removing the oldest synthetic WDs shows that the faint tail disfavours a substantial contribution from WDs with total ages older than about 11 Gyr.
