Title: Open cluster age calibration from colour-magnitude morphological indices using Gaia DR3 data Show Chinese title

Title: 使用盖亚DR3数据从颜色- magnitude形态指数校准疏散星团年龄

Abstract: Star clusters are crucial for understanding how stars evolve. Their colour-magnitude diagrams show the effects of stellar evolution of approximately coeval objects with the same chemical composition. Furthermore, the determination of their astrophysical parameters (age, distance, colour excess and metallicity) together with their spatial distribution provides information about the structure and the evolution of the Galaxy itself. Using data from the \textit{Gaia} DR3 and 2MASS catalogues, we develop methodologies for characterizing open clusters. Precise membership lists, mean astrometric parameters and radii are obtained. Using photometric data from both data sources, we carried out new age calibrations that rely on morphological indices based on colour ($\Delta BR$) and magnitude ($\Delta G$) differences between the red clump and the turnoff for a sample of 34 open clusters with ages covering the interval $8.3 < \log[t({\rm yr})] < 9.9$. A set of age calibration functions based on \textit{Gaia} morphological age indices are determined for the first time. We demonstrate their accuracy, obtaining a mean residual of 0.06 dex in $\log[t(yr)]$. Our results also show that stellar evolution models tend to predict the difference $\Delta G$. However, they typically overestimate the difference $\Delta BR$ for objects younger than $\log[t({\rm yr})] = 8.8$. Show Chinese abstract

Abstract: 星团对于理解恒星的演化至关重要。它们的颜色-亮度图展示了具有相同化学成分的大致同时形成的天体的恒星演化效应。此外，确定它们的天文学参数（年龄、距离、消光和金属丰度）以及空间分布提供了关于星系自身结构和演化的信息。 利用来自 \textit{盖亚} DR3 和 2MASS 星表的数据，我们开发了表征疏散星团的方法。得到了精确的成员名单、平均天文学参数和半径。 使用两个数据源的测光数据，我们进行了新的年龄标定，这些标定依赖于基于颜色（$\Delta BR$）和亮度（$\Delta G$）差异的形态学指数，样本包括34个疏散星团，其年龄覆盖范围为 $8.3 < \log[t({\rm yr})] < 9.9$。首次确定了一组基于 \textit{盖亚} 形态学年龄指数的年龄标定函数。 我们证明了它们的准确性，在 $\log[t(yr)]$中获得了平均残差为 0.06 dex。我们的结果还表明，恒星演化模型倾向于预测 $\Delta G$的差异。 然而，它们通常会高估年龄小于 $\log[t({\rm yr})] = 8.8$ 的物体之间的差异 $\Delta BR$。