Accurate stellar parameters of stars in open clusters can help constrain models of stellar structure and evolution. Here we wish to determine the age and metallicity content of the open cluster NGC 2506. To this end we investigated three detached eclipsing binaries (DEBs; V2032, V4, and V5) for which we determined their masses and radii, as well as four red giant branch stars for which we determined their effective temperatures, surface gravities, and metallicities. Three of the stars in the DEBs have masses close to the cluster turn-off mass, allowing for extremely precise age determination. Comparing the values for the masses and radii of the binaries to BaSTI isochrones we estimated a cluster age of $2.01 \pm 0.10$ Gyr. This does depend on the models used in the comparison, where we have found that the inclusion of convective core-overshooting is necessary to properly model the cluster. From red giant branch stars we determined values for the effective temperatures, the surface gravities, and the metallicities. From these we find a cluster metallicity of $-0.36 \pm 0.10$ dex. Using this value and the values for the effective temperatures we determine the reddening to be E$(b - y) = 0.057 \pm 0.004$ mag. Furthermore, we derived the distance to the cluster from Gaia parallaxes and found $3.101 \pm 0.017$ kpc, and we have performed a radial velocity membership determination for stars in the field of the cluster. Finally, we report on the detection of oscillation signals in $\gamma$ Dor and $\delta$ Scuti members in data from the TESS mission, including the possible detection of solar-like oscillations in two of the red giants.

中文翻译：

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使用分离的食双星获得疏散星团 NGC 2506 的极其精确的年龄和金属丰度

疏散星团中恒星的准确恒星参数有助于约束恒星结构和演化的模型。在这里，我们希望确定疏散星团 NGC 2506 的年龄和金属含量。为此，我们调查了三个分离的食双星（DEB；V2032、V4 和 V5），我们确定了它们的质量和半径，以及四个红色我们确定了它们的有效温度、表面重力和金属丰度的巨型分支星。DEB 中的三颗恒星的质量接近星团关闭质量，可以非常精确地确定年龄。将双星的质量和半径值与 BaSTI 等时线进行比较，我们估计星团年龄为 $2.01 \pm 0.10 $ Gyr。这确实取决于比较中使用的模型，我们发现包含对流核心超调对于正确建模集群是必要的。从红巨星分支星，我们确定了有效温度、表面重力和金属丰度的值。从这些我们发现簇金属度为 $-0.36 \pm 0.10$ dex。使用这个值和有效温度的值，我们确定红化为 E$(b - y) = 0.057 \pm 0.004$ mag。此外，我们从盖亚视差推导出到星团的距离，发现 $3.101 \pm 0.017$ kpc，并且我们已经对星团领域中的恒星进行了径向速度隶属确定。最后，我们报告了 TESS 任务数据中 $\gamma$ Dor 和 $\delta$ Scuti 成员中振荡信号的检测，