发表机构
National Research Institute of Astronomy & Geophysics (NRIAG); Institute of Graduate Studies in Science, Istanbul University; Faculty of Science, Cairo University（国家天文与地球物理研究所; 伊斯坦布尔大学理学院研究生研究所; 开罗大学理学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究基于Gaia DR3数据，利用UPMASK算法等方法分析类毕星团NGC 2423和NGC 2482的多维度参数，得出其基本参数与运动学特性，探讨其与毕星团的关联。
AI 中文摘要
我们基于Gaia DR3数据开展了对类毕星团疏散星团NGC 2423和NGC 2482的均匀测光、天体测量及运动学研究。利用UPMASK算法在（赤经α、赤纬δ、三角视差、赤经自行μ_α cosδ、赤纬自行μ_δ）的多参数空间中确定星团成员，在径向速度可用时将其纳入分析。对天体测量分布进行高斯建模，得出NGC 2423和NGC 2482的平均三角视差分别为1.060±0.035 mas和0.735±0.061 mas，对应的天体测量距离分别为944±31 pc和1361±113 pc。通过PARSEC等时线拟合推导基本参数，得出年龄分别为1250±100 Myr和445±50 Myr，观测距离模数（m-M）_obs分别为9.90±0.10 mag和10.80±0.20 mag，红化值E(G_BP-G_RP)分别为0.07±0.01和0.10±0.02，等效为E(B-V)=0.054和0.078，对应的测光距离分别为892±50 pc和1311±146 pc。我们进一步利用速度椭球参数、会聚点法及作用角动量诊断工具研究两个星团的内部和整体运动学。推导的运动学特性显示，NGC 2482与毕星团流的速度空间特征高度匹配，而NGC 2423具有类毕星团群体的特征旋转速度和角动量，但在U分量上存在偏移。两个星团均占据文献中与类毕星团及棒相关共振相关的角动量范围，不过该关联是基于它们当前的运动学和作用空间位置，而非对共振捕获的直接动力学证明。
英文摘要
We present a homogeneous photometric, astrometric, and kinematic study of the Hyades-like open clusters NGC 2423 and NGC 2482 based on Gaia DR3 data. Cluster memberships are determined using the UPMASK algorithm in the multi-dimensional parameter space of (alpha, delta, parallax, mu_alpha cos(delta), mu_delta), with radial velocities incorporated when available. Gaussian modelling of the astrometric distributions yields mean trigonometric parallaxes of 1.060 +/- 0.035 mas and 0.735 +/- 0.061 mas, corresponding to astrometric distances of 944 +/- 31 pc and 1361 +/- 113 pc for NGC 2423 and NGC 2482, respectively. Fundamental parameters are derived through PARSEC isochrone fitting, resulting in ages of 1250 +/- 100 Myr and 445 +/- 50 Myr, observed distance moduli (m-M)_obs = 9.90 +/- 0.10 and 10.80 +/- 0.20 mag, and reddening values E(G_BP-G_RP) = 0.07 +/- 0.01 and 0.10 +/- 0.02 mag, equivalent to E(B-V) = 0.054 and 0.078. The corresponding photometric distances are 892 +/- 50 pc and 1311 +/- 146 pc. We further investigate the internal and global kinematics of both clusters using velocity-ellipsoid parameters, the convergent-point method, and action-angular-momentum diagnostics. The derived kinematic properties show that NGC 2482 closely matches the velocity-space characteristics of the Hyades stream, while NGC 2423 shares the characteristic rotational velocity and angular momentum of the Hyades-like population but is offset in its U component. Both clusters occupy the angular-momentum range associated in the literature with Hyades-like clusters and bar-related resonances, although this association is based on their present-day kinematics and action-space locations rather than a direct dynamical demonstration of resonance trapping.
Comments25 pages, including 15 figures and 7 tables, accepted for publication in the Journal of Astrophysics and Astronomy
