The membership determination for open clusters in noisy environments of the Milky Way is still an open problem. In this paper, our main aim is to provide the membership probability of stars using proper motions and parallax values of stars using Gaia Third Data Release astrometry. Apart from the Gaia astrometry, we have also used other photometric data sets like the UKIRT Infrared Deep Sky Survey, WISE, the American Association of Variable Star Observers (AAVSO) Photometric All-Sky Survey, and Pan-STARRS1 in order to understand cluster properties from optical to mid-infrared regions. We selected 438 likely members with membership probabilities higher than $50\%$ and G ≤ 20 mag. We obtained the mean value of proper motion as μx = 1.27 ± 0.001 and μy = −0.73 ± 0.002 mas yr−1. The cluster’s radius is determined as ${7{^{\prime }_{.}}5}$ (5.67 pc) using radial density profile. Our analysis suggests that NGC 1348 is located at a distance of 2.6 ± 0.05 kpc. The mass function slope is found to be 1.30 ± 0.18 in the mass range 1.0–4.1 M⊙, which is in fair agreement with Salpeter’s value within the 1σ uncertainty. The present study validates that NGC 1348 is a dynamically relaxed cluster. We computed the apex coordinates (A, D) for NGC 1348 as (A°, D°) = (−23.°815 ± 0.°135, −22.°228 ± 0.°105). In addition, calculations of the velocity ellipsoid parameters (VEPs), matrix elements μij, direction cosines (lj, mj, nj), and the galactic longitude of the vertex have been conducted in this analysis.

中文翻译：

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使用多色光度法和 GAIA EDR3 天体测量法对研究较少的北部疏散星团 NGC 1348 进行详细分析

银河系嘈杂环境中疏散星团的成员资格确定仍然是一个悬而未决的问题。在本文中，我们的主要目的是使用 Gaia Third Data Release 天体测量法提供恒星的自行和视差值来提供恒星的隶属概率。除了 Gaia 天体测量，我们还使用了其他光度数据集，如 UKIRT 红外深空巡天、WISE、美国变星观测者协会 (AAVSO) 光度全天巡天和 Pan-STARRS1，以了解星团属性从光学到中红外区域。我们选择了 438 个成员概率高于 $50\%$ 且 G ≤ 20 mag 的可能成员。我们获得了自行运动的平均值为 μx = 1.27 ± 0.001 和 μy = -0.73 ± 0.002 mas yr-1。集群的半径被确定为 ${7{^{\prime }_{.}}5}$ (5. 67 pc) 使用径向密度分布。我们的分析表明 NGC 1348 位于 2.6 ± 0.05 kpc 的距离处。在 1.0-4.1 M⊙ 的质量范围内，质量函数的斜率为 1.30 ± 0.18，这与 Salpeter 的值在 1σ 不确定性内相当吻合。本研究证实 NGC 1348 是一个动态松弛的星团。我们将 NGC 1348 的顶点坐标 (A, D) 计算为 (A°, D°) = (-23.°815 ± 0.°135, -22.°228 ± 0.°105)。此外，本次分析还计算了速度椭球参数（VEP）、矩阵元素μij、方向余弦（lj、mj、nj）和顶点的银河经度。这在 1σ 不确定性内与 Salpeter 的值相当一致。本研究证实 NGC 1348 是一个动态松弛的星团。我们将 NGC 1348 的顶点坐标 (A, D) 计算为 (A°, D°) = (-23.°815 ± 0.°135, -22.°228 ± 0.°105)。此外，本次分析还计算了速度椭球参数（VEP）、矩阵元素μij、方向余弦（lj、mj、nj）和顶点的银河经度。这在 1σ 不确定性内与 Salpeter 的值相当一致。本研究证实 NGC 1348 是一个动态松弛的星团。我们将 NGC 1348 的顶点坐标 (A, D) 计算为 (A°, D°) = (-23.°815 ± 0.°135, -22.°228 ± 0.°105)。此外，本次分析还计算了速度椭球参数（VEP）、矩阵元素μij、方向余弦（lj、mj、nj）和顶点的银河经度。