In the context of understanding star formation in the galactic plane, we present the results from the analysis of four young open clusters using archival data from Gaia Data Release 3, the Two-Micron All Sky Survey (2MASS) and Panoramic Survey Telescope and Rapid Response System (Pan-STARRS). The open clusters—[BDB2003]G085.25−00.02, [BDS2003]48, [BDS2003]65 and [FSR2007]0584 are situated close to the galactic plane between the galactic latitudes, \(b = -0.23^{\circ }\) and \(0.837^{\circ }\). The likely cluster members and mean proper motions were determined using a Gaussian likelihood model fit to the proper motion data provided by Gaia DR3. The cluster radii are estimated to be in the range of 2–3.3 arcmin. From the H–K vs. J–H color–color diagram, we identified probable young stellar objects. Using the J–H vs. J–K color–color diagram and PARSEC isochrones, we determined the line-of-sight interstellar reddening E(J–H) as \(0.56\pm 0.03\) mag, \(0.4\pm 0.09\) mag, \(0.4\pm 0.1\) mag and \(0.42\pm 0.08\) mag for [BDB2003]G085.25−00.02, [BDS2003]48, [BDS2003]65 and [FSR2007]0584, respectively. From the fit of isochrones to color–magnitude diagrams, we determined the distances and ages of the clusters. [BDB2003] G085.25−00.02 is located at a distance of \(2.88\pm 0.15\) kpc, [BDS2003]48 is located at a distance of \(4.78\pm 0.18\) kpc, [BDS2003]65 is located at a distance of \(2.18\pm 0.07\) kpc and [FSR2007]0584 is located at a distance \(3.31\pm 0.14\) kpc. We obtained the \(\log (\textrm{age})\) of [BDB2003] G085.25−00.02 as \(6.85\pm 0.2\), the \(\log (\textrm{age})\) [BDS2003]48 as \(6.2\pm 0.5\), the \(\log (\textrm{age})\) of [BDS2003]65 as \(\log (\textrm{age})\) of \(6.7\pm 0.16\) and the \(\log (\textrm{age})\) of [FSR2007]0584 as \(6.9\pm 0.55\). From the stellar masses predicted by the fitted isochrones for the cluster members, we obtained the present-day mass-functions of the clusters. The mass-function slopes are \(-2.47\pm 0.14\) for [BDB2003]G085.25−00.02, \(-2.1\pm 0.25\) for [BDS2003]48, \(-2.61\pm 0.22\) for [BDS2003]65 and \(-2.4\pm 0.23\) for [FSR2007]0584. Within the limits of error of a least-squares fit, the mass-function slopes are in fair agreement with the Salpeter slope of \(-2.35\).

在了解银道面恒星形成的背景下，我们展示了使用盖亚数据版本 3、两微米全天巡天 (2MASS) 以及全景巡天望远镜和快速响应的档案数据对四个年轻疏散星团进行分析的结果系统（Pan-STARRS）。疏散星团——[BDB2003]G085.25−00.02、[BDS2003]48、[BDS2003]65 和 [FSR2007]0584 位于银道纬度之间靠近银道面的位置，\( b = -0.23^{\circ } \)和\(0.837^{\circ }\)。使用适合 Gaia DR3 提供的自行数据的高斯似然模型来确定可能的簇成员和平均自行。簇半径估计在 2-3.3 弧分范围内。从 H-K 与 J-H 颜色图，我们识别出了可能的年轻恒星物体。使用 J–H 与 J–K 颜色图和 PARSEC 等时线，我们确定了视线星际红化 E(J–H) 为 \(0.56 \pm 0.03\) mag，\(0.4\pm 0.09\)星等、\(0.4\pm 0.1\)星等和\(0.42\pm 0.08\)分别为[BDB2003]G085.25−00.02、[BDS2003]48、[BDS2003]65和[FSR2007]0584。从等时线到颜色星等图的拟合，我们确定了星团的距离和年龄。[BDB2003] G085.25−00.02 位于距离\(2.88\pm 0.15\) kpc，[BDS2003]48 位于距离\(4.78\pm 0.18\) kpc，[BDS2003]65 位于距离在距离\(2.18\pm 0.07\) kpc 处，[FSR2007]0584 位于距离\(3.31\pm 0.14\) kpc 处。我们得到[BDB2003] G085.25−00.02 的\(\log (\textrm{age})\)为\(6.85\pm 0.2\)，\(\log (\textrm{age})\) [ BDS2003]48 为\(6.2\pm 0.5\)，[BDS2003]65 的\(\log (\textrm{age})\)为\(6.7\pm 0.16\)的\(\log (\textrm{age})\)和\(\log (\textrm [FSR2007]0584 的{age})\)为\(6.9\pm 0.55\)。根据星团成员的拟合等时线预测的恒星质量，我们获得了星团当前的质量函数。[BDB2003]G085.25−00.02 的质量函数斜率是\(-2.47\pm 0.14\) ，[BDS2003]48的质量函数斜率是 \(-2.1\pm 0.25\)， [BDS2003]48 的质量函数斜率是\(-2.61\pm 0.22\) [BDS2003]65 和[FSR2007]0584 的\(-2.4\pm 0.23\) 。在最小二乘拟合的误差范围内，质量函数斜率与 Salpeter 斜率相当一致\(-2.35\)。