We analysed the open clusters Czernik 2 and NGC 7654 using CCD UBV photometric and Gaia Early Data Release 3 (EDR3) photometric and astrometric data. Structural parameters of the two clusters were derived, including the physical sizes of Czernik 2 being \(r=5^{\prime}\) and NGC 7654 as \(8^{\prime}\). We calculated membership probabilities of stars based on their proper motion components as released in the Gaia EDR3. To identify member stars of the clusters, we used these membership probabilities taking into account location and the impact of binarity on main-sequence stars. We used membership probabilities higher than \(P=0.5\) to identify 28 member stars for Czernik 2 and 369 for NGC 7654. The mean proper motion components (\(\mu _{\alpha}\cos \delta \), \(\mu _{\delta}\)) of Czernik 2 were derived as (\(-4.03 \pm 0.04\), \(-0.99 \pm 0.05\)) mas yr⁻¹ and for NGC 7654 as (\(-1.89 \pm 0.03\), \(-1.20 \pm 0.03\)) mas yr⁻¹. We estimated colour-excesses and metallicities separately using \((U-B) \times (B-V)\) two-colour diagrams to derive homogeneously determined parameters. The derived \(E(B-V)\) colour excess is \(0.46 \pm 0.02\) mag for Czernik 2 and \(0.57 \pm 0.04\) mag for NGC 7654. [Fe/H] metallicities were obtained for the first time for both clusters, \(-0.08 \pm 0.02\) dex for Czernik 2 and \(-0.05 \pm 0.01\) dex for NGC 7654. Keeping the reddening and metallicity as constant quantities, we fitted PARSEC models using \(V\times (B-V)\) and \(V\times (U-B)\) colour-magnitude diagrams, resulting in estimated distance moduli and ages of the two clusters. We obtained the distance modulus for Czernik 2 as \(12.80 \pm 0.07\) mag and for NGC 7654 as \(13.20\pm 0.16\) mag, which coincide with ages of \(1.2\pm 0.2\) Gyr and \(120\pm 20\) Myr, respectively. The distances to the clusters were calculated using the Gaia EDR3 trigonometric parallaxes and compared with the literature. We found good agreement between the distances obtained in this study and the literature. Present day mass function slopes for both clusters are comparable with the value of Salpeter (1955), being \(X=-1.37\pm 0.24\) for Czernik 2 and \(X=-1.39\pm 0.19\) for NGC 7654.

我们使用 CCD UBV光度测量和Gaia Early Data Release 3 (EDR3) 光度测量和天体测量数据分析了疏散星团 Czernik 2 和 NGC 7654 。推导出了两个星团的结构参数，包括 Czernik 2 的物理尺寸为\(r=5^{\prime}\)和 NGC 7654的物理尺寸为\(8^{\prime}\)。我们根据Gaia EDR3 中发布的自行分量计算了恒星的成员概率。为了识别星团的成员星，我们使用了这些成员概率，同时考虑了位置和双星对主序星的影响。我们使用高于\(P=0.5\) 的成员概率确定 Czernik 2 的 28 颗成员星和 NGC 7654 的 369 颗成员星。 Czernik 的平均自行分量 ( \(\mu _{\alpha}\cos \delta \) , \(\mu _{\delta}\) ) 2 导出为 ( \(-4.03 \pm 0.04\) , \(-0.99 \pm 0.05\) ) mas yr ^-1和 NGC 7654 为 ( \(-1.89 \pm 0.03\) , \(-1.20 \ pm 0.03\) ) mas yr ^-1。我们使用\((UB) \times (BV)\)双色图分别估计颜色过量和金属量，以推导出均匀确定的参数。对于 Czernik 2，导出的\(E(BV)\)颜色过量是\(0.46 \pm 0.02\) mag\(0.57 \pm 0.04\) mag 为 NGC 7654。[Fe/H] 金属丰度首次获得两个星团，\(-0.08 \pm 0.02\) dex 为 Czernik 2 和\(-0.05 \pm 0.01 \) NGC 7654 的 dex。保持红化和金属丰度为常数，我们使用\(V\times (BV)\)和\(V\times (UB)\)颜色-幅度图拟合 PARSEC 模型，从而估计两个星团的距离模数和年龄。我们获得了 Czernik 2 的距离模数为\(12.80 \pm 0.07\) mag 和 NGC 7654的距离模数为\(13.20\pm 0.16\) mag，这与\(1.2\pm 0.2\) Gyr 和\( 120\下午 20\)分别是密尔。使用Gaia EDR3 三角视差计算到集群的距离并与文献进行比较。我们发现本研究中获得的距离与文献之间有很好的一致性。目前两个星团的质量函数斜率与 Salpeter (1955) 的值相当，Czernik 2为\(X=-1.37\pm 0.24 \)，NGC 7654 为\(X=-1.39\pm 0.19\)。