标题： 疏散星团 Tr 1 和 Be 11 的深紫外 BRI CCD 光度学研究 显示英文标题

标题： A deep UVBRI CCD photometric study of open clusters Tr 1 and Be 11

摘要： 我们展示了年轻疏散星团 Tr 1 和 Be 11 的深度 $UBVRI$ CCD 光度学数据。Be 11 的 CCD 数据为首次获取。样本由 $\sim$ 1500 颗星组成，最暗达到 $V$ $\sim$ 21 星等。对恒星面密度径向分布的分析表明，Tr 1 和 Be 11 的半径值分别为 2.3 和 1.5 秒差距。成像星团区域内的星际消光似乎不均匀，对于 Tr 1 和 Be 11 分别具有平均值 $E(B-V)$ = 0.60$\pm$0.05 和 0.95$\pm$0.05 魔氏。 在两个星团中都存在$E(B-V)$的随机位置变化。 在 Be 11 星团中，随机位置变化的原因可能是 HII 区域 (S 213) 的明显关联。 结合 Be 11 星团中的光学数据，2MASS$JHK$数据得出$E(J-K)$= 0.40$\pm$0.20 mag 和$E(V-K)$= 2.20$\pm$0.20 mag。 色余量图表明，在 Be 11 星团的方向上遵循正常的星际消光定律。 Tr 1 和 Be 11 的距离分别估计为 2.6$\pm$± 0.10 和 2.2$\pm$± 0.10 千秒差距 (Kpc)，而根据明亮团簇成员拟合的理论恒星演化等年龄线表明，Tr 1 和 Be 11 的年龄分别为 40$\pm$± 10 和 110$\pm$± 10 百万年 (Myr)。 已针对场星污染和数据不完整性对两个团簇的质量函数进行了修正。 Tr 1 和 Be 11 的斜率$1.50\pm0.40$和$1.22\pm0.24$分别与萨尔皮特值一致。 两个团簇中观测到的质量分离可能是动力学演化或恒星形成过程的印记，或者两者共同作用的结果。 显示英文摘要

摘要： We present deep $UBVRI$ CCD photometry for the young open star clusters Tr 1 and Be 11. The CCD data for Be 11 is obtained for the first time. The sample consists of $\sim$ 1500 stars reaching down to $V$ $\sim$ 21 mag. Analysis of the radial distribution of stellar surface density indicates that radius values for Tr 1 and Be 11 are 2.3 and 1.5 pc respectively. The interstellar extinction across the face of the imaged clusters region seems to be non-uniform with a mean value of $E(B-V)$ = 0.60$\pm$0.05 and 0.95$\pm$0.05 mag for Tr 1 and Be 11 respectively. A random positional variation of $E(B-V)$ is present in both the clusters. In the cluster Be 11, the reason of random positional variation may be apparent association of the HII region (S 213). The 2MASS $JHK$ data in combination with the optical data in the cluster Be 11 yields $E(J-K)$ = 0.40$\pm$0.20 mag and $E(V-K)$ = 2.20$\pm$0.20 mag. Colour excess diagrams indicate a normal interstellar extinction law in the direction of cluster Be 11. The distances of Tr 1 and Be 11 are estimated as 2.6$\pm$0.10 and 2.2$\pm$0.10 Kpc respectively, while the theoretical stellar evolutionary isochrones fitted to the bright cluster members indicate that the cluster Tr 1 and Be 11 are 40$\pm$10 and 110$\pm$10 Myr old. The mass functions corrected for both field star contamination and data incompleteness are derived for both the clusters. The slopes $1.50\pm0.40$ and $1.22\pm0.24$ for Tr 1 and Be 11 respectively are in agreement with the Salpeter's value. Observed mass segregations in both clusters may be due to the result of dynamical evolutions or imprint of star formation processes or both.