论文标题
对开放群集Czernik 14，Haffner 14，Haffner 17和King 10的全面研究，使用多色光度法和Gaia DR2 Astrometry
A Comprehensive study of open clusters Czernik 14, Haffner 14, Haffner 17 and King 10 using multicolour photometry and Gaia DR2 astrometry
论文作者
论文摘要
本文使用Gaia DR2，2 Mass，Wise，Wise，Apass和Pan-Starrs1数据集对四个开放簇Czernik 14，Haffner 14，Haffner 14和King 10进行了调查。我们发现这些簇的十二光度带中的正常星际灭绝。对于Czernik 14，Haffner 14，Haffner 17和King 10分别使用GAIA DR2适当的运动数据，可能将群集成员分别确定为225、353、350和395。半径为Czernik 14，Haffner 14，Haffner 17和King 10分别确定为3.5、3.7、6.2和5.7 Arcmin。 RA和DEC中的平均正确运动估计为（-0.42 \ pm 0.02，-0.38 \ pm 0.01），（-1.82 \ pm 0.009，1.73，1.73 \ pm 0.008），（-1.17 \ pm 0.007，1.88，1.88 \ pm pm 0.006）和（-2.75 \ pm 0.006）和y.2.75 \ pm 0.008，-ik f pm 0.008，-ik，-ik，-ik，-ik，-ik f pm th 14，Haffner 14，Haffner 17和King 10。对这些群集的观察到的CMD的比较导致570 \ pm 60、320 \ pm 35、90 \ pm 10和45 \ pm 5 Myr的年龄。距离2.9 \ pm 0.1、4.8 \ pm 0.4、3.6 \ pm 0.1和3.8 \ pm 0.1 kpc使用视差确定的距离与等速异隆拟合方法得出的值可比。发现质量斜率与Salpeter值非常吻合。总质量分别为Czernik 14，Haffner 14，Haffner 17和King 10分别为348、595、763和1088太阳能块。在每个群集中都观察到存在质量分离效应的证据。使用银河电位模型，为簇得出了银河轨道。本研究表明，研究下的所有簇围绕银河中心周围的圆形路径。
This paper presents an investigation on the four open clusters Czernik 14, Haffner 14, Haffner 17 and King 10 located near the Perseus arm of Milky Way Galaxy using Gaia DR2, 2MASS, WISE, APASS and Pan-STARRS1 data sets. We find normal interstellar extinction in twelve photometric bands for these clusters. Likely cluster members are identified as 225, 353, 350 and 395 for Czernik 14, Haffner 14, Haffner 17 and King 10, respectively by using Gaia DR2 proper motion data. Radii are determined as 3.5, 3.7, 6.2 and 5.7 arcmin for Czernik 14, Haffner 14, Haffner 17 and King 10 respectively. Mean proper motions in RA and DEC are estimated as (-0.42 \pm 0.02, -0.38 \pm 0.01), (-1.82 \pm 0.009, 1.73 \pm 0.008), (-1.17 \pm 0.007, 1.88 \pm 0.006) and (-2.75 \pm 0.008, -2.04 \pm 0.006) mas/yr for Czernik 14, Haffner 14, Haffner 17 and King 10, respectively. The comparison of observed CMDs with solar metallicity isochrones leads to an age of 570 \pm 60, 320 \pm 35, 90 \pm 10 and 45 \pm 5 Myr for these clusters. The distances 2.9 \pm 0.1, 4.8 \pm 0.4, 3.6 \pm 0.1 and 3.8 \pm 0.1 kpc determined using parallax are comparable with the values derived by the isochrone fitting method. Mass function slopes are found to be in good agreement with the Salpeter value. The total masses are derived as 348, 595, 763 and 1088 solar mass for the clusters Czernik 14, Haffner 14, Haffner 17 and King 10, respectively. Evidence for the existence of mass-segregation effect is observed in each cluster. Using the Galactic potential model, Galactic orbits are derived for the clusters. The present study indicates that all clusters under study fallow a circular path around the Galactic center.
