探索银河系中心：利用Gaia DR3数据对Bulge OCs HSC 25、HSC 37、HSC 2878的全面研究
Exploring the Near Galactic Centre: A Comprehensive Study of Bulge OCs HSC 25, HSC 37, HSC 2878 Utilising Gaia DR3 Data
AI总结：
利用Gaia DR3数据研究银河系中心开放星团的动态演化和起源
摘要：
我们对位于银河系盘最内区域的开放星团HSC 25、HSC 37和HSC 2878进行了全面的光度和运动学研究。利用Gaia DR3数据和UPMASK成员算法，我们分别确定了HSC 25、HSC 37和HSC 2878的最可能成员为44、55和112个。HSC 25、HSC 37和HSC 2878的平均自行分量分别为(-5.901±0.41, -6.213±0.40)、(-3.231±0.56, -4.564±0.47)和(-3.830±0.51, -5.198±0.44) mas yr⁻¹。这些开放星团覆盖了广泛的演化阶段，估计年龄为log(t/yr)=8.38±0.08、7.04±0.09和9.04±0.09，对应的银心距离为7.36±0.37、6.79±0.18和6.17±0.22 kpc。获得的金属度分别为0.0388±0.0039、0.0259±0.0028和0.0209±0.0023。总质量估计为135、755和204个太阳质量，显示出星团中恒星含量的显著差异。动态弛豫时间的分析表明，HSC 25和HSC 2878已动态演化，而年轻的HSC 37仍处于动态演化的早期阶段。这些星团的高空间速度和轨道参数揭示了显著偏离典型盘运动学。HSC 25和HSC 37表现出偏心轨道和小近银心距离，与在银河系晕内动态加热或吸积起源一致。相比之下，HSC 2878的放松、平面轨道表明其尽管年龄较大但仍属于银心成员。这些发现表明这些星团具有异质的动态起源，对银河系中心的恒星形成和演化有重要意义。
英文摘要：
We present a comprehensive photometric and kinematic study of the open clusters HSC 25, HSC 37, and HSC 2878, located in the innermost regions of the Galactic disc. Utilizing data from Gaia DR3 and the UPMASK membership algorithm, we identify 44, 55, and 112 most probable members for HSC 25, HSC 37, and HSC 2878, respectively. The mean proper-motion components are obtained as (-5.901 +/- 0.41, -6.213 +/- 0.40), (-3.231 +/- 0.56, -4.564 +/- 0.47), and (-3.830 +/- 0.51, -5.198 +/- 0.44) mas yr^-1 for HSC 25, HSC 37, and HSC 2878, respectively. The open clusters span a broad range of evolutionary stages, with estimated ages of log(t/yr) = 8.38 +/- 0.08, 7.04 +/- 0.09, and 9.04 +/- 0.09, and corresponding heliocentric distances of 7.36 +/- 0.37, 6.79 +/- 0.18, and 6.17 +/- 0.22 kpc. The obtained metallicities are 0.0388 +/- 0.0039, 0.0259 +/- 0.0028, and 0.0209 +/- 0.0023, respectively. Total mass estimates are 135, 755, and 204 solar masses, respectively, highlighting notable differences in stellar content across the clusters. An analysis of dynamical relaxation times suggests that HSC 25 and HSC 2878 are dynamically evolved, whereas the much younger HSC 37 is still in an early phase of dynamical evolution. The high space velocities and orbital parameters of these clusters reveal significant deviations from typical disc kinematics. HSC 25 and HSC 37 exhibit eccentric orbits and small perigalactic distances, consistent with dynamically heated or accreted origins within the Galactic bulge. In contrast, HSC 2878's relaxed, planar orbit suggests in situ bulge membership despite its age. These findings point toward a heterogeneous dynamical origin for the clusters, with implications for star formation and evolution in the inner Milky Way.
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