THE ORBITAL MOTION OF THE QUINTUPLET CLUSTER—A COMMON ORIGIN FOR THE ARCHES AND QUINTUPLET CLUSTERS?
THE ORBITAL MOTION OF THE QUINTUPLET CLUSTER—A COMMON ORIGIN FOR THE ARCHES AND QUINTUPLET CLUSTERS?
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五联体星团的轨道运动 拱门和五联体星团的共同起源？
DOI：
10.1088/0004-637x/789/2/115
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
Matthews
中科院分区：
文献类型：
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作者：
Stolte;Hußmann;Morris;Brandner;Clarkson;Habibi;Matthews
我们研究了银河系中心附近的五重星系团的轨道运动，目的是约束年轻的大质量星星团在核环境中的形成方案。利用凯克/NIRC2和甚大望远镜/NAOS-CONICA系统在5.8年的时间基线上获得了三个时期的自适应光学高角分辨率成像，提供了0.5 - 1 mas yr-1的天体测量精度。自行得出的集群参考框架，并被用来区分集群成员的大部分密集的领域星星人口的内部隆起。用二维高斯模型拟合团簇和场的自行分布，首次导出团簇的轨道运动。五重态相对于场以132 ± 15 km s-1的二维速度沿着银河平面沿着移动，当与之前已知的径向速度结合时，产生的三维轨道速度为167 ± 15 km s-1。从三个历元中测量的119颗恒星的样本中，我们得出了五重星系团核心的速度色散的上限σ 1D <10 km s − 1。知识的三个速度分量的五重态使我们能够模拟集群轨道的潜在的内银河系。在假设五重星系目前位于200 pc中心的情况下，这些模拟排除了星系团在圆形轨道上运动的可能性。比较五重态的轨道与我们先前测量的拱轨道，我们讨论了这两个集群起源于中央分子区（CMZ）的同一区域的可能性。根据宾尼等人的模型，两个稳定的云轨道家族位于沿着银河棒的长轴和短轴，分别命名为x1和x2轨道。这些星系团的形成轨迹与最外层的x2轨道一致，可能暗示位于银河棒短轴尖端的x1和x2轨道族之间的过渡区域发生了云碰撞。本文在由棒势引起的致密气体沟道作用的框架下讨论了环核中年轻大质量星星团的形成。我们的结论是，一个大规模的酒吧的存在起着重要的作用，在支持正在进行的星星和集群的形成，不仅在附近的螺旋星系与环核环，而且在银河系的CMZ。
We investigate the orbital motion of the Quintuplet cluster near the Galactic center with the aim of constraining formation scenarios of young, massive star clusters in nuclear environments. Three epochs of adaptive optics high-angular resolution imaging with the Keck/NIRC2 and Very Large Telescope/NAOS-CONICA systems were obtained over a time baseline of 5.8 yr, delivering an astrometric accuracy of 0.5–1 mas yr− 1. Proper motions were derived in the cluster reference frame and were used to distinguish cluster members from the majority of the dense field star population toward the inner bulge. Fitting the cluster and field proper motion distributions with two-dimensional (2D) Gaussian models, we derive the orbital motion of the cluster for the first time. The Quintuplet is moving with a 2D velocity of 132±15 km s− 1 with respect to the field along the Galactic plane, which yields a three-dimensional orbital velocity of 167±15 km s− 1 when combined with the previously known radial velocity. From a sample of 119 stars measured in three epochs, we derive an upper limit to the velocity dispersion of σ 1D< 10 km s− 1 in the core of the Quintuplet cluster. Knowledge of the three velocity components of the Quintuplet allows us to model the cluster orbit in the potential of the inner Galaxy. Under the assumption that the Quintuplet is located in the central 200 pc at the present time, these simulations exclude the possibility that the cluster is moving on a circular orbit. Comparing the Quintuplet's orbit with our earlier measurements of the Arches' orbit, we discuss the possibility that both clusters originated in the same area of the central molecular zone (CMZ). According to the model of Binney et al., two families of stable cloud orbits are located along the major and minor axes of the Galactic bar, named x1 and x2 orbits, respectively. The formation locus of these clusters is consistent with the outermost x2 orbit and might hint at cloud collisions at the transition region between the x1 and x2 orbital families located at the tip of the minor axis of the Galactic bar. The formation of young, massive star clusters in circumnuclear rings is discussed in the framework of the channeling in of dense gas by the bar potential. We conclude that the existence of a large-scale bar plays a major role in supporting ongoing star and cluster formation, not only in nearby spiral galaxies with circumnuclear rings, but also in the Milky Way's CMZ.
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DOI：
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发表时间：
1998
期刊：
影响因子：
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作者：
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10.1088/0004-6256/135/2/479
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2007
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The Astronomical Journal
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1990
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