The central dynamics of M3, M13, and M92: stringent limits on the masses of intermediate-mass black holes
The central dynamics of M3, M13, and M92: stringent limits on the masses of intermediate-mass black holes
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M3、M13和M92的中心动力学：中等质量黑洞质量的严格限制
DOI：
10.1051/0004-6361/201322183
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发表时间：
2014
影响因子：
6.5
通讯作者：
Wisotzki
中科院分区：
文献类型：
--
作者：
Kamann;Wisotzki
我们使用PMAS积分场摄谱仪获得了三个北方银河系球状星团M3、M13和M92中心区域的大量径向速度。利用拥挤场三维光谱技术，我们测量了每个星团中心~10″范围内约80颗恒星的径向速度。这些是迄今为止在这些星团最内部获得的最大光谱数据集。为了获得整个范围内的集群的运动学数据，我们补充我们的数据与文献中的测量。我们结合联合收割机我们的速度测量与表面亮度配置文件使用球形牛仔裤模型分析每个集群的内部动力学，并调查我们的数据是否提供了证据，在任何集群的中等质量黑洞。表面亮度分布显示，所有三个集群是一致的核心配置文件，虽然浅尖不能排除。我们发现，具有恒定质光比的球形牛仔裤模型提供了一个很好的整体表示的运动学数据。在这三个星团中，没有一个需要大质量黑洞来解释观察到的运动学。我们的1σ（3σ）上限是M3的5300 M（12000 M），M13的8600 M（13000 M），M92的980 M（2700 M）。一个令人困惑的情况是在M3和M13中存在几颗潜在的高速恒星，因为它们的存在可以解释我们与M92相比在质量极限中发现的大部分差异。
We used the PMAS integral field spectrograph to obtain large sets of radial velocities in the central regions of three northern Galactic globular clusters: M3, M13, and M92. By applying the novel technique of crowded field 3D spectroscopy, we measured radial velocities for about 80 stars within the central ~10″ of each cluster. These are by far the largest spectroscopic datasets obtained in the innermost parts of these clusters up to now. To obtain kinematical data across the whole extent of the clusters, we complement our data with measurements available in the literature. We combine our velocity measurements with surface brightness profiles to analyse the internal dynamics of each cluster using spherical Jeans models, and investigate whether our data provide evidence for an intermediate-mass black hole in any of the clusters. The surface brightness profiles reveal that all three clusters are consistent with a core profile, although shallow cusps cannot be excluded. We find that spherical Jeans models with a constant mass-to-light ratio provide a good overall representation of the kinematical data. A massive black hole is required in none of the three clusters to explain the observed kinematics. Our 1σ(3σ) upper limits are 5300M⊙(12 000M⊙) for M3, 8600M⊙(13 000M⊙) for M13, and 980M⊙(2700M⊙) for M92. A puzzling circumstance is the existence of several potential high velocity stars in M3 and M13, as their presence can account for the majority of the discrepancies that we find in our mass limits compared to M92.