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arXiv 2407.06274astro-ph.GA
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利用脉冲星计时探测球状星团47 Tuc和Terzan 5中暗恒星遗迹的星群

Probing populations of dark stellar remnants in the globular clusters 47 Tuc and Terzan 5 using pulsar timing

Peter J. Smith, Vincent Hénault-Brunet, Nolan Dickson, Mark Gieles, Holger Baumgardt

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33 pages, 19 figures. Accepted for publication in ApJ
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摘要：

提出了一种结合多质量平衡动力学模型和脉冲星计时数据来约束银河系球状星团（GC）质量分布和剩余粒子数的新方法。我们首先将这种方法应用到47 Tuc，一个集群，其中存在着丰富的恒星运动学数据，这也是主机到一个大的人口毫秒恒星。我们证明，脉冲星定时数据使我们能够对整体质量分布和残余人口的强约束，即使没有恒星运动学拟合。我们的模型倾向于在这个星系团中有一小群恒星质量的黑洞（总质量为$446^{+75}_{-72} \mathrm{M_\odot}$），反对需要一个大的（$ > 2000 \ \mathrm{M_\odot}$）中央中等质量黑洞。然后，我们将该方法应用于泰山5，一个严重模糊的隆起集群，拥有最大的人口的毫秒星系的任何银河系GC和传统的恒星运动学数据的收集是非常有限的。我们改善现有的限制，这个集群的质量分布和结构参数，并严格限制其黑洞的内容，找到一个上限的质量在BH的$\sim 4000 \ \mathrm{M_\odot}$。这种方法使我们能够探测中央动态的GC，即使在没有恒星运动学数据，可以很容易地应用到其他GC脉冲星定时数据，数据集将继续增长与下一代射电望远镜。

英文摘要：

We present a new method to combine multimass equilibrium dynamical models and pulsar timing data to constrain the mass distribution and remnant populations of Milky Way globular clusters (GCs). We first apply this method to 47 Tuc, a cluster for which there exists an abundance of stellar kinematic data and which is also host to a large population of millisecond pulsars. We demonstrate that the pulsar timing data allow us to place strong constraints on the overall mass distribution and remnant populations even without fitting on stellar kinematics. Our models favor a small population of stellar-mass BHs in this cluster (with a total mass of $446^{+75}_{-72} \mathrm{M_\odot}$), arguing against the need for a large ($ > 2000 \ \mathrm{M_\odot}$) central intermediate-mass black hole. We then apply the method to Terzan 5, a heavily obscured bulge cluster which hosts the largest population of millisecond pulsars of any Milky Way GC and for which the collection of conventional stellar kinematic data is very limited. We improve existing constraints on the mass distribution and structural parameters of this cluster and place stringent constraints on its black hole content, finding an upper limit on the mass in BHs of $\sim 4000 \ \mathrm{M_\odot}$. This method allows us to probe the central dynamics of GCs even in the absence of stellar kinematic data and can be easily applied to other GCs with pulsar timing data, for which datasets will continue to grow with the next generation of radio telescopes.

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