NGC1023中的模糊星团是合并星团复合体的残留
Faint Fuzzy Star Clusters in NGC1023 as Remnants of Merged Star Cluster Complexes
摘要：
在透镜状星系NGC 1023中，Larsen和Brodie在蓝色和红色GC群旁边发现了第三个球状星团（GC）群，称为暗模糊（FF）。虽然这些FF的颜色与红色星群相当，但新的星群更暗，更大（R_eff > 7 pc），最重要的是，显示出与NGC 1023星系盘共同旋转的明显迹象。我们提出了N体模拟验证的假设，这些磁盘相关的FF有关的年轻的大规模集群复合体（CC）观察到的巴斯蒂安等。在M51中，他发现了这些CC的质量-半径关系。我们的模型有一个初始配置的基础上，从M51的观测，并放置在不同的轨道上的银河系的潜力推导出NGC 1023。所有的计算结束后，一个稳定的对象包含10至60%的初始CC质量后，积分时间为5 Gyr。转换为目视星等表明，所得到的对象正好覆盖了观测到的FF范围。此外，模拟对象显示投影半质量半径在3.6和13.4 pc之间，与观察到的FF大小一致。我们的结论是，像M51中年轻的大质量CC的对象可能是在NGC 1023中观察到的FF的祖先。
英文摘要：
In the lenticular galaxy NGC1023 a third population of globular clusters (GCs), called faint fuzzies (FFs), was discovered next to the blue and red GC populations by Larsen & Brodie. While these FFs have colors comparable to the red population, the new population is fainter, larger (R_eff > 7 pc) and, most importantly, shows clear signs of co-rotation with the galactic disk of NGC1023. We present N-body simulations verifying the hypothesis that these disk-associated FFs are related to the young massive cluster complexes (CCs) observed by Bastian et. al in M51, who discovered a mass-radius relation for these CCs. Our models have an initial configuration based on the observations from M51 and are placed on various orbits in a galactic potential derived for NGC1023. All computations end up with a stable object containing 10 to 60% of the initial CC mass after an integration time of 5 Gyr. A conversion to visual magnitudes demonstrates that the resulting objects cover exactly the observed range for FFs. Moreover, the simulated objects show projected half-mass radii between 3.6 and 13.4 pc, in good agreement with the observed FF sizes. We conclude that objects like the young massive CCs in M51 are likely progenitors of the FFs observed in NGC1023.
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