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arXiv 1105.5840astro-ph.CO
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星团作为斯蒂芬五重奏相互作用的示踪剂（希克森紧致群92）

Star Clusters as Tracers of Interactions in Stephan's Quintet (Hickson Compact Group 92)

K. Fedotov, S. C. Gallagher, I. S. Konstantopoulos, R. Chandar, N. Bastian, J. C. Charlton, B. Whitmore, G. Trancho

备注：
41 pages, 15 figures. Accepted for publication in The Astronomical Journal
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摘要：

斯蒂芬五重星系（SQ）是一个紧凑的星系群，其成员之间存在许多相互作用的迹象。使用高分辨率图像的SQ在B438，V606和I814波段从早期发布的科学项目获得的宽视场相机3的哈勃太空望远镜，我们确定496星团候选人（SCC），位于整个星系本身以及星系际区域。与以前的工作相比，我们的测光工作深入了\sim 2等，并覆盖了另外三个区域，即旧尾，NGC 7317和南部碎片区域。通过比较候选星团B438 - V606和V606 - I814的颜色与简单的恒星星族合成模型，我们能够限制星团年龄。特别是SQ中质量最大的星系NGC 7319，在其整个历史中表现出连续的恒星形成，尽管在过去的几十万年中速度较低。NGC 7318 A/B和北极星暴区域都显示出正在进行的活跃恒星形成;有一些星团的年龄小于1000万年。NGC 7318 A/B在星团的颜色分布中也有一个特殊的间隙，可以用来确定最近爆发的开始日期。在年轻的尾巴中发现的大多数SCC形成于1.5亿至2亿年前，而在老尾巴中星团颜色的紧密分布使我们能够将其形成的年龄限制在\sim 4亿年前。南部碎片区的星团似乎分为两组，年龄分别为50和\sim 5亿年，几乎所有在NGC 7317中探测到的SCC都超过2 Gyr。根据这些年龄，我们估计的时间间隔SQ成员之间的相互作用，触发了大质量恒星团簇形成。

英文摘要：

Stephan's Quintet (SQ) is a compact group of galaxies that exhibits numerous signs of interactions between its members. Using high resolution images of SQ in B438, V606, and I814 bands from the Early Release Science project obtained with the Wide Field Camera 3 on the Hubble Space Telescope, we identify 496 star cluster candidates (SCCs), located throughout the galaxies themselves as well as in intergalactic regions. Our photometry goes \sim2 mag deeper and covers an additional three regions, the Old Tail, NGC 7317, and the Southern Debris Region, compared to previous work. Through comparison of the B438 - V606 and V606 - I814 colors of the star cluster candidates with simple stellar population synthesis models we are able to constrain cluster ages. In particular, the most massive galaxy of SQ, NGC 7319, exhibits continuous star formation throughout its history, although at a lower rate over the past few tens of Myr. NGC 7318 A/B and the Northern Star Burst region both show ongoing active star formation; there are a number of star clusters that are younger than 10 Myr. NGC 7318 A/B also features a peculiar gap in the color distribution of the star clusters that can be used to date the onset of the recent burst. The majority of the SCCs detected in the Young Tail were formed 150-200 Myr ago whereas the tight distribution of star cluster colors in the Old Tail, allow us to constrain its age of formation to \sim400 Myr ago. The star clusters in the Southern Debris region are seemingly divided into two groups with ages of 50 and \sim500 Myr and virtually all of the SCCs detected in NGC 7317 are over 2 Gyr old. Based on these ages, we estimate time intervals for the interactions between SQ members that triggered the massive star cluster formation.

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