THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY. III. MEASURING AGES AND MASSES OF PARTIALLY RESOLVED STELLAR CLUSTERS
THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY. III. MEASURING AGES AND MASSES OF PARTIALLY RESOLVED STELLAR CLUSTERS
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DOI：
10.1088/0004-637x/760/2/104
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发表时间：
2012-09
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通讯作者：
L. Beerman;L. Johnson;M. Fouesneau;J. Dalcanton;D. Weisz;A. Seth;B. Williams;E. Bell;L. Bianchi;N. Caldwell;A. Dolphin;D. Gouliermis;J. Kalirai;S. Larsen;J. Melbourne;H. Rix;E. Skillman
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文献类型：
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作者：
L. Beerman;L. Johnson;M. Fouesneau;J. Dalcanton;D. Weisz;A. Seth;B. Williams;E. Bell;L. Bianchi;N. Caldwell;A. Dolphin;D. Gouliermis;J. Kalirai;S. Larsen;J. Melbourne;H. Rix;E. Skillman
恒星初始质量函数（IMF）的随机采样可以强烈地影响星团的视年龄和质量，当从低质量星团（104 M）的综合颜色推断时。我们使用模拟的星星集群表明，这些影响最小化时，最明亮的，快速发展的恒星在一个集群可以解决，和光线较暗，更多的未解决的恒星可以单独分析。当比较来自亮度较低的星团成员的光与未解析光的模型时，可以获得比在假设IMF完全填充的情况下分析来自整个星团的集成光时更准确的年龄估计。我们展示了这种技术的成功，首先使用模拟集群，然后与恒星集群在M31。这种方法代表了一种方法占离散的，随机抽样的恒星IMF在质量较小的集群，并可以利用在整个本地集团和其他附近星系的集群的研究。
The apparent age and mass of a stellar cluster can be strongly affected by stochastic sampling of the stellar initial mass function (IMF), when inferred from the integrated color of low-mass clusters (≲104 M☉). We use simulated star clusters to show that these effects are minimized when the brightest, rapidly evolving stars in a cluster can be resolved, and the light of the fainter, more numerous unresolved stars can be analyzed separately. When comparing the light from the less luminous cluster members to models of unresolved light, more accurate age estimates can be obtained than when analyzing the integrated light from the entire cluster under the assumption that the IMF is fully populated. We show the success of this technique first using simulated clusters, and then with a stellar cluster in M31. This method represents one way of accounting for the discrete, stochastic sampling of the stellar IMF in less massive clusters and can be leveraged in studies of clusters throughout the Local Group and other nearby galaxies.