半人马座ω核心的最新HST天文光度学分析。III。主序列的多重种群
The State-of-the-Art HST Astro-Photometric Analysis of the core of ωCentauri. III. The Main Sequence's Multiple Populations Galore
摘要：
我们利用本系列第一篇论文中提出的欧米茄Cen核心的哈勃空间望远镜26滤光器天文光度表的精美质量和第二篇论文中提出的经验微分红化校正，以便将主序列提取为其组成群体。为此，我们将自己限制在五个最有用的过滤器：F275W，F336W和F438W的神奇“三重奏”，以及F606W和F814W。我们开发了一种识别颜色系统的策略，其中不同的人群最明显，然后我们隔离这些人群，并在其他过滤器中检查它们，在这些过滤器中，它们的子人群也会出现。通过这种方式，我们已经确定了至少15个子群体，每个子群体都有一个独特的基准曲线，通过我们的5维光度空间。我们确认MSa被分成两个子组件，并发现bMS和rMS被分成三个子组件。此外，我们还发现了另外两个MS组：MSd（有三个子组分）与bMS具有相似的性质，而MSe（有四个子组分）具有与rMS更相似的性质。我们一起检查基准曲线，并使用合成光谱来推断相对重元素，轻元素和氦丰度的人口。我们的研究结果表明，欧米茄Cen的恒星星族和恒星形成历史比以前推断的更为复杂。最后，作为对原始星表的补充，我们提供了一个列表，该列表确定了每颗恒星最有可能与哪个种群相关。
英文摘要：
We take advantage of the exquisite quality of the Hubble Space Telescope 26-filter astro-photometric catalog of the core of Omega Cen presented in the first paper of this series and the empirical differential-reddening correction presented in the second paper in order to distill the main sequence into its constituent populations. To this end, we restrict ourselves to the five most useful filters: the magic "trio" of F275W, F336W, and F438W, along with F606W and F814W. We develop a strategy for identifying color systems where different populations stand out most distinctly, then we isolate those populations and examine them in other filters where their sub-populations also come to light. In this way, we have identified at least 15 sub-populations, each of which has a distinctive fiducial curve through our 5-dimensional photometric space. We confirm the MSa to be split into two subcomponents, and find that both the bMS and the rMS are split into three subcomponents. Moreover, we have discovered two additional MS groups: the MSd (which has three subcomponents) shares similar properties with the bMS, and the MSe (which has four subcomponents), has properties more similar to those of the rMS. We examine the fiducial curves together and use synthetic spectra to infer relative heavy-element, light-element, and Helium abundances for the populations. Our findings show that the stellar populations and star formation history of Omega Cen are even more complex than inferred previously. Finally, we provide as a supplement to the original catalog a list that identifies for each star which population it most likely is associated with.
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