标题： ICM中的金属丰度作为团簇历史的诊断工具 显示英文标题

标题： Metal Abundances in the ICM as a Diagnostics of the Cluster History

摘要： 具有密集冷却核的星系团显示出星系团内部介质的金属丰度中央增加。最近，XMM-Newton的研究详细展示了几个重元素相对丰度的结果，表明高中心丰度主要归因于Ia型超新星的贡献。主导来源是星系团中心星系的恒星群体。通过识别重元素的起源以及椭圆星系中观测到的Ia型超新星率，可以将中心丰度峰值用作诊断星系团核心区域历史的工具。我们发现，对于四个附近的冷却核心星系团，即使在过去有更高的Ia型超新星率，中心峰值的富集时间也大于6至10亿年。这表明这些星系团核心区域年龄较老且历史相对平静。元素丰度比的详细分析提供了证据，表明中心星系团中的Ia型超新星产额比用于解释银河系重元素富集的Ia型超新星模型在中间质量元素（如硅和硫）上更加丰富。 显示英文摘要

摘要： Galaxy clusters with a dense cooling core exhibit a central increase in the metallicity of the intracluster medium. Recent XMM-Newton studies with detailed results on the relative abundances of several heavy elements show that the high central abundances are mostly due to the contribution from supernovae type Ia. The dominant source is the stellar population of the central cluster galaxy. With this identification of the origin of heavy elements and the observed rates of SN Ia in elliptical galaxies, the central abundance peak can be used as a diagnostic for the history of the cluster core region. We find for four nearby cooling core clusters that the enrichment times for the central peaks are larger than 6 - 10 Gyrs even for a higher SN Ia rate in the past. This points to an old age and a relatively quiet history of these cluster core regions. A detailed analysis of the element abundance ratios provides evidence that the SN Ia yields in the central cluster galaxies are more rich in intermediate mass elements, like Si and S, compared to the SN Ia models used to explain the heavy element enrichment in our Galaxy.