Intermediate-Element Abundances in Galaxy Clusters

Intermediate-Element Abundances in Galaxy Clusters
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星系团中的中间元素丰度

DOI：
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发表时间：
2002
期刊：
影响因子：
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通讯作者：
R. Mushotzky
R. Mushotzky
中科院分区：
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文献类型：
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作者：
W. Baumgartner;W. Baumgartner;W. Baumgartner;M. Loewenstein;M. Loewenstein;D. Horner;R. Mushotzky

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我们提出的平均丰度的中间元素进行堆叠分析的所有星系团的档案中的X射线望远镜ASCA。我们确定的Fe，Si，S，和Ni的丰度作为集群温度（质量）的函数从1-10千电子伏，并把强上限的Ca和Ar的丰度。一般来说，Si和Ni相对于Fe过剩，而Ar和Ca非常不足。Si、S、Ar和Ca的丰度之间的差异表明α-元素并不均匀地表现为单个组。我们发现，最确定的元素Fe，Si和S的丰度与最近的理论超新星产量不给一个一致的解决方案，在任何温度或质量的Ia型和II型超新星产生的物质的分数。总的趋势是，对于温度较高的星团，II型超新星比Ia型超新星产生更多的金属。我们的结果与银河系丰度的不一致表明，螺旋星系不是主要的金属贡献者的团内介质（ICM）。元素丰度的模式需要一个额外的金属来源超过标准的Ia型和II型超新星富集。这个新来源的性质与II型超新星的性质非常匹配，具有非常大的贫金属祖星。这些结果与早期第三星族恒星产生的ICM金属的重要部分一致。
We present the average abundances of the intermediate elements obtained by performing a stacked analysis of all the galaxy clusters in the archive of the X-ray telescope ASCA. We determine the abundances of Fe, Si, S, and Ni as a function of cluster temperature (mass) from 1-10 keV and place strong upper limits on the abundances of Ca and Ar. In general, Si and Ni are overabundant with respect to Fe, while Ar and Ca are very underabundant. The discrepancy between the abundances of Si, S, Ar, and Ca indicate that the α-elements do not behave homogeneously as a single group. We show that the abundances of the most well-determined elements Fe, Si, and S in conjunction with recent theoretical supernova yields do not give a consistent solution for the fraction of material produced by Type Ia and Type II supernovae at any temperature or mass. The general trend is for higher temperature clusters to have more of their metals produced in Type II supernovae than in Type Ia supernovae. The inconsistency of our results with abundances in the Milky Way indicate that spiral galaxies are not the dominant metal contributors to the intracluster medium (ICM). The pattern of elemental abundances requires an additional source of metals beyond standard Type Ia and Type II supernova enrichment. The properties of this new source are well matched to those of Type II supernovae with very massive, metal-poor progenitor stars. These results are consistent with a significant fraction of the ICM metals produced by an early generation of Population III stars.