星系团的化学演化：剖析团内介质的铁质量收支
The Chemical Evolution of Galaxy Clusters: Dissecting the Iron Mass Budget of the Intracluster Medium
摘要：
我们通过对ICM中的铁质量进行分析，研究了星系团的化学演化。我们使用钱德拉档案观测的186个形态规则的星系团在红移范围[0.04，1.07]。对于每个集群，我们计算铁丰度和气体密度分布。我们的目的是在铁分布中确定一个与BCG相关的中心峰，以及一个与早期富集相关的近似恒定的平台。我们能够在样品的重要部分中确定这两种成分，仅仅依靠丰度分布的拟合。我们计算了铁峰和平台中包含的铁质量，以及气体质量加权铁丰度，直到$r_{500}$。虽然铁平台没有显示出演化，但我们发现随着铁峰的红移而略有下降。我们测量到铁峰值质量分数通常占$r_{500}$内总铁质量的几个百分比（~1%）。因此，由于总的铁质量预算主要是由高原，我们发现一致的全球气体质量加权铁丰度并没有显着演变。我们还能够重现过去的全球铁丰度演化的说法，这是由于使用不同选择方法的聚类样本，结合使用排放加权而不是气体质量加权丰度值。最后，虽然内在的分散在铁平台质量是一致的零，铁峰值质量表现出大的分散，在符合的事实，即峰值后产生的Virialization的晕，并取决于形成的托管冷核心和相关的反馈过程。我们的结论是，只有一个空间解决的方法可以解决的ICM铁演变的问题，调和在过去十年中获得的矛盾的结果。
英文摘要：
We study the chemical evolution of galaxy clusters by measuring the iron mass in the ICM after dissecting the abundance profiles into different components. We use Chandra archival observations of 186 morphologically regular clusters in the redshift range [0.04, 1.07]. For each cluster we compute the iron abundance and gas density profiles. We aim at identifying in the iron distribution a central peak associated with the BCG, and an approximately constant plateau associated with early enrichment. We are able to firmly identify the two components in a significant fraction of the sample, simply relying on the fit of the abundance profile. We compute the iron mass included in the iron peak and plateau, and the gas mass-weighted iron abundance out to $r_{500}$. While the iron plateau shows no evolution, we find marginal decrease with redshift in the iron peak. We measure that the fraction of iron peak mass is typically a few percent (~1%) of the total iron mass within $r_{500}$. Therefore, since the total iron mass budget is dominated by the plateau, we find consistently that the global gas mass-weighted iron abundance does not evolve significantly. We are also able to reproduce past claims of evolution in the global iron abundance, which turn out to be due to the use of cluster samples with different selection methods combined to the use of emission-weighted instead of gas mass-weighted abundance values. Finally, while the intrinsic scatter in the iron plateau mass is consistent with zero, the iron peak mass exhibits a large scatter, in line with the fact that the peak is produced after the virialization of the halo and depends on the formation of the hosting cool core and the associated feedback processes. We conclude that only a spatially-resolved approach can resolve the issue of the ICM iron evolution, reconciling the contradictory results obtained in the last ten years.
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