XMM-Newton spectroscopy of the cluster of galaxies 2A 0335+096
XMM-Newton spectroscopy of the cluster of galaxies 2A 0335+096
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DOI：
10.1051/0004-6361:20053868
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发表时间：
2005-12
影响因子：
6.5
通讯作者：
N. Werner;J. Plaa;J. Plaa;J. Kaastra;J. Vink;J. Vink;J. Bleeker;J. Bleeker;T. Tamura;J. Peterson;F. Verbunt
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文献类型：
--
作者：
N. Werner;J. Plaa;J. Plaa;J. Kaastra;J. Vink;J. Vink;J. Bleeker;J. Bleeker;T. Tamura;J. Peterson;F. Verbunt
本文介绍了对星系团2A 0335+096进行深（130 ks）XMM-牛顿观测的结果。深度曝光使我们能够详细研究其温度结构和元素丰度。我们拟合了三种不同的热模型，发现多温度wdem模型最适合我们的数据。我们发现，该集群的丰度结构是一致的情况下，Ia型超新星的相对数量的集群内介质的富集作出贡献的是{approx} 25%，而核心塌陷超新星的相对数量是{approx} 75%。将观测到的丰度与超新星产额进行比较，并不能使我们对Pop III星对ICM富集的贡献施加任何限制。径向丰度剖面显示Ia型和核心坍缩超新星产物都有一个强中心峰。温度图和铁丰度图都显示出在表面亮度的拉长形态的方向上的不对称性。特别是温度图显示了核心南侧亮度边缘的急剧变化，这在钱德拉数据中被确定为冷锋。这表明该集群正在与一个子集群合并。此外，我们发现，在集群的核心钱德拉发现的斑点或细丝，与以前的结果相反，比周围的气体更冷，他们似乎是在压力平衡与他们的环境。
We present here the results of a deep (130 ks) XMM-Newton observation of the cluster of galaxies 2A 0335+096. The deep exposure allows us to study in detail its temperature structure and its elemental abundances. We fit three different thermal models and find that the multi-temperature wdem model fits our data best. We find that the abundance structure of the cluster is consistent with a scenario where the relative number of Type Ia supernovae contributing to the enrichment of the intra-cluster medium is {approx}25%, while the relative number of core collapse supernovae is {approx}75%. Comparison of the observed abundances to the supernova yields does not allow us to put any constrains on the contribution of Pop III stars to the enrichment of the ICM. Radial abundance profiles show a strong central peak of both Type Ia and core collapse supernova products. Both the temperature and iron abundance maps show an asymmetry in the direction of the elongated morphology of the surface brightness. In particular the temperature map shows a sharp change over a brightness edge on the southern side of the core, which was identified as a cold front in the Chandra data. This suggests that the cluster is in the process of a merger with a subcluster. Moreover, we find that the blobs or filaments discovered in the core of the cluster by Chandra are, contrary to the previous results, colder than the ambient gas and they appear to be in pressure equilibrium with their environment.