arXiv 0806.14452008-06-09astro-ph

用XMM-牛顿观测大样本星系团的径向金属丰度分布

Radial metallicity profiles for a large sample of galaxy clusters observed with XMM-Newton

A. Leccardi, S. Molendi

备注：: 6 pages, 7 figures, accepted for publication in A&A
DOI：: 10.1051/0004-6361:200810113

摘要：

目标。我们测量了从XMM-牛顿档案中选出的~50个热的、中等红移的星系团样本的径向金属丰度分布。方法.与我们之前的论文一样，我们使用了背景建模而不是背景减除，使用了Cash统计量而不是卡方。该方法需要仔细表征所有背景成分。我们还进行了蒙特卡洛模拟，以评估系统的影响。结果平均金属丰度曲线在中心显示一个峰值，并逐渐下降至0.2 R_{180}。超过0.2 R_{180}，金属丰度大约是0.2太阳，与最近公布的基于模拟的预期不同，与平坦一致。我们没有发现从z=0.1到z=0.3的轮廓演化的证据。当比较我们的平均配置文件与BeppoSAX和钱德拉最近的作品所获得的，我们发现在整个径向范围显着的协议。

英文摘要：

Aims. We measured radial metallicity profiles for a sample of ~50 hot, intermediate redshift galaxy clusters, selected from the XMM-Newton archive. Methods. As in our previous paper, we used background modeling rather than background subtraction, and the Cash statistic rather than the chi square. This method requires a careful characterization of all background components. We also performed montecarlo simulations to assess systematic effects. Results. The mean metallicity profile shows a peak in the center, and gently declines out to 0.2 R_{180}. Beyond 0.2 R_{180} the metallicity is roughly 0.2 solar and, at variance with recently published expectations based on simulations, consistent with being flat. We find no evidence of profile evolution from z=0.1 to z=0.3. When comparing our mean profile to those obtained by recent works with BeppoSAX and Chandra, we find remarkable agreement over the entire radial range.

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