标题： 仙女座星系团中铁峰元素的太阳丰度比 显示英文标题

标题： Solar abundance ratios of the iron-peak elements in the Perseus Cluster

摘要： 热等离子体的金属丰度代表了数十亿颗超新星产生的重元素的积累。因此，星系团内介质的X射线光谱学提供了一个机会，以研究在宇宙时间上整合的超新星爆炸的性质。特别是铁峰元素（铬、锰、铁和镍）的丰度对于理解典型Ia型超新星前体的演化和爆炸方式至关重要。最近对星系团内介质的X射线研究发现，这些元素的丰度比与太阳中的明显不同，表明星系团中的Ia型超新星和银河系中的Ia型超新星的性质存在差异。然而，由于铬和锰的K壳层跃迁线较弱，而铁和镍的跃迁线在光子能量上非常接近，因此需要高分辨率光谱学才能准确确定这些元素的丰度。在这里，我们报告了对Perseus星系团的观测，统计上显著地检测到了铬、锰和镍的共振发射。我们的测量结果结合最新的原子模型显示，这些元素相对于铁的丰度比接近太阳值，这与之前的说法相反。我们的结果与现代核合成计算之间的比较不支持Ia型超新星前体仅是质量远低于钱德拉塞卡极限（约1.4倍太阳质量）的白矮星的假设。观察到的铁峰元素的丰度模式可以通过考虑近钱德拉塞卡质量和亚钱德拉塞卡质量Ia型超新星系统的组合来解释，这进一步加强了证据，表明这两种前体类型都对宇宙化学富集做出了重要贡献。 显示英文摘要

摘要： The metal abundance of the hot plasma that permeates galaxy clusters represents the accumulation of heavy elements produced by billions of supernovae. Therefore, X-ray spectroscopy of the intracluster medium provides an opportunity to investigate the nature of supernova explosions integrated over cosmic time. In particular, the abundance of the iron-peak elements (chromium, manganese, iron and nickel) is key to understanding how the progenitors of typical type Ia supernovae evolve and explode. Recent X-ray studies of the intracluster medium found that the abundance ratios of these elements differ substantially from those seen in the Sun, suggesting differences between the nature of type Ia supernovae in the clusters and in the Milky Way. However, because the K-shell transition lines of chromium and manganese are weak and those of iron and nickel are very close in photon energy, high-resolution spectroscopy is required for an accurate determination of the abundances of these elements. Here we report observations of the Perseus cluster, with statistically significant detections of the resonance emission from chromium, manganese and nickel. Our measurements, combined with the latest atomic models, reveal that these elements have near-solar abundance ratios with respect to iron, in contrast to previous claims. Comparison between our results and modern nucleosynthesis calculations disfavours the hypothesis that type Ia supernova progenitors are exclusively white dwarfs with masses well below the Chandrasekhar limit (about 1.4 times the mass of the Sun). The observed abundance pattern of the iron-peak elements can be explained by taking into account a combination of near- and sub-Chandrasekhar-mass type Ia supernova systems, adding to the mounting evidence that both progenitor types make a substantial contribution to cosmic chemical enrichment.