Solar abundance ratios of the iron-peak elements in the Perseus cluster-猫眼课题宝

DOI：

10.1038/nature24301

发表时间：

2017-11

期刊：

Nature

影响因子：

64.8

通讯作者：

中科院分区：

综合性期刊1区

文献类型：

作者：

Felix Hiroki Fumie Steven W. Lorella Marc Hisamitsu Magn Aharonian Akamatsu Akimoto Allen Angelini Audard A-Felix-Hiroki-Fumie-Steven-W.-Lorella-Marc-Hisamitsu;F. Aharonian;H. Akamatsu;F. Akimoto;S. Allen;L. Angelini;M. Audard;H. Awaki;M. Axelsson;A. Bamba;M. Bautz;R. Blandford;L. Brenneman;G. V. Brown;E. Bulbul;E. Cackett;M. Chernyakova;M. Chiao;P. Coppi;E. Costantini;J. de Plaa;J. D. den Herder;C. Done;T. Dotani;K. Ebisawa;M. Eckart;T. Enoto;Y. Ezoe;A. Fabian;C. Ferrigno;A. Foster;R. Fujimoto;Y. Fukazawa;A. Furuzawa;M. Galeazzi;L. Gallo;P. Gandhi;M. Giustini;A. Goldwurm;L. Gu;M. Guainazzi;Y. Haba;K. Hagino;K. Hamaguchi;I. Harrus;I. Hatsukade;K. Hayashi;T. Hayashi;K. Hayashida;J. Hiraga;A. Hornschemeier;A. Hoshino;J. Hughes;Y. Ichinohe;R. Iizuka;H. Inoue;Y. Inoue;M. Ishida;K. Ishikawa;Y. Ishisaki;M. Iwai;J. Kaastra;T. Kallman;T. Kamae;J. Kataoka;S. Katsuda;N. Kawai;R. Kelley;C. Kilbourne;T. Kitaguchi;S. Kitamoto;T. Kitayama;T. Kohmura;M. Kokubun;K. Koyama;S. Koyama;P. Kretschmar;H. Krimm;A. Kubota;H. Kunieda;P. Laurent;Shiu-Hang Lee;M. Leutenegger;Olivier Limousine;M. Loewenstein;K. Long;D. Lumb;G. Madejski;Y. Maeda;D. Maier;K. Makishima;M. Markevitch;H. Matsumoto;K. Matsushita;D. McCammon;B. McNamara;M. Mehdipour;E. Miller;Jonathan M. Miller;S. Mineshige;K. Mitsuda;I. Mitsuishi;T. Miyazawa;T. Mizuno;H. Mori;K. Mori;K. Mukai;H. Murakami;R. Mushotzky;T. Nakagawa;H. Nakajima;T. Nakamori;S. Nakashima;K. Nakazawa;K. Nobukawa;M. Nobukawa;H. Noda;H. Odaka;T. Ohashi;M. Ohno;T. Okajima;N. Ota;M. Ozaki;F. Paerels;S. Paltani;R. Petre;C. Pinto;F. Porter;K. Pottschmidt;C. Reynolds;S. Safi-Harb;S. Saito;K. Sakai;Toru Sasaki;G. Sato;Kosuke Sato;R. Sato;M. Sawada;N. Schartel;P. Serlemitsos;H. Seta;M. Shidatsu;A. Simionescu;Randall K. Smith;Y. Soong;L. Stawarz;Y. Sugawara;S. Sugita;A. Szymkowiak;H. Tajima;Hiromitsu Takahashi;Tadayuki Takahashi;S. Takeda;Y. Takei;T. Tamagawa;T. Tamura;Takaaki Tanaka;Yasuo Tanaka;Yasuyuki T. Tanaka;M. Tashiro;Y. Tawara;Y. Terada;Y. Terashima;F. Tombesi;H. Tomida;Y. Tsuboi;M. Tsujimoto;H. Tsunemi;Takeshi Go Tsuru;H. Uchida;H. Uchiyama;Y. Uchiyama;S. Ueda;Y. Ueda;S. Uno;C. M. Urry;E. Ursino;C. D. de Vries;S. Watanabe;N. Werner;D. Wik;D. Wilkins;B. Williams;S. Yamada;H. Yamaguchi;K. Yamaoka;N. Yamasaki;M. Yamauchi;S. Yamauchi;T. Yaqoob;Y. Yatsu;D. Yonetoku;I. Zhuravleva;A. Zoghbi

弥漫在星系团中的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，星团内介质的X射线光谱学提供了一个机会来研究超新星爆炸在宇宙时间内的性质。特别是，铁峰元素（铬，锰，铁和镍）的丰度是理解典型Ia型超新星祖先如何进化和爆炸的关键。最近对星团内介质的X射线研究发现，这些元素的丰度比与在太阳中看到的有很大的不同，这表明星团和银河系中Ia型超新星的性质不同。然而，由于铬和锰的K壳层跃迁线很弱，而铁和镍的K壳层跃迁线在光子能量上非常接近，因此需要高分辨率光谱来准确测定这些元素的丰度。在这里，我们报告的观测英仙座集群，从铬，锰和镍的共振发射的统计显着检测。我们的测量，结合最新的原子模型，揭示了这些元素相对于铁具有接近太阳的丰度比，与以前的说法相反。我们的结果和现代核合成计算的比较，不赞成假设Ia型超新星的祖先是专门的白色矮星，质量远低于卡拉塞卡极限（约1.4倍的太阳质量）。观测到的铁峰值元素的丰度模式可以通过考虑近和亚克拉塞卡质量的Ia型超新星系统的组合来解释，增加了越来越多的证据表明这两种祖先类型对宇宙化学富集做出了重大贡献。

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,,.

Solar abundance ratios of the iron-peak elements in the Perseus cluster

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