Solar abundance ratios of the iron-peak elements in the Perseus cluster
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AHARONIAN, F.; H. AKAMATSU; F. AKIMOTO; S.W. ALLEN; L. ANGELINI; M. AUDARD; H. AWAKI; M. AXELSSON; A. BAMBA; M. BAUTZ; R. BLANDFORD; L. BRENNEMAN; G. BROWN; E. BULBUL; E. CACKETT; M. CHERNYAKOVA; M. CHIAO; P. COPPI; E. COSTANTINI; J. DE PLAA; J.W. 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; S. LEE; M. LEUTENEGGER; O. 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; J. 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; T. SASAKI; G. SATO; K. SATO; R. SATO; M. SAWADA; N. SCHARTEL; P. SERLEMITSOS; H. SETA; M. SHIDATSU; A. SIMIONESCU; R. SMITH; Y. SOONG; L. STAWARZ; Y. SUGAWARA; S. SUGITA; A. SZYMKOWIAK; H. TAJIMA; H. TAKAHASHI; T. TAKAHASHI; S. TAKEDA; Y. TAKEI; T. TAMAGAWA; T. TAMURA; T. TANAKA; Y. TANAKA; Y. TANAKA; M. TASHIRO; Y. TAWARA; Y. TERADA; Y. TERASHIMA; F. TOMBESI; H. TOMIDA; Y. TSUBOI; M. TSUJIMOTO; H. TSUNEMI; T. TSURU; H. UCHIDA; H. UCHIYAMA; Y. UCHIYAMA; S. UEDA; Y. UEDA; S. UNO; C. URRY; E. URSINO; C. DE VRIES; S. WATANABE; Norbert WERNER; D. WIK; D. WILKINS; B. J. WILLIAMS; S. YAMADA; H. YAMAGUCHI; K. YAMAOKA; N. YAMASAKI; M. YAMAUCHI; S. YAMAUCHI; T. YAQOOB; Y. YATSU; D. YONETOKU; I. ZHURAVLEVA a A. ZOGHBI
The metal abundance of the hot plasma that permeates galaxy clusters represents the accumulation of heavy elements produced by billions of supernovae(1). 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(2-6). Recent X-ray studies of the intracluster medium found that the abundance ratios of these elements differ substantially from those seen in the Sun(7-11), 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, highresolution 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(12-14) 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(5,15,16).
AHARONIAN, F.; H. AKAMATSU; F. AKIMOTO; S.W. ALLEN; L. ANGELINI; M. AUDARD; H. AWAKI; M. AXELSSON; A. BAMBA; M. BAUTZ; R. BLANDFORD; L. BRENNEMAN; G. BROWN; E. BULBUL; E. CACKETT; M. CHERNYAKOVA; M. CHIAO; P. COPPI; E. COSTANTINI; J. DE PLAA; J.W. 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; S. LEE; M. LEUTENEGGER; O. 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; J. 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; T. SASAKI; G. SATO; K. SATO; R. SATO; M. SAWADA; N. SCHARTEL; P. SERLEMITSOS; H. SETA; M. SHIDATSU; A. SIMIONESCU; R. SMITH; Y. SOONG; L. STAWARZ; Y. SUGAWARA; S. SUGITA; A. SZYMKOWIAK; H. TAJIMA; H. TAKAHASHI; T. TAKAHASHI; S. TAKEDA; Y. TAKEI; T. TAMAGAWA; T. TAMURA; T. TANAKA; Y. TANAKA; Y. TANAKA; M. TASHIRO; Y. TAWARA; Y. TERADA; Y. TERASHIMA; F. TOMBESI; H. TOMIDA; Y. TSUBOI; M. TSUJIMOTO; H. TSUNEMI; T. TSURU; H. UCHIDA; H. UCHIYAMA; Y. UCHIYAMA; S. UEDA; Y. UEDA; S. UNO; C. URRY; E. URSINO; C. DE VRIES; S. WATANABE; Norbert WERNER; D. WIK; D. WILKINS; B. J. WILLIAMS; S. YAMADA; H. YAMAGUCHI; K. YAMAOKA; N. YAMASAKI; M. YAMAUCHI; S. YAMAUCHI; T. YAQOOB; Y. YATSU; D. YONETOKU; I. ZHURAVLEVA a A. ZOGHBI. Solar abundance ratios of the iron-peak elements in the Perseus cluster. Nature. LONDON: NATURE PUBLISHING GROUP, 2017, roč. 551, č. 7681, s. "478"-"+", 16 s. ISSN 0028-0836. Dostupné z: https://doi.org/10.1038/nature24301.
@article{1406172, author = {Aharonian, F. and Akamatsu, H. and Akimoto, F. and Allen, S.W. and Angelini, L. and Audard, M. and Awaki, H. and Axelsson, M. and Bamba, A. and Bautz, M. and Blandford, R. and Brenneman, L. and Brown, G. and Bulbul, E. and Cackett, E. and Chernyakova, M. and Chiao, M. and Coppi, P. and Costantini, E. and De Plaa, J. and den Herder, J.W. and Done, C. and Dotani, T. and Ebisawa, K. and Eckart, M. and Enoto, T. and Ezoe, Y. and Fabian, A. and Ferrigno, C. and Foster, A. and Fujimoto, R. and Fukazawa, Y. and Furuzawa, A. and Galeazzi, M. and Gallo, L. and Gandhi, P. and Giustini, M. and Goldwurm, A. and Gu, L. and Guainazzi, M. and Haba, Y. and Hagino, K. and Hamaguchi, K. and Harrus, I. and Hatsukade, I. and Hayashi, K. and Hayashi, T. and Hayashida, K. and Hiraga, J. and Hornschemeier, A. and Hoshino, A. and Hughes, J. and Ichinohe, Y. and Iizuka, R. and Inoue, H. and Inoue, Y. and Ishida, M. and Ishikawa, K. and Ishisaki, Y. and Iwai, M. and Kaastra, J. and Kallman, T. and Kamae, T. and Kataoka, J. and Katsuda, S. and Kawai, N. and Kelley, R. and Kilbourne, C. and Kitaguchi, T. and Kitamoto, S. and Kitayama, T. and Kohmura, T. and Kokubun, M. and Koyama, K. and Koyama, S. and Kretschmar, P. and Krimm, H. and Kubota, A. and Kunieda, H. and Laurent, P. and Lee, S. and Leutenegger, M. and Limousine, O. and Loewenstein, M. and Long, K. and Lumb, D. and Madejski, G. and Maeda, Y. and Maier, D. and Makishima, K. and Markevitch, M. and Matsumoto, H. and Matsushita, K. and McCammon, D. and McNamara, B. and Mehdipour, M. and Miller, E. and Miller, J. and Mineshige, S. and Mitsuda, K. and Mitsuishi, I. and Miyazawa, T. and Mizuno, T. and Mori, H. and Mori, K. and Mukai, K. and Murakami, H. and Mushotzky, R. and Nakagawa, T. and Nakajima, H. and Nakamori, T. and Nakashima, S. and Nakazawa, K. and Nobukawa, K. and Nobukawa, M. and Noda, H. and Odaka, H. and Ohashi, T. and Ohno, M. and Okajima, T. and Ota, N. and Ozaki, M. and Paerels, F. and Paltani, S. and Petre, R. and Pinto, C. and Porter, F. and Pottschmidt, K. and Reynolds, C. and SafiandHarb, S. and Saito, S. and Sakai, K. and Sasaki, T. and Sato, G. and Sato, K. and Sato, R. and Sawada, M. and Schartel, N. and Serlemitsos, P. and Seta, H. and Shidatsu, M. and Simionescu, A. and Smith, R. and Soong, Y. and Stawarz, L. and Sugawara, Y. and Sugita, S. and Szymkowiak, A. and Tajima, H. and Takahashi, H. and Takahashi, T. and Takeda, S. and Takei, Y. and Tamagawa, T. and Tamura, T. and Tanaka, T. and Tanaka, Y. and Tanaka, Y. and Tashiro, M. and Tawara, Y. and Terada, Y. and Terashima, Y. and Tombesi, F. and Tomida, H. and Tsuboi, Y. and Tsujimoto, M. and Tsunemi, H. and Tsuru, T. and Uchida, H. and Uchiyama, H. and Uchiyama, Y. and Ueda, S. and Ueda, Y. and Uno, S. and Urry, C. and Ursino, E. and de Vries, C. and Watanabe, S. and Werner, Norbert and Wik, D. and Wilkins, D. and Williams, B. J. and Yamada, S. and Yamaguchi, H. and Yamaoka, K. and Yamasaki, N. and Yamauchi, M. and Yamauchi, S. and Yaqoob, T. and Yatsu, Y. and Yonetoku, D. and Zhuravleva, I. and Zoghbi, A.}, article_location = {LONDON}, article_number = {7681}, doi = {https://doi.org/10.1038/nature24301}, keywords = {Galaxies and clusters;High-energy astrophysics}, language = {eng}, issn = {0028-0836}, journal = {Nature}, title = {Solar abundance ratios of the iron-peak elements in the Perseus cluster}, url = {https://www.nature.com/articles/nature24301}, volume = {551}, year = {2017} }
TY - JOUR ID - 1406172 AU - Aharonian, F. - Akamatsu, H. - Akimoto, F. - Allen, S.W. - Angelini, L. - Audard, M. - Awaki, H. - Axelsson, M. - Bamba, A. - Bautz, M. - Blandford, R. - Brenneman, L. - Brown, G. - Bulbul, E. - Cackett, E. - Chernyakova, M. - Chiao, M. - Coppi, P. - Costantini, E. - De Plaa, J. - den Herder, J.W. - Done, C. - Dotani, T. - Ebisawa, K. - Eckart, M. - Enoto, T. - Ezoe, Y. - Fabian, A. - Ferrigno, C. - Foster, A. - Fujimoto, R. - Fukazawa, Y. - Furuzawa, A. - Galeazzi, M. - Gallo, L. - Gandhi, P. - Giustini, M. - Goldwurm, A. - Gu, L. - Guainazzi, M. - Haba, Y. - Hagino, K. - Hamaguchi, K. - Harrus, I. - Hatsukade, I. - Hayashi, K. - Hayashi, T. - Hayashida, K. - Hiraga, J. - Hornschemeier, A. - Hoshino, A. - Hughes, J. - Ichinohe, Y. - Iizuka, R. - Inoue, H. - Inoue, Y. - Ishida, M. - Ishikawa, K. - Ishisaki, Y. - Iwai, M. - Kaastra, J. - Kallman, T. - Kamae, T. - Kataoka, J. - Katsuda, S. - Kawai, N. - Kelley, R. - Kilbourne, C. - Kitaguchi, T. - Kitamoto, S. - Kitayama, T. - Kohmura, T. - Kokubun, M. - Koyama, K. - Koyama, S. - Kretschmar, P. - Krimm, H. - Kubota, A. - Kunieda, H. - Laurent, P. - Lee, S. - Leutenegger, M. - Limousine, O. - Loewenstein, M. - Long, K. - Lumb, D. - Madejski, G. - Maeda, Y. - Maier, D. - Makishima, K. - Markevitch, M. - Matsumoto, H. - Matsushita, K. - McCammon, D. - McNamara, B. - Mehdipour, M. - Miller, E. - Miller, J. - Mineshige, S. - Mitsuda, K. - Mitsuishi, I. - Miyazawa, T. - Mizuno, T. - Mori, H. - Mori, K. - Mukai, K. - Murakami, H. - Mushotzky, R. - Nakagawa, T. - Nakajima, H. - Nakamori, T. - Nakashima, S. - Nakazawa, K. - Nobukawa, K. - Nobukawa, M. - Noda, H. - Odaka, H. - Ohashi, T. - Ohno, M. - Okajima, T. - Ota, N. - Ozaki, M. - Paerels, F. - Paltani, S. - Petre, R. - Pinto, C. - Porter, F. - Pottschmidt, K. - Reynolds, C. - Safi-Harb, S. - Saito, S. - Sakai, K. - Sasaki, T. - Sato, G. - Sato, K. - Sato, R. - Sawada, M. - Schartel, N. - Serlemitsos, P. - Seta, H. - Shidatsu, M. - Simionescu, A. - Smith, R. - Soong, Y. - Stawarz, L. - Sugawara, Y. - Sugita, S. - Szymkowiak, A. - Tajima, H. - Takahashi, H. - Takahashi, T. - Takeda, S. - Takei, Y. - Tamagawa, T. - Tamura, T. - Tanaka, T. - Tanaka, Y. - Tanaka, Y. - Tashiro, M. - Tawara, Y. - Terada, Y. - Terashima, Y. - Tombesi, F. - Tomida, H. - Tsuboi, Y. - Tsujimoto, M. - Tsunemi, H. - Tsuru, T. - Uchida, H. - Uchiyama, H. - Uchiyama, Y. - Ueda, S. - Ueda, Y. - Uno, S. - Urry, C. - Ursino, E. - de Vries, C. - Watanabe, S. - Werner, Norbert - Wik, D. - Wilkins, D. - Williams, B. J. - Yamada, S. - Yamaguchi, H. - Yamaoka, K. - Yamasaki, N. - Yamauchi, M. - Yamauchi, S. - Yaqoob, T. - Yatsu, Y. - Yonetoku, D. - Zhuravleva, I. - Zoghbi, A. PY - 2017 TI - Solar abundance ratios of the iron-peak elements in the Perseus cluster JF - Nature VL - 551 IS - 7681 SP - "478"-"+" EP - "478"-"+" PB - NATURE PUBLISHING GROUP SN - 00280836 KW - Galaxies and clusters;High-energy astrophysics UR - https://www.nature.com/articles/nature24301 N2 - The metal abundance of the hot plasma that permeates galaxy clusters represents the accumulation of heavy elements produced by billions of supernovae(1). 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(2-6). Recent X-ray studies of the intracluster medium found that the abundance ratios of these elements differ substantially from those seen in the Sun(7-11), 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, highresolution 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(12-14) 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(5,15,16). ER -
AHARONIAN, F.; H. AKAMATSU; F. AKIMOTO; S.W. ALLEN; L. ANGELINI; M. AUDARD; H. AWAKI; M. AXELSSON; A. BAMBA; M. BAUTZ; R. BLANDFORD; L. BRENNEMAN; G. BROWN; E. BULBUL; E. CACKETT; M. CHERNYAKOVA; M. CHIAO; P. COPPI; E. COSTANTINI; J. DE PLAA; J.W. 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; S. LEE; M. LEUTENEGGER; O. 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; J. 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; T. SASAKI; G. SATO; K. SATO; R. SATO; M. SAWADA; N. SCHARTEL; P. SERLEMITSOS; H. SETA; M. SHIDATSU; A. SIMIONESCU; R. SMITH; Y. SOONG; L. STAWARZ; Y. SUGAWARA; S. SUGITA; A. SZYMKOWIAK; H. TAJIMA; H. TAKAHASHI; T. TAKAHASHI; S. TAKEDA; Y. TAKEI; T. TAMAGAWA; T. TAMURA; T. TANAKA; Y. TANAKA; Y. TANAKA; M. TASHIRO; Y. TAWARA; Y. TERADA; Y. TERASHIMA; F. TOMBESI; H. TOMIDA; Y. TSUBOI; M. TSUJIMOTO; H. TSUNEMI; T. TSURU; H. UCHIDA; H. UCHIYAMA; Y. UCHIYAMA; S. UEDA; Y. UEDA; S. UNO; C. URRY; E. URSINO; C. DE VRIES; S. WATANABE; Norbert WERNER; D. WIK; D. WILKINS; B. J. WILLIAMS; S. YAMADA; H. YAMAGUCHI; K. YAMAOKA; N. YAMASAKI; M. YAMAUCHI; S. YAMAUCHI; T. YAQOOB; Y. YATSU; D. YONETOKU; I. ZHURAVLEVA a A. ZOGHBI. Solar abundance ratios of the iron-peak elements in the Perseus cluster. \textit{Nature}. LONDON: NATURE PUBLISHING GROUP, 2017, roč.~551, č.~7681, s.~''478''-''+'', 16 s. ISSN~0028-0836. Dostupné z: https://doi.org/10.1038/nature24301.