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

J 2017

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

AHARONIAN, F., H. AKAMATSU, F. AKIMOTO, S.W. ALLEN, L. ANGELINI et. al.

Basic information

Original name

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

Authors

AHARONIAN, F. (276 Germany), H. AKAMATSU (528 Netherlands), F. AKIMOTO (124 Canada), S.W. ALLEN (826 United Kingdom of Great Britain and Northern Ireland), L. ANGELINI (380 Italy), M. AUDARD (250 France), H. AWAKI (208 Denmark), M. AXELSSON (208 Denmark), A. BAMBA (124 Canada), M. BAUTZ (840 United States of America), R. BLANDFORD (826 United Kingdom of Great Britain and Northern Ireland), L. BRENNEMAN (840 United States of America), G. BROWN (840 United States of America), E. BULBUL (840 United States of America), E. CACKETT (826 United Kingdom of Great Britain and Northern Ireland), M. CHERNYAKOVA (804 Ukraine), M. CHIAO (840 United States of America), P. COPPI (840 United States of America), E. COSTANTINI (380 Italy), J. DE PLAA (528 Netherlands), J.W. DEN HERDER (528 Netherlands), C. DONE (826 United Kingdom of Great Britain and Northern Ireland), T. DOTANI (380 Italy), K. EBISAWA (840 United States of America), M. ECKART (840 United States of America), T. ENOTO (840 United States of America), Y. EZOE (840 United States of America), A. FABIAN (826 United Kingdom of Great Britain and Northern Ireland), C. FERRIGNO (380 Italy), A. FOSTER (840 United States of America), R. FUJIMOTO (840 United States of America), Y. FUKAZAWA (840 United States of America), A. FURUZAWA (840 United States of America), M. GALEAZZI (380 Italy), L. GALLO (380 Italy), P. GANDHI (826 United Kingdom of Great Britain and Northern Ireland), M. GIUSTINI (380 Italy), A. GOLDWURM (826 United Kingdom of Great Britain and Northern Ireland), L. GU (528 Netherlands), M. GUAINAZZI (380 Italy), Y. HABA (380 Italy), K. HAGINO (840 United States of America), K. HAMAGUCHI (840 United States of America), I. HARRUS (840 United States of America), I. HATSUKADE (840 United States of America), K. HAYASHI (840 United States of America), T. HAYASHI (840 United States of America), K. HAYASHIDA (840 United States of America), J. HIRAGA (840 United States of America), A. HORNSCHEMEIER (840 United States of America), A. HOSHINO (840 United States of America), J. HUGHES (840 United States of America), Y. ICHINOHE (826 United Kingdom of Great Britain and Northern Ireland), R. IIZUKA (840 United States of America), H. INOUE (840 United States of America), Y. INOUE (840 United States of America), M. ISHIDA (840 United States of America), K. ISHIKAWA (840 United States of America), Y. ISHISAKI (840 United States of America), M. IWAI (840 United States of America), J. KAASTRA (528 Netherlands), T. KALLMAN (840 United States of America), T. KAMAE (840 United States of America), J. KATAOKA (840 United States of America), S. KATSUDA (840 United States of America), N. KAWAI (840 United States of America), R. KELLEY (840 United States of America), C. KILBOURNE (840 United States of America), T. KITAGUCHI (840 United States of America), S. KITAMOTO (840 United States of America), T. KITAYAMA (840 United States of America), T. KOHMURA (840 United States of America), M. KOKUBUN (840 United States of America), K. KOYAMA (840 United States of America), S. KOYAMA (840 United States of America), P. KRETSCHMAR (840 United States of America), H. KRIMM (840 United States of America), A. KUBOTA (840 United States of America), H. KUNIEDA (840 United States of America), P. LAURENT (840 United States of America), S. LEE (840 United States of America), M. LEUTENEGGER (840 United States of America), O. LIMOUSINE (250 France), M. LOEWENSTEIN (840 United States of America), K. LONG (840 United States of America), D. LUMB (826 United Kingdom of Great Britain and Northern Ireland), G. MADEJSKI (616 Poland), Y. MAEDA (840 United States of America), D. MAIER (840 United States of America), K. MAKISHIMA (840 United States of America), M. MARKEVITCH (643 Russian Federation), H. MATSUMOTO (826 United Kingdom of Great Britain and Northern Ireland), K. MATSUSHITA (840 United States of America), D. MCCAMMON (840 United States of America), B. MCNAMARA (840 United States of America), M. MEHDIPOUR (840 United States of America), E. MILLER (840 United States of America), J. MILLER (840 United States of America), S. MINESHIGE (840 United States of America), K. MITSUDA (840 United States of America), I. MITSUISHI (840 United States of America), T. MIYAZAWA (840 United States of America), T. MIZUNO (840 United States of America), H. MORI (840 United States of America), K. MORI (840 United States of America), K. MUKAI (840 United States of America), H. MURAKAMI (840 United States of America), R. MUSHOTZKY (840 United States of America), T. NAKAGAWA (840 United States of America), H. NAKAJIMA (840 United States of America), T. NAKAMORI (840 United States of America), S. NAKASHIMA (840 United States of America), K. NAKAZAWA (840 United States of America), K. NOBUKAWA (840 United States of America), M. NOBUKAWA (840 United States of America), H. NODA (840 United States of America), H. ODAKA (840 United States of America), T. OHASHI (840 United States of America), M. OHNO (528 Netherlands), T. OKAJIMA (840 United States of America), N. OTA (840 United States of America), M. OZAKI (840 United States of America), F. PAERELS (528 Netherlands), S. PALTANI (840 United States of America), R. PETRE (840 United States of America), C. PINTO (380 Italy), F. PORTER (840 United States of America), K. POTTSCHMIDT (840 United States of America), C. REYNOLDS (826 United Kingdom of Great Britain and Northern Ireland), S. SAFI-HARB (840 United States of America), S. SAITO (840 United States of America), K. SAKAI (840 United States of America), T. SASAKI (840 United States of America), G. SATO (840 United States of America), K. SATO (840 United States of America), R. SATO (840 United States of America), M. SAWADA (840 United States of America), N. SCHARTEL (276 Germany), P. SERLEMITSOS (840 United States of America), H. SETA (840 United States of America), M. SHIDATSU (840 United States of America), A. SIMIONESCU (642 Romania), R. SMITH (840 United States of America), Y. SOONG (840 United States of America), L. STAWARZ (840 United States of America), Y. SUGAWARA (840 United States of America), S. SUGITA (840 United States of America), A. SZYMKOWIAK (840 United States of America), H. TAJIMA (840 United States of America), H. TAKAHASHI (840 United States of America), T. TAKAHASHI (840 United States of America), S. TAKEDA (840 United States of America), Y. TAKEI (840 United States of America), T. TAMAGAWA (840 United States of America), T. TAMURA (840 United States of America), T. TANAKA (840 United States of America), Y. TANAKA (840 United States of America), Y. TANAKA (840 United States of America), M. TASHIRO (840 United States of America), Y. TAWARA (840 United States of America), Y. TERADA (840 United States of America), Y. TERASHIMA (840 United States of America), F. TOMBESI (380 Italy), H. TOMIDA (840 United States of America), Y. TSUBOI (840 United States of America), M. TSUJIMOTO (840 United States of America), H. TSUNEMI (840 United States of America), T. TSURU (840 United States of America), H. UCHIDA (840 United States of America), H. UCHIYAMA (840 United States of America), Y. UCHIYAMA (840 United States of America), S. UEDA (840 United States of America), Y. UEDA (840 United States of America), S. UNO (840 United States of America), C. URRY (840 United States of America), E. URSINO (380 Italy), C. DE VRIES (528 Netherlands), S. WATANABE (840 United States of America), Norbert WERNER (703 Slovakia, guarantor, belonging to the institution), D. WIK (840 United States of America), D. WILKINS (840 United States of America), B. J. WILLIAMS (840 United States of America), S. YAMADA (840 United States of America), H. YAMAGUCHI (840 United States of America), K. YAMAOKA (840 United States of America), N. YAMASAKI (840 United States of America), M. YAMAUCHI (840 United States of America), S. YAMAUCHI (840 United States of America), T. YAQOOB (840 United States of America), Y. YATSU (840 United States of America), D. YONETOKU (840 United States of America), I. ZHURAVLEVA (643 Russian Federation) and A. ZOGHBI (528 Netherlands)

Edition

Nature, LONDON, NATURE PUBLISHING GROUP, 2017, 0028-0836

Other information

Language

English

Type of outcome

Článek v odborném periodiku

Field of Study

10308 Astronomy

Country of publisher

United Kingdom of Great Britain and Northern Ireland

Confidentiality degree

není předmětem státního či obchodního tajemství

References:

URL URL

Impact factor

Impact factor: 41.577

RIV identification code

RIV/00216224:14310/17:00099805

Organization unit

Faculty of Science

DOI

http://dx.doi.org/10.1038/nature24301

UT WoS

000416043700039

Keywords in English

Galaxies and clusters;High-energy astrophysics

Abstract

V originále

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).

Citovat

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 and A. ZOGHBI. Solar abundance ratios of the iron-peak elements in the Perseus cluster. Nature. LONDON: NATURE PUBLISHING GROUP, 2017, vol. 551, No 7681, p. "478"-"+", 16 pp. ISSN 0028-0836. Available from: https://dx.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 = {http://dx.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 and A. ZOGHBI. Solar abundance ratios of the iron-peak elements in the Perseus cluster. \textit{Nature}. LONDON: NATURE PUBLISHING GROUP, 2017, vol.~551, No~7681, p.~''478''-''+'', 16 pp. ISSN~0028-0836. Available from: https://dx.doi.org/10.1038/nature24301.

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