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

Hitomi Collaboration

Research output: Contribution to journalArticle

13 Citations (Scopus)

Abstract

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- A nd sub-Chandrasekhar-mass type Ia supernova systems, adding to the mounting evidence that both progenitor types make a substantial contribution to cosmic chemical enrichment.

Original languageEnglish
Pages (from-to)478-480
Number of pages3
JournalNature
Volume551
Issue number7681
DOIs
Publication statusPublished - 23-11-2017

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supernovae
iron
manganese
chromium
nickel
sun
heavy elements
high temperature plasmas
mounting
nuclear fusion
spectroscopy
explosions
x rays
galaxies
high resolution
photons
metals
energy

All Science Journal Classification (ASJC) codes

  • General

Cite this

Hitomi Collaboration. / Solar abundance ratios of the iron-peak elements in the Perseus cluster. In: Nature. 2017 ; Vol. 551, No. 7681. pp. 478-480.
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abstract = "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- A nd sub-Chandrasekhar-mass type Ia supernova systems, adding to the mounting evidence that both progenitor types make a substantial contribution to cosmic chemical enrichment.",
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Solar abundance ratios of the iron-peak elements in the Perseus cluster. / Hitomi Collaboration.

In: Nature, Vol. 551, No. 7681, 23.11.2017, p. 478-480.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Solar abundance ratios of the iron-peak elements in the Perseus cluster

AU - Hitomi Collaboration

AU - Aharonian, Felix

AU - Akamatsu, Hiroki

AU - Akimoto, Fumie

AU - Allen, Steven W.

AU - Angelini, Lorella

AU - Audard, Marc

AU - Awaki, Hisamitsu

AU - Axelsson, Magnus

AU - Bamba, Aya

AU - Bautz, Marshall W.

AU - Blandford, Roger

AU - Brenneman, Laura W.

AU - Brown, Gregory V.

AU - Bulbul, Esra

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AU - Chernyakova, Maria

AU - Chiao, Meng P.

AU - Coppi, Paolo S.

AU - Costantini, Elisa

AU - De Plaa, Jelle

AU - Den Herder, Jan Willem

AU - Done, Chris

AU - Dotani, Tadayasu

AU - Ebisawa, Ken

AU - Eckart, Megan E.

AU - Enoto, Teruaki

AU - Ezoe, Yuichiro

AU - Fabian, Andrew C.

AU - Ferrigno, Carlo

AU - Foster, Adam R.

AU - Fujimoto, Ryuichi

AU - Fukazawa, Yasushi

AU - Furuzawa, Akihiro

AU - Galeazzi, Massimiliano

AU - Gallo, Luigi C.

AU - Furuzawa, Akihiro

AU - Giustini, Margherita

AU - Goldwurm, Andrea

AU - Gu, Liyi

AU - Guainazzi, Matteo

AU - Haba, Yoshito

AU - Hagino, Kouichi

AU - Hamaguchi, Kenji

AU - Harrus, Ilana M.

AU - Hatsukade, Isamu

AU - Hayashi, Katsuhiro

AU - Hayashi, Takayuki

AU - Hayashida, Kiyoshi

AU - Hiraga, Junko S.

AU - Hornschemeier, Ann

PY - 2017/11/23

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N2 - 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- A nd sub-Chandrasekhar-mass type Ia supernova systems, adding to the mounting evidence that both progenitor types make a substantial contribution to cosmic chemical enrichment.

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