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Enrichment of the Hot Intracluster Medium: Observations

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Abstract

Four decades ago, the firm detection of an Fe-K emission feature in the X-ray spectrum of the Perseus cluster revealed the presence of iron in its hot intracluster medium (ICM). With more advanced missions successfully launched over the last 20 years, this discovery has been extended to many other metals and to the hot atmospheres of many other galaxy clusters, groups, and giant elliptical galaxies, as evidence that the elemental bricks of life—synthesized by stars and supernovae—are also found at the largest scales of the Universe. Because the ICM, emitting in X-rays, is in collisional ionisation equilibrium, its elemental abundances can in principle be accurately measured. These abundance measurements, in turn, are valuable to constrain the physics and environmental conditions of the Type Ia and core-collapse supernovae that exploded and enriched the ICM over the entire cluster volume. On the other hand, the spatial distribution of metals across the ICM constitutes a remarkable signature of the chemical history and evolution of clusters, groups, and ellipticals. Here, we summarise the most significant achievements in measuring elemental abundances in the ICM, from the very first attempts up to the era of XMM-Newton, Chandra, and Suzaku and the unprecedented results obtained by Hitomi. We also discuss the current systematic limitations of these measurements and how the future missions XRISM and Athena will further improve our current knowledge of the ICM enrichment.

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Notes

  1. Formally, “ICM” should be restricted to the hot gas pervading galaxy clusters only. For convenience, however, in the following we use this acronym to designate also the hot atmospheres pervading galaxy groups and isolated, massive ellipticals.

  2. http://www.atomdb.org.

  3. https://www.sron.nl/astrophysics-spex.

  4. Cool-core clusters are usually characterised by a centrally peaked surface brightness, together with a stratified ICM entropy and a cooling time that is shorter than the Hubble time (Molendi and Pizzolato 2001).

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Acknowledgements

We thank the anonymous referee for his/her valuable comments which helped to improve this review. This work was supported by the Lendület LP2016-11 grant awarded by the Hungarian Academy of Sciences. P.M. acknowledges support from Russian Science Foundation (grant 14-22-00271). A.S. is grateful for the support from the Women In Science Excel (WISE) programme of the NWO, and thanks the Kavli Institute for the Physics and Mathematics of the Universe for their continued hospitality. S.E. acknowledges financial contribution from the contracts NARO15 ASI-INAF I/037/12/0, ASI 2015-046-R.0 and ASI-INAF n.2017-14-H.0. SRON is supported financially by NWO, the Netherlands Organization for Scientific Research.

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Authors and Affiliations

  1. Lendület Hot Universe Research Group, MTA-Eötvös University, Pázmány Péter sétány 1/A, Budapest, 1117, Hungary

    F. Mernier & N. Werner

  2. Institute of Physics, Eötvös University, Pázmány Péter sétány 1/A, Budapest, 1117, Hungary

    F. Mernier

  3. SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA, Utrecht, The Netherlands

    F. Mernier, A. Simionescu, J. S. Kaastra, J. de Plaa & L. Gu

  4. Physics Department, Astronomy Unit, Trieste University, v. Tiepolo 11, 34143, Trieste, Italy

    V. Biffi

  5. Observatory of Trieste, INAF, v. Tiepolo 11, 34143, Trieste, Italy

    V. Biffi

  6. Institute of Space and Astronautical Science (ISAS), JAXA, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa, 252-5210, Japan

    H. Yamaguchi & A. Simionescu

  7. Space Research Institute of the Russian Academy of Sciences (IKI), 84/32 Profsoyuznaya Str., Moscow, 117997, Russia

    P. Medvedev

  8. Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, Kashiwa, Chiba, 277-8583, Japan

    A. Simionescu

  9. Osservatorio di Astrofisica e Scienza dello Spazio, INAF, via Pietro Gobetti 93/3, 40129, Bologna, Italy

    S. Ettori

  10. Sezione di Bologna, INFN, viale Berti Pichat 6/2, 40127, Bologna, Italy

    S. Ettori

  11. Department of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University, Kotlářská 2, Brno, 611 37, Czech Republic

    N. Werner

  12. School of Science, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, 739-8526, Japan

    N. Werner

  13. Leiden Observatory, Leiden University, PO Box 9513, 2300 RA, Leiden, The Netherlands

    J. S. Kaastra

  14. High Energy Astrophysics Laboratory, RIKEN, 2-1 Hirosawa, Wako, Saitama, 351-0198, Japan

    L. Gu

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  1. F. Mernier
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Clusters of Galaxies: Physics and Cosmology

Edited by Andrei Bykov, Jelle Kaastra, Marcus Brüggen, Maxim Markevitch, Maurizio Falanga and Frederik Bernard Stefan Paerels

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Mernier, F., Biffi, V., Yamaguchi, H. et al. Enrichment of the Hot Intracluster Medium: Observations. Space Sci Rev 214, 129 (2018). https://doi.org/10.1007/s11214-018-0565-7

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