The Metal Content of the Hot Atmospheres of Galaxy Groups

Galaxy groups host the majority of matter and more than half of all the galaxies in the Universe. Their hot (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<msup<<mn<10</mn<<mn<7</mn<<...
Ausführliche Beschreibung

Gespeichert in:

Autor*in:	Fabio Gastaldello [verfasserIn] Aurora Simionescu [verfasserIn] Francois Mernier [verfasserIn] Veronica Biffi [verfasserIn] Massimo Gaspari [verfasserIn] Kosuke Sato [verfasserIn] Kyoko Matsushita [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2021

Schlagwörter:	galaxies:abundances galaxies:clusters:intracluster medium X-rays:galaxies

Übergeordnetes Werk:	In: Universe - MDPI AG, 2015, 7(2021), 7, p 208
Übergeordnetes Werk:	volume:7 ; year:2021 ; number:7, p 208

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3390/universe7070208

Katalog-ID:	DOAJ030090792

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allfieldsGer	10.3390/universe7070208 doi (DE-627)DOAJ030090792 (DE-599)DOAJa26b383814d14739bdfe8d8bb377f7bc DE-627 ger DE-627 rakwb eng QC793-793.5 Fabio Gastaldello verfasserin aut The Metal Content of the Hot Atmospheres of Galaxy Groups 2021 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Galaxy groups host the majority of matter and more than half of all the galaxies in the Universe. Their hot (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<msup<<mn<10</mn<<mn<7</mn<</msup<</semantics<</math<</inline-formula< K), X-ray emitting intra-group medium (IGrM) reveals emission lines typical of many elements synthesized by stars and supernovae. Because their gravitational potentials are shallower than those of rich galaxy clusters, groups are ideal targets for studying, through X-ray observations , feedback effects, which leave important marks on their gas and metal contents. Here, we review the history and present status of the chemical abundances in the IGrM probed by X-ray spectroscopy. We discuss the limitations of our current knowledge, in particular due to uncertainties in the modeling of the Fe-L shell by plasma codes, and coverage of the volume beyond the central region. We further summarize the constraints on the abundance pattern at the group mass scale and the insight it provides to the history of chemical enrichment. Parallel to the observational efforts, we review the progress made by both cosmological hydrodynamical simulations and controlled high-resolution 3D simulations to reproduce the radial distribution of metals in the IGrM, the dependence on system mass from group to cluster scales, and the role of AGN and SN feedback in producing the observed phenomenology. Finally, we highlight future prospects in this field, where progress will be driven both by a much richer sample of X-ray emitting groups identified with eROSITA, and by a revolution in the study of X-ray spectra expected from micro-calorimeters onboard XRISM and ATHENA. galaxies:abundances galaxies:clusters:intracluster medium X-rays:galaxies Elementary particle physics Aurora Simionescu verfasserin aut Francois Mernier verfasserin aut Veronica Biffi verfasserin aut Massimo Gaspari verfasserin aut Kosuke Sato verfasserin aut Kyoko Matsushita verfasserin aut In Universe MDPI AG, 2015 7(2021), 7, p 208 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:7 year:2021 number:7, p 208 https://doi.org/10.3390/universe7070208 kostenfrei https://doaj.org/article/a26b383814d14739bdfe8d8bb377f7bc kostenfrei https://www.mdpi.com/2218-1997/7/7/208 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 7 2021 7, p 208
allfieldsSound	10.3390/universe7070208 doi (DE-627)DOAJ030090792 (DE-599)DOAJa26b383814d14739bdfe8d8bb377f7bc DE-627 ger DE-627 rakwb eng QC793-793.5 Fabio Gastaldello verfasserin aut The Metal Content of the Hot Atmospheres of Galaxy Groups 2021 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Galaxy groups host the majority of matter and more than half of all the galaxies in the Universe. Their hot (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<msup<<mn<10</mn<<mn<7</mn<</msup<</semantics<</math<</inline-formula< K), X-ray emitting intra-group medium (IGrM) reveals emission lines typical of many elements synthesized by stars and supernovae. Because their gravitational potentials are shallower than those of rich galaxy clusters, groups are ideal targets for studying, through X-ray observations , feedback effects, which leave important marks on their gas and metal contents. Here, we review the history and present status of the chemical abundances in the IGrM probed by X-ray spectroscopy. We discuss the limitations of our current knowledge, in particular due to uncertainties in the modeling of the Fe-L shell by plasma codes, and coverage of the volume beyond the central region. We further summarize the constraints on the abundance pattern at the group mass scale and the insight it provides to the history of chemical enrichment. Parallel to the observational efforts, we review the progress made by both cosmological hydrodynamical simulations and controlled high-resolution 3D simulations to reproduce the radial distribution of metals in the IGrM, the dependence on system mass from group to cluster scales, and the role of AGN and SN feedback in producing the observed phenomenology. Finally, we highlight future prospects in this field, where progress will be driven both by a much richer sample of X-ray emitting groups identified with eROSITA, and by a revolution in the study of X-ray spectra expected from micro-calorimeters onboard XRISM and ATHENA. galaxies:abundances galaxies:clusters:intracluster medium X-rays:galaxies Elementary particle physics Aurora Simionescu verfasserin aut Francois Mernier verfasserin aut Veronica Biffi verfasserin aut Massimo Gaspari verfasserin aut Kosuke Sato verfasserin aut Kyoko Matsushita verfasserin aut In Universe MDPI AG, 2015 7(2021), 7, p 208 (DE-627)820684236 (DE-600)2813994-X 22181997 nnns volume:7 year:2021 number:7, p 208 https://doi.org/10.3390/universe7070208 kostenfrei https://doaj.org/article/a26b383814d14739bdfe8d8bb377f7bc kostenfrei https://www.mdpi.com/2218-1997/7/7/208 kostenfrei https://doaj.org/toc/2218-1997 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 7 2021 7, p 208
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author	Fabio Gastaldello
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topic	misc QC793-793.5 misc galaxies:abundances misc galaxies:clusters:intracluster medium misc X-rays:galaxies misc Elementary particle physics
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title	The Metal Content of the Hot Atmospheres of Galaxy Groups
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title_auth	The Metal Content of the Hot Atmospheres of Galaxy Groups
abstract	Galaxy groups host the majority of matter and more than half of all the galaxies in the Universe. Their hot (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<msup<<mn<10</mn<<mn<7</mn<</msup<</semantics<</math<</inline-formula< K), X-ray emitting intra-group medium (IGrM) reveals emission lines typical of many elements synthesized by stars and supernovae. Because their gravitational potentials are shallower than those of rich galaxy clusters, groups are ideal targets for studying, through X-ray observations , feedback effects, which leave important marks on their gas and metal contents. Here, we review the history and present status of the chemical abundances in the IGrM probed by X-ray spectroscopy. We discuss the limitations of our current knowledge, in particular due to uncertainties in the modeling of the Fe-L shell by plasma codes, and coverage of the volume beyond the central region. We further summarize the constraints on the abundance pattern at the group mass scale and the insight it provides to the history of chemical enrichment. Parallel to the observational efforts, we review the progress made by both cosmological hydrodynamical simulations and controlled high-resolution 3D simulations to reproduce the radial distribution of metals in the IGrM, the dependence on system mass from group to cluster scales, and the role of AGN and SN feedback in producing the observed phenomenology. Finally, we highlight future prospects in this field, where progress will be driven both by a much richer sample of X-ray emitting groups identified with eROSITA, and by a revolution in the study of X-ray spectra expected from micro-calorimeters onboard XRISM and ATHENA.
abstractGer	Galaxy groups host the majority of matter and more than half of all the galaxies in the Universe. Their hot (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<msup<<mn<10</mn<<mn<7</mn<</msup<</semantics<</math<</inline-formula< K), X-ray emitting intra-group medium (IGrM) reveals emission lines typical of many elements synthesized by stars and supernovae. Because their gravitational potentials are shallower than those of rich galaxy clusters, groups are ideal targets for studying, through X-ray observations , feedback effects, which leave important marks on their gas and metal contents. Here, we review the history and present status of the chemical abundances in the IGrM probed by X-ray spectroscopy. We discuss the limitations of our current knowledge, in particular due to uncertainties in the modeling of the Fe-L shell by plasma codes, and coverage of the volume beyond the central region. We further summarize the constraints on the abundance pattern at the group mass scale and the insight it provides to the history of chemical enrichment. Parallel to the observational efforts, we review the progress made by both cosmological hydrodynamical simulations and controlled high-resolution 3D simulations to reproduce the radial distribution of metals in the IGrM, the dependence on system mass from group to cluster scales, and the role of AGN and SN feedback in producing the observed phenomenology. Finally, we highlight future prospects in this field, where progress will be driven both by a much richer sample of X-ray emitting groups identified with eROSITA, and by a revolution in the study of X-ray spectra expected from micro-calorimeters onboard XRISM and ATHENA.
abstract_unstemmed	Galaxy groups host the majority of matter and more than half of all the galaxies in the Universe. Their hot (<inline-formula<<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"<<semantics<<msup<<mn<10</mn<<mn<7</mn<</msup<</semantics<</math<</inline-formula< K), X-ray emitting intra-group medium (IGrM) reveals emission lines typical of many elements synthesized by stars and supernovae. Because their gravitational potentials are shallower than those of rich galaxy clusters, groups are ideal targets for studying, through X-ray observations , feedback effects, which leave important marks on their gas and metal contents. Here, we review the history and present status of the chemical abundances in the IGrM probed by X-ray spectroscopy. We discuss the limitations of our current knowledge, in particular due to uncertainties in the modeling of the Fe-L shell by plasma codes, and coverage of the volume beyond the central region. We further summarize the constraints on the abundance pattern at the group mass scale and the insight it provides to the history of chemical enrichment. Parallel to the observational efforts, we review the progress made by both cosmological hydrodynamical simulations and controlled high-resolution 3D simulations to reproduce the radial distribution of metals in the IGrM, the dependence on system mass from group to cluster scales, and the role of AGN and SN feedback in producing the observed phenomenology. Finally, we highlight future prospects in this field, where progress will be driven both by a much richer sample of X-ray emitting groups identified with eROSITA, and by a revolution in the study of X-ray spectra expected from micro-calorimeters onboard XRISM and ATHENA.
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title_short	The Metal Content of the Hot Atmospheres of Galaxy Groups
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The Metal Content of the Hot Atmospheres of Galaxy Groups

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