Redshift evolution of the hot intracluster gas metallicity in the C-EAGLE cluster simulations. Pearce, F. A., Kay, S. T., Barnes, D. J., Bahe, Y. M., & Bower, R. G. arXiv e-prints, 2005:arXiv:2005.12391, May, 2020. ![Redshift evolution of the hot intracluster gas metallicity in the C-EAGLE cluster simulations [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex The abundance and distribution of metals in galaxy clusters contains valuable information about their chemical history and evolution. By looking at how metallicity evolves with redshift, it is possible to constrain the different metal production channels. We use the C-EAGLE clusters, a sample of 30 high resolution (\$m_\{gas\} {\textbackslash}simeq 1.8{\textbackslash}times 10{\textasciicircum}\{6\}\$ M\$_\{{\textbackslash}odot\}\$) cluster zoom simulations, to investigate the redshift evolution of metallicity, with particular focus on the cluster outskirts. The early enrichment model, in which the majority of metals are produced in the core of cluster progenitors at high redshift, suggests that metals in cluster outskirts have not significantly evolved since \$z=2\$. With the C-EAGLE sample, we find reasonable agreement with the early enrichment model as there is very little scatter in the metallicity abundance at large radius across the whole sample, out to at least \$z=2\$. The exception is Fe for which the radial dependence of metallicity was found to evolve at low redshift as a result of being mainly produced by Type Ia supernovae, which are more likely to be formed at later times than core-collapse supernovae. We also found considerable redshift evolution of metal abundances in the cores of the C-EAGLE clusters which has not been seen in other simulations or observation based metallicity studies. Since we find this evolution to be driven by accretion of low metallicity gas, it suggests that the interaction between outflowing, AGN heated material and the surrounding gas is important for determining the core abundances in clusters.
@article{pearce_redshift_2020,
title = {Redshift evolution of the hot intracluster gas metallicity in the {C}-{EAGLE} cluster simulations},
volume = {2005},
url = {http://adsabs.harvard.edu/abs/2020arXiv200512391P},
abstract = {The abundance and distribution of metals in galaxy clusters contains
valuable information about their chemical history and evolution. By
looking at how metallicity evolves with redshift, it is possible to
constrain the different metal production channels. We use the C-EAGLE
clusters, a sample of 30 high resolution (\$m\_\{gas\} {\textbackslash}simeq 1.8{\textbackslash}times
10{\textasciicircum}\{6\}\$ M\$\_\{{\textbackslash}odot\}\$) cluster zoom simulations, to investigate the
redshift evolution of metallicity, with particular focus on the cluster
outskirts. The early enrichment model, in which the majority of metals
are produced in the core of cluster progenitors at high redshift,
suggests that metals in cluster outskirts have not significantly evolved
since \$z=2\$. With the C-EAGLE sample, we find reasonable agreement with
the early enrichment model as there is very little scatter in the
metallicity abundance at large radius across the whole sample, out to at
least \$z=2\$. The exception is Fe for which the radial dependence of
metallicity was found to evolve at low redshift as a result of being
mainly produced by Type Ia supernovae, which are more likely to be
formed at later times than core-collapse supernovae. We also found
considerable redshift evolution of metal abundances in the cores of the
C-EAGLE clusters which has not been seen in other simulations or
observation based metallicity studies. Since we find this evolution to
be driven by accretion of low metallicity gas, it suggests that the
interaction between outflowing, AGN heated material and the surrounding
gas is important for determining the core abundances in clusters.},
urldate = {2020-06-04},
journal = {arXiv e-prints},
author = {Pearce, Francesca A. and Kay, Scott T. and Barnes, David J. and Bahe, Yannick M. and Bower, Richard G.},
month = may,
year = {2020},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
pages = {arXiv:2005.12391},
}
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We use the C-EAGLE clusters, a sample of 30 high resolution (\\$m_\\{gas\\} {\\textbackslash}simeq 1.8{\\textbackslash}times 10{\\textasciicircum}\\{6\\}\\$ M\\$_\\{{\\textbackslash}odot\\}\\$) cluster zoom simulations, to investigate the redshift evolution of metallicity, with particular focus on the cluster outskirts. The early enrichment model, in which the majority of metals are produced in the core of cluster progenitors at high redshift, suggests that metals in cluster outskirts have not significantly evolved since \\$z=2\\$. With the C-EAGLE sample, we find reasonable agreement with the early enrichment model as there is very little scatter in the metallicity abundance at large radius across the whole sample, out to at least \\$z=2\\$. The exception is Fe for which the radial dependence of metallicity was found to evolve at low redshift as a result of being mainly produced by Type Ia supernovae, which are more likely to be formed at later times than core-collapse supernovae. We also found considerable redshift evolution of metal abundances in the cores of the C-EAGLE clusters which has not been seen in other simulations or observation based metallicity studies. Since we find this evolution to be driven by accretion of low metallicity gas, it suggests that the interaction between outflowing, AGN heated material and the surrounding gas is important for determining the core abundances in clusters.","urldate":"2020-06-04","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Pearce"],"firstnames":["Francesca","A."],"suffixes":[]},{"propositions":[],"lastnames":["Kay"],"firstnames":["Scott","T."],"suffixes":[]},{"propositions":[],"lastnames":["Barnes"],"firstnames":["David","J."],"suffixes":[]},{"propositions":[],"lastnames":["Bahe"],"firstnames":["Yannick","M."],"suffixes":[]},{"propositions":[],"lastnames":["Bower"],"firstnames":["Richard","G."],"suffixes":[]}],"month":"May","year":"2020","keywords":"Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics","pages":"arXiv:2005.12391","bibtex":"@article{pearce_redshift_2020,\n\ttitle = {Redshift evolution of the hot intracluster gas metallicity in the {C}-{EAGLE} cluster simulations},\n\tvolume = {2005},\n\turl = {http://adsabs.harvard.edu/abs/2020arXiv200512391P},\n\tabstract = {The abundance and distribution of metals in galaxy clusters contains \nvaluable information about their chemical history and evolution. By\nlooking at how metallicity evolves with redshift, it is possible to\nconstrain the different metal production channels. We use the C-EAGLE\nclusters, a sample of 30 high resolution (\\$m\\_\\{gas\\} {\\textbackslash}simeq 1.8{\\textbackslash}times\n10{\\textasciicircum}\\{6\\}\\$ M\\$\\_\\{{\\textbackslash}odot\\}\\$) cluster zoom simulations, to investigate the\nredshift evolution of metallicity, with particular focus on the cluster\noutskirts. The early enrichment model, in which the majority of metals\nare produced in the core of cluster progenitors at high redshift,\nsuggests that metals in cluster outskirts have not significantly evolved\nsince \\$z=2\\$. With the C-EAGLE sample, we find reasonable agreement with\nthe early enrichment model as there is very little scatter in the\nmetallicity abundance at large radius across the whole sample, out to at\nleast \\$z=2\\$. The exception is Fe for which the radial dependence of\nmetallicity was found to evolve at low redshift as a result of being\nmainly produced by Type Ia supernovae, which are more likely to be\nformed at later times than core-collapse supernovae. We also found\nconsiderable redshift evolution of metal abundances in the cores of the\nC-EAGLE clusters which has not been seen in other simulations or\nobservation based metallicity studies. Since we find this evolution to\nbe driven by accretion of low metallicity gas, it suggests that the\ninteraction between outflowing, AGN heated material and the surrounding\ngas is important for determining the core abundances in clusters.},\n\turldate = {2020-06-04},\n\tjournal = {arXiv e-prints},\n\tauthor = {Pearce, Francesca A. and Kay, Scott T. and Barnes, David J. and Bahe, Yannick M. and Bower, Richard G.},\n\tmonth = may,\n\tyear = {2020},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},\n\tpages = {arXiv:2005.12391},\n}\n\n","author_short":["Pearce, F. A.","Kay, S. T.","Barnes, D. J.","Bahe, Y. M.","Bower, R. 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