A census of cool core galaxy clusters in IllustrisTNG. Barnes, D. J., Vogelsberger, M., Kannan, R., Marinacci, F., Weinberger, R., Springel, V., Torrey, P., Pillepich, A., Nelson, D., Pakmor, R., Naiman, J., Hernquist, L., & McDonald, M. arXiv:1710.08420 [astro-ph], October, 2017. arXiv: 1710.08420![A census of cool core galaxy clusters in IllustrisTNG [link]](https://bibbase.org/img/filetypes/link.svg "link")
Paper abstract bibtex The thermodynamic structure of hot gas in galaxy clusters is sensitive to astrophysical processes and typically difficult to model with galaxy formation simulations. We explore the fraction of cool-core (CC) clusters in a large sample of \$370\$ clusters from IllustrisTNG, examining six common CC definitions. IllustrisTNG produces continuous CC criteria distributions, the extremes of which are classified as CC and non-cool-core (NCC), and the criteria are increasingly correlated for more massive clusters. At \$z=0\$ the CC fraction is systematically lower than observed for the complete sample, selecting massive systems increases the CC fraction for \$3\$ criteria and reduces it for others. This result is partly driven by systematic differences between the simulated and observed gas fraction profiles. The simulated CC fraction increases more rapidly with redshift than observed, independent of mass or redshift range, and the CC fraction is overpredicted at \$z{\textbackslash}geq1\$. The conversion of CCs to NCCs begins later and acts more rapidly in the simulations. Examining the fraction of CCs and NCCs defined as relaxed we find no evidence that CCs are more relaxed, suggesting that mergers are not solely responsible for disrupting CCs. A comparison of the median thermodynamic profiles defined by different CC criteria shows that the extent to which they evolve in the cluster core is dependent on the CC criteria. We conclude that the thermodynamic structure of galaxy clusters in IllustrisTNG shares many similarities with observations, but achieving better agreement most likely requires modifications of the underlying galaxy formation model.
@article{barnes_census_2017,
title = {A census of cool core galaxy clusters in {IllustrisTNG}},
url = {http://arxiv.org/abs/1710.08420},
abstract = {The thermodynamic structure of hot gas in galaxy clusters is sensitive to astrophysical processes and typically difficult to model with galaxy formation simulations. We explore the fraction of cool-core (CC) clusters in a large sample of \$370\$ clusters from IllustrisTNG, examining six common CC definitions. IllustrisTNG produces continuous CC criteria distributions, the extremes of which are classified as CC and non-cool-core (NCC), and the criteria are increasingly correlated for more massive clusters. At \$z=0\$ the CC fraction is systematically lower than observed for the complete sample, selecting massive systems increases the CC fraction for \$3\$ criteria and reduces it for others. This result is partly driven by systematic differences between the simulated and observed gas fraction profiles. The simulated CC fraction increases more rapidly with redshift than observed, independent of mass or redshift range, and the CC fraction is overpredicted at \$z{\textbackslash}geq1\$. The conversion of CCs to NCCs begins later and acts more rapidly in the simulations. Examining the fraction of CCs and NCCs defined as relaxed we find no evidence that CCs are more relaxed, suggesting that mergers are not solely responsible for disrupting CCs. A comparison of the median thermodynamic profiles defined by different CC criteria shows that the extent to which they evolve in the cluster core is dependent on the CC criteria. We conclude that the thermodynamic structure of galaxy clusters in IllustrisTNG shares many similarities with observations, but achieving better agreement most likely requires modifications of the underlying galaxy formation model.},
journal = {arXiv:1710.08420 [astro-ph]},
author = {Barnes, David J. and Vogelsberger, Mark and Kannan, Rahul and Marinacci, Federico and Weinberger, Rainer and Springel, Volker and Torrey, Paul and Pillepich, Annalisa and Nelson, Dylan and Pakmor, Rüdiger and Naiman, Jill and Hernquist, Lars and McDonald, Michael},
month = oct,
year = {2017},
note = {arXiv: 1710.08420},
keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
}
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IllustrisTNG produces continuous CC criteria distributions, the extremes of which are classified as CC and non-cool-core (NCC), and the criteria are increasingly correlated for more massive clusters. At \\$z=0\\$ the CC fraction is systematically lower than observed for the complete sample, selecting massive systems increases the CC fraction for \\$3\\$ criteria and reduces it for others. This result is partly driven by systematic differences between the simulated and observed gas fraction profiles. The simulated CC fraction increases more rapidly with redshift than observed, independent of mass or redshift range, and the CC fraction is overpredicted at \\$z{\\textbackslash}geq1\\$. The conversion of CCs to NCCs begins later and acts more rapidly in the simulations. Examining the fraction of CCs and NCCs defined as relaxed we find no evidence that CCs are more relaxed, suggesting that mergers are not solely responsible for disrupting CCs. A comparison of the median thermodynamic profiles defined by different CC criteria shows that the extent to which they evolve in the cluster core is dependent on the CC criteria. 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