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Formation and evolution of globular clusters in cosmological simulations

Published online by Cambridge University Press:  11 March 2020

Hui Li Open the ORCID record for Hui Li [Opens in a new window]  and
Oleg Gnedin Open the ORCID record for Oleg Gnedin [Opens in a new window]
Hui Li
Affiliation:
Department of Physics, Kavli Institute for Astrophysics and Space Research, MIT, Cambridge, MA02139, USA email: hliastro@mit.edu
Oleg Gnedin
Affiliation:
Department of Astronomy, University of Michigan, Ann Arbor, MI48109, USA email: ognedin@umich.edu
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Abstract

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In a series of three papers, we introduced a novel cluster formation model that describes the formation, growth, and disruption of star clusters in high-resolution cosmological simulations. We tested this model on a Milky Way-sized galaxy and found that various properties of young massive clusters, such as the mass function and formation efficiency, are consistent with observations in the local universe. Interestingly, most massive clusters – globular cluster candidates – are preferentially formed during major merger events. We follow the dynamical evolution of clusters in the galactic tidal field. Due to tidal disruption, the cluster mass function evolves from initial power law to a peaked shape. The surviving clusters at z = 0 show a broad range of metallicity [Fe/H] from -3 to -0.5. A robust prediction of the model is the age–metallicity relation, in which metal-rich clusters are systematically younger than metal-poor clusters by up to 3 Gyr.

Keywords

methods: numericalglobular clusters: generalgalaxies: evolutiongalacies: star clusters: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S351: Star Clusters: From the Milky Way to the Early Universe , May 2019 , pp. 34 - 39
Copyright
© International Astronomical Union 2020

Footnotes

†

Hui Li is a Hubble fellow.

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