Globular cluster formation and evolution in the context of cosmological galaxy assembly: open questions
We discuss some of the key open questions regarding the formation and evolution of globular clusters (GCs) during galaxy formation and assembly within a cosmological framework. The current state-of-the-art for both observations and simulations is described, and we briefly mention directions for futu...
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| Main Authors: | , |
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| Format: | Article (Journal) Chapter/Article |
| Language: | English |
| Published: |
Version v2
2018
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| In: |
Arxiv
Year: 2018, Pages: 1-28 |
| DOI: | 10.48550/arXiv.1801.05818 |
| Online Access: | Resolving-System, kostenfrei, Volltext: https://doi.org/10.48550/arXiv.1801.05818 Verlag, kostenfrei, Volltext: http://arxiv.org/abs/1801.05818 
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| Author Notes: | Duncan A. Forbes, Nate Bastian, Mark Gieles, Robert A. Crain, J.M. Diederik Kruijssen, Søren S. Larsen, Sylvia Ploeckinger, Oscar Agertz, Michele Trenti, Annette M.N. Ferguson, Joel Pfeffer, Oleg Y. Gnedin |
MARC
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| 520 | |a We discuss some of the key open questions regarding the formation and evolution of globular clusters (GCs) during galaxy formation and assembly within a cosmological framework. The current state-of-the-art for both observations and simulations is described, and we briefly mention directions for future research. The oldest GCs have ages $\ge$ 12.5 Gyr and formed around the time of reionisation. Resolved colour-magnitude diagrams of Milky Way GCs and direct imaging of lensed proto-GCs at z $\sim$ 6 with JWST promise further insight. Globular clusters are known to host multiple populations of stars with variations in their chemical abundances. Recently, such multiple populations have been detected in $\si |2 Gyr old compact, massive star clusters. This suggests a common, single pathway for the formation of GCs at high and low redshift. The shape of the initial mass function for GCs remains unknown, however for massive galaxies a power-law mass function is favoured. Significant progress has been made recently modelling GC formation in the context of galaxy formation, with success in reproducing many of the observed GC-galaxy scaling relations. | ||
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