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Resolving Globular Cluster Formation within a Cosmological Context
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We place constraints on the formation redshifts for blue globular clusters (BGCs), independent of the details of hydrodynamics and population III star formation. The observed radial distribution of BGCs in the Milky Way Galaxy suggests that they formed in biased dark matter halos at high redshift. As a result, simulations of a ~1 Mpc box up to z~10 must resolve BGC formation in LCDM. We find that most halo stars could be produced from destroyed BGCs and other low-mass clusters that formed at high redshift. We present a proof-of-concept simulation that captures the formation of globular-like star clusters.
Forward citations
Cited by 2 Pith papers
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Too shy to spin? Cosmic wallflowers as proto-globular clusters
Star clusters forming in cosmic filaments at z≈7.6 are systematically slow rotators, and a gas-rich subset overlaps the kinematic and density locus of Milky Way globular clusters, making them plausible proto-globular ...
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The Formation of Globular Clusters
Globular clusters are best understood as the surviving remnants of ordinary, high-pressure star formation in high-redshift galaxies.
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