A new histogram-free likelihood method applied to simulated JWST observations of brown dwarfs shows that globular cluster ages can be determined with formal errors under 0.2 Gyr.
A., et al., 2018, @doi [Proceedings of the Royal Society of London Series A] 10.1098/rspa.2017.0616 , https://ui.adsabs.harvard.edu/abs/2018RSPSA.47470616F 474, 20170616
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Milky Way globular clusters formed with initial half-mass densities of ~10^6.4 M_sun/pc^3, bottom-light IMFs, and small present-day black hole mass fractions, inferred by coupling rapid evolution models with multimass equilibrium models fitted to present-day observations.
Baryonic fraction in certain galaxies correlates with baryonic acceleration as approximately a_bar inverse, placing known dark-matter-deficient galaxies at the high-acceleration extreme and predicting low dark matter content for ultra-diffuse galaxies brighter than 25 mag arcsec^{-2}.
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 clusters.
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New SBF distance confirms NGC5846_UDG1 lies in the NGC 5846 group and reconciles prior GC counts to ~50 members, supporting a massive dark matter halo.
GaiaNIR retains sensitivity to extended dark matter halos in globular clusters under strong extinction while Gaia degrades, enabling studies in obscured regions.
Globular cluster deficits in several Coma galaxies, revealed by Voronoi density maps and asymmetry tests, provide evidence for environmental stripping.
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