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.
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9 Pith papers cite this work, alongside 671 external citations. Polarity classification is still indexing.
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Pith papers citing it
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representative citing papers
Spectroscopic measurements confirm a tight 6D phase-space clump of four RGB stars as part of the distant southern spur of the Sagittarius stream, likely stripped from Sagittarius's halo in the earliest interaction phases.
300S stellar stream exhibits three density peaks, smooth width variations, a possible 4.7 degree gap, and a kink modeled as resulting from Large Magellanic Cloud interaction across its full known footprint.
Accretion laws with super-linear mass dependence produce divergent population evolution that broadens compact-object mass distributions and drives binary mass ratios toward unity, providing a pathway to massive gravitational-wave sources.
Ages inferred for red giant stars via machine learning are generally insensitive to hyperparameters and architecture but somewhat sensitive to training set choice, especially for the oldest, coolest, and lowest-metallicity stars.
New abundance measurements for NGC 6723 align its chemical patterns with other metal-intermediate globular clusters rather than indicating a transition to metal-rich properties.
N-body simulations show that mutual interactions between Terzan 2, 4, and 5 raise mass-loss rates for the smaller clusters and drive prolate deformations absent in isolated runs.
Apparent sodium spread in NGC 188 is attributed to measurement uncertainties of 0.16 dex rather than multiple populations.
A review of theoretical models for the first stars and observational strategies including JWST searches, near-field studies, and lensing, noting growing candidates and narrowing parameter space.
citing papers explorer
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Fast Dynamical Modelling of Milky Way Globular Clusters -- I. Implications for Initial Cluster Densities
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.
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Tracing the very early disruption of the Sagittarius dwarf galaxy in the distant Milky Way halo
Spectroscopic measurements confirm a tight 6D phase-space clump of four RGB stars as part of the distant southern spur of the Sagittarius stream, likely stripped from Sagittarius's halo in the earliest interaction phases.
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Sifting for a Stream: The Morphology of the $300S$ Stellar Stream
300S stellar stream exhibits three density peaks, smooth width variations, a possible 4.7 degree gap, and a kink modeled as resulting from Large Magellanic Cloud interaction across its full known footprint.
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Accretion-Driven Evolution of Compact-Object Populations in Gas-Rich Environments and the Origin of Massive Gravitational-Wave Sources
Accretion laws with super-linear mass dependence produce divergent population evolution that broadens compact-object mass distributions and drives binary mass ratios toward unity, providing a pathway to massive gravitational-wave sources.
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Evaluating the Sensitivity of the Age Inferences of Red Giant Stars to Machine Learning Methodology
Ages inferred for red giant stars via machine learning are generally insensitive to hyperparameters and architecture but somewhat sensitive to training set choice, especially for the oldest, coolest, and lowest-metallicity stars.
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Chemical abundances in the metal-intermediate GC NGC 6723
New abundance measurements for NGC 6723 align its chemical patterns with other metal-intermediate globular clusters rather than indicating a transition to metal-rich properties.
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Dynamical evolution of Milky Way globular clusters on the cosmological timescale II. Terzan 2, 4, and 5 mass loss and collision tracking
N-body simulations show that mutual interactions between Terzan 2, 4, and 5 raise mass-loss rates for the smaller clusters and drive prolate deformations absent in isolated runs.
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On the APOGEE DR14 sodium spread in the Galactic open cluster NGC 188
Apparent sodium spread in NGC 188 is attributed to measurement uncertainties of 0.16 dex rather than multiple populations.
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How can we finally see the first light? Status and perspective in the search for Population III stars
A review of theoretical models for the first stars and observational strategies including JWST searches, near-field studies, and lensing, noting growing candidates and narrowing parameter space.