Simulation study proposes that weakly rotating, gas-rich cosmic wallflowers at high redshift are natural proto-globular cluster candidates based on kinematics and densities.
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Stellar streams encode the initial mass function of globular clusters, recovered as a declining power-law with slope 1.3 for streams above 1000 solar masses.
AuriGLOBES is a new subgrid model implemented in Auriga simulations that incorporates compressive tides and compact-object mass loss to transform an initial Schechter mass function into observed globular cluster populations while reproducing the GC system mass-halo mass relation.
Disrupted dense star clusters release ~300,000 white dwarf, 150,000 black hole, and 1,000 neutron star binaries into the Milky Way, but Gaia DR3/DR4 detect only a handful of white dwarf systems with none for the others.
FIRE-3 cosmological simulations of Seyfert galaxies produce episodic AGN feedback and gas clearing but no clear anti-correlation between nuclear gas concentration and AGN luminosity, highlighting timing mismatches with observations.
Globular cluster mass fractions, in-situ fractions, metallicity spreads, and spatial profiles in simulated compact galaxies can identify massive relic analogs with early assembly histories.
N-body models of young and old dense star clusters show BBH mergers span primary masses from ~6 to >100 solar masses with a peak near 8 solar masses, reproducing the LIGO-inferred distribution, with low-mass mergers mostly from metal-rich clusters.
Overview of HI modeling methods finds consistency in cosmic HI density but systematic differences in HI-halo mass relation shape and redshift evolution.
Review of state-of-the-art cosmological galaxy formation models for HI, molecular gas and radio continuum in preparation for SKA, advocating coordinated multi-scale simulations, forward modelling and AI emulators.
citing papers explorer
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Mass Distribution of Binary Black Hole Mergers from Young and Old Dense Star Clusters
N-body models of young and old dense star clusters show BBH mergers span primary masses from ~6 to >100 solar masses with a peak near 8 solar masses, reproducing the LIGO-inferred distribution, with low-mass mergers mostly from metal-rich clusters.