FLAMINGO simulation analysis shows IA amplitude for LRGs depends on halo assembly history and exhibits redshift evolution beyond mass effects, yielding an empirical mass-redshift model.
G., Schaye J., 2022, @doi [ ] 10.1093/mnras/stab3166 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.511.2367B 511
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COLIBRE simulations find the galaxy gas-phase MZR already in place at z≈10 with little evolution until z≈5, then shallowens at low z, with high-mass turnover set by AGN feedback and low-mass end by core-collapse supernovae.
tSZ cross-correlations with large-scale structure tracers prefer low S8 and strong baryonic feedback, yielding S8 = 0.72 and low group baryon fraction in FLAMINGO simulations.
New hydrodynamical simulations show that dwarf galaxy stellar mass-halo mass relations and star formation histories are more influenced by host halo concentration than by the 5 cMpc scale environment.
N-body+hydro simulation of an isolated Milky Way-like galaxy shows bar-spiral reconnections produce episodic star formation bursts in nuclear stellar discs and clusters after the initial bar-driven burst.
COLIBRE simulations underpredict bright-end UV galaxy luminosities by 1 to 2.5 magnitudes at z=7-15 compared with observations, with the discrepancy persisting after dust attenuation and uncertainty accounting.
COLIBRE simulations with SKIRT post-processing match observed galaxy luminosity functions from FUV to submm at z=0, except underpredicting bright mid-IR galaxies.
COLIBRE simulations find kinematic galaxy morphology peaks in rotational support at stellar masses of 1-2 x 10^10 solar masses and correlates more with internal properties like gas richness than with host halo properties.
COLIBRE simulations match observed galaxy stellar mass functions, star formation rates, and quenched fractions from z=17 to z=0, including JWST massive quiescent galaxies at high redshift.
COLIBRE calibrates supernova and AGN feedback parameters in multi-phase ISM cosmological simulations using emulator-based fitting to reproduce the z=0 galaxy stellar mass function and size-stellar mass relation at three resolutions.
Splitting particle structs into access-pattern-based substructs reduces GPU data packing time by 20-40% in SPH simulations.
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Memory Layouts for GPU-Data Transfer Buffering in SPH
Splitting particle structs into access-pattern-based substructs reduces GPU data packing time by 20-40% in SPH simulations.