Using 1000 mock realizations matched to the ASPIRE survey, the authors find cosmic variance increases clustering errors by ~3x over Poisson estimates and widens minimum halo mass uncertainties by 1.5-3x for z~6 quasars and emission-line galaxies.
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5 Pith papers cite this work. Polarity classification is still indexing.
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Pith papers citing it
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2026 5representative citing papers
Simulation comparison finds bulgeless galaxies host more centrally concentrated, disc-aligned satellites with steeper faint-end luminosity functions than bulge-dominated controls, reflecting co-evolution and quieter merger histories.
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.
citing papers explorer
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The Impact of Cosmic Variance and Satellites on JWST Clustering Measurements at Redshift around 6
Using 1000 mock realizations matched to the ASPIRE survey, the authors find cosmic variance increases clustering errors by ~3x over Poisson estimates and widens minimum halo mass uncertainties by 1.5-3x for z~6 quasars and emission-line galaxies.
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Bulgeless Evolution And the Rise of Discs (BEARD) III. A numerical simulation view of satellites around Milky-Way analogues
Simulation comparison finds bulgeless galaxies host more centrally concentrated, disc-aligned satellites with steeper faint-end luminosity functions than bulge-dominated controls, reflecting co-evolution and quieter merger histories.
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The galaxy ultraviolet luminosity function from $z=7$ to $15$ in the COLIBRE simulations
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.
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Galaxy luminosity functions from far-UV to submillimetre at $z=0$ in the COLIBRE simulations
COLIBRE simulations with SKIRT post-processing match observed galaxy luminosity functions from FUV to submm at z=0, except underpredicting bright mid-IR galaxies.
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The morphologies of present-day galaxies in the COLIBRE simulations
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.