The Shark semi-analytic model, calibrated only to the z~0.1 stellar mass function, reproduces the JWST UV luminosity function at z=6-17, with disk-instability-driven starbursts as the key mechanism.
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Adding the number density of bright sub-millimetre galaxies as a direct MCMC constraint produces calibrated L-Galaxies models that match SMG counts while remaining consistent only with the lower limits of the observed massive quiescent galaxy density.
The TNG SAM reproduces TNG hydro simulation gas and metal flows plus galaxy and halo properties within 30% accuracy out to z=6 via five targeted updates to the Santa Cruz SAM calibrated on stellar feedback-dominated galaxies.
COLIBRE simulations with SKIRT post-processing match observed galaxy luminosity functions from FUV to submm at z=0, except underpredicting bright mid-IR galaxies.
Using high-resolution galaxy simulations, the authors show that the scatter in the IRX-beta relation is dominated by variations in the intrinsic ultraviolet spectral slope, and that the high-redshift infrared excess deficit can be explained by a redshift-dependent dust temperature correction.
citing papers explorer
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Bright star-forming galaxies naturally forming at z>10 in the Shark semi-analytic model
The Shark semi-analytic model, calibrated only to the z~0.1 stellar mass function, reproduces the JWST UV luminosity function at z=6-17, with disk-instability-driven starbursts as the key mechanism.
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Simultaneously Modelling Dusty Star Forming Galaxies and Massive Quiescents: A Calibration Framework for Galaxy Formation Models
Adding the number density of bright sub-millimetre galaxies as a direct MCMC constraint produces calibrated L-Galaxies models that match SMG counts while remaining consistent only with the lower limits of the observed massive quiescent galaxy density.
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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 IRX-$\beta$ relation of high-redshift galaxies
Using high-resolution galaxy simulations, the authors show that the scatter in the IRX-beta relation is dominated by variations in the intrinsic ultraviolet spectral slope, and that the high-redshift infrared excess deficit can be explained by a redshift-dependent dust temperature correction.