A score-based diffusion generative model on deep infrared galaxy photometry yields a star formation rate density peaking at z=1.3 and shows distinct non-parametric star formation histories plus AGN activity peaking during the quenching transition of massive galaxies.
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Direct Te-based metallicities at z≈10 are 3× lower than at z=0-3, extending the gradual FMR offset and pointing to pristine gas inflows during early galaxy assembly.
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.
Upper limits on the cosmic abundance of Kardashev Type III radio-broadcasting populations are set at less than one per 10^17 stars using radio source counts and commensal SETI field limits.
citing papers explorer
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pop-cosmos: Star formation over 12 Gyr from generative modelling of a deep infrared-selected galaxy catalogue
A score-based diffusion generative model on deep infrared galaxy photometry yields a star formation rate density peaking at z=1.3 and shows distinct non-parametric star formation histories plus AGN activity peaking during the quenching transition of massive galaxies.
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Novel $z\sim~10$ auroral line measurements extend the gradual offset of the FMR deep into the first Gyr of cosmic time
Direct Te-based metallicities at z≈10 are 3× lower than at z=0-3, extending the gradual FMR offset and pointing to pristine gas inflows during early galaxy assembly.
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The evolution of the galaxy stellar mass function and star formation rates in the COLIBRE simulations from redshift 17 to 0
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.
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Artificial Broadcasts as Galactic Populations: III. Constraints on Radio Broadcasts from the Cosmic Population of Inhabited Galaxies
Upper limits on the cosmic abundance of Kardashev Type III radio-broadcasting populations are set at less than one per 10^17 stars using radio source counts and commensal SETI field limits.