Lumina runs a 500 cMpc radiation-hydrodynamic simulation combining IllustrisTNG galaxy formation with six-bin M1 radiation transport to predict late stellar-driven HI reionization ending around z=4.75 and AGN-driven HeII reionization nearly complete by z=3.
E., Tacchella, S., Johnson, B
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JADES DR5 delivers 2081 z_phot > 8 galaxy candidates with UV slope trends, morphological evidence of clumpy growth, and improved photo-z methods tested on a spectroscopic subsample.
Simulations predict ngVLA at 100 GHz can detect galaxies above 10^9 solar masses at any redshift while SKA low frequencies reach massive dusty galaxies to z=5-7.
Simulations show that bursty supernova feedback produces fewer bright [OIII] emitters by z=5 than smooth feedback due to less effective metal enrichment, while [OIII] traces shock-heated and radiatively ionized gas.
citing papers explorer
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Introducing the Lumina project: large-volume radiation-hydrodynamic simulations of the epochs of hydrogen and helium reionization
Lumina runs a 500 cMpc radiation-hydrodynamic simulation combining IllustrisTNG galaxy formation with six-bin M1 radiation transport to predict late stellar-driven HI reionization ending around z=4.75 and AGN-driven HeII reionization nearly complete by z=3.
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JWST Advanced Deep Extragalactic Survey (JADES) Data Release 5: Photometrically Selected Galaxy Candidates at z > 8
JADES DR5 delivers 2081 z_phot > 8 galaxy candidates with UV slope trends, morphological evidence of clumpy growth, and improved photo-z methods tested on a spectroscopic subsample.
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Prospects for Observing Galaxy Spectral Energy Distribution from the Radio to the far-Infrared in the Era of Next-Generation Radio Telescopes
Simulations predict ngVLA at 100 GHz can detect galaxies above 10^9 solar masses at any redshift while SKA low frequencies reach massive dusty galaxies to z=5-7.
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New constraints on stellar feedback through [O III] emission: interpreting ALMA and JWST observations with SPICE simulations
Simulations show that bursty supernova feedback produces fewer bright [OIII] emitters by z=5 than smooth feedback due to less effective metal enrichment, while [OIII] traces shock-heated and radiatively ionized gas.