A data-driven model using UV luminosity functions and halo accretion matching predicts star formation efficiencies peaking at 0.8-0.9 at z>9, with bursty formation and the need for variable IMF or dust to avoid unphysical values.
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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.
SHARP on the E-ELT is proposed to enable spatially resolved IMF measurements in high-redshift ETGs to test time-dependent IMF evolution scenarios.
citing papers explorer
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How galaxies acquire their stellar mass at high redshift: High star formation efficiencies and the relative roles of dust and initial mass function
A data-driven model using UV luminosity functions and halo accretion matching predicts star formation efficiencies peaking at 0.8-0.9 at z>9, with bursty formation and the need for variable IMF or dust to avoid unphysical values.
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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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Probing IMF Variations in High-Redshift Early-Type Galaxies with SHARP
SHARP on the E-ELT is proposed to enable spatially resolved IMF measurements in high-redshift ETGs to test time-dependent IMF evolution scenarios.