JWST observations of absorption lines in z~3 galaxies show inclination-dependent gas flows, with face-on systems exhibiting stronger outflows and inclined systems more inflows.
C., Leja J., Johnson B
11 Pith papers cite this work. Polarity classification is still indexing.
11
Pith papers citing it
representative citing papers
Lumen modeling of IllustrisTNG50 shows that high ionization parameters from massive star clusters plus enhanced nitrogen abundances are needed to reproduce the extreme [OIII]/Hβ, [OIII]/[OII], and [NII]/Hα ratios seen in z>3 galaxies.
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.
Simulation-based inference on the color distribution of z~2 massive galaxies yields a quenched fraction of 0.24 and a quenching timescale distribution with mode 97 Myr and median 182 Myr.
Milky Way abundance trends act as effective empirical proxies for nucleosynthetic yields, recovering alpha and Fe-peak abundances in quiescent galaxies with 0.05 dex median offset versus 0.23 dex for theory, indicating largely universal yields.
Star formation histories inferred for z=2-5 massive quiescent galaxies imply past number densities that align with observed rapid evolution since z~7.
LAEs at z=2.4-4.5 are smaller and more starbursting than typical SFGs, with Lyα strength correlating negatively with size and positively with Sersic index and recent SFR ratio.
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.
Different SED fitting techniques and data types produce stellar parameters and xi_ion values differing by up to 1.1 dex even for a homogeneous sample of z=3 EoR-analog galaxies, with apparent redshift evolution of xi_ion appearing only under consistent methodology.
NIRCam-selected AGN hosts split into a 'bridge' group with moderate-to-low SFRs and a 'branch' group above the SFMS with SFR rising with AGN fraction; both populations show recent transitions between star formation and quiescence.