JWST and ALMA data provide the earliest direct evidence of ram-pressure stripping in a post-starburst galaxy at z=3.06, implying the process can quench star formation in nascent groups at z>3.
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Anisotropic quenching is detected at the highest redshift yet and linked to preprocessing dominating over intrahalo effects by ~20% along the major axis in a delay-then-rapid quenching model informed by cluster accretion histories.
ALMA and JWST data reveal an extreme ram-pressure stripping event removing most cold gas from a massive galaxy in a z=4.3 protocluster core.
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.
Multi-phase observations of NGC 1427A indicate tidal torquing from a dwarf fly-by has pre-conditioned its gas for ram-pressure stripping by the Fornax intracluster medium, placing the galaxy at the onset of environmental quenching with a declining star formation rate.
JWST observations of high-redshift galaxies show no evolution in dust geometry to z~2.4 and yield an empirical calibration linking resolved differential reddening to SFR surface density.
Low-mass filament galaxies in TNG50 exhibit smaller asymmetric cold gas discs due to cosmic web tidal fields causing altered accretion or starvation and late-time stripping, while integrated stellar and halo properties remain similar to field counterparts after mass and environment controls.
Analysis of 3 million HSC galaxies finds that galaxy bulge-to-total ratio depends on environment at fixed stellar mass, with the strength and scale of this dependence varying by redshift and galaxy mass.
ALMA observations of five DSFGs in the Spiderweb protocluster reveal disturbed molecular gas kinematics, field-like gas fractions that are lower in massive/AGN hosts, and declining gas content and sSFR with proximity to the central galaxy.
The SFR-M_* relation develops a high-mass decline at low redshifts, driven mainly by morphological quenching from internal structure rather than environmental effects on star-forming galaxies.
MAUVE-MUSE finds Virgo cluster disks have elevated [N II]/Hα, [S II]/Hα and [O III]/Hβ ratios plus broader kinematics because star formation is suppressed, leaving diffuse ionized gas dominant instead of widespread direct environmental excitation.
High-mass quiescent galaxies in clusters assemble more luminous stellar halos than field galaxies while low-mass cluster galaxies assemble less luminous ones over 0.1 < z < 1.