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.
Title resolution pending
26 Pith papers cite this work. Polarity classification is still indexing.
26
Pith papers citing it
representative citing papers
Using 1000 mock realizations matched to the ASPIRE survey, the authors find cosmic variance increases clustering errors by ~3x over Poisson estimates and widens minimum halo mass uncertainties by 1.5-3x for z~6 quasars and emission-line galaxies.
The satellite metallicity enhancement profile around clusters declines steeply in the core, plateaus near the virial radius due to enriched inflow, and declines further out, with mass loss and quenching dominating the core.
JWST observations identify all massive young embedded star clusters in the Antennae, revealing they are extremely young, heavily obscured, and account for ~60% of the ionizing luminosity.
A JWST census detects neutral ISM absorption in 76 of 309 galaxies at 0.6<z<4 and outflows in 26, indicating AGN-driven neutral outflows dominate in quiescent systems at cosmic noon.
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.
Post-starburst galaxies show compact morphologies with minimal wavelength-dependent structural change and low overall disturbance levels, except for enhanced residual asymmetry in massive systems at z > 1, supporting two distinct quenching pathways.
Morphology-density and morphology-mass relations are present at z~1.6 in both cluster and field galaxies.
In 37 massive ETGs, the IMF becomes less bottom-heavy with radius, with average α_IMF falling from 2.16 to 1.74 and IMF gradients dominating M/L variations over stellar population effects.
NEFERTITI simulations show that the Milky Way's most metal-poor stars largely come from a handful of accreted massive dwarf galaxies, while reproducing the JWST Hebe galaxy at z~11 as a pure Population III system.
Black hole occupation fraction rises with stellar mass but its normalization, shape, and redshift trend depend strongly on BH mass threshold, central vs satellite galaxies, simulation box, resolution, and sampled population in the FEGA25 model.
JWST MIRI observations of post-starburst galaxies find no mid-IR excess in high-mass systems, constraining hidden AGN to Eddington ratios below 1 percent, with low-mass systems showing residual star formation instead.
Simulations show observationally selected protocluster candidates at z ≳ 5 include significant interlopers, undergo 2-6 major mergers, and exhibit stronger clustering than observed, requiring total galaxy mass within 10 cMpc for reliable progenitor identification.
Barred galaxies transition from actively star-forming at z~1-2 to quiescent at z~0, with the fraction of quiescent galaxies hosting bars increasing steeply over cosmic time.
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.
In TNG50, compact dwarf satellites (log M_star 8.4-9.2) form via DM-rich gas inflows in low-merger environments, tidal stripping for DM-poor cases, and ram-pressure starbursts for some metal-rich ones.
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.
ATTILA tool identifies 24 new ultra-diffuse galaxies in Hydra I, doubling the known population to 48, plus 92 additional low surface brightness galaxies, while recovering over 80% of previously known ones.
Stacking analysis shows mean SFR in massive galaxies at 2<z<4.5 declines along the Hubble sequence from ~280 M⊙/yr in irregulars to ~80 M⊙/yr in spheroids, with a simple chemical evolution model explaining the rise in dust-to-stellar mass ratio out to z~8.
Multiple galaxy formation simulations show that low-mass quenched galaxies at z>3 are predominantly environmentally quenched satellites, often only temporarily so, and match JWST observations.
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.
Massive quiescent galaxies at high redshifts show elevated fractions in small-scale overdensities, indicating environmental quenching via galaxy interactions plays a major role.
Simulations constrain the mass scale for efficient ISM stripping of dwarf satellites to M_star ≲ 10^7 M_sun in MW-like halos, 0.5-1 dex below observed values, indicating additional quenching mechanisms are needed.
Composite cluster stellar mass functions show marginal M* evolution at high z and a factor of 2.5 growth in stellar mass fraction from z=0.8 to 0.2 after accounting for halo mass growth.
citing papers explorer
-
Anisotropic quenching beyond $z=1$ and its implications for preprocessing around high-redshift galaxy clusters
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.
-
The Impact of Cosmic Variance and Satellites on JWST Clustering Measurements at Redshift around 6
Using 1000 mock realizations matched to the ASPIRE survey, the authors find cosmic variance increases clustering errors by ~3x over Poisson estimates and widens minimum halo mass uncertainties by 1.5-3x for z~6 quasars and emission-line galaxies.
-
Satellite Metallicity Enhancement I: Suppressed Star Formation, Stellar Mass Loss, and Enriched Inflow of DESI and EAGLE Galaxies around Massive Clusters
The satellite metallicity enhancement profile around clusters declines steeply in the core, plateaus near the virial radius due to enriched inflow, and declines further out, with mass loss and quenching dominating the core.
-
Nowhere Left to Hide: Uncovering All of the Massive Young Embedded Star Clusters in the Antennae with JWST
JWST observations identify all massive young embedded star clusters in the Antennae, revealing they are extremely young, heavily obscured, and account for ~60% of the ionizing luminosity.
-
A Census of Na D-traced neutral ISM and outflows at $0.6<z<4$
A JWST census detects neutral ISM absorption in 76 of 309 galaxies at 0.6<z<4 and outflows in 26, indicating AGN-driven neutral outflows dominate in quiescent systems at cosmic noon.
-
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.
-
The multiwavelength structure of post-starburst galaxies at 0.5 < z < 3 with JWST PRIMER: compact morphologies and residual disturbances
Post-starburst galaxies show compact morphologies with minimal wavelength-dependent structural change and low overall disturbance levels, except for enhanced residual asymmetry in massive systems at z > 1, supporting two distinct quenching pathways.
-
Cluster vs Field: Clear Evidence for a Morphology-Density Relation in All Environments at $z\sim1.6$
Morphology-density and morphology-mass relations are present at z~1.6 in both cluster and field galaxies.
-
The MASSIVE SURVEY XXI: Local Variations in the Stellar Initial Mass Function of MASSIVE Early-Type Galaxies
In 37 massive ETGs, the IMF becomes less bottom-heavy with radius, with average α_IMF falling from 2.16 to 1.74 and IMF gradients dominating M/L variations over stellar population effects.
-
NEFERTITI: Linking early galaxy formation to the assembly of the Milky Way
NEFERTITI simulations show that the Milky Way's most metal-poor stars largely come from a handful of accreted massive dwarf galaxies, while reproducing the JWST Hebe galaxy at z~11 as a pure Population III system.
-
Black Hole Occupation Fraction: Dependence on Black Hole Mass Threshold, Environment, Resolution and Redshift
Black hole occupation fraction rises with stellar mass but its normalization, shape, and redshift trend depend strongly on BH mass threshold, central vs satellite galaxies, simulation box, resolution, and sampled population in the FEGA25 model.
-
No hidden monsters: Probing recently-quenched galaxies for obscured AGN with JWST-PRIMER MIRI and NIRCam
JWST MIRI observations of post-starburst galaxies find no mid-IR excess in high-mass systems, constraining hidden AGN to Eddington ratios below 1 percent, with low-mass systems showing residual star formation instead.
-
On the later evolution of observationally selected protocluster candidates at $z\,{\gtrsim}\,5$
Simulations show observationally selected protocluster candidates at z ≳ 5 include significant interlopers, undergo 2-6 major mergers, and exhibit stronger clustering than observed, requiring total galaxy mass within 10 cMpc for reliable progenitor identification.
-
Exploring the Relationship Between Bars, Star Formation Activity, and Host Galaxy Properties from $\mathbf{z \sim 0}$ to $\mathbf{z \sim 2}$
Barred galaxies transition from actively star-forming at z~1-2 to quiescent at z~0, with the fraction of quiescent galaxies hosting bars increasing steeply over cosmic time.
-
Spatially Resolved Nebular-Stellar Reddening with JWST/NIRISS
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.
-
Satellite compaction pathways: environmental drivers shaping dwarf galaxy corpulence in the TNG50 simulation
In TNG50, compact dwarf satellites (log M_star 8.4-9.2) form via DM-rich gas inflows in low-merger environments, tidal stripping for DM-poor cases, and ram-pressure starbursts for some metal-rich ones.
-
Cosmic web stripping and starvation of low-mass filament galaxies in TNG50
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.
-
Advancing the detection of low surface brightness galaxies. I. ATTILA: multi-tAsking deTecTIon tool for Lsb gAlaxies
ATTILA tool identifies 24 new ultra-diffuse galaxies in Hydra I, doubling the known population to 48, plus 92 additional low surface brightness galaxies, while recovering over 80% of previously known ones.
-
COSMOS-Web: Star formation along the early Hubble sequence and the evolution of dust over the redshift range 0<z<12
Stacking analysis shows mean SFR in massive galaxies at 2<z<4.5 declines along the Hubble sequence from ~280 M⊙/yr in irregulars to ~80 M⊙/yr in spheroids, with a simple chemical evolution model explaining the rise in dust-to-stellar mass ratio out to z~8.
-
Environmental Quenching of High-Redshift Galaxies: Interpreting JWST Observations with Simulations
Multiple galaxy formation simulations show that low-mass quenched galaxies at z>3 are predominantly environmentally quenched satellites, often only temporarily so, and match JWST observations.
-
The Evolution of the SFR-M_* relation at 0.1<z<4: Environmental and Morphological Dependencies
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.
-
The role of small-scale environments in the quenching of massive galaxies at $1<z<5$
Massive quiescent galaxies at high redshifts show elevated fractions in small-scale overdensities, indicating environmental quenching via galaxy interactions plays a major role.
-
Too Big to Quench? I. Constraining ISM Stripping of Dwarf Satellites in Milky Way-like Halos
Simulations constrain the mass scale for efficient ISM stripping of dwarf satellites to M_star ≲ 10^7 M_sun in MW-like halos, 0.5-1 dex below observed values, indicating additional quenching mechanisms are needed.
-
The Atacama Cosmology Telescope: stellar mass growth in massive galaxy clusters from DR5 over the past 7 billion years
Composite cluster stellar mass functions show marginal M* evolution at high z and a factor of 2.5 growth in stellar mass fraction from z=0.8 to 0.2 after accounting for halo mass growth.
-
The Role of Cluster Environments in Quiescent Galaxy Stellar Halo Assembly
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.
-
Resolved HI and Environmental Dynamics
SKA-mid AA4 will enable deep, spatially resolved HI imaging over hundreds of square degrees at column densities down to 10^18 cm^{-2} to study environmental gas processes from isolated galaxies to clusters.