MeerKAT observations detect radio halos in 27% of 30 massive clusters at z>1, a rate lower than at intermediate redshifts but above model predictions, with power-mass scaling similar to lower-z samples.
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Extending to wCDM mainly suppresses the leading Planck Fisher eigenvalue to 2.7% of its LambdaCDM value with only modest eigenmode rotation, while late-time data adds curvature that limits tension relief.
tSZ cross-correlations with large-scale structure tracers prefer low S8 and strong baryonic feedback, yielding S8 = 0.72 and low group baryon fraction in FLAMINGO simulations.
Baryonic fraction in certain galaxies correlates with baryonic acceleration as approximately a_bar inverse, placing known dark-matter-deficient galaxies at the high-acceleration extreme and predicting low dark matter content for ultra-diffuse galaxies brighter than 25 mag arcsec^{-2}.
Corrected empirical limits show the most massive galaxies never exceed the theoretical baryonic maximum of 0.16 times halo virial mass, keeping observations consistent with LambdaCDM at all redshifts.
SHAMe-SF modeling of small-scale DESI ELG clustering delivers 6% precision on σ8 and Ωm h², matching full DR1 results with 1% volume.
kSZ measurements constrain the gravitational acceleration between galaxy halos to follow g ∝ 1/r^{2.1±0.3}, consistent with Newtonian gravity in ΛCDM.
BayeSN analysis of ZTF Type Ia supernovae confirms a ~0.1 mag intrinsic environmental step in standardized brightness that is not explained by differences in dust extinction properties.
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.
Restricting analysis to the top 1% most luminous galaxies in GW localization volumes yields 1-4 candidate hosts for three specific events, with 29-36% probability of random association.
A search of repeating FRBs identifies RM flare candidates in FRB 20121102A, FRB 20201124A, and FRB 20180916B, suggesting such events may be common and tied to dynamic magneto-ionic environments.
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.
TNG50 shows most massive high-z star-forming galaxies are dynamically hotter than ALMA data indicate, with rare cold discs forming from aligned accretion and evolving into one-third discs and two-thirds early-type galaxies by z=0.
Simulations find [C II] traces star formation robustly but underestimates outflow speeds and mass-loading factors by factors of 2-5, with feedback type affecting disk settling but not distinguishable from [C II] spatial or spectral properties alone.
Convolutional neural networks can infer galaxy cluster virial masses and scale radii from 2D projected position and line-of-sight velocity distributions with nearly unbiased results and reduced scatter when richness is added or training is limited to relaxed systems.
ASTRID simulation with dust model calibrated to SDSS at z=0 produces validated luminosity functions and LSST-ready mock catalogs of 378 million galaxies with predicted number counts in ugrizy bands from z=0 to 2.
Early kinematically persistent planes of satellite galaxies are fossil remnants of high-redshift anisotropic mass collapse along the principal directions of the local cosmic web during the fast assembly phase of host halos.
A convLSTM classifier identifies lensed SNe Ia in simulated LSST-like time series, reaching ~60% true-positive rate at O(10^{-4}) false-positive rate by the seventh epoch even after adding realistic PSF variations and foreground SN contaminants.
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.
AGN with ultra-fast outflows exhibit larger radio extensions and steeper spectra matching wind-driven shock models, suggesting a link between X-ray winds and radio-emitting outflows.
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.
Updated Planck CMB measurements give ns = 0.9649 ± 0.0042, r < 0.056, confirm flatness at 0.4 percent, and show no evidence for scale-dependent features or non-slow-roll dynamics in the inflaton potential.
The PINK updates enhance the CELEBI FRB pipeline with better astrometry, time-frequency gating, polarization calibration, DM optimization tools, and a software container for improved efficiency and localization of events like FRB 20251019A.
citing papers explorer
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The MeerKAT Massive Distant Clusters Survey: a search for diffuse radio emission in 30 massive SZ-selected clusters at $z > 1$
MeerKAT observations detect radio halos in 27% of 30 massive clusters at z>1, a rate lower than at intermediate redshifts but above model predictions, with power-mass scaling similar to lower-z samples.
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Information-Geometric Perspective on the Hubble Tension: Eigenmode Rotation and Curvature Suppression in wCDM
Extending to wCDM mainly suppresses the leading Planck Fisher eigenvalue to 2.7% of its LambdaCDM value with only modest eigenmode rotation, while late-time data adds curvature that limits tension relief.
-
FLAMINGO: The thermal history of the Universe from tSZ effect cross-correlations and its dependencies on cosmology and baryon physics
tSZ cross-correlations with large-scale structure tracers prefer low S8 and strong baryonic feedback, yielding S8 = 0.72 and low group baryon fraction in FLAMINGO simulations.
-
A correlation predicting galaxies without dark matter
Baryonic fraction in certain galaxies correlates with baryonic acceleration as approximately a_bar inverse, placing known dark-matter-deficient galaxies at the high-acceleration extreme and predicting low dark matter content for ultra-diffuse galaxies brighter than 25 mag arcsec^{-2}.
-
Empirical estimates of how massive galaxies can be in {\Lambda}CDM
Corrected empirical limits show the most massive galaxies never exceed the theoretical baryonic maximum of 0.16 times halo virial mass, keeping observations consistent with LambdaCDM at all redshifts.
-
Cosmological constraints from the small scale clustering of Emission Line Galaxies
SHAMe-SF modeling of small-scale DESI ELG clustering delivers 6% precision on σ8 and Ωm h², matching full DR1 results with 1% volume.
-
The Atacama Cosmology Telescope: A Test of the Gravitational Force Law on Cosmological Scales Using the Kinematic Sunyaev-Zeldovich Effect
kSZ measurements constrain the gravitational acceleration between galaxy halos to follow g ∝ 1/r^{2.1±0.3}, consistent with Newtonian gravity in ΛCDM.
-
On the origin of the environmental step: A BayeSN view of the ZTF SN Ia DR2
BayeSN analysis of ZTF Type Ia supernovae confirms a ~0.1 mag intrinsic environmental step in standardized brightness that is not explained by differences in dust extinction properties.
-
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.
-
Finding the one: identifying the host of compact binary mergers
Restricting analysis to the top 1% most luminous galaxies in GW localization volumes yields 1-4 candidate hosts for three specific events, with 29-36% probability of random association.
-
A Search for Rotation Measure Flare Candidates in Repeating Fast Radio Bursts
A search of repeating FRBs identifies RM flare candidates in FRB 20121102A, FRB 20201124A, and FRB 20180916B, suggesting such events may be common and tied to dynamic magneto-ionic environments.
-
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.
-
Dynamically cold discs in high-redshift galaxies: comparison between ALMA observations and TNG50
TNG50 shows most massive high-z star-forming galaxies are dynamically hotter than ALMA data indicate, with rare cold discs forming from aligned accretion and evolving into one-third discs and two-thirds early-type galaxies by z=0.
-
Stellar feedback SPICEs up [C II] emission in the first galaxies
Simulations find [C II] traces star formation robustly but underestimates outflow speeds and mass-loading factors by factors of 2-5, with feedback type affecting disk settling but not distinguishable from [C II] spatial or spectral properties alone.
-
Inferring Halo Mass and Scale Radius of Galaxy Clusters Using Convolutional Neural Networks and Uchuu-UniverseMachine Catalogs
Convolutional neural networks can infer galaxy cluster virial masses and scale radii from 2D projected position and line-of-sight velocity distributions with nearly unbiased results and reduced scatter when richness is added or training is limited to relaxed systems.
-
The Galaxy Luminosity Functions in ASTRID: Predictions for LSST
ASTRID simulation with dust model calibrated to SDSS at z=0 produces validated luminosity functions and LSST-ready mock catalogs of 378 million galaxies with predicted number counts in ugrizy bands from z=0 to 2.
-
A statistical look on kinematic planes of satellite galaxies II: The physics behind their early formation in TNG50 MW/M31-like galaxies
Early kinematically persistent planes of satellite galaxies are fossil remnants of high-redshift anisotropic mass collapse along the principal directions of the local cosmic web during the fast assembly phase of host halos.
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HOLISMOKES XXI: Detecting strongly lensed type Ia supernovae from time series of multi-band LSST-like imaging data -- Part II
A convLSTM classifier identifies lensed SNe Ia in simulated LSST-like time series, reaching ~60% true-positive rate at O(10^{-4}) false-positive rate by the seventh epoch even after adding realistic PSF variations and foreground SN contaminants.
-
PEARLS: Two Distinct Populations of AGN Hosts Moving Between Star Formation and Quiescence
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.
-
Supermassive Black Hole Winds in X-rays: SUBWAYS IV. Tracing Radio Emission and Unveiling the Role of Winds
AGN with ultra-fast outflows exhibit larger radio extensions and steeper spectra matching wind-driven shock models, suggesting a link between X-ray winds and radio-emitting outflows.
-
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.
-
Planck 2018 results. X. Constraints on inflation
Updated Planck CMB measurements give ns = 0.9649 ± 0.0042, r < 0.056, confirm flatness at 0.4 percent, and show no evidence for scale-dependent features or non-slow-roll dynamics in the inflaton potential.
-
A PINK update: Improvements to the CELEBI fast radio burst data reduction and analysis pipeline
The PINK updates enhance the CELEBI FRB pipeline with better astrometry, time-frequency gating, polarization calibration, DM optimization tools, and a software container for improved efficiency and localization of events like FRB 20251019A.