TNG50 stellar disks are grouped into four j-types from sAM surface density maps, revealing a redshift-dependent sequence from irregular to barred forms driven by gas content and V/σ.
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Four parameters suffice to describe dust attenuation curve diversity in TNG simulations, yielding a new symbolic-regression model that recovers curves and fluxes better than existing parameterizations while linking parameters to SFR surface density, metallicity, and geometry.
RUBIES JWST sample shows U increases with redshift and sSFR, decreases with mass, rising by a factor of ~4 from z=2 to z=6 at fixed mass and sSFR, with 0.3 dex systematic uncertainty from photoionization model range.
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 local Tremaine-Weinberg framework integrates the continuity equation over flexible loops to measure galactic pattern speeds, recovering standard methods as special cases and validated on IllustrisTNG simulations.
IllustrisTNG yields γ=2.23±0.20 for luminosity density evolution that explains the Tolman and distance-duality test signals in standard cosmology.
A homogenized ICL definition applied to Horizon-AGN, TNG100, Gizmo-Simba and Hydrangea yields consistent z=0 fractions of 0.1-0.2 with no significant redshift evolution and dominant contributions from satellites of 10^10.5-10^11.5 solar masses.
Information-theoretic analysis of TNG50 simulations finds high mutual information (0.4-0.8) between bar and spiral parameters and comparable transfer entropy (0.33-0.42) in both directions, indicating mutual co-regulation.
JWST measurements of pitch angles in 593 spiral galaxies to z=3.5 show no overall redshift evolution but reveal correlations with mass and sSFR only below z=1.25, implying a transition from locally driven to globally regulated spiral arms.
Mutual information analysis of TNG50 simulations shows gravitational potential and total energy retain merger mass and infall time information longest, while radial velocity loses it within ~5 Gyr, with washout depending on radius, merger age, and mass.
In TNG-50, 80% of Milky Way-mass galaxies align their present-day angular momentum with the orbital angular momentum of their most massive merger, and 81% of their stellar halos rotate prograde relative to the disk.
TNG50 MW analogues reproduce global soft X-ray luminosity, inner surface brightness, emission measure and O VII absorption but show too-steep radial decline in X-ray brightness and 65% lower O VIII absorption than observed, indicating overly central feedback.
SHAMe-SF modeling of small-scale DESI ELG clustering delivers 6% precision on σ8 and Ωm h², matching full DR1 results with 1% volume.
Machine learning on cosmological simulations achieves 91-94% accuracy classifying over-massive versus under-massive SMBH growth regimes from LSST photometry, with 83-89% cross-simulation transfer accuracy driven primarily by host galaxy colors.
Milky Way-mass dark matter density profiles in IllustrisTNG are largely insensitive to astrophysics and cosmology variations, dominated by halo-to-halo variance instead.
New JWST data on 23 galaxies at 0.5<z<1.7 show median dark matter fraction of 0.63 at effective radius with 0.2 dex scatter, and a mix of rising, flat, and falling rotation curves.
TNG50 simulation analysis finds early-forming halos show higher stellar mass, metallicity, lower CGM gas mass and sSFR at z=0, with mass-dependent CGM metallicity reversal and cold-gas kinematics differences.
The TNG SAM reproduces TNG hydro simulation gas and metal flows plus galaxy and halo properties within 30% accuracy out to z=6 via five targeted updates to the Santa Cruz SAM calibrated on stellar feedback-dominated galaxies.
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.
PRFM-vol and PRFM-int subgrid models, calibrated from TIGRESS, produce shorter gas depletion times than IllustrisTNG and match TIGRESS star formation rates at high resolution while remaining robust at lower resolutions.
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.
TNG-Cluster simulations find that in galaxy cluster centers turbulence accounts for under half the total velocity dispersion (typically 50-75 km/s), is mostly subsonic, provides sub-percent pressure support, and is primarily driven by SMBH feedback.
Resolved photometry of four high-redshift quiescent galaxies reveals negative color gradients that lower estimated stellar masses by 0.1 dex relative to slit measurements, reducing model tensions under an age-driven interpretation.
Simulations of evolving galaxies show strong L_nu-SFR and L_nu-V_rot correlations up to z~3, with turbulent magnetic fields dominating at low redshift and large-scale fields growing in importance at higher redshift.
citing papers explorer
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IllustrisTNG50 angular momentum maps: tracing the morpho-kinematic evolution of galaxies
TNG50 stellar disks are grouped into four j-types from sAM surface density maps, revealing a redshift-dependent sequence from irregular to barred forms driven by gas content and V/σ.
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Learning the Universe: The Structure of Dust Attenuation Curves in Galaxy Simulations
Four parameters suffice to describe dust attenuation curve diversity in TNG simulations, yielding a new symbolic-regression model that recovers curves and fluxes better than existing parameterizations while linking parameters to SFR surface density, metallicity, and geometry.
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RUBIES: The Evolution of the Ionization Parameter from 0 < z < 9
RUBIES JWST sample shows U increases with redshift and sSFR, decreases with mass, rising by a factor of ~4 from z=2 to z=6 at fixed mass and sSFR, with 0.3 dex systematic uncertainty from photoionization model range.
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Origins of Extreme Emission-Line Ratios in z > 3 Galaxies: Insights from the Lumen Model
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.
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The Local Tremaine-Weinberg Method for Galactic Pattern Speed: Theory and its Application to IllustrisTNG
A local Tremaine-Weinberg framework integrates the continuity equation over flexible loops to measure galactic pattern speeds, recovering standard methods as special cases and validated on IllustrisTNG simulations.
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Forward-modelling the Tolman and distance-duality tests with IllustrisTNG
IllustrisTNG yields γ=2.23±0.20 for luminosity density evolution that explains the Tolman and distance-duality test signals in standard cosmology.
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A Consistent Comparison of Intracluster Light Assembly in Simulations I. Redshift Evolution and Progenitor Galaxies
A homogenized ICL definition applied to Horizon-AGN, TNG100, Gizmo-Simba and Hydrangea yields consistent z=0 fractions of 0.1-0.2 with no significant redshift evolution and dominant contributions from satellites of 10^10.5-10^11.5 solar masses.
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Co-evolution of bar and spiral arms in TNG50 simulations using Information Theory
Information-theoretic analysis of TNG50 simulations finds high mutual information (0.4-0.8) between bar and spiral parameters and comparable transfer entropy (0.33-0.42) in both directions, indicating mutual co-regulation.
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Spiral arms across cosmic time: JWST measurements of the pitch angles of spiral galaxies at $z<3.5$
JWST measurements of pitch angles in 593 spiral galaxies to z=3.5 show no overall redshift evolution but reveal correlations with mass and sSFR only below z=1.25, implying a transition from locally driven to globally regulated spiral arms.
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Galactic Amnesia: The Information Washout of the Milky Way Merger History
Mutual information analysis of TNG50 simulations shows gravitational potential and total energy retain merger mass and infall time information longest, while radial velocity loses it within ~5 Gyr, with washout depending on radius, merger age, and mass.
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Classifying Supermassive Black Hole Growth Regimes to Observables Across Cosmological Simulations with Forecasts for LSST
Machine learning on cosmological simulations achieves 91-94% accuracy classifying over-massive versus under-massive SMBH growth regimes from LSST photometry, with 83-89% cross-simulation transfer accuracy driven primarily by host galaxy colors.
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The DREAMS Project: Disentangling the Impact of Halo-to-Halo Variance and Baryonic Feedback on Milky Way Dark Matter Density Profiles
Milky Way-mass dark matter density profiles in IllustrisTNG are largely insensitive to astrophysics and cosmology variations, dominated by halo-to-halo variance instead.
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MSA-3D: Rotation Curves and Dark Matter Fractions at z~0.5-1.7 with JWST/NIRSpec
New JWST data on 23 galaxies at 0.5<z<1.7 show median dark matter fraction of 0.63 at effective radius with 0.2 dex scatter, and a mix of rising, flat, and falling rotation curves.
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The dependence of Circumgalactic Medium properties on halo assembly histories in the IllustrisTNG simulations
TNG50 simulation analysis finds early-forming halos show higher stellar mass, metallicity, lower CGM gas mass and sSFR at z=0, with mass-dependent CGM metallicity reversal and cold-gas kinematics differences.
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TNG SAM: Bridging Hydrodynamical Complexity and Semi-Analytic Efficiency to Model Galaxy Formation
The TNG SAM reproduces TNG hydro simulation gas and metal flows plus galaxy and halo properties within 30% accuracy out to z=6 via five targeted updates to the Santa Cruz SAM calibrated on stellar feedback-dominated galaxies.
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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.
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Pressure-regulated feedback-modulated star formation as a subgrid model for galaxy formation simulations
PRFM-vol and PRFM-int subgrid models, calibrated from TIGRESS, produce shorter gas depletion times than IllustrisTNG and match TIGRESS star formation rates at high resolution while remaining robust at lower resolutions.
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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.
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Bulk vs. turbulent motions at the centres of galaxy clusters: AGN-driven turbulence according to TNG-Cluster
TNG-Cluster simulations find that in galaxy cluster centers turbulence accounts for under half the total velocity dispersion (typically 50-75 km/s), is mostly subsonic, provides sub-percent pressure support, and is primarily driven by SMBH feedback.
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Unbreaking the Universe: MINERVA Measurements of Color Gradients in Massive Quiescent Galaxies Can Help Ease Too-Early Star Formation Tensions
Resolved photometry of four high-redshift quiescent galaxies reveals negative color gradients that lower estimated stellar masses by 0.1 dex relative to slit measurements, reducing model tensions under an age-driven interpretation.
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Radio Continuum Emission from Evolving Star-Forming Galaxies -- I. Correlations Involving the Total Synchrotron Luminosity
Simulations of evolving galaxies show strong L_nu-SFR and L_nu-V_rot correlations up to z~3, with turbulent magnetic fields dominating at low redshift and large-scale fields growing in importance at higher redshift.
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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.
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Bulgeless Evolution And the Rise of Discs (BEARD) III. A numerical simulation view of satellites around Milky-Way analogues
Simulation comparison finds bulgeless galaxies host more centrally concentrated, disc-aligned satellites with steeper faint-end luminosity functions than bulge-dominated controls, reflecting co-evolution and quieter merger histories.
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Bulgeless Evolution And the Rise of Discs (BEARD) I. Physical drivers of the mass-size relation for Milky Way-like galaxies
Bulgeless galaxies trace the upper envelope of the mass-R1 relation with scatter driven by central stellar density and the spatial configuration of mergers rather than their number.
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A Universal Dance of Galactic Disks: Ubiquitous Precession and Its Implications
IllustrisTNG simulations indicate galactic disk precession is common, driven by external tidal torques within 30 kpc, inducing warps and influencing evolution at all redshifts.
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The LISA Astrophysics MBHcatalogues Project: A comparison of predictions of simulated massive black hole binaries
A large collaboration compiles and compares merger rate predictions for massive black holes across multiple galaxy formation models to forecast LISA detections and quantify uncertainties.
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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.
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Analysis of synthetic OVI absorption associated with galaxy groups in SIMBA and TNG50 simulations
Both SIMBA and TNG50 simulations underpredict OVI covering fractions around galaxy groups compared to observations, with most absorbers being gravitationally bound.
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Tracing the relic nature of compact galaxies through their globular cluster systems
Globular cluster mass fractions, in-situ fractions, metallicity spreads, and spatial profiles in simulated compact galaxies can identify massive relic analogs with early assembly histories.
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FOGGIE: Figuring Out Gas & Galaxies In Enzo XII. The Formation and Evolution of Extended HI Galactic Disks and Warps with a Dynamic Circumgalactic medium
FOGGIE cosmological simulations find that less HI-populated CGMs produce thin, coherently rotating extended disks while more populated CGMs yield irregular morphologies, with all systems settling kinematically by z=0 independent of mass.
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Cosmological Simulations of Stellar Halos with Gaia Sausage-Enceladus Analogues: Two Sausages, One Bun?
TNG50 simulations of 98 Milky Way analogues find GSE-like debris in 32 cases, with two-merger GSEs in one third; single- and two-merger cases differ in median infall time (5.9 vs 10.7 Gyr ago), abundances, and star-formation histories.
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Resolved Ages and Stellar Metallicities in Progenitors of Milky Way Analogs: A Closer Look at their Star Formation Histories since $z=5$
Resolved stellar property gradients in Milky Way analog progenitors show inside-out assembly with minor, temporary disruption from major mergers.
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Signature of Bursty Star Formation in the High-Redshift Galaxies Detected with JWST
Shorter star formation timescales in a semi-analytical UV LF model explain the slow evolution observed by JWST at z>10 without requiring changes in star formation efficiency.
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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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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.
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Low-ionization Metal Absorption at $0.7 \lesssim z \lesssim 2$ Confronting Cosmological Simulations with Observations
IllustrisTNG with a uniform UVB reproduces observed MgI, MgII and FeII column-density PDFs and low-EW MgII incidence but underestimates the number of strong MgII systems and fails to capture their rise toward z~2.
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Dynamical evolution of Milky Way globular clusters on the cosmological timescale II. Terzan 2, 4, and 5 mass loss and collision tracking
N-body simulations show that mutual interactions between Terzan 2, 4, and 5 raise mass-loss rates for the smaller clusters and drive prolate deformations absent in isolated runs.
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Interpreting "Interpretability" and Explaining "Explainability" in Machine Learning in Physics
The paper defines interpretability as model structural transparency and explainability as scientific content mapping, discusses their trade-offs, and frames both as deliberate modeling choices for ML in physics.
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Cosmological Galaxy Formation Modelling in the Era of the Square Kilometre Array
Review of state-of-the-art cosmological galaxy formation models for HI, molecular gas and radio continuum in preparation for SKA, advocating coordinated multi-scale simulations, forward modelling and AI emulators.