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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representative citing papers
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.
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.
Galactic disks precess ubiquitously from tidal torques, causing warps, orbital heating, and radial alignments of satellites.
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.
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.
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.
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.
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.
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.
Both SIMBA and TNG50 simulations underpredict OVI covering fractions around galaxy groups compared to observations, with most absorbers being gravitationally bound.
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.
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.
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.
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.
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.
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.
Clustered dark matter may enable small seed black holes to grow to over 10^7 solar masses by redshift 10 in dense nuclear star clusters, with special behavior for ultralight dark matter due to its de Broglie wavelength.
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.
citing papers explorer
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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.
-
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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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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A Universal Dance of Galactic Disks: Ubiquitous Precession and Its Implications
Galactic disks precess ubiquitously from tidal torques, causing warps, orbital heating, and radial alignments of satellites.
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Galaxy mergers and disk angular momentum evolution: stellar halos as a critical test
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.
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Probing the Hot Gaseous Halos of Milky Way-like Galaxies in the TNG50 simulation
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.
-
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.
-
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.
-
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.
-
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.
-
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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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.
-
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.
-
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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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.
-
Dark Matter and the Early Formation of Supermassive Black Holes
Clustered dark matter may enable small seed black holes to grow to over 10^7 solar masses by redshift 10 in dense nuclear star clusters, with special behavior for ultralight dark matter due to its de Broglie wavelength.
-
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.