{"total":33,"items":[{"citing_arxiv_id":"2607.06933","ref_index":116,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Constructing a Mock Galaxy Catalog for the All-sky SPECtroscopic Survey of Nearby Galaxies (A-SPEC) Using the Machine-assisted Semi-Simulation Model","primary_cat":"astro-ph.CO","submitted_at":"2026-07-08T02:52:51+00:00","verdict":"CONDITIONAL","verdict_confidence":"HIGH","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A machine learning model trained on IllustrisTNG predicts galaxy baryonic properties from dark matter subhalo features, producing a mock catalog for the A-SPEC survey that matches observed galaxy clustering.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27182","ref_index":41,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Forward-modelling the Tolman and distance-duality tests with IllustrisTNG","primary_cat":"astro-ph.CO","submitted_at":"2026-06-25T15:47:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"IllustrisTNG yields γ=2.23±0.20 for luminosity density evolution that explains the Tolman and distance-duality test signals in standard cosmology.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26262","ref_index":77,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Stellar Role Reversal: Multiple Features in the Mass and Mass Ratio Distributions of Merging Binary Black Holes from Stable Mass Transfer","primary_cat":"astro-ph.SR","submitted_at":"2026-06-24T18:03:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Stable mass transfer produces two distinct peaks in merging binary black hole primary mass and mass ratio distributions via mass ratio reversal under conservative mass transfer.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24735","ref_index":71,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The dependence of Circumgalactic Medium properties on halo assembly histories in the IllustrisTNG simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-06-23T15:59:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24071","ref_index":49,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Universal Fitting Formulae for the Peak Concentration of Dark Matter Halos","primary_cat":"astro-ph.CO","submitted_at":"2026-06-23T02:28:20+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23798","ref_index":206,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The PICO-Cluster Project: presenting the galaxy cluster sample and studying magnetic field growth, Faraday rotation and Braginskii heating","primary_cat":"astro-ph.GA","submitted_at":"2026-06-22T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Presents 24 AREPO+IllustrisTNG zoom-in simulations of clusters above 10^15 solar masses showing converged magnetic fields with volume-averaged plasma beta approximately 100 inside R200 after z~1.2, declining Faraday rotation profiles, and intermittent Braginskii heating approaching cooling rates in ","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20175","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Consistent Comparison of Intracluster Light Assembly in Simulations I. Redshift Evolution and Progenitor Galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-18T12:44:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"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.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"mented following the Pillepich et al. (2018a) model, and dual-mode AGN feedback switched according to accretion rate is implemented following the Weinberger et al. (2017) model. 2.1.3The Three Hundred Gizmo-Simba 7K TheThe Three Hundredsimulation suite 3 (Cui et al. 2018) con- sistsofhydrodynamicalzoom-insimulationsofthe324mostmassive haloes (masses∈ [10 14.8,10 15.5]M ⊙) drawn from theMultiDark Planck 2cosmological N-body simulation (side length1ℎ −1 Gpc; Klypin et al. 2016). In this work we use data from the newGIZMO- SIMBA 7Ksimulation runs (Cui et al. in prep.), a higher-resolution and otherwise improved follow-up of the originalGIZMO-SIMBA (3K)simulations (Cui et al. 2022). The meshless finite-mass La- grangian hydrodynamics solverGIZMO(Hopkins 2015, Hopkins"},{"citing_arxiv_id":"2606.18352","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"TNG SAM: Bridging Hydrodynamical Complexity and Semi-Analytic Efficiency to Model Galaxy Formation","primary_cat":"astro-ph.GA","submitted_at":"2026-06-16T18:00:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"flow and outflow rates for a subset of TNG galaxies ex- tracted by Oren et al. (2025), we aim to emulate the un- derlying baryon cycle modeled in TNG, resulting in the creation of a new \"TNG SAM.\" This endeavor serves four primary goals: (1) to simplify and distill TNG's complex feedback and baryon cycling behaviors into a more interpretable semi-analytic framework, (2) to fa- cilitate direct comparisons between SAMs and hydrody- namical simulations, clarifying their respective strengths and limitations, (3) to develop a framework that enables efficient exploration of alternative subgrid physics mod- els that are otherwise too computationally expensive to vary directly within hydrodynamical simulations, and (4) to ultimately extend the predictive power of SAMs"},{"citing_arxiv_id":"2606.17189","ref_index":127,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Exploring the Relationship Between Bars, Star Formation Activity, and Host Galaxy Properties from $\\mathbf{z \\sim 0}$ to $\\mathbf{z \\sim 2}$","primary_cat":"astro-ph.GA","submitted_at":"2026-06-15T18:27:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11313","ref_index":65,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Comparison and verification methods to trace interaction-driven disturbances in galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-09T18:01:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"SSL model detects galaxy interaction signatures with recall 0.86 and low contamination while CAS at A>0.35 has recall 0.20 but higher precision, benchmarked on visual classification of 25.1% disturbed fraction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10038","ref_index":80,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Learning the Universe with the 2nd Generation of CAMELS: Varying 35 parameters of the IllustrisTNG model in (50Mpc/h)^3 boxes","primary_cat":"astro-ph.CO","submitted_at":"2026-06-08T18:12:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"New CAMELS simulations in larger (50 Mpc/h)^3 boxes with 35 varied parameters produce tighter neural-network constraints on model parameters than prior smaller-volume runs, with public data release.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10026","ref_index":50,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Pressure-regulated feedback-modulated star formation as a subgrid model for galaxy formation simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-06-08T18:08:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09997","ref_index":97,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A universal model for the accretion rates and formation times of dark matter halos","primary_cat":"astro-ph.CO","submitted_at":"2026-06-08T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A six-parameter function of peak height ν, power spectrum slope n_eff, and growth rate α_eff accurately describes median halo mass accretion rates from simulations in ΛCDM and Einstein-de Sitter cosmologies at z=0-14.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.30433","ref_index":85,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Consistent Implementation of Cluster Strong Lensing in Cosmological Simulation Light Cones","primary_cat":"astro-ph.CO","submitted_at":"2026-05-28T18:00:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A simulation-based procedure for cluster strong lensing that remaps uniform boxes and traces rays through resolved particles, finding uncorrelated line-of-sight structure shifts images by arcseconds and changes critical areas by 16+20-14 percent at zs=4.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15893","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Probing the faint end of simulated galaxy counts at z>3","primary_cat":"astro-ph.CO","submitted_at":"2026-05-15T12:22:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"TNG100 and EAGLE hydrodynamical simulations underproduce faint compact galaxies at z>3 relative to CANDELS observations even after forward modeling and completeness corrections, with the mismatch linked to both detection effects and simulation physics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.08364","ref_index":46,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Identification of Compact Groups of Galaxies in IllustrisTNG300","primary_cat":"astro-ph.GA","submitted_at":"2026-05-08T18:19:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Compact galaxy groups identified in TNG300 show that ~80% of velocity-selected groups are line-of-sight interlopers, with a stellar-mass versus velocity-dispersion scaling relation serving as an effective diagnostic.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07511","ref_index":97,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dynamical evolution of Milky Way globular clusters on the cosmological timescale II. Terzan 2, 4, and 5 mass loss and collision tracking","primary_cat":"astro-ph.GA","submitted_at":"2026-05-08T09:41:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.06769","ref_index":224,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Origins of Extreme Emission-Line Ratios in z > 3 Galaxies: Insights from the Lumen Model","primary_cat":"astro-ph.GA","submitted_at":"2026-05-07T18:00:01+00:00","verdict":"CONDITIONAL","verdict_confidence":"HIGH","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Extreme z>3 emission-line ratios are reproduced only by combining harder ionizing spectra, ionization parameters from massive star clusters, and enhanced nitrogen abundances.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05972","ref_index":71,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A statistical look on kinematic planes of satellite galaxies II: The physics behind their early formation in TNG50 MW/M31-like galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-05-07T10:18:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04176","ref_index":43,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Matter Clustering in Astrid: Reduced Baryonic Suppression from Realistic Black Hole Dynamics","primary_cat":"astro-ph.GA","submitted_at":"2026-05-05T18:13:07+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.03008","ref_index":166,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Environmental Quenching of High-Redshift Galaxies: Interpreting JWST Observations with Simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-05-04T18:00:06+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.00349","ref_index":57,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Universal Dance of Galactic Disks: Ubiquitous Precession and Its Implications","primary_cat":"astro-ph.GA","submitted_at":"2026-05-01T02:15:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"IllustrisTNG simulations indicate galactic disk precession is common, driven by external tidal torques within 30 kpc, inducing warps and influencing evolution at all redshifts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.00092","ref_index":216,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The LISA Astrophysics MBHcatalogues Project: A comparison of predictions of simulated massive black hole binaries","primary_cat":"astro-ph.GA","submitted_at":"2026-04-30T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.24836","ref_index":83,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Thermodynamic and Kinematic Evolution of Circumgalactic Gas around $z=1$ in the IllustrisTNG model","primary_cat":"astro-ph.GA","submitted_at":"2026-04-27T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"In the IllustrisTNG model, CGM gas around z=1 galaxies mixes quickly and separates into cold inner and warm-hot outer phases within 500 Myr due to feedback, with kinematic decorrelation over 400 Myr and ion-specific phases lasting different durations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.24494","ref_index":46,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Probing the Hot Gaseous Halos of Milky Way-like Galaxies in the TNG50 simulation","primary_cat":"astro-ph.GA","submitted_at":"2026-04-27T13:59:12+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19543","ref_index":46,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dynamically cold discs in high-redshift galaxies: comparison between ALMA observations and TNG50","primary_cat":"astro-ph.GA","submitted_at":"2026-04-21T15:02:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19449","ref_index":122,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Cosmological constraints from the small scale clustering of Emission Line Galaxies","primary_cat":"astro-ph.CO","submitted_at":"2026-04-21T13:32:04+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"SHAMe-SF modeling of small-scale DESI ELG clustering delivers 6% precision on σ8 and Ωm h², matching full DR1 results with 1% volume.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18209","ref_index":181,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Galaxy Populations in the IllustrisTNG Caustic Skeleton","primary_cat":"astro-ph.CO","submitted_at":"2026-04-20T12:56:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Galaxy properties in IllustrisTNG form a continuum across the multiscale caustic skeleton, with formation time of web components influencing colors and star formation activity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.16539","ref_index":53,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Classifying Supermassive Black Hole Growth Regimes to Observables Across Cosmological Simulations with Forecasts for LSST","primary_cat":"astro-ph.GA","submitted_at":"2026-04-16T23:53:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.10595","ref_index":66,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Low-ionization Metal Absorption at $0.7 \\lesssim z \\lesssim 2$ Confronting Cosmological Simulations with Observations","primary_cat":"astro-ph.CO","submitted_at":"2026-04-12T12:04:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.02993","ref_index":55,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Tracing the relic nature of compact galaxies through their globular cluster systems","primary_cat":"astro-ph.GA","submitted_at":"2026-04-03T12:13:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.03132","ref_index":88,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The DREAMS Project: Disentangling the Impact of Halo-to-Halo Variance and Baryonic Feedback on Milky Way Dark Matter Density Profiles","primary_cat":"astro-ph.GA","submitted_at":"2025-12-02T19:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Milky Way-mass dark matter density profiles in IllustrisTNG are largely insensitive to astrophysics and cosmology variations, dominated by halo-to-halo variance instead.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.22179","ref_index":54,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The impact of cosmic filaments on the abundance of satellite galaxies","primary_cat":"astro-ph.GA","submitted_at":"2025-09-26T10:38:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Satellite abundance is higher in filaments than the field by factors of 1.9-3.5, but reduced up to 79% after halo mass matching and further suppressed by dark matter tracer choice in IllustrisTNG.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}