{"total":21,"items":[{"citing_arxiv_id":"2607.00077","ref_index":80,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Hot or Cold? Radial Redistribution of Stars in FIRE Simulations of Milky Way-Mass Galaxies and the Asymmetry of Inward versus Outward Migrators","primary_cat":"astro-ph.GA","submitted_at":"2026-06-30T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Simulations of Milky Way-mass galaxies reveal direction-dependent dynamical heating during stellar radial migration, with inward migrators heating, some cooling, and cold preservation uncommon especially for older stars.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28559","ref_index":58,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI DR2 Reference Mocks: Clustering results from UCHUU ELGs and QSOs","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T19:22:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Mock catalogs for DESI DR2 ELGs and QSOs are constructed via modified subhalo abundance matching on the Uchuu simulation to reproduce observed number density and clustering statistics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24071","ref_index":5,"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":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Empirical universal fitting formula for the peak (most probable) concentration of dark matter halos derived from lognormal fits to simulation distributions and shown to be invariant across cosmologies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19443","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The impact of evolving cosmic filaments on mass and spin evolution of dark matter halos","primary_cat":"astro-ph.CO","submitted_at":"2026-06-17T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A new algorithm traces filament evolution in simulations and finds suppressed halo mass accretion plus non-random spin alignment changes near dense filaments.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12137","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Unified Halo Mass Function Across Dark Matter Models from High-Resolution Multi-Scale Simulations","primary_cat":"astro-ph.CO","submitted_at":"2026-06-10T14:32:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A calibrated fitting function for the halo mass function that unifies predictions across CDM and non-CDM models over 10 orders of magnitude in mass with typical 12% precision after modeling systematics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10038","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"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":"2606.10024","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Learning the Universe with cosmological rescaling of merger trees and semi-analytic galaxy formation models","primary_cat":"astro-ph.CO","submitted_at":"2026-06-08T18:08:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Rescaling merger trees with a halo-profile correction enables cheap generation of galaxy summary statistics across cosmologies using semi-analytic models, matching dedicated simulation accuracy with far fewer base runs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09997","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"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":"2606.09817","ref_index":138,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Satellite compaction pathways: environmental drivers shaping dwarf galaxy corpulence in the TNG50 simulation","primary_cat":"astro-ph.GA","submitted_at":"2026-06-08T17:56:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.03753","ref_index":51,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"The impact of source and survey modelling on the connection between [O III] emitters and Ly $\\alpha$ forest transmission at z ~ 6","primary_cat":"astro-ph.CO","submitted_at":"2026-06-02T15:03:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Empirical halo-to-[O III] emitter modeling with realistic JWST survey mocks produces cross-correlations consistent with z~6 data within large scatter, but with a ~10 cMpc offset in the 1D peak.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02566","ref_index":7,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Mergers Matter: Gravothermal Collapse in Dwarf Halos with Self-Interacting Dark Matter","primary_cat":"astro-ph.GA","submitted_at":"2026-06-01T17:55:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"SIDM simulations of dwarf halos show that quiescent merger histories produce gravothermal core collapse while sustained mergers prevent collapse and can yield central densities below gravothermal fluid model predictions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.24104","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Resolving galaxy formation in the early Universe with BonFIRE and CampFIRE","primary_cat":"astro-ph.GA","submitted_at":"2026-05-22T18:09:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"BonFIRE and CampFIRE simulations show bursty clustered star formation in early galaxies and predict UV luminosity functions matching observations at faint magnitudes with a turnover at M_UV approx -14 but overpredicting brighter galaxies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19323","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Correlation between baryonic process and galaxy assembly bias","primary_cat":"astro-ph.GA","submitted_at":"2026-05-19T04:02:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations show gas cooling and stellar feedback dominate assembly bias for stellar-mass selected galaxies while star formation gives way to gas cooling for SFR-selected galaxies as number density rises.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18987","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"How High-Specific-Energy Winds Regulate the Circumgalactic Medium of Dwarf Galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-05-18T18:05:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations demonstrate that high-specific-energy supernova outflows sustain hot CGM at virial temperature, raise t_cool/t_ff above 10, and transition dwarf galaxy feedback from ejective to preventive mode around 5 Gyr.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"In comparison with the minimalist regulator model presented in Voit et al. (2024a) (where radiative loss is assumed to be negligible), we find that our high stellar mass is likely driven byηE = 0.01−0.05. 3.3.Sustaining the Virial Temperature The first question we address is whether SNe wind- induced shock heating can sustain the CGM at∼T vir: Tvir = µmp 2kB GMvir Rvir (8) where we ignore external pressure (Lochhaas et al. 2021) and assume the mean molecular weightµ= 0.59. 8 As discussed in§1, the present-day halo masses of our sample lie near the peak of the cooling curve. Therefore, we naively expect the CGM to cool on a short timescale compared to the halo free-fall time (t cool ≪t ff) (White & Frenk 1991). 3.3."},{"citing_arxiv_id":"2605.04138","ref_index":31,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Galactic Amnesia: The Information Washout of the Milky Way Merger History","primary_cat":"astro-ph.GA","submitted_at":"2026-05-05T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.00450","ref_index":12,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Measuring $f\\sigma_8$ and BAO scale in the Local Universe: a joint real and redshift space analysis from CosmicFlows-4++","primary_cat":"astro-ph.CO","submitted_at":"2026-05-01T06:36:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Joint real and redshift space analysis of CosmicFlows-4++ yields BAO scales of 132±8 h^{-1}Mpc (real) and 139±7 h^{-1}Mpc (redshift) at z=0.07 together with fσ8=0.344±0.105.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.23147","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A graph-based Neural Network surrogate model for accelerating semi-analytical model of galaxy formation and evolution","primary_cat":"astro-ph.GA","submitted_at":"2026-04-25T05:17:06+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A conditional graph neural network serves as an accurate and fast surrogate for semi-analytic galaxy formation models, predicting key properties across cosmic time.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"νSF,0 Normalization of the quiescent star formation law [10−10,10 −8] ϵ⋆ Efficiency parameter for star formation in the spheroid [0.01,1] α⋆ Exponent parameter for star formation in the spheroid [−3,3] βmax,d Maximum of the mass loading factor in the disk [100,1000] Voutflow,d Velocity of the outflow in the disk [10,300] αoutflow,d Powerlawindexofthediskout- flow prescription [1,4] βmax,s Maximum of the mass loading factor in the spheroid [100,1000] Voutflow,s Velocity of the outflow in the spheroid [10,300] αoutflow,s Power law index of the spheroid outflow prescription [1,4] fcore Core radius of the hot halo in units of the virial radius of the host dark matter halo [0.01,0.8] fAge factor for the computation of the time available for cooling"},{"citing_arxiv_id":"2604.22013","ref_index":20,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"An Extended Parametric Model for Self-interacting Dark Matter Halos","primary_cat":"astro-ph.GA","submitted_at":"2026-04-23T19:07:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"An extended parametric model for SIDM halos incorporates mass accretion to delay core collapse and reduces errors in predicted V_max at z=0 relative to the prior Yang et al. (2024b) model.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"However, we expect the gravitational potentials of our two paired CDM and SIDM halos to differ based on how far the SIDM halo has evolved; thus,ϕ SIDM ̸=ϕ CDM. LSIDM can also be simplified toL SIDM =ϕ SIDMρSIDM/tc. Putting this together, we find: ˙E(t) = ϕSIDMρSIDM tc +ϕ SIDM ˙ρSIDM −ϕ CDM ˙ρCDM, (19) ˙E(t) =ϕ SIDMρSIDM \u0012 1 tc + ˙ρSIDM ρSIDM − ϕCDM ˙ρSIDM ϕSIDMρSIDM \u0013 , (20) ˙E=ϕ SIDMρSIDM 1 tc + ˙M M − ˙M M ϕCDM ϕSIDM ! .(21) We posit thatϕCDM is related toϕ SIDM through a func- tion ofτalone: ϕCDM =f(τ)ϕ SIDM,(22) such that ˙E=ϕ SIDMρSIDM 1 tc + ˙M M − ˙M M f(τ) ! .(23) f(τ) can be Taylor expanded to first orderf(τ) = f(0) +f (1)τ+. . .resulting in: ˙E=ϕ SIDMρSIDM 1 tc + ˙M M − ˙M M h f(0) +f (1)τ i! . (24) Looking back to Equation 22, atτ= 0 there has been"},{"citing_arxiv_id":"2604.21790","ref_index":16,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Informative Priors on Primordial Non-Gaussianity Bias $b_{\\phi}$ From Galaxy Formation","primary_cat":"astro-ph.CO","submitted_at":"2026-04-23T15:46:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Conditioning CAMELS-SAM simulations on the stellar mass function or stellar-to-halo mass relation reduces uncertainty in b_phi by 88-97% for DESI emission line galaxy samples while remaining consistent across galaxy formation variations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"1088/0004-637X/762/2/109. URLhttps://dx.doi.org/10.1088/0004-637X/762/2/109. [15] P. S. Behroozi, R. H. Wechsler, H.-Y. Wu, M. T. Busha, A. A. Klypin, et al. Gravitationally consistent halo catalogs and merger trees for precision cosmology.The Astrophysical Journal, 763(1):18, dec 2012. doi: 10.1088/0004-637X/763/1/18. URL https://dx.doi.org/10.1088/0004-637X/763/1/18. [16] M. Bernardi, A. Meert, R. K. Sheth, V. Vikram, M. Huertas-Company, et al. The massive end of the luminosity and stellar mass functions: dependence on the fit to the light profile.Monthly Notices of the Royal Astronomical Society, 436(1):697-704, 09 2013. ISSN 0035-8711. doi: 10.1093/mnras/stt1607. URLhttps://doi.org/10.1093/mnras/stt1607. [17] M. Bernardi, R."},{"citing_arxiv_id":"2604.15932","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Inferring Halo Mass and Scale Radius of Galaxy Clusters Using Convolutional Neural Networks and Uchuu-UniverseMachine Catalogs","primary_cat":"astro-ph.CO","submitted_at":"2026-04-17T10:49:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.00158","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"FOGGIE: Figuring Out Gas & Galaxies In Enzo XII. The Formation and Evolution of Extended HI Galactic Disks and Warps with a Dynamic Circumgalactic medium","primary_cat":"astro-ph.GA","submitted_at":"2025-10-31T18:07:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}