{"total":13,"items":[{"citing_arxiv_id":"2606.31042","ref_index":184,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"An Acceleration is Worth a Hundred Thousand Phase Space Measurements","primary_cat":"astro-ph.GA","submitted_at":"2026-06-30T02:23:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"One acceleration measurement equals ~10^5 phase-space measurements for local dark matter density estimation, with acceleration outperforming Jeans modeling in both equilibrium and perturbed Milky Way simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.30718","ref_index":29,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tidal origin of dark-matter free dwarf galaxies in the NGC 1052 group","primary_cat":"astro-ph.GA","submitted_at":"2026-06-29T18:00:01+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":"2606.28482","ref_index":78,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Strongest constraints on dark acoustic oscillations from the Lyman-alpha forest","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First constraints from Ly-alpha forest limit DAO participation to at most 30% of dark matter for peaks below 50 h/Mpc at 95% CL using a deep kernel emulator of simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25025","ref_index":157,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Investigating black hole accretion and feedback self-regulation in Seyfert galaxies using the FIRE-3 cosmological hydrodynamic simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-06-23T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"FIRE-3 cosmological simulations of Seyfert galaxies produce episodic AGN feedback and gas clearing but no clear anti-correlation between nuclear gas concentration and AGN luminosity, highlighting timing mismatches with observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21651","ref_index":58,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Resolved Ages and Stellar Metallicities in Progenitors of Milky Way Analogs: A Closer Look at their Star Formation Histories since $z=5$","primary_cat":"astro-ph.GA","submitted_at":"2026-06-19T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Resolved stellar property gradients in Milky Way analog progenitors show inside-out assembly with minor, temporary disruption from major mergers.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17636","ref_index":39,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A fast spectral-multigrid Poisson solver in non-Cartesian geometries","primary_cat":"astro-ph.IM","submitted_at":"2026-06-16T07:46:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A spectral-multigrid Poisson solver for spherical and cylindrical coordinates achieves second-order accuracy on uniform and logarithmic radial grids with vacuum boundary handling via screening mass and scales to 4096 cores.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12605","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Feedback-Free Star Formation in Clusters within a Galaxy Simulated at High Resolution in Cosmic Dawn","primary_cat":"astro-ph.GA","submitted_at":"2026-06-10T19:02:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"High-resolution zoom-in simulation of a z~10 galaxy produces over 10^5 star clusters with scale-free mass function, 90% of star formation in clusters, global SFE 0.2-0.3, and reproduces JWST super-bright galaxies via feedback-free bursts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.08494","ref_index":22,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Virial-based extraction of structures in numerical simulations: The vibes tool","primary_cat":"astro-ph.SR","submitted_at":"2026-06-07T07:48:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Vibes is a new algorithm that extracts physically motivated core structures from numerical star formation simulations by applying the virial theorem iteratively around density peaks to determine boundaries from energy balance rather than user-set density thresholds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04827","ref_index":154,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Steep Redshift Evolution of the Ionizing Escape Fraction at $z = 5$--$12$: Empirical Constraints and Comparison with Simulations","primary_cat":"astro-ph.CO","submitted_at":"2026-06-03T12:50:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Empirical three-parameter fit to f_esc(M_h,z) yields steep redshift evolution with population-averaged escape fraction rising from ~2% at z=5 to ~9% at z=12.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04740","ref_index":96,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"TDEs on FIRE: Illuminating the Cosmic Evolution of Tidal Disruption Rates","primary_cat":"astro-ph.HE","submitted_at":"2026-06-03T11:22:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"FIRE-2 simulations show per-galaxy tidal disruption rates peak near z=2.5 at 4e-4 per year, correlate with SFR and central density, and remain high in satellite galaxies at early times.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04081","ref_index":19,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The role of major mergers in triggering super-Eddington accretion","primary_cat":"astro-ph.GA","submitted_at":"2026-06-02T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"High-resolution cosmological zoom-in simulations find that major mergers do not trigger sustained super-Eddington black hole accretion in low-mass halos when feedback is included; episodes occur only immediately after seeding or with feedback disabled.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15275","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Simulated Oxygen Shortage (SOS): Mapping the Missing OVI in Simulated Dwarf Galaxies to Subgrid Physics","primary_cat":"astro-ph.GA","submitted_at":"2026-05-14T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The paper identifies underproduction of oxygen in low-mass simulated dwarf galaxies as the likely cause of missing OVI in the CGM, based on comparisons across two simulation suites.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"In contrast, M24 provides a sample with strong isolation criteria and mass estimates extending to 3Rvir. From the observed column densities, M24 estimates the total Ovimass within a radial annulus betweenR inner andR outer using the mean column density measured in that annulus,⟨N OVI⟩. The mass is computed as, M M24 OVI ≈π(R 2 outer −R 2 inner)m OVI κOVI ⟨NOVI⟩,(1) wherem OVI is the mass of an Oviion andκ OVI is the covering fraction of detections. This calculation is per- formed separately for strong (N OVI >10 14 cm−2) and weak (10 13.5 < N OVI <10 14 cm−2) detections, with non-detections accounted for via bootstrapping, and the resulting masses are summed. The resulting total Ovi mass within 0≤b/R vir ≤2 isM M24"},{"citing_arxiv_id":"2605.13472","ref_index":49,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"First Light And Reionization Epoch Simulations (FLARES) XXI: The UV Indices of Galaxies in the Early Universe","primary_cat":"astro-ph.GA","submitted_at":"2026-05-13T12:59:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations of high-redshift galaxies show the 1719 Å UV index reliably traces stellar metallicity while others are more sensitive to star formation history.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}