{"total":18,"items":[{"citing_arxiv_id":"2606.25359","ref_index":200,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological Galaxy Formation Modelling in the Era of the Square Kilometre Array","primary_cat":"astro-ph.GA","submitted_at":"2026-06-24T03:44:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":1.0,"formal_verification":"none","one_line_summary":"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.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09817","ref_index":215,"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":"2606.06599","ref_index":26,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Halo mass functions in mixed cold and fuzzy dark matter models","primary_cat":"astro-ph.CO","submitted_at":"2026-06-04T18:00:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations show fuzzy dark matter fraction up to 0.3 suppresses low-mass halos in mixed DM models, and a redshift- and fraction-dependent suppression function maps CDM HMFs to MDM HMFs within 0.1-0.2 dex accuracy for z=1-4.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04827","ref_index":6,"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":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"reduces the emissivity evaluation to a single array op- eration, enabling the∼10 4 evaluations required by the MCMC. 3.5.Reionization ODE The volume-averaged ionized fractionQ(z)≡1− ¯xHI(z) evolves according to (Madau et al. 1999; Bolton & Haehnelt 2007): dQ dt = ˙nion(z) nH,0 −C HII(z)α B nH,0 (1+z)3 Q(z),(8) wheren H,0 = 1.89×10 −7 cm−3 is the comoving hy- drogen number density,C HII(z) = 2.9 [(1+z)/6] −1.1 is the clumping factor (Shull et al. 2012), andα B = 1.52×10 −13 cm3 s−1 is the case-B recombination coef- ficient atT= 2×10 4 K. We integrate numerically with 400 Euler steps fromz= 30 toz= 4.5. The Thomson optical depth is τe = Z zmax 0 1.08n H,0 (1+z)2 Q(z)σ T c H(z) dz ,(9) where the factor 1.08 accounts for singly-ionized helium. 3.6.Statistical framework"},{"citing_arxiv_id":"2606.00221","ref_index":78,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"It's Not Just Star Formation: A trend of low dark matter densities in the Andromeda dwarf galaxy system","primary_cat":"astro-ph.GA","submitted_at":"2026-05-29T18:00:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Five of seven modeled M31 dwarf spheroidals show anomalously low central DM densities at 150 pc, with star formation heating disfavored as the sole cause.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.25071","ref_index":19,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Field Sources for Dark Matter Black Holes","primary_cat":"gr-qc","submitted_at":"2026-05-24T13:29:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Dark matter halo profiles admit effective nonlinear electrodynamics completions that source regular black holes exhibiting de Sitter cores for finite central density and Schwarzschild asymptotics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15330","ref_index":12,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A metric solution for rotating black holes embedded in dark matter halos with central spikes","primary_cat":"gr-qc","submitted_at":"2026-05-14T18:51:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"An exact analytic metric is constructed for rotating black holes embedded in generic dark matter halos with a central density spike that vanishes beyond a truncation radius near the horizon, generalizing prior spherical solutions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.23353","ref_index":11,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Testing Scalar Field Dark Matter models in M31 galaxy through the Rotation Curve analysis","primary_cat":"astro-ph.CO","submitted_at":"2026-04-25T15:39:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Fuzzy dark matter with smooth cored halos provides the most consistent description of M31's rotation curve among scalar field models when paired with a two-bulge baryonic configuration.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Within the standard cosmological paradigm, DM is usually described as a cold and collisionless particle component (CDM). Numerical simulations within this framework predict cuspy density profiles such as the Navarro-Frenk-White (NFW) profile [10]. However, observational studies of galaxy RCs often indicate the presence of central cores rather than cusps, giving rise to the well-known core-cusp problem [11, 12]. This discrepancy has motivated the investigation of alternative DM scenarios capable of naturally producing cored density distributions. Among the proposed alternatives, Scalar Field Dark Matter (SFDM) models have attracted considerable attention because they provide a physically motivated mechanism for addressing several small-scale challenges of the standard"},{"citing_arxiv_id":"2604.22441","ref_index":81,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"How lonely are the Binary Compact Objects Detected by the LIGO-Virgo-KAGRA Collaboration?","primary_cat":"astro-ph.HE","submitted_at":"2026-04-24T10:59:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"No three-body encounter signatures detected in GW170817, GW190814, and GW230627_015337, constraining intermediate-mass black holes above 100 solar masses within roughly 0.1 AU of these binaries.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Comparison between the perturbed (h pert) and vacuum (h vac) GW polarisations for the same configuration shown in Fig. 3. The upper panels show the plus and cross polarisations evolved up to ISCO, while the lower panels display the residual δh=h pert −h vac. The fly-by interaction produces a cumulative phase deformation that becomes more pronounced toward late times. The explicit form of the 2.5PN radiation-reaction ac- celeration is given by [81, 82] a2.5PN 1 = 4 5c5 G2m1m2 r3 \"\u00122G r (m1 −4m 2)−v 2 \u0013 v + r·v r \u001252Gm2 3r − 6Gm1 r + 3v2 \u0013 r r # , (9) and a2.5PN 2 =− 4 5c5 G2m1m2 r3 \"\u00122G r (m2 −4m 1)−v 2 \u0013 v + r·v r \u001252Gm1 3r − 6Gm2 r + 3v2 \u0013 r r # , (10) wherev=|v|andcis the speed of light. No conserva- tive post-Newtonian corrections are included; radiation- reaction acts only within the compact binary, and no"},{"citing_arxiv_id":"2604.19726","ref_index":8,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Breaking the UV Luminosity Function Degeneracy:Self-Interacting Dark Matter Constraints from Reionization Topology","primary_cat":"astro-ph.CO","submitted_at":"2026-04-21T17:50:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"21 cm reionization topology breaks the degeneracy between self-interacting dark matter and astrophysical parameters that limits UV luminosity function constraints, enabling robust SIDM limits of σ/m ≳ 1-2 cm²/g independent of star formation models.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"0007 [astro-ph.CO]. [5] A. A. Klypin, A. V. Kravtsov, O. Valenzuela, and F. Prada, Astrophys. J.522, 82 (1999), arXiv:astro- ph/9901240. [6] A. Kamada, M. Kaplinghat, A. B. Pace, and H.-B. Yu, Phys. Rev. Lett.119, 111102 (2017), arXiv:1611.02716 [astro-ph.GA]. [7] C. A. Correa, Mon. Not. Roy. Astron. Soc.503, 920 (2021), arXiv:2007.02958 [astro-ph.GA]. [8] D. N. Spergel and P. J. Steinhardt, Phys. Rev. Lett.84, 3760 (2000), arXiv:astro-ph/9909386. [9] S. Tulin and H.-B. Yu, Phys. Rept.730, 1 (2018), arXiv:1705.02358 [hep-ph]. [10] M. Kaplinghat, S. Tulin, and H.-B. Yu, Phys. Rev. Lett. 116, 041302 (2016), arXiv:1508.03339 [astro-ph.CO]. [11] M. Markevitch, A. H. Gonzalez, D. Clowe, A. Vikhlinin, L. David, W."},{"citing_arxiv_id":"2604.12189","ref_index":20,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing Collapsed Dark Matter Halos with Fast Radio Bursts","primary_cat":"astro-ph.CO","submitted_at":"2026-04-14T01:41:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Core-collapsed SIDM halos produce longer FRB image time delays than CDM halos, enabling future surveys to constrain self-interaction cross sections above roughly 18-40 cm²/g depending on collapse timing.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Peter, X. Du, S. Yang, A. Benson, F.-Y. Cyr-Racine, F. Jiang, C. Mace, and R. B. Met- calf, Phys. Rev. D 111, 063001 (2025), arXiv:2310.09910 [astro-ph.GA]. [18] D. Yang, E. O. Nadler, H.-B. Yu, and Y.-M. Zhong, JCAP 02, 032 (2024), arXiv:2305.16176 [astro-ph.CO]. [19] W. J. G. de Blok, Adv. Astron. 2010, 789293 (2010), arXiv:0910.3538 [astro-ph.CO]. [20] M. Boylan-Kolchin, J. S. Bullock, and M. Kapling- hat, Mon. Not. Roy. Astron. Soc. 415, L40 (2011), arXiv:1103.0007 [astro-ph.CO]. [21] D. Gilman, J. Bovy, T. Treu, A. Nierenberg, S. Birrer, A. Benson, and O. Sameie, Mon. Not. Roy. Astron. Soc. 507, 2432 (2021), arXiv:2105.05259 [astro-ph.CO]. [22] D. Gilman, Y.-M. Zhong, and J. Bovy, Phys. Rev. D"},{"citing_arxiv_id":"2604.10726","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Reionization Topology as a Probe of Self-Interacting Dark Matter","primary_cat":"astro-ph.CO","submitted_at":"2026-04-12T16:59:09+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Self-interacting dark matter increases the Euler characteristic of the reionization ionization field by 60-70% for cross-sections above 2 cm2/g through changes in ionizing source populations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Oh, C. Brook, F. Governato, E. Brinks, L. Mayer, W. J. G. de Blok, A. Brooks, and F. Walter, The central slope of dark matter cores in dwarf galaxies: Simulations vs. THINGS, Astron. J. 142, 24 (2011), arXiv:1011.2777 [astro-ph.CO]. [3] B. Moore, Evidence against dissipationless dark mat- ter from observations of galaxy haloes, Nature 370, 629 (1994). [4] W. J. G. de Blok, The Core-Cusp Problem,Adv. Astron. 2010, 789293 (2010), arXiv:0910.3538 [astro-ph.CO]. [5] M. Boylan-Kolchin, J. S. Bullock, and M. Kaplinghat, Too big to fail? The puzzling darkness of massive Milky Way subhaloes, Mon. Not. Roy. Astron. Soc. 415, L40 (2011), arXiv:1103.0007 [astro-ph.CO]. [6] A. A. Klypin, A. V. Kravtsov, O. Valenzuela, and"},{"citing_arxiv_id":"2601.17117","ref_index":131,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Non-Equilibrium Relativistic Core Collapse of Self-Interacting Dark Matter Halos -- Limits On Seed Black Hole Mass","primary_cat":"astro-ph.CO","submitted_at":"2026-01-23T19:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Non-equilibrium relativistic SIDM halo collapse produces seed black holes of mass ~3e-8 of the halo mass at apparent horizon formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.18959","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Scalar-Mediated Inelastic Dark Matter as a Solution to Small-Scale Structure Anomalies","primary_cat":"hep-ph","submitted_at":"2025-12-22T02:16:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A scalar-mediated inelastic dark matter model with 100 eV splitting, Z2 symmetry forbidding elastic scattering, and a dimension-5 dipole operator reconciles dwarf galaxy observations with cosmological bounds via resonant enhancement and provides a distinct direct detection signal.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.16971","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing Dark Matter Substructure with Image Number Anomaly in Strong Lensing Systems","primary_cat":"astro-ph.CO","submitted_at":"2025-11-21T05:54:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Null detection of extra lensed images in 3500 mock systems constrains PBH abundance to ≲0.04-0.125% and excludes FDM masses below 0.4-3.5×10^{-22} eV at 95% CL depending on angular resolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.09306","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Self-Interaction of Super-Resonant Dark Matter","primary_cat":"hep-ph","submitted_at":"2025-11-12T13:17:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Super-resonant dark matter at O(100) GeV masses amplifies self-scattering and annihilation cross sections via combined resonance and Sommerfeld effects, necessitating coupled Boltzmann equations to match observed relic density.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2407.01690","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Structure-wide dark matter density depletion induced by local degeneracies","primary_cat":"astro-ph.GA","submitted_at":"2024-07-01T18:02:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Degeneracy-induced depletion from fermionic DM in subhalos creates structure-wide low-density cores consistent with observations, linking profile diversity to formation history.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1906.10316","ref_index":20,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraining light fermionic dark matter with binary pulsars","primary_cat":"astro-ph.GA","submitted_at":"2019-06-25T04:15:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Dynamical friction from a degenerate fermionic dark matter background induces measurable secular decay in binary pulsar orbital periods, with sensitivity to fermion masses ≳50 eV and example upper bounds around 1 keV from Milky Way data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}