{"total":11,"items":[{"citing_arxiv_id":"2606.26218","ref_index":256,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark Matter in Draco and Bo\\\"otes I: Hints of a Core in an Ultra-Faint Dwarf from Simulation-Based Inference","primary_cat":"astro-ph.GA","submitted_at":"2026-06-24T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"GraphNPE recovers a significantly lower central density for Boötes I consistent with a core while Draco remains marginally cuspy, and demonstrates that higher-order velocity moments reduce bias in dynamical modeling.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04827","ref_index":16,"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":"background","top_context_polarity":"background","context_text":"luminosity-weighted value of 0.13. We conclude that αz ∼2 is a data-driven result, not a prior artifact. 7.6.Broken power-law test We test whether the data prefer a more flexible broken power-law model,f esc(Mh)∝M αM,lo h below Mh = 10 9.5 M⊙ and∝M αM,hi h above-motivated by SPHINX's prediction of a steepening below 10 9.5 M⊙ Table 6.Prior Sensitivity forα z αz prior Median [16%,84%] [−1,3] (fiducial) 1.98 [1.30,2.55] [−1,5] 2.01 [1.51,2.56] [−2,8] 2.21 [1.46,2.63] [0,3] 1.74 [1.26,2.28] (Rosdahl et al. 2022). Scanning over the four-parameter space (f0, αM,lo, αM,hi, αz) at fixed break mass, the best fit achievesχ 2 = 7.80, an improvement of only ∆χ 2 = 0.21 over the single power-law (χ 2 = 8.0). With one additional degree of freedom, this is far from significant"},{"citing_arxiv_id":"2605.27513","ref_index":37,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on a Light Leptophilic Scalar from Dark-Sector Couplings","primary_cat":"hep-ph","submitted_at":"2026-05-26T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"A parameter space analysis of a leptophilic scalar mediator model for Majorana dark matter yields a viable sub-GeV region after applying relic density, cosmological, astrophysical, and laboratory constraints.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19873","ref_index":21,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Self-Interaction and Galactic Magnetic Field Bounds on Millicharged Magnetic Monopole Dark Matter","primary_cat":"hep-ph","submitted_at":"2026-04-21T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Self-interaction constraints and the Parker effect from galactic magnetic fields bound the kinetic mixing and other parameters of millicharged magnetic monopole dark matter.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"JHEP03, 105 (2022), arXiv:2105.05769 [hep-ph]. [19] M. Rocha, A. H. G. Peter, J. S. Bullock, M. Kapling- hat, S. Garrison-Kimmel, J. Onorbe, and L. A. Mous- takas, Mon. Not. Roy. Astron. Soc.430, 81 (2013), arXiv:1208.3025 [astro-ph.CO]. [20] A. H. G. Peter, M. Rocha, J. S. Bullock, and M. Kapling- hat, Mon. Not. Roy. Astron. Soc.430, 105 (2013), arXiv:1208.3026 [astro-ph.CO]. [21] R. Lasenby, JCAP11, 034 (2020), arXiv:2007.00667 [hep-ph]. [22] A. Cruz and M. McQuinn, JCAP04, 028 (2023), arXiv:2202.12464 [astro-ph.CO]. [23] W. DeRocco and P. Giffin, Phys. Rev. D111, 095031 (2025), arXiv:2411.11958 [hep-ph]. [24] E. N. Parker, Astrophys. J.160, 383 (1970). [25] M. S. Turner, E. N. Parker, and T. J. Bogdan, Phys. Rev. D26, 1296 (1982)."},{"citing_arxiv_id":"2604.19726","ref_index":20,"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":"method","top_context_polarity":"use_method","context_text":"Sutanto, K. Takahashi, and B. Vulcani, \"Beacon: Jwst nircam pure-parallel imaging survey. iii. constraints on the uv lf and the clustering of z 7-14 galax- ies,\" (2026), arXiv:2604.17963 [astro-ph.GA]. [18] Z. Wang, (2026), arXiv:2604.10726 [astro-ph.CO]. [19] C. Mason, M. Trenti, and T. Treu, Astrophys. J.813, 21 (2015), arXiv:1508.01204 [astro-ph.GA]. [20] R. H. Wechsler and J. L. Tinker, Ann. Rev. Astron. As- trophys.56, 435 (2018), arXiv:1804.03097 [astro-ph.GA]. [21] R. K. Sheth and G. Tormen, Mon. Not. Roy. Astron. Soc. 308, 119 (1999), arXiv:astro-ph/9901122. [22] R. C. Kennicutt, Jr., Ann. Rev. Astron. Astrophys.36, 189 (1998), arXiv:astro-ph/9807187. [23] R. Endsley, D. P. Stark, L. Whitler, M."},{"citing_arxiv_id":"2604.08647","ref_index":58,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Bypassed Core Formation in Milky Way-Mass SIDM Halos: Implications for the Local Group Past-Pericenter Scenario","primary_cat":"astro-ph.GA","submitted_at":"2026-04-09T17:59:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"MW-mass SIDM halos bypass core formation and enter immediate core collapse due to baryonic preconditioning, allowing the compact stellar disk and bulge to survive close pericenter passages while the diffuse halo is more easily disrupted.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Halo shapes versus observations, Mon. Not. Roy. Astron. Soc.430, 105 (2013), arXiv:1208.3026 [astro-ph.CO]. [57] A. Robertson, D. Harvey, R. Massey, V. Eke, I. G. McCarthy, M. Jauzac, B. Li, and J. Schaye, Observable tests of self- interactingdarkmatteringalaxyclusters: cosmologicalsimu- lations with SIDM and baryons, Mon. Not. Roy. Astron. Soc. 488, 3646 (2019). [58] A. McDaniel, T. Jeltema, and S. Profumo, X-ray shapes of elliptical galaxies and implications for self-interacting dark matter, JCAP2021(5), 020. [59] J. Merten, D. Coe, R. Dupke, R. Massey, A. Zitrin, E. S. Cypriano, N. Okabe, B. Frye, F. G. Braglia, Y. Jiménez- Teja, N. Benítez, T. Broadhurst, J. Rhodes, M. Meneghetti, L. A. Moustakas, L. Sodré, Jr."},{"citing_arxiv_id":"2602.02678","ref_index":42,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Axion-Like Electrophilic Portal for Pion Dark Matter","primary_cat":"hep-ph","submitted_at":"2026-02-02T19:00:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A minimal electrophilic ALP portal for SIMP pion dark matter widens the allowed parameter space, making an ALP mass of order 10 MeV viable and consistent with the X17 anomaly.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.17117","ref_index":77,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the scale height that corresponds to the local dynamical time H= p v2/(4πρ). In the short mean free path (SMFP) regime, whereλ≪H, the conductivity follows the stan- dard formκ SMFP =(3/2)bρλ 2/(amt0). Here, the constants area= √16/πandb=25 √π/32 [108], whilet 0 =λ/(av) is the relaxation time. Conversely, in the long mean free path (LMFP) regime (λ≫H), heat transport is described by κLMFP =(3/2)CρH 2/(mt0) [77], whereCserves as a calibra- tion parameter. Following Koda and Shapiro [89], we adopt C=0.75, a value that enables the fluid evolution to match N-body simulation results. To smoothly interpolate between these two limits, the effective conductivity is constructed as κ−1 =κ −1 SMFP +κ −1 LMFP [72]. In the LMFP regime, heat flux is di- rectly proportional to the collision rate, so thatκ∝σ; while in"},{"citing_arxiv_id":"2512.18959","ref_index":27,"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":"2504.17064","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Imprints of energy injection by compact dark stars in the 21-cm signal","primary_cat":"hep-ph","submitted_at":"2025-04-23T19:17:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Compact dark stars from asymmetric dark matter may inject energy that significantly deviates the 21-cm brightness temperature evolution from standard cosmology, offering a new probe for particle dark matter.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2005.01515","ref_index":70,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Dark Photon","primary_cat":"hep-ph","submitted_at":"2020-05-04T14:31:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The paper surveys theoretical motivations, experimental searches, and bounds on the dark photon as a kinetically mixed gauge boson from a dark sector, covering both massive and massless cases along with related milli-charged fermion constraints.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Kaplinghat, \"Cosmological Simulations with Self-Interacting Dark Matter II: Halo Shapes vs. Observations,\"Mon. Not. Roy. Astron. Soc. 430 (2013) 105, arXiv:1208.3026 [astro-ph.CO] . [69] M. Pospelov and T. ter Veldhuis, \"Direct and indirect limits on the electromagnetic form-factors of WIMPs,\" Phys. Lett. B 480 (2000) 181-186, arXiv:hep-ph/0003010. [70] K. Sigurdson, M. Doran, A. Kurylov, R. R. Caldwell, and M. Kamionkowski, \"Dark-matter electric and magnetic dipole moments,\"Phys. Rev. D70 (2004) 083501, arXiv:astro-ph/0406355 [astro-ph]. [Erratum: Phys. Rev.D73,089903(2006)]. [71] T. Banks, J.-F. Fortin, and S. Thomas, \"Direct Detection of Dark Matter Electromagnetic Dipole Moments,\" arXiv:1007."}],"limit":50,"offset":0}