{"total":13,"items":[{"citing_arxiv_id":"2606.27479","ref_index":114,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Bright Future of the Dark and Dim Universe","primary_cat":"astro-ph.GA","submitted_at":"2026-06-25T18:57:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Review chapter on SKA observations of RELHICs and dim galaxies to constrain LambdaCDM and baryonic physics via HIMF, HIVF, and bTFR down to 10^6 solar masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26445","ref_index":105,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Columba: isolated dwarf galaxy populations in diverse cosmological environments simulated with a cold interstellar medium","primary_cat":"astro-ph.GA","submitted_at":"2026-06-24T23:14:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New hydrodynamical simulations show that dwarf galaxy stellar mass-halo mass relations and star formation histories are more influenced by host halo concentration than by the 5 cMpc scale environment.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17176","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tracing Ultra Light Axions in Post-reionization, Lyman-$\\alpha$ and CMB Missions","primary_cat":"astro-ph.CO","submitted_at":"2026-06-15T18:15:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Fisher forecasts indicate joint post-reionization LSS cross-spectra and CMB-S4-like data can reach O(10^{-4}) uncertainty on ultra-light axion fraction for m_a ≲ 10^{-28} eV, with peak sensitivity near 10^{-25} eV.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10020","ref_index":187,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Manticore Project II: Bayesian digital twins of cosmic structure across the SDSS and BOSS volumes","primary_cat":"astro-ph.CO","submitted_at":"2026-06-08T18:07:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Manticore-Deep uses tiled Bayesian field-level inference on SDSS and BOSS data to produce posterior ensembles of 3D cosmic fields that are consistent with LCDM and validated by 7.4σ CMB lensing and 3.5σ kSZ detections.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06599","ref_index":27,"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":9,"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":"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 We construct the joint log-likelihood. For the Thom- son optical depth and the six Gaussian neutral-fraction points (Table 1) we use standardχ 2 terms. For the two one-sided constraints (z= 9.5 andz= 11; Table 1) we penalise only models that predict ¯xHI below the observed"},{"citing_arxiv_id":"2606.00221","ref_index":10,"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":"2605.18975","ref_index":48,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bulgeless Evolution And the Rise of Discs (BEARD) III. A numerical simulation view of satellites around Milky-Way analogues","primary_cat":"astro-ph.GA","submitted_at":"2026-05-18T18:01:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulation comparison finds bulgeless galaxies host more centrally concentrated, disc-aligned satellites with steeper faint-end luminosity functions than bulge-dominated controls, reflecting co-evolution and quieter merger histories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02172","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constraints on Ultralight Scalar and Dark Photon Dark Matter from PPTA-DR3 and EPTA-DR2","primary_cat":"astro-ph.CO","submitted_at":"2026-05-04T03:05:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian analysis of PPTA-DR3 and EPTA-DR2 finds no statistically significant ULDM signals and sets 95% CL upper limits on scalar and dark photon dark matter, improving prior bounds in most mass ranges.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Constraints on Singular Dark Matter Halos,\" Astrophys. J. Lett. 427, L1 (1994), arXiv:astro-ph/9402004. [4] B. Moore, \"Evidence against dissipation-less dark matter from observations of galaxy haloes,\" Nature370, 629 (1994). [5] A. Klypin, A. V. Kravtsov, O. Valenzuela, and F. Prada, \"Where Are the Missing Galactic Satellites?\" Astrophys. J.522, 82 (1999), arXiv:astro-ph/9901240. [6] B. Moore, S. Ghigna, F. Governato, G. Lake, T. Quinn, J. Stadel, and P. Tozzi, \"Dark Matter Substructure within Galactic Halos,\" Astrophys. J. Lett.524, L19 (1999), arXiv:astro-ph/9907411. [7] 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),"},{"citing_arxiv_id":"2604.26072","ref_index":39,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Caught in the Cosmic Web: Environmental Impacts on the Halo Substructure Boosts to Dark Matter Annihilation Signals","primary_cat":"astro-ph.CO","submitted_at":"2026-04-28T19:21:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"At fixed host-halo mass, filament halos show mass-dependent boost modulation from 15% suppression to 12% enhancement, walls are intermediate, and void halos are suppressed by 30-33% relative to the cosmic-mean prediction.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"structure of the host halo and the modulation imposed by the large-scale cosmic web, which can substantially affect the predicted DM annihilation signal. D. Subhalo concentration The internal density structure of subhalos strongly in- fluences their contribution to the DM annihilation signal. We characterize subhalo compactness using the charac- teristic concentration,c v, defined as [39, 40, 79]: cv = 2 \u0012 Vmax H0Rmax \u00132 ,(8) whereV max is the maximum circular velocity,Rmax the radius at which it occurs, andH0 the Hubble constant, includedsothatc v remainsadimensionlessconcentration proxy. This definition is particularly suitable for subha- los, whose outer regions are often stripped tidally and lack well-defined virial radii. Unlike traditional mass-"},{"citing_arxiv_id":"2604.10726","ref_index":6,"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":"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 F. Prada, Where are the missing Galactic satellites?,As- trophys. J. 522, 82 (1999), arXiv:astro-ph/9901240. [7] A. Kamada, M. Kaplinghat, A. B. Pace, and H.-B. Yu, How the Self-Interacting Dark Matter Model Explains the Diverse Galactic Rotation Curves, Phys. Rev. Lett. 119, 111102 (2017), arXiv:1611."},{"citing_arxiv_id":"2512.18959","ref_index":20,"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":4,"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}],"limit":50,"offset":0}