{"total":23,"items":[{"citing_arxiv_id":"2606.29710","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Size Dependence of the Sommerfeld Enhancement for Puffy Dark Matter","primary_cat":"hep-ph","submitted_at":"2026-06-29T02:27:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Finite size of puffy dark matter is identified as a fundamental factor affecting Sommerfeld enhancement, characterized via two dimensionless parameters, with nugget-type DM showing resonant behavior akin to point-like particles.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25537","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing the Fundamental Nature of Particle Dark Matter","primary_cat":"astro-ph.CO","submitted_at":"2026-06-24T08:13:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Review summarizing radio searches for WIMP and ALP dark matter with SKA precursors and forecasts for SKA-Low and SKA-Mid telescopes.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"clusters) and convection, since their effects are often subdominant in the context of DM searches. The total synchrotron emissivity at a given frequency𝜈is obtained by folding the𝑒+ +𝑒 − number density𝑛 𝑒 with the total radiative emission power𝑃𝑠𝑦𝑛𝑐ℎ over the electron/position energy𝐸 (Rybicki and Lightman, 1986): 𝑗𝑠𝑦𝑛𝑐ℎ (𝜈, 𝑟)= ∫ 𝑑𝐸 𝑃 𝑠𝑦𝑛 (𝑟, 𝐸, 𝜈)𝑛 𝑒 (𝑟, 𝐸)(4) ForthetypicalsystemsconsideredinWIMPsearches,absorptionalongthelineofsightandwithin the source can be disregarded. The flux density measured with the SKA telescopes can be estimated as 𝑆𝑡 ℎ(𝜈, 𝜃 0)= ∫ 𝑑𝜙 𝑑𝜃sin𝜃G (𝜃, 𝜙, 𝜃 0) ∫ 𝑑ℓ 𝑗𝑠𝑦𝑛𝑐ℎ (𝜈, 𝑟(ℓ, 𝜃, 𝜙)) 4𝜋 ,(5) whereℓlabels the coordinate along the line of sight,𝜃and𝜙describe the polar and azimuthal"},{"citing_arxiv_id":"2605.27521","ref_index":81,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"From WIMP to FIMP during reheating: collider vs non-collider probes for p-wave annihilation","primary_cat":"hep-ph","submitted_at":"2026-05-26T18:00:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Collider experiments can strongly constrain p-wave-suppressed derivative operators and thereby limit reheating temperature, DM mass, and interaction scale needed to match observed DM abundance during reheating.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[78]Planckcollaboration,Planck 2018 results. VI. Cosmological parameters,Astron. Astrophys. 641(2020) A6 [1807.06209]. [79] K. Kaneta, Y. Mambrini and K.A. Olive,Radiative production of nonthermal dark matter, Phys. Rev. D99(2019) 063508 [1901.04449]. - 46 - [80] B. Barman, A. Ghoshal, B. Grzadkowski and A. Socha,Measuring Inflaton Couplings via Primordial Gravitational Waves,2305.00027. [81] M.W. Goodman and E. Witten,Detectability of certain dark-matter candidates,Phys. Rev. D 31(1985) 3059. [82] J.D. Lewin and P.F. Smith,Review of mathematics, numerical factors, and corrections for dark matter experiments based on elastic nuclear recoil,Astroparticle Physics6(1996) 87. [83] G. Jungman, M. Kamionkowski and K. Griest,Supersymmetric dark matter,Phys."},{"citing_arxiv_id":"2605.22245","ref_index":52,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing freeze-in dark matter using Bose-Einstein condensate in neutron star","primary_cat":"hep-ph","submitted_at":"2026-05-21T09:51:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bose-Einstein condensate formation in neutron stars enhances dark matter annihilation by 10^15-10^20, allowing freeze-in models to produce observable heating and probe neutrino-fog scattering cross-sections.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16994","ref_index":64,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Determination of the best dark matter profile for the Milky Way with Gaia DR3 using Bayesian Model Comparison","primary_cat":"astro-ph.GA","submitted_at":"2026-05-16T13:42:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian comparison of Gaia DR3 rotation curves favors the Einasto dark matter profile over NFW, prefers cored over cuspy profiles, and finds MOND variants provide poorer fits than the best dark matter models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.10467","ref_index":1,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Axial Quasi-normal Modes of Admixed Neutron Stars","primary_cat":"hep-ph","submitted_at":"2026-05-11T12:33:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Increasing the bosonic dark matter fraction in admixed neutron stars shifts axial quasi-normal mode frequencies and damping times, can reorder mode hierarchy, and drives a transition from neutron-star-like to boson-star-like ringdown behavior.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"realistic dynamical scenarios, including tidally deformed stars, rotating configurations, and merger remnants. These extensions will be important for assessing the detectability of the distinctive spectral patterns predicted in this work with third-generation gravitational-wave observatories. Acknowledgments The work of BBK is supported by IBS under the project code IBS-R018-D3. References [1] G. Jungman, M. Kamionkowski, and K. Griest,Supersymmetric dark matter,Phys. Rept.267 (1996) 195-373, [hep-ph/9506380]. - 25 - [2] G. Bertone, D. Hooper, and J. Silk,Particle dark matter: Evidence, candidates and constraints, Phys. Rept.405(2005) 279-390, [hep-ph/0404175]. [3] L. Bergstr¨ om,Nonbaryonic dark matter: Observational evidence and detection methods,Rept."},{"citing_arxiv_id":"2605.07616","ref_index":44,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing the Inert Doublet Dark Matter with Stellar-Mass Black Hole Mini-Spikes","primary_cat":"hep-ph","submitted_at":"2026-05-08T11:43:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Fermi LAT data on mini-spikes around stellar-mass black holes rules out substantial regions of Inert Doublet Model dark matter parameter space, especially at multi-TeV masses.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Indirect detection offers a complementary probe of dark matter by searching for the stable products of its annihilation in astrophysical environments. The strength of such signals depends sensitively on the dark matter density, as the annihilation rate scales with its square, making compact and highly concentrated systems particularly attractive targets [44]. In this context, stellar-mass black holes (sBHs) can act as efficient enhancers of annihilation signals. The gravitational potential of a black hole can significantly distort the surrounding dark matter distribution, increasing the density in its vicinity and thereby enhancing the expected gamma-ray flux. In this work, we adopt the framework developed in Ref."},{"citing_arxiv_id":"2604.26072","ref_index":5,"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":"background","top_context_polarity":"background","context_text":"Villa, N. Vittorio, B. D. Wandelt, I. K. We- hus, M.White, S.D.M.White, A.Zacchei,andA.Zonca, 14 A&A641, A6 (2020), arXiv:1807.06209 [astro-ph.CO]. [3] B. Carr and F. Kuhnel, arXiv e-prints , arXiv:2110.02821 (2021), arXiv:2110.02821 [astro-ph.CO]. [4] G. Jungman, M. Kamionkowski, and K. Griest, Phys. Rep.267, 195 (1996), arXiv:hep-ph/9506380 [hep- ph]. [5] G. Bertone, D. Hooper, and J. Silk, Phys. Rep.405, 279 (2005), arXiv:hep-ph/0404175 [hep-ph]. [6] T. Bringmann and C. Weniger, Physics of the Dark Uni- verse1, 194 (2012), arXiv:1208.5481 [hep-ph]. [7] L. Roszkowski, E. M. Sessolo, and S. Trojanowski, Re- ports on Progress in Physics81, 066201 (2018). [8] S. J. Asztalos, L. J. Rosenberg, K. van Bibber, P."},{"citing_arxiv_id":"2604.26005","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Asteroid-mass Primordial Black Holes as Dark Matter from Supersymmetry","primary_cat":"hep-ph","submitted_at":"2026-04-28T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Supersymmetry with heavy particles above ~10^5 GeV enhances asteroid-mass PBH production via transient equation-of-state softening, allowing them to comprise all dark matter unlike in the Standard Model.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Caravano for insight- ful discussions on PBH formation and inflation. We ac- knowledge the support by the research project TAsP (Theoretical Astroparticle Physics) funded by the Isti- tuto Nazionale di Fisica Nucleare (INFN). [1] G. Jungman, M. Kamionkowski, and K. Griest, Super- symmetric dark matter, Phys. Rept.267, 195 (1996), arXiv:hep-ph/9506380. [2] G. Bertone, D. Hooper, and J. Silk, Particle dark mat- ter: Evidence, candidates and constraints, Phys. Rept. 405, 279 (2005), arXiv:hep-ph/0404175. [3] D. J. E. Marsh, Axion Cosmology, Phys. Rept.643, 1 (2016), arXiv:1510.07633 [astro-ph.CO]. [4] K. Choi, S. H. Im, and C. Sub Shin, Recent Progress in the Physics of Axions and Axion-Like Particles, Ann."},{"citing_arxiv_id":"2604.21976","ref_index":32,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cosmic-Ray Signatures of Annihilating and Semi-Annihilating Dark Matter via One-Step Cascades","primary_cat":"hep-ph","submitted_at":"2026-04-23T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A largely model-independent framework links dark matter annihilation, mediator decays, and semi-annihilation to both thermal freeze-out and present-day gamma-ray, neutrino, and antimatter fluxes, with benchmarks showing how their relative strengths shape observable spectra.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"there is no matter-antimatter asymmetry in the dark sector, such that the number densities satisfyn S =n S⋆. We track the evolution of the DM particleSabundance; the total DM number density then differs only by an overall factor of2. The fundamental tool to describe the evolution of the DM number density is the Boltzmann equation, which takes the general form (see, e.g., Refs. [32, 35, 36] for a complete derivation) dnS dt + 3HnS =−Σ ann \u0010 n2 S −n eq 2 S \u0011 −Σ semi n2 S −n Sneq S \u0001 .(2.3) The left-hand side of the Boltzmann equation encodes the effect of the expansion of the universe through the Hubble parameterH. We assume that DM production takes place during the radiation-dominated epoch, in which the Hubble rate scales with the temperature"},{"citing_arxiv_id":"2604.20456","ref_index":7,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"How Invisible: Regressing The Key Model Parameter for Semi-visible Jet Searches","primary_cat":"hep-ph","submitted_at":"2026-04-22T11:25:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A regression model reconstructs the key parameter r_inv for semi-visible jets at higher precision than prior analytical methods and may unify s- and t-channel production searches.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[4]DEScollaboration,Dark Energy Survey Year 1 Results: Curved-Sky Weak Lensing Mass Map,Mon. Not. Roy. Astron. Soc.475(2018) 3165 [1708.01535]. [5]Planckcollaboration,Planck 2018 results. VI. Cosmological parameters,Astron. Astrophys.641(2020) A6 [1807.06209]. [6] G. Jungman, M. Kamionkowski and K. Griest,Supersymmetric dark matter,Phys. Rept. 267(1996) 195 [hep-ph/9506380]. [7]ATLAScollaboration,Search for new phenomena in events with an energetic jet and missing transverse momentum inppcollisions at √s=13 TeV with the ATLAS detector, Phys. Rev. D103(2021) 112006 [2102.10874]. [8]CMScollaboration,Search for new particles in events with energetic jets and large missing transverse momentum in proton-proton collisions at √s= 13 TeV,JHEP11(2021) 153"},{"citing_arxiv_id":"2604.18007","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"In-depth analysis of the clustering of dark matter particles around primordial black holes. Part III: CMB constraints","primary_cat":"astro-ph.CO","submitted_at":"2026-04-20T09:30:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"CMB data limits the s-wave annihilation cross section of thermal dark matter particles to ≲ 10^{-30} cm³/s scaled by PBH fraction and mass for PBHs heavier than ~10^{-10} solar masses.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"xkd = 102 / bb xkd = 104 / bb xkd = 102 / + xkd = 104 / + Figure 9. Posterior distributions of the MCMC parameters and their correlations, in the case the DM fraction in BHsf BH is let free. This example is for BHs of 10 −4M⊙. References [1] P. J. E. Peebles,Primeval adiabatic perturbations - effect of massive neutrinos,ApJ258(July, 1982) 415-424. [2] G. Jungman, M. Kamionkowski and K. Griest,Supersymmetric dark matter,Phys. Rep.267 (Mar., 1996) 195-373, [hep-ph/9506380]. [3] J. L. Feng,Dark Matter Candidates from Particle Physics and Methods of Detection,ARA&A 48(Sept., 2010) 495-545, [1003.0904]. [4] M. Cirelli, A. Strumia and J. Zupan,Dark matter,arXiv e-prints(June, 2024) arXiv:2406.01705, [2406."},{"citing_arxiv_id":"2604.17869","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing Cosmic-Ray-Boosted and Supernova-Sourced Sub-GeV Dark Matter with Paleo-Detectors","primary_cat":"hep-ph","submitted_at":"2026-04-20T06:30:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Paleo-detectors can achieve high sensitivity to sub-GeV dark matter boosted by cosmic rays and supernovae, covering previously inaccessible parameter space with orders of magnitude better reach than current experiments.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"YSBR-092), and the China Manned Space Program (grant No. CMS-CSST-2025-A03). X.C. is funded by the National Natural Science Foundation of China (grant No. E4146602 and No. 12547104), and the Fundamental Research Funds for the Central Universities (grant 12 No. E4EQ6605X2 and E5ER6601A2). [1] B. W. Lee and S. Weinberg, Phys. Rev. Lett.39, 165 (1977). [2] G. Jungman, M. Kamionkowski, and K. Griest, Phys. Rept.267, 195 (1996), hep-ph/9506380. [3] J. Chang et al., Nature456, 362 (2008). [4] F. Aharonian et al. (H.E.S.S.), Astron. Astrophys.508, 561 (2009), 0905.0105. [5] O. Adriani et al. (PAMELA), Nature458, 607 (2009), 0810.4995. [6] D. Hooper and L. Goodenough, Phys. Lett. B697, 412 (2011), 1010.2752."},{"citing_arxiv_id":"2604.15541","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing inelastic sub-GeV dark matter at the DUNE near detector","primary_cat":"hep-ph","submitted_at":"2026-04-16T21:46:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"DUNE's ND-LAr can probe sub-GeV inelastic dark matter parameter space consistent with relic abundance via dark Higgs-mediated annihilation, especially at large dark photon-to-DM mass ratios.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"3 Simulation of DM interactions at the ND 9 3.4 Statistical analysis for DUNE's sensitivity 11 4 Results 12 5 Conclusions 14 1 Introduction Despite the overwhelming evidence of the existence of Dark Matter (DM) [1] and large efforts to understand its properties, the DM nature remains unknown. Weakly interacting massive particles (WIMPs) have been the most widely studied candidates [2, 3]. They naturally arise in beyond the Standard Model (SM) theories with the additional advantage of being thermally produced and allow for their detection through different search strategies-actually WIMPs have been the primary target of experimental searches for decades [4-6]. However, the absence of signals at the electroweak scale from direct detection (DD) [7-9] and collider"},{"citing_arxiv_id":"2601.06457","ref_index":51,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Physical implications of a double right-handed gauge symmetry","primary_cat":"hep-ph","submitted_at":"2026-01-10T06:52:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A double right-handed U(1) gauge extension generates the Standard Model fermion mass hierarchy at tree and loop levels and stabilizes a viable scalar singlet dark matter particle consistent with relic density and direct detection bounds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.07567","ref_index":49,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark Matter Heating in Evolving Proto-Neutron Stars: A Two-Fluid Approach","primary_cat":"astro-ph.HE","submitted_at":"2025-11-10T19:22:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Dark matter cores heat baryonic matter in evolving proto-neutron stars by deepening the gravitational potential while halos cool it, providing a diagnostic distinct from hyperons.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.07511","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Seasons of Dark Matter Freeze-In Shaped by the Weather of the Early Universe","primary_cat":"hep-ph","submitted_at":"2025-11-10T19:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Variations in pre-nucleosynthesis cosmology produce distinct seasons in the phase-space distribution of freeze-in dark matter, directly affecting its warmness and mass bounds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.07070","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reviving WIMP dark matter with temperature-dependent couplings","primary_cat":"hep-ph","submitted_at":"2025-09-08T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Temperature-dependent DM couplings mediated by a scalar field's VEV that drops after a first-order phase transition allow sufficient early-universe annihilations for the observed relic density while evading current direct detection bounds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.20932","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Novel probes for electron-muon flavor violation from exotic Higgs decays","primary_cat":"hep-ph","submitted_at":"2025-08-28T15:57:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Novel multilepton signatures from Higgs decays to a light pseudoscalar decaying to e-mu pairs in type-III 2HDM can set stronger limits on LFV couplings than low-energy experiments.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.08676","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"WIMP Dark Matter within the dark photon portal","primary_cat":"hep-ph","submitted_at":"2025-08-12T06:50:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Derives lower limits on dark photon parameters from thermal relic density for Dirac fermion and complex scalar WIMPs and compares resulting spin-independent cross sections to direct detection upper bounds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.01895","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Freeze-In Dark Matter and Leptogenesis: a $\\psi'$SM route","primary_cat":"hep-ph","submitted_at":"2025-07-02T17:09:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"In an E6-derived ψ'SM extension, a singlet fermion acts as freeze-in dark matter with relic density set by scalar decays for masses from a few MeV to hundreds of GeV, while type-I seesaw neutrinos simultaneously produce the observed baryon asymmetry via leptogenesis.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2312.11704","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Ultralight dark matter in long-baseline accelerator neutrino oscillations","primary_cat":"hep-ph","submitted_at":"2023-12-18T21:04:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Systematic study of scalar and vector ULDM interactions on long-baseline neutrino oscillations finds order-of-magnitude weaker constraints for m_φ ≲ 10^{-17} eV due to stochastic effects, with combined T2K+NOvA data showing no alleviation of δ_CP discrepancy.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.08010","ref_index":202,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological searches for the neutrino mass scale and mass ordering","primary_cat":"astro-ph.CO","submitted_at":"2019-07-18T12:03:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Thesis summarizing an upper limit of 0.12 eV on the neutrino mass sum, bias calibration via CMB lensing cross-correlations, and tighter limits plus stronger normal-ordering preference in non-phantom dynamical dark energy models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}