{"total":14,"items":[{"citing_arxiv_id":"2606.04827","ref_index":69,"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":"2605.22210","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on Schwarzschild Black Hole in a Generalized Dehnen-Type $(1,4,\\gamma)$ Dark Matter Halo via the S2 Star Orbit around Sgr A$^\\star$","primary_cat":"gr-qc","submitted_at":"2026-05-21T09:15:49+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Derives perihelion shift equations for S2 star in generalized Schwarzschild-Dehnen BH-DM spacetime and constrains gamma, rho_s, rs via MCMC on Do et al. and Gillessen et al. datasets.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11630","ref_index":27,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Long-lived sterile neutrinos from axionlike particles at the Super Tau-Charm Facility","primary_cat":"hep-ph","submitted_at":"2026-05-12T06:55:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"STCF can reach |V_eN|^2 values one to two orders of magnitude below current bounds for heavy neutral leptons via displaced-vertex searches from ALP decays in D-meson production.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Rev. D94, 073009 (2016), arXiv:1512.04119 [hep-ph]. [23] I. Boiarska, K. Bondarenko, A. Boyarsky, V. Gorkavenko, M. Ovchynnikov, and A. Sokolenko, JHEP11, 162 (2019), arXiv:1904.10447 [hep-ph]. [24] L. B. Okun, Sov. Phys. JETP56, 502 (1982). [25] P. Galison and A. Manohar, Phys. Lett. B136, 279 (1984). [26] B. Holdom, Phys. Lett. B166, 196 (1986). [27] C. Boehm and P. Fayet, Nucl. Phys. B683, 219 (2004), arXiv:hep-ph/0305261. [28] M. Pospelov, Phys. Rev. D80, 095002 (2009), arXiv:0811.1030 [hep-ph]. [29] D. Curtin, R. Essig, S. Gori, and J. Shelton, JHEP02, 157 (2015), arXiv:1412.0018 [hep-ph]. [30] K. Kaneta, H.-S. Lee, and S. Yun, Phys. Rev. Lett.118, 101802 (2017), arXiv:1611.01466 [hep-ph]."},{"citing_arxiv_id":"2604.21969","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Dive deeper with SUBMARINE: SUB-Mev dArk matter diRect detectIon using bilayer grapheNE","primary_cat":"hep-ph","submitted_at":"2026-04-23T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bilayer graphene enables sub-MeV dark matter detection via electronic excitations with small exposure and sidereal modulation signatures.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"(LZ) Experiment, Phys. Rev. Lett.135, 011802 (2025), arXiv:2410.17036 [hep-ex]. [7] E. Aprileet al.(XENON), WIMP Dark Matter Search Using a 3.1 Tonne-Year Exposure of the XENONnT Experiment, Phys. Rev. Lett.135, 221003 (2025), arXiv:2502.18005 [hep-ex]. [8] C. Boehm and P. Fayet, Scalar dark matter candidates, Nucl. Phys. B683, 219 (2004), arXiv:hep-ph/0305261. [9] S. Gori, S. Knapen, T. Lin, P. Munbodh, and B. Suter, Spin-dependent scattering of sub-GeV dark matter: Models and constraints, Phys. Rev. D112, 075019 (2025), arXiv:2506.11191 [hep-ph]. [10] A. Berlin and N. Blinov, Thermal Dark Matter Be- low an MeV, Phys. Rev. Lett.120, 021801 (2018), arXiv:1706.07046 [hep-ph]. [11] J. H. Chang, R. Essig, and A."},{"citing_arxiv_id":"2604.18674","ref_index":69,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Hunting Sterile Neutrino Dark Matter in the MeV Gap","primary_cat":"hep-ph","submitted_at":"2026-04-20T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Future MeV telescopes are projected to improve existing limits on sterile neutrino dark matter decay rates by several orders of magnitude.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"COSI, a NASA endeavour, is planned for launch in 2027. In addition, many pro- posed telescopes like MeVCube [61], the Galactic Ex- plorer with a Coded Aperture Mask Compton Telescope (GECCO) [62, 63], the All-sky Medium Energy Gamma- ray Observatory (AMEGO) [64-66], the Enhanced AS- TROGAM (e-ASTROGAM) [67, 68], the Gamma-Ray and AntiMatter Survey (GRAMS) [69, 70], the Ad- vanced Energetic Pair Telescope (AdEPT) [71], the PAir- productioN Gamma-ray Unit (PANGU) [72] are in dis- cussion. These instruments provide a unique opportunity to probe sterile neutrino DM through both monochro- matic photon lines and continuum emission from three- body decays. These efforts will not only revolutionise our understanding of the MeV gap but also help us uncover"},{"citing_arxiv_id":"2604.17869","ref_index":21,"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":"Queiroz, Eur. Phys. J. C78, 203 (2018), 1703.07364. [17] M. Cirelli, A. Strumia, and J. Zupan (2024), 2406.01705. [18] H. Pagels and J. R. Primack, Phys. Rev. Lett.48, 223 (1982). [19] S. Dodelson and L. M. Widrow, Phys. Rev. Lett.72, 17 (1994), hep-ph/9303287. [20] C. Boehm, T. A. Ensslin, and J. Silk, J. Phys. G30, 279 (2004), astro-ph/0208458. [21] C. Boehm and P. Fayet, Nucl. Phys. B683, 219 (2004), hep-ph/0305261. [22] G. Bertone and T. Tait, M. P., Nature562, 51 (2018), 1810.01668. [23] S. Matsumoto, Y.-L. S. Tsai, and P.-Y. Tseng, JHEP07, 050 (2019), 1811.03292. [24] T. Binder, S. Chakraborti, S. Matsumoto, and Y. Watanabe, JHEP01, 106 (2023), 2205.10149. [25] Y.-T. Chen, S. Matsumoto, T."},{"citing_arxiv_id":"2604.17726","ref_index":31,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Searching for dark photons in $J/\\psi$ decays","primary_cat":"hep-ph","submitted_at":"2026-04-20T02:21:28+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Fayet, \"Effects of the Spin 1 Partner of the Goldstino (Gravitino) on Neutral Current Phenomenology,\" Phys. Lett. B 95 (1980), 285-289 23 [29] P. Fayet, \"Light spin 1/2 or spin 0 dark matter particles,\" Phys. Rev. D70 (2004), 023514 [arXiv:hep-ph/0403226 [hep-ph]]. [30] C. Boehm and P. Fayet, \"Scalar dark matter candidates,\" Nucl. Phys. B 683 (2004), 219-263 [arXiv:hep-ph/0305261 [hep-ph]]. [31] M. Pospelov, A. Ritz and M. B. Voloshin, \"Secluded WIMP Dark Matter,\" Phys. Lett. B 662 (2008), 53-61 [arXiv:0711.4866 [hep-ph]]. [32] B. Batell, M. Pospelov and A. Ritz, \"Probing a Secluded U(1) at B-factories,\" Phys. Rev. D 79 (2009), 115008 [arXiv:0903.0363 [hep-ph]]. [33] G. Agakishiev et al. [HADES], \"Searching a Dark Photon with HADES,\" Phys."},{"citing_arxiv_id":"2512.18959","ref_index":68,"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":"2510.26260","ref_index":126,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Letter of Intent: The Forward Physics Facility","primary_cat":"hep-ex","submitted_at":"2025-10-30T08:40:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Proposes construction of the Forward Physics Facility at the HL-LHC with four complementary detectors to exploit forward neutrinos and new-particle fluxes for neutrino, QCD, astroparticle, and dark-matter measurements.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"interactions with the Earth's atmosphere as discussed in Sec. II C. Forward Charm Production as a Window into Uncharted Regions of QCD:An addi- tional component of the neutrino flux stems from the decay of charm hadrons. In contrast to light 17 hadron production, forward charm production can, in principle, be modeled using perturbative QCD methods [25, 126-128]. Forward charm quarks offer a unique probe of gluon dynamics, as they are mainly produced via the gluon fusion process that generates ac¯cpair. A simple kinematic estimate shows that, to obtain TeV-energy forward neutrinos from charm decays, one of the initial state gluons needs to carry a large momentum fractionx∼E ν/Eproton ∼1, while the other carries a very small momentum"},{"citing_arxiv_id":"2508.08676","ref_index":33,"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":"2507.13432","ref_index":113,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"INTEGRAL, eROSITA and Voyager Constraints on Light Bosonic Dark Matter: ALPs, Dark Photons, Scalars, $B-L$ and $L_{i}-L_{j}$ Vectors","primary_cat":"hep-ph","submitted_at":"2025-07-17T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"This work sets new upper limits on decay lifetimes and couplings for axion-like particles, dark photons, scalars, and B-L or L_i-L_j vector bosons using 511 keV line, X-ray continuum, and cosmic-ray flux observations.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"De la Torre Luque, A. Lella, and L. Mastrototaro, Phys. Rev. D 111, 083053 (2025), arXiv:2501.07725 [hep-ph]. [110] T. Linden, T. T. Q. Nguyen, and T. M. P. Tait, (2024), arXiv:2406.19445 [hep-ph]. [111] K. Cheung, C. J. Ouseph, P.-Y. Tseng, and S. K. Kang, (2025), arXiv:2503.04175 [hep-ph]. [112] W. Elbers et al. (DESI), (2025), arXiv:2503.14744 [astro-ph.CO]. [113] C. Boehm and P. Fayet, Nucl. Phys. B 683, 219 (2004), arXiv:hep-ph/0305261. [114] S. Kraml, T. Q. Loc, D. T. Nhung, and L. D. Ninh, SciPost Phys. 7, 052 (2019), arXiv:1908.03952 [hep-ph]. [115] P. S. B. Dev, R. N. Mohapatra, and Y. Zhang, JCAP 05, 014 (2021), arXiv:2010.01124 [hep-ph]. [116] M. Bertrand, S. Kraml, T. Q. Loc, D. T. Nhung, and L. D."},{"citing_arxiv_id":"2503.03683","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"First Limits on Light Dark Matter Interactions in a Low Threshold Two Channel Athermal Phonon Detector from the TESSERACT Collaboration","primary_cat":"hep-ex","submitted_at":"2025-03-05T17:22:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A 0.233 g silicon athermal phonon detector with 361.5 MeV/c² rms resolution sets the strongest direct-detection limits on dark matter-nucleon cross sections for masses 44–87 MeV/c² after 12 hours of exposure.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2501.14864","ref_index":83,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Super-Kamiokande Strongly Constrains Leptophilic Dark Matter Capture in the Sun","primary_cat":"astro-ph.HE","submitted_at":"2025-01-24T19:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Super-Kamiokande data constrains the DM-electron scattering cross-section for leptophilic dark matter to ~4e-41 cm2 below 100 GeV, exceeding direct detection by over an order of magnitude.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"Palomares-Ruiz, JCAP 05, 042 (2022), arXiv:2104.12757 [hep-ph]. [80] J. F. Acevedo, R. K. Leane, and J. Smirnov, JCAP 04, 038 (2024), arXiv:2303.01516 [hep-ph]. [81] E. Aprile et al. (XENON), Phys. Rev. Lett. 123, 251801 (2019), arXiv:1907.11485 [hep-ex]. [82] R. Essig, M. Fernandez-Serra, J. Mardon, A. Soto, T. Volansky, and T.-T. Yu, JHEP 05, 046 (2016), arXiv:1509.01598 [hep-ph]. [83] C. Boehm and P. Fayet, Nucl. Phys. B 683, 219 (2004), arXiv:hep-ph/0305261. [84] C. Boehm, P. Fayet, and J. Silk, Phys. Rev. D 69, 101302 (2004), arXiv:hep-ph/0311143. [85] P. Fayet, Phys. Rev. D 70, 023514 (2004), arXiv:hep-ph/0403226. [86] S.-M. Choi, Y. Hochberg, E. Kuflik, H. M. Lee, Y. Mambrini, H. Murayama, and M. Pierre, JHEP 10, 162 (2017),"},{"citing_arxiv_id":"2005.01515","ref_index":84,"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":"is related to the relic densityρχ (as reviewed in appendix 5.2), or, in terms of the normalized quantity Ωχ = ρχ/ρc as Ωχ h2≈ 2.5× 10−10 GeV−2 ⟨σχχ→ff v⟩ . (1.27) The general interplay between the massive dark photon and dark matter was originally discussed in [82] and, more recently, in [83]. 1.3. DARK MATTER AND THE DARK PHOTON 15 It has been suggested [84] that the best variable to plot most effectively the constraints in the case of LDM is by means of theyield variable y≡ ε2αD ( mχ mA′ )4 (1.28) because, from Eq. (1.26) ⟨σχχ→ff v⟩≃ 16παy m2χ (1.29) and therefore the relic density is brought into the plot. Moreover, the scaling of these limits is made less dependent on the nature of the LDM. We add the limits in the plane {y-mχ} to those in the"}],"limit":50,"offset":0}