{"total":36,"items":[{"citing_arxiv_id":"2605.21436","ref_index":124,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Euclid preparation: Testing multi-field inflation with galaxy power spectrum and bispectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-05-20T17:26:36+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Validates redshift-space power spectrum and bispectrum analysis on Abacus-PNG mocks to recover unbiased f_NL constraints for Euclid spectroscopic sample.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21212","ref_index":54,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Detection of a dark matter subhalo in the strongly lensed system PJ011646","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T14:07:43+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A subhalo of M200 = 2.78e10 solar masses and concentration 30 is detected at 5.8 sigma in PJ011646 via ALMA imaging and grid-based NFW search after fitting an elliptical power-law plus multipole macromodel.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20117","ref_index":68,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The potential of diffuse Galactic Ridge neutrino measurements to constrain dark matter","primary_cat":"astro-ph.HE","submitted_at":"2026-05-19T17:05:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"ANTARES Galactic Ridge neutrino measurements can constrain annihilating and decaying dark matter for various masses and profiles while comparing to astrophysical backgrounds, with forecasts for future observatories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19121","ref_index":59,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Ringdown Signatures of Dehnen Dark Matter Halos: Fluid Modes and Detectability with Space-Based Detectors","primary_cat":"gr-qc","submitted_at":"2026-05-18T21:15:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Numerical ringdown waveforms for black holes in Dehnen dark matter profiles are generated and analyzed for detectability and parameter inference using second-generation TDI in space-based detectors such as LISA, Taiji, and TianQin.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16994","ref_index":53,"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":"2605.16505","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Feedback driven interactions between dark and luminous matter to explain tight galaxy scaling relations","primary_cat":"astro-ph.GA","submitted_at":"2026-05-15T18:01:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"NIHAO simulations reproduce the Rd-r0 relation and its mild evolution from z=2 to z=0 through stellar feedback without dark matter modifications.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15330","ref_index":4,"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":"2605.15264","ref_index":135,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. II. Mass Mapping and Overdensity Characterization","primary_cat":"astro-ph.GA","submitted_at":"2026-05-14T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First near-IR weak-lensing analysis of CANDELS fields detects 12 shear-selected overdensities with masses 0.2-2.2 x 10^14 solar masses at redshifts 0.22-0.9 and mean z=0.68.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.08010","ref_index":67,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Producing the GeV Galactic Center Excess via Cosmic Ray-Dark Matter Scattering","primary_cat":"hep-ph","submitted_at":"2026-05-08T17:01:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Cosmic ray protons scattering off dark matter produce the Galactic Center gamma-ray excess through inelastic up-scattering followed by decay or direct elastic 2-to-3 photon production.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"(decay-likeJ-factor) integrated over the ROI and the line-of-sight,dσ(E p)/dEγ denotes the differential cross section of CR-DM scattering with respect to the photon energyE γ, for an incoming CR proton of energyEp, and dΦp/dEp is the CR proton flux integrated over the solid angle4π. In this analysis,ρ DM(r)is considered to be the gen- eralized Navarro-Frenk-White (gNFW) profile [67] (with γ=1.25 [66]) given by ρgNFW(r) =ρ s r rs !−γ 1 + r rs !γ−3 ,(4) whereρ s andr s are the scale density and scale radius, respectively. In Eq. (4), the scale densityρs is given by ρs =ρ ⊙ r⊙ rs !γ 1 + r⊙ rs !3−γ ,(5) wherer ⊙ = 8.5kpc,r s = 20.0kpc, andρ ⊙ = 0.4GeV/cm 3 are the distance between the Sun and the Galactic Center, scale radius, and local density, re-"},{"citing_arxiv_id":"2605.05588","ref_index":3,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Self-interacting dark matter and core formation in field low-surface-brightness galaxies","primary_cat":"astro-ph.CO","submitted_at":"2026-05-07T02:13:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Order-of-magnitude estimates exclude a self-interaction cross section of 1 cm²/g for dark matter in isolated low-surface-brightness galaxies while favoring 0.1 cm²/g.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02633","ref_index":114,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Axial tidal Love numbers of black holes in matter environments","primary_cat":"gr-qc","submitted_at":"2026-05-04T14:20:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Axial tidal Love numbers for black holes in anisotropic fluid environments are derived analytically and numerically, with non-compact support density profiles producing logarithmic terms that obstruct standard tidal matching due to the lack of a strictly vacuum exterior.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"Hernquist, Astrophys. J.356, 359 (1990). [111] R. Vicente, T. K. Karydas, and G. Bertone, Phys. Rev. Lett.135, 211401 (2025), arXiv:2505.09715 [gr-qc]. [112] P. Salucci, Astron. Astrophys. Rev.27, 2 (2019), arXiv:1811.08843 [astro-ph.GA]. [113] A. W. Graham, D. Merritt, B. Moore, J. Diemand, and B. Terzic, Astron. J.132, 2685 (2006), arXiv:astro- ph/0509417. [114] F. Prada, A. A. Klypin, E. Simonneau, J. Betancort- Rijo, S. Patiri, S. Gottlober, and M. A. Sanchez- Conde, Astrophys. J.645, 1001 (2006), arXiv:astro- ph/0506432. [115] L. Sadeghian, F. Ferrer, and C. M. Will, Phys. Rev. D 88, 063522 (2013), arXiv:1305.2619 [astro-ph.GA]. [116] J. F. M. Delgado, C. A. R. Herdeiro, and E. 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J.490, 493 (1997), arXiv:astro-ph/9611107. [67] R. Schödel, T. Ott, R. Genzel, A. Eckart, N. Mouawad, and T. Alexander, ApJ596, 1015 (2003), arXiv:astro- ph/0306214 [astro-ph]. [68] N. Neumayer, A. Seth, and T. Böker, A&A Rev.28, 4 (2020), arXiv:2001.03626 [astro-ph.GA]. [69] G. Bertone, A. R. A. C. Wierda, D. Gaggero, B. J. Ka- vanagh, M. Volonteri, and N. Yoshida, Phys. Rev. D112, 043537 (2025), arXiv:2404."},{"citing_arxiv_id":"2605.00818","ref_index":68,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"$4\\times3$ Point Correlation Functions in Galaxy Surveys: Impact of Baryonic Feedback","primary_cat":"astro-ph.CO","submitted_at":"2026-05-01T17:57:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Baryonic feedback affects galaxy-galaxy, galaxy-shear, and shear-shear three-point correlation functions more strongly than two-point functions on small scales, reaching up to 90 percent suppression depending on redshift and model parameters.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"one at a time while the other parameter is fixed at its fiducial value.Mc governs the amount of gas expelled beyond the halo boundary, andθ ej encodes the maximal ejection radius relative to the halo boundary. Our fiducial BCM model corresponds toM c = 10×10 13M⊙, and θej = 4. whereρ NFW(r) andρ 2h(r) represent a generalized Navarro-Frenk-White (NFW) profile [68] and the 2-halo term, respectively. This profile depends on the cosmological parameters of the simulation, the halo mass (more precisely on the parameterM 200), and its concentration (c200). Both of these halo parameters are measured within a radius where the density is 200 times the critical density of the universe. The two-halo term is measured from the"},{"citing_arxiv_id":"2605.00648","ref_index":57,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Anisotropy of Cosmic Background Photons from Annihilating/Decaying Dark Matter","primary_cat":"hep-ph","submitted_at":"2026-05-01T13:29:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A comprehensive formulation is given for the angular power spectrum of photons from dark matter annihilation or decay, stressing that detector energy resolution is essential for accurate evaluation of line photon signals.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Halo mass functionAs for the dark matter halo mass function, we use the Sheth-Tormen formula [56] that takes into account the effect of ellipsoidal collapse: dnh(M;z) dM =A ¯ρm0 M 2 \u0012eν 2π \u0013 1 2 \u0012 1 + 1 eνq \u0013 e−eν/2dlnν dlnM ,(B.1) where the overall normalization constant isA= 0.322 so that R dM M dnh dM = ρm0,ν= δ2 c(z)/σ2(M),eν=bνwithb= 0.707,q= 0.3. 11 The original Press-Schechter formula [57] based on the spherical collapse model is reproduced forq→0, b→1 andA→1/2. 12 Below we present how to evaluate the varianceσ(M), critical overdensityδc(z) and the linear matter power spectrumP (lin) ρ (k;z). The resulting halo mass function, in terms ofM 2 dnh dM /ρm0, is shown in Fig. 10 forz= 0,5,10. This represents the fraction of halo with massMin the"},{"citing_arxiv_id":"2604.26022","ref_index":71,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Secondary Dependence of Baryonic Effects on the Density Profile of Dark Matter Halos","primary_cat":"astro-ph.CO","submitted_at":"2026-04-28T18:05:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Baryonic effects on dark matter halo density profiles exhibit strong secondary dependence on concentration (up to 15% variations at small scales for lower-mass halos) and weaker dependence on large-scale environment (~2%).","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"We extend our analysis to a higher redshift ofz= 0.5 in Section 3.3. Appendix B presents results for two additional secondary properties: halo spin and velocity dispersion. 3.1 The Secondary Dependence on Concentration The halo concentration is defined as the Navarro-Frenk-White (NFW) concentration param- eter, c = R vir/Rs, where R vir is the virial radius of the halo and R s is the scale radius [71]. - 6 - In this work, we use the common proxy for the concentration of each DMO halo as the ratio between the maximum circular velocity of the halo, Vmax, and the virial velocity, Vvir [72, 73]: c = Vmax/Vvir where Vvir is the circular velocity at the virial radius. This velocity-based proxy for concen- tration is particularly useful when the NFW halo profile is difficult to determine or fit, as it"},{"citing_arxiv_id":"2604.26015","ref_index":103,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Kinematic Lensing Ratio: Reviving Weak Lensing Cosmography as a Geometric Dark Energy Probe","primary_cat":"astro-ph.CO","submitted_at":"2026-04-28T18:00:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"KiLeR combines shear ratios with kinematic intrinsic shapes to mitigate first-order lensing systematics and forecasts a 192% improvement in dark energy constraints from the Roman telescope.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Kneib, and M. Guitton, MNRAS545, staf2116 (2026), arXiv:2508.07311 [astro-ph.CO]. [101] J. Tinker, A. V. Kravtsov, A. Klypin, K. Abazajian, M. Warren, G. Yepes, S. 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Rev."},{"citing_arxiv_id":"2604.12189","ref_index":14,"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":"support","context_text":"where ρs is the scale density and rs ≡ r200/c200 is the scale radius. Here r200 is the radius within which the arXiv:2604.12189v1 [astro-ph.CO] 14 Apr 2026 2 mean density is 200 times the critical density, and c200 is the concentration, which we determine using the mass- concentration relation of Ref. [49]. The inner density of the profile (1) scales as ρ ∝ r−1. By contrast, simula- tions [14, 50-53] show that core-collapsed SIDM halos develop a much cuspier profile, which can be modeled by the cored power law [22], ρ(r) = ρ0 1 + r2/r2 c \u0001−γ/2 , (2) where γ characterizes the inner slope (a.k.a., cuspiness) and is typically in the range 2 ≲ γ ≲ 3 [14, 50-54]. rc is the collapsed core radius, which corresponds to the size of the secondary core of a collapsed halo."},{"citing_arxiv_id":"2604.10726","ref_index":14,"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":"The core-cusp problem [ 2-4], the too-big-to-fail problem [ 5, 6], and the diversity of ro- tation curves [ 7, 8] have motivated self-interacting dark matter (SIDM) with momentum-transfer cross-sections σ/m ∼ 0.1-10 cm 2/g [9-13]. SIDM thermalizes the in- ner regions of halos on a timescale set by the scatter- ing rate, producing constant-density cores in place of the cuspy NFW [14] profiles predicted by CDM [ 15-17]. This structural transformation has been extensively studied in dwarf galaxies [7, 15], galaxy clusters [ 18, 19], and cosmo- logical simulations [ 20, 21]. However, its implications for the epoch of reionization (EoR) [ 22, 23] remain entirely unexplored. In this Letter, we propose that SIDM leaves a distinc- tive, observable imprint on the topology of reionization."},{"citing_arxiv_id":"2602.04858","ref_index":97,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Primordial black holes as cosmic accelerators of light dark matter: Novel direct detection constraints","primary_cat":"hep-ph","submitted_at":"2026-02-04T18:43:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Primordial black hole evaporation generates light fermionic dark matter capable of producing electron recoils in XENONnT, LZ, and PandaX-4T, enabling new constraints on DM-electron interactions after including Earth attenuation effects.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"Thaler,(In)direct Detection of Boosted Dark Matter, JCAP10(2014) 062, [1405.7370]. [95] K. Kong, G. Mohlabeng and J.-C. 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[99]CDEXcollaboration, Z."},{"citing_arxiv_id":"2602.02678","ref_index":38,"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":"2601.19386","ref_index":107,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on Primordial Black Holes from Galactic Diffuse Synchrotron Emissions","primary_cat":"hep-ph","submitted_at":"2026-01-27T09:17:54+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Galactic synchrotron emissions above 20 MHz can set tighter upper limits on the abundance of primordial black holes with masses above 10^16 grams than previous cosmic-ray electron data.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"propagation, which can significantly modify the low-energy CR spectra. We considerV a to be constant throughout the diffusion halo, which should be understood as an effective parameter. In some semi-analytic frameworks, the re-acceleration is assumed to be confined 6 in the Galactic disc and normalized to a half-width ofh∼0.1 kpc, which allows for fast calculations for CR propagation [107]. The value ofV a obtained in this semi-analytical approach should be roughly rescaled by a factor of p h/zh when compared with the one adopted in this work. The CR source termqin Eq. (6) includes both the primary and secondary components. The primary CRs are believed to be accelerated by supernova remnants (SNRs) and pulsar wind nebulae, whose source term is modeled as the product of a broken power-law rigidity"},{"citing_arxiv_id":"2601.17117","ref_index":128,"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":"accelerated core collapse,\" (2025), arXiv:2511.14912 [astro- ph.GA]. [125] H. Bondi, Mon. Not. Roy. Astron. Soc.112, 195 (1952). [126] J. Hu, Y . Shen, Y .-Q. Lou, and S. Zhang, Mon. Not. R. Astron. Soc.365, 345 (2006), arXiv:astro-ph/0510222 [astro-ph]. [127] R. Courant, K. Friedrichs, and H. Lewy, IBM Journal of Re- search and Development11, 215 (1967). [128] J. Gurian and S. May, Phys. Rev. Lett.135, 221001 (2025), arXiv:2505.15903 [astro-ph.CO]."},{"citing_arxiv_id":"2601.04340","ref_index":55,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark QCD Origin of the NANOGrav Signal and Self-Interacting Dark Matter","primary_cat":"astro-ph.CO","submitted_at":"2026-01-07T19:21:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A dark QCD model with a first-order phase transition at 5-6 MeV produces the NANOGrav SGWB amplitude while supplying self-interacting dark matter via a 40 GeV baryon and 20-50 MeV dilaton, linked by entropy dilution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.18959","ref_index":14,"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":"2512.09036","ref_index":52,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing the origin of the kilonova candidate GRB 230307A: analysis of host galaxy and offset","primary_cat":"astro-ph.HE","submitted_at":"2025-12-09T19:00:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Host galaxy analysis rules out a globular cluster origin for the GRB 230307A kilonova and shows a disk-formed BNS merger with natal kicks can reach the observed offset in only 0.1% of population-synthesis realizations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.05694","ref_index":128,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nearly Degenerate Majorana Dark Matter and Its Self-Interactions in a Gauged $U(1)_{L_\\mu - L_\\tau}$ Model","primary_cat":"hep-ph","submitted_at":"2025-12-05T13:22:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A gauged U(1)_{Lμ-Lτ} model generates nearly degenerate Majorana dark matter whose self-interactions via a light scalar mediator set the relic density, resolve core-cusp anomalies, and fit LZ direct detection plus muon g-2 bounds.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Murayama, T. Takahashi and N. Yoshida, \"Matter Power Spectrum in Hidden Neutrino Interacting Dark Matter Models: A Closer Look at the Collision Term,\" JCAP11, 043 (2016) [arXiv:1602.07624 [hep-ph]]. [127] J. F. Navarro, C. S. Frenk and S. D. M. White, \"A Universal density profile from hierarchical clustering,\" Astrophys. J.490, 493 (1997) [astro-ph/9611107]. [128] J. F. Navarro, C. S. Frenk and S. D. M. White, \"The Structure of cold dark matter halos,\" Astrophys. J.462, 563 (1996) [astro-ph/9508025]. [129] G. Elor, N. L. Rodd and T. R. Slatyer, \"Multistep cascade annihilations of dark matter and the Galactic Center excess,\" Phys. Rev. D91, 103531 (2015) [arXiv:1503.01773 [hep-ph]]. [130] K. C. Yang, \"Search for Scalar Dark Matter via Pseudoscalar Portal Interactions: In Light of the"},{"citing_arxiv_id":"2512.00145","ref_index":36,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Role of prompt cusps in driving the core collapse of SIDM halos","primary_cat":"astro-ph.GA","submitted_at":"2025-11-28T19:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Prompt cusps delay core formation by a factor of ~2 in SIDM halos but later collapse tracks align after rescaling, with ~5% late-stage deviations depending on concentration and outer velocity dispersion.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.27424","ref_index":72,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Extracting Properties of Dark Dense Environments around Black Holes from Gravitational Waves","primary_cat":"gr-qc","submitted_at":"2025-10-31T12:24:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A novel quantity derived from GW signals encodes the density profile of dark dense environments around black holes, allowing characterization of the condensate type and DM properties via multi-wavelength observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.25325","ref_index":144,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Direct Collapse Black Hole Candidates from Decaying Dark Matter","primary_cat":"hep-ph","submitted_at":"2025-09-29T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Axion dark matter decay injects 1-13.6 eV photons that suppress H2, enabling atomic cooling halos and direct collapse black hole seeds for axion masses 24.5-26.5 eV and couplings down to 4e-12/GeV.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"we assume an intensity that is equally spread across the Lyman-Werner band. B.1 Dark Matter Distibution We assume that axion dark matter follows anNFWprofile [143] ρa(r, z) = ρ0(z) chr Rvir(z) \u0010 1 + chr Rvir(z) \u00112 ρ0(z) = \u0012 M(z) 4πRvir(z)3 \u0013 c3 h ln (1 +ch)− ch 1+ch ,(B.1) The choice of the concentration parameter ch = 4is appropriate for small proto-halos undergoing rapid growth [144]. The virial radius is, see e.g. Ref. [53, eq. 3.30], Rvir(M, z) = (784pc) \u0012 Ωm0 Ωm(z) ∆c 18π2 \u0013−1/3\u0012 M(z) 108 h2 M⊙ \u00131/3\u00121 +z 10 \u0013−1 .(B.2) The matter density parameter and mean overdensity at collapse are Ωm(z) = Ωm0(1 +z) 3 ΩΛ0 + Ωm0(1 +z) 3 ∆c = 18π2 + 82d−39d 2 ≈200,(B.3) where d = Ωm(zcol) − 1is evaluated at the redshift of collapse,zcol.∆ c is the ratio of the"},{"citing_arxiv_id":"2509.08043","ref_index":119,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Testing Viability of Benchmark Dark Matter Models for the Galactic Center Excess","primary_cat":"hep-ph","submitted_at":"2025-09-09T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Updated constraints on two simplified dark matter models for the Galactic Center Excess leave unconstrained parameter space after applying recent multi-experiment data.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"•Direct detection: the latest result from the LZ experiment in 2024 [43]; •CMB bound: the latest Planck result in 2018 [87]; •Accelerator and beam dump search for dark photon: the summary plot in [92]; •Gamma-ray line search: a recent analysis using data from the Fermi Gamma-Ray Space Telescope result in 2023 [44]; •Collider measurements: the measurements from LHC run 2 of the invisible Higgs decay [119], theB 0 s →µ +µ− decay [106], the mono-Higgs search [120], and the mono-Z search [81, 118] for the 2HDM+amodel. - 22 - Figure 9. Constraints for the secluded hypercharge model at differentm χ. Note that for eachm χ, we plotted the correspondingm Z′ from 1×10 −2 GeV up tom χ. The black dotted lines indicate wherem Z′ = 0.1mχ. Atm Z′ ∼0.1m χ, our result is similar to the thermalization floor in Ref."},{"citing_arxiv_id":"2508.02869","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Attenuation of the ultra-high-energy neutrino flux by dark matter scatterings","primary_cat":"hep-ph","submitted_at":"2025-08-04T19:55:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"UHE neutrino flux is attenuated by DM scatterings in intergalactic and galactic media, enabling cross-section limits from events like KM3230213A under mild astrophysical assumptions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2504.13004","ref_index":36,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Calibrating the SIDM Gravothermal Catastrophe with N-body Simulations","primary_cat":"astro-ph.GA","submitted_at":"2025-04-17T15:14:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"N-body simulations with Arepo calibrate the β parameter in the SIDM gravothermal model, showing it is independent of cross-section, concentration, and mass for velocity-independent scattering, and introduce an effective β model for the long-mean-free-path regime.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2504.02476","ref_index":78,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Globular cluster distributions as a dynamical probe of dark matter","primary_cat":"astro-ph.GA","submitted_at":"2025-04-03T10:53:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"N-body and semianalytic simulations indicate that globular cluster distributions in UDG1 and Fornax require dark matter halos via dynamical friction, while DF44 yields no strong constraint.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2406.13394","ref_index":75,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gravitational Wave Birefringence from Fuzzy Dark Matter","primary_cat":"gr-qc","submitted_at":"2024-06-19T09:38:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Fuzzy dark matter induces frequency-dependent amplitude birefringence in gravitational waves with periodic time modulation set by the scalar mass, but no velocity birefringence.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}