{"total":15,"items":[{"citing_arxiv_id":"2606.01103","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Self-gravitating quantum stars with a globally relevant Bohm potential","primary_cat":"hep-th","submitted_at":"2026-05-31T08:44:58+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The equilibrium radius of self-gravitating dark fermion stars is determined by the fermion mass once the total mass is given, with the Bohm potential supplying outward pressure for heavier species and inward tension for lighter ones.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17211","ref_index":8,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constraints on Self-Interacting Fuzzy Dark Matter from the Stellar Kinematics of the Dwarf Galaxy Leo II","primary_cat":"astro-ph.CO","submitted_at":"2026-05-17T01:00:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Using Jeans analysis of Leo II stellar kinematics, the paper constrains the fuzzy dark matter mass m_a and self-interaction parameter f_a, finding 95% CL lower limits on m_a in the (1-10)×10^{-22} eV range for |f_a^{-1}| ≲ 10^{-14} GeV^{-1}.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02172","ref_index":9,"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":"on sub-galactic scales. These include the \"core-cusp problem\" [3, 4], \"missing-satellite problem\" [5, 6], and the \"too-big-to- fail problem\" [7], see Ref [8] for a review. While some of these small-scale issues may be alleviated through baryonic feedback ∗ siyuan.chen@shao.ac.cn † liukuo@shao.ac.cn ‡ zhuxj@bnu.edu.cn mechanisms in astrophysical modeling [9], accurately captur- ing such processes remains challenging due to their complex dependence on galaxy formation physics. Alongside these astrophysical approaches, several particle physics frameworks offer alternative pathways to address the observed discrepan- cies. These include warm [10], self-interacting [11], and fuzzy dark matter [12]. Among these candidates, fuzzy dark matter has emerged as"},{"citing_arxiv_id":"2604.15006","ref_index":20,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cosmology of Inelastic Self-Interacting Dark Matter: Linear Evolution and Observational Constraints","primary_cat":"astro-ph.CO","submitted_at":"2026-04-16T13:33:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Inelastic self-interacting dark matter with small mass splitting produces a cutoff in the matter power spectrum at k > 1 h Mpc^{-1} whose location depends on cross-section normalization, velocity dependence, dark matter mass and mass splitting, yielding non-monotonic exclusion regions from Lyman-α森林","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"S. Tsai, C.-T. Lu and V.Q. Tran,Confronting dark matter co-annihilation of Inert two Higgs Doublet Model with a compressed mass spectrum,JHEP06(2020) 033 [1912.08875]. [19] S. Banerjee, S. Matsumoto, K. Mukaida and Y.-L.S. Tsai,WIMP Dark Matter in a Well-Tempered Regime: A case study on Singlet-Doublets Fermionic WIMP,JHEP11(2016) 070 [1603.07387]. [20] Y.-Z. Fan, T.-P. Tang, Y.-L.S. Tsai and L. Wu,Inert Higgs Dark Matter for CDF II W-Boson Mass and Detection Prospects,Phys. Rev. Lett.129(2022) 091802 [2204.03693]. [21] R.A. Flores and J.R. Primack,Observational and theoretical constraints on singular dark matter halos,Astrophys. J. Lett.427(1994) L1 [astro-ph/9402004]. [22] B. Moore,Evidence against dissipationless dark matter from observations of galaxy haloes,"},{"citing_arxiv_id":"2604.12189","ref_index":3,"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":"background","context_text":"In addition, strong lensing observations reveal ultra-dense substructures [4-11] that are difficult to reconcile with the cold and collisionless dark mat- ter (CDM) of ΛCDM, which predicts halos with univer- sal Navarro-Frenk-White density profiles [12, 13]. Self- interacting dark matter (SIDM) has emerged as a com- pelling alternative (see review [3]). The self-interactions of dark matter drive gravothermal evolution, leading first to core formation and later to core collapse of the halo [14-18]. While core formation can address the core- cusp and too-big-to-fail problems [19, 20], core collapse produces halos with ultra-dense central regions that yield distinctive observational signatures. In particular, they"},{"citing_arxiv_id":"2602.11093","ref_index":58,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"New constraints on cosmic anisotropy from galaxy clusters using an improved dipole fitting method","primary_cat":"astro-ph.CO","submitted_at":"2026-02-11T18:01:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Galaxy cluster observations yield two preferred directions with cosmic anisotropy amplitude of about 5.3 times 10 to the minus 4 at roughly 1 sigma overall significance, though higher in the XMM-Newton subsample.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"creasing challenges as the volume and precision of observations continue to grow. In addition to the recent hot issues such as Hubble constant (H0) tension [17-25], S8 tension [26-30], dy- namic dark energy [16, 31-40], evolutionary behavior of H0 [41-48], there are also the growth tension [49-51], age of the universe [52-54], Baryon Acoustic Oscillation (BAO) curiosities [55-57], small-scale curiosities [58, 59] and cosmic anisotropy [60-68]. Research related to the above topics indicates that the ΛCDM model might have limitations in describing the structure and evolution of the Universe. Thus, its status as the standard cosmological model remains contingent upon validation through more precise astronomical observations [69, 70]. The cosmological principle, as a basic assumption of the ΛCDM model, requires that"},{"citing_arxiv_id":"2601.17117","ref_index":70,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"success of CDM [61, 64-69]. This is achieved because self- interactions thermalize the central halo, creating the necessary structural diversity-where profiles can be cored or cuspy de- pending on the cross-section as well as the formation time of the halo-to match observations. According to current obser- vations, the cross section per unit particle mass is constrained to [70, 71]σ∼1−100 cm 2/g, with possible velocity depen- dence that makes the cross section decrease sharply beyond a relative velocity of∼100 km/s [63]. By heat conduction from the inner core to the outer region [61], these collisions eventu- ally lead to a run-away gravothermal core collapse that occurs within several hundred relaxation timescales [72, 73]."},{"citing_arxiv_id":"2601.04340","ref_index":29,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":12,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":10,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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},{"citing_arxiv_id":"2511.09306","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Self-Interaction of Super-Resonant Dark Matter","primary_cat":"hep-ph","submitted_at":"2025-11-12T13:17:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Super-resonant dark matter at O(100) GeV masses amplifies self-scattering and annihilation cross sections via combined resonance and Sommerfeld effects, necessitating coupled Boltzmann equations to match observed relic density.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.07511","ref_index":19,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Robust Measurement of Stellar Streams Around the Milky Way: Correcting Spatially Variable Observational Selection Effects in Optical Imaging Surveys","primary_cat":"astro-ph.GA","submitted_at":"2025-10-08T20:18:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A method using Balrog synthetic injections corrects spatially variable detection and classification rates in DES Y3 data, reducing relative detection rate standard deviation by a factor of five and lowering bias in stellar stream density power spectra.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2506.14898","ref_index":1,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Self-Interacting Dark Matter with Mass Segregation: A Unified Explanation of Dwarf Cores and Small-Scale Lenses","primary_cat":"astro-ph.CO","submitted_at":"2025-06-17T18:13:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Two-component SIDM with velocity-dependent inter- and intra-species interactions produces mass segregation that forms dwarf cores and boosts small-scale strong lensing efficiency by a factor of a few.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.04473","ref_index":295,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"CMB-S4 Science Case, Reference Design, and Project Plan","primary_cat":"astro-ph.IM","submitted_at":"2019-07-10T01:01:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Presents the science case, reference design, and project plan for the CMB-S4 ground-based CMB experiment.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Given the large array of possible DM theories to constrain, it is useful to pick a simple benchmark DM-DR model to assess the sensitivity of CMB-S4 to the effects described in the previous paragraph. A particularly useful model is one in which the interaction between DM and DR is mediated by a particle with mass of order a few MeV. Such theories have been put forward in the context of self-interacting DM [295, 296, 297] in order to obtain a velocity-dependent self-interaction cross-section that can fit both the observed density profiles of dwarf galaxies and of large galaxy clusters. For these models, the momentum-transfer rate between the DR and DM in the early Universe can be written as ˙ κDR−DM∝ ΩDMh2a4(1 + z)4, where a4 is a parameter that controls the strength of the DM-DR interaction that depends on the exact Lagrangian used (see Ref."},{"citing_arxiv_id":"1906.09798","ref_index":9,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Investigating Dark Matter and MOND Models with Galactic Rotation Curve Data: Analysing the Gas-Dominated Galaxies","primary_cat":"astro-ph.GA","submitted_at":"2019-06-24T09:11:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Gas-dominated galaxies in SPARC exhibit rightward curving geometry in normalized g2-space (r_obs > r_bar), unlike the full sample, indicating the true dynamics and radial dependence of disk mass-to-light ratios.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}