{"total":13,"items":[{"citing_arxiv_id":"2606.27927","ref_index":31,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Large-scale structures of the Universe: physics, phenomenology, statistics","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T10:20:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"Lecture series on the physics, phenomenology, and statistics of large-scale cosmic structure evolution and non-Gaussian predictions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23651","ref_index":98,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting the 'Lensing is Low' Problem with UNIONS","primary_cat":"astro-ph.CO","submitted_at":"2026-06-22T17:36:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New UNIONS galaxy-galaxy lensing data around CMASS galaxies indicates no significant lensing is low problem, with joint HOD fits to GGL and GC favoring a slightly lower matter power spectrum amplitude than Planck.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18437","ref_index":128,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Impact of inhomogeneous curvature on growth rate measurements from magnitude fluctuations","primary_cat":"astro-ph.CO","submitted_at":"2026-06-16T19:40:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Full-GR simulations find that inhomogeneous curvature produces only sub-dominant systematic offsets in growth-rate measurements from magnitude fluctuations at z ≲ 0.2 relative to current statistical errors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12255","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Towards Practical Field-Level Inference for Weak Lensing","primary_cat":"astro-ph.CO","submitted_at":"2026-06-10T15:57:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Field-level inference from weak lensing maps yields significantly tighter cosmological constraints than power-spectrum analysis when using the same forward-modeling pipeline, especially on small scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.29806","ref_index":48,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The observer power spectrum for lightcone statistics, integrated relativistic observables and wide angle effects","primary_cat":"astro-ph.CO","submitted_at":"2026-05-28T11:52:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Introduces the observer power spectrum as a diagonal Fourier-space statistic for lightcone observables by transforming over observer positions rather than sources.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15264","ref_index":92,"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":"2605.15078","ref_index":173,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"KiDS+VIKING-450 cosmology with Bayesian hierarchical model redshift distributions","primary_cat":"astro-ph.CO","submitted_at":"2026-05-14T17:02:28+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian hierarchical modeling of photometric redshifts in KiDS+VIKING-450 raises S8 to 0.756 ± 0.039 and reduces Planck tension to 1.9σ.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13547","ref_index":45,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"UNIONS-3500 Weak Lensing: III. 2D Cosmological Constraints in Configuration Space","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T13:55:32+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"UNIONS-3500 weak lensing data yields S_8 = 0.831^{+0.067}_{-0.078} in flat LCDM from 2D cosmic shear, consistent with Planck within 1 sigma.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02807","ref_index":1,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Hadronic lensing","primary_cat":"gr-qc","submitted_at":"2026-05-04T16:45:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Hadrons described by the nonlinear sigma model minimally coupled to Maxwell theory modify photon paths away from null geodesics, enabling analytic hadronic corrections to gravitational lensing deflection angles.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"other questions for future investigations. ACKNOWLEDGMENTS The authors thank Jorge Cuadra, Astor Sandoval, and Leonardo Sanhueza for discussions. This work is par- tially funded by the Agencia Nacional de Investigaci' on y Desarrollo (ANID) through Fondecyt Regular grants No. 1240043, 1240048, 1252053, 1251523, 1261016, as well as by ANID Proyecto de Exploraci' on 1325001. [1] N. Kaiser and G. Squires, Astrophys. J.404, 441 (1993). [2] M. Bartelmann and P. Schneider, Phys. Rept.340, 291 6 (2001), arXiv:astro-ph/9912508. [3] H. Hoekstra, M. Bartelmann, H. Dahle, H. Israel, M. Limousin, and M. Meneghetti, Space Sci. Rev.177, 75 (2013), arXiv:1303.3274 [astro-ph.CO]. [4] R. Mandelbaum, Proceedings of the International Astro-"},{"citing_arxiv_id":"2604.13223","ref_index":59,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Observational constraints on nonlocal black holes via gravitational lensing","primary_cat":"gr-qc","submitted_at":"2026-04-14T18:48:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Nonlocal black holes remain consistent with general relativity at the 1.13-sigma level after joint lensing and quasinormal-mode constraints.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"HE]. [55] R. La Placa, P. Bakala, L. Stella, and M. Falanga, Res. Notes AAS3, 99 (2019), arXiv:1907.11786 [gr-qc]. [56] J. Poutanen, Astron. Astrophys.640, A24 (2020), arXiv:1909.05732 [astro-ph.HE]. [57] P. Bakala, A. Bakalov' a, R. L. Placa, M. Falanga, and L. Stella, Astron. Astrophys.673, A164 (2023). [58] N. Kaiser, Astrophys. J.388, 272 (1992). [59] M. Bartelmann and P. Schneider, Phys. Rept.340, 291 (2001), arXiv:astro-ph/9912508. [60] C. R. Keeton and A. O. Petters, Phys. Rev. D72, 104006 (2005), arXiv:gr-qc/0511019. [61] L. Amendola, M. Kunz, and D. Sapone, JCAP04, 013 (2008), arXiv:0704.2421 [astro-ph]. [62] G. Crisnejo and E. Gallo, Phys. Rev. D97, 124016 (2018), arXiv:1804.05473 [gr-qc]."},{"citing_arxiv_id":"2511.16244","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraining interacting dark energy models with black hole superradiance","primary_cat":"astro-ph.CO","submitted_at":"2025-11-20T11:24:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Black hole superradiance constrains the coupling strength in interacting dark energy-dark matter models through modifications to the effective mass of ultralight bosons in two scenarios.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2312.11704","ref_index":3,"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":"1807.06209","ref_index":35,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Planck 2018 results. VI. Cosmological parameters","primary_cat":"astro-ph.CO","submitted_at":"2018-07-17T04:05:07+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Final Planck CMB data confirms the flat 6-parameter ΛCDM model with Ω_c h² = 0.120 ± 0.001, Ω_b h² = 0.0224 ± 0.0001, n_s = 0.965 ± 0.004, τ = 0.054 ± 0.007, H_0 = 67.4 ± 0.5 km/s/Mpc, and no strong evidence for extensions.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"trum results over the full multipole range are consistent with the lensing likelihood. It is also interesting to compare to parameter constraints from the CMB power spectrum multipoles ℓ≤ 801 combined with the lensing and BAO, which gives H0 = (67.85± 0.52) km s−1Mpc−1, σ8 = 0.8058± 0.0063, Ωm = 0.3081± 0.0065.  68 %, TT,TE,EE [ℓ≤ 801]+lowE +lensing+BAO. (35) These results are entirely independent of the cosmological pa- rameter fit to the ℓ≥ 801 power spectra, but agree well at the 1 σ level with the full joint results in Table 1 (which have sim- ilar errors on these parameters). An equivalent result could be obtained using WMAP data after replacing their low-ℓ polariza- tion with the Planck HFI measurement (i."}],"limit":50,"offset":0}