{"total":11,"items":[{"citing_arxiv_id":"2606.10024","ref_index":61,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Learning the Universe with cosmological rescaling of merger trees and semi-analytic galaxy formation models","primary_cat":"astro-ph.CO","submitted_at":"2026-06-08T18:08:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Rescaling merger trees with a halo-profile correction enables cheap generation of galaxy summary statistics across cosmologies using semi-analytic models, matching dedicated simulation accuracy with far fewer base runs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04793","ref_index":43,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cooler Phases of the Circumgalactic Medium Are More Centrally Concentrated: Constraints from Multiphase Absorption Lines","primary_cat":"astro-ph.GA","submitted_at":"2026-06-03T12:19:28+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.06636","ref_index":34,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"What You Don't Know Won't Hurt You: Self-Consistent Hierarchical Inference with Unknown Follow-up Selection Strategies","primary_cat":"astro-ph.IM","submitted_at":"2026-05-07T17:46:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Hierarchical Bayesian inference allows accurate recovery of intrinsic astrophysical source populations even when follow-up selection is unknown and correlated with parameters of interest.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.24034","ref_index":19,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"LStein: A new approach to visualizing sparse 2.5-dimensional data","primary_cat":"astro-ph.IM","submitted_at":"2026-04-27T04:36:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"LStein is presented as a novel visualization approach for sparse 2.5-dimensional data, implemented in Python and demonstrated on astronomical lightcurves.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.15440","ref_index":56,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing the large-scale structure with 21cm-galaxy cross-bispectrum: Estimates from simulations and forecasts for upcoming cosmological surveys","primary_cat":"astro-ph.CO","submitted_at":"2026-04-16T18:01:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Forecasts indicate 10-sigma detection for squeezed triangles and 100-sigma for combined shapes in the 21cm-galaxy cross-bispectrum with 100 hours of SKA-Mid interferometric observations on scales 0.2 to 0.9 per Mpc.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.09147","ref_index":76,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Euclid preparation. XCVIII. Cosmology Likelihood for Observables in Euclid (CLOE). 5: Extensions beyond the standard modelling of theoretical probes and systematic effects","primary_cat":"astro-ph.CO","submitted_at":"2025-10-10T08:49:24+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"CLOE has been extended to model magnification bias, massive neutrinos, and modified gravity for Euclid probes and validated via posterior sampling on synthetic data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.18689","ref_index":67,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmic dipole tensions: confronting the cosmic microwave background with infrared and radio populations of cosmological sources","primary_cat":"astro-ph.CO","submitted_at":"2025-09-23T06:14:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian tension analysis shows Planck CMB dipole in >5σ disagreement with CatWISE infrared sources and moderate-to-strong disagreement with radio surveys NVSS and RACS, with evidence for shared astrophysical signals in some catalogs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.09202","ref_index":94,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Interacting $k$-essence field with non-pressureless Dark Matter: Cosmological Dynamics and Observational Constraints","primary_cat":"astro-ph.CO","submitted_at":"2025-09-11T07:18:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Interacting k-essence dark energy and non-pressureless dark matter models with two interaction forms are shown to reproduce major cosmological epochs and fit observations comparably to LambdaCDM while admitting late-time de Sitter attractors.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"tic Oscillation (BAO) measurements from the Dark Energy Spectroscopic Instrument (DESI) Release II [38, 93], an improved version of DESI DRI. The observ- ables are the ratios{𝐷 𝑀 /𝑟𝑑, 𝐷 𝐻 /𝑟𝑑, 𝐷 𝑉 /𝑟𝑑 }, where 𝐷 𝑀 is the comoving angular distance,𝐷 𝐻 is the co- moving Hubble distance,𝐷 𝑉 is the spherically averaged distance, and𝑟 𝑑 is the sound horizon at the drag epoch [94]. The sound horizon is computed as 𝑟𝑑 = ∫ ∞ 𝑧𝑑 3×10 5𝑑˜𝑧 𝐻( ˜𝑧) √︂ 3 \u0010 1+ 3Ω𝑏 ℎ2 4Ω𝛾 ℎ2 (1+˜𝑧) \u0011 ,(4.1) where𝑧 𝑑 is estimated using the Hu-Sugiyama fitting formula [95], 𝑧d =1345 Ωmℎ2\u00010.251 h 1+𝑏 1 Ωbℎ2\u0001 𝑏2 \u0011i 1+0.659 (Ωmℎ2)0.828 , 𝑏1 =0.313 Ωmℎ2\u0001 −0.419 h 1+0.607 Ωmℎ2\u00010.674i , 𝑏2 =0.238 Ωmℎ2\u00010.223 . (4.2) Here,Ω 𝑚 denotes the total matter density (dark matter"},{"citing_arxiv_id":"2508.08638","ref_index":100,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Interacting bosonic dark energy and fermionic dark matter in Einstein scalar Gauss-Bonnet gravity","primary_cat":"astro-ph.CO","submitted_at":"2025-08-12T05:03:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Models of interacting bosonic dark energy and fermionic dark matter in Einstein-scalar-Gauss-Bonnet gravity with exponential and power-law potentials are dynamically analyzed and constrained by observational data, showing consistency with LambdaCDM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.23355","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"SPT-3G D1: Axion Early Dark Energy with CMB experiments and DESI","primary_cat":"astro-ph.CO","submitted_at":"2025-07-31T09:04:47+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"CMB-only data give f_EDE < 0.07 at 95% CL with no strong AEDE signal, while CMB+DESI yields f_EDE = 0.055^{+0.024}_{-0.047} at 68% CL and lowers Hubble tension to 2.6 sigma.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.05207","ref_index":25,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Interacting Scalar Fields as Dark Energy and Dark Matter in Einstein scalar Gauss Bonnet Gravity","primary_cat":"gr-qc","submitted_at":"2025-07-07T17:16:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Interacting scalar fields coupled to Gauss-Bonnet gravity yield viable dark energy and dark matter models that match Pantheon+ and DES supernova data while preferring over LambdaCDM at high redshifts with Roman mocks.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"surements of Baryon Acoustic Oscillations and Cosmological Constraints (2025), arXiv:2503.14738 [astro-ph.CO]. [23] A. G. Adame et al. (DESI), DESI 2024 VI: cosmological con- straints from the measurements of baryon acoustic oscillations, JCAP 02, 021, arXiv:2404.03002 [astro-ph.CO]. [24] M. E. Levi et al. (DESI), The Dark Energy Spectroscopic Instrument (DESI) (2019), arXiv:1907.10688 [astro-ph.IM]. [25] J. Moon et al. , First detection of the BAO signal from early DESI data, Mon. Not. Roy. Astron. Soc. 525, 5406 (2023), arXiv:2304.08427 [astro-ph.CO]. [26] Q. Gao, Z. Peng, S. Gao, and Y. Gong, On the Evi- dence of Dynamical Dark Energy, Universe 11, 10 (2025), arXiv:2411.16046 [astro-ph.CO]. [27] A. Sousa-Neto, C. Bengaly, J. E. Gonzalez, and J. Alcaniz, Evi-"}],"limit":50,"offset":0}