{"total":22,"items":[{"citing_arxiv_id":"2606.28559","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI DR2 Reference Mocks: Clustering results from UCHUU ELGs and QSOs","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T19:22:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Mock catalogs for DESI DR2 ELGs and QSOs are constructed via modified subhalo abundance matching on the Uchuu simulation to reproduce observed number density and clustering statistics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24868","ref_index":142,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Exploring Gravitational Wave Signatures Due to Primordial Non-gaussianity and Large Scale Structure Using SKAO","primary_cat":"astro-ph.CO","submitted_at":"2026-06-23T17:47:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Explores SKAO detection of scalar-induced GW backgrounds as probes of primordial non-Gaussianity and parity violation, with LSS cross-correlation to improve SNR.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19429","ref_index":89,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"BayeSN $\\times$ Dovekie: Joint Photometric Cross-calibration and SED Modelling of Type Ia Supernovae","primary_cat":"astro-ph.CO","submitted_at":"2026-06-17T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Joint photometric cross-calibration and SED modeling in BayeSN yields G26 model with 12% NMAD scatter reduction on DES-SN5YR supernovae at z<0.7.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.07730","ref_index":235,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The X-ray-to-UV relation does not evolve in homogeneous quasar samples","primary_cat":"astro-ph.HE","submitted_at":"2026-06-05T17:53:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A bias-controlled quasar sample of ~2000 objects demonstrates that the X-ray-to-UV luminosity relation remains constant from redshift 0.7 to 5.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02660","ref_index":33,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Late-Time Cosmology and Structure Formation in Quadratic $f(Q)$ Gravity","primary_cat":"physics.gen-ph","submitted_at":"2026-06-01T07:16:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Quadratic f(Q) gravity adds an H^4 term to the Friedmann equation and introduces a time-dependent G_eff that suppresses linear growth and halo abundance, offering a modified-gravity route to easing the S8 tension.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00411","ref_index":20,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The sound of dynamical dark energy and modified gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-05-29T23:05:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Using CMB, SN, BAO and shear data, the work shows dynamical dark energy in MG models correlates with deviations from GR below z=2 at >95% CL, a link that holds for varying sound speed but vanishes for a cosmological constant.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19188","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Lossless Compression of Cosmological Information from Type Ia Supernova Distance Measurements","primary_cat":"astro-ph.CO","submitted_at":"2026-05-18T23:27:05+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Compressing SN Ia distance-redshift data to eleven Gaussian log r_p(z) points with covariance is shown to be operationally lossless for cosmological inference across multiple models and datasets.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.22372","ref_index":34,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Testing $\\Lambda$CDM with ANN-Reconstructed Expansion History from Cosmic Chronometers","primary_cat":"astro-ph.CO","submitted_at":"2026-04-24T09:06:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The ANN-reconstructed Hubble parameter H(z) from cosmic chronometers aligns with Lambda CDM predictions within uncertainties.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"CO]. [30] A. Shafieloo, Mon. Not. Roy. Astron. Soc. 380, 1573 (2007), arXiv:astro-ph/0703034 [astro-ph]. [31] M. Seikel, C. Clarkson, and M. Smith, JCAP 2012 (06), 036, arXiv:1204.2832 [astro-ph.CO]. [32] M.-J. Zhang and H. Li, Eur. Phys. J. C 78, 460 (2018), arXiv:1806.02981 [astro-ph.CO]. [33] Y. Hwang, H. Noh, and C.-G. Park, JCAP 2023 (04), 071. [34] T. Holsclaw, U. Alam, B. Sansó, H. Lee, K. Heitmann, S. Ha bib, D. Higdon, and D. Bruhwiler, Phys. Rev. Lett. 105, 241302 (2010), arXiv:1011.3079 [astro-ph.CO]. [35] T. Holsclaw, U. Alam, B. Sansó, H. Lee, K. Heitmann, S. Ha bib, D. Higdon, and D. Bruhwiler, Phys. Rev. D 82, 103502 (2010), arXiv:1009.5443 [astro-ph.CO]. [36] S. Nesseris and J. García-Bellido, JCAP 2012 (11), 033, arXiv:1205."},{"citing_arxiv_id":"2604.18053","ref_index":59,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A barotropic alternative to Early Dark Energy for alleviating the $H_0$ tension","primary_cat":"astro-ph.CO","submitted_at":"2026-04-20T10:22:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A barotropic fluid with ω_s ≈ 0.29 and Ω_s ≈ 1.5×10^{-5} raises the inferred H0 to match SH0ES while remaining consistent with Planck CMB, DESI BAO, and Pantheon data.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":",(41) whereσ Hi denotes the uncertainty associated with each measurement ofH(z). The contour plots obtained from our analyses are pre- sented in Appendix A, while the mean parameter val- ues and their corresponding uncertainties are reported in 11 z H(z) References [km/s/Mpc] 0.07 69.0±19.6 [58] 0.09 69.0±12.0 [57] 0.12 68.6±26.2 [58] 0.17 83.0±8.0 [59] 0.179 75.0±4.0 [60] 0.199 75.0±5.0 [60] 0.20 72.9±29.6 [58] 0.27 77.0±14.0 [59] 0.28 88.8±36.6 [58] 0.352 83.0±14.0 [61] 0.38 83.0±13.5 [61] 0.4 95.0±17.0 [59] 0.4004 77.0±10.2 [61] 0.425 87.1±11.2 [61] 0.445 92.8±12.9 [61] 0.47 89.0±23.0 [62] 0.4783 80.9±9.0 [61] 0.48 97.0±62.0 [63] 0.593 104.0±13.0 [60] 0.68 92.0±8.0 [60] 0.75 98.8±33.6 [64] 0.781 105."},{"citing_arxiv_id":"2604.12587","ref_index":12,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Impact of the SNe Ia Magnitude Transition at 20 Mpc on Cosmological Parameter Estimation","primary_cat":"astro-ph.CO","submitted_at":"2026-04-14T11:10:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A 0.19 mag step in supernova absolute magnitude at 20 Mpc improves data fit and increases the Hubble constant by 2% while leaving matter density and dark energy parameters stable.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"CO]. [10] R. Kessler and D. Scolnic, \"Correcting type ia super- nova distances for selection biases and contamination in photometrically identified samples,\" The Astrophysical Journal836, 56 (2017). [11] Adam G. Riesset al., \"A 2.4% Determination of the Local Value of the Hubble Constant,\" Astrophys. J.826, 56 (2016), arXiv:1604.01424 [astro-ph.CO]. [12] N. Aghanimet al.(Planck), \"Planck 2018 results. VI. Cosmological parameters,\" Astron. Astrophys.641, A6 (2020), arXiv:1807.06209 [astro-ph.CO]. [13] N. Aghanimet al.(Planck), \"Planck 2018 results. I. Overview and the cosmological legacy of Planck,\" Astron. Astrophys.641, A1 (2020), arXiv:1807.06205 [astro- ph.CO]. [14] G.E. Addison, Y. Huang, D.J."},{"citing_arxiv_id":"2604.11883","ref_index":15,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Model-Independent Analysis of Type Ia Supernova Datasets and Implications for Dark Energy","primary_cat":"astro-ph.CO","submitted_at":"2026-04-13T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Apparent dynamical dark energy signals from SNe Ia with DESI data are consistent with LambdaCDM when accounting for dataset-specific Omega_m inconsistencies rather than requiring evolving dark energy.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"so averaging in magnitude space is biased by Jensen's inequality (⟨logF⟩ ̸= log⟨F⟩). On the modeling side, rigid parameterizations likew 0-wa impose a specific evolutionary form on dark energy [1], which may mask more complex dynamics or create artificial tensions between datasets. In this work we address both fronts. To handle systematics due to weak lensing, we apply flux averaging [13] to three 1 SNe Ia compilations (Pantheon [15], Pantheon+ [9], and DES-Dovekie [16], a reanalysis of DESY5 [10]) and combine the results with DESI DR2 BAO and Planck CMB distance priors [17]. Flux averaging operates in flux space, where the lensing magnification PDF has unit mean, thereby eliminating the Jensen's inequality bias. It also serves as a diagnostic: a dataset resulting in distance estimates insensitive to the"},{"citing_arxiv_id":"2603.25999","ref_index":92,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological constraints on the big bang quantum cosmology model","primary_cat":"astro-ph.CO","submitted_at":"2026-03-27T01:31:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The JCDM model yields H0 of 66.95 plus or minus 0.51 km/s/Mpc and Omega_m of 0.3419 plus or minus 0.0065 in a flat universe, rising to H0 of 69.13 plus or minus 0.56 with slight positive curvature, fitting late-time data but struggling with full early-universe consistency.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"the literature, we are able to deduce that [91] χ2 SN(θ) = A(θ) − B2(θ) C (25) where A(θ) = NX i=1 (µobs(zi) − 5log10(DL(zi)))2 σ2 i (26) B(θ) = NX i=1 µobs(zi) − 5log10(DL(zi)) σ2 i (27) C(θ) = NX i=1 1 σ2 i (28) DL(zi) = H0 c × dl(zi) (29) In this study, we utilize a sample of 1048 supernovae from the Pantheon compilation, spanning a redshift range of 0.01 and 2.3 [92]. IV. MODEL ANALYSIS, RESULTS, AND RELEVANT DISCUSSIONS We will incorporate data from various sources, includ- ing Baryon Acoustic Oscillations (BAO) measurements from the Dark Energy Spectroscopic Instrument (DESI DR1), Cosmic Microwave Background (CMB) data, cos- mic chronometers (CC), and observations of type Ia su- pernovae (SNIa). By utilizing the Markov Chain Monte"},{"citing_arxiv_id":"2603.21125","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Model-Independent Reconstruction of Quintessence Potential and Kinetic Energy from DESI DR2 and Pantheon+ Supernovae","primary_cat":"astro-ph.CO","submitted_at":"2026-03-22T08:46:57+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Quintessence potential decreases monotonically with redshift while kinetic energy crosses zero near z=1, with negative values at intermediate redshifts being statistical artifacts from derivative reconstruction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2602.22840","ref_index":86,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Redshift evolution of the Hubble constant: Constraints and new insights from an interacting dark energy model","primary_cat":"astro-ph.CO","submitted_at":"2026-02-26T10:27:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Modified IDE model with interaction parameter alpha ~0.01 from late-universe data shows H0 decreasing with redshift, tightening to 10^-5 when CMB priors are added.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2602.11093","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"from galaxy clusters using the DF method. There are two best fits (two peaks) for parameters l, b, and A. Acknowledgements This work was supported by the National Natural Science Foundation of China (grant No. No. 12494575, 12273009, No. 12373026, No. 12003020) and Shaanxi Fundamental Science Research Project for Mathematics and Physics (grant No. 23JSY015). References [1] D.M. Scolnic, D.O. Jones, A. Rest, Y.C. Pan, R. Chornock, R.J. Foley et al., The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample , ApJ 859 (2018) 101 [1710.00845]. [2] T.M.C. Abbott, A. Alarcon, S. Allam, P. Andersen, F. Andrade-Oliveira, J. Annis et al."},{"citing_arxiv_id":"2512.02526","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Updates on dipolar anisotropy in local measurements of the Hubble constant from Cosmicflows-4","primary_cat":"astro-ph.CO","submitted_at":"2025-12-02T08:42:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Local Hubble constant anisotropy in Cosmicflows-4 data is primarily attributed to peculiar velocities and survey structure rather than cosmic-scale isotropy violation, with limited implications for the Hubble tension.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.10631","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Bayesian Perspective on Evidence for Evolving Dark Energy","primary_cat":"astro-ph.CO","submitted_at":"2025-11-13T18:54:40+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian evidence favors a constant dark energy model for DESI plus Planck data and shows that apparent support for evolving dark energy with added supernova data stems from a 2.95 sigma tension between DESI and DES-SN5YR that the flexible model resolves.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.24732","ref_index":78,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Quintom theory of dark energy after DESI DR2","primary_cat":"astro-ph.CO","submitted_at":"2025-05-30T15:54:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"This review traces the history of dynamical dark energy, presents the no-go theorem against single-field crossing of w = -1, and surveys viable Quintom constructions including multi-field models and modified gravity in light of DESI DR2 hints.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"Incorporating JLA data with Planck2013 results brought the constraints on dark energy back in line with ΛCDM. In Planck2015 [74, 75], which adopted JLA as its default SN dataset, the previous SNLS-induced deviation from the standard model was similarly resolved. The final result is w=−1.006 +0.085 −0.091. Moreover, the emergence of new observational data sets including DESY1 [76, 77], Pantheon [78], Planck2018 [79], and DESY3 [80, 81] further constrained thewCDM andw 0waCDM models [82]. In all of these studies, the joint analyses have continued to show no significant deviation ofwfrom−1. In 2022, the Pantheon+ supernova compilation [83] reportedw=−0.90±0.14 (SN only) andw=−0.978 +0.024 −0.031 when combined with CMB and BAO data. Although the fit tow 0 andw a remained consistent with ΛCDM within the 2σconfidence level, the results"},{"citing_arxiv_id":"2503.14744","ref_index":176,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on Neutrino Physics from DESI DR2 BAO and DR1 Full Shape","primary_cat":"astro-ph.CO","submitted_at":"2025-03-18T21:14:18+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"DESI DR2 BAO and full-shape data plus CMB yield ∑m_ν < 0.0642 eV (95% CL) under ΛCDM, in 3σ tension with oscillation lower limits, relaxed to <0.163 eV in w0waCDM.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"024 eV (95%; IO) . (23) This is a significant improvement with respect to a similar analysis utilizing BOSS DR12 [172], Planck 2015 [173], Pantheon SNe Ia [174], and BBN information [175], that yielded ml < 0.086 eV (95%) [36]. The result may also be compared with the constraint, ml < 0.040 eV [37] from Planck 2018 [38], BOSS DR12 [172], the DR7 Main Galaxy Survey [176], and the Six-degree-Field Galaxy Survey (6dFGS) [177]. In the general case, the data prefer the normal mass or- dering. Assuming ΛCDM, we find a posterior probability from DESI BAO + CMB + NuFIT of P (NO) = 1 − P (IO) = 0.91. (24) This corresponds to a Bayes factor of K = 10. The evidence is slightly weaker for the alternative CMB like- lihoods ( K = 6 for L-H and K = 8 for plik)."},{"citing_arxiv_id":"2211.04492","ref_index":32,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Hubble Tension and Early Dark Energy","primary_cat":"astro-ph.CO","submitted_at":"2022-11-08T19:00:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The Hubble tension between local and early-universe expansion-rate measurements may be resolved by early dark energy that speeds up expansion before recombination while satisfying existing constraints.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2105.13549","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dark Energy Survey Year 3 Results: Cosmological Constraints from Galaxy Clustering and Weak Lensing","primary_cat":"astro-ph.CO","submitted_at":"2021-05-28T01:58:58+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DES Y3 3x2pt analysis constrains S8=0.776±0.017 and Ωm=0.339±0.032 in flat ΛCDM, consistent with Planck CMB results at p=0.13-0.48.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Conley et al. 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