{"total":10,"items":[{"citing_arxiv_id":"2605.23367","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological constraints from neighbor-density-weighted marked correlation functions","primary_cat":"astro-ph.CO","submitted_at":"2026-05-22T08:33:44+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":"2605.15078","ref_index":109,"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":"2604.23793","ref_index":73,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"From Big Bang Nucleosynthesis to Late-Time Acceleration in $f(Q,L_m)$ Gravity","primary_cat":"gr-qc","submitted_at":"2026-04-26T16:35:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The f(Q, L_m) gravity model fits observational data from BBN to late-time acceleration, acting as a viable quintessence-like alternative to the standard LambdaCDM model.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"90 [78] 0.20 72.90 29.60 [87] 0.40 82.04 2.03 [71] 0.27 77.00 14.00 [88] 0.43 86.45 3.68 [69] 0.28 88.80 36.60 [87] 0.44 82.60 7.80 [80] 0.352 83.00 14.00 [89] 0.44 84.81 1.83 [71] 0.3802 83.00 13.50 [91] 0.48 87.79 2.03 [71] 0.4 95.00 17.00 [88] 0.56 93.33 2.32 [71] 0.4004 77.00 10.20 [91] 0.57 87.60 7.80 [79] 0.4247 87.10 11.20 [91] 0.57 96.80 3.40 [73] 0.4497 92.80 12.90 [91] 0.59 98.48 3.19 [71] 0.47 89.00 50.00 [100] 0.60 87.90 6.10 [80] 0.4783 80.90 9.00 [91] 0.61 97.30 2.10 [78] 0.48 97.00 62.00 [100] 0.64 98.82 2.99 [71] 0.593 104.00 13.00 [89] 0.978 113.72 14.63 [74] 0.68 92.00 8.00 [89] 1.23 131.44 12.42 [74] 0.781 105.00 12.00 [89] 1.48 153.81 6.39 [81] 0.875 125.00 17.00 [89] 1.526 148."},{"citing_arxiv_id":"2604.22450","ref_index":55,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Exploring Cosmic Evolution in R\\'enyi Entropic Cosmology with Constraints from DESI DR2 BAO and GW Data","primary_cat":"gr-qc","submitted_at":"2026-04-24T11:08:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Rényi entropic corrections to cosmology are constrained by DESI DR2 BAO and GW data to a viable quintessence-like model that approaches ΛCDM without phantom behavior and satisfies BBN bounds.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"90 [60] 0.20 72.90 29.60 [69] 0.40 82.04 2.03 [53] 0.27 77.00 14.00 [70] 0.43 86.45 3.68 [51] 0.28 88.80 36.60 [69] 0.44 82.60 7.80 [62] 0.352 83.00 14.00 [71] 0.44 84.81 1.83 [53] 0.3802 83.00 13.50 [73] 0.48 87.79 2.03 [53] 0.4 95.00 17.00 [70] 0.56 93.33 2.32 [53] 0.4004 77.00 10.20 [73] 0.57 87.60 7.80 [61] 0.4247 87.10 11.20 [73] 0.57 96.80 3.40 [55] 0.4497 92.80 12.90 [73] 0.59 98.48 3.19 [53] 0.47 89.00 50.00 [82] 0.60 87.90 6.10 [62] 0.4783 80.90 9.00 [73] 0.61 97.30 2.10 [60] 0.48 97.00 62.00 [82] 0.64 98.82 2.99 [53] 0.593 104.00 13.00 [71] 0.978 113.72 14.63 [56] 0.68 92.00 8.00 [71] 1.23 131.44 12.42 [56] 0.781 105.00 12.00 [71] 1.48 153.81 6.39 [63] 0.875 125.00 17.00 [71] 1.526 148.11 12."},{"citing_arxiv_id":"2507.01070","ref_index":108,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Barrow holographic dark energy interacting model in the presence of radiation and matter","primary_cat":"gr-qc","submitted_at":"2025-07-01T07:51:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Numerical study of interacting Barrow holographic dark energy in non-flat universes with radiation, showing EoS transitions and higher fitted H0 values that may address Hubble tension.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2404.03002","ref_index":59,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations","primary_cat":"astro-ph.CO","submitted_at":"2024-04-03T18:41:51+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First-year DESI BAO data are consistent with flat LambdaCDM and, when combined with CMB, show a 2.5-3.9 sigma preference for evolving dark energy (w0 > -1, wa < 0) that strengthens with certain supernova datasets.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"acoustic oscillation measurement from the reconstructed 6-degree field galaxy survey , MNRAS 481 (2018) 2371 [ 1803.01746]. [58] L. Anderson, E. Aubourg, S. Bailey, D. Bizyaev, M. Blanton, A.S. Bolton et al., The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Data Release 9 spectroscopic galaxy sample , MNRAS 427 (2012) 3435 [1203.6594]. [59] L. Anderson, 'E. Aubourg, S. Bailey, F. Beutler, V. Bhardwaj, M. Blanton et al., The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: baryon acoustic oscillations in the Data Releases 10 and 11 Galaxy samples , MNRAS 441 (2014) 24 [1312.4877]. [60] S. Alam, M. Ata, S. Bailey, F. Beutler, D. Bizyaev, J.A. Blazek et al."},{"citing_arxiv_id":"2404.03000","ref_index":112,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars","primary_cat":"astro-ph.CO","submitted_at":"2024-04-03T18:41:49+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI measures BAO scales in six redshift bins with 0.52% combined precision using 5.7 million objects, detecting the signal at up to 9.1 sigma and finding larger scales than Planck LCDM at z<0.8.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the former is quoted as the detection significance. 29 The flat likelihood of the noBAO fit is a trivial result of the improved separation between the BAO and noBAO modeling in Eq. (4.1) that the DESI DR1 analysis adopted, i.e., the noBAO modeling now has naturally no dependence on αiso, in contrast to previous configuration space analyses (see, e.g., the right-hand panel of figure 12 in [112]). The detection significance, in the increasing order, is 4.0σ for BGS, 4.2σ for QSO, 6.4σ for LRG1, 6.8σ for LRG2, 7.0σ for ELG2, and 8.7σ for LRG3, with the most significant case being 9 .1σ for LRG3+ELG1, closely correlated with the precision. 7.3 BAO constraints projected onto α⊥ and α∥ The parameterisation of the BAO-scale fitting by αiso and αAP provides a natural separation"},{"citing_arxiv_id":"2105.13549","ref_index":54,"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":"330, 506 (2002), arXiv:astro-ph/0008392 [astro-ph]. [51] W. J. Percival et al. (2dFGRS), Mon. Not. Roy. Astron. Soc. 327, 1297 (2001), arXiv:astro-ph/0105252. [52] N. Padmanabhan et al. (SDSS), Mon. Not. Roy. Astron. Soc. 378, 852 (2007), arXiv:astro-ph/0605302. [53] L. Anderson et al. (BOSS), Mon. Not. Roy. Astron. Soc. 441, 24 (2014), arXiv:1312.4877 [astro-ph.CO]. [54] S. Ho et al., Astrophys. J. 761, 14 (2012), arXiv:1201.2137 [astro-ph.CO]. [55] J. Carrick, S. J. Turnbull, G. Lavaux, and M. J. Hudson, Mon. Not. Roy. Astron. Soc. 450, 317 (2015), arXiv:1504.04627 [astro-ph.CO]. [56] D. Huterer, D. Shafer, D. Scolnic, and F. Schmidt, JCAP 05, 015 (2017), arXiv:1611.09862 [astro-ph.CO]. [57] A. Nicola, A. Refregier, and A."},{"citing_arxiv_id":"1807.06209","ref_index":23,"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":"density also a ffects the amount of lensing in the CMB spectra and the amplitude of the CMB-lensing reconstruction spectrum. The matter density is well constrained to be Ωmh2 = 0.1430± 0.0011 (68 %, Planck TT,TE,EE +lowE+lensing). (22) The matter mostly consists of cold dark matter, with density con- strained at the percent level: Ωch2 = 0.1200± 0.0012 (68 %, Planck TT,TE,EE +lowE+lensing). (23) Changes in the baryon density a ffect the spectrum in character- istic ways, modifying the relative heights of the even and odd acoustic peaks, due to the effect of baryons on the depth of first and subsequent acoustic (de)compressions. Despite comprising less than a sixth of the total matter content, the baryon e ffects on the power spectra are sufficiently distinctive that the baryon-"},{"citing_arxiv_id":"1611.00036","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The DESI Experiment Part I: Science,Targeting, and Survey Design","primary_cat":"astro-ph.IM","submitted_at":"2016-10-31T20:47:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"DESI will target luminous red galaxies to z=1, emission-line galaxies to z=1.7, quasars for tracers and Ly-alpha forest at 2.1<z<3.5, plus a bright galaxy survey, to obtain more than 30 million redshifts for BAO and matter power spectrum measurements.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"This has been achieved with high statistical significance in several measurements spanning the redshift range from z = 0 to z = 1. 2 SCIENCE MOTIV ATION AND REQUIREMENTS 7 Figure 2.2: The angle-averaged correlation functions [left] and power spectra [right], before [top] and after [bottom] reconstruction measured using the BOSS DR11 CMASS galaxy sample [6]. The BAO feature is clearly detected at over 7σ as a peak in the correlation function and a corresponding set of oscillations in the power spectrum. The highest significance detection (> 7σ) is currently that of the Baryon Oscillation Spectroscopic Survey (BOSS) using the z >0.45 sample [6, 7]. We show representative data in Figure 2.2. These data measured the distance-like quantity DV (z)≡ ((1 +z)DA)2/3(cz/H(z))1/3 to a redshift of 0."}],"limit":50,"offset":0}