{"total":30,"items":[{"citing_arxiv_id":"2606.26237","ref_index":189,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"First full-shape joint analysis of the two- and three-point correlation functions on real data: $\\Lambda$CDM cosmological constraints from BOSS DR12","primary_cat":"astro-ph.CO","submitted_at":"2026-06-24T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"First joint 2PCF+3PCF full-shape analysis on BOSS DR12 real data improves σ(h) by ~29%, σ(ω_cdm) by ~10%, and σ(A_s) by ~24% over 2PCF alone via extra BAO information in 3PCF triangles.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18437","ref_index":16,"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":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"Thetheoreticalangular power spectrum of the lensing convergence in the FLRW model is given by, C κκ ℓ = \u00123ΩmH2 0 2c2 \u00132Z χH 0 dχ [W κ(χ)]2 a2(χ) P \u0012 ℓ χ , χ \u0013 ,(15) whereχ H is the horizon distance, andWκ(χ)is the con- vergence window function of the sources depending on their distance distributionw(χ)defined above, W κ(χ) = Z χH χ dχs w(χs) \u0012 χs −χ χs \u0013 .(16) Assuming a delta-function source distribution as in Sec. 2.3, and an Einstein de-Sitter growth history appro- priate to our simulations described in Sec. 3, such that P(k, χ) =P(k,0)a 2(χ), we find, C κκ ℓ = \u00123ΩmH2 0 2c2 \u00132Z χ0 0 dχ \u0012 χ0 −χ χ0 \u00132 P \u0012 ℓ χ ,0 \u0013 . (17) Using Eq. (7), the predicted FLRW angular power spec- trum of magnitude fluctuations due to lensing is then,"},{"citing_arxiv_id":"2605.26050","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Early- and Late-Time Modifications to $\\Lambda$CDM: Implications for the Hubble Tension","primary_cat":"astro-ph.CO","submitted_at":"2026-05-25T17:12:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"An extended model with decaying dark matter around equality and w0 dark energy yields H0 ≈ 70 km/s/Mpc from Planck+ACT+DESI data, reducing Hubble tension to ~2.2σ while producing Bayesian evidence comparable to ΛCDM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17813","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Positive Running of the Spectral Index for Scalar Theory and Modified Gravity","primary_cat":"gr-qc","submitted_at":"2026-05-18T03:39:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Positive running of the spectral index is achievable in Einstein-Gauss-Bonnet gravity with viable inflation, unlike standard scalar field and F(R) models which face challenges.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Oikonomou, Phys. Rev. D108(2023) no.4, 043516 doi:10.1103/PhysRevD.108.043516 [arXiv:2306.17351 [astro-ph.CO]]. [18] T. Louiset al.[ACT], [arXiv:2503.14452 [astro-ph.CO]]. [19] E. Calabreseet al.[ACT], [arXiv:2503.14454 [astro-ph.CO]]. [20] A. G. Adameet al.[DESI], JCAP04(2025), 012 doi:10.1088/1475-7516/2025/04/012 [arXiv:2404.03000 [astro-ph.CO]]. [21] D. H. Lee, W. Yang, E. Di Valentino, S. Pan and C. van de Bruck, [arXiv:2507.11432 [astro-ph.CO]]. [22] E. ¨Oz¨ ulker, E. Di Valentino and W. Giar` e, [arXiv:2506.19053 [astro-ph.CO]]. [23] D. A. Kessler, L. A. Escamilla, S. Pan and E. Di Valentino, [arXiv:2504.00776 [astro-ph.CO]]. [24] S. Nojiri, S. D. Odintsov and V. K. Oikonomou, [arXiv:2506.21010 [gr-qc]]."},{"citing_arxiv_id":"2605.14027","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"A No-Go Theorem for Topological Bridges with Matter-Vacuum Coupling","primary_cat":"gr-qc","submitted_at":"2026-05-13T18:38:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Matter-vacuum coupling cannot eliminate the need for null energy condition violation in static zero-tidal-force traversable topological bridges.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11079","ref_index":45,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"New Isocurvature Constraints from JWST UV Luminosity Function","primary_cat":"astro-ph.CO","submitted_at":"2026-05-11T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"First UVLF-based constraints on model-agnostic isocurvature power spectra for CDM, baryon, neutrino, and dark radiation modes yield consistent 95% credible envelopes over k ~ 0.5-10 Mpc^{-1}.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"with Photometrically Classified Pan-STARRS Supernovae. II. Cosmological Parameters,Astrophys. J. 857(2018) 51, [1710.00846]. 20 [44] P. A. Oesch, R. J. Bouwens, G. D. Illingworth, I. Labbé and M. Stefanon,The dearth of z∼ 10 galaxies in all hst legacy fields-the rapid evolution of the galaxy population in the first 500 myr*,The Astrophysical Journal855 (mar, 2018) 105. [45] R. J. Bouwens, P. A. Oesch, M. Stefanon, G. Illingworth, I. Labbé, N. Reddy et al.,New determinations of the uv luminosity functions from z∼9 to 2 show a remarkable consistency with halo growth and a constant star formation efficiency,The Astronomical Journal162(jul, 2021) 47. [46] C. T. Donnan, R. J. McLure, J. S. Dunlop, D. J. McLeod, D. Magee, K."},{"citing_arxiv_id":"2605.10102","ref_index":68,"ref_count":2,"confidence":0.9,"is_internal_anchor":true,"paper_title":"From Large Telescopes to the MUltiplexed Survey Telescope (MUST)","primary_cat":"astro-ph.IM","submitted_at":"2026-05-11T07:18:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"MUST is a new 6.5 m telescope designed to deliver simultaneous optical spectra for over 20,000 targets across a 5 deg² field, enabling the largest 3D spectroscopic map of the Universe with redshifts for more than 100 million objects over an 8-year survey.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The ten spectrographs split the light into three channels that overall cover the wavelength of 360-980 nm with a resolution of 2000 to 5000. Till now, DESI has constructed the largest and most precise 3D map of the universe. DESI's first-year data have provided unprecedented precision, with measure- ments of the Universe's expansion history, achieving a cur- rent accuracy of nearly or slightly better than 1% [68-70]. The Prime Focus Spectrograph (PFS) on the Subaru Tele- scope is currently conducting its commissioning [71]. PFS is a powerful multi-object spectrograph designed to take ad- vantage of Subaru's 1.3 deg 2 field of view at its prime fo- cus [38, 72]. Developed by an international collaboration led by the Kavli Institute for the Physics and Mathematics of"},{"citing_arxiv_id":"2604.27954","ref_index":110,"ref_count":2,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Axion dark matter from extended misalignment with a constant-$\\omega_\\phi$ pre-oscillatory phase and dark radiation","primary_cat":"astro-ph.CO","submitted_at":"2026-04-30T14:51:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Extended misalignment for axion-like particles with constant-ω_ϕ pre-oscillation and dark radiation coupling yields data-driven constraints favoring negative ω_ϕ and f_ϕ in [80, 1.5×10^10] TeV but does not ease cosmological tensions.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"whereP µ is the conjugated momentum of the coordinatex µ. Following Ref. [88] we get the relation between the conjugate momentum and the momentum at a fixed spatial coordinate pi =p i. In general, one defines the action LDR = 1 2 gµνuµ DRuν DR,(109) whereu µ DR =dx µ DR/dτis the dark photon 4-velocity. Then, the conjugated momentum is given by Pµ = ∂L ∂uµ DR =g µνuν DR →P µ =u µ DR (110) For the zero-th component we have P 0 =u 0 DR.(111) From the action above, the geodesic equation is thus duµ DR dτ + Γµ νρuν DRuρ DR = 0.(112) Using that duµ DR dτ = dP µ dτ =P ′µu0 =P 0P ′µ,(113) the geodesic equation becomes P 0P ′µ + Γµ νρP νP ρ = 0.(114) This together with the restriction of null-geodesic gµνuµ DRuν DR = 0→g µνP µP ν = 0,(115)"},{"citing_arxiv_id":"2604.26915","ref_index":107,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Testing Scale-Dependent Modified Gravity with DESI DR1","primary_cat":"astro-ph.CO","submitted_at":"2026-04-29T17:26:36+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"DESI DR1 constrains the modified gravity parameter to log10 |f_R0| < -4.59 at 95% CL, implying no detectable fifth force on scales below about 18 Mpc.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"[105]DESIcollaboration, H. Zhang et al.,Enhancing DESI DR1 full-shape analyses using HOD-informed priors,JCAP11(2025) 049, [2504.10407]. [106] M. M. Ivanov, A. Obuljen, C. Cuesta-Lazaro and M. W. Toomey,Full-shape analysis with simulation-based priors: Cosmological parameters and the structure growth anomaly,Phys. Rev. D111(2025) 063548, [2409.10609]. [107] S. Paradiso, M. Bonici, M. Chen, W. J. Percival, G. D'Amico, H. Zhang et al.,Reducing nuisance prior sensitivity via non-linear reparameterization, with application to EFT analyses of large-scale structure,2412.03503. [108] DESI Collaboration, A. G. Adame, J. Aguilar, S. Ahlen, S. Alam, D. M. Alexander et al., DESI 2024 II: sample definitions, characteristics, and two-point clustering statistics, J."},{"citing_arxiv_id":"2604.05213","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Local primordial non-Gaussianity using cross-correlations of DESI tracers","primary_cat":"astro-ph.CO","submitted_at":"2026-04-06T22:18:36+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Cross-correlating LRG and QSO samples in DESI DR1 yields f_NL^loc = 2.1 with 68% uncertainties of +8.8 and -8.3, an incremental improvement over auto-correlations alone.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.13053","ref_index":68,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"A unified harmonic framework for dark siren cosmology","primary_cat":"astro-ph.CO","submitted_at":"2026-03-13T15:03:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The GW-galaxy cross-correlation method, unified with spectral sirens in a harmonic framework, can measure H0 to 1% and Omega_m to 5% precision with 2 years of data from next-generation detectors like Einstein Telescope and Cosmic Explorer.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Wide-Angle Galaxy Surveys, ApJL498, L1 (1998), arXiv:astro-ph/9712007 [astro-ph]. [66] C. Bonvin and R. Durrer, What galaxy surveys really measure, PhRvD84, 063505 (2011), arXiv:1105.5280 [astro-ph.CO]. [67] S. Mastrogiovanni, C. Karathanasis, J. Gair, G. Ash- ton, S. Rinaldi, H.-Y. Huang, and G. D' alya, Cosmol- ogy with Gravitational Waves: A Review, AnP536, 2200180 (2024). [68] A. Palmese and S. Mastrogiovanni, Gravitational Wave Cosmology, arXiv , arXiv:2502.00239 (2025), arXiv:2502.00239 [astro-ph.CO]. [69] R. Essick and M. Fishbach, Ensuring Consistency be- tween Noise and Detection in Hierarchical Bayesian In- ference, ApJ962, 169 (2024), arXiv:2310.02017 [gr-qc]. [70] P. J. E. Peebles,The Large-Scale Structure of the Uni-"},{"citing_arxiv_id":"2603.10787","ref_index":119,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Measuring neutrino mass in light of ACT DR6 and DESI DR2","primary_cat":"astro-ph.CO","submitted_at":"2026-03-11T14:00:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New ACT and DESI data yield model-dependent upper limits on sum of neutrino masses, with holographic dark energy giving the tightest bounds and a consistent preference for degenerate hierarchy.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"In this context, baryon acoustic oscillation (BAO) mea- surements play a central role, and the Dark Energy Spectroscopic Instrument (DESI) collaboration has pro- vided substantial evidence for a dynamical DE compo- nent [118], based on BAO measurements using galax- ies, quasars, and Lyman- α forest tracers from the first data release (DR1) of DESI [119, 120]. Interestingly, this dynamical DE evidence is further supported [121, 122] by the DESI second data release (DR2), which includes more than 14 million galaxies and quasars, based on three years of operation [123]. Beyond the evidence for dynam- ical DE, DESI BAO data have also been widely used in various cosmological analyses [48, 53, 124-180]."},{"citing_arxiv_id":"2601.21432","ref_index":135,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Cosmological analysis of the DESI DR1 Lyman alpha 1D power spectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-01-29T09:08:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI DR1 Lyman-alpha data yields Δ²★=0.379±0.032 and n★=-2.309±0.019 at k★=0.009 km⁻¹s and z=3, sharpening N_eff, α_s, and β_s constraints by factors of 1.18-1.90 when combined with other probes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"measurements probe much smaller scales than those accessed byPlanck. We derive constraints on ΛCDM extensions by combining our measurements with three different datasets: a)PlanckT&E measurements; b) the combination of DESI-DR2 BAO measurements (DESI BAO; [38, 39]) and temperature, polarization, and lensing data from Planck, ACT-DR6, and SPT-3G (CMB-SPA; [35]); and c) the combination BAO [112, 135, - 40 - 0.9 1.0 1.1 1.2 Ly P1D CMB T&E DESI P1D Planck T&E: CDM 0.9 1.0 1.1 1.2 Ly P1D CMB T&E Planck T&E: m Planck T&E: Neff 10 4 10 3 10 2 k[km 1s] 0.9 1.0 1.1 1.2 Ly P1D CMB T&E Planck T&E: s Planck T&E: s, s Plin(k, z = 3)/P CDM lin (k, z = 3) Figure 22. Constraints on the shape of the linear matter power spectrum atz= 3. The blue datapoints display the ratio of our constraints on ∆ 2 ⋆ andn ⋆ and those fromPlanckT&E for ΛCDM, with the error bar and shaded area indicating the 1σregion for the first and second, respectively."},{"citing_arxiv_id":"2511.20757","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Reanalyzing DESI DR1: 2. Constraints on Dark Energy, Spatial Curvature, and Neutrino Masses","primary_cat":"astro-ph.CO","submitted_at":"2025-11-25T19:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Reanalysis of DESI full-shape clustering data tightens constraints on neutrino mass, spatial curvature, and dark energy equation-of-state parameters relative to BAO-only results.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Chudaykin, M. M. Ivanov, and O. H. E. Philcox, (2025), arXiv:2507.13433 [astro-ph.CO]. [2] M. Abdul Karimet al.(DESI), (2025), arXiv:2503.14738 [astro-ph.CO]. [3] K. Lodhaet al.(DESI), (2025), arXiv:2503.14743 [astro-ph.CO]. [4] G. Guet al.(DESI), (2025), arXiv:2504.06118 [astro-ph.CO]. 17 [5] A. G. Adameet al.(DESI), (2024), arXiv:2411.12020 [astro-ph.CO]. [6] A. G. Adameet al.(DESI), (2024), arXiv:2404.03000 [astro-ph.CO]. [7] A. G. Adameet al.(DESI), JCAP01, 124 (2025), arXiv:2404.03001 [astro-ph.CO]. [8] A. G. Adameet al.(DESI), JCAP02, 021 (2025), arXiv:2404.03002 [astro-ph.CO]. [9] D. Broutet al., Astrophys. J.938, 110 (2022), arXiv:2202.04077 [astro-ph.CO]. [10] T. M. C. Abbottet al.(DES), Astrophys."},{"citing_arxiv_id":"2511.18657","ref_index":49,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"How Complex is Dark Energy? A Bayesian Analysis of CPL Extensions with Recent DESI BAO Measurements","primary_cat":"astro-ph.CO","submitted_at":"2025-11-23T23:56:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian evidence from DESI BAO plus CMB and SN data favors the standard CPL evolving dark energy model over both simpler constant-w and more complex higher-order extensions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.08266","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Euclid preparation: LXXXVII. Non-Gaussianity of 2-point statistics likelihood: Precise analysis of the matter power spectrum distribution","primary_cat":"astro-ph.CO","submitted_at":"2025-11-11T13:59:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Matter power spectrum measurements show strong non-Gaussian skewness on nonlinear scales at low redshift, driven by pentaspectrum contributions and amplified by survey geometry and integral constraint.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.06453","ref_index":32,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Inflationary models in a minimally coupled $f(R,T)$ gravity: Constraints from $Planck$, BICEP/$Keck$, and ACT","primary_cat":"gr-qc","submitted_at":"2025-11-09T16:37:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Three standard inflationary potentials remain compatible with Planck, BICEP/Keck, DESI DR2, and ACT DR6 data when placed in minimally coupled f(R,T)=R+16πGλT gravity for suitable ranges of the model parameters and coupling λ.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.19149","ref_index":75,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"$H_0$ Without the Sound Horizon (or Supernovae): A 2% Measurement in DESI DR1","primary_cat":"astro-ph.CO","submitted_at":"2025-10-22T00:46:39+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A heuristic power-spectrum rescaling applied to DESI DR1 BAO data plus CMB acoustic scale anchor yields H0 values of 69.2 to 70.3 km/s/Mpc at sub-2% precision across three independent late-time datasets.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.05467","ref_index":39,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Combined tracer analysis for DESI 2024 BAO","primary_cat":"astro-ph.CO","submitted_at":"2025-08-07T15:06:22+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Combining LRG and ELG tracers with bias weighting improves BAO constraints by 11% on alpha_iso and 7% on alpha_AP in DESI DR1 data for the 0.8<z<1.1 bin.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.24732","ref_index":5,"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":", Measurements of Ω and Λ from 42 High Redshift Supernovae, Astrophys. J. 517 (1999) 565-586. arXiv:astro-ph/9812133. [3] A. Aghamousa, et al., The DESI Experiment Part I: Science,Targeting, and Survey Design (10 2016).arXiv:1611.00036. [4] B. Abareshi, et al., Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument, Astron. J. 164 (5) (2022) 207.arXiv:2205.10939. [5] A. G. Adame, et al., DESI 2024 III: baryon acoustic oscillations from galaxies and quasars, JCAP 04 (2025) 012. arXiv:2404.03000. [6] A. G. Adame, et al., DESI 2024 IV: Baryon Acoustic Oscillations from the Lyman alpha forest, JCAP 01 (2025) 124. arXiv:2404.03001. [7] A. G. Adame, et al., DESI 2024 VI: cosmological constraints from the measurements of baryon acoustic oscillations,"},{"citing_arxiv_id":"2505.10534","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"ACT-ing on inflation: Implications of non Bunch-Davies initial condition and reheating on single-field slow roll models","primary_cat":"astro-ph.CO","submitted_at":"2025-05-15T17:45:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Non-Bunch-Davies initial conditions substantially improve the fit of various single-field slow-roll inflation models to updated n_s-r constraints from ACT DR6 combined with Planck, DESI, and BICEP/Keck data.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"652, C4 (2021)], arXiv:1807.06209 [astro-ph.CO]. [7] F. Geet al.(SPT-3G), Phys. Rev. D111, 083534 (2025), arXiv:2411.06000 [astro-ph.CO]. [8] T. Louiset al.(ACT), (2025), arXiv:2503.14452 [astro- ph.CO]. [9] E. Calabreseet al.(ACT), (2025), arXiv:2503.14454 [astro-ph.CO]. [10] A. G. Adameet al.(DESI), JCAP04, 012 (2025), arXiv:2404.03000 [astro-ph.CO]. [11] A. G. Adameet al.(DESI), JCAP02, 021 (2025), arXiv:2404.03002 [astro-ph.CO]. [12] P. A. R. Adeet al.(BICEP2, Keck Array), Phys. Rev. Lett.121, 221301 (2018), arXiv:1810.05216 [astro- ph.CO]. [13] P. A. R. Adeet al.(BICEP, Keck), Phys. Rev. Lett.127, 151301 (2021), arXiv:2110.00483 [astro-ph.CO]. [14] M. Tristramet al., Phys. Rev. D105, 083524 (2022),"},{"citing_arxiv_id":"2503.14744","ref_index":96,"ref_count":1,"confidence":0.9,"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":"(including visual inspections [88, 89]) with an early data release [90]. DESI survey operations [91] already pro- vided us with the first data release (DR1) [92], and mea- surements of galaxy clustering [93] were used to derive precise BAO measurements, from both galaxy and quasar clustering [94] and the Lyman- α forest [95], as well as a FS analysis of galaxies and quasars [96]. DR1 cosmolog- ical results were presented in [42, 43]. The second data release (DR2), used in this analysis, includes three years of observations, which were processed with spectroscopic reduction [97] and redshift estimation [98, 99] pipelines. A. DESI DR2 BAO We use BAO measurements from DESI DR2, based on 14 million galaxy and quasar spectroscopic redshift"},{"citing_arxiv_id":"2503.14743","ref_index":39,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Extended Dark Energy analysis using DESI DR2 BAO measurements","primary_cat":"astro-ph.CO","submitted_at":"2025-03-18T21:14:17+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Extended analysis of DESI DR2 data confirms robust evidence for dynamical dark energy with phantom crossing preference, stable under parametric and non-parametric modeling.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"and its successful survey validation [35] based on early data [36] showed that it meets the expected requirements of a Stage-IV survey. In particular, its Data Release 1 (DR1 [37]) has already provided new insights into the be- havior of dark energy. DESI DR1 measured the baryon acoustic oscillations (BAO) signature in the clustering of galaxies and quasars [38], as well as the Lyman- α for- est [39]. The combined constraints from DESI DR1 BAO and external data [40], followed up with a similar analysis 4 that combines the BAO with the full clustering informa- tion from DESI galaxies and other tracers [41, 42], as well as the supporting DESI DR1 papers that considered al- ternative descriptions of the dark energy sector [43, 44], all showed tantalizing hints of the departures from the"},{"citing_arxiv_id":"2503.14739","ref_index":57,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"DESI DR2 Results I: Baryon Acoustic Oscillations from the Lyman Alpha Forest","primary_cat":"astro-ph.CO","submitted_at":"2025-03-18T21:14:13+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"DESI DR2 delivers 0.65% precision BAO measurements from the LyA forest at z_eff=2.33, with D_H/r_d = 8.632 ± 0.098 ± 0.026 and D_M/r_d = 38.99 ± 0.52 ± 0.12.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2503.14738","ref_index":22,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"DESI DR2 Results II: Measurements of Baryon Acoustic Oscillations and Cosmological Constraints","primary_cat":"astro-ph.CO","submitted_at":"2025-03-18T21:14:12+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI DR2 BAO data exhibits 2.3 sigma tension with CMB in Lambda-CDM but prefers evolving dark energy (w0 > -1, wa < 0) at 3.1 sigma with CMB and 2.8-4.2 sigma when including supernovae.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ferent reconstruction algorithms in the context of DESI [72]. The reconstructed catalogs are used for the clus- tering and associated BAO measurements from galaxies and quasars presented throughout the rest of this paper. B. Lyman- α forest catalog The DESI DR2 quasar catalog for the Lyα forest anal- ysis was constructed in a similar manner to the DR1 cat- alog described in [22]. The catalog contains high-redshift quasars and is built from the outputs of three automatic classifiers that analyze all quasar targets: the Redrock redshift estimator [57] that classifies based on templates, including quasar templates optimized for DESI quasars [73, 74], a Mg II afterburner that searches for broad Mg II emission in quasar candidates classified as galaxies, and"},{"citing_arxiv_id":"2411.12022","ref_index":64,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements","primary_cat":"astro-ph.CO","submitted_at":"2024-11-18T20:03:35+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI DR1 full-shape clustering yields Ω_m = 0.2962 ± 0.0095 and σ_8 = 0.842 ± 0.034 in flat ΛCDM, tightening to H_0 = 68.40 ± 0.27 km/s/Mpc with CMB and DESY3, while favoring w_0 > -1, w_a < 0 and limiting neutrino mass sum to < 0.071 eV.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"observations from DESI, which is based on DESI Data Release 1 (DR1; [62]). This is the second paper that focuses on key cosmological parameter measurements from DESI DR1; in the first paper [63], we presented cosmological measurements from the information in baryon acoustic oscillations in DESI DR1 data, based on the analysis of galaxy and quasar clustering [64], and that in the Ly α forest data [65]. In this paper, we significantly extend those results by complementing the BAO information with the \"full-shape\" analysis which models the overall clustering signal of DESI tracers across time and space, and report the resulting cosmological constraints from the combined BAO + full-shape analysis. - 2 - The data behind the analysis, and the plans for their release, are presented in [62], while"},{"citing_arxiv_id":"2411.12021","ref_index":73,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars","primary_cat":"astro-ph.CO","submitted_at":"2024-11-18T20:03:34+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI DR1 full-shape galaxy clustering constrains Omega_m = 0.296 ± 0.010, H0 = 68.63 ± 0.79 km/s/Mpc, and sigma_8 = 0.841 ± 0.034, consistent with LambdaCDM and Planck.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"After validating these mod- elling approaches on simulations we apply them to the DESI data release 1 (DR1) galaxy samples. Our analysis yields the best constraints on the clustering amplitude to date and the most precise cosmological constraints from DESI DR1 data alone, combining our galaxy Full-Shape measurements with the galaxy and quasar BAO measurements presented in [73] and the LyαBAO presented in [74]. The detailed cosmological inference including the com- bination with other cosmological probes is covered in a companion paper [1]. An analysis of the power spectrum to constrain potential primordial non-Gaussian signals is also presented in [75]. This paper is organised as follows, in Section 2 we present the DESI DR1 large-scale"},{"citing_arxiv_id":"2411.07970","ref_index":14,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"MUltiplexed Survey Telescope (MUST) Science White Paper I: Overview of Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Surveys","primary_cat":"astro-ph.CO","submitted_at":"2024-11-12T17:51:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"MUST is a planned 6.5m Stage-V spectroscopic survey telescope targeting 100M+ galaxies and quasars to z~5.5 for large-scale structure cosmology studies.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"verse at low and intermediate redshift (z≲3). Clustering measurements from spectroscopic surveys of galaxies and quasars have become a key probe of cosmology. They pro- vide precise measurements on the baryon acoustic oscilla- tions (BAO) scale [12] and the linear growth rate of structure fσ 8 through redshift space distortions (RSD) [13]. Recent results from the DESI collaboration [14] suggest a poten- tial deviation from the cosmological constant to time-varying dark energy. By the end of this decade, we expect to have sub-percent-level constraints on dark energy and gravity from galaxy clustering up to redshiftz∼2. When the DESI project concludes, we will have completed the spectroscopic survey component of the four stages outlined in the Dark Energy"},{"citing_arxiv_id":"2404.03002","ref_index":79,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"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":"expansion of the universe [74-77]. In this paper, we report the constraints derived from the measurements of baryon acous- tic oscillations with the first year of data from DESI as part of a larger series of papers. The results of this paper build upon the two-point measurements and validation, as detailed in [78]; the BAO measurement from galaxies and quasars as summarised in [79]; and the Ly- α forest BAO measurements and validation described in [80]. In a follow-up paper, the cluster- ing analysis of the first year of DESI data is also performed over a wider range of scales than just the BAO feature including the effects of redshift space distortions (RSD) [81]. The Data 1An exception is the Ly α BAO measurement, limited by the number of spectra and their signal-to-noise,"},{"citing_arxiv_id":"2404.03001","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI 2024 IV: Baryon Acoustic Oscillations from the Lyman Alpha Forest","primary_cat":"astro-ph.CO","submitted_at":"2024-04-03T18:41:50+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI measures BAO from the Lyα forest at z_eff=2.33, reporting H(z) = (239.2 ± 4.8) (147.09 Mpc/rd) km/s/Mpc and DM(z) = (5.84 ± 0.14) (rd/147.09 Mpc) Gpc.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"DR1, [5]), covering data collected until June 14, 2022, contains about 13 million galaxies, 1.5 million quasars, and 4 million stars over an area of more than 9 500 square degrees 1. DESI has obtained seven BAO measurements at different redshifts with this DR1 dataset. The BAO measurements from the clustering of DESI galaxies and quasars at z < 2 are presented in [6]. In this publication we present a BAO measurement at z = 2.33 using the auto-correlation of the Lyman- α (Lyα) forest dataset from DESI DR1 and its cross- correlation with quasar positions. Neutral hydrogen along the line-of-sight towards high- redshift quasars cause absorption features in their spectra. While gas pressure dominates the distribution of gas on scales of tens of kiloparsecs [7], on larger scales the Ly α forest is"}],"limit":50,"offset":0}