{"total":43,"items":[{"citing_arxiv_id":"2605.18615","ref_index":81,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Primordial power spectrum reconstructions from BOSS + eBOSS","primary_cat":"astro-ph.CO","submitted_at":"2026-05-18T16:25:02+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Non-parametric knot-based reconstruction of the primordial power spectrum P_R(k) from BOSS+eBOSS data up to k=0.3 h/Mpc favors a quasi-scale-invariant power law and constrains n_s = 0.976 ± 0.021 with no evidence for primordial features.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12482","ref_index":61,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Unveiling $f(R)$ Gravity with Void-Galaxy Cross-Correlation Multipoles","primary_cat":"astro-ph.CO","submitted_at":"2026-05-12T17:57:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Semi-analytical calculation of void-galaxy cross-correlation multipoles in Hu-Sawicki f(R) gravity reveals size-dependent deviations from LambdaCDM up to 29.7 percent for small voids, amplified by nonlinear evolution and potentially observable in Stage-IV surveys.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"86, 157 (2007), arXiv:0706.2041 [astro-ph]. [59] P. Brax, A.-C. Davis, B. Li, H. A. Winther, and G.-B. Zhao, Systematic simulations of modified grav- ity: chameleon models, JCAP10, 002, arXiv:1206.3568 [astro-ph.CO]. [60] Y. Nan and K. Yamamoto, Large-scale inhomogeneity of dark energy produced in the ancestor vacuum, Phys. Rev. D99, 123512 (2019). [61] Y. Nan and K. Yamamoto, Dark energy model with very large scale inhomogeneity, Phys. Rev. D105, 063518 (2022). [62] E. L. D. Perico, R. Voivodic, M. Lima, and D. F. Mota, Cosmic voids in modified gravity scenarios, Astron. Astrophys.632, A52 (2019), arXiv:1905.12452 [astro- ph.CO]. [63] M. Sahlen, Cluster-void degeneracy breaking: dark en- ergy, Planck, and the largest cluster and void, Phys."},{"citing_arxiv_id":"2605.11890","ref_index":34,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"A cosmology-to-ringdown EFT consistency map for scalar-tensor gravity","primary_cat":"gr-qc","submitted_at":"2026-05-12T10:05:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"An EFT consistency map transports cosmology-conditioned posteriors from scalar-tensor FLRW backgrounds to black-hole quasinormal-mode kernels, showing tensor-speed effects fall below ringdown detectability while other operators remain potentially active near black holes.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"level, but it is sufficiently complete to exercise the full transport chain. The data vector is a deterministic, survey-calibrated simulation with fiducial background given by the Planck-2018 flat-ΛCDM point,(Ω m0,h,σ8) = (0.315, 0.674, 0.811)[ 33]; its distance/growth redshifts and fractional errors follow the structure of public BAO/RSD compressed summaries [34]. The likelihood is transparent, repeatable, and readily replaceable by a full EFTCAMB/hi_class chain. The compressed data vector contains BAO-like distance measurements, RSD-like growth measurements, and a GW170817-like homogeneous tensor-speed datum, dmock ={DM(zi)/rd, DH(zi)/rd, fσ8(zj), τT}, τT≡1015αT0,(2.4) where zi = (0.38, 0.51, 0.61, 0.85, 1."},{"citing_arxiv_id":"2605.11658","ref_index":22,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"GI BAO as a cosmological consistency check","primary_cat":"astro-ph.CO","submitted_at":"2026-05-12T07:20:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"GI BAO provides a robust consistency check for density BAO and shear data, with the first photometric measurement on DES Y3 showing agreement at α = 0.966 ± 0.252.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"BAO measurement, shear measurement, and alignment model. Discrepancy between them hints at the existence of untreated systematics in any of these parts. As an example, we measure the GI BAO on a photo- metric data sample from the Dark Energy Survey (DES) Y3 and demonstrate its consistency with the density BAO measurement. DES has presented the transverse (density)BAOmeasurementintheirY1[20], Y3[22], and Y6 [24] analyses. DES Y3 BAO analysis yields a 2.7% constraint on the transverse BAO, and interestingly, it shows 2σdeviation from the Planck cosmology [31]. The difference persists in the more recent Y6 analysis [24], which was later used to perform a joint analysis with the DES 5 Yr SNe sample [32] and was found to support the evolving dark energy model [33], in agreement with"},{"citing_arxiv_id":"2605.10102","ref_index":62,"ref_count":1,"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":"From 2014 to 2020, SDSS-IV further ex- panded the survey's capabilities with projects such as the ex- tended BOSS (eBOSS) and the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA). The eBOSS aimed to refine cosmological parameters by mapping the distribution of galaxies and quasars over a larger volume, enhancing the precision of BAO measurements [22, 62]. MaNGA focused on integral field spectroscopy of around 10,000 nearby galax- ies, allowing detailed studies of their internal structures, star formation processes, and evolutionary states [63]. SDSS represents a triumph for spectroscopic telescopes. As evidenced by [57], SDSS, despite its modest aperture of 2.5 m, has surpassed both the Hubble Space Telescope and"},{"citing_arxiv_id":"2605.07720","ref_index":54,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"TopoFisher: Learning Topological Summary Statistics by Maximizing Fisher Information","primary_cat":"stat.ML","submitted_at":"2026-05-08T13:25:25+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"TopoFisher optimizes trainable filtrations, vectorizations, and compressors in persistent homology to maximize Fisher information, yielding higher information than fixed cosmological summaries and approaching neural baselines with far fewer parameters while generalizing better under simulator shifts","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.22372","ref_index":38,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"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":"Alam, B. 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INTRODUCTION Over the past decade, precision cosmology has entered an era in which multiple independent probes can map the expansion history of the Universe with unprecedented accuracy. The measurements of cosmic microwave back- ground (CMB) by Planck [ 1], baryon acoustic oscilla- tion (BAO) measurements from eBOSS [ 2] as well as DESI [ 3], and large Type Ia supernova (SN) compila- tions including PantheonPlus [ 4] and the recent DES five-year supernova analysis [ 5] together provide remark- ably stringent tests of the standard cosmological frame- work. Within this observational landscape, the Λ-cold- dark-matter ( ΛCDM) model has achieved extraordinary success and remains the benchmark description of mod-"},{"citing_arxiv_id":"2603.21125","ref_index":9,"ref_count":1,"confidence":0.9,"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":"2602.11936","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing Dynamical Dark Energy with Late-Time Data: Evidence, Tensions, and the Limits of the $w_0w_a$CDM Framework","primary_cat":"astro-ph.CO","submitted_at":"2026-02-12T13:35:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Evidence for dynamical dark energy in the w0waCDM framework is strongly dataset-dependent, driven by mismatches in low-redshift BAO distance ratios that produce divergent expansion histories and inconsistent Hubble tension relief.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"08991 [astro-ph.CO]. 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Babu, inTheoretical Advanced Study Institute in Elementary Particle Physics: The"},{"citing_arxiv_id":"2512.19186","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Illuminating the Dark Sector: Understanding Modified Gravity Signatures with Cross-Correlations of Gravitational Waves and Large-Scale Structure","primary_cat":"astro-ph.CO","submitted_at":"2025-12-22T09:19:39+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Forecasts indicate that LSS-GW cross-correlations with Stage-IV surveys and Einstein Telescope tighten constraints on modified gravity parameters beyond those from LSS observations alone.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.07236","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Counting voids and filaments: Betti Curves as a Powerful Probe for Cosmology","primary_cat":"astro-ph.CO","submitted_at":"2025-12-08T07:33:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Betti curves from persistent homology of large-scale structure provide complementary cosmological constraints on ns, sigma8, and Om, with tighter bounds when analyzed jointly with the power spectrum.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.09202","ref_index":95,"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":"method","top_context_polarity":"use_method","context_text":"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 + baryons),Ω 𝑏 is the baryon density, andℎ≡𝐻 0/1004. The photon density is fixed toΩ 𝛾 ℎ2 =2.47×10 −5. •PLA Data:This data set is a compressed ver- sion of the full Planck likelihood [24], reported in"},{"citing_arxiv_id":"2508.08638","ref_index":102,"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":"2508.05467","ref_index":10,"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 0.83σ while the effective equation of state stays above w=-1 and other tensions on neutrino mass and growth rate are relieved.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"constant in the late Universe. Such a non-minimal coupling is preferred over 3 σ confidence level. The worsened Ωm tension and S8 tension in the w0waCDM model are also resolved in our model. Introduction.- The Planck measurement of cosmic microwave background (CMB) [1], along with the com- pleted Sloan Digital Sky Survey (SDSS) of baryon acous- tic oscillations (BAO) [2] and the PantheonPlus compila- tion of Type Ia supernovae (SNe Ia) [3], all agree roughly on the same parameter region of Λ-cold-dark-matter (ΛCDM) model. However, the recent data release 2 (DR2) of BAO results from three-year (Y3) observations with Dark Energy Spectroscopic Instrument (DESI) [4], when combined with both Planck-CMB and five-year compilation of Dark Energy Survey (DESY5) [5] of SNe"},{"citing_arxiv_id":"2507.09981","ref_index":78,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"New Insights into Dark Energy from DESI DR2 with CMB and SNIa","primary_cat":"astro-ph.CO","submitted_at":"2025-07-14T06:55:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Systematic dataset swaps show DESY5 low-redshift SNIa, Planck CMB plus lensing, and DESI-DR2 BAO as the dominant sources of w0waCDM tension with ΛCDM, while other combinations remain consistent.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.05207","ref_index":141,"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":"observables correspond to distance priors - the acoustic scale 𝑙 𝐴 and shift parameter 𝑅. These priors effectively encode information about the CMB temperature power 10 spectrum. The acoustic scale characterizes the angular scale of the sound horizon, influencing peak spacing, while the shift parameter affects the line-of-sight direc- tion, impacting peak heights. The shift parameter is defined as [141]: 𝑅(𝑧∗) ≡ (1 + 𝑧∗)𝐷 𝐴(𝑧∗) √︃ Ω𝑚0 𝐻2 0 𝑐 , (6.4) where 𝑧∗ = 1089.92 is the redshift at photon decoupling [71], and 𝐷 𝐴 is the angular diameter distance for a flat geometry given by: 𝐷 𝐴 = 𝑐 (1 + 𝑧) ∫ 𝑧 0 𝑑𝑧 𝐻 (𝑧) . (6.5) Here, Ω𝑚0 denotes the total matter density at present. For the minimally coupled case, where both bary- onic and dark matter are pressureless and indi-"},{"citing_arxiv_id":"2506.13537","ref_index":14,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting $\\Lambda$CDM extensions in light of re-analyzed CMB data","primary_cat":"astro-ph.CO","submitted_at":"2025-06-16T14:26:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Re-analysis with PR4 Planck likelihoods reduces lensing anomaly significance and curvature preference in Lambda CDM extensions while indicating a preference for evolving dark energy consistent with DESI.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2505.22066","ref_index":72,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmic Strings as Dynamical Dark Energy: Novel Constraints","primary_cat":"astro-ph.CO","submitted_at":"2025-05-28T07:45:53+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Cosmic string networks are constrained to less than ~1% of the energy density using CMB+BAO+SN data, with some models preferring mildly negative densities but no Bayesian evidence favoring them over LambdaCDM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2503.14744","ref_index":72,"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":"background","top_context_polarity":"background","context_text":"arXiv:astro-ph/0208512 [astro-ph]. 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Astrophys."},{"citing_arxiv_id":"2503.14739","ref_index":4,"ref_count":1,"confidence":0.98,"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":42,"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":"Escoffier, and others, MNRAS 470, 2617 (2017), arXiv:1607.03155 [astro-ph.CO]. [41] S. Alam, M. Aubert, S. Avila, C. Balland, J. E. Bautista, M. A. Bershady, D. Bizyaev, M. R. Blan- ton, A. S. Bolton, J. Bovy, J. Brinkmann, J. R. Brown- stein, E. Burtin, S. Chabanier, M. J. Chapman, and oth- ers, Phys. Rev. D 103, 083533 (2021), arXiv:2007.08991 [astro-ph.CO]. [42] DES Collaboration, T. M. C. Abbott, M. Acevedo, M. Adamow, M. Aguena, A. Alarcon, S. Allam, O. Alves, F. Andrade-Oliveira, J. Annis, P. Arm- strong, S. Avila, D. Bacon, K. Bechtol, J. Blazek, and others, arXiv e-prints , arXiv:2503.06712 (2025), arXiv:2503.06712 [astro-ph.CO]. [43] J. Frieman, M. Turner, and D. Huterer, Ann. Rev. As- tron. Astrophys."},{"citing_arxiv_id":"2411.12022","ref_index":27,"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":"baseline","top_context_polarity":"baseline","context_text":"constraints from shear measured in the photometric KiDS-1000 survey combined with spec- troscopic galaxy clustering in BOSS and the 2-degree Field Lensing Survey (2dFLenS) (KiDS- 1000+BOSS+2dFLenS; [144]); and the combined shear and clustering 3 × 2-pt analysis from the DESY3 data [102]. The second-to-bottom whisker shows the constraints from the SDSS RSD+BAO analysis [27] that used a full-shape analysis that was substantially different in de- tail to our Full Modeling. We observe an excellent agreement between DESI DR1 (FS+BAO) and the CMB, both of which are slightly higher than the values inferred from the weak lens- ing surveys. There remains some modest difference between our constraint in Eq. (3.2) and that from the lensing probes; for example, the DESY3 measurement is S8 = 0."},{"citing_arxiv_id":"2411.12021","ref_index":84,"ref_count":1,"confidence":0.98,"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":"The large-scale structures (LSS) catalogues that are created from the redshift and parent target catalogues, together with the two-point function measurements, are described in [83]. In total, over 5.7 million unique object spectra were collected during the first year of ob- servations and used for galaxy and quasar BAO measurements in DR1 [73], a factor of∼3 increase compared to SDSS DR16 [84]. However, for the Full-Shape type of analyses pre- sented in this paper, the ELG bin between 0.8< z <1.1 (ELG1) was not included as it failed to pass the required tests before unblinding (see Section 6 for a full description of the unblinding process). Unlike the rest of the samples,ELG1showed uncorrected systematic effects related to fibre collisions, which suggested that the mitigation techniques used in this"},{"citing_arxiv_id":"2411.07970","ref_index":10,"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":"This monumental achievement has contributed signifi- cantly to the establishment of the current cosmological model ΛCDM, along with other cosmological probes, i.e., cosmic microwave background (CMB; [3, 4]), Type-Ia supernovae (SN; [5-7]), or measurements of weak lensing (e.g., [8, 9]). For two decades (2000-2020), major experiments such as the Sloan Digital Sky Survey (SDSS; [10]), followed by the on- going (2021-2026) survey from the Dark Energy Spectro- scopic Instrument1) (DESI; [11]), have mapped the 3D uni- 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-"},{"citing_arxiv_id":"2404.03002","ref_index":139,"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":"on the gravitational field inferred from the observed tracer distribution [135, 136]. Applying these reversed displacements to tracers sharpens the BAO signature4 and mitigates the small (< 0.3%) nonlinear shift of the BAO-scale in late-time clustering, allowing for more accurate cosmological inferences [137, 138]. The reconstruction algorithm used has been updated relative to that used for eBOSS [139] and the specific choice of algorithm and settings were validated as described in [140]. For the galaxy and quasar BAO data points considered in this paper we make use of the post-reconstruction clustering measurements in configuration space presented in [79]. Anisotropic BAO measurements are obtained for LRG and ELG samples, but we restrict to isotropic fits for BGS and QSO samples due to the lower signal-to-noise ratio of the"},{"citing_arxiv_id":"2404.03001","ref_index":3,"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":"Weinberg, M. J. Mortonson, D. J. Eisenstein, C. Hirata, A. G. Riess and E. Rozo, Observational probes of cosmic acceleration, Phys. Rept. 530 (2013) 87 [ 1201.2434]. [2] Planck Collaboration, N. Aghanim, Y. Akrami, M. Ashdown, J. Aumont, C. Baccigalupi et al., Planck 2018 results. VI. Cosmological parameters , Astron. Astrophys. 641 (2020) A6 [1807.06209]. [3] S. Alam, M. Aubert, S. Avila, C. Balland, J. E. Bautista, M. A. Bershady et al., Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Cosmological implications from two decades of spectroscopic surveys at the Apache Point Observatory , Phys. Rev. D 103 (2021) 083533 [ 2007.08991]. [4] DESI Collaboration, A. Aghamousa, J. Aguilar, S."},{"citing_arxiv_id":"2404.03000","ref_index":159,"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":"that we perform only the ξ(r) fit to the combined tracer, as we have only the RascalC covariance available for the combined tracer. 7.6 Comparison to previous analyses Given the changes described above in our pipeline, we revisit the SDSS (BOSS and eBOSS) data previously analyzed to quantify the impact of these changes on previously published results [159]. We do so in two stages. First, we refit the published correlation functions (using the published covariance matrices) to measure the distance scale. Second, we rerun the reconstruction pipeline using our new convention and then re-fit the updated correlation functions. Figure 13 shows the results of these comparisons for the three redshift bins used"},{"citing_arxiv_id":"2211.04492","ref_index":5,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"To provide some indication of the state of the art, the transverse and radial BAO scales were measured in BOSS to ∼ 1.6% and ∼ 2.7% in redshift bins of width ∆ z∼ 0.25 (82). The degeneracy betweenH0 and Ωm inH(z) or DA(z) is different at high and low redshifts, and so can be broken by combining BAO measurements at different redshifts (e.g., Figure 5 in Ref. (5)), and the BAO measurements now span the range 0 .15 <∼ z <∼ 3. Using the sound horizon inferred either from the CMB or from the value obtained by fixing the baryon density from big-bang nucleosynthesis then allows a determination of the Hubble parameter with a similar error. In practice, galaxy-survey analyses typically add to this \"pure-BAO\" measurement"},{"citing_arxiv_id":"2206.07773","ref_index":45,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"CMB lensing from Planck PR4 maps","primary_cat":"astro-ph.CO","submitted_at":"2022-06-15T19:17:41+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Planck PR4 maps with optimal filtering yield CMB lensing amplitude 1.004 ± 0.024 and σ8 Ωm^0.25 = 0.599 ± 0.016, the tightest lensing constraint yet.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2204.05305","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Galaxy and halo angular clustering in LCDM and Modified Gravity cosmologies","primary_cat":"astro-ph.CO","submitted_at":"2022-04-11T17:58:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"N-body light-cone mocks show 2-4 sigma deviations in third-order angular clustering between LCDM and f(R)/nDGP models at z=0.15-0.3 for halos and galaxies, with stronger signals in the dark-matter field.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2105.13549","ref_index":22,"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":"Aubourg et al., Phys. 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