{"total":24,"items":[{"citing_arxiv_id":"2607.07875","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Alcock-Paczynski Blinding Scheme for the Ly-$\\alpha$ Forest Analysis","primary_cat":"astro-ph.CO","submitted_at":"2026-07-08T19:18:54+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A catalog-level Alcock-Paczynski wavelength-shift blinding scheme for the Lyman-alpha forest robustly hides the expansion history and correctly shifts the BAO peak on DESI DR1 data and mocks.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.05326","ref_index":51,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Weak Evolution of Cosmic Atomic Hydrogen over the Past 4.5 Billion Years","primary_cat":"astro-ph.GA","submitted_at":"2026-07-06T17:02:03+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Combining FAST and DESI data for 2.5 million galaxies shows cosmic atomic hydrogen density declined by only a factor of 1.35 over 4.5 Gyr, far less than the 2.46-fold decline in star formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27115","ref_index":43,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Clustering of high-redshift quasars with DESI DR2","primary_cat":"astro-ph.CO","submitted_at":"2026-06-25T14:49:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI DR2 quasar sample yields bias b_Q(z=2.48)=3.61 that evolves as b(z)=0.230[(1+z)^2-6.565]+2.394, consistent with constant ~10^12 M_sun halo mass and weak luminosity dependence at fixed redshift.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24852","ref_index":65,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The 3D clustering of Lyman Alpha Emitters measured with DESI","primary_cat":"astro-ph.CO","submitted_at":"2026-06-23T17:31:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI LAE clustering measurements give a linear bias of 2.31-2.62 with constraints on radiative transfer effects and halo occupation from correlation functions and power spectra.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24651","ref_index":42,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Measuring local primordial non-Gaussianity from the clustering of DESI DR1 LRGs and QSOs","primary_cat":"astro-ph.CO","submitted_at":"2026-06-23T14:45:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Reports first config-space f_NL measurement from DESI DR1 LRG/QSO 2pcf, yielding joint f_NL = -3^{+12}_{-12} at 68% CL using simulation-based modeling and imaging systematics mitigation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23936","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cosmological constraints from the DESI DR1 Bispectrum Full-Shape and DR2 BAO","primary_cat":"astro-ph.CO","submitted_at":"2026-06-22T20:56:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"DESI DR1 bispectrum plus DR2 BAO data raise σ8 and S8 by ~1.1-1.2σ while tightening uncertainties, shift DESI-only w0waCDM toward ΛCDM, produce a 2.8σ deviation from ΛCDM when combined with CMB, and yield a neutrino mass sum posterior of 0.26±0.17 eV.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21035","ref_index":32,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Quality Assessment of Spectroscopic Data Reduction Pipelines Using Artificial Intelligence: Scrutinizing Data Release 2 from the DESI Survey","primary_cat":"astro-ph.IM","submitted_at":"2026-06-19T01:58:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Unsupervised UMAP plus Friends-of-Friends clustering on 58 million DESI DR2 spectra identifies 1.1 million outlier candidates where visual checks show 67 percent have reduction artifacts missed by the standard pipeline.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18581","ref_index":44,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"DESI Data Release 2 ELGs: Property-dependent subsamples, imaging systematics, and clustering","primary_cat":"astro-ph.CO","submitted_at":"2026-06-17T01:09:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Property-dependent systematic weights derived separately on ELG subsamples, with separate DES footprint treatment, mitigate spurious clustering in ~10% of subsamples but are not optimal for the full sample.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.26915","ref_index":80,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"background","top_context_polarity":"background","context_text":"A FS analysis from BOSS DR12 givesf R0 <10 −4.82 = 1.53×10 −5 [34], which is somewhat stronger than our result, although the analysis assumes co-evolution theory for bias, tighter priors on EFT parameters, and fixesn s to the Planck value. Finally, a joint cosmic shear analysis combining DES-Y3, KiDS-1000, and HSC-Y3, together with CMB and BAO data [80], reports|f R0|<10 −4.98 = 1.05×10 −5. 3 Datasets The main observational data in our FS analysis is the DESI DR1 [3], available athttps: //data.desi.lbl.gov/doc/releases/dr1/. The DESI wide-angle instrument is capable of taking around 5000 simultaneous spectra using robotic-fiber positioners over the optically corrected focal plane [81-83], and ten high-resolution spectrographs [84]."},{"citing_arxiv_id":"2604.19744","ref_index":45,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Precision Kinematic Sunyaev--Zel'dovich Measurements Across Halo Mass and Redshift with DESI DR2 and ACT DR6: Part I. Luminous Red Galaxies","primary_cat":"astro-ph.CO","submitted_at":"2026-04-21T17:59:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"High-significance kSZ measurements around LRGs show gas is redistributed beyond gravitational collapse and imply more efficient feedback in group-scale halos than in standard hydrodynamical models.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"simultaneous spectra for nearly 5000 objects across a ∼3 ◦ field of view [43, 44]. Over its planned eight-year op- eration, DESI will observe approximately 17,000 deg 2 of sky, targeting an estimated 63 million spectroscopically- confirmed galaxies and quasars spanning redshifts 0.1< z <1.6, substantially exceeding the original forecast of 39 million objects [45]. The survey's scale requires sophisticated supporting infrastructure, including dedi- cated software pipelines for spectroscopic reduction and survey operations [46, 47]. Cosmological analyses using the First Data Release DR1 [48] have yielded results from full-shape modeling of galaxy clustering [49] and baryon acoustic oscillations [50], with ongoing work utilizing the"},{"citing_arxiv_id":"2604.05213","ref_index":22,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2604.04867","ref_index":92,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Measurement of the galaxy-velocity power spectrum of DESI tracers with the kinematic Sunyaev-Zeldovich effect using DESI DR2 and ACT DR6","primary_cat":"astro-ph.CO","submitted_at":"2026-04-06T17:16:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI DR2 and ACT DR6 data yield 17σ LRG-velocity, 8.3σ ELG-velocity, and 6.8σ QSO-velocity detections plus a 3.1σ velocity-velocity signal, producing f_NL^loc = 15.9_{-34.4}^{+34.6} from the velocity field.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"survey of about 17,000 deg 2 of the sky. The full survey will lead to 63 million spectroscopically-confirmed galax- ies and quasars, compared to the initial forecasts of 39 million [53]. The scale and complexity of the DESI exper- iment necessitate a suite of supporting software pipelines and products to effectively exploit its data [89-91]. We use the Luminous Red Galaxy (LRG) [92], Emis- sion Line Galaxy (ELG) [93], and Quasar (QSO) [94] samples from the DESI DR2 dataset, which comprises observations collected between 14 May 2021 and 9 April 2024 [51]. The corresponding cosmological interpreta- tions from BAO measurements are presented in [95, 96]. Summary statistics for these samples, restricted to the area overlapping with ACT DR6, are reported in Ta-"},{"citing_arxiv_id":"2601.21432","ref_index":49,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"simulations used to train theP 1D emulator and to validate the analysis pipeline in section 2.2. 2.1 DESI DR1 measurements DESI is a robotic, multi-fiber spectrograph mounted on the Mayall 4-meter telescope at Kitt Peak National Observatory [46, 47]. It can obtain spectra for nearly 5000 sources per exposure thanks to its high-precision focal plane [48], corrector [49], and fiber system [50] together with a sophisticated survey operation planning [51]. DESI spectra cover wavelengths from the near UV to the near infrared (3600 to 9800 ˚A) with spectral resolution ranging from 2000 to 5000 [52], which enables measurements of the Lyαforest in quasars atz >2.1. DESI uses three automated classification algorithms to identify and compute the red-"},{"citing_arxiv_id":"2512.17865","ref_index":62,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constraining primordial non-Gaussianity from DESI DR1 quasars and Planck PR4 CMB Lensing","primary_cat":"astro-ph.CO","submitted_at":"2025-12-19T18:14:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Cross-correlation of DESI DR1 quasars with Planck PR4 CMB lensing constrains local f_NL to 2^{+28}_{-34} (p=1.6) or 6^{+20}_{-24} (p=1.0), tightening previous limits by 35%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.19149","ref_index":69,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2509.14322","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing the limits of cosmological information from the Lyman-$\\alpha$ forest 2-point correlation functions","primary_cat":"astro-ph.CO","submitted_at":"2025-09-17T18:00:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Using idealized synthetic data, knowing the true continuum in Lyα forest auto- and cross-correlations reduces uncertainties on the AP parameter and Ω_m by ~10%, with extension to 240 h^{-1}Mpc scales adding up to ~15% further improvement equivalent to a 40% larger survey area.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.05467","ref_index":44,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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 -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":"DESI collects the light for 5000 spectra per observation with a robotic focal plane assembly [51] that can quickly align the positions of fiber optics cables [52] across the seven square degree field of view of the prime focus corrector [53]. For each observation, there is a custom focal plane configuration or 'tile' that defines the DESI 'target' [54] associated with each robotic positioner. When repeated observations of a tile are required to obtain the minimum effective ob- serving time [55], these maintain the same configuration. The light of each of these targets, along with calibration stars and sky spectra, are recorded from 360-980 nm with ten bench-mounted spectrographs that are located in a"},{"citing_arxiv_id":"2411.12022","ref_index":54,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"Alam, D.M. Alexander et al., Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument , AJ 164 (2022) 207 [ 2205.10939]. [53] J.H. Silber, P. Fagrelius, K. Fanning, M. Schubnell, J.N. Aguilar, S. Ahlen et al., The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI) , AJ 165 (2023) 9 [ 2205.09014]. [54] T.N. Miller, P. Doel, G. Gutierrez, R. Besuner, D. Brooks, G. Gallo et al., The Optical Corrector for the Dark Energy Spectroscopic Instrument , AJ 168 (2024) 95 [ 2306.06310]. [55] E.F. Schlafly, D. Kirkby, D.J. Schlegel, A.D. Myers, A. Raichoor, K. Dawson et al., Survey Operations for the Dark Energy Spectroscopic Instrument , AJ 166 (2023) 259 [ 2306."},{"citing_arxiv_id":"2411.12021","ref_index":17,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"measurement of baryon acoustic oscillations (BAO, [7-9]) and tests of gravity through redshift space distortions (RSD, [10, 11]). The Dark Energy Spectroscopic Instrument (DESI [12-15]) represents the next step in this evolution. DESI is designed to collect spectra for about 40 million galaxies and quasars in the redshift range 0< z <4 thanks to its 5,000 robotic fibre positioners [16] and to the 3.2-degree diameter prime focus corrector [17]. DESI targets five main classes of tracers: low-redshift galaxies from the Bright Galaxy Survey (BGS), luminous red galaxies (LRG), emission line galaxies (ELG), quasars (QSO), and the Lyαforest. The BGS targets correspond to the 'bright time' spectroscopic pipeline, whereas the rest of samples to the 'dark time' (see [18, 19] for a detailed description of the spectroscopic pipeline and distinct"},{"citing_arxiv_id":"2404.03001","ref_index":35,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"We conclude in section 8. 2 Data Sample We use quasar spectra collected during the first year of the DESI main survey. The obser- vations were conducted with the Mayall 4-m telescope at Kitt Peak National Observatory, in Arizona, with a new prime focus, multi-fiber spectrograph. It consists of a new corrector equipped with an atmospheric dispersion compensator [35] providing a 3.2 degree diameter field of view, and a focal plane composed of 5000 robotically actuated fibers [36] that dis- - 2 - tribute the light to 10 spectrographs situated below the telescope, in a temperature-controlled room. Each spectrograph is composed of three arms, blue (3600-5930 ˚A), red (5600-7720 ˚A) and near infrared (7470-9800 ˚A)."}],"limit":50,"offset":0}