{"total":18,"items":[{"citing_arxiv_id":"2604.26915","ref_index":82,"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":"Rev. Lett.117(2016) 051101, [1607.00184]. [80] J. Bai, J.-Q. Xia and G.-B. Zhao,Testing f(R) Gravity from Cosmic Shear Measurements, Astrophys. J.992(2025) 205, [2412.04807]. [81] C. Poppett, L. Tyas, J. Aguilar, C. Bebek, D. Bramall, T. Claybaugh et al.,Overview of the Fiber System for the Dark Energy Spectroscopic Instrument, AJ168(Dec., 2024) 245. [82] T. N. Miller, P. Doel, G. Gutierrez, R. Besuner, D. Brooks, G. Gallo et al.,The Optical Corrector for the Dark Energy Spectroscopic Instrument, AJ168(Aug., 2024) 95, [2306.06310]. [83] 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),"},{"citing_arxiv_id":"2604.19744","ref_index":48,"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":"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 forthcoming DR2 dataset [51]. The survey employs multiple galaxy tracers optimized for different science goals, with Luminous Red Galax- ies (LRGs) being particularly well-suited for kSZ studies. LRGs serve as highly-biased tracers of large-scale struc-"},{"citing_arxiv_id":"2604.08895","ref_index":52,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"FolpsD: combining EFT and phenomenological approaches for joint power spectrum and bispectrum analyses","primary_cat":"astro-ph.CO","submitted_at":"2026-04-10T02:59:01+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"FolpsD combines EFT power spectrum and tree-level bispectrum with damping to enable joint analyses that improve cosmological constraints from DESI-like galaxy mocks by up to 30% on As and omega_cdm while extending the usable k-range without significant biases for LRG samples.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"5 million galaxy and quasar redshifts, along with 1.3 million Lyman- αspectra. DESI, a robotic, fiber-fed, highly multiplexed spectroscopic survey instrument mounted on the Mayall 4-meter telescope at Kitt Peak National Observatory [51], has been designed to cover approximately17,000square degrees over eight years, with a target of 63 million spectroscopically confirmed galaxies and quasars [52, 53]. The DESI Data Release 1 (DR1; [54]), which includes spectra for more than 18 million unique targets, is now publicly available. Early DESI results have already provided new constraints on dark energy [55-58], - 2 - modified gravity [55, 59], neutrino physics [56, 60], and PNG [61]. In particular, the DR2 release has delivered precise BAO measurements across a wide redshift range, demonstrating"},{"citing_arxiv_id":"2604.05213","ref_index":27,"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":93,"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":"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- ble III, and the observational footprint is shown in Fig-"},{"citing_arxiv_id":"2601.21432","ref_index":52,"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":"unclear","context_text":"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- shift of quasars [53], which are pre-selected through a dedicated targeting strategy [54, 55]. The primary tool is the template-fitting coderedrock[56], which classifies sources as stars, galaxies, or quasars and estimates their redshifts."},{"citing_arxiv_id":"2510.19149","ref_index":70,"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":21,"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":50,"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":"per presents the analysis of the main survey data that will be released with the second data release or DR2, 1 The majority of the redshifts not used are from the low redshift bright time program, as described in the following subsection. which includes observations through 9 April 2024. The DESI spectroscopic reduction [56] and redshift estima- tion ( Redrock [57, 58]) pipelines were applied to the DR2 dataset in a homogeneous processing run denoted as 'Kibo'. An error in the processing involved in the co-addition of spectra from separate exposures was sub- sequently identified and fixed, and the pipeline was rerun and denoted 'Loa'. Approximately 0.1% of the measured redshifts change significantly between Kibo and Loa."},{"citing_arxiv_id":"2411.12022","ref_index":56,"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":"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 [ 2306.06309]. [56] J. Guy, S. Bailey, A. Kremin, S. Alam, D.M. Alexander, C. Allende Prieto et al., The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument , AJ 165 (2023) 144 [ 2209.14482]. [57] C. Hahn, M.J. Wilson, O. Ruiz-Macias, S. Cole, D.H. Weinberg, J. Moustakas et al., The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation , AJ 165 (2023)"},{"citing_arxiv_id":"2411.12021","ref_index":18,"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":"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 program observations). This broad range of tracers allows DESI to probe different epochs of the cosmic expansion history. Additionally, DESI includes a high-density Milky Way Survey, which focuses on stellar evolution and kinematics within our galaxy [20]. The distribution of galaxies traces the underlying matter distribution, which encodes"},{"citing_arxiv_id":"2404.03002","ref_index":104,"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":"covered tile surface area is of order 7 , 500 deg 2, just over half of the expected final coverage of 14 , 200 deg 2. However, the completeness within this area will significantly increase, as one can infer given an expected final number of 9,929 dark and 5,676 bright observed tiles [103]. The combined effective volume is expected to increase by more than a factor 3 [79]. The observed data are processed by the DESI spectroscopic pipeline [104] on a daily basis for immediate quality checks. The redshift catalogs used for this analysis and released with DESI DR1 are obtained from a spectroscopic reduction run with a fixed pipeline version internally denoted as \"iron\". Large-scale structure catalogs of galaxy and quasar positions suitable for the clustering analysis are built from the redshift and parent target catalogs and their two-point function"},{"citing_arxiv_id":"2404.03001","ref_index":37,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2404.03000","ref_index":37,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"and will result in a spectroscopic sample that will be an order of magnitude larger than previous surveys, both in the volume surveyed and in the number of galaxies measured. It achieves this with a combination of new instrumentation, including a 5000-fiber multi-object spectrograph [34, 35] new imaging surveys and efficient target selection algorithms [36], and optimized data pipelines [37]. In addition, DESI builds in a number of internal systematics checks using multiple tracer populations to probe common volumes. The early data from DESI was presented in [38, 39]. These data were used to make an initial BAO measurements in [40] and [41] which presented initial BAO measurements with the DESI galaxy and Lyman- α samples respectively."}],"limit":50,"offset":0}