{"total":19,"items":[{"citing_arxiv_id":"2607.07875","ref_index":11,"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":"2607.07329","ref_index":90,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Beyond traditional emission-line diagnostics: using autoencoders to uncover active galactic nuclei in DESI spectra","primary_cat":"astro-ph.GA","submitted_at":"2026-07-08T12:21:19+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":5.5,"formal_verification":"none","one_line_summary":"SPENDER autoencoder plus k-d tree nearest-neighbor classification on DESI spectra identifies AGN and broad-line AGN at accuracies 0.952 and 0.965, recovering sources missed by single-line diagnostics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24852","ref_index":64,"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":"2606.23936","ref_index":32,"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":"2606.18581","ref_index":43,"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":81,"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":",The SRG-eROSITA All-Sky Survey : Constraints on f(R) Gravity from Cluster Abundance,2402.08459. [79] X. Liu et al.,Constrainingf(R)Gravity Theory Using Weak Lensing Peak Statistics from the Canada-France-Hawaii-Telescope Lensing Survey,Phys. 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."},{"citing_arxiv_id":"2604.05213","ref_index":23,"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":90,"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":"background","top_context_polarity":"background","context_text":"Gallo et al.,The Optical Corrector for the Dark Energy Spectroscopic Instrument,The Astronomical Journal168(2024) 95 [2306.06310]. [89] J. Guy, S. Bailey, A. Kremin, S. Alam, D. M. Alexander, C. A. Prieto et al.,The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument,The Astronomical Journal165(2023) 144 [2209.14482]. [90] A. D. Myers, J. Moustakas, S. Bailey, B. A. Weaver, A. P. Cooper, J. E. Forero-Romero et al.,The Target-selection Pipeline for the Dark Energy Spectroscopic Instrument,The Astronomical Journal 165(2023) 50 [2208.08518]. [91] 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,The"},{"citing_arxiv_id":"2601.21432","ref_index":48,"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":"2510.19149","ref_index":68,"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":"2508.05467","ref_index":42,"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<z<1.1 bin.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2503.14744","ref_index":83,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"cise spectroscopic galaxy survey [50-52]. The instrument is equipped with 5,000 fibers [80] in a robotic focal plate 6 assembly [81] on the Mayall Telescope at Kitt Peak Na- tional Observatory. With a high-performing optical de- sign based on a 3.2 degree prime-focus corrector [82], DESI plans to measure over 40 million galaxy redshifts during a five-year period [83]. Indeed, with its target selection [84] over the imaging Legacy Survey [85, 86], DESI had a successful survey validation campaign [87] (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"},{"citing_arxiv_id":"2503.14743","ref_index":31,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"background","top_context_polarity":"background","context_text":"are motivated to study these time-evolving alternatives by the recent cosmological results from the Dark Energy Spectroscopic Instrument (DESI) [27, 28]. DESI is able to measure multiple spectra simultaneously by means of its 5,000 fibers [29] and a robotic plane assembly [30] across the field of view given its 3 .2◦ diameter prime focus corrector [31]. This is complemented by a high- performance spectroscopic data processing pipeline [32] and a streamlined operations plan [33]. DESI is designed to help better understand the nature of dark energy [34] 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"},{"citing_arxiv_id":"2503.14739","ref_index":44,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":52,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"efficient instrument that can measure thousands of spec- tra in a single observation [6], combined with the light- gathering power of the 4-m Nicholas U. Mayall Telescope at the Kitt Peak National Observatory. 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."},{"citing_arxiv_id":"2411.12022","ref_index":53,"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":"Aguilar, S. Ahlen, S. Alam, L.E. Allen et al., The DESI Experiment Part II: Instrument Design , arXiv e-prints (2016) arXiv:1611.00037 [1611.00037]. [52] DESI Collaboration, B. Abareshi, J. Aguilar, S. Ahlen, S. 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."},{"citing_arxiv_id":"2411.12021","ref_index":16,"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"},{"citing_arxiv_id":"2404.03002","ref_index":98,"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":"Mayall Telescope at Kitt Peak National Observatory in Arizona. Each observation field is covered by a \"tile\", consisting in a set of targets located within that sky area [97] and assigned to each of the 5000 fibers in the focal plane of the telescope. Each fiber is placed at the celestial coordinates of its assigned target by a robotic positioner [98, 99] andcarries the target's light from the focal plane to one of the ten DESI spectrographs. DESI observing time is dynamically separated into a \"bright\" time program (when BGS are observed) and \"dark\" time observations (when LRG, ELG, and QSO are targeted) depending on observing conditions. Redshift distributions, exposure times, calibration and observation"},{"citing_arxiv_id":"2404.03001","ref_index":36,"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":"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). In this analysis we use only data from the blue arms. In each blue camera, the light from 500 fibers is dispersed and refocused, forming 500 spec-"}],"limit":50,"offset":0}