{"total":17,"items":[{"citing_arxiv_id":"2606.29735","ref_index":43,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Modeling survey-window and integral-constraint effects on PNG in the galaxy power spectrum with light-cone mocks","primary_cat":"astro-ph.CO","submitted_at":"2026-06-29T03:19:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Light-cone mocks demonstrate that analytical corrections for survey-window and integral-constraint effects on PNG in galaxy power spectra lose accuracy below the equality scale and fail when PNG is present, enabling unbiased large-scale measurements.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23651","ref_index":206,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting the 'Lensing is Low' Problem with UNIONS","primary_cat":"astro-ph.CO","submitted_at":"2026-06-22T17:36:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New UNIONS galaxy-galaxy lensing data around CMASS galaxies indicates no significant lensing is low problem, with joint HOD fits to GGL and GC favoring a slightly lower matter power spectrum amplitude than Planck.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20845","ref_index":188,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"LEGGOS I: The JWST LEGGOS Survey -- LEnsing and Galaxy Growth: Observing Substructures -- Unpacks the Nature of Clumpy Star Formation and Quenching in Gravitationally Lensed Galaxies beyond Cosmic Noon","primary_cat":"astro-ph.GA","submitted_at":"2026-06-18T18:27:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"LEGGOS presents a uniform framework that jointly models lensing, photometry, and integral-field spectroscopy to disentangle stellar populations in clumps of high-redshift lensed galaxies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.16844","ref_index":33,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The cosmic tetrarchy: four estimators breaking the assumption degeneracy in cosmological distance tensions","primary_cat":"astro-ph.CO","submitted_at":"2026-06-15T15:22:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The cosmic tetrarchy decomposes BAO-based measurements into four channels that isolate distinct assumptions to test whether the dimensionless sound-horizon ratio remains a single redshift-independent number.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06226","ref_index":47,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A New Member of the Fast and Furious Family: A Relativistic and Time-Variable UV Outflow in a Luminous Quasar","primary_cat":"astro-ph.GA","submitted_at":"2026-06-04T14:36:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Detection of a time-variable relativistic UV outflow at velocities up to 0.3c in quasar J2318, with estimated mass-loss rate and kinetic luminosity above typical feedback thresholds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22489","ref_index":20,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Machine Learning Techniques for Astrophysics and Cosmology: Lyman-$\\alpha$ forest","primary_cat":"astro-ph.CO","submitted_at":"2026-05-21T13:43:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Review of machine learning applications for analyzing Lyman-alpha forest observations to probe cosmology, reionization, and dark matter.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Annis, N.A. Bahcall et al.,The Sloan Digital Sky Survey: Technical Summary,AJ 120(2000) 1579 [astro-ph/0006396]. [19] D.J. Eisenstein, D.H. Weinberg, E. Agol, H. Aihara, C. Allende Prieto, S.F. Anderson et al.,SDSS-III: Massive Spectroscopic Surveys of the Distant Universe, the Milky Way, and Extra-Solar Planetary Systems,AJ142(2011) 72 [1101.1529]. [20] K.S. Dawson, J.-P. Kneib, W.J. Percival, S. Alam, F.D. Albareti, S.F. Anderson et al.,The SDSS-IV Extended Baryon Oscillation Spectroscopic Survey: Overview and Early Data,AJ151(2016) 44 [1508.04473]. [21] N.G. Busca, T. Delubac, J. Rich, S. Bailey, A. Font-Ribera, D. Kirkby et al., Baryon acoustic oscillations in the Lyαforest of BOSS quasars,A&A552"},{"citing_arxiv_id":"2605.10102","ref_index":22,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2601.21432","ref_index":13,"ref_count":1,"confidence":0.98,"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":"in recent years, driven by the steady increase in the number of Lyαforest measurements. For two decades, the Sloan Digital Sky Survey (SDSS [11]) and its successors provided the bulk of these data: SDSS measured≃12 000 Lyαforest over eight years, the Baryon Oscillation Spectroscopic Survey (BOSS [12]) expanded this number to≃160 000 over five years, and the extended Baryon Oscillation Spectroscopic Survey (eBOSS [13]) further increased it to ≃210 000 over six years. This number rose dramatically with the advent of the Dark Energy Spectroscopic Instrument survey (DESI [14]). Remarkably, DESI measured≃55 000 Lyα forests [15, 16] within the Early Data Release (EDR [17]), which contains observations from the six-month Survey Validation period (SV [18]) and the first two months of the main"},{"citing_arxiv_id":"2510.14888","ref_index":48,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Modeling nonlinear scales for dynamical dark energy cosmologies with COLA","primary_cat":"astro-ph.CO","submitted_at":"2025-10-16T17:07:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"COLA-based hybrid emulator reproduces nonlinear power spectrum boosts in w0wa models to <2% error vs EuclidEmulator2 and produces <0.3σ shifts in LSST-like cosmic shear parameter constraints.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"2, Monthly Notices of the Royal Astronomical Society 473, 4773 (2018), arXiv:1705.06373 [astro-ph.CO]. [47] S. A. Rodríguez-Torres, J. Comparat, F. Prada, G. Yepes, E. Burtin,et al., Clustering of quasars in the first year of the SDSS-IV eBOSS survey: interpretation and halo occupa- tion distribution, Monthly Notices of the Royal Astronomical Society468, 728 (2017), arXiv:1612.06918 [astro-ph.CO]. [48] A. D. Myers, N. Palanque-Delabrouille, A. Prakash, I. Pâris, C. Yeche,et al., The SDSS-IV Extended Baryon Os- cillation Spectroscopic Survey: Quasar Target Selection, The Astrophysical Journal Supplement221, 27 (2015), arXiv:1508.04472 [astro-ph.CO]. [49] H. Gil-Marín, J. Guy, P. Zarrouk, E. Burtin, C.-H. Chuang, et al., The clustering of the SDSS-IV extended Baryon Oscil-"},{"citing_arxiv_id":"2509.14322","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2503.14739","ref_index":25,"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":13,"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":"a central role in observational cosmology. The key tech- nical requirement is a large-volume spectroscopic survey with sufficient sampling density, and previous surveys de- signed with BAO measurements as a defining goal include WiggleZ [9], the Baryon Oscillation Spectroscopic Survey (BOSS) [10] of SDSS-III [11], and its extension eBOSS [12] in SDSS-IV [13]. In addition to galaxy and quasar redshifts, BOSS and eBOSS measured BAO in the Ly α forest absorption spectra of z > 2 quasars, an approach first proposed by [14, 15]. Transverse BAO can also be measured in photometric surveys (e.g., [16]), though the precision obtained for a given number of tracers is much higher with spectroscopic redshifts. DESI is designed"},{"citing_arxiv_id":"2411.12022","ref_index":21,"ref_count":1,"confidence":0.98,"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":"complementary to that from the cosmic microwave background (CMB) measurements. The above-mentioned long history of measurements of galaxy clustering has, over the past decade or so, been reinvigorated with the data from the Baryon Oscillation Spectroscopic Survey (BOSS) [19] which has been part of the third phase of the Sloan Digital Sky Survey (SDSS-III; [20]), and its extension eBOSS [21]. Full-shape analyses of galaxy and quasar clus- tering in BOSS have been carried out by the BOSS [22-26] and eBOSS [27-33] collaborations, as well as independent teams who typically studied BOSS and/or eBOSS data [34-46]. The tools developed in these analyses have enabled reliable extraction of cosmological information from clustering. The Dark Energy Spectroscopic Instrument (DESI) is the first Stage-IV galaxy survey in"},{"citing_arxiv_id":"2411.07970","ref_index":85,"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":"values of zero thus constitutes a test of deviations from GR. Galaxy spectroscopic surveys enable measurements of structure growth through both correlations of galaxy veloc- ities and comparisons of the spatial clustering of galaxies across different redshifts. Testing gravity is, therefore, a pri- mary scientific motivation of recent spectroscopic surveys, such as SDSS and DESI [11, 85]. Currently, measurements of structure growth atz≲1 have achieved precision at the ≲10 % level (e.g., [10], see also Section 5.3). While results from spectroscopic surveys are generally consistent with pre- dictions of the GR-ΛCDM model, the structure growth his- tory at high redshifts remains largely unexplored. Probing this regime is essential for differentiating between various"},{"citing_arxiv_id":"2404.03002","ref_index":196,"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":"dataset","top_context_polarity":"baseline","context_text":"the change in the degeneracy directions with redshift is that the combination of all tracers provides a tight final constraint, shown in the right panel of Figure 2. 3.3 Comparison to BAO results from SDSS The region of the sky and the range of redshifts observed by DESI partially overlap with those observed by the previous generation of BOSS [195] and eBOSS [196] survey programs of SDSS [197], whose final BAO results were presented in [139]. It is therefore pertinent to compare - 18 - 70 80 90 100 110 120 130 H0rd [100 km s−1] 0.1 0.2 0.3 0.4 0.5 0.6 0.7 Ωm BGS LRG1 LRG2 LRG3+ELG1 ELG2 QSO Ly-α All 96 98 100 102 104 106 H0rd [100 km s−1] 0.26 0.28 0.30 0.32 0.34 0.36 Ωm DESI BAO SDSS BAO (DESI+SDSS) BAO CMB"},{"citing_arxiv_id":"2404.03001","ref_index":25,"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":"release (DR11, [18]), BOSS presented as well the first BAO measurement from the cross- correlation of quasars and the Ly α forest [19], which doubled the amount of information available from the same dataset. Updated Ly α BAO measurements were published following subsequent SDSS data re- leases [20-24], including data from the Extended Baryon Oscillation Spectroscopic Survey (eBOSS, [25]). The final Ly α BAO results used 210 000 Lyα forests from BOSS and eBOSS observations in the 16th data release (SDSS DR16, [26]). These results were published in du Mas des Bourboux et al. (2020) [27] and are referred to as dMdB20 in the rest of this article. dMdB20 has been the state-of-the art in Ly α BAO measurements until this publication, and"},{"citing_arxiv_id":"2105.13549","ref_index":39,"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":"Jap. 70, S4 (2018), arXiv:1704.05858 [astro-ph.IM]. [36] T. Hamana et al. (HSC), Publ. Astron. Soc. Jap.72, 16 (2020), arXiv:1906.06041 [astro-ph.CO]. [37] K. Kuijken et al. (KiDS), Mon. Not. R. 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