{"total":33,"items":[{"citing_arxiv_id":"2606.18437","ref_index":176,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Impact of inhomogeneous curvature on growth rate measurements from magnitude fluctuations","primary_cat":"astro-ph.CO","submitted_at":"2026-06-16T19:40:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Full-GR simulations find that inhomogeneous curvature produces only sub-dominant systematic offsets in growth-rate measurements from magnitude fluctuations at z ≲ 0.2 relative to current statistical errors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12405","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bounding the Effect of HOD Assumptions on Small-Scale Clustering Constraints","primary_cat":"astro-ph.CO","submitted_at":"2026-06-10T17:59:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The fraction of AbacusSummit cosmologies excluded at 3σ by small-scale clustering multipoles drops from 81% to 25% when moving from fixed HOD parameters to broad marginalization over the five-parameter HOD model.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04090","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Mapping the nuclear environments of extreme coronal line emitting galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-02T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Multi-epoch spectroscopy of 33 ECLEs shows coronal lines emitted at intermediate radii with log(distance)-log(black hole mass) slopes of 0.63 and 0.69 for [O III] and [Fe VII], consistent with photoionization setting the radii.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21483","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Velocityformer: Broken-Symmetry-Matched Equivariant Graph Transformers for Cosmological Velocity Reconstruction","primary_cat":"astro-ph.CO","submitted_at":"2026-05-20T17:59:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Velocityformer achieves 35% higher velocity correlation than linear theory by matching graph transformer inductive bias to the line-of-sight broken symmetry and conditioning on long-wavelength physics, while training efficiently on only four low-fidelity simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18938","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"First detection of the moving lens effect with ACT and DESI LS","primary_cat":"astro-ph.CO","submitted_at":"2026-05-18T17:59:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"First observational detection of the moving lens effect via cross-correlation of ACT CMB temperature with DESI galaxies, yielding amplitude b_ML = 1.24 ± 0.26 at 4.8σ consistent with halo-model prediction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13325","ref_index":8,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Fixing the Renormalization of Inflationary Loops via Ward Identities","primary_cat":"gr-qc","submitted_at":"2026-05-13T10:39:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Ward identities from large gauge symmetry impose model-independent constraints on renormalizing inflationary loops and non-perturbatively govern the infrared power spectrum evolution.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"CO]. [4] Y. Akramiet al.(Planck), Astron. Astrophys.641, A9 (2020), arXiv:1905.05697 [astro-ph.CO]. [5] T. Louiset al.(ACT), (2025), arXiv:2503.14452 [astro- ph.CO]. [6] S. Alamet al.(BOSS), Mon. Not. Roy. Astron. Soc. 470, 2617 (2017), arXiv:1607.03155 [astro-ph.CO]. [7] A. G. Adameet al.(DESI), JCAP02, 021 (2025), arXiv:2404.03002 [astro-ph.CO]. [8] A. G. Adameet al.(DESI), JCAP07, 028 (2025), arXiv:2411.12022 [astro-ph.CO]. [9] A. A. Starobinsky, Phys. Lett. B117, 175 (1982). [10] V. F. Mukhanov, H. A. Feldman, and R. H. Branden- berger, Phys. Rept.215, 203 (1992). [11] V. F. Mukhanov, H. A. Feldman, and R. H. Branden- berger, Physics Reports215, 203 (1992). [12] A. M. Green and B. J. Kavanagh, J."},{"citing_arxiv_id":"2605.11956","ref_index":8,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Probing the small-scale primordial power spectrum via relic neutrinos and acoustic reheating","primary_cat":"hep-ph","submitted_at":"2026-05-12T11:08:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Dissipation of small-scale primordial perturbations after neutrino decoupling cools relic neutrinos and reduces their abundance, enabling PTOLEMY to constrain the primordial curvature power spectrum to O(0.1) on scales k ≲ 3×10^5 Mpc^{-1}.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"Ballardini, F. Finelli, F. Marulli, L. Moscardini, and A. Veropalumbo, Phys. Rev. D107, 043532 (2023), arXiv:2202.08819 [astro-ph.CO]. [6] M. Ballardiniet al.(Euclid), Astron. Astrophys.683, A220 (2024), arXiv:2309.17287 [astro-ph.CO]. [7] A. Antony, F. Finelli, D. K. Hazra, D. Paoletti, and A. Shafieloo, JCAP03, 029 (2026), arXiv:2403.19575 [astro-ph.CO]. [8] A. G. Adameet al.(DESI), JCAP07, 028 (2025), arXiv:2411.12022 [astro-ph.CO]. [9] A. Raffaelli and M. Ballardini, JCAP07, 077 (2025), arXiv:2503.10609 [astro-ph.CO]. [10] A. Chudaykin, M. M. Ivanov, and O. H. E. Philcox, Phys. Rev. D113, 063552 (2026), arXiv:2512.04266 [astro-ph.CO]. [11] A. Achucarro, J.-O. Gong, S. Hardeman, G. A. Palma, and S. P."},{"citing_arxiv_id":"2604.26915","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"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":"method","top_context_polarity":"use_method","context_text":"signal is still present it would be implausible, from a pure background evolution, to interpret it as modification to the gravitational theory, instead of a particle physics component which is minimally coupled to gravity. At the next order in a cosmological perturbation expansion, the DESI collaboration has also analyzed a two-parameter family of modifications to Einstein's theory, which are constant or smoothly dependent on time [6, 7]. This analysis shows that the DESI data are compatible with general relativity (GR). However, a point to notice is that modified gravity (MG) generally introduces new characteristic length scales, hence the importance to contrast this paradigm with observations. In this context, what characterizes DESI over other cosmological probes at the present time is its unique power to test alternative theories"},{"citing_arxiv_id":"2604.20958","ref_index":12,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Characterizing the GD-1 Stream with DESI DR2 Data: Thin Stream and Hot Cocoon","primary_cat":"astro-ph.GA","submitted_at":"2026-04-22T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI data on the GD-1 stream identifies a thin cold core and a hot cocoon with 30% of members whose dispersion is consistent with 11 Gyr of dark matter subhalo heating.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19745","ref_index":55,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Precision Kinematic Sunyaev--Zel'dovich Measurements Across Halo Mass and Redshift with DESI DR2 and ACT DR6: Part II. Bright Galaxy Survey and Emission-Line Galaxies","primary_cat":"astro-ph.CO","submitted_at":"2026-04-21T17:59:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"High-significance kSZ detections for BGS and ELG tracers reveal low gas fractions near virial radii in BGS halos likely due to AGN feedback and higher gas fractions in ELG halos suggesting weaker feedback.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19744","ref_index":51,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"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":"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- ture, residing in massive dark matter halos with typical massesM 200c ∼10 13 −10 14 M⊙ [52]. Their distinctive spectral features enable robust photometric and spectro-"},{"citing_arxiv_id":"2604.14504","ref_index":97,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Forecasting neutrino mass constraints from the Nancy Grace Roman Space Telescope","primary_cat":"astro-ph.CO","submitted_at":"2026-04-16T00:37:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Roman Space Telescope forecasts using Hα galaxy mocks yield m_ν < 0.276 eV (68% CL) with Planck priors via EFT of LSS, and m_ν < 0.36 eV via model-independent phenomenological analysis.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"We can see that in our realistic forecast, if ΛCDM is as- sumed, the Roman data by itself could provide constraints on the sum of neutrino masses that are tighter than the current upper bound obtained from galaxy clustering data. In particular, we obtain neutrino mass constraints that are∼8% tighter than the DESI DR1 EFT Full Shape + DR1 BAO analysis in [ 97] and∼42% smaller than the ΛCDM constraints from the DESI DR1 Full shape Shape- Fit + DR2 BAO in [ 99], using the same choice of priors on the baryon density, the spectral index, and the same range of scales. Furthermore, our analysis shows that Roman could measureH 0,Ω m, σ8 with 1.3%,4.3%,2.9% precision at 68% C.L, respectively, in line with DESI"},{"citing_arxiv_id":"2604.13535","ref_index":196,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Double the axions, half the tension: multi-field early dark energy eases the Hubble tension","primary_cat":"astro-ph.CO","submitted_at":"2026-04-15T06:29:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Two-field axion-like early dark energy reduces Hubble tension to 1.5 sigma residual and improves high-ell CMB fits over single-field models.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"3σagreement with the PArthENoPE estimate [194]). Interpreted more broadly, our results indicate that the Hubble tension may point to a complex pre- recombination expansion history, not captured by single- field EDE models. Extending our framework over a wider redshift range, confronting it with SPT-3G [12], ACT DR6 [195], and large-scale structure data [196], and ex- ploring model-independent reconstructions of the pre- recombination expansion history [197-200], are natural avenues for future work. 5 Acknowledgments.- V.P. acknowledges the Eu- ropean Union's Horizon Europe research and innova- tion programme under the Marie Sk lodowska-Curie Staff Exchange grant agreement no. 101086085 - ASYMME- TRY."},{"citing_arxiv_id":"2604.11694","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Cosmological inference with halo clustering reconstructed from the redshift-space galaxy distribution","primary_cat":"astro-ph.CO","submitted_at":"2026-04-13T16:33:23+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Halo reconstruction from redshift-space galaxies allows unbiased EFT full-shape inference with >20% tighter fσ8 constraints and stable results to smaller scales on DESI mocks.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"standard route to cosmological inference from redshift- space two-point statistics. Early work already exploited the full anisotropic correlation function at the linear- theory level [8]. More recent studies have extended these analyses using perturbative modeling of the galaxy power spectrum and emulator-based halo-model approaches [9- 12] (see also [13] for the latest full-shape RSD results and a comprehensive overview). In practice, however, ex- tracting this information increasingly relies on modeling modes deep into the quasi-nonlinear regime, where the mapping from real to redshift space is affected by nonlin- ear evolution, nonlinear bias, and, most importantly for galaxy samples, the virial motions of satellite galaxies."},{"citing_arxiv_id":"2604.08895","ref_index":54,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"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":"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":35,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"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":"2604.04886","ref_index":3,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Light neutrinos, Dark matter and leptogenesis near electroweak scale and $Z_4$ symmetry","primary_cat":"hep-ph","submitted_at":"2026-04-06T17:33:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Z4-symmetric Type I seesaw fits neutrino data with minimal parameters and enables freeze-in dark matter plus resonant leptogenesis via soft symmetry breaking.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"particle (FIMP) to act as a dark matter candidate via the freeze-in [39] mechanism provided that the soft breakingM 5 is considered in gMR in Eq. (28). In our setup, demanding a softz 4 symmetry breaking small off-diagonal element (M 5 ∼10 −10 GeV or less) in the interaction 2 cosmological observations indicate preference towards the normal hierarchy case [3] 18 basis, will lead to the emergence of very small parameters in the first column ofM D i.e., MD𝛼1 ∼ \u0010 MD𝛼3 M5 M6 \u0011 which is obtained after performing the diagonalization of the gMR matrix. Finally, due to this diagonalisation we writegMR as gMR = ©­­­­ « fM1 0 0 0 fM2 0 0 0 fM3 ª®®®® ¬ .(42) This diagonalization however, make negligible change in (11) element in the above matrix in"},{"citing_arxiv_id":"2604.04423","ref_index":52,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Dynamical CP Violation from Non-Invertible Selection Rules","primary_cat":"hep-ph","submitted_at":"2026-04-06T05:02:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Dynamical generation of leptonic CP violation and light sterile neutrino masses via radiative breaking of non-invertible selection rules, illustrated in the Inverse Seesaw model.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The KamLAND-Zen collaboration gives an upper bound onm ee at the 90% confidence level (CL) [51] as mee <(28−122) meV.(28) The third one is on effective electron neutrino mass that is defined bym νe ≡ P i D2 νi|UPMNSei|2. It is model independent observable, and given by mνe = q D2 ν1c2 13c2 12 +D 2 ν2c2 13s2 12 +D 2 ν3s2 13 .(29) Its upper bound at 90% CL from KATRIN [52] is given by mνe ≤450 meV,(30) which is weaker than the other constraints. The last one comes from non-unitarity constraints and mass hierarchy betweenM D and mD, which is determined by several experiments such as the effective Weinberg angle, SM W boson mass, several ratios of Z boson fermionic decays, invisible decay of Z, electroweak universality, measurements of Cabbibo-Kobayashi-Maskawa matrix, and lepton flavor viola-"},{"citing_arxiv_id":"2604.03167","ref_index":20,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Mapping the redshift drift at various redshifts through cosmography","primary_cat":"astro-ph.CO","submitted_at":"2026-04-03T16:44:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Cosmographic Taylor and Padé models fitted to Pantheon+SH0ES+GRB+DESI BAO data yield redshift drift predictions compatible with ΛCDM and ω0ω1CDM at 1-2σ, with mock drift data tightening q0 and j0 bounds.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":", Living Reviews in Relativity25, 6 (2022), 2201.07241. [17] A. G. Adame, J. Aguilar, S. Ahlen, S. Alam, D. M. Alexander, et al., JCAP2025, 028 (2025), 2411.12022. [18] M. Abdul Karim, J. Aguilar, S. Ahlen, S. Alam, L. Allen, et al., Phys. Rev. D112, 083515 (2025), 2503.14738. [19] S. M. Carroll, W. H. Press, and E. L. Turner, Annual Rev. of Astron. Astrophys.30, 499 (1992). [20] S. M. Carroll, Living Reviews in Relativity4, 1 (2001), astro-ph/0004075. [21] P. J. Peebles and B. Ratra, Reviews of Modern Physics 75, 559 (2003), astro-ph/0207347. [22] O. Luongo and M. Muccino, A&A690, A40 (2024), 2404.07070. [23] A. C. Alfano, O. Luongo, and M. Muccino, JCAP2024, 055 (2024), 2408.02536. [24] Y. Carloni, O. Luongo, and M. Muccino, Phys."},{"citing_arxiv_id":"2603.09278","ref_index":25,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraining Neutrino Mass with the Void Weak Lensing Effect","primary_cat":"astro-ph.CO","submitted_at":"2026-03-10T07:03:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Simulations of void-shear cross-correlation demonstrate that void lensing can constrain total neutrino mass to σ(M_ν)=0.096 eV without shape noise and 0.340 eV with Stage-III-like noise.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.21432","ref_index":40,"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":"with temperature, polarization, and lensing data fromPlanck[28-30], ACT DR6 [31-34], and SPT-3G D1 [35-37] (CMB-SPA [35]) and DESI-DR2 BAO measurements [38, 39] to measure the sum of neutrino masses, the effective number of relativistic species, the running of the spectral index, and the running of the running. We also combine our measurements with DESI full-shape [40] and Big Bang Nucleosynthesis [41] constraints to set upper limits on the sum of neutrino masses independent of CMB measurements. On the other hand, we find that our measurements are not precise enough to improve upon existing constraints on the dark energy equation of state. Measuring the aforementioned quantities has important physical implications."},{"citing_arxiv_id":"2512.17865","ref_index":72,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2511.20757","ref_index":68,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reanalyzing DESI DR1: 2. Constraints on Dark Energy, Spatial Curvature, and Neutrino Masses","primary_cat":"astro-ph.CO","submitted_at":"2025-11-25T19:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Reanalysis of DESI full-shape clustering data tightens constraints on neutrino mass, spatial curvature, and dark energy equation-of-state parameters relative to BAO-only results.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"energy, curvature, and neutrinos, utilizing the FS clustering data from the DESI DR1 public release [ 5, 66-68], in combination with theoretical models derived from the Effective Field Theory of Large Scale Structure (EFT, [e.g., 69-92])4. This builds on the Λ CDM analysis pipeline presented in [ 1] (hereafter Paper 1), and extends the official DESI analysis of [ 68] by adding the power spectrum hexadecapole moment (whose utility was demonstrated in [ 113]) and the large-scale bispectrum monopole (which has been analyzed only in the compressed ShapeFit paradigm [ 121]). This is made possible through the quasi-optimal estimators and analysis pipeline discussed in Paper 1 (based on [ 122]), which allow for robust treatment of various systematic effects, including fiber collisions in both the power spectrum"},{"citing_arxiv_id":"2510.19149","ref_index":54,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2510.09153","ref_index":28,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Euclid preparation. XCVI. Cosmology Likelihood for Observables in Euclid (CLOE). 3. Inference and Forecasts","primary_cat":"astro-ph.CO","submitted_at":"2025-10-10T08:57:09+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"CLOE pipeline produces forecasts showing Euclid can reach FoM >400 for dark energy w0 and wa by combining primary probes on synthetic data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.09147","ref_index":27,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Euclid preparation. XCVIII. Cosmology Likelihood for Observables in Euclid (CLOE). 5: Extensions beyond the standard modelling of theoretical probes and systematic effects","primary_cat":"astro-ph.CO","submitted_at":"2025-10-10T08:49:24+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"CLOE has been extended to model magnification bias, massive neutrinos, and modified gravity for Euclid probes and validated via posterior sampling on synthetic data.","context_count":0,"top_context_role":"background","top_context_polarity":"background","context_text":"where we definedP ΥΥ as the Weyl power spectrum, given by the Weyl transfer functionΥ=k 2(Φ+Ψ)/2. For all purposes, the approach ofCLOEcan also be written by defining a new power spectrum, ˜Pdd, included in theC γγ i j (ℓ), assuming that the conver- sion above can be used also at nonlinear scales (see Sect. 4.2 for more details) ˜Pdd[kℓ(z),z]=Γ 2(z)P NL m [kℓ(z),z].(27) This leads to the definition of a new window function ˜W γ i (z)=f K [r(z)] Z zmax z dz′ nL i (z′) fK [r(z′)−r(z) ] fK [r(z′)] ,(28) which only depends on geometrical quantities. The angular power spectrum can be written as Cγγ i j (ℓ)=c Z zmax zmin dz ˜W γ i (z) ˜W γ j (z) H(z)f 2 K(z) ˜Pdd[kℓ(z),z].(29) We want to introduce this change of definition inCLOE, re-"},{"citing_arxiv_id":"2510.04179","ref_index":12,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Crosschecking Cosmic Distances from DESI BAO and DES SNe","primary_cat":"astro-ph.CO","submitted_at":"2025-10-05T12:41:23+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.14322","ref_index":23,"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":"2503.14744","ref_index":45,"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":"the number of neutrino species at the time when they are relativistic. The radiation density, in excess of that due to photons, can be expressed in terms of an effective num- ber of neutrino species, Neff. In addition to the properties of cosmic neutrinos, measurements of Neff constrain the existence of new neutrino-like relics that were in thermal equilibrium with the primordial plasma [45, 46]. The Standard Model prediction is Neff = 3.044 for the non- instantaneous decoupling of three neutrino species, incor- porating corrections from flavour oscillations and finite temperature quantum electrodynamics [47-49]. DESI [50-52], in combination with CMB data from Planck [53, 54] and the Atacama Cosmology Telescope (ACT) [55, 56], has set the strongest current astrophysi-"},{"citing_arxiv_id":"2503.14743","ref_index":42,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"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":"dataset","top_context_polarity":"use_dataset","context_text":"2025, 124 20 (2025), arXiv:2404.03001 [astro-ph.CO]. [40] DESI Collaboration, A. G. Adame, J. Aguilar, S. Ahlen, and others, J. Cosmology Astropart. Phys. 2025, 021 (2025), arXiv:2404.03002 [astro-ph.CO]. [41] DESI Collaboration, A. G. Adame, J. Aguilar, S. Ahlen, and others, arXiv e-prints , arXiv:2411.12022 (2024), arXiv:2411.12022 [astro-ph.CO]. [42] DESI Collaboration, A. G. Adame, J. Aguilar, S. Ahlen, and others, arXiv e-prints , arXiv:2411.12021 (2024), arXiv:2411.12021 [astro-ph.CO]. [43] R. Calderon and others (DESI), JCAP 10, 048, arXiv:2405.04216 [astro-ph.CO]. [44] K. Lodha and others (DESI), Phys. Rev. D 111, 023532 (2025), arXiv:2405.13588 [astro-ph.CO]. [45] DESI Collaboration, in preparation (2026)."},{"citing_arxiv_id":"2503.14739","ref_index":59,"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":47,"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":"model and intriguing hints of evolving dark energy, with significances ranging from ∼ 2.5σ to ∼ 3.9σ depending on the combination of datasets used for the analysis. The analysis of the full shape of the power spectrum mea- sured with galaxies and quasars [45, 46] confirmed these findings and added new information on the amplitude of perturbations and modified gravity parameters [47]. Rapidly evolving dark energy, with |wa| ∼ 1, would be an astounding discovery, and these results have inspired both enthusiastic theorizing and healthy skepticism. In our analysis here of the DESI DR2 BAO results, we pay particular attention to the nature and statistical signif- icance of the evidence for evolving dark energy and to how that evidence depends on the choice of datasets."},{"citing_arxiv_id":"2411.12021","ref_index":1,"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":"Additionally, we measure the amplitude of clusteringσ 8 = 0.841±0.034. The DESI DR1 galaxy clustering results are in agreement with the ΛCDM model based on general relativity with parameters consistent with those fromPlanck. The cosmological interpretation of these results in combination with DESI DR1 Ly-αforest data and external datasets are presented in the companion paper [1]. Contents 1 Introduction 1 2 An Overview of the DESI samples and the LSS catalogues 4 2.1 DESI DR1 4 2.2 DR1 Large-scale structure catalogues 5 2.3 Blinding 6 3 Mocks 8 3.1Abacus8 3.2EZmocks10 3.3 Simulations of DR1 10 4 Methodology 11 4.1 Two-point function codes 11 4.2 Compression vs Full Modelling 12 4.2.1 Full Modelling 13 4.2.2 Standard compression 14"}],"limit":50,"offset":0}