{"total":14,"items":[{"citing_arxiv_id":"2606.31280","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Galaxy bias renormalization: Two-loop Power Spectrum, One-loop Trispectrum and Bispectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-06-30T07:54:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Complete fifth-order galaxy bias renormalization in real space enables consistent two-loop power spectrum and one-loop bispectrum/trispectrum calculations for biased tracers with operator-level counterterms.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28172","ref_index":97,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Searching for primordial features with radio surveys: synergy between the power spectrum and bispectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T15:04:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Joint power spectrum and bispectrum analysis from future HI intensity mapping surveys improves constraints on primordial feature amplitudes by 30-40% and achieves percent-level precision on oscillation frequencies when combined with CMB measurements.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Z2(ki,k j, z) =b 1(z)F2(ki,k j) +f(z)µ 2 ijG2(ki,k j) + b2(z) 2 + bs2(z) 2 S2(ki,k j) + f(z)µ ijkij 2 \u0014 µi ki Z1(kj, z) + µj kj Z1(ki, z) \u0015 ,(2.28) wheref(z)≡d lnD/d lnais the linear growth rate,µ i = ˆki · ˆzwith ˆzthe line-of-sight vector, µij = (µiki +µ jkj)/kij andk 2 ij = (ki +k j)2. The kernelsF2 andG 2 are the second-order symmetric SPT kernels [97],S2(k1,k 2) = (ˆk1 · ˆk2)2 −1/3is the tidal kernel [98, 99]. We include a Gaussian FoG damping [100, 101] DP FOG(k) = exp h − kµσP \u00012i ,(2.29) DB FOG(k1,k 2,k 3) = exp \u0002 − k2 1µ2 1 +k 2 2µ2 2 +k 2 3µ2 3 \u0001 σ2 B \u0003 ,(2.30) - 6 - with fiducial valuesσP =σ B = 2σ v, where the pairwise peculiar velocity dispersion along the line of sight is estimated as"},{"citing_arxiv_id":"2606.26234","ref_index":89,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Lyman-Alpha Forest and its Cross-Correlation with High-Redshift Galaxies in Effective Field Theory at the Field Level","primary_cat":"astro-ph.CO","submitted_at":"2026-06-24T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"An EFT-based field-level forward model for the Lyman-alpha forest matches simulations at the percent level on quasi-linear scales and generates mocks for DESI and DESI-II analyses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10679","ref_index":35,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Balancing bias, baryons, and scale cuts in LSST 3x2pt analysis","primary_cat":"astro-ph.CO","submitted_at":"2026-06-09T10:32:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A minimal bias model yields unbiased LambdaCDM constraints up to k_max=0.7 h/Mpc but biases neutrino mass estimates, while higher-order bias mimics baryonic suppression in LSST 3x2pt analyses using the new MGL pipeline.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04830","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmic variance or galaxy bias? Disentangling finite-volume and galaxy formation effects in cosmological analysis","primary_cat":"astro-ph.CO","submitted_at":"2026-06-03T12:53:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Develops a galaxy-biasing formalism for cosmic variance using perturbation theory and tests it on the non-linear BAO shift against N-body simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21436","ref_index":75,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Euclid preparation: Testing multi-field inflation with galaxy power spectrum and bispectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-05-20T17:26:36+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Validates redshift-space power spectrum and bispectrum analysis on Abacus-PNG mocks to recover unbiased f_NL constraints for Euclid spectroscopic sample.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.26915","ref_index":42,"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":"method","top_context_polarity":"use_method","context_text":"90(2003) 091301, [astro-ph/0208512]. [40] R. J. Scherrer,Mapping the Chevallier-Polarski-Linder parametrization onto Physical Dark Energy Models,Phys. Rev. D92(2015) 043001, [1505.05781]. [41] S. M. Carroll, V. Duvvuri, M. Trodden and M. S. Turner,Is Cosmic Speed-Up Due to New Gravitational Physics?,Phys. Rev. D70(2004) 043528, [astro-ph/0306438]. [42] F. Bernardeau, S. Colombi, E. Gaztanaga and R. Scoccimarro,Large scale structure of the universe and cosmological perturbation theory,Phys. Rept.367(2002) 1-248, [astro-ph/0112551]. [43] P. McDonald and A. Roy,Clustering of dark matter tracers: generalizing bias for the coming era of precision LSS,JCAP0908(2009) 020, [0902.0991]. [44] D. Baumann, A."},{"citing_arxiv_id":"2604.09407","ref_index":25,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Analytic compression of the effective field theory of the Lyman-alpha forest","primary_cat":"astro-ph.CO","submitted_at":"2026-04-10T15:20:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Analytic compression of EFT parameters for Lyα forest P1D via Fisher matrix and linearization allows efficient marginalization, saturating constraints with linear bias plus five effective terms and forecasting 10% and 2% precision on Δ²_p and n_p at k_p=0.7 Mpc^{-1}.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Palanque-Delabrouille, C. Y` eche, J.-M.L. Goff, E. Armengaud, J. Bautista et al.,The one-dimensional power spectrum from the SDSS DR14 Lyαforests,J. Cosmol. Astropart. Phys.2019(2019) 017. [24] M.A. Fernandez, S. Bird and M.-F. Ho,Cosmological constraints from the eBOSS Lyman-α forest using the PRIYA simulations,J. Cosmol. Astropart. Phys.2024(2024) 029 [2309.03943]. [25] P. McDonald and A. Roy,Clustering of dark matter tracers: generalizing bias for the coming era of precision LSS,JCAP0908(2009) 020 [0902.0991]. [26] D. Baumann, A. Nicolis, L. Senatore and M. Zaldarriaga,Cosmological Non-Linearities as an Effective Fluid,JCAP1207(2012) 051 [1004.2488]. [27] J.J.M. Carrasco, S. Foreman, D. Green and L. Senatore,The Effective Field Theory of Large"},{"citing_arxiv_id":"2604.08895","ref_index":3,"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":"Numerically, one findsσv ∼6D +(z)h −1Mpc. Upon expanding the damping functionD, the linear coefficient can be absorbed by the LO counterterm, but beyond that, the terms are new to the theory. We note that this expansion neglects terms proportional tok2mk2n ∥ withm >0, which can also be expected due to the short-range nonlocality induced by nonlinear processes in galaxy formation [3]. That is, we assume that the real-space galaxy power spectrum can be modeled with high accuracy using only the one-loop EFT up to somekmax, and the goal of the NLO counterterms in equation (2.6) is to achieve a similar level of accuracy for the redshift-space power spectrum. However, by resumming the expansion we effectively impose a specific functional relation"},{"citing_arxiv_id":"2511.20757","ref_index":91,"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":"background","top_context_polarity":"unclear","context_text":"Sibiryakov, JCAP1607, 052 (2016), arXiv:1512.05807 [astro-ph.CO]. [88] D. Blas, M. Garny, M. M. Ivanov, and S. Sibiryakov, JCAP1607, 028 (2016), arXiv:1605.02149 [astro-ph.CO]. [89] M. M. Ivanov and S. Sibiryakov, JCAP1807, 053 (2018), arXiv:1804.05080 [astro-ph.CO]. [90] P. McDonald, Phys. Rev. D74, 103512 (2006), [Erratum: Phys.Rev.D 74, 129901 (2006)], arXiv:astro-ph/0609413. [91] P. McDonald and A. Roy, JCAP0908, 020 (2009), arXiv:0902.0991 [astro-ph.CO]. [92] M. M. Ivanov, (2022), arXiv:2212.08488 [astro-ph.CO]. [93] M. P. Ib' a˜ nez, R. E. Angulo, and J. A. Peacock, (2024), arXiv:2407.07949 [astro-ph.CO]. [94] G. D'Amico, Y. Donath, M. Lewandowski, L. Senatore, and P. Zhang, (2022), arXiv:2206.08327 [astro-ph.CO]. [95] G."},{"citing_arxiv_id":"2503.14744","ref_index":110,"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":"method","top_context_polarity":"use_method","context_text":"Santos, M. Ho, and others, arXiv e-prints , arXiv:2503.14740 (2025), arXiv:2503.14740 [astro-ph.CO]. [108] P. McDonald and A. Roy, J. Cosmology Astropart. Phys. 2009, 020 (2009), arXiv:0902.0991 [astro-ph.CO]. [109] D. Baumann, A. Nicolis, L. Senatore, and M. Zaldar- riaga, J. Cosmology Astropart. Phys. 2012, 051 (2012), arXiv:1004.2488 [astro-ph.CO]. [110] J. J. M. Carrasco, M. P. Hertzberg, and L. Sena- tore, Journal of High Energy Physics 2012, 82 (2012), arXiv:1206.2926 [astro-ph.CO]. [111] Z. Vlah, M. White, and A. Aviles, J. Cosmology Astropart. Phys. 2015, 014 (2015), arXiv:1506.05264 [astro-ph.CO]. [112] H. E. Noriega, A. Aviles, H. Gil-Mar' ın, S. Ramirez- Solano, and others, J. Cosmology Astropart."},{"citing_arxiv_id":"2411.12021","ref_index":40,"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":"velocileptorsalso includes an Eulerian Perturbation Theory 11 (EPT) module, with the 10We employ the concept of conformity as a property of galaxies of a different type to tend to occupy different haloes. See for e.g., [136]. 11This option is also referred to in some papers or codes, such asdesilikeas Resummed Eulerian Pertur- bation Theory (REPT). - 17 - terms organised via an Eulerian bias expansion as in [40] and IR resummation performed via the wiggle no-wiggle split [43]. In the DESI DR1 analyses we will sample the Eulerian bias parameters as reparametrisations of the Lagrangian ones following the convention in [48], such that the nonlinear bias priors are centred at their advected predictions correspond- ing to zero Lagrangian bias, in order to harmonise the prior choices between the EPT and"},{"citing_arxiv_id":"2408.03036","ref_index":64,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Modeling and measuring the anisotropic halo 3-point correlation function: a coordinated study","primary_cat":"astro-ph.CO","submitted_at":"2024-08-06T08:38:35+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Novel implementation of anisotropic 3PCF model and estimator tested on 298 halo catalogs shows degeneracy breaking between f and b1 in 3PCF-only analysis but limited added value in joint 2PCF+3PCF due to tree-level model shortcomings on small scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1611.00036","ref_index":54,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The DESI Experiment Part I: Science,Targeting, and Survey Design","primary_cat":"astro-ph.IM","submitted_at":"2016-10-31T20:47:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"DESI will target luminous red galaxies to z=1, emission-line galaxies to z=1.7, quasars for tracers and Ly-alpha forest at 2.1