{"total":20,"items":[{"citing_arxiv_id":"2606.29735","ref_index":26,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2606.26237","ref_index":38,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"First full-shape joint analysis of the two- and three-point correlation functions on real data: $\\Lambda$CDM cosmological constraints from BOSS DR12","primary_cat":"astro-ph.CO","submitted_at":"2026-06-24T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"First joint 2PCF+3PCF full-shape analysis on BOSS DR12 real data improves σ(h) by ~29%, σ(ω_cdm) by ~10%, and σ(A_s) by ~24% over 2PCF alone via extra BAO information in 3PCF triangles.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"placed byN ∗ SV, yielding corrections significantly closer to unity than in the uncompressed case. 4.3. Likelihood and MCMC sampling We perform the cosmological inference in a Bayesian frame- work, sampling the posterior distribution of the model param- etersθ. The posterior is proportional to the product of the likeli- hood and the prior, P(θ|d)∝ L(d|θ)π(θ),(38) whereπ(θ) denotes the prior distribution. We adopt a Gaussian likelihood for the data vectord, −2 lnL(θ)=χ 2(θ)= d−m(θ) \u0001T ˆΨd−m(θ) \u0001 ,(39) For the 2PCF-only analysis,d=ξand ˆΨ = ˆΨξξ. For the joint 2PCF+3PCF analysis, the data vector is the concatenationd= (ξ,ζ) T and the precision matrix is computed from the full joint covariance of Eq. (30), which retains the cross-covariance block"},{"citing_arxiv_id":"2606.02686","ref_index":10,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"On-Shell Bootstrap of Loop Inflation Correlators with Spectral Dispersion","primary_cat":"hep-th","submitted_at":"2026-06-01T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Introduces spectral dispersion bootstrap combining dS spectral decomposition and dispersion relations to compute 3- and 4-point loop correlators with massive scalar and vector exchanges.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.01529","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Optimal Transport Reconstruction of Biased Tracers in Primordial Non-Gaussian Fields","primary_cat":"astro-ph.CO","submitted_at":"2026-06-01T01:21:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Optimal transport reconstruction of initial conditions from biased tracers in local PNG fields improves when a realistic model for the scale-dependent clustering of the unobserved dust is included.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.03783","ref_index":26,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"New constraints on primordial non-Gaussianity from large-scale cross-correlations of CMB lensing and the cosmic infrared background","primary_cat":"astro-ph.CO","submitted_at":"2026-05-05T14:09:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Dust-cleaned CIB and CMB lensing cross-correlations yield f_NL^local = 43 ± 23, tightening constraints on local primordial non-Gaussianity.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"20992 (2025), 2504.20992. [23] J. Krywonos, S. C. Hotinli, and M. C. Johnson, arXiv e-prints arXiv:2408.05264 (2024), 2408.05264. [24] A. Lagu¨ e, M. S. Madhavacheril, K. M. Smith, S. Fer- raro, and E. Schaan, Phys. Rev. Lett.134, 151003 (2025), 2411.08240. [25] S. C. Hotinli, K. M. Smith, and S. Ferraro, arXiv e-prints arXiv:2506.21657 (2025), 2506.21657. [26] F. McCarthy, B. Hadzhiyska, J. R. Bond, W. R. Coulton, J. Dunkley, C. Embil Villagra, M. C. Johnson, K. Moodley, T. Namikawa, B. Ried Guachalla, et al., arXiv e-prints arXiv:2511.15701 (2025), 2511.15701. [27] S. Chiarenza, A. Krolewski, M. Bonici, E. Chaus- sidon, R. d. Belsunce, W. Percival, J. N. Aguilar, S. Ahlen, A. B. Lizancos, D. Bianchi, et al."},{"citing_arxiv_id":"2605.02999","ref_index":195,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Peering down the barrel with DESI DR2: 10 000+ inflows at $z$ < 0.6 reveal how galaxies accrete cold gas","primary_cat":"astro-ph.GA","submitted_at":"2026-05-04T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI DR2 identifies 50,088 galaxies with moderate and 27,420 with strong evidence for down-the-barrel NaI D absorption revealing inflows at ~20 km/s and multiple accretion pathways at z < 0.6.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.21790","ref_index":25,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Informative Priors on Primordial Non-Gaussianity Bias $b_{\\phi}$ From Galaxy Formation","primary_cat":"astro-ph.CO","submitted_at":"2026-04-23T15:46:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Conditioning CAMELS-SAM simulations on the stellar mass function or stellar-to-halo mass relation reduces uncertainty in b_phi by 88-97% for DESI emission line galaxy samples while remaining consistent across galaxy formation variations.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"Large-scale structure surveys access a larger number of large-scale modes than the CMB through their three-dimensional maps of the galaxy distribution, making them well-suited probes of local-type PNG. Non-zerofloc NL imprints a scale-dependent signature on the galaxy distribution that is most prominent at large scales[32]. The tightest current LSS constraint is f loc NL =−0.0±4.1from [25], which exploits the full DESI DR1 dataset combining the galaxy power spectrum and bispectrum. Forthcoming analyses from the DESI collaboration [27] and surveys including Euclid [4] and SPHEREx [20, 35] are expected to improve upon these constraints through their larger survey volumes. SPHEREx in particular, is projected to achieveσ f loc NL \u0001 ∼1by combining power spectrum and bispectrum measurements, meeting"},{"citing_arxiv_id":"2604.18581","ref_index":62,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"If at First You Don't Succeed, Trispectrum: I. Estimating the Matter Power Spectrum Covariance with Higher-Order Statistics","primary_cat":"astro-ph.CO","submitted_at":"2026-04-20T17:59:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Estimators from squeezed bispectrum and collapsed trispectrum recover unbiased small-scale matter power spectrum covariance at the percent level using 25 Quijote simulations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"[58] T. Louiset al.(Atacama Cosmology Telescope), JCAP 11, 062 (2025), arXiv:2503.14452 [astro-ph.CO]. [59] E. Chaussidonet al., JCAP06, 029 (2025), arXiv:2411.17623 [astro-ph.CO]. [60] O. H. E. Philcox, Phys. Rev. D103, 103504 (2021), arXiv:2012.09389 [astro-ph.CO]. [61] O. H. E. Philcox, Phys. Rev. D104, 123529 (2021), arXiv:2107.06287 [astro-ph.CO]. [62] O. H. E. Philcox, Phys. Rev. D107, 123516 (2023), arXiv:2303.08828 [astro-ph.CO]. [63] O. H. E. Philcox, Phys. Rev. D108, 063506 (2023), arXiv:2306.03915 [astro-ph.CO]. [64] O. H. E. Philcox and T. Fl¨ oss, Phys. Rev. D112, 063507 (2025), arXiv:2404.07249 [astro-ph.CO]. [65] D. Gualdi, S. Novell-Masot, H. Gil-Marin, and L. Verde, JCAP01, 015 (2021), arXiv:2009."},{"citing_arxiv_id":"2604.15219","ref_index":11,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Nonperturbative stochastic inflation in perturbative dynamical background","primary_cat":"astro-ph.CO","submitted_at":"2026-04-16T16:50:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Derives stochastic equations from Schwinger-Keldysh formalism that include quantum diffusion and classical metric perturbations for non-perturbative ultra-slow-roll inflation, validated on Starobinsky and critical Higgs models.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"from galaxy power spectra and bispectra,\" Phys. Rev. D113, 063552 (2026), arXiv:2512.04266 [astro-ph.CO]. [9] Ya. B. Zel'dovich and I. D. Novikov, \"The Hypothesis of Cores Retarded during Expansion and the Hot Cosmological Model,\" Sov. Astron.10, 602 (1967). [10] Stephen Hawking, \"Gravitationally collapsed objects of very low mass,\" Mon. Not. Roy. Astron. Soc.152, 75 (1971). [11] Bernard J. Carr and S. W. Hawking, \"Black holes in the early Universe,\" Mon. Not. Roy. Astron. Soc.168, 399-415 (1974). [12] Bernard J. Carr, \"The Primordial black hole mass spectrum,\" Astrophys. J.201, 1-19 (1975). [13] Misao Sasaki, Teruaki Suyama, Takahiro Tanaka, and Shuichiro Yokoyama, \"Primordial black holes-perspectives in gravitational wave astronomy,\" Class."},{"citing_arxiv_id":"2604.08895","ref_index":58,"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":",Desi dr2 results. ii. measurements of baryon acoustic oscillations and cosmological constraints,Phys. Rev. D112(Oct, 2025) 083515, [2503.14738]. [57] K. Lodha, R. Calderon, W. L. Matthewson, A. Shafieloo, M. Ishak, J. Pan et al.,Extended Dark Energy analysis using DESI DR2 BAO measurements,arXiv e-prints(Mar., 2025) arXiv:2503.14743, [2503.14743]. [58]DESIcollaboration, C. Garcia-Quintero et al.,Cosmological implications of DESI DR2 BAO measurements in light of the latest ACT DR6 CMB data,Phys. Rev. D112(2025) 083529, [2504.18464]. [59] M. Ishak, J. Pan, R. Calderon, K. Lodha, G. Valogiannis, A. Aviles et al.,Modified Gravity Constraints from the Full Shape Modeling of Clustering Measurements from DESI 2024,arXiv"},{"citing_arxiv_id":"2604.04867","ref_index":43,"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":"primordial non-Gaussianity from intrinsic alignments of SDSS-III BOSS galaxies,Physical Review D108 (2023) 083533. [42] M. S. Cagliari, M. Barberi-Squarotti, K. Pardede, E. Castorina and G. D'Amico,Bispectrum constraints on Primordial Non-Gaussianities with the eBOSS DR16 quasars,Journal of Cosmology and Astroparticle Physics2025(2025) 043 [2502.14758]. [43] S. Chiarenza, A. Krolewski, M. Bonici, E. Chaussidon, R. de Belsunce, W. Percival et al.,Constraining primordial non-Gaussianity from DESI DR1 quasars and Planck PR4 CMB Lensing,arXiv e-prints23 (2025) 40 [2512.17865]. [44] A. Chudaykin, M. M. Ivanov and O. H. E. Philcox, Reanalyzing DESI DR1: 3. Constraints on Inflation from Galaxy Power Spectra and Bispectra,arXiv"},{"citing_arxiv_id":"2603.09278","ref_index":14,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2512.17865","ref_index":11,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2512.03824","ref_index":38,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The impact of our peculiar motion on primordial non-Gaussianity measurements using the LIGER4GAL framework","primary_cat":"astro-ph.CO","submitted_at":"2025-12-03T14:16:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LIGER4GAL finds that omitting the finger-of-the-observer effect biases f_nl by more than 1 sigma in 40% of realizations for k_min=0.0015 h/Mpc scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.08787","ref_index":106,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Parity Violation in Galaxy Shapes: Primordial Non-Gaussianity","primary_cat":"astro-ph.CO","submitted_at":"2025-09-10T17:15:21+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The parity-odd intrinsic alignment power spectrum probes the collapsed limit of the parity-odd primordial trispectrum and can tighten constraints on parity-violating PNG when bias parameters are calibrated from N-body simulations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"parameter introduced before redefining the final ampli- tude parameterA ℓm (without the tilde) in Eq. (112). Note that Eq. (102) corresponds to (ℓ, m) = (0,0). With the quadratic correction given in Eq. (105), we obtain the leading-order trispectrum (see Appendix D 2 for details): TΦ(k1,k 2,k 3,k 4) = X ℓℓ′m ρℓℓ′ ˜Aℓm ˜Aℓ′m(−1)ℓYℓm(ˆk1; ˆk12)Y ∗ ℓ′m(ˆk3; ˆk12) ×P ϕ(k1)Pϕ(k3)Pσ(k12) + 11 perms,(106) which includes the typical collapsed-type scale depen- denceP ϕ(k1)Pϕ(k3)Pσ(k12), along with the angular de- pendence expressed as the product of two spherical har- monics that capture the orientations of the two trian- gles sharing the diagonal ˆk12 (see Fig. 5 for an illustra- tion). As shown in Appendix D 2, this trispectrum tem- plate has both nonzero parity-even (real) and parity-odd"},{"citing_arxiv_id":"2504.20992","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constraints on primordial non-Gaussianity from Quaia","primary_cat":"astro-ph.CO","submitted_at":"2025-04-29T17:58:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Reports f_NL = -20.5^{+19.0}_{-18.1} (68% CL) from combined Quaia quasar auto-correlation and CMB lensing cross-correlation assuming p_phi=1, or -28.7^{+26.1}_{-24.6} for p_phi=1.6.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2503.14739","ref_index":101,"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":68,"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":"To minimize the risk of confirmation bias in our analy- sis, we used a blinding scheme to deliberately conceal the true position of the BAO peak observed from the data until all choices about our inference pipeline were final- ized. This blinding was applied at the level of the LSS catalogs, using the same prescription as was applied to DR1 and detailed in [68], but with a new random seed to produce unknown (but controlled) shifts to galaxy red- shifts that conceal the true BAO peak position. A num- ber of validation tests of both the data and the analysis pipeline were performed on the blinded data catalogs, as described in [48]. Once these tests were passed and the pipeline frozen, the blinding was removed and true"},{"citing_arxiv_id":"2411.12021","ref_index":75,"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":"Full-Shape measurements with the galaxy and quasar BAO measurements presented in [73] and the LyαBAO presented in [74]. The detailed cosmological inference including the com- bination with other cosmological probes is covered in a companion paper [1]. An analysis of the power spectrum to constrain potential primordial non-Gaussian signals is also presented in [75]. This paper is organised as follows, in Section 2 we present the DESI DR1 large-scale catalogues; in Section 3 the mock synthetic catalogues used in this paper, used for validating the pipeline and for producing the final covariances; in Section 4 we describe the methods used to extract cosmological information from the DESI catalogues and describe the different"},{"citing_arxiv_id":"2411.07970","ref_index":104,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"The state-of-the-art constraint comes from CMB mea- surements by Planck, withf local NL =−0.9±5.1 [101]. Mean- while, galaxy spectroscopic surveys are becoming increas- ingly promising, as LSS clustering can be highly sensitive to the PNG through scale-dependent galaxy bias [87, 102, 103]. Current bound on the local shape PNG from spectroscopic surveys is f local NL ∼ O(10) [104]. MUST, as a Stage-V spec- troscopic survey, is expected to improve the constraints on fNL significantly with the benefit of the increasing survey vol- ume and redshift range, surpassing current CMB constraints (see Section 5.4). Besides the traditional PNG searches, recent years have witnessed the fast development of new directions, such as cosmological collider (CC) physics."}],"limit":50,"offset":0}