{"total":16,"items":[{"citing_arxiv_id":"2606.24868","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Exploring Gravitational Wave Signatures Due to Primordial Non-gaussianity and Large Scale Structure Using SKAO","primary_cat":"astro-ph.CO","submitted_at":"2026-06-23T17:47:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Explores SKAO detection of scalar-induced GW backgrounds as probes of primordial non-Gaussianity and parity violation, with LSS cross-correlation to improve SNR.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21436","ref_index":80,"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":"2605.18938","ref_index":9,"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":"2605.03783","ref_index":16,"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":"Raccanelli, E. Aubourg, D. Bizyaev, H. Brewington, J. Brinkmann, et al., MNRAS428, 1116 (2013), 1208.1491. [14] B. Leistedt, H. V. Peiris, and N. Roth, Phys. Rev. Lett.113, 221301 (2014), 1405.4315. [15] T. Giannantonio, A. J. Ross, W. J. Percival, R. Crittenden, D. Bacher, M. Kilbinger, R. Nichol, and J. Weller, Phys. Rev. D89, 023511 (2014), 1303.1349. [16] T. Giannantonio and W. J. Percival, MNRAS441, L16 (2014), 1312.5154. [17] E.-M. Mueller, M. Rezaie, W. J. Percival, A. J. Ross, R. Ruggeri, H.-J. Seo, H. Gil-Mar' ın, J. Bautista, J. R. Brownstein, K. Dawson, et al., MNRAS514, 3396 (2022). [18] F. McCarthy, M. S. Madhavacheril, and A. S. Maniyar, Physical Review D108, 083522 (2023), ISSN 2470-0010, 2470-0029, URLhttps://link."},{"citing_arxiv_id":"2605.02882","ref_index":43,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Tracing Primordial Gravitational Waves via non-Gaussian Signatures of Halo Bias","primary_cat":"astro-ph.CO","submitted_at":"2026-05-04T17:51:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Tensor-induced non-Gaussianity from primordial gravitational waves generates a unique scale-dependent halo bias correction that can reach order-one amplitude for rare high-redshift halos at z=7.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"07521 [astro-ph.CO]. [39] E. Dimastrogiovanni, M. Fasiello, and T. FujitaJCAP01, 019, arXiv:1608.04216 [astro-ph.CO]. [40] B. Grinstein and M. B. WiseAstrophys. J.310, 19 (1986). [41] S. Matarrese, F. Lucchin, and S. A. BonomettoAstrophys. J. Lett.310, L21 (1986). [42] S. Matarrese and L. VerdeAstrophys. J. Lett.677, L77 (2008), arXiv:0801.4826 [astro-ph]. [43] N. Dalal, O. Dore, D. Huterer,et al.Phys. Rev. D77, 123514 (2008), arXiv:0710.4560 [astro-ph]. [44] A. Slosar, C. Hirata, U. Seljak,et al.JCAP08, 031, arXiv:0805.3580 [astro-ph]. [45] L. Verde and S. MatarreseAstrophys. J. Lett.706, L91 (2009), arXiv:0909.3224 [astro-ph.CO]. [46] V. Desjacques, D. Jeong, and F. SchmidtPhys. Rev. D 84, 063512 (2011), arXiv:1105."},{"citing_arxiv_id":"2604.04897","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Fast Radio Burst Dispersion Measure--Timing Cross-Correlations: Bias Self-Calibration and Primordial Non-Gaussianity Constraints","primary_cat":"astro-ph.CO","submitted_at":"2026-04-06T17:44:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DM-Shapiro timing cross-correlations self-calibrate electron bias b_e, recovering sigma(f_NL) within 1.0-1.9 of fixed-bias performance after marginalization.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"The current best constraint from the CMB bispectrum is fNL =−0.9±5.1(68% CL)[5]. - 1 - The theoretical threshold at which single-field inflation can be distinguished from multi- field models sits atσ(fNL)∼1[6], fueling ambitious efforts to map large-scale structure. Local PNG imprints a characteristick−2 scale-dependent bias on biased tracers of the matter density [4, 7-9]: beff(k, z) =b(z) + ∆b NG(k, z),∆b NG = 3fNL δc (b−1) Ω mH2 0 c2 a k2 .(1.2) Since the PNG signal diverges at smallk, measurements on the largest accessible scales are most powerful. Fast radio bursts (FRBs) are extragalactic radio transients with millisecond durations [10- 18]. Their dispersion measures; the frequency-integrated column density of free electrons along"},{"citing_arxiv_id":"2604.04867","ref_index":34,"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":"Zel'dovich velocity reconstruction from Planck and unWISE,arXiv e-prints(2024) [2405.00809]. [33] F. McCarthy, N. Battaglia, R. Bean, J. Richard Bond, H. Cai, E. Calabrese et al.,The Atacama Cosmology Telescope: Large-scale velocity reconstruction with the kinematic Sunyaev-Zel'dovich effect and DESI LRGs, Journal of Cosmology and Astroparticle Physics2025 (2025) 057. [34] J. Krywonos, S. C. Hotinli and M. C. Johnson, Constraints on cosmology beyondΛCDM with kinetic Sunyaev Zel'dovich velocity reconstruction,arXiv e-prints(2024) [2408.05264]. [35] A. Lagu¨ e, M. S. Madhavacheril, K. M. Smith, S. Ferraro and E. Schaan,Constraints on Local Primordial Non-Gaussianity with 3D Velocity Reconstruction from the Kinetic Sunyaev-Zeldovich"},{"citing_arxiv_id":"2512.17865","ref_index":10,"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":"2509.08787","ref_index":91,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"11 Note that since there is no fiducial signal inP EB and no contributions other than shape noise inP BB, the covariance does not contain terms proportional toP 2(k). Additionally, in practice, since (b 2D K )2P(k)< σ 2 γ/¯ng, the 11 Here,γrefers to the shear, which is defined as the measured ellipticityϵdivided by the shear responsivity factor 2R ≡2(1− σ2 ϵ ), i.e.,γ=ϵ/(2R) [91]. The amplitude parameter shown in Eq. (137) is also defined with this normalization. For the sample used in Ref. [88],R ≃0.93, which corresponds toσ ϵ ≃0.27 [92]. covariance is dominated by shape noise. As a result, the covariance matrix for the multipoles per mode is approx- imately diagonal. We adopt survey parameters motivated by the final year dataset of the Dark Energy Spectroscopic Instru-"},{"citing_arxiv_id":"2504.20992","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2411.12021","ref_index":94,"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":"More details on how this blinding technique has been tailored to DESI needs can be found in [93]. We adopt another - third - kind of blinding in cosmological analyses that test for primordial non-Gaussianity (that is when we constrain the parameterf NL). Becausef NL primarily affects the power spectrum by producing a scale-dependent bias that increases at large scales [88, 94, 95], the BAO and RSD blinding described above are insufficient. Instead, we apply to individual galaxies a set of weights that alter the imaging systematics to mimic anf NL signal.2 In what follows, we briefly summarise the procedure, but the full details of the specific methodology applied can be found in [88, 93]. We start by randomly choosing the variables{w 0, wa, fNL}, wherew 0 andw a are the parameters describing the time-variable"},{"citing_arxiv_id":"2411.07970","ref_index":102,"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":"There have been active searches off NL, especially for the local shape (f local NL ), but a firm detection has not been made yet. 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"},{"citing_arxiv_id":"2209.07472","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A $(D_\\tau,D_x)$-manifold with $N$-correlators of $N_t$-objects","primary_cat":"physics.gen-ph","submitted_at":"2022-08-05T22:57:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Constructs a (D_τ,D_x)-manifold with N-correlators of N_t-objects using field theory, topology, algebra, statistics and Fourier transforms, and discusses applicability across cosmological scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.04473","ref_index":132,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"CMB-S4 Science Case, Reference Design, and Project Plan","primary_cat":"astro-ph.IM","submitted_at":"2019-07-10T01:01:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Presents the science case, reference design, and project plan for the CMB-S4 ground-based CMB experiment.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Of course the measurement of both modes will in practice be noisy and limit the effect of sample-variance cancellation. Two different methods have recently been proposed for how to use high-resolution CMB maps to measure the matter field δm in conjunction with a large-scale galaxy survey for sample-variance cancellation: the reconstructed CMB lensing potential [132]; and the kSZ reconstruction [133]. Interestingly these two techniques trace different modes, since lensing probes transverse modes and kSZ velocities probe radial modes of the underlying matter distribution. We now discuss each technique in more detail. CMB-S4 Science Case, Reference Design, and Project Plan 1.2 Primordial gravitational waves and inflation 23"},{"citing_arxiv_id":"1807.06209","ref_index":91,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Planck 2018 results. VI. Cosmological parameters","primary_cat":"astro-ph.CO","submitted_at":"2018-07-17T04:05:07+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Final Planck CMB data confirms the flat 6-parameter ΛCDM model with Ω_c h² = 0.120 ± 0.001, Ω_b h² = 0.0224 ± 0.0001, n_s = 0.965 ± 0.004, τ = 0.054 ± 0.007, H_0 = 67.4 ± 0.5 km/s/Mpc, and no strong evidence for extensions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1611.00036","ref_index":154,"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