{"total":15,"items":[{"citing_arxiv_id":"2606.27927","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Large-scale structures of the Universe: physics, phenomenology, statistics","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T10:20:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"Lecture series on the physics, phenomenology, and statistics of large-scale cosmic structure evolution and non-Gaussian predictions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23781","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Accurate modeling for 3$\\times$2pt analyses in Roman and Rubin: a study of model approximations","primary_cat":"astro-ph.CO","submitted_at":"2026-06-22T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulated likelihood analysis shows Limber approximation, neglected RSD, and approximate nonlinear power spectra each induce cosmological biases of ~1 sigma or more (exceeding 2 sigma for Rubin) in Roman and Rubin 3x2pt studies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18437","ref_index":85,"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":"2605.13547","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"UNIONS-3500 Weak Lensing: III. 2D Cosmological Constraints in Configuration Space","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T13:55:32+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"UNIONS-3500 weak lensing data yields S_8 = 0.831^{+0.067}_{-0.078} in flat LCDM from 2D cosmic shear, consistent with Planck within 1 sigma.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Following the notation of Hu & Jain (2004), the Gaussian covari- MNRAS000, 1-22 (2026) UNIONS-3500 Weak Lensing: III. 2D Cosmological constraints in configuration space7 ance term of any galaxy𝑔or shear𝛾field can be expressed as CovG = \u0002 (2ℓ1 +1)𝑓 sky Δℓ \u0003 −1 𝛿K ℓ1ℓ2 × 4 ( h 𝐶 𝐴𝐶,𝑖𝑘 ℓ1 +𝑁 𝐴𝐶,𝑖𝑘 ℓ1 i h 𝐶 𝐵𝐷, 𝑗𝑙 ℓ2 +𝑁 𝐵𝐷, 𝑗𝑙 ℓ2 i + h 𝐶 𝐴𝐷,𝑖𝑙 ℓ1 +𝑁 𝐴𝐷,𝑖𝑙 ℓ1 i h 𝐶 𝐵𝐶, 𝑗 𝑘 ℓ2 +𝑁 𝐵𝐶, 𝑗 𝑘 ℓ2 i ) (18) where𝐴, 𝐵, 𝐶, 𝐷represents either𝑔or𝛾for the observed fraction of the sky𝑓 sky, and noise power spectra𝑁𝑖 𝑗. In the case of cosmic shear,𝐴=𝐵=𝐶=𝐷=𝛾, hence it is simply𝑁 𝛾𝛾,𝑖 𝑗 ℓ = 𝜎2𝒆 2 ¯𝑛𝑖 𝛿K 𝑖 𝑗. Here¯𝑛𝑖 isthemeangalaxynumberdensityofbin𝑖and𝜎 𝒆 theshape noise,while𝛿 K 𝑖 𝑗 denotestheKroneckerdelta.However,transitioning to small scales, the cosmic shear field becomes significantly non-"},{"citing_arxiv_id":"2605.12877","ref_index":56,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Machine-learning applications for weak-lensing cosmology","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T01:45:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Machine learning techniques can mitigate limitations in traditional weak-lensing analyses and enhance extraction of cosmological information from galaxy imaging surveys.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"separates errors arising from the lensing kernelWκ and from the matter power spec- trumP m. The former is dominated by uncertainties in the photometric redshift dis- tribution of source galaxies, typically calibrated using external datasets and data- driven techniques [50]. The latter relies on large suites of cosmological simula- tions. Foundational training datasets have been constructed from gravity-only N- body simulations [51, 52, 53, 54, 55, 56, 57, 58, 59, 60, 61], while considerable effort has gone into modeling baryonic effects using hydrodynamical simulations and semi-analytic prescriptions [62, 63, 64, 65, 66, 67, 68, 69, 70, 71, 72, 73, 74, 75, 76, 77, 78, 79]. For summary statistics beyond the two-point level, simulation-based emula- tors are commonly employed. Ensemble averages over mock surveys allow the"},{"citing_arxiv_id":"2605.08465","ref_index":56,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"How to augment cosmic shear measurements with radio polarimetry of galaxies?","primary_cat":"astro-ph.CO","submitted_at":"2026-05-08T20:31:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A Gaussian statistical model of galaxy shapes and radio polarizations yields unbiased, minimum-variance estimators for cosmic shear, intrinsic alignment, and line-of-sight rotation that are accurate to first order.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ment (Γ1,Γ 2), we decompose them into E and B modes [52, 53]. In the linear regime on large angular scales, the B modes vanish for the physical weak lensing shear [54]. While both E and B modes may exist for intrinsic alignment [55], we assume the latter are vanishing. We compute a realistic angular power spectrumC γE γE ℓ for the E modes of lensing shear using - 12 - thehalofitmodel [56] of nonlinear matter power spectrum. Instead of adopting realistic physical models, we prescribe the angular power spectra for intrinsic alignment and polarization rotation for the purpose of validation. The power spectrum for the rotation angleα, which we assume to be uncorrelated with shear or intrinsic alignment, is set to be scale-invariant, Cαα"},{"citing_arxiv_id":"2603.13053","ref_index":53,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A unified harmonic framework for dark siren cosmology","primary_cat":"astro-ph.CO","submitted_at":"2026-03-13T15:03:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The GW-galaxy cross-correlation method, unified with spectral sirens in a harmonic framework, can measure H0 to 1% and Omega_m to 5% precision with 2 years of data from next-generation detectors like Einstein Telescope and Cosmic Explorer.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Karagiannis, M. Liguori, N. Bartolo, Y. Bouffanais, N. Giacobbo, M. Mapelli, and S. Matarrese, Gravitational Wave mergers as trac- ers of Large Scale Structures, JCAP2021(2), 035, arXiv:2007.06905 [astro-ph.CO]. [52] S. Kumar, Probing Cosmology with Baryon Acoustic Oscillations Using Gravitational Waves, ApJ959, 35 (2023), arXiv:2203.04273 [astro-ph.CO]. [53] A. Dehghani, J. L. Kim, D. S. Hosseini, A. Krolewski, S. Mukherjee, and G. Geshnizjani, The gravitational wave bias parameter from angular power spectra: bridg- ing between galaxies and binary black holes, JCAP 2025(4), 056, arXiv:2411.11965 [astro-ph.GA]. [54] E. L. Gagnon, D. Anbajagane, J. Prat, C. Chang, and J. Frieman, Cosmological Constraints from Combining"},{"citing_arxiv_id":"2510.14888","ref_index":127,"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":"U [𝑎, 𝑏]denotes an uniform distribution with edges[𝑎, 𝑏], whileN [𝑎, 𝑏]denotes a Gaussian distribution with mean𝑎and standard deviation𝑏. Tomographic bin indices are denoted by𝑖, and all our priors are the same for all bins. III. ANALYSIS OF LSST-Y1 SIMULATED DATA A. Simulating Cosmic Shear Data We simulate cosmic shear observations based on LSST-Y1, following the methodology of [127, 128] and detailed in [99]. Surveyspecifications,sourcegalaxyredshiftdistributions,and nuisance parameter priors are taken from the LSST DESC ScienceRequirementsDocument[65],andsummarizedinTa- ble II. The redshift distribution is modeled as a Smail distri- butionconvolvedwithaGaussianuncertainty0.02(1+𝑧)and divided into five tomographic bins with equal galaxy number"},{"citing_arxiv_id":"2510.00753","ref_index":53,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Impact of projection-induced optical selection bias on the weak lensing mass calibration of galaxy clusters","primary_cat":"astro-ph.CO","submitted_at":"2025-10-01T10:40:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Projection-induced selection bias causes 20-50% overestimation of weak lensing masses for optically selected galaxy clusters, larger on scales >3 Mpc.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2506.10469","ref_index":57,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraining the lensing dispersion from the angular clustering of binary black hole mergers","primary_cat":"astro-ph.CO","submitted_at":"2025-06-12T08:20:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Angular auto-correlation of gravitational wave sources decreases with lensing dispersion, and joint cross-correlation with galaxies partially breaks the degeneracy with source bias.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2411.12022","ref_index":104,"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":"method","top_context_polarity":"use_method","context_text":"[102] DES collaboration, Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and weak lensing , Phys. Rev. D 105 (2022) 023520 [ 2105.13549]. [103] VIRGO Consortium collaboration, Stable clustering, the halo model and nonlinear cosmological power spectra, Mon. Not. Roy. Astron. Soc. 341 (2003) 1311 [astro-ph/0207664]. - 41 - [104] R. Takahashi, M. Sato, T. Nishimichi, A. Taruya and M. Oguri, Revising the Halofit Model for the Nonlinear Matter Power Spectrum , Astrophys. J. 761 (2012) 152 [ 1208.2701]. [105] DES collaboration, Dark Energy Survey Year 3 results: Constraints on extensions to ΛCDM with weak lensing and galaxy clustering , Phys. Rev. D 107 (2023) 083504 [ 2207.05766]."},{"citing_arxiv_id":"2411.07970","ref_index":283,"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":"method","top_context_polarity":"use_method","context_text":"puted using either full-shape models or a template-based ap- proach. For the full-shape model, we use the forecast tool FishLSS15) described in [16]. FishLSS computes the non- linear tracer power spectrum using Lagrangian perturbation theory with a linear tracer bias model, refined by a single- parameter counter-term for small-scale corrections [282] that is calibrated to the HaloFit prescription [283]. Shot noise and the finger-of-god effect are incorporated based on the density of the tracers. The template-based approach is used only for thefσ 8 forecasts (Section 5.3). In this case, we use a code16) developed for a recent spectroscopic survey forecast [284], which refers to the RSD template from [285]. 5.1.2 Cosmological inference To convert the cosmological distances from BAO and struc-"},{"citing_arxiv_id":"2304.05202","ref_index":97,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and its Implications for Structure Growth","primary_cat":"astro-ph.CO","submitted_at":"2023-04-11T13:13:13+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"ACT DR6 yields a 2.3% precise CMB lensing power spectrum with A_lens = 1.013 ± 0.023 relative to Planck 2018 Lambda CDM, giving S8 = 0.818 ± 0.022 and no evidence for suppressed structure growth.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2105.13549","ref_index":182,"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":"method","top_context_polarity":"use_method","context_text":"CosmoSIS This pipeline uses the CAMB Boltzmann code [178, 179] to compute underlying background quantities and the linear matter power spectrum, and the H ALOFIT [180] version pre- sented in Ref. [181] for the non-linear power spectrum. It then generates theory predictions following the model de- scribed in section IV A, and using the Fast-PT method [182] for non-linear galaxy bias and the TATT model for intrinsic alignments. Non-Limber integrals are computed following the method of [169]. Accuracy parameters throughout the pipeline are chosen by requiring the log-likelihood to differ by less than 0.05 from a high precision calculation. For chains including Planck CMB measurements [13], we use thePlanck"},{"citing_arxiv_id":"2005.05290","ref_index":31,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cobaya: Code for Bayesian Analysis of hierarchical physical models","primary_cat":"astro-ph.IM","submitted_at":"2020-05-11T17:49:03+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Cobaya is a modular Bayesian analysis code that exploits model interdependencies via automatic caching and a novel parameter-blocking algorithm to minimize sampling cost.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}