{"total":39,"items":[{"citing_arxiv_id":"2605.23367","ref_index":37,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological constraints from neighbor-density-weighted marked correlation functions","primary_cat":"astro-ph.CO","submitted_at":"2026-05-22T08:33:44+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":"2605.22407","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Hostless extragalactic transients in Fink: Results from the ELEPHANT pipeline","primary_cat":"astro-ph.IM","submitted_at":"2026-05-21T12:35:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"ELEPHANT flags hostless transients from ZTF alerts with 0.84 accuracy, confirming 67 genuine cases mostly as Type Ia supernovae from 877 candidates between 2023 and 2025.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19615","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reassessing the Statistical Necessity of Stellar Velocity Anisotropy in Strong-Lensing Cosmology with Lens-by-Lens Photometric Constraints","primary_cat":"astro-ph.CO","submitted_at":"2026-05-19T09:55:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Analysis of 107 matched strong-lensing and supernova pairs with lens-specific luminosity slopes finds that free stellar anisotropy is statistically required and reveals negative redshift evolution in early-type galaxy density profiles.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19476","ref_index":79,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Prospect of Measuring the Cosmic Dipole by Strongly Lensed Gravitational Waves Associated with Galaxy Surveys","primary_cat":"astro-ph.CO","submitted_at":"2026-05-19T07:28:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Simulations forecast that 10 years of Einstein Telescope and Cosmic Explorer data could detect the cosmic dipole magnitude using strongly lensed GW events, with tighter bounds from combining double, triple, and quadruple lensed systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19188","ref_index":14,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Lossless Compression of Cosmological Information from Type Ia Supernova Distance Measurements","primary_cat":"astro-ph.CO","submitted_at":"2026-05-18T23:27:05+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Compressing SN Ia distance-redshift data to eleven Gaussian log r_p(z) points with covariance is shown to be operationally lossless for cosmological inference across multiple models and datasets.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18938","ref_index":17,"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":"2605.18161","ref_index":126,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"SDSS-V: Revealing a weak accretion state in X-ray selected red quasars","primary_cat":"astro-ph.GA","submitted_at":"2026-05-18T10:05:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Red quasars are intrinsically X-ray weak with low alpha_OX values, tracing a distinct evolutionary stage of suppressed black hole accretion relative to stellar mass growth.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13219","ref_index":34,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Comparative analysis of missing data imputation methods for CSST survey: Impact on photometric redshift estimation performance","primary_cat":"astro-ph.GA","submitted_at":"2026-05-13T09:12:58+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"KNN imputation gives highest photo-z accuracy under ideal random missingness with complete training data, while SAITS is more robust for incomplete training sets and realistic mixed missingness patterns in CSST data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11709","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Synergy between the Cherenkov Telescope Array Observatory and the Vera C. Rubin Observatory","primary_cat":"astro-ph.HE","submitted_at":"2026-05-12T08:01:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"CTAO and Rubin Observatory synergies in multi-messenger time-domain astronomy for non-thermal extragalactic sources could help address the origins of TeV-PeV neutrinos and multi-EeV cosmic rays, with the Fink broker proposed to manage Rubin's high alert volume.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.06799","ref_index":169,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"On the origin of the environmental step: A BayeSN view of the ZTF SN Ia DR2","primary_cat":"astro-ph.CO","submitted_at":"2026-05-07T18:01:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"BayeSN analysis of ZTF Type Ia supernovae confirms a ~0.1 mag intrinsic environmental step in standardized brightness that is not explained by differences in dust extinction properties.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.27511","ref_index":26,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Finding Strongly Lensed Supernovae from Blended Light Curves","primary_cat":"astro-ph.IM","submitted_at":"2026-04-30T07:09:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A model-independent method fits blended supernova light curves as superpositions of two time-delayed components and finds only one candidate above a 12-day delay threshold in 445 ZTF Type Ia supernovae, for a 0.22% false positive rate.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ing can complement other probes such as supernovae and the CMB to constrain dark energy, while [25] analyzed the potential of lensed events forH 0 and other cosmo- logical parameter constraints. Building on these develop- ments, efforts have also been made to improve the iden- tification and exploitation of lensed supernovae in large surveys. For example, [26] proposed model-independent cosmological inference using Gaussian processes applied to lensing time delays, and other studies have demon- strated the use of multiply imaged supernovae for direct H0 measurements [27]. Recently, [28] searched the ZTF archive for candidate lensed supernovae Ia using vari- able source selection, thereby motivating flexible detec-"},{"citing_arxiv_id":"2604.27420","ref_index":7,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The Solar System Notification Alert Processing System (SNAPS): Public access to SNAPS data and products","primary_cat":"astro-ph.EP","submitted_at":"2026-04-30T04:51:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"SNAPS is a public data broker for moving object detections from ZTF and LSST surveys.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.24330","ref_index":69,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Pre-localization of Massive Black Hole Binaries in the Millihertz Band","primary_cat":"gr-qc","submitted_at":"2026-04-27T11:21:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A neural spline flow pipeline performs amortized inference on millihertz MBHB signals, delivering ~20 deg² pre-merger sky localizations in ~1 minute while matching PTMCMC sky modes and parameter uncertainties.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"the most promising candidates for benefiting from rapid inference in support of pre-merger EM follow-up. By contrast, if the clustered sky localization is broad or frag- 15 TABLE VII. Illustrative tiling times for a 90% credible sky areaA 90 = 20 deg2 with 8 modes Facility FoV [deg 2]t read [s]t exp [s]N tile Imaging time [min] Reference Rubin/LSST 9.6 2 30 8≈8×(30 + 2)/60≈4.3 [69] ZTF 47 10 30 8≈8×(30 + 10)/60≈5.3 [70] Pan-STARRS1 7.068 - 45 - 60 8≈8×60/60 = 8 [71, 72] Athena 0.44 - 10 4 −10 5 46≈46×(10 5)/60 = 76.7 [5, 73] TABLE VIII. Sky localization for 10 independent noise re- alizations of the same injected signal. For each realization, we report the recovered 90% credible sky areaA 90. Since the number of predicted sky modes is consistently 8 across"},{"citing_arxiv_id":"2604.19746","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Calibration-Induced Systematics in SALT3 Training and Their Impact on Dark Energy Constraints from Stage IV Supernova Surveys","primary_cat":"astro-ph.CO","submitted_at":"2026-04-21T17:59:47+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Calibration uncertainties during supernova light-curve fitting cause roughly 50% degradation in dark energy figure of merit for Stage IV surveys, dominating over 13% degradation from model training errors and showing near-degeneracy with cosmology.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18910","ref_index":45,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Predicting Redshift in Seyfert Galaxies Using Machine Learning","primary_cat":"astro-ph.GA","submitted_at":"2026-04-20T23:27:10+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Random Forest regression on combined optical plus mid-infrared colors yields NMAD of 0.0188, R-squared of 0.9561, and 0.294 percent outliers for photometric redshifts in 23,797 Seyfert II galaxies selected from SDSS and WISE.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18859","ref_index":61,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Testing $\\Lambda$CDM versus dynamical dark energy in one year: A DESI spectroscopic follow-up program for Rubin supernovae","primary_cat":"astro-ph.CO","submitted_at":"2026-04-20T21:33:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A coordinated Rubin-DESI supernova survey could distinguish dynamical dark energy from Lambda CDM at over 5 sigma in one year using 2300 spectroscopically confirmed SNe Ia at low redshift.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.14802","ref_index":48,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Euclid. Populating a dark universe with galaxies using SciPIC","primary_cat":"astro-ph.CO","submitted_at":"2026-04-16T09:25:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"SciPICal calibrates galaxy properties in halo-based mocks for Euclid, delivering improved clustering predictions and a deep catalogue validated to 15 percent against observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.07134","ref_index":41,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"LightCurveLynx: Forward Modeling of Time-Domain Surveys with Application to ZTF SN Ia DR2","primary_cat":"astro-ph.IM","submitted_at":"2026-04-08T14:28:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LightCurveLynx is a flexible forward-modeling tool that produces supernova light-curve simulations matching ZTF observations with low KL divergence and consistent completeness limits.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"fragmented and features vary from solution to solution. At the same time, the demand for a unified, flexible, scalable, and user-friendly simulation framework has grown rapidly as new facilities with unprecedented discovery power and photometric precision, such as the Vera C. Rubin Observatory's Legacy Survey of Space and Time (LSST, LSST Science Collaborations and LSST Project 2009; ˇZ. Ivezi' c et al. 2019) and the Nancy Grace Roman Space Telescope (D. Spergel et al. 2015), begin operations. LightCurveLynx, developed by the LINCC Frameworks team, is designed to meet these community needs. It provides a unified, open-source framework for forward-simulation of transient and time-varying phenomena that supports both a variety of surveys and model types."},{"citing_arxiv_id":"2604.04867","ref_index":51,"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":"dataset","top_context_polarity":"use_dataset","context_text":"robust discrimination among competing inflationary sce- narios [49]. In particular, slow-roll single field inflation predict a tiny amount of local PNG:f loc NL ∼0.01 [50]. In this work, we extend the work of [11, 35] by using the large-scale clustering of the Luminous Red Galaxy (LRG), Emission Line Galaxy (ELG) and quasar (QSO) samples from the second data release (DR2) [51] of the Dark Energy Spectroscopic Instrument (DESI) [52, 53]. At the time of writing, the galaxy-galaxy power spectrum is still blinded and cannot be included in this analysis. Once allowed, we will combine it with the result of this paper to take advantage of gains from sample variance cancellation [18]. Note the two other companion anal- yses: [54] explores the synergies between spectroscopic"},{"citing_arxiv_id":"2603.18223","ref_index":68,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Gamma-Ray Bursts as an Independent High-Redshift Probe of Dark Energy","primary_cat":"astro-ph.CO","submitted_at":"2026-03-18T19:14:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Forecasts show that ~66 optical GRBs can achieve σ_w ≈ 0.47 in wCDM using Dainotti relations, matching Planck precision and enabling independent high-redshift tests of dark energy.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"67 using the Amati relation which relates the spectral peak energy to the isotropic equivalent radiated energy for 182 GRBs calibrated on the Pantheon+ SNe Ia sample (D. Scolnic et al. 2022). A similar approach is found in H. Wang & N. Liang (2024), but considering thew0waCDM model. The w0waCDM model, known also as the Chevallier-Polarski-Linder (CPL) parametrization (M. Chevallier & D. Polarski 2001; E. V. Linder 2003), considers a varying Energy equation-of-state (EoS) wherewis parametrized as an evolving function of redshift. An important question to answer is to what extent the precision on the cosmological parameterwcan be expected from the new observations of the GRBs. To tackle this goal, we need to have the smallest possible scatter in the GRB 2D correlations."},{"citing_arxiv_id":"2603.13053","ref_index":70,"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":"modeling the underlying matter field and its Poisson trac- ers as a GRF, beginning with the 3D power spectrum in Section III B 1 and changing to spherical coordinates in Section III B 2. For simplicity we will assume perfect lo- calizations and complete sky coverage, and leave treating noise for Section V. Much of the information in this sec- tion can be found in standard cosmology texts [70, 71] . 1. The 3D power spectrum It is well-known that the primordial dark matter field which formed the initial seeds of LSS is a GRF. That is, the random realization of initial dark matter fluctu- ations can be modeled as a draw from its characteristic power spectrum. In linear perturbation theory, the mat- ter density field at late times can still be considered to"},{"citing_arxiv_id":"2603.12504","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Exploring Beyond {\\Lambda}CDM with the Weak Lensing Power Spectrum and Bispectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-03-12T22:49:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Fisher forecasts show the weak lensing bispectrum reduces errors on CPL w0 and IDE coupling parameters but leaves f(R) scalaron constraints essentially unchanged after full marginalization over nuisance parameters.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"it a clean tracer of large-scale structure. Current gener- ation (Stage-III) surveys like KiDS [18], DES [19], Hy- per Suprime-Cam [20] have already placed competitive tomographic constraints on theΛCDM parameter space, particularly on theS 8 ≡σ 8 p Ωm/0.3 combination. The forthcoming (Stage IV) program Vera C. Rubin Observa- tory Legacy Survey of Space and Time (LSST) [21, 22], Euclid [23, 24], Nancy Grace Roman Space Telescope [25] will extend these measurements to substantially higher source densities and redshifts, and are projected to yield percent-level constraints on both the Hubble expansion rateH(a) and the linear growth factorD(a;k) through measurements of the nonlinear matter power spectrum [26, 27, 21, 22]."},{"citing_arxiv_id":"2601.21111","ref_index":42,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Euclid preparation. Decomposing components of the extragalactic background light using multi-band intensity mapping cross-correlations","primary_cat":"astro-ph.CO","submitted_at":"2026-01-28T23:01:02+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Multi-band EBL intensity mapping cross-correlated with cosmic shear and galaxy clustering recovers IHL, IGL, and EoR parameters with 10-35% smaller uncertainties than intensity mapping alone.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.14554","ref_index":23,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"IRMaGiC: Extending Luminous Red Galaxy Selection into the Infrared with Joint Rubin Observatory's Large Survey of Space Time and Roman's High Latitude Imaging Survey","primary_cat":"astro-ph.CO","submitted_at":"2026-01-21T00:29:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"IRMaGiC extends redMaGiC to z=1-2 using joint LSST optical and Roman infrared data, reducing photo-z scatter and bias for LRGs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.19783","ref_index":38,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"SN 2025ogs: A Spectroscopically-Normal Type Ia Supernova at z = 2 as a Benchmark for Redshift Evolution","primary_cat":"astro-ph.CO","submitted_at":"2025-12-22T19:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"SN 2025ogs is a spectroscopically normal Type Ia supernova at z=2.05 whose luminosity distance and properties are consistent with low-z standards and current LambdaCDM constraints.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.23073","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraining dark matter halo profiles with symbolic regression","primary_cat":"astro-ph.CO","submitted_at":"2025-11-28T11:02:30+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Exhaustive symbolic regression on mock weak lensing excess surface density data recovers NFW profiles at 5% fractional errors with as few as 20 clusters but favors simpler functions at higher uncertainties because errors are smallest in the outskirts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.12488","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The first AKRA mass map reconstruction from HSC Y1 data","primary_cat":"astro-ph.CO","submitted_at":"2025-11-16T07:53:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"AKRA produces the first unbiased kappa maps from HSC Y1 shear catalogs, with simulation tests confirming no bias in power spectrum, variance, skewness, and PDF statistics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.11147","ref_index":44,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Galactic foreground residue biases in cosmic-microwave-background lensing-convergence reconstruction and delensing of B-mode maps","primary_cat":"astro-ph.CO","submitted_at":"2025-11-14T10:25:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Galactic foreground residuals after component separation bias lensing reconstruction errors at cosmic-variance levels with Gaussian terms dominating, while non-Gaussian errors are three orders smaller; residuals become a leading error for high-efficiency delensing.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2511.05653","ref_index":76,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing Dark Energy Microphysics with kSZ Tomography","primary_cat":"astro-ph.CO","submitted_at":"2025-11-07T19:00:02+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Fisher-matrix forecasts for LSST- and CMB-S4-like surveys show kSZ tomography tightens constraints on dark energy parameters w0 and wa by 15% and 32% while assessing detectability of perturbations for different sound speeds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.21521","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Synergy between CSST and third-generation gravitational-wave detectors: Inferring cosmological parameters using cross-correlation of dark sirens and galaxies","primary_cat":"astro-ph.CO","submitted_at":"2025-10-24T14:43:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Forecasts that cross-correlating 3G GW dark sirens with CSST photometric galaxies yields 1.04% precision on H0 and 2.04% on Omega_m while also constraining GW clustering bias.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"cross-correlation of dark sirens and galaxies. I. INTRODUCTION Exploring the distribution of the three-dimensional large-scale structure (LSS) of the universe is one of the central goals of modern cosmology. Current optical sur- vey projects, such as the Dark Energy Spectroscopic In- strument (DESI) [1], Euclid [2, 3], the Vera Rubin Obser- vatory [4], and the China Space Station Survey Telescope (CSST) [5], aim to map the distribution of tens of millions to billions of galaxies across a wide redshift range. By em- ploying statistical tools such as power spectra [6, 7], cor- relation functions [8, 9], and tomographic angular power spectra [10, 11], these observations can precisely char- acterize LSS, thereby providing high-precision data to"},{"citing_arxiv_id":"2509.17696","ref_index":38,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tracing the high-z cosmic web with Quaia: catalogues of voids and clusters in the quasar distribution","primary_cat":"astro-ph.CO","submitted_at":"2025-09-22T12:33:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Using 708,483 quasars at 0.8