{"total":17,"items":[{"citing_arxiv_id":"2606.31988","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Joint inference of weak lensing convergence map and cosmology with diffusion models","primary_cat":"astro-ph.CO","submitted_at":"2026-06-30T17:25:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A transformer-based diffusion model learns the joint distribution of convergence maps and cosmology from log-normal weak lensing simulations and generates calibrated posterior samples matching MCMC results.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.31978","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"COSMOS-Web: does halo mass alone shape the clustering of star-forming and quiescent galaxies?","primary_cat":"astro-ph.GA","submitted_at":"2026-06-30T17:18:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Quiescent galaxies cluster more strongly than star-forming ones by 0.5-1 dex after halo-mass matching, with one-halo conformity up to z~2 that disappears at higher redshifts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28489","ref_index":200,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"pop-cosmos: Galaxy size evolution across structural and star-formation classifications in COSMOS-Web","primary_cat":"astro-ph.GA","submitted_at":"2026-06-26T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Galaxy size-mass relations exhibit double power-law breaks at different pivot masses for quiescent versus bulge-dominated samples, coinciding with AGN activity scales.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"Dashes are used for parameters where we do not have galaxies to constrain them. To compare with the scale radius𝑅0 in the single-power law fits, instead of reporting𝛾, we report log10 (𝑅 ∗/kpc), which is the value of the scale radius𝑅50 at𝑀 ∗ =5×10 10 M⊙ in Equation 3. sample redshift log10 (𝑅 ∗/kpc)𝛼 𝛽 𝛿 𝜎int 𝑁gal 𝑁gal bin dex( ≤10.3 M ⊙ ) (>10.3 M ⊙ ) quiescent:[0.0,0.5)0.39±0.02 0.15±0.02>1.52(4.13)>11.56(12.08)0.15±0.01633 304 log10 (sSFR/yr −1 ) [0.5,1.0)0.19±0.01−0.15±0.05 1.07±0.21 10.76±0.18 0.14±0.01665 1315 ≤ −11[1.0,1.5)0.07±0.02−0.45±0.19 0.98±0.21 10.45±0.25 0.15±0.01221 898 [1.5,2.0) −0.01±0.02-0.94±0.34-0.15±0.0152 529 [2.0,3.0) −0.16±0.04->0.71(0.99)-0.14±0.0211 166 bulge-dominated:[0.0,0.5)0.40±0.02 0.24±0.10 † <1.47(7.05)>12.52(12.94) † 0.20±0.01454 205 B/T≥0.6[0.5,1.0)0.24±0.02−0.01±0.03 1.70±1.16 11.35±0.21 0.18±0.011298 1099 [1.0,1.5)0.19±0.01−0.10±0.05 0.97±0.30 10.83±0.26 0.18±0.011379 1519 [1.5,2.0)0.11±0.02−0.11±0.05>1.10(1.66)>11.04(11.31)0.19±0.011014 1016 [2.0,3.0)0.03±0.03−0.11±0.04>1.33(4.10)>11.42(11.96)0.21±0.011348 545 early-type:[0.0,0.5)0.42±0.03 0.28±0.03>0.74(2.89)>11.66(12.37)0.21±0.01396 350 𝑛 >2.5[0.5,1.0)0.27±0.01 0.08±0.03>1.15(1.82)>11.24(11.54)0.18±0.011189 1660 [1.0,1.5)0.18±0.02−0.01±0.03>1.52(2.99)>11.40(11.77)0.20±0.011450 1290 [1.5,2.0)0.13±0.02−0.06±0.02>1.38(3.58)>11.38(11.88)0.21±0.011247 981 [2.0,3.0)0.08±0.03−0.04±0.05>0.68(3.07)>11.34(12.08)0.22±0.011948 636 † Bimodal posterior, only the main mode reported. Table 7.Posterior median and 68 per cent credible interval for the parameters describing the size-redshift relation. samplelog 10 (𝐵 𝑧 /kpc)𝛽 𝑧 full0.64±0.02 0.71±0.07 star-forming:log 10 (sSFR/yr −1 )>−11 0.74±0.03 0.82±0.04 quiescent, linear:log10 (sSFR/yr −1 ) ≤ −11 0.52±0.06 1.12±0.09 quiescent, double-power law:log10 (sSFR/yr −1 ) ≤ −11 0.48±0.07 1.16±0.22 disc-dominated:B/T≤0.2 0.77±0.02 0.66±0.04 intermediate:0.2<B/T<0.6 0.59±0.03 0.81±0.07 bulge-dominated, linear:B/T≥0.6 0.49±0.06 0.74±0.09 "},{"citing_arxiv_id":"2606.25583","ref_index":79,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Weak Lensing with SKAO: Cosmic Shear Cosmology","primary_cat":"astro-ph.CO","submitted_at":"2026-06-24T08:56:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Forecasts indicate SKAO cosmic shear can constrain S8 to 5% alone and 3% combined with LSST or Euclid, with added benefits from polarization and kinematics for separating lensing signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18437","ref_index":206,"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":"2606.12255","ref_index":67,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Towards Practical Field-Level Inference for Weak Lensing","primary_cat":"astro-ph.CO","submitted_at":"2026-06-10T15:57:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Field-level inference from weak lensing maps yields significantly tighter cosmological constraints than power-spectrum analysis when using the same forward-modeling pipeline, especially on small scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11308","ref_index":198,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"pop-cosmos: Disentangling galaxy properties from observables using data-driven approaches","primary_cat":"astro-ph.GA","submitted_at":"2026-06-09T18:00:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A beta-VAE analysis of pop-cosmos models finds that five latent dimensions capture the rest-frame optical SED, corresponding to stellar mass, recent star formation, dust, and two gas ionization states.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11305","ref_index":22,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Modeling the impact of filter-substrate refraction in the Roman point spread function","primary_cat":"astro-ph.IM","submitted_at":"2026-06-09T18:00:05+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Filter-substrate refraction causes dominant lateral shifts yielding 0.3-0.4% PSF size and ellipticity residuals across most Roman bands that exceed weak lensing requirements by an order of magnitude, while longitudinal defocus shifts remain negligible.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06175","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"AKRA 3.0: A matrix-free Inversion Framework for Weak Lensing Mass Mapping and Its Application to DES Y3 Data","primary_cat":"astro-ph.CO","submitted_at":"2026-06-04T13:48:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"AKRA 3.0 uses conjugate gradient to solve the normal equations for weak lensing mass mapping, producing the highest-resolution DES Y3 convergence map to date and demonstrating unbiased power spectra extracted directly from the map.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15264","ref_index":138,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Near-IR Weak-lensing (NIRWL) Measurements in the CANDELS Fields. II. Mass Mapping and Overdensity Characterization","primary_cat":"astro-ph.GA","submitted_at":"2026-05-14T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First near-IR weak-lensing analysis of CANDELS fields detects 12 shear-selected overdensities with masses 0.2-2.2 x 10^14 solar masses at redshifts 0.22-0.9 and mean z=0.68.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15078","ref_index":58,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"KiDS+VIKING-450 cosmology with Bayesian hierarchical model redshift distributions","primary_cat":"astro-ph.CO","submitted_at":"2026-05-14T17:02:28+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian hierarchical modeling of photometric redshifts in KiDS+VIKING-450 raises S8 to 0.756 ± 0.039 and reduces Planck tension to 1.9σ.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.06790","ref_index":19,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Machine Learning Techniques for Astrophysics and Cosmology: Photometric Redshifts","primary_cat":"astro-ph.IM","submitted_at":"2026-05-07T18:00:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"AI techniques for photometric redshift estimation have converged and are now limited by the size, systematics, and selection effects in spectroscopic training samples rather than by methodology.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"signal-to-noise ratio. Photo-zoutliers suppress clustering amplitudes and bias in- ferred halo occupation interpretations unless their rate is known and accounted for. Cosmology, in turn, uses galaxies as tracers of the large scale structure growth. For this, redshifts or ensemble redshift distributions are always required. Weak grav- itational lensing analyses [19, 20] typically bin source galaxies by redshift, making their respectiveN(z)a first-order ingredient in predicting weak lensing shear ob- servables. Galaxy clustering and 3×2pt analyses (using shear-shear, galaxy-galaxy lensing, and galaxy clustering correlation functions) in addition depend on theN(z) of a \"lens\" galaxy sample. This encodes how likely two galaxies near one another"},{"citing_arxiv_id":"2604.26015","ref_index":16,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Kinematic Lensing Ratio: Reviving Weak Lensing Cosmography as a Geometric Dark Energy Probe","primary_cat":"astro-ph.CO","submitted_at":"2026-04-28T18:00:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"KiLeR combines shear ratios with kinematic intrinsic shapes to mitigate first-order lensing systematics and forecasts a 192% improvement in dark energy constraints from the Roman telescope.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"the number densityn g corresponding to the statistical er- ror levels. In the bottom panel, KiLeR+BAO with an extra LRG2 lens bin is plotted in red plus signs to illustrate the self- calibration potential of KiLeR. Themconstraint from DES Y6 and the requirement for Roman WL are shown as the ver- tical dashed and dotted lines, respectively, for comparison. weak-lensing calibration formalism [16]: γobs = (1 +m)γ true +c+N(0, σ 2 γ) +O(γ 2 true),(8) where theσ γ term represents the shape noise. Global additive bias (c) is easily removed by enforcing a zero mean shear in each tomographic bin, assuming cosmic isotropy. Multiplicative bias (m), however, typically re- quires rigorous calibration to prevent biased cosmological inference. KiLeR naturally self-calibratesm[57]."},{"citing_arxiv_id":"2510.18741","ref_index":242,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Nonlinear Matter Power Spectrum from relativistic $N$-body Simulations: $\\Lambda_{\\rm s}$CDM versus $\\Lambda$CDM","primary_cat":"astro-ph.CO","submitted_at":"2025-10-21T15:46:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Relativistic N-body simulations of Lambda_s CDM produce a redshift-dependent crest in the matter power spectrum ratio, peaking at 20-25% near the transition and leaving a 15-20% uplift at z=0 on group scales.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Watson, Toward the Standard Population Syn- thesis Model of the X-Ray Background: Evolution of X-Ray Luminosity and Absorption Functions of Active Galactic Nuclei Including Compton-Thick Populations, Astrophys. J.786, 104 (2014), 1402.1836. [241] M. Kilbinger, Cosmology with cosmic shear observations: a review, Rept. Prog. Phys.78, 086901 (2015), 1411.0115. [242] R. Mandelbaum, Weak lensing for precision cosmol- ogy, Ann. Rev. Astron. Astrophys.56, 393 (2018), 1710.03235. [243] J. C. Hill and D. N. Spergel, Detection of thermal SZ- CMB lensing cross-correlation in Planck nominal mission data, JCAP02, 030, 1312.4525. [244] E. M. Georgeet al., A measurement of secondary cos- mic microwave background anisotropies from the 2500-"},{"citing_arxiv_id":"2510.13962","ref_index":34,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Simulation budgeting for hybrid effective field theories","primary_cat":"astro-ph.CO","submitted_at":"2025-10-15T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Forecasts that under 225 N-body simulations suffice for 1-2% accurate HEFT emulators over wide w0waCDM + m_nu parameter space, with as few as 80 for restricted volumes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Dolag,Demnuni: the clustering of large-scale structures in the presence of massive neutrinos,Journal of Cosmology and Astroparticle Physics2015(2015) 043-043. [33] A.E. Bayer, A. Banerjee and Y. Feng,A fast particle-mesh simulation of non-linear cosmological structure formation with massive neutrinos,Journal of Cosmology and Astroparticle Physics2021(2021) 016-016. [34] R. Mandelbaum,Weak Lensing for Precision Cosmology,ARA&A56(2018) 393 [1710.03235]. [35] J. Prat and D. Bacon,Weak Gravitational Lensing,Encyclopedia of Astrophysics (First Edition)(2025) 508 [2501.07938]. [36] O. Truttero, J. Zuntz, A. Pourtsidou and N. Robertson,Baryon-frees8 tension with stage iv cosmic shear surveys,The Open Journal of Astrophysics8(2025) ."},{"citing_arxiv_id":"2105.13549","ref_index":23,"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":"background","top_context_polarity":"background","context_text":"(BOSS), Mon. Not. Roy. Astron. Soc.470, 2617 (2017), arXiv:1607.03155 [astro-ph.CO]. [20] J. Elvin-Poole et al. (DES), Phys. Rev. D 98, 042006 (2018), arXiv:1708.01536 [astro-ph.CO]. [21] S. Alam et al. (eBOSS), (2020), arXiv:2007.08991 [astro- ph.CO]. [22] R. Mandelbaum, Ann. Rev. of Astr. & Astroph. 56, 393 (2018), arXiv:1710.03235 [astro-ph.CO]. [23] T. Schrabback et al., Astron. Astrophys. 516, A63 (2010), arXiv:0911.0053 [astro-ph.CO]. 30 [24] C. Heymans et al., Mon. Not. Roy. Astron. Soc. 432, 2433 (2013), arXiv:1303.1808 [astro-ph.CO]. [25] M. J. Jee, J. A. Tyson, S. Hilbert, M. D. Schneider, S. Schmidt, and D. Wittman, Astrophys. J. 824, 77 (2016), arXiv:1510.03962 [astro-ph.CO]. [26] M."},{"citing_arxiv_id":"0805.2366","ref_index":266,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"LSST: from Science Drivers to Reference Design and Anticipated Data Products","primary_cat":"astro-ph","submitted_at":"2008-05-15T18:10:13+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"LSST will image 18,000 square degrees of sky about 800 times across six bands over 10 years to a coadded depth of r~27.5, producing a public database of 40 billion objects and 32 trillion observations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"come standard in analyses of precursor datasets (e.g. DES Collaboration et al. 2017; Joudaki et al. 2018). WL and LSS are highly complementary probes, and the combination of their auto- and cross-correlations will constrain the properties of the late-time accelerated expansion while provid- ing internal cross-checks for marginalizing over systematic uncertainties (e.g., Mandelbaum 2017). These measurements consist of the two-point auto- and cross-correlations of shear and positions for billions of galaxies across ∼ 10 redshift bins. As described in the following two items, the galaxy- 34 Ivezi'c, Kahn, Tyson, Abel, Acosta, Allsman, Alonso, AlSayyad, Anderson, et al. Figure 23. Marginalized 1σ errors on the comoving distance (open triangles) and growth factor (open circles) parameters"}],"limit":50,"offset":0}