{"total":12,"items":[{"citing_arxiv_id":"2606.31503","ref_index":97,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Large-Scale Structure of the Universe through the SKA lenses","primary_cat":"astro-ph.CO","submitted_at":"2026-06-30T11:22:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":1.0,"formal_verification":"none","one_line_summary":"This review chapter summarizes the cosmic web's theoretical framework, recent radio observations of diffuse gas, and the expected impact of the SKA on detecting baryons in filaments and cluster outskirts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24288","ref_index":17,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The large scale structure probes of dark energy","primary_cat":"astro-ph.CO","submitted_at":"2026-06-23T08:08:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review summarizing direct and auxiliary large-scale structure probes for constraining dark energy and demonstrating their combined precision and accuracy.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19875","ref_index":22,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The SPHEREx View of Galaxy Clusters: A Simulation-based Validation of the Forced Photometry Pipeline for Extended Sources","primary_cat":"astro-ph.GA","submitted_at":"2026-06-18T07:33:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations show SPHEREx photometry is generally unbiased but source blending drives outliers; with brightness selection, photometric redshifts reach σ_NMAD ≈ 0.003-0.01 and cluster redshifts are recovered to |Δz|/(1+z) < 0.002 at z ≲ 0.5.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17626","ref_index":67,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"PSZ: The meta-catalogue of Planck Sunyaev-Zeldovich sources","primary_cat":"astro-ph.CO","submitted_at":"2026-06-16T07:31:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"PSZ is a new meta-catalogue of 1500 confirmed Planck SZ clusters incorporating 281 new confirmations, 262 invalidations, updated redshifts for 552 clusters, and homogeneously derived masses corrected for selection effects.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.13359","ref_index":35,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Galaxy clusters in the VIDEO fields: detection and characterisation in the context of MOONRISE","primary_cat":"astro-ph.GA","submitted_at":"2026-06-11T13:46:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Reports a catalog of 519 cluster candidates (74 at z>1.5) from VIDEO fields via AMICO and WaZP, shows red-sequence galaxies consistent with passive evolution since high redshift, and evaluates MOONRISE detection strategies up to z~1.7.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02719","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Beyond Self-Similarity: Reconciling X-Ray Scaling Relations in Galaxy Clusters and Groups","primary_cat":"astro-ph.CO","submitted_at":"2026-06-01T18:00:05+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Power-law modeling of gas mass fraction and temperature variation reconciles observed X-ray scaling relations in galaxy clusters, reducing >3σ tensions from 49% to 11% and yielding a redshift-independent mass proxy Y_LGT0.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"some classical X-ray scaling laws:M−T(dot);M−M g (square); M−Y X (diamond);M−L(triangle). where the relations (3+2aL)α+3β+2γ=3 θ=a L α+γ ϕ=2α+β(5) among the exponents hold, anda L indicates the power index of the temperature-dependence of the cooling function in different energy bands and yields, e.g.−0.13,−0.12,0.45 and 1/2 in the bands [0.1-2.4] keV , [0.5-2] keV , [0.01-100] keV , also known as the pseudo-bolometric one, and the ideal bolometric one, respec- tively. A graphical representation of these relations is shown in Fig. 1. These relations are recovered from the scaling between the observables of interest and the mass:M∼f −1 g Mg;M∼R T r ∼ M1/3Tr ∼T 3/2 r ∼(f T T) 3/2, whereT r is the value of reference"},{"citing_arxiv_id":"2605.20027","ref_index":92,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"ComPACT: Mass-Redshift Properties of the galaxy cluster catalogue","primary_cat":"astro-ph.CO","submitted_at":"2026-05-19T15:51:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"ComPACT is a new SZ-selected galaxy cluster catalogue from CNN analysis of ACT+Planck data with 2,962 candidates, ~60% confirmation, 116 new redshifts, 158 new masses, and five new massive clusters at z>0.7 that increase the known high-mass high-z population by ~10%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15444","ref_index":13,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Clusters Hiding Under Millimeter Sources (CHUMS) I: Extreme CHUMS","primary_cat":"astro-ph.CO","submitted_at":"2026-05-14T21:58:46+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"AGN emission from central galaxies hides galaxy clusters in SZ surveys; CARMA-based subtraction recovers high-SNR detections in ACT maps for three specific clusters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15264","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Full details of the shape-fitting pipeline are described in (Finner et al. 2017, 2020). The elliptical Gaussian model has seven parameters: the background level (A0), the amplitude (A1), the centroid position (x, y), the complex ellipticity components (e 1,e 2), and the semi-major axis size (a). The ellipticity and its compo- nents are defined as e= a−b a+b ,(1) e1 =ecos(2θ),(2) e2 =esin(2θ),(3) wherebis the semi-minor axis andθis the position angle of the ellipse. The best-fit model parameters are obtained by mini- mizing theχ 2 statistic, χ2 = X\u0012 I−P⊛G σrms \u00132 ,(4) withMPFIT(Markwardt 2009), whereIis the image cutout,Pis the PSF model,Gis the Gaussian model, andσ rms is the rms image cutout. We construct galaxy cutouts from the F160W mosaics with a size equal to"},{"citing_arxiv_id":"2605.00988","ref_index":98,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Tidal pre-conditioning and ram-pressure stripping in NGC 1427A. Deep VLT/MUSE spectroscopy and FUV-to-radio observations trace a Fornax Cluster dwarf in transformation","primary_cat":"astro-ph.GA","submitted_at":"2026-05-01T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Multi-phase observations of NGC 1427A indicate tidal torquing from a dwarf fly-by has pre-conditioned its gas for ram-pressure stripping by the Fornax intracluster medium, placing the galaxy at the onset of environmental quenching with a declining star formation rate.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.22105","ref_index":18,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Backlighting the Cosmic Web with Fast Radio Bursts: An Anthology of Dispersion Measure Cross-Correlations with Large-Scale Structure and Baryon Tracers","primary_cat":"astro-ph.CO","submitted_at":"2026-04-23T22:27:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"FRB DMs correlate at 2.6-5 sigma with galaxies, weak lensing, CIB, CMB lensing, tSZ, X-ray clusters, SXRB and radio continuum, consistent with moderate feedback models while ruling out weak feedback at 3.5 sigma via SXRB-DM.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"of stellar mass between the central and satellite galax- ies. The collisionless matter profile starts from a trun- cated NFW profile and is adiabatically relaxed in re- sponse to the redistribution of baryons, by mapping an initial sphere of radiusr i with massM i =M tNFW(< r i) to a final radiusr f with massM f =f clm(Mi)MtNFW(< ri) +M gas(< r f) +M cga(< r f) via rf ri = 1 +a ψ \u0014\u0012 Mi Mf \u0013nψ −1 \u0015 ,(18) where the mass fraction of collisionless matter is fclm(M) = 1− Ωb Ωm +f sga(M),(19) and the satellite galaxy mass fraction isf sga(M) = fstar(M)−f cga(M). We fixτ δ = 0,a ψ = 0.3 and nψ = 2, following standard practices in baryonification literature (Schneider & Teyssier 2015; Schneider et al. 2019; Giri & Schneider 2021). 3.1.3.Galaxy and CMB Weak Gravitational Lensing"},{"citing_arxiv_id":"2604.17162","ref_index":71,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Signatures of Suppressed Matter Clustering revealed by Fast Radio Bursts","primary_cat":"astro-ph.CO","submitted_at":"2026-04-18T22:37:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"FRB dispersion measures directly constrain suppression of the matter power spectrum due to feedback at k ~ 0.1-3 h/Mpc, reduce posterior variance by a factor of ~8 at k~1 h/Mpc, and exclude extreme large-scale feedback scenarios at ~2 sigma.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"The Astronomical Journal165, 58, DOI: https://dx.doi.org/10.3847/1538-3881/aca5fb (2023). 2208. 08515. [70] Bulbul, E. et al. The SRG/eROSITA All-Sky Survey. The first catalog of galaxy clusters and groups in the Western Galactic Hemisphere. Astronomy and Astrophysics685, A106, DOI: https://dx.doi. org/10.1051/0004-6361/202348264 (2024). 2402.08452. [71] Kluge, M. et al. The SRG/eROSITA All-Sky Survey. Optical identification and properties of galaxy clusters and groups in the western galactic hemisphere. Astronomy and Astrophysics688, A210, DOI: https://dx.doi.org/10.1051/0004-6361/202349031 (2024). 2402.08453. [72] Lee, K.-G. et al. Constraining the Cosmic Baryon Distribution with Fast Radio Burst Foreground"}],"limit":50,"offset":0}