{"total":62,"items":[{"citing_arxiv_id":"2607.00827","ref_index":38,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Cosmology from HI galaxy surveys with the SKA","primary_cat":"astro-ph.CO","submitted_at":"2026-07-01T11:49:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Predictions of HI galaxy number counts versus redshift and cosmological forecasts for SKAO-MID surveys, bracketed by multiple HI mass function models due to redshift uncertainty.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.00764","ref_index":183,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The age of the Universe from a large sample of the oldest Galactic 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geometry.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28506","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Twin Peaks: Resolving Features in the Binary Black Hole Mass Function with COSMIC-METISSE","primary_cat":"astro-ph.HE","submitted_at":"2026-06-26T18:02:39+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New MESA stellar tracks with varied winds and convective mixing produce a primary black hole mass function with twin peaks near 8 and 13 solar masses in most variations, the higher peak dominated by mass-ratio-reversal systems, with rates varying by a factor of six.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27182","ref_index":37,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Forward-modelling the Tolman and distance-duality tests with IllustrisTNG","primary_cat":"astro-ph.CO","submitted_at":"2026-06-25T15:47:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"IllustrisTNG yields γ=2.23±0.20 for luminosity density evolution that explains the Tolman and distance-duality test signals in standard cosmology.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26320","ref_index":224,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Probing the molecular gas content of galaxies in an over-dense group at z~0.7: a test case for environmental 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observations of 634 galaxies at 0.2<z<2 yield IR luminosity functions with faint-end slope α≈0.147, implying lower dust-obscured SFRD than previous ALMA/Herschel/Spitzer studies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11309","ref_index":264,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dark Energy Survey Year 3 results: optimized $w$CDM simulation-based inference with weak lensing map-level hybrid statistics","primary_cat":"astro-ph.CO","submitted_at":"2026-06-09T18:00:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DES Y3 weak lensing analysis with hybrid map-level statistics and simulation-based inference yields S8 = 0.808 ± 0.017, Ωm = 0.325 ± 0.024, and w < -0.766, improving the figure of merit by 60% over prior state-of-the-art.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09997","ref_index":81,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A universal model for the accretion rates and formation times of dark matter halos","primary_cat":"astro-ph.CO","submitted_at":"2026-06-08T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A six-parameter function of peak height ν, power spectrum slope n_eff, and growth rate α_eff accurately describes median halo mass accretion rates from simulations in ΛCDM and Einstein-de Sitter cosmologies at z=0-14.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09616","ref_index":242,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Blowing star formation away in AGN hosts (BAH) -- V: The 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two-channel model of binary black hole populations with possible mild evidence for an AGN-related third channel.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.27225","ref_index":18,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"GWTC-5.0: Observations from the Second Part of the Fourth LIGO-Virgo-KAGRA Observing Run and Updates to the Gravitational-Wave Transient Catalog","primary_cat":"gr-qc","submitted_at":"2026-05-26T16:09:49+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":8.0,"formal_verification":"none","one_line_summary":"GWTC-5.0 adds 161 new compact binary coalescence candidates from O4b with p_astro >= 0.5, detailed properties for 104, all binary black holes, for a cumulative total of 390.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"10,−2.90] [250, 400] 20.88 GW240629_145256 - L - - 20.88 GW240629_145256 - V - - 20.88 Table 10continued 38 Table 10(continued) Candidate GPS time [s] Detector Time window [s] Frequency range [Hz]f low [Hz] GW240705_053215 1404192753.92 V[0.90,1.10][50, 100] - GW240902_143306 1409322804.76 V [−0.10,0.10] [300, 400] - GW240908_082628 1409819206.41 V[−0.18,0.03][164, 210] - GW240908_082628 - L - - 30 GW240908_125134 1409835112.27 L [0.60,1.20] [20, 30] - GW240919_061559 1410761777.19 H[0.20,0.80][20, 30] - GW240920_124024 1410871242.88 L [0.002,0.30] [20, 35] - GW240921_201835 1410985133.79 L[−4.60,−4.20][10, 30] - GW240922_142106 1411050084.39 H [−0.40,−0.20] [150, 250] - GW240923_204006 - H - - 21.28 GW240923_204006 - L - - 21."},{"citing_arxiv_id":"2605.27224","ref_index":43,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"GWTC-5.0: Methods for Identifying and Characterizing Gravitational-wave 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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":"2605.06766","ref_index":28,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A PINK update: Improvements to the CELEBI fast radio burst data reduction and analysis pipeline","primary_cat":"astro-ph.IM","submitted_at":"2026-05-07T18:00:00+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"The PINK updates enhance the CELEBI FRB pipeline with better astrometry, time-frequency gating, polarization calibration, DM optimization tools, and a software container for improved efficiency and localization of events like FRB 20251019A.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05972","ref_index":56,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A statistical look on kinematic planes of satellite galaxies II: The physics behind their early formation in TNG50 MW/M31-like galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-05-07T10:18:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Early kinematically persistent planes of satellite galaxies are fossil remnants of high-redshift anisotropic mass collapse along the principal directions of the local cosmic web during the fast assembly phase of host halos.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05318","ref_index":15,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"HOLISMOKES XXI: Detecting strongly lensed type Ia supernovae from time series of multi-band LSST-like imaging data -- Part II","primary_cat":"astro-ph.IM","submitted_at":"2026-05-06T18:00:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A convLSTM classifier identifies lensed SNe Ia in simulated LSST-like time series, reaching ~60% true-positive rate at O(10^{-4}) false-positive rate by the seventh epoch even after adding realistic PSF variations and foreground SN contaminants.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04645","ref_index":7,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The MeerKAT Massive Distant Clusters Survey: a search for diffuse radio emission in 30 massive SZ-selected clusters at $z > 1$","primary_cat":"astro-ph.GA","submitted_at":"2026-05-06T08:46:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"MeerKAT observations detect radio halos in 27% of 30 massive clusters at z>1, a rate lower than at intermediate redshifts but above model predictions, with power-mass scaling similar to lower-z samples.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"Ascension of the SZ centre (J2000); (3) Declination of the SZ centre (J2000); (4) cluster redshift; (5) source/type of redshift information, with values drawn from aSouth Pole Telescope (SPT) (Bocquet et al. 2019; Bleem et al. 2020),bzCluster (Hilton et al. 2021),cMassive and Distant Clusters of WISE Survey (MaDCoWS), dACT(Menanteauetal.2013;Sifónetal.2016;Hiltonetal.2018),or eCAMIRA(Ogurietal.2018).Columns(6)and(7)listtheACTSZ-based mass calibrated via weak lensing, and the uncorrected ACT SZ mass, respectively. The latter quantity is not corrected for Eddington bias, enabling direct comparison withPlanckPSZ2 masses. Column (8) and (9) reports the𝑅500c in kpc and the ACT signal-to-noise ratio (SNR), receptively. Column (10) gives the adopted diffuse radio-emission classification: RH = radio halo, U = uncertain/candidate, NDE = no diffuse emission detected, and EX = excluded from the"},{"citing_arxiv_id":"2605.03008","ref_index":206,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Environmental Quenching of High-Redshift Galaxies: Interpreting JWST Observations with Simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-05-04T18:00:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Multiple galaxy formation simulations show that low-mass quenched galaxies at z>3 are predominantly environmentally quenched satellites, often only temporarily so, and match JWST observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.00822","ref_index":65,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"PEARLS: Two Distinct Populations of AGN Hosts Moving Between Star Formation and Quiescence","primary_cat":"astro-ph.GA","submitted_at":"2026-05-01T17:58:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"NIRCam-selected AGN hosts split into a 'bridge' group with moderate-to-low SFRs and a 'branch' group above the SFMS with SFR rising with AGN fraction; both populations show recent transitions between star formation and quiescence.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.28132","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Finding the one: identifying the host of compact binary mergers","primary_cat":"astro-ph.CO","submitted_at":"2026-04-30T17:17:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Restricting analysis to the top 1% most luminous galaxies in GW localization volumes yields 1-4 candidate hosts for three specific events, with 29-36% probability of random association.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"host-galaxy association, such events are extremely rare, with only a single confirmed case to date (Abbott et al. 2017a,b). arXiv:2604.28132v1 [astro-ph.CO] 30 Apr 2026 2 T able 1.The five best-localized events in O3 and O4 and their properties: GraceDB 90% sky area and distance, estimated comoving volume, and number of galaxies to retainN g. 90% Sky area [deg 2] Distance [Mpc] Volume [×10 3 Mpc3]N g S250207bg 19 180±38 18.1 2 GW190814 19 241±26 23.9 2 S250830bp 3.73 427±69 33.0 3 S240925n 14 331±70 76.9 8 S241011k 72 212±37 99.7 10 Recent studies demonstrated that targeting the most luminous galaxies in a catalog can preserve unbiased cos- mological inference, despite discarding the majority of potential hosts (e."},{"citing_arxiv_id":"2604.21405","ref_index":33,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Supermassive Black Hole Winds in X-rays: SUBWAYS IV. Tracing Radio Emission and Unveiling the Role of Winds","primary_cat":"astro-ph.GA","submitted_at":"2026-04-23T08:20:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"In X-ray selected AGN, those hosting ultra-fast outflows exhibit larger radio extensions and steep spectra matching wind-driven shock models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20814","ref_index":162,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Search for Rotation Measure Flare Candidates in Repeating Fast Radio Bursts","primary_cat":"astro-ph.HE","submitted_at":"2026-04-22T17:44:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A search of repeating FRBs identifies RM flare candidates in FRB 20121102A, FRB 20201124A, and FRB 20180916B, suggesting such events may be common and tied to dynamic magneto-ionic environments.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20411","ref_index":208,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Evolution of the SFR-M_* relation at 0.1<z<4: Environmental and Morphological Dependencies","primary_cat":"astro-ph.GA","submitted_at":"2026-04-22T10:29:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The SFR-M_* relation develops a high-mass decline at low redshifts, driven mainly by morphological quenching from internal structure rather than environmental effects on star-forming galaxies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19543","ref_index":48,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dynamically cold discs in high-redshift galaxies: comparison between ALMA observations and TNG50","primary_cat":"astro-ph.GA","submitted_at":"2026-04-21T15:02:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"TNG50 shows most massive high-z star-forming galaxies are dynamically hotter than ALMA data indicate, with rare cold discs forming from aligned accretion and evolving into one-third discs and two-thirds early-type galaxies by z=0.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19449","ref_index":174,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Cosmological constraints from the small scale clustering of Emission Line Galaxies","primary_cat":"astro-ph.CO","submitted_at":"2026-04-21T13:32:04+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"SHAMe-SF modeling of small-scale DESI ELG clustering delivers 6% precision on σ8 and Ωm h², matching full DR1 results with 1% volume.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18730","ref_index":158,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"New constraints on stellar feedback through [O III] emission: interpreting ALMA and JWST observations with SPICE simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-04-20T18:28:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations show that bursty supernova feedback produces fewer bright [OIII] emitters by z=5 than smooth feedback due to less effective metal enrichment, while [OIII] traces shock-heated and radiatively ionized gas.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18731","ref_index":48,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Stellar feedback SPICEs up [C II] emission in the first galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-04-20T18:28:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations find [C II] traces star formation robustly but underestimates outflow speeds and mass-loading factors by factors of 2-5, with feedback type affecting disk settling but not distinguishable from [C II] spatial or spectral properties alone.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.15932","ref_index":41,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Inferring Halo Mass and Scale Radius of Galaxy Clusters Using Convolutional Neural Networks and Uchuu-UniverseMachine Catalogs","primary_cat":"astro-ph.CO","submitted_at":"2026-04-17T10:49:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Convolutional neural networks can infer galaxy cluster virial masses and scale radii from 2D projected position and line-of-sight velocity distributions with nearly unbiased results and reduced scatter when richness is added or training is limited to relaxed systems.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.14327","ref_index":30,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Atacama Cosmology Telescope: A Test of the Gravitational Force Law on Cosmological Scales Using the Kinematic Sunyaev-Zeldovich Effect","primary_cat":"astro-ph.CO","submitted_at":"2026-04-15T18:34:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"kSZ measurements constrain the gravitational acceleration between galaxy halos to follow g ∝ 1/r^{2.1±0.3}, consistent with Newtonian gravity in ΛCDM.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"The best-fit curves for each model are shown in Fig. 1. The ΛCDM velocity curve estimated using our formalism is shown in blue, and the MOND best fit case is shown in orange. The color bands show the 1σuncertainty on the fitted amplitude. The black, segmented line shows the ΛCDM theoretical prediction using Eq. (3) withPlanckcosmological parameters [30], as fitted in Ref. [9] for the full galaxy sample with L >4.3×10 10L⊙. Note that our ΛCDM prediction fits that of previous work well [9]. The posterior for the joint two-parameter fit (con- straining the optical depth ¯τand force law indexn) is shown in Fig. 2, where contours show 1,2,3σintervals. We normalize ¯τby the best-fit ΛCDM as in Ref. [9], ex-"},{"citing_arxiv_id":"2604.04422","ref_index":21,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Information-Geometric Perspective on the Hubble Tension: Eigenmode Rotation and Curvature Suppression in wCDM","primary_cat":"astro-ph.CO","submitted_at":"2026-04-06T04:59:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Extending to wCDM mainly suppresses the leading Planck Fisher eigenvalue to 2.7% of its LambdaCDM value with only modest eigenmode rotation, while late-time data adds curvature that limits tension relief.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"between best-fit parameters or shifts in posterior means expressed in units of the combined variance [5- 8]. A variety of statistical diagnostics have been formulated to assess dataset concordance, including parameter-difference statistics and index-of-inconsistency measures [18, 19], Bayesian evidence ratios for model comparison [20], information-theoretic metrics based on relative entropy [21], and suspiciousness- based measures of dataset tension [22]. While these approaches provide scalar measures of disagreement, they implicitly conflate two distinct ingredients: the parameter displacement and the directional stiffness (likelihood curvature) with which each dataset constrains the corresponding parameter combinations [19, 22]. Therefore, the statistical significance of a shift depends not only on its magnitude, but also on the"}],"limit":50,"offset":0}