{"total":39,"items":[{"citing_arxiv_id":"2605.16924","ref_index":83,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Magnetised CGM Gas at z~1 revealed by SPICE-RACS","primary_cat":"astro-ph.GA","submitted_at":"2026-05-16T10:30:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A 4.5σ excess RM dispersion of 4.13 ± 0.91 rad m^{-2} is found in 191 Mg II sightlines versus controls, implying model-dependent CGM magnetic fields of 0.4-0.8 μG at projected radii 20-150 kpc and z~1.14.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16485","ref_index":51,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Halo-driven Origin and Suppression of Over-massive Black Holes and Little Red Dots","primary_cat":"astro-ph.GA","submitted_at":"2026-05-15T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Halo-driven transient rapid growth followed by thermodynamic suppression explains over-massive black holes and Little Red Dots as precursors to standard SMBH-galaxy coevolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16200","ref_index":285,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"No Stream Left Unscathed: The imprint of a host galaxy","primary_cat":"astro-ph.GA","submitted_at":"2026-05-15T17:13:55+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Host galaxy potentials alone produce complex morphological features in most stellar streams, with pericentric distance as the strongest predictor of smoothness.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16132","ref_index":89,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Nucleosynthesis in the fast ejecta of a neutron star merger","primary_cat":"astro-ph.HE","submitted_at":"2026-05-15T16:15:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20227","ref_index":48,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Cosmological perturbations with $f(R)$ gravity scalarons : Galaxy power spectra and the scalaron mass","primary_cat":"astro-ph.CO","submitted_at":"2026-05-15T08:22:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"In a viable f(R) model transitioning from early GR-like to late non-GR behavior, matter power spectra show higher monopole and quadrupole power at small scales with quadrupole elevated at large scales up to k~0.02, while scalaron mass decreases over time to GR limits on galactic scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13843","ref_index":45,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Galaxy Luminosity Functions in ASTRID: Predictions for LSST","primary_cat":"astro-ph.GA","submitted_at":"2026-05-13T17:59:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"ASTRID simulation with dust model calibrated to SDSS at z=0 produces validated luminosity functions and LSST-ready mock catalogs of 378 million galaxies with predicted number counts in ugrizy bands from z=0 to 2.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11083","ref_index":17,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"FLAMINGO: The thermal history of the Universe from tSZ effect cross-correlations and its dependencies on cosmology and baryon physics","primary_cat":"astro-ph.CO","submitted_at":"2026-05-11T18:00:10+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"tSZ cross-correlations with large-scale structure tracers prefer low S8 and strong baryonic feedback, yielding S8 = 0.72 and low group baryon fraction in FLAMINGO simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11070","ref_index":227,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A correlation predicting galaxies without dark matter","primary_cat":"astro-ph.GA","submitted_at":"2026-05-11T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Baryonic fraction in certain galaxies correlates with baryonic acceleration as approximately a_bar inverse, placing known dark-matter-deficient galaxies at the high-acceleration extreme and predicting low dark matter content for ultra-diffuse galaxies brighter than 25 mag arcsec^{-2}.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.08353","ref_index":269,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Empirical estimates of how massive galaxies can be in {\\Lambda}CDM","primary_cat":"astro-ph.GA","submitted_at":"2026-05-08T18:05:26+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Corrected empirical limits show the most massive galaxies never exceed the theoretical baryonic maximum of 0.16 times halo virial mass, keeping observations consistent with LambdaCDM at all redshifts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.06799","ref_index":250,"ref_count":2,"confidence":0.88,"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":"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"},{"citing_arxiv_id":"2602.10192","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Forged by Feedback: Stellar Properties of Brightest Group Galaxies in Cosmological Simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-02-10T19:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The OBSIDIAN simulation with its three-regime AGN feedback best reproduces the observed stellar masses, star formation rates, and ages of brightest group galaxies, unlike the other simulations which show mismatches in quenching behavior.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"lusIGrM density criterion to theSimba-based simu- lations and find no significant difference in the result- ing IGrM X-ray luminosities compared to those com- puted using the conventionaln H <0.13 cm −3 thresh- old. We additionally find that within each simulation, the calculated group X-ray luminosities are insensitive to the choice of temperature threshold within the range T∈[2×10 5,10 6] K. Given this robustness, we adopt the conventional density criterion for theSimba-based simulations for consistency with the broader literature, while retaining theρ <500ρ crit definition forRomulus, and use a temperature threshold ofT >5×10 5 K for all simulations. The particle X-ray luminosities are calculated by XI- GrM13 using X-ray spectra generated by PyAtomDB"},{"citing_arxiv_id":"2511.17310","ref_index":50,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Search for new physics in the final state with a single photon and large missing transverse momentum in proton-proton collisions at $\\sqrt{s}$ = 13 TeV","primary_cat":"hep-ex","submitted_at":"2025-11-21T15:25:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Combined LHC data shows no deviation from the standard model in single-photon plus missing momentum events, establishing the strongest limits to date on simplified dark matter models and large extra dimensions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.07174","ref_index":71,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Archival Inference for Eccentric Stellar-Mass Binary Black Holes in Space-Based Gravitational Wave Observations","primary_cat":"astro-ph.HE","submitted_at":"2025-10-08T16:15:55+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Ground-triggered Bayesian analysis enables detection and tight constraints on eccentricity and chirp mass for a GW190521-like eccentric binary black hole in one year of LISA or TianQin data at SNR ~7.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.13220","ref_index":50,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dynamic or Systematic? Bayesian model selection between dark energy and supernova biases","primary_cat":"astro-ph.CO","submitted_at":"2025-09-16T16:27:46+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A magnitude offset between low- and high-redshift supernovae beats the Bayesian evidence for flexknot dark energy and reduces DES-5Y/DESI tension.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.07453","ref_index":57,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Cross-correlations between the CLAMATO Lyman-alpha forest and galaxies within the COSMOS field","primary_cat":"astro-ph.CO","submitted_at":"2025-09-09T07:25:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Cross-correlation of CLAMATO Lyman-alpha forest with COSMOS galaxies yields stellar-mass-dependent biases of approximately 2.1, 3.2, and 3.8, corresponding to halo masses of log M_h ~ 10.5, 11.7, and 12.1 from Bolshoi-Planck mocks, with hints of enhanced low-mass star formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.16115","ref_index":92,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Simba Simulation: The Effect of Feedback Physics on Matter Distribution in the Cosmic Web","primary_cat":"astro-ph.CO","submitted_at":"2025-07-22T00:07:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simba simulations find that IGM gas fractions in cosmic web structures vary by only a few percent across feedback variants, while jet feedback noticeably enhances diffuse gas on the outskirts of filaments and knots.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2408.02723","ref_index":113,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Cosmological Simulations of Stellar Halos with Gaia Sausage-Enceladus Analogues: Two Sausages, One Bun?","primary_cat":"astro-ph.GA","submitted_at":"2024-08-05T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"TNG50 simulations of 98 Milky Way analogues find GSE-like debris in 32 cases, with two-merger GSEs in one third; single- and two-merger cases differ in median infall time (5.9 vs 10.7 Gyr ago), abundances, and star-formation histories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2304.05203","ref_index":129,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Parameters","primary_cat":"astro-ph.CO","submitted_at":"2023-04-11T13:13:14+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"ACT DR6 CMB lensing map gives σ8 = 0.819 ± 0.015 and H0 = 68.3 ± 1.1 km/s/Mpc, consistent with Planck ΛCDM but 1.7-2.1σ higher in S8 than KiDS, DES, and HSC galaxy surveys.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2206.14220","ref_index":66,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package","primary_cat":"astro-ph.IM","submitted_at":"2022-06-28T18:01:54+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The paper reports on the Astropy v5.0 release, project updates, ecosystem connections, and challenges facing the community-oriented open-source astronomy software effort.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2006.12611","ref_index":32,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"GW190814: Gravitational Waves from the Coalescence of a 23 M$_\\odot$ Black Hole with a 2.6 M$_\\odot$ Compact Object","primary_cat":"astro-ph.HE","submitted_at":"2020-06-22T20:56:34+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Detection of GW190814 from the coalescence of a 23 solar-mass black hole and a 2.6 solar-mass compact object, the most unequal-mass binary yet observed with gravitational waves.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1906.08174","ref_index":41,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Optical follow-up study of 32 high-redshift galaxy cluster candidates from Planck with the William Herschel Telescope","primary_cat":"astro-ph.GA","submitted_at":"2019-06-19T15:47:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Optical follow-up of 32 Planck SZ candidates yields photometric redshifts and richness estimates confirming 18 (7) as at least half as rich as expected at z>0.5 (z>0.8), highlighting Eddington bias and projection effects.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1807.06211","ref_index":43,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Planck 2018 results. X. Constraints on inflation","primary_cat":"astro-ph.CO","submitted_at":"2018-07-17T04:05:09+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Updated Planck CMB measurements give ns = 0.9649 ± 0.0042, r < 0.056, confirm flatness at 0.4 percent, and show no evidence for scale-dependent features or non-slow-roll dynamics in the inflaton potential.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"\"curvaton II\" Planck 2015 TT+lowP+lensing 1 0 .5 0 .5 0 .5 −100 [ −4.40 :−0.40] −0.6 \"curvaton II\" Planck TT+lowE+lensing 1 0 .5 0 .5 0 .5 −100 [ −4.40 :−0.35] −0.4 −7.2 \"curvaton II\" Planck TT,TE,EE+lowE+lensing 1 0 .1 0 .1 0 .1 −100 [ −2.04 :−0.13] 0 −9.2 Special CDI cases (two isocurvature parameters): Uncorrelated, nII free \"axion II\" Planck TT+lowE+lensing 2 2 .3 [3 : 43] [6 : 75] 0 [0 .03 : 1.24] −0.5 −6.7 \"axion II\" Planck TT,TE,EE+lowE+lensing 2 1 .1 [5 : 38] [10 : 77] 0 [0 .07 : 0.66] −2.8 −6.3 Arbitrarily correlated, nII = nRR \"curvaton III\" Planck TT+lowE+lensing 2 4 .7 4 .7 4 .7 [ −75 : 28] [ −3.38 : 1.99] −0.4 −10.0 \"curvaton III\" Planck TT,TE,EE+lowE+lensing 2 3 .9 3 .9 3 .9 [ −41 : 31] [ −1.30 : 2.10] 0 −10."}],"limit":50,"offset":0}