{"total":343,"items":[{"citing_arxiv_id":"2605.23844","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Minor Merger, Major Growth: An Overmassive, Highly Accreting Black Hole Powering a Secondary AGN In a Cosmic Noon Minor Merger","primary_cat":"astro-ph.HE","submitted_at":"2026-05-22T16:54:59+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":"2605.23818","ref_index":33,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"An extremely bright slow-rising afterglow from an off-axis jet in GRB 260310A","primary_cat":"astro-ph.HE","submitted_at":"2026-05-22T16:18:43+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Multi-wavelength data on GRB 260310A support an off-axis jet model explaining weak prompt emission and bright delayed afterglow, including reverse-shock signatures and late X-ray rebrightening.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23768","ref_index":218,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"GMRT Survey of Radio Emission from Magnetic Massive Stars -- I: Emission from Single Stars at sub-GHz Frequencies","primary_cat":"astro-ph.SR","submitted_at":"2026-05-22T15:38:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"GMRT sub-GHz survey of 44 magnetic hot stars detects emission in 11 cases and finds scaling of radio luminosity with magnetic field and rotation period consistent with higher-frequency work.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23686","ref_index":190,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The FAST Hundred-Deg$^2$ HI Deep (HD$^2$) Survey: Early Results from the Pilot Survey","primary_cat":"astro-ph.GA","submitted_at":"2026-05-22T14:45:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Pilot FAST HD² survey reports 339 new HI detections in 10 deg² with 0.45 mJy rms, high DESI optical matching rates, and gas fraction relations consistent with ALFALFA, DINGO, and xGASS.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23489","ref_index":10,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A comparison between Galactic magnetic field models and polarized synchrotron emission with C-BASS at 4.76 GHz and S-PASS at 2.3 GHz","primary_cat":"astro-ph.GA","submitted_at":"2026-05-22T10:51:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Comparison of Galactic magnetic field models to polarized synchrotron observations shows good agreement on angles but poor match on intensity, indicating local foreground structures must be incorporated.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"We apply a template-fitting (or correlation) analysis, a well-established method for studying Galactic foregrounds (Kogut et al. 1996; Planck Collaboration et al. 2011; Peel et al. 2012; Planck Collaboration et al. 2016a; Harper et al. 2022). This involves modelling the sky signaldas a linear combination ofN Z templates and adding a noise vectorn: d=Za+n,(10) where each column ofZ(N pix ×N Z) represents the pixel val- ues of a template. In our case, we use the modelled polarized synchrotron emission as the sole template. The coefficient vectorais solved for via least squares as ˆa= \u0010 ZTN−1Z \u0011−1 ZTN−1d,(11) and ˆarepresents the amplitude needed for the model to best match the observed 4.76 GHz polarized synchrotron data."},{"citing_arxiv_id":"2605.23469","ref_index":47,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"TOI-7154b: A Close-in Massive Brown Dwarf in an Eccentric Orbit","primary_cat":"astro-ph.EP","submitted_at":"2026-05-22T10:27:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"TOI-7154b is a 71.7 M_J brown dwarf in an 8.86-day eccentric orbit around a G star, with eccentricity and age suggesting stellar-like fragmentation origins.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23457","ref_index":174,"ref_count":4,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cosmic web stripping and starvation of low-mass filament galaxies in TNG50","primary_cat":"astro-ph.GA","submitted_at":"2026-05-22T10:16:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Low-mass filament galaxies in TNG50 exhibit smaller asymmetric cold gas discs due to cosmic web tidal fields causing altered accretion or starvation and late-time stripping, while integrated stellar and halo properties remain similar to field counterparts after mass and environment controls.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23452","ref_index":45,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Insights from Analytical Theory of Eccentric Circumbinary Disks II. Forced Modes and Resonance for Precessing Binaries","primary_cat":"astro-ph.GA","submitted_at":"2026-05-22T10:07:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Semi-analytical theory derives radial scalings for forced disk eccentricity (E ~ r^{-1} or r^{-2}) and resonance criteria for precessing binaries, plus a conjecture that cavity size tunes the ground eccentric mode to the binary precession frequency.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23018","ref_index":74,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Gaia Exoplanet Orbits, Demographics, and Evolution Survey (GEODES): Characteristics of Three Long-Period Companions Accelerating their Host Stars","primary_cat":"astro-ph.EP","submitted_at":"2026-05-21T20:41:14+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Three accelerating stars yield one stellar companion at 166 AU, one 45 Jupiter-mass object at ~18 AU, and one 9.5 Jupiter-mass object at 6.4 AU that is 65% likely to be a planet.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23006","ref_index":41,"ref_count":3,"confidence":0.9,"is_internal_anchor":false,"paper_title":"\\texttt{calypso}: a Parameter-Conditioned Stochastic Surrogate Model for Circumbinary Accretion Time-Series","primary_cat":"astro-ph.HE","submitted_at":"2026-05-21T20:25:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Calypso is a parameter-conditioned stochastic surrogate model for circumbinary accretion flows using PCA and multivariate Gaussian modeling, released as open-source software with a closed-form likelihood for parameter inference from time series.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"This work is based on a suite of hydrodynamic simulations of circumbinary accretion disks described in Siwek et al. (2023a,b), as well as new simulations to fill in the param- eter space, run with the same methods. We refer the reader to these papers for an in-depth description of the simulation setup, but briefly summarize the key points here. The simu- lations were performed using theArepocode (Springel 2010; Pakmor et al. 2016) in its Navier-Stokes version (Mu˜ noz et al. 2013). The simulations include a central binary represented by two sink particles, which move on fixed Keplerian orbits with eccentricitye b and mass ratioq b. The sink particles ac- crete gas from the surrounding disk, and the accretion rates onto each sink are recorded on-the-fly."},{"citing_arxiv_id":"2605.22918","ref_index":186,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Strong X-ray Variability of I Zwicky 1: Obscuration from Clumpy Accretion-Disk Winds","primary_cat":"astro-ph.HE","submitted_at":"2026-05-21T18:00:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Variable column density and covering factor of three ionized absorbers in clumpy disk winds explain the X-ray variability in I Zw 1 with stable corona.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22754","ref_index":4,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Mass Segregation in the CMZoom Survey","primary_cat":"astro-ph.GA","submitted_at":"2026-05-21T17:22:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"MST analysis of CMZoom data finds mass segregation in 5 of 17 CMZ clouds, inverse segregation or none in the rest, and no clear link to evolutionary stage or star-formation activity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22630","ref_index":41,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Towards precision cosmology with Void x CMB correlations (II): Impact of mock catalogs on the Void x CMB lensing signal","primary_cat":"astro-ph.CO","submitted_at":"2026-05-21T15:38:42+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Void x CMB lensing from Roman mocks is robust to catalog construction choices and forecasts S/N of 13-31 sigma with Planck, SO, and CMB-S4-like data for 2D and 3D voids.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22545","ref_index":49,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Configuration of the $\\xi$ Tau system constrained by multi-technique observations","primary_cat":"astro-ph.SR","submitted_at":"2026-05-21T14:28:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Multi-technique observations constrain the configuration of the ξ Tau system, detecting orbital oscillations on multiple timescales and suggesting component C is itself a binary.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22388","ref_index":45,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A Weak Fe K$\\beta$ Emission Line in the Broad-Line Radio Galaxy 3C 111 Observed with XRISM: An Ionized Wind Absorption Feature?","primary_cat":"astro-ph.HE","submitted_at":"2026-05-21T12:20:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"XRISM observation of 3C 111 finds weak Fe Kβ possibly caused by blueshifted absorption from an ionized wind at 4600 or 17200 km/s, with kinetic power 10^41-10^44 erg/s smaller than the jet power.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22225","ref_index":73,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Silicate cosmic dust grain collisions in the interstellar medium: A molecular dynamics study","primary_cat":"astro-ph.GA","submitted_at":"2026-05-21T09:28:23+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":"2605.21955","ref_index":19,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"On the Presence of a Tertiary Compact Object in GW190814","primary_cat":"gr-qc","submitted_at":"2026-05-21T03:40:56+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Extended-data Bayesian reanalysis of GW190814 finds no evidence for tertiary-induced line-of-sight acceleration or residual eccentricity due to strong degeneracy between the two effects.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21950","ref_index":57,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Discovery of a Featureless Tidal Disruption Event at z~1 with the Wide Field Survey Telescope","primary_cat":"astro-ph.HE","submitted_at":"2026-05-21T03:30:21+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":"2605.21840","ref_index":31,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Powerful Radio Sources in the Southern Sky. IV. Observations of the G4Jy-3CRE Catalog with the Australian Square Kilometre Array Pathfinder","primary_cat":"astro-ph.GA","submitted_at":"2026-05-21T00:19:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New ASKAP continuum imaging classifies jet morphologies in 173 G4Jy-3CRE sources (66% of sample) including 37 newly detected jets and identifies six new optical counterparts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21735","ref_index":101,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Milky Way Mapper decoded abundances -- II: From patterns to paths","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T20:51:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Reprojects abundances of 199k stars into 4 patterns, identifying enrichment pathways with strong chemo-spatial, age, and vertical correlations plus a transition at ~6 Gyr.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21599","ref_index":20,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"JWST Advanced Deep Extragalactic Survey (JADES) Data Release 5: stellar population catalogue for galaxies in GOODS-N and GOODS-S","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T18:04:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"JADES DR5 delivers a public catalog of Bayesian-inferred stellar masses, SFRs, SFHs, dust, metallicities, and AGN contributions for ~500k galaxies via Prospector with an evolving SFMS prior.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"vated by a broad range of previous studies (e.g., Leja et al. 2017, 2018, 2019, 2020; Tacchella et al. 2022c,b, 2023a; Mathews et al. 2023; Wang et al. 2023, 2024; Duan et al. 2024; Wan et al. 2024; Turner et al. 2025; Harvey et al. 2025b). All parameters and their associated priors are summarised in Table 2. We use a uniform redshift prior over the interval[0.01,20 ]. For galaxy stellar mass, we implement the stellar mass function prior from Wang et al. (2023). This mass function prior is the normalized stellar mass function at each redshift, such that lower-mass galax- ies have higher probability density in the prior, which helps avoid spurious high-mass solutions. Stellar metallicity is linked to stellar mass using the empirical mass-metallicity relation of Gallazzi et al."},{"citing_arxiv_id":"2605.21588","ref_index":23,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Decomposing cool stellar populations with H-band spectral fluctuations: Long-period variable stars in NGC 5128 and carbon stars in NGC 5102","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"PCA of H-band IFU pixel spectra decomposes cool stellar populations in NGC 5128 and NGC 5102, identifying M-giant, long-period variable, and carbon star contributions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21580","ref_index":27,"ref_count":3,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Massquerade: Impacts of Mass Ratio Reversals on Binary Black Hole Merger Rates and Mass Distributions","primary_cat":"astro-ph.HE","submitted_at":"2026-05-20T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Mass ratio reversals produce qualitatively different contributions to BBH merger rates and masses in COMPAS versus SEVN simulations, with core-growth dominating and most systems arising from massive low-metallicity progenitors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21436","ref_index":26,"ref_count":12,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Euclid preparation: Testing multi-field inflation with galaxy power spectrum and bispectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-05-20T17:26:36+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Validates redshift-space power spectrum and bispectrum analysis on Abacus-PNG mocks to recover unbiased f_NL constraints for Euclid spectroscopic sample.","context_count":3,"top_context_role":"background","top_context_polarity":"background","context_text":"M−1(k1)+M −1(k2) i ,(31) whereµ i = ˆki · ˆnis the cosine of the angle of each wave-vector with respect to the LoS direction, withµ 3 satisfying the relation µ3 =−k 1 k−1 3 µ1 −k 2 k−1 3 µ2, andµ 12 = ˆk1 · ˆk2. Therefore, the clustering contribution to the galaxy bispectrum at tree-level is given by Bs clust(k1,k 2,k 3)=Z 1(k1)Z 1(k2)Z 1(k3)B 0(k1,k 2,k 3) + [2Z 1(k1)Z 1(k2)Z 2(k1,k 2)P(k 1)P(k 2) +2 perms.\u0003 ,(32) whereB 0 is the linear matter bispectrum sourced by a given non- zero primordial gravitational potential bispectrumB ϕ, B0(k1,k 2,k 3)=M(k 1)M(k 2)M(k 3)B ϕ(k1,k 2,k 3).(33) For local PNG, we have Bloc ϕ (k1,k 2,k 3)=2f loc NL h Pϕ(k1)P ϕ(k2)+2 perms. i .(34) Retaining all linear-in-f NL terms inZ 1 andZ 2, we have terms up to cubic order inf NL in the bispectrum. Nevertheless, for the fiducial value off NL =30 in our simulations, the higher-order fNL terms are not relevant. The (stochastic) shot noise contribu- tion to the bispectrum is given by Bs shot(k1,k 2,k 3)= 1 ¯n (h (1+˜s1)b 1 +(1+˜s 3)fµ 2 1 i Z1(k1)P(k 1) +2 perms. ) + 1+˜s2 ¯n2 ,(35) where we used ˜si to denote the free amplitudes to distinguish them from shot parameters of the power spectrums i. While the tree-level bispectrum does not strictly require counterterms, phenomenological corrections are often intro- duced to extend the perturbative reach of the model to smaller scales by accounting for the impact of small-scale velocities, known as the Fingers of God (FoG). The work of Ivanov et al. (2022) introduces a FoG counterterm directly in theZ 1 kernel, Z1(k)→Z FoG 1 (k)=Z 1(k)−c FoG 1 µ2 k2 .(36) In contrast, Eggemeier et al. (2025) adopt a non-perturbative modelling of redshift-space distortions via the velocity- difference generator (VDG). A low-kexpansion of the VDG mo- tivates a bispectrum-level counterterm, while leaving the stan- dard kernelZ 1 unchanged, Bs ctr(k1,k 2,k 3) =c B VDG f 2 [kµ]2 123 Bs clust (k1,k 2,k 3) ,(37) Table 1.Summary of simulations used in this work."},{"citing_arxiv_id":"2605.21294","ref_index":32,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Optical Super-orbital Modulation of SMC X-1: Disk Precession and a Revised Pulsar Mass","primary_cat":"astro-ph.HE","submitted_at":"2026-05-20T15:25:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A modified ellipsoidal modulation model with precessing disk irradiation effects revises the SMC X-1 pulsar mass to approximately 1.35 solar masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21101","ref_index":185,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"B-Fields and Star Formation across Scales with TRAO (B-FROST): CO Abundances, Dynamics and Relative Orientations in the Translucent High Latitude Cloud MBM12","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T12:30:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Observational study of MBM12 shows CO-to-H2 conversion factor near galactic average with density-dependent variations, high virial parameters decreasing at small scales, broken power-law mass-size relations indicating external pressure, and magnetic field orientation transition at N(H2) = 4.5e21 cm-","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21062","ref_index":293,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models","primary_cat":"astro-ph.SR","submitted_at":"2026-05-20T11:46:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Population synthesis from binary evolution models predicts periodic neutron star-companion interactions in more than half of surviving hydrogen-poor core-collapse supernovae, with periods peaking at 20-50 days and lasting 0.5-10 years.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20887","ref_index":80,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Difference Between Half-mass Radius and Half-light Radius of Galaxies at 0.2 $< z <$ 2.5 Revealed by JWST/NIRCam Data","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T08:26:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"JWST data shows half-light radii larger than half-mass radii in galaxies at 0.2