{"total":219,"items":[{"citing_arxiv_id":"2606.30438","ref_index":253,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"CARMApy: An Open-Source Python Framework for Simulating Microphysical Clouds in Planetary Atmospheres","primary_cat":"astro-ph.EP","submitted_at":"2026-06-29T15:13:37+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"CARMApy provides a Python interface to the ExoCARMA microphysics code, enabling simulation of cloud particle size distributions and rates in exoplanet atmospheres with claimed consistency to prior versions and speed gains of 1.9x single-threaded and 3.8x multithreaded.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28561","ref_index":213,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"JWST observations of SN 2024abup: First Detection of CO in a broad-lined Type Ic Supernova and Constraints on r-process Nucleosynthesis","primary_cat":"astro-ph.HE","submitted_at":"2026-06-26T19:30:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"JWST spectra of SN 2024abup show CO, C, O, and Mg features plus possible dust emission, with no clear r-process signatures identified via SUMO modeling.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28497","ref_index":45,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Stellar discs and intermediate-mass black holes in galactic nuclei I. Fragmenting the disc in an isotropic stellar potential","primary_cat":"astro-ph.GA","submitted_at":"2026-06-26T18:00:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations demonstrate that a retrograde IMBH with mass ratio ~0.67 to the disc mass fragments a stellar disc into inner, misaligned, and outer components within 10-20 Myr.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28489","ref_index":165,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"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":"background","top_context_polarity":"unclear","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":"2606.28267","ref_index":88,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Early Optical Follow-up of Gamma-Ray Bursts: The Critical Role of Robotic Telescopes","primary_cat":"astro-ph.HE","submitted_at":"2026-06-26T17:00:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A review of early optical GRB features including prompt emission, reverse shocks, and afterglow onset, highlighting robotic telescopes' role in constraining jet Lorentz factors and magnetization.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28159","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Southern Massive Stars at High Angular Resolution (SMaSH+): Properties of hierarchical massive triples","primary_cat":"astro-ph.SR","submitted_at":"2026-06-26T14:55:39+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"SMaSH+ survey data yields the first observationally grounded distributions of key parameters for 26 hierarchical massive triples, dominated by tight inner binaries and wider tertiaries with no strong mass-separation correlations.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"(2013), (3) Stickland & Lloyd (2001), (4) Gomez & Grindlay (2021), (5) Sana & Evans (2011), (6) Pozo Nuñez et al. (2019), (7) Sana et al. (2011), (8) Mayer et al. (2014b),(9) Penny et al. (2001), (10) Sana et al. (2013b), (11) Niemela & Gamen (2005), (12) Mahy et al. (2018), (13) Le Bouquin et al. (2017), (14) Linder et al. (2007), (15) Leitherer et al. (1987), (16) Ibanoglu et al. (2013), (17) Martins (2018), (18) Gies et al. (2002), (19) Sana et al. (2011), (20) Mahy et al. (2022), (21) (Negueruela et al. 2004), (22) Chini et al. (2012), (23) Mayer et al. (2017), (24) Trepl et al. (2012), (25) Mayer et al. (2014a), (26) Stickland et al. (1998), (27) Chini et al. (2012), (28) Walborn (1973), (29) Sana et al. (2009), (30) Nasseri et al. (2014), (31) Sana et al."},{"citing_arxiv_id":"2606.28115","ref_index":32,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A Unified Model for the Emission of Supernova-Associated Fast X-ray Transients: Case Studies of EP240414a, EP250108a, and GRB~171205A","primary_cat":"astro-ph.HE","submitted_at":"2026-06-26T14:16:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A magnetar model unifies emission phases of supernova-associated fast X-ray transients EP240414a, EP250108a, and GRB 171205A via jet, cocoon, wind, and PWN components.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28088","ref_index":1,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A Rare Gamma-ray Flaring episode of the Narrow-Line Seyfert 1 Galaxy 1H 0323+342","primary_cat":"astro-ph.HE","submitted_at":"2026-06-26T13:50:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Multi-wavelength monitoring of a gamma-ray flare in 1H 0323+342 reveals sub-hour variability, jet-corona transition, and ~10^46 erg/s jet power via external Compton modeling of disk and BLR photons.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"fromthesynchrotronemission,whichisexpectedtolieinthe radio band. For example, the observed synchrotron flux can be expressed as (Finke et al., 2008) 𝑓 𝑠𝑦𝑛 𝜖 = √ 3𝛿4𝜖′𝑒3𝐵 4𝜋ℎ𝑑 2 𝐿 ∫ ∞ 1 𝑑𝛾 ′ 𝑁 ′ 𝑒(𝛾 ′)𝑅(𝑥).(2) where𝑥= 4𝜋𝜖 ′𝑚2 𝑒𝑐3 3𝑒𝐵ℎ𝛾 ′2 andprimedquantitiesaremeasuredin the comoving frame. The approximated expression for𝑅(𝑥) is given by 𝑅(𝑥) = { 1.80842𝑥 1∕3 𝑥 ≪1 𝜋 2 𝑒−𝑥 [ 1 − 99 162𝑥 ] 𝑥 ≫1 (3) Here,𝑚 𝑒 and𝑒are the electron mass and charge, re- spectively, while𝜖and𝜖 ′ are the photon energies in the observed and in the co-moving frame. Since there are no radioobservationsavailablequasi-simultaneoustothe𝛾-ray flare, a reasonable approximation would be to consider the synchrotron emission at the level of the archival radio flux, i."},{"citing_arxiv_id":"2606.28019","ref_index":156,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Simulating megaparsec-scale jets of radio galaxies: Magneto-hydrodynamics of jets reaching 5 Mpc","primary_cat":"astro-ph.GA","submitted_at":"2026-06-26T12:22:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"3D MHD simulations show high-thrust, magnetically stabilized jets reach 5 Mpc in 15 Myr while weaker jets disrupt at ~3 Mpc over 35 Myr.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27927","ref_index":54,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Large-scale structures of the Universe: physics, phenomenology, statistics","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T10:20:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"Lecture series on the physics, phenomenology, and statistics of large-scale cosmic structure evolution and non-Gaussian predictions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27675","ref_index":43,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"OzSSy1: The Australian Southern Seyfert-1 Spectroscopic Atlas and Catalogue at z < 0.1","primary_cat":"astro-ph.GA","submitted_at":"2026-06-26T03:13:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Presents a public spectroscopic atlas of 887 Southern broad-line AGNs at low redshift, including continuum decompositions and emission-line fits.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27419","ref_index":65,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Revisiting the picture of circumbinary disc truncation","primary_cat":"astro-ph.EP","submitted_at":"2026-06-25T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Cavity truncation in circumbinary discs is set by binary parameters together with instantaneous cavity eccentricity and relative apsidal orientation, yielding a prescription for pericentre radius Rp and semi-major axis acav.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27195","ref_index":115,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"HALO II: Constraining Hubble constant $H_{0}$ through continuum delay fitting of Fairall 9","primary_cat":"astro-ph.GA","submitted_at":"2026-06-25T15:55:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Using simultaneous modeling of continuum lag-spectrum and broadband SED of Fairall 9 with the H0RIZON-AGN model, the authors obtain H0 = 72.4_{-3.7}^{+3.4} km s^{-1} Mpc^{-1}.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26961","ref_index":34,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Broad-band Spectral Modeling of Large-Scale X-ray Jets in High-Redshift Quasars: An MHD-Informed Approach","primary_cat":"astro-ph.HE","submitted_at":"2026-06-25T12:35:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"An MHD-informed model with self-consistent radial profiles applied to ten z >= 2.5 quasar jets yields higher jet powers than one-zone models, favors electron distributions tied to gas pressure, and finds low magnetization with no clear redshift trend in Lorentz factor.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26827","ref_index":237,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Probing outflow physics through CH$_3$CN and CH$_3$OH chemistry","primary_cat":"astro-ph.GA","submitted_at":"2026-06-25T10:06:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The CH₃OH/CH₃CN ratio in the S68N outflow is constant at ~100-200 and matches gas-phase astrochemical models only when cosmic-ray ionization rates are raised to ~10^{-14} s^{-1}.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26462","ref_index":27,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Nautilus: Fast Time-Resolved Spectroscopy of GKM Stellar Flares and Their Implications for Planetary Habitability","primary_cat":"astro-ph.SR","submitted_at":"2026-06-24T23:44:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Proposes the Nautilus observatory concept for time-resolved flare spectroscopy on GKM stars to create empirical spectral templates for improved planetary habitability simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25814","ref_index":224,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Compact radio galaxies: the case of FR0s","primary_cat":"astro-ph.GA","submitted_at":"2026-06-24T13:30:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"FR0 radio galaxies are abundant compact sources whose small sizes challenge standard evolutionary models, and SKA observations are expected to clarify their jet physics and demographics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25746","ref_index":38,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Exploring the physics of ram pressure stripping with radio continuum observations in the SKA era","primary_cat":"astro-ph.GA","submitted_at":"2026-06-24T12:15:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Perspective on using SKA-Low and SKA-Mid radio continuum to extend ram pressure stripping studies to southern clusters and z~0.5.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25648","ref_index":30,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Long-term Orbital Period Variations of the Eclipsing Dwarf Nova HT Cas","primary_cat":"astro-ph.SR","submitted_at":"2026-06-24T09:57:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"MCMC modeling of the O-C diagram for HT Cas indicates two circumbinary companions causing the long-term period variations, yielding a negative quadratic term consistent with standard CV evolution below the period gap.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25158","ref_index":208,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Early phases of star formation with SKAO: synchrotron emission from dense starless cores in molecular clouds","primary_cat":"astro-ph.GA","submitted_at":"2026-06-23T20:45:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"SKAO will enable detection of synchrotron emission from prestellar cores to probe their magnetic field properties in nearby star-forming regions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25081","ref_index":284,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cosmology from Clustering of Continuum Galaxies","primary_cat":"astro-ph.CO","submitted_at":"2026-06-23T18:41:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Forecasts angular clustering for a 20,000 sq deg SKAO radio continuum survey reaching O(300-400 million) sources and discusses needed corrections for telescope systematics and population modeling.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25070","ref_index":7,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A Look at Eight Outbursts of Comet 7P/Pons-Winnecke","primary_cat":"astro-ph.EP","submitted_at":"2026-06-23T18:24:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Analysis of eight 2021 outbursts on comet 7P/Pons-Winnecke using ground-based photometry yields ejecta masses of 10^5-10^6 kg and normalized rates comparable to several other comets but discrepant with 67P spacecraft data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25043","ref_index":113,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Evolution of AGN Across Cosmic Epochs with the SKAO","primary_cat":"astro-ph.GA","submitted_at":"2026-06-23T18:01:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Simulated SKA-Mid surveys reach radio-AGN completeness at L_1.4GHz ~ 10^23 W Hz^-1 up to z~6.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24846","ref_index":120,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Using SKAO to Understand the Clustering of Gravitational Wave Sources","primary_cat":"astro-ph.CO","submitted_at":"2026-06-23T17:25:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Forecasts show SKA-Mid cross-correlations with ET/CE gravitational wave events can constrain GW source bias and time-delay distributions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24992","ref_index":56,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Synergies Between Pulsar Timing Array and Astrometry","primary_cat":"astro-ph.IM","submitted_at":"2026-06-23T15:33:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Joint SKA PTA and astrometry analysis improves gravitational wave background detection sensitivity by 10-50%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24383","ref_index":36,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Evaluating the Sensitivity of the Age Inferences of Red Giant Stars to Machine Learning Methodology","primary_cat":"astro-ph.SR","submitted_at":"2026-06-23T10:15:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Ages inferred for red giant stars via machine learning are generally insensitive to hyperparameters and architecture but somewhat sensitive to training set choice, especially for the oldest, coolest, and lowest-metallicity stars.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"at various metallicities, color-coded by age. In each of these metallicity bins, we see a coherent pattern, with ages of the first ascent red giant branch correlating with temperature in the expected way. The core-helium-burning stars follow a different pattern as predicted, with the youngest core-helium- burning stars near solar metallicity populating the secondary clump (L. Girardi 1999), and older core helium burning stars at lower gravity. These patterns are extremely consistent with theoretical expectations (M. H. Pinsonneault et al. 2026) and well-vetted datasets (M. H. Pinsonneault et al. 2025), adding additional confidence in our inferred ages. In Figure 15, we show the chemical makeup of the galaxy at different times. At the oldest ages (Age>8 Gyr, see lower"},{"citing_arxiv_id":"2606.24159","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A First Measurement of Circumgalactic Dust Reddening from Only 4.6 deg$^2$ of the Rubin Observatory's DP1","primary_cat":"astro-ph.GA","submitted_at":"2026-06-23T05:27:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The first circumgalactic dust reddening measurement from Rubin DP1 data finds A_V proportional to r_perp to the -1.8 power within 120 kpc, consistent with prior SDSS/KiDS/DES results despite 1000x smaller area and fainter foreground sample.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24032","ref_index":3,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The MASSIVE SURVEY XXI: Local Variations in the Stellar Initial Mass Function of MASSIVE Early-Type Galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-23T00:14:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"In 37 massive ETGs, the IMF becomes less bottom-heavy with radius, with average α_IMF falling from 2.16 to 1.74 and IMF gradients dominating M/L variations over stellar population effects.","context_count":1,"top_context_role":"other","top_context_polarity":"unclear","context_text":"07 withinR e/2 and 1.53+0.09 −0.08 withinR e for the lin- ear-radius fit, and 1.71+0.11 −0.10 withinR e/2 and 1.62+0.09 −0.09 within Re for the log-radius fit. The intensity profile follows I(R) =I e exp \" −bn \u0012 R Re \u00131/n −1 !# (2) andb 4 = 7.669 (L. Ciotti 1991). The stellar mass in the given aperture is calculated as M(r) = Z Raperture 0 2πI(r)(M/L)(r)r dr(3) The resulting enclosed mass-ratio profile is shown in Fig- ure 9, indicating how much the stellar mass within a spe- cific aperture will change with the IMF derived from the fiducial sample. The thin lines represent 500 realizations based on the measurement uncertainties of the slope and intercept ofM/L. Within half an effective radius, the factor is 1."},{"citing_arxiv_id":"2606.23904","ref_index":125,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Deep Newtonian Afterglows: Theoretical Light Curves for Quasi-spherical Outflows","primary_cat":"astro-ph.HE","submitted_at":"2026-06-22T20:05:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"An analytical model for multiwavelength synchrotron emission from decelerated quasi-spherical ejecta with energy injection in stratified environments is developed for the deep Newtonian regime of GRB afterglows.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23790","ref_index":1,"ref_count":4,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Anisotropic quenching beyond $z=1$ and its implications for preprocessing around high-redshift galaxy clusters","primary_cat":"astro-ph.GA","submitted_at":"2026-06-22T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Anisotropic quenching is detected at the highest redshift yet and linked to preprocessing dominating over intrahalo effects by ~20% along the major axis in a delay-then-rapid quenching model informed by cluster accretion histories.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"are measured using theFASTcode (Kriek et al. 2015) with the stel- lar population synthesis model of Bruzual & Charlot (2003). See van der Burg et al. (2020) for the details. Publications of the Astronomical Society of Japan(0000), Vol. 00, No. 03 Table 1.Cluster properties used in this study Name Redshiftσ vel R200 M200 Ks,lim a log(M∗,lim)b Nall Nq [kms −1] [Mpc] [10 14 M⊙] [mag] [M ⊙] SPT0205 1.320678±57 0.79±0.12 2.22 +0.89 −0.70 23.25 9.90 55 37 SPT0546 1.067977±68 1.17±0.09 6.11 +1.52 −1.30 23.47 9.64 144 88 SPT2106 1.1321055±83 1.23±0.10 7.65 +2.02 −1.72 23.19 9.79 160 106 SpARCS0035 1.335840±52 0.93±0.07 4.14 +1.00 −0.87 23.81 9.70 99 41 SpARCS0219 1.325810±77 0.79±0.12 2.51 +1.33 −0.98 23.27 9."},{"citing_arxiv_id":"2606.23649","ref_index":1,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The EDGE-CALIFA Survey: Star Formation Efficiency and Galaxy Quenching across 62 Main Sequence, Green Valley, and Red Galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-22T17:36:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New CO survey of 62 CALIFA galaxies shows median molecular gas depletion times rising from 2.1 Gyr on the main sequence to 128 Gyr in red galaxies, with SFE declining systematically below the SFMS independent of CO-to-H2 conversion factor choice.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23106","ref_index":19,"ref_count":3,"confidence":0.9,"is_internal_anchor":false,"paper_title":"RAD@home discovery of a bow-and-arrow radio galaxy tracing a ~560 kpc bow-shock structure in a multi-halo environment","primary_cat":"astro-ph.GA","submitted_at":"2026-06-22T09:50:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Citizen science discovery of a bow-and-arrow radio galaxy with ~560 kpc bow-shock-like structure in a multi-halo environment at z=0.159.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.22559","ref_index":28,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Migration Traps as Variability Attractors: Optical/UV Signatures of Embedded Stellar-Mass Black Holes in Active Galactic Nucleus Disks","primary_cat":"astro-ph.GA","submitted_at":"2026-06-21T15:33:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Migration traps concentrate stellar-mass black holes in AGN disks, generating self-regulated magnetic reconnection heating that yields excess short-timescale optical/UV variability, flattened structure functions, and deviations from the τ∝λ^{4/3} lag relation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.22432","ref_index":73,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Tracing Large-scale Structure with the MeerKLASS On-the-Fly Survey: Angular Clustering of Radio Sources at 816 MHz","primary_cat":"astro-ph.CO","submitted_at":"2026-06-21T10:45:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"First measurement of angular clustering w(theta) for radio sources at 816 MHz over 800 deg2 yields positive signal and effective bias 1.53-2.0 depending on N(z) prior.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21827","ref_index":26,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Do Prompt Gamma-ray Burst Fireball Composition Impact on Afterglow Emission? Cases Study for Long GRBs 080916C/090902B and Short GRBs 090510/130603B","primary_cat":"astro-ph.HE","submitted_at":"2026-06-20T01:32:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Case study of four GRBs finds afterglow light curves shaped by ambient density, not prompt fireball composition, with cascade pairs affecting only long GRB early optical emission.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21656","ref_index":21,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The $M$-$\\sigma$ Relation Has to Break","primary_cat":"astro-ph.GA","submitted_at":"2026-06-19T18:01:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Capture-driven growth model predicts M ≈ 10^5 M_⊙ × (σ/50 km s^{-1})^{2.5}, requiring the M-σ relation to flatten to 2.26 < β < 2.5 below 10^5 M_⊙.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21105","ref_index":79,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Little Red Dots as Supermassive Analogs of SS 433","primary_cat":"astro-ph.HE","submitted_at":"2026-06-19T05:15:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"UNKNOWN","novelty_score":6.0,"formal_verification":"none","one_line_summary":"LRDs are interpreted as high-inclination hyper-Eddington accreting SMBHs analogous to SS 433, with V-shaped SEDs, X-ray weakness, and Balmer breaks emerging from disk self-shielding geometry.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20810","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Investigating the Spectral Properties of Dual Nuclei in Galaxy Mergers from the GOTHIC survey: Supermassive Black Hole Growth, metal enrichment and Dual AGN","primary_cat":"astro-ph.GA","submitted_at":"2026-06-18T18:01:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Spectroscopic analysis of dual nuclei shows SMBH masses higher in galaxy mergers than single nuclei at fixed stellar mass.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20800","ref_index":75,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"No hidden monsters: Probing recently-quenched galaxies for obscured AGN with JWST-PRIMER MIRI and NIRCam","primary_cat":"astro-ph.GA","submitted_at":"2026-06-18T18:00:05+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"JWST MIRI observations of post-starburst galaxies find no mid-IR excess in high-mass systems, constraining hidden AGN to Eddington ratios below 1 percent, with low-mass systems showing residual star formation instead.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20265","ref_index":116,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"UCLCHEM 4.0: An open source gas-grain astrochemistry simulation framework","primary_cat":"astro-ph.GA","submitted_at":"2026-06-18T14:13:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"UCLCHEM 4.0 is an updated open-source framework that solves time-dependent gas-grain chemical networks with built-in parametrizations for cloud collapse, cores, and shocks.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19862","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Multi-band Structural Analysis of KiDS-selected Low Surface Brightness Galaxies with Hyper Suprime-Cam Imaging","primary_cat":"astro-ph.GA","submitted_at":"2026-06-18T07:16:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"KiDS-selected LSBG candidates are confirmed as genuine low surface brightness galaxies, predominantly red with median B-band central surface brightness 24.55 mag arcsec^{-2} and Sersic index distributions peaking near 0.7 across bands.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19463","ref_index":235,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"On the later evolution of observationally selected protocluster candidates at $z\\,{\\gtrsim}\\,5$","primary_cat":"astro-ph.GA","submitted_at":"2026-06-17T18:01:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations show observationally selected protocluster candidates at z ≳ 5 include significant interlopers, undergo 2-6 major mergers, and exhibit stronger clustering than observed, requiring total galaxy mass within 10 cMpc for reliable progenitor identification.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19104","ref_index":89,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"PHANTOM: A MATLAB and Octave Toolbox Connecting Linear Field Statistics to Dark Matter Halo Observables","primary_cat":"astro-ph.CO","submitted_at":"2026-06-17T14:17:18+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"PHANTOM is a public MATLAB/Octave toolbox for linear field statistics and halo observables in dark matter cosmology, validated to sub-percent agreement with Python packages colossus, hmf, and halomod.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18352","ref_index":32,"ref_count":2,"confidence":0.9,"is_internal_anchor":false,"paper_title":"TNG SAM: Bridging Hydrodynamical Complexity and Semi-Analytic Efficiency to Model Galaxy Formation","primary_cat":"astro-ph.GA","submitted_at":"2026-06-16T18:00:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The TNG SAM reproduces TNG hydro simulation gas and metal flows plus galaxy and halo properties within 30% accuracy out to z=6 via five targeted updates to the Santa Cruz SAM calibrated on stellar feedback-dominated galaxies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17270","ref_index":110,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Dust in the Average Galaxy: Attenuation, Emission, and Opacity from 0<z<7","primary_cat":"astro-ph.GA","submitted_at":"2026-06-15T20:29:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"UV/optical attenuation underpredicts IR luminosity by 3-10x across 0<z<7 while κ_UV/κ_FIR falls by over an order of magnitude, pointing to evolving dust grain properties in average galaxies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17189","ref_index":1,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Exploring the Relationship Between Bars, Star Formation Activity, and Host Galaxy Properties from $\\mathbf{z \\sim 0}$ to $\\mathbf{z \\sim 2}$","primary_cat":"astro-ph.GA","submitted_at":"2026-06-15T18:27:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Barred galaxies transition from actively star-forming at z~1-2 to quiescent at z~0, with the fraction of quiescent galaxies hosting bars increasing steeply over cosmic time.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"The following steps are adopted to calculate the quies- cent bar fraction. First, quiescent galaxies are identified using both the sSFR selection method and the main se- quence selection method (Section 3.4). Among these quiescent galaxies, the bar fractionF Q bar is calculated from a sample of moderately inclined disk galaxies using the equation below: fbar = Nbar Ndisk (1) whereN bar is the number of barred galaxies identified in a sample of moderately inclined disks (in this case quiescent moderately inclined disks) with total sample sizeN disk. For CEERS, Sections 3.1 to 3.3 outline how mod- erately inclined disks and bars are identified from the study by Y. Guo et al. (2025). Y. Guo et al. (2025) identified bars in CEERS using visual classification and"},{"citing_arxiv_id":"2606.17153","ref_index":175,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Chemical hints of Population III stars from silicon abundances in massive galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-15T18:00:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"High [Si/Mg] = 0.67 in NGC 1277 cannot be explained by standard models and suggests pair-instability supernovae from very massive early stars.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17142","ref_index":61,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Hawai`i Supernova Flows: Bulk Flow Measurements using SNe Ia in the Optical and NIR","primary_cat":"astro-ph.CO","submitted_at":"2026-06-15T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Bulk flow measurements from Hawai`i Supernova Flows SNe Ia yield speeds of 100-400 km/s consistent with ΛCDM expectations at z ≲ 0.1.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.13538","ref_index":107,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A local Universe catalogue of structures and voids dynamically identified using Cosmic-Flows4++ZOA peculiar velocities","primary_cat":"astro-ph.CO","submitted_at":"2026-06-11T16:23:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A catalogue of 37 voids (radii 13-38 h^{-1} Mpc) and 42 knots (volumes 10^4 to 3.3x10^5 h^{-3} Mpc^3) is presented using V-web on CF4++ZOA peculiar velocities within z=0.1.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.13359","ref_index":45,"ref_count":1,"confidence":0.9,"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}],"limit":50,"offset":0}