{"total":96,"items":[{"citing_arxiv_id":"2605.23599","ref_index":117,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Investigation of the Two-Dimensional Velocity Field of the Large-Scale Coronal Wave from September 6, 2011 using the SOLERwave Tool","primary_cat":"astro-ph.SR","submitted_at":"2026-05-22T13:08:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Analysis of the September 6, 2011 coronal wave with the SOLERwave multi-sector method reveals over 40% speed variation (750-1500 km/s) between northward and northwestward segments, attributed to differences in magnetosonic speed from an MHD solution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.22618","ref_index":13,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"HWO Target Stars and Systems: Activity and Rotation Catalog (ARC) of Potential Target Stars for the Habitable Worlds Observatory","primary_cat":"astro-ph.SR","submitted_at":"2026-05-21T15:30:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Collates archival stellar activity and rotation data for potential HWO targets, finding measurements for at least 70% of high-interest systems but activity cycles for fewer than 20%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21212","ref_index":97,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Detection of a dark matter subhalo in the strongly lensed system PJ011646","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T14:07:43+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A subhalo of M200 = 2.78e10 solar masses and concentration 30 is detected at 5.8 sigma in PJ011646 via ALMA imaging and grid-based NFW search after fitting an elliptical power-law plus multipole macromodel.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20027","ref_index":101,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"ComPACT: Mass-Redshift Properties of the galaxy cluster catalogue","primary_cat":"astro-ph.CO","submitted_at":"2026-05-19T15:51:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"ComPACT is a new SZ-selected galaxy cluster catalogue from CNN analysis of ACT+Planck data with 2,962 candidates, ~60% confirmation, 116 new redshifts, 158 new masses, and five new massive clusters at z>0.7 that increase the known high-mass high-z population by ~10%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19000","ref_index":14,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Exoplanets in ancient stellar populations: occurrence constraints and hot-Jupiter candidates in the Galactic halo","primary_cat":"astro-ph.EP","submitted_at":"2026-05-18T18:19:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Hot Jupiter occurrence in the Galactic halo is low at ~0.13% with no significant difference between in-situ and accreted populations, well below disk rates.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18995","ref_index":221,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Blue Straggler Stars in Old Open Clusters and the Kraft Break","primary_cat":"astro-ph.SR","submitted_at":"2026-05-18T18:13:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Blue straggler stars in old open clusters exhibit a Kraft break in rotation, with rapid rotators above the break and slow rotators below, indicating their envelopes behave like those of single stars.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18513","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A 4200-hour HyperFlash and \\'ECLAT campaign on the hyperactive FRB 20240114A: constraining energetics with the most brilliant bursts","primary_cat":"astro-ph.HE","submitted_at":"2026-05-18T15:06:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A 4200-hour campaign on FRB 20240114A finds that the highest-energy bursts account for most of the observed radio energy release, with a break in the energy distribution at ~2×10^40 erg and a linear DM rise of +0.96 pc cm^{-3} over 318 days.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17786","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The First Insights into an Ultraluminous X-ray Pulsar with XRISM: Phase-Resolved High-Resolution Spectroscopy of the Fe K-shell Band of M82 X-2","primary_cat":"astro-ph.HE","submitted_at":"2026-05-18T03:09:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Phase-resolved high-resolution spectroscopy of M82 X-2 with XRISM Resolve finds broader Fe Kα line during pulse peak, indicating origin in the accretion flow with velocity dispersion of about 1700 km/s.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.14187","ref_index":218,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Distribution of Blue Straggler Stars in the Color-Magnitude Diagrams of Old Open Clusters","primary_cat":"astro-ph.SR","submitted_at":"2026-05-13T23:10:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Blue straggler stars in old open clusters predominantly appear near the terminal-age main sequence because mass transfer from asymptotic giant branch donors enriches their cores with helium.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12424","ref_index":65,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Self-consistent dynamical modelling of the Milky Way bar with orbital frequency analysis","primary_cat":"astro-ph.GA","submitted_at":"2026-05-12T17:21:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"An updated orbital frequency method shows multiple Milky Way bar lengths and pattern speeds are consistent with star data within 5 percent.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12391","ref_index":77,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Trajectory-Agnostic Asteroid Detection in TESS with Deep Learning","primary_cat":"astro-ph.EP","submitted_at":"2026-05-12T16:56:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A W-Net deep learning model detects asteroids in TESS data independently of trajectory by rotating training image cubes and using adaptive normalization for data scaling.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12356","ref_index":216,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Simulating the jittering-jets explosion mechanism: Supernova remnant G11.2-0.3","primary_cat":"astro-ph.HE","submitted_at":"2026-05-12T16:30:41+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Hydrodynamic simulations of three jet pairs in the jittering-jets mechanism reproduce the ring-and-bar morphology of supernova remnant G11.2-0.3.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11074","ref_index":151,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Observational Signatures and Constraints on the Intermediate Neutron-Capture Process. The Case of the CEMP star TYC 6044-714-1 (RAVE J094921.8-161722)","primary_cat":"astro-ph.SR","submitted_at":"2026-05-11T18:00:02+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":"2605.11067","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Spectroscopic Bolometric Corrections and Empirical Zero-point Constants of \\textit{Gaia} Magnitudes, $G$, $G_{\\rm BP}$, and $G_{\\rm RP}$, from \\textit{Gaia} XP Spectra","primary_cat":"astro-ph.SR","submitted_at":"2026-05-11T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Empirical zero-point constants for Gaia bolometric corrections are derived as weighted averages 0.8677, 1.0449, and 2.0510 mag for G, GBP, and GRP from 88 stars, yielding corresponding magnitude zero-points via IAU definitions.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"for a large group of stars using their absolute bolometric (MBol) and filtered (Mξ) magnitudes and fractional luminosities (Lξ/L), which also requires accurate stellar parameters (R,Teff), photometric and astrometric data in addition to the spectra covering the wavelength ranges of theGaiabands (G,G BP andG RP). Then, the mean of the computedC2(ξ)values could be used in the formula as BC ξ = 2.5 log Lξ L +C 2(ξ),(8) to calculate the spectroscopicBC ξ from a fractional luminosity valueLξ/L. The fractional lumi- nosities, however, are obtained according to the formula Lξ L = R ∞ 0 Sλ(ξ)Fλ dλR ∞ 0 Fλ dλ = Fξ σTeff4 ,(9) whereS λ (ξ)is the function representing the transparency profile for one of theGaiabands (G, GBP, andG RP) andF λ is the surface flux per unit wavelength, thereforeFξ is the filtered flux out"},{"citing_arxiv_id":"2605.10940","ref_index":40,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Electromagnetic Follow-up of the Sub-Solar Mass Gravitational Wave Candidate S251112cm: Kilonova Constraints and a Coincident IIb Supernova","primary_cat":"astro-ph.HE","submitted_at":"2026-05-11T17:59:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"No kilonova detected from sub-solar GW candidate S251112cm, but coincident IIb supernova SN 2025adtq yields suggestive evidence for the superkilonova channel, though inconclusive after accounting for chance coincidence.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.10212","ref_index":116,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Isolating Broadband Radio Technosignatures (BRaTs): A Framework for Detecting Planetary-Scale Leakage","primary_cat":"astro-ph.IM","submitted_at":"2026-05-11T08:55:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A tiered observational strategy is outlined to identify planetary-scale broadband radio technosignatures (BRaTs) from advanced civilizations up to 100 pc away using multi-parameter diagnostics to separate them from natural signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.09837","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Simulating Star Formation and Star Cluster Assembly in the Aquila Rift Using Archival Observations","primary_cat":"astro-ph.GA","submitted_at":"2026-05-11T00:40:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations of the Aquila Rift show uneven clumps accreting gas and merging along filaments to form a fractal cluster whose velocity anisotropies, rotation, and expansion record the assembly history even after gas removal.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"a filament are sampled randomly between a z-distance of −18 pc and +18 pc. We determine this value using the G. Edenhofer et al. (2024) dust map to determine the column density of dust along the line of sight pointed in the direction of the Aquila rift (l≈28.8 ◦ andb≈3.5 ◦). We convert the temperature maps from the HGBS into internal energy maps using upixel = 3kBTpixel 2µH2 (1) where u pixel is the internal energy in each pixel, k B is the Boltzmann constant, and T pixel is the temperature at each pixel. Each SPH particle is given the inter- nal energy corresponding to the pixel within which it is placed. 2.2.2.Green Bank: Dense Gas Kinematics The Green Bank Ammonia Survey (R. K. Friesen et al. 2017) performed spectroscopy of the NH 3 gas present in"},{"citing_arxiv_id":"2605.09637","ref_index":23,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A NICER and AstroSat view of the neutron star low-mass X-ray binary 1A 1246-588","primary_cat":"astro-ph.HE","submitted_at":"2026-05-10T16:33:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Multi-epoch observations of 1A 1246-588 show blackbody temperature rising from 0.28 to 0.39 keV with emitting radius 6.9-13.8 km and Comptonization photon index varying 1.8-2.3, consistent with atoll-state changes from accretion power redistribution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.09340","ref_index":45,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"GSC 08227-00723: An Unusually Large PSH Excess AH Pic Candidate","primary_cat":"astro-ph.SR","submitted_at":"2026-05-10T05:41:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"GSC 08227-00723 is classified as a new AH Pic-type nova-like variable with recurrent stunted outbursts and an exceptionally large positive superhump excess of approximately 0.19.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.08353","ref_index":107,"ref_count":1,"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":"2605.08340","ref_index":6,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"You Shall Not Pass (Without Modeling): High-Resolution Analysis of KMT-2019-BLG-0253 using MORIA","primary_cat":"astro-ph.EP","submitted_at":"2026-05-08T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"MORIA pipeline applied to HST data for KMT-2019-BLG-0253 halves the number of viable solutions and measures a 0.65 solar-mass host with a 7-9 Earth-mass planet at 2.64 kpc.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07918","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Constraining the Galactic bar using the M92 stellar stream","primary_cat":"astro-ph.GA","submitted_at":"2026-05-08T15:55:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Spectroscopic members of the M92 stream yield a Milky Way bar pattern speed of 29.1 +0.7/-0.4 km s^{-1} kpc^{-1}.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"gravitiesandeffectivetemperaturesfollowingByströmetal.(2025), but do not find any close to the stream track. SGB candidates are identified by selecting all stars in the photometric sample that have astrometry in agreement with the selections in Eqs. 1 and 2, fall within the colour range0.27<(𝑔 0 −𝑟 0)<0.40, and have sky coordinates in the range: |𝜙 2 − (0.041𝜙 1 −0.176𝜙 2 1 +0.001𝜙 3 1)|<1.3,(4) where the polynomial is an approximation of the M92 stream track definedbyThomasetal.(2020).FortheSGBcandidatesthatpassthe abovecuts,wecomputetheirabsolutemagnitudes𝑀 𝑟 assumingthat they are at the GC distance of 8.3 kpc. From the resulting colour- absolute magnitude diagram (CAMD), we choose stars along this sequence to interpolate a relationship of𝑀𝑟 as a function of colour"},{"citing_arxiv_id":"2605.07684","ref_index":147,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The diverse morphologies and evolution of low-luminosity edge-brightened radio galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-05-08T12:54:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Low-luminosity FRII radio galaxies show higher core prevalence, comparable hotspots, and ~32% restarting/remnant behavior compared to bright FRIIs, revealing a highly diverse population where FRII dynamics occur at low powers.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.06799","ref_index":48,"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":"2605.06781","ref_index":127,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Radial redistribution of stellar orbits in FIRE simulations of Milky-Way-mass galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-05-07T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"FIRE-2 simulations show that stellar radial redistribution scatter saturates at ~2 kpc for stars older than ~3 Gyr, with net orbital changes depending on age and current radius, broadly matching Milky Way observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.06778","ref_index":34,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"An HST Wide Field Survey of the Galactic Bulge: Overview, Strategy, and First Results","primary_cat":"astro-ph.GA","submitted_at":"2026-05-07T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A new HST wide-field survey of the Galactic Bulge supplies high-angular-resolution data to enhance Roman exoplanet detections and serve as a community legacy dataset for stellar populations and dynamics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.06766","ref_index":44,"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":"2605.06648","ref_index":72,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A preliminary exploration of the effects of baseline length for the LIFE space mission","primary_cat":"astro-ph.IM","submitted_at":"2026-05-07T17:55:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LIFE mission simulations show that baselines of 25-80 m or even discrete values can achieve planet yield and fringe tracking with less than 10% performance loss compared to wider ranges.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05760","ref_index":165,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"ATOMIUM: Inner circumstellar envelopes of oxygen-rich AGB stars as revealed by highly excited SiO lines","primary_cat":"astro-ph.SR","submitted_at":"2026-05-07T06:55:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"ALMA Band 6 data detect SiO emission and masers up to v=8 in AGB stars, showing clumpy distributions, velocity gradients, and a tentative link between emission radius and mass-loss rate.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05412","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Dual-Band Centimetre Continuum Monitoring Survey of Young Stellar Objects in the Coronet Cluster","primary_cat":"astro-ph.GA","submitted_at":"2026-05-06T20:13:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Dual-frequency monitoring detects 20 radio sources in the Coronet Cluster, showing steeper spectral indices in Class 0/I YSOs than in Class II and ubiquitous variability independent of stage.","context_count":1,"top_context_role":"method","top_context_polarity":"unclear","context_text":"0], where𝐾 𝑠 corresponds to the 2MASS band centred at 2.2𝜇m (Skrutskie et al. 2006) and the 8.0𝜇m band comes from IRAC-Spitzer (Fazio et al. 2004). The radio spectral index was computed as described in Sec. 3.2. The near-IR vs. IRAC colour-colourdiagramscanbeusedtoidentifysourceswithdisksor circumstellarenvelopes(e.g.,Allenetal.2004;Teixeiraetal.2012). Colours such as𝐾 𝑠 − [4.5]or𝐾 𝑠 − [8.0]are typically associated with different classes: low values with Class III YSOs (disk-less), intermediatevalueswithClassIIYSOs(withdisks),andhighvalues with the more embedded YSOs. Complementarily, the bolometric temperature is also useful to trace the evolutionary stage of the em- beddedYSOs,withlower𝑇 bolvaluescorrespondingtoyoungerYSOs"},{"citing_arxiv_id":"2605.05380","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Eye of Sauron in SN 2025ngs: a Short-plateau Cousin of SN 1998S with Evidence for a Ring-like Circumstellar Medium","primary_cat":"astro-ph.SR","submitted_at":"2026-05-06T19:02:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"SN 2025ngs is a short-plateau supernova resembling SN 1998S but fainter, with spectral evidence for interaction with a proximate ring-like circumstellar medium around a supergiant progenitor.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05298","ref_index":17,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Kinematic Stratification in Extremely Red Quasars Revealed by JWST","primary_cat":"astro-ph.GA","submitted_at":"2026-05-06T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"JWST observations of ERQs show stratified gas kinematics via deblended optical emission lines, with UV lines dominated by scattered light and optical lines mixing scattered and obscured emission.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"both the outflows traced by 0834-A and 0834-C and the NLR-like gas traced by 0834-B - are relatively dust-free. Comparing Figures 3 and 5, it is clear that 0834-A pro- 10000 7500 5000 2500 0 2500 5000 7500 10000 Velocity [km s 1] 0 5 10 15 20 25 C IV 1548,51 SDSS X-Shooter JWST H (scaled) 0 2 4 6 8 10 12 O I 1304 8446 JWST 8446 (scaled) X-Shooter 1304 SDSS 1304 Flux [10 17 erg s 1 cm 2 Å 1] Fig. 5.-Top:Velocity profiles of the OIλ8446 line from the JWST spectrum and the OIλ1304 line from the SDSS and X- Shooter spectra. The JWST spectrum is scaled to match the flux of the UV spectra with an observed OIλ1304:λ8446 flux ratio of 1:3-5, depending on the scaling used. We also include the template fits to the OIλ8446 profile that are also shown in Fig."},{"citing_arxiv_id":"2605.04818","ref_index":140,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"AGILE detection of transient {\\gamma}-ray emission from the region of the supergiant fast X-ray transient source IGR J17354-3255","primary_cat":"astro-ph.HE","submitted_at":"2026-05-06T12:07:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"AGILE archival data reveal gamma-ray flares from a source matching IGR J17354-3255, with orbital phase correlation supporting physical association and high-energy emission from SFXTs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04141","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Tale of a Hungry Subgiant and Its Brown Dwarf: Interior Radiative Damping Dominates the Tidal Evolution of TOI-5882","primary_cat":"astro-ph.SR","submitted_at":"2026-05-05T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Radiative damping of internal gravity waves dominates tidal evolution in TOI-5882, shortening the brown dwarf's engulfment timescale by a factor of 2-6 relative to classical models.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"timestep to provide computational flexibility. When this cadence condition is met, a snapshot of the stellar struc- ture is exported along with the tidal forcing parameters to a wrapper module that constructs a corresponding GYREmodel. The forced oscillation response is then solved for each{ℓ, m, k}and the outputs are used to calculate the quantities in Equations (7) and (9). To stay consistent withMESAconvention and allow these quantities to represent changes to the orbit, the hookother jdot lsis defined as, ˙Jls =−⟨T ⟩ primary − ⟨T ⟩ secondary,(10) and the hookother edot tidalis defined as, ˙Etidal =− 1 |Eorb|(⟨P⟩ primary +⟨P⟩ secondary), (11a) Eorb =−q GM 2 2a .(11b) These quantities are cached and supplied to theMESA"},{"citing_arxiv_id":"2605.02998","ref_index":121,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The SRG/eROSITA diffuse soft X-ray background II. spectra and morphology of the eROSITA bubbles in the western Galactic hemisphere","primary_cat":"astro-ph.HE","submitted_at":"2026-05-04T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Spectra of the western eROSITA bubbles reveal two uniform components at 0.60 keV and 0.21 keV with sub-solar abundances, plus a geometrical model constraining horizontal size to ~6 kpc but leaving vertical extent uncertain.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.01105","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Resolving the Unresolved Galactic Winds in Multi-phase Models. I. Methodology and Application","primary_cat":"astro-ph.GA","submitted_at":"2026-05-01T21:20:47+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A new fitting methodology applied to UV absorption data recovers radial trends in galactic wind velocities and mass-loading factors by constraining initial hot and cool phase parameters in a multiphase model.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":", the width of the high-speed wing withv < v cl. We do not use the full width because the FB22 model pro- duces only outflows, so the modeled profiles occupy only the blueshifted side (v <0). FB22 model directly yields the velocity and num- ber density of outflow clouds at each radius (v cl(r) and nH,cl (r)). From that, we have: dNH,cl dv (r) =n H,cl(r) dvcl(r) dr (2) We then measureNH,cl ,v cl, HWHMcl from this modeled dNH/dvprofile and fit them to the ones measured from observations. Next, we identify the key free parameters varied in the model. Fielding & Bryan (2022) have identified the primary ones that govern the outputs. On the one hand, these include galaxy-scale properties, e.g., SFR, the depth of the gravitational potential (quanti-"},{"citing_arxiv_id":"2605.00988","ref_index":79,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Tidal pre-conditioning and ram-pressure stripping in NGC 1427A. Deep VLT/MUSE spectroscopy and FUV-to-radio observations trace a Fornax Cluster dwarf in transformation","primary_cat":"astro-ph.GA","submitted_at":"2026-05-01T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Multi-phase observations of NGC 1427A indicate tidal torquing from a dwarf fly-by has pre-conditioned its gas for ram-pressure stripping by the Fornax intracluster medium, placing the galaxy at the onset of environmental quenching with a declining star formation rate.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.00822","ref_index":3,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ing the SFR to stellar mass and redshift calibrated by observations of many star-forming galaxies (e.g., J. S. Speagle et al. 2014; P. Popesso et al. 2023). The re- sult is a 4-tiered classification scheme for galaxies that includes (1) nominal star formation consistent with the SFMS, (2) starburst (enhanced star formation signifi- cantly above the SFMS), (3) transitional (star forma- tion that is below the SFMS and that may be \"ramping down\"), and (4) quiescence, which is characterized by star formation significantly below the SFMS or not de- tectable. In the context of AGN-host studies, quiescence may be taken to mean quenched, though they are not always synonymous. Observationally calibrated models"},{"citing_arxiv_id":"2605.00720","ref_index":126,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A bright wideband radio burst from the isolated neutron star 2XMM J104608.7$-$594306","primary_cat":"astro-ph.HE","submitted_at":"2026-05-01T15:08:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A second coherent radio burst spanning 704-4032 MHz with spectral index -2.18, 54% linear and 22% circular polarization, and an orthogonal polarization angle jump was detected from 2XMM J104608.7-594306, showing rare radio activity in sources thought to be radio-quiet.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.25991","ref_index":40,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The GlimmIr: Spectroscopic Variability in a z~7 LRD Indicates Rapid Changes in Both the Narrow and Broad Line Regions","primary_cat":"astro-ph.GA","submitted_at":"2026-04-28T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"First spectroscopic variability in a z~7 LRD shows rapid changes in both narrow and broad line regions, implying direct ionization from the central source to surrounding nebular gas.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.24494","ref_index":1,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Probing the Hot Gaseous Halos of Milky Way-like Galaxies in the TNG50 simulation","primary_cat":"astro-ph.GA","submitted_at":"2026-04-27T13:59:12+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"TNG50 MW analogues reproduce global soft X-ray luminosity, inner surface brightness, emission measure and O VII absorption but show too-steep radial decline in X-ray brightness and 65% lower O VIII absorption than observed, indicating overly central feedback.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.22932","ref_index":2,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Characterization of the Volatile Properties of 133P/Elst-Pizarro and Other Main-Belt Comets with JWST and Ground-Based Observations","primary_cat":"astro-ph.EP","submitted_at":"2026-04-24T18:05:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"JWST observations of 133P/Elst-Pizarro yield water outgassing rates of (1.9 ± 0.6) × 10^25 and (1.4 ± 0.4) × 10^25 molecules/s at true anomalies 8° and 37.4°, with hypervolatile depletion Q(CO2)/Q(H2O) < 0.009 and an average log(Afrho/Q(H2O)) = -24.6 ± 0.2 across three MBCs.","context_count":1,"top_context_role":"dataset","top_context_polarity":"baseline","context_text":"c Measured upper limit CO 2 production rate in molecules s −1 and kg s −1. d Measured upper limit CH 3OH production rate in molecules s −1 and kg s −1. e CO to H2O production rate ratio (by number of molecules). f CO2 to H2O production rate ratio (by number of molecules). g CH3OH to H2O production rate ratio (by number of molecules). h References: [1] This work; [2] M. S. P. Kelley et al. (2023); [3] H. H. Hsieh et al. (2025); [4] J. W. Noonan et al. (2025). also has a semimajor axis interior to the 5A:2J mean- motion resonance with Jupiter. This reasoning is also consistent with the much smaller heliocentric distance of 457P's activity onset point (rh ∼2.35 au; J. W. Noonan et al. 2025) compared to those for MBCs with semima-"},{"citing_arxiv_id":"2604.22931","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Emerging Diversity Among the Main-Belt Comets: Insights from JWST and Ground-Based Observations of 457P/Lemmon-PANSTARRS","primary_cat":"astro-ph.EP","submitted_at":"2026-04-24T18:04:51+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"457P shows dust activity without detectable H2O, CO, CO2, or CH3OH, with Q(H2O) < 2e24 molecules/s, indicating it may be more volatile-depleted than other main-belt comets.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"24×10 16π pV 100.4[m⊙,V −md,V (1,1,0)] (4) (Y. Kim et al. 2022), where we assume a geometric albedo ofp V = 0.05, and usem ⊙,V =−26.71±0.03 (J. Hardorp 1980). Using this method, we find a total dust scattering cross section ofC d = (0.7±0.6) km 2. The dust mass,M d, corresponding to this scattering cross-section can be estimated using Md = 4 3 Cd¯adρd (5) where ¯ad is the effective mean dust grain radius andρ d is the dust grain bulk density, assuming that the coma is optically thin. Assuming ¯a d = 100µm andρ d = 2500 kg m−3 similar to that of CI and CM carbonaceous chondrites (D. T. Britt et al. 2002), we find a dust coma mass ofM d = (2.4±1.8)×10 5 kg. The dust velocity measured by HST during the 2020"},{"citing_arxiv_id":"2604.22559","ref_index":6,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Quasar--Companion System Without AGN Outflow at $z \\sim 6$: The Case of PSO J083+11","primary_cat":"astro-ph.GA","submitted_at":"2026-04-24T13:54:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New ALMA [C II] and FIR data on PSO J083+11 at z=6.34 reveal ordered rotation, typical star-forming ratios, and no outflow signatures in either galaxy, interpreted as a pre-AGN-feedback accretion phase.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"All luminosities are in solar units (𝐿⊙);log(𝐿 [Cii] /𝐿FIR)quanti- fies the [Cii] deficit, andΣFIR denotes FIR surface brightness in 𝐿 ⊙ kpc−2. MNRAS000, 1-16 (2025) 14M. A. Husain et al. Table A1: Galaxy sample for AGN feedback analysis. References: [1] Hughes et al. (2017), [2] Brisbin et al. (2015), [3] Stacey et al. (2010), [4] Schaerer et al. (2015), [5] Gullberg et al. (2015), [6] Wagg et al. (2010), [7] Iono et al. (2006), [8] Venemans et al. (2020), [9] Walter et al. (2012),[10]Riechersetal.(2014),[11]DeBreucketal.(2011),[12]Marsdenetal.(2005),[13]Hashimotoetal.(2019). 𝑎 ΣFIR estimatedvia the size-luminosity relation of Lutz et al. (2016);𝑏direct measurement from Decarli et al. (2018). Galaxy𝑧log(𝐿 [Cii] )log(𝐿 FIR)log(𝐿 [Cii] /𝐿FIR)log(Σ FIR)Ref"},{"citing_arxiv_id":"2604.21184","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Predicting the thermodynamics in the chromosphere from the translation of SDO data into the IRIS$^{2}$ inversion results using a visual transformer model","primary_cat":"astro-ph.SR","submitted_at":"2026-04-23T01:00:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A visual transformer model trained on IRIS inversions predicts chromospheric temperature and density from SDO data with correlations around 0.8 on 80% of test cases.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The contribution from AIA 193 Å might look suspicious to the correlation at this optical depth, but it is similar to the values atlog(τ)=-5.2 andlog(τ)=-4.2. 6.CONCLUSIONS We have developed a new tool, named SDO2IRIS 2, that uses SDO/AIA images and the SDO/HMI magnetograms to predict the thermodynamics in the chromosphere at three optical depths,log(τ)=[-5.2, -4.2, -3.2], roughly covering a region from the temperature minimum to the middle and high chromosphere. We have shown that the predictions of the thermodynamics provided by SDO2IRIS2 (using SDO/AIA 1600 Å, 1700 Å, and 304 Å bandpass images and SDO/HMI magnetograms) when compared with the inversion results obtained by IRIS 2 show a strong correlation for T andn e (mode ofr≈0."},{"citing_arxiv_id":"2604.21013","ref_index":88,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Archival Multiband Gravitational-Wave Signals from Massive Black Hole Binary Mergers","primary_cat":"astro-ph.HE","submitted_at":"2026-04-22T19:00:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Massive black hole binary mergers produce orphaned low-frequency signals in PTA pulsar terms that can be stacked for archival multiband gravitational-wave detection.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20814","ref_index":10,"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":"2604.20722","ref_index":59,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Photometric Identification of Unresolved Binary Stars in Nearby Open Star Clusters","primary_cat":"astro-ph.GA","submitted_at":"2026-04-22T16:07:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Empirical isochrones in photometric diagrams enable identification of unresolved binaries in eight nearby open clusters, yielding binary fractions of 0.16-0.44 and mass ratio modes around 0.4-0.8.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20262","ref_index":30,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Measuring Tianlai's primary beam using sky model","primary_cat":"astro-ph.IM","submitted_at":"2026-04-22T07:10:37+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The primary beam of the Tianlai array is shown to be factorizable into independent E-W and N-S components, with E-W profiles measured from the Sun and N-S obtained via sky model fitting.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20195","ref_index":106,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Photometric Super-Resolution for Improving Galaxy Morphological Measurements using Conditional Generative Adversarial Networks","primary_cat":"astro-ph.IM","submitted_at":"2026-04-22T05:23:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Neo, a cGAN, super-resolves HSC images to HST-like quality and improves galaxy morphological parameter accuracy by factors of 2-10.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}