{"total":42,"items":[{"citing_arxiv_id":"2606.24114","ref_index":9,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Kepler Image-Subtracted Light Curves and Variable Star Catalog of NGC 6819","primary_cat":"astro-ph.SR","submitted_at":"2026-06-23T04:01:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Kepler image-subtracted photometry yields 81,498 light curves and a catalog of 87 periodic variable candidates in NGC 6819, including 26 newly discovered ones.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18386","ref_index":150,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Reconstructing Galactic Gravitational Potentials from Stellar Kinematics with Physics-Informed Neural Networks","primary_cat":"astro-ph.GA","submitted_at":"2026-06-16T18:31:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A PINN approach learns galactic gravitational potentials from acceleration data, achieving sub-percent errors on simulations while outperforming analytic models and retaining interpretability via structured priors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12517","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Hubble Missing Globular Clusters Survey IV. Ultra-faint compact satellites of the Milky Way. The case of Koposov 2","primary_cat":"astro-ph.GA","submitted_at":"2026-06-10T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Koposov 2 is shown to be an old (13.7 Gyr) star cluster with half-light radius 2.7 pc, absolute magnitude -0.95, and stellar mass 372 solar masses, supporting a star cluster classification over a dwarf galaxy.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"[deg] [deg] [mas yr −1] [mas yr −1] [kpc] [km s −1] Koposov 2 119.571 (1) 26.255 (1)−0.745±0.056 (2) 0.140±0.042 (2) 23.4±0.6 (4) 112±9 (3) Notes.Numbered references are: (1) Vasiliev & Baumgardt (2021), (2) Libralato et al. (2026), (3) Ceccarelli et al. (2026), and (4) this work. Table C.2.Orbital parameters for Koposov 2. Potential EnergyL z Lperp rperi rapo Zmax circ P orb [105 km2 s−2] [10 3 kpc km s−1] [10 3 kpc km s−1] [kpc] [kpc] [kpc] [Gyr] McM17−0.76 +0.02 −0.02 7.86+0.29 −0.19 2.94+0.18 −0.18 28.7+0.7 −0.7 59.9+4.8 −3.4 20.3+1.4 −1.5 0.83+0.01 −0.02 0.96+0.04 −0.04 DL26−0.37 +0.02 −0.02 7.85+0.23 −0.23 2.95+0.13 −0.13 29.1+0.8 −0.8 101.8+9.8 −9.8 35.3+3.2 −3.2 0.88+0.03 −0.03 1.84+0.18 −0.18 DL26+LMC−0.37 +0.02 −0.02 7.85+0."},{"citing_arxiv_id":"2606.11293","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"A systematic survey for hypervelocity runaways from thermonuclear supernovae","primary_cat":"astro-ph.SR","submitted_at":"2026-06-09T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A systematic survey with complete spectroscopic classification finds 13 hypervelocity D6 and LP 40-365 stars and shows that intermediate-heating evolutionary models best reproduce the observed population at birth rates of only a few percent of the Galactic SN Ia rate.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10623","ref_index":160,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Rogue Ones: Orbital census of Galactic Cepheids and their Anomalies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-09T09:22:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A 6D kinematic census identifies 18 anomalous Cepheids with extreme orbits, including one possibly scattered by globular cluster E3, and finds consistency between dynamical and stellar ages.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.08961","ref_index":23,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Rapid intermediate-mass black hole formation via runaway mergers of black holes","primary_cat":"astro-ph.GA","submitted_at":"2026-06-08T03:00:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"N-body simulations demonstrate runaway GW BBH mergers in dense BH clusters (≥5×10^9 M⊙/pc³) produce ~10³ M⊙ IMBHs within 10 Myr.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Mare the total masses of the BH subsystem, the stellar halo, and the entire system.m•, m⋆, and mrepresent their corresponding mean particle masses. The Coulomb logarithm is taken asln Λ = 0.02N, following M. Giersz & D. C. Heggie (1996). The parametersk1 andγare adopted from Figures 4 and 6 of L. Wang (2020). Then, the stellar halo potential is included in simulations using the packagegalpy(J. Bovy 2015). 3.RESULTS 3.1.IMBH Formation To investigate how IMBH mass evolution depends on the initial conditions, we present the evolutionary curves of the system's maximum BH mass (m•,max) over time (t) in Figure 1. IMBHs can form within 10 Myr from the formation of the BH subsystem. Specifically, an initial mass of5×104 M⊙ is necessary. Models such as M50k-SM-BH-r0."},{"citing_arxiv_id":"2606.06248","ref_index":26,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bar-induced deflection of open cluster tidal tails","primary_cat":"astro-ph.GA","submitted_at":"2026-06-04T14:50:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Test-particle simulations show that Galactic bar pattern speed systematically deflects open-cluster tidal tail orientations, with NGC 2632 and Hyades tails disfavouring moderate speeds.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05321","ref_index":14,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Hot Degenerate Components in Blue Stragglers: A Multi-Wavelength SED Analysis of Nine Open Clusters with Swift/UVOT","primary_cat":"astro-ph.SR","submitted_at":"2026-06-03T18:08:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"SED analysis of blue stragglers in open clusters finds UV excesses indicating hot degenerate companions in 15 of 35 candidates, supporting binary evolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04827","ref_index":170,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Steep Redshift Evolution of the Ionizing Escape Fraction at $z = 5$--$12$: Empirical Constraints and Comparison with Simulations","primary_cat":"astro-ph.CO","submitted_at":"2026-06-03T12:50:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Empirical three-parameter fit to f_esc(M_h,z) yields steep redshift evolution with population-averaged escape fraction rising from ~2% at z=5 to ~9% at z=12.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04624","ref_index":220,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Blue Straggler Stars in Berkeley 18: A Multiwavelength Study of Their Physical Properties and Dynamical Evolution","primary_cat":"astro-ph.SR","submitted_at":"2026-06-03T08:59:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Multiwavelength study identifies 24 BSS candidates in Berkeley 18, derives their properties via SEDs, and infers binary evolution as the dominant channel from low dynamical interaction indicators.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04567","ref_index":86,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"The GALAH Survey: Neutron-Capture Elemental Abundances for 350,000 Gaia-RVS Spectra and the Chemodynamics of Accreted Structures","primary_cat":"astro-ph.GA","submitted_at":"2026-06-03T07:54:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Derives stellar labels for 357k RVS giants via The Cannon and uses abundance-based logistic regression to tag GSE debris with consistent patterns after kinematic filtering.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.03901","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The VMC survey -- LV. The coherent expansion of the SMC","primary_cat":"astro-ph.GA","submitted_at":"2026-06-02T16:56:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Improved VMC proper motions show SMC expansion along SE-NW axes consistent with LMC tides, radial inward motions with no rotation, and northward motion in older RGB stars from a prior interaction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23801","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Unsupervised Chemo-Dynamical Dissection of the Inner Galactic Halo: Discovery of Five Accreted Substructures with SDSS-V and Gaia","primary_cat":"astro-ph.GA","submitted_at":"2026-05-22T15:59:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A blind 12D chemo-dynamical clustering analysis with UMAP and HDBSCAN on SDSS-V DR19 and Gaia DR3 data recovers seven known halo substructures and reports five new tightly bound candidates FO1-FO5.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23746","ref_index":13,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Gaia-Sausage-Enceladus: Lithium evolution from early red-giant-branch and main-sequence stars","primary_cat":"astro-ph.GA","submitted_at":"2026-05-22T15:20:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A lithium chemical evolution model for the GSE galaxy matches survey data showing Spite-like and eRGB plateaus at low metallicity with a hint of reduced nova contributions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21735","ref_index":18,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"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":"2605.20487","ref_index":7,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Milky Way Mapper decoded abundances -- I. Shared disc enrichment patterns","primary_cat":"astro-ph.GA","submitted_at":"2026-05-19T20:52:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A data-driven decomposition of stellar abundance vectors into four latent patterns identifies distinct contributions from core-collapse supernovae, Type Ia supernovae, and AGB stars across the Milky Way disc.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20322","ref_index":5,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Inferring Globular Cluster Initial Mass Function from Stellar Streams","primary_cat":"astro-ph.GA","submitted_at":"2026-05-19T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Stellar streams encode the initial mass function of globular clusters, recovered as a declining power-law with slope 1.3 for streams above 1000 solar masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19000","ref_index":53,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":228,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"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":"2605.18131","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Inferring stellar metallicity and elemental abundances from kinematic and spectroscopic data using machine learning -- Implications for exoplanet host stars","primary_cat":"astro-ph.EP","submitted_at":"2026-05-18T09:35:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"ML regressors trained on APOGEE DR17 red giants predict C, O, Mg, Si abundances from kinematics and [Fe/H] more accurately than [Fe/H] baseline, with external validation on HARPS FGK dwarfs and reproduction of Galactic chemical evolution trends.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.14187","ref_index":225,"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":98,"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":"2605.11074","ref_index":119,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"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":"2605.07511","ref_index":26,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dynamical evolution of Milky Way globular clusters on the cosmological timescale II. Terzan 2, 4, and 5 mass loss and collision tracking","primary_cat":"astro-ph.GA","submitted_at":"2026-05-08T09:41:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"N-body simulations show that mutual interactions between Terzan 2, 4, and 5 raise mass-loss rates for the smaller clusters and drive prolate deformations absent in isolated runs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07392","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Mass Production of 2023 KMTNet Microlensing Planets. III: Three Planets from the Subprime Field","primary_cat":"astro-ph.EP","submitted_at":"2026-05-08T07:47:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Three new planets detected via 2023 KMTNet microlensing with mass ratios log q ~ -1.9, -2.0, -2.6; overall 2023 sample of 25 planets matches prior mass-ratio distribution.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"1±3.1 43.1±3.5 ρ(10−3) 1.08±0.27 1.16±0.27 α(deg) 240.1±1.1 239.2±1.2 s 1.257±0.009 1.044±0.019 logq −1.903±0.046−1.974±0.054 IS,KMTC 20.953±0.023 21.083±0.022 NOTE-HJD ′ = HJD−2460000. closest approach, the impact parameter expressed in units of the angular Einstein radiusθ E, and the Einstein timescale, respectively, θE = p κMLπrel, t E = θE µrel ,(1) whereκ= 4G/(c 2au)≃8.144,masM −1 ⊙ ,M L is the to- tal lens mass, and(π rel, µrel)denote the lens-source relative parallax and proper motion. The binary lens configuration is encoded by(s, q, α), representing the projected separation normalized toθ E, the binary mass ratio, and the trajectory angle. The final parameter,ρ=θ ∗/θE, is the normalized"},{"citing_arxiv_id":"2605.05708","ref_index":75,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"IY Lyr: A Thick-Disk first-overtone RR Lyrae Star with a Possible Neutron Star Companion","primary_cat":"astro-ph.SR","submitted_at":"2026-05-07T05:52:56+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"IY Lyr is a thick-disk RRc star with a 1.37 solar-mass companion most likely a neutron star in a 3.94-year eccentric orbit, confirmed by photometry, spectroscopy, and astrometry.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05622","ref_index":11,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The formation of the C-19 progenitor: a primordial cluster heated by gas expulsion","primary_cat":"astro-ph.GA","submitted_at":"2026-05-07T03:22:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Severe gas expulsion and expansion in a primordial star cluster, combined with a top-heavy IMF, can reproduce the high velocity dispersion and broad stream of C-19 without dark matter subhalos.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"2020), which provide prescrip- tions for the evolution of both single and binary stars. In particular,BSEEMPoffers fitting formulae for the evolu- tionary tracks of massive stars in extremely metal-poor environments, which satisfy the needs of our simulations of star clusters under such conditions. In addition, the external tidal field is modeled with theGALPYpackage (Bovy 2015), where we include the gravitational potential of the Milky Way to account for its influence on the cluster evolution. 2.2.Galactic potential We use theMcMillan17Milky Way potential (McMil- lan 2017), comprising bulge, halo, and disk components. The Galactic bulge adopts an axisymmetric assumption, 3 with its density distribution based on the parametric"},{"citing_arxiv_id":"2605.05293","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Life is But a Stream: The Distribution of Planetary Systems Along Stellar Streams and their Properties","primary_cat":"astro-ph.EP","submitted_at":"2026-05-06T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations show stars at the edges of stellar streams are more likely to retain unperturbed planetary systems than stars near the stream center.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Star Cluster Simulation We simulate a cluster of 12500 stars with an initial mass of 7500M ⊙ and an initial half-mass radius of 4pc. The stellar initial mass function is taken from P. Kroupa (2001) and the initial density profile is a H. C. Plum- mer (1911) sphere. The cluster is given a circular orbit at 5 kpc in a Milky Way-like tidal field (MWPOTEN- TIAL2014 from J. Bovy (2015)). The system evolved 5 https://www.amusecode.org/ until its complete dissolution, which we denote to be the time when the cluster has less than 100 energetically bound stars remaining. Given this criteria, cluster dis- solution occurs after 1088 Myr, with a long thin stream remaining. To study how planetary systems evolve around Sun- like stars in this cluster, we select all main sequence"},{"citing_arxiv_id":"2605.01436","ref_index":82,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Constraints on Einstein-aether gravity from the precision timing of PSR J1738+0333","primary_cat":"gr-qc","submitted_at":"2026-05-02T13:19:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Precision timing of PSR J1738+0333 from EPTA and NANOGrav data yields the tightest strong-field constraints on Einstein-aether parameters from any single binary pulsar.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"This accounts for the effect of sensitivities and PN con- tributions, as well as effects of the pulsar center-of-mass motion, on orbital decay. Appendix B: Galactic contribution to ˙Pb To accurately correct the observed orbital period derivative ˙Pb for Galactic acceleration, we computed the line-of-sight acceleration using thegalpypackage with theMWPotential2014Milky Way potential [82], which provides a self-consistent three-dimensional model in- cluding contributions from the Galactic bulge, disk, and dark matter halo. The pulsar's equatorial coordinates (α, δ), determined from the timing solution, are first converted to Galactic coordinates (l, b) usingAstropy[83]. Together with the distanced, these are used to compute the Galactocentric"},{"citing_arxiv_id":"2604.24456","ref_index":17,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Mapping the Milky Way with Gaia Bp/Rp spectra-IV: the broken and asymmetric density profile of the stellar disk traced by a large sample of red clumps","primary_cat":"astro-ph.GA","submitted_at":"2026-04-27T13:26:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The Milky Way stellar disk shows a broken radial density profile with four components, azimuthal dependence, inner and outer flaring, and a density-metallicity bump possibly from radial migration.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"We use the conventions from Python package astropy ( Astropy Collaboration et al. 2018), adopting a solar motion of (+12.9,+245.6,+7.78) km s −1 (K. Abazajian et al. 2004; GRAVITY Collaboration et al. 2018). The guiding radiusR gis defined asL z/V0, whereL z is the star's angular momentum andV 0 = 235 km s−1 is the circular velocity of local standard of rest (LSR) (J. Bovy 2015). Following S. Nepal et al. (2024), we constrained the RC sample to the solar radius by requiring 8< R <9.5 kpc. We only kept stars with|Z|<0.15 kpc because the metallicity/density bump is dominated by stars near the plane. In S. Nepal et al. (2024), the bimodal distribution first appears at [M/H]∼0.1 and becomes very significant at [M/H]> 0.25. Therefore, we divided the RC sample into three different types of 0."},{"citing_arxiv_id":"2604.21646","ref_index":6,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"An Old, Low-mass, Metal-poor Hypervelocity Star Candidate Consistent with a Galactic Center Origin","primary_cat":"astro-ph.GA","submitted_at":"2026-04-23T13:03:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI-HVS1 is the first reported old, low-mass, metal-poor hypervelocity star candidate whose reconstructed orbit points to a Galactic Center origin.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20010","ref_index":86,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The First Infrared Portrait of A Solar-Like Host Star with Debris Disk: Pioneering High-Resolution H- and K-Band Spectroscopy of HD115617 with Comparative Optical Spectrum Analysis","primary_cat":"astro-ph.SR","submitted_at":"2026-04-21T21:39:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The first NIR high-resolution spectroscopy of solar analog HD115617 shows a 250 K temperature discrepancy with optical data but confirms solar composition, main-sequence status, and no chemical signature of planetary formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19413","ref_index":176,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Oort Cloud Ecology -- IV. Exchanging Asteroids","primary_cat":"astro-ph.EP","submitted_at":"2026-04-21T12:45:16+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":"2604.14502","ref_index":11,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Last Galactic Firework: Timing the last significant merger with stars, globular clusters and $\\omega$Centauri","primary_cat":"astro-ph.GA","submitted_at":"2026-04-16T00:33:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The Gaia-Sausage-Enceladus merger occurred 11.2 ± 0.1 Gyr ago, coinciding with the formation of a group of globular clusters and potentially leaving ω Centauri as its remnant, while placing disk formation at z ≳ 4.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.12494","ref_index":18,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Multiwavelength Study of Blue Straggler Stars in Tombaugh 2: Evidence for Binary Mass Transfer and Constraints on Cluster Dynamical State","primary_cat":"astro-ph.SR","submitted_at":"2026-04-14T09:19:08+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"In Tombaugh 2, 32% of blue straggler stars show ultraviolet excess from hot companions consistent with recent binary mass transfer, supporting this channel over mergers in a low-density cluster.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"92±17.87 Orbital Parameters Zmax (kpc) 0.83±0.21 Rp (kpc) 12.40±1.33 Ra (kpc) 13.77±1.67 Rm (kpc) 13.09±1.50 e0.05±0.01 Tp (Myr) 385±49 To further characterize the dynamical environment, we derived the Galactic orbit of Tombaugh 2 using its complete six-dimensional phase-space information. Or- bit integrations were performed with thegalpypackage (J. Bovy 2015) in the axisymmetricMWPotential2014. The resulting orbital parameters are summarized in Ta- ble 7, and the orbit projections are shown in Figure 10. The integrated orbit shows that Tombaugh 2 resides in the outer Galactic disk at a Galactocentric distance ofR GC ≈13 kpc and follows a low-eccentricity orbit (e <0.1). Such an orbit implies that the cluster has"},{"citing_arxiv_id":"2601.22490","ref_index":9,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"SED and Galactic kinematic diagnostics for dormant BH/NS binary candidates","primary_cat":"astro-ph.SR","submitted_at":"2026-01-30T03:00:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"SED fitting plus kinematic diagnostics identify 182 top dormant BH/NS binary candidates from Gaia DR3, with 19 likely black hole systems having companion masses >=3 solar masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.12789","ref_index":11,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Classical Be Stars and Classical Be Star Binaries from LAMOST DR12","primary_cat":"astro-ph.SR","submitted_at":"2026-01-19T07:42:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"From LAMOST DR12, 504 classical Be stars are cataloged with 141 new, 14 RV-variable binaries, 60 RUWE-based candidates, 34 cluster members, and 37 runaways.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.09576","ref_index":25,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Build-up and survival of the disc: From numerical models of galaxy formation to the Milky Way","primary_cat":"astro-ph.GA","submitted_at":"2025-09-11T16:11:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations show that observed rotation in 13.5-Gyr-old alpha-rich stars constrains the Gaia-Sausage-Enceladus merger to mass ratios below 1:4, with interaction and starburst times both near 11 Gyr.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.07678","ref_index":7,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"3I/ATLAS: In Search of the Witnesses to Its Voyage","primary_cat":"astro-ph.EP","submitted_at":"2025-09-09T12:44:21+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"No stellar flybys within the past 10 Myr and 500 pc in Gaia DR3 explain the present trajectory of 3I/ATLAS, which matches thin-disk kinematics despite its high peculiar velocity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2506.21410","ref_index":16,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Sifting for a Stream: The Morphology of the $300S$ Stellar Stream","primary_cat":"astro-ph.GA","submitted_at":"2025-06-26T15:57:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"300S stellar stream exhibits three density peaks, smooth width variations, a possible 4.7 degree gap, and a kink modeled as resulting from Large Magellanic Cloud interaction across its full known footprint.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2206.14220","ref_index":20,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package","primary_cat":"astro-ph.IM","submitted_at":"2022-06-28T18:01:54+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The paper reports on the Astropy v5.0 release, project updates, ecosystem connections, and challenges facing the community-oriented open-source astronomy software effort.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.00987","ref_index":56,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Applying Liouville's Theorem to Gaia Data","primary_cat":"astro-ph.GA","submitted_at":"2019-07-01T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Phase-space density is recovered from Gaia data for M4 and disrupted streams by correcting entropy injection and minimizing stream entropy, enabling original mass inference via Liouville's theorem.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}