{"total":40,"items":[{"citing_arxiv_id":"2606.27480","ref_index":67,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Self-interacting dark matter promotes bar formation in disk galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-25T18:58:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"SIDM halos accelerate bar formation and growth in disk galaxies through enhanced angular momentum exchange, independent of core formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24114","ref_index":7,"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":"2606.23926","ref_index":62,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Detection of relativistic orbital deformation from improved timing of PSR J1757$-$1854","primary_cat":"astro-ph.HE","submitted_at":"2026-06-22T20:44:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First detection of relativistic angular deformation δ_θ in PSR J1757−1854 via MeerKAT-enhanced timing, ruling out two of four prior geometric solutions while confirming GR consistency for orbital decay.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23317","ref_index":27,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Galactic Cosmic Ray Transport in the Giant Circumgalactic Medium Halo","primary_cat":"astro-ph.HE","submitted_at":"2026-06-22T13:31:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Galactic cosmic rays in a giant CGM halo develop an extended 1/r spatial tail and broader age distribution while remaining consistent with secondary-to-primary ratio data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21651","ref_index":148,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Resolved Ages and Stellar Metallicities in Progenitors of Milky Way Analogs: A Closer Look at their Star Formation Histories since $z=5$","primary_cat":"astro-ph.GA","submitted_at":"2026-06-19T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Resolved stellar property gradients in Milky Way analog progenitors show inside-out assembly with minor, temporary disruption from major mergers.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.20201","ref_index":23,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Kick bimodality of neutron stars and mode dependence of their parameters","primary_cat":"astro-ph.HE","submitted_at":"2026-06-18T13:15:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Classification of pulsars into bimodal kick modes shows low-B objects overabundant in the low-velocity mode, with no high-velocity examples below 10^11 G.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18849","ref_index":111,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Disentangling the Distant Stellar Halo Using K-Giants in the DESI Year 3 Data","primary_cat":"astro-ph.GA","submitted_at":"2026-06-17T09:29:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"DESI K-giant catalog identifies Aleph, Sagittarius, GSE, Cetus-Palca and Orphan-Chenab, then shows residual halo high-angular-momentum stars have bimodal MDFs unlike GSE or Sagittarius.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18608","ref_index":229,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Log-Uniform Initial Magnetic Field Distribution Explains Pulsar and Magnetar Populations through Magnetic Inclination Alignment","primary_cat":"astro-ph.HE","submitted_at":"2026-06-17T02:10:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Magnetic inclination alignment with timescale proportional to B to the minus two suppresses observed numbers of strong-field neutron stars, unifying pulsars and magnetars under one log-uniform initial B distribution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18386","ref_index":54,"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":141,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10623","ref_index":159,"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":"2606.06457","ref_index":83,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dynamical evolution and dissolution timescale of young stellar clusters in the Orion star-forming complex","primary_cat":"astro-ph.GA","submitted_at":"2026-06-04T17:50:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Gaia-derived parameters for 13 Orion clusters fed into N-body simulations reveal two regimes: seven with α_vir ≲ 7 retain bound cores for ≳170 Myr while six with α_vir ≳ 7 dissolve before 120 Myr.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06248","ref_index":82,"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":"2605.23801","ref_index":40,"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":"2605.20117","ref_index":3,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"The potential of diffuse Galactic Ridge neutrino measurements to constrain dark matter","primary_cat":"astro-ph.HE","submitted_at":"2026-05-19T17:05:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"ANTARES Galactic Ridge neutrino measurements can constrain annihilating and decaying dark matter for various masses and profiles while comparing to astrophysical backgrounds, with forecasts for future observatories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19000","ref_index":69,"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":"2605.16501","ref_index":82,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Co-evolution of Supermassive Black Holes and their Host L* galaxies: implications for Milky Way and M31","primary_cat":"astro-ph.GA","submitted_at":"2026-05-15T18:00:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"ARTEMIS and EAGLE simulations classify L* galaxies by central BH-to-stellar-mass ratio and trace how merger history drives divergence in BH growth, star formation, and morphology, offering an explanation for the observed scatter and for MW/M31 differences.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16192","ref_index":56,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Simulations of gas inflow in the Milky Way I. Stellar-Feedback-Regulated Transport from the Central Molecular Zone to the Circumnuclear disk","primary_cat":"astro-ph.GA","submitted_at":"2026-05-15T17:10:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Stellar feedback regulates radial gas inflow in the Milky Way center, yielding time-averaged rates that fall from 5e-3 to 1e-6 solar masses per year with both smooth secular and episodic components.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16050","ref_index":53,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"The Low-$\\alpha$ Splash Population in the Milky Way","primary_cat":"astro-ph.GA","submitted_at":"2026-05-15T15:18:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Observational identification of a low-α Splash population in APOGEE DR17 and GASTRO simulations showing that clumpy proto-disk scattering, but not a major merger alone, heats old thin-disk stars to form both high- and low-α Splash components.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.14308","ref_index":52,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reconstructing the Stripping History of the Sagittarius Stream with Neural Networks","primary_cat":"astro-ph.GA","submitted_at":"2026-05-14T03:21:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A neural network trained on simulations infers stripping times for Sagittarius stream stars from phase-space data, measuring a 0.3 dex/Gyr metallicity gradient and estimating ages for globular clusters such as Pal 12 and NGC 2419.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11074","ref_index":120,"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":"2605.06659","ref_index":13,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Pulsar Radial Acceleration Relation","primary_cat":"astro-ph.GA","submitted_at":"2026-05-07T17:58:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Pulsar timing tests the vector RAR but current measurements are dominated by the Solar acceleration, producing similar chi-squared fits to a constant-acceleration model.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05708","ref_index":76,"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":53,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04138","ref_index":295,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Galactic Amnesia: The Information Washout of the Milky Way Merger History","primary_cat":"astro-ph.GA","submitted_at":"2026-05-05T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Mutual information analysis of TNG50 simulations shows gravitational potential and total energy retain merger mass and infall time information longest, while radial velocity loses it within ~5 Gyr, with washout depending on radius, merger age, and mass.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.00990","ref_index":98,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"NEFERTITI: Linking early galaxy formation to the assembly of the Milky Way","primary_cat":"astro-ph.GA","submitted_at":"2026-05-01T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"NEFERTITI simulations show that the Milky Way's most metal-poor stars largely come from a handful of accreted massive dwarf galaxies, while reproducing the JWST Hebe galaxy at z~11 as a pure Population III system.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.21646","ref_index":33,"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":"2604.18278","ref_index":108,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Characterizing the velocity anisotropy of the Milky Way's stellar halo","primary_cat":"astro-ph.GA","submitted_at":"2026-04-20T13:52:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A large sample of blue horizontal-branch stars reveals that the Milky Way halo anisotropy increases from the center, stays radially dominated after removing merger debris, and shows older stars on colder, less radial orbits in the inner regions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.13482","ref_index":47,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Substructures of the Milky Way's Retrograde Halo: Evidence for Multiple Accretion Events","primary_cat":"astro-ph.GA","submitted_at":"2026-04-15T05:12:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The Milky Way retrograde halo contains debris from multiple accreted dwarf galaxies, shown by distinct metallicity distribution peaks that remain separate even when combined with orbital dynamics.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"show a clear peak, we gradually expand therapo interval and repeat the inspection of the MDF. SUBSTRUCTURES IN THERETROGRADEHALO5 0.0 0.1 0.2 0.3 0.4 n/N N = 582 Low− e LRS 1 N = 50 Low− e LRS 5 0 ≤ e ≤ 0.3 St ̈ackel −3 −2 −1 [ Fe/ H] 0.00 0.05 0.10 0.15 0.20 0.25 0.30 n/N N = 1170 Low− e LRS 3 N = 161 Low− e LRS 4 N = 190 (143) Low− e LRS 1 N = 52 (47) Low− e LRS 5 McMillan −3 −2 −1 [ Fe/ H] N = 1189 (9 21) Low− e LRS 3 N = 167 (12 9) Low− e LRS 4 0.00 0.05 0.10 0.15 0.20 0.25 0.30 N = 2 931 Intermediate− e LRS 1 N = 1362 Intermediate− e LRS 2 N = 96 Intermediate− e LRS 5 0.3 < e ≤ 0.5 St ̈ackel −3 −2 −1 [ Fe/ H] 0.0 0.1 0.2 0.3 0.4 N = 819 Intermediate− e LRS 3 N = 82 Intermediate− e LRS 4 N = 2425 (1987) Intermediate− e LRS 1"},{"citing_arxiv_id":"2604.05059","ref_index":67,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Implications of low neutron star merger rates for gamma-ray bursts, r-process production and Galactic double neutron stars","primary_cat":"astro-ph.HE","submitted_at":"2026-04-06T18:08:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Lower BNS merger rates from GWTC-4 data produce tensions of factors 3.6-18 with SGRB rates, 0.9-4.1 with r-process rates, and 2.3-5.1 with Galactic DNS rates.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"We estimate the solar-metallicity-equivalent baryonic mass of the MW to be 11.9×10 10 M⊙, about two times larger than previous calculations. The main components of the baryonic mass are the stellar mass, the interstellar medium (ISM), and the circumgalactic medium (CGM). The total stellar mass is 5.4×10 10 M⊙, and the ISM mass is≈20% of the stellar mass (P. J. McMillan 2017). As with previous studies, we assume that all stars and ISM have the samer-process mass fraction as the Sun. The CGM mass in MW analogues is observationally found to be at least 6.5×10 10 M⊙ (J. K. Werk et al. 2014), but at lower than Solar metallicity such that the amount of metals in the CGM is similar to or slightly more than those found in stars and the ISM (M."},{"citing_arxiv_id":"2601.22490","ref_index":33,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"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":48,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"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":"2512.23458","ref_index":78,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Observations of the Fermi bubbles and the Galactic center excess with the DArk Matter Particle Explorer","primary_cat":"astro-ph.HE","submitted_at":"2025-12-29T13:34:23+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DAMPE independently detects the Fermi bubbles at 26 sigma and the Galactic center GeV excess at 7 sigma, with the excess spectrum and morphology matching Fermi-LAT and fitting a 50 GeV dark matter particle annihilating to b quarks.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"To be compatible with the previous works, we set the scale radius of rs = 20 kpc and the inner den- sity slope of γ = 1 .2. The normalization ρ0 is de- termined by ρdm(R0) = 0 .4 GeV cm−3 (R. Catena & P. Ullio 2010) and R0 = 8 .5 kpc ( A. M. Ghez et al. 2008). The J-factor template is shown in Figure 12a. There are indeed updated measure- ments on local DM density (e.g. P. J. McMillan 2017; P. F. de Salas & A. Widmark 2021) and distance to GC ( T. Do et al. 2019; K. Abd El Dayem et al. 2024). If we take the parameters (R0, rs, ρdm(R0)) = (8.28 kpc, 25 kpc, 0.38 GeV cm−3) (P. J. McMillan 2017; K. Abd El Dayem et al. 2024), the J-factor would be decreased by ∼ 22% on average. But the change can be mostly absorbed into the normalization of the GC"},{"citing_arxiv_id":"2512.20594","ref_index":71,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Sensitivity of PUEO to Cosmogenic Neutrinos and Exotic Physics Scenarios","primary_cat":"astro-ph.HE","submitted_at":"2025-12-23T18:42:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"PUEO will constrain the proton fraction of ultrahigh-energy cosmic rays under strong source evolution and set leading neutrino constraints on ultraheavy dark matter decays and some cosmic string models above 10^19 eV.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.00377","ref_index":71,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Redshifted civilizations, galactic empires, and the Fermi paradox","primary_cat":"gr-qc","submitted_at":"2025-10-01T00:50:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Civilizations can achieve galaxy-spanning reach within biological lifetimes via time-dilated orbits near black hole photon spheres using classical general relativity, with a Type II civilization enabling 10^4 dilation factors.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"In the neighborhood of the sun, which is situated at a radius r⊙ =27,000 ly from the galactic center. the density of stellar black holes has been estimated to be [68, 69]. It is perhaps ap- propriate to assume that the density profile of stellar mass black holes is proportional to the stellar disk density, which takes the exponential form [70, 71]: ρd ∝exp(−r/r d),(25) with a scale length ofr d ∼8.5×10 3 ly [71]. This model in- dicates that at a radius ofr∼10,000 ly, the density of black holes increases by a factor of 10 to aboutnBH ∼10 −4 ly−3. This confirms that the stellar mass black hole density is too low to naturally form a closed trajectory in the Milky way. A civilization must therefore move black holes to form a ring that can deflect the trajectory of a vessel into a closed tra-"},{"citing_arxiv_id":"2506.21410","ref_index":84,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"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":"2501.12213","ref_index":39,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Black holes surrounded by dark matter spike: Spacetime metrics and gravitational wave ringdown waveforms","primary_cat":"gr-qc","submitted_at":"2025-01-21T15:30:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Black hole spacetimes in dark matter spikes are solved analytically from TOV equations; ringdown quasinormal frequencies differ from Schwarzschild by up to order 10^{-4}.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2408.02723","ref_index":96,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Cosmological Simulations of Stellar Halos with Gaia Sausage-Enceladus Analogues: Two Sausages, One Bun?","primary_cat":"astro-ph.GA","submitted_at":"2024-08-05T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"TNG50 simulations of 98 Milky Way analogues find GSE-like debris in 32 cases, with two-merger GSEs in one third; single- and two-merger cases differ in median infall time (5.9 vs 10.7 Gyr ago), abundances, and star-formation histories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.00987","ref_index":60,"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},{"citing_arxiv_id":"1906.08264","ref_index":53,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Directly testing gravity with Proxima Centauri","primary_cat":"astro-ph.SR","submitted_at":"2019-06-19T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Proposes that 10 years of 0.5 μas astrometry of Proxima Centauri can distinguish MOND from Newtonian gravity in the low-acceleration regime.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}