{"total":12,"items":[{"citing_arxiv_id":"2606.28299","ref_index":140,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The impact of stellar binaries and star cluster dynamics on pair-instability supernovae","primary_cat":"astro-ph.HE","submitted_at":"2026-06-26T17:46:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Binary interactions and cluster dynamics boost PISN rates by up to 3x versus single stars, enabling constraints on stellar-wind mass loss and galaxy metallicity distributions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23456","ref_index":56,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Stellar winds of O-type stars traced by high ionization fine-structure emission lines with JWST/MIRI","primary_cat":"astro-ph.SR","submitted_at":"2026-06-22T15:06:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"JWST/MIRI detects [Ne V] 14.3 micron emission from O-star winds in 5 of 22 observed stars, enabling wind speed and mass-loss rate estimates even in weak-wind regimes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.13666","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Centrally concentrated star formation in young clusters II: Jet feedback","primary_cat":"astro-ph.GA","submitted_at":"2026-06-11T17:57:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Jet feedback in centrally concentrated clouds reduces star formation efficiency to 12-16% and yields cluster structures more consistent with observations than models without jets.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12536","ref_index":23,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Getting to know the Stellar Clusters in NGC 1569: Bayesian inference of stellar cluster properties in a dwarf starburst galaxy","primary_cat":"astro-ph.GA","submitted_at":"2026-06-10T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian IMF-aware inference on NGC 1569 clusters yields correlations between cluster mass-function truncation mass, galactocentric distance, metallicity, and gas ionization state.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10558","ref_index":34,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Hector Galaxy Survey: Linking the low- and high-mass ends of the initial mass function in star-forming galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-09T08:25:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Simultaneous measurement of low- and high-mass IMF slopes in 214 star-forming galaxies reveals diversity, weak correlation between ends, and links to stellar mass, star formation rate, and metallicity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10022","ref_index":194,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Learning the Universe with PRFM-vol: Introducing a new subgrid model for star formation in cosmological simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-06-08T18:07:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"PRFM-vol is a new subgrid star formation model for cosmological simulations that computes SFR from ambient densities via PRFM theory and a modified effective EOS, producing taller stellar scale heights, slightly higher stellar mass, and morphology changes including Toomre-driven clumps compared to p","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04740","ref_index":121,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"TDEs on FIRE: Illuminating the Cosmic Evolution of Tidal Disruption Rates","primary_cat":"astro-ph.HE","submitted_at":"2026-06-03T11:22:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"FIRE-2 simulations show per-galaxy tidal disruption rates peak near z=2.5 at 4e-4 per year, correlate with SFR and central density, and remain high in satellite galaxies at early times.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00221","ref_index":33,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"It's Not Just Star Formation: A trend of low dark matter densities in the Andromeda dwarf galaxy system","primary_cat":"astro-ph.GA","submitted_at":"2026-05-29T18:00:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Five of seven modeled M31 dwarf spheroidals show anomalously low central DM densities at 150 pc, with star formation heating disfavored as the sole cause.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21593","ref_index":102,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Predicting intermediate-mass black hole formation in star clusters with machine learning","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T18:00:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Machine learning regressors trained on Rapster simulations forecast that globular clusters rarely host black holes above 100 solar masses while a few nuclear star clusters may exceed this threshold.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"presence of a high-mass IMBH formed through repeated mergers is strongly disfavored. Both the NN and RFR models instead suggest that the system is more likely devoid of BHs more massive than100M⊙. Nevertheless, we find non-negligible support at the∼10%level for the presence of a BH with mass> 60M⊙, implying that 47 Tucanae may have hosted merger events within the upper mass gap. A recent study [102] performed semianalytical cluster simulations using thecBHBdcode, and also predicts the formation of a massive BH in 47 Tucanae. 2.ωCentauri The heaviest GC in the Milky Way isωCentauri, with a mass of about3 .9×106M⊙[70]. It was sug- gested thatωCentauri hosts a(4-5)×104M⊙IMBH based on a rise in the core velocity dispersion [25, 103]. However, anisotropic modeling limits the IMBH mass"},{"citing_arxiv_id":"2605.15310","ref_index":36,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Introducing the Lumina project: large-volume radiation-hydrodynamic simulations of the epochs of hydrogen and helium reionization","primary_cat":"astro-ph.CO","submitted_at":"2026-05-14T18:23:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Lumina runs a 500 cMpc radiation-hydrodynamic simulation combining IllustrisTNG galaxy formation with six-bin M1 radiation transport to predict late stellar-driven HI reionization ending around z=4.75 and AGN-driven HeII reionization nearly complete by z=3.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13472","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"First Light And Reionization Epoch Simulations (FLARES) XXI: The UV Indices of Galaxies in the Early Universe","primary_cat":"astro-ph.GA","submitted_at":"2026-05-13T12:59:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations of high-redshift galaxies show the 1719 Å UV index reliably traces stellar metallicity while others are more sensitive to star formation history.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.03568","ref_index":74,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing dense environments around Sgr A* with S-stars dynamics","primary_cat":"astro-ph.GA","submitted_at":"2025-09-03T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Models apsidal precession and dynamical friction from extended matter to extend GRAVITY constraints on boson clouds around Sgr A* and assess impacts on S-star orbits.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}