{"total":10,"items":[{"citing_arxiv_id":"2607.00206","ref_index":86,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The evolution of high-z proto-star clusters into local globular clusters","primary_cat":"astro-ph.GA","submitted_at":"2026-06-30T21:37:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"N-body simulations show high-z proto-star clusters with multiple populations can survive strong early tidal fields and evolve into systems with properties matching Galactic globular clusters after 12 Gyr.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.30746","ref_index":87,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Introducing AuriGLOBES: the effect of compressive tides, compact object-induced mass loss, and size evolution on modelling globular clusters","primary_cat":"astro-ph.GA","submitted_at":"2026-06-29T18:00:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"AuriGLOBES is a new subgrid model implemented in Auriga simulations that incorporates compressive tides and compact-object mass loss to transform an initial Schechter mass function into observed globular cluster populations while reproducing the GC system mass-halo mass relation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.27426","ref_index":231,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Too shy to spin? Cosmic wallflowers as proto-globular clusters","primary_cat":"astro-ph.GA","submitted_at":"2026-06-25T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Simulation study proposes that weakly rotating, gas-rich cosmic wallflowers at high redshift are natural proto-globular cluster candidates based on kinematics and densities.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25969","ref_index":154,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"HI Simulations for Cosmology with the SKA Observatory","primary_cat":"astro-ph.CO","submitted_at":"2026-06-24T15:39:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Overview of HI modeling methods finds consistency in cosmic HI density but systematic differences in HI-halo mass relation shape and redshift evolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25359","ref_index":145,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Cosmological Galaxy Formation Modelling in the Era of the Square Kilometre Array","primary_cat":"astro-ph.GA","submitted_at":"2026-06-24T03:44:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":1.0,"formal_verification":"none","one_line_summary":"Review of state-of-the-art cosmological galaxy formation models for HI, molecular gas and radio continuum in preparation for SKA, advocating coordinated multi-scale simulations, forward modelling and AI emulators.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25025","ref_index":228,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Investigating black hole accretion and feedback self-regulation in Seyfert galaxies using the FIRE-3 cosmological hydrodynamic simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-06-23T18:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"FIRE-3 cosmological simulations of Seyfert galaxies produce episodic AGN feedback and gas clearing but no clear anti-correlation between nuclear gas concentration and AGN luminosity, highlighting timing mismatches with observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18419","ref_index":59,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Contribution of Disrupted Dense Star Clusters to Gaia's Compact Object Binaries","primary_cat":"astro-ph.GA","submitted_at":"2026-06-16T19:13:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Disrupted dense star clusters release ~300,000 white dwarf, 150,000 black hole, and 1,000 neutron star binaries into the Milky Way, but Gaia DR3/DR4 detect only a handful of white dwarf systems with none for the others.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20322","ref_index":30,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":"2604.02993","ref_index":46,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Tracing the relic nature of compact galaxies through their globular cluster systems","primary_cat":"astro-ph.GA","submitted_at":"2026-04-03T12:13:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Globular cluster mass fractions, in-situ fractions, metallicity spreads, and spatial profiles in simulated compact galaxies can identify massive relic analogs with early assembly histories.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2507.07183","ref_index":42,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Mass Distribution of Binary Black Hole Mergers from Young and Old Dense Star Clusters","primary_cat":"astro-ph.HE","submitted_at":"2025-07-09T18:00:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"N-body models of young and old dense star clusters show BBH mergers span primary masses from ~6 to >100 solar masses with a peak near 8 solar masses, reproducing the LIGO-inferred distribution, with low-mass mergers mostly from metal-rich clusters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}