{"total":12,"items":[{"citing_arxiv_id":"2606.30757","ref_index":222,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Unveil the nature of JWST-AGN and Little Red Dots with SKAO continuum surveys","primary_cat":"astro-ph.GA","submitted_at":"2026-06-29T18:00:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"SKAO continuum surveys will detect radio emission from JWST AGN and LRDs and distinguish between Compton-thick absorption, intrinsically weak accretion, and dense gas cocoon scenarios.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.30746","ref_index":14,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2606.25359","ref_index":32,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2606.23014","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"When bars and spirals conspire: recurrent build-up of the nuclear regions of disc galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-22T08:24:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"N-body+hydro simulation of an isolated Milky Way-like galaxy shows bar-spiral reconnections produce episodic star formation bursts in nuclear stellar discs and clusters after the initial bar-driven burst.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19463","ref_index":77,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On the later evolution of observationally selected protocluster candidates at $z\\,{\\gtrsim}\\,5$","primary_cat":"astro-ph.GA","submitted_at":"2026-06-17T18:01:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations show observationally selected protocluster candidates at z ≳ 5 include significant interlopers, undergo 2-6 major mergers, and exhibit stronger clustering than observed, requiring total galaxy mass within 10 cMpc for reliable progenitor identification.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10020","ref_index":104,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Manticore Project II: Bayesian digital twins of cosmic structure across the SDSS and BOSS volumes","primary_cat":"astro-ph.CO","submitted_at":"2026-06-08T18:07:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Manticore-Deep uses tiled Bayesian field-level inference on SDSS and BOSS data to produce posterior ensembles of 3D cosmic fields that are consistent with LCDM and validated by 7.4σ CMB lensing and 3.5σ kSZ detections.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05151","ref_index":233,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Mapping the star formation peak with LIGO A# and Next-Generation detectors","primary_cat":"gr-qc","submitted_at":"2026-06-03T17:53:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations show LIGO-A# constrains the peak redshift of binary black hole merger rate (tracing star formation) to ±0.1 in one year, improving to ±0.02 with next-generation detectors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.03753","ref_index":133,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The impact of source and survey modelling on the connection between [O III] emitters and Ly $\\alpha$ forest transmission at z ~ 6","primary_cat":"astro-ph.CO","submitted_at":"2026-06-02T15:03:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Empirical halo-to-[O III] emitter modeling with realistic JWST survey mocks produces cross-correlations consistent with z~6 data within large scatter, but with a ~10 cMpc offset in the 1D peak.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02725","ref_index":111,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Can current models predict the local black hole merger rate?","primary_cat":"astro-ph.HE","submitted_at":"2026-06-01T18:00:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Theoretical predictions for local BBH merger rates exceed observations by a factor >10 under conservative SFRD and metallicity assumptions, indicating need for revisions in stellar evolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16501","ref_index":20,"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":"2605.15893","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing the faint end of simulated galaxy counts at z>3","primary_cat":"astro-ph.CO","submitted_at":"2026-05-15T12:22:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"TNG100 and EAGLE hydrodynamical simulations underproduce faint compact galaxies at z>3 relative to CANDELS observations even after forward modeling and completeness corrections, with the mismatch linked to both detection effects and simulation physics.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"for both TNG100 (×0.98 on average) and EAGLE (×0.99 on av- erage), across all four redshifts. At higher redshifts (z=3,4), the agreement between the full snapshot and the FORECAST mass densities is particularly strong, with minimal scatter between re- alizations. Atz=1 andz=2, while the average mass densities re- 1 2 3 4 redshift 107 108 Mass density [M Mpc 3] IU TNG100 IU EAGLE full box TNG100 full box EAGLE S22 W23 Fig. A.1: Stellar mass density comparison across redshifts for TNG100 and EAGLE simulations (considering only virialized objects, i.e. subhalos). Full snapshot values are shown as golden dots (TNG100) and green dots (EAGLE). Average mass den- sities from N=200 FORECAST realizations are represented by"},{"citing_arxiv_id":"2605.08353","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"(15) and (10), the observed GSMF,ϕ obs, takes the form of a double convolution (see e.g., Behroozi et al. 2013a; Rodríguez-Puebla et al. 2017): ϕ∗,obs(M∗) = Z Z Perror(x−logM ∗)× Hgal-halo(y−x)ϕ ∗,intr(y)dydx. (16) UndertheassumptionthatbothP error andH gal-halofollowGaussian distributions, this simplifies to ϕ∗,obs(M∗) = Z G(x−logM ∗)ϕ∗,intr(x)dx,(17) whereGrepresentstheconvolutionofP error andH gal-halo,i.e.P error ◦ Hgal-halo. As recently discussed in Rodríguez-Puebla et al. (2025), the 1-σ distribution of stellar mass uncertainties reported in various studies tends to increase with redshift. Figure 1 presents different models for random errors as a function of redshift, as reported by Behroozi"}],"limit":50,"offset":0}