{"total":11,"items":[{"citing_arxiv_id":"2607.08657","ref_index":126,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"VAPOLA -- A multi-year, multi-band polarization survey of AGN and Sgr A* at mm wavelengths with ALMA I. Survey Overview and Science-Ready Archival Products","primary_cat":"astro-ph.GA","submitted_at":"2026-07-09T16:26:32+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"VAPOLA releases multi-epoch multi-band ALMA full-Stokes products and polarimetric fits for AGN and Sgr A* via an automated pipeline and web portal.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.08090","ref_index":63,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Multi-wavelength Constraints on the Transient EP250905a","primary_cat":"astro-ph.HE","submitted_at":"2026-07-09T03:55:45+00:00","verdict":"CONDITIONAL","verdict_confidence":"HIGH","novelty_score":5.0,"formal_verification":"none","one_line_summary":"EP250905a is best explained as a mildly off-axis structured-jet afterglow at z=2.714, possibly weakly magnified by a foreground galaxy at z=0.374.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.07750","ref_index":210,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Multi-Wavelength Signatures of a Giant Cometary Radio Halo in MACSJ0417-1154","primary_cat":"astro-ph.HE","submitted_at":"2026-07-08T11:28:23+00:00","verdict":"CONDITIONAL","verdict_confidence":"HIGH","novelty_score":6.0,"formal_verification":"none","one_line_summary":"MACSJ0417’s giant radio halo shows spectral steepening and radio–X-ray correlation consistent with turbulence from a 6:1 off-axis merger that preserved the cool core; pure hadronic models are energetically excluded.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.05182","ref_index":12,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Spectropolarimetric detection of baryonic mass loading in a transient relativistic jet: application to the black hole X-ray binary Swift J1727.8$-$1613","primary_cat":"astro-ph.HE","submitted_at":"2026-07-06T15:00:04+00:00","verdict":"CONDITIONAL","verdict_confidence":"UNKNOWN","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Transient Faraday-complex spectropolarimetric structure detected during radio flaring of Swift J1727 implies internal Faraday rotation from electron-proton jet plasma with rotating mass ~10^21 g, a small fraction of accreted mass.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"early polarised flux density and polarisation angle at the reference wavelength squared are then estimated from the complex peak of the Faraday spectrum (with a different bias correction; Hales et al. 2012), |𝑃0|2 =|𝐹(πœ™ 𝑓 ,peak)| 2 βˆ’2.3𝜎 2 𝑓 ,where𝜎 π‘„π‘ˆ ∼𝜎 𝑓 ,(10) πœ“(πœ† 2 0)= 1 2 arctan Im \u0002 𝐹(πœ™ 𝑓 ,peak) \u0003 Re \u0002 𝐹(πœ™ 𝑓 ,peak) \u0003 ! .(11) The corresponding intrinsic polarisation angle is then πœ“0 =πœ“(πœ† 2 0) βˆ’πœ™ 𝑓 ,peakπœ†2 0.(12) For the convention adopted here,πœ†2 0 =0, this reduces directly to πœ“0 =πœ“(πœ† 2 0). This simple interpretation becomes less direct when components areonlymarginallyseparatedorunresolvedinFaradaydepth,orwhen the emission is intrinsically extended in Faraday space. A canonical example is the Burn slab model, in which synchrotron-emitting and Faraday-rotating material are mixed within a homogeneous plasma,"},{"citing_arxiv_id":"2607.02342","ref_index":55,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The VLA-COSMOS 3 GHz Large Project: Polarised source counts and catalogue","primary_cat":"astro-ph.GA","submitted_at":"2026-07-02T15:48:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Deep 3 GHz polarised source counts detect 65 sources (51 deg^{-2}), consistent with 1.4 GHz literature due to spectral index and depolarisation, with a 2Οƒ upper limit of <2.0 deg^{-2} on polarised SFG density.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26072","ref_index":23,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Observations of the Cosmic Dawn and Epoch of Reionization with the SKAO: Observational Lessons Learned from Precursors and Pathfinder Instruments","primary_cat":"astro-ph.IM","submitted_at":"2026-06-24T17:47:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Summarizes observational lessons on simulation pipelines and systematic mitigation from SKAO precursors for Cosmic Dawn and EoR studies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25631","ref_index":25,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Non-Negativity Iterative Approach to Image Deconvolution for SKA","primary_cat":"astro-ph.IM","submitted_at":"2026-06-24T09:37:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Presents a non-negativity constrained iterative deconvolution method for SKA radio images that is fast and performs well on simulated point and extended sources in noise-free conditions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18333","ref_index":89,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Polarisation and Faraday rotation measure imaging at metre wavelengths with sub-arcsecond resolution: a foundational calibration strategy","primary_cat":"astro-ph.IM","submitted_at":"2026-06-16T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A calibration strategy using full-Jones corrections with an in-field unpolarised calibrator and visibility-based multi-epoch alignment enables sub-arcsecond polarimetric imaging with LOFAR at metre wavelengths.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.13493","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The ultra low-frequency spectral properties of bright extended radio galaxies in the 3CRR catalogue","primary_cat":"astro-ph.GA","submitted_at":"2026-06-11T15:42:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Presents ultra-low frequency spectral index maps for 22 bright extended radio galaxies showing indices of ~0.5 near cores rising to >1.0 in lobes for FR I sources and 0.5-0.9 in FR II hotspots.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06213","ref_index":139,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing a new subclass of llGRB-SN transients: Insights from EP250304a and its associated supernova","primary_cat":"astro-ph.HE","submitted_at":"2026-06-04T14:23:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"EP250304a/SN 2025fhm is presented as a member of an emerging subclass of shocked cocoon-dominated low-luminosity GRB-SNe based on spectral, photometric, and light-curve modeling comparisons to prior events.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19658","ref_index":114,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The PARADIGM Project II: Characterising Nuclear and Diffuse Radio Components in Local U/LIRGs","primary_cat":"astro-ph.GA","submitted_at":"2026-05-19T10:51:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Multi-scale radio observations of 15 local U/LIRGs decompose emission to show nuclear components contribute ~50% on average while diffuse SF-related emission dominates ~80% of total power, with radio excess linked to AGN rather than boosted star formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}