{"paper":{"title":"The radio evolution of supernova SN$\\,$2008iz in M$\\,$82","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"A. Brunthaler, C. Henkel, G. C. Bower, H. Falcke, I. Mart\\'i-Vidal, K. M. Menten, K. Sendlinger, N. Kimani, R.J. Beswick, T. W. B. Muxlow","submitted_at":"2016-06-28T14:45:10Z","abstract_excerpt":"We report on multi-frequency Very Large Array (VLA) and Very Long Baseline Interferometry (VLBI) radio observations for a monitoring campaign of supernova SN$\\,$2008iz in the nearby irregular galaxy M$\\,$82. We fit two models to the data, a simple time power-law, S$\\propto$ t$^\\beta$, and a simplified Weiler model, yielding decline indices, $\\beta$ of -1.22$\\pm$0.07 (days 100-1500) and -1.41$\\pm$0.02 (days 76-2167), respectively. The late-time radio light curve evolution shows flux-density flares at $\\sim\\,$970 and $\\sim\\,$1400 days which are a factor of $\\sim\\,$2 and $\\sim\\,$4 higher than the"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1606.08742","kind":"arxiv","version":1},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}