{"paper":{"title":"The supernova impostor PSN J09132750+7627410 and its progenitor","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"A. Morales-Garoffolo, A. Pastorello, E. Cappellaro, E. E. O. Ishida, G. Cortini, L. Tartaglia, L. Tomasella, N. Elias-Rosa, P. Ochner, S. Benetti, S. Taubenberger, S. Zaggia, U. M. Noebauer, V. Granata","submitted_at":"2016-04-15T20:00:01Z","abstract_excerpt":"We report the results of our follow-up campaign of the supernova impostor PSN J09132750+7627410, based on optical data covering $\\sim250\\,\\rm{d}$. From the beginning, the transient shows prominent narrow Balmer lines with P-Cygni profiles, with a blue-shifted absorption component becoming more prominent with time. Along the $\\sim3\\,\\rm{months}$ of the spectroscopic monitoring, broad components are never detected in the hydrogen lines, suggesting that these features are produced in slowly expanding material. The transient reaches an absolute magnitude $M_r=-13.60\\pm0.19\\,\\rm{mag}$ at maximum, a"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1604.04628","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"}