{"paper":{"title":"ALMA spectral survey of Supernova 1987A --- molecular inventory, chemistry, dynamics and explosive nucleosynthesis","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"astro-ph.SR","authors_text":"(10) Stockholm University, (11) European Southern Observatory (ESO), (12) The University of Western Australia, 13), (13) ARC Centre of Excellence for All-Sky Astrophysics (CAASTRO), (14) University of Oxford, (15) Oskar Klein Centre, (16) Keele University, (17) University of Texas, (18) Universiteit Gent, (19) NASA Goddard Space Flight Center, 2), (20) Space Telescope Science Institute, 21), (21) Johns Hopkins University, (22) University of Hong Kong, (2) University College London, (3) University of Virginia, 4), (4) National Radio Astronomy Observatory, (5) University of California, (6) Observatorio Astronomico Nacional (OAN-IGN), (7) Universidad de Valencia, (8) University of California, (9) Westminster College, AlbaNova, Austin, Australia, Belgium, Berkeley, C. Fransson (10), China), C.-Y. Ng (22), E. Dwek (19), F.J. Abellan (7), Garching, Germany, G. Sonneborn (19), G. Zanardo (12), H.L. Gomez (1), Hong Kong, I De Looze (2), J.C. Wheeler (17), J. Kamenetzky (9), J. Larsson (15), J. M. Marcaide (7), J. Spyromilio (11), J.Th. van Loon (16), J. Yates (2) ((1) Cardiff University, L. Staveley-Smith (12, M. Baes (18), M. J. Barlow (2), M. Matsuura (1, M. Meixner (20, P. Cigan (1), P. Lundqvist (10), P. Roche (14), R. Chevalier (3), R. Indebetouw (3, R. McCray (8), Salt Lake City, Santa Cruz, Spain, S. Viti (2), Sweden, S. Woosley (5), UK, USA, V. Bujarrabal (6)","submitted_at":"2017-04-07T18:00:02Z","abstract_excerpt":"We report the first molecular line survey of Supernova 1987A in the millimetre wavelength range. In the ALMA 210--300 and 340--360 GHz spectra, we detected cold (20--170 K) CO, 28SiO, HCO+ and SO, with weaker lines of 29SiO from ejecta. This is the first identification of HCO+ and SO in a young supernova remnant. We find a dip in the J=6--5 and 5--4 SiO line profiles, suggesting that the ejecta morphology is likely elongated. The difference of the CO and SiO line profiles is consistent with hydrodynamic simulations, which show that Rayleigh-Taylor instabilities cause mixing of gas, with heavie"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1704.02324","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"}