Journal
NATURE PHYSICS
Volume 13, Issue 5, Pages 510-517Publisher
NATURE PUBLISHING GROUP
DOI: 10.1038/NPHYS4025
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Funding
- EU/FP7 via an ERC grant
- Quantum Universe I-Core programme by the Israeli Committee for planning and budgeting
- ISF
- Minerva
- Weizmann-UK 'making connections' programme
- Kimmel
- ARCHES
- Yes award
- Hubble Fellowship - Space Telescope Science Institute [HST-HF-51296.01-A]
- European Union (EU) [H2020-MSCA-IF-2014-660113]
- AMBIZIONE grant of the Swiss NSF
- Arye Dissentshik career development chair
- Israel Science Foundation
- Weizmann-UK
- I-Core programme
- National Science Foundation for the GROWTH project [1545949]
- Christopher R. Redlich Fund
- TABASGO Foundation
- US NSF [AST-1211916]
- NASA through the Einstein Fellowship Program [PF6-170148]
- US Department of Energy as part of the Laboratory Directed Research and Development programme
- Swedish Research Council
- Knut and Alice Wallenberg Foundation
- National Aeronautics and Space Administration (NASA) [NNX09AH71G, NNX09AT02G, NNX10AI27G, NNX12AE66G]
- CONACyT [INFR-2009-01-122785, CB-2008-101958]
- UNAM PAPIIT [IN113810, IG100414]
- UCMEXUS-CONACyT
- W. M. Keck Foundation
- NASA
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With the advent of new wide-field, high-cadence optical transient surveys, our understanding of the diversity of core-collapse supernovae has grown tremendously in the last decade. However, the pre-supernova evolution of massive stars, which sets the physical backdrop to these violent events, is theoretically not well understood and difficult to probe observationally. Here we report the discovery of the supernova iPTF 13dqy = SN 2013fs a mere similar to 3 h after explosion. Our rapid follow-up observations, which include multiwavelength photometry and extremely early (beginning at similar to 6 h post-explosion) spectra, map the distribution of material in the immediate environment (less than or similar to 1015 cm) of the exploding star and establish that it was surrounded by circumstellar material (CSM) that was ejected during the final similar to 1 yr prior to explosion at a high rate, around 10(-3) solar masses per year. The complete disappearance of flash-ionized emission lines within the first several days requires that the dense CSM be confined to within less than or similar to 10(15) cm, consistent with radio non-detections at 70-100 days. The observations indicate that iPTF 13dqy was a regular type II supernova; thus, the finding that the probable red supergiant progenitor of this common explosion ejected material at a highly elevated rate just prior to its demise suggests that pre-supernova instabilities may be common among exploding massive stars.
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