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  Signatures of circumstellar interaction in the Type IIL supernova ASASSN-15oz

Bostroem, K. A., Valenti, S., Horesh, A., Morozova, V., Kuin, N. P. M., Wyatt, S., et al. (2019). Signatures of circumstellar interaction in the Type IIL supernova ASASSN-15oz. Monthly Notices of the Royal Astronomical Society, 485(4), 5120-5141. doi:10.1093/mnras/stz570.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0004-70FF-F Version Permalink: http://hdl.handle.net/21.11116/0000-0004-7100-C
Genre: Journal Article

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Bostroem, K. Azalee, Author
Valenti, Stefano, Author
Horesh, Assaf, Author
Morozova, Viktoriya, Author
Kuin, N. Paul M., Author
Wyatt, Samuel, Author
Jerkstrand, Anders1, Author              
Sand, David J., Author
Lundquist, Michael, Author
Smith, Mathew, Author
Sullivan, Mark, Author
Hosseinzadeh, Griffin, Author
Arcavi, Iair, Author
Callis, Emma, Author
Cartier, Régis, Author
Gal-Yam, Avishay, Author
Galbany, Lluís, Author
Gutiérrez, Claudia, Author
Howell, D. Andrew, Author
Inserra, Cosimo, Author
Kankare, Erkki, AuthorLópez, Kristhell Marisol, AuthorMcCully, Curtis, AuthorPignata, Giuliano, AuthorPiro, Anthony L., AuthorRodríguez, Ośmar, AuthorSmartt, Stephen J., AuthorSmith, Kenneth W., AuthorYaron, Ofer, AuthorYoung, David R., Author more..
Affiliations:
1Stellar Astrophysics, MPI for Astrophysics, Max Planck Society, ou_159882              

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 Abstract: Hydrogen-rich, core-collapse supernovae are typically divided into four classes: IIP, IIL, IIn, and IIb. Recent hydrodynamic modelling shows that circumstellar material is required to produce the early light curves of most IIP/IIL supernovae. In this scenario, IIL supernovae experience large amounts of mass-loss before exploding. We test this hypothesis on ASASSN-15oz, a Type IIL supernova. With extensive follow-up in the X-ray, UV, optical, IR, and radio, we present our search for signs of interaction and the mass-loss history indicated by their detection. We find evidence of short-lived intense mass-loss just prior to explosion from light-curve modelling, amounting in 1.5 M<sub>⊙</sub> of material within 1800 R<sub>⊙</sub> of the progenitor. We also detect the supernova in the radio, indicating mass-loss rates of 10<sup>−6</sup> to 10<sup>−7</sup> M<sub>⊙</sub> yr<sup>−1</sup> prior to the extreme mass-loss period. Our failure to detect the supernova in the X-ray and the lack of narrow emission lines in the UV, optical, and NIR do not contradict this picture and place an upper limit on the mass-loss rate outside the extreme period of <10<sup>−4</sup> M<sub>⊙</sub>  yr<sup>−1</sup>. This paper highlights the importance gathering comprehensive data on more Type II supernovae to enable detailed modelling of the progenitor and supernova which can elucidate their mass-loss histories and envelope structures and thus inform stellar evolution models.

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 Dates: 2019-02-26
 Publication Status: Published online
 Pages: -
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 Rev. Method: Peer
 Identifiers: DOI: 10.1093/mnras/stz570
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Title: Monthly Notices of the Royal Astronomical Society
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Source Genre: Journal
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Publ. Info: OXFORD : OXFORD UNIV PRESS
Pages: - Volume / Issue: 485 (4) Sequence Number: - Start / End Page: 5120 - 5141 Identifier: ISSN: 0035-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000021470