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  SN 2017gci: a nearby Type I Superluminous Supernova with a bumpy tail

Fiore, A., Chen, T.-W., Jerkstrand, A., Benetti, S., Ciolfi, R., Inserra, C., et al. (2021). SN 2017gci: a nearby Type I Superluminous Supernova with a bumpy tail. Monthly Notices of the Royal Astronomical Society, 502(2), 2120-2139. doi:10.1093/mnras/staa4035.

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Fiore, A., Author
Chen, T.-W.1, Author           
Jerkstrand, A., Author
Benetti, S., Author
Ciolfi, R., Author
Inserra, C., Author
Cappellaro, E., Author
Pastorello, A., Author
Leloudas, G., Author
Schulze, S., Author
Berton, M., Author
Burke, J., Author
McCully, C., Author
Fong, W., Author
Galbany, L., Author
Gromadzki, M., Author
Guti´errez, C. P., Author
Hiramatsu, D., Author
Hosseinzadeh, G., Author
Howell, D. A., Author
Kankare, E., AuthorLunnan, R., AuthorMuller-Bravo, T. E., AuthorNeill, D. O, AuthorNicholl, M., AuthorRau, A.1, Author           Sollerman, J., AuthorTerreran, G., AuthorValenti, S., AuthorYoung, D. R., Author more..
Affiliations:
1High Energy Astrophysics, MPI for Extraterrestrial Physics, Max Planck Society, ou_159890              

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 Abstract: We present and discuss the optical spectrophotometric observations of the nearby (z = 0.087) Type I superluminous supernova (SLSN I) SN 2017gci, whose peak K-corrected absolute magnitude reaches Mg = −21.5 mag. Its photometric and spectroscopic evolution includes features of both slow- and of fast-evolving SLSN I, thus favoring a continuum distribution between the two SLSN-I subclasses. In particular, similarly to other SLSNe I, the multiband light curves (LCs) of SN 2017gci show two re-brightenings at about 103 and 142 d after the maximum light. Interestingly, this broadly agrees with a broad emission feature emerging around 6520 Å after ∼51 d from the maximum light, which is followed by a sharp knee in the LC. If we interpret this feature as Hα, this could support the fact that the bumps are the signature of late interactions of the ejecta with a (hydrogen-rich) circumstellar material. Then we fitted magnetar- and CSM-interaction-powered synthetic LCs on to the bolometric one of SN 2017gci. In the magnetar case, the fit suggests a polar magnetic field Bp ≃ 6 × 1014 G, an initial period of the magnetar Pinitial ≃ 2.8 ms, an ejecta mass Mejecta≃9M and an ejecta opacity κ≃0.08cm2g−1⁠. A CSM-interaction scenario would imply a CSM mass ≃5M and an ejecta mass ≃12M⁠. Finally, the nebular spectrum of phase + 187 d was modeled, deriving a mass of ∼10M for the ejecta. Our models suggest that either a magnetar or CSM interaction might be the power sources for SN 2017gci and that its progenitor was a massive (⁠40M⁠) star.

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Language(s): eng - English
 Dates: 2021-01-05
 Publication Status: Published online
 Pages: -
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 Rev. Type: Peer
 Identifiers: DOI: 10.1093/mnras/staa4035
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Title: Monthly Notices of the Royal Astronomical Society
  Abbreviation : Mon. Not. Roy. Astron. Soc.
Source Genre: Journal
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Pages: - Volume / Issue: 502 (2) Sequence Number: - Start / End Page: 2120 - 2139 Identifier: ISSN: 0035-8711
ISSN: 1365-8711