Please use this identifier to cite or link to this item:
http://hdl.handle.net/20.500.12386/34380
DC Field | Value | Language |
---|---|---|
dc.contributor.author | Fiore, A. | en_US |
dc.contributor.author | Chen, T. -W. | en_US |
dc.contributor.author | Jerkstrand, A. | en_US |
dc.contributor.author | BENETTI, Stefano | en_US |
dc.contributor.author | CIOLFI, RICCARDO | en_US |
dc.contributor.author | Inserra, C. | en_US |
dc.contributor.author | CAPPELLARO, Enrico | en_US |
dc.contributor.author | PASTORELLO, Andrea | en_US |
dc.contributor.author | Leloudas, G. | en_US |
dc.contributor.author | Schulze, S. | en_US |
dc.contributor.author | Berton, M. | en_US |
dc.contributor.author | Burke, J. | en_US |
dc.contributor.author | McCully, C. | en_US |
dc.contributor.author | Fong, W. | en_US |
dc.contributor.author | Galbany, L. | en_US |
dc.contributor.author | Gromadzki, M. | en_US |
dc.contributor.author | Gutiérrez, C. P. | en_US |
dc.contributor.author | Hiramatsu, D. | en_US |
dc.contributor.author | Hosseinzadeh, G. | en_US |
dc.contributor.author | Howell, D. A. | en_US |
dc.contributor.author | Kankare, E. | en_US |
dc.contributor.author | Lunnan, R. | en_US |
dc.contributor.author | Müller-Bravo, T. E. | en_US |
dc.contributor.author | O'Neill, D. | en_US |
dc.contributor.author | Nicholl, M. | en_US |
dc.contributor.author | Rau, A. | en_US |
dc.contributor.author | Sollerman, J. | en_US |
dc.contributor.author | Terreran, G. | en_US |
dc.contributor.author | Valenti, S. | en_US |
dc.contributor.author | Young, D. R. | en_US |
dc.date.accessioned | 2023-09-13T12:01:59Z | - |
dc.date.available | 2023-09-13T12:01:59Z | - |
dc.date.issued | 2021 | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/34380 | - |
dc.description.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 M<SUB>g</SUB> = -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 B<SUB>p</SUB> ≃ 6 × 10<SUP>14</SUP> G, an initial period of the magnetar P<SUB>initial</SUB> ≃ 2.8 ms, an ejecta mass $M_{\rm ejecta}\simeq 9\, \mathrm{M}_\odot $ and an ejecta opacity $\kappa \simeq 0.08\, \mathrm{cm}^{2}\, \rm{g}^{-1}$. A CSM-interaction scenario would imply a CSM mass $\simeq 5\, \mathrm{M}_\odot $ and an ejecta mass $\simeq 12\, \mathrm{M}_\odot $. Finally, the nebular spectrum of phase + 187 d was modeled, deriving a mass of $\sim 10\, {\rm M}_\odot$ 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 ($40\, {\rm M}_\odot$) star. | en_US |
dc.language.iso | eng | en_US |
dc.title | SN 2017gci: a nearby Type I Superluminous Supernova with a bumpy tail | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.1093/mnras/staa4035 | en_US |
dc.identifier.scopus | 2-s2.0-85115843692 | en_US |
dc.identifier.url | https://academic.oup.com/mnras/article/502/2/2120/6064317 | en_US |
dc.identifier.url | http://arxiv.org/abs/2012.12755v1 | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 502 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | 2120 | en_US |
dc.relation.lastpage | 2139 | en_US |
dc.type.referee | REF_1 | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2021MNRAS.502.2120F | en_US |
dc.description.apc | no | en_US |
dc.description.oa | 1 – prodotto con file in versione Open Access (allegare il file al passo 5-Carica) | en_US |
item.openairecristype | http://purl.org/coar/resource_type/c_18cf | - |
item.openairetype | Article | - |
item.languageiso639-1 | en | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
item.fulltext | With Fulltext | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.orcid | 0000-0002-3256-0016 | - |
crisitem.author.orcid | 0000-0003-3140-8933 | - |
crisitem.author.orcid | 0000-0001-5008-8619 | - |
crisitem.author.orcid | 0000-0002-7259-4624 | - |
crisitem.journal.journalissn | 0035-8711 | - |
crisitem.journal.ance | E112946 | - |
Appears in Collections: | 1.01 Articoli in rivista |
Files in This Item:
File | Description | Size | Format | |
---|---|---|---|---|
118-F+.pdf | PDF editoriale | 2.84 MB | Adobe PDF | View/Open |
Page view(s)
4
checked on May 9, 2024
Download(s)
1
checked on May 9, 2024
Google ScholarTM
Check
Altmetric
Altmetric
Items in DSpace are published in Open Access, unless otherwise indicated.