Utilizza questo identificativo per citare o creare un link a questo documento:
http://hdl.handle.net/20.500.12386/27498
Campo DC | Valore | Lingua |
---|---|---|
dc.contributor.author | Chen, T. -W. | en_US |
dc.contributor.author | Inserra, C. | en_US |
dc.contributor.author | Fraser, M. | en_US |
dc.contributor.author | Moriya, T. J. | en_US |
dc.contributor.author | Schady, P. | en_US |
dc.contributor.author | Schweyer, T. | en_US |
dc.contributor.author | Filippenko, A. V. | en_US |
dc.contributor.author | Perley, D. A. | en_US |
dc.contributor.author | Ruiter, A. J. | en_US |
dc.contributor.author | Seitenzahl, I. | en_US |
dc.contributor.author | Sollerman, J. | en_US |
dc.contributor.author | Taddia, F. | en_US |
dc.contributor.author | Anderson, J. P. | en_US |
dc.contributor.author | Foley, R. J. | en_US |
dc.contributor.author | Jerkstrand, A. | en_US |
dc.contributor.author | Ngeow, C. -C. | en_US |
dc.contributor.author | Pan, Y. -C. | en_US |
dc.contributor.author | PASTORELLO, Andrea | en_US |
dc.contributor.author | Points, S. | en_US |
dc.contributor.author | Smartt, S. J. | en_US |
dc.contributor.author | Smith, K. W. | en_US |
dc.contributor.author | Taubenberger, S. | en_US |
dc.contributor.author | Wiseman, P. | en_US |
dc.contributor.author | Young, D. R. | en_US |
dc.contributor.author | BENETTI, Stefano | en_US |
dc.contributor.author | Berton, M. | en_US |
dc.contributor.author | BUFANO, FILOMENA | en_US |
dc.contributor.author | Clark, P. | en_US |
dc.contributor.author | DELLA VALLE, Massimo | en_US |
dc.contributor.author | Galbany, L. | en_US |
dc.contributor.author | Gal-Yam, A. | en_US |
dc.contributor.author | Gromadzki, M. | en_US |
dc.contributor.author | Gutiérrez, C. P. | en_US |
dc.contributor.author | Heinze, A. | en_US |
dc.contributor.author | Kankare, E. | en_US |
dc.contributor.author | Kilpatrick, C. D. | en_US |
dc.contributor.author | Kuncarayakti, H. | en_US |
dc.contributor.author | Leloudas, G. | en_US |
dc.contributor.author | Lin, Z. -Y. | en_US |
dc.contributor.author | Maguire, K. | en_US |
dc.contributor.author | Mazzali, P. | en_US |
dc.contributor.author | McBrien, O. | en_US |
dc.contributor.author | Prentice, S. J. | en_US |
dc.contributor.author | Rau, A. | en_US |
dc.contributor.author | Rest, A. | en_US |
dc.contributor.author | Siebert, M. R. | en_US |
dc.contributor.author | Stalder, B. | en_US |
dc.contributor.author | Tonry, J. L. | en_US |
dc.contributor.author | Yu, P. -C. | en_US |
dc.date.accessioned | 2020-09-28T15:24:58Z | - |
dc.date.available | 2020-09-28T15:24:58Z | - |
dc.date.issued | 2018 | en_US |
dc.identifier.issn | 2041-8205 | en_US |
dc.identifier.uri | http://hdl.handle.net/20.500.12386/27498 | - |
dc.description.abstract | We present observations of supernova (SN) 2017ens, discovered by the ATLAS survey and identified as a hot blue object through the GREAT program. The redshift z = 0.1086 implies a peak brightness of M <SUB> g </SUB> = -21.1 mag, placing the object within the regime of superluminous supernovae. We observe a dramatic spectral evolution, from initially being blue and featureless, to later developing features similar to those of the broadlined Type Ic SN 1998bw, and finally showing ∼2000 km s<SUP>-1</SUP> wide Hα and Hβ emission. Relatively narrow Balmer emission (reminiscent of a SN IIn) is present at all times. We also detect coronal lines, indicative of a dense circumstellar medium. We constrain the progenitor wind velocity to ∼50-60 km s<SUP>-1</SUP> based on P-Cygni profiles, which is far slower than those present in Wolf-Rayet stars. This may suggest that the progenitor passed through a luminous blue variable phase, or that the wind is instead from a binary companion red supergiant star. At late times we see the ∼2000 km s<SUP>-1</SUP> wide Hα emission persisting at high luminosity (∼3 × 10<SUP>40</SUP> erg s<SUP>-1</SUP>) for at least 100 day, perhaps indicative of additional mass loss at high velocities that could have been ejected by a pulsational pair instability. | en_US |
dc.language.iso | eng | en_US |
dc.title | SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IIn | en_US |
dc.type | Article | - |
dc.identifier.doi | 10.3847/2041-8213/aaeb2e | en_US |
dc.identifier.scopus | 2-s2.0-85056739355 | en_US |
dc.identifier.isi | 000450221300001 | en_US |
dc.identifier.url | https://iopscience.iop.org/article/10.3847/2041-8213/aaeb2e | en_US |
dc.relation.medium | STAMPA | en_US |
dc.relation.volume | 867 | en_US |
dc.relation.issue | 2 | en_US |
dc.relation.firstpage | L31 | en_US |
dc.type.referee | REF_1 | en_US |
dc.description.numberofauthors | 49 | en_US |
dc.description.international | sì | en_US |
dc.relation.scientificsector | FIS/05 - ASTRONOMIA E ASTROFISICA | en_US |
dc.relation.journal | THE ASTROPHYSICAL JOURNAL LETTERS | en_US |
dc.type.miur | 262 Articolo in rivista | - |
dc.identifier.adsbibcode | 2018ApJ...867L..31C | 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.fulltext | With Fulltext | - |
item.cerifentitytype | Publications | - |
item.grantfulltext | open | - |
crisitem.journal.journalissn | 2041-8205 | - |
crisitem.journal.ance | E196528 | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Padova | - |
crisitem.author.dept | O.A. Catania | - |
crisitem.author.dept | O.A. Capodimonte | - |
crisitem.author.orcid | 0000-0002-7259-4624 | - |
crisitem.author.orcid | 0000-0002-3256-0016 | - |
crisitem.author.orcid | 0000-0002-3429-2481 | - |
crisitem.author.orcid | 0000-0003-3142-5020 | - |
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