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http://hdl.handle.net/20.500.12386/31848
Title: | SN 2017ivv: two years of evolution of a transitional Type II supernova | Authors: | Gutiérrez, C. P. Pastorello, A. Jerkstrand, A. Galbany, L. Sullivan, M. Anderson, J. P. Taubenberger, S. Kuncarayakti, H. González-Gaitán, S. Wiseman, P. Inserra, C. Fraser, M. Maguire, K. Smartt, S. Müller-Bravo, T. E. Arcavi, I. Benetti, S. Bersier, D. Bose, S. Bostroem, K. A. Burke, J. Chen, P. Chen, T. -W. DELLA VALLE, Massimo Dong, Subo Gal-Yam, A. Gromadzki, M. Hiramatsu, D. Holoien, T. W. -S. Hosseinzadeh, G. Howell, D. A. Kankare, E. Kochanek, C. S. McCully, C. Nicholl, M. Pignata, G. Prieto, J. L. Shappee, B. Taggart, K. TOMASELLA, Lina Valenti, S. Young, D. R. |
Issue Date: | 2020 | Journal: | MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | Number: | 499 | Issue: | 1 | First Page: | 974 | Abstract: | We present the photometric and spectroscopic evolution of the Type II supernova (SN II) SN 2017ivv (also known as ASASSN-17qp). Located in an extremely faint galaxy (M<SUB>r</SUB> = -10.3 mag), SN 2017ivv shows an unprecedented evolution during the 2 yr of observations. At early times, the light curve shows a fast rise (˜6-8 d) to a peak of ${\it M}^{\rm max}_{g}= -17.84$ mag, followed by a very rapid decline of 7.94 ± 0.48 mag per 100 d in the V band. The extensive photometric coverage at late phases shows that the radioactive tail has two slopes, one steeper than that expected from the decay of <SUP>56</SUP>Co (between 100 and 350 d), and another slower (after 450 d), probably produced by an additional energy source. From the bolometric light curve, we estimated that the amount of ejected <SUP>56</SUP>Ni is ˜0.059 ± 0.003 M⊙. The nebular spectra of SN 2017ivv show a remarkable transformation that allows the evolution to be split into three phases: (1) Hα strong phase (<200 d); (2) Hα weak phase (between 200 and 350 d); and (3) Hα broad phase (>500 d). We find that the nebular analysis favours a binary progenitor and an asymmetric explosion. Finally, comparing the nebular spectra of SN 2017ivv to models suggests a progenitor with a zero-age main-sequence mass of 15-17 M<SUB>⊙</SUB>. | URI: | http://hdl.handle.net/20.500.12386/31848 | URL: | https://academic.oup.com/mnras/article/499/1/974/5910509 | ISSN: | 0035-8711 | DOI: | 10.1093/mnras/staa2763 | Bibcode ADS: | 2020MNRAS.499..974G | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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staa2763.pdf | Pdf editoriale | 6.52 MB | Adobe PDF | View/Open |
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