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http://hdl.handle.net/20.500.12386/27498
Title: | SN 2017ens: The Metamorphosis of a Luminous Broadlined Type Ic Supernova into an SN IIn | Authors: | Chen, T. -W. Inserra, C. Fraser, M. Moriya, T. J. Schady, P. Schweyer, T. Filippenko, A. V. Perley, D. A. Ruiter, A. J. Seitenzahl, I. Sollerman, J. Taddia, F. Anderson, J. P. Foley, R. J. Jerkstrand, A. Ngeow, C. -C. Pan, Y. -C. PASTORELLO, Andrea Points, S. Smartt, S. J. Smith, K. W. Taubenberger, S. Wiseman, P. Young, D. R. BENETTI, Stefano Berton, M. BUFANO, FILOMENA Clark, P. DELLA VALLE, Massimo Galbany, L. Gal-Yam, A. Gromadzki, M. Gutiérrez, C. P. Heinze, A. Kankare, E. Kilpatrick, C. D. Kuncarayakti, H. Leloudas, G. Lin, Z. -Y. Maguire, K. Mazzali, P. McBrien, O. Prentice, S. J. Rau, A. Rest, A. Siebert, M. R. Stalder, B. Tonry, J. L. Yu, P. -C. |
Issue Date: | 2018 | Journal: | THE ASTROPHYSICAL JOURNAL LETTERS | Number: | 867 | Issue: | 2 | First Page: | L31 | 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. | URI: | http://hdl.handle.net/20.500.12386/27498 | URL: | https://iopscience.iop.org/article/10.3847/2041-8213/aaeb2e | ISSN: | 2041-8205 | DOI: | 10.3847/2041-8213/aaeb2e | Bibcode ADS: | 2018ApJ...867L..31C | Fulltext: | open |
Appears in Collections: | 1.01 Articoli in rivista |
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Chen_2018_ApJL_867_L31.pdf | Pdf editoriale | 2.61 MB | Adobe PDF | View/Open |
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