Progenitor, environment, and modelling of the interacting transient AT 2016jbu (Gaia16cfr)

S. J. Brennan, M. Fraser, J. Johansson, A. Pastorello, R. Kotak, H. F. Stevance, T. W. Chen, J. J. Eldridge, S. Bose, P. J. Brown, E. Callis, R. Cartier, M. Dennefeld, Subo Dong, P. Duffy, N. Elias-Rosa, G. Hosseinzadeh, E. Hsiao, H. Kuncarayakti, A. Martin-CarrilloB. Monard, G. Pignata, D. Sand, B. J. Shappee, S. J. Smartt, B. E. Tucker, L. Wyrzykowski, H. Abbot, S. Benetti, J. Bento, S. Blondin, Ping Chen, A. Delgado, L. Galbany, M. Gromadzki, C. P. Gutierrez, L. Hanlon, D. L. Harrison, D. Hiramatsu, S. T. Hodgkin, T. W.S. Holoien, D. A. Howell, C. Inserra, E. Kankare, S. Kozłowski, T. E. Müller-Bravo, K. Maguire, C. Mccully, P. Meintjes, N. Morrell, M. Nicholl, D. O'neill, P. Pietrukowicz, R. Poleski, J. L. Prieto, A. Rau, D. E. Reichart, T. Schweyer, M. Shahbandeh, J. Skowron, J. Sollerman, I. Soszyński, M. D. Stritzinger, M. Szymański, L. Tartaglia, A. Udalski, K. Ulaczyk, D. R. Young, M. Van Leeuwen, B. Van Soelen

Research output: Contribution to journalArticlepeer-review

13 Scopus citations

Abstract

We present the bolometric light curve, identification and analysis of the progenitor candidate, and preliminary modelling of AT 2016jbu (Gaia16cfr). We find a progenitor consistent with a ∼22-25 M⊙ yellow hypergiant surrounded by a dusty circumstellar shell, in agreement with what has been previously reported. We see evidence for significant photometric variability in the progenitor, as well as strong Hα emission consistent with pre-existing circumstellar material. The age of the environment, as well as the resolved stellar population surrounding AT 2016jbu, supports a progenitor age of >10 Myr, consistent with a progenitor mass of ∼22 M⊙. A joint analysis of the velocity evolution of AT 2016jbu and the photospheric radius inferred from the bolometric light curve shows the transient is consistent with two successive outbursts/explosions. The first outburst ejected material with velocity ∼650 km s-1, while the second, more energetic event ejected material at ∼4500 km s-1. Whether the latter is the core collapse of the progenitor remains uncertain. We place a limit on the ejected 56Ni mass of <0.016 M⊙. Using the Binary Population And Spectral Synthesis (BPASS) code, we explore a wide range of possible progenitor systems and find that the majority of these are in binaries, some of which are undergoing mass transfer or common-envelope evolution immediately prior to explosion. Finally, we use the SuperNova Explosion Code (SNEC) to demonstrate that the low-energy explosions within some of these binary systems, together with sufficient circumstellar material, can reproduce the overall morphology of the light curve of AT 2016jbu.

Original languageEnglish (US)
Pages (from-to)5666-5685
Number of pages20
JournalMonthly Notices of the Royal Astronomical Society
Volume513
Issue number4
DOIs
StatePublished - Jul 1 2022

Keywords

  • stars: Massive
  • supernovae: General
  • supernovae: Individual: AT 2016jbu

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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