Updated Photometry of the Yellow Supergiant Progenitor and Late-time Observations of the Type IIb Supernova SN 2016gkg

Abstract We present Hubble Space Telescope (HST) observations of the Type IIb supernova (SN) SN 2016gkg at 652, 1698, and 1795 days from explosion with the Advanced Camera for Surveys (ACS) and Wide Field Camera 3 (WFC3). Comparing to pre-explosion imaging from 2001 obtained with the Wide Field Plan...

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Bibliographic Details
Published inThe Astrophysical journal Vol. 936; no. 2; pp. 111 - 118
Main Authors Kilpatrick, Charles D., Coulter, David A., Foley, Ryan J., Piro, Anthony L., Rest, Armin, Rojas-Bravo, César, Siebert, Matthew R.
Format Journal Article
LanguageEnglish
Published Philadelphia The American Astronomical Society 01.09.2022
IOP Publishing
Subjects
Astrophysics
Binary stars
Cameras
Companion stars
Core-collapse supernovae
Decay rate
Emissions
Evolution
Field cameras
Hubble Space Telescope
Light curve
Radioisotopes
Space telescopes
Spectral energy distribution
Spectroscopy
Stellar envelopes
Stellar evolution
Supernova
Wide field planetary camera
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Summary:Abstract We present Hubble Space Telescope (HST) observations of the Type IIb supernova (SN) SN 2016gkg at 652, 1698, and 1795 days from explosion with the Advanced Camera for Surveys (ACS) and Wide Field Camera 3 (WFC3). Comparing to pre-explosion imaging from 2001 obtained with the Wide Field Planetary Camera 2, we demonstrate that SN 2016gkg is now fainter than its candidate counterpart in the latest WFC3 imaging, implying that the counterpart has disappeared and confirming that it was the SN progenitor star. We show the latest light curve and Keck spectroscopy of SN 2016gkg, which imply that SN 2016gkg is declining more slowly than the expected rate for 56 Co decay during its nebular phase. We find that this emission is too luminous to be powered by other radioisotopes and infer that SN 2016gkg is entering a new phase in its evolution where it is powered primarily by interaction with circumstellar matter. Finally, we reanalyze the progenitor star spectral energy distribution and late-time limits in the context of binary evolution models. Including emission from a potential companion star, we find that all such predicted companion stars would be fainter than our limiting magnitudes.
Bibliography:High-Energy Phenomena and Fundamental Physics
AAS36428
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/ac8a4c