Strong late-time circumstellar interaction in the peculiar supernova iPTF14hls
AffiliationUniv Arizona, Steward Observ
supernovae: individual: iPTF14hls
stars: winds outflows
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PublisherOXFORD UNIV PRESS
CitationJennifer E Andrews, Nathan Smith; Strong late-time circumstellar interaction in the peculiar supernova iPTF14hls, Monthly Notices of the Royal Astronomical Society, Volume 477, Issue 1, 11 June 2018, Pages 74–79, https://doi.org/10.1093/mnras/sty584
Rights© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
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AbstractWe present a moderate-resolution spectrum of the peculiar Type II supernova (SN) iPTF14hls taken on day 1153 after discovery. This spectrum reveals the clear signature of shock interaction with dense circumstellar material (CSM). We suggest that this CSM interaction may be an important clue for understanding the extremely unusual photometric and spectroscopic evolution seen over the first 600 d of iPTF14hls. The late-time spectrum shows a double peaked intermediate-width II alpha line indicative of expansion speeds around 1000 km s(-1), with the double-peaked shape hinting at a disc-like geometry in the CSM. If the CSM were highly asymmetric, perhaps in a disc or torus that was ejected from the star 3-6 yr prior to explosion, the CSM interaction could have been overrun and hidden below the SN ejecta photosphere from a wide range of viewing angles. In that case, CSM interaction luminosity would have been thermalized well below the photosphere, potentially sustaining the high luminosity without exhibiting the traditional observational signatures of strong CSM interaction (narrow Ha emission and X-rays). Variations in density structure of the CSM could account for the multiple rebrightenings of the light curve. We propose that a canonical 1 x 10(51) erg explosion energy with enveloped CSM interaction as seen in some recent SNe, rather than an entirely new explosion mechanism, may be adequate to explain the peculiar evolution of iPTE14hls.
VersionFinal published version
SponsorsNSF [AST-131221, AST-151559]; Scialog grant from the Research Corporation for Science Advancement