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- W2886616908 abstract "Hydrogen-poor superluminous supernovae (SLSN-I) are a class of rare and energetic explosions discovered in untargeted transient surveys in the past decade. The progenitor stars and the physical mechanism behind their large radiated energies ($sim10^{51}$ erg) are both debated, with one class of models primarily requiring a large rotational energy, while the other requires very massive progenitors to either convert kinetic energy into radiation via interaction with circumstellar material (CSM), or engender a pair-instability explosion. Observing the structure of the CSM around SLSN-I offers a powerful test of some scenarios, though direct observations are scarce. Here, we present a series of spectroscopic observations of the SLSN-I iPTF16eh, which reveal both absorption and time- and frequency-variable emission in the Mg II resonance doublet. We show that these observations are naturally explained as a resonance scattering light echo from a circumstellar shell. Modeling the evolution of the emission, we find a shell radius of 0.1 pc and velocity of 3300 km s$^{-1}$, implying the shell was ejected three decades prior to the supernova explosion. These properties match theoretical predictions of pulsational pair-instability shell ejections, and imply the progenitor had a He core mass of $sim 50-55~{rm M}_{odot}$, corresponding to an initial mass of $sim 115~{rm M}_{odot}$." @default.
- W2886616908 created "2018-08-22" @default.
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- W2886616908 date "2018-09-10" @default.
- W2886616908 modified "2023-09-30" @default.
- W2886616908 title "A UV resonance line echo from a shell around a hydrogen-poor superluminous supernova" @default.
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- W2886616908 doi "https://doi.org/10.1038/s41550-018-0568-z" @default.
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