High-resolution spectroscopy of SN 2017hcc and its blueshifted line profiles from post-shock dust formation
AffiliationSteward Observatory, University of Arizona
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PublisherOxford University Press
CitationSmith, N., & Andrews, J. E. (2020). High-resolution spectroscopy of SN 2017hcc and its blueshifted line profiles from post-shock dust formation. Monthly Notices of the Royal Astronomical Society, 499(3), 3544-3562.
Rights©2020 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
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AbstractSN 2017hcc was remarkable for being a nearby and strongly polarized superluminous Type IIn supernova (SN). We obtained high-resolution Echelle spectra that we combine with other spectra to investigate its line-profile evolution. All epochs reveal narrow P Cygni components from pre-shock circumstellar material (CSM), indicating an axisymmetric outflow from the progenitor of 40-50 km s−1. Broad and intermediate-width components exhibit the classic evolution seen in luminous SNe IIn: symmetric Lorentzian profiles from pre-shock CSM lines broadened by electron scattering at early times, transitioning at late times to multicomponent, irregular profiles coming from the SN ejecta and post-shock shell. As in many SNe IIn, profiles show a progressively increasing blueshift, with a clear flux deficit in red wings of the intermediate and broad velocity components after day 200. This blueshift develops after the continuum luminosity fades, and in the intermediate-width component, persists at late times even after the SN ejecta fade. In SN 2017hcc, the blueshift cannot be explained as occultation by the SN photosphere, pre-shock acceleration of CSM, or a lopsided explosion of CSM. Instead, the blueshift arises from dust formation in the post-shock shell and in the SN ejecta. The effect has a wavelength dependence characteristic of dust, exhibiting an extinction law consistent with large grains. Thus, SN 2017hcc experienced post-shock dust formation and had a mildly bipolar CSM shell, similar to SN 2010jl. Like other superluminous SNe IIn, the progenitor lost around 10 M☉ due to extreme eruptive mass-loss in the decade before exploding. © 2020 The Author(s)
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SponsorsNational Science Foundation